Cardiff University | Prifysgol Caerdydd ORCA
Online Research @ Cardiff 
WelshClear Cookie - decide language by browser settings

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, M., Dunne, L., Eales, Stephen Anthony, Maddox, S., Auld, Robbie Richard, Baes, M., Bonfield, D. G., Buttiglione, S., Cava, A., Clements, D. L., Cooray, A., Dariush, Aliakbar, Dye, Simon, Fritz, J., Herranz, D., Hopwood, R., Ibar, E., Ivison, R., Jarvis, M. J., Kaviraj, S., López-Caniego, M., Massardi, M., Michałowski, M. J., Pascale, Enzo, Pohlen, Michael, 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. Astrophysical Journal 742 (1) , 24. 10.1088/0004-637X/742/1/24

Full text not available from this repository.

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 μm 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 μm 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 > QB Astronomy
Uncontrolled Keywords: galaxies: evolution; galaxies: formation; galaxies: high-redshift; submillimeter: galaxies
Publisher: Institute of Physics
ISSN: 0004-637X
Last Modified: 06 Mar 2019 20:43
URI: http://orca-mwe.cf.ac.uk/id/eprint/19404

Citation Data

Cited 146 times in Google Scholar. View in Google Scholar

Cited 111 times in Scopus. View in Scopus. Powered By Scopus® Data

Actions (repository staff only)

Edit Item Edit Item