Discovery of a massive X-ray luminous galaxy cluster at<i>z</i> = 1.579

Santos, J. S.; Fassbender, R.; Nastasi, A.; Böhringer, H.; Rosati, P.; Šuhada, R.; Pierini, D.; Nonino, M.; Muehlegger, Martin; Quintana, H.; Schwope, A. D.; Lamer, G.; Hoon, A. de; Strazzullo, V.

doi:10.1051/0004-6361/201117190

Cited by 84 publications

(108 citation statements)

References 31 publications

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“…An additional multi-band analysis has revealed that the star formation activity in this cluster increases with the environment density, with star forming galaxies being mainly located at the center of the system (Tran et al 2010). A similar trend has been observed in three other X-ray selected galaxy clusters, two newly confirmed at z = 1.56 ) and z = 1.58 (Santos et al 2011) and one at z = 1.46 (Hilton et al , 2010. However, the galaxy red-sequence of these systems has not yet been fully established yet, indicating that the members are still building their stellar mass via star formation activity.…”

Section: Introductionsupporting

confidence: 76%

Discovery of the X-ray selected galaxy cluster XMMU J0338.8+0021 atz= 1.49

Nastasi¹,

Fassbender²,

Böhringer³

et al. 2011

A&A

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We report the discovery of a galaxy cluster at z = 1.490 originally selected as an extended X-ray source in the XMM-Newton Distant Cluster Project. Further observations carried out with the VLT-FORS2 spectrograph allowed the spectroscopic confirmation of seven secure cluster members, providing a median system redshift of z = 1.490 ± 0.009. The color-magnitude diagram of XMMU J0338.8+0021 reveals the presence of a well-populated red sequence with z − H ≈ 3, albeit with an apparent significant scatter in color. Since we do not detect indications of any strong star formation activity in these objects, the color spread could represent the different stellar ages of the member galaxies. In addition, we found the brightest cluster galaxy in a very active dynamical state, with an interacting, merging companion located at a physical projected distance of d ≈ 20 kpc. From the X-ray luminosity, we estimate a cluster mass of M 200 ∼ 1.2 × 10 14 M . The data appear to be consistent with a scenario in which XMMU J0338.8+0021 is a young system, possibly caught in a moment of active ongoing mass assembly.

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Section: Introductionsupporting

confidence: 76%

Discovery of the X-ray selected galaxy cluster XMMU J0338.8+0021 atz= 1.49

Nastasi¹,

Fassbender²,

Böhringer³

et al. 2011

A&A

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“…More generally, we note that the X-ray emission of all four z > 1.5 known clusters appears to be significantly affected by point sources (there is no Chandra image published yet for Santos et al 2011;Fassbender et al 2011, but the XMM images look very compact). Furthermore, clusters like IRC-0218A will certainly always escape direct X-ray detection in the XMM or Chandra archive for techniques solely based on the search for extended X-ray emission.…”

Section: Discussionmentioning

confidence: 75%

“…Two of them have been primarily detected in the X-ray waveband Santos et al 2011). The other two were identified through an overdensity of red galaxies; weak X-ray emission was found a posteriori to be associated with both of them (Papovich et al 2010;Gobat et al 2011).…”

