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authorKarl Berry <karl@freefriends.org>2006-01-09 00:45:48 +0000
committerKarl Berry <karl@freefriends.org>2006-01-09 00:45:48 +0000
commit5dc602d16c5be2fd035b254ca23484a90aebd6dc (patch)
tree72efb15fba318cc2096a8cc6999ed3fa0bff317d /Master/texmf-dist/doc/plain/mnras
parentb4fc5f639874db951177ec539299d20908adb654 (diff)
doc 5
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-rw-r--r--Master/texmf-dist/doc/plain/mnras/mnguide.tex1988
-rw-r--r--Master/texmf-dist/doc/plain/mnras/mnland.tex82
-rw-r--r--Master/texmf-dist/doc/plain/mnras/mnsample.tex705
-rw-r--r--Master/texmf-dist/doc/plain/mnras/readme.txt15
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+% FONTTEST.TEX
+%
+% Test all the possible font combinations in the MN design
+%
+% v0.4 --- released 25th August 1994 (M. Reed)
+% v0.3 --- released 22nd February 1994
+% v0.25 --- released 24th July 1992
+% v0.1 --- first released 27th February 1992
+%
+% Copyright Cambridge University Press
+
+% The following line automatically loads the mn macros if you are not
+% using a format file.
+\ifx\mnmacrosloaded\undefined \input mn\fi
+
+
+% If your system has the AMS fonts version 2.0 installed, MN.tex can be
+% made to use them by uncommenting the line: %\AMStwofontstrue
+%
+% By doing this, you will be able to obtain upright Greek characters.
+% e.g. \umu, \upi etc. See the section on "Upright Greek characters" in
+% the author guide for further information.
+
+\newif\ifAMStwofonts
+%\AMStwofontstrue
+
+\ifCUPmtplainloaded
+ \AMStwofontstrue
+\else
+ \NewTextAlphabet{textbfit} {cmbxti10} {}
+ \NewTextAlphabet{textbfss} {cmssbx10} {}
+ \NewMathAlphabet{mathbfit} {cmbxti10} {} % for math mode
+ \NewMathAlphabet{mathbfss} {cmssbx10} {} % " " "
+ %
+ \ifAMStwofonts
+ \NewSymbolFont{upmath} {eurm10}
+ \NewSymbolFont{AMSa} {msam10}
+ \NewMathSymbol{\upi} {0}{upmath}{19}
+ \NewMathSymbol{\umu} {0}{upmath}{16}
+ \NewMathSymbol{\upartial}{0}{upmath}{40}
+ \NewMathSymbol{\leqslant}{3}{AMSa}{36}
+ \NewMathSymbol{\geqslant}{3}{AMSa}{3E}
+ \let\oldle=\le \let\oldleq=\leq
+ \let\oldge=\ge \let\oldgeq=\geq
+ \let\leq=\leqslant \let\le=\leqslant
+ \let\geq=\geqslant \let\ge=\geqslant
+ \fi
+ %
+\fi
+
+\def\tface{\ifCUPmtplainloaded (Monotype Times)\else (Computer Modern)\fi}
+
+\parindent=0pt
+
+\onecolumn
+
+\pageoffset{-2.5pc}{0pc}
+
+\begintopmatter
+\title{A test file showing all of the possible font combinations}
+
+\shortauthor{Monthly Notices font test \tface}
+\shorttitle{Monthly Notices font test \tface}
+\maketitle
+
+\overfullrule=0pt
+
+\loadboldmathnames
+
+% not available in sub, sub sub and super, super super script:
+% \it, \sl, \tt, \sc and \sf (Computer Modern version)
+
+\def\digs{0123456789}
+\def\testfont#1{%
+ \advance\baselineskip by 5pt
+ {\tenrm #1:}\medskip
+ {$\rm Roman^{\rm Roman^{\rm Roman}}$}\ \
+ {$\bf Boldface^{\bf Boldface^{\bf Boldface}}$}\par
+%
+ \ifCUPmtplainloaded % Times version
+ {$\it Italic^{\it Italic^{\it Italic}}$}\ \
+ {$\sl Slanted^{\sl Slanted^{\sl Slanted}}$}\par
+ {$\tt Typewriter^{\tt Typewriter^{\tt Typewriter}}$}\ \
+ {$\sc Small\ Caps^{\sc Small\ Caps^{\sc Small\ Caps}}$}\par
+ {$\sf Sans\ Serif^{\sf Sans\ Serif^{\sf Sans\ Serif}}$}\par
+ \else
+ {\it Italic}\ \
+ {\sl Slanted}\ \
+ {\tt Typewriter}\par
+ {\sc Small Caps}\ \
+ {\sf Sans Serif}\par
+ \fi
+ %
+ {\textbfit{Bold text italic}%
+ $^{\mathbfit{Bold\ text\ italic^{\mathbfit{Bold\ text\ italic}}}}$}\par
+ {\textbfss{Bold sans-serif}%
+ $^{\mathbfss{Bold\ sans-serif}^{\mathbfss{Bold\ sans-serif}}}$}\par
+ %
+ \ifAMStwofonts
+ Upright math, and others $\upi^{\upi^{\upi}}, \umu^{\umu^{\umu}},
+ \upartial^{\upartial^{\upartial}}, \le^{\le^{\le}}, \ge^{\ge^{\ge}}$
+ \par
+ \fi
+ %
+ {$\cal CALAGRAPHIC^{\cal CALAGRAPHIC^{\cal CALAGRAPHIC}}$}\par
+ {$\bmath{\cal BOLD\ CALAGRAPHIC^{\cal BOLD\ CALAGRAPHIC^{\cal BOLD\ CALAGRAPHIC}}}$}\par
+
+ {$Math\ italic^{Math\ italic^{Math\ italic}}$}\par
+ {$\bmath{Bold\ math\ italic^{Bold\ math\ italic^{Bold\ math\ italic}}}$}\par
+
+ {${\rm Oldstyle}\ \oldstyle \digs^{\oldstyle \digs^{\oldstyle \digs}}$}\par
+ {${\rm Bold\ oldstyle}\ \bmath{\oldstyle \digs^{\oldstyle \digs^{\oldstyle \digs}}}$}\par
+
+ {\rm Math symbols}\ \
+ $\gamma^{\gamma^{\gamma}}\quad \theta^{\theta^{\theta}}
+ \quad \nu^{\nu^{\nu}}\quad \nabla^{\nabla^{\nabla}}$\par
+ {\rm Bold math symbols}\ \
+ $\bgamma^{\bgamma^{\bgamma}}\quad \btheta^{\btheta^{\btheta}}
+ \quad \bnu^{\bnu^{\bnu}}\quad \bnabla^{\bnabla^{\bnabla}}$\par
+% $$
+% \bar x_1-\bar x_2-\left (t_{1-{\alpha\over 2}}
+% \ \times \ s\sqrt{{1\over n_1}+{1\over n_2}}\right )\ {\rm to} \ \bar
+% x_1-\bar x_2+\left (t_{1-{\alpha\over 2}}
+% \times s\sqrt{{1\over n_1}+{1\over n_2}}\right )
+% $$
+% }%
+ Special symbols:
+ $\la$\ $\ga$\ $\getsto$\ $\cor$\ $\lid$\ $\gid$\ $\sol$\ $\sog$\
+ $\lse$\ $\gse$\ $\grole$\ $\leogr$\ $\loa$\ $\goa$\ \sun\ \degr\
+ \diameter\ $\sq$\ \fd\ \fh\ \fm\ \fs\ \fdg\ \fp\ \farcs\ \farcm\
+ \arcsec\ \arcmin\ $\bbbr$ $\bbbm$ $\bbbn$ $\bbbf$ $\bbbh$ $\bbbk$
+ $\bbbp$ $\bbbone$ $\bbbc$ $\bbbq$ $\bbbt$ $\bbbs$ $\bbbz$\par
+ %
+ \ifCUPmtplainloaded
+ \Half
+ \noindent (Monotype Times version only)\par
+ \noindent AMS symbol fonts:
+ $\boxplus$, $\boxtimes$, $\blacksquare$, $\centerdot$, $\lozenge$,
+ $\blacklozenge$, $\yen$, $\checkmark$, $\circledR$, $\maltese$,
+ $\nleqq$, $\ngeqq$,
+ $\precneqq$, $\succneqq$, $\precnapprox$, $\succnapprox$, $\lnapprox$,
+ $\gnapprox$\par
+ \noindent Blackboard Bold: $\Bbb{A}\ldots\Bbb{Z}$\par
+ \fi
+ \Two
+}
+
+
+\eightpoint\testfont{8 point}%
+
+\ninepoint\testfont{9 point}%
+
+\vfil\eject
+
+\tenpoint\testfont{10 point}%
+
+\elevenpoint\testfont{11 point}%
+
+\vfil\eject
+
+\fourteenpoint\testfont{14 point}%
+
+\vfil\eject
+
+\seventeenpoint\testfont{17 point}%
+
+\bye
+
+% end of fonttest.tex
diff --git a/Master/texmf-dist/doc/plain/mnras/mnguide.tex b/Master/texmf-dist/doc/plain/mnras/mnguide.tex
new file mode 100644
index 00000000000..f68e7a06bef
--- /dev/null
+++ b/Master/texmf-dist/doc/plain/mnras/mnguide.tex
@@ -0,0 +1,1988 @@
+% MNGUIDE.TEX
+%
+% Authors' guide for the plain TeX MN macros
+%
+% v1.5 --- released 25th August 1994 (M. Reed)
+% v1.4 --- released 22nd February 1994
+% v1.3 --- released 21st December 1992
+%
+% Copyright Cambridge University Press
+
+% The following line automatically loads the mn macros if you are not
+% using a format file.
+\ifx\mnmacrosloaded\undefined \input mn\fi
+
+% If your system has the AMS fonts version 2.0 installed, MN.tex can be
+% made to use them by uncommenting the line: %\AMStwofontstrue
+%
+% By doing this, you will be able to obtain upright Greek characters.
+% e.g. \umu, \upi etc. See the section on "Upright Greek characters" in
+% this guide for further information.
+
+\newif\ifAMStwofonts
+%\AMStwofontstrue
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%% Macros for this guide %%%%%%%%%%%%%%%%%%%%%%%%%%%
+\makeatletter
+\newskip\ttglue \ttglue=0pt
+
+\chardef\other=12
+\def\ttverbatim{\begingroup \catcode`\\=\other \catcode`\{=\other
+ \catcode`\}=\other \catcode`\$=\other \catcode`\&=\other
+ \catcode`\#=\other \catcode`\%=\other \catcode`\~=\other
+ \catcode`\_=\other \catcode`\^=\other
+ \obeyspaces \obeylines \tt}%
+{\obeyspaces\gdef {\ }}
+
+\outer\def\begintt{$$\let\par=\endgraf \ttverbatim \parskip=0pt%
+ \catcode`\|=0 \rightskip=-5pc \ttfinish}
+
+{\catcode`\|=0 |catcode`|\=\other
+ |obeylines
+ |gdef|ttfinish#1^^M#2\endtt{#1|vbox{#2}|endgroup$$}}
+
+\catcode`\|=\active
+{\obeylines\gdef|{\ttverbatim\spaceskip=\ttglue\let^^M=\ \let|=\endgroup}}
+
+\newdimen\macind \macind=1em % the default indent
+
+\def\beginlines{\par\begingroup\nobreak\Half
+ \leftskip=\macind
+ \parindent=0pt%
+ \nobreak \obeylines \everypar{\strut}%
+}
+\def\endlines{\endgroup\Half\noindent}
+
+\def\hang#1#2{%
+ \par\hangindent=70pt%
+ \advance\hangindent by 1em
+ \noindent\hskip 1em \rlap{\tt #1}\hskip 70pt\relax
+ #2\par%
+}
+
+\def\beginexhang#1{\par\bgroup\let\item=\ex@hang}
+
+\def\ex@hang#1{%
+ \everypar{}\par
+ \Half
+ \everypar{\noindent \ignorespaces}%
+ \noindent %\hskip-\hangindent
+ \boxw{\tt\char"5C #1}\quad\ignorespaces
+}
+
+\def\endexhang{\par\egroup\Half}
+
+\def\beginquote{\bgroup\par\Half\leftskip=2em \rightskip=2em
+ \eightpoint\noindent\ignorespaces}
+\def\endquote{\par\Half\egroup\noindent}
+
+\newdimen\fboxrule \fboxrule=.4pt
+\newdimen\fboxsep \fboxsep=3pt
+\newdimen\tempdimA
+\newbox\BoxA
+
+\newif\ifnocr
+\def\boxw#1{{\global\nocrtrue \fboxsep=2pt \boxit{#1}}}
+
+\long\def\boxit#1{%
+ \setbox\BoxA=\hbox{\kern\fboxsep #1\kern\fboxsep}%
+ \tempdimA=\fboxrule
+ \advance\tempdimA by \fboxsep
+ \advance\tempdimA by \dp\BoxA
+ \noindent \hbox{\lower\tempdimA
+ \hbox{%
+ \vbox{%
+ \hrule height \fboxrule
+ \hbox{%
+ \vrule width \fboxrule \hskip-\fboxrule
+ \vbox{\vskip\fboxsep \box\BoxA\vskip.5\fboxsep}%
+ \hskip -\fboxrule \vrule width \fboxrule
+ }%
+ \hrule height \fboxrule
+ }%
+ }%
+ }%
+ \ifnocr \global\nocrfalse\else \par\medskip\noindent\ignorespaces\fi
+}
+
+\def\multi{\vbox\bgroup\advance\hsize by -2\fboxsep \def\\{\hfil\break}}
+\def\endmulti{\egroup}
+
+\def\Notes{%
+ \if@nobreak \everypar{}\half \else \addpen{\gds@cbrk}\addvspace{\half}\fi
+ \noindent\@nohdbrk {\em Notes}\par
+ \nobreak \vskip\half \nobreak \@noafterindent
+}
+
+
+\def\LaTeX{La\TeX}
+\makeatother
+%%%%%%%%%%%%%%%%%%%%%% End of macros for guide %%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+\ifCUPmtplainloaded \else
+ \NewTextAlphabet{textbfit} {cmbxti10} {}
+ \NewTextAlphabet{textbfss} {cmssbx10} {}
+ \NewMathAlphabet{mathbfit} {cmbxti10} {} % for math mode
+ \NewMathAlphabet{mathbfss} {cmssbx10} {} % " " "
+ %
+ \ifAMStwofonts
+ %
+ \NewSymbolFont{upmath} {eurm10}
+ \NewSymbolFont{AMSa} {msam10}
+ \NewMathSymbol{\upi} {0}{upmath}{19}
+ \NewMathSymbol{\umu} {0}{upmath}{16}
+ \NewMathSymbol{\upartial}{0}{upmath}{40}
+ \NewMathSymbol{\leqslant}{3}{AMSa}{36}
+ \NewMathSymbol{\geqslant}{3}{AMSa}{3E}
+ \let\oldle=\le \let\oldleq=\leq
+ \let\oldge=\ge \let\oldgeq=\geq
+ \let\leq=\leqslant \let\le=\leqslant
+ \let\geq=\geqslant \let\ge=\geqslant
+ \else
+ \def\umu{\mu}
+ \def\upi{\pi}
+ \def\upartial{\partial}
+ \fi
+\fi
+
+% Marginal adjustments using \pageoffset maybe required when printing
+% proofs on a Laserprinter (this is usually not needed).
+% Syntax: \pageoffset{ +/- hor. offset}{ +/- vert. offset}
+% e.g. \pageoffset{-3pc}{-4pc}
+
+\pageoffset{-2.5pc}{0pc}
+
+\loadboldmathnames
+
+\begintopmatter % start the two spanning material
+
+\title{Monthly Notices of the Royal Astronomical Society:\hfil\break
+ plain \TeX\ style guide for authors}
+\author{M. A. Reed}
+\affiliation{Cambridge University Press, Shaftesbury Road,
+ Cambridge CB2 2BS}
+
+\shortauthor{M. A. Reed}
+\shorttitle{Monthly Notices: plain \TeX\ guide for authors}
+
+\acceptedline{Accepted 1993 December 11. Received 1993 March 17}
+
+\abstract {This guide is for authors who are preparing papers for the
+Monthly Notices of the Royal Astronomical Society using the
+Monthly Notices plain \TeX\ macros.}
+
+\keywords {Plain \TeX, {\tt mn.tex} -- sample text -- user guide.}
+\pagerange{1--13}%%
+\pubyear{1994}
+
+\maketitle
+
+% Start of main text
+
+\section{Introduction}
+
+In addition to the standard submission of hardcopy from authors,
+Monthly Notices accepts machine-readable forms of papers in \TeX.
