Статья

Dependence of galaxy quenching on halo mass and distance from its centre

Joanna WooRacah Institute of Physics, The Hebrew University, Jerusalem 91904, IsraelAvishai DekelRacah Institute of Physics, The Hebrew University, Jerusalem 91904, IsraelS. M. FaberUCO/Lick Observatory and Department of Astronomy and Astrophysics, University of California, Santa Cruz, 1156 High Street, Santa Cruz, CA 95064, USAK. G. NoeskeSpace Telescope Science Institute, Baltimore, MD 21218, USADavid C. KooUCO/Lick Observatory and Department of Astronomy and Astrophysics, University of California, Santa Cruz, 1156 High Street, Santa Cruz, CA 95064, USABrian F. GerkeKavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, M/S 29, 2575 Sand Hill Rd., Menlo Park, CA 94025, USAMichael C. CooperCenter for Galaxy Evolution, Department of Physics and Astronomy, University of California, Irvine, 4129 Frederick Reines Hall, Irvine, CA 92697, USASamir SalimDepartment of Astronomy, Indiana University, Bloomington, IN 47404, USAAaron A. DuttonDepartment of Physics and Astronomy, Elliot Building, 3800 Finnerty Road, University of Victoria, Victoria BC, V8P 5C2, CanadaJeffrey A. NewmanDepartment of Physics and Astronomy, University of Pittsburgh, 3941 O'Hara Street, Pittsburgh, PA 15260, USABenjamin J. WeinerSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USAKevin BundyKavli Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa 277-8583, JapanChristopher N. A. WillmerSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USAMarc DavisDepartment of Astronomy, University of California, Berkeley, CA 94705, USARenbin YanDepartment of Physics and Astronomy, University of Kentucky, Lexington KY, 40506-0055, USA

2012en

ABI

Аннотация

We study the dependence of star formation quenching on galaxy mass and environment, in the Sloan Digital Sky Survey (SDSS; z 0.1) and the All-Wavelength Extended Groth Strip International Survey (AEGIS; z 1). It is crucial that we define quenching by low star formation rate rather than by red colour, given that one-third of the red galaxies are star forming. We address stellar mass M * , halo mass M h , density over the nearest N neighbours N and distance to the halo centre D. The fraction of quenched galaxies appears more strongly correlated with M h at fixed M * than with M * at fixed M h , while for satellites quenching also depends on D. We present the M * -M h relation for centrals at z 1. At z 1, the dependence of quenching on M * at fixed M h is somewhat more pronounced than at z 0, but the quenched fraction is low (10 per cent) and the haloes are less massive. For satellites, M * -dependent quenching is noticeable at high D, suggesting a quenching dependence on subhalo mass for recently captured satellites. At small D, where satellites likely fell in more than a few Gyr ago, quenching strongly depends on M h and not on M * . The M h dependence of quenching is consistent with theoretical wisdom where virial shock heating in massive haloes shuts down accretion and triggers ram-pressure stripping, causing quenching. The interpretation of N is complicated by the fact that it depends on the number of observed group members compared to N, motivating the use of D as a better measure of local environment.

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Идентификаторы

DOI: 10.1093/mnras/sts274

Цитирования и источники

Цитирований: 2Использованных источников: 0

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