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EVOLUTION OF GALAXIES AND THEIR ENVIRONMENTS AT <i>z</i> = 0.1-3 IN COSMOS

N. Z. ScovilleCalifornia Institute of Technology, MC 249-17, 1200 East California Boulevard, Pasadena, CA 91125, USAS. ArnoutsAix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, F-13388 Marseille, FranceH. AusselAIM Unité Mixte de Recherche CEA CNRS, Université Paris VII UMR n158, Paris, FranceAndrew BensonCalifornia Institute of Technology, MC 249-17, 1200 East California Boulevard, Pasadena, CA 91125, USAA. BongiornoINAF-Osservatorio Astronomico di Roma, Via di Frascati 33, I-00040 Monteporzio Catone, Rome, ItalyK. BundyInstitute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa 277-8582, JapanMiguel A. Aragón-CalvoDepartment of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218-2686, USAP. CapakSpitzer Science Center, MS 314-6, California Institute of Technology, Pasadena, CA 91125, USAC. M. CarolloInstitute for Astronomy, ETH Zurich, Wolfgang-Pauli-strasse 27, CH-8093 Zurich, SwitzerlandF. CivanoHarvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAJ. S. DunlopInstitute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ, UKM. ElvisHarvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAAndreas L. FaisstInstitute for Astronomy, ETH Zurich, Wolfgang-Pauli-strasse 27, CH-8093 Zurich, SwitzerlandA. FinoguenovMax Planck Institut für Extraterrestrische Physik, D-85478 Garching, GermanyHai FuCalifornia Institute of Technology, MC 249-17, 1200 East California Boulevard, Pasadena, CA 91125, USAMauro GiavaliscoDepartment of Astronomy, University of Massachusetts, Amherst, MA 01003, USAQi GuoMax Planck Institut für Extraterrestrische Physik, D-85478 Garching, GermanyO. IlbertLaboratoire d'Astrophysique de Marseille, B. P. 8, Traverse du Siphon, F-13376 Marseille Cedex 12, FranceA. IovinoINAF-Osservatorio Astronomico di Brera, via Brera, 28, 20159 Milano, ItalyMasaru KajisawaPhysics Department, Graduate School of Science, Ehime University, 2-5 Bunkyou, Matsuyama 790-8577, JapanJ. S. KartaltepeAix-Marseille UniversitéAlexie LeauthaudInstitute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa 277-8582, JapanO. Le FèvreLaboratoire d'Astrophysique de Marseille, B. P. 8, Traverse du Siphon, F-13376 Marseille Cedex 12, FranceE. LeFlochAIM Unité Mixte de Recherche CEA CNRS, Université Paris VII UMR n158, Paris, FranceS. J. LillyInstitute for Astronomy, ETH Zurich, Wolfgang-Pauli-strasse 27, CH-8093 Zurich, SwitzerlandCharles LiuAstrophysical Observatory, Department of Engineering Science and Physics, CUNY College of Staten Island, 2800 Victory Boulevard, Staten Island, NY 10314, USAS. ManoharCalifornia Institute of Technology, MC 249-17, 1200 East California Boulevard, Pasadena, CA 91125, USAR. MasseyInstitute for Astronomy, Blackford Hill, Edinburgh EH9 3HJ, UKDaniel MastersDepartment of Physics and Astronomy, University of California, Riverside, CA 92521, USAH. J. McCrackenInstitut d'Astrophysique de Paris, UMR7095 CNRS, Université Pierre et Marie Curie, 98 bis Boulevard Arago, F-75014 Paris, FranceB. MobasherDepartment of Physics and Astronomy, University of California, Riverside, CA 92521, USAY. PengInstitute for Astronomy, ETH Zurich, Wolfgang-Pauli-strasse 27, CH-8093 Zurich, SwitzerlandA. RenziniINAF-Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, ItalyJason RhodesCalifornia Institute of Technology, MC 249-17, 1200 East California Boulevard, Pasadena, CA 91125, USAM. SalvatoCalifornia Institute of Technology, MC 249-17, 1200 East California Boulevard, Pasadena, CA 91125, USAD. B. SandersInstitute for Astronomy, 2680 Woodlawn Drive, University of Hawaii, Honolulu, HI 96822, USABehnam Darvish SarvestaniDepartment of Physics and Astronomy, University of California, Riverside, CA 92521, USAClaudia ScarlataDepartment of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USAEva SchinnererMax Planck Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, GermanyKartik ShethNational Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USAP. L. ShopbellCalifornia Institute of Technology, MC 249-17, 1200 East California Boulevard, Pasadena, CA 91125, USAV. SmolčićArgelander Institut for Astronomy, Auf dem Hügel 71, D-53121 Bonn, GermanyY. TaniguchiPhysics Department, Graduate School of Science, Ehime University, 2-5 Bunkyou, Matsuyama 790-8577, JapanJames E. TaylorDepartment of Physics and Astronomy, University of Waterloo, Waterloo, Ontario N2L 3G1, CanadaSimon D. M. WhiteMax Planck Institut für Extraterrestrische Physik, D-85478 Garching, GermanyLin YanSpitzer Science Center, MS 314-6, California Institute of Technology, Pasadena, CA 91125, USA

2013en

ABI

Annotatsiya

Large-scale structures (LSS) out to z $< 3.0$ are measured in the Cosmic Evolution Survey (COSMOS) using extremely accurate photometric redshifts (photoz). The Ks-band selected sample (from Ultra-Vista) is comprised of 155,954 galaxies. Two techniques -- adaptive smoothing and Voronoi tessellation -- are used to estimate the environmental densities within 127 redshift slices. Approximately 250 statistically significant overdense structures are identified out to z $= 3.0$ with shapes varying from elongated filamentary structures to more circularly symmetric concentrations. We also compare the densities derived for COSMOS with those based on semi-analytic predictions for a $Λ$CDM simulation and find excellent overall agreement between the mean densities as a function of redshift and the range of densities. The galaxy properties (stellar mass, spectral energy distributions (SEDs) and star formation rates (SFRs)) are strongly correlated with environmental density and redshift, particularly at z $< 1.0 - 1.2$. Classifying the spectral type of each galaxy using the rest-frame b-i color (from the photoz SED fitting), we find a strong correlation of early type galaxies (E-Sa) with high density environments, while the degree of environmental segregation varies systematically with redshift out to z $\sim 1.3$. In the highest density regions, 80% of the galaxies are early types at z=0.2 compared to only 20% at z = 1.5. The SFRs and the star formation timescales exhibit clear environmental correlations. At z $> 0.8$, the star formation rate density (SFRD) is uniformly distributed over all environmental density percentiles, while at lower redshifts the dominant contribution is shifted to galaxies in lower density environments.

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DOI: 10.1088/0067-0049/206/1/3

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