THE CLUSTERING OF EXTREMELY RED OBJECTS

Journal Article · Sun Feb 10 04:00:00 EST 2013 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/764/1/31· OSTI ID:22167828

Palamara, David P.; Brown, Michael J. I.; Pimbblet, Kevin A. ^[1]; Jannuzi, Buell T.; Dey, Arjun ^[2]; Stern, Daniel ^[3]; Weiner, Benjamin J.; Rieke, Marcia ^[4]; Ashby, Matthew L. N. ^[5]; Kochanek, C. S. ^[6]; Gonzalez, Anthony ^[7]; Brodwin, Mark ^[8]; Le Floc'h, Emeric ^[9]

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1. School of Physics, Monash University, Clayton, Victoria 3800 (Australia)
2. National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719 (United States)
3. Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 (United States)
4. Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ, 85721 (United States)
5. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)
6. Department of Astronomy, The Ohio State University, 140, West 18th Avenue, Columbus, OH 43210 (United States)
7. Department of Astronomy, University of Florida, Gainesville, FL 32611-2055 (United States)
8. Department of Physics and Astronomy, University of Missouri, 5110 Rockhill Road, Kansas City, MO 64110 (United States)
9. Laboratoire AIM, CEA-Saclay-CNRS-Universite Paris Diderot, Service d'Astrophysique, Orme des Merisiers, F-91191 Gif-sur-Yvette (France)

We measure the clustering of extremely red objects (EROs) in Almost-Equal-To 8 deg{sup 2} of the NOAO Deep Wide Field Survey Booetes field in order to establish robust links between ERO (z Almost-Equal-To 1.2) and local galaxy (z < 0.1) populations. Three different color selection criteria from the literature are analyzed to assess the consequences of using different criteria for selecting EROs. Specifically, our samples are (R - K{sub s} ) > 5.0 (28, 724 galaxies), (I - K{sub s} ) > 4.0 (22, 451 galaxies), and (I - [3.6]) > 5.0 (64, 370 galaxies). Magnitude-limited samples show the correlation length (r {sub 0}) to increase for more luminous EROs, implying a correlation with stellar mass. We can separate star-forming and passive ERO populations using the (K{sub s} - [24]) and ([3.6] - [24]) colors to K{sub s} = 18.4 and [3.6] = 17.5, respectively. Star-forming and passive EROs in magnitude-limited samples have different clustering properties and host dark halo masses and cannot be simply understood as a single population. Based on the clustering, we find that bright passive EROs are the likely progenitors of {approx}> 4L* elliptical galaxies. Bright EROs with ongoing star formation were found to occupy denser environments than star-forming galaxies in the local universe, making these the likely progenitors of {approx}> L* local ellipticals. This suggests that the progenitors of massive {approx}> 4L* local ellipticals had stopped forming stars by z {approx}> 1.2, but that the progenitors of less massive ellipticals (down to L*) can still show significant star formation at this epoch.

• OSTI ID: 22167828
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 764; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
COLOR MODEL
COSMOLOGY
GALACTIC EVOLUTION
MASS
MILKY WAY
RED SHIFT
STARS
STATISTICS
UNIVERSE