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+% %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% %
+%                                                                         %
+% The Project Gutenberg EBook of Publications of the Astronomical Society of
+% the Pacific, by Various                                                 %
+%                                                                         %
+% This eBook is for the use of anyone anywhere at no cost and with        %
+% almost no restrictions whatsoever.  You may copy it, give it away or    %
+% re-use it under the terms of the Project Gutenberg License included     %
+% with this eBook or online at www.gutenberg.org                          %
+%                                                                         %
+%                                                                         %
+% Title: Publications of the Astronomical Society of the Pacific          %
+%        Volume 1                                                         %
+%                                                                         %
+% Author: Various                                                         %
+%                                                                         %
+% Release Date: July 29, 2008 [EBook #26147]                              %
+%                                                                         %
+% Language: English                                                       %
+%                                                                         %
+% Character set encoding: ISO-8859-1                                      %
+%                                                                         %
+% *** START OF THIS PROJECT GUTENBERG EBOOK ASTRONOMICAL SOCIETY OF THE PACIFIC ***
+%                                                                         %
+% %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% %
+
+\def\ebook{26147}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+%%                                                                       %%
+%% Publications of the Astronomical Society of the Pacific               %%
+%%                                                                       %%
+%% No underfull or overfull boxes                                        %%
+%%                                                                       %%
+%% PDF pages: 127                                                        %%
+%%                                                                       %%
+%% Compile sequence:                                                     %%
+%%                                                                       %%
+%%    pdflatex x3                                                        %%
+%%                                                                       %%
+%% Compile History:                                                      %%
+%%                                                                       %%
+%% Dec 07: Nigel Blower.                                                 %%
+%%         This document was processed with Miktex 2.6 on Windows XP.    %%
+%%         The Miktex compiler was run three times, until the Table of   %%
+%%         Contents was complete.                                        %%
+%%         10 illustrations (fig0 thru fig4, fig6 thru fig10) are        %%
+%%         included as .jpg files in the images directory.               %%
+%%         fig4 is used three times.                                     %%
+%%                                                                       %%
+%% Jul 08: dcwilson                                                      %%
+%%         MiKTeX 2.7, Windows XP Pro                                    %%
+%%                                                                       %%
+%%                                                                       %%
+%% July 2008: pglatex.                                                   %%
+%%   Compile this project with:                                          %%
+%%   pdflatex 26147-t.tex ..... THREE times                              %%
+%%                                                                       %%
+%%   pdfeTeX, Version 3.141592-1.30.5-2.2 (Web2C 7.5.5)                  %%
+%%                                                                       %%
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
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+\listfiles
+
+\usepackage[hmargin=3cm, vmargin=3cm]{geometry}[2002/07/08] % required to set margins 3cm
+\usepackage{amsmath}[2000/07/18]           % ams math package
+\usepackage{amssymb}[2002/01/22]           % required for symbols: \therefore, \centerdot
+\usepackage{graphicx}[1999/02/16]          % required for illustrations: \includegraphics
+\usepackage[latin1]{inputenc}[2006/05/05]  % required for accented characters
+\DeclareInputText{176}{\degree{}}          % to prevent warning messages when � used in math
+\usepackage{wasysym}[2003/10/30]           % required for astronomical symbols: \mars, \saturn, \ascnode
+\usepackage{soul}[2003/11/17]              % required for \so{} - spaced out lettering
+\usepackage{multirow}                      % required to combine rows in tables
+\usepackage{longtable}[2004/02/01]         % required for tables spanning multiple pages
+\usepackage{array}[2005/08/23]             % required for array environment
+\usepackage{tabularx}[1999/01/07]          % required for tables to fill page width
+\usepackage{indentfirst}[1995/11/23]       % optional; indents first paragraph after section
+
+%Title for Table of Contents
+\renewcommand{\contentsname}{
+\begin{center}\begin{Large}
+\so{TABLE\; OF\; CONTENTS.}
+\end{Large}\par\shortrule\end{center}}
+
+% Chapter heading
+\def\nbchapterheading{\newpage\begin{center}\begin{Large}\so{PUBLICATIONS}\end{Large}\\[2mm]
+\begin{footnotesize}\so{OF THE}\end{footnotesize}\\[3mm]
+\begin{Huge}Astronomical Society of the Pacific.\end{Huge}\end{center}}
+
+% Chapter banner
+\def\nbchapterbanner#1#2{\noindent{\renewcommand{\arraystretch}{2}\begin{tabular*}{\linewidth}{@{}l@{\extracolsep{\fill}}c@{\extracolsep{\fill}}l}
+\hline\hline
+\rlap{\textsc{#1}}&\textsc{#2}\\[2mm]
+\hline\hline%\\
+\end{tabular*}}}
+
+% Line in ToC for chapter
+\def\nbchaptertoc#1{\addtocontents{toc}{
+\protect\begin{large}\protect\begin{center}
+\textbf{\textit{Publications} #1}
+\protect\end{center}\protect\end{large}}}
+
+\makeatletter
+% Section heading
+%\def\nbsectionheading #1{\begin{large}\begin{center}#1\end{center}\end{large}}
+\newcommand\nbsectionheading{\@startsection {section}{1}{\z@}%
+                                   {-3.5ex \@plus -1ex \@minus -.2ex}%
+                                   {2.3ex \@plus.2ex}%
+                                   {\centering\normalfont\large}*}
+
+% Subsection heading
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+                                   {-3.25ex \@plus -1ex \@minus -.2ex}%
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+% to minimize the chance of one occurring at the top of a page
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+  \shortrule\fi\end{center}\@ifstar{}{\filbreak}}
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+  \longrule\fi\end{center}\@ifstar{}{\filbreak}}
+\makeatother
+
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+% for omitted/missing table entries
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+\newcommand{\degree}{\ensuremath{^{\circ}}}
+
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+\def\compactlisttwo {\begin{list}{}{\leftmargin \parindent \itemindent -\parindent \itemsep 1pt \parsep 1pt}}
+
+% Asterisk & dagger to mark notes in table
+\def\tablenoteasterisk{\begin{footnotesize}*\end{footnotesize}}
+\def\tablenotedagger{\begin{footnotesize}$\dagger$\end{footnotesize}}
+
+% Disable/adjust hyphenation for specific words, e.g. names
+\hyphenation{Schaeberle Edward Donohoe Leuschner Burckhalter Lowden Jordan Andrews Herrick
+             Astro-nomer Astro-nomers}
+
+% For sensible insertion of boilerplate/licence
+% overlong lines will wrap and be indented 0.25in
+% and we put a running head on the license
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+\addto@hook\every@verbatim{\@totalleftmargin0.25in\small}
+\def\ps@licensing{\def\@evenhead{\hfil\textsc{Project Gutenberg Licensing.}\hfil}%
+  \let\@oddhead\@evenhead}
+\makeatother
+
+% for initials at end of paragraph: pushed right and on new line if necessary
+\def\pushright#1{\qquad\hfill\allowbreak\null\nobreak\hfill #1\quad\null}
+
+% to avoid over/underfull boxes without using explicit linebreaks
+\def\stretchyspace{\spaceskip0.5em plus 0.5em minus 0.25em}
+
+% pdf fine-tuning
+\providecommand{\ebook}{2xynb}
+\pdfcatalog{/PageMode /UseNone
+  /ViewerPreferences <</DisplayDocTitle true >>
+  /PageLayout /SinglePage } openaction goto page 1 {/Fit}
+\pdfinfo{/Title (The Project Gutenberg eBook \#\ebook: Publications of the Astronomical Society of the Pacific)
+  /Author (Astronomical Society of the Pacific)
+  /Subject (Volume 1, 1889)
+  /Keywords (Susan Skinner, Nigel Blower, Jonathan Niehof, Distributed Proofreaders)}
+
+% push footnotes to bottom of page
+\renewcommand*{\footnoterule}{\kern-3pt\vfill
+    \hrule width 0.4\columnwidth \kern 2.6pt}
+
+% make float pages unnumbered
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+     \hfil\fi}\let\@evenhead\@empty\let\@evenfoot\@oddfoot}
+\makeatother
+
+\begin{document}
+
+\thispagestyle{empty}
+
+\begin{verbatim}
+The Project Gutenberg EBook of Publications of the Astronomical Society of
+the Pacific, by Various
+
+This eBook is for the use of anyone anywhere at no cost and with
+almost no restrictions whatsoever.  You may copy it, give it away or
+re-use it under the terms of the Project Gutenberg License included
+with this eBook or online at www.gutenberg.org
+
+
+Title: Publications of the Astronomical Society of the Pacific
+       Volume 1
+
+Author: Various
+
+Release Date: July 29, 2008 [EBook #26147]
+
+Language: English
+
+Character set encoding: ISO-8859-1
+
+*** START OF THIS PROJECT GUTENBERG EBOOK ASTRONOMICAL SOCIETY OF THE PACIFIC ***
+\end{verbatim}
+
+\newpage
+
+\pagestyle{plainfloats}
+
+%-----File: 0001.png-----
+
+\begin{titlepage}
+\begin{center}
+\begin{Large}\so{PUBLICATIONS}\end{Large}\\[15mm]
+\so{\textsc{of \;the}}\\[15mm]
+\begin{Huge}ASTRONOMICAL \; SOCIETY\end{Huge}\\[15mm]
+\begin{huge}OF \; THE \; PACIFIC.\end{huge}\\[25mm]
+\begin{large}(\textsc{Founded February~7, 1889}.)\end{large}\\[25mm]
+\shortrule[2ex]\\[3mm]
+\begin{large} \so{VOLUME \;I}.\end{large}\\[3mm]
+\begin{Large}\textbf{1889}.\end{Large}\\[3mm]
+\shortrule\\[25mm]
+SAN FRANCISCO:\\[3mm]
+\textsc{printed \;for \;the \;society}.\\[3mm]
+\begin{large}1889.\end{large}
+\end{center}
+\end{titlepage}
+
+% title page verso: credits and TNs
+\thispagestyle{empty}
+\begin{center}
+\small
+Produced by Susan Skinner, Nigel Blower, Jonathan Niehof
+and the Online Distributed Proofreading Team at
+http://www.pgdp.net
+\end{center}
+\vfill
+Transcriber's notes: the following corrigenda provided in the original volume have been implemented in this text. Other minor corrections are detailed in the source code.
+
+\begin{center}
+\shortrule
+\nbsectionheading{CORRIGENDA.}
+\shortrule
+\end{center}
+
+Page \pageref{cor1}; Insert a star (*) to signify life-membership after the following
+names, viz: \textsc{Charles Goodall}, \textsc{Horace L. Hill}, \textsc{D.~O. Mills}.
+
+Page \pageref{cor2}; \textit{for} $5�7$ \textit{read} $4�5$.
+
+Page \pageref{cor3}; Column ``Star''; \textit{for} W.~H.~Z.\ \textit{read} W.~M.~Z.
+
+Page \pageref{cor4}; \textit{add} to Mr.\ \textsc{Boulton's} address, (Box 2015, New York
+City).
+
+Page \pageref{cor5}; \textit{for} Centreville \textit{read} Warm Springs.
+
+Page \pageref{cor6}; \textit{for} \textsc{Terry} \textit{read} \textsc{Torrey}.
+
+\frontmatter
+
+%-----File: 0002.png-----
+%-----File: 0003.png-----
+%-----File: 0004.png-----
+%-----File: 0005.png-----
+\setcounter{tocdepth}{3}
+\tableofcontents
+
+
+%-----File: 0006.png-----
+%-----File: 001.png-----
+\mainmatter
+
+\nbchapterheading
+\nbchapterbanner{No.\ 1.}{San Francisco, California, February~7, 1889.}
+\nbchaptertoc{No.\ 1. (February~7, 1889).}
+
+\addcontentsline{toc}{section}{List of Officers \textit{pro tem.}}
+
+The Society was organized at a meeting held February~7, 1889, and the distribution
+of the following Circular was ordered. The list of present members is
+given on page 2. The following officers \textit{pro tem.}\ were chosen to serve till the
+annual election on March 30th, next:
+
+\compactlist
+\item EDWARD S. HOLDEN (Lick Observatory), \dotfill\textsc{President}
+\item J.~M. SCHAEBERLE (Lick Observatory), \dotfill\textsc{Secretary}
+\item C. BURCKHALTER (Chabot Observatory, Oakland), \dotfill\textsc{Secretary}
+\item E.~J. MOLERA (850 Van Ness Ave., San Francisco), \dotfill\textsc{Treasurer}
+\end{list}
+
+\ThoughtBreakLong*
+
+\nbsectionheading{\textit{\textso{CIRCULAR}}.}
+\addcontentsline{toc}{section}{Circular}
+
+\begin{flushright}
+\textsc{San Francisco}, February~7, 1889.
+\end{flushright}
+
+\textsc{My Dear Sir}:---The cordial co-operation of many amateur
+and professional astronomers in the very successful observations of
+the Solar Eclipse of January~1, 1889, has again brought forward the
+desirability of organizing an \textsc{Astronomical Society of the Pacific},
+in order that this pleasant and close association may not be lost,
+either as a scientific or as a social force. You are respectfully invited
+to become a member of this organization, and to do your part
+towards making it useful in our community.
+
+The new Society is designed to be popular in the best sense of
+the word. We wish to count in our membership every person on
+the Pacific Coast who takes a genuine interest in Astronomy, whether
+he has made special studies in this direction or not, and we believe
+that every such person will get, and feel that he gets, a full return
+from the Society, either from its publications or from its meetings.
+
+You will observe that the seat of the Society (the place of deposit
+of its library, collections, etc.) is in San Francisco, where rooms
+can doubtless be found. Half of the meetings of the Society are
+to be held there (including the annual meeting). The other half
+are proposed to be held at the Lick Observatory, on certain Saturdays
+of the summer months when clear weather is to be expected.
+It will be easy for the members to organize a trip (at excursion rates)
+from San Francisco to the Lick Observatory, leaving San Francisco
+%-----File: 002.png-----
+at 8:30~\textsc{a.~m.}, and arriving at the Lick Observatory at 4~\textsc{p.~m.} A
+business meeting can be held before 7~\textsc{p.~m.}
+
+At 7~\textsc{p.~m.}\ on Saturdays the telescopes of the Observatory are put
+at the disposition of all visitors, and thus actual demonstrations from
+the heavens can be made of subjects of discussion.
+
+It would seem that, in this way, a vivid interest in our science can
+be created and maintained, and that a Society possessing such
+exceptional advantages ought to grow and prosper, and be of real
+weight in the advancement and in the diffusion of knowledge. We
+should look forward to the establishment of an astronomical journal
+of high class, to the formation of a special astronomical library, and
+especially to the organization of such scientific work as requires
+co-operation and mutual assistance.
+
+\filbreak
+Invitations to join the Society have been sent and are hereby
+extended to each member of the California Academy of Sciences,
+Technical Society, Microscopical Society, Pacific Coast Amateur
+Photographic Association, Geographical Society of the Pacific, San
+Diego Society of Natural History, California Historical Society; to
+each person who is known to have made observations of the Solar
+Eclipse of January~1, 1889; to the President and Faculties of the
+Colleges, Normal and High Schools of California; and to the officers
+of the Government Surveys in California.
+
+\begin{center}
+Very faithfully yours,
+\addcontentsline{toc}{section}{List of Members}\\*[2em]
+\begin{tabular}{l c l c}
+\textsc{E.~J. Molera}, & San Francisco.  & \textsc{Wm.~Irelan}, & San Francisco.\\
+\textsc{A.~P. Redington}, & ``       & \textsc{C. Burckhalter}, & `` \\
+\textsc{Geo.~W. Reed}, & ``      & \textsc{Ed.~Gray}, & `` \\
+\textsc{C.~L. Goddard}, & ``      & \textsc{W.~C. Gibbs}, & `` \\
+\textsc{O.~V. Lange}, &  ``      & \textsc{C.~P. Grimwood}, & Fruitvale,\\
+\textsc{F.~H. McConnell}, & ``      & \textsc{E.~S. Holden}, & Lick Observatory,\\
+\textsc{S.~C. Partridge}, & ``      & \textsc{S.~W. Burnham}, & `` \\
+\textsc{W.~H. Lowden}, & ``      & \textsc{J.~M. Schaeberle}, & `` \\
+\textsc{E.~W. Runyon}, &  ``      & \textsc{J.~E. Keeler}, & `` \\
+\textsc{Wm. Boericke}, &  ``      & \textsc{E.~E. Barnard}, & `` \\
+\textsc{W.~A. Dewey}, &  ``      & \textsc{C.~B. Hill}, & `` \\
+\textsc{F.~R. Ziel}, &   ``      & \textsc{J.~R. Jarboe}, & San Francisco.\\
+\textsc{Wm.~M. Pierson}, & ``     & \textsc{P.~R. Jarboe}, & `` \\
+\textsc{Chase Gitchell}, & ``      & \textsc{John Le Conte}, & Berkeley. \\
+\textsc{George Tasheira}, & ``      & \textsc{I. Stringham}, & `` \\
+\textsc{V.~J.~A. Rey}, &  ``      & \textsc{F. Soul�}, & `` \\
+\textsc{A.~J. Treat}, &   ``      & \textsc{T. Guy Phelps}, & Belmont.\\
+\textsc{J.~H. Johnson}, &  ``      & \textsc{Arthur Rodgers}, & San Francisco.\\
+\textsc{S.~C. Passavant}, &  ``      & \textsc{Wm.~Norris}, & `` \\
+\textsc{W.~B. Tyler}, &  ``      & \textsc{C. Webb Howard}, & ``
+\end{tabular}
+\end{center}
+\clearpage
+%-----File: 003.png-----
+\nbsectionheading{\begin{huge}\so{BY-LAWS}\end{huge}\\
+\begin{footnotesize}\so{OF THE}\end{footnotesize}\\[2mm]
+ASTRONOMICAL SOCIETY OF THE PACIFIC.}
+
+\addcontentsline{toc}{section}{By-Laws}
+
+\nbsubsubsectionheading{\footnotesize
+(Adopted February~7, 1889.)\\*
+\shortrule}
+
+\nbsubsubsectionheading{ARTICLE I.}
+
+This Society shall be styled the \textsc{Astronomical Society of the
+Pacific}. Its object shall be to advance the Science of Astronomy,
+and to diffuse information concerning it.
+
+\nbsubsubsectionheading{ARTICLE II.}
+
+This Society shall consist of Active, Life, Corresponding and
+Honorary members.
+
+1. Active members shall consist of persons who shall have been
+elected to membership, and shall have paid their dues as hereinafter
+provided.
+
+2. Life members shall consist of persons who shall have been
+elected to life membership and shall have paid \$50 (fifty dollars) to
+the Treasurer of the Society.
+
+3. Corresponding members shall consist of persons not residing
+on the Pacific Coast, who shall have been elected by the Society as
+such.
+
+4. Honorary members shall consist of persons specially distinguished
+for their attainments in Astronomy, who shall have been
+elected to honorary membership.
+
+Corresponding and Honorary members shall pay no dues, shall
+not be eligible to office, and shall have no votes.
+
+\nbsubsubsectionheading{ARTICLE III.}
+
+At each annual election there shall be elected a Board of eleven
+Directors, and a Committee on Publication consisting of three members.
+The officers of this Society shall be a President, three Vice-Presidents,
+%-----File: 004.png-----
+two Secretaries and a Treasurer. The Directors shall
+organize immediately after their election and elect from their number
+the officers of the Society. They may also appoint a Librarian, and
+such other assistants as may be required.
+
+The Library of the Society shall be kept in San Francisco, and
+shall be open to the use of all the members.
+
+
+\nbsubsubsectionheading{ARTICLE IV.}
+
+The President, or, in his absence, one of the three Vice-Presidents,
+or, in the absence of both the President and the Vice-Presidents,
+any member whom the Society may appoint shall preside at the meetings
+of the Society. It shall be the duty of the President to preserve
+order, to regulate the proceedings of the meetings, and to have
+a general supervision of the affairs of the Society.
+
+\nbsubsubsectionheading{ARTICLE V.}
+
+The Secretaries shall keep and have the custody of the records;
+they shall have the custody of all other property of the Society, excepting
+the money thereof; they shall give timely notice of the time
+and place of meetings; they shall keep in books a neat and accurate
+record of all orders and proceedings of the Society, and properly
+index them; they shall conduct the correspondence of the Society;
+they shall preserve and index the originals of all communications
+addressed to the Society; and keep a copy of all their letters, properly
+indexed; and they shall prepare for publication an accurate
+summary of the transactions of the Society at each of its meetings.
+
+\nbsubsubsectionheading{ARTICLE VI.}
+
+The Treasurer shall receive and deposit in such bank as may be
+designated by the Directors, to the credit of the Society, all donations
+and bequests of money and all other sums belonging to the Society.
+He shall keep an account of all money received and paid by him, and
+at the annual meeting render a particular statement of the same to the
+Society. Money shall be paid by him only on the written order of
+the Finance Committee of the Board of Directors.
+
+\nbsubsubsectionheading{ARTICLE VII.}
+
+Candidates for membership may be proposed at any meeting, and
+voted for at any subsequent meeting. The vote shall be by ballot,
+%-----File: 005.png-----
+and a majority of the members present shall be required for an
+election.
+
+\nbsubsubsectionheading{ARTICLE VIII.}
+
+Each active member shall pay an annual subscription of five dollars,
+due on the first of January of each year, in advance. Each
+active member shall, on his election, pay into the Treasury of this
+Society the sum of five dollars, which shall be in lieu of the annual
+subscription to the first of January following his election. No one
+shall be deemed an active member, or receive a diploma, until he
+has signed the register of members, or accepted his election to membership
+in writing, and paid his dues for the current year. Any
+member may be released from annual dues by the payment of
+fifty dollars at one time, and placed on the roll of life members
+by the vote of the Board of Directors. Any failure on the part
+of a member to pay his dues within six months after the time the
+same shall have become payable, shall be considered equivalent to a
+resignation.
+
+\nbsubsubsectionheading{ARTICLE IX.}
+
+The annual meeting of this Society shall be held on the last Saturday
+in March at eight o'clock \textsc{p.~m.}, at the rooms of the Society in
+San Francisco; and bi-monthly meetings shall be held on the last
+Saturday of each alternate month, for the ordinary transactions and
+purposes of the Society, as follows:
+
+The meetings for the months of May, July and September shall
+be held in the Library of the Lick Observatory, Mount Hamilton,
+at a suitable hour; and the meetings for January, March and
+November shall be held in the rooms of the Society, in San Francisco,
+at eight o'clock \textsc{p.~m.}
+
+A special meeting may be called by the President, or, in his
+absence or disability, by one of the Vice-Presidents; or, in the
+absence or disability of both the President and the Vice-Presidents,
+by the Secretary, on the written requisition of ten active members;
+and the object of such meeting shall be stated in the notice by
+which it is called.
+
+The annual election shall be held on the day of the annual
+meeting, during such hours as the Directors may appoint.
+
+Only active and life members shall be permitted to vote at any
+meeting of the Society, and no one shall vote who has not paid all
+his dues for past and current years.
+%-----File: 006.png-----
+
+\nbsubsubsectionheading{ARTICLE X.}
+
+Ten active or life members shall be a quorum for the transaction
+of business.
+
+\nbsubsubsectionheading{ARTICLE XI.}
+
+No papers or manuscripts shall be published by the Society without
+the consent of the Directors. Any motion to print an address,
+or other paper read before the Society, or any other matter belonging
+to the Society, shall be referred to the Committee on Publication,
+who shall report to the Directors. The Committee on Publication
+may make suggestions to the Directors, from time to time, with
+reference to the publication of such papers as in their judgment
+should be published by the Society; and this committee shall have
+the care, direction and supervision of the publication of all papers
+which the Directors may authorize to have published.
+
+Members of the Society shall receive all the publications of the
+Society free of charge.
+
+\nbsubsubsectionheading{ARTICLE XII.}
+
+This Society may, by a vote of the majority of all its active and
+life members, become a branch of an American Astronomical
+Society, should one be formed.
+
+\nbsubsubsectionheading{ARTICLE XIII.}
+
+It shall be the duty of the Directors, in case any circumstances
+shall arise likely to endanger the harmony, welfare or good order of
+the Society, to call a special meeting of the Society; and if, at such
+meeting, after an examination of the charges, and hearing the
+accused, who shall have personal notice of such proceedings, it shall
+be proposed that the offending member or members shall be expelled,
+a vote by ballot shall be taken, and if two-thirds of the members
+present vote in favor thereof, the offending member or members
+shall be expelled.
+
+\nbsubsubsectionheading{ARTICLE XIV.}
+
+The Directors shall meet one hour before the stated time of each
+bi-monthly meeting, and at such other times as they may appoint.
+The President, or in his absence, any one of the Vice-Presidents,
+may call special meetings of the Board of Directors at any time.
+Notice of the time and place of such meeting shall be given by the
+%-----File: 007.png-----
+Secretaries, by depositing in the postoffice at San Francisco, a notice
+of the time and place, addressed to each Director personally, at his
+last known place of residence, with the postage thereon prepaid, six
+days before the time of meeting.
+
+
+\nbsubsubsectionheading{ARTICLE XV.}
+
+The By-Laws may be amended at any time by a consenting vote
+of nine members of the Board of Directors at any regular meeting
+thereof.
+
+\vfil
+\[
+  \includegraphics{images/fig0.jpg}
+\]
+
+%-----File: 008.png-----
+%[Blank Page]
+%-----File: 009.png-----
+
+\nbchapterheading
+\nbchapterbanner{No.\ 2.}{San Francisco, California, March~30, 1889.}
+\nbchaptertoc{No.\ 2. (March~30, 1889).}
+
+\nbsectionheading{THE WORK OF AN ASTRONOMICAL SOCIETY.
+\addcontentsline{toc}{section}{The Work of an Astronomical Society. Address by \textsc{Edward S. Holden}}\\*[4ex]
+\shortrule[2ex]}
+
+\textit{Address delivered before the Astronomical Society of the Pacific,
+March~30, 1889, by} \textsc{Edward S. Holden, LL.~D.}, \textit{Director of the
+Lick Observatory.}
+
+\medskip
+In the year 1820 the state of Astronomy in England was
+somewhat as follows: The Royal Observatory at Greenwich
+was pursuing its regular routine observations of the positions
+of the sun, moon and stars under the direction of the Astronomer
+Royal, \textsc{Pond}, whose chief service to Astronomy
+consisted in the minute accuracy of his observations and in
+the faithfulness with which they were amassed and discussed.
+His controversy with \textsc{Brinkley} (Astronomer of the Dublin
+Observatory) on the latter's determination of stellar parallaxes,
+cleared the way for the great researches of \textsc{Bessel} and
+\textsc{Struve} on the same subject, which followed a dozen years
+later. The Radcliffe Observatory at Oxford was in operation,
+but no observations were published. The Cambridge
+Observatory was just founded. The Observatory at Edinburgh
+was barely built, and was not yet a public institution.
+The Armagh Observatory had no instruments of importance
+and was doing no work. \textsc{Groombridge's} private observatory
+at Blackheath was busy with his catalogue of 4243 circumpolar
+stars. Sir~\textsc{William Herschel}, the greatest of practical astronomers
+and the glory of England (then 82 years old),
+was resting from his labors. His son, Sir~\textsc{John Herschel},
+had not yet begun that long series of observations which has
+made his name illustrious.
+
+On the Continent, the magnificent labors of \textsc{Bessel}, \textsc{Gauss},
+\textsc{Olbers} and \textsc{Struve} were laying the foundations of the
+science of to-day. The spirit of their methods made itself
+known in England and deeply affected some of the younger
+men at the universities---notably \textsc{Babbage}, \textsc{Dean Peacock},
+and Sir~\textsc{John Herschel}. These three entered into a compact,
+%-----File: 010.png-----
+which was most fruitfully carried out, ``to leave the
+world wiser than they found it.'' One of the most important
+results of this resolution was the founding of the Royal Astronomical
+Society of London---an institution which has done
+incalculable good in fostering the science of Astronomy, not
+only in England, but throughout the whole civilized world.
+It is not part of my purpose to trace the influence of this
+society, nor to show in detail what its work has been. I
+rather wish to quote here a few paragraphs from the ``Address
+of the Society, Explanatory of their Views and Objects,''
+which was circulated in the year 1820, at the time of
+its foundation. And I wish to do this for two reasons: because,
+first, the need of such an association in our own midst
+is much the same as that felt by \textsc{Herschel} and \textsc{Babbage} in
+England sixty years ago; and, secondly, because the programme
+of this society may point out to us along what lines
+we should proceed to make our own newly formed Astronomical
+Society equally useful in its own sphere.
+
+The times have changed since then, no doubt. The immediate
+problems of Astronomy are different; but the spirit
+of the methods by which they are to be attacked and solved
+is eternally the same; and the need for co-operation and concentration
+of forces is more and more pressing as the complexity
+of processes becomes greater and greater.
+
+I ask you, then, to listen to a few brief extracts from the
+first printed paper of the Royal Astronomical Society, and
+to imagine to yourself the state of English Astronomy of that
+day, when the elder \textsc{Herschel} had finished his work, and
+when the host of English amateurs of to-day was represented
+by \textsc{Groombridge}, toiling at the observations and the reductions
+of his polar catalogue:
+
+\medskip
+\begin{small}
+``In a country like Great Britain, in which the sciences in general
+are diligently cultivated, and \textit{Astronomy} in particular has made
+extensive progress and attracted a large share of attention, it must
+seem strange that no society should exist peculiarly devoted to the
+cultivation of this science; and that Astronomy, the sublimest branch
+of human knowledge, has remained up to the present time unassisted
+by that most powerful aid; and has relied for its advancement on
+the labors of insulated and independent individuals.
+
+``It may be conceived by some that Astronomy stands less in need
+of assistance of this kind than any other of the sciences; and that, in
+the state of perfection which its physical % Transcriber's note: original reads "physicial"
+ theory has already reached,
+%-----File: 011.png-----
+its ulterior progress may safely be intrusted to individual zeal and
+to the great national establishment exclusively appropriated to celestial
+observations; or, at all events, to those public institutions and academies
+in all civilized nations whose object is the general cultivation
+of the mathematical and physical sciences. It may therefore be necessary
+to state the useful objects which may be accomplished, and
+the impediments which may be removed, by the formation of a society
+devoted solely to the encouragement and promotion of Astronomy.
+
+``Owing to the great perfection which the construction of optical
+instruments has attained in England, and the taste for scientific research
+universally prevalent, there have arisen in various parts of the kingdom
+a number of private and public observatories, in which the celestial
+phenomena are watched, and registered with assiduity and accuracy,
+by men whose leisure and talents peculiarly adapt them for such
+pursuits; while others, with a less splendid establishment, but by the
+sacrifice of more valuable time, pursue the same end with equal zeal
+and perseverance. Considerable collections of valuable observations
+have thus originated; by far the greater part of which, however,
+owing to the expense and difficulty of publication and various other
+causes, must inevitably perish, or at least remain buried in obscurity,
+and be lost to all useful purposes, unless collected and brought together
+by the establishment of a common center of communication and classification,
+to which they may respectively be imparted.
+
+``This great desideratum, it is presumed, will be attained by a
+society founded on the model of other scientific institutions, having
+for one of its objects the formation of a collection or deposit of manuscript
+observations, etc., open at all times for inspection, to which
+the industrious observer may consign the results of his labors, with
+the certainty of their finding a place, among the material of knowledge
+so amassed, exactly proportioned to their intrinsic value. At the
+same time it will thus be rendered practicable to form a connected
+series from a mass of detached and incomplete fragments; and the
+society will render a valuable service to science by publishing from
+time to time from this collection such communications or digests as
+seem calculated by their nature and accuracy either to supply deficiencies
+or to afford useful materials to the theoretical astronomer.
+
+\bigskip
+\centerline{*\qquad\qquad*\qquad\qquad*\qquad\qquad*\qquad\qquad*\qquad\qquad*\qquad\qquad*}
+\medskip
+
+``It is almost unnecessary to enumerate the advantages likely to
+accrue from the encouragement which an Astronomical Society may
+hold out; but among others may be mentioned the perfecting of our
+knowledge of the latitudes and longitudes of places in every region
+of the globe; the improvement of the lunar theory, and that of the
+figure of the earth, by occultations, appulses, and eclipses simultaneously
+observed in different situations; the advancement of our knowledge
+of the laws of atmospherical refraction in different climates,
+by corresponding observations of the fixed stars; the means of determining
+more correctly the orbits of comets, by observations made in
+the most distant parts of the world; and, in general, the frequent
+opportunities, afforded to a society holding extensive correspondence,
+%-----File: 012.png-----
+of amassing materials which (though, separately of small importance)
+may by their union become not only interesting at the present time,
+but also valuable as subjects of reference in future.
+
+``By means of corresponding members, or associates, in distant countries,
+the society may hope to unite the labors of foreign observers
+with their own; and by thus establishing communication with eminent
+astronomers and institutions in all parts of the world, to obtain the
+earliest intelligence of new discoveries and improvements, which it
+may, perhaps, be desirable to circulate among such of its members as
+may profess themselves anxious to receive it, without loss of time.
+
+``The circulation also of notices of remarkable celestial phenomena
+about to happen (with a view to drawing the attention of observers
+to points which may serve important purposes in the determination
+of elements or coefficients) may form another, and perhaps not the
+least interesting object of the society. To have the same phenomena
+watched for by many observers is the only sure way of having them
+observed by some; and moreover, the attention of an astronomer
+may frequently be aroused by a formal notice, especially when accompanied
+with directions for observing the phenomenon in the most
+effective way, when probably the mere ordinary mention of it in
+an ephemeris might fail to attract his observation.
+
+``One of the collateral advantages of a society including many
+practical astronomers among its members (but which will appear of
+no small importance to those who possess good instruments) will be
+the mutual understandings which will be propagated among amateur
+astronomers, by frequent meetings and discussion, as to the relative
+merits of their instruments; and as to the talents and ingenuity of
+the various artists, both of our own and of foreign nations; not to
+mention the emulation which this must naturally excite to possess
+the best instruments; and the consequent tendency of such discussion
+towards a further improvement in their construction, or to the discovery
+of new ones.
+
+``As the extent of the funds of the society must depend on the
+number of its members, it is impossible to conjecture at present how
+far its views respecting their application may extend. Besides the
+ordinary expenses attending an institution of this nature, the annual
+or occasional publication of communicated observations; the payment
+of computers employed in the reduction and arrangement of observations,
+or in computing the orbits of new planets, comets or other
+interesting bodies; the formation of an extensive astronomical library,
+not only of manuscripts, but also of printed books; and perhaps, at
+some future period, the proposals of prizes for the encouragement
+of particular departments of the science, either theoretical or practical,
+or for the improvement of astronomical instruments or tables, may
+be mentioned as worthy objects on which they may be bestowed.
+
+``Such are the principal considerations which have actuated a number
+of individuals to form themselves into a society, under the name
+of the \textit{Astronomical Society of London}, and to give this publicity to
+their determination, with a view of inviting others to unite in the
+%-----File: 013.png-----
+prosecution of their plans. They have at the very commencement met
+with the most flattering success, which induces them to hope that,
+in a short time, every assiduous cultivator of the science will be found
+to have added his name to the list of members.
+
+``The objects of the original members may be sufficiently gathered
+from what has been already said, and may be thus summed up in a
+few words, viz: to encourage and promote their peculiar science by
+every means in their power, but especially, by collecting, reducing
+and publishing useful observations and tables, by setting on foot a
+minute and systematic observation of the heavens, by encouraging
+a general spirit of inquiry in practical Astronomy, by establishing
+communications with foreign observers, by circulating notices of all
+remarkable phenomena about to happen and of discoveries as they
+arise, by comparing the merits of different artists eminent in the
+construction of astronomical instruments, by proposing prizes for the
+improvement of particular departments, and bestowing medals or
+rewards on successful research in all; and, finally, by acting as far
+as possible in concert with every institution, both in England and
+abroad, whose objects have anything in common with their own; but
+avoiding all interference with the objects and interests of established
+scientific bodies.''
+
+\end{small}
+\medskip
+
+In our own case, we must remember how various are the
+opportunities and attainments of our different members, and
+try to lay the foundations of our efforts so broadly that
+every class will find a sphere of action in our programme, a
+stimulus in our proceedings, and a support in our friendly
+association. The few professional astronomers in our midst
+will here lose that sense of intellectual and professional isolation
+which is a drawback and a danger. Nothing that is
+clearly conceived is too technical to be placed before an assemblage
+of intelligent men, and the very effort to explain
+gives a lucidity to the original conception which it might
+otherwise lack. There is a moral force, too, in knowing that
+one does not need to wait for sympathetic appreciation, but
+that it is to be found every day and all around one. The
+opportunity to communicate the results of one's work readily
+and quickly is of the highest value; and ``the end of all observation
+is communication.''
+
+By far the greater number of our members will be amateurs,
+and here again we must recognize the fact that there are
+many classes with many differing opportunities and means
+for work and study. Some among us already possess telescopes
+of no inconsiderable power. In 1820, there was no
+refractor in Europe more powerful than the 5-inch telescope
+%-----File: 014.png-----
+with which \textsc{Herschel} and \textsc{South} observed their double stars.
+It should be the aim of the society to point out the directions
+in which such instruments can be used, so that either some
+useful result will be attained for the science, or so that, at
+least, the maximum amount of pleasure and personal profit
+can be had by the owners. I presume there are few amateurs
+who have not experienced a sense of disappointment in the
+use of their telescopes. It is not that the heavens are less
+glorious, nor that the observer is less devoted and enthusiastic,
+but it is because he often comes to feel that there is an aimlessness
+in his work which he finds to be disheartening. If
+at this moment some word or hint can be given to him which
+will show him how to employ his time and energies to some
+real advantage, either to science or to himself, the old enthusiasm
+will return and the labor will again become delightful.
+It is precisely such words and such hints that he may expect
+to find here among his colleagues.
+
+There is an important class of our amateur members whose
+photographic experience and skill can bear the most useful
+fruits if they are directed toward certain astronomical ends.
+We also have professional astronomers among us, whose
+photographic knowledge is second to none. The association
+which this society makes easy and puts into an organized
+form, has already led to important results in the observations
+of the Solar Eclipse of last January by photographic means,
+and will, no doubt, continue to be fruitful. There are many
+other fields of research open to this method of observation.
+We have other members, also, who have no apparatus for
+observation, but who have the ability, the leisure and the desire
+to forward Astronomy by computing the observations of
+others. There is a boundless field for such amateurs, and I
+am not sure that their efforts, if rightly directed, might not
+be of more real importance than any others. The Lick Observatory
+alone could provide the observations to keep a score
+of computers busy, and this work could be so selected as to
+be of all grades of difficulty and to employ every variety of
+talent.
+
+Finally, we have among us those who have joined as learners;
+who are here to listen, to observe, to read and to study.
+They, in turn, should find in our meetings what they seek for
+and require. Their reading and their study can be guided,
+%-----File: 015.png-----
+and it is among them that we may look for our workers after
+the next few years. Every class of talent and opportunity
+ought to find its profit either in our meetings or in our publications.
+
+One word with regard to the conduct of our meetings. My
+own experience in scientific societies has led me to think that
+their meetings should never consist of mere lectures, no matter
+how interesting. There should be discussion, questions, remarks,
+interchange of ideas, contact of active minds. Let
+each member feel that he has a part to bear, both in the actual
+meetings and outside of them, among his associates. In one
+word, let our society be a live one---active, intelligent, modest,
+competent. It has a doubled interest in its two-fold place of
+meeting. The astronomers of the Lick Observatory can
+promise that the meetings held at Mount Hamilton shall be
+interesting and fruitful. The meetings held in San Francisco
+will also be full of interest.
+
+One of the chief uses of the society will be to make an
+astronomical library available to the amateur observer. We
+have already made a beginning in this direction. It is not
+necessary that our collection should be very extensive. A
+complete astronomical library would contain, perhaps, 20,000
+volumes. But it is desirable that we should own a full set
+of the most important astronomical journals. The progress
+of the science can be traced in their pages from day to day,
+and their past volumes give its history.
+
+I have thought it worth while to give in a list which follows
+the titles of the more important astronomical periodicals, and
+I have ventured to add the names of some twenty or thirty
+books which our members would do well to own personally.
+It is not necessary to buy all of them at once, but the possession
+of one will lead to the desire for another, as the scope
+of observation or of reading is enlarged. The society library
+should begin by owning these volumes. It will grow subsequently
+as our wants develop, both by purchase and by
+exchange with other scientific institutions:
+%-----File: 016.png-----
+
+\nbsubsubsectionheading{\textsc{Astronomical Journals.}}
+
+\compactlist
+\item \textit{Astronomische Nachrichten} (established 1821); 2 vols.\ a year. Kiel; price, \$8.00.
+\item \textit{Astronomical Journal} (established 1851). Cambridge, Mass.; \$5.00.
+\item \textit{Bulletin Astronomique} (established 1884). Paris; \$4.75.
+\item \textit{L'Astronomie} (established 1882). Paris; about \$3.75.
+\item \textit{The Observatory} (established 1877). London; \$3.50.
+\item \textit{Ciel et Terre} (established 1880). Brussels; \$2.60.
+\item \textit{Himmel und Erde} (established 1888). Berlin; \$5.00.
+\item \textit{Sirius} (established 1868). Leipzig; \$2.60.
+\item \textit{Wochenschrift f�r Astronomie} (established 1847). Halle; \$2.70.
+\item \textit{The Sidereal Messenger} (established 1882). Northfield, Minn.; \$2.00.
+\item \textit{Nature.} London; \$6.00.
+\item \textit{La Nature.} Paris; \$6.00.
+\item \textit{The Companion to the Observatory.} London; published annually; 1s.~6d.
+ [This latter work will take the place to the amateur observer which the
+ \textit{Nautical Almanac} holds to the professional.]
+\end{list}
+
+\medskip
+
+\nbsubsubsectionheading{\textsc{Publications of Astronomical Societies.}}
+
+\compactlist
+\item \textit{Publicationen der Astronomischen Gesellschaft.} Leipzig; 4to (at irregular intervals).
+\item \textit{Vierteljahrsschrift der Ast.\ Gesell.} Leipzig; quarterly.
+\item \textit{\stretchyspace Memoirs and Monthly Notices of the Royal Astronomical Society.} London; yearly and monthly.
+\item \textit{Journal of the Liverpool Astronomical Society.} Liverpool; monthly.
+\item \textit{Bulletin de la Soci�t� Astronomique de France.} Paris; yearly (?).
+\item \textit{Publications of the Astronomical Society of the Pacific.} San Francisco.
+\end{list}
+
+\medskip
+
+\nbsubsubsectionheading{\textsc{List of Some Books of Reference in Astronomy.}}
+
+\compactlist
+\item \textsc{Houzeau}: Vade Mecum de l'Astronome; 8vo.
+\item \textsc{Wolf}: Geschichte der Astronomie; 8vo.
+\item \textsc{Delaunay}: Cours El�mentaire de l'Astronomie; 12mo.
+\item \textsc{Loomis}: Treatise on Astronomy; 8vo.
+%-----File: 017.png-----
+\item \textsc{Chauvenet}: Spherical and Practical Astronomy; 8vo; 2 vols.
+\item \textsc{Ball}: Elements of Astronomy; 12mo.
+\item \textsc{Young}: General Astronomy; 8vo.
+\item \textsc{Herschel}: Outlines of Astronomy; 8vo.
+\item \textsc{Arago}: Astronomie Populaire; 8vo; 4 vols.
+\item \textsc{Flammarion}: Astronomie Populaire; 8vo.
+\item \textsc{Newcomb}: Popular Astronomy; 8vo.
+\item \textsc{Webb}: Celestial Objects for Common Telescopes; 12mo.
+\item \textsc{Oliver}: Astronomy for Amateurs; 12mo.
+\item \textsc{Proctor}: The Sun; 8vo.
+\item \textsc{Proctor}: The Moon; 8vo.
+\item \textsc{Proctor}: Saturn and His System; 8vo.
+\item \textsc{Ledger}: The Sun, Its Planets and Their Satellites; 8vo.
+\item \textsc{Watson}: A Popular Treatise on Comets, etc.; 12mo.
+\item \textsc{Smyth}: Celestial Cycle; 2d ed.; revised by Chambers, 8vo.
+\item \textsc{Klein}: Star-Atlas (translation by \textsc{McClure}.)
+\item \textsc{Gledhill}: Handbook of Double Stars; 8vo.
+\item \textsc{Chambers}: Descriptive Astronomy; 8vo.
+\item \textsc{Grant}: History of Physical Astronomy; 8vo.
+\item \textsc{Clerke}: History of Astronomy in the XIX Century; 2d ed.; 8vo.
+\item \textsc{Delambre}: Histoire de l'Astronomie; 4to; 6 vols.
+\end{list}
+
+If our own publications are valuable and worthy, they will
+bring to us through exchanges many works of permanent
+value. This brings me naturally to the question of what and
+how much we ought to publish. On this I shall give my own
+opinion freely, from my personal point of view. It may
+easily be that my ideas on this question, which are rather positive,
+require correction. If they do, the experience of the
+society will be sure to show it.
+
+It seems to me, then, that we should be extremely careful
+to make our publications fully worthy of the society. Any
+observation faithfully made and properly recorded well deserves
+a permanent place. Our very constitution, as a society
+of amateurs, will usually prevent us from presenting these
+long series of observations which can be amassed by professional
+observers in fixed observatories. But we should be
+careful not to make our publications a vehicle for the expression
+of mere unsupported opinion. A theory should always
+be accompanied by its vouchers. I would give more for one
+%-----File: 018.png-----
+careful measure of a double-star, for one faithful observation
+of a comet, than for pages of speculation regarding the origin
+of the solar system. Such speculations have their place in
+science, no doubt, but to be valuable they must follow after
+years of work. We should make our papers a record of actual
+work accomplished. There is room, too, for \textit{r�sum�s} of the
+work of other observers and for papers relating to the
+best methods of making our own observations. Important
+papers in other periodicals may well be translated and printed
+here. The pages of our journal should be truly representative
+of the work and thought of the society in general. It would
+be easy for the Lick Observatory staff to contribute enough
+material to completely fill such a journal; but it appears to
+me that, in general, the work of our observatory should appear
+in abstract only, and that the observations and communications
+from the amateur members of the society should always
+constitute the greater part of the publication. At the same
+time the observatory can serve a very useful end by furnishing
+a series of abstracts of work done and in progress and
+by printing notes on work proposed, especially if it is such
+that our members can co-operate in it. It will be a source
+of pride to us, if after many years we can look back over what
+has been printed by the society, and see that every part of it
+is the record of useful work faithfully done, and possesses a
+permanent value.
+
+It is for this reason that it seems to me we should not
+attempt to print at any regular intervals, as monthly or
+quarterly. Let us keep our papers until we have enough
+material to form a number of 8, 16, 24 pages, and then issue
+and distribute this to our members and to our correspondents.
+
+It is tolerably certain that the time has not yet come for us
+to perform another function of an astronomical society. I
+refer to the foundation and to the bestowal of the medal of
+the society as a reward for astronomical work of the highest
+class. It is certain, however, that in the future, if such a
+medal were founded, and if it were bestowed only for work
+of the highest class, as I have said, and never, under any
+circumstances, to one of our own members, that the responsibility
+of the award would constitute an important stimulus
+to the society itself, which would have to judge of the merits
+of the various works proposed to be rewarded; and that such
+%-----File: 019.png-----
+awards, if always bestowed with judgment and discretion,
+would soon make the voice of our society respected everywhere.
+In fact, there is probably no way in which the society
+could do more good, and in which it could be more quickly
+influential, than by the bestowal of its medal upon those
+astronomers whose works fully deserve it. And there is probably
+no way in which a mistake of judgment would so quickly
+discredit us, as in the bestowal of our highest award upon
+insufficient scientific grounds, or for personal reasons.
+
+It is probably quite time that I should leave these general
+considerations and come to the more special questions of the
+work which our members may reasonably expect to do. In
+any particular case this depends very largely upon the time
+available for such occupation, upon the instrumental equipment
+at hand, and upon the individual aptitude and ability.
+I have already said that for those of us who are willing to
+calculate the observations made by others, there is an endless
+variety of work to do, of all grades of importance and difficulty.
+For those who have only the leisure to interest and
+divert themselves with observing, there is a rational and
+useful method to follow, instead of a random one, which
+will inevitably lead to disappointment. For those who are
+willing to spend a very little time and money, there are many
+fields, both old and new, needing cultivation. Let me mention
+a few of these fields---speaking very briefly of each one:
+
+A very cheap telescope will serve to photograph the sun,
+provided it be of tolerably long focus. It is highly desirable
+to obtain enlarged pictures of the solar spots, and to repeat
+in this country the solar photographs of \textsc{Janssen}, which are
+taken with extremely short exposures---say, from one one-thousandth
+to one two-thousandth of a second of time. A
+series of careful counts of the number of new groups and new
+spots can be made with a very small telescope, and will be very
+useful. If any one of the society will charge himself with the
+necessary measurements, we, at Mt.\ Hamilton, will undertake
+to furnish daily photographs of the Sun on a scale of $4\frac{1}{2}$ inches
+to the solar diameter for the purpose.
+
+I believe that much can be done by studying the moon's
+surface with comparatively small telescopes. In such studies
+I think it desirable to confine the attention to very limited
+areas, and to study and draw these over and over again, under
+%-----File: 020.png-----
+every possible variety of illumination, until the telescope and
+the observer can do no more. In this way it may be that
+only small areas will be covered, but it is certain that our
+knowledge can be materially increased. The observation of
+the occultations of stars is most useful, provided the position
+of the observing station and the local time are accurately
+known. The Lick Observatory time-signals can be readily
+made available for this purpose. Probably little can be added
+to our knowledge of the surface features of the planets by
+observations with the smaller telescopes. It is, however, well
+worth the labor for several of our members to maintain a
+series of observations of the eclipses of the satellites of
+\textit{Jupiter}. There is nowhere in America, I believe, such a series
+maintained. The results of this work will be directly comparable
+with the observations on which the present tables are
+founded, and constants of reduction can be determined by
+which these observations can be employed in conjunction with
+long series already obtained elsewhere. In this case, as in
+so many others, our great distance in longitude from the
+centers of observation, will give to our work a peculiar value.
+We are eight hours west of Greenwich and three hours west
+of Washington, and there is no astronomical establishment
+between us and Japan, and no active observatory between
+California and Australia. There is a whole field of photometric
+work (both visual and photographic) which is open
+to amateurs, and which needs cultivation. I refer especially
+to the photometry of different portions of the sky under
+illumination by the sun or by the moon.
+
+Photographs of the planets and neighboring stars of about
+the same brilliancy on the same plate may very likely be of
+use in comparing their relative brightness. Should a bright
+comet appear, no chance should be lost to photograph it, to
+study the changes in its head, and to map the position of its
+tail among the stars.
