The Clowes-Campusano Large Quasar Group Survey. I. GALEX Selected Sample of Lyman Break Galaxies at z ~ 1

Creators: Haberzettl, L.; Williger, G. M.; Lauroesch, J. T.; Haines, C. P.; Valls-Gabaud, D.; Harris, K. A.; Koekemoer, A. M.; Loveday, J.; Campusano, L. E.; Clowes, R. G.; Davé, R.; Graham, M. J.; Söchting, I. K.

Abstract

The nature of galaxy structures on large scales is a key observational prediction for current models of galaxy formation. The Sloan Digital Sky Survey (SDSS) and the 2dF galaxy survey have revealed a number of structures on 40-150 h^(–1) Mpc scales at low redshifts, and some even larger ones. To constrain galaxy number densities, luminosities, and stellar populations in large structures at higher redshift, we have investigated two sheet-like structures of galaxies at z = 0.8 and 1.3 spanning 150 h^(–1) comoving Mpc embedded in large quasar groups (LQGs) extending over at least 200 h(^–1) Mpc. We present first results of an analysis of these sheet-like structures using two contiguous 1 deg Galaxy Evolution Explorer (GALEX) fields (FUV and NUV) cross-correlated with optical data from the SDSS. We derive a sample of 462 Lyman break galaxy (LBG) candidates coincident with the sheets. Using the GALEX and SDSS data, we show that the overall average spectral energy distribution of a LBG galaxy at z ~ 1 is flat (in f_λ) in the rest-frame wavelength range from 1500 Å to 4000 Å, implying evolved populations of stars in the LBGs. From the luminosity functions we get indications for overdensities in the two LQGs compared to their foreground regions. Similar conclusions come from the calculation of the 2-point correlation function, showing a 2σ overdensity for the LBGs in the z ~ 0.8 LQG on scales of 1.6 to 4.8 Mpc, indicating similar correlation scales for our LBG sample as their z ~ 3 counterparts.

Additional Information

© 2009. The American Astronomical Society. Received 2008 October 23; accepted 2009 June 23; published 2009 August 13. This publication makes use of data from GALEX Cycle 1 observations and is supported by NASA grant NNX05GK42G. Chris Hains acknowledges financial support from STFC. We thank David Koo, David Rosario, and Dave Schiminovich for their very useful comments. This paper includes data gathered with 6.5 m Magellan Telescope located at Las Campanas Observatory, Chile. L.E.C. received partial support from Center of Excellence in Astrophysics and Associated Technologies (PFB 06). Funding for the Sloan Digital Sky Survey (SDSS) and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, and the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. The SDSS ismanaged by theAstrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, The University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck- Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.

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