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author | Karl Berry <karl@freefriends.org> | 2006-01-09 00:45:48 +0000 |
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committer | Karl Berry <karl@freefriends.org> | 2006-01-09 00:45:48 +0000 |
commit | 5dc602d16c5be2fd035b254ca23484a90aebd6dc (patch) | |
tree | 72efb15fba318cc2096a8cc6999ed3fa0bff317d /Master/texmf-dist/doc/plain/mnras | |
parent | b4fc5f639874db951177ec539299d20908adb654 (diff) |
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git-svn-id: svn://tug.org/texlive/trunk@81 c570f23f-e606-0410-a88d-b1316a301751
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-rw-r--r-- | Master/texmf-dist/doc/plain/mnras/fonttest.tex | 169 | ||||
-rw-r--r-- | Master/texmf-dist/doc/plain/mnras/mnguide.tex | 1988 | ||||
-rw-r--r-- | Master/texmf-dist/doc/plain/mnras/mnland.tex | 82 | ||||
-rw-r--r-- | Master/texmf-dist/doc/plain/mnras/mnsample.tex | 705 | ||||
-rw-r--r-- | Master/texmf-dist/doc/plain/mnras/readme.txt | 15 |
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diff --git a/Master/texmf-dist/doc/plain/mnras/fonttest.tex b/Master/texmf-dist/doc/plain/mnras/fonttest.tex new file mode 100644 index 00000000000..c84aa89bc44 --- /dev/null +++ b/Master/texmf-dist/doc/plain/mnras/fonttest.tex @@ -0,0 +1,169 @@ +% 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 diff --git a/Master/texmf-dist/doc/plain/mnras/readme.txt b/Master/texmf-dist/doc/plain/mnras/readme.txt new file mode 100644 index 00000000000..167ae336a0c --- /dev/null +++ b/Master/texmf-dist/doc/plain/mnras/readme.txt @@ -0,0 +1,15 @@ +% 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. |