+
+The observations of \textsc{Gothard}, on nebul�, by means of
+long-exposure photographs have proved that even comparatively
+small telescopes (provided with driving clocks), properly
+used, are capable of giving the most brilliant and important
+results. It is at least possible that the Zodiacal Light,
+the Milky Way, the Twilight Arch, the Aurora, can be photographed.
+I know of no direction where the skill of amateur
+%-----File: 020a.png-----
+photographers could be better spent than in experiments upon
+these subjects. The problem is of the same nature as the
+photography of the faint outlying streamers of the Solar
+Corona, in which our California amateurs have been so successful.
+
+The field in which amateurs can render the greatest service,
+however, is in the observation of the variable stars. If these
+are to be observed by the eye, the use of a mere opera-glass
+or of a very small telescope is usually sufficient to fix the time
+of maximum or minimum light with accuracy, by comparisons
+with neighboring stars which do not vary. Professor
+\textsc{Pickering} has already presented to the Society a set of
+printed instructions for making such observations. If the
+observer has a photographic telescope or camera, the most
+elegant and accurate method might be to allow the star's
+image to \textit{trail} over the plate. When the trail is weakest the
+Star has reached its minimum. A scale of time can be put
+upon the plate by capping or uncapping the lens at known
+instants. If the star is too faint to trail on the plate while
+the latter remains at rest, a very simple clock-work motion
+can be devised which will cause the telescope to follow the
+star towards the west at a slow rate. This rate can be so
+chosen by experiment as to make the \textit{trail} of suitable brightness
+for measurement.
+
+There are scores of other researches of interest and importance
+which I have not time to mention and which are
+well within the reach of amateurs. One competent sextant
+observer, acting in concert with the Lick Observatory, could
+render a real service to the geography of the State, with very
+little expenditure of time and money, by determining the
+latitudes and longitudes of important points. If such an observer
+were to fix the positions of the eclipse stations occupied
+by the various parties on the 1st of last January, he could
+thus make a positive contribution to science. Mr.\ \textsc{Keeler}, of
+the Lick Observatory, has just completed a determination of
+the position of Norman, for this purpose, as a beginning.
+
+I believe the radiant points of the brighter and more slowly
+moving meteors can be accurately fixed by photography, and
+at any rate the experiment is worth a trial. Statistics of the
+number of telescopic meteors in different parts of the sky and
+at different hours are very much needed and are extremely
+easy to obtain.
+%-----File: 020b.png-----
+\filbreak % try to encourage signature to stay with this paragraph
+I have thus hastily gone over the principal lines along which
+we, as a society, may hope to work with success. If we
+undertake all or any of the work thus indicated, and if we
+carry it on with faithfulness and industry, we may be sure
+that our efforts will be a veritable aid to science. Whatever
+we do, let us do thoroughly. Whatever we say, let it be well
+considered. Let us clearly understand the objects for which
+we are organized, and let us pursue these with entire confidence.
+The scope and membership of this society are such
+that it can have no antagonisms and rivalries with any other.
+But we may look forward to a career of real usefulness, not
+only to our members, but to the science of Astronomy. In
+our own time and way we may hope to make advances in this
+path, and we may be sure that we can diffuse information in
+its regard, and help to increase the intelligence, the activity
+and the pleasure of all our members.
+
+\begin{flushright}
+\textsc{Edward S. Holden.}\qquad
+\end{flushright}
+
+\textsc{Lick Observatory}, February~15, 1889.
+\clearpage
+%-----File: 021.png-----
+\nbsubsectionheading{Extract from the Minutes of the Annual Meeting of the Astronomical
+Society of the Pacific, held at 8~p.~m., March~30, 1889,
+at 605 Merchant Street, San Francisco.}
+
+\addcontentsline{toc}{section}{Minutes of the First Annual Meeting, March~30, 1889}
+
+\nbsubsubsectionheading{\footnotesize
+(Prepared by the Secretaries for publication.)}
+
+The minutes of the meeting of February~7, 1889, were read and
+approved.
+
+{\stretchyspace
+The following named persons (proposed February 7th) were
+elected to membership: Messrs.\ \textsc{William Alvord, J.~M. Selfridge,
+A.~O. Leuschner, William F. Herrick, E.~M. Bixby, H.~T. Compton,
+C.~F. Montealegre, W. Letts Oliver, E.~B. Jordan, James G. Jones,
+Eugene Frost, C. Mitchell Grant, J.~T. Wallace, T.~P. Andrews},
+and Miss \textsc{Rosa O'Halloran}.
+
+}A Board of eleven Directors and a Publication Committee of
+three members were elected.
+
+An address on ``The Work of an Astronomical Society'' was read
+by Mr.\ \textsc{Holden}. This is printed in the present number. A paper on
+``The Solar Corona,'' by Mr.\ \textsc{Pierson}, was received and its reading
+postponed to the next meeting.
+
+After hearing the reports of the officers \textit{pro tem.}, the Society
+adjourned to meet at Mount Hamilton, May 25th.
+
+The following resolution was adopted:
+
+\textit{Resolved}. That the Publications of the Astronomical Society of
+the Pacific be regularly sent to the following Observatories, etc., and
+that the Secretaries of the Society be instructed to notify them of
+this resolution, and to request that they exchange their publications
+with our own; and that the list of these Corresponding Societies and
+Observatories be printed in the Publications of the Astronomical
+Society of the Pacific:
+
+\addcontentsline{toc}{section}{List of Corresponding Observatories, Academies of Science, etc.}
+\begin{small}
+\newcounter{Lcount}
+\begin{list}{\arabic{Lcount}.}{\usecounter{Lcount} \itemsep 0pt \parsep 0pt}
+\item Dudley Observatory, Albany, New York.
+\item Detroit Observatory, Ann Arbor, Michigan.
+\item Royal Observatory, Berlin, Germany.
+\item University Observatory, Bonn, Germany.
+\item Royal Observatory, Brussels, Belgium.
+\item University Observatory, Cambridge, England.
+\item Harvard College Observatory, Cambridge, Massachusetts.
+\item Royal Observatory, Capetown, Africa.
+\item University Observatory, Cincinnati, Ohio.
+\item University Observatory, Dorpat, Russia.
+\item Royal Observatory, Greenwich, England.
+\item Ducal Observatory, Karlsr�he, Germany.
+\item University Observatory, Kasan, Russia.
+\item University Observatory, Koenigsberg, Prussia.
+\item Royal Observatory, Kopenhagen, Denmark.
+\item University Observatory, Leiden, Holland.
+\item University Observatory, Leipzig, Germany.
+\item Royal Observatory, Milan, Italy.
+\item Observatory, Melbourne, Australia.
+\item University Observatory, Moscow, Russia.
+\item Lick Observatory, Mount Hamilton, California.
+\item Royal Observatory, Munich, Germany.
+\item Carleton College Observatory, Northfield, Minnesota.
+\item Radcliffe Observatory, Oxford, England.
+\item Savilian Observatory, Oxford, England.
+\item National Observatory, Paris, France.
+\item Astrophysikalishes Institut, Potsdam, Germany.
+\item Imperial Observatory, Pulkowa, Russia.
+%-----File: 022.png-----
+\item Observatory of the Roman College, Rome, Italy.
+\item University Observatory, Stockholm, Sweden.
+\item University Observatory, Strassburg, Germany.
+\item McCormick Observatory, University of Virginia, Virginia.
+\item Naval Observatory, Washington, District of Columbia.
+\item Imperial Observatory, Vienna, Austro-Hungary.
+\item Royal Astronomical Society, London, England.
+\item Liverpool Astronomical Society, Liverpool, England.
+\item Astronomical Society of France, Paris, France.
+\item Astronomical Society, Chicago, Illinois.
+\item Astronomical Society of Germany, Leipzig, Germany.
+\item Gesellschaft Urania, Berlin, Germany.
+\item National Academy of Sciences, Washington, District of Columbia.
+\item Smithsonian Institution, Washington, District of Columbia.
+\item California Academy of Sciences, San Francisco, California.
+\item Bureau des Longitudes, Paris, France.
+\item The Nautical Almanac, London, England.
+\item The American Ephemeris, Washington, District of Columbia.
+\item Berliner Jahrbuch, Berlin, Germany.
+\end{list}
+\end{small}
+
+At a meeting of the Board of Directors held immediately after
+the meeting of the Society, the officers of the Society for the ensuing
+year were elected. (For list of officers see below.) Mr.\ \textsc{William
+Alvord} was elected to life membership. The Secretaries were instructed
+to correspond with the members of the Society, with a view
+to ascertain what instruments were in their possession, etc.
+
+\ThoughtBreak
+
+\nbsectionheading{OFFICERS OF THE SOCIETY.}
+\addcontentsline{toc}{section}{Officers of the Society}
+
+\noindent
+\begin{tabular*}{\textwidth}{@{\extracolsep{\fill}}lcr}
+EDWARD S. HOLDEN (Lick Observatory),
+&& \textsc{President}\\
+WM. M. PIERSON (76 Nevada Block, S.~F.),
+& \multirow{3}{1em}{\Bigg\}}&\\
+W. H. LOWDEN (213 Sansome Street, S.~F.)
+&& \textsc{Vice-Presidents}\\
+FRANK SOUL� (Students' Observatory, Berkeley),&&\\
+CHAS. BURCKHALTER (Chabot Observatory, Oakland),
+&\multirow{2}{1em}{\Big\}}
+&\multirow{2}*{\textsc{Secretaries}}\\
+J. M. SCHAEBERLE (Lick Observatory),&&\\
+E. J. MOLERA (850 Van Ness Avenue, S.~F.),
+&& \textsc{Treasurer}
+\end{tabular*}
+
+\compactlisttwo
+\item[] \textit{Finance Committee}---\textsc{W.\ C.\ Gibbs, Wm.\ M.\ Pierson, E.\ J.\ Molera}.
+\item[] \textit{Board of Directors}---Messrs.\ \textsc{Alvord, Boericke, Burckhalter, Gibbs,
+Grant, Holden, Lowden, Molera, Pierson, Schaeberle, Soul�}.
+\item[] \textit{Committee on Publication}---Messrs.\ \textsc{Dewey, Treat, Ziel}.
+\end{list}
+
+\ThoughtBreak
+
+\nbsectionheading{NOTICE.}
+\addcontentsline{toc}{section}{Notice to Members}
+
+Members are requested to preserve the copies of the \textit{Publications} of the
+Society as sent to them. At certain intervals a title page and
+index of the preceding numbers will also be sent to the members, who
+can then bind the numbers together into a volume.
+
+The titles of papers for reading should be communicated to either of the
+Secretaries as early as possible.
+
+Those members who propose to attend any or all of the meetings
+at Mount Hamilton during the summer should communicate with Mr.\ \textsc{Burckhalter}
+without delay, in order that arrangements may be made
+for transportation, lodging, etc.
+%-----File: 023.png-----
+%[Blank Page]
+%-----File: 024.png-----
+\clearpage % if this was twoside we would need to clear to verso here
+\nbchaptertoc{No.\ 3. (July~27, 1889).}
+
+\begin{center}\Large Plate I\end{center}
+\addcontentsline{toc}{section}{Plate of the Helical Nebul�}
+
+\begin{center}
+\begin{tabular}{c@{\hspace{2cm}}c}
+  \includegraphics{images/fig1.jpg}&\includegraphics{images/fig2.jpg}\\
+  {Fig. 1.} & {Fig. 2. The Type-Helix,}\\
+            & {(a) direct; (b) reversed.}\\
+            &\\
+  \multicolumn{2}{c}{\includegraphics{images/fig3.jpg}}\\
+  \multicolumn{2}{c}{Fig. 3.}
+\end{tabular}
+\end{center}
+
+%-----File: 025.png-----
+
+\nbchapterheading
+\nbchapterbanner{No.\ 3.}{San Francisco, California, July~27, 1889.}
+
+\nbsectionheading{ON THE HELICAL NEBUL�.}
+\addcontentsline{toc}{section}{On the Helical Nebul�. By \textsc{Edward S. Holden}}
+\nbsubsubsectionheading{\shortrule\\*
+\textsc{By Edward S. Holden.}\\*
+\shortrule}
+
+The discovery of the helical appearance of the planetary nebula
+H.~iv.~37 (G.~C. 4373) at this Observatory in
+1888\footnote{
+ \textit{See Monthly Notices} R.~A.~S. vol.~48, p.~388.}
+naturally led
+to the search for a method which might enable
+one, in some cases at least, to determine the actual situation of
+the different branches of a nebula in space of three dimensions
+from the data afforded by the projection of these branches upon
+the background of the sky. In general, this problem is hopelessly
+insoluble by our present means.
+
+I have, however, obtained some interesting results for one class
+of nebul�  at least, and perhaps the method employed is capable of
+wider application.
+
+To understand the method, let us consider how it is that
+we see a nebula (Plate~I, Figure~1). The only data that we
+have are the outlines $a$ of a drawing of the nebula as it is
+seen projected against the sky. We must conceive the curve $a$
+to be the base of a cylinder, A, whose elements are straight
+lines (rays of light) extending from the projection $a$ to the eye
+at A\@. If the curve $a$ is complicated and involved, so will also
+be the surface of the cylinder A\@. Any curve whatever which
+is drawn on the surface of the cylinder (as $\alpha'$, $\alpha''$,) will be projected
+into the same curve $a$ on the sky; so that the real nebula
+in space may be any one of the infinite number of curves
+which can be drawn on the surface of this particular cylinder;
+for any such curve will be projected into the curve $a$.
+This is true for any and every nebula, as $\beta$, $b$; $\gamma$, $c$; $\delta$, $d$,
+etc., etc. The only thing we really know about the form
+of a nebula, in general, is that it is projected into a certain
+shape, as $a$, or $b$, or $c$, or $d$. The problem is to find the true
+%-----File: 026.png-----
+curves, $\alpha$, $\beta$, $\gamma$, $\delta$, in space, knowing only the projected curves
+$a$, $b$, $c$, $d$.
+
+In order to fix the ideas, let us think of the elongated strings of
+nebulosity which form the spiral nebul�.
+
+Before going further, it is necessary to remark that the data
+(the curves $a$, $b$, $c$, $d$) are at present to be obtained only from
+drawings, and hence they are affected by various classes of errors,
+due to imperfect telescopic, visual and artistic powers. Photographs
+of nebul�  are subject to a different and less hurtful class
+of errors, and they are free from personality. When the great
+telescope is again in a position to photograph the nebul�, I shall
+hope to resume this research with better data. For the present
+I shall take the drawings of Lord~\textsc{Rosse}, of \textsc{Lassell}, and others,
+as the best available, and shall not concern myself with any errors
+remaining in them, but shall treat them as correct, since they are
+the best we have.
+
+To resume consideration of the special problem in hand, let
+us again examine Figure~1. The only thing we know about the
+nebula in space is that its projection on the sky is $a$. Any curve
+on the cylinder A \emph{may be} the true shape of the nebula itself. It
+is the same for another nebula, $b$, whose curve $b$ is usually different
+from that of $a$. \emph{Any} curve on the surface of B will be projected
+into $b$. In general, the shapes of the two cylinders are so utterly
+different that no two identical curves, $\alpha'$, $\beta'$, can be drawn on their
+surfaces.
+
+Now, if we should find a pair of curves, $a$, $b$, whose cylinders,
+A, B, are of such a shape that the same curve \emph{can} be drawn on
+their surfaces, then there is a certain probability that this identical
+curve is, in fact, the true shape of each nebula in space. If, again,
+we can find another nebula, $c$, whose cylinder, C, is so similar to
+that of $a$ that like curves can be drawn on the three surfaces,
+A, B, C, then there is a still greater probability that the identical
+curve on the three surfaces, A, B, C, is, in fact, the true shape
+of these three nebul�, $a$, $b$, $c$, in space. If we find another nebula,
+$d$, whose cylinder, D, is of such a shape that we can also draw
+the same curve on \emph{its} surface, there is a much higher probability
+that this one curve really represents the true shape of all four
+nebul�, $a$, $b$, $c$, $d$, in space.
+
+As we get more and more examples, all fulfilling the same
+condition, the probability that we have obtained the true shape
+of the nebulous form in space is very rapidly increased; and
+%-----File: 027.png-----
+by finding enough examples we may increase the probability
+to essential certainty; and still more so, if one curve, and
+only one, can be found which is common to all the projecting
+cylinders.
+
+We may attack this problem practically, by seeking through
+trails for a single curve, $\Phi$, which by projection at various angles
+and in various positions will give all the differing curves, $a$, $b$,
+$c$, $d$, $e$, $\ldots z$. If such a curve can be found (by trial), and if
+only one such curve can be found, it will become more and
+more probable that $\Phi$ is, in fact, the true curve of each nebula,
+$\alpha$, $\beta$, $\gamma$, $\delta$, $\ldots \omega$, in proportion as more and more curves,
+$a$, $b$, $c$, $d, \ldots$ accurately correspond to the different projections
+of this type curve, $\Phi$. The idea of such types has been
+suggested to me by observations of nebul�  with the great telescope,
+and I have partially discussed it in \textit{Himmel und Erde}, for
+June, 1889, page~503 \textit{et seq.}
+
+I proceed to give what seems to be the type curve of a certain
+family of spiral nebul�. The accompanying Figure~2 shows several
+representations of a helix of wire, which I have found by trial to be
+capable of being projected into the shape of each one of the following
+nebul�. Figure~2 also gives a scale photographed at the same time
+as the wire model. The diameter of the smallest circle of the scale
+is one inch, and the circles are successively $\frac{1}{10}$ of an inch greater in
+diameter. One inch is also marked near each of the vertical projections.
+
+I give in Figure~3 a selection from projections of the type-helix
+of Figure~2, which were made by placing the wire model in a
+beam of parallel rays and tracing its shadow on a plane. Most
+of the comparisons of drawings of nebul�  with the type-helix
+have been made by placing the eye vertically over the plane of
+the paper and by moving the wire helix (its origin nearly always
+touching the paper in the nucleus of the nebula) until the projection
+of the helix accurately covered the drawing of the nebula.
+Usually the model must be applied $n$ different times for a nebula
+with $n$ branches. I have found no case in which this helix
+will fit one branch of a nebula without fitting every other branch
+also.
+
+I give in what follows a few comparisons of this type-helix with
+drawings of nebul�, and I begin with the admirable series of drawings
+given by \textsc{Mr.\ Lassell} in \textit{Mem.}\ R.~A.~S., vol.~36:
+%-----File: 028.png-----
+\begin{tablesetup}
+\renewcommand{\tabularxcolumn}[1]{>{\hangindent1em\relax}p{#1}}
+\begin{tabularx}{\textwidth}{p{4.5em} | p{4.5em} | X}
+\hline\hline
+&  & \\
+\centering\textsc{Lassell's Figure} & \multirow{2}{*}{\centering G.~C.~No.} & \multirow{2}{11.0cm}{\centering \textsc{Remarks.}}\\
+&  & \\
+\hline
+ &  & \\
+\centering 2  & \hfill 600 & The outlines of this nebula have been exactly
+reproduced (in our Fig.~3, No.~1). [The axis of the type-helix is
+in position angle 280�, and altitude above paper 70� to 75�.]\\
+
+\centering 3   & \hfill 604  & Ditto (when Lassell's figure is reversed).\\
+
+\centering 9  & \hfill 1511 & Ditto. (Compare our Fig.~3, No.~3.)\\
+
+\centering 12 (a) & \hfill 1861 &  Ditto (in our Fig.~3, No.~6); (b) compare the
+last drawing of Fig.~2. The nucleus of the nebula is probably due
+to
+a crossing of two loops of the helix.\\
+
+\centering 12 (b) & \hfill 1861 & The outlines can be reproduced. (Compare our Fig.~3,
+Nos.~13, 24, 25.)\\
+
+\centering 15   & \hfill 2373  & The loop and the following edge of
+\textsc{Lassell's} drawing can be
+exactly reproduced. (Compare our Fig.~3, Nos.~15, 19.)\\
+
+\centering 16 &   \hfill 2838 & The axis of the main curve of the drawing has been
+exactly
+reproduced. (Compare our Fig.~3, No.~20.)\\
+
+\centering 17 &   \hfill 2890 & Both these figures have been accurately reproduced. Each
+branch is a projection of the type-helix. (Compare our
+Fig.~3, Nos.~11, 16, 17.) Inner spiral, position angle
+120�, altitude of axis 80� to 85�; outer spiral, position
+angle 120�, altitude 80�. If we match the inner spiral
+and then revolve the type-helix, keeping its axis in the
+same plane, about 90� in the direction S W N E the
+outer spiral will be matched.\\
+
+\centering 27 & \hfill 3572 \linebreak\phantom{1}\hfill M~15 &  All the principal branches have been accurately reproduced,
+one application of the type-helix for each branch. (Compare
+our Fig.~3, Nos.~1, 7, 11, 16, 17.) Inner spiral,
+P = 150�, Alt.\ = 85� to 90�;
+outer spiral, P = 150�,
+Alt. = about 80�. Revolve type-helix
+nearly 180� from
+the position where it matches the outer spiral in the direction
+N W S E, and it will match the inner spiral.\\
+
+\centering 28  &  \hfill 3606 & When this drawing is reversed the three branches can be
+exactly reproduced by three applications of the type-helix.
+(Compare our Fig.~3, Nos.~8, 14, 15, 19, 20.)
+Is the nucleus due to the crossing of two branches of
+the helix?\\
+
+\centering 29 &  \hfill 3614 & When this is reversed its two branches can be reproduced
+by two applications of the type. (Compare our Fig.~3,
+Nos.~5, 6, etc.)\\
+
+\centering 33  &  \hfill 4403 & (The Omega nebula.) The axes of the loop and of the
+straight following part can be exactly reproduced. (Compare
+our Fig.~3, No.~31.)\\
+&  & \\
+\hline
+\end{tabularx}
+
+\bigskip
+\parbox{\textwidth}{\indent
+N.~B.---Note that the position angle of the axis of the type-helix
+is the same for both spirals of G.~C.~2890; and for both spirals
+of G.~C.~3572.}
+\end{tablesetup}
+\medskip
+%-----File: 029.png-----
+
+\noindent
+\begin{tablesetup}
+\begin{tabular}{@{}c@{}}
+\textsc{Comparisons with Lord Rosse's Drawings in the Philosophical
+Transactions, 1861.} \\[1em]
+\begin{tabularx}{\textwidth}{ p{4.5em} | p{4em} | r@{\textit{h. }} X}
+\hline\hline
+&  & \multicolumn{2}{c}{}\\
+\centering\textsc{Fig.} &\multicolumn{1}{c|}{G.~C.} & \multicolumn{2}{c}{\centering\textsc{Remarks.}}\\
+&  & \multicolumn{2}{c}{}\\
+\hline
+&  & \multicolumn{2}{c}{}\\
+\centering \hspace{6pt}9  & \hspace{6pt}888 & & 327.  (Compare our No.~1.\ etc.)\\
+
+\centering 10 &  \hspace{6pt}532 & & 131.  This can be accurately reproduced when it is reversed
+and its scale changed suitably.\\
+
+\centering 13 & 2053  & & 689. Ditto.\\
+
+\centering 15 & 2216--17 & & 765--6. (Compare our Nos.\ 2, 3, 4, 12, 13, 28, 31.)\\
+
+\centering 16 & 2377 & & 857.  (Compare our Nos.\ 1, 7, 11, 16, 17, etc.)\\
+
+\centering 18 &  2670--1  & & 1052--3. (Compare our Nos.\ 2, 3, 12, etc.)\\
+
+\centering 19 &  2680 & & 1061. Can be reproduced.\\
+
+\centering 21 &  2870 & & 1196. (Compare our Nos.\ 3, 9 (reversed), 12, 29, 30,
+etc.)\\
+
+\centering 23 & 3341--2 & & 1306--8. (Compare our Nos.\ 5, 6, 21, etc., and 11, etc.)\\
+
+\centering 24 & 3085 & & 1337. (Compare Nos.\ 2, 14, twice applied.)\\
+
+\centering 25  & 3151 & & 1385. (Compare our Nos.\ 23, 24; and notice the opening
+on the lower side of the figure (as in Fig.~23) and the
+brightening of the nebula just above this (as in Fig.~23)
+where the right-hand hook bends back.)\\
+
+\centering 26 & 3189--90 & & 1414--15. (Compare our Nos.\ 5, 6, 21, 29, 30.)\\
+
+\centering 28 & 3511  & & 1589. (Compare our Nos.\ 5, 6, etc.)\\
+
+\centering 29 & 3615  & & 1650.  (Compare our No.\ 11, reversed.)\\
+
+\centering 32 &  4160 & & 1946. (Compare our No.\ 1, etc.)\\
+
+\centering 36 &  4594 & & 2084. If this drawing be reversed, each of the four
+branches can be accurately represented by projections
+of the type-helix. I have made a wire model of this
+nebula.\tablenoteasterisk \\
+
+\centering 41 & 4971  & & 2245. (Compare our No.\ 1, etc., reversed.) \\
+&  & \multicolumn{2}{c}{}\\
+\hline
+\end{tabularx}
+\end{tabular}
+\end{tablesetup}
+
+\bigskip\vfil
+
+\begin{footnotesize}* Before the present investigation was begun I succeeded in making a model of this
+nebula of four branches, starting on the assumption that each of the four branches was
+produced by the projection (at four different angles) of one and the same curve in space.
+I finally succeeded in bending a wire so that when it was held in four different positions
+(the origin of the helix always touching the nucleus), the four projections accurately
+covered the four branches as they are laid down in the drawing. I then laid this model to one
+side and constructed a type curve from the nebul�  G.~C. 600, the great Nebula G.~C. 3572
+(M.~51) and others. This second type curve was then applied (reversed) to the nebula 4594,
+and it was found to accurately represent it, and to be the same curve as the one first constructed.
+Probably in this case, as in others, the conviction that the real type of the nebula has been
+discovered is more strongly brought home to the person who has actually constructed the
+models and found them to exactly represent the pictures, than to one who merely reads an account
+of how the experiment was conducted. The only ambiguity in my model of this nebula is
+due to the fact that it is impossible to decide on which side of the plane of projection any or all
+of the branches are situated. We know the real shape of each branch, but we do not know
+whether it lies on the hither or on the farther side of the plane of projection.
+
+\end{footnotesize}
+%-----File: 030.png-----
+
+\noindent
+\begin{tablesetup}
+\begin{tabular}{@{}c@{}}
+\parbox{0.9\textwidth}{\centering
+  \textsc{Comparison with Lord Rosse's Drawings in the Scientific
+  Transactions Royal Dublin Society, Vol.~II.}}\\[1em]
+\begin{tabularx}{\textwidth}{c r@{.}r | p{4em} | X}
+\hline\hline
+\multicolumn{3}{c|}{}&  & \\
+\multicolumn{3}{c|}{\textsc{Plates.}}
+& \multicolumn{1}{c|}{G.~C. \ } & \multicolumn{1}{c}{\textsc{Remarks.}}\\
+\multicolumn{3}{c|}{}&  & \\
+\hline
+\multicolumn{3}{c|}{}&  & \\
+& I & &  1202 & (Compare our Figs.\ 24, 25)??\\
+
+& I &  & 1267 & (Compare our Figs.\ 14, 15, 19, etc., reversed.)\\
+
+& I &  & 1519 & This can be accurately reproduced.\\
+
+& II &  & 1520 & Ditto.\\
+
+& III & &  1861--3  & The principal curves in these nebul�, ditto.\\
+
+& IV &  & 3572 & Ditto.\\
+
+& V &  & 4561 & (Compare our Figs.\ 9, 10, the middle parts only.)\\
+
+& VI &  & 4403 & The axes of this can be accurately reproduced. (See our
+Fig.~31.)\\
+\multicolumn{3}{c|}{}&  & \\
+\hline
+\end{tabularx}
+\end{tabular}
+\end{tablesetup}
+
+\medskip
+
+It is unnecessary to give more examples. Indeed, the cases
+already given include nearly all the spiral nebul�. Those just
+referred to are sufficient to exhibit the whole evidence to any one
+who will construct for himself a type curve from the data in Figure
+2, and who will go over the comparisons with the plates as above
+outlined. The spirals of \textit{Nebula Orionis} are probably of the type just
+given, also. The case of the \textit{Omega} nebula (G.~C. 4403) is very
+striking. I have also found remarkable analogies in various spiral
+streams of stars.
+
+It may be objected to the suggestions given above that the forms
+of the nebul�  are so indefinite that a very great latitude is allowed
+in matching the drawings with the projections of any particular type
+curve. This is undoubtedly true. The only remedy for it is to obtain
+better representations of the nebul�  themselves by photographic
+means.
+
+A second objection is that Figure 3 shows that a particular spiral,
+once assumed, may be projected into many forms, and that these
+might be sufficiently varied to be fitted to a comparatively small
+number of objects out of the many thousands of known nebul�. To
+this it may be said that it is undoubtedly true that the projection of
+many different curves can be made to fit a certain number of the
+drawings referred to. Still, it appears to me, after trials, that the helix
+of Figure 2 comes nearer to being the type curve of the nebul�  in
+question than any other that I can now construct. It certainly will
+need to be corrected, but it seems to be a good first approximation.
+%-----File: 031.png-----
+The difficulty of improving it can be best appreciated by making
+the trial.
+
+Again, it must be remembered that while there are many thousands
+of nebul�, there are only comparatively few spiral nebul�, and
+that the type curve fits a very great percentage of these, while it cannot
+be tortured into a resemblance to other nebul�  not spiral.
+
+If the helix given in Figure 2 is indeed the type of a certain
+class of nebul�, many interesting questions may receive a solution.
+For example, what are the directions in space of the \emph{axes} of these
+different nebul�? Is there anything systematic in these directions?
+What is the law of the force by which particles of matter are expelled
+from (or attracted to?) the central nucleus? Have we here in the
+nebul�  different types of spirals somewhat analogous to the different
+types of comets' tails so ably discussed by Professor \textsc{Bredichin}?
+
+Some of the parts of these nebul�  must be approaching the
+earth, some receding from it. Can we by the spectroscope discriminate
+between such motions?
+
+\filbreak
+A suggestion which holds out even the hope of successfully
+attacking such problems is not without its value, and I have, therefore,
+no hesitation in presenting the foregoing paper in its present
+incomplete form.
+\begin{flushright}
+\textsc{Edward S. Holden.}
+\end{flushright}
+\textsc{Lick Observatory}, July~12, 1889.
+
+\ThoughtBreakLong
+\bigskip
+
+\nbsectionheading{ON THE ORBIT OF COMET BARNARD (1889, \textsc{June} 23).}
+\addcontentsline{toc}{section}{On the Orbit of Comet Barnard (1889, June~23). By \textsc{A. O. Leuschner}}
+
+\nbsubsubsectionheading{\shortrule\\*
+\textsc{By A.~O. Leuschner.}\\*
+\shortrule}
+
+From Mr.\ \textsc{Barnard's} observations of June 23, 24, 25, I have
+deduced the following elements:
+\[
+\begin{array}{l}
+\quad T = 1889, \textrm{ June~20. 1480 G.~m.~t.}\\
+\;\; \left.
+\begin{array}{r@{\;}l}
+  \Omega &=           271�\, \phantom{0}4'.1 \\
+  \omega &= \phantom{0}59�\,           20'.7\\
+  i      &= \phantom{0}31�\,           14'.6
+\end{array}
+\right\} 1889.0\\
+  \log q = 0.04236
+\end{array}
+\]
+
+Obsd.---Computed; $\Delta\lambda \cos \beta = -0'.3, \Delta\beta = 0'.0$.
+
+\ThoughtBreakLong
+\bigskip
+
+%-----File: 032.png-----
+\nbsubsubsectionheading
+	{[\textsc{Abstract}.]}
+\nbsectionheading{ON THE OCCULTATIONS OF JUPITER (\begin{small}VISIBLE IN\end{small} 1889);
+AND ON THE ECLIPSES OF SATELLITE IV.}
+\addcontentsline{toc}{section}{On the Occultations of Jupiter (visible in 1889) and on the Eclipses of Satellite IV\@. By \textsc{Charles B. Hill}}
+
+\nbsubsubsectionheading{\shortrule\\*
+\textsc{By Charles B. Hill.}\\*
+\shortrule}
+
+Mr.\ \textsc{Hill} spoke of the various phenomena of \textit{Jupiter's} satellites,
+etc., of special interest, and called the attention of members especially
+to
+\nbsubsubsectionheading
+{\textit{The Eclipse (reappearance) of Satellite IV:}}
+\noindent1889, August~18, at 8h.\ 37m., P.~s.~t.; and to
+\nbsubsubsectionheading
+{\textit{The Occultation of Jupiter by the Moon:}}
+\noindent
+\begin{tabular}{@{} l@{}l@{ }r@{ }c@{ }c@{ }c}
+1889, Sept.~3---& \textit{Immersion}, &   I & contact, & 5h.\ 32.5m., & P.~s.~t.\\
+                &                     &  II &  ``      & 5h.\ 34.5m., &  ``\\
+                & \textit{Emersion},  & III &  ``      & 6h.\ 26.0m., &  ``\\
+                &                     &  IV &  ``      & 6h.\ 28.0m., &  ``\\
+
+&\multicolumn{5}{@{}l}{
+  \begin{tabular}{@{} *{4}{c@{ }} l@{ }l}
+    Angle & from & North & Point, & Imm.  & = 149�\\
+     ``   &  ``  &  ``   &  ``    & Emer. & = 234�
+  \end{tabular} }
+\end{tabular}
+\medskip
+
+The above prediction is based on an approximate (graphical)
+computation for the position of Mt.\ Hamilton. The occultation will
+be visible in the United States generally. In California it will take
+place shortly before sunset, the moon being one day past \textit{First
+Quarter}.
+
+\ThoughtBreakLong
+\medskip
+
+\nbsubsubsectionheading
+	{[\textsc{Abstract}.]}
+\nbsectionheading{ON PHOTOGRAPHING THE CORONA IN FULL SUNSHINE;
+AND ON PHOTOGRAPHS OF THE MOON IN THE DAYTIME.}
+\addcontentsline{toc}{section}{On Photographing the Corona in full Sunshine
+and on Photographs of the Moon in the Daytime. By \textsc{James E. Keeler}}
+
+\nbsubsubsectionheading{\shortrule\\*
+\textsc{By J.~E. Keeler.}\\*
+\shortrule}
+
+Mr. \textsc{Keeler} gave a brief account of the attempts that had been
+made to see and to photograph the corona in full sunshine, and
+spoke of the evidence of the eclipse photographs on the practicability
+of the latter experiment. It had been shown by Professor \textsc{Holden}
+in the Eclipse Report of 1889 that if the intrinsic brilliancy of the
+daylight near the sun was 1000, the intrinsic brilliancy of the daylight
+%-----File: 033.png-----
+\emph{plus} corona was not above 1002. Hence, to photograph the
+corona in full sunshine, we must be able to record a difference of
+brilliancy, a contrast, of $\frac{1}{500}$. The eye could detect a contrast of
+$\frac{1}{60}$ only, and hence the attempt seemed hopeless, as the rays and
+streamers of the corona had a continuous spectrum like that of diffused
+daylight. He also exhibited some photographs of the moon
+taken in the daytime by Mr.\ \textsc{Burnham}, with a lens of aperture $ = {}^3\!/\!_4$
+inch, focus = 9~inches, stop f$/_{\displaystyle\!44}$, time $\frac{1}{60}$ to $\frac{1}{100}$ of a second. The
+moon was more than 120� from the sun at the time.
+
+Experiments on this matter were recommended to the amateur
+photographers of the Society, and it was asked that successful trials
+might be communicated to the Lick Observatory. Photographs of
+the dark side of the moon before first quarter might be included in
+the plan. Each plate exposed should be marked with the observer's
+name; the aperture, stop, and plate employed; the hour and minute
+of exposure; the length of exposure.
+
+Mr.\ \textsc{Keeler} exhibited some prints made on ordinary dry plates
+and on ortho-chromatic plates, and recommended the attention of
+the members of the Society to the excellent results attained by the
+use of the latter plates, and suggested a trial of them for pictures of
+the moon in the daytime, as the moon was relatively rich in light
+of greater wave length than F.
+
+\bigskip
+\ThoughtBreakLong
+\bigskip
+
+\nbsectionheading{NOTICES FROM THE LICK OBSERVATORY.}
+\addcontentsline{toc}{section}{\textit{Notices from the Lick Observatory}}
+
+\nbsubsubsectionheading{\shortrule\\*
+{\small \textsc{Prepared by Members of the Staff.}}\\*
+\shortrule}
+
+The desire is expressed, on many sides, that the Publications of
+the Society should contain brief notices of the work current at the
+Lick Observatory, because much of this work is necessarily published
+in Eastern and foreign journals and therefore may escape the attention
+of our members.
+
+Such notices must evidently be of the briefest and most popular
+character, and very often can be nothing more than a reference
+to the title and place of publication of a paper. Even such references
+as these may serve, it is said, to call the attention of our members
+to the existence of a paper which may be of interest to several
+of them.
+
+It is therefore proposed, as an experiment merely, to include in
+%-----File: 034.png-----
+each of our Publications a few pages of items relating to the work
+of the Lick Observatory. Should these meet the want which has
+been expressed, it will be easy to continue them in the future. In
+this way an acquaintance with the work of the Observatory can be
+maintained, without taking too much space in the pages of our Publications,
+which should be reserved for longer articles by the members
+of the Society in general.
+
+As the Observatory commenced active operations not long before
+the foundation of the Society, the present number of the \textit{Notices} may
+well be devoted to a list of the mere titles of the different papers, etc.,
+which have been sent to various scientific journals and magazines
+since June~1, 1888, by the members of the Observatory staff.
+Articles printed in newspapers, etc., are not included, as these are
+generally of transient interest only. This list, then, will bring the
+history of the astronomical activity of the Observatory up to the
+present time, and leave a clear field for the subsequent numbers of
+these \textit{Notices}.\pushright{E.~S.~H.}
+
+\ThoughtBreak*
+\bigskip
+
+\nbsubsectionheading{Photograph of the Davidson Comet.}
+\addcontentsline{toc}{subsection}{\qquad Photographs of the Davidson Comet. By \textsc{E. S. Holden}}
+
+The comet discovered by Mr.\ \textsc{Davidson} at Queensland, on July
+21, was photographed at the Observatory by Mr.\ \textsc{Barnard}, with the
+new \textsc{Willard} lens (about 5~inches aperture, 30~inches focus) on
+July~30. A Seed~26 plate was used, and an exposure of ninety
+minutes was given. The camera was mounted on the top of the
+twelve-inch equatorial, and the camera was kept directed at the comet
+by moving the slow motion screws in R.~A. and in Dec. As the
+comet had a rapid motion in reference to the stars, the latter appeared
+as \textit{trails} about $13'$ to $14'$ long. This was the comet's motion
+in ninety minutes of time. The head of the comet shows as a neat
+round mass. The tail is fan-shaped, with its borders convex to the
+axis, and very narrow at the root. It can easily be traced $20'$ and it
+is evident for about $53'$. Mr.\ \textsc{Barnard} could trace it no further
+than $50'$ or so, with the telescope. After the picture of the comet
+was taken, the negative was exposed to the light of our standard
+lamp for 1, 5, 10, 15, 20, 25 and 30 seconds, making a series of
+squares of standard intensity. (See Lick Observatory Eclipse Report,
+page~12.) The night-sky was less intense than the square exposed
+one second. The brightest part of the tail of the comet $2'$ or so from
+the head matched the standard square exposed ten seconds. Hence
+the comet is about nine and one-half times as bright as its background.
+%-----File: 035.png-----
+Omitting any consideration of the absorption of the atmosphere,
+and of the absorption of the lens (as yet undetermined), I
+find that the intrinsic brilliancy of this portion of the comet was
+0.000,000,15 units of the standard lamp. The full moon has an
+intrinsic brilliancy of 1.66 units (\textsc{Pickering}) and the brightest parts
+of the corona of January~1, 1889, had an intrinsic brilliancy of 0.08
+units. Hence the comet is 10,000,000 times fainter than the full
+moon, area for area; and 500,000 times fainter than the brightest
+parts of the corona of last January. According to Mr.\ \textsc{Pickering's}
+measures, the intrinsic brilliancy (actinic) of the sky within 5� from
+the full moon is 0.000,064 units; and thus the sky near the moon is
+400 times brighter than the comet, and more than 4000 times as
+bright as the night-sky. These measures relate only to the photographic
+brilliancy of the comet. The visual brilliancy would be
+much higher relatively, as the observations of Mr.\ \textsc{Keeler} show the
+most refrangible end of its spectrum to be very weak.
+
+The results just given are interesting and important in themselves,
+and they also have an historical value; since this is the first occasion
+on which the light of a comet has been actually measured with accuracy.\footnote{
+Since the above was written, I have seen a reference to a measure of the light of the comet
+of 1881 (?) by \textsc{Janssen} (\textit{Ann.\ Bureau Long.}\ 1882, p.~781), which is stated as 300,000 times
+fainter than the full moon. This book is not accessible to me, and I do not know if the brilliancy
+was measured, or only inferred from the time of exposure compared with that of the moon.}
+
+The preceding experiment also suggests various applications.
+For example: we may measure the total amount of a comet's light
+on various dates, and compare this measured light with the amount
+of light reflected to us by the comet from the sun, which latter quantity
+can be accurately calculated. Thus, we might find
+
+\medskip
+
+\begin{small}
+\begin{tabular}{l rrr rrr rrr}
+&\multicolumn{3}{r}{\textsc{Jan.~1.}}
+&\multicolumn{3}{r}{\textsc{Jan.~2.}}
+&\multicolumn{3}{r}{\textsc{Jan.~3, etc.}}\\
+Measured light from the comet   &&=& L, &&=& M, &&=& N, etc.\\
+Calculated light from the comet &&=& A, &&=& B, &&=& C, etc.\\
+$\therefore$ Native light of the comet\;
+&\multicolumn{3}{r}{$\mathrm{= L - A,}$}
+&\multicolumn{3}{r}{$\mathrm{= M - B,}$}
+&\multicolumn{3}{r}{$\mathrm{= N - C, etc.}$}
+\end{tabular}
+\end{small}
+
+\medskip
+
+It has long been known that the brilliancy of comets increases
+beyond the theoretical amount as they approach the sun, owing to
+native light emitted by them under the influence of the sun. It
+appears that there is now some hope of tracing such changes of brilliancy
+from day to day, by photographic means, and of obtaining in
+this way some clue to the energy of the forces which produce these
+observed changes.\pushright{E.~S.~H.}\\*[0.5ex]
+{\small\indent 1889, July~31.}
+
+%-----File: 036.png-----
+
+\nbsubsectionheading{Spectrum of Davidson's Comet.}
+\addcontentsline{toc}{subsection}{\qquad Spectrum of Davidson's Comet. By \textsc{James E. Keeler}}
+
+The spectrum of Davidson's comet was observed here with the
+twelve-inch equatorial, on July 31st, and with the thirty-six-inch
+equatorial, on August 1st. The \textit{coma} showed a spectrum consisting
+of three somewhat diffuse bright bands, which were found to be identical
+in position with the carbon fluting given by the blue flame of a
+spirit lamp. A faint luminosity connected the bands, so that the
+spaces between them were not perfectly dark.
+
+The nucleus gave a continuous spectrum not extending below
+the D line, with slight brightenings at the positions of the carbon
+flutings. Such a spectrum would probably be given by the material
+of the \textit{coma} at an increased pressure. Although the comet is now
+rated at about the sixth magnitude, its spectrum is much fainter than
+that of a star of this brightness, on account of the diffusion of its
+light over a large area.\pushright{J.~E.~K.}\\*[0.5ex]
+{\small\indent Aug.~2, 1889.}
+
+\nbsubsectionheading{New Double Stars.}
+\addcontentsline{toc}{subsection}{\qquad New Double Stars. By \textsc{S. W. Burnham}}
+
+One of the more recent double-star discoveries with the thirty-six-inch
+telescope is a seventh-magnitude star (D.~M. 30�, 4809) near $\eta$
+Pegasi. The measures on three nights give:
+\begin{small}
+\[
+  1889.55 \qquad 335�.3 \qquad 0''.23 \qquad 7.2 \qquad 8.2
+\]
+\end{small}
+
+The 4--5~m.\ star, \textit{$\psi$ Cassiopei�}, % Transcriber's note; original reads "Cassiope�"
+ has been known since the first
+\textsc{Herschel} as a triple star, from a small double companion at a distance
+of $28''$ from the large star. The Lick telescope shows a small
+star of about 13--15~m.\ % Transcriber's note: Original text reads 13--5 m.
+% Washington Visual Double Star Catalog, 1996.0 (Worley+, 1996) gives magnitude 14,
+% discoverer S.~W.\ Burnham, 1889
+at a distance of $3''.2$ in the direction of 41�.2.
+
+A careful set of measures of the close pair, \textit{$\kappa$ Pegasi} ($\beta$ 989)
+has been made with the thirty-six-inch telescope. The change in
+both angle and distance has been very great since its discovery with
+the Chicago telescope in 1880. As the distance now is only $0''.14$,
+it could hardly be seen, or measured, with any instrument much
+smaller than the Lick telescope. The components differ by only
+about half a magnitude, and there is a possibility of the wrong
+quadrant having been given in my first measures made in 1880,
+although at the time this was carefully looked after. Taking the
+early measures as they stand, the motion (direct) would be 235� in
+nine years. If the first angle should be reversed, the change would
+be only 56�.
+
+There is a small star $11''$ distant, which makes the double, $\Sigma 2824$.
+This is fixed with reference to the bright star.
+%-----File: 037.png-----
+
+28 \textit{Andromed�} is also a new double star. The following is the
+mean of three nights' measures with the thirty-six-inch refractor:
+\begin{small}
+\[
+  1889.51 \qquad 360�.1 \qquad 2''.42 \qquad 5.5 \qquad 13.3
+\]
+\end{small}
+
+\textsc{Herschel}, at the Cape of Good Hope, noted a small double star
+in the fine cluster and nebula, \textsc{Messier}~8, and entered it as No.\ 5009
+of the Cape Catalogue. The Lick telescope shows that the principal
+star of \textsc{Herschel}'s pair is a close pair. The mean of four measures
+is:---
+\begin{small}
+\[
+  1889.40 \qquad 55�.6 \qquad 0''.63 \qquad 8.7 \qquad 9.5
+\]
+\end{small}
+
+There is probably no change in \textsc{Herschel}'s more distant star.
+\begin{tablesetup}
+\begin{tabular}{*{5}{r@{.}lc}l}
+\multicolumn{3}{c}{ } & \multicolumn{2}{c}{�} && \multicolumn{2}{c}{\raisebox{-0.5ex}{$''$}} \\
+1837&70 &\qquad& 20&8 &\qquad& 2& &\qquad& 10& &\qquad& 12& &\qquad& 1n H \\
+1880&58 && 19&9 && 3&86 && 9&0 && 9&5 && 1n Cin \\
+1889&40 && 23&3 && 4&05 && 8&7 && 9&6 && 4n $\beta$
+\end{tabular}
+\end{tablesetup}
+
+For many years $\Sigma~2438$ has been found to be single with all telescopes.
+A recent set of measures with the large refractor of the
+Lick Observatory gives for the distance $0''.24$, and the position angle
+46�.2. The angle when measured by \textsc{Struve} in 1832 was 340�.6.
+
+With powers up to 2000, the thirty-six-inch shows the large star
+of $\Sigma~3130$ as single. It has not been seen double during the last
+thirty years.\pushright{S.~W.~B.}
+
+\nbsubsectionheading{Meridian Circle Observations of \textit{Victoria} and Comparison
+Stars.}
+\addcontentsline{toc}{subsection}{\qquad \protect\stretchyspace Meridian Circle Observations of Victoria and Comparison Stars. By \textsc{J.~E. Schaeberle}}
+
+In connection with astronomers in the northern hemisphere, the
+Astronomer Royal at the Cape of Good Hope, Dr.\ \textsc{David Gill}, is
+observing the planet \textit{Victoria}, for the determination of its parallax
+(and hence of the Solar Parallax). He has requested various observatories
+to determine, by meridian observations, the positions of the
+planet and of thirty-seven comparison stars. This work has been
+done at the Lick Observatory by eighteen nights of observations, between
+June~8 and July~8, and the results will soon be ready for publication.
+From a series of experiments, it was found that (thanks to
+the designer of the large pivots, nearly four inches in diameter) much
+better results could be obtained when the observations were made
+without clamping the instrument. The clamp was accordingly removed
+(some months ago), so that all of the observations referred to
+above were made with the nearly counterpoised instrument hanging
+freely in the wyes. % OED: "Wyes, the supports of the telescope in the theodolite and level"
+ That this variation from the usual method is to
+be approved, when the proper precautions are taken, seems to be
+shown by the smallness of the probable errors of observation, which,
+%-----File: 038.png-----
+for a single observation in R.~A. and Dec., are about $0^\text{s}.020$ and
+$0''.25$ respectively. These figures also show that the \textsc{Repsold} meridian
+circle is capable of first-class work, and that the refraction as
+given in Vol.~1, \textit{Publications Lick Observatory}, is not very far out of
+the way.\pushright{J.~M.~S.}
+
+\nbsubsectionheading{New Double Stars.}
+\addcontentsline{toc}{subsection}{\qquad New Double Stars. By \textsc{E. E. Barnard}}
+
+I have found the stars, 2~\textit{Piscium} and W~\textsc{xxiii}.803 to be double
+with the twelve-inch equatorial. Mr.\ \textsc{Burnham} has kindly measured
+these stars with the thirty-six-inch and supplied me with his results
+for publication. From the inequality of the components, 2~\textit{Piscium}
+is a difficult object with the twelve-inch.
