The lack of star formation gradients in galaxy groups up to z tilde 1.6

F. Ziparo, P. Popesso, A. Biviano, A. Finoguenov, S. Wuyts, D. Wilman, M. Salvato, M. Tanaka, O. Ilbert, K. Nandra, D. Lutz, D. Elbaz, M. Dickinson, B. Altieri, H. Aussel, S. Berta, A. Cimatti, D. Fadda, R. Genzel, E. Le Flo'chB. Magnelli, R. Nordon, A. Poglitsch, F. Pozzi, M. S. Portal, L. Tacconi, F. E. Bauer, W. N. Brandt, N. Cappelluti, M. C. Cooper, J. S. Mulchaey

Research output: Contribution to journalArticle

24 Citations (Scopus)
26 Downloads (Pure)

Abstract

In the local Universe, galaxy properties show a strong dependence on environment. In cluster cores, early-type galaxies dominate, whereas star-forming galaxies are more and more common in the outskirts. At higher redshifts and in somewhat less dense environments (e.g. galaxy groups), the situation is less clear. One open issue is that of whether and how the star formation rate (SFR) of galaxies in groups depends on the distance from the centre of mass. To shed light on this topic, we have built a sample of X-ray selected galaxy groups at 0 < z < 1.6 in various blank fields [Extended Chandra Deep Field South (ECDFS), Cosmological Evolution Survey (COSMOS), Great Observatories Origin Deep Survey (GOODS)]. We use a sample of spectroscopically confirmed group members with stellar mass M⋆ > 1010.3 M⊙ in order to have a high spectroscopic completeness. As we use only spectroscopic redshifts, our results are not affected by uncertainties due to projection effects. We use several SFR indicators to link the star formation (SF) activity to the galaxy environment. Taking advantage of the extremely deep mid-infrared Spitzer MIPS and far-infrared Herschel1 PACS observations, we have an accurate, broad-band measure of the SFR for the bulk of the star-forming galaxies. We use multi-wavelength Spectral Energy Distribution (SED) fitting techniques to estimate the stellar masses of all objects and the SFR of the MIPS and PACS undetected galaxies. We analyse the dependence of the SF activity, stellar mass and specific SFR on the group-centric distance, up to z ∼ 1.6, for the first time. We do not find any correlation between the mean SFR and group-centric distance at any redshift. We do not observe any strong mass segregation either, in agreement with predictions from simulations. Our results suggest that either groups have a much smaller spread in accretion times with respect to the clusters and that the relaxation time is longer than the group crossing time.
Original languageEnglish
Pages (from-to)3089-3103
Number of pages15
JournalMonthly Notices of the Royal Astronomical Society
Volume434
Issue number4
Early online date25 Jul 2013
DOIs
Publication statusPublished - 1 Oct 2013

Fingerprint

galactic clusters
star formation rate
star formation
galaxies
gradients
stellar mass
stars
blanks
completeness
spectral energy distribution
rate
observatory
center of mass
accretion
observatories
wavelength
universe
relaxation time
projection
broadband

Keywords

  • galaxies:
  • groups: general
  • galaxies: evolution
  • galaxies: stellar content
  • infrared: galaxies
  • X-rays: galaxies
  • clusters
  • galaxies: star formation

Cite this

Ziparo, F., Popesso, P., Biviano, A., Finoguenov, A., Wuyts, S., Wilman, D., ... Mulchaey, J. S. (2013). The lack of star formation gradients in galaxy groups up to z tilde 1.6. Monthly Notices of the Royal Astronomical Society, 434(4), 3089-3103. https://doi.org/10.1093/mnras/stt1222

The lack of star formation gradients in galaxy groups up to z tilde 1.6. / Ziparo, F.; Popesso, P.; Biviano, A.; Finoguenov, A.; Wuyts, S.; Wilman, D.; Salvato, M.; Tanaka, M.; Ilbert, O.; Nandra, K.; Lutz, D.; Elbaz, D.; Dickinson, M.; Altieri, B.; Aussel, H.; Berta, S.; Cimatti, A.; Fadda, D.; Genzel, R.; Le Flo'ch, E.; Magnelli, B.; Nordon, R.; Poglitsch, A.; Pozzi, F.; Portal, M. S.; Tacconi, L.; Bauer, F. E.; Brandt, W. N.; Cappelluti, N.; Cooper, M. C.; Mulchaey, J. S.

In: Monthly Notices of the Royal Astronomical Society, Vol. 434, No. 4, 01.10.2013, p. 3089-3103.

