Evidence for a change in the dominant satellite galaxy quenching mechanism at<i>z</i> = 1

Balogh, Michael L.; McGee, Sean L.; Mok, Angus; Muzzin, Adam; Burg, R. F. J. van der; Bower, Richard G.; Finoguenov, A.; Hoekstra, Henk; Lidman, C.; Mulchaey, John S.; Noble, Allison; Parker, Laura C.; Tanaka, Masayuki; Wilman, David J.; Webb, Tracy; Wilson, Gillian; Yee, H. K. C.

doi:10.1093/mnras/stv2949

Cited by 133 publications

(282 citation statements)

References 106 publications

(187 reference statements)

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“…Van der Burg et al (2013), Kovač et al (2014), and Balogh et al (2016) have found that the environment plays an important role in determining the star formation activity of satellites, at least up to z ∼ 1. However these works have only probed relatively massive haloes (M h 10 13 M ⊙ ).…”

Section: Passive Fractionsmentioning

confidence: 99%

“…This parameter, sometimes called the satellite quenching efficiency, quantifies the fraction of galaxies that had their star formation activity quenched by environment specific processes since they accreted as satellites into a more massive halo (see also Kovač et al 2014;Hirschmann et al 2014;Balogh et al 2016). It is defined as:…”

Section: Satellite Quenching Efficiencymentioning

confidence: 99%

“…By exploiting the multiplexing of spectroscopic instruments at 8-10 meter class telescopes (e.g. VIMOS and GMOS, Lilly et al 2007;Kurk et al 2013;Balogh et al 2014), these works showed that the environment plays a role in quenching the star formation activity of galaxies accreted onto massive haloes (satellite galaxies) up to z ∼ 1 (Muzzin et al 2012;Quadri et al 2012;Knobel et al 2013;Kovač et al 2014;Balogh et al 2016), although the samples are limited to massive galaxies or a small number of objects.…”

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confidence: 99%

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

Fossati

Wilman

Mendel

et al. 2017

ApJ

118

131

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We make publicly available a catalog of calibrated environmental measures for galaxies in the five 3D-HST/CANDELS deep fields. Leveraging the spectroscopic and grism redshifts from the 3D-HST survey, multi wavelength 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 < 24 mag in the redshift range 0.5 < z < 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 is a central or a satellite galaxy. The same procedure is applied to a z = 0 sample selected from SDSS. 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 quench ∼ 2 − 5 Gyr; 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 10 14 M ⊙ ), satellites are quenched by exhaustion of their gas reservoir in 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 (τ f ∼ 0.4 − 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.

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Section: Passive Fractionsmentioning

confidence: 99%

Section: Satellite Quenching Efficiencymentioning

confidence: 99%

mentioning

confidence: 99%

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

Fossati

Wilman

Mendel

et al. 2017

ApJ

118

131

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“…Since we only observe environmental effects within the dense groups of this protocluster, this suggests that environmental effects will become more prominent simply due to the hierarchical growth of clusters. However, this picture is too simplistic as the mechanism that quenches satellite galaxies may not be the same in the distant and local Universe (Balogh et al 2016).…”

Section: The Evolution Of Environmental Effects In Protoclustersmentioning

confidence: 99%

The impact of protocluster environments atz= 1.6

Hatch

Cooke

Muldrew

et al. 2016

Mon. Not. R. Astron. Soc.

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We investigate the effects of dense environments on galaxy evolution by examining how the properties of galaxies in the z = 1.6 protocluster Cl 0218.3−0510 depend on their location. We determine galaxy properties using spectral energy distribution fitting to 14-band photometry, including data at three wavelengths that tightly bracket the Balmer and 4000Å breaks of the protocluster galaxies. We find that two-thirds of the protocluster galaxies, which lie between several compact groups, are indistinguishable from field galaxies. The other third, which reside within the groups, differ significantly from the intergroup galaxies in both colour and specific star formation rate. We find that the fraction of red galaxies within the massive protocluster groups is twice that of the intergroup region. These excess red galaxies are due to enhanced fractions of both passive galaxies (1.7 times that of the intergroup region) and dusty star-forming galaxies (3 times that of the intergroup region). We infer that some protocluster galaxies are processed in the groups before the cluster collapses. These processes act to suppress star formation and change the mode of star formation from unobscured to obscured.

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“…By way of secular cluster processes, blue galaxies of different masses and brightnesses are shown to transition on different timescales across different epochs (e.g. Balogh et al 2016;Muzzin et al 2014;Ilbert et al 2015). A variety of short and long-term mechanisms could result in a starburst in the past ∼1 Gyr followed by rapid quenching, to produce the current post-starburst population.…”

Section: Discussionmentioning

confidence: 99%

Star Formation in the Cluster Merger DLSCL J0916.2+2953

Mansheim

Lemaux

Dawson

et al. 2017

ApJ

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We investigate star formation in DLSCL J0916.2+2953, a dissociative merger of two clusters at z=0.53 that has progressed 1.1 +1.3 −0.4 Gyr since first pass-through. We attempt to reveal the effects a collision may have had on the evolution of the cluster galaxies by tracing their star formation history. We probe current and recent activity to identify a possible star formation event at the time of the merger using EW(Hδ), EW([OII]), and D n (4000) measured from the composite spectra of 64 cluster and 153 coeval field galaxies. We supplement Keck DEIMOS spectra with DLS and HST imaging to determine the color, stellar mass, and morphology of each galaxy and conduct a comprehensive study of the populations in this complex structure. Spectral results indicate the average cluster and cluster red sequence galaxies experienced no enhanced star formation relative to the surrounding field during the merger, ruling out a predominantly merger-quenched population. We find that the average blue galaxy in the North cluster is currently active and in the South cluster is currently post-starburst having undergone a recent star formation event. While the North activity could be latent or longterm merger effects, a young blue stellar population and irregular geometry suggest the cluster was still forming prior the collision. While the South activity coincides with the time of the merger, the blue early-type population could be a result of secular cluster processes. The evidence suggests that the dearth or surfeit of activity is indiscernible from normal cluster galaxy evolution.

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Evidence for a change in the dominant satellite galaxy quenching mechanism atz = 1

Cited by 133 publications

References 106 publications

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

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

The impact of protocluster environments atz= 1.6

Star Formation in the Cluster Merger DLSCL J0916.2+2953

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