Section: Introductionmentioning

confidence: 97%

AChandraview of thez = 1.62 galaxy cluster IRC-0218A

Pierre

Clerc

Maughan

et al. 2012

A&A

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Context. Very few z > 1.5 clusters of galaxies are currently known. It is important to study the properties of galaxies in these clusters and the intra-cluster medium and, furthermore, to cross-check the reliability of the various mass estimates. This will help to clarify the process of structure formation and how distant clusters may be used to constrain cosmology. Aims. We present a 84 ks Chandra observation of IRC-0218A, a cluster of galaxies inferred by the presence of a galaxy overdensity in the infrared at a redshift of 1.62 and associated with some XMM emission. Methods. We performed a spatial analysis of the Chandra X-ray photon distribution. Results. The Chandra observation of IRC-0218A appears to be entirely dominated by a point source located at the centroid of the mid-infrared galaxy density. In addition, we detected weak extended emission (2.3σ) out to a radius of 25 with a flux of ∼3 × 10 −15 erg s −1 cm −2 in the [0.3-2] keV band. Assuming that clusters evolve similarly, we infer a virial mass of M 200 = 7.7(±3.8) × 10 13 M . This is marginally compatible with our current estimate of the cluster dynamical mass (based on 10 redshifts), although there is no evidence that the galaxy peculiar velocities correspond to the motions of a virialized structure. The stellar mass enclosed in the inferred X-ray virial radius is estimated to be 1-2 × 10 12 M . We provide a detailed account of 28 X-ray point sources detected in the field.

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“…Also, they will provide a key to understanding the origin of the environmental dependence of galaxy properties observed at low redshifts (e.g., Lewis et al 2002;Gómez et al 2003;Tanaka et al 2004). Dedicated effort has identified a number of high-redshift groups and clusters of galaxies at z 1.5 (e.g., Kurk et al 2009;Tanaka et al 2010aTanaka et al , 2013Fassbender et al 2011;Gobat et al 2011;Nastasi et al 2011;Santos et al 2011;Spitler et al 2012;Stanford et al 2012;Muzzin et al 2013). Among them, a z = 1.61 group, which is likely a progenitor of a present-day massive cluster, is carefully studied by Tanaka et al (2013) and they showed that the group already exhibits a prominent red sequence of quiescent early-type galaxies formed at z f = 3 (single stellar population equivalent).…”

Section: Introductionmentioning

confidence: 99%

ON THE FORMATION TIMESCALE OF MASSIVE CLUSTER ELLIPTICALS BASED ON DEEP NEAR-INFRARED SPECTROSCOPY ATz∼ 2

Tanaka

Toft

Marchesini

et al. 2013

ApJ

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We present improved constraints on the formation timescale of massive cluster galaxies based on rest-frame optical spectra of galaxies in a forming cluster located at z = 2.16. The spectra are obtained with MOIRCS on the Subaru Telescope with an integration time of ∼7 hr. We achieve accurate redshift measurements by fitting spectral energy distributions using the spectra and broadband photometry simultaneously, allowing us to identify probable cluster members. Clusters at low redshifts are dominated by quiescent galaxies, but we find that quiescent galaxies and star-forming galaxies coexist in this z = 2 system. Interestingly, the quiescent galaxies form a weak red sequence in the process of forming. By stacking the spectra of star-forming galaxies, we observe strong emission lines such as [O ii] and [O iii] and we obtain a tentative hint of active galactic nucleus activities in these galaxies. On the other hand, the stacked spectrum of the quiescent galaxies reveals a clear 4000 Å break with a possible Ca ii H+K absorption feature and strong emission lines such as [O ii] are absent in the spectrum, confirming the quiescent nature of these galaxies. We then perform detailed spectral analyses of the stacked spectrum, which suggest that these massive quiescent galaxies formed at redshifts between 3 and 4 on a timescale of 0.5 Gyr. This short formation timescale is not reproduced in recent numerical simulations. We discuss possible mechanisms for how these galaxies form 10 11 M stellar mass on a short timescale and become red and quiescent by z = 2.

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Discovery of a massive X-ray luminous galaxy cluster atz = 1.579

Cited by 84 publications

References 31 publications

Discovery of the X-ray selected galaxy cluster XMMU J0338.8+0021 atz= 1.49

Discovery of the X-ray selected galaxy cluster XMMU J0338.8+0021 atz= 1.49

AChandraview of thez = 1.62 galaxy cluster IRC-0218A

ON THE FORMATION TIMESCALE OF MASSIVE CLUSTER ELLIPTICALS BASED ON DEEP NEAR-INFRARED SPECTROSCOPY ATz∼ 2

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