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Title:
The Evolution of Galaxy Mergers and Morphology at z < 1.2 in the Extended Groth Strip
Authors:
Lotz, Jennifer M.; Davis, M.; Faber, S. M.; Guhathakurta, P.; Gwyn, S.; Huang, J.; Koo, D. C.; Le Floc'h, E.; Lin, Lihwai; Newman, J.; Noeske, K.; Papovich, C.; Willmer, C. N. A.; Coil, A.; Conselice, C. J.; Cooper, M.; Hopkins, A. M.; Metevier, A.; Primack, J.; Rieke, G.; Weiner, B. J.
Affiliation:
AA(National Optical Astronomical Observatories, 950 North Cherry Avenue, Tucson, AZ 85719; .; Leo Goldberg Fellow.), AB(Department of Astronomy, University of California, Berkeley, CA.), AC(UCO/Lick Observatory, Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA.), AD(UCO/Lick Observatory, Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA.), AE(Department of Physics and Astronomy, University of Victoria, Victoria, BC, Canada.), AF(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA.), AG(UCO/Lick Observatory, Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA.), AH(Institute for Astronomy, University of Hawaii, Honolulu, HI.; Observatoire de Paris, Meudon, France.; Spitzer Fellow.), AI(UCO/Lick Observatory, Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA.), AJ(Lawrence Berkeley National Laboratory, Livermore, CA.; Hubble Fellow.), AK(UCO/Lick Observatory, Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA.), AL(Spitzer Fellow.; Steward Observatory, University of Arizona, Tucson, AZ.), AM(Steward Observatory, University of Arizona, Tucson, AZ.), AN(Hubble Fellow.; Steward Observatory, University of Arizona, Tucson, AZ.), AO(School of Physics and Astronomy, University of Nottingham, Nottingham, UK.), AP(Department of Astronomy, University of California, Berkeley, CA.), AQ(School of Physics, University of Sydney, Sydney, Australia.), AR(UCO/Lick Observatory, Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA.; NSF Astronomy and Astrophysics Postdoctoral Fellow.), AS(Department of Physics, University of California, Santa Cruz.), AT(Steward Observatory, University of Arizona, Tucson, AZ.), AU(Steward Observatory, University of Arizona, Tucson, AZ.)
Publication:
The Astrophysical Journal, Volume 672, Issue 1, pp. 177-197. (ApJ Homepage)
Publication Date:
01/2008
Origin:
UCP
ApJ Keywords:
Galaxies: Evolution, Galaxies: High-Redshift, Galaxies: Interactions, Galaxies: Structure
DOI:
10.1086/523659
Bibliographic Code:
2008ApJ...672..177L

Abstract

We present the quantitative rest-frame B morphological evolution and galaxy merger fraction at 0.2<z<1.2 as observed by the All-Wavelength Extended Groth Strip International Survey (AEGIS). We use the Gini coefficient and M20 to identify major mergers and classify galaxy morphology for a volume-limited sample of 3009 galaxies brighter than 0.4L*B, assuming pure luminosity evolution. We find that the merger fraction remains roughly constant at 10%+/-2% for 0.2<z<1.2. The fraction of E/S0/Sa galaxies increases from 21%+/-3% at z~1.1 to 44%+/-9% at z~0.3, while the fraction of Sb-Ir galaxies decreases from 64%+/-6% at z~1.1 to 47%+/-9% at z~0.3. The majority of z<1.2 Spitzer MIPS 24 μm sources with L(IR)>1011 Lsolar are disk galaxies, and only ~15% are classified as major merger candidates. Edge-on and dusty disk galaxies (Sb-Ir) are almost a third of the red sequence at z~1.1, while E/S0/Sa make up over 90% of the red sequence at z~0.3. Approximately 2% of our full sample are red mergers. We conclude (1) the merger rate does not evolve strongly between 0.2<z<1.2 (2) the decrease in the volume-averaged star formation rate density since z~1 is a result of declining star formation in disk galaxies rather than a disappearing population of major mergers; (3) the build-up of the red sequence at z<1 can be explained by a doubling in the number of spheroidal galaxies since z~1.2.
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