------------------------------------------------------------------------ stsci06.tex arXiv:0803.1619v2 Content-Type: text/plain; charset=ISO-8859-1; format=flowed Content-Transfer-Encoding: 7bit X-MailScanner-Information: Please contact the postmaster@aoc.nrao.edu for more information X-MailScanner: Found to be clean X-MailScanner-SpamCheck: not spam, SpamAssassin (not cached, score=0, required 5, autolearn=disabled) X-MailScanner-From: cmtpci@cis.rit.edu X-Spam-Status: No http://arxiv.org/abs/0803.1619 %astro-ph/0803.1619 %http://www.cis.rit.edu/~dffpci/private/papers/stsci06/stsci06.pdf % conf2esa.tex -- sample pages for CUP conference proceedings document class % (based on v1.1 jfm2esam.tex) % v0.1 released 20 September 2000 by Alison Woollatt % Copyright (2000) Cambridge University Press \NeedsTeXFormat{LaTeX2e} %\input{psfig} \documentclass{cupconf} \usepackage{graphicx} \usepackage{subfigure} \usepackage{natbib} % See if the author has AMS Euler fonts installed: If they have, attempt % to use the 'upmath' package to provide upright math. \checkfont{eurm10} \iffontfound \IfFileExists{upmath.sty} {\typeout{^^JFound AMS Euler Roman fonts on the system, using the 'upmath' package.^^J}% \usepackage{upmath}} {\typeout{^^JFound AMS Euler Roman fonts on the system, but you dont seem to have the}% \typeout{'upmath' package installed. cupconf.cls can take advantage of these fonts,^^Jif you use 'upmath' package.^^J}% \providecommand\upi{\pi}% } \else \providecommand\upi{\pi}% \fi % See if the author has AMS symbol fonts installed: If they have, attempt % to use the 'amssymb' package to provide the AMS symbol characters. \checkfont{msam10} \iffontfound \IfFileExists{amssymb.sty} {\typeout{^^JFound AMS Symbol fonts on the system, using the 'amssymb' package.^^J}% \usepackage{amssymb}% \let\le=\leqslant \let\leq=\leqslant \let\ge=\geqslant \let\geq=\geqslant }{} \fi % See if the author has the AMS 'amsbsy' package installed: If they have, % use it to provide better bold math support (with \boldsymbol). \IfFileExists{amsbsy.sty} {\typeout{^^JFound the 'amsbsy' package on the system, using it.^^J}% \usepackage{amsbsy}} {\providecommand\boldsymbol[1]{\mbox{\boldmath $##1$}}} %%% Example macros (some are not used in this sample file) %%% \def\hh{H$_{2}$} \def\cc{C$_{2}$} \def\km/s{km~s$^{-1}$} \def\um{${\mu}$m} \def\Vlsr{v$_{LSR}$} \def\wvnum{cm$^{-1}$} \def\hhhp{H$_{3}^{+}$} \def\hhp{H$_{2}^{+}$} \def\kco{{\it k}$_{CO}$} \def\ke{{\it k}$_{e}$} \def\ne{n$_{e}$} \def\CO{$^{12}$CO} \def\co{$^{13}$CO} \def\Lo{L$_\odot$} \def\Vinf{\hbox{$V_\infty$}} \def\HeI{He\,{\sc i}} \def\HeII{He\,{\sc ii}} \def\HII{H\,{\sc ii}} \def\CII{C\,{\sc ii}} \def\CIII{C\,{\sc iii}} \def\NI{N\,{\sc i}} \def\NII{N\,{\sc ii}} \def\OII{O\,{\sc ii}} \def\OIII{O\,{\sc iii}} \def\NaI{Na\,{\sc i}} \def\MgII{Mg\,{\sc ii}} \def\FeII{Fe\,{\sc ii}} \def\NiII{Ni\,{\sc ii}} \def\SiIII{Si\,{\sc iii}} \def\SiII{Si\,{\sc ii}} \def\Mdot{\.{M}} \def\Msun{\hbox{\it M$_\odot$}} \def\Lsun{\hbox{\it L$_\odot$}} \def\Myr{Myr} \def\Gyr{Gyr} \def\Minit{\hbox{M$_{\rm initial}$}} \def\Msunyr{\hbox{M$_\odot\,$yr$^{-1}$}} \def\Teff{\hbox{\it T$_{\rm eff}$}} \def\Vinf{\hbox{$v_\infty$}} \def\kms{\hbox{km$\,$s$^{-1}$}} \def\FMM362{FMM362} \def\mnras{{\it Monthly Notices of the Royal Astronomical Society\, }} \def\qjras{{\it Quarterly Journal of the Royal Astronomical Society\, }} \def\aap{{\it Astronomy \& Astrophysics\, }} \def\nat{{\it Nature\, }} \def\apj{{\it Astrophysical Journal\, }} \def\apjs{{\it Astrophysical Journal Supplements\, }} \def\aj{{\it Astronomical Journal\, }} \def\pasp{{\it Publications of the Astronomical Society of the Pacific\, }} \def\apjl{{\it Astrophysical Journal Letters\, }} \def\araa{{\it Annual Review of Astronomy and Astrophysics\, }} \def\simgr{\mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$>$}}}} \def\simls{\mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$<$}}}} \def\micron{$\mu$m} \long\def\symbolfootnote[#1]#2{\begingroup% \def\thefootnote{\fnsymbol{footnote}}\footnote[#1]{#2}\endgroup} % For