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The stellar masses of ∼40 000 UV selected Galaxies from the WiggleZ survey at 0.3 < z < 1.0: analogues of Lyman break galaxies?

Banerji, Manda and Forster, Karl and Martin, D. Christopher and Wyder, Ted K. (2013) The stellar masses of ∼40 000 UV selected Galaxies from the WiggleZ survey at 0.3 < z < 1.0: analogues of Lyman break galaxies? Monthly Notices of the Royal Astronomical Society, 431 (3). pp. 2209-2229. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20130612-145312186

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Abstract

We characterize the stellar masses and star formation rates in a sample of ∼40 000 spectroscopically confirmed UV-luminous galaxies at 0.3 < z < 1.0 selected from within the WiggleZ Dark Energy Survey. In particular, we match this UV bright population to wide-field infrared surveys such as the near-infrared (NIR) UKIDSS Large Area Survey (LAS) and the mid-infrared Wide-Field Infrared Survey Explorer (WISE) All-Sky Survey. We find that ∼30 per cent of the UV-luminous WiggleZ galaxies, corresponding to the brightest and reddest subset, are detected at >5σ in the UKIDSS-LAS at all redshifts. An even more luminous subset of 15 per cent are also detected in the WISE 3.4 and 4.6 μm bands. In addition, 22 of the WiggleZ galaxies are extremely luminous at 12 and 22 μm and have colours consistent with being star formation dominated. We compute stellar masses for this very large sample of extremely blue galaxies and quantify the sensitivity of the stellar mass estimates to various assumptions made during the spectral energy distribution (SED) fitting. The median stellar masses are log10(M_*/M_⊙) = 9.6 ± 0.7, 10.2 ± 0.5 and 10.4 ± 0.4 for the IR undetected, UKIDSS detected and UKIDSS+WISE detected galaxies, respectively. We demonstrate that the inclusion of NIR photometry can lead to tighter constraints on the stellar masses by bringing down the upper bound on the stellar mass estimate. The mass estimates are found to be most sensitive to the inclusion of secondary bursts of star formation as well as changes in the stellar population synthesis models, both of which can lead to median discrepancies of the order of 0.3 dex in the stellar masses. We conclude that even for these extremely blue galaxies, different SED fitting codes therefore produce extremely robust stellar mass estimates. We find, however, that the best-fitting M/L_K is significantly lower than that predicted by simple optical colour-based estimators for many of the WiggleZ galaxies. The simple colour-based estimator overpredicts M/L_K by ∼0.4 dex on average. The effect is more pronounced for bluer galaxies with younger best-fitting ages. The WiggleZ galaxies have star formation rates of 3–10 M_⊙ yr^(−1) and mostly lie at the upper end of the main sequence of star-forming galaxies at these redshifts. Their rest-frame UV luminosities and stellar masses are comparable to both local compact UV-luminous galaxies as well as Lyman break galaxies at z ∼ 2–3. The stellar masses from this paper will be made publicly available with the next WiggleZ data release.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1093/mnras/stt320DOIArticle
http://mnras.oxfordjournals.org/content/431/3/2209.abstractPublisherArticle
http://dx.doi.org/10.1093/mnras/stu2478ErrataErratum
http://mnras.oxfordjournals.org/content/447/1/325ErrataErratum
Additional Information:© 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2013 February 18. In original form 2013 February 12. Received 2012 December 4. First published online: March 20, 2013. We thank the anonymous referee for a constructive report that has helped improve this paper. MB acknowledges Paul Hewett and Richard McMahon for many constructive discussions and Claudia Maraston and Joel Brownstein for access to the BOSS LRG stellar masses. MB wishes to acknowledge financial support from the STFC through grants held both at the Institute of Astronomy, Cambridge, and University College London. We acknowledge financial support from the Australian Research Council (grants DP1093738, DP0772084, LX0881951, LE0668442), Swinburne University of Technology, the University of Queensland and the Anglo-Australian Observatory for the WiggleZ survey. The WiggleZ survey would not be possible without the dedicated work of the staff of the Australian Astronomical Observatory in the development and support of the AAOmega spectrograph, and the running of the AAT. KG also acknowledges support from Australian Research Council grant DP1094370 for galaxy evolution studies. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASAs support for construction, operation and science analysis for the GALEX mission, developed in cooperation with the Centre National dEtudes Spatiales of France and the Korean Ministry of Science and Technology.
Group:Space Astrophysics Laboratory
Funders:
Funding AgencyGrant Number
Science and Technology Facilities Council (STFC)UNSPECIFIED
Australian Research Council DP1093738
Australian Research CouncilDP0772084
Australian Research CouncilLX0881951
Australian Research CouncilLE0668442
Swinburne University of TechnologyUNSPECIFIED
University of QueenslandUNSPECIFIED
Anglo-Australian Observatory UNSPECIFIED
Australian Research CouncilDP1094370
Subject Keywords: galaxies: evolution galaxies: formation galaxies: stellar content
Record Number:CaltechAUTHORS:20130612-145312186
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20130612-145312186
Official Citation: Manda Banerji, Karl Glazebrook, Chris Blake, Sarah Brough, Matthew Colless, Carlos Contreras, Warrick Couch, Darren J. Croton, Scott Croom, Tamara M. Davis, Michael J. Drinkwater, Karl Forster, David Gilbank, Mike Gladders, Ben Jelliffe, Russell J. Jurek, I-hui Li, Barry Madore, D. Christopher Martin, Kevin Pimbblet, Gregory B. Poole, Michael Pracy, Rob Sharp, Emily Wisnioski, David Woods, Ted K. Wyder, and H. K. C. Yee The stellar masses of ∼ 40 000 UV selected Galaxies from the WiggleZ survey at 0.3<z<1.0: analogues of Lyman break galaxies? MNRAS (May 21, 2013) Vol. 431 2209-2229 first published online March 20, 2013 doi:10.1093/mnras/stt320
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:38930
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:12 Jun 2013 22:57
Last Modified:28 Aug 2016 20:16

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