+
+Following are Mr.\ \textsc{Burnham's} measures.\pushright{E.~E.~B.}\\*[.5ex]
+{\small\indent 1889, August~5.}
+
+\begin{gather*}
+ \mathit{2~Piscium.}
+\\
+\left. \begin{gathered}
+  \text{22h.~53m.~18s.}  \\  0�~19'
+\end{gathered} \right\}
+\\
+\begin{array}{r@{} *{2}{r@{.}l@{}c@{}}
+                        r@{.}l@{}     c r@{} c@{} r@{.}l@{} l}
+   \multicolumn{3}{c}{ }
+&& \multicolumn{2}{c}{�}
+&& \multicolumn{2}{c}{ \raisebox{-0.5ex}{$''$} }
+\\
+& 1889&553  &\mbox{\qquad\qquad\quad}
+&   96&0    &\mbox{\qquad\qquad}
+&    3&87   &\mbox{\qquad\qquad\;}
+&    6      &\mbox{\qquad\qquad\quad}
+&   14
+\\
+&     &556  &&  91&8  &&  3&88  &&  6  &&  13&5  \\
+&     &589  &&  93&1  &&  3&68  &&  6  &&  13&5  \\
+\cline{2-3} \cline{5-6} \cline{8-9} \cline{11-11} \cline {13-14}
+& 1889&57   &&  93&6  &&  3&81  &&  6  &&  13&7
+\end{array}
+\end{gather*}
+
+\begin{gather*}
+\text{W \textsc{xxiii}.803.}
+\\
+\left. \begin{gathered}
+  \text{23h.~40m.~53s.}  \\  4�~35'
+\end{gathered} \right\}
+\\
+\begin{array}{r@{} *{2}{r@{.}l@{}c@{}}
+                        r@{.}l@{}     c r@{} c r@{.}l@{} l}
+   \multicolumn{3}{c}{ }
+&& \multicolumn{2}{c}{�}
+&& \multicolumn{2}{c}{ \raisebox{-0.5ex}{$''$} }
+\\
+& 1889&553  &\mbox{\qquad\qquad}
+&  166&2    &\mbox{\qquad\qquad}
+&    0&49   &\mbox{\qquad\qquad}
+&  8.7      &\mbox{\qquad\qquad}
+&    8&7
+\\
+&     &556  &&  166&5  &&  0&59  &&  8.6  &&  8&6  \\
+&     &589  &&  166&0  &&  0&53  &&  8.5  &&  8&5  \\
+\cline{2-3} \cline{5-6} \cline{8-9} \cline{11-11} \cline {13-14}
+& 1889&57   &&  166&2  &&  0&54  &&  8.6  &&  8&6
+\end{array}
+\end{gather*}
+
+\bigskip
+
+\nbsubsectionheading{List of the Articles, Etc., Contributed to Scientific and
+other Journals by the Astronomers of the Lick Observatory since June~1, 1888.\\*[2ex]
+{\footnotesize \textsc{[Compiled by Mr.\ C.~B. Hill.]}}}
+\addcontentsline{toc}{subsection}{\qquad List of the Articles, etc., contributed to Scientific and other Journals by the Astronomers of the Lick Observatory since June~1, 1888. Compiled by \textsc{Charles B. Hill}}
+
+\nbsubsubsectionheading{\textit{Writings of Edward S.\ Holden.}}
+
+\compactlisttwo
+\item[]
+Hand-Book of the Lick Observatory. San Francisco, June, 1888.
+32\textsuperscript{o}, pp.~135. % transcriber's note: original appears to read "32�"
+\item[]
+Stellar Photography.---\textit{Overland Monthly}, June, 1888.
+\item[]
+Note on Earthquake Intensity in San Francisco, 1808--1888.---\textit{American
+Journal of Science}, June, 1888.
+\item[]
+The Total Solar Eclipse of 1889, January 1st, in California.---\textit{Monthly
+Notices Royal Astronomical Society}, vol.~48.
+%-----File: 039.png-----
+\item[]
+Occultation of 47 Libr�  by Jupiter, June~9, 1888.---\textit{Astronomical
+Journal}, vol.~8, p.~64.
+\item[]
+The Ring Nebula in Lyra.---\textit{Monthly Notices Royal Astronomical
+Society}, vol.~48, p.~383.
+\item[]
+Regarding Sir W. Herschel's observations of Volcanoes in the Moon.
+\textit{The Observatory}, 1888, p.~334.
+\item[]
+Earthquakes in California, Washington and Oregon, 1769--1888.
+Communicated to the \textit{California Academy of Sciences} in July, 1888.
+\item[]
+Sidereal Astronomy, Old and New. 2~papers.---\textit{The Century} for
+August and September, 1888.
+\item[]
+Occultation of a Star (11th magnitude) by Mars.---\textit{Astronomical
+Journal}, vol.~8, p.~102.
+\item[]
+Observations of the Lunar Eclipse of July~22, 1888, at the Lick Observatory
+of the University of California. Communicated to the
+\textit{National Academy of Sciences}. [By all the astronomers].
+\item[]
+Suggestions for Observing the Total Eclipse of the Sun on January~1,
+1889. (Printed by Authority of the Regents of the University of
+California). State Printing Office, Sacramento, 1888. 8vo, pamphlet.
+\item[]
+Hypothetical Parallax of Binary Pairs.---\textit{Sidereal Messenger}, October,
+1888, p.~356.
+\item[]
+Physical Observations of Mars during the Opposition of 1888, at the
+Lick Observatory. (With a plate).---\textit{Astronomical Journal}, vol.~8,
+p.~97.
+\item[]
+The Same.---\textit{Journal of Liverpool Astronomical Society}, vol.~7,
+November, 1888, p.~7, with plates.
+\item[]
+Saturn and his Satellites.---\textit{Sidereal Messenger}, January, 1889.
+\item[]
+Observations of Nebul�  at the Lick Observatory (by E.~S. Holden
+and J.~M. Schaeberle).---\textit{Monthly Notices Royal Astronomical
+Society}, vol.~48 (1888) p.~388.
+\item[]
+The Lick Observatory.---\textit{The Universal Review} (London), February
+15, 1889, (illustrated).
+\item[]
+Earthquakes in California (1888).---\textit{American Journal of Science},
+May, 1889, p.~392.
+\item[]
+On the Solar Eclipse of January~1, 1889.---\textit{Observatory}, March,
+1889, page~130; May, p.~221.
+\item[]
+The Lick Observatory.---\textit{Himmel und Erde} (Berlin; illustrated),
+May and June, 1889.
+\item[]
+On the Photographs of the Corona at the Solar Eclipse of January,~1,
+1889.---\textit{Monthly Notices Royal Astronomical Society}, vol.~49,
+p.~343.
+\item[]
+Reported Changes in the Rings of Saturn. (Observations by E.~S.
+Holden, J.~M. Schaeberle, J.~E. Keeler, E.~E. Barnard.)---\textit{Astronomical
+Journal}, vol.~8, p.~180.
+%-----File: 040.png-----
+\item[]
+Occultation of the Planet Jupiter, as observed at the Lick Observatory,
+March~23, 1889. (Observations by J.~E. Keeler, E.~E. Barnard,
+C.~B. Hill, A.~O. Leuschner.)---\textit{Sidereal Messenger}, May, 1889,
+p.~221.
+\item[]
+Address before the Astronomical Society of the Pacific ``On the Work
+of an Astronomical Society.''---\textit{Publications Astronomical Society
+of the Pacific}, No.~2, March~30, 1889.
+\item[]
+Reports on the Observations of the Total Solar Eclipse of January~1,
+1889. Published by the Lick Observatory, 8vo.
+\item[]
+Great Telescopes and their Work.---\textit{Observatory}, March, 1889, p.~138.
+\item[]
+Recent Discoveries in the Nebul�  by means of Photography.---\textit{Scientific
+American}, July~27, 1889.
+\item[]
+On the Helical Nebul�.---\textit{Publications Astronomical Society of the
+Pacific}, No.~3, July~27, 1889. Die Helikalischen Nebel.---\textit{Himmel
+und Erde}.
+\item[]
+Astronomical Photography.---\textit{The Pacific Review}, September, 1889.
+\end{list}
+
+\nbsubsubsectionheading{\textit{Writings of S.~W. Burnham.}}
+\compactlisttwo
+\item[]
+Double Star Observations made at the Lick Observatory.---\textit{Astronomische
+Nachrichten}, No.\ 2875.
+\item[]
+New Double Stars Discovered at the Lick Observatory.---\textit{Astronomical
+Journal}, vol.~8, p.~141.
+\item[]
+Companion to Sirius.---\textit{Astronomische Nachrichten}, No.~2884.
+\item[]
+The Trapezium of Orion.---\textit{Monthly Notices Royal Astronomical
+Society}, 1889, vol.~49, p.~352.
+\item[]
+The Double Star, $\epsilon$~Hydr�.---\textit{Sidereal Messenger}, May, 1889.
+\item[]
+New Double Star, $\alpha$~Urs�  Majoris.---\textit{Astronomische Nachrichten},
+No.~2891.
+\item[]
+Seventeen Com�  Berenices.---\textit{Observatory}, May, 1889, p.~227.
+\item[]
+Double Star Observations made with the 36-inch refractor of the Lick
+Observatory.---\textit{Astro\-nomische Nachrichten}, No.~---.
+\item[]
+$\eta$~Ophiuchi, $\theta$~Cygni.---\textit{Astronomische Nachrichten}, No.~2912.
+\end{list}
+
+\smallskip
+
+\nbsubsubsectionheading{\textit{Writings of J.~M. Schaeberle.}}
+\compactlisttwo
+\item[]
+Elements and Ephemeris of Barnard's Comet (e), 1888.---\textit{Astronomical
+Journal}, vol.~8, p.~102; \textit{Sidereal Messenger}, October, 1888,
+p.~357. Communicated to the \textit{California Academy of Sciences}.
+\item[]
+Orbit and Proper Motion of 85 Pegasi ($\beta$~733).---\textit{Astronomical
+Journal}, vol.~8, p.~129. Communicated to the \textit{California Academy
+of Sciences}.
+\item[]
+Elements and Ephemeris of Barnard's Comet (f), 1888.---\textit{Astronomical
+Journal}, vol.~8, p.~144; \textit{Sidereal Messenger}, December, 1888.
+Communicated to the \textit{California Academy of Sciences}.
+%-----File: 041.png-----
+\item[]
+Observations of Nebul�  at the Lick Observatory (by E.~S. Holden
+and J.~M. Schaeberle).---\textit{Monthly Notices Royal Astronomical
+Society}, vol.~48 (1888), p.~388.
+\item[]
+Meridian Observations of Polyhymnia and Harmonia.---\textit{Astronomische
+Nachrichten}, No.~2877.
+\item[]
+Corrections to the Lick Observatory Time Signals for December~30.0,
+December~31.0, January~1.0, and January~2.0.---\textit{Astronomical
+Journal}, vol.~8, p.~168.
+\item[]
+Elements and Ephemeris of Barnard's Comet (March~31). Communicated
+to the \textit{California Academy of Sciences}; telegraphed to
+\textit{Astronomical Journal}, and printed in vol.~8, pp.~183 and 191;
+\textit{Astronomische Nachrichten}, No.~2839. See also \textit{Astronomische
+Nachrichten}, No.~2903.
+\item[]
+Reports on the Solar Eclipse of January~1, 1889.---In \textit{Lick Observatory
+Reports}, p.~23.
+\end{list}
+
+\nbsubsubsectionheading{\textit{Writings of J.~E. Keeler.}}
+
+\compactlisttwo
+\item[]
+The 36-inch Equatorial of the Lick Observatory.---\textit{Scientific American},
+June~16, 1888.
+\item[]
+Recent Astronomical Work at the Lick Observatory.---\textit{Scientific
+American}, November~10, 1888.
+\item[]
+Observations of the Satellites of Mars.---\textit{Astronomical Journal}, No.~178,
+pp.~73--78.
+\item[]
+The Appearance of Saturn in the 36-inch Equatorial of the Lick
+Observatory.---\textit{Ciel et Terre}, No.~21, January, 1889, p.~514.
+\item[]
+The Outer Ring of Saturn.---\textit{Ciel et Terre}, No.~3, April, 1889.
+\textit{Astronomical Journal}, vol.~8, p.~175.
+\item[]
+Report on the Total Solar Eclipse of January~1, 1889.---In the \textit{Lick
+Observatory Report}, p.~31.
+\item[]
+On the Spectra of Saturn and Uranus.---\textit{Astronomische Nachrichten},
+No.~---.
+\end{list}
+
+\nbsubsubsectionheading{\textit{Writings of E.~E. Barnard.}}
+\compactlisttwo
+\item[]
+Discovery and Observations of a Comet (e~1888).---\textit{Astronomical
+Journal}, vol.~8, p.~102; \textit{Astronomische Nachrichten}, No.~2862.
+\item[]
+Drawings of Comet, 1888, I.---\textit{Astronomische Nachrichten}, No.~2859.
+(With a plate.)
+\item[]
+Discovery of a Comet (f, 1888).---\textit{Astronomical Journal}, vol.~8, p.~128. Communicated to \textit{California Academy of Sciences}.
+\item[]
+Observations of Olbers' Comet (1887, V).---\textit{Astronomische Nachrichten},
+No.~2861.
+\item[]
+Discovery and Observations of a Comet (f, 1888).---\textit{Astronomische
+Nachrichten}, No.~2871, p.~237; \textit{Astronomical Journal}, vol.~8,
+p.~134.
+\item[]
+Note on the Orbit of Comet (e), 1888.---\textit{Astronomical Journal}, vol.~8, p.~120.
+%-----File: 042.png-----
+\item[]
+On a Search for the Comet reported January~15, 1889, by
+\textsc{Mr.\ Brooks}.---\textit{Astronomical
+Journal}, vol.~8, p.~168.
+\item[]
+Partial Eclipse of the Moon, January~16, 1889.---\textit{Sidereal Messenger},
+March 1889, p.~137.
+\item[]
+Discovery and Observations of Comet Barnard (March~31).---\textit{Astronomical
+Journal}, vol.~8, p.~183; \textit{Astronomische Nachrichten}, No.\
+2894; \textit{Astronomical Journal}, vol.~9, p.~5; \textit{Astronomische Nachrichten},
+No.\ 2899; \textit{Astronomische Nachrichten}, No.\ 2901.
+\item[]
+Report on the Total Eclipse of January~1, 1889.---In the \textit{Lick Observatory
+Report}, p.~56.
+\item[]
+Observations of Faye's Comet.---\textit{Astronomische Nachrichten}, No.\ ---;
+\textit{Astronomical Journal}, vol.~9, p.~29.
+\item[]
+Anomalous Tail of Comet I, 1889.---\textit{Astronomical Journal}, vol.~9,
+p.~32; \textit{Astronomische Nachrichten}, No.\ 2906.
+\item[]
+The Nebula G.~C. 2091.---\textit{Monthly Notices Royal Astronomical
+Society}, vol.~49, p.~418.
+\item[]
+The Cluster G.~C. 1420, and the Nebula N.~G.~C. 2237. \textit{Astronomische
+Nachrichten}, No.\ ---.
+\item[]
+Discovery and Observations of a Comet (June~23).---\textit{Astronomische
+Nachrichten}, No.\ 2906; \textit{Astronomical Journal}, vol.~9, p.~47.
+\end{list}
+
+\nbsubsubsectionheading{\textit{Writings of C.~B. Hill.}}
+
+\compactlisttwo
+\item[]
+Observations of Comet, 1888, I.---\textit{Astronomische Nachrichten},
+No.\ 2877.
+\item[]
+Report on the Total Solar Eclipse of January~1, 1889.---In \textit{Lick
+Observatory Report}, p.~74.
+\end{list}
+
+\nbsubsubsectionheading{\textit{Writings of A.~O. Leuschner.}}
+
+\compactlisttwo
+\item[]
+Bahn des Cometen Barnard (Marz 31) aus Beobachtungen mit eintaegigen
+Zwischenzeiten nach v.\ Oppolzer's Methode.---\textit{Astro\-nom\-ische
+Nachrichten}, No.\ 2907.
+\item[]
+Reports on the Total Eclipse of January~1, 1889---In the \textit{Lick Observatory
+Report}, p.~81.
+\item[]
+Orbit of Comet Barnard (1889, June~23).---\textit{Astronomische Nachrichten},
+No.\ 2909; \textit{Astronomical Journal}, vol.~9, p.~40; \textit{Publications
+of the Astronomical Society of the Pacific}, No.~3.
+\end{list}
+\clearpage
+%-----File: 043.png-----
+
+\nbsectionheading{\textsc{Minutes of the Meeting of the Board of Directors, held
+July~27, 1889, at the Lick Observatory.}}
+\addcontentsline{toc}{section}{Minutes of the Meeting of the Board of Directors, held July~27, 1889}
+
+\begin{small}
+A quorum was present.
+
+The Committee on the Diploma was authorized to expend not to exceed \$50.
+
+It was \textit{Resolved}, That the \textsc{Publications of the Astronomical Society
+of the Pacific} be regularly sent to the following Observatories, etc., and that
+the Secretaries of the Society be instructed to notify them of this resolution, and to
+request that they exchange their publications with our own; and that the list of
+these Corresponding Societies and Observatories be printed in the \textsc{Publications
+of the Astronomical Society of the Pacific}:
+
+\addcontentsline{toc}{subsection}{\qquad List of Corresponding Observatories, Academies of Science, etc.}
+\compactlist
+\item[]  Dudley Observatory, Albany, New York.
+\item[]  Detroit Observatory, Ann Arbor, Michigan.
+\item[]  Royal Observatory, Berlin, Germany.
+\item[]  University Observatory, Bonn, Germany.
+\item[]  Royal Observatory, Brussels, Belgium.
+\item[]  University Observatory, Cambridge, England.
+\item[]  Harvard College Observatory, Cambridge, Massachusetts.
+\item[]  Royal Observatory, Capetown, Africa.
+\item[]  University Observatory, Cincinnati, Ohio.
+\item[]  University Observatory, Dorpat, Russia.
+\item[]  Royal Observatory, Greenwich, England.
+\item[]  Ducal Observatory, Karlsr�he, Germany.
+\item[]  University Observatory, Kasan, Russia.
+\item[]  University Observatory, Koenigsberg, Prussia.
+\item[]  Royal Observatory, Kopenhagen, Denmark.
+\item[]  University Observatory, Leiden, Holland.
+\item[]  University Observatory, Leipzig, Germany.
+\item[]  Royal Observatory, Milan, Italy.
+\item[]  Observatory, Melbourne, Australia.
+\item[]  University Observatory, Moscow, Russia.
+\item[]  Lick Observatory, Mount Hamilton, California.
+\item[]  Royal Observatory, Munich, Germany.
+\item[]  Carleton College Observatory, Northfield, Minnesota.
+\item[]  Radcliffe Observatory, Oxford, England.
+\item[]  Savilian Observatory, Oxford, England.
+\item[]  National Observatory, Paris, France.
+\item[]  Astrophysikalishes Institut, Potsdam, Germany.
+\item[]  Imperial Observatory, Pulkowa, Russia.
+\item[]  Observatory of the Roman College, Rome, Italy.
+\item[]  University Observatory, Stockholm, Sweden.
+\item[]  University Observatory, Strassburg, Germany.
+\item[]  McCormick Observatory, University of Virginia, Virginia.
+\item[]  Naval Observatory, Washington, District of Columbia.
+\item[]  Imperial Observatory, Vienna, Austro-Hungary.
+\item[]  Royal Astronomical Society, London, England.
+\item[]  Liverpool Astronomical Society, Liverpool, England.
+\item[]  Astronomical Society of France, Paris, France.
+\item[]  Astronomical Society, Chicago, Illinois.
+\item[]  Astronomical Society of Germany, Leipzig, Germany.
+\item[]  Gesellschaft Urania, Berlin, Germany.
+\item[]  National Academy of Sciences, Washington, District of Columbia.
+\item[]  Smithsonian Institution, Washington, District of Columbia.
+\item[]  California Academy of Sciences, San Francisco, California.
+\item[]  Bureau des Longitudes, Paris, France.
+\item[]  The Nautical Almanac, London, England.
+\item[]  The American Ephemeris, Washington, District of Columbia.
+\item[]  Berliner Jahrbuch, Berlin, Germany.
+\item[]  Library of the Mechanics Institute, San Francisco, California.
+\item[]  Library of Congress, Washington, District of Columbia.
+\item[]  Mercantile Library, San Francisco, California.
+%-----File: 044.png-----
+\item[]  Library of the University of California, Berkeley, California.
+\item[]  Chabot Observatory, Oakland, California.
+\item[]  Royal Observatory, Edinburgh, Scotland.
+\item[]  University Observatory, Cambridge, England.
+\item[]  Observatory, Nice, France.
+\item[]  Observatory, Marseilles, France.
+\item[]  Observatory, Bordeaux, France.
+\item[]  Observatory, Lyons, France.
+\item[]  Observatory, Toulouse, France.
+\item[]  Observatory, Kiel, Germany.
+\item[]  Observatory, Gotha, Germany.
+\item[]  Observatory, Hamburg, Germany.
+\item[]  Observatory of Geneva, Switzerland.
+\item[]  Observatory of Zurich, Switzerland.
+\item[]  Observatory of Berne, Switzerland.
+\item[]  Observatory of Neuch�tel, Switzerland.
+\item[]  Observatory of Madrid, Spain.
+\item[]  Observatory of Lisbon, Portugal.
+\item[]  Observatory of Naples, Italy.
+\item[]  Observatory of Palermo, Italy.
+\item[]  Observatory of Upsala, Sweden.
+\item[]  Observatory of Lund, Sweden.
+\item[]  Observatory of Christiania, Sweden.
+\item[]  Observatory of Helsingfors, Russia.
+\item[]  Observatory of Tacubaya, Mexico.
+\item[]  Observatory of Cordoba, Argentine Republic.
+\item[]  Observatory of Rio Janeiro, Brazil.
+\item[]  Observatory of Santiago, Chile.
+\item[]  Observatory of Madras, India.
+\item[]  Observatory of Sydney, New South Wales.
+\item[]  Observatory of Amherst College, Massachusetts.
+\item[]  Observatory of Clinton, New York.
+\item[]  Observatory of Georgetown, District of Columbia.
+\item[]  Observatory of Glasgow, Missouri.
+\item[]  Observatory of Hanover, New Hampshire.
+\item[]  Washburn Observatory, Madison, Wisconsin.
+\item[]  Winchester Observatory, New Haven, Connecticut.
+\item[]  Halstead Observatory, Princeton, New Jersey.
+\item[]  La Plata Observatory, La Plata, Argentine Republic.
+\item[]  Williams College Observatory, Williamstown, Massachusetts.
+\item[]  University Observatory, Tokio, Japan.
+\end{list}
+
+\bigskip
+
+\addcontentsline{toc}{subsection}{\qquad Action regarding the Comet Medal}
+
+{\stretchyspace Mr.\ \textsc{Holden} presented to the Board of Directors a communication from
+Hon.\ \textsc{Joseph A. Donohoe}, of Menlo Park, relating to the establishment of a
+comet medal, and it was
+
+\textit{Resolved}, That the Board of Directors recommends to the Society the acceptance
+of Mr.\ \textsc{Donohoe's} generous gift.
+
+}\textit{Resolved}, That on the acceptance of the gift by the Society, Mr.\ \textsc{Donohoe's}
+name be placed on the roll of Life-Members; that the \textit{Donohoe Fund for the
+maintenance of the Comet Medal of the Astronomical Society of the Pacific} be
+placed under the immediate charge of the Finance Committee; and that the
+Committee on the Comet Medal shall, until the next annual meeting, or until
+their successors are appointed, be composed as follows:
+
+The Director of the Lick Observatory, \textit{ex officio}, and of Messrs.\ \textsc{Schaeberle}
+and \textsc{Burckhalter} on the part of the Society.
+\smallskip
+
+\addcontentsline{toc}{subsection}{\qquad Amendment to Article VII of the By-Laws}
+It was \textit{Resolved}, That Article VII of the By-Laws of the Astronomical
+Society of the Pacific be amended so as to read as follows:
+
+\nbsubsubsectionheading{``\textsc{Article VII.}}
+
+``Candidates for membership may be proposed at any meeting of the Society
+and may be elected at the same meeting by unanimous consent of those present.
+In case of dissent of any one member, candidates so proposed shall be voted for
+at the next succeeding meeting. The vote shall be by ballot, and a majority of
+the members present shall be required for an election.''
+\smallskip
+%-----File: 045.png-----
+
+{\stretchyspace
+This was adopted by the consenting votes of nine members of the Board of
+Directors, namely: Messrs.\ \textsc{Alvord}, \textsc{Burckhalter}, \textsc{Gibbs}, \textsc{Grant}, \textsc{Holden},
+\textsc{Lowden}, \textsc{Molera}, \textsc{Pierson}, \textsc{Schaeberle}, and therefore takes the place of
+Article VII in the By-Laws as printed in Publications No.~1.
+
+}The printing of Publications No.~3 and the preparation of photo-lithographic
+plates to illustrate it and Publications No.~4, was ordered.
+
+The life-members whose names are marked with a star (*) in the list of members
+given in full in the minutes of the meeting of the Society July~27, were duly
+elected by the Board of Directors. Adjourned.
+
+\end{small}
+\bigskip
+\ThoughtBreakLong
+\bigskip
+
+\nbsectionheading{\textsc{Minutes of the Meeting of the Astronomical Society of the
+Pacific, held July~27, 1889, at the Lick Observatory}}
+\addcontentsline{toc}{section}{Minutes of the Meeting of the Society, July~27, 1889}
+
+\nbsubsubsectionheading
+{\footnotesize \textsc{[Prepared by the Secretaries for Publication.]}}
+
+\begin{small}
+The minutes of the meeting of May~25, 1889, were read and approved.
+
+Sixty-five persons were elected to membership under the provisions of the
+newly adopted Article VII of the By-Laws. For the convenience of the Society
+a full list of its present members is given below. This list includes the members
+elected at the present meeting. All are active members, except those whose
+names are marked with a star (*), to signify that they have been elected to life-membership.
+
+\medskip
+
+\nbsubsectionheading{LIST OF MEMBERS, JULY 27, 1889.}
+\addcontentsline{toc}{subsection}{\qquad List of Members}
+
+\begin{longtable}{@{}p{0.37\linewidth}@{} p{0.63\linewidth}@{}}
+\multicolumn{1}{c}{\tiny NAME.} & {\qquad\qquad\qquad \tiny ADDRESS.}\\
+T.~P. \textsc{Andrews},\dotfill & 529 Commercial Street, San Francisco, Cal.\\
+Hon.\ \textsc{Henry B. Alvord},*\dotfill & San Jose, Cal.\\
+Hon.\ \textsc{Wm.\ Alvord},*\dotfill & Bank of California, San Francisco, Cal.\\
+Mrs.\ \textsc{Wm.\ Alvord},*\dotfill & Palace Hotel, San Francisco, Cal.\\
+Director \textsc{Angel Anguiano},\dotfill & National Observatory, Tacubaya, Mexico.\\
+Dr.\ \textsc{Wm.\ Boericke},\dotfill & 834 Sutter Street, San Francisco, Cal.\\
+S.~W. \textsc{Burnham},\dotfill & Lick Observatory, Mt.\ Hamilton, Cal.\\
+E.~E. \textsc{Barnard},\dotfill & Lick Observatory, Mt.\ Hamilton, Cal.\\
+\textsc{Chas.\ Burckhalter},\dotfill & Chabot Observatory, Oakland, Cal.\\
+E.~M. \textsc{Bixley},\dotfill & 317 California Street, San Francisco, Cal.\\
+\textsc{John C. Bullock},\dotfill & 1626 Twelfth Street, Oakland, Cal.\\
+D.~P. \textsc{Belknap},\dotfill & 604 Merchant Street, San Francisco, Cal.\\
+Hon.\ \textsc{John H. Boalt},\dotfill & 332 Haight Street, San Francisco, Cal.\\
+H.~F. \textsc{Compton},\dotfill & 966 Chester Street, Oakland, Cal.\\
+Col.\ C.~F. \textsc{Crocker},\dotfill & 4th \& Townsend Streets, San Francisco, Cal.\\
+J.~C. \textsc{Cebrian},\dotfill & Pine \& Octavia Streets, San Francisco, Cal.\\
+J. \textsc{Costa},\dotfill & 406 Montgomery Street, San Francisco, Cal.\\
+E. \textsc{Bentley Church},\dotfill & 1036 Valencia Street, San Francisco, Cal.\\
+\textsc{Chas.\ S. Cushing},\dotfill & 1669 Thirteenth Street, Oakland, Cal.\\
+Dr.\ J. \textsc{Callandreau},\dotfill & 1307 Stockton Street, San Francisco, Cal.\\
+C.~H. \textsc{Clement},\dotfill & Livermore, Cal.\\
+Dr.\ W.~A. \textsc{Dewey},\dotfill & 834 Sutter Street, San Francisco, Cal.\\
+L.~L. \textsc{Dunbar, D.~D.~S.},\dotfill & 500 Sutter Street, San Francisco, Cal.\\
+Hon.\ \textsc{Joseph A. Donohoe},*\dotfill & Menlo Park, Cal.\\
+\textsc{Eugene Frost},\dotfill & Alameda, Cal.\\
+\textsc{Arthur W. Foster},*\dotfill & 322 Pine Street, San Francisco, Cal.\\
+Hon.\ \textsc{James G. Fair},*\dotfill & 230 Montgomery Street, San Francisco, Cal.\\
+T.~W. \textsc{Fenn},\dotfill & 319 California Street, San Francisco, Cal.\\
+\textsc{Andrew B. Forbes},*\dotfill & 401 California Street, San Francisco, Cal.\\
+\textsc{Robert D. Fry},*\dotfill & 1812 Jackson Street, San Francisco, Cal.\\
+\textsc{Chas.\ W. Friend},\dotfill & Carson City, Nevada.\\
+\textsc{Edmund Gray},\dotfill & 2925 Jackson Street, San Francisco, Cal.\\
+Dr.\ C.~L. \textsc{Goddard},\dotfill & 131 Post Street, San Francisco, Cal.\\
+\textsc{Chase Gitchell},\dotfill & 609 Sacramento Street, San Francisco, Cal.\\
+C.~P. \textsc{Grimwood},\dotfill & Fruitvale, Cal.\\
+%-----File: 046.png-----
+W.~C. \textsc{Gibbs},\dotfill & 303 California Street, San Francisco, Cal.\\
+C. \textsc{Mitchell Grant},\dotfill & 331 Kearny Street, San Francisco, Cal.\\
+\textsc{Adam Grant},*\dotfill & Bush \& Sansome Streets, San Francisco, Cal.\\
+\textsc{Joseph D. Grant},*\dotfill & Bush \& Sansome Streets, San Francisco, Cal.\\
+Capt.\ \textsc{Charles Goodall},*\dotfill & McAllister \& Pierce Sts., San Francisco, Cal.\label{cor1}\\ % corrected per corrigenda
+\textsc{Camilo Gonzalez},\dotfill & National Observatory, Tacubaya, Mexico.\\
+Hon.\ J.~M. \textsc{Gitchell},\dotfill & 609 Sacramento Street, San Francisco, Cal.\\
+C. \textsc{Webb Howard},*\dotfill & Pacific Union Club, San Francisco, Cal.\\
+Prof.\ E.~S. \textsc{Holden},\dotfill & Lick Observatory, Mt.\ Hamilton, Cal.\\
+C.~B. \textsc{Hill},\dotfill & Lick Observatory, Mt.\ Hamilton, Cal.\\
+\textsc{Wm.\ F. Herrick},\dotfill & 439 California Street, San Francisco, Cal.\\
+Dr.\ H.~W. \textsc{Harkness},\dotfill & California Academy of Sciences, \\
+ & cor.\ California \& Dupont Sts., San Francisco, Cal.\\
+F.~H. \textsc{Hausman},\dotfill & 328 Montgomery Street, San Francisco, Cal.\\
+Judge S.~G. \textsc{Hillborn},\dotfill & 401 California Street, San Francisco, Cal.\\
+\textsc{Horace L. Hill},*\dotfill & 314 California Street, San Francisco, Cal.\\ % corrected per corrigenda
+\textsc{Wm.\ Ireland},\dotfill & 301 California Street, San Francisco, Cal.\\
+J.~R. \textsc{Jarboe},\dotfill & 917 Pine Street, San Francisco, Cal.\\
+P.~R. \textsc{Jarboe},\dotfill & 917 Pine Street, San Francisco, Cal.\\
+E.~B. \textsc{Jordan},\dotfill & 581 Market Street, San Francisco, Cal.\\
+J.~H. \textsc{Johnson},\dotfill & 414 Buchanan Street, San Francisco, Cal.\\
+\textsc{James G. Jones},*\dotfill & Room 61, Flood Building, San Francisco, Cal.\\
+Hon.\ \textsc{John P. Jones},*\dotfill & Gold Hill, Nevada.\\
+Miss \textsc{Fidelia Jewett},\dotfill & San Francisco High School, San Francisco, Cal.\\
+J.~E. \textsc{Keeler},\dotfill & Lick Observatory, Mt.\ Hamilton, Cal.\\
+\textsc{Henry Kahn},\dotfill & 212 Kearny Street, San Francisco, Cal.\\
+O.~V. \textsc{Lange},\dotfill & 1025 Market Street, San Francisco, Cal.\\
+W.~H. \textsc{Lowden},\dotfill & 213 Sansome Street, San Francisco, Cal.\\
+Prof.\ \textsc{John Le Conte},\dotfill & Berkeley, Cal.\\
+A.~O. \textsc{Leuschner},\dotfill & Lick Observatory, Mt.\ Hamilton, Cal.\\
+W.~B. \textsc{Lewitt, M. D.},\dotfill & Cor.\ Hayes \& Laguna Streets, San Francisco, Cal.\\
+\textsc{Joseph G. Lavery},\dotfill & 410 California Street, San Francisco, Cal.\\
+Miss L.~J. \textsc{Martin},\dotfill & San Francisco High School, San Francisco, Cal.\\
+F.~H. \textsc{McConnell},\dotfill & 618 Market Street, San Francisco, Cal.\\
+E.~J. \textsc{Molera},\dotfill & 850 Van Ness Avenue, San Francisco, Cal.\\
+C.~F. \textsc{Montealegre},\dotfill & 230 California Street, San Francisco, Cal.\\
+\textsc{Alexander Montgomery},*\dotfill & N. W. cor.\ Leavenworth \& Vallejo Streets, San Francisco, Cal.\\
+Mrs.\ \textsc{Alexander Montgomery},*\dotfill & N. W. cor.\ Leavenworth \& Vallejo Streets, San Francisco, Cal.\\
+Hon.\ J.~W. \textsc{McClymonds},\dotfill & City Hall, Oakland, Cal.\\
+Hon.\ D.~O. \textsc{Mills},*\dotfill & 224 Montgomery Street, San Francisco, Cal.\\ % corrected per corrigenda
+Rev.\ \textsc{Robert Mackenzie},\dotfill & First Presbyterian Church, San Francisco, Cal.\\
+Hon.\ \textsc{Wm.\ Norris},\dotfill & 927 Bush Street, San Francisco, Cal.\\
+Miss \textsc{Rosa O'Halloran},\dotfill & 1511 Clay Street, San Francisco, Cal.\\
+W. \textsc{Letts Oliver},\dotfill & 1110 Twelfth Street, Oakland, Cal.\\
+\textsc{Sam.\ C. Partridge},\dotfill & 529 Commercial Street, San Francisco, Cal.\\
+\textsc{Wm.\ M. Pierson},\dotfill & 76 Nevada Block, San Francisco, Cal.\\
+Hon.\ T. \textsc{Guy Phelps},\dotfill & Belmont, Cal.\\
+Dr.\ S.~C. \textsc{Passavant},\dotfill & 306 Guerrero Street, San Francisco, Cal.\\
+Hon.\ \textsc{Geo.\ C. Perkins},*\dotfill & Oakland, Cal.\\
+\textsc{John Perry, Jr.}\dotfill & Occidental Hotel, San Francisco, Cal.\\
+\textsc{John Partridge},\dotfill & 214 California Street, San Francisco, Cal.\\
+Dr.\ \textsc{Geo.\ C. Pardee},\dotfill & 526 Montgomery Street, San Francisco, Cal.\\
+Se�or \textsc{Manuel G. Prieto},\dotfill & Tacubaya, Mexico.\\
+\textsc{Lawrence H. Pierson},\dotfill & Pacific Pine Lumber Co., San Francisco, Cal.\\
+\textsc{Feodoro Quintano},\dotfill & National Observatory, Tacubaya, Mexico.\\
+\textsc{Alfred P. Redington},\dotfill & 53 Stevenson Street, San Francisco, Cal.\\
+%-----File: 047.png-----
+\textsc{Geo.\ W. Reed},\dotfill & 506 Battery Street, care W.~B. Tyler, San Francisco, Cal.\\
+E.~W. \textsc{Runyon},\dotfill & 53 Stevenson Street, San Francisco, Cal.\\
+V.~J.~A. \textsc{Rey},\dotfill & 829 Union Street, San Francisco, Cal.\\
+A.~W. \textsc{Ross, Jr.},\dotfill & 224 California Street, San Francisco, Cal.\\
+Hon.\ \textsc{Arthur Rodgers},\dotfill & Nevada Block, San Francisco, Cal.\\
+Rev.\ J.~L. \textsc{Ricard},\dotfill & Santa Clara, Cal.\\
+\textsc{Lester L. Robinson},*\dotfill & 320 Sansome Street, San Francisco, Cal.\\
+\textsc{Francisco Rodriguez Rey},\dotfill & National Observatory, Tacubaya, Mexico.\\
+\textsc{Albert Raymond},\dotfill & 76 Nevada Block, San Francisco, Cal.\\
+J.~M. \textsc{Schaeberle},\dotfill & Lick Observatory, Mt.\ Hamilton, Cal.\\
+Prof.\ I. \textsc{Stringham},\dotfill & Berkeley, Cal.\\
+Prof.\ F. \textsc{Soul�},\dotfill & Berkeley, Cal.\\
+J.~M. \textsc{Selfridge},\dotfill & Oakland (Box 37), Cal.\\
+\textsc{John R. Spring},*\dotfill & 328 Montgomery Street, San Francisco, Cal.\\
+\textsc{George H. Strong},\dotfill & 220 Market Street, San Francisco, Cal.\\
+M.~J. \textsc{Sullivan, D.~D.~S.},\dotfill & 30 Post Street, San Francisco, Cal.\\
+A.~J. \textsc{Treat},\dotfill & 224 McAllister Street, San Francisco, Cal.\\
+W.~B. \textsc{Tyler},\dotfill & 506 Battery Street, San Francisco, Cal.\\
+\textsc{Edward G. Thomas},\dotfill & 234 Montgomery Street, San Francisco, Cal.\\
+C.~W. \textsc{Tiedeman},\dotfill & 312 Sixth Street, San Francisco, Cal.\\
+Hon.\ \textsc{Alfred L. Tubbs},*\dotfill & 611 Front Street, San Francisco, Cal.\\
+\textsc{Charles R. Tisdale},\dotfill & Alameda, Cal.\\
+\textsc{Jacob Voorsanger},\dotfill & 2316 California Street, San Francisco, Cal.\\
+\textsc{Rudolph E. Voight},\dotfill & 207 California Street, San Francisco, Cal.\\
+Se�or \textsc{Felipe Valle},\dotfill & National Observatory, Tacubaya, Mexico.\\
+Prof.\ J.~T. \textsc{Wallace},\dotfill & Highland Park, Oakland, Cal.\\
+R.~H. \textsc{White},\dotfill & 1216 Haight Street, San Francisco, Cal.\\
+J.~C.~L. \textsc{Wadsworth},\dotfill & Pacific-Union Club, San Francisco, Cal.\\
+\textsc{Charles G. Yale},\dotfill & 220 Market Street, San Francisco, Cal.\\
+F.~R. \textsc{Ziel},\dotfill & 410 California Street, San Francisco, Cal.\\
+\end{longtable}
+
+The list of presents received was read by the Secretary, and the thanks of
+the Society were voted to the donors. It was reported from the Committee on
+the Diploma that a design was now preparing and would soon be ready for
+examination. Also that designs for the comet medal had been sought for.
+
+\addcontentsline{toc}{subsection}{\qquad Note regarding Professor \textsc{Tacchini's} Work on the Solar Eclipses of 1870, 1882, 1883, 1886 and 1887}
+The attention of the members of the Society was called to the volume
+recently published by Professor \textsc{Tacchini}, in which he gives an account of his
+expeditions to observe the total solar eclipses of 1870, 1882, 1883, 1886 and 1887,
+together with many plates and illustrations. This volume has been prepared by
+Professor \textsc{Tacchini}, in order that the proceeds of its sale might be devoted to
+the erection of a suitable monument to the noted Italian astronomer, Padre
+\textsc{Secchi}. The work can be had through B.~\textsc{Westermann} \& Co. (Box 2306,
+New York City), at a cost of about \$2.
+
+\addcontentsline{toc}{subsection}{\qquad Telegram of Congratulation to Director \textsc{Otto v. Struve}}
+It was also \textit{Resolved}, That the Astronomical Society of the Pacific will join
+with the Astronomers of the Lick Observatory in sending a telegram of greeting
+and congratulation to Director \textsc{Otto v.\ Struve}, on August~19, 1889, the fiftieth
+anniversary of the founding of the Pulkowa Observatory and of Director
+\textsc{Struve's} official connection with it.
+
+\addcontentsline{toc}{subsection}{\qquad The Comet Medal of the Astronomical Society of the Pacific founded by Hon.\  \textsc{Joseph A. Donohoe}}
+A communication from the Hon.\ \textsc{Joseph A. Donohoe}, of Menlo Park, was
+presented to the Society by Mr.\ \textsc{Holden}. In this communication Mr.\ \textsc{Donohoe}
+offers to establish a perpetual fund to provide for the bestowal of a medal of
+bronze upon the actual discoverer of each new comet according to the provisions
+hereafter given.
+
+Mr.\ \textsc{Donohoe} will provide the necessary dies for the medal, and will present
+to the Society ten finished medals, and also an invested fund of \$500 to be known
+as the \textit{Donohoe Fund for the Maintenance of the Comet Medal of the Astronomical
+Society of the Pacific}. The conditions of the gift follow:
+
+\end{small}
+%-----File: 048.png-----
+
+\addcontentsline{toc}{subsubsection}{\qquad \qquad Rules governing its bestowal}
+\begin{center}
+\textsc{Comet Medal of the Astronomical Society of the Pacific.}
+\end{center}
+
+I\@. A medal of bronze is established as a perpetual foundation to
+be given for the discovery of comets as follows:
+
+The medal is to bear on the obverse the effigy of a bright comet
+among stars, with the legend ``\textit{Astronomical Society of the Pacific}''
+around the border; and on the reverse the inscription ``\textit{This medal,
+founded in 1890 by Joseph A. Donohoe, is presented to} \rule[0.5ex]{1cm}{0.5pt} [the
+name of the discoverer] \textit{to commemorate the discovery of a comet}
+\rule[0.5ex]{1cm}{0.5pt} [the date].''
+
+It is to be understood that this medal is intended solely as a
+recognition of merit, and not as a reward.
+
+II\@. The medal will be given to the actual discoverer of any unexpected
+comet, when the discovery is made in the course of regular
+astronomical occupations; and to that observer of any telescopic
+periodic comet who obtains and promptly publishes the first precise
+determination of its position at any one of its expected returns.
+
+III\@. The discoverer is to make his discovery known in the usual
+way; and he must also address a letter, giving his first observation,
+to the Director of the Lick Observatory, by the first mail after the
+discovery. This letter must state the exact time of the discovery, the
+position of the comet, the direction of its motion (when this can be
+determined), and the physical appearance of the object.
+
+If the observations of one night are not sufficient to settle all
+these points, the discovery must nevertheless be communicated as
+prescribed, and a second letter can be sent, giving the missing items
+of information, when they are obtained. The expectation of obtaining
+a second observation will never be received as a reason for
+postponing the communication of the first one. No application for
+the bestowal of the medal is required. The letters received from
+discoverers of comets will be preserved in the records of the Lick
+Observatory. Cable telegrams to the Lick Observatory are to be
+addressed to ``Astronomer, San Francisco.''
+
+IV\@. All such communications will be referred to a committee
+consisting of the Director of the Lick Observatory, \textit{ex officio}, and of
+two other persons, members of the Astronomical Society of the
+Pacific, who are to be annually appointed by the Board of Directors.
+The decisions of this committee are to be final upon all points
+relating to the award of the medal. The committee will print an
+annual statement of its operations in the Publications of the Society.
+
+Under ordinary circumstances the medal for the discovery of a
+%-----File: 049.png-----
+comet will be awarded within two months after the receipt of the
+letter of the discoverer which contains the record of his first observation.
+In cases of doubt a longer period may elapse. The medal
+will not be awarded (unless under the most exceptional circumstances)
+for the discovery of a comet until enough observations are
+secured (by the discoverer or by others) to permit the calculation
+and the verification of its orbit.
+
+V\@. This medal is to be a perpetual foundation from and after
+January~1, 1890.
+
+\medskip
+
+\begin{small}
+It was, on the recommendation of Board of Directors,
+
+\addcontentsline{toc}{subsubsection}{\qquad \qquad Formal Acceptance of the gift of Mr.\ \textsc{Donohoe}}
+\textit{Resolved}, That the Astronomical Society of the Pacific accepts the generous
+gift of Mr.\ \textsc{Donohoe} under the conditions named by him, and
+
+\textit{Resolved}, That the Secretaries of the Society be instructed to notify Mr.\ \textsc{Donohoe}
+of the acceptance of the Society, and to assure him that his gift is certain
+to promote and encourage the discovery and observation of comets, not only
+now, but always.
+
+By a vote of the Directors Mr.\ \textsc{Donohoe's} name has been placed on the roll
+of life-members.
+
+\addcontentsline{toc}{subsection}{\qquad The Lick Observatory Eclipse Expedition (December~21, 1889), sent at the cost of Hon. C.~F. \textsc{Crocker}}
+It was also announced to the Society that Hon.\ C.~F. \textsc{Crocker}, a member
+of the Society, had generously offered to bear the expense of sending an expedition
+from the Lick Observatory to Cayenne, South America, to observe the total
+solar eclipse of December~21, 1889. The Regents of the University have authorized
+Messrs.\ \textsc{Burnham} and \textsc{Schaeberle} to take part in this work, and to use
+such instruments of the Lick Observatory as may be useful. Mr.\ F.~G. \textsc{Blinn},
+of Oakland, and Captain R.~L. \textsc{Phythian}, U.~S. Navy, Superintendent of the
+U.~S. Naval Observatory at Washington, have also materially aided the expedition
+by the loan of instruments and apparatus. Messrs.\ \textsc{Burnham} and
+\textsc{Schaeberle} will probably leave California about November 1st, and arrive
+at Cayenne about December~1st, 1889. The eclipse will be observed at Cayenne
+by an English party under Rev.\ S.~J. \textsc{Perry}, F.~R.~S., Director of the Stonyhurst
+College Observatory, and in Africa by two parties, one under Professor
+D.~P. \textsc{Todd}, of Amherst College, the other under Mr.\ \textsc{Taylor}, F.~R.~A.~S.,
+Assistant in the Private Observatory of Mr.\ A.~A. \textsc{Common}, F.~R.~S., of London.
+
+Papers were then read to the Society by Mr.\ \textsc{Keeler}, on the photography
+of the Corona in full sunshine, etc.; by Mr.\ \textsc{Leuschner}, on the orbit of comet
+Barnard (June~23); by Mr.\ \textsc{Hill}, on occultations of \textit{Jupiter} during 1889; by Mr.\ \textsc{Holden},
+on the Helical Nebul�. These papers are printed in full or in abstract
+in the preceding pages.
+
+Mr.\ \textsc{Barnard} exhibited a beautiful negative of a portion of the Milky Way
+(R.~A. 18h.\ 11m., Dec., 20� S.) near \textit{Jupiter}, which he took on July~24, with
+the Willard photographic lens of the Lick Observatory,\footnote{Bought by Hon.\ C.~F. \textsc{Crocker} for the expedition to observe the eclipse of December
+21, 1889.}
+giving an exposure
+of 1h.\ 48m.
+
+The Society then adjourned to meet at the Lick Observatory September~28, 1889.
+%-----File: 050.png-----
+
+\nbsectionheading{OFFICERS OF THE SOCIETY}
+\addcontentsline{toc}{section}{List of Officers, etc.}
+\noindent
+\begin{tabular*}{\textwidth}{@{\extracolsep{\fill}}lcr}
+\textsc{Edward S. Holden} (Lick Observatory),
+&& \textit{President}\\
+\textsc{Wm.~M. Pierson} (76 Nevada Block, S.~F.),
+&\multirow{3}{1em}{\Bigg\}}&\\
+\textsc{W.~H. Lowden} (213 Sansome Street, S.~F.)
+&& \textit{Vice-Presidents}\\
+\textsc{Frank Soul�} (Students' Observatory, Berkeley),&&\\
+\textsc{Chas. Burckhalter} (Chabot Observatory, Oakland),
+&\multirow{2}{1em}{\Big\}}
+&\multirow{2}{5em}{\textit{Secretaries}}\\
+\textsc{J.~M. Schaeberle} (Lick Observatory),&&\\
+\textsc{E.~J. Molera} (850 Van Ness Avenue, S.~F.),
+&& \textit{Treasurer}
+\end{tabular*}
+
+\compactlisttwo\stretchyspace
+\item[] \textit{Board of Directors}---Messrs.\ \textsc{Alvord}, \textsc{Boericke}, \textsc{Burckhalter}, \textsc{Gibbs},
+\textsc{Grant}, \textsc{Holden}, \textsc{Lowden}, \textsc{Molera}, \textsc{Pierson}, \textsc{Schaeberle}, \textsc{Soul�}.
+\item[] \textit{Finance Committee}---Messrs.\ \textsc{Gibbs}, \textsc{Pierson}, \textsc{Molera}.
+\item[] \textit{Committee on Publication}---Messrs.\ \textsc{Dewey}, \textsc{Treat}, \textsc{Ziel}.
+\item[] \textit{Committee on the Comet Medal}---Messrs.\ \textsc{Holden} (\textit{ex officio}), \textsc{Schaeberle},
+\textsc{Burckhalter}.
+\end{list}
+
+\ThoughtBreak
+
+\nbsectionheading{NOTICE.}
+
+Members are requested to preserve the copies of the Publications of the
+Society as sent to them. At certain intervals a title page and index of the preceding
+numbers will also be sent to the members, who can then bind the numbers
+together into a volume.
+
+The titles of papers for reading should be communicated to either of the
+Secretaries as early as possible.
+
+Those members who propose to attend any or all of the meetings at Mount
+Hamilton during the summer should communicate with Mr.\ \textsc{Burckhalter}, at
+the rooms of the Society, 408 California Street, San Francisco, in order that
+arrangements may be made for transportation, lodging, etc.
