Basu-Zych, Antara R. and Schiminovich, David and Heinis, Sebastien and Overzier, Roderik and Heckman, Tim and Zamojski, Michel and Ilbert, Olivier and Koekemoer, Anton M. and Barlow, Tom A. and Bianchi, Luciana and Conrow, Tim and Donas, Jose and Forster, Karl and Friedman, Peter G. and Lee, Young-Wook and Madore, Barry F. and Martin, D. Christopher and Milliard, Bruno and Morrissey, Patrick and Neff, Susan G. and Rich, R. Michael and Salim, Samir and Seibert, Mark and Small, Todd A. and Szalay, Alex S. and Wyder, Ted K. and Yi, Sukyoung K. (2009) Studying Large- and Small-Scale Environments of Ultraviolet Luminous Galaxies. Astrophysical Journal, 699 (2). pp. 1307-1320. ISSN 0004-637X http://resolver.caltech.edu/CaltechAUTHORS:20090806-102256755
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Studying the environments of 0.4 < z < 1.2 ultraviolet (UV)-selected galaxies, as examples of extreme star-forming galaxies (with star formation rates (SFRs) in the range of 3-30 M_☉ yr^(–1)), we explore the relationship between high rates of star formation, host halo mass, and pair fractions. We study the large- and small-scale environments of local ultraviolet luminous galaxies (UVLGs) by measuring angular correlation functions. We cross-correlate these systems with other galaxy samples: a volume-limited sample (ALL), a blue luminous galaxy sample, and a luminous red galaxy (LRG) sample. We determine the UVLG comoving correlation length to be r_0 = 4.8^(+11.6)_(–2.4) h^(–1) Mpc at z = 1.0, which is unable to constrain the halo mass for this sample. However, we find that UVLGs form close (separation <30 kpc) pairs with the ALL sample, but do not frequently form pairs with LRGs. A rare subset of UVLGs, those with the highest FUV surface brightnesses, are believed to be local analogs of high-redshift Lyman break galaxies (LBGs) and are called Lyman break analogs (LBAs). LBGs and LBAs share similar characteristics (i.e., color, size, surface brightness, specific SFRs, metallicities, and dust content). Recent Hubble Space Telescope images of z ~ 0.2 LBAs show disturbed morphologies, signs of mergers and interactions. UVLGs may be influenced by interactions with other galaxies and we discuss this result in terms of other high star-forming, merging systems.
|Additional Information:||© 2009. The American Astronomical Society. Received 2008 September 13; accepted 2009 March 26; published 2009 June 23. 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. The HST COSMOS program was supported through NASA grant HST-GO- 09822. More information on the COSMOS survey is available at http://www.astro.caltech.edu/cosmos. We thank Michael Blanton for access to the IDL kcorrect (version 4.1.4) analysis package. This work has greatly benefitted from the careful comments and suggestions made by the anonymous referee. A.R.B. gratefully recognizes Ian McGreer and Andrei Mesinger for their contributions to this analysis, and David Hogg for insightful discussions.|
|Subject Keywords:||galaxies: evolution galaxies: halos galaxies: interactions galaxies: starburst methods: statistical|
|Official Citation:||Studying Large- and Small-Scale Environments of Ultraviolet Luminous Galaxies Antara R. Basu-Zych, David Schiminovich, Sebastien Heinis, Roderik Overzier, Tim Heckman, Michel Zamojski, Olivier Ilbert, Anton M. Koekemoer, Tom A. Barlow, Luciana Bianchi, Tim Conrow, Jose Donas, Karl G. Forster, Peter G. Friedman, Young-Wook Lee, Barry F. Madore, D. Christopher Martin, Bruno Milliard, Patrick Morrissey, Susan G. Neff, R. Michael Rich, Samir Salim, Mark Seibert, Todd A. Small, Alex S. Szalay, Ted K. Wyder, and Sukyoung Yi 2009 ApJ 699 1307-1320 doi: 10.1088/0004-637X/699/2/1307|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Ruth Sustaita|
|Deposited On:||01 Sep 2009 22:36|
|Last Modified:||04 Mar 2013 17:51|
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