Reversal or no reversal: The evolution of the star formation rate-density relation up to z ~ 1.6

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

Research output: Contribution to journalArticle

29 Citations (Scopus)

Abstract

We investigate the evolution of the star formation rate (SFR)-density relation in the Extended Chandra Deep Field South and the Great Observatories Origin Deep Survey fields up to z ~ 1.6. In addition to the 'traditional method', in which the environment is defined according to a statistical measurement of the local galaxy density, we use a 'dynamical' approach, where galaxies are classified according to three different environment regimes: group, 'filamentlike' and field. Both methods show no evidence of an SFR-density reversal. Moreover, group galaxies show a mean SFR lower than other environments up to z ~ 1, while at earlier epochs group and field galaxies exhibit consistent levels of star formation (SF) activity. We find that processes related to a massive dark matter halo must be dominant in the suppression of the SF below z ~ 1, with respect to purely density-related processes. We confirm this finding by studying the distribution of galaxies in different environments with respect to the so-called main sequence (MS) of star-forming galaxies. Galaxies in both group and 'filament-like' environments preferentially lie below the MS up to z ~ 1, with group galaxies exhibiting lower levels of star-forming activity at a given mass. At z > 1, the star-forming galaxies in groups reside on the MS. Groups exhibit the highest fraction of quiescent galaxies up to z ~ 1, after which group, 'filament-like' and field environments have a similar mix of galaxy types. We conclude that groups are the most efficient locus for SF quenching. Thus, a fundamental difference exists between bound and unbound objects, or between dark matter haloes of different masses.

Original languageEnglish (US)
Article numberstt1901
Pages (from-to)458-474
Number of pages17
JournalMonthly Notices of the Royal Astronomical Society
Volume437
Issue number1
DOIs
StatePublished - Jan 1 2014
Externally publishedYes

Fingerprint

star formation rate
galaxies
star formation
galactic clusters
stars
halos
dark matter
filaments
field survey
rate
observatory
loci
observatories
quenching
time measurement
retarding

Keywords

  • Galaxies: evolution
  • Galaxies: groups: general
  • Galaxies: star formation
  • Infrared: galaxies

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Ziparo, F., Popesso, P., Finoguenov, A., Biviano, A., Wuyts, S., Wilman, D., ... Mulchaey, J. S. (2014). Reversal or no reversal: The evolution of the star formation rate-density relation up to z ~ 1.6. Monthly Notices of the Royal Astronomical Society, 437(1), 458-474. [stt1901]. https://doi.org/10.1093/mnras/stt1901

Reversal or no reversal : The evolution of the star formation rate-density relation up to z ~ 1.6. / Ziparo, F.; Popesso, P.; Finoguenov, A.; Biviano, A.; Wuyts, S.; Wilman, D.; Salvato, M.; Tanaka, M.; Nandra, K.; Lutz, D.; Elbaz, D.; Dickinson, M.; Altieri, B.; Aussel, H.; Berta, S.; Cimatti, A.; Fadda, D.; Genzel, R.; Le Floc'h, E.; Magnelli, B.; Nordon, R.; Poglitsch, A.; Pozzi, F.; Sanchez Portal, M.; Tacconi, L.; Bauer, F. E.; Brandt, W. N.; Cappelluti, Nico; Cooper, M. C.; Mulchaey, J. S.

In: Monthly Notices of the Royal Astronomical Society, Vol. 437, No. 1, stt1901, 01.01.2014, p. 458-474.