Research output: Contribution to journalArticle

Ziparo, F, Popesso, P, Biviano, A, Finoguenov, A, Wuyts, S, Wilman, D, Salvato, M, Tanaka, M, Ilbert, O, Nandra, K, Lutz, D, Elbaz, D, Dickinson, M, Altieri, B, Aussel, H, Berta, S, Cimatti, A, Fadda, D, Genzel, R, Le Flo'ch, E, Magnelli, B, Nordon, R, Poglitsch, A, Pozzi, F, Portal, MS, Tacconi, L, Bauer, FE, Brandt, WN, Cappelluti, N, Cooper, MC & Mulchaey, JS 2013, 'The lack of star formation gradients in galaxy groups up to z tilde 1.6', Monthly Notices of the Royal Astronomical Society, vol. 434, no. 4, pp. 3089-3103. https://doi.org/10.1093/mnras/stt1222
Ziparo, F. ; Popesso, P. ; Biviano, A. ; Finoguenov, A. ; Wuyts, S. ; Wilman, D. ; Salvato, M. ; Tanaka, M. ; Ilbert, O. ; Nandra, K. ; Lutz, D. ; Elbaz, D. ; Dickinson, M. ; Altieri, B. ; Aussel, H. ; Berta, S. ; Cimatti, A. ; Fadda, D. ; Genzel, R. ; Le Flo'ch, E. ; Magnelli, B. ; Nordon, R. ; Poglitsch, A. ; Pozzi, F. ; Portal, M. S. ; Tacconi, L. ; Bauer, F. E. ; Brandt, W. N. ; Cappelluti, N. ; Cooper, M. C. ; Mulchaey, J. S. / The lack of star formation gradients in galaxy groups up to z tilde 1.6. In: Monthly Notices of the Royal Astronomical Society. 2013 ; Vol. 434, No. 4. pp. 3089-3103.
@article{5a3bb11f6e8141dd804426242f9b1a6f,
title = "The lack of star formation gradients in galaxy groups up to z tilde 1.6",
abstract = "In the local Universe, galaxy properties show a strong dependence on environment. In cluster cores, early-type galaxies dominate, whereas star-forming galaxies are more and more common in the outskirts. At higher redshifts and in somewhat less dense environments (e.g. galaxy groups), the situation is less clear. One open issue is that of whether and how the star formation rate (SFR) of galaxies in groups depends on the distance from the centre of mass. To shed light on this topic, we have built a sample of X-ray selected galaxy groups at 0 < z < 1.6 in various blank fields [Extended Chandra Deep Field South (ECDFS), Cosmological Evolution Survey (COSMOS), Great Observatories Origin Deep Survey (GOODS)]. We use a sample of spectroscopically confirmed group members with stellar mass M⋆ > 1010.3 M⊙ in order to have a high spectroscopic completeness. As we use only spectroscopic redshifts, our results are not affected by uncertainties due to projection effects. We use several SFR indicators to link the star formation (SF) activity to the galaxy environment. Taking advantage of the extremely deep mid-infrared Spitzer MIPS and far-infrared Herschel1 PACS observations, we have an accurate, broad-band measure of the SFR for the bulk of the star-forming galaxies. We use multi-wavelength Spectral Energy Distribution (SED) fitting techniques to estimate the stellar masses of all objects and the SFR of the MIPS and PACS undetected galaxies. We analyse the dependence of the SF activity, stellar mass and specific SFR on the group-centric distance, up to z ∼ 1.6, for the first time. We do not find any correlation between the mean SFR and group-centric distance at any redshift. We do not observe any strong mass segregation either, in agreement with predictions from simulations. Our results suggest that either groups have a much smaller spread in accretion times with respect to the clusters and that the relaxation time is longer than the group crossing time.",
keywords = "galaxies: , groups: general, galaxies: evolution, galaxies: stellar content, infrared: galaxies, X-rays: galaxies, clusters, galaxies: star formation",
author = "F. Ziparo and P. Popesso and A. Biviano and A. Finoguenov and S. Wuyts and D. Wilman and M. Salvato and M. Tanaka and O. Ilbert and K. Nandra and D. Lutz and D. Elbaz and M. Dickinson and B. Altieri and H. Aussel and S. Berta and A. Cimatti and D. Fadda and R. Genzel and {Le Flo'ch}, E. and B. Magnelli and R. Nordon and A. Poglitsch and F. Pozzi and Portal, {M. S.} and L. Tacconi and Bauer, {F. E.} and Brandt, {W. N.} and N. Cappelluti and Cooper, {M. C.} and Mulchaey, {J. S.}",
year = "2013",
month = "10",
day = "1",
doi = "10.1093/mnras/stt1222",
language = "English",
volume = "434",
pages = "3089--3103",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "4",

}

TY - JOUR

T1 - The lack of star formation gradients in galaxy groups up to z tilde 1.6

AU - Ziparo, F.

AU - Popesso, P.

AU - Biviano, A.

AU - Finoguenov, A.

AU - Wuyts, S.

