A large-scale galaxy structure at<i>z</i> = 2.02 associated with the radio galaxy MRC 0156-252

Galametz, A.; Stern, Daniel; Pentericci, L.; Breuck, C. De; Vernet, J.; Wylezalek, Dominika; Fassbender, R.; Hatch, N. A.; Kurk, J.; Overzier, Roderik; Rettura, Alessandro; Seymour, N.

doi:10.1051/0004-6361/201322345

Cited by 41 publications

(41 citation statements)

References 67 publications

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“…These environments are highly likely to be proto-clusters or clusters, several of which have already been confirmed (Venemans et al 2007;Galametz et al 2010;Hatch et al 2011b;Galametz et al 2013). However, Fig.…”

Section: Heating the Intracluster Mediummentioning

confidence: 64%

“…Distant clusters and proto-clusters are reliably found near powerful radio-loud AGN (Venemans et al 2007;Galametz et al 2010Galametz et al , 2013Hatch et al 2011a,b;Wylezalek et al 2013) so it is possible that every cluster progenitor experienced a powerful feedback episode during 1.3 < z < 3.2. We estimate that each powerful radio-loud galaxy is active for at least 60 Myr, and if the jets contain protons, then this feedback could provide enough energy per gas particle to pre-heat the forming ICM.…”

Section: Discussionmentioning

confidence: 99%

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Why z > 1 radio-loud galaxies are commonly located in protoclusters

Hatch¹,

Wylezalek²,

Kurk³

et al. 2014

Monthly Notices of the Royal Astronomical Society

102

120

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Distant powerful radio-loud active galactic nuclei (RLAGN) tend to reside in dense environments and are commonly found in proto-clusters at z > 1.3. We examine whether this occurs because RLAGN are hosted by massive galaxies which preferentially reside in rich environments. We compare the environments of powerful RLAGN at 1.3 < z < 3.2 from the CARLA survey to a sample of radio-quiet galaxies matched in mass and redshift. We find the environments of RLAGN are significantly denser than those of radio-quiet galaxies, implying that not more than 50% of massive galaxies in this epoch can host powerful radio-loud jets. This is not an observational selection effect as we find no evidence to suggest it is easier to observe the radio emission when the galaxy resides in a dense environment. We therefore suggest that the dense Mpc-scale environment fosters the formation of a radio-jet from an AGN. We show that the number density of potential RLAGN host galaxies is consistent with every > 10 14 M ⊙ cluster having experienced powerful radio-loud feedback of duration ∼60 Myr during 1.3 < z < 3.2. This feedback could heat the intracluster medium to the extent of 0.5-1 keV per gas particle, which could limit the amount of gas available for further star formation in the proto-cluster galaxies.

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Section: Heating the Intracluster Mediummentioning

confidence: 64%

Section: Discussionmentioning

confidence: 99%

Why z > 1 radio-loud galaxies are commonly located in protoclusters

Hatch¹,

Wylezalek²,

Kurk³

et al. 2014

Monthly Notices of the Royal Astronomical Society

102

120

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“…Indeed the sensitivity required to detect L å galaxies at z∼0.7 with mid-infrared observations, which Spitzer reaches in <2 minute integrations, is sufficient to detect such galaxies to z2. 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

Self Cite

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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“…In recent years the study of galaxy clusters has meaningfully entered the z>1 regime, with several surveys identifying large samples via X-ray (Fassbender et al 2011;Mehrtens et al 2012), Sunyaev-Zel'dovich (SZ, Hasselfield et al 2013;Bleem et al 2015;Planck Collaboration et al 2015), infrared (IR, Eisenhardt 2008;Muzzin et al 2009;Papovich et al 2010;Rettura et al 2014), and radio (Wylezalek et al 2013;Galametz et al 2013;Blanton et al 2014;R. Paterno-Mahler et al 2015, in preparation) selections.…”

Section: Introductionmentioning

confidence: 99%

IDCS J1426.5+3508: THE MOST MASSIVE GALAXY CLUSTER AT z > 1.5

Brodwin

McDonald

Gonzalez

et al. 2016

ApJ

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We present a deep (100 ks) Chandra observation of IDCSJ1426.5+3508, a spectroscopically confirmed, infraredselected galaxy cluster at z=1.75. This cluster is the most massive galaxy cluster currently known at z>1.5, based on existing Sunyaev-Zel'dovich (SZ) and gravitational lensing detections. We confirm this high mass via a variety of X-ray scaling relations, including T X -M, f g -M, Y X -M, and L X -M, finding a tight distribution of masses from these different methods, spanning M 500 =2.3-3.3×1014 M e , with the low-scatter Y X -based mass M Y 500, X =2.6 10 0.5 1.5 14 -+ M e . IDCSJ1426.5+3508 is currently the only cluster at z>1.5 for which X-ray, SZ, and gravitational lensing mass estimates exist, and these are in remarkably good agreement. We find a relatively tight distribution of the gas-to-total mass ratio, employing total masses from all of the aforementioned indicators, with values ranging from f gas,500 =0.087-0.12. We do not detect metals in the intracluster medium (ICM) of this system, placing a 2σ upper limit of Z r R Z 0.18 500 ( ) < <  . This upper limit on the metallicity suggests that this system may still be in the process of enriching its ICM. The cluster has a dense, low-entropy core, offset by ∼30 kpc from the X-ray centroid, which makes it one of the few "cool core" clusters discovered at z>1, and the first known cool core cluster at z>1.2. The offset of this core from the large-scale centroid suggests that this cluster has had a relatively recent (500 Myr) merger/interaction with another massive system.

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A large-scale galaxy structure atz = 2.02 associated with the radio galaxy MRC 0156-252

Cited by 41 publications

References 67 publications

Why z > 1 radio-loud galaxies are commonly located in protoclusters

Why z > 1 radio-loud galaxies are commonly located in protoclusters

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

IDCS J1426.5+3508: THE MOST MASSIVE GALAXY CLUSTER AT z > 1.5

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