VVDS-SWIRE. Clustering evolution from a spectroscopic sample of galaxies with redshift 0.2 < z < 2.1 selected from Spitzer IRAC 3.6 mum and 4.5 mum photometry
Sylvain de la Torre
(1)
,
Olivier Le Fèvre
(1)
,
S. Arnouts
(1)
,
L. Guzzo
(2)
,
D. Farrah
(3)
,
Angela Iovino
(2)
,
C. J. Lonsdale
(4)
,
Baptiste Meneux
(2)
,
Seb Oliver
(5)
,
Agnieszka Pollo
(1, 6)
,
I. Waddington
(5)
,
D. Bottini
(7)
,
F. Fang
(8)
,
Bianca Garilli
(7)
,
V. Le Brun
(1)
,
D. Maccagni
(7)
,
J.-P. Picat
(9)
,
R. Scaramella
(10)
,
Marco Scodeggio
(7)
,
D. L. Shupe
(4)
,
Jason A. Surace
(8)
,
Laurence Tresse
(1)
,
G. Vettolani
(10)
,
A. Zanichelli
(10)
,
C. Adami
(1)
,
Sandro Bardelli
(11)
,
M. Bolzonella
(11)
,
A. Cappi
(11)
,
Stéphane Charlot
(12, 13)
,
Paolo Ciliegi
(11)
,
Thierry Contini
(9)
,
S. Foucaud
(14)
,
P. Franzetti
(7)
,
I. Gavignaud
(15)
,
Olivier Ilbert
(16)
,
Fabrice Lamareille
(17)
,
Henry J. Mccracken
(13, 18)
,
B. Marano
(17)
,
Christian Marinoni
(19)
,
A. Mazure
(1)
,
R. Merighi
(11)
,
S. Paltani
(20)
,
R. Pello
(9)
,
L. Pozzetti
(11)
,
M. Radovich
(21)
,
G. Zamorani
(11)
,
E. Zucca
(11)
,
M. Bondi
(10)
,
Angela Bongiorno
(17)
,
J. Brinchmann
(22)
,
O. Cucciati
(2)
,
Yannick Mellier
(13, 18)
,
P. Merluzzi
(21)
,
Sonia Temporin
(2)
,
D. Vergani
(7)
,
C. Jakob Walcher
(1)
1
LAM -
Laboratoire d'Astrophysique de Marseille
2 INAF-Osservatorio Astronomico di Brera
3 Department of Astronomy, Cornell University
4 IPAC - Infrared Processing Analysis Center, California Institute of Technology
5 University of Sussex
6 Observatoire Astronomique de l'Université de Genève
7 IASF-Milano - Istituto di Astrofisica Spaziale e Fisica Cosmica
8 SSC - Spitzer Science Center, California Institute of Technology
9 LATT - Laboratoire Astrophysique de Toulouse-Tarbes
10 IRA-INAF, Bologna
11 OABO - INAF-Osservatorio Astronomico di Bologna
12 MPA - Max-Planck-Institut für Astrophysik
13 IAP - Institut d'Astrophysique de Paris
14 UON - University of Nottingham, UK
15 AIP - Astrophysikalisches Institut Potsdam
16 Institute for Astronomy, University of Hawaii
17 UNIBO - Alma Mater Studiorum Università di Bologna = University of Bologna
18 LERMA - Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique
19 CPT - Centre de Physique Théorique - UMR 7332
20 INTEGRAL Science Data Centre
21 INAF-OAC - INAF-Osservatorio Astronomico di Capodimonte
22 Universidade do Porto = University of Porto
2 INAF-Osservatorio Astronomico di Brera
3 Department of Astronomy, Cornell University
4 IPAC - Infrared Processing Analysis Center, California Institute of Technology
5 University of Sussex
6 Observatoire Astronomique de l'Université de Genève
7 IASF-Milano - Istituto di Astrofisica Spaziale e Fisica Cosmica
8 SSC - Spitzer Science Center, California Institute of Technology
9 LATT - Laboratoire Astrophysique de Toulouse-Tarbes
10 IRA-INAF, Bologna
11 OABO - INAF-Osservatorio Astronomico di Bologna
12 MPA - Max-Planck-Institut für Astrophysik
13 IAP - Institut d'Astrophysique de Paris
14 UON - University of Nottingham, UK
15 AIP - Astrophysikalisches Institut Potsdam
16 Institute for Astronomy, University of Hawaii
17 UNIBO - Alma Mater Studiorum Università di Bologna = University of Bologna
18 LERMA - Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique
19 CPT - Centre de Physique Théorique - UMR 7332
20 INTEGRAL Science Data Centre
21 INAF-OAC - INAF-Osservatorio Astronomico di Capodimonte
22 Universidade do Porto = University of Porto
Résumé
Aims:By combining data from the VIMOS VLT Deep Survey (VVDS) with the Spitzer Wide-area InfraRed Extragalactic survey (SWIRE), we have built the currently largest spectroscopic sample of high redshift galaxies selected in the rest-frame near-infrared. We have obtained 2040 spectroscopic redshifts of galaxies with (m3.6)_AB < 21.5 at 3.6 mu m, and 1255 spectroscopic redshifts of galaxies with (m4.5)_AB < 21. These allow us to investigate the clustering evolution of galaxies selected via their rest-frame near-infrared luminosity in the redshift range 0.2 < z < 2.1.
