# Galaxy Environment in the 3D-HST Fields: Witnessing the Onset of Satellite Quenching at z ~ 1–2

M. Fossati, D. J. Wilman, J. T. Mendel, R. P. Saglia, A. Galametz, A. Beifiori, R. Bender, J. C. C. Chan, M. Fabricius, K. Bandara, G. B. Brammer, R. Davies, N. M. Förster Schreiber, R. Genzel, W. Hartley, S. K. Kulkarni, P. Lang, I. G. Momcheva, E. J. Nelson, R. SkeltonL. J. Tacconi, K. Tadaki, H. Übler, P. G. Van Dokkum, E. Wisnioski, K. E. Whitaker, E. Wuyts, S. Wuyts

Research output: Contribution to journalArticle

35 Citations (Scopus)

### Abstract

We make publicly available a catalog of calibrated environmental measures for galaxies in the five 3D-Hubble Space Telescope (HST)/CANDELS deep fields. Leveraging the spectroscopic and grism redshifts from the 3D-HST survey, multiwavelength photometry from CANDELS, and wider field public data for edge corrections, we derive densities in fixed apertures to characterize the environment of galaxies brighter than ${{JH}}_{140}\lt 24$ mag in the redshift range $0.5\lt z\lt 3.0$. By linking observed galaxies to a mock sample, selected to reproduce the 3D-HST sample selection and redshift accuracy, each 3D-HST galaxy is assigned a probability density function of the host halo mass, and a probability that it is a central or a satellite galaxy. The same procedure is applied to a z = 0 sample selected from Sloan Digital Sky Survey. We compute the fraction of passive central and satellite galaxies as a function of stellar and halo mass, and redshift, and then derive the fraction of galaxies that were quenched by environment specific processes. Using the mock sample, we estimate that the timescale for satellite quenching is ${t}_{\mathrm{quench}}\sim 2\mbox{--}5\,\mathrm{Gyr};$ it is longer at lower stellar mass or lower redshift, but remarkably independent of halo mass. This indicates that, in the range of environments commonly found within the 3D-HST sample (${M}_{h}\lesssim {10}^{14}\,{M}_{\odot }$), satellites are quenched by exhaustion of their gas reservoir in the absence of cosmological accretion. We find that the quenching times can be separated into a delay phase, during which satellite galaxies behave similarly to centrals at fixed stellar mass, and a phase where the star formation rate drops rapidly (${\tau }_{f}\sim 0.4\mbox{--}0.6$ Gyr), as shown previously at z = 0. We conclude that this scenario requires satellite galaxies to retain a large reservoir of multi-phase gas upon accretion, even at high redshift, and that this gas sustains star formation for the long quenching times observed.
Original language English 153 37 Astrophysical Journal 835 2 24 Jan 2017 https://doi.org/10.3847/1538-4357/835/2/153 Published - 1 Feb 2017

### Fingerprint

Hubble Space Telescope
quenching
galaxies
stellar mass
halos
accretion
probability density function
gas
exhaustion
star formation rate
probability density functions
timescale
gases
catalogs
photometry
star formation
apertures
vapor phases
estimates

### Cite this

Galaxy Environment in the 3D-HST Fields : Witnessing the Onset of Satellite Quenching at z ~ 1–2. / Fossati, M.; Wilman, D. J.; Mendel, J. T.; Saglia, R. P.; Galametz, A.; Beifiori, A.; Bender, R.; Chan, J. C. C.; Fabricius, M.; Bandara, K.; Brammer, G. B.; Davies, R.; Förster Schreiber, N. M.; Genzel, R.; Hartley, W.; Kulkarni, S. K.; Lang, P.; Momcheva, I. G.; Nelson, E. J.; Skelton, R.; Tacconi, L. J.; Tadaki, K.; Übler, H.; Van Dokkum, P. G.; Wisnioski, E.; Whitaker, K. E.; Wuyts, E.; Wuyts, S.

In: Astrophysical Journal, Vol. 835, No. 2, 153, 01.02.2017.

