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Herschel-ATLAS galaxy counts and high-redshift luminosity functions: the formation of massive early-type galaxies

Lapi, A., González-Nuevo, J., Fan, L., Bressan, A., De Zotti, G., Danese, L., Negrello, Mattia, Dunne, Loretta, Eales, Stephen, Maddox, Steve, Auld, R., Baes, M., Bonfield, D. G., Buttiglione, S., Cava, A., Clements, D. L., Cooray, A., Dariush, A., Dye, S., Fritz, J., Herranz, D., Hopwood, R., Ibar, E., Ivison, R, Jarvis, M. J., Kaviraj, S., López-Caniego, M., Massardi, M., Micha?owski, M. J., Pascale, Enzo, Pohlen, M., Rigby, E., Rodighiero, G., Serjeant, S., Smith, D. J. B., Temi, P., Wardlow, J. and van der Werf, P. 2011. Herschel-ATLAS galaxy counts and high-redshift luminosity functions: the formation of massive early-type galaxies. The Astrophysical Journal 742 (1) , p. 24. 10.1088/0004-637X/742/1/24

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Abstract

Exploiting the Herschel Astrophysical Terahertz Large Area Survey Science Demonstration Phase survey data, we have determined the luminosity functions (LFs) at rest-frame wavelengths of 100 and 250 ?m and at several redshifts z gsim 1, for bright submillimeter galaxies with star formation rates (SFRs) gsim 100 M ? yr?1. We find that the evolution of the comoving LF is strong up to z ? 2.5, and slows down at higher redshifts. From the LFs and the information on halo masses inferred from clustering analysis, we derived an average relation between SFR and halo mass (and its scatter). We also infer that the timescale of the main episode of dust-enshrouded star formation in massive halos (M H gsim 3 × 1012 M ?) amounts to ~7 × 108?yr. Given the SFRs, which are in the range of 102-103 M ? yr?1, this timescale implies final stellar masses of the order of 1011-1012 M ?. The corresponding stellar mass function matches the observed mass function of passively evolving galaxies at z gsim 1. The comparison of the statistics for submillimeter and UV-selected galaxies suggests that the dust-free, UV bright phase is gsim 102 times shorter than the submillimeter bright phase, implying that the dust must form soon after the onset of star formation. Using a single reference spectral energy distribution (SED; the one of the z ? 2.3 galaxy SMM J2135-0102), our simple physical model is able to reproduce not only the LFs at different redshifts >1 but also the counts at wavelengths ranging from 250 ?m to ?1?mm. Owing to the steepness of the counts and their relatively broad frequency range, this result suggests that the dispersion of submillimeter SEDs of z > 1 galaxies around the reference one is rather small.

Item Type: Article
Date Type: Publication
Status: Published
Schools: Physics and Astronomy
Subjects: Q Science > QC Physics
Publisher: IHOP Publishing
ISSN: 0004637X
Last Modified: 25 Dec 2017 21:02
URI: http://orca.cf.ac.uk/id/eprint/84012

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