Methods: We use the projected two-point correlation function w_p(r_p) to study the three dimensional clustering properties of galaxies detected at 3.6 mu m and 4.5 mu m with the InfraRed Array Camera (IRAC) in the SWIRE survey with measured spectroscopic redshifts from the first epoch VVDS. We compare these properties to those of a larger sample of 16672 SWIRE galaxies for which we have accurate photometric redshifts in the same field.
Results: We find that in the 3.6 mu m and 4.5 mu m flux limited samples, the apparent correlation length does not change from redshift ~2 to the present. The measured correlation lengths have a mean value of r0 ~= 3.9±0.5 h-1 Mpc for the galaxies selected at 3.6 mu m and a mean value of r0 ~= 4.4±0.5 h-1 Mpc for the galaxies selected at 4.5 mu m, across the whole redshift range explored. These values are larger than those typicaly found for I-band selected galaxies at I_AB < 24, for which r0 varies from 2.69 h-1 Mpc to 3.63 h-1 Mpc between z = 0.5 to z = 2.1. We find that the difference in correlation length between I-band and 3.6-4.5 mum selected samples decreases with increasing redshift, becoming comparable at z ~= 1.5. We interpret this as evidence that galaxies with older stellar populations and galaxies actively forming stars reside in comparably over-dense environments at epochs earlier than z ~= 1.5, supporting the recently reported flattening of the color-density relation at high redshift. The increasing difference in correlation length with cosmic time observed between rest-frame UV-optical and near-infrared selected samples could then be an indication that star formation is gradually shifting to lower density regions with decreasing redshift, while the older, passively evolving galaxies remain in the most over-dense peaks.
Methods: We use the projected two-point correlation function w_p(r_p) to study the three dimensional clustering properties of galaxies detected at 3.6 mu m and 4.5 mu m with the InfraRed Array Camera (IRAC) in the SWIRE survey with measured spectroscopic redshifts from the first epoch VVDS. We compare these properties to those of a larger sample of 16672 SWIRE galaxies for which we have accurate photometric redshifts in the same field.
Results: We find that in the 3.6 mu m and 4.5 mu m flux limited samples, the apparent correlation length does not change from redshift ~2 to the present. The measured correlation lengths have a mean value of r0 ~= 3.9±0.5 h-1 Mpc for the galaxies selected at 3.6 mu m and a mean value of r0 ~= 4.4±0.5 h-1 Mpc for the galaxies selected at 4.5 mu m, across the whole redshift range explored. These values are larger than those typicaly found for I-band selected galaxies at I_AB < 24, for which r0 varies from 2.69 h-1 Mpc to 3.63 h-1 Mpc between z = 0.5 to z = 2.1. We find that the difference in correlation length between I-band and 3.6-4.5 mum selected samples decreases with increasing redshift, becoming comparable at z ~= 1.5. We interpret this as evidence that galaxies with older stellar populations and galaxies actively forming stars reside in comparably over-dense environments at epochs earlier than z ~= 1.5, supporting the recently reported flattening of the color-density relation at high redshift. The increasing difference in correlation length with cosmic time observed between rest-frame UV-optical and near-infrared selected samples could then be an indication that star formation is gradually shifting to lower density regions with decreasing redshift, while the older, passively evolving galaxies remain in the most over-dense peaks.
Domaines
Astrophysique [astro-ph]
Origine : Fichiers éditeurs autorisés sur une archive ouverte