Research output: Contribution to journalArticle

Fossati, M, Wilman, DJ, Mendel, JT, Saglia, RP, Galametz, A, Beifiori, A, Bender, R, Chan, JCC, Fabricius, M, Bandara, K, Brammer, GB, Davies, R, Förster Schreiber, NM, Genzel, R, Hartley, W, Kulkarni, SK, Lang, P, Momcheva, IG, Nelson, EJ, Skelton, R, Tacconi, LJ, Tadaki, K, Übler, H, Van Dokkum, PG, Wisnioski, E, Whitaker, KE, Wuyts, E & Wuyts, S 2017, 'Galaxy Environment in the 3D-HST Fields: Witnessing the Onset of Satellite Quenching at z ~ 1–2', Astrophysical Journal, vol. 835, no. 2, 153. https://doi.org/10.3847/1538-4357/835/2/153
Fossati, M. ; Wilman, D. J. ; Mendel, J. T. ; Saglia, R. P. ; Galametz, A. ; Beifiori, A. ; Bender, R. ; Chan, J. C. C. ; Fabricius, M. ; Bandara, K. ; Brammer, G. B. ; Davies, R. ; Förster Schreiber, N. M. ; Genzel, R. ; Hartley, W. ; Kulkarni, S. K. ; Lang, P. ; Momcheva, I. G. ; Nelson, E. J. ; Skelton, R. ; Tacconi, L. J. ; Tadaki, K. ; Übler, H. ; Van Dokkum, P. G. ; Wisnioski, E. ; Whitaker, K. E. ; Wuyts, E. ; Wuyts, S. / Galaxy Environment in the 3D-HST Fields : Witnessing the Onset of Satellite Quenching at z ~ 1–2. In: Astrophysical Journal. 2017 ; Vol. 835, No. 2.
@article{1c94068a48614998b4d6da758afebdcd,
title = "Galaxy Environment in the 3D-HST Fields: Witnessing the Onset of Satellite Quenching at z ~ 1–2",
abstract = "We make publicly available a catalog of calibrated environmental measures for galaxies in the five 3D-Hubble Space Telescope (HST)/CANDELS deep fields. Leveraging the spectroscopic and grism redshifts from the 3D-HST survey, multiwavelength photometry from CANDELS, and wider field public data for edge corrections, we derive densities in fixed apertures to characterize the environment of galaxies brighter than ${{JH}}_{140}\lt 24$ mag in the redshift range $0.5\lt z\lt 3.0$. By linking observed galaxies to a mock sample, selected to reproduce the 3D-HST sample selection and redshift accuracy, each 3D-HST galaxy is assigned a probability density function of the host halo mass, and a probability that it is a central or a satellite galaxy. The same procedure is applied to a z = 0 sample selected from Sloan Digital Sky Survey. We compute the fraction of passive central and satellite galaxies as a function of stellar and halo mass, and redshift, and then derive the fraction of galaxies that were quenched by environment specific processes. Using the mock sample, we estimate that the timescale for satellite quenching is ${t}_{\mathrm{quench}}\sim 2\mbox{--}5\,\mathrm{Gyr};$ it is longer at lower stellar mass or lower redshift, but remarkably independent of halo mass. This indicates that, in the range of environments commonly found within the 3D-HST sample (${M}_{h}\lesssim {10}^{14}\,{M}_{\odot }$), satellites are quenched by exhaustion of their gas reservoir in the absence of cosmological accretion. We find that the quenching times can be separated into a delay phase, during which satellite galaxies behave similarly to centrals at fixed stellar mass, and a phase where the star formation rate drops rapidly (${\tau }_{f}\sim 0.4\mbox{--}0.6$ Gyr), as shown previously at z = 0. We conclude that this scenario requires satellite galaxies to retain a large reservoir of multi-phase gas upon accretion, even at high redshift, and that this gas sustains star formation for the long quenching times observed.",
author = "M. Fossati and Wilman, {D. J.} and Mendel, {J. T.} and Saglia, {R. P.} and A. Galametz and A. Beifiori and R. Bender and Chan, {J. C. C.} and M. Fabricius and K. Bandara and Brammer, {G. B.} and R. Davies and {F{\"o}rster Schreiber}, {N. M.} and R. Genzel and W. Hartley and Kulkarni, {S. K.} and P. Lang and Momcheva, {I. G.} and Nelson, {E. J.} and R. Skelton and Tacconi, {L. J.} and K. Tadaki and H. {\"U}bler and {Van Dokkum}, {P. G.} and E. Wisnioski and Whitaker, {K. E.} and E. Wuyts and S. Wuyts",
year = "2017",
month = "2",
day = "1",
doi = "10.3847/1538-4357/835/2/153",
language = "English",
volume = "835",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing",
number = "2",

}

TY - JOUR

T1 - Galaxy Environment in the 3D-HST Fields

T2 - Witnessing the Onset of Satellite Quenching at z ~ 1–2

AU - Fossati, M.

AU - Wilman, D. J.

AU - Mendel, J. T.

AU - Saglia, R. P.

AU - Galametz, A.

AU - Beifiori, A.

AU - Bender, R.

AU - Chan, J. C. C.

AU - Fabricius, M.

AU - Bandara, K.

