IR spectra, star formation rates, and metallicities in submillimeter galaxies

Details IR spectra, star formation rates, and metallicities in submillimeter galaxies IR spectra, star formation rates, and metallicities in submillimeter galaxies

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008sptz.prop50324r&link_type=abstract

Spitzer Proposal ID #50324

Physics

Scientific paper

Sub-millimeter continuum observations probe the long-wavelength side of far-IR dust emission from distant galaxies, detecting cold dust and dusty galaxies at higher redshifts. This makes the sub-mm uniquely sensitive to types of dusty galaxies that are disfavored by shorter-wavelength selection, such as at 24 microns. However, for the same reason, only a relatively small number of sub-mm galaxies have high-quality Spitzer/IRS spectra. We propose to obtain IRS spectra of a carefully selected sample of 7 galaxies with sub-mm detections, firm radio and infrared cross-IDs and positions, sufficient 24 micron flux, and in several cases, detections at 70 and even 160 microns. These galaxies are in fields with deep IRAC and MIPS photometry and sensitive multiwavelength coverage from X-ray to radio. The IRS spectra will determine the restframe mid-IR PAH emission, silicate absorption, and continuum shape. These features along with far-IR dust temperatures and multiwavelength data will enable us to construct SEDs for cool, dusty galaxies at z ~ 0.5-2, and to determine whether the properties of such galaxies are similar to local unusually cool ULIRGs (e.g. Arp 220) or have evolved with redshift. We are also proposing to take deep IRS exposures to measure Brackett alpha, [Ne II] and [Ne III] mid-IR lines in 3 of the galaxies. These lines yield measurements of star formation rate and metallicity that are unaffected by extinction. We will test whether IR-luminous galaxies at z~1 are lower metallicity than local examples, and whether metallicity evolution is affecting far-IR estimates of star formation rate. This is part 2 of program 50323.

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