DISCOVERY AND COSMOLOGICAL IMPLICATIONS OF SPT-CL J2106-5844, THE MOST MASSIVE KNOWN CLUSTER AT z&gt;1

Foley, R. J.; Andersson, Karl; Bazin, G.; Haan, T. de; Ruel, J.; Ade, Peter A. R.; Aird, K. A.; Armstrong, R.; Ashby, M. L. N.; Bautz, Marshall W.; Benson, B. A.; Bleem, L. E.; Bonamente, Massimiliano; Brodwin, M.; Carlstrom, J. E.; Chang, C. L.; Clocchiatti, A.; Crawford, T. M.; Crites, A. T.; Desai, S.; Dobbs, M.; Dudley, J. P.; Fazio, G. G.; Forman, W.; Garmire, G. P.; George, E. M.; Gladders, M. D.; Gonzalez, Anthony H.; Halverson, N. W.; High, F. W.; Holder, G. P.; Holzapfel, W. L.; Hoover, S.; Hrubes, J. D.; Jones, C.; Joy, M.; Keisler, R.; Knox, L.; Lee, A. T.; Leitch, E. M.; Lueker, M.; Luong-Van, D.; Marrone, Daniel P.; McMahon, Jeffrey; Mehl, J.; Meyer, S. S.; Mohr, J. J.; Montroy, T. E.; Murray, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Reichardt, Christian; Rest, A.; Ruhl, J. E.; Saliwanchik, B. R.; Saro, A.; Schaffer, K. K.; Shaw, L.; Shirokoff, E.; Song, J.; Spieler, H.; Stalder, B.; Stanford, S. A.; Staniszewski, Z.; Stark, A. A.; Story, K. T.; Stubbs, C. W.; Vanderlinde, K.; Vieira, J. D.; Vikhlinin, A.; Williamson, A. R.; Zenteno, A.

doi:10.1088/0004-637x/731/2/86

Cited by 115 publications

(134 citation statements)

References 51 publications

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“…Its [0.1−2.4] keV band luminosity of (22.7 ± 0.8) × 10 44 erg s −1 is equal to that of the fifth most luminous object in the MCXC compilation of Piffaretti et al (2011), MACS J0717.5+3745 at z = 0.55, discovered in the RASS by Edge et al (2003). Moreover, its [0.5−2.0] keV band luminosity is consistent with that of SPT-CL J2106−5844, the most luminous cluster known beyond z = 1 (Foley et al 2011). Collectively, these three clusters are the most luminous systems at z > 0.5.…”

Section: An Exceptionally Luminous and Massive Clustersupporting

confidence: 75%

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Planckearly results. XXVI. Detection withPlanckand confirmation byXMM-Newtonof PLCK G266.6–27.3, an exceptionally X-ray luminous and massive galaxy cluster atz ~ 1

Aghanim¹,

Arnaud²,

Ashdown³

et al. 2011

A&A

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We present first results on PLCK G266.6−27.3, a galaxy cluster candidate detected at a signal-to-noise ratio of 5 in the Planck All Sky survey. An XMM-Newton validation observation has allowed us to confirm that the candidate is a bona fide galaxy cluster. With these X-ray data we measure an accurate redshift, z = 0.94 ± 0.02, and estimate the cluster mass to be M 500 = (7.8 ± 0.8) × 10 14 M . PLCK G266.6−27.3 is an exceptional system: its luminosity of L X [0.5−2.0 keV] = (1.4 ± 0.05) × 10 45 erg s −1 equals that of the two most luminous known clusters in the z > 0.5 universe, and it is one of the most massive clusters at z ∼ 1. Moreover, unlike the majority of high-redshift clusters, PLCK G266.6−27.3 appears to be highly relaxed. This observation confirms Planck's capability of detecting high-redshift, high-mass clusters, and opens the way to the systematic study of population evolution in the exponential tail of the mass function.

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Section: An Exceptionally Luminous and Massive Clustersupporting

confidence: 75%

“…They offer an ideal way to identify massive, high-redshift clusters. One recent illustration is the detection of SPT-CL J2106−5844 at z = 1.13 by the South Pole Telescope (SPT) survey (Foley et al 2011). With an estimated mass of M 200 = (1.27 ± 0.21) × 10 15 M , SPT-CL J2106−5844 is nearly twice as massive as XMMU J2235.3−2557.…”

Section: Introductionmentioning

confidence: 99%

Planckearly results. XXVI. Detection withPlanckand confirmation byXMM-Newtonof PLCK G266.6–27.3, an exceptionally X-ray luminous and massive galaxy cluster atz ~ 1

Aghanim¹,

Arnaud²,

Ashdown³

et al. 2011

A&A

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“…A resolved temperature drop at high-redshift has only been observed in 3C 186 at z = 1.1 (Siemiginowska et al 2010), a cluster that harbors a bright quasar in its center. More recently, the analysis of relatively shallow Chandra data of SPT-CL J2106-5844, a galaxy cluster at z = 1.1 discovered with the South Pole Telescope, hints at a temperature drop from 11.0 +2.6 −1.9 keV to 6.5 +1.7 −1.1 keV in the core (Foley et al 2011), with a drop factor of 1.7 ± 0.5. Similarly, the very massive merging cluster ACT-CL J0102-4215 at z = 0.87, shows temperature variations ranging from 22 ± 6 to 6.6 ± 0.7 keV (Menanteau et al 2011), corresponding to a drop factor of ∼2, from the global, core-excluded temperature, to the cluster center.…”