+\vfil
+\[
+  \includegraphics{images/fig4.jpg}
+\]
+
+\end{small}
+
+%-----File: 051.png-----
+
+\nbchapterheading
+\nbchapterbanner{No.\ 4.}{San Francisco, California, September~28, 1889.}
+\nbchaptertoc{No.\ 4. (September~28, 1889).}
+
+\nbsectionheading{ON THE PHOTOGRAPHIC BRIGHTNESS OF THE FIXED STARS.}
+\addcontentsline{toc}{section}{On the Photographic Brightness of the Fixed Stars. By \textsc{J.~M. Schaeberle}}
+
+\nbsubsubsectionheading{\shortrule\\*
+\textsc{By J.~M. Schaeberle, Astronomer of the Lick Observatory.}\\*
+\shortrule}
+
+The investigations relating to the photographic brightness of the
+fixed stars contained in this paper were made with the aid of an
+equatorially mounted \textsc{Dallmeyer} portrait-lens of 6\textsuperscript{in}.05 aperture,
+loaned to this Observatory by the U.~S.~N. Observatory for the purpose
+of photographing the next total solar eclipse at Cayenne, South
+America.
+
+Professor \textsc{Holden} placed this instrument in my charge, and
+requested me to make a series of experiments on atmospheric absorption
+of the light, and on the photographic brightness, of the fixed
+stars, so that the extended work of the same character which it is
+intended to execute in South America could be more intelligently
+and profitably performed.
+
+The photographic focus was carefully determined by making
+several series of short exposures, and trails, of bright stars both inside
+and outside of the adopted position of the plate. The position of
+the plate for each setting was read off on a scale which I cut on the
+tube. All the exposures were made on $4�5$ Seed~26 plates.\label{cor2} % corrected per corrigenda
+
+Leaving the work relating to atmospheric absorption to a future
+paper, let us consider the subject of the photographic brightness of
+stars as determined by the dimensions of their circular images on the
+sensitive plate. (As the dimensions---widths---of the trails could only
+be accurately determined for the brighter stars, I finally avoided
+examining trails for this special investigation.)
+
+As the whole subject was comparatively new to me, several weeks
+were spent in work of an experimental character. A careful study
+of the data given on the exposed plate was made with the aid of our
+excellent measuring engine. I finally came to the conclusion that
+the diameter of the image of an ``over-exposed'' star could be used
+%-----File: 052.png-----
+to determine the star's brightness with accuracy. To find the law
+of variation of the diameter of the photographic image for a variation
+of both the aperture of the objective and the time of exposure, seven
+different stops, varying in diameter from 5.41 inches to 1.91 inches,
+were used, and exposures of 1\textsuperscript{s}, 2\textsuperscript{s},
+ 4\textsuperscript{s}, 8\textsuperscript{s}, 16\textsuperscript{s},
+ 32\textsuperscript{s}, 64\textsuperscript{s}, and 128\textsuperscript{s} duration
+made for each stop. In order to be sure of the effective
+aperture of the stops, they were placed centrally in front of the
+objective, and not in the usual place between the lenses. The
+diameters of these stops, which we will number 1, 2, 3, etc., are as
+follows:
+\begin{tablesetup}
+\begin{tabular}{c | c | c | c | c | c | c | c}
+\hline \hline
+  No. &\footnotesize 1 &\footnotesize 2 &\footnotesize 3 &\footnotesize 4
+      &\footnotesize 5 &\footnotesize 6 &\footnotesize 7 \\
+  \hline
+  &\footnotesize in. &\footnotesize in. &\footnotesize in. &\footnotesize in.
+  &\footnotesize in. &\footnotesize in. &\footnotesize in. \\
+Diameter \ldots & 5.41 & 4.59 & 3.81 & 3.31 & 2.72 & 2.31 & 1.91 \\ \hline
+\end{tabular}
+\end{tablesetup}
+
+The figures in the following table give the diameters of the
+images of \textit{Polaris}, in inches, as measured on one of the plates:
+
+\begin{tablesetup}
+\begin{tabular}{cr@{}l | r | r | r | r | r | r | r}
+\multicolumn{10}{c}{\textit{\textsc{Polaris}}}
+\\ \hline \hline
+\multicolumn{3}{c|}{\footnotesize \textsc{Exposure}}
+& \multicolumn{7}{c}{\footnotesize \textsc{Diameters of Image for different Stops and Times.}}
+\\ \cline{4-10}
+\multicolumn{3}{c|}{\footnotesize \textsc{Times.} }
+  & \multicolumn{1}{c|}{\footnotesize 1}
+  & \multicolumn{1}{c|}{\footnotesize 2}
+  & \multicolumn{1}{c|}{\footnotesize 3}
+  & \multicolumn{1}{c|}{\footnotesize 4}
+  & \multicolumn{1}{c|}{\footnotesize 5}
+  & \multicolumn{1}{c|}{\footnotesize 6}
+  & \multicolumn{1}{c }{\footnotesize 7}
+\\ \hline
+&&& \multicolumn{1}{c|}{\footnotesize in.}
+  & \multicolumn{1}{c|}{\footnotesize in.}
+  & \multicolumn{1}{c|}{\footnotesize in.}
+  & \multicolumn{1}{c|}{\footnotesize in.}
+  & \multicolumn{1}{c|}{\footnotesize in.}
+  & \multicolumn{1}{c|}{\footnotesize in.}
+  & \multicolumn{1}{c}{\footnotesize in.}
+\\
+&   1&\textsuperscript{s}
+  & 0.0048 & 0.0049 & 0.0049 & 0.0048 & 0.0045 & 0.0041 & 0.0036\\
+&   2&
+  &  58 &  57 &  59 &  52 &  47 &  45 & 37 \\
+&   4&
+  &  68 &  66 &  58 &  59 &  57 &  55 & 40 \\
+&   8&
+  &  78 &  74 &  70 &  72 &  40 & --- & 48 \\
+&  16&
+  &  81 & --- &  72 &  64 &  56 &  52 & 50 \\
+&  32&
+  &  92 &  72 &  74 &  76 &  65 &  61 & 53 \\
+&  64&
+  & 116 &  90 &  91 &  86 &  78 &  68 & 59 \\
+& 128&
+  & 139 & 117 & 102 &  96 &  84 &  78 & 67 \\
+\hline
+\end{tabular}
+\end{tablesetup}
+
+I tried to represent these numbers by various equations of the
+second and third degrees as functions of the aperture and time, but
+finally concluded that they could only be represented by an equation
+of the $n^\text{th}$ degree, or, in other words, that the logarithms of the variables
+enter into the equation. I then made a similar set of exposures,
+using $\alpha$~\textit{Lyr�} (discussed further on), and found that the function
+which represented the diameters was of precisely the same form. I
+%-----File: 053.png-----
+have deduced the following general expression for the diameter of
+the photographic image of a star:
+\[
+d = \alpha + \beta\centerdot\log{D} + \gamma\centerdot D\centerdot\log{t}     \tag{1}
+\]
+In which, for a given star,
+\medskip
+
+\begin{tablesetup}
+\begin{tabular}{ r@{\ } *{10}{c@{\ }} }
+$d =$ &\multicolumn{10}{l}{\hspace{-5pt}\footnotesize
+the measured diameter of the photographic image;}
+\\
+$\alpha =$ &\footnotesize  a &\footnotesize  constant
+&\footnotesize  depending &\footnotesize  only on
+&\footnotesize  the &\footnotesize  sensitive
+&\footnotesize  plate &\footnotesize  and the
+&\footnotesize  atmospheric &\footnotesize  state;
+\\
+$\beta = $ && `` & `` & `` && `` & `` & `` & `` & ``  \\
+$\gamma =$ && `` & `` & `` && `` & `` & `` & `` & ``
+\\
+$D =$ &\multicolumn{10}{l}{\hspace{-5pt}\footnotesize
+the effective diameter of the objective (stop);}
+\\
+$t =$ &\multicolumn{10}{l}{\hspace{-5pt}\footnotesize
+the time of exposure expressed in seconds.}
+\end{tabular}
+\end{tablesetup}
+\medskip
+
+\noindent In order to determine the most probable values of $\alpha$, $\beta$, and $\gamma$ for a
+particular case it will be more convenient to place
+\begin{align*}
+\alpha + \beta\log{D} &= a   \tag{2}\\
+\gamma D &= b    \tag{3}
+\end{align*}
+Equation (1) then becomes
+\[
+d = a + b\log{t}     \tag{4}
+\]
+
+In selecting the unit for $D$ it must be remembered that with a
+small stop the images, for comparatively short exposures, are small
+and faint. Greater accuracy may therefore be expected from large
+apertures. I have accordingly chosen six inches (6\textsuperscript{in}) as the unit of
+$D$. The diameters of the stops in terms of this unit are therefore
+as given below:
+
+\begin{tablesetup}
+\begin{tabular}{l*{7}{|r@{.}l}}
+\hline \hline
+  \multicolumn{1}{c|}{\footnotesize\textsc{Stop.}}
+& \multicolumn{2}{c|}{\footnotesize 1}
+& \multicolumn{2}{c|}{\footnotesize 2}
+& \multicolumn{2}{c|}{\footnotesize 3}
+& \multicolumn{2}{c|}{\footnotesize 4}
+& \multicolumn{2}{c|}{\footnotesize 5}
+& \multicolumn{2}{c|}{\footnotesize 6}
+& \multicolumn{2}{c}{\footnotesize 7}
+\\ \hline
+Diameter \ldots & 0&902 & 0&765 & 0&635 & 0&552 & 0&453 & 0&385 & 0&318 \\ \hline
+Log.\ of Diam. & -0&045 & -0&116 & -0&197 & -0&258 & -0&344 & -0&415 & -0&498 \\ \hline
+\end{tabular}
+\end{tablesetup}
+
+Equation (1) shows that when $t = 1^\text{s}$ and $D = 6^\text{in}$, we have
+$d = \alpha$; in other words, $\alpha$ is the diameter of the photographic image
+of the star for an aperture of six inches and an exposure time of one
+second.
+
+Taking \textit{Polaris} for the standard star, the above-measured diameters
+give the following values for $a$ and $b$ as found by the method
+of least squares; each equation of condition being of the form:
+\[
+d = a + b\log{t}
+\]
+%-----File: 054.png-----
+
+\begin{tablesetup}
+\begin{tabular}{c | r | r}
+\hline \hline
+\footnotesize\textsc{Stop.} & \multicolumn{1}{c|}{$a$} & \multicolumn{1}{c}{$b$} \\ \hline
+ & \multicolumn{1}{c|}{\footnotesize in.} & \multicolumn{1}{c}{\footnotesize in.} \\
+1 & 0.0051 & 0.0032 \\
+2 & 53 & 22 \\
+3 & 51 & 19 \\
+4 & 46 & 22 \\
+5 & 43 & 15 \\
+6 & 43 & 13 \\
+7 & 36 & 12 \\
+\hline
+\end{tabular}
+\end{tablesetup}
+
+To find the value of $\alpha$ and $\beta$ we have the following equations of
+condition
+\begin{tablesetup}
+\begin{tabular}{l@{ $-$ }r@{.}l@{ = }r@{.}l}
+$\alpha$ & $0^\text{in}$&$045\, \beta$& $0^\text{in}$&0051\\
+$\alpha$ & &$116\, \beta$& &0053\\
+$\alpha$ & &$197\, \beta$& &0051\\
+$\alpha$ & &$258\, \beta$& &0046\\
+$\alpha$ & &$344\, \beta$& &0043\\
+$\alpha$ & &$415\, \beta$& &0043\\
+$\alpha$ & &$498\, \beta$& &0036
+\end{tabular}
+\end{tablesetup}
+The solution of which by the method of least squares gives for
+values of $\alpha$ and $\beta$
+\[
+\alpha = 0^\text{in}.0055 \qquad\qquad \beta = 0^\text{in}.0033
+\]
+The diameter of the photographic image of \textit{Polaris} for six inches
+aperture and one second exposure is therefore, for this particular
+case, $0^\text{in}.0055$.
+
+The independent values of $\gamma$ given by the expression $\gamma = \dfrac{b}{D}$ are
+
+\begin{tablesetup}
+\begin{tabular}{r | r | r@{ }c@{ }l@{ }l}
+\hline \hline
+\multicolumn{1}{c|}{$b$} & \multicolumn{1}{c|}{$D$} & \multicolumn{4}{c}{$\gamma$} \\ \hline
+\multicolumn{1}{c|}{\footnotesize in.} & & \multicolumn{1}{c}{\footnotesize in.} & & & \\
+0.0032 & 0.902 & 0.0035 & from & 8 different exposures with Stop &1\\
+22 & .765 & 0029 & `` & 7 ditto &2\\
+19 & .635 & 0030 & `` & 8 ditto &3\\
+22 & .552 & 0040 & `` & 8 ditto &4\\
+15 & .453 & 0033 & `` & 8 ditto &5\\
+13 & .385 & 0034 & `` & 7 ditto &6\\
+12 & .318 & 0038 & `` & 8 ditto &7\\ \hline
+\end{tabular}
+\end{tablesetup}
+%-----File: 055.png-----
+Taking the mean of the values of $\gamma$, we have for the images of \textit{Polaris}
+the equation
+\[
+d = 0^\text{in}.0055 + 0.0033\log{D} + 0.0034 D \log{t}    \tag{5}
+\]
+The residuals obtained by subtracting the diameters computed by
+the above formula from the measured diameters are as follows:
+\begin{tablesetup}
+\begin{tabular}{cr@{}l *{7}{|c@{\,}r@{.}l}}
+\multicolumn{24}{c}{\large\textit{\textsc{Polaris.}}} \\ \hline \hline
+\multicolumn{3}{c|}{\footnotesize\textsc{Exposure}} & \multicolumn{21}{c}{\footnotesize\textsc{Observation---Computation.}} \\ \cline{4-24}
+\multicolumn{3}{c|}{\footnotesize\textsc{Time.}}
+& \multicolumn{3}{c|}{\footnotesize 1}
+& \multicolumn{3}{c|}{\footnotesize 2}
+& \multicolumn{3}{c|}{\footnotesize 3}
+& \multicolumn{3}{c|}{\footnotesize 4}
+& \multicolumn{3}{c|}{\footnotesize 5}
+& \multicolumn{3}{c|}{\footnotesize 6}
+& \multicolumn{3}{c}{\footnotesize 7}
+\\ \hline
+&& & \multicolumn{3}{c|}{\footnotesize in.}
+& \multicolumn{3}{c|}{\footnotesize in.}
+& \multicolumn{3}{c|}{\footnotesize in.}
+& \multicolumn{3}{c|}{\footnotesize in.}
+& \multicolumn{3}{c|}{\footnotesize in.}
+& \multicolumn{3}{c|}{\footnotesize in.}
+& \multicolumn{3}{c}{\footnotesize in.}
+\\
+& $1$&\textsuperscript{s} &$-$&0&0005 &$-$&0&0002 & &0&0000 &+&0&0001 &+&0&0001 & &0&0000 &$-$&0&0003 \\
+&   2& &$-$& &0005 &$-$& &0002 &+& &0004 & & &0000 &$-$& &0001 & & &0000 &$-$& &0004 \\
+&   4& &$-$& &0004 &$-$& &0001 &$-$& &0004 &$+$& &0001 &$+$& &0004 &$+$& &0006 &$-$& &0005 \\
+&   8& &$-$& &0003 &$-$& &0001 &$+$& &0002 &$+$& &0008 & \multicolumn{3}{c|}{------} & \multicolumn{3}{c|}{------} & & &0000 \\
+&  16& &$-$& &0009 & \multicolumn{3}{c|}{------} &$-$& &0003 &$-$& &0005 &$-$& &0004 &$-$& &0005 &$-$& &0002 \\
+&  32& &$-$& &0008 & \multicolumn{3}{r|}{(0018)} &$-$& &0007 &$+$& &0001 & & &0000 & & &0000 &$-$& &0001 \\
+&  64&  &$-$& &0007 &$-$& &0008 &$+$& &0003 &$+$& &0006 &$+$& &0008 &$+$& &0003 &$+$& &0001 \\
+& 128&  &$-$& &0020 &$-$& &0011 &$+$& &0008 &$+$& &0010 &$+$& &0010 &$+$& &0009 &$+$& &0006 \\ \hline
+\end{tabular}
+\end{tablesetup}
+\medskip
+The diameters of the images of $\alpha$ \textit{Lyr�} on a plate exposed Sept.\ 2,
+are as follows:
+\begin{tablesetup}
+\begin{tabular}{cr@{}l *{7}{|r}}
+\multicolumn{10}{c}{\large$\alpha$ \textit{\textsc{Lyr�.}}} \\ \hline \hline
+\multicolumn{3}{c|}{\footnotesize\textsc{Exposure}}
+& \multicolumn{7}{c}{\footnotesize \textsc{Diameters of Images for different Stops and Times.}}
+\\ \cline{4-10}
+\multicolumn{3}{c|}{\footnotesize\textsc{\footnotesize Time.}}
+& \multicolumn{1}{c|}{\footnotesize 1}
+& \multicolumn{1}{c|}{\footnotesize 2}
+& \multicolumn{1}{c|}{\footnotesize 3}
+& \multicolumn{1}{c|}{\footnotesize 4}
+& \multicolumn{1}{c|}{\footnotesize 5}
+& \multicolumn{1}{c|}{\footnotesize 6}
+& \multicolumn{1}{c}{\footnotesize 7}
+\\ \hline
+& $1$&\textsuperscript{s} &0.0093 &0.0088 &0.0073 &0.0061 &0.0055 &0.0046 &0.0045 \\
+&  2 & &114 &91 &--- &70 &63 &55 &48 \\
+&  4 & &123 &96 &--- &80 &70 &--- &57 \\
+&  8 & &148 &107 &102 &109 &80 &71 &66 \\
+& 16 & &\tablenoteasterisk \quad --- &125 &114 &114 &88 &--- &72 \\
+& 32 & &\tablenoteasterisk \quad --- &146 &133 &122 &104 &--- &83 \\
+& 64 & &\tablenoteasterisk \quad --- &169 &151 &145 &119 &--- &--- \\ \hline
+\end{tabular}
+\end{tablesetup}
+
+\begin{footnotesize}* In this table, as in the one for \textit{Polaris}, the missing figures belong to cases in which the
+images, on account of imperfect pointing, are not circular but elongated; while for stop 1 the
+images are so close together that the larger ones overlap, and, consequently, were not used.
+
+\end{footnotesize}
+
+\medskip
+%-----File: 056.png-----
+
+The equation which fairly represents these diameters is:
+\[
+d = 0^\text{in}.0070 + 0^\text{in}.0050\log D + 0.0074 D\log{t}   \tag{6}
+\]
+the individual values of $\gamma$, found by dividing each $b$ by
+the corresponding $D$, are:
+\begin{tablesetup}
+\begin{tabular}{r@{ }c@{ }l@{ }c@{ }r}
+  \multicolumn{1}{c}{\footnotesize $b$} & {\footnotesize $\div$}
+& \multicolumn{1}{c}{\footnotesize $D$} & {\footnotesize $=$}
+& \multicolumn{1}{c}{\footnotesize $\gamma$}\\
+0.0067 & $\div$ & .902 & = & 0.0074 \\
+46 & &.765 & &.0060 \\
+42 & &.635 & &.0066 \\
+46 & &.552 & &.0083 \\
+34 & &.453 & &.0075 \\
+30 & &.385 & &.0078 \\
+27 & &.318 & &.0085
+\end{tabular}
+\end{tablesetup}
+The observed values of $d$, minus the values computed by equation
+(6), are as given below:
+\begin{tablesetup}
+\begin{tabular}{c r@{}l *{7}{|r@{\,}r@{.}l}}
+\multicolumn{24}{c}{\large$\alpha$ \textit{\textsc{Lyr� .}}} \\
+\hline \hline
+\multicolumn{3}{c|}{
+  \multirow{2}{5em}[-1ex]{\centering\textsc{Exposure Time.}}}
+& \multicolumn{21}{|c}{\textsc{\rule{0pt}{3ex} Observation---Computation.}}
+\\[1ex]
+\cline{4-24}
+&&& \multicolumn{3}{c|}{1\rule{0pt}{3ex}}
+& \multicolumn{3}{c|}{2} & \multicolumn{3}{c|}{3}
+& \multicolumn{3}{c|}{4} & \multicolumn{3}{c|}{5}
+& \multicolumn{3}{c|}{6} & \multicolumn{3}{c}{7}
+\\[1ex] \hline
+&  1&\textsuperscript{s} &$+$&0&0005
+&\multicolumn{1}{@{}r@{}}{$(+$}&0&\multicolumn{1}{@{}l@{}|}{0024)}
+&$+$&0&0013 &$+$&0&0004 &$+$&0&0002 &$-$&0&0002 & &0&0000
+\\
+&  2& &$+$& &0006 & & &0010 &\multicolumn{3}{c|}{------} &$+$& &0001 & & &0000 &$-$& &0001 &$-$& &0004 \\
+&  4& &$-$& &0005 &$-$& &0002 &\multicolumn{3}{c|}{------} &$-$& &0001 &$-$& &0003 &\multicolumn{3}{c|}{------} &$-$& &0002 \\
+&  8& &\multicolumn{3}{c|}{------} &$-$& &0008 & & &0000 &$+$& &0015 &$-$& &0003 &$-$& &0002 & & &0000 \\
+& 16& &\multicolumn{3}{c|}{------} &$-$& &0007 &$-$& &0002 &$+$& &0008 &$-$& &0005 &\multicolumn{3}{c|}{------} &$-$& &0001 \\
+& 32& &\multicolumn{3}{c|}{------} &$-$& &0003 &$-$& &0001 &$-$& &0004 &$+$& &0001 &\multicolumn{3}{c|}{------} &$+$& &0003 \\
+\mbox\quad
+& 64& &\multicolumn{3}{c|}{------} &$+$& &0003 &$+$& &0006 &$-$& &0009
+&$+$& &0006
+&\multicolumn{3}{c|}{------} &\multicolumn{3}{c}{------} \\
+\hline
+\end{tabular}
+\end{tablesetup}
+
+From equation (6) we infer that, for six inches aperture and one
+second exposure time, the diameter of $\alpha$ \textit{Lyr�'s} image on this particular
+plate is $0^\text{in}.0070$. Comparing equation (6) with equation (5)
+we learn that the increase in the diameter of the image of $\alpha$ \textit{Lyr�} on
+this plate for any $t$ is 2.2 times as rapid as it is in the case of \textit{Polaris}
+for the same $t$ on the plate first described; so that, if other things
+were equal, the difference between the photographic energy of two
+stars could be more accurately determined from comparatively long exposures than from short ones. (The \emph{rate} of increase, of course,
+varies inversely as $t$.)
+
+Now, let
+\[
+d = \alpha_0 + \beta_0\log{D} + \gamma_0 D\log{t} \tag{7}
+\]
+%-----File: 057.png-----
+be the equation giving the diameters for a particular star taken as a
+standard, and let
+\[
+d' = \alpha + \beta\log{D_0} + \gamma D_0 \log{t}   \tag{8}
+\]
+be the equation which gives the diameter of the image of \emph{any} star
+for the \emph{constant aperture} $D_0$ (unity $= 6^\text{in}$); then if $Q$ represents the
+particular aperture in equation~(7)
+which, for the same value of $t$
+makes $d = d'$, the reciprocal of this quantity, or \begin{large}$\frac{1}{Q}$\end{large}, substituted in
+place of $D_0$ must, for all values of $t$, satisfy equation~(8)
+for $d' = d$
+if the assumed law\footnote{The law expressed in equations (1) and (7).}
+is theoretically exact. $Q$, then, becomes a measure
+of the square root of the relative brightness of the two stars, since,
+if we assume that the amount of energy required to produce a given
+impression on a given plate is always the same, whatever the unit of
+energy (intensity) may be, the total amount of energy for the same
+telescope can be considered as varying directly with the area of the
+aperture, or with $D^2$. Hence, if $B_0$ and $B$ denote respectively the
+brightness of the standard and comparison stars, we can at once
+write:
+\[
+\left(\frac{Q}{D_0}\right)^2 = \frac{B}{B_0} \tag{10}
+\]
+$Q$ being that value of $D$ which when substituted in the equation for
+the standard star (equation~7) will make $d = d'$. In other words,
+\textit{$Q$ is the diameter of the aperture which the standard star would
+require to produce, in the time $t$, an image having the same diameter
+as that of any other star photographed with an aperture $D_0$} (= six
+inches) \emph{in the same time $t$}. Equation~(7) can therefore be written:
+\[
+d' = \alpha_0 + \beta_0\log{Q} + \gamma_0 Q\log{t} \tag{11}
+\]
+
+Let us now take the equations deduced from the measured diameters
+of the images of \textit{Polaris} and $\alpha$ \textit{Lyr�}, and see to what degree
+of accuracy the necessary theoretical relations between $Q$ and $D_0$ will
+represent the observed data. For $d = d'$ we have the equation:
+\[
+0.0055 + 0.0033\log{Q} + 0.0034 Q \log{t} = 0.0070 + 0.0050\log{D_0} + 0.0074 D_0\log{t}
+\]
+
+After a few trials, for different values of $t$, we obtain the approximate
+value $D_0 = 0.48$ when $Q = 1$, and, according to the above
+considerations, we should also have $Q = 2.10$ when $D_0 = 1$. Both
+of these conditions should be fulfilled for all values of $t$.
+
+As the images of the two stars are on different plates I have not
+thought it worth while to derive a more accurate relation between $Q$
+and $D_0$ for this particular case.
+%-----File: 058.png-----
+
+The approximate relation will, however, serve to show the agreement
+between our theory and the data derived from actual observations.
+
+The accompanying table contains the computed values of $d$ and
+$d'$ for each $t$, for reciprocal values of $Q$ and $D_0$:
+\begin{tablesetup}
+\begin{tabular}{c r@{}l | r@{.}l | r@{.}l || r@{.}l | r@{.}l }
+\hline\hline
+ \multicolumn{3}{c|}{
+\multirow{2}{5em}{\centering\footnotesize\textsc{
+    Exposure Time.}} }
+& \multicolumn{4}{m{8em}@{ }||}{\centering\footnotesize $
+    \begin{array}{l@{ }l}
+      D_0 &= 1.00  \\  Q &= 2.10
+    \end{array}$}
+& \multicolumn{4}{@{ }m{8em}}{\centering\footnotesize $
+    \begin{array}{r@{ }l}
+      D &= 0.48  \\  Q &= 1.00
+    \end{array}$}
+\\  \cline{4-11}
+&&&\multicolumn{2}{m{4em}|}{\centering\footnotesize\textit{
+    Polaris \\ d}}
+& \multicolumn{2}{m{4em}||}{\centering\footnotesize\textit{
+    $\alpha$ \textit{Lyr�} \\ $d'$}}
+& \multicolumn{2}{m{4em}|}{\centering\footnotesize\textit{
+    Polaris \\ d}}
+& \multicolumn{2}{m{4em}}{\centering\footnotesize\textit{
+    $\alpha$ \textit{Lyr�} \\ $d'$}}
+\\  \hline
+\mbox\quad&  1&\textsuperscript{s}
+         &\ 0&0070 &\ 0&0066 &\ 0&0055 &\ 0&0054 \\
+&  2&    &   &0087 &   &0092 &   &0065 &   &0065 \\
+&  4&    &   &0109 &   &0114 &   &0075 &   &0075 \\
+&  8&    &   &0130 &   &0140 &   &0086 &   &0086 \\
+& 16&    &   &0151 &   &0159 &   &0096 &   &0097 \\
+& 32&    &   &0173 &   &0181 &   &0106 &   &0107 \\
+& 64&    &   &0195 &   &0204 &   &0117 &   &0118 \\
+\hline
+\end{tabular}
+\end{tablesetup}
+
+If the two sets of star images had been impressed upon the same
+plate, we would have inferred the photographic brightness of $\alpha$ \textit{Lyr�}
+to be about 4.4 times that of \textit{Polaris}.\footnote{
+  Neglecting atmospheric absorption.}
+As, however, the diameters
+of the star images on different plates taken from the same box are
+not always the same for equal exposures, it became necessary to make
+a separate investigation covering this particular phenomenon.
+
+I found that if we express the diameters of the image of \textit{Polaris}
+on any plate in terms of the diameters given on the plate for which
+equation~(5) holds good (which we will call the standard plate), we
+have only to multiply the second member of equation~(5) by such a
+number $x$ that for a given $t$ the measured $d$ will be satisfied. From
+a series of comparisons I find that $x$ is practically constant for the
+different values of $t$. The general equation for any No.~26 Seed
+plate exposed in the stellar focus of the particular telescope used in
+these investigations I therefore assume to be
+\[
+\frac{d}{x}=0^{\text{in}}.0055 + 0^{\text{in}}.0033 (\log{Q}+Q\log{t})   \tag{12}
+\]
+since, for all practical purposes, $\beta_{0}$ and $\gamma_{0}$ in equation~(5) are the same.
+%-----File: 059.png-----
+
+To find the value of $Q$ from this equation we can write:
+\begin{equation}
+\log{Q} + Q\log{t} = \log{(Qt^Q)} = \frac{d}{0.0033 \centerdot x} - 1.67 \quad.    \tag{13}
+\end{equation}
+
+In order, however, to facilitate the determination of $Q$ for certain
+observed values of $d$ and $t$, I have computed the following table, by
+means of which $Q$ can be obtained by simple interpolation.
+
+The horizontal argument is $Q$, the vertical argument is $t$, and the
+tabular function corresponding to these arguments is the measured $d$
+of equation (13) for $x = 1.00$.
+
+\begin{tablesetup}
+\renewcommand{\tabcolsep}{4pt}
+\begin{tabular}{c *{10}{|r@{.}l}}
+\hline \hline
+\footnotesize \textsc{Exposure} & \multicolumn{20}{c}{\textsc{Q.}}
+\\ \cline{2-21}
+\footnotesize \textsc{Time.}
+& \multicolumn{2}{c|}{\footnotesize 0.40}
+& \multicolumn{2}{c|}{\footnotesize 0.80}
+& \multicolumn{2}{c|}{\footnotesize 1.20}
+& \multicolumn{2}{c|}{\footnotesize 1.60}
+& \multicolumn{2}{c|}{\footnotesize 2.00}
+& \multicolumn{2}{c|}{\footnotesize 2.40}
+& \multicolumn{2}{c|}{\footnotesize 2.80}
+& \multicolumn{2}{c|}{\footnotesize 3.20}
+& \multicolumn{2}{c|}{\footnotesize 3.60}
+& \multicolumn{2}{c}{\footnotesize 4.00}
+\\ \hline
+$2^\text{s}$             &0&0046 &0&0060 &0&0070 &0&0078 &0&0085 &0&0091 &0&0098 &0&0103 &0&0109 &0&0114 \\
+$4^{\phantom{\text{s}}}$ & &0050 & &0068 & &0081 & &0093 & &0105 & &0115 & &0125 & &0135 & &0145 & &0154 \\
+$8^{\phantom{\text{s}}}$ & &0054 & &0078 & &0093 & &0109 & &0125 & &0139 & &0153 & &0167 & &0181 & &0194 \\ \hline
+\end{tabular}
+\end{tablesetup}
+
+If for a particular plate any measured diameter is $d$, the argument
+for entering the above table is $x\centerdot d$, and $x$ is to be taken as a
+constant for the same plate.
+
+We will now give a few examples illustrating the application of
+the formulas for determining the brightness of the fixed stars:
+
+\textsc{Example I.\@} On September 5th, 1889, \textit{Polaris}, $\alpha$ \textit{Aurig�},
+$\gamma$ \textit{Cephei} and $\alpha$ \textit{Tauri} were photographed on the same plate with
+exposures of $2^\text{s}$, $4^\text{s}$ and $8^\text{s}$. The measured diameters are:
+
+\begin{tablesetup}
+\begin{tabular}{c *{4}{|r@{.}l}}
+\hline \hline
+\footnotesize \textsc{Exposure}
+& \multicolumn{8}{c}{\footnotesize \textsc{Measured Diameters} ($= d$).}
+\\ \cline{2-9}
+\footnotesize \textsc{Time.}
+& \multicolumn{2}{c|}{\footnotesize \textit{Polaris.}}
+& \multicolumn{2}{c|}{\footnotesize $\alpha$ \textit{Aurig�.}}
+& \multicolumn{2}{c|}{\footnotesize $\gamma$ \textit{Cephei.}}
+& \multicolumn{2}{c}{\footnotesize $\alpha$ \textit{Tauri.}}
+\\ \hline
+$2^\text{s}$             &0&0064 &0&0081 &0&0042 &0&0060 \\
+$4^{\phantom{\text{s}}}$ & &0074 & &0090 & &0052 & &0061 \\
+$8^{\phantom{\text{s}}}$ & &0080 & &0109 & &0056 & &0072 \\ \hline
+\end{tabular}
+\end{tablesetup}
+
+The aperture being six inches for all the exposures, we first
+assume the plate to be a standard one, and find $d$ with the argument
+$Q = 1$, either by means of equation (5) or, by interpolation, from
+the table:
+%-----File: 060.png-----
+
+\begin{tablesetup}
+\begin{tabular}{c|c|c}
+\multicolumn{3}{c}{\large\textit{\textsc{Polaris.}}}
+\\ \hline \hline
+\footnotesize \textsc{Exposure Time.}
+& \footnotesize \textsc{Computed} $d$. & \footnotesize O $-$ C.
+\\ \hline
+$2^\text{s} $&$ 0.0065 $&$ -0.0001 $\\
+$4^\text{s} $&$ \phantom{0}.0074 $&$ \phantom{-}0.0000 $\\
+$8^\text{s} $&$ \phantom{0}.0085 $&$ -0.0005 $\\ \hline
+\end{tabular}
+\end{tablesetup}
+
+As the measured values are slightly smaller than those given by
+our assumed standard plate, we give $x$ such a value that the (O~$-$~C)
+quantities will nearly balance each other. Placing $x = 1.03$ and
+multiplying the observed values of $d$ by 1.03, the residuals (O~$-$~C)
+become respectively $+0.0001$, $+0.0001$, and $-0.0003$.
+
+To obtain the value of $Q$ by direct computation, for any star whose
+image is on this particular plate, we would therefore use the equation
+\begin{equation}
+\log{Q} + Q\log{t} = \frac{d}{0.0034} - 1.67      \tag{15}
+\end{equation}
+in which $d$ is the measured diameter corresponding to the time $t$.
+
+The tabular values at once give the desired quantities by interpolation,
+first multiplying each measured $d$ by 1.03 for the argument:
+\begin{tablesetup}
+\begin{tabular}{p{6em}|c|c|c|c}
+\hline \hline
+\centering \footnotesize \textsc{Exposure}
+& \multicolumn{4}{|c}{\footnotesize \textsc{Values of} $Q - \sqrt{B}$}
+\\ \cline{2-5}
+\centering \footnotesize \textsc{Time.}
+& \footnotesize \textit{Polaris.}
+& \footnotesize $\alpha$ \textit{Aurig�.}
+& \footnotesize $\gamma$ \textit{Cephei.}
+& \footnotesize $\alpha$ \textit{Tauri.}
+\\ \hline
+\centering $2^\text{s}$\phantom{\tablenotedagger} & 1.04 & 1.89 & 0.32 & 0.84 \\
+\centering $4^\text{s}$\phantom{\tablenotedagger} & 1.05 & 1.60 & 0.32 & 0.69 \\
+\centering $8^\text{s}$\tablenotedagger & 0.90 & 1.68 & 0.47 & 0.73 \\ \hline
+\centering \footnotesize Mean & 1.00 & 1.72 & 0.42 & 0.75 \\ \hline
+\multicolumn{5}{l}{\footnotesize$\dagger$ Transcriber's note: Original text reads $5^\text{s}$}
+\end{tabular}
+\end{tablesetup}
+Using the mean values of $Q$, we obtain the following residuals:
+
+\begin{tablesetup}
+\begin{tabular}{p{6em} *{4}{|c@{\,}r@{.}l}}
+\hline \hline
+%\centering \footnotesize \textsc{Exposure Time.}
+\centering \footnotesize \textsc{Exposure} &
+\multicolumn{12}{|c}{\multirow{2}{*}{\footnotesize \textsc{Observation $-$ Computation}}} \\
+\centering \footnotesize \textsc{Time.} & \multicolumn{12}{c}{}\\ \hline
+\centering $2^\text{s}$ &   &0&0000 &$+$&0&0003 &$-$&0&0003 &$+$&0&0003 \\
+\centering $4^{\phantom{\text{s}}}$ &$+$& &0002 &$-$& &0004 &$+$& &0002 &$-$& &0003 \\
+\centering $8^{\phantom{\text{s}}}$ &$-$& &0003 &$-$& &0002 &$+$& &0003 &$-$& &0001 \\ \hline
+\end{tabular}
+\end{tablesetup}
+
+If we use the familiar expression for the light-ratio of visual magnitudes,
+\begin{equation*}
+B = (0.4)^{m - 1}
+\end{equation*}
+%-----File: 061.png-----
+(in which $B$ and $m$ are respectively the visual brightness and visual
+magnitude of any star) for expressing also the light-ratio for the photographic
+magnitudes $m'$, we can write
+\[
+    m' = 1 - \frac{\operatorname{log.}(\kappa \cdot Q^2)}
+                  {\operatorname{log.} 0.4}    \tag{17}
+\]
+in which $\kappa$ is a constant depending upon the photographic magnitude
+of the standard star. For the purpose of comparing the photographic
+with the visual magnitudes, let us take \textit{Polaris} as the standard star,
+and assume its photographic magnitude to be 2.00; equation~(17)
+becomes
+\[
+ m' = 2 - \frac{\log Q^2}{0.4}
+\]
+
+The values of $m'$, for certain values of $Q$, can be taken from the
+accompanying table, which I have computed for illustration:
+\begin{tablesetup}
+\begin{tabular}{r@{.}l||*{4}{r@{.}l|} r@{.}l}
+\hline \hline
+\multicolumn{2}{c||}{\footnotesize $Q$\rule{0pt}{4ex}}
+& \multicolumn{2}{c|}{\footnotesize 0.00}
+& \multicolumn{2}{c|}{\footnotesize 0.20}
+& \multicolumn{2}{c|}{\footnotesize 0.40}
+& \multicolumn{2}{c|}{\footnotesize 0.60}
+& \multicolumn{2}{c}{\footnotesize 0.80} \\[1ex]
+\hline
+  0&00   & \multicolumn{2}{c|}{} & 5&49    & 3&99   & 3&11
+& 2&48\rule{0pt}{3ex}
+\\[1ex]
+  1&00   & 2&00  & 1&60    & 1&27   & 0&98  & 0&72 \\[1ex]
+  2&00   & 0&50  & 0&29    & 0&10   & $-0$&07 & $-0$&24 \\[1ex]
+ \mbox\quad 3&00\mbox\quad &\mbox\ $-0$&39\mbox\quad
+&\mbox\  $-0$&53\mbox\quad &\mbox\ $-0$&66\mbox\quad
+&\mbox\  $-0$&78\mbox\quad &\mbox\ $-0$&90\mbox\quad \\[1ex]
+\hline
+\end{tabular}
+\end{tablesetup}
+
+From an inspection of the table and the values of $Q$ given in the
+next example, we see at once that if we wish to avoid negative numbers
+for expressing some observed magnitudes we must either represent
+the magnitude of \textit{Polaris} by a greater number or change the
+light-ratio.
+
+I have tabulated the photographic magnitudes of the four stars,
+together with the probable errors. The visual magnitudes as given
+in Volume~XIV, \textit{Harvard College Observatory Annals}, and the
+differences between the photographic and visual magnitudes, are also
+added:
+\begin{tablesetup}
+\begin{tabular}{r@{ }l|c|c|c|c}
+\hline \hline
+\multicolumn{2}{c|}{\footnotesize\textsc{Star.}}
+& {\footnotesize \textsc{Photog.~Mag.}}
+& {\footnotesize \textsc{Probable Error.}}
+& {\footnotesize \textsc{Visual Mag.}}
+& {\footnotesize \textsc{Vis.~$-$ Photog.}}\\
+\hline
+         & \textit{Polaris}  &$ 2.02 $&$ \pm 0.11\phantom{\pm} $&$ 2.2 $&$ +0.2 $\\
+$\alpha$ & \textit{Aurig�} &$ 0.82 $&$ 0.11 $&$ 0.2 $&$ -0.6 $\\
+$\gamma$ & \textit{Cephei}   &$ 4.20 $&$ 0.28 $&$ 3.4 $&$ -0.8 $\\
+$\alpha$ & \textit{Tauri}    &$ 2.62 $&$ 0.13 $&$ 1.0 $&$ -1.6 $\\
+\hline
+\end{tabular}
+\end{tablesetup}
+%-----File: 062.png-----
+
+\textsc{Example II\@.} During the night of September~6, in bright moonlight,
+I made exposures of 2\textsuperscript{s}, 4\textsuperscript{s} and 8\textsuperscript{s} on \textit{Polaris}, $\alpha$ \textit{Lyr�}, $\alpha$ \textit{Cygni},
+$\alpha$ \textit{Aquil�}, and four hours later the same plate was exposed on
+$\alpha$ \textit{Pisces Australis}, $\beta$ \textit{Ceti}, $\alpha$ \textit{Aurig�}, $\alpha$ \textit{Arietis} and $\alpha$ \textit{Andromed�}.
+The measured diameters are tabulated below. For this plate we see
+at once that the differences between the observed and computed values
+of $d$ are such that the $(C - O)$ values (+0.0001, -0.0003 and
++0.0003) practically balance each other; hence we place $x = 1.00$
+and use equation (13) (or the table) to obtain the values of $Q$ given
+below. For the $(O - C)$ values the computed quantities are obtained
+by substituting the mean values of $Q$ in equation (12):
+
+\begin{tablesetup}
+\renewcommand{\tabcolsep}{3pt}
+\begin{tabular}{c|c|c|c|c|c|c|c|c|c}
+\hline \hline
+ &\multicolumn{9}{c}{\footnotesize}\\
+ &\multicolumn{9}{c}{\footnotesize\textsc{Measured Values of} \textit{d}}\\
+\footnotesize\textsc{Exposure} &\multicolumn{9}{c}{\footnotesize}\\
+\cline{2-10}
+\footnotesize\textsc{Time.}& \multirow{2}{*}{\footnotesize\textit{Polaris.}}& \footnotesize$\alpha$ & \footnotesize$\alpha$ & \footnotesize$\alpha$ & \footnotesize$\alpha$ \textit{Pis.}& \footnotesize$\beta$ & \footnotesize$\alpha$ & \footnotesize$\alpha$ & \footnotesize$\alpha$ \\
+& & \footnotesize\textit{Lyr�.}& \footnotesize\textit{Cygni.}& \footnotesize\textit{Aquil�.}& \footnotesize\textit{Aust.}& \footnotesize\textit{Ceti.}& \footnotesize\textit{Aurig�.}& \footnotesize\textit{Arietis.}& \footnotesize\textit{Androm.}\\
+\hline
+$2^\text{s}$            & 0.0066& 0.0103& 0.0092& 0.0090& 0.0077& 0.0049& 0.0075& 0.0053& 0.0079\\
+$4^{\phantom{\text{s}}}$& \phantom{0}.0072& \phantom{0}.0134& \phantom{0}.0116& \phantom{0}.0106& \phantom{0}.0087& \phantom{0}.0054& \phantom{0}.0094& \phantom{0}.0063& \phantom{0}.0090\\
+$8^{\phantom{\text{s}}}$& \phantom{0}.0088& \phantom{0}.0169& \phantom{0}.0136& \phantom{0}.0129& \phantom{0}.0099& \phantom{0}.0060& \phantom{0}.0106& \phantom{0}.0066& \phantom{0}.0116\\
+\hline\hline
+\multirow{3}{*}{\begin{tabular}{c}\footnotesize\textsc{Exposure}\\\footnotesize\textsc{Time.}\end{tabular}}\\
+ &\multicolumn{9}{c}{\footnotesize\textsc{Resulting Values of} $Q=\sqrt{B}$.}\\
+ &\multicolumn{9}{c}{}\\
+\hline
+$2^\text{s}$&          1.04&  3.20&  2.46&  2.33&  1.55&  0.49&  1.45&  0.60&  1.66\\
+$4^{\phantom{\text{s}}}$& 0.92&  3.16&  2.44&  2.04&  1.40&  0.49&  1.63&  0.69&  1.50\\
+$8^{\phantom{\text{s}}}$& 1.07&  3.26&  2.31&  2.11&  1.35&  0.50&  1.52&  0.60&  1.77\\
+\hline
+                & 1.01&  3.21&  2.30&  2.15&  1.43&  0.49&  1.53&  0.63&  1.64\\
+\hline\hline
+\multirow{3}{*}{\begin{tabular}{c}\footnotesize\textsc{Exposure}\\\footnotesize\textsc{Time.}\end{tabular}}\\
+ &\multicolumn{9}{c}{\footnotesize\textsc{The Mean Values of $Q$, give the Residuals.}}\\
+ &\multicolumn{9}{c}{\footnotesize}\\
+\hline
+$2^\text{s} $&$  +0.0000 $&$ \phantom{+}0.0000 $&$ +0.0002 $&$ +0.0003 $&$ +0.0002 $&$ \phantom{+}0.0000 $&
+  $ -0.0002 $&$  -0.0001 $&$ \phantom{+}0.0000 $\\
+$4^{\phantom{\text{s}}} $&$ +\phantom{0}.0001 $&$ -\phantom{0}.0001 $&$ \phantom{0}+.0003 $&$ -\phantom{0}.0002 $&
+  $ \phantom{+0}.0000 $&$ \phantom{+0}.0000 $&$ +\phantom{0}.0003 $&$ +\phantom{0}.0003 $&$ -\phantom{0}.0004 $\\
+$8^{\phantom{\text{s}}} $&$ -\phantom{0}.0003 $&$ +\phantom{0}.0002 $&$ \phantom{+0}.0000 $&$ -\phantom{0}.0001 $&
+  $ -\phantom{0}.0003 $&$ +\phantom{0}.0001 $&$ +\phantom{0}.0001 $&$ -\phantom{0}.0001 $&$ +\phantom{0}.0005 $\\
+\hline\hline
+\end{tabular}
+\end{tablesetup}
+
+
+The numbers expressing the photographic brightness of each star
+in terms of that of \textit{Polaris} are therefore, in the above order, 10.3,
+5.3, 4.6, 2.0, 0.2, 2.3, 0.4 and 2.7. The only star of the list which
+was near to the zenith at the time its image was formed on the photographic
+plate is $\alpha$ \textit{Lyr�}; the effect of moonlight, atmospheric
+%-----File: 063.png-----
+absorption and haze would therefore be at a minimum for this star,
+and its relative brightness would apparently be near a maximum.
+The same remarks apply to the results given in the next table as in
+the last example:
+\begin{tablesetup}
+\begin{tabular}{r@{ }l|c|c|c|c}
+\hline \hline
+\multicolumn{2}{m{5em}|}{\centering\footnotesize\textsc{
+    Star.}}
+& \multicolumn{1}{m{5em}|}{\centering\footnotesize\textsc{
+    Photog.\ Mag.}}
+& \multicolumn{1}{m{5em}|}{\centering\footnotesize\textsc{
+    Probable Error.}}
+& \multicolumn{1}{m{5em}|}{\centering\footnotesize\textsc{
+    Visual Mag.}}
+ & \multicolumn{1}{m{5em}}{\centering\footnotesize\textsc{
+    Vis.~$-$ Photog.}} \\[2ex]
+\hline
+\mbox\quad &\textit{Polaris}\rule{0pt}{3ex} & +1.95 & $\pm$0.05 & +2.2 & +0.2 \\
+$\alpha$& \textit{Lyr�}     & $-0.53$ & $\pm$0.02 & +0.2 & +0.7 \\
+$\alpha$& \textit{Cygni}      & +0.10 & $\pm$0.03 & +1.5 & +1.4 \\
+$\alpha$& \textit{Aquil�}   & +0.34 & $\pm$0.06 & +1.0 & +0.7 \\
+$\alpha$& \textit{Pis.~Aust.}\mbox\ & +1.22 & $\pm$0.05 & +1.3 & +0.1 \\
+$\beta$ & \textit{Ceti}       & +3.53 & $\pm$0.01 & +2.1 & $-1.4$ \\
+$\alpha$& \textit{Aurig�}   & +1.08 & $\pm$0.05 & +0.2 & $-0.9$ \\
+$\alpha$& \textit{Arietis}    & +3.01 & $\pm$0.07 & +2.0 & $-1.0$ \\
+$\alpha$& \textit{Androm.}    & +0.93 & $\pm$0.07 & +2.1 & +1.2 \\[1ex]
+\hline
+\end{tabular}
+\end{tablesetup}
+
+No corrections for absorption, etc., have as yet been applied to
+the above results, which consequently refer to the apparent magnitude
+at the instant of exposure. The last column of the above table
+plainly shows that we can make no definite \textit{a priori} estimate as to
+what the photographic magnitude of a star is if we simply know its
+visual magnitude. There is therefore no advantage (as Professor
+Holden has pointed out in his ``Memorandum'' to the Paris Photographic
+Conference) in following the methods used for visual magnitudes.
+
+It is evident that we must first know the law of atmospheric
+absorption of the photographic rays before we can determine the true
+relative brightness of the stars; since each observed brightness
+requires a certain plus correction, depending directly upon the zenith
+distance, to reduce it to the brightness which would have been
+obtained at the zenith. Or each observed brightness could be
+reduced to what it would be at a certain zenith distance, as, for
+instance, that of the celestial pole at a given place. The photographs
+already taken show that this correction is quite sensible, even
+at small zenith distances. From some preliminary reductions I find
+that for this Observatory (altitude 4209 feet) the absorption of stellar
+%-----File: 064.png-----
+photographic brightness at 80� zenith distance is considerably more
+than fifty per cent.\ of the brightness reduced to 0� zenith distance.
+After a complete series of observations bearing upon this subject has
+been obtained at sea-level near the earth's equator, I hope to give,
+in a more or less complete state, the photographic magnitudes of a
+large number of the brighter stars in both hemispheres. Just how
+far down the scale of magnitudes the formul�  will hold good I am,
+as yet, unable to say.
+
+In photographing faint stars the exposure time should evidently
+be so long as to make the diameters of the disks as great or greater
+than the faint penumbral image which, in the telescope used, surrounds
+the primitive umbral image in short exposures on faint stars;
+when this precaution is taken, it seems that the formul� give consistent
+results, judging from a few experimental exposures. This form
+of image for short exposures on faint stars may, of course, be peculiar
+to this particular telescope. Too much stress cannot be laid upon
+the statement, \emph{that if reliable results are to be obtained}, the objective
+must be of the first order of excellence and \emph{the plate must be kept
+exactly in the stellar focus}.
+
+Throughout this whole discussion I have purposely avoided bringing
+in any relation between aperture and focal length, as it seems
+probable that different telescopes must be compared before any definite
+conclusions can be drawn.
+
+The results contained in the present paper are only to be considered
+as preliminary to a much more extended investigation to be
+undertaken in South America under the auspices of this Observatory,
+made possible through the generosity of Col.\ \textsc{Crocker}.
