Stellar mass function of cluster galaxies at<i>z</i>~ 1.5: evidence for reduced quenching efficiency at high redshift

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

doi:10.1051/0004-6361/201628663

Cited by 97 publications

(152 citation statements)

References 92 publications

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“…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%

“…SpARCS033056-284300 (z=1.626) and SpARCS022426-032331 (z 1.633; = hereafter J0330 and J0224) were both presented in Lidman et al (2012), with J0224 additionally described in Muzzin et al (2013). SpARCS022546-035517 at z=1.598 (hereafter J0225) was presented in Nantais et al (2016). The clusters are likely not fully virialized and the difficulty in obtaining spectroscopic redshifts for the passive members in the central core inhibits the ability to derive robust velocity dispersions; however, richness measurements suggest lower cluster mass limits of M 10 14  .…”

Section: Cluster Samplementioning

confidence: 99%

“…For clusters J0224, J0225, and J0330, 11 to 12 band (not including additional HST imaging described below) photometry is available. All three clusters have optical ugriz, near-infrared YK s , and infrared (3.6 μ, 4.5 μm, 5.8 μm, 8.0 μm), with additional near-infrared J available for clusters J0224 and J0330 (Nantais et al 2016). J1049 has 8 band photometry available with ugrz from CFHT (Tudorica et al 2017), JK s from UKIDSS (Lawrence et al 2007), and IRAC 3.6 μm, 4.5 μm from SERVS (Mauduit et al 2012).…”

Section: Cluster Samplementioning

confidence: 99%

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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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Section: Discussionmentioning

confidence: 99%

Section: Cluster Samplementioning

confidence: 99%

Section: Cluster Samplementioning

confidence: 99%

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Galaxy Merger Candidates in High-redshift Cluster Environments

Delahaye

Webb

Nantais

et al. 2017

ApJ

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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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“…Studying the faint, and more common, galaxy population at 1 < z < 1.5 usually relies heavily on photometric redshifts (e.g. Nantais et al 2016).…”

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confidence: 99%

Gemini Observations of Galaxies in Rich Early Environments (GOGREEN) I: survey description

Balogh

Gilbank

Muzzin

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We describe a new Large Program in progress on the Gemini North and South telescopes: Gemini Observations of Galaxies in Rich Early Environments (GOGREEN). This is an imaging and deep spectroscopic survey of 21 galaxy systems at 1 < z < 1.5, selected to span a factor >10 in halo mass. The scientific objectives include measuring the role of environment in the evolution of low-mass galaxies, and measuring the dynamics and stellar contents of their host haloes. The targets are selected from the SpARCS, SPT, COSMOS, and SXDS surveys, to be the evolutionary counterparts of today's clusters and groups. The new red-sensitive Hamamatsu detectors on GMOS, coupled with the nod-and-shuffle sky subtraction, allow simultaneous wavelength coverage over λ ∼ 0.6-1.05 µm, and this enables a homogeneous and statistically complete redshift survey of galaxies of all types. The spectroscopic sample targets galaxies with AB magnitudes z < 24.25 and [3.6] µm < 22.5, and is therefore statistically complete for stellar masses M * 10 10.3 M , for all galaxy types and over the entire redshift range. Deep, multiwavelength imaging has been acquired over larger fields for most systems, spanning u through K, in addition to deep IRAC imaging at 3.6 µm. The spectroscopy is ∼50 per cent complete as of semester 17A, and we anticipate a final sample of ∼500 new cluster members. Combined with existing spectroscopy on the brighter galaxies from GCLASS, SPT, and other sources, GOGREEN will be a large legacy cluster and field galaxy sample at this redshift that spectroscopically covers a wide range in stellar mass, halo mass, and clustercentric radius.

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Stellar mass function of cluster galaxies atz~ 1.5: evidence for reduced quenching efficiency at high redshift

Cited by 97 publications

References 92 publications

Galaxy Merger Candidates in High-redshift Cluster Environments

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

Gemini Observations of Galaxies in Rich Early Environments (GOGREEN) I: survey description

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