units of measure \newcommand\dynpercm{\nobreak\mbox{$\;$dynes\,cm$^{-1}$}} \newcommand\cmpermin{\nobreak\mbox{$\;$cm\,min$^{-1}$}} % Various bold symbols \providecommand\bnabla{\boldsymbol{\nabla}} \providecommand\bcdot{\boldsymbol{\cdot}} \newcommand\biS{\boldsymbol{S}} \newcommand\etb{\boldsymbol{\eta}} % For multiletter symbols \newcommand\Real{\mbox{Re}} % cf plain TeX's \Re and Reynolds number \newcommand\Imag{\mbox{Im}} % cf plain TeX's \Im \newcommand\Rey{\mbox{\textit{Re}}} % Reynolds number \newcommand\Pran{\mbox{\textit{Pr}}} % Prandtl number, cf TeX's \Pr product \newcommand\Pen{\mbox{\textit{Pe}}} % Peclet number \newcommand\Ai{\mbox{Ai}} % Airy function \newcommand\Bi{\mbox{Bi}} % Airy function % For sans serif characters: % The following macros are setup in cupconf.cls for sans-serif fonts in text % and math. % % \textsfi, \mathsfi : sans-serif slanted % \textsfb, \mathsfb : sans-serif bold % \textsfbi, \mathsfbi : sans-serif bold slanted (doesnt exist in CM fonts) % % For san-serif roman use \textsf and \mathsf as normal. % \newcommand\ssC{\mathsf{C}} % for sans serif C \newcommand\sfsP{\mathsfi{P}} % for sans serif sloping P \newcommand\slsQ{\mathsfbi{Q}} % for sans serif bold-sloping Q % Hat position \newcommand\hatp{\skew3\hat{p}} % p with hat \newcommand\hatR{\skew3\hat{R}} % R with hat \newcommand\hatRR{\skew3\hat{\hatR}} % R with 2 hats \newcommand\doubletildesigma{\skew2\tilde{\skew2\tilde{\Sigma}}} % italic Sigma with double tilde % array strut to make delimiters come out right size both ends \newsavebox{\astrutbox} \sbox{\astrutbox}{\rule[-5pt]{0pt}{20pt}} \newcommand{\astrut}{\usebox{\astrutbox}} \newcommand\GaPQ{\ensuremath{G_a(P,Q)}} \newcommand\GsPQ{\ensuremath{G_s(P,Q)}} \newcommand\p{\ensuremath{\partial}} \newcommand\tti{\ensuremath{\rightarrow\infty}} \newcommand\kgd{\ensuremath{k\gamma d}} \newcommand\shalf{\ensuremath{{\scriptstyle\frac{1}{2}}}} \newcommand\sh{\ensuremath{^{\shalf}}} \newcommand\smh{\ensuremath{^{-\shalf}}} \newcommand\squart{\ensuremath{{\textstyle\frac{1}{4}}}} \newcommand\thalf{\ensuremath{{\textstyle\frac{1}{2}}}} \newcommand\Gat{\ensuremath{\widetilde{G_a}}} \newcommand\ttz{\ensuremath{\rightarrow 0}} \newcommand\ndq{\ensuremath{\frac{\mbox{$\partial$}}{\mbox{$\partial$} n_q}}} \newcommand\sumjm{\ensuremath{\sum_{j=1}^{M}}} \newcommand\pvi{\ensuremath{\int_0^{\infty}% \mskip -33mu-\quad}} \newcommand\etal{\mbox{\textit{et al.}}} \newcommand\etc{etc.\ } \newcommand\eg{e.g.\ } \newtheorem{theorem}{Theorem}[section] \newtheorem{lemma}{Lemma} \newtheorem{corollary}{Corollary} \title[Massive Star Formation in the Galactic Center]{Massive Star Formation \\ in the Galactic Center} \author[D. F. Figer {\it et al.\/}]% {D\ls o\ls n\ls~F.\ns F\ls i\ls g\ls e\ls r% } \affiliation{Rochester Institute of Technology, Rochester, NY, USA\\[\affilskip] } \pubyear{2006} \volume{1} \pagerange{1} \setcounter{page}{1} \begin{document} \maketitle \begin{abstract} The Galactic center is a hotbed of star formation activity, containing the most massive star formation site and three of the most massive young star clusters in the Galaxy. Given such a rich environment, it contains more stars with initial masses above 100~\Msun\ than anywhere else in the Galaxy. This review concerns the young stellar population in the Galactic center, as it relates to massive star formation in the region. The sample includes stars in the three massive stellar clusters, the population of younger stars in the present sites of star formation, the stars surrounding the central black hole, and the bulk of the stars in the field population. The fossil record in the Galactic center suggests that the recently formed massive stars there are present-day examples of similar populations that must have been formed through star formation episodes stretching back to the time period when the Galaxy was forming. \end{abstract}