+The layout design for Monthly Notices has been implemented as a
+\TeX\ format. This guide is not a substitute for the \TeX\ manual
+itself. Authors planning to submit their papers in \TeX\ are advised
+to use |mn.tex| as early as possible in the creation of their files.
+
+
+\subsection{The MN macros}
+
+MN is a set of plain \TeX\ macros for the Monthly Notices design,
+incorporating both the single- and double-column formats.
+MN.STY is the corresponding \LaTeX\ style file.
+The MN design package consists of the following files; do not edit these
+files in any way.
+\Half
+\hang{MN.TEX} {the macro definitions}
+\hang{MNGUIDE.TEX} {the input file for this guide}
+\hang{MNSAMPLE.TEX} {the input file for a sample article}
+\hang{MNLAND.TEX} {a landscape figure for use with the sample article}
+\hang{FONTTEST.TEX} {a file to test all of the fonts used in MN}
+\Half
+\noindent The input files for the guide, sample pages, landscape sample and
+fonttest automatically call in the MN macros if you haven't preloaded them
+by using a format file.
+Therefore, this guide can be typeset by typing: |tex MNGUIDE|, or
+|tex &mn MNGUIDE|.
+
+When your article is printed in the Monthly Notices journal, it is typeset
+in Monotype Times. As most authors do not have this font, it is likely that
+the make-up will change with the change of font. For this reason, we ask
+you to ignore details such as slightly long lines, page stretching, or
+figures falling out of synchronization, because these details can be dealt with at a later stage.
+
+
+\subsection{General style issues}
+
+For general style issues, authors are referred to the `Instructions for
+Authors' on the inside back cover of Monthly Notices. Authors who are
+interested in the details of style are referred to Butcher (1992) and
+The Chicago Manual (1982). The language of the journal is British
+English and spelling should conform to this.
+
+
+\subsection{Submission of \TeX\ articles to the journal}
+
+Authors are urged to state that electronic submission is intended when
+first submitting their paper. Papers should initially be submitted in the
+usual way to the Executive Secretary, Royal Astronomical Society, Burlington
+House, London W1V~0NL, as set out on the inside front cover of each issue
+of Monthly Notices. Three hard copies should be supplied. One of these
+copies should be single-sided and double-spaced throughout, while the other
+two should be weight-reduced, by being either single-spaced or double-sided.
+Note that articles, or revised versions thereof, may not be submitted by
+electronic mail. Appropriate gaps should be left for figures, original
+versions and copies of which should also be supplied. Authors should ensure
+that their figures are suitable (in terms of lettering, size, etc.) for the
+reduction they intend.
+
+Authors who wish to include PostScript artwork dir\-ectly into their
+articles can do so, by using either Tomas Rokicki's {\sf EPSF} macros
+or Trevor Darrell's {\sf PSFIG} macros (both of which are supplied with
+the DVIPS PostScript driver). Please remember to supply any additional
+figure macros you use with your article.
+Please also supply hard copies of your figures, for the use of production
+editors and as a back-up.
+Authors should not attempt to
+use implementation specific |\special|'s directly.
+
+The correct Monthly Notices House
+Style should be used -- details are given in the Instructions for Authors,
+in the Style Guide published in the 1~January 1993 issue (\hbox{MNRAS},
+260,~1), and in Appendix C of this guide.
+No disk should be submitted at this initial stage. When the paper has been
+accepted, the double-spaced copy will be marked up by the subeditors at
+Blackwell Science (BS) and returned to you for correction.
+When the requested corrections have been made, you should send the following
+material to BS:
+\beginlist
+\item (i) a 3.5-inch or 5.25-inch disk for PC (double or high density or
+Apple Mac), containing the {\em corrected\/} version of the paper; the file
+for the final version should be text-only, with no source-dependent control
+codes (i.e. an ASCII file);
+
+\item (ii) two hard copies of the corrected version, plus the original
+marked up copy of the article; {\em any further author corrections should
+be clearly indicated on the latter\/};
+
+\item (iii) a signed statement that the revised hard copy and the disk do
+indeed correspond.
+\endlist
+In addition, you should submit the following information concerning the disk
+and its contents:
+\beginlist
+\item (i) the disk format (e.g. PC 360k);
+
+\item (ii) how many files the disk contains, their names, a description of
+the file contents and the number of pages each file will produce when
+printed; details of any user-defined macros;
+
+\item (iii) the computer system and implementation of \TeX\ used (e.g.
+IBM~PC-386, PC\TeX~v3.14).
+\endlist
+Unless the layout of the paper has to be significantly changed by the
+typesetter (for example, if the gaps left for figures are not suitable), it
+will not be necessary to send you a typeset proof to check, as the paper
+will be set directly from your submitted disk. However, you should note
+that, if serious problems are encountered with the coding of your paper
+(missing author-defined macros, for example), it may prove necessary to
+divert the paper to conventional typesetting.
+
+
+\section{General instructions for installation}
+
+The simplest way to use this macro package is to copy the above files into a
+suitable directory or work area on your computer. Write your
+article using the macros described below (or use the sample article as a
+template) and ensure that the following is included at the very beginning of your input file:
+\beginlines
+|\ifx\mnmacrosloaded\undefined \input mn\fi|
+\endlines
+
+When you typeset your article using |tex <article file name>| the macro
+definitions will be loaded automatically before your text is processed.
+This will happen rather slowly on a small computer and you may find it much
+faster to work with the \TeX\ format file for the MN macros.
+This can be created by using the program INITEX:
+\beginlines
+|initex &plain mn|
+\endlines
+This usage of this command will vary from one installation of \TeX\ to
+another. In {\sc Unix} implementations of \TeX\ the `|&|' character must
+be `escaped' with a `|\|` because it is a magic character,
+e.g. |initex \&plain mn|.
+In PC\TeX\ you type the following (seek local advice if you
+are not sure how to use INITEX on your system):
+\beginlines
+|tex &plain mn /i|
+\endlines
+
+When the process is complete type |\dump| at the \TeX\ prompt.
+This creates the format file |MN.FMT|. Type the following command to
+typeset your article:
+\beginlines
+|tex &mn <article file name>|
+\endlines
+\TeX\ will process your article at high speed.
+
+
+\subsection{The font test and sample pages}
+
+Once you have installed the MN macros, run the following test. The file
+|FONTTEST.TEX| produces a sample of each font size used in the MN design.
+To use this do |tex FONTTEST| or |tex &mn FONTTEST| (after creating the
+|MN.FMT| format file).
+Preview the resulting |DVI| file on-screen and generate hard copy output on
+your facilities. It will show you whether any of the fonts selected by the
+Monthly Notices design are going to cause problems on your system.
+
+As a final test of the installation, typeset the sample article, using
+|tex MNSAMPLE| or |tex &mn MNSAMPLE|.
+Use this article in conjunction with the instructions in this guide to
+work out how to typeset an article for Monthly Notices.
+
+
+\subsubsection{Page margins}
+
+Some \TeX\ sites may find that pages from the MN design are positioned
+incorrectly on the paper from local laserprinters. This can be corrected by the
+use of the |\pageoffset| macro. It takes two parameters, the first being
+the horizontal offset, the second the vertical offset, e.g.
+\beginlines
+|\pageoffset{-1pc}{2pc}|
+\endlines
+The above example will shift the output one pica to the left, and two picas
+down the page. Usually there is no need to use this macro; only use it if
+required.
+
+
+\subsubsection{Author macro names}
+
+For efficiency, some authors may wish to write their own macros. Those who
+intend to do this will be aware of the problem of creating unique
+identifiers (macro names). The most common way around this problem has been
+to include |@| somewhere in the identifier, e.g. |\@utput| or |\sec@tion|.
+Knuth, the creator of \TeX, has adopted this method in the plain \TeX\
+definitions and it can also be found in other format packages such as
+\LaTeX.
+
+However, use of this method can cause problems if the internals of plain
+\TeX\ or the MN macros get `over-ridden'. There is a simpler method which is
+much safer. Simply prefix your macro names with your initials,
+e.g.\ |\MARmacro|.
+
+
+\section{The design macros}
+
+Refer to the source code of the sample pages for examples of the following
+design macros in use. It is very important that the article should end
+with a |\bye| as this typesets `This paper$\ldots$' at the very end.
+
+
+\subsection{Article opening}
+
+There are certain macros that should appear near the top of your input file.
+The following is the recommended way to begin your article.
+%
+\beginexhang{begintopmatter}
+\item{onecolumn} Selects single-column output (default = two-column).
+ The |\onecolumn| command {\em must\/} be used before |\begintopmatter|
+ for the article opening to work correctly.
+
+ You should not use |\onecolumn| unless your article has a high
+ mathematical content which won't fit into the two-column measure easily.
+ Selection of one-column output also affects the actions of other macros,
+ particularly those controlling figures and tables.
+
+\item {Referee} This selects referee mode (double spaced) if required
+ (default = not selected). Figure captions and Tables are not double
+ spaced by this option.
+
+\item {authorcomment} This creates a catchline at the bottom of the page
+ which authors may wish to use to keep track of the versions of their
+ article.
+
+\item {begintopmatter} This macro should be used just before defining the
+ article title and author names. If you omit this macro \TeX\ will
+ complain loudly when it reaches the |\maketitle| macro.
+
+\item {title} Set the article title, e.g.
+\beginlines
+|\title{Dust envelopes around RV Tauri stars}|
+\endlines
+
+\item {author} Set the article author(s), e.g.
+\beginlines
+|\author{A. V. Raveendran}|
+\endlines
+
+\item {affiliation} Set the author affiliation(s), e.g.
+\beginlines
+|\affiliation{Indian Institute of Astrophysics..}|
+\endlines
+Multiple author names should be set as follows. Do not use
+`\&' between names, always use `and'. Each author name is
+listed, followed by a reference mark (usually a superscripted
+number). The reference mark refers to each author's
+respective affiliations in a list which follows afterwards.
+For example,
+\beginlines
+\vbox{%
+|\author{A.~Moorhouse,$^{1,2}$|
+| P.~W.~J.~L.~Brand,$^1$|
+| T.~R.~Geballe$^3$ and M.~G.~Burton$^4$}|
+|\affiliation{$^1$ Department of Astronomy, ...}|
+|\affiliation{$^2$ Present address: Dublin|
+| Institute for ...}|
+|\affiliation{$^3$ Joint Astronomy Centre ...}|
+|\affiliation{$^4$ NASA Ames Research Center ...}|
+}%
+\endlines
+Note that the `present address' in
+the above example is treated as though it were an affiliation. Similarly,
+fellowships or other posts, for example `Visiting Observer, Mount John
+University Observatory \dots' should be listed in the acknowledgments.
+
+\item {shortauthor} Define the even-page running head.
+\beginlines
+|\shortauthor{R. A. Stathakis and E. M. Sadler}|
+\endlines
+Initials only should be used in running heads; use `and',
+not~`\&', to separate the final two names. When there is a
+long list of authors (four or more) use the form
+\beginlines
+|\shortauthor{D.~T.~Wickramasinghe et al.}|
+\endlines
+
+\item {shorttitle} Define the odd-page running head.
+\beginlines
+|\shorttitle{The H\,{\eightit I} spectra}|
+\endlines
+Notice the use of the |\,| (thinspace) after the `H' in the above example.
+The |\eightit| simulates the effect of an italic small-caps.
+If you require roman (upright) text in the short-title, say for `IRAS',
+you would use:
+\beginlines
+|\shorttitle{...{\rm IRAS}...}|
+\endlines
+It may also be necessary to add an italic correction |\/| before the |\rm|
+to improve the spacing.
+
+\item {abstract} Set the abstract information, e.g.
+\beginlines
+|\abstract {This is the text of the abstract ...}|
+\endlines
+This design macro requires that the text (which can be
+longer than one paragraph) is enclosed in braces.
+The abstract must fit on to the
+first page of the article when typeset.
+
+\item {keywords} Set any article key words, e.g.
+\beginlines
+|\keywords {circumstellar matter|
+| -- infrared: stars.}|
+\endlines
+The same applies for |\keywords| as for the |\abstract| macro.
+
+\item {maketitle} This macro must be used just before the first section
+ or the first text paragraph.
+\endexhang
+
+
+\subsection{Headings}
+
+Some headings are capitalized. Where this is true the design macro will
+automatically capitalize whatever you key. As a rule, it is advisable to
+capitalize the first letter, and any words that normally start with a capital,
+i.e. proper nouns, abbreviations, but key all other words in lower case.
+
+The |\section|, |\subsection| and |\subsubsection| mac\-ros are
+automatically numbered. To produce unnumbered headings, `star' forms of
+these macros exist, e.g. |\section*|.
+%
+\beginexhang{subsubsection}
+\item {section} Start a new section, e.g.
+\beginlines
+|\section{Introduction}|
+\endlines
+For main section headings such as `Acknowledgments' and
+`References' use the |\section*| macro, e.g.
+\beginlines
+|\section*{Acknowledgments}|
+\endlines
+The |\section| command is also used to produce appendices
+(see Subsection~3.11 for more information).%%
+
+\item {subsection} Start a new subsection, e.g.
+\beginlines
+|\subsection{Colour--colour diagram}|
+\endlines
+
+\item {subsubsection} Start a new subsubsection, e.g.
+\beginlines
+|\subsubsection{Correlation with subgroups}|
+\endlines
+
+\item {paragraph} Start a new subsubsubsection, e.g.
+\beginlines
+|\paragraph{Correlation with subgroups.} Text|
+| runs on after heading...|
+\endlines
+It is important to note that text runs on after a
+|\paragraph|. There should be no break between this heading
+and the next paragraph.
+\endexhang
+
+\noindent The macro |\section| forces the text of the heading into upper
+case, and |\subsection| emboldens the text. When headings contain names
+with lowercase or small capital letters, place these letters in the
+argument of |\lowercase|, e.g.
+\beginlines
+|N\lowercase{a}\,{\sixbf I}/%|
+|C\lowercase{a}\,{\sixbf II}|
+\endlines
+to get `\dots\ {\bf Na\,{\sixbf I}/Ca\,{\sixbf II}}\ \dots' in a section
+heading. The |\sixbf| commands produce a simulated bold small-caps.
+This technique can also be applied to the running heads; see the example in
+|\shorttitle|.
+
+The paragraph indent on any text following a |\section|, |\subsection|
+or |\subsubsection| is automatically removed by the macros.
+
+
+\subsection{Lists}
+\subsubsection{Numbered lists}
+
+Numbered lists are keyed in a simple and straightforward way. They begin
+with a |\beginlist| command. Each item is marked with |\item| with its
+number (in round braces) followed by the text for the item. The number
+should be in lower case roman numerals. The list is ended with |\endlist|.
+For example,
+\beginlines
+|\beginlist|
+|\item (i) the attenuated and diluted stellar|
+| radiation;|
+|\item (ii) scattered radiation, and|
+|\item (iii) reradiation from other grains.|
+|\endlist|
+\endlines
+
+\Notes
+
+\beginlist
+\item (i) Extra white space is automatically added above and below the list.
+\item (ii) Outside the scope of the |\beginlist| and |\endlist| commands the
+ |\item| command reverts to its plain \TeX\ definition. Don't use the
+ plain \TeX\ |\item| command on its own, as the spacing and indents will
+ be incorrect.
+\item (iii) The paragraph indentation on the first paragraph following the
+ |\endlist| command is removed automatically if you leave no blank
+ line between the |\endlist| and the text.
+\endlist
+
+
+\subsubsection{Unnumbered lists}
+
+These should be keyed in the same way as numbered lists (described above),
+except that each item in the list has no number in round braces.
+
+
+\subsection{Illustrations (or figures)}
+
+Figures should be keyed as follows:
+\beginlines
+|\beginfigure{|{\em n\/}|}|
+| \vskip 3cm|
+| \caption{{\bf Figure |{\it f}|.} An example figure in|
+| which space has been left for the artwork.}|
+|\endfigure|
+\endlines
+Figure captions should be below the figure itself, therefore
+the |\caption| command should appear after the figure or space
+left for an illustration.
+The {\em n\/} value is the logical figure number. This number determines
+the output order of the figure (in two-column mode).