+
+In conclusion, I wish to express my obligations to Professor
+\textsc{Holden}, Director of this Observatory, for his readiness in placing
+at my disposal everything which could in any way aid me in past and
+future investigations; for his practical help and advice relating to a
+subject which has claimed his attention for some time past, and
+which is destined to become the most important method of investigation
+in our science, viz: \textit{Astronomical Photography}.
+
+\filbreak
+I also wish to thank Mr.\ \textsc{Burnham} for his kind and willing
+assistance in the photographic work.\\*
+\rightline{\textsc{J.~M. Schaeberle}.\quad}\\*[1ex]
+{\small\indent \textsc{Lick Observatory}, September~21, 1889.}
+
+\ThoughtBreakLong
+%-----File: 065.png-----
+
+\nbsectionheading{ON THE ESTABLISHMENT OF A STANDARD MERIDIAN
+LINE FOR SANTA CLARA COUNTY, CALIFORNIA.}
+\addcontentsline{toc}{section}{On the Establishment of a Standard Meridian Line for Santa Clara County, California. By \textsc{J.~E. Keeler}}
+
+\nbsubsubsectionheading{\shortrule\\*
+\textsc{By \textsc{James E. Keeler.}}\\*
+\shortrule}
+
+A few months ago, at the suggestion of Professor \textsc{Holden}, Mr.\ \textsc{Chas.\ Herrmann},
+County Surveyor of Santa Clara county, and Mr.\ \textsc{A.~T. Herrmann},
+Surveyor and Civil Engineer, obtained the permission
+of the County Supervisors to establish a standard meridian
+line in San Jos�, for the benefit of surveyors, with a sufficient sum of
+money to provide suitable monuments.
+
+It was agreed that the astronomical staff of the Observatory
+should make the necessary observations without expense to the
+county, and I was appointed to carry out the work.
+
+Absolute directions on the earth can only be determined by reference
+to the heavenly bodies. The magnetic needle has been and
+still is extensively used as a secondary means of determining directions,
+but the angle which the magnetic needle makes with the true
+meridian is constantly changing, and is, moreover, subject to sudden
+and irregular variations, so that, even with the greatest precautions, the
+compass is an unsafe guide. Ignorance of these facts, or of the
+amount of necessary allowance from lack of a suitable standard of
+reference, has given rise to an endless amount of litigation in this
+country. It is safe to say, that if each county in the Union had
+legally established a standard meridian in the early days of its settlement,
+the gain to the country would have to be estimated by hundreds
+of thousands of dollars.
+
+The remedy for the evils resulting from the secular change of
+the magnetic declination has been repeatedly pointed out, ever since
+the days of \textsc{Rittenhouse}. Prof.\ \textsc{Gillespie}, in his well-known work
+on Land Surveying, says (p.~210): ``The only complete remedy for
+the disputes, and the uncertainty of bounds, resulting from the continued
+change in the variation, is this: Let a meridian, \textit{i.~e.}, a true
+north and south line, be established in every town or county, by the
+authority of the State; monuments, such as stones set deep in the
+ground, being placed at each end of it. Let every surveyor be
+obliged by law to test his compass by this line, at least once in each
+year. .~~.~~.~~. Let the variation thus ascertained be inserted in the
+notes of the survey and recorded in the deed. Another surveyor,
+years or centuries afterward, could test his compass by taking the
+%-----File: 066.png-----
+bearing of the same monuments, and the difference between this and
+the former bearing would be the change of variation. He could thus
+determine, with entire certainty, the proper allowance to be made in
+order to retrace the original line, no matter how much, or how irregularly,
+the variation may have changed, or how badly adjusted was the
+compass of the original survey.''
+
+But although these evils have been thus forcibly stated, even in
+the text-books of every school, and the remedy so clearly pointed out,
+very little interest has been taken in the matter by State authorities.
+Professor \textsc{Holden}, while Director of the Washburn Observatory,
+once proposed to establish a standard meridian in every county-seat
+in the State of Wisconsin, for the bare personal and traveling expenses
+of an observer, an offer which was declined without thanks.
+
+There is no doubt that the Lick Observatory would assist in such
+a plan for California, by every means in its power, should the proper
+authorities be willing to pay the bare expense of the undertaking.
+
+It may be noted that the value of a standard line of reference is
+particularly great in a newly settled country, where the compass is
+more relied upon than it is in older communities with well-established
+boundaries and landmarks.
+
+The scene of our operations in San Jos� was what is known as
+the ``Meridian Road,'' because it is supposed to be in the line of the
+Mt.\ Diablo meridian. It has been the practice of surveyors to test
+their instruments by sighting up and down this road, which, however,
+contains no marks sufficiently definite to admit of a precise determination
+by this method. The north end of the road terminates at a
+high board fence which forms the southern boundary of the Fair
+Ground, and on a shelf secured to this fence a mark was put up,
+consisting of a hole one-half inch in diameter in a thin plate, illuminated
+from behind by a bull's-eye lantern. Two thousand feet south
+of the mark a substantial pier of brick and cement was built for the
+support of the instrument. The mark was as nearly in the meridian
+of the pier as could be determined with the aid of a compass. At
+the pier it subtended an angle of $4''$, and to the naked eye appeared
+as a star of about the first magnitude.
+
+The instrument employed was the \textsc{Repsold} altazimuth briefly
+described in Vol.~I, Publications of the Lick Observatory, and more
+completely in my report on the geographical position of Norman,
+California, in the Reports on Observations of the Total Eclipse of
+January~1, 1889, published by the Lick Observatory. It has vertical
+and horizontal circles ten inches in diameter, read to $2''$ by micrometer
+%-----File: 067.png-----
+microscopes, or by estimation to $0''.2$. All necessary attachments
+are provided for exact astronomical work. The time-piece used was
+a sidereal chronometer, Negus 1720.
+
+Preliminary observations were made on the night of August 5th,
+and more accurate ones on August 6th and 7th. The azimuth of the
+mark was determined by alternate readings on the mark and on
+\textit{Polaris} near eastern elongation, the instrument being reversed during
+the measurements to eliminate the error of collimation. The latitude
+of the pier was determined, with sufficient accuracy, by measuring
+the zenith distances of four stars with the vertical circle, and the local
+sidereal time by using the altazimuth as a transit instrument. No elaborate
+time observations were made, as a knowledge of the time to
+within one second is amply sufficient for computing the small reductions
+to elongation. The horizontal circle was turned one-third round on August
+7th, in order to bring different divisions under the microscopes.
+
+Ten observations of the mark and ten of \textit{Polaris}, on August 6th,
+made the mark $1�~22'~48''.0$ west of the vertical circle passing through
+the point of elongation. The computed azimuth of the star corrected
+for diurnal aberration, was $1�~37'~7''.2$, hence the azimuth of
+the mark was $+0�~14'~19''.2$.
+
+From six observations of the star and six of the mark, on August
+7th the mark was west of the star $1�~22'~50''.6$. The computed
+azimuth of the star was $1�~37'~6''.8$, and hence the azimuth of the
+mark was $+ 0�~14'~16''.2$. The adopted azimuth of the mark was
+$14'~17''.7$ east, which, at a distance of 2000 feet, corresponds to 8
+feet 3.8 inches, and the mark was moved this distance to the west
+to bring it into the meridian of the centre mark on the pier. The
+estimated probable error of the meridian is $2''$ or about one-quarter
+of an inch at a distance of 2000 feet, a quantity thirty times smaller
+than the smallest angle which is measured with ordinary surveying
+instruments. From the above data permanent monuments will be
+established by the Messrs.\ \textsc{Herrmann}.
+
+For the convenience of those who cannot avail themselves of this
+meridian line, I have computed the following table of azimuths and
+times of elongation of \textit{Polaris} for the latitude and longitude of San
+Jos�. The azimuths are given to the nearest $10''$; the times of
+elongation in \textit{Standard Pacific Time} to the nearest minute. For
+San Francisco the azimuths must be increased by $40''$, and the times
+of elongation will be about two minutes later. An error of thirteen
+minutes in the time of elongation will produce an error of only
+$10''$ in the azimuth. The formul�  from which this table was computed
+%-----File: 068.png-----
+may be found in \textsc{Doolittle's} Practical Astronomy (p.~527).
+
+If the meridian is determined from observations of \textit{Polaris} near
+elongation by a surveyor's transit, the line of collimation must be
+adjusted with especial care, so as to travel on a truly vertical line. As
+there are several minutes near elongation during which the azimuth
+of the star does not differ appreciably from the tabulated value, it is
+better to make two observations of the star, one with reversed position
+of the telescope, and take the mean of the readings of the horizontal
+circle. It must be remembered that the reading of the compass
+needle, when the sight line of the instrument is in the meridian, is
+not necessarily the magnetic declination, since the line of zeros of
+the compass circle may not be in the same plane with the line of collimation
+(as, of course, it should be). The reading of the needle will,
+however, be the declination \emph{for that particular instrument}, and true
+bearings can be taken just as well as if the adjustment were perfect.
+\bigskip
+
+\addcontentsline{toc}{section}{Table of Azimuths and Elongations of \textit{Polaris} for 1889 and 1890}
+
+\begin{small}
+\begin{longtable}{c@{ }c@{ }r@{}|rr@{ }c@{ }|rr@{ }c@{ }|crrcc}
+\multicolumn{14}{c}{\textsc{Table of Azimuths and Times of Elongation of \textit{Polaris}.}}
+\\
+\multicolumn{14}{c}{\footnotesize (Computed for the latitude and longitude of San Jos�, Cal., by \textsc{J. E. Keeler}.)}
+\\
+\hline \hline
+  \multicolumn{3}{c|}{\footnotesize\textsc{ Date. }}
+& \multicolumn{3}{c|}{\footnotesize\textsc{ W. Elongation. }}
+& \multicolumn{3}{c|}{\footnotesize\textsc{ E. Elongation. }}
+& \multicolumn{5}{c}{ \footnotesize\textsc{ Azimuth.\rule{0pt}{3ex} }}\\[1ex]
+\hline
+&&& {\footnotesize\textit{h.}} & {\footnotesize\textit{m.}}
+&&  {\footnotesize\textit{h.}} & {\footnotesize\textit{m.}}
+&&&{\footnotesize�}
+&  \multicolumn{1}{c}{\footnotesize$'$}
+&  \multicolumn{1}{c}{\footnotesize$''$}
+\endfirsthead
+\hline \hline
+  \multicolumn{3}{c|}{\footnotesize\textsc{ Date. }}
+& \multicolumn{3}{c|}{\footnotesize\textsc{ W. Elongation. }}
+& \multicolumn{3}{c|}{\footnotesize\textsc{ E. Elongation. }}
+& \multicolumn{5}{c}{ \footnotesize\textsc{ Azimuth.\rule{0pt}{3ex} }}\\[1ex]
+\hline
+&&& {\footnotesize\textit{h.}} & {\footnotesize\textit{m.}}
+&&  {\footnotesize\textit{h.}} & {\footnotesize\textit{m.}}
+&&&{\footnotesize�}
+&  \multicolumn{1}{c}{\footnotesize$'$}
+&  \multicolumn{1}{c}{\footnotesize$''$}
+\endhead
+1889. & Sept. &  6\ldots &  8 & 19 & \textsc{a.m.} &  8 & 25 & \textsc{p.m.}  &&  1 & 37 & 00  \\
+& ``   & 16\ldots &  7 & 39 & `` &  7 & 46 & ``  && 1 & 36 & 50  \\
+& ``   & 26\ldots &  7 & 00 & `` &  7 & 06 & ``  && 1 & 36 & 50  \\
+& Oct. &  6\ldots &  6 & 21 & `` &  6 & 27 & ``  && 1 & 36 & 40  \\
+& ``   & 16\ldots &  5 & 42 & `` &  5 & 48 & ``  && 1 & 36 & 40  \\
+& ``   & 26\ldots &  5 & 03 & `` &  5 & 08 & ``  && 1 & 36 & 30  \\
+& Nov. &  5\ldots &  4 & 23 & `` &  4 & 29 & ``  && 1 & 36 & 30  \\
+& ``   & 15\ldots &  3 & 44 & `` &  3 & 50 & ``  && 1 & 36 & 20  \\
+& ``   & 25\ldots &  3 & 05 & `` &  3 & 11 & ``  && 1 & 36 & 20  \\
+& Dec. &  5\ldots &  2 & 25 & `` &  2 & 31 & ``  && 1 & 36 & 20  \\
+& ``   & 15\ldots &  1 & 46 & `` &  1 & 52 & ``  && 1 & 36 & 10  \\
+& ``   & 25\ldots &  1 & 06 & `` &  1 & 12 & ``  && 1 & 36 & 10  \\
+1890 & Jan. &  4\ldots & \ 12 & 27 & `` & \ 12 & 33 & ``  && 1 & 36 & 10  \\
+& ``   & 14\ldots & 11 & 43 & \textsc{p.m.} & 11 & 53 & \textsc{a.m.}  && 1 & 36 & 10  \\
+& ``   & 24\ldots & 11 & 04 & `` & 11 & 14 & ``  && 1 & 36 & 10  \\
+& Feb. &  3\ldots & 10 & 24 & `` & 10 & 34 & ``  && 1 & 36 & 10  \\
+& ``   & 13\ldots &  9 & 45 & `` &  9 & 55 & ``  && 1 & 36 & 10  \\
+& ``   & 23\ldots &  9 & 06 & `` &  9 & 16 & ``  && 1 & 36 & 10  \\
+%-----File: 069.png-----
+& Mar. & 5\ldots & 8 & 26 & \textsc{p.m.} & 8 & 36 & \textsc{a.m.} && 1 & 36 & 20  \\
+& ``     & 15\ldots &  7 & 47 & `` &  7 & 57 & `` && 1 & 36 & 20  \\
+& ``     & 25\ldots &  7 & 07 & `` &  7 & 17 & `` && 1 & 36 & 20  \\
+& April  &  4\ldots &  6 & 28 & `` &  6 & 38 & `` && 1 & 36 & 30  \\
+& ``     & 14\ldots &  5 & 48 & `` &  5 & 58 & `` && 1 & 36 & 30  \\
+& ``     & 24\ldots &  5 & 09 & `` &  5 & 19 & `` && 1 & 36 & 40  \\
+& May    &  4\ldots &  4 & 30 & `` &  4 & 40 & `` && 1 & 36 & 40  \\
+& ``     & 14\ldots &  3 & 50 & `` &  4 & 00 & `` && 1 & 36 & 40  \\
+& ``     & 24\ldots &  3 & 11 & `` &  3 & 21 & `` && 1 & 36 & 50  \\
+& June   &  3\ldots &  2 & 32 & `` &  2 & 42 & `` && 1 & 36 & 50  \\
+& ``     & 13\ldots &  1 & 53 & `` &  2 & 03 & `` && 1 & 36 & 50  \\
+& ``     & 23\ldots &  1 & 14 & `` &  1 & 23 & `` && 1 & 36 & 50  \\
+& July   &  3\ldots &\ 12 & 35 & `` &\ 12 & 44 & `` && 1 & 36 & 50  \\
+& `` & 13\ldots & 11 & 55 & \textsc{a.m.} & 12 & 04 & `` && 1 & 36 & 50  \\
+& `` & 23\ldots & 11 & 16 & `` & 11 & 22 & \textsc{p.m.} && 1 & 36 & 50  \\
+& Aug.   &  2\ldots & 10 & 37 & `` & 10 & 43 & `` && 1 & 36 & 40  \\
+& ``     & 12\ldots &  9 & 58 & `` & 10 & 04 & `` && 1 & 36 & 40  \\
+& ``     & 22\ldots &  9 & 19 & `` &  9 & 25 & `` && 1 & 36 & 40  \\
+& Sept.  &  1\ldots &  8 & 40 & `` &  8 & 46 & `` && 1 & 36 & 30  \\
+& ``     & 11\ldots &  8 & 00 & `` &  8 & 06 & `` && 1 & 36 & 30  \\
+& ``     & 21\ldots &  7 & 21 & `` &  7 & 27 & `` && 1 & 36 & 30  \\
+& Oct.   &  1\ldots &  6 & 42 & `` &  6 & 48 & `` && 1 & 36 & 20  \\
+& ``     & 11\ldots &  6 & 02 & `` &  6 & 08 & `` && 1 & 36 & 20  \\
+& ``     & 21\ldots &  5 & 23 & `` &  5 & 29 & `` && 1 & 36 & 10  \\
+& ``     & 31\ldots &  4 & 44 & `` &  4 & 50 & `` && 1 & 36 & 00  \\
+& Nov.   & 10\ldots &  4 & 05 & `` &  4 & 10 & `` && 1 & 36 & 00  \\
+& ``     & 20\ldots &  3 & 25 & `` &  3 & 31 & `` && 1 & 36 & 00  \\
+& ``     & 30\ldots &  2 & 46 & `` &  2 & 52 & `` && 1 & 35 & 50  \\
+& Dec.   & 10\ldots &  2 & 07 & `` &  2 & 12 & `` && 1 & 35 & 50  \\
+& ``     & 20\ldots &  1 & 27 & `` &  1 & 33 & `` && 1 & 35 & 50  \\
+& ``     & 30\ldots & 12 & 48 & `` & 12 & 54 & `` && 1 & 35 & 50  \\
+1891 & Jan. &  9\ldots & 12 & 09 & `` & 12 & 14 & `` && 1 & 35 & 40 \\
+\hline
+\end{longtable}
+\end{small}
+
+\clearpage
+%-----File: 070.png-----
+
+\nbsectionheading{OCCULTATIONS OF STARS BY THE MOON.}
+\addcontentsline{toc}{section}{Occultations of Stars by the Moon. Observed by \textsc{A.~O. Leuschner}}
+
+\nbsubsubsectionheading{\shortrule[6ex]\\*
+\textsc{Observed by A.~O. Leuschner.}}
+
+\bigskip
+\begin{tablesetup}
+\begin{tabular}{c@{\ }r| l@{\ }r@{\ }r@{}| rrr@{\ }| c|c|lll}
+\hline\hline
+  \multicolumn{2}{m{3em}|}{\centering\footnotesize\textsc{
+    Date.}}
+& \multicolumn{3}{m{10em}|}{\centering\footnotesize\textsc{
+    Star.}}
+& \multicolumn{3}{m{6em}|}{\centering\footnotesize\textsc{
+    Mt.\ H. M.~T. of Disappearance.}\rule{0pt}{3ex}}
+& \multicolumn{1}{m{4em}|}{\centering\footnotesize\textsc{
+    Telescope.}}
+& \multicolumn{1}{m{4em}|}{\centering\footnotesize\textsc{
+    Power.}}
+& \multicolumn{3}{m{5em}}{\centering\footnotesize\textsc{
+    Remarks.}}
+\\[1ex]  \hline
+  \multicolumn{2}{c|}{1889.}
+&&&& {\footnotesize h.} & {\footnotesize m.}
+& \multicolumn{1}{c|}{\footnotesize s.} &&&&&
+\\
+  Aug. & 29 & S D. ( $-$ & 3�) & 3459\dotfill &  7 & 26 & 31.9
+& 12-in. & 80 & \multicolumn{3}{l}{ Good. }
+\\
+  `` & 29 & S D. ( $-$ &  3�) & 3468\dotfill & 8 &  5 & 26.6
+& `` & ``  \\
+  `` & 29 & S D. ( $-$ &  3�) & 3469\dotfill & 8
+& \multicolumn{1}{@{}c@{}}{[10]} &  2.3
+& `` & `` & \multicolumn{3}{m{5em}}{\raggedright Minute probably 10.}
+\\
+  `` & 29 & S D. ( $-$ &  3�) & 3470\dotfill & 8 & 13 & 40.1
+& `` & `` & \multicolumn{3}{l}{ Good.}
+\\
+  `` & 30 & S D. ( $-$ &  8�) & 3733\dotfill & 7 & 27 & 22.5
+& `` & `` && ``
+\\
+  `` & 30 & S D. ( $-$ &  8�) & 3736\dotfill & 7 & 39 & 51.1
+& `` & `` && ``
+\\
+  `` & 30 & S D. ( $-$ &  9�) & 3896\dotfill & 7 & 58 & 51.5
+& `` & `` && ``
+\\
+  `` & 30 & S D. ( $-$ &  8�) & 3739\dotfill & 8 & 17 & 24.7
+& `` & `` && ``
+\\
+  `` & 30 & S D. ( $-$ &  9�) & 3898\dotfill & 8 & 19 & 24.0
+& `` & `` && ``
+\\
+  Sept. &  2 & S D. ( $-$ & 21�) & 4494\dotfill & 7 & 48 & 45.1
+& 6-in. & 75 && ``
+\\
+  `` &  2 & S D. ( $-$ & 21�) & 4496\dotfill & 7 & 50 & 32.9
+& `` & `` && ``
+\\
+  `` &  2 & S D. ( $-$ & 21�) & 4512\dotfill & 9 & 10 & 59.9
+& 12-in. & 80 && ``
+\\
+  `` &  3 & \multicolumn{2}{l}{ C Z. \textsc{xvii} h. } & 3871\dotfill
+&  7 & 54 & 10.9 & `` & ``
+\\
+  `` &  3 & \multicolumn{2}{l}{ C Z. \textsc{xvii} h. } & 3960\dotfill
+&  8 & 13 & 50.7 & `` & ``
+\\
+  `` &  3 & \multicolumn{2}{l}{ C Z. \textsc{xvii} h. } & 3978\dotfill
+&  8 & 22 & 40.4 & `` & `` && ``
+\\
+  `` &  3 & \multicolumn{3}{l|}{ Anonymous 9.0 } &&&&&&&&  \\
+&& \multicolumn{3}{l|}{ \tablenoteasterisk17h.\ 58m.\ 26s.; $-23�\, 16'.0$ }
+&  9 & 12 & 46.4 & `` & `` && ``
+\\
+  `` &  3 & \multicolumn{3}{l|}{ Anonymous 9.0 } &&&&&&&&  \\
+&& \multicolumn{3}{l|}{ \tablenoteasterisk17h.\ 58m.\ 37s.; $-23�\, 18'.7$ }
+&  9 & 15 & 28.9 & `` & `` && ``
+\\
+  `` &  3 & \multicolumn{3}{l|}{ Anonymous 9.0 } &&&&&&&&  \\
+&& \multicolumn{3}{l|}{ \tablenoteasterisk17h.\ 58m.\ 12s.; $-23�\, 27'.3$ }
+&  9 & 34 & 24.5 & `` & `` && ``
+\\
+  `` &  3 & \multicolumn{3}{l|}{ \label{cor3}W M Z\@. 175\dotfill} &  9 & 50 & 8.6 % corrected per corrigenda
+& `` & `` && ``
+\\
+  `` &  3 & \multicolumn{3}{l|}{ Anonymous 8.0 } &&&&&&&&  \\
+&& \multicolumn{3}{l|}{ \tablenoteasterisk18h.\ 0m.\ 1s.; $-23�\, 27'.0$ }
+& 10 &  0 &  0.2 & `` & `` && ``
+\\
+  `` &  3 & \multicolumn{3}{l|}{ Anonymous 8.5 } &&&&&&&&  \\
+&& \multicolumn{3}{l|}{ \tablenoteasterisk18h.\ 0m.\ 41s.; $-23�\, 26'.4$ }
+& 10 & 21 &  8.4 & ``  & ``  && ``
+\\
+`` &  3 & \multicolumn{2}{l}{ C Z. \textsc{xvii} h. } & 133\dotfill
+& \ 10 & 23 & 24.4 & ``  & ``  && ``
+\\  \hline
+& \multicolumn{10}{l}{\footnotesize * These positions are for 1850.0.}
+\end{tabular}
+\end{tablesetup}
+%-----File: 071.png-----
+
+\nbsectionheading{CONJUNCTION OF MARS AND SATURN (\textsc{Sept.~20, 1889}).}
+\addcontentsline{toc}{section}{Conjunction of Mars and Saturn (September~20, 1889). By \textsc{W.~E. Downs.}}
+
+\nbsubsubsectionheading{\shortrule\\*
+\textsc{By W.~E. Downs.}\\*
+\shortrule}
+
+The observations were made with the four-inch broken-tube
+comet-seeker. The times were noted on a watch running on P.S.T.
+A magnifying power of about thirty diameters was used.
+
+\begin{description}
+\item[$4^\text{h}$ $00^\text{m}$.] First sight of \textit{Saturn} and \textit{Mars} in the telescope, through
+a very dense haze. \textit{Mars} appeared as a very red, ill-defined spot of
+light. \textit{Saturn} was very red, but less so than \textit{Mars. Regulus} was
+also visible in the same field, to the south, and eight or ten times
+more distant from the planets than the space between them, and
+was of a lighter red color and fainter than either planet.
+
+\item[$4^\text{h}$ $15^\text{m}$.] Both planets were visible to the naked eye, and easily
+separated as soon as seen.
+
+\item[$4^\text{h}$ $25^\text{m}$.] \textit{Saturn}, in the telescope, was of an orange color, and
+\textit{Mars} of a light red.
+
+\item[$4^\text{h}$ $45^\text{m}$.] To the eye \textit{Saturn} was about as bright as \textit{Polaris}, and
+\textit{Mars} a little fainter.
+
+\item[$5^\text{h}$ $15^\text{m}$.] Broad daylight approached fast. $\theta$ \textit{Tauri} was still
+easily visible to the naked eye, and \textit{c Orionis}, fifth magnitude, was
+barely visible and disappeared at $5^\text{h}$ $20^\text{m}$. $\theta$ \textit{Orionis} disappeared at
+$5^\text{h}$ $23^\text{m}$, and \textit{Saturn} and \textit{Mars} at $5^\text{h}$ $30^\text{m}$.
+
+\item[$5^\text{h}$ $40^\text{m}$.] \textit{Saturn} and \textit{Mars} were of a very light yellow color in
+the telescope; \textit{Mars} being very slightly tinged with red. \textit{Regulus}
+was white.
+
+\item[$5^\text{h}$ $50^\text{m}$.] \textit{Venus} was still easily visible to the eye. The clouds
+were getting ruddy in the east. \textit{Saturn} and \textit{Mars} were growing
+very rapidly fainter. After this \textit{Regulus} was not kept in the field of
+the telescope.
+
+\item[$5^\text{h}$ $55^\text{m}$.] \textit{Mars} was easier to see than \textit{Saturn}, the light from it
+being more vivid.
+
+\item[$6^\text{h}$ $00^\text{m}$.] \textit{Saturn} and \textit{Mars} last seen in the telescope, and the
+sun's disc about two-thirds up. As the sun rose, its disc was round
+and red, and was crossed by horizontal cloud-belts.
+
+\item[$6^\text{h}$ $05^\text{m}$.] \textit{Venus} was still visible to the eye.
+
+\item[$6^\text{h}$ $10^\text{m}$.] Lost sight of \textit{Venus}, and did not again recover it. The
+sun was too far up to look at comfortably.
+\end{description}
+%-----File: 072.png-----
+
+\textit{Regulus, Saturn} and \textit{Mars} formed an interesting triangular
+group, the angle at \textit{Saturn} being slightly obtuse. This angle remained
+sensibly the same throughout the observations, although the
+planets were separating.\\*
+\rightline{\textsc{W.~E. Downs}.\quad}\\*[1ex]
+{\small\indent \textsc{Mt.~Hamilton}, 1889, Sept.~22.}
+
+
+\nbsectionheading{A VERY REMARKABLE COMET.}
+\addcontentsline{toc}{section}{A very remarkable Comet (\textsc{Brooks}, July~7, 1889). By \textsc{E.~E. Barnard}}
+
+\nbsubsubsectionheading{\shortrule\\*
+\textsc{By Edward E. Barnard.}\\*
+\shortrule}
+
+On the morning of July 7th, a small comet was discovered by
+Mr.\ \textsc{Brooks} in the constellation Cetus. The moon coming into the
+morning sky blotted the comet out before any observations (except
+three at the Lick Observatory) could be made of it. When a sufficiently
+long interval was obtained the orbit was computed, and from
+the small inclination of its path to that of the earth it was at once
+suspected to be periodic; the suspicion has since been verified, the
+comet having a period of about seven or eight years. This was sufficient
+of itself to make it of more than ordinary interest. While
+observing this object in the first part of August I discovered that it
+was attended by at least four companions, which were moving through
+space in advance of the main comet. Two of these companions
+were discovered with the twelve-inch on August 1st, and the other
+two on August 4th with the great telescope. These last two were
+seen several times, but always remained too faint to be measured,
+and finally disappeared.
+
+The two brighter companions were perfect miniatures of the
+larger comet, each having a small, fairly well-defined head and
+nucleus, with a faint, hazy tail, the more distant one being the larger
+and less-developed. The three comets were in a straight line, nearly
+east and west, their tails lying along this line. There was no connecting
+nebulosity between these objects, the tails of the two smaller
+not reaching each other or the large comet. To all appearance they
+were absolutely independent comets. The four which were discovered
+here I have named B, C, D, E, in the order of increasing right
+ascension, A being the original comet discovered by Mr.\ \textsc{Brooks}. As
+D and E disappeared after a few observations, they will not be again
+referred to; they were both north following C and in a line with it.
+
+Since discovery I have measured these objects on every available
+%-----File: 073.png-----
+occasion, using the micrometer of the thirty-six-inch equatorial. It
+was found that these two were separating from the main comet quite
+rapidly; the more distant one moving the fastest. Towards the latter
+half of August the nearer companion B ceased to recede, and
+then underwent a remarkable change. It enlarged rapidly, becoming
+extremely diffused, and losing all appearance of central condensation.
+It could be measured only with the utmost difficulty.
+Throughout its visibility its position angle remained almost constant;
+towards the last, however, this angle began slowly but sensibly to
+increase as if the companion were in orbital motion. Unfortunately,
+at this most important point in the observations, the companion
+faded rapidly and totally from view, being last seen on the 5th of
+September. It disappeared as absolutely from the face of the
+heavens as did Biela's comet, which doubtless underwent a similar
+dissolution.
+
+In the meantime the more distant companion continued to recede,
+and increased very much in brightness and size, until on August 31st
+it was perceptibly brighter than the larger comet! In the latter half
+of September it, too, became stationary with reference to the principal
+comet; remaining thus for some days, it began slowly to lessen its
+distance, having attained a maximum distance of $356''$. This object
+has also undergone a change in appearance similar to that in the
+lost companion. Its tail has disappeared, and the head has become
+large and much diffused, its brightness in the meantime having
+diminished very greatly. The position angle of this object has
+remained remarkably constant for the past two months; it attained
+a maximum of about 62� in the middle of September; since then it
+has been slowly decreasing, until it is now the same as when first
+observed.
+
+Measures of the companion B on twenty-two nights were obtained,
+and up to the present date measures of C have been made
+on forty nights.
+
+The following, selected from the observations, will give an idea
+of the relative positions of this group:
+\begin{tablesetup}
+\begin{tabular}{l@{ }r *{5}{c@{ }} l@{ } *{4}{c@{ }} r}
+&&&&&&&\multicolumn{1}{c}{�\mbox\;}
+&&&&&  \multicolumn{1}{c}{$''$}  \\
+  Aug. &  1. & Position & angle & A & and & B, & 59.4;
+& distance & A & and & B, & 64.1.\\
+  Sept.&  4. & ``        & ``     & `` &  ``  & ``\;  & 65.0
+&    ``     & `` &  ``  & ``\;  & 71.5.\\
+  Aug. &  4. & ``        & ``     & A & and & C, & 61.5
+&    ``     & A & and & C, &267.6.\\
+  Sept.& 15. & ``        & ``     & `` &  ``  & ``\;  & 62.1
+&    ``     & `` &  ``  & ``\;  &356.4.\\
+  Sept.& 30. & ``        & ``     & `` &  ``  & ``\;  & 61.4
+&    ``     & `` &  ``  & ``\;  &352.1.
+\end{tabular}
+\end{tablesetup}
+
+It is hoped that through measures of the relative positions of
+%-----File: 074.png-----
+these bodies we shall be enabled to detect orbital motion of the
+smaller ones about the larger. If this were shown to exist, we
+should at once have the means of determining the mass of this
+cometary system. These changes may, however, be due to perspective.
+
+So far as we know, the phenomenon presented by this comet is
+extremely rare. It is needless to repeat the story of Biela's comet.
+In 1845 it separated into two distinct comets, which traveled side by
+side, and returning at the appointed time, they were seen to be
+widely separated---indeed, moving in distinctly separate paths; they
+then disappeared, to be seen no more in the heavens. One of the
+comets of 1861 was seen double for a few days. Some companions
+were seen moving with the Great Comet of 1882, but no measurements
+were made. This covers our knowledge of multiple comets,
+or comets with companions, unless, indeed, we accept the evidence
+of the Chinese records, which possibly describe comets that consisted
+of two or more parts.\\*[1ex]
+{\small\indent\textsc{Mt.~Hamilton,} September~30, 1889.}
+
+\medskip
+\begin{small}
+\textsc{Note.}---In order not to delay the publication of the present number, the
+printing of two papers on Drawings of \textit{Jupiter} in the years 1875--1883, by Messrs.\ \textsc{Holden}
+and \textsc{Barnard}, is postponed to the next number.
+
+\end{small}
+
+\ThoughtBreakLong
+
+
+\nbsectionheading{NOTICES FROM THE LICK OBSERVATORY.}
+\addcontentsline{toc}{section}{\textit{Notices from the Lick Observatory}}
+
+\nbsubsubsectionheading{\shortrule\\*
+{\small \textsc{Prepared by Members of the Staff.}}\\*
+\shortrule}
+
+\nbsubsectionheading{Photographing the Milky Way.}
+\addcontentsline{toc}{subsection}{\qquad Photographing the Milky Way. By \textsc{E.~S. Holden}}
+
+The great success obtained by Mr.\ \textsc{Barnard} in his preliminary
+experiments with the \textsc{Willard} portrait lens ($a=5.9$, $f=30.7$) has
+led to the determination to employ it in making a systematic study
+of the Milky Way by photography. For this purpose it has been
+mounted at the object-glass end of the tube of the great telescope,
+and arrangements made by which the lens can be capped and uncapped
+from the eye end. The driving clock of the great telescope
+(with a control) will keep the camera directed at the star-group
+chosen during an exposure of two hours. An independent equatorial
+stand for this instrument is very desirable, but cannot be had
+%-----File: 075.png-----
+at present. Plates $8�10$ are used, which correspond to about 16
+by 20 degrees. The definition is good over the central 10 or 11
+degrees.\pushright{E.~S.~H.}
+
+\bigskip
+
+
+\nbsubsectionheading{Occultation of \textit{Jupiter}, 1889, September~3.}
+\addcontentsline{toc}{subsection}{\qquad Occultation of Jupiter, 1889, September~3}
+
+\begin{tablesetup}
+\begin{tabular}{l|l|l|l|l}
+\hline\hline
+\multicolumn{1}{c|}{
+\multirow{6}{*}{\footnotesize\textsc{Phenomenon Observed.}}}
+&\multicolumn{4}{c}{}\\
+&\multicolumn{4}{c}{\footnotesize\textsc{
+    Initials of the Observer.}}\\
+&\multicolumn{4}{c}{}\\
+\cline{2-5}
+&\multicolumn{4}{c}{}\\
+&\multicolumn{4}{c}{\footnotesize\textsc{
+    Lick Observatory Mean Time.}}\\
+&\multicolumn{4}{c}{}\\
+\hline
+& \multicolumn{1}{c|}{J.~E.~K.}& \multicolumn{1}{c|}{E.~E.~B.}
+& \multicolumn{1}{c|}{C.~B.~H.}
+& \multicolumn{1}{c }{A.~O.~L.\rule{0pt}{3ex}}\\
+& \multicolumn{1}{c|}{\rule[0.5ex]{2em}{.2pt}}
+& \multicolumn{1}{c|}{\rule[0.5ex]{2em}{.2pt}}
+& \multicolumn{1}{c|}{\rule[0.5ex]{2em}{.2pt}}
+& \multicolumn{1}{c }{\rule[0.5ex]{2em}{.2pt}}
+\\
+& \textit{\footnotesize h.\ m.\quad s.}
+& \textit{\footnotesize\,m.\quad s.}
+& \textit{\footnotesize\,m.\quad s.}
+& \textit{\footnotesize\,m.\quad s.}\\
+
+First Contact of \textit{Jupiter}\dotfill
+& 5 25 39.1&  25 41.3&  25 43.5\tablenoteasterisk&  25 41.6\\[1ex]
+Second Contact of \textit{Jupiter}\dotfill
+& 5 27 50.7&  27 47.3&   27 47.8&   27 43.9\\[1ex]
+Reappearance of Satellite II\dotfill
+&  6 11 33$\pm$
+& \multicolumn{1}{c|}{\ldots\ldots}
+& \multicolumn{1}{c|}{\ldots\ldots}
+& \multicolumn{1}{c }{\ldots\ldots}
+\\[1ex]
+Reappearance of Satellite IV.
+&  6 16 46.2
+& \multicolumn{1}{c|}{\ldots\ldots}
+& \multicolumn{1}{c|}{\ldots\ldots}
+& \multicolumn{1}{c }{\ldots\ldots}
+\\[1ex]
+Third Contact of \textit{Jupiter}\dotfill
+& 6 19 17.2
+& \multicolumn{1}{c|}{\ldots\ldots}
+& \multicolumn{1}{c|}{\ldots\ldots}
+&  19 26.2\\[1ex]
+Fourth Contact of \textit{Jupiter}\dotfill
+& 6 21 39$\pm$&  21 38.3::&  21 39.5::&  21 32.2\\[1ex]
+Reappearance of Satellite I\dotfill
+&  6 23 12.8&  23 15.7::&  23 16.0\tablenotedagger
+& \multicolumn{1}{c }{\ldots\ldots}
+\\
+& \multicolumn{1}{c|}{\rule[0.5ex]{2em}{.2pt}}
+& \multicolumn{1}{c|}{\rule[0.5ex]{2em}{.2pt}}
+& \multicolumn{1}{c|}{\rule[0.5ex]{2em}{.2pt}}
+& \multicolumn{1}{c }{\rule[0.5ex]{2em}{.2pt}}
+\\
+(Instrument employed)\dotfill
+& \multicolumn{1}{c|}{\textit{36-inch Tel.}}
+& \multicolumn{1}{c|}{\textit{\ 12-inch Tel.}}
+& \multicolumn{1}{c|}{\textit{6\,\raisebox{.2ex}{\tiny$^{1}\!/\!_{2}$}-in. Tel.}}
+& \multicolumn{1}{c }{\textit{Comet seeker.}}\\[1ex]
+\hline
+\multicolumn{5}{l}{\begin{footnotesize}
+\textsc{Observers' Notes}.---* 3--5 secs.\ late; \quad$\dagger$ 2--3 secs.\ late.
+\end{footnotesize}}
+\end{tabular}
+\end{tablesetup}
+
+\begin{small}
+\medskip
+Mr.\ \textsc{Schaeberle} obtained several photographs of the Moon and \textit{Jupiter}
+after IVth Contact.
+
+\medskip
+\textit{Observers}: \;Mr.\ \textsc{Keeler}\,=\,J.~E.~K.; \;Mr.\ \textsc{Barnard}\,=\,E.~E.~B.;
+\;Mr.\ \textsc{Hill}\,=\,C.~B.~H.; \;Mr.\ \textsc{Leuschner}\,=\,A.~O.~L.
+
+These observations have been printed \textit{in extenso} in the \textit{Astronomical Journal},
+Vol.~9, page~84 \textit{et seq.}
+
+\end{small}
+
+
+\nbsubsectionheading{Examination of Stellar Photographs.}
+\addcontentsline{toc}{subsection}{\qquad Examination of Stellar Photographs. By \textsc{E.~S. Holden}}
+
+If it is desired to obtain \emph{all} the information which can be had
+from a given negative, it is necessary to make a positive copy of it on
+glass, and to examine both negative and positive independently.
+Each presents a different set of contrasts. The negative will show
+the empty spaces and lanes between stars; the positive will show the
+arrangement of the stars themselves. It is only by examining both
+that \emph{all} the information can be had from a given exposure. This is
+certainly true for stellar photographs, and it is even more important
+in regard to photographs of surfaces,---as nebul�, the corona, etc.
+It should also be remembered that no single negative can establish
+the existence of a new nebula. At least two are required.
+%-----File: 076.png-----
+
+Experiments by Mr.\ \textsc{Barnard} have shown that many features
+may be brought out by the simple device of copying the whole of an
+$8�10$ plate on a plate of $3\frac{1}{4} � 4\frac{1}{4}$ inches. This process is analogous
+to the automatic one by which a person places a picture to be
+viewed at an appropriate distance for seeing the particular details he
+wishes to examine. Enlargements of negatives are sometimes serviceable,
+also. These simple precautions are worth mentioning, as
+they help to emphasize a fundamental point, namely,---that it is far
+more important to extract all possible information from a few photographs,
+than to make large collections of negatives without sufficiently
+examining each of them.\pushright{E.~S.~H.}
+
+\nbsubsectionheading{Review of the Early Numbers of the \textit{Publications of the Astronomical Society of the Pacific}.}
+\addcontentsline{toc}{subsection}{\qquad Review of the early numbers of the Publications of the Astronomical Society of the Pacific [by Professor \textsc{E.~Schoenfeld}]}
+
+The \textit{Vierteljahrsschrift} of the German Astronomical Society
+(Vol.~24, 1889, p.~210) has a very friendly review of the Nos.~1
+and 2 of our own \textit{Publications}, written by Professor E. \textsc{Schoenfeld},
+Director of the Observatory of Bonn. The last paragraph is:
+``The Reviewer has no right to speak in this place in the name of
+the \textit{Astronomische Gesellschaft}; but, in his own name and in that
+of other members, he expresses a hearty greeting to the new Society
+which has been founded on the Coast of the Pacific Ocean and
+wishes for it all success and prosperity.''
+
+It will be gratifying to our members to know of this early and
+courteous recognition of our modest beginnings.\pushright{E.~S.~H.}
+
+\nbsubsectionheading{Note on the Corona of January~1, 1889.}
+\addcontentsline{toc}{subsection}{\qquad Note on the Corona of January~1, 1889 [by Professor \textsc{P. Tacchini}]}
+
+Professor \textsc{Tacchini} has a note in the \textit{Atti della R. Accademia
+dei Lincei} 1889, page 472, on the corona as shown in a positive-copy
+on glass of one of Mr.\ \textsc{Barnard's} negatives. The corona extends,
+he says, from $+64�$ to $-68�$ on the west limb of the Sun, and
+from $+53�$ to $-68�$ on the east limb. These are about the limits
+of the zone of the maximum frequency of protuberances defined by
+Professor \textsc{Tacchini's} own observations. Two of the protuberances
+of the photograph were observed at Rome and at Palermo. The
+other protuberances shown on the photograph were not seen by the
+spectroscope, and Professor \textsc{Tacchini} surmises that they belong to
+the class of \emph{white} protuberances discovered by him at the eclipses
+of 1883 and 1886. This surmise is completely corroborated by
+%-----File: 077.png-----
+the observations of Professor \textsc{Swift} (L.~O. Eclipse Report, 1889,
+Page~203).\pushright{E.~S.~H.}
+\medskip
+
+\nbsubsectionheading{Zenographical Fragments.}
+\addcontentsline{toc}{subsection}{\qquad Zenographical Fragments [by \textsc{A. Stanley Williams, F.~R.~A.~S.}]. Notice by \textsc{E.~S. Holden}}
+
+\nbsubsubsectionheading
+{\textit{The Motions and Changes of the Markings on Jupiter, during 1886--7.}}
+
+Under this title Mr.\ A.~\textsc{Stanley Williams}, F.R.A.S., has
+printed a handsome octavo volume, of 118 pages and nine carefully
+executed plates, which gives the results of his own observations during
+1886--7 with a $6\frac{1}{2}$ inch reflecting telescope (power 170). The
+work consists of seven sections, as follows: Section I treats of the
+instrument and the methods of observation (usually transits over
+the central meridian, 312 of which were observed); II treats of the
+construction of the chart of the markings on \textit{Jupiter} (which gives
+the relative positions of all the spots from all the observations, reduced
+to the positions which they would have occupied had every
+observation been made April~21, 1887, the date of opposition);
+III speaks of the general arrangement of the belts, and gives an excellent
+system of nomenclature for the various separate features;
+IV, by far the longest section, presents the observations of the different
+spots in a most convenient form; V gives a summary of rotation
+periods in different Jovian latitudes; VI relates to the different
+altitudes (in \textit{Jupiter's} atmosphere) of the different features; while
+VII treats of the repellant influence apparently exercised by the
+Red Spot on markings in its neighborhood.
+
+This work deserves an extended notice, which cannot be given
+here; but it should not be allowed to pass without remark, since it
+affords an admirable example of just the kind of work which amateur
+observers can prosecute with great success. Its author (a professional
+man, constantly occupied) has chosen a definite problem, suitable
+to his instrumental equipment, and by dint of clear conceptions
+of the nature of the problem to be solved and of persevering observations
+in his leisure moments, has produced a work of lasting value.
+It appears that this volume is to be followed by others on the same
+subject from the same hand. It can be obtained from \textsc{Mitchell \&
+Hughes}, publishers, 140 Wardour street, London. The price is
+not stated.\pushright{E.~S.~H.}
+
+\nbsubsectionheading{Accommodation for Visitors to the Observatory.}
+\addcontentsline{toc}{subsection}{\qquad Accommodation for Visitors to the Observatory}
+
+In order to accommodate visitors to the Observatory on the public
+evenings, a continuous bench, long enough to seat one hundred
+%-----File: 078.png-----
+persons, has been built on the east, south and west sides of the upper
+gallery of the large dome. As we sometimes have as many as
+two hundred and fifty visitors to the Observatory during one of our
+public nights, this addition has become necessary.
+
+The Gundlach Optical Co., of Rochester, N.~Y., is making a
+low-power eye-piece with a large field---something like half a degree---for
+the use of visitors who come to see the Moon. Such an eye-piece
+will show enough of the lunar surface to make a \emph{picture} with a
+background of sky, which is what is really needed to convey the
+effect. The eye-pieces used in the regular astronomical observations
+have fields of view of hardly more than $10'$ of arc, and, hence, only
+serve to show a limited portion of the Moon's surface---less than
+one-tenth, usually. As the image of the Moon in the large telescope
+is 6.51 inches in diameter, it follows that the field lens of the new
+eye-piece must be of about the same dimensions. It will be useful
+in real work also, for objects like nebul�  and comets, where a large
+field and full contrast are required.\pushright{E.~S.~H.}
+
+\nbsubsectionheading{American Equatorial Mountings on Sale in Berlin.}
+\addcontentsline{toc}{subsection}{\qquad American Equatorial Mountings in Berlin}
+
+The Observatory has lately received the price-list of \textsc{Th. Wegener}
+of Berlin. So far as I have examined it, the instruments appear to be
+well-designed. It is not for this reason that it is mentioned, but
+because, on page 6, there is given a full-page wood-cut of the equatorial
+telescope and mounting of the Observatory of Beloit College,
+Wisconsin. This admirable mounting was made by \textsc{Warner \&
+Swasey}, of Cleveland, from their own designs, and it is an excellent
+model to follow. It would have been more straightforward for Herr
+\textsc{Wegener} to have made some acknowledgment of the source from
+which he derived his model. His wood-cut has no title, and conveys
+the impression that the design was made by him. Messrs.\ \textsc{Warner
+\& Swasey} have, however, no cause to complain. Imitation is the
+sincerest flattery. I can heartily recommend the design of the mounting
+which Herr \textsc{Wegener} proposes to make.\pushright{E.~S.~H.}
+
+\nbsubsectionheading{Notes on Double Stars.}
+\addcontentsline{toc}{subsection}{\qquad Notes on Double Stars. By \textsc{S.~W. Burnham}}
+
+The \textsc{Herschel} companion to $\phi^{1}$ \textit{Aquarii} is shown in the 36-inch
+telescope to be a very close double star. From a single measure
+the distance appears to be less than $0''.15$, and, of course, it is a different
+object, even in a large refractor. This companion has the
+same proper motion as the large star, and the relative change is
+%-----File: 079.png-----
+practically nothing since the measures of \textsc{Struve}, in 1836, when
+the distance was $49''.63$ in the position-angle of 312�.2.
+
+Prof. \textsc{Hough} found the neighboring star $\phi^{3}$(95) \textit{Aquarii} double,
+with the Chicago $18\frac{1}{2}$-inch refractor, in 1884, the companion being
+eleventh magnitude, at a distance of a little more than $1''$. Last year
+this was noted independently here with the 12-inch, and measured
+on three nights, the result being substantially the same as the
+single measure by \textsc{Hough} in 1884. In the course of the observations
+given above, this star was looked at with the 36-inch on two or
+three nights, but there was not the faintest trace of the companion.
+I am wholly unable to account for this failure, as there was apparently
+no change in the preceding four years. It should be carefully
+watched hereafter.
+
+The sixth magnitude star, 44 \textit{Cassiopei�}, has a minute attendant,
+hitherto unseen, at a distance of $1''.7$ from the principal star.
+
+Several new pairs have been found in the \textit{Pleiades}, one of them
+following \textit{Alcyone} $64^{\text{s}}$ and about $4'$ north. This is a difficult pair, as
+the distance is only $0''.3$, and the components below the ninth magnitude.
+Another new pair, still more difficult, is $55^{\text{s}}$ following \textit{Pleione}
+(28 \textit{Tauri}). The distance of this pair is about $0''.4$, but the components
+are only $11\frac{1}{2}$ magnitude.
+
+Since the time of \textsc{Herschel}, 67 \textit{Ophiuchi} has been known as a
+wide double star ($54''$). The large telescope shows a very faint star
+at a distance of $6''.8$.
+
+The star D.~M. 63�, 1618, has a very small companion at a distance
+of $4''.3$. The principal star is brighter than sixth magnitude,
+but is strangely wanting in nearly all of the star catalogues covering
+this part of the heavens. It is not in the B.~A.~C., Radcliffe (1 and 2),
+Lalande, Argelander U.~N., Heis, Piazzi, Bradley, Romberg, AOe,
+Grant, D'Agelet, Armagh, Yarnall, Bonn observations. In fact, it is
+found only in the D.~M. and Rumker (No. 8289), the magnitudes
+being 5.9 and 5.6, respectively. In the Harvard Photometry the
+magnitude is 5.82. In observing it here as a double star the magnitude
+was estimated 5.8. It does not appear to be variable, and is
+probably a rare example of star catalogue omissions. The attention
+of meridian observers is called to this object.\footnote{This star will be observed by Professor \textsc{Schaeberle} with the L.~O. meridian circle.---E.~S.~H.}
+
+The double star, $\Sigma 2816$, consists of a sixth magnitude primary,
+and two $7\frac{1}{2}$ m.\ companions with distances from the larger star of
+about $12''$ and $20''$, respectively. These stars have remained relatively
+%-----File: 080.png-----
+fixed since 1832. The large telescope shows a minute companion
+within $1''.5$ of the large star.
