2015A&A...574A.105P


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.13CEST23:49:43

2015A&A...574A.105P - Astronomy and Astrophysics, volume 574A, 105-105 (2015/2-1)

The evolution of galaxy star formation activity in massive haloes.

POPESSO P., BIVIANO A., FINOGUENOV A., WILMAN D., SALVATO M., MAGNELLI B., GRUPPIONI C., POZZI F., RODIGHIERO G., ZIPARO F., BERTA S., ELBAZ D., DICKINSON M., LUTZ D., ALTIERI B., AUSSEL H., CIMATTI A., FADDA D., ILBERT O., LE FLOCH E., NORDON R., POGLITSCH A. and XU C.K.

Abstract (from CDS):

There is now a large consensus that the current epoch of the cosmic star formation history (CSFH) is dominated by low mass galaxies while the most active phase, between redshifts 1 and 2, is dominated by more massive galaxies, which evolve more quickly. Massive galaxies tend to inhabit very massive haloes, such as galaxy groups and clusters. We aim to understand whether the observed ``galaxy downsizing'' could be interpreted as a ``halo downsizing'', whereas the most massive haloes, and their galaxy populations, evolve more rapidly than the haloes with lower mass. We studied the contribution to the CSFH of galaxies inhabiting group-sized haloes. This is done through the study of the evolution of the infra-red (IR) luminosity function of group galaxies from redshift 0 to redshift ∼1.6. We used a sample of 39 X-ray-selected groups in the Extended Chandra Deep Field South (ECDFS), the Chandra Deep Field North (CDFN), and the COSMOS field, where the deepest available mid- and far-IR surveys have been conducted with Spitzer MIPS and with the Photodetector Array Camera and Spectrometer (PACS) on board the Herschel satellite. Groups at low redshift lack the brightest, rarest, and most star forming IR-emitting galaxies observed in the field. Their IR-emitting galaxies contribute ≤10% of the comoving volume density of the whole IR galaxy population in the local Universe. At redshift >1, the most IR-luminous galaxies (LIRGs and ULIRGs) are mainly located in groups, and this is consistent with a reversal of the star formation rate (SFR) vs. density anti-correlation observed in the nearby Universe. At these redshifts, group galaxies contribute 60-80% of the CSFH, i.e. much more than at lower redshifts. Below z ∼1, the comoving number and SFR densities of IR-emitting galaxies in groups decline significantly faster than those of all IR-emitting galaxies. Our results are consistent with a ``halo downsizing'' scenario and highlight the significant role of ``environment'' quenching in shaping the CSFH.

Abstract Copyright:

Journal keyword(s): galaxies: evolution - galaxies: clusters: general - galaxies: luminosity function, mass function - galaxies: groups: general

Simbad objects: 9

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Number of rows : 9

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NAME GOODS Southern Field reg 03 32 28.0 -27 48 30           ~ 995 1
2 NAME Extended Chandra Deep Field South reg 03 32 30.0 -27 48 20           ~ 585 0
3 ACO 3266 ClG 04 31 11.9 -61 24 23           ~ 363 0
4 ClG 0657-56 ClG 06 58 29.6 -55 56 39           ~ 773 1
5 NAME COSMOS Field reg 10 00 28.60 +02 12 21.0           ~ 1876 0
6 NAME Chandra Deep Field-North reg 12 36.8 +62 13           ~ 601 0
7 NAME GOODS-N Field reg 12 36 55.0 +62 14 15           ~ 872 1
8 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4092 2
9 NAME SHAPLEY-CENTAURUS CL SCG 13 06.0 -33 04           ~ 474 0

    Equat.    Gal    SGal    Ecl

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2019.10.13-23:49:43

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