Evidence for strong evolution in galaxy environmental quenching efficiency between z = 1.6 and z = 0.9

Nantais, Julie; Muzzin, Adam; Burg, R. F. J. van der; Wilson, Gillian; Lidman, C.; Foltz, Ryan; DeGroot, A.; Noble, Allison; Cooper, Michael C.; Demarco, R.

doi:10.1093/mnrasl/slw224

Cited by 95 publications

(133 citation statements)

References 58 publications

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“…as seen in Figure 7, at least for the clusters shown. This is at odds with the work by Nantais et al (2017), where environmental quenching efficiency was shown to strongly evolve between z = 1.6 and z = 0.9. However, the apparent absence of evolution at high masses that we find would be consistent with the scenario discussed previously, in which the three high-redshift clusters given in Figure 5 were more evolved than the average z 1.6…”

contrasting

confidence: 70%

“…We also calculated the cluster conversion fraction, or efficiency of quenching due to environment, according to the relation f f Phillips et al 2014;Balogh et al 2016;Nantais et al 2017). We give these values in Table 1 to facilitate comparison with other cluster studies, but leave interpretation of our values for future work.…”

Section: The Quiescent Fraction In Irc 0218 and The Fieldmentioning

confidence: 99%

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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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contrasting

confidence: 70%

Section: The Quiescent Fraction In Irc 0218 and The Fieldmentioning

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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“…Simulations by Muldrew et al (2015) indicate that with increasing redshift, the properties and halo distributions of current epoch massive clusters vary significantly. Variations in quenching efficiencies in cluster environments are found to be largest in higher redshift samples (Nantais et al 2017), suggesting halo mass or age may be dominant factors in galaxy evolution within cluster environments. The halo mass may also directly play a role in the number of mergers seen (Brodwin et al 2013), with more massive clusters assembling mass at earlier epochs whereas proto-clusters of the same epoch will still be assembling and accreting members.…”

Section: Discussionmentioning

confidence: 99%

“…to z 1 (e.g., van der Burg et al 2013;Darvish et al 2016;Nantais et al 2016Nantais et al , 2017) is thus unlikely to be due to enhanced galaxy-galaxy merging, at least in the most massive cluster systems. This suggests that the driving forces in quenching cluster galaxies are more likely to be due to interactions within the intracluster medium (such as ram-pressure stripping), harassment, or mass-induced selfquenching (e.g., Peng et al 2010;Bialas et al 2015).…”

Section: Discussionmentioning

confidence: 99%

Galaxy Merger Candidates in High-redshift Cluster Environments

Delahaye

Webb

Nantais

et al. 2017

ApJ

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We compile a sample of spectroscopically and photometrically selected cluster galaxies from four high-redshift galaxy clusters ( z 1.59 1.71 < <) from the Spitzer Adaptation of the Red-Sequence Cluster Survey (SpARCS), and a comparison field sample selected from the UKIDSS Deep Survey. Using near-infrared imaging from the Hubble Space Telescope, we classify potential mergers involving massive (M M 3 10 10 * ´) cluster members by eye, based on morphological properties such as tidal distortions, double nuclei, and projected near neighbors within 20 kpc. With a catalog of 23 spectroscopic and 32 photometric massive cluster members across the four clusters and 65 spectroscopic and 26 photometric comparable field galaxies, we find that after taking into account contamination from interlopers, 11.0 % 5.6 7.0 -+ of the cluster members are involved in potential mergers, compared to 24.7 % 4.6 5.3 -+ of the field galaxies. We see no evidence of merger enhancement in the central cluster environment with respect to the field, suggesting that galaxy-galaxy merging is not a stronger source of galaxy evolution in cluster environments compared to the field at these redshifts.

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“…Several large projects are exploiting mid-infrared data to search for high-redshift galaxy clusters using Spitzer and WISE (e.g., Eisenhardt et al 2008;Galametz et al 2010Galametz et al , 2013Papovich et al 2010;Stanford et al 2012Stanford et al , 2014Muzzin et al 2013;Rettura et al 2014;Wylezalek et al 2014;Brodwin et al 2015Brodwin et al , 2016PaternoMahler et al 2017). Such work has, for example, proved useful for (i) measuring the galaxy cluster autocorrelation function out to z∼1.5, which provides a measure of the typical galaxy cluster mass (Brodwin et al 2007); (ii) targeted cosmological surveys for z>1 SNe Ia in dust-free environments (Suzuki et al 2012); (iii) probing evolution in the σ-T x correlation (Brodwin et al 2011); (iv) using the rest-frame near-infrared luminosity function and rest-frame optical colors to probe the formation epoch of cluster galaxies (Mancone et al 2010Snyder et al 2012;Wylezalek et al 2014;Cooke et al 2015; Nantais et al 2016); (v) probing the role of AGN feedback in forming clusters (Galametz et al 2009;Martini et al 2013); (vi) leading cosmological investigations based on the incidence of massive, high-redshift clusters Gonzalez et al 2012);and (vii) probing the dependency of galaxy quenching on environment (Muzzin et al 2014, Nantais et al 2017.…”

Section: Introductionmentioning

confidence: 99%

HST Grism Confirmation of 16 Structures at 1.4 < z < 2.8 from the Clusters Around Radio-Loud AGN (CARLA) Survey

Noirot

Stern

Mei

et al. 2018

ApJ

109

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We report spectroscopic results from our 40-orbit Hubble Space Telescope slitless grism spectroscopy program observing the 20 densest Clusters Around Radio-Loud AGN (CARLA) candidate galaxy clusters at 1.4<z<2.8. These candidate rich structures, among the richest and most distant known, were identified on the basis of [3.6]-[4.5] color from a 408hr multi-cycle Spitzer program targeting 420 distant radio-loud AGN. We report the spectroscopic confirmation of 16 distant structures at 1.4<z<2.8 associated with the targeted powerful highredshift radio-loud AGN. We also report the serendipitous discovery and spectroscopic confirmation of seven additional structures at 0.87<z<2.12 not associated with the targeted radio-loud AGN. We find that 10 10 -10 11 M e member galaxies of our confirmed CARLA structures form significantly fewer stars than their field counterparts at all redshifts within 1.4z2. We also observe higher star-forming activity in the structure cores up to z=2, finding similar trends as cluster surveys at slightly lower redshifts (1.0 < z < 1.5). By design, our efficient strategy of obtaining just two grism orbits per field only obtains spectroscopic confirmation of emission line galaxies. Deeper spectroscopy will be required to study the population of evolved, massive galaxies in these (forming) clusters. Lacking multi-band coverage of the fields, we adopt a very conservative approach of calling all confirmations "structures," although we note that a number of features are consistent with some of them being bona fide galaxy clusters. Together this survey represents a unique and large homogenous sample of spectroscopically confirmed structures at high redshifts, potentially more than doubling the census of confirmed, massive clusters at z>1.4.

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Evidence for strong evolution in galaxy environmental quenching efficiency between z = 1.6 and z = 0.9

Cited by 95 publications

References 58 publications

The Ages of Passive Galaxies in a z = 1.62 Protocluster

The Ages of Passive Galaxies in a z = 1.62 Protocluster

Galaxy Merger Candidates in High-redshift Cluster Environments

HST Grism Confirmation of 16 Structures at 1.4 < z < 2.8 from the Clusters Around Radio-Loud AGN (CARLA) Survey

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