K+a galaxies in the zCOSMOS Survey: Physical properties of systems in their post-starburst phase
D. Vergani
(1)
,
G. Zamorani
(2)
,
S. J. Lilly
(2)
,
F. Lamareille
(3)
,
C. Halliday
,
M. Scodeggio
(4)
,
C. Vignali
(5)
,
P. Ciliegi
(6)
,
M. Bolzonella
(5)
,
M. Bondi
(6)
,
K. Kovac
(2)
,
C. Knobel
(2)
,
E. Zucca
(7)
,
K. Caputi
(2)
,
L. Pozzetti
(6)
,
S. Bardelli
(6)
,
M. Mignoli
(2)
,
A. Iovino
(2)
,
C. M. Carollo
(8)
,
T. Contini
(3)
,
J. -P. Kneib
(3)
,
O. Le Fevre
(9)
,
V. Mainieri
(2)
,
A. Renzini
(2)
,
A. Bongiorno
(5)
,
G. Coppa
(2)
,
O. Cucciati
(10)
,
S. de La Torre
(2)
,
L. de Ravel
(2)
,
P. Franzetti
(2)
,
B. Garilli
(2)
,
P. Kampczyk
(2)
,
J. -F. Le Borgne
(11)
,
V. Le Brun
(9)
,
C. Maier
(2)
,
R. Pello
(3)
,
Y. Peng
(12)
,
E. Perez Montero
(13)
,
E. Ricciardelli
(2)
,
J. D. Silverman
(2)
,
M. Tanaka
(14)
,
L. Tasca
(9)
,
L. Tresse
(9)
,
U. Abbas
(2)
,
D. Bottini
(2)
,
A. Cappi
(15)
,
P. Cassata
(2)
,
Alessandro Cimatti
(2)
,
L. Guzzo
(2)
,
A. M. Koekemoer
(16)
,
A. Leauthaud D. Maccagni
,
Christian Marinoni
(17, 18)
,
H. J. Mccracken
(19)
,
P. Memeo
(2)
,
B. Meneux
(9)
,
P. Oesch
(2)
,
C. Porciani
(2)
,
R. Scaramella
(2)
,
P. Capak
(20)
,
D. Sanders
(21)
,
N. Scoville
(22)
,
Y. Taniguchi
(2)
1
OAA -
INAF - Osservatorio Astrofisico di Arcetri
2 AUTRES
3 LATT - Laboratoire Astrophysique de Toulouse-Tarbes
4 INAF- Milano
5 UNIBO - Alma Mater Studiorum Università di Bologna = University of Bologna
6 OABO - INAF - Osservatorio Astronomico di Bologna
7 OAB - INAF - Osservatorio Astronomico di Brera
8 University of Chicago
9 LAM - Laboratoire d'Astrophysique de Marseille
10 Dipartimento di Fisica
11 LATT - Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées
12 Dipartimento di Fisica e Astronomia [Bologna]
13 Glycosciences Laboratory
14 Tokai University
15 IASF-Bo - Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna
16 STSci - Space Telescope Science Institute
17 CPT - Centre de Physique Théorique - UMR 6207
18 CPT - Centre de Physique Théorique - UMR 7332
19 IAP - Institut d'Astrophysique de Paris
20 MPIA - Max-Planck-Institut für Astronomie
21 Materials & Process technology
22 CALTECH - California Institute of Technology
2 AUTRES
3 LATT - Laboratoire Astrophysique de Toulouse-Tarbes
4 INAF- Milano
5 UNIBO - Alma Mater Studiorum Università di Bologna = University of Bologna
6 OABO - INAF - Osservatorio Astronomico di Bologna
7 OAB - INAF - Osservatorio Astronomico di Brera
8 University of Chicago
9 LAM - Laboratoire d'Astrophysique de Marseille
10 Dipartimento di Fisica
11 LATT - Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées
12 Dipartimento di Fisica e Astronomia [Bologna]
13 Glycosciences Laboratory
14 Tokai University
15 IASF-Bo - Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna
16 STSci - Space Telescope Science Institute
17 CPT - Centre de Physique Théorique - UMR 6207
18 CPT - Centre de Physique Théorique - UMR 7332
19 IAP - Institut d'Astrophysique de Paris
20 MPIA - Max-Planck-Institut für Astronomie
21 Materials & Process technology
22 CALTECH - California Institute of Technology
G. Zamorani
- Fonction : Auteur
- PersonId : 755662
- ORCID : 0000-0002-2318-301X
- IdRef : 190956429
C. Halliday
- Fonction : Auteur
C. Vignali
- Fonction : Auteur
- PersonId : 759209
- ORCID : 0000-0002-8853-9611
M. Bondi
- Fonction : Auteur
- PersonId : 755966
- ORCID : 0000-0002-9553-7999
E. Zucca
- Fonction : Auteur
- PersonId : 755651
- ORCID : 0000-0002-5845-8132
S. Bardelli
- Fonction : Auteur
- PersonId : 755650
- ORCID : 0000-0002-8900-0298
T. Contini
- Fonction : Auteur
- PersonId : 178293
- IdHAL : thierry-contini
- ORCID : 0000-0003-0275-938X
- IdRef : 112340571
O. Le Fevre
- Fonction : Auteur
- PersonId : 17465
- IdHAL : olivier-le-fevre
- ORCID : 0000-0001-5891-2596
- IdRef : 070374678
S. de La Torre
- Fonction : Auteur
- PersonId : 21320
- IdHAL : sylvain-de-la-torre
- IdRef : 133617238
L. Tresse
- Fonction : Auteur
- PersonId : 743336
- IdHAL : laurence-tresse
- ORCID : 0000-0001-8776-0958
- IdRef : 088004031
A. Leauthaud D. Maccagni
- Fonction : Auteur
Christian Marinoni
- Fonction : Auteur
- PersonId : 7013
- IdHAL : christian-marinoni
- IdRef : 157113582
P. Capak
- Fonction : Auteur
- PersonId : 757663
- ORCID : 0000-0003-3578-6843
D. Sanders
- Fonction : Auteur
- PersonId : 755291
- ORCID : 0000-0002-1233-9998
Résumé
The identities of the main processes triggering and quenching star-formation in galaxies remain unclear. A key stage in evolution, however, appears to be represented by post-starburst galaxies. To investigate their impact on galaxy evolution, we initiated a multiwavelength study of galaxies with k+a spectral features in the COSMOS field. We examine a mass-selected sample of k+a galaxies at z=0.48-1.2 using the spectroscopic zCOSMOS sample. K+a galaxies occupy the brightest tail of the luminosity distribution. They are as massive as quiescent galaxies and populate the green valley in the colour versus luminosity (or stellar mass) distribution. A small percentage (<8%) of these galaxies have radio and/or X-ray counterparts (implying an upper limit to the SFR of ~8Msun/yr). Over the entire redshift range explored, the class of k+a galaxies is morphologically a heterogeneous population with a similar incidence of bulge-dominated and disky galaxies. This distribution does not vary with the strength of the Hdelta absorption line but instead with stellar mass in a way reminiscent of the well-known mass-morphology relation. Although k+a galaxies are also found in underdense regions, they appear to reside typically in a similarly rich environment as quiescent galaxies on a physical scale of ~2-8Mpc, and in groups they show a morphological early-to-late type ratio similar to the quiescent galaxy class. With the current data set, we do not find evidence of statistical significant evolution in either the number/mass density of k+a galaxies at intermediate redshift with respect to the local values, or the spectral properties. Those galaxies, which are affected by a sudden quenching of their star-formation activity, may increase the stellar mass of the red-sequence by up to a non-negligible level of ~10%.