Other
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007sptz.prop40441h&link_type=abstract
Spitzer Proposal ID #40441
Other
Scientific paper
The formative phase of the most massive galaxies may be extremely luminous, characterized by intense star formation and AGN activity. Few such galaxies have been unambiguously identified at high redshift, and thus far we have been restricted to studying low-redshift ultraluminous infrared galaxies as possible analogs. We have recently discovered a sample of objects which may represent this early phase in galaxy formation, and we are undertaking an extensive multiwavelength study of this population. These objects are optically extremely faint (R > 25), but bright at mid-infrared wavelengths (f(24) >= 0.5 mJy). Mid-infrared spectroscopy with Spitzer/IRS reveals that they lie at 2 < z < 3, implying luminosities of ~10^13 Lsun. Their mid-infrared SEDs fall into two broad categories. Sources with brighter 24 micron flux densities exhibit power-law SEDs and mid-infrared spectra characteristic of AGN; fainter sources show the redshifted 1.6 micron bump from a stellar population and mid-infrared PAH emission characteristic of star formation. How do these star-forming extreme bump sources relate to other high-redshift populations, such as the submillimeter galaxies? To find out, we have obtained IRS spectroscopy and MIPS 70 and 160 micron imaging for 16 extreme bump sources at z~2. We aim to obtain a similar data set for a sample of 8 extreme bump sources at 2.5 < z < 3. In this GTO proposal, we request 24 hours to obtain low-resolution IRS spectroscopy of these 8 sources. Our primary goals are to verify their photometric redshifts and to determine whether AGN activity or star formation dominates the mid-infrared luminosity. Accurate redshifts are necessary for estimating the bolometric luminosities, star formation rates, and stellar masses for these sources. In a separate small GO proposal, we request 70 and 160 micron imaging of these same sources in order to improve on the bolometric luminosity and star formation estimates that we can obtain with 24 micron data alone.
Desai Vandana
Houck James R.
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