C.D.S. - SIMBAD4 rel 1.7 - 2020.05.25CEST01:36:20

2013MNRAS.434..423K - Mon. Not. R. Astron. Soc., 434, 423-436 (2013/September-1)

On the evolution and environmental dependence of the star formation rate versus stellar mass relation since z ∼ 2.


Abstract (from CDS):

This paper discusses the evolution of the correlation between galaxy star formation rates (SFRs) and stellar mass (M*) over the last ∼ 10 Gyr, particularly focusing on its environmental dependence. We first present the mid-infrared (MIR) properties of the Hα-selected galaxies in a rich cluster Cl 0939+4713 at z = 0.4. We use wide-field Spitzer/MIPS 24µm data to show that the optically red Hα emitters, which are most prevalent in group-scale environments, tend to have higher SFRs and higher dust extinction than the majority population of blue Hα sources. With an MIR stacking analysis, we find that the median SFR of Hα emitters is higher in higher density environment at z = 0.4. We also find that star-forming galaxies in high-density environment tend to have higher specific SFR (SSFR), although the trend is much less significant compared to that of SFR. This increase of SSFR in high-density environment is not visible when we consider the SFR derived from Hα alone, suggesting that the dust attenuation in galaxies depends on environment; galaxies in high-density environment tend to be dustier (by up to ∼ 0.5 mag), probably reflecting a higher fraction of nucleated, dusty starbursts in higher density environments at z = 0.4. We then discuss the environmental dependence of the SFR-M* relation for star-forming galaxies since z ∼ 2, by compiling our comparable, narrow-band-selected, large Hα emitter samples in both distant cluster environments and field environments. We find that the SSFR of Hα-selected galaxies (at the fixed mass of log(M*/M☉) = 10) rapidly evolves as (1 + z)3, but the SFR-M* relation is independent of the environment since z ∼ 2, as far as we rely on the Hα-based SFRs (with M*-dependent extinction correction). Even if we consider the possible environmental variation in the dust attenuation, we conclude that the difference in the SFR-M* relation between cluster and field star-forming galaxies is always small ( ≲ 0.2dex level) at any time in the history of the Universe since z ∼ 2.

Abstract Copyright: © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2013)

Journal keyword(s): galaxies: clusters: individual: Cl 0939+4713 - galaxies: evolution - large-scale structure of Universe

Status at CDS:  

Simbad objects: 6

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Number of rows : 6

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
1 NAME Hubble Ultra Deep Field reg 03 32 39.0 -27 47 29           ~ 1270 0
2 ACO 851 ClG 09 42 56.6 +46 59 22           ~ 307 0
3 NAME COSMOS Field reg 10 00 28.60 +02 12 21.0           ~ 2037 0
4 NAME Spiderweb Galaxy AGN 11 40 48.3 -26 29 09     22.00     ~ 249 1
5 NAME MRC 1138-262 Protocluster ClG 11 40 48.4 -26 29 11           ~ 22 0
6 ClG J1716+6708 ClG 17 16 49.6 +67 08 30           ~ 130 0

    Equat.    Gal    SGal    Ecl

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