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The WiggleZ Dark Energy Survey: star formation in UV-luminous galaxies from their luminosity functions

Jurek, Russell J. and Forster, Karl and Martin, D. Christopher and Wyder, Ted K. (2013) The WiggleZ Dark Energy Survey: star formation in UV-luminous galaxies from their luminosity functions. Monthly Notices of the Royal Astronomical Society, 434 (1). pp. 257-281. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20131115-120041384

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Abstract

We present the ultraviolet (UV) luminosity function of galaxies from the GALEX Medium Imaging Survey with measured spectroscopic redshifts from the first data release of the WiggleZ Dark Energy Survey. Our sample consists of 39 996 NUV < 22.8 emission line galaxies in the redshift range 0.1 < z < 0.9. This sample selects galaxies with high star formation rates: at 0.6 < z < 0.9 the median star formation rate is at the upper 95th percentile of optically selected (r < 22.5) galaxies and the sample contains about 50 per cent of all NUV < 22.8, 0.6 < z < 0.9 starburst galaxies within the volume sampled. The most luminous galaxies in our sample (−21.0 > M_NUV > −22.5) evolve very rapidly with a number density declining as (1 + z)5±1 from redshift z = 0.9 to 0.6. These starburst galaxies (MNUV < −21 is approximately a star formation rate of 30 M_⊙ yr^−1) contribute about 1 per cent of cosmic star formation over the redshift range z = 0.6–0.9. The star formation rate density of these very luminous galaxies evolves rapidly, as (1 + z)^4±1. Such a rapid evolution implies that the majority of star formation in these large galaxies must have occurred before z = 0.9. We measure the UV luminosity function in Δz = 0.05 redshift intervals spanning 0.1 < z < 0.9, and provide analytic fits to the results. Our measurements of the luminosity function over this redshift range probe further into the bright end (1–2 mag further) than previous measurements, e.g. Arnouts et al., Budavári et al. and Treyer et al., due to our much larger sample size and sampled volume. At all redshifts z > 0.55 we find that the bright end of the luminosity function is not well described by a pure Schechter function due to an excess of very luminous (MNUV < −22) galaxies. These luminosity functions can be used to create a radial selection function for the WiggleZ survey or test models of galaxy formation and evolution. Here we test the AGN feedback model in Scannapieco, Silk & Bouwens, and find that this AGN feedback model requires AGN feedback efficiency to vary with one or more of the following: stellar mass, star formation rate and redshift.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1093/mnras/stt1015DOIArticle
http://mnras.oxfordjournals.org/content/434/1/257PublisherArticle
http://arxiv.org/abs/1306.4031arXivDiscussion Paper
Additional Information:© 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2013 June 6. Received 2013 May 2; in original form 2012 November 17. First published online: July 8, 2013. This project would not have been possible without the superb AAOmega/2dF facility provided by the Australian Astronomical Observatory. We wish to thank all the AAO staff for their support, especially the night assistants, support astronomers and Russell Cannon (who greatly assisted with the quality control of the 2dF system). We wish to acknowledge financial support from the Australian Research Council (grants DP0772084, DP1093738 and LX0881951 directly for the WiggleZ project, and grant LE0668442 for programming support), Swinburne University of Technology, the University of Queensland, the Anglo-Australian Observatory and the Gregg Thompson Dark Energy Travel Fund. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA’s support for construction, operation and science analysis for the GALEX mission, developed in cooperation with the Centre National d’Etudes Spatiales of France and the Korean Ministry of Science and Technology. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, theMax Planck Society and theHigher Education Funding Council for England. The SDSS website is http://www.sdss.org/. Funding for the DEEP2 survey has been provided by NSF grants AST95-09298, AST-0071048, AST-0071198, AST-0507428 and AST-0507483 as well as NASA LTSA grant NNG04GC89G. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.
Group:Space Astrophysics Laboratory
Funders:
Funding AgencyGrant Number
Australian Research CouncilDP0772084
Australian Research CouncilDP1093738
Australian Research CouncilLX0881951
Swinburne University of TechnologyUNSPECIFIED
University of QueenslandUNSPECIFIED
Anglo-Australian ObservatoryUNSPECIFIED
Gregg Thompson Dark Energy Travel FundUNSPECIFIED
NASAUNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
NSFUNSPECIFIED
Department of Energy (DOE)UNSPECIFIED
Japanese MonbukagakushoUNSPECIFIED
Max Planck SocietyUNSPECIFIED
Higher Education Funding Council for EnglandUNSPECIFIED
NSFAST95-09298
NSFAST-0071048
NSFAST-0071198
NSFAST-0507428
NSFAST-0507483
NASA LTSANNG04GC89G
W. M. Keck FoundationUNSPECIFIED
Subject Keywords:galaxies: luminosity function, mass function; galaxies: starburst; ultraviolet: galaxies
Record Number:CaltechAUTHORS:20131115-120041384
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20131115-120041384
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:42503
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:18 Nov 2013 15:51
Last Modified:28 Aug 2016 20:14

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