AU - Wilman, D.

AU - Salvato, M.

AU - Tanaka, M.

AU - Ilbert, O.

AU - Nandra, K.

AU - Lutz, D.

AU - Elbaz, D.

AU - Dickinson, M.

AU - Altieri, B.

AU - Aussel, H.

AU - Berta, S.

AU - Cimatti, A.

AU - Fadda, D.

AU - Genzel, R.

AU - Le Flo'ch, E.

AU - Magnelli, B.

AU - Nordon, R.

AU - Poglitsch, A.

AU - Pozzi, F.

AU - Portal, M. S.

AU - Tacconi, L.

AU - Bauer, F. E.

AU - Brandt, W. N.

AU - Cappelluti, N.

AU - Cooper, M. C.

AU - Mulchaey, J. S.

PY - 2013/10/1

Y1 - 2013/10/1

N2 - In the local Universe, galaxy properties show a strong dependence on environment. In cluster cores, early-type galaxies dominate, whereas star-forming galaxies are more and more common in the outskirts. At higher redshifts and in somewhat less dense environments (e.g. galaxy groups), the situation is less clear. One open issue is that of whether and how the star formation rate (SFR) of galaxies in groups depends on the distance from the centre of mass. To shed light on this topic, we have built a sample of X-ray selected galaxy groups at 0 < z < 1.6 in various blank fields [Extended Chandra Deep Field South (ECDFS), Cosmological Evolution Survey (COSMOS), Great Observatories Origin Deep Survey (GOODS)]. We use a sample of spectroscopically confirmed group members with stellar mass M⋆ > 1010.3 M⊙ in order to have a high spectroscopic completeness. As we use only spectroscopic redshifts, our results are not affected by uncertainties due to projection effects. We use several SFR indicators to link the star formation (SF) activity to the galaxy environment. Taking advantage of the extremely deep mid-infrared Spitzer MIPS and far-infrared Herschel1 PACS observations, we have an accurate, broad-band measure of the SFR for the bulk of the star-forming galaxies. We use multi-wavelength Spectral Energy Distribution (SED) fitting techniques to estimate the stellar masses of all objects and the SFR of the MIPS and PACS undetected galaxies. We analyse the dependence of the SF activity, stellar mass and specific SFR on the group-centric distance, up to z ∼ 1.6, for the first time. We do not find any correlation between the mean SFR and group-centric distance at any redshift. We do not observe any strong mass segregation either, in agreement with predictions from simulations. Our results suggest that either groups have a much smaller spread in accretion times with respect to the clusters and that the relaxation time is longer than the group crossing time.

AB - In the local Universe, galaxy properties show a strong dependence on environment. In cluster cores, early-type galaxies dominate, whereas star-forming galaxies are more and more common in the outskirts. At higher redshifts and in somewhat less dense environments (e.g. galaxy groups), the situation is less clear. One open issue is that of whether and how the star formation rate (SFR) of galaxies in groups depends on the distance from the centre of mass. To shed light on this topic, we have built a sample of X-ray selected galaxy groups at 0 < z < 1.6 in various blank fields [Extended Chandra Deep Field South (ECDFS), Cosmological Evolution Survey (COSMOS), Great Observatories Origin Deep Survey (GOODS)]. We use a sample of spectroscopically confirmed group members with stellar mass M⋆ > 1010.3 M⊙ in order to have a high spectroscopic completeness. As we use only spectroscopic redshifts, our results are not affected by uncertainties due to projection effects. We use several SFR indicators to link the star formation (SF) activity to the galaxy environment. Taking advantage of the extremely deep mid-infrared Spitzer MIPS and far-infrared Herschel1 PACS observations, we have an accurate, broad-band measure of the SFR for the bulk of the star-forming galaxies. We use multi-wavelength Spectral Energy Distribution (SED) fitting techniques to estimate the stellar masses of all objects and the SFR of the MIPS and PACS undetected galaxies. We analyse the dependence of the SF activity, stellar mass and specific SFR on the group-centric distance, up to z ∼ 1.6, for the first time. We do not find any correlation between the mean SFR and group-centric distance at any redshift. We do not observe any strong mass segregation either, in agreement with predictions from simulations. Our results suggest that either groups have a much smaller spread in accretion times with respect to the clusters and that the relaxation time is longer than the group crossing time.

KW - galaxies:

KW - groups: general

KW - galaxies: evolution

KW - galaxies: stellar content

KW - infrared: galaxies

KW - X-rays: galaxies

KW - clusters

KW - galaxies: star formation

UR - http://mnras.oxfordjournals.org/content/434/4/3089

U2 - 10.1093/mnras/stt1222

DO - 10.1093/mnras/stt1222

M3 - Article

VL - 434

SP - 3089

EP - 3103

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 4

ER -