+
+The fifth magnitude star, 2 \textit{Andromed�}, is a very close and difficult
+pair, the distance being only $0''.8$, and the components quite
+unequal. This was suspected with the 12-inch, and verified and
+measured with the 36-inch.
+
+\textsc{Herschel} noted a ninth magnitude companion to $\alpha$ \textit{Cassiopei�} at
+a distance of $63''$. The large telescope shows a very faint star at a
+distance of $17''.5$.
+
+The distance of the close pair in $\gamma$ \textit{Andromed�} (0$\Sigma$38) is now
+less than $0''.1$. It is very difficult, and the best conditions are
+necessary to see the elongation at all with the large telescope.
+
+The binary star, 7 \textit{Tauri}, has been rapidly changing. The distance
+now is $0''.30$.
+
+The large refractor fails to show any third star in the system of
+70 \textit{Ophiuchi}, and both components are single with all powers. At
+one time 72 \textit{Ophiuchi} was thought to be double (0$\Sigma$342), but no
+companion can be seen here.\pushright{S.~W.~B.}
+
+\medskip
+\nbsubsectionheading{Notes on Stellar Spectra.}
+\addcontentsline{toc}{subsection}{\qquad Notes on Stellar Spectra. By \textsc{J.~E. Keeler}}
+
+The spectra of the following stars (among many others) have been
+examined here during the past summer with a small spectroscope
+attached to the 36-inch equatorial, and in response to inquiries which
+have been made, I give below a preliminary statement of the results.
+The spectroscope which was used has no measuring apparatus, and
+the positions of lines are merely eye estimates.
+
+$\gamma$ \textit{Cassiopei�}. This star is the most conspicuous example of
+\textsc{Vogel's} class I\textit{c}, and remarkable changes in the bright lines in its
+spectrum have been observed by \textsc{von Konkoly}, \textsc{von Gothard} and
+others. I have therefore examined it frequently, but, so far, no
+changes have been seen. The C and F lines are brilliant, narrow
+and sharp; H$\gamma$, in the violet, is seen with some difficulty. The
+green is full of very fine, delicate dark lines, seen only under good
+atmospheric conditions, the \textit{b} group being somewhat more prominent
+than the others. There is also an appearance of faint bright lines in
+the green, which may be due to the actual existence of bright lines,
+or, perhaps, to spaces between the fine dark lines just mentioned,
+seeming bright by contrast. It is difficult to decide on this point.
+There are in all eight or ten such places. Somewhat nearer to C
+than to the estimated position of D is a fairly prominent dark band,
+%-----File: 081.png-----
+or, more probably, group of fine lines. Not the slightest trace of
+either dark or bright lines can be seen in the vicinity of D. The
+continuous spectrum close to the bright hydrogen lines appears
+somewhat darker than it does elsewhere, but this I have considered
+to be the effect of contrast.
+
+\textit{U Cygni}. This is a very red star, with a spectrum described by
+\textsc{Dun�r} as III\textit{b}. When examined with the 36-inch refractor it was
+of about the tenth magnitude, and the spectrum was dim, but the
+zones in the lower part could be distinguished. The blue was
+excessively faint. There was no appearance of bright lines.
+
+\textit{V Cygni} is also a very red star, and when examined with the
+spectroscope was of about the same brightness as \textit{U Cygni}. Its
+spectrum is described by \textsc{Dun�r} as III\textit{b}! The sky was remarkably
+smoky when observations were made here, and the spectrum was
+dim, but at three places in the yellow and green shone with such
+comparative brightness that these places appeared like bright lines.
+The brightest was the more refrangible yellow line. It is possible
+that these lines may be the edges of the usual zones of class III\textit{b},
+as \textsc{Dun�r} says the yellow and green zones are very bright, but the
+appearance was more like that of bright lines.
+
+\textit{D.~M. 43�, No}.~3571. This is a star recently found by Prof.\ \textsc{Pickering},
+by the aid of photography (A.~N. 2912), to belong to
+class II\textit{b}. It is much like the other stars of this class found by
+Prof.\ \textsc{Pickering} and by \textsc{Wolf} and \textsc{Rayet}. The faint spectrum
+connecting the principal bright lines in the spectra of these stars
+appears to be continuous with a small instrument, but with the
+36-inch refractor is seen to be an extremely complicated range of
+absorption bands and faint bright lines. The above star differs
+from others that I have examined in the unusual broadness and
+diffuseness of these faint bands.\pushright{J.~E.~K.}
+
+\nbsubsectionheading{``An Improved Astronomical Mirror.''}
+\addcontentsline{toc}{subsection}{\qquad ``An Improved Astronomical Mirror''}
+
+A device for constructing large telescope mirrors, which has recently
+been patented (at an expense of \$60), is described under the
+above title in the \textit{Scientific American} for September~7, 1889. The
+mirror is a flat, circular disc of metal, supported around its circumference
+by a flange or shoulder on the cell. Through a hole in its centre
+passes a bolt, and by turning a nut on the outside of the cell, the
+mirror is ``buckled'' into shape. The inventor has omitted to mention
+that by carrying the motion of the nut to a convenient position
+%-----File: 082.png-----
+near the eye-piece a ready adjustment of the focus will be obtained.
+This method has the great advantages of simplicity and cheapness;
+its defects will be ascertained by the inventor when he comes to
+try it.\pushright{J.~E.~K.}
+
+\nbsubsectionheading{Observations on the near approach of Mars and Saturn on
+September~19, 1889.}
+\addcontentsline{toc}{subsection}{\qquad Observations of the near approach of Mars and Saturn, September~19 1889. By \textsc{E.~E. Barnard}}
+% Transcriber's note: Original text reads "September 29" in the table of contents
+% In the Smithsonian/NASA Astrophysics Data System is a document (Bibliographic code: 1889QB384.M37......),
+% entitled "On the close conjunction of Mars and Saturn near Ragulus on Sept. 19, 1889", author Albert Marth.
+
+The eastern sky was thick with haze when the two planets rose,
+and they were not visible until a considerable altitude was attained.
+At about 4~\textsc{a.~m.}\ they could be seen dimly with the naked eye;
+\textit{Mars}, small and insignificant, slightly east of \textit{Saturn}. As soon as
+the images were at all measurable, I made a series of micrometrical
+observations of the two for position angle and distance, and for
+differences of right ascension and declination, using the 12-inch
+equatorial.
+
+Following are the measures which are corrected for refraction in
+distance and in the $\Delta \delta$ and $\Delta \alpha$; the times being Mt.\ Hamilton
+mean time:
+\begin{tablesetup}
+\begin{tabular}{*{5}{c@{ }}c c@{ }c@{ }l@{ }c c@{ }l@{ } c@{ }c@{ }l}
+&&\multicolumn{1}{r@{ }}{\footnotesize\textit{d.}}
+& \multicolumn{1}{r@{ }}{\footnotesize\textit{h.}}
+& \multicolumn{1}{c@{ }}{\footnotesize\textit{m.}}
+& \multicolumn{1}{c@{ }}{\footnotesize\textit{s.\;}}
+\\
+1889.& Sept.& 19 & 16 & 16 & 39.
+& \multicolumn{9}{l}{Position angle of \textit{Mars}, $101�.0$ (3).}
+\\
+``& ``&  19 & 16 & 24 & 24.
+& Dist. & betw'n & outer & \multicolumn{2}{@{}l}{limbs of}
+& \textit{Mars} & and & \textit{Saturn},
+& $356''.1$ (3).
+\\
+``& ``&  19 & 16 & 29 & 14.
+& ``& ``& \multicolumn{2}{@{}l}{nearer} & ``\mbox\quad & ``& ``& ``
+& $342''.3$ (3).
+\\
+``& ``&  19 & 16 & 34 & 19.
+& ``& ``& \multicolumn{7}{@{}l}{center and center, $358''.8$ (3).}
+\\
+``& ``&  19  & 16 & 39 & 49.
+& \multicolumn{9}{l}{Position angle of \textit{Mars}, $101�.8$ (4).}
+\\
+``& ``&  19 & 17 & 36 & \multicolumn{1}{@{}c@{}}{29.\footnotemark[7]}
+& \multicolumn{9}{l}{
+    $\Delta~\delta$ \hspace{2.5mm}\mars\ $-$ \saturn \hspace{2mm}
+    $-1'\;\,39''.2$ (5) apparent.}
+\\
+``& ``&  19 & 17 & 45 & \multicolumn{1}{@{}c@{}}{49.\footnotemark[7]}
+& \multicolumn{9}{l}{
+    $\Delta~\alpha$ \hspace{2mm}\mars\ $-$ \saturn \hspace{2mm}
+    $-0^\text{m} 29^\text{s}.91$ (11) apparent.}
+\end{tabular}
+\end{tablesetup}
+\footnotetext[7]{These times are for the bisection of \textit{Mars}.}
+
+The most striking feature was when the two planets were fading
+from the advent of daylight. At the approach of day \textit{Saturn} assumed
+a pale, ashy hue, with a slight tinge of yellow, while \textit{Mars}
+retained its lustre in a surprising manner, being of a strong orange
+yellow in color; its north polar cap stood out strikingly towards the
+close of the observations, a dark marking being also visible near the
+middle of the disc. \textit{Saturn} ceased to be visible in the telescope at
+18h.\ 6m., the last glimpse being had a few seconds earlier. At this
+time \textit{Mars} was easily conspicuous, the sun being 5� or 6� high and the
+sky pretty thick. At 18h.\ 10m.\ \textit{Mars} began to grow pale. At 18h.\ 25m.\ it
+was still visible but very pale and easily lost in the field, though
+it could have been followed for some time longer. By the time the
+%-----File: 083.png-----
+planets were high enough to observe with the large telescope they
+had separated too far to be brought into the field of view of the
+largest eye-piece.\pushright{E.~E.~B.}\\*[1ex]
+{\small\indent\textsc{Mt. Hamilton}, Sept. 20th, 1889.}
+
+\nbsubsectionheading{The Uses of Trails of Stars in Measurements of Position
+or of Brightness.}
+\addcontentsline{toc}{subsection}{\qquad The Uses of Trails of Stars in Measurements of Position or of Brightness. By \textsc{E.~S. Holden}}
+
+Photographs of star groups may be made for either one of three
+important objects. They may serve---(\textit{a}) to give a picture merely;
+(\textit{b}) for measurement of the relative positions of the stars of the group;
+or, (\textit{c}) for measurement of the photographic magnitudes of the stars
+of the group. For the first purpose the stars must be photographed
+as points or \emph{dots}. Such dots may also be used for the purposes \textit{b}
+and \textit{c}. For the purposes \textit{b} and \textit{c} it will often be very advantageous
+to employ \emph{trails} instead of \emph{dots}. The difference of declination of
+two stars, A and B, can be more accurately determined from measures
+made of the distance apart of their \emph{trails} than from measures of the
+distance of the corresponding \emph{dots}; just as a star can be more accurately
+bisected in declination by a Z.~D. micrometer than in R.~A.\ by
+a fixed thread. Hence the use of trails in R.~A. If now we can
+produce trails in declination, a corresponding advantage can be had
+for measures of differences of R.~A. The negative plate of the
+great equatorial is to be mounted on a compound slide-rest. The
+upper slide-rest which carries the plate has a motion in any desired
+direction (usually in R.~A.), and the lower slide-rest, which carries
+both plate and upper rest, has a motion at right angles to the direction
+for the upper slide.
+
+If a clock-work motion is attached to the lower slide, this slide
+can be moved in declination (say) for a certain distance (only).
+It will finally come to the end of its run. Suppose the telescope at
+rest, the objective covered and the lower slide-rest moving in declination.
+If an exposure is now made, we shall have trails suitable
+for measuring differences of R.~A. After a few minutes, the lower
+slide comes to the end of its run. Trails in R.~A. are now produced,
+which are suitable for measures of differences of declination.
+
+The direction of motion of the lower slide may be ordered in
+\emph{any} desired position angle. Thus we may choose the direction of
+the first set of trails so as to be most advantageous for the subsequent
+measures. The second set of trails will always be in R.~A.
+The angle between the first and second directions will define the
+%-----File: 084.png-----
+position angle of the first trails. It is believed that this simple
+method will have important bearings on the determination of stellar
+parallax by photography, a research for which the great equatorial
+is especially fitted.
+
+Trails may also be used to determine the magnitudes of the stars.
+The blackening of the plate is proportional to the photographic magnitude
+of the star and to the star's rate of motion on the plate (and
+to other things, also).
+
+Two stars at different declinations will move at different rates on
+the plate and hence will produce trails of different intensity. A
+(theoretical) correction for the different rates of motion can be made
+and the measures of the relative intensities of the trails can be taken
+as measures of the relative magnitudes of the stars. This method
+has been extensively used by the Harvard College Observatory.
+
+I will not here discuss the objections to the method, but will
+simply show how all objections can be overcome by adopting an ingenious
+proposal made by Professor \textsc{Schaeberle}. His suggestion is
+to photograph the trails of all stars on a plate moving in declination
+at the same rate that an equatorial star moves in R.~A. All trails
+will then have the same exposure. The rate of the clock which
+drives the plate in declination can be tested at any time by photographing
+\emph{both} trails (R.~A. and Dec.) of the same equatorial star.
+
+It appears to me that a photometry of all stars sufficiently bright
+to give such trails should be made by this method. For fainter stars
+the method described by Professor \textsc{Schaeberle} \textit{(Publ.\ Ast.\ Soc.\ Pacific},
+No.~4) should be employed.\pushright{E.~S.~H.}\\*[1ex]
+{\small\indent\textsc{Lick Observatory}, July~15, 1889.}
+
+\clearpage
+%-----File: 085.png-----
+
+\nbsectionheading{\textsc{Minutes of the Meeting of the Board of Directors, held
+September~28, 1889, at the Lick Observatory.}}
+\addcontentsline{toc}{section}{Minutes of the Meeting of the Board of Directors, September~28, 1889}
+
+A quorum was present.
+
+The report of the Treasurer was received and ordered on file.
+
+The printing of a circular of information was authorized.
+
+Hon. R.~W. \textsc{Waterman}, Governor of California; \textsc{Henry Lord Boulton},
+Esq., Caracas, Venezuela; Mrs. \textsc{Anna Palmer Draper}, New York City, were
+duly elected as life members of the Society.
+
+It was \textit{Resolved}, That the design for the Society's diploma recommended by
+the Committee be adopted, and that 500 copies of it be printed by Messrs.\ \textsc{Button}
+\& \textsc{Rey}.
+
+Mr.\ \textsc{Pierson} reported that the Society had been incorporated on August
+28, 1889.
+
+The thanks of the Board of Directors were offered to Mr.\ \textsc{Pierson} for his
+kind services in the matter of incorporating the Society, and also to Mr.\ \textsc{Knox},
+notary. The fees to State officers were ordered paid.
+
+It was ordered that the Secretary in San Francisco be furnished with a revolving
+fund of \$10 for the payment of petty bills. Adjourned.
+
+\nbsectionheading{\textsc{Minutes of the Meeting of the Astronomical Society of the
+Pacific, held September~28, 1889, at the
+Lick Observatory.}}
+\addcontentsline{toc}{section}{Minutes of the Meeting of the Astronomical Society of the Pacific, September~28, 1889}
+
+\nbsubsubsectionheading{\small
+\textsc{[Prepared by the Secretaries for Publication.]}}
+
+The minutes of the meeting of July~27 were read and approved.
+
+A list of presents to the Society was read, and thanks were returned to the
+donors.
+
+The following persons were elected to membership (the names of life-members,
+duly elected by the Board of Directors, are marked with a star (*):
+\addcontentsline{toc}{subsection}{\qquad List of Members elected}
+
+\begin{longtable}[l]{@{}ll}
+\textsc{Henry Lord Boulton}, F.R.A.S.,*& Caracas, Venezuela.\label{cor4} \rlap{(Box 2015, New York
+City)}\\ % corrected per corrigenda
+Rev. \textsc{A.~L. Brewer},& San Mateo, Cal.\\
+\textsc{George W. Beaver},& 418 California Street, San Francisco, Cal.\\
+Hon. \textsc{John L. Beard},& Warm Springs, Alameda Co., Cal.\label{cor5}\\ % corrected per corrigenda
+\textsc{A.~J. Burnham},& Lick Observatory, Cal.\\
+Mrs. \textsc{Anna Palmer Draper},*& 271 Madison Avenue, New York City.\\
+\textsc{W.~E. Downs},& Berkeley, Cal.\\
+\textsc{S.~J. Cunningham},& Swarthmore College, Delaware Co., Penn.\\
+Prof. \textsc{Geo. C. Edwards},& Berkeley, Cal.\\
+Prof. \textsc{T.~C. George},& University of the Pacific, San Jos�, Cal.\\
+Prof. \textsc{Alfred Higbie},& University of the Pacific, San Jos�, Cal.\\
+Dr. \textsc{J.~C. Hawyer},& Auburn, Cal.\\
+Hon. \textsc{W.~H. Jordan},& 328 Montgomery Street, San Francisco, Cal.\\
+Prof. \textsc{Josiah Keep},& Mills College, Alameda Co., Cal.\\
+Miss \textsc{Laura Kimber},& Occidental Hotel, San Francisco, Cal.\\
+Dr. \textsc{A. Liliencrantz},& 1459 Telegraph Avenue, Oakland, Cal.\\
+\textsc{F.~G. Montealegre},& 230 California Street, San Francisco, Cal.\\
+President \textsc{C.~C. Stratton},& Mills College, Alameda Co., Cal.\\
+\textsc{Frederick C. Torrey},& 529 Commercial Street, San Francisco, Cal.\label{cor6}\\ % corrected per corrigenda
+\textsc{Otto Von Geldern},& 1905 Polk Street, San Francisco, Cal.\\
+Rev. \textsc{J.~H. Wyeth},& Oakland, Cal.\\
+Hon. \textsc{R.~W. Waterman},*& Sacramento, Cal.\\
+\textsc{E.~C. Winchell},& 1214 Grove Street, Oakland, Cal.\\
+\textsc{Edward B. Young},& 430 Montgomery Street, San Francisco, Cal.\\
+\end{longtable}
+
+\medskip
+The design for the Society's diploma, which was recommended by the Committee
+and has been adopted by the Board of Directors, was exhibited to the
+meeting.
+%-----File: 086.png-----
+
+\nbsubsubsectionheading{(Extract from the Report of the Committee on the Diploma.)}
+\addcontentsline{toc}{subsection}{\qquad Report of the Committee on the Diploma}
+
+``A design for this diploma was prepared by the Committee and sent to Mr.\ \textsc{P.~R. Calvert}
+of Nashville, who has made the finished drawing.
+
+``As the Astronomical Society of the Pacific owes its origin to the association
+of amateur and professional astronomers in the observation of the Total Solar
+Eclipse of January~1, 1889, it was thought appropriate to give a chief position in
+the diploma of the Society to the Sun's Corona as then displayed. Accordingly,
+the centre of the upper panel contains the Sun, the Moon and the Corona of
+January, 1889. To the left and right of this are the symbols of the eight major
+planets. The twelve medallions of the lower panel include the twelve Zodiacal
+signs, copied from the beautiful designs of Mr.\ \textsc{Vedder}. The right hand panels
+represent first, the great comet of 1858, and second, the configuration of the
+Constellation of Orion. The stars of this constellation may stand for the stellar
+universe; while they also remind us that the central star of the sword-handle
+is the nucleus of the grandest of all the nebul�. The drawing of the Muse of
+Astronomy---\textit{Urania}---in the left-hand panel is copied from the antique statue of
+the Vatican. The national coat of arms in the upper left-hand panel designates
+the country in which the Society has its seat, and to which the work of our members
+should bring increasing honor as time goes on.''
+\pushright{\hbox{\textsc{E.~S. Holden, E.~E. Barnard, W.~B. Tyler}, \textit{Committee}.}\quad}
+
+\medskip
+\addcontentsline{toc}{subsection}{\qquad Designs for the Comet Medal by \textsc{M.~Alph�e Dubois}}
+It was announced that Mr.\ \textsc{Donohoe} had secured very satisfactory designs for
+the Comet Medal from M. \textsc{Dubois} in Paris, and that the dies were now making.
+
+\medskip
+\addcontentsline{toc}{subsection}{\qquad Expeditions to Observe the Eclipse of December~21, 1889}
+The Society was also notified that Messrs.\ \textsc{Burnham} and \textsc{Schaeberle} were
+to leave California September 29th or 30th for South America, on the expedition
+to observe the Total Eclipse of December 21st. Thanks to the generosity of Mr.\ \textsc{Crocker},
+the expedition is completely equipped, and, barring bad weather, is
+sure of success.
+
+The U.~S. Government will send an expedition in the U.~S.~S. \textit{Pensacola}.
+Five thousand dollars has been appropriated to cover the expenses. The expedition
+is under Professor \textsc{Todd}. The vessel will touch at St. Paul de Loanda
+and from thence two parties will, it is said, separate and go to points on the
+Coanza River.
+
+The English expedition to South America under Rev. Father S.~J. \textsc{Perry},
+F.~R.~S., will take station at Salute I., near Cayenne. Mr.\ \textsc{Taylor}, F.~R.~A.~S.,
+goes to St. Paul de Loanda. Each of these expeditions has the same programme
+and twin instruments, viz: an \textsc{Abney} 4-inch photographic lens and a 20-inch
+reflector of 45 inches focus. It is hoped to get sixteen pictures at each station.
+No spectroscopic work is to be attempted. Miss \textsc{Brown} and Miss \textsc{Jefferys},
+who observed the eclipse of 1887 in Russia, expect to observe that of next December
+in Trinidad. H.~M.~S. \textit{Comus} is placed at the disposal of the English
+expeditions by the British Admiralty.
+
+It is to be regretted that the Lick Observatory Expedition is (apparently) the
+only one provided with a lens of more than 45-inch focus. The experience of
+last January seems to have shown that the solar images from lenses of less than
+60 or 70 inches focus are too small to show much detail in the \emph{inner} corona.
+
+\medskip
+The papers presented were:
+\addcontentsline{toc}{subsection}{\qquad Papers presented}
+
+On the Companions to \textsc{Brooks}' Comet (July~23, 1889) discovered at the Lick
+Observatory, by E.~E. \textsc{Barnard}.
+
+Drawings of \textit{Jupiter} made with the 26-inch Equatorial at Washington during
+1875, by E.~S. \textsc{Holden}.
+
+Drawings of \textit{Jupiter} made with a 5-inch Equatorial at Nashville during the
+years 1879--1883, by E.~E. \textsc{Barnard}.
+
+(The drawings of \textit{Jupiter} made by Mr.\ \textsc{Keeler} with the 36-inch Equatorial
+during the present opposition were not exhibited for lack of time.)
+
+On the Establishment of a Standard Meridian Line for Santa Clara County,
+California, by \textsc{James E. Keeler}.
+
+Occultations of Stars by the Moon, by A.~O. \textsc{Leuschner}.
+
+Conjunction of \textit{Mars} and \textit{Saturn}, September~20, 1889, by W.~E. \textsc{Downs}.
+
+On the Photographic Brightness of the Fixed Stars, by J.~M. \textsc{Schaeberle}.
+%-----File: 087.png-----
+
+These papers will be printed in full or in abstract in numbers 4 and 5 of the
+Publications.
+
+\medskip
+The Society then adjourned to meet at its rooms, 408 California Street, San
+Francisco, on November~30, 1889.
+
+\ThoughtBreakLong
+
+
+\nbsectionheading{OFFICERS OF THE SOCIETY.}
+\addcontentsline{toc}{section}{List of Officers}
+
+\begin{tabular*}{0.95\textwidth}{@{\extracolsep{\fill}}lcr}
+\textsc{Edward S. Holden} (Lick Observatory),
+&& \textit{President}\\
+\textsc{Wm.~M. Pierson} (76 Nevada Block, S.~F.),
+& \multirow{3}{1em}{\Bigg\}}&\\
+\textsc{W.~H. Lowden} (213 Sansome Street, S.~F.)
+&& \textit{Vice-Presidents}\\
+\textsc{Frank Soul�} (Students' Observatory, Berkeley),&&\\
+\textsc{Chas. Burckhalter} (Chabot Observatory, Oakland),
+&\multirow{2}{1em}{\Big\}}
+&\multirow{2}{5em}{\textit{Secretaries}}\\
+\textsc{J.~M. Schaeberle} (Lick Observatory),&&\\
+\textsc{E.~J. Molera} (850 Van Ness Avenue, S.~F.),
+&& \textit{Treasurer}
+\end{tabular*}
+
+\compactlisttwo\stretchyspace
+\item[] \textit{Board of Directors}---Messrs.\ \textsc{Alvord, Boericke, Burckhalter, Gibbs,
+Grant, Holden, Lowden, Molera, Pierson, Schaeberle, Soul�}.
+\item[] \textit{Finance Committee}---Messrs.\ \textsc{Gibbs, Pierson, Molera}.
+\item[] \textit{Committee on Publication}---Messrs.\ \textsc{Dewey, Treat, Ziel}.
+\item[] \textit{Committee on the Comet Medal}---Messrs.\ \textsc{Holden} (\textit{ex officio}), % original has ex-officio
+\textsc{Schaeberle}, \textsc{Burckhalter}.
+\end{list}
+
+\ThoughtBreak
+
+\nbsectionheading{NOTICE}
+
+Members are requested to preserve the copies of the Publications of the
+Society as sent to them. At certain intervals a title page and index of the preceding
+numbers will also be sent to the members, who can then bind the numbers
+together into a volume.
+
+The titles of papers for reading should be communicated to either of the
+Secretaries as early as possible.
+
+Those members who propose to attend any or all of the meetings at Mount
+Hamilton during the summer should communicate with Mr.\ \textsc{Burckhalter}, at
+the rooms of the Society, 408 California Street, San Francisco, in order that
+arrangements may be made for transportation, lodging, etc.
+\vfil
+\[
+  \includegraphics{images/fig4.jpg}
+\]
+%-----File: 088.png-----
+%-----File: 089.png-----
+
+\nbchapterheading
+\nbchapterbanner{No.\ 5.}{San Francisco, California, November~30, 1889.}
+\nbchaptertoc{No.\ 5. (November~30, 1889).}
+
+\nbsectionheading{OBSERVATIONS OF \textit{JUPITER} WITH A FIVE-INCH
+REFRACTOR, DURING THE YEARS 1879--1886.}
+\addcontentsline{toc}{section}{Observations of Jupiter with a 5-inch Refractor during the years 1879 to 1886.
+By \textsc{E.~E. Barnard}. (Plates I, II, III, IV accompany)}
+
+\nbsubsubsectionheading{\shortrule\\*
+\textsc{By \textsc{E.~E. Barnard}.}\\*
+\shortrule}
+
+During the years 1879 and 1880 I was constantly employed in
+the daytime with my business duties; but every possible opportunity
+was used in astronomical observations at night. The latter part
+of 1879 and the major part of 1880 were devoted to an extended
+series of observations and drawings of \textit{Jupiter.}
+
+These observations were made at Nashville, Tennessee, ($\lambda =
++0^{\text{h}}39^{\text{m}}.0; \phi = +36�10'$), and before I was connected with the
+Vanderbilt University Observatory.
+
+The telescope was a five-inch refractor, mounted on a portable
+tripod, without a driving clock. A magnifying power of 173 diameters
+was nearly always employed---the instability of the mounting
+preventing the use of a much higher power. A right-angled prism
+was used with the eye-piece. This shows the planet reversed, but not
+inverted. In sketching, a small wooden box or desk was used, with
+a glass in the top, on which the paper was laid. A faint illumination
+from below, through the sketching paper, was obtained from the
+reflected light of a candle. By this means I could sit with the desk
+on my knees and compare the telescopic image directly with the
+drawing.
+
+The drawings were very carefully made, and faithfully show the
+markings as they appeared upon the planet at the time of observation.
+Professor \textsc{Holden} has lately seen these drawings, and suggested
+that I collect them together and prepare them for reproduction
+by photo-lithography. I have, therefore, selected forty-five of them
+as fairly representing the phenomena of \textit{Jupiter} during the period of
+observation, and they are reproduced in Plates I, II, III, IV, following.
+Constant reference should be made to the plates by the reader.
+In these plates the top of each drawing is north; the bottom is south;
+%-----File: 090.png-----
+the right-hand side is east, or following; the left-hand side is west,
+or preceding.
+
+During the observations the usual appearance of the planet was
+about as follows: Around the equatorial regions was a broad band
+or belt, which could really be said to be two belts; for it was always
+divided longitudinally by a sinuous, lighter portion, which was sometimes
+much broken by diffusions from the belts and by cloud-like
+forms. In the observations, I have considered this great belt as two,
+and have called the parts, respectively, the north and the south equatorial
+belts, or, collectively, the equatorial belt. Considered as one,
+the belt was about one-fifth the polar diameter of the planet in width.
+
+Just south of the equatorial belt was situated the Great Red Spot,
+covering an area of over two hundred million square miles---greater
+than the entire surface of our earth.
+
+On the inner part of the south equatorial belt was frequently seen
+a brilliant white spot, which had a very strong proper motion with
+reference to the Red Spot.
+
+To the north of the equator were situated three narrow lines or
+belts. I have designated these as the first, second and third linear
+belts. The third was usually the border of the north polar cap, while
+the first became the scene of remarkable changes about the 1st of
+November, 1880.
+
+What principally attracted my attention to the planet was the
+appearance of the Great Red Spot. The early history of this object
+seems to be rather obscure, but it was certainly seen as early as July,
+1878, by Professor \textsc{Pritchett}, at Glasgow, Missouri, and was probably
+seen at intervals as early as 1870.
+
+It was first seen by me in the early morning of August~3, 1879.
+I had heard nothing of it; and while observing and sketching \textit{Jupiter}
+it came into view around the following limb, and was so remarkable
+in form and color that I was at once struck with its appearance. On
+this date the form of the spot was different from what it was at any
+of my subsequent observations. While the south edge of the spot
+was nearly straight and the following end blunt, the north edge
+tapered towards the preceding end, strikingly like the drawing by
+\textsc{Trouvelot} in the \textit{Observatory} for April, 1879 (p.~411).
+
+It will be seen that my drawings nearly all show some phase of
+the Red Spot. I have so selected them because it was the principal
+object of interest with a small telescope, and therefore received the
+most attention. Though the Red Spot was watched carefully, I
+never saw any details on its surface until the latter part of the observations,
+%-----File: 091.png-----
+when a whitish cloud formed upon it. Changes were sometimes
+seen, however, in the form of the spot. These were confined
+to the ends, which occasionally appeared rounded, and, again, were
+very much pointed, or cigar-shaped. Faint trails were frequently
+seen running from one end or the other of the spot, and sometimes
+from both ends at the same time; the most persistent of these was
+the trail from the preceding end.
+
+One of the most interesting features of the Great Spot was the
+repulsion it seemed to exert upon adjacent markings on the planet.
+For a time it was surrounded by a sea of light that completely encircled
+it for a distance of three or four thousand miles (see drawing of
+October~3, 1879), and which appeared as a visible barrier against
+the approach of any spot or marking. So manifest was this repellant
+force that, as early in the observations as 1879, I called attention to
+it in the \textit{English Mechanic} (Vol.~30, p.~166).
+
+There was, however, one striking exception to this general rule:
+In July, 1880, a dense, smoky shading was seen apparently attached
+to the south side of the Red Spot, extending to the south preceding,
+and covering an area but little less than the Great Spot itself. This
+eventually passed the Red Spot, and, having a shorter period, soon
+left it far behind, and finally became squeezed out into a short longitudinal
+belt or spot, some twenty-five or thirty thousand miles long.
+Two white belts, one on each side, seemed to compress it into a definite
+form, that now extended east and west, instead of southwest and
+northeast, its primitive direction.
+
+During the observations, a great number of estimates were made of
+the instant that the Great Spot was in transit across the central meridian
+of the disc of \textit{Jupiter}. In discussing his micrometer measures
+of such transits from June to December, 1880, on thirty-one days,
+Prof. \textsc{Hough} says that his observations ``gave for the mean error of
+a single pair of measures $\pm 0^{\text{m}}.9$, and for the average mean probable
+error for any day, $\pm 0^{\text{m}}.4$, on the observed transit of the Red Spot
+over the central meridian,'' and further remarks: ``It may be inferred
+from these results that the use of a micrometer is infinitely preferable
+to any method of estimation.'' Among the observations of
+the Red Spot I have forty-four complete and carefully estimated
+transits---that is, observations of the preceding end, middle, and
+following end of the spot. Twenty-one of these are from a single
+but careful estimate of each phase. These give the probable error
+of a transit of the center from the mean of the three observations =
+$\pm 1^{\text{m}}.0$. In twenty-three of these transits three estimations were
+%-----File: 092.png-----
+made of each phase; from these I get for the transit of the middle
+from the mean of the nine observations the error of the transit, $=
+\pm 0^{\text{m}}.7$. These values are comparable with the best micrometer measures.
+It is evident that they should be so. The Red Spot moves
+through an angle of about 0�.6 in $1^{\text{m}}$. At transit this amounts to a
+change of distance from the limb of about $0''.2$. It is clear, that with
+a five-inch telescope the position of the spot could not have been
+fixed more closely with a micrometer (even if I had been provided
+with one, which was not the case) than it was by the method of transits.
+I think the sole advantage of micrometer measures in a case of this
+kind is that they can be made \emph{near} the transit, thus saving time
+by not having to wait for special phases, and that they can be
+repeated until the accidental error of the result is reduced to a small
+quantity.
+
+I have inserted the above comparisons to show what accuracy
+may be obtained by carefully made estimates, and as an encouragement
+to those who have not all the accurate appliances of an observatory
+to work with.
+
+During the observations, which frequently extended over an
+interval before the appearance of the Red Spot at the following
+limb and until after it had disappeared at the preceding limb, I
+several times noted the moment when the first trace of the Red Spot
+could be seen at the \textit{f.}\ limb. The mean of seven such observations,
+compared with the observed transit of the center of the spot, gave the
+interval $2^{\text{h}}1^{\text{m}}$ from the first trace of the \textit{p.}\ end of the Red Spot at the
+\textit{f.}\ limb, until the center of the spot was in transit. This gives $1^{\text{h}}36^{\text{m}}$
+as the time that a mark of the same distinctness as the Red Spot,
+and at the same distance from the equator, could be seen before its
+transit; $3^{\text{h}}12^{\text{m}}$ is, therefore, the total duration of visibility of \emph{any}
+point of the Red Spot during a rotation. Thus the spot could never
+be altogether invisible through rotation for a greater interval than
+$5^{\text{h}}53^{\text{m}}$ from the time the \textit{f.}\ end disappeared at the \textit{p.}\ limb until the \textit{p.}\ end
+reappeared at the \textit{f.}\ limb. The mean of two estimates gave $1^{\text{h}}9^{\text{m}}$ as
+the interval between the time when the spot was clearly seen free
+within the \textit{f.}\ limb and the time of transit of its center. Slight variations
+in the tint and depth of color of the spot were noticed, and it
+was frequently contrasted with some portion of the equatorial belt;
+but as the belt itself was probably subject to a far greater change in
+depth and color than the Red Spot, such a comparison would not be
+very conclusive proof of change.
+
+It would take up too much space to give the observations, even in
+%-----File: 093.png-----
+an abbreviated form, so I shall briefly summarize the most important
+points:
+
+\nbsubsectionheading{The Color of the Red Spot.}
+
+\begin{description}
+\item[1879.] Aug.~2, it is described as of the color of red-hot iron.
+
+\item[1880.] July~11, a clear, darkish Indian red, brighter in color than
+equatorial belt; July~24, a clearer red than equatorial belt; July~29,
+a light Indian red, the belts a duller red; Aug.~16, a brick-dust
+color---same tint as north equatorial belt; Sept.~14, a lighter red,
+very much lighter than north belt; Sept. 16, a brick red, more
+strongly marked than the north band; Sept. 25, a deep brick-dust
+color; Sept. 30, a distinct red, the equatorial bands a heavier red;
+Oct.~7, a redder color than the belts; Oct.~13, a heavy red, clear
+and sharp; Oct.~20, a light, clear red; Nov.~1, a pale red; Nov.~3,
+a deep brick-dust color; Nov.~11, a solid red, well outlined; Nov.~20,
+a little less deep in color, but very much redder than the belts.
+
+\item[1881.] Jan.~7, not so well defined at edges, but a deeper tint at
+the middle; July~2, a pale light red; July~9, the spot is even of a
+deeper tint than last year; Oct.~31, lightish red.
+
+\item[1882.] Jan.~23, faintish red, very pale.
+
+\item[1885.] April~25, it is very faint---quite difficult to observe---a
+very pale red; April~28, it is very well seen, and is clearly outlined
+all round; May~12, very faint; May~15, fairly distinct, probably a
+white mass superposed on it.
+
+\item[1886.] April~8, a long white cloud clearly seen on the Red Spot;
+April~22, very faint, a whitish strip of cloud on it, north of middle.
+\end{description}
+
+\nbsubsectionheading{Trails from the Ends of the Red Spot.}
+
+Faint reddish trails were recorded on the following dates:
+
+\begin{description}
+\item[1879.] Oct.~3, faint trail from following end.
+
+\item[1880.] July~11, faint trail from preceding end; July~18, faint
+trail from each end; Aug.~16, faint trail from each end; Aug.~30,
+faint trail from each end; Sept. 16, faint trail from each end; Nov.
+18, faint trail from preceding end; Nov.~20, faint trail from preceding
+end.
+
+\item[1886.] Nov.~5, faint trail from preceding end.
+\end{description}
+
+These usually were about 2$''$ or 3$''$ long.
+
+
+\nbsubsectionheading{Size of the Red Spot.}
+
+Frequent estimations were made, at the telescope, of the relative
+size of the Red Spot, on dates extending from July, 1880, to December
+14, 1880. Following are the estimations:
+%-----File: 094.png-----
+
+\begin{description}
+\item[\textit{Breadth}:] From twelve estimates of its breadth north and south,
+it was just perceptibly less than one-half the breadth of the equatorial
+band = estimate I; while eight estimates made it exactly one-half
+= estimate II\@. One estimate placed it perceptibly greater than one-half
+= estimate III.
+
+\item[\textit{Length}:] Sixteen estimates made the length very slightly less than
+one-third the length of the same parallel of the disc of \textit{Jupiter}
+= estimate I; while the mean of six other estimates made it 0.32
+that distance in length = estimate II.
+
+\item[\textit{Distance of North Edge of Spot from South Edge of Belt}:]
+Twenty-four estimates of the distance between the north edge of the
+spot and the south edge of the equatorial belt gave it 0.40 of the
+width of the spot, with decided and considerable variability (which
+never, however, exceeded one-half).
+\end{description}
+
+Adopting from the \textit{Report} of the Dearborn Observatory for 1882
+Professor \textsc{Hough}'s micrometer measures of the breadth of the equatorial
+bands (for a period exactly covering my estimation) as $= 7''.04$,
+and his value for the radius of the parallel of the center of the Red
+Spot $= 17''.94$, we have the above estimations expressed in seconds
+of arc at the distance unity.
+\medskip
+
+\begin{small}
+\noindent\begin{tabular}{@{}llrl}
+\textsc{Breadth of Spot}:& Estimate & I &= very slightly less than $3''.5$.\\
+&Estimate & II &= $3''.5$.\\
+&Estimate & III &greater than $3''.5$.\\
+\textsc{Length of Spot}:&  Estimate & I &= very slightly less than $12''.0$.\\
+&Estimate & II &$= 11''.5$.\\
+\end{tabular}
+
+\smallskip
+\noindent\textsc{Distance North Edge of Spot From South Edge of Belt}: Assuming,
+with the above estimates, the breadth of spot to equal $3''.5$, the estimates give
+the distance above as $1''.4$.
+
+\end{small}
+
+\nbsubsectionheading{The Bay at the Red Spot Formed by the South Equatorial
+Belt.}
+
+This singular recurring feature of the south equatorial belt is
+worthy of particular attention. As it seems intimately connected
+with the Red Spot, it had best be mentioned here. In a drawing
+published in the \textit{Observatory} for April, 1879 (p.~411), \textsc{Trouvelot}
+shows a sharp curvature of the south side of the equatorial belt
+around the preceding end of the Great Spot, forming, as it were, a
+bay. He says it had disappeared and reappeared no less than three
+times in a little over a year, always reappearing at the same place
+with reference to the Red Spot. This bay, or a similar one, is shown
+in my drawing of October~3, 1879. It then curved south, following
+%-----File: 095.png-----
+the Red Spot, the southern limit diffusing very greatly, but sharply
+terminated where it curved down following the spot. It is shown
+thus also in a drawing of September~14, 1879. It was wholly absent
+throughout 1880, the south edge of the equatorial band being perfectly
+straight all around the planet. The first indication I have of
+its return is February 4, 1882, (the observations had, however, ceased to
+be continuous after 1880), when I recorded that the south equatorial
+band ``appeared to blend southwards, following the Red Spot.'' In
+1885, this feature was distinctly marked---the appearance being the
+same as in 1879, except that its extreme south edge did not blend so
+much as in that year. Its presence was marked on April~25, May~12,
+May~15, and, 1866, April~22, when the planet was examined. The
+absence of other dates indicates only that the region of the Red Spot
+was not examined, and not that the bay existed only on these dates.
+At the Lick Observatory I have seen it frequently at the present
+opposition just as it was in 1879. That this is intimately connected
+with the forces that produce the Red Spot there is no doubt. In connection
+with this feature and the Red Spot, I would mention a singular
+thin red line that sprung out from the south edge of the equatorial band
+like a spur, and, curving backwards, ran along parallel to the south
+edge of the equatorial belt for some distance. This is shown in
+the drawings of 1880, September~18, 28, 30, and October~10. Prof.
+\textsc{Hough} has figured this singular object in a drawing made September
+9, 1880, with the 18$\frac{1}{2}$-inch refractor, just as I have seen it,
+except that he does not show it of a red color. (See \textit{Report Dearborn
+Observatory}, 1882.) It occupied a place near the preceding
+curve of the bay. Though this spur-line joined the south edge of the
+equatorial belt, to which it seemed attached, it did not partake of its
+motion; for throughout its visibility it retained the same position with
+reference to the Red Spot, showing that its period was the same
+as that of the spot, while the period of the belt is about $5\frac{1}{2}^{\text{m}}$
+shorter.
+
+I have already mentioned the smoky shading which, in July,
+1880, seemed to be attached to the Red Spot, and which finally
+passed by it through a more rapid rotation. It is shown on a great
+many of the drawings. I would specially call attention to those of
+Pl. I (July 24, 29, August, 16, 17, September~9, 11); Pl. II (September
+30, October~7, 10, November~1). The drawing of July~24,
+1880, shows a very small spot near transit in the southern hemisphere.
+This small spot was usually quite hard to see, but was
+clearly defined and dusky when best seen; it was probably about 4000
+%-----File: 096.png-----
+miles long and some 2000 miles wide. The remarkable features were
+its permanency and its slow rotation period. Its period being somewhat
+less than the Red Spot, it slowly drifted westward from that
+object, and probably, in course of time, completed a circuit of the
+planet, which it would do in a little over two years, when it would
+again be in the region of the Red Spot. It is shown in several of
+the drawings.
+
+\nbsubsectionheading{The Equatorial White Spot.}
+
+Throughout the entire period of my observations, there was
+present on the planet a very remarkable White Spot, situated on, or
+generally imbedded in, the north edge of the south equatorial band.
+This object was subject to remarkable changes of form and brightness.
+It required but a few observations to show that it was in
+rapid motion with reference to the Red Spot. Its period was nearly
+five and a-half minutes shorter than that of the Great Spot. Its westward
+drift with reference to that object was about 8� of longitude
+per day, or about 2430 miles, at every rotation of the planet. This
+rapid relative motion with reference to the Red Spot would therefore
+carry it completely around the planet in forty-five days, and a number
+of such revolutions were actually observed. It required but four
+days for this swiftly moving body to completely pass the Red Spot,
+which it soon left far behind, and in twenty-two and one-half days it
+would be on the opposite side of the planet. I would refer to the
+drawings of Plate~III (November~18, 20, 22 and 23), where one of
+these passages of the Red Spot is shown. The motion of this object
+was not perfectly uniform. At times it seemed to slacken its speed,
+and then to spurt forward again. Among the surprising things about
+this spot were its great changes, both of form and brightness. At
+times it became so bright as to glisten like a star. When in this
+condition it was by far the brightest object on the planet. For a
+while it would appear as a rather small, inconspicuous, light, oval
+spot, imbedded in the dark matter of the north edge of the south
+equatorial band. In this state it would scarcely attract attention.
+It would next be seen brilliantly white, burying its head in the dusky
+matter of the belt, with a vast, luminous train streaming backwards
+along the equatorial regions, like the tail of a comet. Sometimes
+this train was composed of white, cloud-like balls, that streamed eastward
+on the planet. After continuing thus for some time, it would
+seem to have wasted its energies, and would then assume the quiescent
+state. I have tried to connect these changes of brightness with
+the changes of motion, but have not been able to do so, though there
+%-----File: 097.png-----
+is doubtless a relation between them. When at its brightest it seemed
+to burrow in the south band and plow the matter before it. A long,
+sinuous rift in the northern part of the north equatorial band had
+constantly the same relative position to the White Spot, and was
+perhaps in the same layer of the planet's atmosphere. Probably all
+the objects in the equatorial regions had the same motion as the
+White Spot, or were stationary, relative to it. Indeed, the entire
+belt is revolving around the planet once in forty-five days, relatively
+to the Red Spot.
+
+I will select a few of the many notes I have on this object and
+those connected with it:
+
+\begin{description}
+\item[1880.] Aug.~13 ($13^\text{h}~33^\text{m}$), a brilliant white spot appearing at the
+\textit{f.}\ limb; Aug.\ 16 ($11^\text{h}$), very white; Aug.\ 18, bright spot n.~f.\ Red
+Spot, followed by light, cloudy masses; Aug.\ 23, the bright spot of
+the 18th has toned down; Aug.\ 30, bright; Sept.\ 10 ($10^\text{h}\ 30^\text{m}$),
+brilliant, with train; Sept.\ 15 ($9^\text{h}\ 30^\text{m}$), very bright, with train of
+white, cloudy masses; Sept.\ 24 (about $9^\text{h}$), a bright head, with long,
+curved stream of white matter following; Sept.\ 28 ($11^\text{h}\ 30^\text{m}$), bright;
+Sept.\ 31 ($7^\text{h}\ 33^\text{m}$), two large white spots about midway the disc, a
+smaller one between them---they all shine with a very white luster;
+Nov.\ 11, a great number of white balls seen near $10^\text{h}$; Nov.\ 18,
+white; Nov.\ 20, it is more isolated from the other matter---pale
+white, diffused at edges; Nov.\ 22, smaller and pale, about the size
+of Satellite I, but much paler; Nov.\ 23, it is smaller and paler;
+Nov.\ 24 ($9^\text{h}\ 20^\text{m}$), light; Nov.\ 29, white. When best seen, it is
+roundish. It seems to push a dark mass in front of it; it is as large
+as a satellite.
+
+\item[1881.] Jan.\ 7, very bright and well-defined---it keeps the mass
+of matter pushed up in front of it as before; Aug.\ 3, a small white
+spot; Oct.\ 29, a very bright spot, with luminous and clouded train;
+Nov.\ 1, bright, and plowing its way along the equatorial regions;
+Nov.\ 12, white and distinct, about the size of a satellite, a clouded
+train following.
+
+\item[1882.] Feb.\ 4, white---fainter, luminous train.
+
+\item[1886.] May~13, white, luminous train.
+\end{description}
+
+The above times do not necessarily refer to its transit. These
+apparitions were doubtless the same object, as they refer to a bright
+body imbedded in the inner edge of the south band, and just south
+of the equator. From the comparisons of its size to the satellites, it
+was probably about two or three thousand miles in diameter. It is
+shown on the drawings for (Pl.~I) Aug.\ 13, 16, Sept.\ 10; (Pl.~II)
+%-----File: 098.png-----
+Sept.~24, 28, 30, Nov.~7; (Pl.~III) Nov.~18, 22, 23, and (Pl.~IV)
+Nov.~5, 1881.
+
+\nbsubsectionheading{The Equatorial Belts.}
+
+The equatorial belts were subject to many internal changes.
+These changes, though frequent, are not so great as one would be
+led to think from examining, say, that region just north of the Great
+Spot. Part of the changes are due to the continual drift of the belt
+past the Red Spot; thus every few days presenting an entirely different
+part of the belt to view from any one standpoint. As an illustration
+of this, we have only to follow the White Spot in its journey
+around the planet. I would also refer to (Pl.~II) the drawings of
+September~30 and October~7, where a decided drift of the dusky
+masses is shown. These belts changed in strength and depth of
+color. When I first examined the belts, in 1879, the northern one
+was reddish, while the southern was bluish; the two being separated
+by a whitish, serpentine division. Though my notes contain
+frequent reference to the colors of these belts, it will probably be
+best, considering the limited space, to very briefly state a few of the
+observations in a general form.
+
+\nbsubsectionheading{Colors of the Equatorial Belts.}
+
+North of the narrow, light rift in the northern part of the north
+belt, the color was frequently of a deep, rich vermilion, while the rest
+of the belt towards the equator was of a much lighter red, though
+at times it became a very deep, darkish red. The south belt remained
+bluish for a long time, and I first began to call it reddish about the
+middle of August, 1880. Even in September I have called it a drab
+color. On September~9, 1880, when the Red Spot was in transit,
+the north band was a warm purple, while the south one was a cold
+purple. On October~10, 1880, at $10^\text{h}$, part of the north band, north
+of rift, was a dark, heavy red, while the south band was a bluish-gray,
+mixed with red; while on October~13, at $8^\text{h}$--$9^\text{h}$, they were both
+a deep red. On October~10, 1881, both sides of the belt were reddish,
+while the inside was bluish.
+
+\nbsubsectionheading{Forms in the Equatorial Bands, etc.}
+
+The belts were usually clearly and sharply defined at their polar
+edges and perfectly straight. The peculiar disturbances to which they
+were subject were confined to their inner edges or to parts near the
+equator. Besides the famous White Spot that has been mentioned,
+there were sometimes the most exquisitely beautiful forms at the equator.