Research output: Contribution to journalArticle

Ziparo, F, Popesso, P, Finoguenov, A, Biviano, A, Wuyts, S, Wilman, D, Salvato, M, Tanaka, M, Nandra, K, Lutz, D, Elbaz, D, Dickinson, M, Altieri, B, Aussel, H, Berta, S, Cimatti, A, Fadda, D, Genzel, R, Le Floc'h, E, Magnelli, B, Nordon, R, Poglitsch, A, Pozzi, F, Sanchez Portal, M, Tacconi, L, Bauer, FE, Brandt, WN, Cappelluti, N, Cooper, MC & Mulchaey, JS 2014, 'Reversal or no reversal: The evolution of the star formation rate-density relation up to z ~ 1.6', Monthly Notices of the Royal Astronomical Society, vol. 437, no. 1, stt1901, pp. 458-474. https://doi.org/10.1093/mnras/stt1901
Ziparo, F. ; Popesso, P. ; Finoguenov, A. ; Biviano, A. ; Wuyts, S. ; Wilman, D. ; Salvato, M. ; Tanaka, M. ; Nandra, K. ; Lutz, D. ; Elbaz, D. ; Dickinson, M. ; Altieri, B. ; Aussel, H. ; Berta, S. ; Cimatti, A. ; Fadda, D. ; Genzel, R. ; Le Floc'h, E. ; Magnelli, B. ; Nordon, R. ; Poglitsch, A. ; Pozzi, F. ; Sanchez Portal, M. ; Tacconi, L. ; Bauer, F. E. ; Brandt, W. N. ; Cappelluti, Nico ; Cooper, M. C. ; Mulchaey, J. S. / Reversal or no reversal : The evolution of the star formation rate-density relation up to z ~ 1.6. In: Monthly Notices of the Royal Astronomical Society. 2014 ; Vol. 437, No. 1. pp. 458-474.
@article{e1dc490e33de4425a3e6960e14fafb71,
title = "Reversal or no reversal: The evolution of the star formation rate-density relation up to z ~ 1.6",
abstract = "We investigate the evolution of the star formation rate (SFR)-density relation in the Extended Chandra Deep Field South and the Great Observatories Origin Deep Survey fields up to z ~ 1.6. In addition to the 'traditional method', in which the environment is defined according to a statistical measurement of the local galaxy density, we use a 'dynamical' approach, where galaxies are classified according to three different environment regimes: group, 'filamentlike' and field. Both methods show no evidence of an SFR-density reversal. Moreover, group galaxies show a mean SFR lower than other environments up to z ~ 1, while at earlier epochs group and field galaxies exhibit consistent levels of star formation (SF) activity. We find that processes related to a massive dark matter halo must be dominant in the suppression of the SF below z ~ 1, with respect to purely density-related processes. We confirm this finding by studying the distribution of galaxies in different environments with respect to the so-called main sequence (MS) of star-forming galaxies. Galaxies in both group and 'filament-like' environments preferentially lie below the MS up to z ~ 1, with group galaxies exhibiting lower levels of star-forming activity at a given mass. At z > 1, the star-forming galaxies in groups reside on the MS. Groups exhibit the highest fraction of quiescent galaxies up to z ~ 1, after which group, 'filament-like' and field environments have a similar mix of galaxy types. We conclude that groups are the most efficient locus for SF quenching. Thus, a fundamental difference exists between bound and unbound objects, or between dark matter haloes of different masses.",
keywords = "Galaxies: evolution, Galaxies: groups: general, Galaxies: star formation, Infrared: galaxies",
author = "F. Ziparo and P. Popesso and A. Finoguenov and A. Biviano and S. Wuyts and D. Wilman and M. Salvato and M. Tanaka 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 Floc'h}, E. and B. Magnelli and R. Nordon and A. Poglitsch and F. Pozzi and {Sanchez Portal}, M. and L. Tacconi and Bauer, {F. E.} and Brandt, {W. N.} and Nico Cappelluti and Cooper, {M. C.} and Mulchaey, {J. S.}",
year = "2014",
month = "1",
day = "1",
doi = "10.1093/mnras/stt1901",
language = "English (US)",
volume = "437",
pages = "458--474",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "1",

}

TY - JOUR

T1 - Reversal or no reversal

T2 - The evolution of the star formation rate-density relation up to z ~ 1.6

AU - Ziparo, F.

