Non-linearity and environmental dependence of the star-forming galaxies main sequence
P. Popesso
(1, 2)
,
A. Finoguenov
(1)
,
D. Wilman
(1)
,
S. Wuyts
(1)
,
A. Biviano
(3)
,
M. Salvato
(1, 2)
,
M. Mirkazemi
,
L. Morselli
,
F. Ziparo
(1)
,
K. Nandra
,
D. Lutz
(1)
,
D. Elbaz
(4)
,
M. Dickinson
(5)
,
M. Tanaka
,
M. B. Altieri
,
H. Aussel
(4)
,
F. Bauer
(6)
,
S. Berta
(1)
,
R. M. Bielby
(7)
,
N. Brandt
,
N. Cappelluti
(8)
,
Alessandro Cimatti
(8)
,
M. C. Cooper
,
D. Fadda
(9)
,
O. Ilbert
(10)
,
E. Le Floch
(4)
,
B. Magnelli
(1)
,
J. S. Mulchaey
,
R. Nordon
(1)
,
J. A. Newman
,
A. Poglitsch
(1)
,
F. Pozzi
(11)
,
G. Erfanianfar
1
MPE -
Max-Planck-Institut für Extraterrestrische Physik
2 Excellence Cluster Universe
3 OAT - INAF - Osservatorio Astronomico di Trieste
4 AIM (UMR7158 / UMR_E_9005 / UM_112) - Astrophysique Interprétation Modélisation
5 NOAO - National Optical Astronomy Observatory
6 IRFU - Institut de Recherches sur les lois Fondamentales de l'Univers
7 Durham University
8 OABO - INAF - Osservatorio Astronomico di Bologna
9 AUTRES
10 LAM - Laboratoire d'Astrophysique de Marseille
11 UNIBO - Alma Mater Studiorum Università di Bologna = University of Bologna
2 Excellence Cluster Universe
3 OAT - INAF - Osservatorio Astronomico di Trieste
4 AIM (UMR7158 / UMR_E_9005 / UM_112) - Astrophysique Interprétation Modélisation
5 NOAO - National Optical Astronomy Observatory
6 IRFU - Institut de Recherches sur les lois Fondamentales de l'Univers
7 Durham University
8 OABO - INAF - Osservatorio Astronomico di Bologna
9 AUTRES
10 LAM - Laboratoire d'Astrophysique de Marseille
11 UNIBO - Alma Mater Studiorum Università di Bologna = University of Bologna
P. Popesso
- Fonction : Auteur
- PersonId : 980617
A. Finoguenov
- Fonction : Auteur
- PersonId : 756645
- ORCID : 0000-0002-4606-5403
A. Biviano
- Fonction : Auteur
- PersonId : 755569
- ORCID : 0000-0002-0857-0732
- IdRef : 233130799
M. Mirkazemi
- Fonction : Auteur
L. Morselli
- Fonction : Auteur
K. Nandra
- Fonction : Auteur
D. Lutz
- Fonction : Auteur
- PersonId : 755584
- ORCID : 0000-0003-0291-9582
M. Dickinson
- Fonction : Auteur
- PersonId : 766451
- ORCID : 0000-0001-5414-5131
M. Tanaka
- Fonction : Auteur
M. B. Altieri
- Fonction : Auteur
H. Aussel
- Fonction : Auteur
- PersonId : 178304
- IdHAL : haussel
- ORCID : 0000-0002-1371-5705
- IdRef : 253124654
S. Berta
- Fonction : Auteur
- PersonId : 765477
- ORCID : 0000-0002-0320-1532
N. Brandt
- Fonction : Auteur
M. C. Cooper
- Fonction : Auteur
B. Magnelli
- Fonction : Auteur
- PersonId : 761091
- ORCID : 0000-0002-6777-6490
- IdRef : 137976607
J. S. Mulchaey
- Fonction : Auteur
J. A. Newman
- Fonction : Auteur
G. Erfanianfar
- Fonction : Auteur
Résumé
Using data from four deep fields (COSMOS, AEGIS, ECDFS, and CDFN), we study the correlation between the position of galaxies in the star formation rate (SFR) versus stellar mass plane and local environment at z \textless 1.1. To accurately estimate the galaxy SFR, we use the deepest available Spitzer/MIPS 24 and Herschel/PACS data sets. We distinguish group environments (M-halo similar to 10(12.5-14.2)M(circle dot)) based on the available deep X-ray data and lower halo mass environments based on the local galaxy density. We confirm that the main sequence (MS) of star-forming galaxies is not a linear relation and there is a flattening towards higher stellar masses (M-* \textgreater 10(10.4-10.6) M-circle dot), across all environments. At high redshift (0.5 \textless z \textless 1.1), the MS varies little with environment. At low redshift (0.15 \textless z \textless 0.5), group galaxies tend to deviate from the mean MS towards the region of quiescence with respect to isolated galaxies and less-dense environments. We find that the flattening of the MS towards low SFR is due to an increased fraction of bulge-dominated galaxies at high masses. Instead, the deviation of group galaxies from the MS at low redshift is caused by a large fraction of red disc-dominated galaxies which are not present in the lower density environments. Our results suggest that above a mass threshold (similar to 10(10.4)-10(10.6) M-circle dot) stellar mass, morphology and environment act together in driving the evolution of the star formation activity towards lower level. The presence of a dominating bulge and the associated quenching processes are already in place beyond z similar to 1. The environmental effects appear, instead, at lower redshifts and have a long time-scale.