EVOLUTION OF STAR FORMATION PROPERTIES OF HIGH-REDSHIFT CLUSTER GALAXIES SINCE<i>z</i>= 2

Lee, Seong-Kook; Im, Myungshin; Kim, Jae-Woo; Lotz, Jennifer M.; McPartland, Conor; Peth, Michael; Koekemoer, Anton M.

doi:10.1088/0004-637x/810/2/90

Cited by 43 publications

(65 citation statements)

References 124 publications

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“…This offset is probably due to the relatively unreliable photometric redshifts from the UDS DR1 catalogue used by van Breukelen et al (2006), which was much shallower than the DR8 catalogue. We recover 85.2% (17/20) of the cluster candidates listed in Lee et al (2015), where they locate clusters as galaxy overdensities in spatial and photometric redshift space. We also locate 78.5% (11/14) of the X-ray selected cluster candidates in Finoguenov et al (2010).…”

Section: Comparison With Previous Studies Of Clusters In the Udsmentioning

confidence: 83%

“…Clusters in the UDS have been located by Finoguenov et al (2010) through the detection of extended XMM-Newton Xray emission; by van Breukelen et al (2006) and Lee et al (2015), who searched for galaxy overdensities in the optical and near infrared photometric surveys, and by Geach et al (2007), who used low-power radio galaxies as beacons for overdensities. We compare cluster samples derived from these methods with our FoF cluster sample to check the robustness of our detection method.…”

Section: Comparison With Previous Studies Of Clusters In the Udsmentioning

confidence: 99%

“…Detected byvan Breukelen et al (2006), b detected byLee et al (2015), c detected byFinoguenov et al (2010), d detected byGeach et al (2007) …”

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confidence: 99%

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The enhancement of rapidly quenched galaxies in distant clusters at 0.5 < z < 1.0

Socolovsky

Almaini

Hatch

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We investigate the relationship between environment and galaxy evolution in the redshift range 0.5 < z < 1.0. Galaxy overdensities are selected using a Friends-of-Friends algorithm, applied to deep photometric data in the Ultra-Deep Survey (UDS) field. A study of the resulting stellar mass functions reveals clear differences between cluster and field environments, with a strong excess of low-mass rapidly quenched galaxies in cluster environments compared to the field. Cluster environments also show a corresponding deficit of young, low-mass star-forming galaxies, which show a sharp radial decline towards cluster centres. By comparing mass functions and radial distributions, we conclude that young star-forming galaxies are rapidly quenched as they enter overdense environments, becoming post-starburst galaxies before joining the red sequence. Our results also point to the existence of two environmental quenching pathways operating in galaxy clusters, operating on different timescales. Fast quenching acts on galaxies with high specific star-formation rates, operating on timescales shorter than the cluster dynamical time (< 1 Gyr). In contrast, slow quenching affects galaxies with moderate specific star-formation rates, regardless of their stellar mass, and acts on longer timescales ( 1 Gyr). Of the cluster galaxies in the stellar mass range 9.0 < log(M/M ) < 10.5 quenched during this epoch, we find that 73% were transformed through fast quenching, while the remaining 27% followed the slow quenching route. Peng et al. (2010) compare the stellar mass and environment of galaxies with their star formation rate (SFR), and conclude that there are two separate quenching processes that cause galaxies to cease forming stars. They call these processes "environmental quenching" and "mass quenching". The efficiency of environmental quenching depends on the environment of a galaxy, such that galaxies in high density environments are more likely to be quenched. Independently, the efficiency of mass quenching correlates with the stellar mass of the galaxy, such that more massive galaxies are more likely to be quenched. Additionally, there is morphological quenching (Martig et al. 2009), in which the structure of the galaxy changes first, leading to a more stable configuration which prevents gas from collapsing into stars. However, the physical processes that are responsible for these quenching pathways remain unclear.The most popular mechanisms used to explain mass

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Section: Comparison With Previous Studies Of Clusters In the Udsmentioning

confidence: 83%

Section: Comparison With Previous Studies Of Clusters In the Udsmentioning

confidence: 99%

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The enhancement of rapidly quenched galaxies in distant clusters at 0.5 < z < 1.0

Socolovsky

Almaini

Hatch

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…Several studies (e.g., Peng et al (2010), Lee et al (2015) and Hirschmann et al (2016)) find that this environmental quenching is important especially for low-mass satellite galaxies. For completeness, we show in Fig.…”

