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Title:
The numbers of z ˜ 2 star-forming and passive galaxies in 2.5 square degrees of deep CFHT imaging
Authors:
Arcila-Osejo, Liz; Sawicki, Marcin
Affiliation:
AA(Department of Astronomy & Physics and the Institute for Computational Astrophysics, Saint Mary's University, 923 Robie Street, Halifax, Nova Scotia B3H 3C3, Canada; ), AB(Department of Astronomy & Physics and the Institute for Computational Astrophysics, Saint Mary's University, 923 Robie Street, Halifax, Nova Scotia B3H 3C3, Canada)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 435, Issue 1, p.845-860 (MNRAS Homepage)
Publication Date:
10/2013
Origin:
OUP
Astronomy Keywords:
galaxies: evolution, galaxies: formation, galaxies: luminosity function, mass function
Abstract Copyright:
2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:
10.1093/mnras/stt1354
Bibliographic Code:
2013MNRAS.435..845A

Abstract

We use an adaptation of the BzKs technique to select ˜40 000 z ˜ 2 galaxies (to KAB = 24), including ˜5000 passively evolving (PE) objects (to KAB = 23), from 2.5 deg2 of deep Canada-France-Hawaii Telescope (CFHT) imaging. The passive galaxy luminosity function (LF) exhibits a clear peak at R = 22 and a declining faint-end slope (alpha = -0.12 ^{+0.16}_{-0.14}), while that of star-forming galaxies is characterized by a steep faint-end slope [alpha = -1.43± 0.02(systematic)^{+0.05}_{-0.04}(random)]. The details of the LFs are somewhat sensitive (at the <25 per cent level) to cosmic variance even in these large (˜0.5 deg2) fields, with the D2 field (located in the Cosmological Evolution Survey, COSMOS field) most discrepant from the mean. The shape of the z ˜ 2 stellar mass function of passive galaxies is remarkably similar to that at z ˜ 0.9, save for a factor of ˜4 lower number density. This similarity suggests that the same mechanism may be responsible for the formation of passive galaxies seen at both these epochs. This same formation mechanism may also operate down to z ˜ 0 if the local PE galaxy mass function, known to be two-component, contains two distinct galaxy populations. This scenario is qualitatively in agreement with recent phenomenological mass-quenching models and extends them to span more than three quarters of the history of the Universe.
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