+%-----File: 099.png-----
+These came and went---at times filling the interior of the great
+belt with dusky, cloud-like forms and softly delicate plumes that
+were very transitory. At times the belts appeared as one, being
+completely filled in with one solid tint. Such was the case, 1880,
+September 25, when the part visible (with the Great Spot central)
+was dusky and evenly filled in, and the belt in every respect was one
+solid, unbroken shade. I have never seen it, before or since, so
+absolutely uniform in tint. A few days after this (September~28)
+faint forms began to appear in the equatorial regions near the Red
+Spot. The south band was usually well-defined at both edges, and
+rather narrow, the inner edge being more or less undulating. At
+other times, there were large, soft, dusky, feathery projections from
+it, spreading out to the equator; in almost every case, these streamed
+backward, towards the east limb, as if the south belt were moving
+faster than the equatorial region. The north band was markedly
+different from this. It was always much diffused towards the equator.
+The edges were sometimes festooned with dusky, cloud-like forms. I
+would refer to the drawings of Pl.~III (November~10, 22); Pl.~II
+(October~7, 10, etc.), as showing the differences in the two belts. A
+long light rift was frequently visible near the extreme north edge of
+the north band. From the fact that this always bore the same relative
+position to the bright spot in the south band, I infer that the north
+component of the equatorial band rotated in the same time as the
+south component; but from the retarded appearance of the dusky
+masses projected from the inner edge of the south band, and frequently
+from the north band, one might also infer a somewhat slower
+rotation at the equator. This, however, is a mere conjecture, with no
+other warrant than appearances.
+
+In reference to this retardation of the masses projected from the
+south band toward the equator, I quote an observation of mine on
+April~1, 1886, respecting one of the most remarkable appearances
+that I have seen on \textit{Jupiter}: ``At $12^\text{h}\,45^\text{m}$, three of the dark projections
+ranged along the inner edge of the belt and just south of the
+equator. I noticed that from the summit of each there extended for
+a short distance in a following direction, a dusky streak, looking like
+smoke. I was strongly impressed with the resemblance to what might
+be called a silhouette view of three volcanic peaks, ranged in a line
+and vomiting smoke, which a strong wind was carrying eastward!''
+(\textit{Sid.~Mess.}, May, 1886, p.~156.)
+%-----File: 100.png-----
+
+\nbsubsectionheading{The History of the Formation of a New Belt.}
+
+In all the drawings previous to the 1st of November, 1880, a
+very thin line or belt is shown, just north of the north equatorial belt.
+In the first observation, in 1879, this narrow line was reddish, and
+formed a neat border to the north side of a delicate band or space
+that lay between it and the equatorial band. It was also the south
+edge or border to a delicate broad white band that encircled the
+northern hemisphere. Finally, the delicate band south of it faded,
+and became of the same tint as the light band to the north, thus leaving
+the border occupying the position of a distinct linear belt around the
+planet. This is what I have called the first north linear belt, or, simply,
+the first linear belt. It continued thus perfectly linear, without a mark
+on it, until the latter part of October, when it rapidly underwent a
+change so remarkable that I have thought it worth describing in detail.
+On the night of October~21, 1880, at $9^\text{h}\,30^\text{m}$, this belt appeared a little
+swollen, or thicker than usual. On the 23d, the entire planet seemed to
+be undergoing a great change, so much so that I wrote in my note book:
+``\textit{Jupiter} is undergoing some remarkable changes now; there are a
+great many degrees of shade, somewhat like ill-defined spots and
+light spaces, appearing in the southern hemisphere near the Great
+Spot. The space between the north edge of the north equatorial
+band and the first linear belt is deepening in tint, as it was last year---a
+grayish green. At $8^\text{h}$ the first linear belt near the following limb is
+knobbed in appearance, as if several little dark beads were strung on
+it, and at $9^\text{h}$ it was seen to have two pretty distinct, dusky spots on it,
+close to each other.''
+
+On account of the remarkable character of these changes I feel
+that it is proper, strictly as a matter of record, to give my notes
+in full:
+
+\begin{description}
+\item[1880.\; Nov.~1.] \textit{Jupiter} has been undergoing some remarkable
+changes. From the time the Red Spot began to appear until after
+its transit, the first linear belt was composed of a string of large dusky
+spots. I counted five, each as large as the shadow of a satellite.
+Under the best definition, they appeared as black as the shadows of
+the two satellites (I and II, shown in the drawing), and the belt elsewhere
+appeared thicker than usual.
+
+\item[Nov.~2.] At $6^\text{h}\,30^\text{m}$ the affected belt observed last night appeared
+very heavily marked.
+
+\item[Nov.~3.] $7^\text{h}\,45^\text{m}$. The disturbed portion of the belt just appearing.
+At $8^\text{h}\,25^\text{m}$, the affected part reaches from the following limb to near
+%-----File: 101.png-----
+midway the disc. It is heavy, broad and uneven. $8^{\text{h}}40^{\text{m}}$. The first
+portion of this is in transit; a number of roundish, cloudy masses
+on it clear to the following limb.
+
+\item[Nov.~4.] It is heavily marked, and its following portion transited
+at $6^{\text{h}}9^{\text{m}}$.
+
+\item[Nov.~7.] $8^{\text{h}}$. The belt faint and undecided; no trace of the
+affected part.
+
+\item[Nov.~8.] Near $7^{\text{h}}$. The belt now is heavily marked all the way
+across the disc, and dark, with remarkably large, distinct, knotty
+lumps, in places quite broad with them. The disturbed region
+plainly visible; almost the most conspicuous part of the planet.
+Near $9^{\text{h}}$, that portion of the belt visible is not affected at all, but was
+faint and ill-defined.
+
+\item[Nov.~10.] From $7^{\text{h}}30^{\text{m}}$ until $11^{\text{h}}$, the belt was very heavy and dark.
+It consisted of a strip of ``veiling,'' pretty even at its northern edge,
+but undulating southwards; it was heavily nucleated at several points
+by heavy, blackish spots, and at these points the ``veiling'' was
+pressed outwards towards the equator. Later, that portion opposite
+the Red Spot, which was so heavily affected on November~1, was
+seen to be slightly wavy, but faint and ill-defined.
+
+\item[Nov.~11.] Before the Red Spot had appeared the belt was affected
+as before. That portion opposite the Red Spot at transit was diffused
+and slightly wavy. Near $10^{\text{h}}$, after the spot had disappeared, the belt
+was a pale blue, broader than usual.
+
+\item[Nov.~18.] $7^{\text{h}}$ to $8^{\text{h}}$. Opposite the Red Spot, the belt was very
+diffused and broad, and appeared slightly wavy where the spots of
+November~1 appeared.
+
+\item[Nov.~20.] $9^{\text{h}}49^{\text{m}}$. The belt is very diffused and faint, with no
+spots on it.
+
+\item[Nov.~23.] $8^{\text{h}} 35^{\text{m}}$. Three large and intensely \emph{black spots} nearing
+transit. The spots are as black as the shadows of the satellites.
+
+\item[Dec.~1.] $7^{\text{h}}$. The belt is broad, heavy and distinct across the
+entire disc. It is dotted with black spots. $7^{\text{h}}20^{\text{m}}$. It is now
+heavier to the preceding side of the disc, and is faded and diffused
+following. $8^{\text{h}}45^{\text{m}}$. The belt is now faint and diffused across the
+entire disc.
+
+\item[Dec.~2.] $6^{\text{h}}51^{\text{m}}$. It is faint and diffused, and no dark spots on
+it. At $7^{\text{h}}37^{\text{m}}$, it is heavy with separate ``blocks'' or oblong spots.
+These are probably the ones seen on November~1, which have gone
+completely around the planet, and have now arrived at the point
+where they where first seen. They are about as conspicuous as
+%-----File: 102.png-----
+the equatorial belts, and are moving around the planet with great
+velocity.
+
+\item[Dec.~5.] The large spots have drifted past the Red Spot, and
+appear as at last observation---broken---forming a disjointed belt.
+At $8^{\text{h}}$, the belt is composed of a number of dusky spots that stretch
+from limb to limb.
+
+\item[Dec.~7.] $7^{\text{h}}19^{\text{m}}$. The belt is heavy and broken.
+
+\item[Dec.~9.] $8^{\text{h}}$ to $10^{\text{h}}$. The belt is heavy and uneven. The south
+edge has a light rim or border.
+
+\item[Dec.~10.] The northern hemisphere is delicately beautiful. The
+south side of the new belt consists of beautiful curves, their inner
+(south) edge bordered with a light line. I notice that the equatorial
+edge of the north equatorial band has the same or corresponding
+curves to those in the new belt.
+
+\item[Dec.~14.] $6^{\text{h}}35^{\text{m}}$. The new belt consists of several large dusky
+spots.
+
+\item[Dec.~29.] $7^{\text{h}}40^{\text{m}}$. The new belt faint, the scolloped % OED: legit variant spelling
+ edge seen with difficulty.
+
+\item[Dec.~30.] About $9^{\text{h}}$, it is heavy and undulating.
+
+\item[Dec.~31.] $8^{\text{h}}$. The new belt is faint.
+
+\item[1881. \; Jan.~7.] $8^{\text{h}}$ to $9^{\text{h}}$. The new belt is deeply scolloped---long
+and regular sweeps; it fades northwards. There is no white rim to
+the scollops. The belt diffuses north as a grayish shade all over the
+northern hemisphere. The second and third linear belts that crossed
+the northern hemisphere in 1880 cannot be seen.
+
+\item[March~6.] $7^{\text{h}} 30^{\text{m}}$. The new belt is much scolloped.
+
+\item[July~2.] $15^{\text{h}}$. There is a heavy diffused belt north of the equatorial
+belts, where, in 1880, existed the first linear belt. This is the
+final result of the spots that broke out on it November~1, 1880.
+
+\item[July~9.] $14^{\text{h}}30^{\text{m}}$. The new belt is broad and diffused, and of a
+brick-dust red.
+
+\item[Oct.~3.] The new belt is very diffused. There is a dark line
+running through it a little north of the middle of the belt. [Is this
+the first linear belt?] A small, white spot, like a satellite, on its
+south edge, transited at $10^{\text{h}} 15^{\text{m}}$.
+
+\item[Oct.~14.] $10^{\text{h}}$. The new, diffused, reddish belt is double.
+\end{description}
+
+This is the complete history of the formation of at least \emph{one} of
+the belts of \textit{Jupiter}; and probably no more remarkable outburst has
+been witnessed.
+
+During the time these striking changes were taking place the
+%-----File: 103.png-----
+weather was very bad, and only occasional glimpses of the planet
+could be had. These glimpses, though, gave sufficient evidence of
+the rapid changes that were taking place. These changes were so
+rapid and peculiar, and the weather so unpropitious, that no transits
+that could be positively identified as belonging to the same portion
+of the affected belt could be obtained, and therefore the motions of
+these spots could only be estimated. But it was clearly evident that
+they were extremely rapid. If the sketches refer to identical objects,
+the period, with reference to the Red Spot, would not be far from
+thirty days, or two-thirds of the period of the White Spot, with reference
+to the Great Spot.
+
+Let us briefly review what the notes tell us about this disturbance.
+For, at least, over one year, a thin, uniformly even stripe
+around \textit{Jupiter} existed north of his equatorial belt. About the last
+of October, 1880, both hemispheres of the planet were greatly
+affected by a disturbance that finally culminated in a great outbreak
+on this thin stripe, just mentioned. First, it became swollen in
+places; then, lumpy spaces appeared on it; next, small black spots
+were formed, each with a penumbra---not unlike a sun-spot; these
+had a very rapid motion westward on the planet, and enlarged and
+increased in longitudinal extent, becoming large, oblong, dusky
+spots, without a black nucleus. They then diffused into a ``veiling,''
+with condensations in it. This ``veiling'' became beautifully scolloped,
+its southern side consisting of graceful, light-rimmed curves,
+which decreased in sweep as they extended eastwards. Finally, these
+encircled the planet completely, diffusing northwards quite to the
+pole. The energies that produced the disturbance finally died out,
+and the beautiful curve-bordered belt lost its characteristic features
+and toned down to a broad, diffused, red belt, surrounding the
+planet; and this finally became double, and was apparently a fixed
+feature of the surface when I ceased to observe it.
+
+
+\nbsubsectionheading{The Polar Caps.}
+
+The north polar cap was variable in its color and in the distance
+to which it extended. It was frequently noted to be of a delicate
+wine tint; at other times it was pale gray. Its usual limit was the
+third linear belt, though on several occasions it extended nearer the
+equator. At these times the third belt was seen crossing it.
+
+The edges of the south cap were seldom well-defined. I have
+never seen it of a warm tint. These caps have never been very
+deeply marked. One striking fact was noted on several occasions.
+%-----File: 104.png-----
+When dawn had whitened the sky the poles appeared to grow darker
+and more dusky in color. There was usually a marked difference
+in the appearance of the northern and southern hemispheres of the
+planet. The northern was free of spots, except several tiny \emph{black}
+ones, which were visible for a long time on the third linear belt,
+and which did not have a greatly different period from that of the
+Red Spot. Graceful, narrow linear belts crossed this hemisphere,
+and light bands were often seen. In the southern hemisphere there
+was no such symmetry. The Great Red Spot, dusky shadings, strips
+or fragments of belts, were the characteristic features of the southern
+hemisphere.
+
+It is a very difficult question as to which portion of the surface
+of the planet is the highest---whether the belts are at a lower depth
+than the whiter surface or otherwise. During these observations I
+was frequently impressed with the idea that the general matter of the
+equatorial belts was at a lower altitude. I was particularly struck
+with this on several occasions. A peculiar brushing-out or smearing
+of the bright surface adjacent to the south band, which was recorded
+on several dates, had every appearance of a blending of the light
+surface over and above the belt. Several times in 1886 a luminous
+spot was seen close to the northern edge of the north equatorial
+band that seemed to push the white surface over and above the belt
+The more rapid rotation of the belt is also consistent with its being
+at a lower altitude.
+
+At a number of occultations of the satellites I watched carefully
+for any evidences of their being seen through the edges of the
+planet, but saw nothing of the kind. Professor \textsc{Holden} informs
+me, however, that, with the thirty-six-inch equatorial, the whole disc
+of a satellite has been visible within the planet's atmosphere, at
+every occultation he has observed. (See, also, the observations of
+47~\textit{Libr�} by \textit{Jupiter}, as observed by Professor \textsc{Holden} and myself,
+June~9, 1888. \textit{A.~J.}, vol.~8, p.~64.)
+
+I would call special attention to the second drawing of 1880, November~1
+(Plate~II). There is a large lithograph of \textit{Jupiter} published
+by the \textsc{Scribners}, from a drawing by \textsc{Trouvelot}. This was made
+in Cambridge, Mass., November~1, 1880, ($9^\text{h}\,30^\text{m}$, Cambridge mean
+time). The difference of longitude between Nashville and Cambridge
+is $1^\text{h}\,3^\text{m}$. My drawing was made at $8^\text{h}\,30^\text{m}$, Nashville mean
+time, adding the difference of longitude, and we have $9^\text{h}\,33^\text{m}$, Cambridge
+mean time, for my drawing, or within three minutes of the
+time of the drawing by \textsc{Trouvelot}. That is to say, that while my
+%-----File: 105.png-----
+pencil, in Nashville, was marking on the paper, \textsc{Trouvelot}, at
+Cambridge, Mass., was, at that identical instant, drawing the same
+thing. The two drawings are exactly similar in the main features.
+His telescope was larger than mine, and he, therefore, saw more
+details. To the left below the belt, on this drawing, are the first
+and second satellites; the first nearer the belt. On the Red Spot
+is the shadow of the second satellite, while near the equatorial belt is
+the shadow of the first moon.
+
+I have collected nearly all the observations of transits of spots
+over the central meridian of \textit{Jupiter's} disc, and present them in the
+following table. I would state, in reference to these observations,
+that the first ones to the latter part of September may be affected by
+an error in the times of as much as two or three minutes outside of
+the error of observation. I had no means of determining my time,
+and depended upon the tower clock of the University, which, I
+afterwards found, had not been carefully looked after during the
+vacation season. I therefore give them with the above caution. I
+regret this; for I believe the observations themselves were made
+with much accuracy for simple eye-estimates. Some that were
+obviously far out, from the above cause, I have rejected altogether.
+
+In conclusion, I would express my indebtedness to Professor
+\textsc{Holden}, without whose interest and encouragement these observations
+and drawings would never have been published.
+
+
+\nbsubsectionheading{Descriptions of the Drawings.}
+
+\nbsubsubsectionheading{\textit{Plate I.}}
+
+\begin{description}
+\item[1879. \; Oct.~3.] Shows the Red Spot and the area of light surrounding
+it, and the peculiar diffusion of the south band towards the
+south, which forms a bay around the following end of the spot.
+North of the equatorial bands is shown the narrow linear belt, which
+later on plays an important part in the drawings. This we have
+designated the first linear belt north.
+
+\item[1880. \; July~24.] A very small dusky spot is seen between the
+equatorial belts and the south pole. The Red Spot is appearing at
+the following limb.
+
+\item[July~30.] The peculiar mass of shading, referred to in the notes,
+is seen attached to the south preceding portion of the Red Spot.
+
+\item[Aug.~13.] This shows the famous White Spot in the south part
+of the equatorial bands, near the following limb.
+
+\item[Aug.~16.] The White Spot is nearer the Red Spot.
+
+\item[Aug.~17.] Shows a group of small spots, and the mass of shading
+%-----File: 106.png-----
+and the Red Spot just coming into view around the following
+limb. The left-hand one of the three small spots is the same as
+that shown in the drawings of July~24 and August~1.
+
+\item[Sept.~10.] The White Spot is shown in one of its brightest
+phases, with a luminous train following it near the equator. It has
+passed the Red Spot and left it far behind.
+
+\item[Sept.~16.] Shows the shading now separated from the Red Spot,
+which it is leaving slowly behind.
+\end{description}
+
+\nbsubsubsectionheading{\textit{Plate II.}}
+
+\begin{description}
+\item[1880. \; Sept.~18.] This shows the thin red line springing from the
+south side of the equatorial belt and streaming backwards parallel to the
+equator, near the following end of the Red Spot. Two very small,
+very black spots are seen. One of these was visible for a great
+length of time on the second linear belt north. Though the Red
+Spot is shown in this drawing, the white one is invisible, being indeed
+on the other side of the planet at this time.
+
+\item[Sept.~24.] The Red Spot is disappearing at the preceding limb,
+while the White Spot, with its train of light, is near the middle of the
+disc.
+
+\item[Sept.~28.] The Red Spot is just past the middle of the disc, and
+the White Spot is fully within the following limb.
+
+\item[Sept.~30.] (I) Satellite I is seen on the Red Spot, while its
+shadow is on the edge of the spot. The shading and two of the
+small spots in the southern hemisphere are also seen. (II) Satellite
+I and its shadow have now left the Red Spot. On this occasion I
+transited most of the disc as a dusky brown spot, south following its
+shadow. The White Spot is appearing at the following limb.
+
+\item[Oct.~7.] Satellites I and II are in transit, partially hiding their
+shadows, which are close north following them.
+
+\item[Oct.~23.] (I) The Red Spot is disappearing, and some dusky
+lumps are coming into view on the first linear belt north. These are
+the first indication of the great outbreak on that belt. (II) These
+swollen places in the belt are shown in transit.
+
+\item[Nov.~1.] (I) The Red Spot is appearing, while the shadow of I
+is just skirting its north preceding end, and the shadow of II is on
+the spot. Near the middle of the disc, south of the equator, satellite
+I itself is shown as a dusky spot near transit, while satellite II is lost in
+the brightness of the disc. Near the north following limb a string of
+dark spots is coming into view on the first linear belt. (II) Both
+satellites now appear as small pale discs, relieved by the slight
+%-----File: 107.png-----
+duskiness of the planet near the preceding limb. The shadows
+have changed their places with respect to the Red Spot. The row
+of dark spots on the first linear belt is now in transit. These look
+like sun-spots---a black umbra surrounded by a penumbra. These are,
+doubtless, the same spots that are shown in an incipient stage of
+development in the sketches of October~23. They are, therefore, in
+rapid motion around the planet. (Compare their relative position to
+the Red Spot in the first drawing of October~23 with that of the
+second drawing of November~1.)
+
+\item[Nov.~7.] We have the White Spot in this drawing on the opposite
+side of the planet to the Red Spot. Two other bright spots are just
+ahead of it.
+\end{description}
+
+\nbsubsubsectionheading{\textit{Plate III.}}
+
+\begin{description}
+\item[1880. \; Nov.~8.] The second satellite is seen as a white spot on
+the south following end of the Red Spot, while I is partially on the
+north preceding end as a dusky spot, and its shadow is shown to the
+right of the center below the equatorial belt. That portion of the first
+linear belt north now visible with the Red Spot has not as yet been
+affected by the eruptive spots.
+
+\item[Nov.~10.] (I) The shadow of III is seen at a high southern latitude,
+and a mass of dusky shading is north following it. Another
+phase of the new spots on the first linear belt is shown. (II) The
+Red Spot is now visible, and the affected part of the belt has been
+carried off the disc by rotation. That portion now seen is faint and
+wavy.
+
+\item[Nov.~18.] The White Spot is in one of its brilliant phases, just
+above the following end of the Red Spot.
+
+\item[Nov.~20.] The White Spot has now moved to a point near the
+preceding end of the Red Spot, and is in one of its quieter phases.
+
+\item[Nov.~22.] (I) Another phase of the northern spots is shown.
+The two small spots in the southern hemisphere have been shown in
+previous sketches. The Red Spot is not in sight. (II) The Red
+Spot and the White Spot are both visible---the White Spot having left
+the Red Spot far behind.
+
+\item[Nov.~23.] (I) The distance between the White and Red Spots
+has sensibly increased since the drawing of last night. (II) The Red
+Spot is disappearing, and the first portion of the affected belt is coming
+into view at the north following limb.
+
+\item[Dec.~2.] (I), (II), (III) show further phases of the disturbance.
+\end{description}
+%-----File: 108.png-----
+
+\nbsubsubsectionheading{\textit{Plate IV.}}
+
+\begin{description}
+\item[1880. \; Dec.~9.] Shows the spots becoming connected by long
+loops bordered with a brilliant line on the equatorial side.
+
+\item[Dec.~10.] (I) Another portion of the new belt visible when the
+Great Spot is leaving the disc---the shadow of a satellite on it. (II)
+This drawing was made after the Red Spot had disappeared.
+
+\item[1881. \; Aug.~29.] In the place of the first linear belt north there is
+now a broad diffused reddish belt that completely encircles the planet.
+The remarkable spots and the beautiful light-rimmed curves have disappeared,
+and all the other singular transformations that the first
+linear belt north underwent have finally ended in the formation of this
+now persistent diffused red belt.
+
+\item[Nov.~5.] The Red and the White Spots are again near each
+other. The diffused red belt, the scene of the great disturbance
+of 1880, remains unchanged. Two of the small black spots previously
+seen are shown on the second linear belt north---which, suffering
+almost total obliteration during the changes of 1880, is now as
+marked as ever.
+
+\item[1885. May~12.] The Great Spot is now very faint. The south
+equatorial band diffuses southwards around the following end of the
+Red Spot, as in 1879.
+
+\item[1886. April~22.] A white cloud has formed over the middle of
+the great Red Spot, almost obliterating it. The peculiar bay formed
+around the following end of the spot by the south band is now very
+persistent.
+\end{description}
+
+I have observed a few abnormal transits of Satellites I, III and
+IV, which are given here, so that they may be available for a study
+of the causes of these dark and black transits.
+
+\nbsubsectionheading{Satellite I.}
+
+\begin{description}
+\item[1880.] Sept.~30, occasionally seen during transit as a brownish
+spot; Nov.~1, seen in mid-transit as a dusky spot; Nov.~8, seen in
+mid-transit as a dusky, brownish spot; Dec.~1, seen in mid-transit
+quite plainly as a dark spot---quite dark.
+\end{description}
+
+\nbsubsectionheading{Satellite III.}
+
+\begin{description}
+\item[1879.] Aug.~2, very black nearly all the way across---mistaken
+for shadow; Sept.~14, black during transit.
+
+\item[1880.] Sept.~28, carefully watched throughout transit, not visible
+except near limbs---not a black transit; Dec.~30, at $8^\text{h}\,30^\text{m}$, seen
+in a high south latitude as a small, black spot; continued visible as
+%-----File: 109.png-----
+black spot until near \textit{p}.\ limb, and only lost its blackness at $9^\text{h}\, 4^\text{m}$.
+Ten minutes after emergence it was certainly as bright as that part
+of disc on which it appeared as black as a shadow.
+
+\item[1880.] Nov.~10, the shadow of III appeared fuzzy and not
+black. It seemed to be affected by penumbra.
+
+\item[1881.] Oct.~13, at inferior conjunction it passed the south pole
+with only three-quarters of its disc on the planet---carefully estimated.
+
+\item[1883.] Feb.~12 ($9^\text{h}\, 40^\text{m}$), small, black.
+
+\item[1885.] May~9 ($7^\text{h}\, 15^\text{m}$), on north edge of belt very black, and
+remained dark until close to limb.
+\end{description}
+
+\nbsubsectionheading{Satellite IV.}
+
+\begin{description}
+\item[1885.] Feb.~27, at $6^\text{h}\, 15^\text{m}$, it is as black as its shadow, and about
+half as large---it remained dark up to nearly the moment of emergence.
+
+\item[1886.] May~8 ($9^\text{h}\, 20^\text{m}$), IV near north pole, very black.
+\end{description}
+
+\begin{small}
+\begin{center}
+\begin{longtable}{c@{ }r@{\,}| *{7}{r@{ }l|} r@{ }l}
+\multicolumn{18}{c}{\textsc{
+    Observed Transits of Spots on \textit{Jupiter}.}}
+\\[1ex]
+\multicolumn{18}{c}{\textsc{\footnotesize
+    (nashville mean time.)}}
+\\[1ex]
+\hline\hline
+  \multicolumn{2}{c|}{\multirow{2}{*}{\centering\textsc{
+    Date.}}}
+& \multicolumn{6}{c|}{\textsc{
+    red spot.}\rule{0pt}{3ex}}
+& \multicolumn{2}{m{3em}|}{\multirow{2}{3em}{\centering\textsc{%
+\rule{0pt}{2ex}white spot.}}}
+& \multicolumn{2}{c|}{\multirow{2}{*}{\centering\textit{ a }}}
+& \multicolumn{2}{c|}{\multirow{2}{*}{\centering\textit{ b }}}
+& \multicolumn{2}{c|}{\multirow{2}{*}{\centering\textit{ c }}}
+& \multicolumn{2}{c}{\multirow{2}{*}{\centering\textit{ d }}}
+\\[1ex]
+\cline{3-8}
+&&\multicolumn{2}{c|}{\footnotesize\textit{ P.~End.\rule{0pt}{3.5ex}}}
+& \multicolumn{2}{c|}{\footnotesize\textit{ Middle. }}
+& \multicolumn{2}{c|}{\footnotesize\textit{ F.~End. }}
+&&&&&&&&&&\\[1ex]
+\hline
+  \multicolumn{2}{c|}{\footnotesize 1880.}
+& \footnotesize\textit{h.} & \footnotesize\textit{m.}
+& \footnotesize\textit{h.} & \footnotesize\textit{m.}
+& \footnotesize\textit{h.} & \footnotesize\textit{m.}
+& \footnotesize\textit{h.} & \footnotesize\textit{m.}
+& \footnotesize\textit{h.} & \footnotesize\textit{m.}
+& \footnotesize\textit{h.} & \footnotesize\textit{m.}
+& \footnotesize\textit{h.} & \footnotesize\textit{m.}
+& \footnotesize\textit{h.} & \footnotesize\textit{m.}
+\endfirsthead
+\hline\hline
+  \multicolumn{2}{c|}{\multirow{2}{*}{\centering\textsc{
+    Date.}}}
+& \multicolumn{6}{c|}{\textsc{
+    red spot.}\rule{0pt}{3ex}}
+& \multicolumn{2}{m{3em}|}{\multirow{2}{3em}{\centering\textsc{%
+\rule{0pt}{2ex}white spot.}}}
+& \multicolumn{2}{c|}{\multirow{2}{*}{\centering\textit{ a }}}
+& \multicolumn{2}{c|}{\multirow{2}{*}{\centering\textit{ b }}}
+& \multicolumn{2}{c|}{\multirow{2}{*}{\centering\textit{ c }}}
+& \multicolumn{2}{c}{\multirow{2}{*}{\centering\textit{ d }}}
+\\[1ex]
+\cline{3-8}
+&&\multicolumn{2}{c|}{\footnotesize\textit{ P.~End.\rule{0pt}{3.5ex}}}
+& \multicolumn{2}{c|}{\footnotesize\textit{ Middle. }}
+& \multicolumn{2}{c|}{\footnotesize\textit{ F.~End. }}
+&&&&&&&&&&\\[1ex]
+\hline
+  \multicolumn{2}{c|}{}
+& \footnotesize\textit{h.} & \footnotesize\textit{m.}
+& \footnotesize\textit{h.} & \footnotesize\textit{m.}
+& \footnotesize\textit{h.} & \footnotesize\textit{m.}
+& \footnotesize\textit{h.} & \footnotesize\textit{m.}
+& \footnotesize\textit{h.} & \footnotesize\textit{m.}
+& \footnotesize\textit{h.} & \footnotesize\textit{m.}
+& \footnotesize\textit{h.} & \footnotesize\textit{m.}
+& \footnotesize\textit{h.} & \footnotesize\textit{m.}
+\endhead
+\multicolumn{1}{r@{ }}{July} &10.
+&\ 14&40  &\ 15&22  &\ 15&47
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &17. &  15&20  &  15&44  &  16&04
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &24. &  16&12  &  16&40  &  16&57
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &29. &  15&17  &  15&43  &  16&11
+&\Skipped
+&\ 14&00
+&\Skipped &\Skipped
+&\Skipend
+\\
+
+\multicolumn{1}{r@{ }}{Aug.} & 1.
+&  16&52  &  17&18   & 17&42  & &&\ 15&18
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` & 7.
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&  16&09
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &11.
+&\Skipped
+&  11&32 & 12&01
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &13. &  12&36  &  13&\multicolumn{1}{@{}l@{\,}|}{04.5} & 13&32
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &16. &  10&\multicolumn{1}{@{}l@{\,}|}{16.5}&  10&35   & 10&56
+&\Skipped &\Skipped
+&\ 10&36
+&\Skipped &\Skipend
+\\
+ `` &17. &  15&55  &  16&19   & 16&41
+&\Skipped
+&\ 14&14
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &23. &  10&\multicolumn{1}{@{}l@{\,}|}{54.5}&  11&19
+& 11&\multicolumn{1}{@{}l@{\,}|}{40.5}
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &28.
+&\Skipped
+& 10&\multicolumn{1}{@{}l@{\,}|}{24.5}
+& 10&\multicolumn{1}{@{}l@{\,}|}{48.5}
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &30. &  11&\multicolumn{1}{@{}l@{\,}|}{34.7}
+&  11&\multicolumn{1}{@{}l@{\,}|}{58.2}
+&  12&\multicolumn{1}{@{}l@{\,}|}{24.2}
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+
+\multicolumn{1}{r@{ }}{Sept.} & 9.
+&   9&\multicolumn{1}{@{}l@{\,}|}{51.7}
+&  10&\multicolumn{1}{@{}l@{\,}|}{15.2}
+&  10&\multicolumn{1}{@{}l@{\,}|}{39.2}
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &14.
+&\Skipped
+&   9&\multicolumn{1}{@{}l@{\,}|}{27$\pm$}
+&\Skipped &\Skipped
+&\Skipped
+&\ 10&21
+&\Skipped &\Skipend
+\\
+ `` &15.
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipped
+&   9&47
+&\Skipped &\Skipend
+\\
+ `` &16. &  10&32  &  11&02     &  11&24
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &18. &  12&14  &  12&\multicolumn{1}{@{}l@{\,}|}{37.7}
+&  13&03
+&\Skipped &\Skipped
+&  12&22
+&\Skipped &\Skipend
+\\
+ `` &25. &  12&58  &  13&24     &  13&45
+&\Skipped
+&\ 10&46
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &28. &  10&28  &  10&53     &  11&17
+&\Skipped &\Skipped
+&  10&38 &11&40
+&\Skipend
+\\
+ `` &30. &  12&\multicolumn{1}{@{}l@{\,}|}{01.5}
+&  12&\multicolumn{1}{@{}l@{\,}|}{29.5}
+&  12&54
+&\Skipped
+&   9&48  &  12&11
+&\Skipped &\Skipend
+\\
+
+\multicolumn{1}{r@{ }}{Oct.} & 1.
+&  7&57  &  8&25  &  8&52
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\ \ 7&28
+\\
+ `` & 6. &  7&\multicolumn{1}{@{}l@{\,}|}{01.5}
+&  7&\multicolumn{1}{@{}l@{\,}|}{29.5}
+&  7&\multicolumn{1}{@{}l@{\,}|}{57.5}
+&\Skipped &\Skipped
+&\Skipped
+&  8&18
+&\Skipend
+\\
+ `` & 7. & 12&45  & 13&13  & 13&40
+&\Skipped
+&\ 10&24
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &10. & 10&\multicolumn{1}{@{}l@{\,}|}{13.5}
+& 10&\multicolumn{1}{@{}l@{\,}|}{39.5}
+& 11&\multicolumn{1}{@{}l@{\,}|}{08.5}
+&\Skipped &\Skipped
+&\ 10&\multicolumn{1}{@{}l@{\,}|}{26.5}
+&\Skipped &\Skipend
+\\
+ `` &13. &  7&44  &  8&10  &  8&36
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &20. &  8&29  &  8&53  &  9&17
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &22.
+&\Skipped
+& 10&30
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipped &\Skipend
+\\
+%-----File: 110.png-----
+\multicolumn{1}{l@{ }}{Nov.} & 1.
+        &   8&19 &  8&48
+&   9&\multicolumn{1}{@{}l@{\,}|}{10.5}
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` & 4.&\Skipped      &  6&15 &  6&39
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` & 7.
+&\Skipped &\Skipped
+&\Skipped
+&  7&59
+&\Skipped &\Skipped
+&\Skipped &\Skipend
+\\
+ `` & 8.&   9&06 &   9&31 &   9&57
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &10.&\ 10&44 &\ 11&09 &\ 11&33
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &11.&   6&34 &  6&57 &   7&25
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &18.&   7&17 &  7&42 &   8&09
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &20.&   8&58 &  9&22 &   9&48
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &22.&  10&40 & 11&01 &  11&29  &\ 10&18 & 7&46
+&\Skipped &\Skipped
+& 9&07
+\\
+ `` &23.&   6&32 &  6&53 &   7&20
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+
+\multicolumn{1}{l@{ }}{Dec.} & 2.
+        &   8&56 &  9&15 &  9&41  &  6&27
+&\Skipped &\Skipped
+& 7&33 & 7&23
+\\
+ `` & 5.&   6&28 &  6&46 &   7&11
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` & 6.
+&\Skipped  &\Skipped
+&\Skipped
+&  8&\multicolumn{1}{@{}l@{\,}|}{53$\pm$}
+&\Skipped &\Skipped
+&\Skipped &\Skipend
+\\
+ `` & 7.&   7&59 &  8&23
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipped &\Skipend
+\\
+ `` & 9.&   9&37 & 10&01 &\ 10&24
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &14.&   8&46 &  9&09 &   9&34  &  9&20
+&\Skipped &\Skipped
+&\Skipped &  7&05
+\\
+ `` &29.&\Skipped
+&\Skipped  &\Skipped
+&  7&41
+&\Skipped &\Skipped
+&\Skipped &\Skipend
+\\
+ `` &31.&   7&45 &  8&\multicolumn{1}{@{}l@{\,}|}{08.5}&  8&33
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+
+\multicolumn{2}{c|}{\footnotesize 1881.} &&&&&&&&&&&&&&&&
+\\
+\multicolumn{1}{l@{ }}{Jan.} & 7.
+         &  8&39 &  9&01 &  9&24 &  8&02.5
+&\Skipped &\Skipped
+&\Skipped &\Skipend
+\\
+\multicolumn{1}{l@{ }}{Mar.} & 6.
+         &  6&52 &  7&14 &  7&36
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+
+\multicolumn{1}{l@{ }}{July} & 2.
+&\Skipped   &\Skipped
+& 15&21
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &  9.& 15&12  & 15&34  & 15&57
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` & 11.& 16&47
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` & 21.& 15&\multicolumn{1}{@{}l@{\,}|}{04.5}&  15&27 & 15&50
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` & 28.& 15&53  &  16&12 & 16&36
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+
+\multicolumn{1}{l@{ }}{Aug.} & 3.
+&\Skipped &\Skipped
+&\Skipped
+&  14&\multicolumn{1}{@{}l@{\,}|}{42.5}
+&\Skipped &\Skipped
+&\Skipped &\Skipend
+\\
+ `` & 5.&\Skipped
+&\Skipped &\Skipped
+&  15&46   &  16&06
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &29.
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&  15&\multicolumn{1}{@{}l@{\,}|}{39.5}
+&\Skipped &\Skipped
+&\Skipend
+\\
+
+\multicolumn{1}{l@{ }}{Oct.} & 10.
+&\Skipped &\Skipped
+&  17&32
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &29.
+&\Skipped &\Skipped
+&\Skipped
+&  10&25
+&\Skipped
+& 10&\multicolumn{1}{@{}l@{\,}|}{15$\pm$}
+&\Skipped &\Skipend
+\\
+
+\multicolumn{1}{l@{ }}{Nov.} & 3.
+&\Skipped &   6&\multicolumn{1}{@{}l@{\,}|}{50$\pm$}
+&\Skipped
+&  8&24
+&\Skipped &\Skipped
+&\Skipped &\Skipend
+\\
+ `` & 5.&    8&09     &   8&30  &  8&54 &  9&34
+&\Skipped
+&  9&20
+&\Skipped &\Skipend
+\\
+ `` &12.&    9&52     &   9&14  &  9&42 &  8&44
+&\Skipped &\Skipped
+&\Skipped &\Skipend
+\\
+ `` &15.&     &       &   6&45  &  7&08
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &26.&\Skipped
+&\Skipped
+&   7&27
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ `` &29.&    8&54     &   8&15  &  8&37
+&\Skipped
+&  8&\multicolumn{1}{@{}l@{\,}|}{30$\pm$}
+&\Skipped &\Skipped
+&\Skipend
+\\[1ex]
+
+\multicolumn{2}{c|}{\footnotesize 1882.} &&&&&&&&&&&&&&&&\\
+\multicolumn{1}{l@{ }}{Jan.} &23.
+&    8&19     &   8&40  &  9&03
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+\multicolumn{1}{l@{ }}{Feb.} & 4.
+        &    8&08     &   8&28  &  8&49 &   9&07
+&\Skipped &\Skipped
+&\Skipped &\Skipend
+\\
+\multicolumn{1}{l@{ }}{April} &27.
+&\Skipped &\Skipped
+&  6&\multicolumn{1}{@{}l@{\,}|}{50$\pm$}
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\[1ex]
+
+\multicolumn{2}{c|}{\footnotesize 1885.} &&&&&&&&&&&&&&&&\\
+\multicolumn{1}{l@{ }}{April} &25.
+&\Skipped
+& 10&\multicolumn{1}{@{}l@{\,}|}{41.5}
+&\Skipped
+&  7&\multicolumn{1}{@{}l@{\,}|}{56.5}
+&\Skipped &\Skipped
+&\Skipped &\Skipend
+\\
+\multicolumn{1}{l@{ }}{May} &12.
+&\Skipped
+&  9&43
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipped &\Skipend
+\\
+\multicolumn{1}{l@{ }}{May} &13.
+&\Skipped &\Skipped
+&\Skipped
+&   8&48
+&\Skipped &\Skipped
+&\Skipped &\Skipend
+\\[1ex]
+
+\multicolumn{2}{c|}{\footnotesize 1886.} &&&&&&&&&&&&&&&&\\
+\multicolumn{1}{l@{ }}{April} &22.
+&\Skipped
+&   10&18.6
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipped &\Skipend
+\\[1ex]
+
+\multicolumn{2}{c|}{\footnotesize 1888.} &&&&&&&&&&&&&&&&\\
+\multicolumn{1}{l@{ }}{\tablenoteasterisk July} &24.
+&  11&\multicolumn{1}{@{}l@{\,}|}{51.9}
+&  12&\multicolumn{1}{@{}l@{\,}|}{08.4}
+&  12&\multicolumn{1}{@{}l@{\,}|}{29.8}
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\[1ex]
+
+\multicolumn{2}{c|}{\footnotesize 1889.} &&&&&&&&&&&&&&&&\\
+\multicolumn{1}{l@{ }}{\tablenoteasterisk May} &31.
+&\Skipped &\Skipped
+&  15&\multicolumn{1}{@{}l@{\,}|}{09.3}
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+\multicolumn{1}{l@{ }}{\tablenoteasterisk June} & 9.
+&\Skipped &\Skipped
+&  17&\multicolumn{1}{@{}l@{\,}|}{48.4}
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipend
+\\
+ ``  &17.&\Skipped
+&  13&\multicolumn{1}{@{}l@{\,}|}{53.0}
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipped &\Skipend
+\\
+\multicolumn{1}{l@{ }}{\tablenoteasterisk July} & 2.
+&\Skipped
+&  11&19.1
+&\Skipped &\Skipped
+&\Skipped &\Skipped
+&\Skipped &\Skipend
+\\[1ex]
+\hline
+\multicolumn{18}{l}{\footnotesize* With twelve inch at Lick Observatory. Like the others, in Nashville mean time.}
+\end{longtable}
+\end{center}
+\end{small}
+
+%-----File: 111.png-----
+The transits of a few objects were observed with the six-inch, at
+the Vanderbilt University Observatory, as follows:
+\begin{tablesetup}
+\begin{tabular}{c@{~}c@{~}r@{}c|cccc|cccc|cccc}
+\hline\hline
+\strut&&&&&&&&&&&&&&&\\
+&\multicolumn{2}{@{}c}{\textsc{date.}}&\phantom{1885.}&\multicolumn{4}{c|}{$e$}&\multicolumn{4}{c|}{$f$}&\multicolumn{4}{c}{$g$}\\
+\strut&&&&&&&&&&&&&&&\\
+\hline
+&&&&&\footnotesize\textit{h}.&\footnotesize\textit{m}.
+&&&\footnotesize\textit{h}.&\footnotesize\textit{m}.
+&&&\footnotesize\textit{h}.&\footnotesize\textit{m}.\\
+1885.& April& 21&\dotfill&&8&02.5&&&\multicolumn{2}{@{}c}{\dotfill}&&&\multicolumn{2}{@{}c}{\dotfill}\\
+  `` & ``  &  22&\dotfill&&\multicolumn{2}{@{}c}{\dotfill}&&&7 &05.5&&&   6& 55.7\\
+  `` & ``  &  25&\dotfill&& 7 & 08.2&&&\multicolumn{2}{@{}c}{\dotfill}&&&\multicolumn{2}{@{}c}{\dotfill}\\
+  `` & ``  &  29&\dotfill&&\multicolumn{2}{@{}c}{\dotfill}&&& 7 &54.5 &&&  7 &46.5\\
+  `` & May &   9&\dotfill&& 8& 42.5 &&&\multicolumn{2}{@{}c}{\dotfill}&&&\multicolumn{2}{@{}c}{\dotfill}\\[1ex]
+\hline
+\end{tabular}
+\end{tablesetup}
+
+{\footnotesize
+\textsc{Note} (explanatory of the table of transits).---$a$ is the small spot mentioned
+as having been seen 1880, July~24, and subsequently; $b$ is a small black spot, the
+\textit{p}.\ of two shown on the second linear belt north in the drawing of 1880, September
+28, and subsequently; $c$ is the second of these two black spots; $d$ is the shading
+spoken of in connection with the Red Spot; $e$ is a luminous spot, sometimes
+recorded as a notch in the north edge of the north equatorial band, probably not
+all the same object; $f$ is a very small, intensely black spot \emph{on} the south part of
+the equatorial belt---round, and like a satellite's shadow, but smaller; $g$ is a luminous
+spot or notch in the north edge of north equatorial band.
+
+}\ThoughtBreakLong
+
+\nbsectionheading{DRAWINGS OF \textit{JUPITER} MADE WITH THE 26-INCH
+EQUATORIAL, AT WASHINGTON, DURING 1875.}
+\addcontentsline{toc}{section}{Drawings of Jupiter made with the 26-inch Equatorial at Washington during 1875. By \textsc{E.~S. Holden}. (Plate V accompanies)}
+
+\nbsubsubsectionheading{\shortrule\\*
+\textsc{By Edward S. Holden.}\\*
+\shortrule}
+
+During June and July, 1875, I made drawings of \textit{Mars} and
+\textit{Jupiter}, in colored crayons, for the purpose of comparing the
+tints on those two planets. The drawings were all made with
+the twenty-six-inch equatorial of the United States Naval Observatory,
+usually with a magnifying power of 400, and no pains were
+spared to make correct delineations, both as to forms and colors.
+From one cause and another, these drawings have not been published.
+
+I beg to present a photograph of the sketches of \textit{Jupiter} to the
+Society.
+
+The original colored drawings [exhibited to the meeting] will be
+deposited in the library of the Lick Observatory, where they will
+always be available for comparison with more recent work. Below,
+I give the few notes which should accompany the drawings, which
+are reproduced in Plate~V. It will be interesting to compare these
+%-----File: 112.png-----
+drawings with the admirable series by Mr.\ \textsc{Barnard}, which are given
+in Plates~I to IV.
+
+There are three general remarks to be made on these drawings.
+In the first place, while the general features of the planet's surface
+have remained about the same from 1875 to 1889, there has been an
+entire change as to the form and disposition of the details. In the
+second place, the disposition of color on the surface of the planet
+has entirely changed, also. In 1889 there is very little of the red
+color to be seen, except in the great central belt, while in 1875 red
+belts were seen almost to the poles. Thirdly, the characteristic red
+color itself has changed in a surprising manner since 1875.
+
+The color of the red markings in 1875 was most carefully
+matched in crayons, and I was finally satisfied with the tint of the
+drawings. In 1881 I found that the same crayons (pieces of which
+I had preserved) would no longer match the red belts. In 1889
+the color of the red belts is entirely different from that previously
+drawn. All the observations were made with \textsc{Clark} objectives (of
+26, $15\frac{1}{2}$ and 36 inches aperture), which had their color-corrections
+very much alike. Unfortunately, it is not practicable to reproduce
+these colors in Plate~V. The notes follow:
+
+The top of the drawing is south; the right-hand side is east, or
+following.
+
+1875. June~16, seeing not good; June~18, hazy; June~24,
+the columnar structure in the southernmost belt is somewhat too
+coarse; July~13, the position of the shadow of the satellite is for
+$8^\text{h}~40^\text{m}$; July~16, planet unsteady.
+
+\ThoughtBreakLong
+
+\nbsectionheading{NOTICES FROM THE LICK OBSERVATORY.}
+\addcontentsline{toc}{section}{\textit{Notices from the Lick Observatory}}
+
+\nbsubsubsectionheading{\shortrule\\*
+{\small \textsc{Prepared by Members of the Staff.}}\\*
+\shortrule}
+
+\nbsubsectionheading{On the Determination of the Brightness of Stars by Means
+ of Photography.}
+\addcontentsline{toc}{subsection}{\qquad On the Determination of the Brightness of Stars by means of Photography. [Containing a Review of \textsc{Charlier}; \textit{Publ. Astr. Gesell}., No. XIX, 1889.] By \textsc{Edward S. Holden}}
+
+
+Dr.\ \textsc{Charlier}, assistant in the Observatory at Stockholm, has
+prepared a memoir\footnote
+{\textit{Ueber die Anwendung der Sternphotographie zu Helligkeitsmessungen der Sterne}, von
+\textsc{C.V.L.~Charlier}. \textit{Publication der Astronomischen Gesellschaft}, XIX. Leipzig 1889. 4to.
+(pp.~viii, 31).}
+on the use of photography in determinations of
+the brightness of stars, which has been published by the Astronomical
+%-----File: 113.png-----
+Society of Germany, and dedicated to the Pulkowa Observatory,
+on the occasion of the fiftieth anniversary of its foundation, August
+19, 1889.
+
+The subject treated is so new and so important that it will not be
+out of place to give a brief review of Dr.\ \textsc{Charlier's} excellent treatise
+here, and to add some general considerations on the same question.
+The importance of this subject will be obvious, when we consider that
+within the next decade we may expect to have at least two sets of
+photographic maps, covering the whole sky from pole to pole, and
+including millions of stars down to the fourteenth magnitude.
+
+Besides these systematic maps, hundreds of charts of special
+regions will be made. Each star on each of these maps will have
+impressed its image on a negative plate as a disc of measurable size.
+Hence the magnitude of each and every star \emph{can} be determined if
+necessary, and when the catalogue of the stars to the eleventh magnitude,
+also proposed by the Congress, is constructed, the magnitude
+of each one of these two million stars \emph{must} be given.
+
+There are two imperative questions to be settled before the principles
+on which this great work is to be done can be considered to
+be established. The first and more special question is, What is the
+relation between the diameter of the photographic image of a star ($d$)
+the aperture and focus of the telescope employed ($a$, $f$) and the exposure
+time ($t$), and what is the relation between the (photographic)
+brightness of a star and the diameter of its image? Having satisfactorily
+determined the relations just named, the second and more
+general question presents itself, namely: On what fundamental principles
+ought the photographic magnitudes of the stars to be assigned?
+
+\smallskip
+These two questions are not treated separately in the work before
+us. Its second paragraph states the problem of the photographic
+photometry of stars as follows: It is ``to determine the function
+which gives the relation between the size of the photographic image
+and the photographic brightness of the star, and to determine the
+constant quantities in this function \emph{in such a manner that the resulting
+photographic brilliancies shall correspond accurately throughout
+with the brilliancies determined visually}.''
+
+\smallskip
+In my judgment, this is by no means the problem of stellar photographic
+photometry. It is impossible, in general, to fulfill that portion
+of the above statement which I have printed in italics. The
+difference between the photographic and the photometric magnitudes
+of \textit{Aldebaran}, for example, is more than one and one-half
+%-----File: 114.png-----
+magnitudes, and so with other stars. We may leave this part of the
+question for the moment, and proceed to give a brief analysis of Dr.\ \textsc{Charlier's}
+memoir, laying stress principally on the novel portions
+of his work.
+
+The observations which he discusses were made with a photographic
+lens by \textsc{Steinheil} of 3.19 inches aperture and 39.37 inches
+focus ($\frac{f}{a} = 13$). The plates took in an area of twenty square
+degrees. The images were satisfactory over a field of about three
+degrees in diameter. Stars to eighth magnitude, inclusive, left trails.