AU - Popesso, P.

AU - Finoguenov, A.

AU - Biviano, A.

AU - Wuyts, S.

AU - Wilman, D.

AU - Salvato, M.

AU - Tanaka, M.

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 Floc'h, E.

AU - Magnelli, B.

AU - Nordon, R.

AU - Poglitsch, A.

AU - Pozzi, F.

AU - Sanchez Portal, M.

AU - Tacconi, L.

AU - Bauer, F. E.

AU - Brandt, W. N.

AU - Cappelluti, Nico

AU - Cooper, M. C.

AU - Mulchaey, J. S.

PY - 2014/1/1

Y1 - 2014/1/1

N2 - We investigate the evolution of the star formation rate (SFR)-density relation in the Extended Chandra Deep Field South and the Great Observatories Origin Deep Survey fields up to z ~ 1.6. In addition to the 'traditional method', in which the environment is defined according to a statistical measurement of the local galaxy density, we use a 'dynamical' approach, where galaxies are classified according to three different environment regimes: group, 'filamentlike' and field. Both methods show no evidence of an SFR-density reversal. Moreover, group galaxies show a mean SFR lower than other environments up to z ~ 1, while at earlier epochs group and field galaxies exhibit consistent levels of star formation (SF) activity. We find that processes related to a massive dark matter halo must be dominant in the suppression of the SF below z ~ 1, with respect to purely density-related processes. We confirm this finding by studying the distribution of galaxies in different environments with respect to the so-called main sequence (MS) of star-forming galaxies. Galaxies in both group and 'filament-like' environments preferentially lie below the MS up to z ~ 1, with group galaxies exhibiting lower levels of star-forming activity at a given mass. At z > 1, the star-forming galaxies in groups reside on the MS. Groups exhibit the highest fraction of quiescent galaxies up to z ~ 1, after which group, 'filament-like' and field environments have a similar mix of galaxy types. We conclude that groups are the most efficient locus for SF quenching. Thus, a fundamental difference exists between bound and unbound objects, or between dark matter haloes of different masses.

AB - We investigate the evolution of the star formation rate (SFR)-density relation in the Extended Chandra Deep Field South and the Great Observatories Origin Deep Survey fields up to z ~ 1.6. In addition to the 'traditional method', in which the environment is defined according to a statistical measurement of the local galaxy density, we use a 'dynamical' approach, where galaxies are classified according to three different environment regimes: group, 'filamentlike' and field. Both methods show no evidence of an SFR-density reversal. Moreover, group galaxies show a mean SFR lower than other environments up to z ~ 1, while at earlier epochs group and field galaxies exhibit consistent levels of star formation (SF) activity. We find that processes related to a massive dark matter halo must be dominant in the suppression of the SF below z ~ 1, with respect to purely density-related processes. We confirm this finding by studying the distribution of galaxies in different environments with respect to the so-called main sequence (MS) of star-forming galaxies. Galaxies in both group and 'filament-like' environments preferentially lie below the MS up to z ~ 1, with group galaxies exhibiting lower levels of star-forming activity at a given mass. At z > 1, the star-forming galaxies in groups reside on the MS. Groups exhibit the highest fraction of quiescent galaxies up to z ~ 1, after which group, 'filament-like' and field environments have a similar mix of galaxy types. We conclude that groups are the most efficient locus for SF quenching. Thus, a fundamental difference exists between bound and unbound objects, or between dark matter haloes of different masses.

KW - Galaxies: evolution

KW - Galaxies: groups: general

KW - Galaxies: star formation

KW - Infrared: galaxies

UR - http://www.scopus.com/inward/record.url?scp=84890096099&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84890096099&partnerID=8YFLogxK

U2 - 10.1093/mnras/stt1901

DO - 10.1093/mnras/stt1901

M3 - Article

AN - SCOPUS:84890096099

VL - 437

SP - 458

EP - 474

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 1

M1 - stt1901

ER -