+It must start at~1 and increase with each successive figure.
+\beginfigure{1}
+ \vskip 3cm
+ \caption{{\bf Figure 1.} An example figure in which space has been
+ left for the artwork.}
+\endfigure
+The |\caption| macro is only valid in the scope of
+|\beginfigure|$\ldots$|\endfigure|.
+
+The example above will produce a single-column figure in two-column mode.
+To produce a double-spanning figure use:
+\beginlines
+|\beginfigure*{|{\em n\/}|}|
+| |$\ldots$
+| \caption{|$\ldots$|}|
+|\endfigure|
+\endlines
+Notice that |\beginfigure*| ends with |\endfigure|. If the text in the
+caption is less than one line long it is centred automatically, otherwise
+it is set full-out.
+
+\Notes
+
+\beginlist
+\item (i) If there is more than one figure panel to a caption, the depth
+ value should increase by 13pt (4.5mm) for every extra figure (if they are
+ one above another). This allows for a gap between each figure panel.
+
+\item (ii) If a figure occupies one complete page, insert a depth that does
+ not completely fill the page, otherwise the figure may be output at the
+ end of the paper (or not at all)!
+\endlist
+
+See `Instructions for Authors' in Monthly Notices for submission of
+artwork.
+
+\subsubsection{Points to note for figures in one-column articles}
+
+\beginlist
+\item (i) All figures (and their captions) will be set to full width even
+ if they are keyed using |\beginfigure|$\ldots$|\endfigure|.
+ Captions shorter than one line will be centred as normal.
+
+\item (ii) The logical figure number is ignored in one-column mode.
+ Therefore the figures are output in the order in which they appear in
+ the source.
+
+\item (iii) If a figure is placed very early in the source code,
+ it is possible for it to float to the top of the first page
+ (above the title). In this case, move the figure one paragraph down and
+ try again. It may be necessary to do this with other figures to keep the
+ output order correct.
+\endlist
+
+
+\subsection{Tables}
+
+Tables should be keyed something like this:
+\beginlines
+|\begintable{|{\em n\/}|}|
+| \caption{{\bf Table |{\em t\/}|.} |$\ldots$|}|
+| \halign{| $<$alignment$>$ |}|
+| \tabletext{| text below table, table footnotes, etc. |}|
+|\endtable|
+\endlines
+The {\em n\/} value is the logical table number, and {\em t\/} is the
+table number. The logical table number determines the output order of the
+table (in two-column mode).
+It must start at~1 and increase with each successive table.
+
+The table caption should appear before the body of the table.
+The |\tabletext| macro is provided for table notes, and table footnotes.
+It can contain more than one paragraph of text. Ten points of space are
+automatically added above |\tabletext|. Only one |\tabletext| is allowed
+per table. The usage of |\tabletext| is optional.
+
+If you wish to insert non-aligned text into the body of the alignment do
+not use |\noalign{|{\em text\/}|}| as this will make the table appear to
+be full width to the macros, resulting in the table being set flush left.
+In this case you can either use |\multispan| or use
+|\noalign{\hbox{|{\em text\/}|}}|.
+
+The caption, and any text below the table will be set to the table
+width, when the table is centred by the macros.
+The |\caption| and |\tabletext| macros are only valid in the scope of the
+|\begintable|$\ldots$|\endtable|.
+
+Table~1 is produced with the following code:
+\beginlines
+|\begintable{1}|
+| \caption{{\bf Table 1.} Radio-band beaming|
+| model parameters for FSRQs and BL Lacs.}|
+| \halign{#\hfil & \quad \hfil#\hfil\quad &|
+| \hfil#\hfil\quad & \hfil#\hfil\quad &|
+| \hfil#\hfil\quad & \hfil#\hfil\quad &|
+| \hfil#\hfil\cr|
+| Class & $\gamma_1$ & $\gamma_2$ & $\langle|
+| \gamma \rangle$ & $G$ & $f$|
+| & $\theta_{\rm c}$ \cr|
+| BL Lacs & 5 & 36 & 7 & $-4.0$ & $1.0\times|
+| 10^{-2}$ & 10$^\circ$ \cr|
+| FSRQs & 5 & 40 & 11 & $-2.3$ & $0.5\times|
+| 10^{-2}$ & 14$^\circ$ \cr|
+| }|
+| \tabletext{{\em G} is the slope of the Lorentz|
+| factor distribution, i.e. $n(\gamma)\propto|
+| \gamma^G$, extending between $\gamma_1$|
+| and $\gamma_2$, with mean value $\langle|
+| \gamma\rangle$, {\em f\/} is the ratio|
+| between the intrinsic jet luminosity and the|
+| extended, unbeamed luminosity, while|
+| $\theta_{{\rm c}}$ is the critical angle|
+| separating the beamed class from the parent|
+| population.}|
+|\endtable|
+\endlines
+
+\begintable{1}
+ \caption{{\bf Table 1.} Radio-band beaming model parameters
+ for FSRQs and BL Lacs.}
+ \halign{#\hfil&\quad \hfil#\hfil\quad& \hfil#\hfil\quad&
+ \hfil#\hfil\quad& \hfil#\hfil\quad& \hfil#\hfil\quad&
+ \hfil#\hfil\cr
+ Class & $\gamma_1$ & $\gamma_2$ & $\langle \gamma \rangle$ & $G$ & $f$
+ & $\theta_{\rm c}$ \cr
+ BL Lacs & 5 & 36 & 7 & $-4.0$ & $1.0\times 10^{-2}$ & 10$^\circ$ \cr
+ FSRQs & 5 & 40 & 11 & $-2.3$ & $0.5\times 10^{-2}$ & 14$^\circ$ \cr
+ }
+ \tabletext{{\em G} is the slope of the Lorentz factor distribution, i.e.
+ $n(\gamma)\propto \gamma ^G$, extending between $\gamma _1$ and
+ $\gamma_2$, with mean value $\langle \gamma \rangle$, {\em f\/} is the
+ ratio between the intrinsic jet luminosity and the extended, unbeamed
+ luminosity, while $\theta_{{\rm c}}$ is the critical angle separating
+ the beamed class from the parent population.}
+\endtable
+
+\noindent The example above will produce a single-column table in two-column
+mode. To produce a double-spanning table use:
+\beginlines
+|\begintable*{|{\em n\/}|}|
+| \caption{|$\ldots$|}|
+| \halign{|$\ldots$|}|
+| \tabletext{|$\ldots$|}|
+|\endtable|
+\endlines
+Notice that |\begintable*| ends with |\endtable|.
+
+Tables are allowed to have single horizontal rules, at the head
+and foot only. Horizontal rules should have 3pt of space above and below
+them. Vertical rules should not be used.
+
+If a table occupies one complete page, you may find it necessary to reduce
+its depth slightly, so that it doesn't completely fill the page, otherwise
+the table may be output at the end of the paper (or not at all)!
+
+
+\subsubsection{Points to note for tables in one-column articles}
+
+\beginlist
+\item (i) Tables that will fit into a column in two-column mode will be
+ centred on the full page width in one-column mode.
+
+\item (ii) The logical table number is ignored in two-column mode.
+ Therefore the tables are output in the order in which they appear in
+ the source.
+
+\item (iii) If a table is placed very early in the source code,
+ it is possible for it to float to the top of the first page
+ (above the title). In this case, move the table one paragraph down and
+ try again. It may be necessary to do this with other tables to keep the
+ output order correct.
+\endlist
+
+
+\subsection{Captions for continued figures and tables}
+
+If a very large figure or table does not fit on one page,
+it must be split into two floats; the second float should use a
+continued caption in the form:
+\smallskip
+\centerline{{\bf Figure 6} -- {\it continued}}
+\smallskip
+\noindent The figure or table number in the continued caption should be
+the same as in the original caption. These captions should be keyed as
+follows:
+\beginlines
+|\begintable{|{\it n\/}|}|
+| \caption{{\bf Table |{\it t\/}|} -- {\it continued}}|
+| :|
+|\endtable|
+\endlines
+Notice that there is no full-point after the figure/table number.
+
+
+\subsection{Landscape pages}
+
+If a table or illustration is too wide to fit the standard measure, it
+must be turned, with its caption, through 90 degrees anticlockwise.
+Landscape illustrations and/or tables cannot be produced directly
+using the MN macros because \TeX\ itself cannot turn the
+page, and not all device drivers provide such a facility.
+
+The first step is to produce blank pages (with a running head) in the
+output, so that the landscape material can be pasted in later. How
+this is done depends on whether your article is in one or two columns.
+
+For one-column articles use the following:
+\beginlines
+|\pageinsert|
+| \vfil\centerline{{\bf Figure |{\em f\/}|.} Landscape|
+| figure to go here.}\vfil|
+|\endinsert|
+\endlines
+otherwise use
+\beginlines
+|\beginfigure*{|{\em n\/}|}|
+| \vbox to 646pt{\vfil \caption{{\bf Figure |{\em f\/}|.}|
+| Landscape figure to go here.}\vfil}|
+|\endfigure|
+\endlines
+for two-column articles. You may find it necessary to move the above code
+up or down the source code until the blank page appears on the page after
+the first reference.
+
+Next create a separate document containing the command |\landscape| near
+the top (or use |mnland.tex| as a template).
+In this file include the complete tables and illustrations (with captions)
+using the figure and table macros provided, remembering to number the
+captions in the correct sequence, e.g.
+\ifCUPmtplainloaded \else \eject\fi %%
+\beginlines
+|\ifx\mnmacrosloaded\undefined \input mn\fi|
+\smallskip
+|% use the following if your driver supports it|
+|% \special{landscape}|
+\smallskip
+|% you may require \pageoffset for landscape|
+|% \pageoffset{0pc}{-1.5pc}|
+\smallskip
+|\landscape|
+|\authorcomment{Landscape material to be pasted|
+| into the article.}|
+\smallskip
+|\begintopmatter|
+|\maketitle|
+\smallskip
+|\beginfigure{1}|
+|\caption{{\bf Figure 4.} Photometric|
+| comparisons |$\ldots$|}|
+|\endfigure|
+\smallskip
+|:|
+\smallskip
+|\bye|
+\endlines
+Once you have successfully processed the new file with the MN macros, you
+can pass the resulting output through your dvi printer driver. Because the
+output of the MN macros is wider than it is deep, the page has to be printed
+landscape on your output device.
+
+Some dvi printer drivers will understand the `landscape' |\special| command
+and will automatically rotate the output, while others need to be told from
+the command line. Consult your local documentation if you don't know how to
+do this.
+
+
+\subsection{Plate pages}
+
+These are provided for tip-in plates, and should only be used for
+these. The plate page macros create a blank page with a special running
+head; its contents can be set using the |\plate| command. The text in the
+head should be keyed as shown below. The {\em no\/} and {\em vol\/}
+numbers will be determined by the typesetter.
+\beginlines
+|\beginplatepage|
+| \plate{Opposite p.~|{\em no\/}|, MNRAS, {\bf |{\em vol\/}|}}|
+| \caption{{\bf Figure |{\em f\/}|.} |$\ldots$|}|
+|\endplatepage|
+\endlines
+If the plate is a `landscape' plate its caption (if any) should be set
+using a separate `landscape' file (as described above). If the plate is
+to be placed `portrait' its caption can be set by using the |\caption|
+command as shown above. The style of the caption should be the same as for
+normal figure captions. If the plate fills most of the page, it is advisable
+to place the caption at the very bottom of the page -- this can be achieved
+by using |\vfill| above the caption.
+
+Plate pages will always appear on the page following the one on which the
+|\endplatepage| command is encountered. At present it is impossible to have
+two plate pages side by side, since there must be at least one page between
+them. If a new plate page is started before a previous one is output the
+first plate page is lost.
+
+
+\subsection{Footnotes}
+
+Footnotes are only available in the one-column format. They should be
+keyed in the standard plain \TeX\ way using |\footnote|, e.g.
+\beginlines
+|text\footnote {|{\em symbol\/}|}{|{\em footnote text}$\ldots$|} text|
+\endlines
+where {\em symbol\/} should be in the sequence:
+$\star$ (|\star|), \dag, \ddag, \S, \P, $\|$, $\star\star$ (|\star\star|),
+\dag\dag, \ddag\ddag, \S\S, \P\P, $\|\|$.
+The |\footnote| command should only be used for footnotes in the main text.
+
+
+\subsection{Bibliography}
+
+References to published literature should be quoted in text by author
+and date: e.g.\ Draine (1978) or (Begelman, Blandford \& Rees 1984).
+Where more than one reference is cited having the same author(s) and date,
+the letters a,b,c, $\ldots$ should follow the date: e.g.\ Smith (1988a),
+Smith (1988b), etc.
+
+
+\subsubsection{References in the text}
+
+References in the text are given by author and date, and, whichever
+method is used to produce the bibliography, the references in the text
+are done in the same way.
+When you introduce a three-author paper, you should list all
+three authors at the first citation, and thereafter use et al.
+
+\subsubsection{The list of references}
+
+The following listing shows how references should be keyed in the style of
+the journal.
+\beginlines
+|\section*{References}|
+\smallskip
+|\beginrefs|
+|\bibitem Butcher J., 1992, Copy-editing:|
+| The Cambridge Handbook, 3rd edn.|
+| Cambridge Univ. Press, Cambridge|
+|\bibitem The Chicago Manual of Style, 1982.|
+| Univ. Chicago Press, Chicago|
+|\bibitem Blanco P., 1991, PhD thesis,|
+| Edinburgh University|
+|\bibitem Brown A. B., Jones C. D., 1989,|
+| in Robinson E. F., Smith G. H., eds,|
+| Proc. IAU Symp. 345, Black Dwarfs.|
+| Kluwer, Dordrecht, p. 210|
+|\bibitem Edelson R. A., 1987, ApJ, 313, 651|
+|\bibitem Lamport L., 1986, \LaTeX: A Document|
+| Preparation System. Addison--Wesley,|
+| New York|
+|\bibitem Mirabel I. F., Sanders D. B., 1989,|
+| ApJ, 340, L53|
+|\bibitem Misner C. W., Thorne K. S.,|
+| Wheeler J. A., 1973, Gravitation.|
+| Freeman, San Francisco|
+|\bibitem Sopp H. M., Alexander P., 1991,|
+| MNRAS, 251, 112|
+|\bibitem Stella L., Campana S., 1991, in|
+| Treves A., Perola G. C., Stella L., eds,|
+| Iron Line Diagnostic in X-ray Sources.|
+| Springer--Verlag, Berlin, p. 230|
+|\endrefs|
+\endlines
+The following rules apply for the ordering of your references:
+\beginlist
+\item (i) if an author has written several papers, some with other authors,
+ the rule is that the single-author papers precede the two-author
+ papers, which, in turn, precede the multi-author papers;
+\item (ii) within the two-author paper citations, the order is determined
+ by the second author's surname, regardless of date;
+\item (iii) within the multi-author paper citations, the order is
+ chronological, regardless of author surnames.
+\endlist
+
+\Notes
+
+\beginlist
+\item (i) The |\bibitem| command is undefined unless it is used in the
+ scope of the |\beginrefs|$\ldots$|\endrefs|.
+\item (ii) Bibliographical items can be longer than one paragraph.
+\item (iii) The paragraph indentation on the first paragraph following the
+ |\endrefs| command is removed automatically if you leave no blank
+ line between the |\endrefs| and the text.
+\endlist
+
+
+\subsection{Appendices}
+
+The appendices section of your article should start with a |\appendix|,
+after which each |\section| starts a new appendix. For example,
+\beginlines
+|\appendix|
+|\section{for authors}|
+\endlines
+will yield:\par
+\smallskip
+\centerline{\bf APPENDIX A:\enskip FOR AUTHORS}\par
+\smallskip
+\noindent The |\appendix| macro should only be used once.
+
+If the appendix has no subtitle, the parameter to the |\section| command
+should be left empty. For example,
+\beginlines
+|\section{}|
+\endlines
+will produce:\par
+\smallskip
+\centerline{\bf APPENDIX B}\par
+\smallskip
+\noindent Any subsections or subsubsections in the appendix are
+automatically numbered.
+You should also note that displayed equations in appendices should be
+numbered (A1), (A2) for Appendix A, and (B1), (B2) for Appendix B, etc.
+
+The numbering for displayed equations can be made automatic by using the
+|\stepeq| macros described in Subsubsection~3.13.2.%%
+
+Figures and Tables should also be numbered in a similar way,
+e.g. Fig. A1, A2, Table A1, A2 in appendices.
