------------------------------------------------------------------------ moving_iron.tex ApJL Submitted Date: Mon, 20 Nov 2006 16:29:14 -0800 X-Mailer: Apple Mail (2.752.2) X-MailScanner-Information: Please contact postmaster@aoc.nrao.edu for more information X-MailScanner: Found to be clean X-MailScanner-SpamCheck: not spam, SpamAssassin (score=0.001, required 5, autolearn=disabled, HTML_MESSAGE 0.00) X-MailScanner-From: mmuno@srl.caltech.edu X-Spam-Status: No --Apple-Mail-22--1069323280 Content-Transfer-Encoding: 7bit Content-Type: text/plain; charset=US-ASCII; delsp=yes; format=flowed %astro-ph/0611651 \documentclass[12pt,preprint]{aastex} \begin{document} \title{Discovery of Variable Iron Fluorescence from Reflection Nebulae in the Galactic Center} \author{ M. P. Muno\altaffilmark{1}, F. K. Baganoff\altaffilmark{2}, W. N. Brandt,\altaffilmark{3}, S. Park,\altaffilmark{3} \& M. R. Morris \altaffilmark{4}} Technology, Pasadena, CA 91125; mmuno@srl.caltech.edu} \altaffiltext{2}{Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139; fkb@space.mit.edu} \altaffiltext{3}{Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802; niel,park@astro.psu.edu} \altaffiltext{4}{Department of Physics and Astronomy, University of California, Los Angeles, CA 90095; morris@astro.ucla.edu} \begin{abstract} Based on three years of deep observations of the Galactic center with the {\it Chandra} X-ray Observatory, we report the discovery of changes in the intensities and morphologies of two hard X-ray nebulosities. The nebulosities are dominated by fluorescent iron emission, and are coincident with molecular clouds. The morphological changes are manifest on parsec scales, which requires that these iron features are scattered X-rays from a 2 or 3-year-long outburst of a point source (either \sgrastar\ or an X-ray binary) with a luminosity of at least $10^{37}$ erg s$^{-1}$. The variability precludes the hypotheses that these nebulae either are produced by keV electrons bombarding molecular clouds, or are iron-rich ejecta from supernovae. Moreover, the morphologies of the reflection nebulae implies that the dense regions of the clouds are filamentary, with widths of $\approx$0.3 pc and lengths of $\approx$ 2 pc. \end{abstract} \keywords{Galaxy: center --- ISM: clouds --- X-rays: ISM} \end{document} Michael Muno (626) 395-2336 110 Downs MC 220-47 Caltech Pasadena, CA 91125 mmuno@srl.caltech.edu --Apple-Mail-22--1069323280 Content-Transfer-Encoding: quoted-printable Content-Type: text/html; charset=ISO-8859-1
\documentclass[12pt,preprint]= {aastex}

\begin{document}
\title{Discovery of = Variable Iron Fluorescence from Reflection Nebulae in the Galactic = Center}

\author{
M. P. = Muno\altaffilmark{1}, F. K. Baganoff\altaffilmark{2}, W. N. = Brandt,\altaffilmark{3}, S. Park,\altaffilmark{3} \& M. R. = Morris\altaffilmark{4}}

\altaffiltext{1}{Space = Radiation Laboratory, California Institute of Technology, Pasadena, CA = 91125; mmuno@srl.caltech.edu}
\altaffiltext{2}{Kavli Institute for Astrophysics and Space = Research,
Massachusetts Institute of Technology, Cambridge, MA = 02139; fkb@space.mit.edu}
\altaff= iltext{3}{Department of Astronomy and Astrophysics,
The = Pennsylvania State University, University Park, PA 16802; niel,park@astro.psu.edu}
\alta= ffiltext{4}{Department of Physics and Astronomy, University of = California,
Los Angeles, CA 90095; morris@astro.ucla.edu}

\begin{abstract}
Ba= sed on three years of deep observations of the Galactic center = with
the {\it Chandra} X-ray Observatory, we report the = discovery of changes in
the intensities and morphologies of = two hard X-ray nebulosities. The
nebulosities are dominated by = fluorescent iron emission, and are
coincident with molecular = clouds. The morphological changes are manifest
on parsec = scales, which requires that these iron features are scattered =
X-rays from a 2 or 3-year-long outburst of a point source =
(either \sgrastar\ or an X-ray binary) with a luminosity of = at least
$10^{37}$ erg s$^{-1}$.=A0 The variability precludes = the
hypotheses that these nebulae either are produced by keV = electrons
bombarding molecular clouds, or are iron-rich ejecta = from
supernovae.=A0 Moreover, the morphologies of the = reflection nebulae implies
that the dense regions of the = clouds are filamentary, with
widths of $\approx$0.3 pc and = lengths of $\approx$ 2 pc.
\end{abstract}

\keywords{Galaxy: center = --- ISM: clouds --- X-rays: ISM}

\end{document}

=

Michael Muno

(626)=A0395-2336

110 Downs
MC = 220-47
Caltech
Pasadena, CA 91125

=

=

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