The Evolution of Environmental Quenching Timescales to z ∼ 1.6: Evidence for Dynamically Driven Quenching of the Cluster Galaxy Population

R. Foltz, G. Wilson, A. Muzzin, M. C. Cooper, J. Nantais, R. F.J. Van Der Burg, P. Cerulo, J. Chan, S. P. Fillingham, J. Surace, T. Webb, A. Noble, M. Lacy, M. McDonald, G. Rudnick, C. Lidman, R. Demarco, J. Hlavacek-Larrondo, H. K.C. Yee, S. PerlmutterB. Hayden

Resultado de la investigación: Article

7 Citas (Scopus)

Resumen

Using a sample of four galaxy clusters at 1.35 < z < 1.65 and 10 galaxy clusters at 0.85 < z < 1.35, we measure the environmental quenching timescale, t Q, corresponding to the time required after a galaxy is accreted by a cluster for it to fully cease star formation. Cluster members are selected by a photometric-redshift criterion, and categorized as star-forming, quiescent, or intermediate according to their dust-corrected rest-frame colors and magnitudes. We employ a "delayed-then-rapid" quenching model that relates a simulated cluster mass accretion rate to the observed numbers of each type of galaxy in the cluster to constrain t Q. For galaxies of mass M 1010.5 M o, we find a quenching timescale of t Q = Gyr in the z ∼ 1.5 cluster sample, and Gyr at z ∼ 1. Using values drawn from the literature, we compare the redshift evolution of t Q to timescales predicted for different physical quenching mechanisms. We find t Q to depend on host halo mass such that quenching occurs over faster timescales in clusters relative to groups, suggesting that properties of the host halo are responsible for quenching high-mass galaxies. Between z = 0 and z = 1.5, we find that t Q evolves faster than the molecular gas depletion timescale and slower than an estimated star formation rate-outflow timescale, but is consistent with the evolution of the dynamical time. This suggests that environmental quenching in these galaxies is driven by the motion of satellites relative to the cluster environment, although due to uncertainties in the atomic gas budget at high redshift, we cannot rule out quenching due to simple gas depletion.

Idioma originalEnglish
Número de artículo136
PublicaciónAstrophysical Journal
Volumen866
N.º2
DOI
EstadoPublished - 20 oct 2018

Huella dactilar

quenching
galaxies
timescale
gas
halos
depletion
outflow
monatomic gases
accretion
molecular gases
star formation rate
dust
budgets
star formation
color
stars
gases
rate

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Foltz, R. ; Wilson, G. ; Muzzin, A. ; Cooper, M. C. ; Nantais, J. ; Van Der Burg, R. F.J. ; Cerulo, P. ; Chan, J. ; Fillingham, S. P. ; Surace, J. ; Webb, T. ; Noble, A. ; Lacy, M. ; McDonald, M. ; Rudnick, G. ; Lidman, C. ; Demarco, R. ; Hlavacek-Larrondo, J. ; Yee, H. K.C. ; Perlmutter, S. ; Hayden, B. / The Evolution of Environmental Quenching Timescales to z ∼ 1.6 : Evidence for Dynamically Driven Quenching of the Cluster Galaxy Population. En: Astrophysical Journal. 2018 ; Vol. 866, N.º 2.
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abstract = "Using a sample of four galaxy clusters at 1.35 < z < 1.65 and 10 galaxy clusters at 0.85 < z < 1.35, we measure the environmental quenching timescale, t Q, corresponding to the time required after a galaxy is accreted by a cluster for it to fully cease star formation. Cluster members are selected by a photometric-redshift criterion, and categorized as star-forming, quiescent, or intermediate according to their dust-corrected rest-frame colors and magnitudes. We employ a {"}delayed-then-rapid{"} quenching model that relates a simulated cluster mass accretion rate to the observed numbers of each type of galaxy in the cluster to constrain t Q. For galaxies of mass M ∗ 1010.5 M o, we find a quenching timescale of t Q = Gyr in the z ∼ 1.5 cluster sample, and Gyr at z ∼ 1. Using values drawn from the literature, we compare the redshift evolution of t Q to timescales predicted for different physical quenching mechanisms. We find t Q to depend on host halo mass such that quenching occurs over faster timescales in clusters relative to groups, suggesting that properties of the host halo are responsible for quenching high-mass galaxies. Between z = 0 and z = 1.5, we find that t Q evolves faster than the molecular gas depletion timescale and slower than an estimated star formation rate-outflow timescale, but is consistent with the evolution of the dynamical time. This suggests that environmental quenching in these galaxies is driven by the motion of satellites relative to the cluster environment, although due to uncertainties in the atomic gas budget at high redshift, we cannot rule out quenching due to simple gas depletion.",
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Foltz, R, Wilson, G, Muzzin, A, Cooper, MC, Nantais, J, Van Der Burg, RFJ, Cerulo, P, Chan, J, Fillingham, SP, Surace, J, Webb, T, Noble, A, Lacy, M, McDonald, M, Rudnick, G, Lidman, C, Demarco, R, Hlavacek-Larrondo, J, Yee, HKC, Perlmutter, S & Hayden, B 2018, 'The Evolution of Environmental Quenching Timescales to z ∼ 1.6: Evidence for Dynamically Driven Quenching of the Cluster Galaxy Population', Astrophysical Journal, vol. 866, n.º 2, 136. https://doi.org/10.3847/1538-4357/aad80d