+
+
+\subsection{Typeface selection}
+
+The normal plain \TeX\ typeface conventions apply. The following faces
+are available as normal: |\rm|, |\it|, |\bf|, |\sl|, |\sf|, |\sc|,
+|\tt|, |\mit|, |\cal| and |\oldstyle|.
+
+Bold versions of |\cal| and |\oldstyle| can be produced in
+combination with |\bmath|. Use of |\bmath| on its own will provide bold
+math italic letters.
+
+A new |\em| command provides {\em emphasis\/} for important words.
+The |\em| command will automatically switch the face of the emphasized
+words to make them stand out. So,
+\beginlines
+|\rm this is an {\em emphasized\/} word.|
+|\it this is an {\em emphasized} word.|
+\endlines
+gives\par
+\centerline{\rm this is an {\em emphasized\/} word.}
+\centerline{\it this is an {\em emphasized\/} word.}
+\Half
+\noindent Notice the use of the italic correction command (|\/|) in the
+above example.
+
+The following are fully loaded in text, script and scriptscript sizes:
+|\rm|, |\bf|, math italic, math symbol, bold math italic and bold symbol.
+The faces |\it|, |\sl|, |\tt|, |\sc| and |\sf| are loaded at text size only.
+See |fonttest.tex| for a better idea of how these work.
+
+
+\subsection{Typesetting mathematics}
+\subsubsection{Displayed mathematics}
+
+Equations should be keyed using normal plain \TeX\ macros.
+Display mathematics are automatically set flush left by the macros.
+The standard plain \TeX\ math commands |\eqalign|, |\eqalignno| will
+work as before. The |\leqalignno| command is switched automatically
+to |\eqalignno| to prevent the equation number from crashing into the
+equation. If you wish to use |\displaylines|, this has to be handled
+in a slightly different way. For example,
+$$
+\displaylines{%
+ \hbox to \hsize{}\cr
+ [\nu_1]-[\nu_2]=-2.5\log [f(\nu_1)/f(\nu_2)],\hfill\stepeq\cr
+ \alpha=-(1+Q)\beta-3,\hfill\stepeq\cr
+ q=2+\gamma -Q.\hfill\stepeq\cr}
+$$
+was produced with:
+\beginlines
+|$$|
+|\displaylines{%|
+| \hbox to \hsize{}\cr|
+| [\nu_1]-[\nu_2]=-2.5\log [f(\nu_1)/f(\nu_2)],|
+| \hfill\stepeq\cr|
+| \alpha=-(1+Q)\beta-3,\hfill\stepeq\cr|
+| q=2+\gamma -Q.\hfill\stepeq\cr}|
+|$$|
+\endlines
+Notice the |\hbox to \hsize{}| to ensure that the equation is set to the
+full width. The |\hfill|'s ensure that the equations are set flush left
+and the equation numbers are set flush right.
+
+If the equations in |\displaylines| are unnumbered, you still need the
+|\hfill|'s to ensure the equations are set flush left.
+
+
+\subsubsection{Automatic equation numbering}
+
+Displayed equations can be numbered automatically by the use of |\stepeq|.
+For example,
+\beginlines
+|$$|
+| \alpha=-(1+Q)\beta-3,\eqno\stepeq|
+|$$|
+\endlines
+which produces:
+$$
+\alpha=-(1+Q)\beta-3,\eqno\stepeq
+$$
+The |\stepeq| macro can be used in any of the places where a equation
+number is normally expected. Sub-equation numbering is also provided,
+allowing equation numbers in the form (2a) to be produced. For example,
+$$
+\eqalignno{%
+ \alpha & =-(1+Q)\beta-3, & \startsubeq\cr
+ q & =2+\gamma -Q. & \stepsubeq\cr
+ [\nu_1]-[\nu_2] & =-2.5\log [f(\nu_1)/f(\nu_2)] & \stepsubeq\cr}
+$$
+was produced by:
+\ifCUPmtplainloaded \else \eject\fi %%
+\beginlines
+|$$|
+|\eqalignno{%|
+| \alpha & =-(1+Q)\beta-3, & \startsubeq\cr|
+| q & =2+\gamma -Q. & \stepsubeq\cr|
+| [\nu_1]-[\nu_2] & =-2.5\log [f(\nu_1)/f(\nu_2)]|
+| & \stepsubeq\cr}|
+|$$|
+\endlines
+The sub-equation number is reset each time a |\stepeq| is used. Equation
+numbering is automatically reset to `(A1)' when a |\appendix| is used.
+
+
+\subsubsection{Bold math italic}
+
+To obtain bold math italic, you should use |\bmath|.
+So to obtain:
+$$
+ d(\bmath{s_{t_u}}) = \langle [RM(\bmath{X_y}
+ + \bmath{s_t}) - RM(\bmath{x_y})]^2 \rangle
+$$
+you would key:
+\beginlines
+|$$|
+| d(\bmath{s_{t_u}}) = \langle [RM(\bmath{X_y}|
+| + \bmath{s_t}) - RM(\bmath{x_y})]^2 \rangle|
+|$$|
+\endlines
+This facility is available in all typesizes.
+
+
+\subsubsection{Bold Greek and other bold symbols}
+
+Bold lowercase Greek characters can be obtained by prefixing
+the normal (unbold) symbol name with a `b', e.g.\ |\bgamma| gives $\bgamma$.
+This rule does not apply to bold |\eta|, as this would lead to a name
+clash with |\beta|. Instead use |\boldeta| for bold eta. Note that there
+is no |\omicron| (so there is no |\bomicron|), just use `o' in math mode
+for omicron and `|\bmath{o}|' for bold omicron.
+
+Bold versions of most of the other symbols in appendix~F in the \TeX book
+can be obtained in the same way.
+
+For bold uppercase Greek, prefix the unbold character name with |\bf|,
+e.g.\ |\bf\Gamma| gives $\bf\Gamma$.
+Upper and lowercase Greek characters are available in all typesizes.
+
+You can then use these definitions in math mode, as you would normal Greek
+characters:
+%
+\beginlines
+|$$|
+| \balpha_{\bmu} = {\bf\Theta} \alpha.|
+|$$|
+\endlines
+%
+will produce
+%
+$$
+ \balpha_{\bmu} = {\bf\Theta} \alpha.
+$$
+To save \TeX's valuable memory the symbol names for the bold math
+characters are not loaded automatically. To load them simply type
+\beginlines
+| \loadboldmathnames|
+\endlines
+in the document. Alternatively, if you only need one or two of them,
+simply copy the appropriate definitions from |mn.tex|
+to your document. For a complete list of the bold math symbols
+supplied, see the file |mn.tex|.
+
+
+\subsubsection{Upright Greek characters}
+
+You can obtain upright Greek characters if you have access to the
+American Maths Society Euler fonts (version 2.0), but you may not
+have these. In this case, you will have to use the normal math italic
+symbols and the typesetter will substitute the corresponding upright
+characters. You will make this easier if you can use the macros |\upi|,
+|\umu| and |\upartial| etc.\ in your text to indicate the need for upright
+characters, together with the following definitions in the preamble
+(before |\begintopmatter|):
+
+\subsubsection*{Authors with AMS fonts}
+
+\beginlines
+|\ifCUPmtplainloaded \else|
+| \NewSymbolFont{upmath} {eurm10}|
+| \NewMathSymbol{\upi} {0}{upmath}{19}|
+| \NewMathSymbol{\umu} {0}{upmath}{16}|
+| \NewMathSymbol{\upartial}{0}{upmath}{40}|
+|\fi|
+\endlines
+
+\subsubsection*{Authors without AMS fonts}
+
+\beginlines
+|\ifCUPmtplainloaded \else|
+| \def\umu{\mu}|
+| \def\upi{\pi}|
+| \def\upartial{\partial}|
+|\fi|
+\endlines
+Wether you have AMS fonts or not, the |\if..| and |\fi| are required in the
+above examples to ensure that when your article is typeset in Monotype
+Times, the correct definitions for these symbols are used.
+
+The sample pages, guide and fonttest can be made to use AMS fonts if you
+have them. To use them, just uncomment the following line in the preamble
+of |mnguide.tex|, |mnsample.tex| and |fonttest.tex|:
+%
+\beginlines
+|%\AMStwofontstrue|
+\endlines
+%
+If you do this, the following upright symbols are used in the
+sample pages, guide and fonttest: |\upi|, |\umu| and |\upartial|.
+
+
+\subsubsection{Special symbols}
+
+The macros for the special symbols in Tables~2 and~3 have been taken from
+the Springer Verlag `Astronomy and Astrophysics' design, with their
+permission. They are directly compatible and use the same macro names.
+These symbols will work in all text sizes, but are only guaranteed to work
+in text and displaystyles. Some of the symbols will not get any smaller
+when they are used in sub- or superscripts, and will therefore be displayed
+at the wrong size. Don't worry about this as the typesetter will be able to
+sort it out.
+%
+\begintable*{2}
+\caption{{\bf Table 2.} Special symbols which can only be used in
+math mode.}
+\advance\baselineskip by 2pt
+\halign{#\hfil\quad&#\hfil\quad&#\hfil\qquad\qquad
+ &#\hfil\quad&#\hfil\quad&#\hfil\cr
+Input & Explanation & Output & Input & Explanation & Output\cr
+\noalign{\vskip 3pt\hrule\vskip 3pt}
+|\la| & less or approx & $\la$ &
+ |\ga| & greater or approx & $\ga$\cr
+|\getsto| & gets over to & $\getsto$ &
+ |\cor| & corresponds to & $\cor$\cr
+|\lid| & less or equal & $\lid$ &
+ |\gid| & greater or equal & $\gid$\cr
+|\sol| & similar over less & $\sol$ &
+ |\sog| & similar over greater & $\sog$\cr
+|\lse| & less over simeq & $\lse$ &
+ |\gse| & greater over simeq & $\gse$\cr
+|\grole| & greater over less & $\grole$ &
+ |\leogr| & less over greater & $\leogr$\cr
+|\loa| & less over approx & $\loa$ &
+ |\goa| & greater over approx & $\goa$\cr
+|\bbbr| & Blackboard bold R & $\bbbr$ &
+ |\bbbm| & Blackboard bold M & $\bbbm$ \cr
+|\bbbn| & Blackboard bold N & $\bbbn$ &
+ |\bbbf| & Blackboard bold F & $\bbbf$ \cr
+|\bbbh| & Blackboard bold H & $\bbbh$ &
+ |\bbbk| & Blackboard bold K & $\bbbk$ \cr
+|\bbbp| & Blackboard bold P & $\bbbp$ &
+ |\bbbone| & Blackboard bold 1 & $\bbbone$ \cr
+|\bbbc| & Blackboard bold C & $\bbbc$ &
+ |\bbbq| & Blackboard bold Q & $\bbbq$ \cr
+|\bbbt| & Blackboard bold T & $\bbbt$ &
+ |\bbbs| & Blackboard bold S & $\bbbs$ \cr
+|\bbbz| & Blackboard bold Z & $\bbbz$ \cr
+%
+\noalign{\vskip 3pt\hrule}
+}
+\endtable
+
+\begintable*{3}
+\caption{{\bf Table 3.} Special symbols which don't have to be
+used in math mode.}
+\advance\baselineskip by 2pt
+\halign{#\hfil\quad&#\hfil\quad&#\hfil\qquad\qquad
+ &#\hfil\quad&#\hfil\quad&#\hfil\cr
+Input & Explanation & Output & Input & Explanation & Output\cr
+\noalign{\vskip 3pt\hrule\vskip 3pt}
+|\sun| & sun symbol & $\sun$ &
+ |\degr| & degree & $\degr$\cr
+|\diameter| & diameter & \diameter &
+ |\sq| & square & $\sq$\cr
+|\fd| & fraction of day & \fd &
+ |\fh| & fraction of hour & \fh\cr
+|\fm| & fraction of minute & \fm &
+ |\fs| & fraction of second & \fs\cr
+|\fdg| & fraction of degree & \fdg &
+ |\fp| & fraction of period & \fp\cr
+|\farcs| & fraction of arcsecond & \farcs &
+ |\farcm| & fraction of arcmin & \farcm\cr
+|\arcsec| & arcsecond & \arcsec &
+ |\arcmin| & arcminute & \arcmin\cr
+\noalign{\vskip 3pt\hrule}
+}
+\endtable
+
+\ifCUPmtplainloaded
+\subsubsection{Extra features in the Monotype Times version}
+
+This section of the guide will only be included if the guide is \TeX ed
+with the Times version of the MN macros (mtmn.tex). The following features
+are only available in the Times version:
+\beginlist
+\item (i) All of the type sizes available are fully loaded.
+\item (ii) Most of the symbols in Table~2 will be substituted
+ with symbols from the |mtxm| font. Only |\sq| is substituted in Table~3.
+\item (iii) All of the symbols in the |mtxm| and |mtym| fonts can be used,
+ at any size (using the normal AMS names).
+ If the author has used |mssymb.tex| then this can be removed, as most
+ of this file is now included in MN. If the author has used the new AMS
+ symbol fonts |msam| and |msbm| -- check the log file for missing
+ characters (once you've removed |msam| and |msbm|).
+ You have to do this because |msam| and |msbm| contain a few extra
+ characters NOT in |mtxm| and |mtym|. If you find missing characters get
+ help!
+\item (iv) Uppercase blackboard bold is available in all sizes. e.g.
+ \beginlines
+ |$\Bbb{A}\ldots\Bbb{Z}$|\qquad gives\qquad $\Bbb{A}\ldots\Bbb{Z}$
+ \endlines
+ If the author has made-up their own uppercase blackboard bold characters
+ you can safely use |\Bbb| instead.
+\item (v) If the author has used the simulated Blackboard bold symbols
+ these are automatically substituted for the real characters, except for
+ |\bbbone| which is redefined to work better with Times fonts.
+\endlist
+\fi
+
+\section{Example of section heading with
+ S{\sevenbf MALL} C{\sevenbf APS},
+ \lowercase{lowercase}, \textbfit{italic}, and bold
+ Greek such as $\bmu^{\bkappa}$}
+
+The above heading was produced with:
+\beginlines
+|\section{Example of section heading with|
+| S{\sevenbf MALL} C{\sevenbf APS},|
+| \lowercase{lowercase}, \textbfit{italic},|
+| and bold Greek such as $\bmu^{\bkappa}$}|
+\endlines
+
+\appendix
+\section{for authors}
+
+Table~A1 is a list of design macros which are unique to |mn.tex|. The list
+displays each macro's name and description.
+%
+\begintable*{4}
+\caption{{\bf Table A1.} Authors' notes.}
+\vbox to 630pt{%
+\halign{#\hfil&\quad #\hfil\cr
+Macro name and syntax & Description\cr
+\noalign{\vskip 3pt\hrule\vskip 3pt}
+|\pageoffset {h-off}{v-off}| & Adjust positioning of text area on paper.\cr
+|\Referee| & Enable double-spaced referee mode.\cr
+|\onecolumn| & Enable one-column mode (default =
+ two-column).\cr
+|\landscape| & Enable landscape mode (default = portrait).\cr
+ & The |\landscape| command automatically calls |\onecolumn|.\cr
+|\loadboldmathnames| & Enable the use of bold symbols, e.g. |\bgamma|\cr
+|\authorcomment| & Catchline for draft version/date.\cr
+\noalign{\Half}
+|\begintopmatter| & Start the two-spanning topmatter.\cr
+|\title {<text>}| & Article title.\cr
+|\author {<text>}| & Author(s).\cr
+|\affiliation {<text>}| & Author affiliation(s).\cr
+|\shortauthor {<text>}| & Set the even-page running head.\cr
+|\shorttitle {<text>}| & Set the odd-page running head.\cr
+|\abstract {<text>}| & Abstract.\cr
+|\keywords {<text>}| & Key words.\cr
+|\maketitle| & End the two-spanning topmatter.\cr
+\noalign{\Half}
+|\section {<text>}| & Heading level A.\cr
+|\section* {<text>}| & Unnumbered A-heading.\cr
+|\subsection {<text>}| & Heading level B.\cr
+|\subsubsection {<text>}| & Heading level C.\cr
+|\paragraph {<text>}| & Heading level D.\cr
+|\appendix| & Start the articles appendix section.