Section: Projected Temperature Profile and Mapmentioning

confidence: 99%

DeepChandraobservation of the galaxy cluster WARPJ1415.1+3612 atz=1

Santos

Tozzi

Rosati

et al. 2012

A&A

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Aims. Using the deepest (370 ks) Chandra observation of a high-redshift galaxy cluster, we perform a detailed characterization of the intra-cluster medium (ICM) of WARPJ1415.1+3612 at z = 1.03, particularly its core region. We also explore the connection between the ICM core properties and the radio/optical properties of the brightest cluster galaxy (BCG). Methods. We perform a spatially resolved analysis of the ICM to obtain temperature, metallicity and surface brightness profiles over the 8-400 kpc radial range. We measure the following cool-core diagnostics: central temperature drop, central metallicity excess, central cooling time, and central entropy. Using the deprojected temperature and density profiles, we accurately derive the cluster hydrostatic mass at different overdensities. In addition to the X-ray data, we use archival radio VLA imaging and optical GMOS spectroscopy of the central galaxy to investigate the feedback between the central galaxy and the ICM. Results. Our spatially resolved spectral analysis shows a significant temperature drop from a maximum of 8.0 keV to a projected core value T c = 4.6 ± 0.4 keV, and a remarkably high central iron abundance peak, Z Fe,c = 3.60 +1.50 −0.85 Z , measured within a radius of 12 kpc. We measure M 500 = M(r < R 500 ) = 2.4 ± 0.4 M and a corresponding gas fraction f gas = 0.10 ± 0.02. The central cooling time is shorter than 0.1 Gyr and the entropy K c is equal to 9.9 keV cm 2 . We detect a strong [OII] emission line in the optical spectra of the BCG with an equivalent width of -25 Å, for which we derive a star formation rate within the range 2-8 M yr −1 . The VLA data reveals a central radio source coincident with the BCG with a luminosity L 1.4 GHz = 2.0 × 10 25 W Hz −1 , and a faint one-sided jet-like feature with an extent of ∼80 kpc. We do not find clear evidence for cavities associated to the radio AGN activity. Conclusions. Our analysis shows that WARPJ1415 has a well developed cool-core with ICM properties similar to those found in the local Universe. Its properties and the clear sign of feedback activity found in the central galaxy in the optical and radio bands, show that feedback processes are already established at z ∼ 1 (a lookback time of 7.8 Gyr). In addition, the presence of a strong metallicity peak shows that the central regions have been promptly enriched by star formation processes in the central galaxy already at z > 1. Our results significantly constrain the timescale for the formation and self-stabilization of cool-cores.

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“…For further details on the framework, assumptions, and details of each method see Appendix B. While the results of this exercise can be used to test the standard ΛCDM concordance model of cosmology, as done in numerous other works investigating high-redshift structures (e.g., Foley et al 2011;Bayliss et al 2013), the goal here is to simply provide a greater context for Cl J0227-0421 with which to compare other high-redshift protostructures and to provide a backdrop for the preliminary investigation of galaxy evolution that follows.…”

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confidence: 99%

VIMOS Ultra-Deep Survey (VUDS): Witnessing the assembly of a massive cluster atz~ 3.3

Lemaux

Cucciati

Tasca

et al. 2014

A&A

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Using new spectroscopic observations obtained as part of the VIMOS Ultra-Deep Survey (VUDS), we performed a systematic search for overdense environments in the early universe (z > 2) and report here on the discovery of Cl J0227-0421, a massive protocluster at z = 3.29. This protocluster is characterized by both the large overdensity of spectroscopically confirmed members, δ gal = 10.5 ± 2.8, and a significant overdensity in photometric redshift members. The halo mass of this protocluster is estimated by a variety of methods to be ∼3 × 10 14 M at z ∼ 3.3, which, evolved to z = 0 results in a halo mass rivaling or exceeding that of the Coma cluster. The properties of 19 spectroscopically confirmed member galaxies are compared with a large sample of VUDS/VVDS galaxies in lower density field environments at similar redshifts. We find tentative evidence for an excess of redder, brighter, and more massive galaxies within the confines of the protocluster relative to the field population, which suggests that we may be observing the beginning of environmentally induced quenching. The properties of these galaxies are investigated, including a discussion of the brightest protocluster galaxy, which appears to be undergoing vigorous coeval nuclear and starburst activity. The remaining member galaxies appear to have characteristics that are largely similar to the field population. Though we find weaker evidence of the suppression of the median star formation rates among and differences in the stacked spectra of member galaxies with respect to the field, we defer any conclusions about these trends to future work with the ensemble of protostructures that are found in the full VUDS sample.

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DISCOVERY AND COSMOLOGICAL IMPLICATIONS OF SPT-CL J2106-5844, THE MOST MASSIVE KNOWN CLUSTER AT z>1

Cited by 115 publications

References 51 publications

Planckearly results. XXVI. Detection withPlanckand confirmation byXMM-Newtonof PLCK G266.6–27.3, an exceptionally X-ray luminous and massive galaxy cluster atz ~ 1

Planckearly results. XXVI. Detection withPlanckand confirmation byXMM-Newtonof PLCK G266.6–27.3, an exceptionally X-ray luminous and massive galaxy cluster atz ~ 1

DeepChandraobservation of the galaxy cluster WARPJ1415.1+3612 atz=1

VIMOS Ultra-Deep Survey (VUDS): Witnessing the assembly of a massive cluster atz~ 3.3

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