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T<FONT size=-1>HE</FONT> A<FONT size=-1>STROPHYSICAL</FONT> J<FONT size=-1>OURNAL</FONT>, 488:L79<IMG SRC="/ucp-entities/ndash.gif" ALT="–" ALIGN="BOTTOM">L82, 1997 October 20
<BR>© 1997. The American Astronomical Society. All rights reserved. Printed in U.S.A.
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<H1 ALIGN="CENTER"><A NAME="title">Molecular Lines as Diagnostics of High-Redshift Objects</H1>
<H2 ALIGN="CENTER"><A NAME="authorlist"><A NAME="au1">J<FONT size=-1>OSEPH</FONT> S<FONT size=-1>ILK</FONT></A></H2>
<H3 ALIGN="CENTER">Departments of Astronomy and Physics, University of California, 601 Campbell Hall, Berkeley, CA 94720</H3>
<H2 ALIGN="CENTER"><FONT size=-1>AND</FONT></H2>
<H2 ALIGN="CENTER"><A NAME="au2">M<FONT size=-1>ARCO</FONT> S<FONT size=-1>PAANS</FONT></A></H2>
<H3 ALIGN="CENTER">Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218-2686</H3>
<H2 ALIGN="CENTER"></A></H2>
<H4 ALIGN="CENTER"><I>Received 1997 June 10; accepted 1997 August 18; published 1997 September 17</I></H4>
<BR><H3 ALIGN="CENTER"><A NAME="abstract">ABSTRACT</A></H3>
<P> Models are presented for CO rotational
line emission by high-redshift starburst galaxies. The influence of the
cosmic microwave background on the thermal balance and the level
populations of atomic and molecular species is explicitly included.
Predictions are made for the observability of starburst galaxies through
line and continuum emission between <I>z</I>=5 and <I>z</I>=30. It is found
that the Millimeter Array could detect a starburst galaxy with
<IMG SRC="/ucp-entities/sim.gif" ALT="∼" ALIGN="BOTTOM">10<SUP>5</SUP>
Orion regions, corresponding to a star formation rate of about
30 <I>M</I><SUB><IMG SRC="/ucp-entities/odot.gif" ALT="⊙" ALIGN="BOTTOM"></SUB>
yr<SUP>-1</SUP>, equally well at <I>z</I>=5 or <I>z</I>=30 because of the
increasing cosmic microwave background temperature with redshift.
Line emission is a potentially more powerful probe than dust continuum
emission of very high redshift objects.</P>
<P><A NAME="keywords"><I>Subject headings: </I></A>cosmology: theory<IMG SRC="/ucp-entities/mdash.gif" ALT="—" ALIGN="BOTTOM">galaxies: evolution<IMG SRC="/ucp-entities/mdash.gif" ALT="—" ALIGN="BOTTOM">galaxies: starburst<IMG SRC="/ucp-entities/mdash.gif" ALT="—" ALIGN="BOTTOM">ISM: molecules</P>
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<H3>CONTENTS</H3>
<UL>
<LI>1. <A HREF="sc1.html#sc1">INTRODUCTION</A></LI>
<LI>2. <A HREF="sc2.html#sc2">COSMOLOGY</A></LI>
<LI>3. <A HREF="sc3.html#sc3">THE MODEL</A></LI>
<LI>4. <A HREF="sc4.html#sc4">RESULTS AND DISCUSSION</A></LI>
<LI><A HREF="ack.html">ACKNOWLEDGMENTS</A></LI>
<LI><A HREF="refs.html">REFERENCES</A></LI>
<LI><A HREF="figs.html">FIGURES</A></LI>
<LI><A HREF="/cgi-bin/get_forward?1997ApJ...488L..79S">REFERENCES TO THIS ARTICLE</A></LI>
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