+ The |\section| command starts\cr
+ & a new appendix.\cr
+\noalign{\Half}
+|\stepeq|, |\startsubeq|, |\stepsubeq| & Automatic equation numbering.\cr
+\noalign{\Half}
+|\beginlist| & Numbered list:\cr
+| \item (i) <text>| & Omit the number and round braces from
+ each |\item| for an unnumbered list.\cr
+| \item (ii) <text>|\cr
+\noalign{\vskip-.25\baselineskip}
+| |$\ldots$\cr
+\noalign{\vskip-.2\baselineskip}
+|\endlist|\cr
+\noalign{\Half}
+|\beginrefs| & Bibliography.\cr
+| \bibitem <text>|\cr
+\noalign{\vskip-.25\baselineskip}
+| |$\ldots$\cr
+\noalign{\vskip-.2\baselineskip}
+|\endrefs|\cr
+\noalign{\Half}
+|\beginfigure{n}| & Figures:\cr
+| <figure space>| & Use the |\beginfigure*| form for a
+ double-spanning figure\cr
+| \caption{{\bf Figure n.} caption}| & in two-column mode.\cr
+|\endfigure|\cr
+\noalign{\Half}
+|\begintable{n}| & Tables:\cr
+| \caption{{\bf Table n.} caption}|
+ & Use the |\begintable*| form for a double-spanning table\cr
+| <alignment>| & in two-column mode.\cr
+| \tabletext{<text>}|\cr
+|\endtable|\cr
+\noalign{\Half}
+|\caption{{\bf Figure n} -- {\it continued}}| & Continued captions.\cr
+|\caption{{\bf Table n} -- {\it continued}}|\cr
+\noalign{\Half}
+|\beginplatepage| & Plate pages.\cr
+| \plate{Opposite p.\ n, MNRAS, {\bf n}}|\cr
+| <figure space>|\cr
+| \caption{{\bf Figure n.} caption}|\cr
+|\endplatepage|\cr
+\noalign{\Half}
+|\Two, \OneHalf, \One, \Half| & Extra vertical space: These macros insert
+ white space, in multiples\cr
+ & of the linefeed, between paragraphs. Use during page make-up in \cr
+ & preference to plain \TeX's |\smallskip|, |\medskip| and |\bigskip|.\cr
+\noalign{\Half}
+|\bmath{math text}|, |\em| & Bold math and emphasized text.\cr
+|\textbfit{text}|, |\mathbfit{text}| & Bold text italic (defined in
+ the preamble of |mnsample.tex|).\cr
+|\textbfss{text}|, |\mathbfss{text}|& Bold text sans serif (defined in
+ the preamble of |mnsample.tex|).\cr
+|\umu|, |\upi|, |\upartial| & Upright math characters. These will only
+ appear upright if you have\cr
+ & AMS v2.0 fonts. See ``upright greek
+ characters" for further information.\cr
+\noalign{\vskip 3pt\hrule\vskip 3pt}
+}}
+\endtable
+
+
+\section{for editors}
+
+The additional features shown in Table~B1 may be used for production
+purposes only.
+%
+\begintable*{5}
+\caption{{\bf Table B1.} Editors' notes.}
+\halign{#\hfil&\quad #\hfil\cr
+Macro name and syntax & Description\cr
+\noalign{\vskip 3pt\hrule\vskip 3pt}
+|\pageno=000| & to set pagination; default = 1.\cr
+|\pagerange{000--000}| & note the use of the en-rule\cr
+|\letters| & for short communications (adds L to folios)\cr
+|\pagerange{L00--L00}| & for short communications\cr
+|\microfiche{MN000/0}| & for articles accompanied by microfiche\cr
+|\pubyear{0000}| & catchline date\cr
+|\volume{000}| & catchline volume\cr
+|\acceptedline{text}| & acceptance date\cr
+|\nofloat| & Position a figure or table at the current position
+ (one-column only).\cr
+ & The |\nofloat| macro should be positioned directly after the\cr
+ & |\beginfigure|/|table|, and will cause the macros to use |\midinsert|\cr
+ & (remember that |\midinsert| will turn into a |\topinsert| if there\cr
+ & is not enough space).\cr
+\noalign{\vskip 3pt\hrule\vskip 3pt}
+}
+\endtable
+
+
+\section{Monthly Notices journal style}
+
+Authors submitting \TeX\ or \LaTeX\ papers to Monthly Notices
+may wish to note the following points regarding journal style.
+Adherence to correct style from the start will obviously save time
+and effort later on, in terms of fewer requested subeditorial
+corrections. The notes given here relate to common style errors found
+in Monthly Notices manuscripts, and are {\it not\/} intended to be
+exhaustive. Please see the editorials in issues 257/2 and 260/1, as
+well as any recent issue of the journal, for more details. As far
+as possible, the subeditor will indicate which of your changes
+would be best done globally, thus saving you time.
+
+\subsection{Punctuation}
+
+When deciding where to add commas, it may be helpful to read
+ through the sentence and note where the natural `pauses' occur.
+The needs of readers for whom English is not a first language
+should be borne in mind when punctuating long sentences.
+\ifCUPmtplainloaded \else \vadjust{\eject}\fi %%
+For example, consider the following sentence as it
+appeared in Monthly Notices:
+`When we do not limit ourselves by constraints arising
+from the choice of an initial fluctuation spectrum, structures in
+an open universe, including the peculiar velocity structure, can
+be reproduced in a flat Lema\^{\i}tre universe for a large part of
+their evolution.' Now consider the same sentence without commas:
+`When we do not limit ourselves by constraints arising
+from the choice of an initial fluctuation spectrum structures in
+an open universe including the peculiar velocity structure can be
+reproduced in a flat Lema\^{\i}tre universe for a large part of their
+evolution.'
+
+
+\subsection{Spelling}
+
+Please use British spelling -- e.g.\ centre not center, labelled
+not labeled. The following style regarding -ise and -ize spellings is
+followed. -ise: devise, surprise, comprise, revise,
+exercise, analyse. -ize: recognize, criticize, minimize, emphasize, organize.
+
+
+\subsection{Titles and section/subsection headings}
+
+With the exception of section headings (e.g.\
+{\bf INTRO\-DUC\-TION}$\ldots$),
+capital letters should be used only where they occur in a normal
+sentence -- e.g.\
+`\textbfit{ROSAT\/} {\bf observations of the unusual star}$\ldots$', not
+`\textbfit{ROSAT\/} {\bf Observations of the Unusual Star}$\ldots$'.
+
+\subsection{Key words}
+
+The list of Monthly Notices key words is published with the 4th
+issue of each volume. No other key words should be used. Please
+use the correct layout for key words:
+\smallskip
+
+\noindent {\bf Key words:} galaxies: active -- galaxies: Seyfert --
+radio continuum: galaxies.
+
+\subsection{Hyphens and N-rules}
+
+\beginlist
+\item (i) Hyphens (one dash in \TeX/\LaTeX). Monthly Notices uses hyphens
+for compound adjectives (e.g.\ low-density gas, least-squares fit,
+two-component model). This also applies to simple units (e.g.\
+1.5-m telescope, 284.5-nm line), but not to complex units or
+ranges, which could become cumbersome (e.g.\ 15 km s$^{-1}$ feature,
+100--200 $\umu$m observations).
+
+\item (ii) N-rules (two dashes in \TeX/\LaTeX). These are used (a) to
+separate key words, (b) as parentheses (e.g.\ `the results --
+assuming no temperature gradient -- are indicative of$\ldots$), (c) to
+denote a range (e.g.\ 1.6--2.2 $\umu$m), and (d) to denote the joining
+of two words (e.g.\ Kolmogorov--Smirnov test, Herbig--Haro
+object).
+
+\item (iii) The M-rule (three dashes in \TeX/\LaTeX) is not used in
+Monthly Notices.
+\endlist
+
+
+\subsection{References}
+
+It is important to use the correct reference style, details of
+which can be found in the editorials cited above, and which is
+demonstrated in any recent issue of the journal. The main points
+are summarized below.
+%
+\beginlist
+\item (i) In text -- for three-author papers, give all three authors
+at first mention, and `et al.' thereafter.
+
+\item (ii) In references list -- no bold or italic, no commas after
+author surnames, and no ampersand between final two author names.
+Use simplified abbreviations for frequently used journals (e.g.\
+MNRAS, ApJ, A\&A, PASP -- see full list in editorial in issue
+260/1). List all authors if eight or less, otherwise `et al.' For
+example,
+\endlist
+
+\beginrefs
+\bibitem Biggs J.D., Lyne A.G., 1992, MNRAS, 254, 257
+
+\bibitem Brown A.B., Jones C.D., 1989, in Robinson E.F.,
+Smith G.H., eds, Proc. IAU Symp. 345, Black Dwarfs. Kluwer, Dordrecht,
+p.~210
+
+\bibitem Felsteiner J., Opher R., 1991, in Treves A., ed.,
+Iron Line Diagnostics in X-ray Sources. Springer-Verlag, Berlin, p.~209
+
+\bibitem Gunn J.E., Knapp G., 1993, in Soifer B.T., ed., ASP
+Conf.\ Ser.\ Vol.~43, Sky Surveys. Astron.\ Soc.\ Pac., San Francisco,
+p.~267
+
+\bibitem Peebles P.J.E., 1980, The Large-Scale Structure of the Universe. Princeton Univ. Press, Princeton, NJ
+
+\bibitem Pounds K.A. et al., 1993, MNRAS, 260, 77
+
+\bibitem Williams B.G., 1992, PhD thesis, Univ.\ Edinburgh
+\endrefs
+
+
+\subsection{Maths}
+
+Scalar variables are italic; vectors are bold italic; matrices
+are `bold Univers' font (like bold sans serif). Differential d,
+complex i, exponential e, sin, cos, tan, log, etc., are roman.
+Sub/superscripts that are physical variables are italic, while
+those that are just labels are roman (e.g.\ $C_p$, but $T_{{\rm eff}}$).
+Equations should be punctuated as part of the sentence.
+
+
+\subsection{Miscellaneous}
+
+e.g., i.e., cf., etc., are roman.
+Single quotes ` ' not double quotes `` ".
+Take care to use correct units -- see recent \hbox{issues} for details.
+Use superscript $-1$, not solidus /, for units -- e.g.\ km~s$^{-1}$ not
+km/s. The unit of arcseconds is arcsec when used to denote angular
+size or separation (e.g.\ `beamsize 12~arcsec', `30~arcsec
+west of the star'); use \arcsec\ for positions (e.g.\
+Dec.~$-30^\circ$~29\arcmin~23\arcsec) (similarly for arcminutes).
+The unit of magnitudes is mag,
+not superscript m. Percentages should be written `per cent', not
+\%. Use the degree symbol $^\circ$ (|$^\circ$|) except to denote, e.g., areas, where
+`deg$^2$' may be more appropriate (e.g.\ `a survey area of 3~deg$^2$').
+Degree symbols should be positioned above the decimal point if
+there is one -- i.e.\ 23\fdg 4 not 23.4$^\circ$ (similarly for
+\ifCUPmtplainloaded \vadjust{\eject}\else\fi %%
+superscript
+h, m, s, and \arcmin, \arcsec\ symbols in coordinates). See guide for coding.
+Ionized species should be denoted by small caps, with a thin
+space -- e.g.\ \hbox{He\,{\sc ii}}, \hbox{C\,{\sc iv}},
+\hbox{[Fe\,{\sc ii}]} 465.8 nm, \hbox{N\,{\sc iii}} 463.4~nm. If
+lack of the correct font at your site prevents this from coming
+out on your printout, it would be helpful if you were to indicate
+as such on your manuscript so that the subeditor knows that there
+is no need for correction.
+Computer software (e.g.\ {\sc figaro}) should be in small capitals.
+Satellite names should be italic (e.g.\ {\it Ginga, IRAS\/}).
+The correct bracket order is $\{[( )]\}$.
+
+
+\section{Trouble-shooting}
+
+Authors may from time to time encounter problems with the preparation
+of their papers in \TeX/\LaTeX. The appropriate action to
+take will depend on the nature of the problem -- the following is
+intended to act as a guide.
+%
+\beginlist
+\item (i) If a problem is with \TeX/\LaTeX\ itself, rather than with the
+actual macros, \ifCUPmtplainloaded \else \vadjust{\eject}\fi %%
+please refer to the appropriate handbooks for
+initial advice.\footnote{\dag}{\TeX : Knuth D., 1986, The \TeX book.
+Addison Wesley; \LaTeX: Lamport L., 1985, \LaTeX\ User's Guide and
+Reference Manual. Addison Wesley.} If the
+solution cannot be found, and you suspect that the problem lies
+with the macros, then please contact the RAS Journal Production
+team at Blackwell Science (BS), 23 Ainslie
+Place, Edinburgh EH3 6AJ, UK (Tel: 031 226 7232; Fax: 031 226 3803;
+omit the first zero if calling from outside the UK).
+The BS office will shortly be
+accessible by email -- please see the Instructions for Authors on
+the inside back cover of Monthly Notices for details. Please
+provide precise details of the problem (what you were trying to
+do -- ideally, include examples of source code as well -- and
+what exactly happened; what error message was received).
+
+\item (ii) Problems with page make-up, particularly in the two-column
+mode (e.g.\ large spaces between paragraphs, or under headings or
+figures; uneven columns; figures/tables appearing out of order).
+Please do {\it not\/} attempt to remedy these yourself using `hard' page
+make-up commands -- the typesetters at Cambridge University Press
+(CUP) will sort out problems when typesetting. (You may, if you
+wish, draw attention to particular problems when submitting the
+final version of your paper.)
+
+\item (iii) If a required font is not available at your site, allow \TeX\
+to substitute the font and report the problem on your disk
+documentation form.
+\endlist
+
+
+\subsection{Fixes for coding problems}
+
+The new versions of the style files and macros have been designed
+to minimize the need for user-defined macros to create special
+symbols. Authors are urged, wherever possible, to use the following
+coding rather than create their own. This will minimize the
+danger of author-defined macros being accidentally `over-ridden'
+when the paper is typeset in Monotype Times (see Subsection~3.13, %%
+`Typesetting mathematics').
+%
+\beginlist
+\item (i) Fonts in sections and paper titles. The following are examples
+of styles that sometimes prove difficult to code.
+\endlist
+
+
+\subsection*{\it P\lowercase{aper titles}}
+
+\boxit{\multi\seventeenpoint\bf
+ A survey of \textbfit{IRAS\/} galaxies\\
+ at $\bmath{\delta > {\bf 50}^\circ}$\endmulti}
+%
+is produced by:
+%
+\beginlines
+|\title{A survey of \textbfit{IRAS\/} galaxies|
+| \hfil\break at $\bmath{\delta>{\bf 50}^\circ}$}|
+\smallskip
+|\shorttitle{A survey of IRAS galaxies at $\delta|
+| > 50^\circ$}|
+\endlines
+\bigskip
+
+\boxit{\multi\seventeenpoint\bf\noindent
+ Observations of compact\\
+ H\,{\elevenbf II} regions\endmulti}
+%
+is produced by:
+%
+\beginlines
+|\title{Observations of compact|
+| H\,{\elevenbf II} regions}|
+\smallskip
+|\shorttitle{Observations of compact|
+| H\,{\eightit II} regions}|
+\endlines
+
+
+\subsection*{\it S\lowercase{ection headings}}
+
+\boxit{\bf 1\quad THE \textbfit{IRAS\/} DATA FOR
+ $\bmath{\delta > {\bf 50}^\circ}$}
+%
+is produced by:
+%
+\beginlines
+|\section{The \textbfit{IRAS\/} data for|
+| $\bmath{\delta>{\bf 50}^\circ}$}|
+\endlines
+\bigskip
+
+\boxit{\bf 2\quad H\,{\sevenbf II} GALAXIES AT
+ $\bmath{\lowercase{z} > {\bf 1.6}}$}
+%
+is produced by:
+%
+\beginlines
+|\section{H\,{\sevenbf II} galaxies at|
+| $\bmath{\lowercase{z}>{\bf 1.6}}$}|
+\endlines
+
+
+\subsection*{\it S\lowercase{ubsection headings}}
+
+\boxit{\multi\bf 2.1\quad The \textbfit{IRAS\/} data for
+ $\bmath{\delta > {\bf 50}^\circ}$: galaxies\\
+ at $\bmath{z > {\bf 1.5}}$\endmulti}
+%
+is produced by:
+%
+\beginlines
+|\subsection{The \textbfit{IRAS\/} data for|
+| $\bmath{\delta > {\bf 50}^\circ}$: galaxies|
+| \hfil\break at $\bmath{z > {\bf 1.5}}$}|
+\endlines
+\bigskip
+
+\boxit{\bf 2.2\quad Observations of compact H\,{\sevenbf II} regions}
+%
+is produced by:
+%
+\beginlines
+|\subsection{Observations of compact|
+| H\,{\sevenbf II} regions}|
+\endlines
+\bigskip
+
+\boxit{\it 2.2.1\quad A survey of radio galaxies
+ for $\delta > {\it 50}^\circ$}
+%
+is produced by:
+%
+\beginlines
+|\subsubsection{A survey of radio galaxies|
+| for $\delta > {\it 50}^\circ$}|
+\endlines
+\bigskip
+
+\boxit{\it 2.2.2\quad Determination of T$_{eff}$ in compact
+ H\,{\sevenit II} regions}
+%
+is produced by:
+%
+\beginlines
+|\subsubsection{Determination of T$_{eff}$ in|
+| compact H\,{\sevenit II} regions}|
+\endlines
+
+\beginlist
+\item (ii) Small capitals and other unusual fonts in table and figure
+captions:
+\par\smallskip
+\boxit{\eightpoint {\bf Figure 1.} Profiles of the H$\alpha$ and
+ N\,{\sc iii} lines observed.}
+%
+is produced by:
+%
+\beginlines
+|\caption{Profiles of the H$\alpha$ and|
+| N\,{\sc iii} lines observed.}|
+\endlines
+
+\item (iii) Multiple author lists (to get the correct vertical spacing
+and wraparound on the title page of a multiple-author paper).