+The plates employed were made in Lyons, by \textsc{Lumi�re}. Four
+plates are discussed. All were exposed on the \textit{Pleiades}, as follows:
+No.~2, $t = 13^\text{m}$; No.~4, $t= 2^\text{h}$; No.~24, $t= 1^\text{h}30^\text{m}$; No.~26, $t = 3^\text{h}$.
+The plates were exposed at very different altitudes, and no account
+is taken of absorption of light by the atmosphere.
+
+Dr.\ \textsc{Charlier} finds two defects in the plates: first, bright rings
+round the larger stars, which he proves to be due to reflections
+from the back of the plate (the well-known halation images); and,
+again, false stars. He finds no less than fifty-six such false stars on
+his plate No.~26. They were probably due to defects in the manufacture
+of the plate itself.
+
+As subjects for experiments he chose the \textit{Pleiades}, because their
+photometric magnitudes are accurately determined, and also because
+they afford a variety of magnitudes within a comparatively small area.
+
+Although he does not expressly mention the fact, the \textit{Pleiades}
+have the special advantage for his purpose of being all of the same
+spectral type. A region containing many very red or many very
+blue stars would have given a corresponding number of anomalous
+results, which are avoided by choosing a group of stars of one type.
+The diameter of each star on each of the four plates was measured.
+Calling $H$ the brightness of a star, and $m$ its magnitude, and
+0.4 the light ratio, Dr.\ \textsc{Charlier} starts with the formula
+\[
+\tag{1}  H =(0.4)^m
+\]
+That is, he assumes that the brightness of a first magnitude star
+($m= 1$) is 0.4. It is better to write this formula, I think,
+\[
+\tag{2}  H_m = (0.4)^{m-1}
+\]
+which for $m= 1$ gives $H_1= 1$. Assuming the equation (1), however,
+and further assuming that when $d$ is zero, $H$ must be zero, he
+finds
+\[
+\tag{3}  m = a - b \log d
+\]
+%-----File: 115.png-----
+Here it may be remarked that, in fact, $H$ is not necessarily zero
+for $d=0$, because all stars below a certain brightness will fail to
+produce an image on the plate, no matter how long the exposure may
+be---for any practical exposure-time. The brightness of a star must
+be above a certain finite limit in order to produce any impression at
+all. The assumption is sufficiently accurate, however, for the purpose
+in hand. The relation between exposure-time and diameter of
+star image is next determined from a series of exposures on \textit{Polaris},
+assuming the form
+\[
+\tag{4}  d = d_0\centerdot t^k
+\]
+That is, that the diameter of the star-image varies as the $k^\text{th}$ power
+of the time. From \textit{Polaris} (two plates) the values of $k$ are 0.243
+and 0.249; from a star 5th mag.\ $k$ results 0.243,---hence, the numerical
+value of the diameter of the star-image varies as the fourth
+root of the time or
+\[
+\tag{5} d=d_0\centerdot\sqrt[4]{t}
+\]
+This formula shows that the diameter $d$ will be doubled when the
+exposure $t$ is increased sixteen-fold.
+
+If there are no limits to the formula it also shows that, for the
+telescope and plates employed, an exposure of $\frac{1}{16}$ second would give
+a perceptible image. Without considering the question of the \emph{range
+of sensitiveness} of plates I may state it as my opinion that the formul� of
+Dr.\ \textsc{Charlier} and those of Professor \textsc{Schaeberle} (\textit{Publ. Ast.
+Soc. Pacific}, No.~4) can (at present) be applied safely only to \emph{over-exposed}
+stars, and that there is a superior limit also beyond which
+they are no longer applicable. Both Dr.\ \textsc{Charlier} and Professor
+\textsc{Schaeberle} have found that the stars with the longest exposure are
+best fitted for the determination of magnitude.
+
+We may now quote, without further remark, the final formula to
+which Dr.\ \textsc{Charlier} is led, which gives the relation between $m$
+(star's magnitude), $d$ (diameter of star-image on plate), and $t$ (exposure
+time). It is
+\[
+\tag{6} m = A + B \log d + C \log t
+\]
+In the particular plates in question the constants $A$, $B$ and $C$ are
+\[
+A=+17.2\quad B=-6.75\quad C=+1.69
+\]
+$A$, $B$ and $C$ are proved to be constant on the four plates in question;
+$t$ is expressed in minutes.
+
+From the formula (6) the photographic magnitudes of fifty-two of
+%-----File: 116.png-----
+the brighter stars in the \textit{Pleiades} were computed, and compared
+with the photometric magnitudes of the same stars as determined
+by Dr.\ \textsc{Lindemann}, at Pulkowa. (Table III.)
+
+The mean difference between the photographic and photometric
+magnitudes is $\pm 0.22$ mag. The differences occur $0.6$ mag.\ (twice),
+$0.5$ (twice), $0.4$ (4 times), $0.3$ (12 times), $0.2$ (12 times), $0.1$ (10
+times), $0.0$ (7 times). Two stars are either variable or red. The
+individual results for the photographic magnitudes from the four
+plates agree well. The mean difference is $0.10$ mag. The largest
+difference is $0.4$ (occurring twice). % Transcriber's note: original reads "occuring"
+
+Dr.\ \textsc{Charlier} makes the important remark that the red stars,
+etc., which are thus discovered in the group of the \textit{Pleiades}, are very
+suitable for a determination of its parallax, since they differ in spectral
+type, and are therefore \emph{presumably} not members of the group.
+A few moments' examination with a small spectroscope will, however,
+be a surer indication in similar cases.
+
+\smallskip
+Section III of the memoir is devoted to a comparison of the
+results of the Stockholm photographs with those obtained by Professor
+\textsc{Pickering}, at Harvard College, and by Dr.\ \textsc{Scheiner}, at
+Potsdam. The linear formula deduced by the latter is shown to be
+inferior to the logarithmic form adopted by Dr.\ \textsc{Charlier}; and
+in Table IX it is shown that the systematic differences between the
+results at Harvard College and at Stockholm are likely to be due to
+constant errors in the H.~C.~O. results. In all this discussion, as has
+been said, the effect of atmospheric absorption is omitted, as it has
+been in all previous publications of the kind. It is of considerable
+amount, however.
+
+\smallskip
+Section IV of the memoir is chiefly concerned with a comparison
+between the photometric magnitudes given by \textsc{Wolf}, of Paris, for
+571 of the \textit{Pleiades} stars and the photographic magnitudes of the
+same stars derived from one plate (only) taken at Stockholm.
+Twenty-eight of \textsc{Wolf's} stars do not appear on this plate; \textit{en
+revanche}, it contains more than 100 stars not in \textsc{Wolf's} catalogue.
+In passing, we may remark that the single Stockholm plate made
+in three hours has a value at least comparable with the chart of
+M.\ \textsc{Wolf}, which was the result of many months of labor. It is
+worth while to remark here that it is highly desirable for the present
+to make every result derived by photography depend on two negatives
+at the very least. A comparison of the scales of \textsc{Wolf} and
+\textsc{Charlier} closes this section and concludes the important work.
+%-----File: 117.png-----
+
+\smallskip
+We may now say that the present memoir and that of Professor
+\textsc{Schaeberle}, previously cited, have fixed the form under which
+discussions of this character must be made in future. For every
+telescope a relation between the diameter of a star image and the
+corresponding exposure must be deduced in the form $d = \varPhi (\log t)$.
+
+The constants of this formula will vary with the aperture, focus,
+plate, site, and with the spectral type of the star, and will probably
+be applicable only within certain limits of absolute brightness and
+within certain limits of exposure time.
+
+The memoir of M. \textsc{Charlier} is an excellent example of the
+method of discussion which must be adopted to determine this
+function for all cases where the prime object is to make the photographic
+magnitudes harmonize as nearly as possible with the photometric.
+The real fundamental question is, however, Should any
+endeavor be made to harmonize them? I proceed to discuss this
+point as briefly as possible, in the light of our present knowledge,
+since it is the most important question remaining open for settlement.
+
+\nbsubsubsectionheading{\textit{Establishment of the Present System of Visual Magnitudes.}}
+
+Let us consider, very briefly, the history of the introduction of the
+present system of visual magnitudes. The main epochs in this history
+are very few. The first is that of \textsc{Ptolemy} (\textsc{a.~d.}\ 150,) who arbitrarily
+assumed the brightest stars to be of the \textit{first}, the faintest which he
+could see, to be of the \textit{sixth} magnitude. The other stars were divided
+into classes of 2d, 3d, 4th, 5th, etc., magnitudes. The second great
+event in this history is the publication of the \textit{Uranometria Nova} by
+\textsc{Argelander}, in 1843. He adopted the general rules laid down by
+\textsc{Ptolemy}, and followed by \textsc{Sufi}, \textsc{Tycho} and \textsc{Bayer}. The brightest
+stars were called first magnitude, the faintest visible to the naked eye
+were called sixth magnitude. Stars of the classes 2, 3, 4, 5, etc., were
+intermediate. By \textsc{Fechner's} law, it necessarily followed that equal
+differences of sensation corresponded to equal \emph{ratios} of light; or that
+the light of a star of $m^\text{th}$ magnitude must be $\dfrac{1}{\delta}$th part of the light
+of a star one magnitude brighter ($m-1$). Measures of this \emph{light-ratio}
+$\delta$ show its numerical value to be 0.4 very nearly, omitting all
+questions of small variations, etc.
+
+The \textit{Durchmusterungen} of \textsc{Argelander}, \textsc{Krueger}, \textsc{Schoenfeld}
+and \textsc{Thome} will determine the visual magnitude of every star in both
+hemispheres as bright as the tenth magnitude by this same scale.
+That is, if the brightness of a star of the first magnitude is unity, the
+brightness of a star of the $m^\text{th}$ magnitude is
+%-----File: 118.png-----
+\[
+H_{m} = (\delta)^{m-1} \quad \text{where } \delta = 0.4 \tag{7}
+\]
+The universal practice of modern observers has extended this scale
+from the tenth down to the sixteenth or seventeenth magnitude (the
+faintest stars now visible in the largest telescopes). Thus the \emph{accidental}
+choice of the sixth magnitude as the limit of the naked-eye
+stars by \textsc{Ptolemy} has fixed the light-ratio and the practice of all
+astronomers with regard to visual magnitudes for all time to come.
+It is to be noted that if \textsc{Ptolemy's} work on visual magnitudes were
+to be done again \textit{de novo}, and absolutely independently, the method
+chosen would be essentially the following: \emph{One} standard star would
+be chosen (\textit{Polaris}, in our hemisphere). This star would be compared
+with a selected group of stars, and the fact of the constancy (or
+the law of the variation) of its light during the course of the observations
+would be established. Every other star would be compared
+with \textit{Polaris}, either directly or indirectly, and its relative light determined.
+Some convenient magnitude would be \emph{arbitrarily} assigned
+to \textit{Polaris}, and some convenient light-ratio would be \emph{arbitrarily}
+assumed. The magnitude of any and every star would then be
+deduced from the measured ratio of its brightness to that of \textit{Polaris}
+by a formula like our (7) in which the numerical value of $\delta$ would be
+assigned on grounds of convenience alone. It is very likely that the
+value $\delta=0.4$ would be again chosen, because the tenth part of
+a magnitude (easily written with one place of decimals), thus defined,
+is about the limit of perception of the most highly trained
+human eye.
+
+\smallskip
+Such, I conceive, would be the process adopted if the whole
+question of visual magnitudes was entirely open, and if a Congress of
+Astronomers were called in 1890 to decide on the proper methods to
+be followed in fixing the visual magnitudes of the stars anew, or for
+the first time. The process is simple, it is complete, it is logical, it
+is sufficiently accurate for all conceivable uses to which visual magnitudes
+are to be put. The use of a visual magnitude assigned to a star
+is chiefly to determine its brightness at one epoch, so that observations
+at other epochs will determine whether there have or have not
+been changes in its light. It is from celestial bodies which are subject
+to change, and chiefly from these, that we can hope to learn anything
+of the nature of celestial bodies in general. A secondary convenience
+in having a magnitude assigned to a star is to aid in
+identifying, classifying and describing it.
+%-----File: 119.png-----
+
+\nbsubsubsectionheading{\textit{Establishment of a System for Determining Photographic Magnitudes.}}
+
+The International Congress of Astronomers will have to decide
+the question as to how to define the photographic magnitude of a
+star. They will soon be in possession of plates on which millions and
+millions of stars have impressed themselves. The diameter of each
+one of these stars can be measured. The photographic brightness
+of each one of these stars relative to the photographic brightness of
+\textit{Polaris} (for example) can be readily determined. What \emph{magnitude}
+shall be assigned to each one of these stars? Dr.\ \textsc{Charlier's}
+answer to this question has already been given. He would assign to
+each one of a group of stars a photographic magnitude, deduced on
+the principle that the mean deviation of their photographic magnitudes
+from their visual magnitudes should be as small as possible.
+If the same star occurs in two or more different groups, it will
+certainly have different magnitudes assigned to it, according as one or
+the other set of standards is employed. The same method has been
+followed by Mr.\ \textsc{Espin} and by the Harvard College Observatory in
+all of its many important publications on this question, notwithstanding
+the fact that (owing to the color of a star) the photographic and
+visual magnitudes not infrequently differ by at least \emph{two whole magnitudes.}
+That is, if the visual brightness be expressed by 1.00, the
+photographic brightness of the same star may be no more than 0.16,
+or only one-sixth part. Such anomalies must in the nature of things
+constantly appear for a considerable percentage of the stars. A
+tolerable agreement is possible for perhaps eighty per cent.\ of the
+larger stars, and even here there will be small persistent differences.
+For those remaining, the disagreement will be more or less marked,
+according as the spectral type of the star in question varies more or
+less from the average type. The reason of this is well known. The
+eye is sensitive to rays which fall between the \textsc{Fraunhofer} lines B
+and G (approximately) of the solar spectrum. The maximum brilliancy
+to the eye is somewhere near the line $b$. The photographic
+plate is sensitive to rays falling between F and N of the solar spectrum
+(approximately). The plates now in use are sensitive in the highest
+degree to rays of about the wave length of the line G.
+
+Whenever we have a group of say five hundred stars, whose spectra
+are nearly all of the same type (as the \textit{Pleiades}, for example,) we can
+measure for each star the relative energy of the light in the portion of
+its spectrum between B and G (by the eye), in that between F and
+N (by the photographic plate), and, \emph{as the energy is distributed according
+%-----File: 120.png-----
+to the same law in the spectrum of each star of the group}, we can
+determine constants of reduction which \emph{will} make the photographic
+magnitudes of the various stars agree well with their visual magnitudes.
+If, however, two hundred of the stars are very red, one hundred very
+blue and two hundred of the ordinary type, it is, in the nature of
+things, impossible to bring the photographic and the visual magnitudes
+to a good agreement. The very red stars will always appear brighter
+to the eye than they do on the plate, and the very blue stars will
+always appear fainter to the eye than on the plate, and there is no
+process of reduction which will smooth away a difference in their
+magnitudes which is inherent in their nature. If there were such a
+process, it would be most unwise to employ it. When I see that a
+star is of the visual magnitude 1 and the photographic magnitude 2.5,
+I at once learn something of the nature of this star's spectrum, and
+so in like cases.
+
+\medskip
+It therefore seems to be a rational and a useful plan to leave out all
+consideration of the visual magnitudes of stars in determining their
+photographic magnitudes. A simple and most satisfactory method of
+procedure would be to assume \textit{Polaris} as the standard star of the
+whole sky, and to fix its magnitude (when in the zenith of a station at
+sea level) at 2.00, once for all; to select a set of secondary standards,
+distributed round the equator, and to determine the brightness of each
+one of these stars in terms of that of \textit{Polaris} (a proof of the constancy
+of the light of \textit{Polaris} being thus attained). Important groups like
+the \textit{Pleiades}, etc., would also have their brightness determined in
+terms of that of the standard. The brightness of the principal Southern
+stars should also be fixed in terms of \textit{Polaris} indirectly through
+the \textit{Pleiades}, etc. A light-ratio should be selected on grounds of convenience
+alone and the photographic magnitude of every star should
+be determined by an equation like our equation (7) in terms of a
+single standard star with a definite light ratio.
+
+If this programme were to be followed, we should simply have to
+add to our star-catalogues another column headed ``Photographic
+Magnitude,'' which would immediately follow the column ``Visual
+Magnitude.'' The agreement or disagreement of the two numbers
+would tell us something of the nature of the spectrum of each star.
+In order to have the work exact, it would be necessary that all the
+stars should be photographed on one kind of plates, as is now done by
+the Harvard College Observatory, and as will be done by the
+International Photographic Congress. The photographic Southern
+%-----File: 121.png-----
+\textit{Durchmusterung} might for convenience have its magnitudes expressed
+in visual units, though the DM of the Cordoba Observatory will make
+this unnecessary, and will, in fact, make it distinctly to the advantage
+of science if the photographic DM is made \emph{entirely} photographic.
+The International map of two million stars to the eleventh magnitude
+should, in my judgment, give photographic magnitudes \emph{alone}. I can
+conceive of no advantage to be gained by determining the approximate
+visual magnitude of these millions of stars at all comparable
+with the labor involved. In any event, it would seem that the
+photographic magnitudes should be given whether the visual magnitudes
+are or are not.
+
+\medskip
+Such, it appears to me, are the general principles which should
+govern in the determination of star magnitudes by photography.
+I have set them forth because no amount of discussion at this stage
+can be called superfluous. After the International Congress has
+once settled its methods of procedure, it will be the duty of all
+co-operating observatories to conform to the spirit and to the letter of
+the methods finally adopted. As long as they are not yet adopted
+any suggestions, however simple, cannot fail to be of use.
+
+\medskip
+The Lick Observatory is endeavoring to make a modest contribution
+to the general subject of which we have spoken. Professor
+\textsc{Schaeberle} has made observations at Mount Hamilton (4209 feet
+above sea), and will make observations at Cayenne, South America,
+(nearly at sea-level), to determine the photographic atmospheric
+absorption at zenith distances between 0� and 70� or 75�. He has
+already compared the \textit{Pleiades} and other stars with \textit{Polaris}, and will
+compare the principal Southern stars with the \textit{Pleiades}, etc. In this
+way, his observations, if successful, will enable us to transfer the
+standards of the Northern Hemisphere into the Southern.
+
+The immense work now in progress in both hemispheres under
+the auspices of the Harvard College Observatory will afford material
+for a thorough discussion of the whole subject. The contributions
+of Dr.\ \textsc{Charlier} and Professor \textsc{Schaeberle} have established the
+final form under which special discussions of this kind must be made.
+The only part of the subject remaining for settlement is that which
+relates to the establishment of the fundamental principles on which the
+final methods of reductions are to be based. I have endeavored, in
+what precedes, to set forth what seems to me to be a satisfactory
+system, at once simple and comprehensive.\pushright{E.~S.~H.}
+%-----File: 122.png-----
+
+\nbsubsectionheading{Variations of the Surface of Mars.}
+\addcontentsline{toc}{section}{Variations of the Surface of Mars [from a note by \textsc{M.~C. Flammarion}]}
+
+In the second volume (1888) of the \textit{Bulletin de la Soci�t� Astronomique
+de France}, M. \textsc{Flammarion} has two long and studied articles
+on the \emph{markings} of the planet \textit{Mars}. He is careful to present a great
+number of \textit{fac-simile} drawings of the planet, which date from 1659 to
+1888, so that the evidence which he has used is before the eyes of
+the reader. After showing that drawings of \textit{Mars} may differ greatly
+from each other on account of differences of eyes, methods, interpretation,
+instruments, atmospheric influences both on \textit{Mars} and the
+earth, and on variations of the inclination of the planet's axis, he goes
+on to show that there still remain variations which are (probably) not
+due to any of these causes, and which therefore are to be attributed
+to real variations in the surface of the planet itself.
+
+Most of the paper is devoted to an examination of the evidence
+of the drawings. (In this connection it is well to refer to a set of
+articles by Professor \textsc{Schiaparelli}, in \textit{Himmel und Erde} for October,
+November and December, 1888, where the same questions are treated
+also in a masterly manner.) At the close of this examination
+M. \textsc{Flammarion} feels authorized to draw the following conclusions
+as established facts---leaving all speculation to one side:
+
+\begin{description}
+\item[I.] ``There are permanent markings on the surface of \textit{Mars,}
+which in all probability represent \textit{(`doivent repr�senter'}) seas, lakes,
+regions of water of various kinds, etc. (It has long been known that
+on this planet there are polar snows which melt in summer, clouds,
+and the vapor of water shown by spectroscopic observations.)
+
+\item[II.] ``These markings are permanent; they are seen to-day in the
+same regions where they were observed in the seventeenth and
+eighteenth centuries. They are not atmospheric products, then, such
+as are shown, for example, on \textit{Jupiter}.
+
+\item[III.] ``However, while they are permanent they are not invariable.
+They change both in extent and in depth of tone, in different years
+and without doubt during different seasons [seasons of \textit{Mars}].
+
+\item[IV.] ``There are some regions which are specially variable.
+These appear to hold a middle place between continents and seas,
+and to be marshy lands, which are in turn elevated above and submerged
+below a thin layer of water.
+
+\item[V.] ``The continents of \textit{Mars} appear to be flat; and subject to
+inundations in nearly all their extent.
+
+\item[VI.] ``The northern hemisphere is more elevated than the
+southern; the seas are chiefly in the southern hemisphere, and
+they do not appear to be deep.
+%-----File: 123.png-----
+
+\item[VII.] ``The evaporation on \textit{Mars} is, without doubt, rapid and
+considerable. Millions of cubic yards of water pass readily from the
+state of vapor to the state of liquid, and millions of acres pass from
+the continental to the maritime aspect.
+
+\item[VIII.] ``Water is perhaps not the only agent concerned in these
+changes. The general order of things is very different on \textit{Mars} and
+on the earth.''
+\end{description}
+
+This is not the place to examine the conclusions critically. In a
+general way, they all depend upon the assumption that the darker
+markings on \textit{Mars} represent bodies of water. As this is quite
+probable (though by no means proved as yet) the eight theorems
+given above may serve as points of departure in the further working
+out of this plausible hypothesis.\pushright{E.~S.~H.}
+
+
+\nbsubsectionheading{Stability of the Great Equatorial.}
+\addcontentsline{toc}{subsection}{\qquad Stability of the Great Equatorial}
+
+{\stretchyspace
+Observations for the position of the great telescope have been
+made by Messrs.\ \textsc{Schaeberle} and \textsc{Keeler}, as below:
+\begin{tablesetup}
+\begin{tabular}{l@{~}l@{~}l@{~}c@{~}l@{~}c@{~}l@{~}r@{~}c@{~}c}
+1888,& July &27,  & azimuth &= $+36''$; & level &=&$ 8''$&too & low.\\
+1889,& May  &18,  &   ``    &= ------   &  ``   &=&$36''$& `` & ``\\
+     & Sept.&16,  &   ``    &= $+83''$  &  ``   &=&$58''$& `` & ``
+\end{tabular}
+\end{tablesetup}
+
+}There appears to be a slight progressive change in level and
+probably in azimuth.
+
+
+\nbsubsectionheading{Mountain Observatories.}
+\addcontentsline{toc}{subsection}{\qquad Mountain Observatories [from the \textit{Opticks} of Sir \textsc{Isaac Newton}]}
+
+Telescopes \ldots ``cannot be formed so as to take away
+that confusion of rays which arises from the tremors of the atmosphere.
+The only remedy is a most serene and quiet air, such as may perhaps
+be found on the tops of the highest mountains above the grosser
+clouds.''---Sir \textsc{Isaac Newton}, in his \textit{Opticks}, \textsc{a.~d.}\ 1730. % original has A.D. here; regularised to match usage on 117.png
+
+\nbsubsectionheading{Rainfall on Mount Hamilton.}
+\addcontentsline{toc}{subsection}{\qquad Rainfall at Mount Hamilton}
+
+Meteorological observations have been kept at Mount Hamilton
+since 1880. The following table of rainfall on the summit is the best
+available summary. This rainfall is considerably more than that in
+the Santa Clara Valley near San Jos� (about 13.4 inches) and it is
+probably considerably less than the fall in some of the ca�ons and
+valleys immediately surrounding the mountain. The great variations
+in the annual amount of rainfall are interesting from a meteorological
+%-----File: 124.png-----
+point of view, and decidedly inconvenient from a practical one,
+especially as our reservoir capacity is not quite adequate.\pushright{E.~S.~H.}
+
+\begin{tablesetup}
+\renewcommand{\tabcolsep}{4pt}
+\begin{tabular}{l@{\,} *{9}{|r@{.}l} }
+\multicolumn{19}{c}{\textit{
+    Rainfall at Mount Hamilton in the Years 1880--89. }}\\[1ex]
+\hline\hline
+\multicolumn{1}{c|}{\footnotesize\textsc{Month.}\rule{0pt}{3ex}}&
+\multicolumn{2}{c|}{\footnotesize 1880--81}&
+\multicolumn{2}{c|}{\footnotesize 1881--82}&
+\multicolumn{2}{c|}{\footnotesize 1882--83}&
+\multicolumn{2}{c|}{\footnotesize 1883--84}&
+\multicolumn{2}{c|}{\footnotesize 1884--85}&
+\multicolumn{2}{c|}{\footnotesize 1885--86}&
+\multicolumn{2}{c|}{\footnotesize 1886--87}&
+\multicolumn{2}{c|}{\footnotesize 1887--88}&
+\multicolumn{2}{c}{\footnotesize 1888--89}\\[1ex]
+\hline
+
+& \multicolumn{2}{c|}{\footnotesize in.}
+& \multicolumn{2}{c|}{\footnotesize in.}
+& \multicolumn{2}{c|}{\footnotesize in.}
+& \multicolumn{2}{c|}{\footnotesize in.}
+& \multicolumn{2}{c|}{\footnotesize in.}
+& \multicolumn{2}{c|}{\footnotesize in.}
+& \multicolumn{2}{c|}{\footnotesize in.}
+& \multicolumn{2}{c|}{\footnotesize in.}
+& \multicolumn{2}{c}{\footnotesize in.}\\
+
+July    & 0&00& 0&00& 0&00& 0&00& 0&00&\ 0&00& 0&00& 0&04& 0&00\\[1ex]
+August   & 0&00& 0&00& 0&00& 0&00& 0&15& 0&00& 0&00& 0&00& 0&02\\[1ex]
+September& 0&00& 0&10& 0&00& 0&65& 0&65& 0&15& 0&00& 0&33& 0&49\\[1ex]
+October  & 0&00& 0&33& 6&16& 2&15& 3&71& 0&05& 0&60& 0&09& 0&03\\[1ex]
+November\tablenoteasterisk & 0&50& 0&91& 3&45& 1&48& 0&01&
+\multicolumn{2}{c|}{------\ \ }& 2&82& 0&90& 3&27\\[1ex]
+December & 9&68& 9&72& 1&93& 2&05&33&84&
+\multicolumn{2}{c|}{------\ \ }& 2&34&11&25& 4&23\\[1ex]
+January  & 3&51& 3&55& 3&10& 5&60& 1&99&
+\multicolumn{2}{c|}{------\ \ }& 2&83&10&04& 1&04\\[1ex]
+February & 5&99& 2&90& 3&75&12&76& 0&57& 1&80& 7&80& 1&38& 1&42\\[1ex]
+March    & 1&13& 5&40& 8&66&16&35& 1&15& 5&77& 1&39& 3&40& 6&17\\[1ex]
+April    & 0&98& 4&70& 2&66&11&96& 2&08& 6&79& 5&75& 0&68& 1&92\\[1ex]
+May      & 0&09& 0&48& 7&55& 1&24& 0&16& 0&70& 0&25& 1&25& 3&21\\[1ex]
+June     & 0&33& 1&06& 0&00& 3&85& 0&36& 0&00& 0&30& 0&67& 0&00\\[1ex]
+\hline
+Sums\rule{0pt}{3ex}      &22&21&29&15&37&26&58&09&44&67&
+\multicolumn{2}{c|}{------\ \ }&24&08&30&03&21&80\\[1ex]
+\hline
+\multicolumn{19}{c}{\footnotesize
+* November, 1880---One shower, amount assumed to be $0^\text{in}.50$. N.~B. December, 1884. }
+\end{tabular}
+\end{tablesetup}
+
+Mean annual rainfall (8 years), \textit{July to July}~=~33.41~in.
+
+\nbsubsectionheading{Great Telescope for Los Angeles.}
+\addcontentsline{toc}{section}{Great Telescope for Los Angeles}
+
+Authentic information regarding the proposed forty-inch refractor
+for Wilson's Peak is difficult to obtain. A newspaper report of an
+interview with Mr.\ A.~G. \textsc{Clark} on September~28, recites that one of
+the discs (now on exhibition at Paris) will probably arrive in Boston
+in October. The other disc is not yet cast, and M. \textsc{Mantois} is,
+apparently, not willing to undertake the work without a contract,
+which is not yet executed. The Trustees of the Fund have, so it is
+said, authorized Mr.\ \textsc{Clark} to pay \$10,000 for two satisfactory forty-inch
+discs, which is not an unreasonable price by any means.
+Mr.\ \textsc{Clark} offered to make the objective and the mounting for
+\$100,000, during his visit to California in the winter of 1888--9. So
+far as is now known, the fund available for the telescope does not yet
+exceed \$150,000. Probably \$300,000 to \$400,000 would build and
+equip the observatory.\pushright{E.~S.~H.}
+%-----File: 125.png-----
+
+\nbsubsectionheading{Force of Gravity at Mt. Hamilton and San Francisco.}
+\addcontentsline{toc}{subsection}{\qquad Force of Gravity at Mount Hamilton and San Francisco, as determined by \textsc{E.~D. Preston} of the U. S. Coast and Geodetic Survey}
+
+Mr.\ E.~D. \textsc{Preston} of the U.~S. Coast and Geodetic Survey has
+published his report on gravity determinations in the Pacific Ocean
+(\textit{Bulletin} No.~11, U.~S.~C. and G.~S., 1889). The force of gravity
+at Washington being 1.000000, that at San Francisco (Professor
+\textsc{Davidson's} Observatory) is 0.999854 and at the Lick Observatory
+it is 0.999544. Determinations of \textit{g} at four stations in the Hawaiian
+Islands and for a station at Caroline Island are also given.\pushright{E.~S.~H.}
+
+
+\nbsubsectionheading{Lick Observatory Photographs of the Moon.}
+\addcontentsline{toc}{subsection}{\qquad Lick Observatory Photographs of the Moon}
+
+\textit{Knowledge} for October~1, 1889, contains an article by the editor
+(Mr.\ \textsc{Ranyard}), on the Moon as seen in the Lick Telescope.
+Excellent reproductions of five silver prints made by the Direct
+Photo-Engraving Company of London, accompany the article.
+Mr.\ \textsc{Ranyard's} remarks upon the temperature of the moon and upon
+the possibility of the existence of snow-fields on its surface, are well
+worth close attention.\pushright{E.~S.~H.}
+
+
+\nbsubsectionheading{American Eclipse Expedition to Africa (December~21, 1889).}
+\addcontentsline{toc}{subsection}{\qquad American Eclipse Expedition to Africa (December~21, 1889)}
+
+The New York \textit{Sun}, for October~17, has an account of the sailing
+of the U.\,S.\,S.\ \textit{Pensacola} with the American Eclipse Expedition
+to Africa. The expedition is under Professor D.~P. \textsc{Todd}, of Amherst
+College, as chief astronomer. His astronomical assistants are
+Messrs.\ \textsc{Bigelow}, \textsc{Davis} and \textsc{Jacobi}. Mr.\ \textsc{Carbutt} goes as photographer,
+with Mr.\ \textsc{Wright} as his assistant; Mr.\ E.~J. \textsc{Loomis} as
+naturalist; Professor \textsc{Abbe} as meteorologist, with G.~E. \textsc{Van
+Guysling} as assistant; Mr.\ \textsc{Preston} as the observer of magnetics
+and for determinations of gravity; Mr.\ W.~H. \textsc{Brown} as osteologist
+and naturalist, with his brother as assistant; Mr.\ \textsc{Orr} as ethnologist
+and ornithologist; H. \textsc{Chatelaine} as interpreter; G.~T. \textsc{Flint} as
+stenographer, and Dr.\ \textsc{Bartlett} as apothecary! Add to these
+names that of Professor \textsc{Alex.\ Agassiz}, who may join the vessel at
+Cape Town to engage in deep-sea dredging. This is carrying the
+war into Africa, indeed. The newspaper account of the astronomical
+outfit is somewhat meagre. It appears that the expedition is provided
+with a photoheliograph, giving an image of the sun four inches
+in diameter. With this the partial phases will be photographed on
+\emph{ortho-chromatic} plates (No.\ 16) and the total phase on \emph{ortho-chromatic}
+plates (No.\ 27). A large mirror, belonging to Professor \textsc{Langley},
+%-----File: 126.png-----
+an equatorial belonging to the Harvard College Observatory, and
+\emph{twenty} cameras are also provided for photography.
+
+It is to be hoped that the expedition will meet with fine weather,
+in order to utilize its unusually large force of observers and instruments.
+Sir \textsc{Isaac Newton} said at the death of his pupil \textsc{Cotes},
+``If \textsc{Cotes} had lived, we should have known something.'' If the
+four minutes of totality are clear at St. Paul de Loanda % TN: original reads "Loando"; modified on frequency grounds
+ we shall certainly
+learn something from these many skilled observers with their
+large equipment.
+
+It now appears that with two expeditions in Africa, and with two
+at least, in America, the observation of this eclipse is thoroughly well
+provided for. It should be a source of gratification to Californians,
+and especially to this Society, that the generosity of one of our members
+has allowed the Lick Observatory to put a strong expedition in
+the field.\pushright{E.~S.~H.}\\*[1ex]
+{\small\indent October~26, 1889.}
+
+\nbsubsectionheading{Eclipse of \textit{Japetus}, the VIII Satellite of \textit{Saturn}, on
+November~1, 1889.}
+\addcontentsline{toc}{subsection}{\qquad Eclipse of \textit{Japetus}, the VIII satellite of \textit{Saturn}. By \textsc{E.~E. Barnard}}
+
+The eclipse of \textit{Japetus} was observed here on November~1 with
+the twelve-inch equatorial. Only a part of this very rare phenomenon
+was visible at this point, the interval between the rising of \textit{Saturn}
+and daylight covering only a small portion of the time occupied by
+the eclipse, or, rather, series of eclipses; for the satellite passed
+through the shadow of the entire ring system as well as that of the
+globe of \textit{Saturn}. The satellite would first pass into the outer edge
+of the shadow of the ring, and would next appear in the sunlight,
+shining through the \textsc{Cassini} division, being visible for probably
+eighteen minutes. It would then pass into the shadow of the inner
+bright ring; from this it would emerge in the semi-shadow of the
+Crape Ring, from which it would pass into the sunlight again between
+the shadow of the Crape Ring and that of the ball. It would next
+enter the shadow of the ball, and, from this point on, a reversal of
+all the first phenomena would happen. The entire series of eclipses
+covered a period of approximately nineteen hours. That portion of
+the eclipse which could be seen from the Lick Observatory was the
+reappearance from the shadow of the globe and passage through the
+semi-shadow of the Crape Ring into the shadow of the inner bright
+ring.
+
+The important questions in connection with this phenomenon
+%-----File: 127.png-----
+were: Would the satellite become visible when it came to the projection
+of the \textsc{Cassini} division? What would be the effect of the Crape
+Ring upon the appearance of the satellite?
+
+The last question only could be answered from this point, as the
+satellite would rise eclipsed in the shadow of the ball, and not reach
+the second part of the \textsc{Cassini} division until long after sun-up.
+
+Carefully watching the point of reappearance of the satellite, it
+was faintly caught at $14^\text{h}\ 38^\text{m}$ Mt.~H. m.~t. It reappeared quite close
+to the satellites \textit{Tethys} and \textit{Enceladus}. It grew pretty rapidly brighter,
+and attained its full brightness at about $14^\text{h}\ 50^\text{m}$. It was then about
+0.1 magnitude less than \textit{Tethys}. The proximity to these two satellites
+gave an excellent means of detecting changes in its brightness
+by comparison with their light. Eighty such comparisons were made,
+and from these I have constructed a curve, which very clearly shows
+what effect the Crape Ring had upon the appearance of the satellite.
+\textit{Japetus} required a little over ten minutes to become wholly free
+from the shadow of the ball. After remaining at its full brightness
+for fifteen minutes, it began very slowly to decrease in light; however,
+changing less than 0.1 magnitude in forty minutes' time. At
+$15^\text{h}\ 54^\text{m}$ the light began to decrease more rapidly, and in sixty-five
+minutes it passed through 0.7 of a magnitude. It then approached
+the shadow of the inner bright ring, and in fifteen minutes its light
+diminished 0.66 of a magnitude, when it totally disappeared, at
+$17^\text{h}\ 11^\text{m}\,{}^1\!/\!_2$.
+
+These observations show us that, after striking the sunlight shining
+through between the ball and the rings, the satellite then passed into
+the shadow of the Crape Ring, which sensibly affected its brightness.
+Passing deeper into this \emph{shade}, the absorption of the sunlight became
+more and more pronounced, until finally the satellite struck the
+shadow of the inner bright ring, which it rapidly entered and within
+which it disappeared.
+
+These observations, therefore, tell us that the Crape Ring is truly
+transparent---the sunlight sifting through it; that the particles composing
+the Crape Ring cut off an appreciable quantity of sunlight;
+that these particles cluster more and more thickly---or, in other
+words, the Crape Ring is denser as it approaches the bright rings.
+
+Observations made elsewhere will tell us whether the satellite was
+seen when it entered the projection of the \textsc{Cassini} division. The
+observations will be published in full in the \textit{Monthly Notices} of the
+Royal Astronomical Society.\pushright{E.~E.~B.}\\*[1ex]
+{\small\indent\textsc{Mt.~Hamilton}, Nov. 6th, 1889.}
+
+%-----File: 128.png-----
+\addcontentsline{toc}{subsection}{\qquad Five full-page plates of drawings of \textit{Jupiter} to follow}
+\begin{figure}[p]
+	\centering
+  \LARGE\textit{Plate I}\\[5mm]
+	\includegraphics{images/fig6.jpg}\\
+  \raggedright \qquad \footnotesize E.E.B. Del\textsuperscript{\underline{t}}\\
+  \centering\LARGE\textit{Jupiter.}
+\end{figure}
+\begin{figure}[p]
+	\centering
+  \LARGE\textit{Plate II}\\[5mm]
+	\includegraphics{images/fig7.jpg}\\
+  \raggedright \qquad \footnotesize E.E.B. Del\textsuperscript{\underline{t}}\\
+  \centering\LARGE\textit{Jupiter.}
+\end{figure}
+\begin{figure}[p]
+	\centering
+  \LARGE\textit{Plate III}\\[5mm]
+	\includegraphics{images/fig8.jpg}\\
+  \raggedright \qquad \footnotesize E.E.B. Del\textsuperscript{\underline{t}}\\
+  \centering\LARGE\textit{Jupiter.}
+\end{figure}
+\begin{figure}[p]
+	\centering
+  \LARGE\textit{Plate IV}\\[5mm]
+	\includegraphics{images/fig9.jpg}\\
+  \raggedright \qquad \footnotesize E.E.B. Del\textsuperscript{\underline{t}}\\
+  \centering\LARGE\textit{Jupiter.}
+\end{figure}
+\begin{figure}[p]
+	\centering
+  \LARGE\textit{Plate V}\\[5mm]
+  \includegraphics{images/fig10.jpg}
+\end{figure}
+
+\nbsectionheading{\textsc{Parabolic Elements of Comet Swift (Nov.~16).}}
+\addcontentsline{toc}{section}{Parabolic Elements of Comet Swift (Nov.~16). By \textsc{A.~O. Leuschner}}
+
+\nbsubsubsectionheading{\shortrule\\*
+By \textsc{A.~O. Leuschner.}\\*
+\shortrule}
+
+From the three successive observations at Lick Observatory,
+November~20, 21, 22, which were kindly communicated to me by
+Professor E.~E. \textsc{Barnard}, I have deduced the following parabolic
+elements by \textsc{Oppolzer's} method:
+\begin{tablesetup}
+\renewcommand{\arraystretch}{1.3}
+\begin{tabular}{r@{ }c@{ }lc}
+T &$=$&\multicolumn{2}{@{}l}{1889, Dec.~11, 8493 G.~M.~T.}\\
+$\ascnode$ &$=$&$ 306�\ 25'$
+& \multirow{3}{*}{\centering \qquad O $-$ C
+  $\left\{ \begin{array}{l@{\ }c@{\ }l}
+     \text{d } \lambda, & \cos\beta & = +1'.2  \\
+     \text{d }\beta     &           &= \pm 0.\,0
+           \end{array} \right.$}
+\\
+$\omega$  &$=$&$ 116�\ 24'$\\
+$i$       &$=$&$ 6�\ 47'$\\
+$\log q$  &$=$&$ 0.0633$\\
+\end{tabular}
+\end{tablesetup}
+
+\filbreak
+The small geocentric arc and the error of $1'.2$ remaining in $\lambda$
+render these elements extremely uncertain. The comet is very likely
+periodic.
+
+\textsc{Berkeley, Cal}., November~27, 1889.
+
+\ThoughtBreakLong
+
+\nbsectionheading{\textsc{Minutes of the Meeting of the Board of Directors, Held
+November~30, 1889, at 408 California Street,
+San Francisco.}}
+\addcontentsline{toc}{section}{Minutes of the Meeting of the Board of Directors, November~30, 1889}
+
+A quorum was present.
+
+The minutes of the last meeting were read and approved.
+
+Bills presented by the Secretary and Treasurer were approved.
+
+Miss C.~W. \textsc{Bruce}, of New York City, was duly elected a life member,
+subject to the action of the Society.
+
+Adjourned.
+
+\bigskip
+\nbsectionheading{\textsc{Minutes of the Meeting of the Astronomical Society Of
+the Pacific, Held November~30, 1889 (by Invitation),
+in the Rooms of the California Academy
+of Sciences, San Francisco.}}
+\addcontentsline{toc}{section}{Minutes of the Meeting of the Society held in San Francisco, November~30, 1889}
+
+\nbsubsubsectionheading{[\small \textsc{Prepared by the Secretaries for Publication}.]}
+
+Owing to the absence of the President, Vice-President \textsc{Pierson} took the
+chair.
+
+The thanks of the Society were tendered to the California Academy of Sciences
+for the use of their rooms.
+
+The minutes of the last meeting were read and approved.
+
+A list of gifts to the Society was read, and thanks were returned to the
+donors.
+%-----File: 129.png-----
+
+The following members were then elected; the names of
+life-members, duly elected by the Board of Directors, being marked
+with a star ($^*$):
+
+\begin{small}
+\begin{longtable}[l]{@{}ll}
+\textsc{Charles S. Aiken,} & Berkeley, Cal.\\
+\textsc{J.~H.~C. Bont�, D.~D.} & Berkeley, Cal.\\
+\textsc{Miss C.~W. Bruce,$^*$} & 39 East Twenty-third Street, N.~Y. City.\\
+\textsc{N.~E. Beckwith,} & Los Gatos, Cal.\\
+\textsc{J.~A. Brashear,} &  Allegheny City, Penn.\\
+\textsc{Charles M. Bakewell,} & Berkeley, Cal.\\
+Miss \textsc{Agnes M. Clerke,} & 68 Redcliffe Square, London, England.\\
+Hon.~\textsc{Horace Davis,} & 1011 Bush Street, San Francisco, Cal.\\
+\textsc{A.~B. Depuy,} & 216 North Sixth Street, Camden, N.~J.\\
+\textsc{Warren B. Ewer,} & 220 Market Street, San Francisco, Cal.\\
+Mrs.~\textsc{Martha McC. Ewer,} & 220 Market Street, San Francisco, Cal.\\
+\textsc{John Gamble,} & Laurel Hall, San Mateo, Cal.\\
+\textsc{Henry Harrison,} & South Bergen, N.~J.\\
+\textsc{Charles F. Hart,} &  N. Temescal, Alameda County, Cal.\\
+\textsc{O.~C. Hastings,} &  Box 166, Victoria, B.~C.\\
+\textsc{John J. Herr,} & 438 California Street, San Francisco, Cal.\\
+\textsc{Whitney Herr,} & 438 California Street, San Francisco, Cal.\\
+\textsc{Frank Jaynes,} &  W.~U. Telegraph Co., San Francisco, Cal.\\
+Rev.~\textsc{George W. James, F.~R.~A.~S.}, & Oleander, Fresno County, Cal.\\
+\textsc{Augustus F. Knudsen,} & Box 2139, Boston, Mass.\\
+Professor \textsc{Joseph Le Conte,} & Berkeley, Cal.\\
+Miss \textsc{Margaret Lepper,} & Box 490, Benecia, Cal.\\
+\textsc{Warren Olney,} & 481 Prospect Avenue, Oakland, Cal.\\
+\textsc{James N. Pemberton,} & Downey, Cal.\\
+\textsc{C.~D. Perrine,} & 211 Clay Street, San Francisco, Cal.\\
+\textsc{J.~E. Richards,} & Los Gatos, Cal.\\
+\textsc{F.~B. Rodolph,} & 969 Washington Street, Oakland, Cal.\\
+\textsc{Wm.~G. Raymond,} & Berkeley, Cal.\\
+Professor \textsc{J.~K. Rees,} & Observatory of Columbia College, New York City.\\
+\textsc{Wm.~F. Smith,} & 2515 Broadway Street, San Francisco, Cal.\\
+\textsc{Garrett P. Serviss} & 8 Middagh Street, Brooklyn, N.~Y.\\
+\textsc{J.~A. Sladky,} & Berkeley, Cal.\\
+\textsc{Irving M. Scott,} & 507 Harrison Street, San Francisco, Cal.\\
+\textsc{John H. Yoell,} &  San Jos�, Cal.
+\end{longtable}
+\end{small}
+
+\medskip
+The Secretary's books show that the Society now consists of 156 active and
+22 life members, or 178 in all. Mr.\ \textsc{Pierson} announced to the Society that
+Hon.\ \textsc{Alexander Montgomery}, a member of the Society, offers the sum of
+\$2500 to the Astronomical Society of the Pacific, for the purpose of establishing
+a gold medal to be awarded annually to the writer of the best paper on the
+subject of Astronomy presented to the Society during the year; the gift to be
+without conditions, and the Society to have the privilege of using this gift for
+other purposes. The Society accepted this generous gift by a rising vote.
+
+A paper ``On the Determination of the Relation between the Exposure Time
+and the consequent Blackening of a Photographic Film'' was then read by Mr.\ \textsc{Leuschner}.
+This was followed by a paper ``On Photographs of the Milky Way,''
+by Mr.\ \textsc{Barnard}. The latter paper was illustrated by lantern slides prepared by
+Mr.\ \textsc{Barnard} from some of his own negatives. The other papers announced for
+the evening were not read.
+
+The Society then adjourned to meet at its rooms, 408 California Street, on
+January~25, 1890.
+%-----File: 130.png-----
+
+\nbsectionheading{OFFICERS OF THE SOCIETY.}
+\noindent
+\begin{tabular*}{\textwidth}{@{\extracolsep{\fill}}lcr}
+\textsc{Edward S. Holden} (Lick Observatory),
+&& \textit{President}\\
+\textsc{Wm.~M. Pierson} (76 Nevada Block, S.~F.),
+& \multirow{3}{1em}{\Bigg\}}&\\
+\textsc{W.~H. Lowden} (213 Sansome Street, S.~F.)
+&& \textit{Vice-Presidents}\\
+\textsc{Frank Soul�} (Students' Observatory, Berkeley),&&\\
+\textsc{Chas. Burckhalter} (Chabot Observatory, Oakland),
+&\multirow{2}{1em}{\Big\}}
+&\multirow{2}{5em}{\textit{Secretaries}}\\
+\textsc{J.~M. Schaeberle} (Lick Observatory),&&\\
+\textsc{E.~J. Molera} (850 Van Ness Avenue, S.~F.),
+&& \textit{Treasurer}
+\end{tabular*}
+
+\compactlisttwo\stretchyspace
+\item[] \textit{Board of Directors}---Messrs.\ \textsc{Alvord, Boericke, Burckhalter, Gibbs,
+Grant, Holden, Lowden, Molera, Pierson, Schaeberle, Soul�}.
+\item[] \textit{Finance Committee}---Messrs.\ \textsc{Gibbs, Pierson, Molera}.
+\item[] \textit{Committee on Publication}---Messrs.\ \textsc{Dewey, Treat, Ziel}.
+\item[] \textit{Committee on the Comet Medal}---Messrs.\ \textsc{Holden} (\textit{ex officio}), % original has ex-officio
+\textsc{Schaeberle}, \textsc{Burckhalter}.
+\end{list}
+
+\ThoughtBreak
+
+\nbsectionheading{NOTICE.}
+
+Members are requested to preserve the copies of the Publications of the
+Society as sent to them. Once each year a title page and index of the preceding
+numbers will also be sent to the members, who can then bind the numbers
+together into a volume.
+
+It is intended that each member of the Society shall receive a copy of each
+one of the Publications for the year in which he was elected to membership and
+for all subsequent years. If there have been (unfortunately) any omissions in this
+matter, it is requested that the Secretaries be at once notified, in order that the
+missing numbers may be supplied.
+
+Complete volumes for past years (preceding the calendar year in which any
+member was elected) will also be supplied to members, so far as the stock in hand
+is sufficient, on the payment of one dollar to either of the Secretaries.
+
+The titles of papers for reading should be communicated to either of the
+Secretaries as early as possible.
+
+Those members who propose to attend any or all of the meetings at Mount
+Hamilton during the summer should communicate with ``The Secretary Astronomical
+Society of the Pacific,'' at the rooms of the Society, 408 California Street,
+San Francisco, in order that arrangements may be made for transportation,
+lodging, etc.
+\vfil
+\[
+ \includegraphics{images/fig4.jpg}
+\]
+
+\backmatter
+\pagestyle{licensing}
+
+\begin{verbatim}
+End of the Project Gutenberg EBook of Publications of the Astronomical
+Society of the Pacific, by Various
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+This eBook, including all associated images, markup, improvements,
+metadata, and any other content or labor, has been confirmed to be
+in the PUBLIC DOMAIN IN THE UNITED STATES.
+
+Procedures for determining public domain status are described in
+the "Copyright How-To" at https://www.gutenberg.org.
+
+No investigation has been made concerning possible copyrights in
+jurisdictions other than the United States. Anyone seeking to utilize
+this eBook outside of the United States should confirm copyright
+status under the laws that apply to them.
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+Project Gutenberg (https://www.gutenberg.org) public repository for
+eBook #26147 (https://www.gutenberg.org/ebooks/26147)