The Evolution of Environmental Quenching Timescales to z ∼ 1.6 : Evidence for Dynamically Driven Quenching of the Cluster Galaxy Population. / Foltz, R.; Wilson, G.; Muzzin, A.; Cooper, M. C.; Nantais, J.; Van Der Burg, R. F.J.; Cerulo, P.; Chan, J.; Fillingham, S. P.; Surace, J.; Webb, T.; Noble, A.; Lacy, M.; McDonald, M.; Rudnick, G.; Lidman, C.; Demarco, R.; Hlavacek-Larrondo, J.; Yee, H. K.C.; Perlmutter, S.; Hayden, B.

En: Astrophysical Journal, Vol. 866, N.º 2, 136, 20.10.2018.

Resultado de la investigación: Article

TY - JOUR

T1 - The Evolution of Environmental Quenching Timescales to z ∼ 1.6

T2 - Evidence for Dynamically Driven Quenching of the Cluster Galaxy Population

AU - Foltz, R.

AU - Wilson, G.

AU - Muzzin, A.

AU - Cooper, M. C.

AU - Nantais, J.

AU - Van Der Burg, R. F.J.

AU - Cerulo, P.

AU - Chan, J.

AU - Fillingham, S. P.

AU - Surace, J.

AU - Webb, T.

AU - Noble, A.

AU - Lacy, M.

AU - McDonald, M.

AU - Rudnick, G.

AU - Lidman, C.

AU - Demarco, R.

AU - Hlavacek-Larrondo, J.

AU - Yee, H. K.C.

AU - Perlmutter, S.

AU - Hayden, B.

PY - 2018/10/20

Y1 - 2018/10/20

N2 - Using a sample of four galaxy clusters at 1.35 < z < 1.65 and 10 galaxy clusters at 0.85 < z < 1.35, we measure the environmental quenching timescale, t Q, corresponding to the time required after a galaxy is accreted by a cluster for it to fully cease star formation. Cluster members are selected by a photometric-redshift criterion, and categorized as star-forming, quiescent, or intermediate according to their dust-corrected rest-frame colors and magnitudes. We employ a "delayed-then-rapid" quenching model that relates a simulated cluster mass accretion rate to the observed numbers of each type of galaxy in the cluster to constrain t Q. For galaxies of mass M ∗ 1010.5 M o, we find a quenching timescale of t Q = Gyr in the z ∼ 1.5 cluster sample, and Gyr at z ∼ 1. Using values drawn from the literature, we compare the redshift evolution of t Q to timescales predicted for different physical quenching mechanisms. We find t Q to depend on host halo mass such that quenching occurs over faster timescales in clusters relative to groups, suggesting that properties of the host halo are responsible for quenching high-mass galaxies. Between z = 0 and z = 1.5, we find that t Q evolves faster than the molecular gas depletion timescale and slower than an estimated star formation rate-outflow timescale, but is consistent with the evolution of the dynamical time. This suggests that environmental quenching in these galaxies is driven by the motion of satellites relative to the cluster environment, although due to uncertainties in the atomic gas budget at high redshift, we cannot rule out quenching due to simple gas depletion.

AB - Using a sample of four galaxy clusters at 1.35 < z < 1.65 and 10 galaxy clusters at 0.85 < z < 1.35, we measure the environmental quenching timescale, t Q, corresponding to the time required after a galaxy is accreted by a cluster for it to fully cease star formation. Cluster members are selected by a photometric-redshift criterion, and categorized as star-forming, quiescent, or intermediate according to their dust-corrected rest-frame colors and magnitudes. We employ a "delayed-then-rapid" quenching model that relates a simulated cluster mass accretion rate to the observed numbers of each type of galaxy in the cluster to constrain t Q. For galaxies of mass M ∗ 1010.5 M o, we find a quenching timescale of t Q = Gyr in the z ∼ 1.5 cluster sample, and Gyr at z ∼ 1. Using values drawn from the literature, we compare the redshift evolution of t Q to timescales predicted for different physical quenching mechanisms. We find t Q to depend on host halo mass such that quenching occurs over faster timescales in clusters relative to groups, suggesting that properties of the host halo are responsible for quenching high-mass galaxies. Between z = 0 and z = 1.5, we find that t Q evolves faster than the molecular gas depletion timescale and slower than an estimated star formation rate-outflow timescale, but is consistent with the evolution of the dynamical time. This suggests that environmental quenching in these galaxies is driven by the motion of satellites relative to the cluster environment, although due to uncertainties in the atomic gas budget at high redshift, we cannot rule out quenching due to simple gas depletion.

KW - galaxies: clusters: general

KW - galaxies: evolution

KW - galaxies: formation

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U2 - 10.3847/1538-4357/aad80d

DO - 10.3847/1538-4357/aad80d

M3 - Article

AN - SCOPUS:85063598438

VL - 866

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

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