+\par\smallskip
+
+\boxit{\multi
+ \seventeenpoint\bf\noindent
+ The variation in the\\
+ strength of low-$\bmath{l}$ solar\\
+ $\bmath{p}$-modes: 1981--2
+ \medskip
+ \fourteenpoint\noindent
+ Y. Elsworth, R. Howe, G.R. Isaac,\\
+ C.P. McLeod, B.A. Miller, R. New,\\
+ C.C. Speake and S.J. Wheeler\endmulti
+}
+%
+is produced by:
+%
+\beginlines
+|\title{The variation in the\hfil\break|
+| strength of low-$\bmath{l}$ solar\hfil\break|
+| $\bmath{p}$-modes: 1981--2}|
+\smallskip
+|\shorttitle{The variation in the strength of|
+| low-$l$ solar $p$-modes: 1981--2}|
+\smallskip
+|\author{Y. Elsworth, R. Howe, G.R. Isaac,|
+| \hfil\break C.P. McLeod, B.A. Miller, R. New,|
+| \hfil\break C.C. Speake and S.J. Wheeler}|
+\smallskip
+|\shortauthor{Y. Elsworth et al.}|
+\endlines
+
+\item (iv) Ionized species (as used in the examples above). The correct
+style calls for the use of small capitals and a thin space after
+the symbol for the element: e.g.\ for \hbox{H\,{\sc ii}}, use the code
+|\hbox{H\,{\sc ii}}|. The use of the |\hbox| will stop the
+H and the {\sc ii} being separated.
+
+\item (v) Lower case greek pi ($\pi$), mu ($\mu$) and partial ($\partial$).
+In certain circumstances, the Monthly Notices style calls for these to be
+roman [when pi is used to denote the constant 3.1415$\ldots$, mu is
+used to denote `micro' in a unit (e.g.\ $\umu$m, $\umu$Jy), and partial
+is a differential symbol]. See Subsubsection~3.13.5 for instructions.
+
+\item (vi) Decimal degrees, arcmin, arcsec, hours, minutes and seconds.
+The symbol needs to be placed vertically above the decimal point.
+For example, the sentence
+%
+\beginquote
+The observations were made along position angle
+120\fdg 5, starting from the central coordinates
+${\rm RA}(1950)=19^{\rm h}~22^{\rm m}~18\fs 2$,
+${\rm Dec.}~(1950)=45^\circ~18'~36\farcs 4$
+\endquote
+%
+uses the following coding:
+%
+\beginlines
+|The observations were made along position angle|
+|120\fdg 5, starting from the central coordinates|
+|${\rm RA}(1950)=19^{\rm h}~22^{\rm m}~18\fs 2$,|
+|${\rm Dec.}~(1950)=45^\circ~18'~36\farcs 4$|
+\endlines
+
+\item (vii) The correct coding for the prime symbol \arcmin\ is
+|\arcmin|, and that for \arcsec\ is |\arcsec|; see the two
+tables on special symbols.
+
+\item (viii) N-rules, hyphens and minus signs (see style guide for
+correct usage). To create the correct symbols in the sentence
+%
+\beginquote
+The high-resolution observations were made along a
+line at an angle of $-15^\circ$ (east from north)
+from the axis of the jet, which runs north--south
+\endquote
+%
+you would use the following code:
+%
+\beginlines
+|The high-resolution observations were made along|
+|a line at an angle of $-15^\circ$ (east from|
+|north) from the axis of the jet, which runs|
+|north--south|
+\endlines
+
+\item (ix) Vectors and matrices should be bold italic and bold sans
+serif respectively. To create the correct fonts for the vector $\bmath{x}$
+and the matrix \textbfss{P}, you should use |$\bmath{x}$| and
+|\textbfss{P}| respectively; |\mathbfss| is for use in
+math mode. Bold face text italic can be obtained by using
+|\textbfit{..}| and |\mathbfit{..}| for math mode.
+\ifCUPmtplainloaded \else \vfil\eject\fi %%
+\item (x) Bold italic superscripts and subscripts. To get these
+to come out in the correct font and the right size, you need to use
+|\bmath|. You can create the output $\bmath{k_x}$ by typing |$\bmath{k_x}$|.
+Try to avoid using \TeX\ commands to determine script sizes that are
+already defined in the macros. For example, macros such as
+%
+\beginlines
+|\def\th{^\hbox{\sevenrm th}}|
+\endlines
+%
+are generating extra work;
+%
+\beginlines
+|\def\th{^{\rm th}}|
+\endlines
+%
+will do, and will get the size of the superscript right whether in main
+text, tables or captions (the use of |\sevenrm| over-rides the macros).
+Also, the |\hbox| is not necessary, as \TeX\ won't split a
+superscript/subscript from its variable at a line break.
+
+\item (xi) Calligraphic letters (uppercase only).
+%
+Normal uppercase calligraphic can be produced with |\cal| as
+normal (in math mode). Bold calligraphic can be produced with |\bmath|,
+e.g.\ |$\bmath{\cal A}$| gives $\bmath{\cal A}$.
+
+\item (xii) Automatic scaling of brackets. The codes |\left| and
+|\right| should be used to scale brackets automatically to
+fit the equation being set. For example, to get
+$$
+ v = x \left( {N+2}\over {N} \right)
+$$
+use the code
+%
+\beginlines
+|$$|
+| v = x \left( {N+2}\over {N} \right)|
+|$$|
+\endlines
+
+\item (xiii) Roman font in equations. It is often necessary to make some
+symbols roman in an equation (e.g.\ units, subscripts). For example,
+to get the following output:
+$$
+ \sigma \simeq (r/13~h^{-1}~{\rm Mpc})^{-0.9},
+ \qquad \omega = {{N-N_{\rm s}}\over {N_{\rm R}}},
+$$
+you should use:
+%
+\beginlines
+|$$|
+| \sigma\simeq (r/13~h^{-1}~{\rm Mpc})^{-0.9},|
+| \qquad\omega={{N-N_{\rm s}}\over {N_{\rm R}}},|
+|$$|
+\endlines
+
+\item (xiv) Continuation figure and table captions.
+See Subsection~3.6. %%
+\endlist
+
+
+\subsection{Springer-Verlag macro names}
+
+These have been incorporated from the Astronomy \& Astrophysics \LaTeX\
+style file, to aid in the creation of various commonly used
+astronomical symbols. Please see Subsubsection~3.13.6 for details. %%
+
+\bye
+
+% end of mnguide.tex
diff --git a/Master/texmf-dist/doc/plain/mnras/mnland.tex b/Master/texmf-dist/doc/plain/mnras/mnland.tex
new file mode 100644
index 00000000000..968077488f8
--- /dev/null
+++ b/Master/texmf-dist/doc/plain/mnras/mnland.tex
@@ -0,0 +1,82 @@
+% MNLAND.TEX
+%
+% A landscape figure for the sample plain TeX Monthly Notices article.
+%
+% v1.1 --- released 25th August 1994 (M. Reed)
+% v1.0 --- first released 17th February 1994
+%
+% Copyright Cambridge University Press
+
+% The following line automatically loads the mn macros if you are not
+% using a format file.
+\ifx\mnmacrosloaded\undefined \input mn\fi
+
+% If your system has the AMS fonts version 2.0 installed, MN.tex can be
+% made to use them by uncommenting the line: %\AMStwofontstrue
+%
+% By doing this, you will be able to obtain upright Greek characters.
+% e.g. \umu, \upi etc. See the section on "Upright Greek characters" in
+% this guide for further information.
+
+% !! AMS fonts are not used in this file. The following code is provided
+% for your convenience !!
+\newif\ifAMStwofonts
+%\AMStwofontstrue
+
+\ifCUPmtplainloaded \else
+ \NewTextAlphabet{textbfit} {cmbxti10} {}
+ \NewTextAlphabet{textbfss} {cmssbx10} {}
+ \NewMathAlphabet{mathbfit} {cmbxti10} {} % for math mode
+ \NewMathAlphabet{mathbfss} {cmssbx10} {} % " " "
+ %
+ \ifAMStwofonts
+ %
+ \NewSymbolFont{upmath} {eurm10}
+ \NewSymbolFont{AMSa} {msam10}
+ \NewMathSymbol{\upi} {0}{upmath}{19}
+ \NewMathSymbol{\umu} {0}{upmath}{16}
+ \NewMathSymbol{\upartial}{0}{upmath}{40}
+ \NewMathSymbol{\leqslant}{3}{AMSa}{36}
+ \NewMathSymbol{\geqslant}{3}{AMSa}{3E}
+ \let\oldle=\le \let\oldleq=\leq
+ \let\oldge=\ge \let\oldgeq=\geq
+ \let\leq=\leqslant \let\le=\leqslant
+ \let\geq=\geqslant \let\ge=\geqslant
+ \else
+ \def\umu{\mu}
+ \def\upi{\pi}
+ \def\upartial{\partial}
+ \fi
+\fi
+
+
+%\special{landscape} % only use this if your driver supports it
+
+% Marginal adjustments using \pageoffset maybe required when printing
+% proofs on a Laserprinter (this is usually not needed).
+% Syntax: \pageoffset{ +/- hor. offset}{ +/- vert. offset}
+% e.g. \pageoffset{-3pc}{-4pc}
+
+\pageoffset{0pc}{-1.5pc}
+
+\landscape
+\authorcomment{Landscape material to be pasted into the article.}
+
+\begintopmatter % these must be here
+\maketitle %
+
+
+\beginfigure{1}
+\caption{{\bf Figure 4.} Photometric comparisons in the overlap areas
+ between the fields. The differences between photometry of individual images
+ from different fields for the overlapping fields 52--51, 50--51, 50--28 and
+ 30--29 are shown for the $B_{\rm J}$ and $R$ wavebands. The axes are as
+ follows. Left-hand panels: $\Delta B$ ($-1$ to 1) against
+ $\langle B \rangle$ (13 to 21). Right-hand panels: $\Delta R$ ($-1$ to 1)
+ against $\langle R \rangle$ (12 to 20).}
+\endfigure
+
+
+\bye
+
+% end of mnland.tex
diff --git a/Master/texmf-dist/doc/plain/mnras/mnsample.tex b/Master/texmf-dist/doc/plain/mnras/mnsample.tex
new file mode 100644
index 00000000000..b19ea01c605
--- /dev/null
+++ b/Master/texmf-dist/doc/plain/mnras/mnsample.tex
@@ -0,0 +1,705 @@
+% MNSAMPLE.TEX
+%
+% A sample plain TeX single/two column Monthly Notices article.
+%
+% v1.5 --- released 25th August 1994 (M. Reed)
+% v1.4 --- released 22nd February 1994
+% v1.3 --- released 8th December 1992
+%
+% Copyright Cambridge University Press
+
+% The following line automatically loads the mn macros if you are not
+% using a format file.
+\ifx\mnmacrosloaded\undefined \input mn\fi
+
+% If your system has the AMS fonts version 2.0 installed, MN.tex can be
+% made to use them by uncommenting the line: %\AMStwofontstrue
+%
+% By doing this, you will be able to obtain upright Greek characters.
+% e.g. \umu, \upi etc. See the section on "Upright Greek characters" in
+% this guide for further information.
+
+\newif\ifAMStwofonts
+%\AMStwofontstrue
+
+\ifCUPmtplainloaded \else
+ \NewTextAlphabet{textbfit} {cmbxti10} {}
+ \NewTextAlphabet{textbfss} {cmssbx10} {}
+ \NewMathAlphabet{mathbfit} {cmbxti10} {} % for math mode
+ \NewMathAlphabet{mathbfss} {cmssbx10} {} % " " "
+ %
+ \ifAMStwofonts
+ %
+ \NewSymbolFont{upmath} {eurm10}
+ \NewSymbolFont{AMSa} {msam10}
+ \NewMathSymbol{\upi} {0}{upmath}{19}
+ \NewMathSymbol{\umu} {0}{upmath}{16}
+ \NewMathSymbol{\upartial}{0}{upmath}{40}
+ \NewMathSymbol{\leqslant}{3}{AMSa}{36}
+ \NewMathSymbol{\geqslant}{3}{AMSa}{3E}
+ \let\oldle=\le \let\oldleq=\leq
+ \let\oldge=\ge \let\oldgeq=\geq
+ \let\leq=\leqslant \let\le=\leqslant
+ \let\geq=\geqslant \let\ge=\geqslant
+ \else
+ \def\umu{\mu}
+ \def\upi{\pi}
+ \def\upartial{\partial}
+ \fi
+\fi
+
+
+% Marginal adjustments using \pageoffset maybe required when printing
+% proofs on a Laserprinter (this is usually not needed).
+% Syntax: \pageoffset{ +/- hor. offset}{ +/- vert. offset}
+% e.g. \pageoffset{-3pc}{-4pc}
+
+\pageoffset{-2.5pc}{0pc}
+
+\loadboldmathnames
+
+% \Referee % uncomment this for referee mode (double spaced)
+
+% \pagerange, \pubyear and \volume are defined at the Journals office and
+% not by an author.
+
+% \onecolumn % enable one column mode
+% \letters % for `letters' articles
+\pagerange{1--7} % `letters' articles should use \pagerange{Ln--Ln}
+\pubyear{1989}
+\volume{226}
+% \microfiche{} % for articles with microfiche
+% \authorcomment{} % author comment for footline
+
+\begintopmatter % start the two spanning material
+
+\title{Dust envelopes around RV Tauri stars}
+\author{A. V. Raveendran}
+\affiliation{Indian Institute of Astrophysics, Bangalore 560034, India}
+
+\shortauthor{A. V. Raveendran}
+\shorttitle{Dust envelopes around RV Tauri stars}
+
+% \acceptedline is to be defined at the Journals office and not
+% by an author.
+
+\acceptedline{Accepted 1988 December 15. Received 1988 December 14;
+ in original form 1988 October 11}
+
+\abstract {In the {\it IRAS\/} [12]--[25], [25]--[60]
+colour--colour diagram, RV Tauri stars are found to populate
+cooler temperature regions $(T<600\,{\rm K})$, distinctly
+different from those occupied by the oxygen and carbon Miras.
+The {\it IRAS\/} fluxes are consistent with the dust density in
+the envelope varying as the inverse square of the radial
+distance, implying that the grain formation processes in these
+objects are most probably continuous and not sporadic. It is
+found that the spectroscopic subgroups A and B are
+well separated in the far-infrared two-colour diagram, with
+group B objects having systematically cooler dust envelopes. We
+interpret this as being due to a difference in the nature of
+grains, including the chemical composition, in the two cases.}
+
+\keywords {circumstellar matter -- infrared: stars.}
+
+\maketitle % finish the two spanning material
+
+
+\section{Introduction}
+
+It has been well established that RV Tauri variables
+possess infrared emission far in excess of their expected
+blackbody continuum, arising from their extended cool dust
+envelopes (Gehrz \& Woolf 1970; Gehrz 1972; Gehrz \& Ney 1972).
