IR and UV Galaxies at z=0.6 --- Evolution of Dust Attenuation and Stellar Mass

Details IR and UV Galaxies at z=0.6 --- Evolution of Dust Attenuation and Stellar Mass IR and UV Galaxies at z=0.6 --- Evolution of Dust Attenuation and Stellar Mass

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.5204x&link_type=abstract

American Astronomical Society, AAS Meeting #211, #52.04; Bulletin of the American Astronomical Society, Vol. 39, p.820

Astronomy and Astrophysics

Astronomy

Scientific paper

We study dust attenuation and stellar mass of z 0.6 star-forming galaxies using new SWIRE observations in IR and GALEX observations in UV. Two samples are selected from the SWIRE and GALEX source catalogs in the SWIRE/GALEX field ELAIS-N1-00 (Ω= 0.8 deg2). The UV selected sample has 600 galaxies with photometric redshift (hereafter photo-z) 0.5 < z < 0.7 and NUV< 23.5 (corresponding to LFUV > 109.6 Lsun). The IR selected sample contains 430 galaxies with f24μ > 0.2 mJy (Ldust > 1010.8 Lsun) in the same photo-z range. It is found that the mean Ldust/LFUV ratios of the z=0.6 UV galaxies are consistent with that of their z=0 counterparts of the same LFUV. For IR galaxies, the mean Ldust/LFUV ratios of the z=0.6 LIRGs (Ldust 1011 Lsun) are about a factor of 2 lower than local LIRGs, whereas z=0.6 ULIRGs (Ldust 1012 Lsun) have the same mean Ldust/LFUV ratios as their local counterparts. This is consistent with the hypothesis that the dominant component of LIRG population has changed from large, gas rich spirals at z > 0.5 to major-mergers at z=0. The stellar mass of z=0.6 UV galaxies of LFUV < 1010.2 Lsun is about a factor 2 less than their local counterparts of the same luminosity, indicating growth of these galaxies. The mass of z=0.6 UV luminous galaxies (UVLGs: LFUV > 1010.2 Lsun) and IR selected galaxies, which are nearly exclusively LIRGs and ULIRGs, is the same as their local counterparts.

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