Section: The Relation Between the Environment And The Star Formation mentioning

confidence: 99%

The morphology–density relation: impact on the satellite fraction

Teklu¹,

Dolag

Burkert

2017

Monthly Notices of the Royal Astronomical Society

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In the past years several authors studied the abundance of satellites around galaxies in order to better estimate, for example, the halo masses of the host galaxies. To investigate this connection, we analyze a sample of galaxies with stellar masses M star ≥ 10 10 M ⊙ , taken from the hydrodynamical cosmological simulation suit Magneticum. We find that the satellite fraction of centrals is independent of their morphology. With the exception of very massive galaxies at low redshift, our results do not support the assumption that the dark matter haloes of spheroidal galaxies are significantly more massive than those of disc galaxies at fixed stellar mass. We show that the density-morphology-relation, i.e. the correlation between the quiescent fraction of satellites and the environmental density, starts to build up at z ∼ 2 and is independent of the star formation properties of the central galaxies. We conclude that environmental quenching is more important for satellite galaxies than for centrals. Our simulations also indicate that conformity is already in place at z = 2, where formation redshift and current star formation rate (SFR) of central and satellite galaxies already clearly correlate. Centrals with low SFRs tend to have formed earlier (at fixed stellar mass) while centrals with high SFR formed later, with a typical formation redshift well in agreement with current observations. However, we confirm the recent observations that the apparent number of satellites of spheroidal galaxies is significantly larger than for disc galaxies. This difference completely originates from the inclusion of companion galaxies, i.e. galaxies that do not sit in the potential minimum of a massive dark matter halo. Thus, due to the density-morphological-relation the number of satellites is not a good tracer for the halo mass, unless samples are restricted to the central galaxies of dark matter haloes only.

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“…In recent years, a steadily increasing number of high-redshift (z 1.5 > ) clusters or protoclusters have been discovered and confirmed (e.g., Andreon et al 2009;Papovich et al 2010;Gobat et al 2011;Santos et al 2011;Stanford et al 2012;Zeimann et al 2012;Muzzin et al 2013b;Mei et al 2015;Webb et al 2015;Cooke et al 2016;Wang et al 2016). What studies have found is that, although significant cluster-to-cluster scatter exists, z 1.5  clusters often still have well-developed red sequences and elevated quiescent fractions relative to the field (Quadri et al 2012;Newman et al 2014;Cooke et al 2016;Nantais et al 2016; but, also see Lee et al 2015). However, it is not yet clear what mechanisms drive the observed enhanced quiescent fractions.…”

Section: Introductionmentioning

confidence: 99%

The Ages of Passive Galaxies in a z = 1.62 Protocluster

Lee-Brown

Rudnick

Momcheva

et al. 2017

ApJ

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We present a study of the relation between galaxy stellar age and mass for 14 members of the z = 1.62 protocluster IRC 0218, using multiband imaging and HST G102 and G141 grism spectroscopy. Using UVJ colors to separate galaxies into star-forming and quiescent populations, we find that, at stellar masses M M 10 10.85 *   , the quiescent fraction in the protocluster is f . Using galaxy D 4000 n ( ) values derived from the G102 spectroscopy, we find no relation between galaxy stellar age and mass. These results may reflect the impact of merger-driven mass redistribution-which is plausible, as this cluster is known to host many dry mergers. Alternately, they may imply that the trend in f Q in IRC 0218 was imprinted over a short timescale in the protocluster's assembly history.Comparing our results with those of other high-redshift studies and studies of clusters at z 1 , we determine that our observed relation between f Q and stellar mass only mildly evolves between z 1.6and z 1 , and only at stellar masses M M 10 10.85 *   . Both the z 1 and z 1.6 results are in agreement that the red sequence in dense environments was already populated at high redshift, z 3  , placing constraints on the mechanism(s) responsible for quenching in dense environments at z 1.5  .

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EVOLUTION OF STAR FORMATION PROPERTIES OF HIGH-REDSHIFT CLUSTER GALAXIES SINCEz= 2

Cited by 43 publications

References 124 publications

The enhancement of rapidly quenched galaxies in distant clusters at 0.5 < z < 1.0

The enhancement of rapidly quenched galaxies in distant clusters at 0.5 < z < 1.0

The morphology–density relation: impact on the satellite fraction

The Ages of Passive Galaxies in a z = 1.62 Protocluster

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