+Recently, Lloyd Evans (1985) and Goldsmith et~al.\ (1987)
+have given detailed descriptions of the near-infrared
+properties of RV Tauri stars. In this paper we present an
+analysis of the {\it IRAS\/} data of RV Tauri stars with the help
+of the far-infrared two-colour diagram and a grid computed
+using a simple model of the dust envelope. Such two-colour plots
+have already been employed extensively by several investigators
+to study the circumstellar envelopes around oxygen-rich and
+carbon-rich objects which are in the late stages of stellar
+evolution (Hacking et~al.\ 1985; Zuckerman \& Dyck 1986;
+van der Veen \& Habing 1988; Willems \& de Jong 1988).
+
+Table~1 summarizes the basic data on the 17 objects
+detected at 60$\,\umu$m. Apart from the {\it IRAS\/} identification
+and the flux densities at 12-, 25-, 60- and 100-$\umu$m wavebands,
+it gives the spectroscopic groups of Preston et~al.\ (1963),
+the light-curve classes of Kukarkin et~al.\ (1969) and the periods of
+light variation. The list, which
+contains about 20 per cent of all the known RV Tauri stars,
+is essentially the same as that given by Jura (1986). The
+spectroscopic subgroups are from either Preston et~al.\ (1963) or
+Lloyd Evans (1985).
+%
+\begintable*{1}
+\caption{{\bf Table 1.} Data on the RV Tauri stars detected by {\it IRAS}.}
+\halign{%
+\rm#\hfil&\qquad\rm#\hfil&\qquad\rm\hfil#&\qquad\rm\hfil
+#&\qquad\rm\hfil#&\qquad\rm\hfil#&\qquad\rm#\hfil
+&\qquad\rm\hfil#&\qquad\rm#\hfil&\qquad\hfil\rm#\cr
+Name&&\multispan4\hskip23pt\hss Flux density (Jy)$^a$\hss \cr
+Variable&{\it IRAS}&12$\;\umu$m&25$\;\umu$m
+&60$\;\umu$m&100$\;\umu$m&Sp.&Period&Light-&$T_0({\rm K})$\cr
+&&&&&&group&(d)\hfill&curve\cr
+&&&&&&&&type\cr
+\noalign{\vskip 10pt}
+TW Cam&04166$+$5719&8.27&5.62&1.82&$<$1.73&A&85.6&a&555\cr
+RV Tau&04440$+$2605&22.53&18.08&6.40&2.52&A&78.9&b&460\cr
+DY Ori&06034$+$1354&12.44&14.93&4.12&$<$11.22&B&60.3&&295\cr
+CT Ori&06072$+$0953&6.16&5.57&1.22&$<$1.54&B&135.6&&330\cr
+SU Gem&06108$+$2734&7.90&5.69&2.16&$<$11.66&A&50.1&b&575\cr
+UY CMa&06160$-$1701&3.51&2.48&0.57&$<$1.00&B&113.9&a&420\cr
+U Mon&07284$-$0940&124.30&88.43&26.28&9.24&A&92.3&b&480\cr
+AR Pup&08011$-$3627&131.33&94.32&25.81&11.65&B&75.0&b&450\cr
+IW Car&09256$-$6324&101/06&96.24&34.19&13.07&B&67.5&b&395\cr
+GK Car&11118$-$5726&2.87&2.48&0.78&$<$12.13&B&55.6&&405\cr
+RU Cen&12067$-$4508&5.36&11.02&5.57&2.01&B&64.7&&255\cr
+SX Cen&12185$-$4856&5.95&3.62&1.09&$<$1.50&B&32.9&b&590\cr
+AI Sco&17530$-$3348&17.68&11.46&2.88&$<$45.62&A&71.0&b&480\cr
+AC Her&18281$+$2149&41.47&65.33&21.12&7.79&B&75.5&a&260\cr
+R Sct&18448$-$0545&20.88&9.30&8.10&$<$138.78&A&140.2&a\cr
+R Sge&20117$+$1634&10.63&7.57&2.10&$<$1.66&A&70.6&b&455\cr
+V Vul&20343$+$2625&12.39&5.72&1.29&$<$6.96&A&75.7&a&690\cr
+}
+\tabletext{\noindent $^a$Observed by {\it IRAS}.}
+\endtable
+
+
+\section{Description of the envelope model}
+
+If we assume that the dust grains in the envelope are
+predominantly of the same kind and are in thermal equilibrium,
+the luminosity at frequency $\nu$ in the infrared is given by
+$$
+ L(\nu)=\mskip-25mu\int\limits_{\rm envelope}\mskip-25mu
+ \rho(r)Q_{{\rm abs}}
+ (\nu)B[\nu,T_{\rm g}(r)]\exp [-\tau(\nu,r)]\> {\rm d}V, \eqno\stepeq
+$$
+where
+$Q_{{\rm abs}}(\nu)$ is the absorption efficiency at frequency $\nu$,
+$\rho(r)$ is the dust grain density,
+$T_{\rm g}(r)$ is the grain temperature,
+$B[\nu,T_{\rm g}(r)]$ is the Planck function and
+$\tau(\nu,r)$ is the optical depth at distance {\it r\/} from the
+centre of the star.
+
+The temperature $T_{\rm g}(r)$ is determined by the condition of
+energy balance: amount of energy radiated = amount of energy
+absorbed. The amount of energy absorbed at any point is
+proportional to the total available energy at that point, which
+consists of:
+\beginlist
+\item (i) the attenuated and diluted stellar radiation;
+\item (ii) scattered radiation, and
+\item (iii) reradiation from other grains.
+\endlist
+
+Detailed solutions of radiative transfer in circumstellar
+dust shells by Rowan-Robinson \& Harris (1983a,b) indicate that
+the effect of heating by other grains becomes significant only at
+large optical depths at the absorbing frequencies $[\tau({\rm
+UV})\gg 10]$, and at optical depths $\tau({\rm UV})<1$ the grains
+have approximately the same temperature that they would have if
+they were seeing the starlight unattenuated and no other
+radiation.
+
+The Planck mean optical depths of circumstellar envelopes
+around several RV Tauri stars, derived from the ratios of the
+luminosities of the dust shell (at infrared wavelengths) and
+the star, range from 0.07 to 0.63 (Goldsmith et~al.\ 1987).
+There is much uncertainty in the nature of the optical
+properties of dust grains in the envelope. The carbon-rich RV
+Tauri stars are also reported to show the 10-$\umu$m silicate
+emission feature typical of oxygen-rich objects (Gehrz \& Ney
+1972; Olnon \& Raimond 1986). The pure terrestrial silicates or
+lunar silicates are found to be completely unsuitable to account
+for the infrared emission from circumstellar dust shells around
+M-type stars (Rowan-Robinson \& Harris 1983a). We assume that
+the absorption efficiency $Q_{{\rm abs}} (\nu)$ in the infrared
+varies as $\nu^{\gamma}$. ${\gamma}=1$ appears to provide a
+reasonable fit in a variety of sources (Harvey, Thronson \&
+Gatley 1979; Jura 1986). Under these circumstances the
+condition of energy balance implies that the dust temperature
+$T_{\rm g}$ will vary as $r^{\beta}$.
+
+In view of the low value of the observed Planck mean optical
+depth for the stellar radiation and the nature of the assumed
+frequency dependence of the absorption efficiency, the
+extinction of the infrared radiation by the dust envelope can
+be neglected. If we consider the envelope to be spherically
+symmetric, equation (1) reduces to
+$$
+ L(\nu)=\!\!\int_{r_{1}}^{r_{2}}\!\!4\upi r^2\rho(r)\> Q_{{\rm abs}}
+ (\nu)B[\nu,T_{\rm g}(r)]\> {\rm d}r, \eqno\stepeq
+$$
+where $r_1$ and $r_2$ are the inner and outer radii of the
+shell. For a dusty density distribution $\rho(r)\propto
+r^{\alpha}$ and $r_2\gg r_1$, equation (2) reduces to
+$$
+ L(\nu)\propto \nu^{2+\gamma-Q}
+ \int_{X_0}^{\infty}{{x^Q}\over{{\rm e}^x-1}}{\rm d}x, \eqno\stepeq
+$$
+where $Q=-(\alpha+\beta+3)/\beta$ and $X_0=(h\nu /kT_0)$.
+$T_0$ represents the temperature at the inner boundary of the
+dust shell where grains start condensing. In a steady radiation
+pressure driven mass outflow in the optically thin case, values of
+$\alpha$ lie near $-2$ (Gilman 1972). $\gamma$ and $\beta$ are
+related by $\beta=-2/(\gamma+4)$.
+
+In the {\it IRAS\/} Point Source Catalog (PSC, Beichman et~al.\ 1985a),
+the flux densities have been quoted at the effective
+wavelengths 12, 25, 60 and 100$\,\umu$m, assuming a flat energy
+spectrum $[\nu F(\nu)=1]$ for the observed sources. For each model
+given by equation (3), using the relative system response, the
+colour-correction factors (Beichman et~al.\ 1985b) in each
+of the {\it IRAS\/} passbands were calculated and the fluxes
+were converted into flux densities expected for a flat energy
+distribution, as assumed in the {\it IRAS\/} PSC, so that the
+computed colours can be directly compared with the colours
+determined from the catalogue quantities. Such a procedure
+is more appropriate than correcting the {\it IRAS\/}
+colours for the energy distribution given by a particular model
+and then comparing them with those computed by the model.
+
+
+\subsection{Colour--colour diagram}
+
+The IR colour is defined as
+$$
+ [\nu_1]-[\nu_2]=-2.5\log [f(\nu_1)/f(\nu_2)],
+$$
+where $\nu_1$ and $\nu_2$ are any two wavebands and
+$f(\nu_1)$ and $f(\nu_2)$ are the corresponding flux densities
+assuming a flat energy spectrum for the source.
+%
+\beginfigure{1}
+\vskip 91mm
+\caption{{\bf Figure 1.} Plot of [25]--[60] colours of
+RV Tauri stars against their [12]--[25] colours after normalizing
+as indicated in Beichman et~al.\ (1985b). Some of the objects
+are identified by their variable-star names. Typical error bars
+are shown in the bottom right-hand corner. The lines represent
+the loci for constant inner shell temperature and the quantity
+$Q$. Note the separation of group A and B stars at $T_0 \sim$
+460$\,$K. Positions occupied by a sample of carbon and oxygen
+Miras are also shown. The $Q=1.0$ line differs from the
+blackbody line by a maximum of $\sim 0.05$.}
+\endfigure
+
+In Fig.~1, we have plotted the [25]--[60] colours of
+RV Tauri stars against their corresponding [12]--[25] colours
+derived from the {\it IRAS\/} data. Filled circles represent
+stars of group A and open circles stars of group B. The two
+sets of near-parallel lines represent the loci of constant
+inner shell temperature $T_0$ and the quantity $Q$ defined
+above. The models correspond to the case of absorption
+efficiency $Q_{{\rm abs}}(\nu)$ varying as $\nu$ (with
+$\gamma=1$ and hence $\beta=-0.4$). We have omitted R Sct in
+Fig.~1 because it shows a large deviation from the average
+relation shown by all the other objects. R Sct has a
+comparatively large excess at 60$\,\umu$m, but the extent of a
+possible contamination by the infrared cirrus (Low et~al.\ 1984)
+is unknown. Goldsmith et~al.\ (1987) found no
+evidence of the presence of a dust envelope at near-IR
+wavelengths and the spectrum was consistent with a stellar
+continuum. This explains why R Sct lies well below the mean
+relation shown by stars of groups A and C between the
+[3.6]--[11.3] colour excess and the photometrically determined
+(Fe/H) (Dawson 1979). R Sct has the longest period of 140$\,$d
+among the RV Tauri stars detected at far-infrared wavelengths
+and does not have the 10-$\umu$m emission feature seen in other
+objects (Gehrz 1972; Olnon \& Raimond 1986). R Sct is probably
+the most irregular RV Tauri star known (McLaughlin 1932).
+
+The inner shell temperatures $(T_0)$ derived for the various
+objects are also given in Table~1 and we find the majority of
+them to have temperatures in the narrow range 400--600$\,$K. If
+the dependences of $Q_{{\rm abs}}(\nu)$ on $\nu$ and $\rho(r)$ on
+$r$ are similar in all the objects considered, then in the
+colour--colour diagram they all should lie along a line
+corresponding to different values of $T_0$ and in Fig.~1 we find
+that this is essentially the case. In view of the quoted
+uncertainties in the flux measurements, we cannot attach much
+significance to the scatter in Fig.~1.
+%
+\beginfigure*{2}
+\vskip 5.9cm
+\caption{{\bf Figure 2.} Plot of the [60]--[100] colours
+of RV Tauri stars against their [25]--[60] colours after normalizing
+as indicated in Beichman et~al.\ (1985b). The solid lines
+represent the loci for constant inner shell temperature and the
+quantity $Q$. The dashed line shows the locus for a blackbody
+distribution.}
+\endfigure
+
+At 100$\,\umu$m the infrared sky is characterized by emission,
+called infrared cirrus, from interstellar dust on all spatial
+scales (Low et~al.\ 1984), thereby impairing the
+measurements at far-infrared wavelengths. In Fig.~2, we have
+plotted the [60]--[100] colours of the six RV Tauri stars
+detected at 100$\,\umu$m against their [25]--[60] colours, along
+with the grid showing the regions of different values for inner
+shell temperature $T_0$ and the quantity $Q$, as in Fig.~1. The
+results indicated by Fig.~2 are consistent with those derived
+from Fig.~1. AR Pup shows a large excess at 100$\,\umu$m but, in
+view of the large values for the cirrus flags given in the
+catalogue, the intrinsic flux at 100$\,\umu$m is uncertain.
+
+
+\subsection{Radial distribution of dust}
+
+From Fig.~1, it is evident that all RV Tauri stars lie
+between the lines corresponding to $Q=1.5$ and $0.5$. With
+$$
+ \alpha=-(1+Q)\beta-3,
+$$
+these values suggest limits of $r^{-2.0}$ and $r^{-2.4}$
+for the dust density variation, indicating a near-constant
+mass-loss rate. Jura (1986) has suggested that the density in
+the circumstellar envelope around RV Tauri stars varies as
+$r^{-1}$, implying a mass-loss rate that was greater in the
+past than it is currently. By fitting a power law to the
+observed fluxes, such that $f(\nu)$ varies as $\nu^q$, values
+of $q$ determined by him for the various objects given in
+Table~1 lie in the range 0.6--1.2, with a mean $\bar q=0.98$. The
+assumption of a power law corresponds to the case of $X_0=0$ in
+equation (3) and hence we get
+$$
+ q=2+\gamma -Q.
+$$
+Since we assume that $Q_{{\rm abs}}(\nu)$ varies as $\nu$,
+the resulting value for $Q$=2.0. None of the objects is found
+to lie in the corresponding region in the colour--colour
+diagram. Even this extreme value for $Q$ implies a density
+which varies as $r^{-1.8}$.
+
+Goldsmith et~al.\ (1987) have reported that the
+simultaneous optical and near-IR data of AC Her can be fitted
+by a combination of two blackbodies at 5680 and 1800$\,$K,
+representing, respectively, the stellar and dust shell
+temperatures, and suggested that in RV Tauri stars the grain
+formation is a sporadic phenomenon and not a continuous
+process. Apparently, they have been influenced by the remark by
+Gehrz \& Woolf (1970) that their data in the 3.5--11$\,\umu$m
+region of AC Her indicated a dust temperature of $\sim300\,$K. We
+find that the {\it K--L\/} colours given by Gehrz (1972), Lloyd
+Evans (1985) and Goldsmith et~al.\ (1987) are all
+consistent with each other. Surely, hot dust ($\sim 1800\,$K), if
+present at the time of observations by Goldsmith et~al.\ (1987),
+would have affected the {\it K--L\/} colour
+significantly. AC Her, like other members of its class, is
+found to execute elongated loops in the ({\it U--B\/}), ({\it
+B--V\/}) plane (Preston et~al.\ 1963), indicating that
+significant departure of the stellar continuum from the
+blackbody is to be expected. Further, their data show only a
+marginal excess at the near-IR wavelengths. We feel that the
+case for the existence of hot dust around AC Her and hence for
+the sporadic grain formation around RV Tauri stars is not
+strong. In Fig.~3 we find that AC Her and
+RU Cen lie very close to R Sct which, according to Goldsmith
+et~al.\ (1987), shows no evidence for the presence of a hot
+dust envelope.