AU - Brammer, G. B.

AU - Davies, R.

AU - Förster Schreiber, N. M.

AU - Genzel, R.

AU - Hartley, W.

AU - Kulkarni, S. K.

AU - Lang, P.

AU - Momcheva, I. G.

AU - Nelson, E. J.

AU - Skelton, R.

AU - Tacconi, L. J.

AU - Übler, H.

AU - Van Dokkum, P. G.

AU - Wisnioski, E.

AU - Whitaker, K. E.

AU - Wuyts, E.

AU - Wuyts, S.

PY - 2017/2/1

Y1 - 2017/2/1

N2 - We make publicly available a catalog of calibrated environmental measures for galaxies in the five 3D-Hubble Space Telescope (HST)/CANDELS deep fields. Leveraging the spectroscopic and grism redshifts from the 3D-HST survey, multiwavelength photometry from CANDELS, and wider field public data for edge corrections, we derive densities in fixed apertures to characterize the environment of galaxies brighter than ${{JH}}_{140}\lt 24$ mag in the redshift range $0.5\lt z\lt 3.0$. By linking observed galaxies to a mock sample, selected to reproduce the 3D-HST sample selection and redshift accuracy, each 3D-HST galaxy is assigned a probability density function of the host halo mass, and a probability that it is a central or a satellite galaxy. The same procedure is applied to a z = 0 sample selected from Sloan Digital Sky Survey. We compute the fraction of passive central and satellite galaxies as a function of stellar and halo mass, and redshift, and then derive the fraction of galaxies that were quenched by environment specific processes. Using the mock sample, we estimate that the timescale for satellite quenching is ${t}_{\mathrm{quench}}\sim 2\mbox{--}5\,\mathrm{Gyr};$ it is longer at lower stellar mass or lower redshift, but remarkably independent of halo mass. This indicates that, in the range of environments commonly found within the 3D-HST sample (${M}_{h}\lesssim {10}^{14}\,{M}_{\odot }$), satellites are quenched by exhaustion of their gas reservoir in the absence of cosmological accretion. We find that the quenching times can be separated into a delay phase, during which satellite galaxies behave similarly to centrals at fixed stellar mass, and a phase where the star formation rate drops rapidly (${\tau }_{f}\sim 0.4\mbox{--}0.6$ Gyr), as shown previously at z = 0. We conclude that this scenario requires satellite galaxies to retain a large reservoir of multi-phase gas upon accretion, even at high redshift, and that this gas sustains star formation for the long quenching times observed.

AB - We make publicly available a catalog of calibrated environmental measures for galaxies in the five 3D-Hubble Space Telescope (HST)/CANDELS deep fields. Leveraging the spectroscopic and grism redshifts from the 3D-HST survey, multiwavelength photometry from CANDELS, and wider field public data for edge corrections, we derive densities in fixed apertures to characterize the environment of galaxies brighter than ${{JH}}_{140}\lt 24$ mag in the redshift range $0.5\lt z\lt 3.0$. By linking observed galaxies to a mock sample, selected to reproduce the 3D-HST sample selection and redshift accuracy, each 3D-HST galaxy is assigned a probability density function of the host halo mass, and a probability that it is a central or a satellite galaxy. The same procedure is applied to a z = 0 sample selected from Sloan Digital Sky Survey. We compute the fraction of passive central and satellite galaxies as a function of stellar and halo mass, and redshift, and then derive the fraction of galaxies that were quenched by environment specific processes. Using the mock sample, we estimate that the timescale for satellite quenching is ${t}_{\mathrm{quench}}\sim 2\mbox{--}5\,\mathrm{Gyr};$ it is longer at lower stellar mass or lower redshift, but remarkably independent of halo mass. This indicates that, in the range of environments commonly found within the 3D-HST sample (${M}_{h}\lesssim {10}^{14}\,{M}_{\odot }$), satellites are quenched by exhaustion of their gas reservoir in the absence of cosmological accretion. We find that the quenching times can be separated into a delay phase, during which satellite galaxies behave similarly to centrals at fixed stellar mass, and a phase where the star formation rate drops rapidly (${\tau }_{f}\sim 0.4\mbox{--}0.6$ Gyr), as shown previously at z = 0. We conclude that this scenario requires satellite galaxies to retain a large reservoir of multi-phase gas upon accretion, even at high redshift, and that this gas sustains star formation for the long quenching times observed.

UR - https://doi.org/10.3847/1538-4357/835/2/153

U2 - 10.3847/1538-4357/835/2/153

DO - 10.3847/1538-4357/835/2/153

M3 - Article

VL - 835

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 153

ER -