+
+
+\subsubsection{Comparison with oxygen and carbon Miras}
+
+In Fig.~1 we have also shown the positions of a sample of
+oxygen-rich and carbon-rich Miras. At the low temperatures
+characteristic of the Miras, a part of the emission at 12$\,\umu$m
+comes from the photosphere. For a blackbody at 2000$\,$K, the ratio
+of fluxes at wavelengths of 12 and 2$\,\umu$m $(f_{12}/f_{2})\sim
+0.18$. The Miras shown in Fig.~1 have $(f_{12}/f_{2})$
+ratios larger than twice the above value. It is clear that the
+three groups of objects populate three different regions of the
+diagram. Hacking et~al.\ (1985) have already noticed that
+there are distinct differences between the {\it IRAS\/} colours
+of oxygen-rich and carbon-rich objects. On the basis of an
+analysis, using a bigger sample of bright giant stars in the
+{\it IRAS\/} catalogue, this has been interpreted by Zuckerman \&
+Dyck (1986) as being due to a systematic difference in the dust
+grain emissivity index. U Mon shows the 10-$\umu$m silicate
+emission convincingly and, in most of the other objects for
+which low-resolution spectra in the near-infrared have been
+reported (Gehrz 1972; Olnon \& Raimond 1986), the 10-$\umu$m
+emission may be partly attributed to silicates. Hence it is
+reasonable to expect that, in the envelopes around at least some
+of the RV Tauri stars, the dust grains are predominantly of
+silicates, as in the case of oxygen Miras (Rowan-Robinson \&
+Harris 1983a). The fact that none of the RV Tauri stars is
+found in the region of the two-colour diagram occupied by the
+oxygen Miras indicates that the emissivity indices of the
+silicate grains in the two cases are different. Because of the
+higher temperatures and luminosities, the environment of grain
+formation will be different in RV Tauri stars.
+
+
+\subsubsection{Correlation with subgroups}
+
+Preston et~al.\ (1963) have identified three spectroscopic
+subgroups, which are designated as groups A, B and C. Objects of
+group A are metal-rich; group C are metal-poor; group~B objects are
+also metal-poor, but show carbon enhancements (Preston et~al.\ 1963;
+Lloyd Evans 1974; Dawson 1979; Baird 1981). It is interesting
+to see that Table~1 contains no group C objects and that in Fig.~1
+there is a clear separation of the two spectroscopic subgroups A
+and B, with the demarcation occurring at an inner shell
+temperature of about 450$\,$K, group~B stars having lower
+temperatures than group A. SX Cen is the only exception. Lloyd
+Evans (1974) has reported that metal lines are stronger in SX Cen
+than in other group~B objects. It may be worth noting that SX Cen
+has the shortest period among the 100 or so objects with the RV
+Tauri classification. RU Cen has the coolest inner shell
+temperature, as already suggested by the near-infrared spectrum
+(Gehrz \& Ney 1972).
+%
+\beginfigure{3}
+\vskip 59mm
+\caption{{\bf Figure 3.} Plot of $(K$--$L)$ colours of
+RV Tauri stars detected by {\it IRAS\/} against their corresponding
+$(J$--$K)$ colours. The position of AR Pup is indicated. The three
+objects lying close to the blackbody line are AC Her, RU Cen and R Sct.}
+\endfigure
+
+Group~B objects follow a different mean relationship from those
+of group~A, having systematically larger 11-$\umu$m excess for a
+given excess at 3$\,\umu$m (Lloyd Evans 1985). For a general
+sample of RV Tauri stars, the distinction between the
+oxygen-rich and carbon-rich objects is not that apparent in the
+{\it JHKL\/} bands. In Fig.~3 we have plotted the near-IR
+magnitudes of the objects given in Table~1 (except V Vul which
+has no available measurements) in the {\it J--K, K--L\/} plane.
+The colours, taken from Lloyd Evans (1985) and Goldsmith
+et~al.\ (1987), are averaged if more than one observation
+exists, because the internal agreements are found to be often
+of the order of observational uncertainties, in accordance with
+the earlier finding by Gehrz (1972) that variability has
+relatively little effect on colours. Barring RU Cen and AC Her,
+it is evident that stars belonging to group~B show
+systematically larger excesses at {\it L\/}~band for a given
+excess at {\it K}. The low excesses at near-IR wavelengths for
+AC Her and RU Cen are consistent with the very low dust
+temperatures indicated by the far-infrared colours.
+%
+\ifsinglecol
+ \pageinsert
+ \vfil
+ \centerline{Landscape figure to go here. This figure was not
+ part of the original paper and is inserted here for illustrative
+ purposes.}
+ \centerline{See the author guide for details on how to handle landscape
+ figures or tables, and {\tt mnland.tex}.}
+ \centerline{{\bf Figure 4.}}
+ \vfil
+ \endinsert
+\else
+ \beginfigure*{4}
+ \vbox to 646pt{\vfil
+ \centerline{Landscape figure to go here. This figure was not
+ part of the original paper and is inserted here for illustrative
+ purposes.}
+ \centerline{See the author guide for details on how to handle landscape
+ figures or tables, and {\tt mnland.tex}.}
+ \caption{{\bf Figure 4.}}
+ \vfil}
+ \endfigure
+\fi
+
+It is already well established that from {\it UBV\/} photometry
+one can distinguish between groups A and~B, members of group~A
+being significantly redder than those of group~B (Preston
+et~al.\ 1963). Similarly, Dawson (1979) has found that the two
+spectroscopic groups are well separated in the DDO
+colour--colour diagrams when mean colours are used for the
+individual objects.
+
+The clear separation of the spectroscopic subgroups A and~B in
+the IR two-colour diagram suggests that the natures of dust
+grains in the envelopes in the two cases are not identical.
+This is to be expected because of the differences in the
+physical properties of the stars themselves. The average
+colours of group~B stars are bluer than group A, but the
+envelope dust temperatures of B are cooler than those of~A. The
+near-IR spectra of AC Her and RU Cen are extremely similar
+(Gehrz \& Ney 1972). The striking similarities in the optical
+spectra of AC Her and RU Cen have been pointed out by Bidelman
+(O'Connell 1961). We feel that the physical properties,
+including the chemical composition, of the grains formed in
+the circumstellar envelope strongly depend on those of the
+embedded star. This, probably, explains the diversity of the
+energy distributions of RV Tauri stars in the near-infrared
+found by Gehrz \& Ney (1972). On the basis of the observed
+differences in chemical abundances and space distribution of RV
+Tauri stars, Lloyd Evans (1985) has already pointed out that
+there is no direct evolutionary connection between group~A and
+group~B objects, thus ruling out the possibility that group~B
+objects are the evolutionary successors of group~A, in which
+grain formation has stopped and the cooler temperatures for the
+former are caused by an envelope expansion.
+
+Kukarkin et~al.\ (1969) have subdivided RV Tauri stars
+into two classes, RVa and RVb, on the basis of their light
+curves; the former shows a constant mean brightness, whereas
+the latter shows a cyclically varying mean brightness.
+Extensive observations in the near-infrared show that, on
+average, RVb stars are redder than RVa stars, and Lloyd Evans
+(1985) has suggested that in RVb stars dust shells are denser
+in the inner regions and hence radiate strongly in the
+1--3$\,\umu$m region. Fig.~3 confirms this; RVb objects show
+systematically larger ({\it J--K\/}) and ({\it K--L\/}) colours than RVa
+objects. Apparently, there is no distinction between objects of
+the two light-curve types at far-infrared wavelengths (Fig.~1).
+
+
+\section{Conclusions}
+
+In the [12]--[25], [25]--[60] colour diagram, RV Tauri
+stars populate cooler temperature regions $(T<600\,\rm {K})$,
+distinctly different from those occupied by the oxygen and
+carbon Miras. Using a simple model in which
+\beginlist
+\item (i) the envelope is spherically symmetric,
+\item (ii) the IR-emitting grains are predominantly of the same kind, and
+\item (iii) in the IR the absorption efficiency $Q_{{\rm abs}} (\nu)\propto\nu$,
+\endlist
+we find that the {\it IRAS\/} fluxes
+are consistent with the density in the envelope $\rho(r)\propto
+r^{-2}$, where {\it r\/} is the radial distance. Such a
+dependence for the dust density implies that the mass-loss
+rates in RV Tauri stars have not reduced considerably during
+the recent past, contrary to the suggestion by Jura (1986). In
+the two-colour diagram, the blackbody line and the line
+corresponding to $\rho(r)\propto r^{-2.2}$ nearly overlap and
+the present data are insufficient to resolve between the two
+cases. The latter case is more physically reasonable, however.
+
+The spectroscopic subgroups A and B are well separated in
+the {\it IRAS\/} two-colour diagram, with group B objects having
+systematically cooler dust envelopes. If we consider only the
+objects detected by {\it IRAS}, we find that stars
+belonging to group B show systematically larger excess at {\it
+L\/}~band for a given excess at {\it K}. Apparently, there is no
+correlation between the light-curve types (RVa and RVb) and the
+far-infrared behaviour of these objects. It is fairly certain
+that the physical properties, including the chemical
+composition, of the embedded stars are directly reflected by
+those of the dust grains. Most probably, the grain formation
+process in RV Tauri stars is continuous and not sporadic as
+suggested by Goldsmith et~al.\ (1987).
+
+
+\section*{Acknowledgments}
+
+I thank Professor N. Kameswara Rao for some helpful
+suggestions, Dr H. C. Bhatt for a critical reading of the
+original version of the paper and an anonymous referee for
+very useful comments that improved the presentation of the paper.
+
+
+\section*{References}
+
+\beginrefs
+\bibitem Baird S.R., 1981, ApJ, 245, 208
+\bibitem Beichman C.A., Neugebauer G., Habing H.J., Clegg P.E.,
+ Chester T.J., 1985a, {\it IRAS\/} Point Source Catalog. Jet
+ Propulsion Laboratory, Pasadena
+\bibitem Beichman C.A., Neugebauer G., Habing H.J., Clegg P.E.,
+ Chester T.J., 1985b, {\it IRAS\/} Explanatory Supplement. Jet
+ Propulsion Laboratory, Pasadena
+\bibitem Dawson D.W., 1979, ApJS, 41, 97
+\bibitem Gerhz R.D., 1972, ApJ, 178, 715
+\bibitem Gerhz R.D., Ney E.P., 1972, PASP, 84, 768
+\bibitem Gerhz R.D., Woolf N.J., 1970, ApJ, 161, L213
+\bibitem Gilman R.C., 1972, ApJ, 178, 423
+\bibitem Goldsmith M.J., Evans A., Albinson J.S., Bode M.F., 1987, MNRAS,
+ 227, 143
+\bibitem Hacking P. et al., 1985, PASP, 97, 616
+\bibitem Harvey P.M., Thronson H.A., Gatley I., 1979, ApJ, 231, 115
+\bibitem Jura M., 1986, ApJ, 309, 732
+\bibitem Kukarkin B.V. et al., 1969, General Catalogue of Variable Stars.
+ Moscow
+\bibitem Lloyd Evans T., 1974, MNRAS, 167, 17{\sc p}
+\bibitem Lloyd Evans T., 1985, MNRAS, 217, 493
+\bibitem Low F.J. et al., 1984, ApJ, 278, L19
+\bibitem McLaughlin D.B., 1932, Publ. Univ. Obs. Mich., 4, 135
+\bibitem O'Connell J.K., 1961, Specola Vaticana Ric. Astron., 6, 341
+\bibitem Olnon F.M., Raimond E., 1986, A\&AS, 65, 607
+\bibitem Preston G.W., Krzeminski W., Smak J., Williams J.A.,
+ 1963, ApJ, 137, 401
+\bibitem Rowan-Robinson M., Harris S., 1983a, MNRAS, 202, 767
+\bibitem Rowan-Robinson M., Harris S., 1983b, MNRAS, 202, 797
+\bibitem van der Veen W.E.C.J., Habing H.J., 1988, A\&A, 194, 125
+\bibitem Willems F.J., de Jong T., 1988, A\&A, 196, 173
+\bibitem Zuckerman B., Dyck H.M., 1986, ApJ, 311, 345
+\endrefs
+
+
+\appendix
+
+\section{Large gaps in {$\bf L\lowercase{y}\balpha$} forests
+ due to fluctuations in line distribution}
+
+(This appendix was not part of the original paper by A.V.~Raveendran and is
+included here just for illustrative purposes.)
+
+Spectroscopic\looseness=1\ observations of bright quasars show that the mean number
+density of ${\rm Ly}\alpha$ forest lines, which satisfy certain criteria,
+evolves
+like ${\rm d}N/{\rm d}z=A(1+z)^\gamma$, where $A$ and~$\gamma$ are two
+constants. Given
+the above intrinsic line distribution we examine the probability of finding
+large gaps in the ${\rm Ly}\alpha$ forests. We concentrate here only on
+the statistics and neglect all observational complications such as the line
+blending effect (see Ostriker, Bajtlik \&~Duncan 1988).
+
+Suppose we have observed a ${\rm Ly}\alpha$ forest between redshifts $z_1$
+and~$z_2$
+and found $N-1$ lines. For high-redshift quasars $z_2$~is usually the emission
+redshift $z_{\rm em}$ and $z_1$ is set to $(\lambda_{\rm Ly\beta}/\lambda_{\rm
+Ly\alpha})(1+z_{\rm em})=0.844(1+z_{\rm em})$ to avoid contamination by
+Ly$\beta$ lines. We want to know whether the largest gaps observed in the
+forest are significantly inconsistent with the above line distribution. To do
+this we introduce a new variable~$x$:
+$$
+ x={(1+z)^{\gamma+1}-(1+z_1)^{\gamma+1} \over
+ (1+z_2)^{\gamma+1}-(1+z_1)^{\gamma+1}}. \eqno\stepeq
+$$
+$x$ varies from 0 to 1. We then have ${\rm d}N/{\rm d}x=\lambda$,
+where $\lambda$ is the mean number of lines between $z_1$ and $z_2$ and is
+given by
+$$
+ \lambda\equiv{A[(1+z_2)^{\gamma+1}-(1+z_1)^{\gamma+1}]\over\gamma+1}.
+ \eqno\stepeq
+$$
+This means that the ${\rm Ly}\alpha$ forest lines are uniformly distributed
+in~$x$.
+The probability of finding $N-1$ lines between $z_1$ and~$z_2$, $P_{N-1}$, is
+assumed to be the Poisson distribution.
+%
+\beginfigure{5}
+\vskip 11pc
+\caption{{\bf Figure A1.} $P(>x_{\rm gap})$ as a function of
+$x_{\rm gap}$ for, from left to right, $N=160$, 150, 140, 110, 100, 90, 50,
+45 and~40.}
+\endfigure
+
+\subsection{Subsection title}
+
+We plot in Fig.~A1 $P(>x_{\rm gap})$ for several $N$ values.
+We see that, for $N=100$ and $x_{\rm gap}=0.06$, $P(>0.06)\approx 20$
+per cent. This means that the
+\ifsinglecol\else \vadjust{\vfill\eject}\fi
+probability of finding a gap with a size
+larger than six times the mean separation is not significantly small.
+When the mean number of lines is large, $\lambda\sim N>>1$, our
+$P(>x_{\rm gap})$ approaches the result obtained by Ostriker et~al.\ (1988)
+for small (but still very large if measured in units of the mean separation)
+$x_{\rm gap}$, i.e., $P(>x_{\rm gap})\sim N(1-x_{\rm gap})^{N-1}\sim N
+{\rm exp}(-\lambda x_{\rm gap})$.
+
+
+\bye
+
+% end of mnsample.tex
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+% readme.txt (v1.1 released 2nd September 1994)
+% for Monthly Notices (plain TeX)
+%
+% The files for MN are as follows:
+%
+% README.TXT this file
+% FONTTEST.TEX a file to test all of the fonts used in the MN design
+% with your output device
+% MN.TEX the design macros
+% MNGUIDE.TEX authors' instructions
+% MNSAMPLE.TEX sample pages
+% MNLAND.TEX landscape page for sample pages
+%
+% Typeset MNGUIDE.TEX, MNSAMPLE.TEX and MNLAND.TEX for instructions
+% and examples.