Multiwavelength observations of a rich galaxy cluster at <i>z</i> $\thicksim$ 1

Santos, J. S.; Rosati, P.; Gobat, R.; Lidman, C.; Dawson, Kyle; Perlmutter, S.; Böehringer, H.; Balestra, I.; Mullis, C. R.; Fassbender, R.; Kohnert, J.; Lamer, G.; Rettura, Alessandro; Rité, C.; Schwope, A. D.

doi:10.1051/0004-6361/200811546

Cited by 34 publications

(58 citation statements)

References 63 publications

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“…2, we note that the red sequence of X0338 appears well populated. The eleven red galaxies, with colors 2.6 ≤ z − H ≤ 3.5 and brighter than the completeness limit, have a median (average) color of z − H = 2.9 mag (3.0 mag), which is consistent with the model prediction of z− H 3.0 mag for a stellar formation redshift of z f = 3, which represents an evolved red-sequence population, as seen in other distant clusters (XMMUJ1229, Santos et al 2009;XMMUJ2235, Strazzullo et al 2010. From the observed color spread of δ obs z−H ≈ 0.25 mag, with an assumed flat slope and a Monte Carlo estimated contribution of the photometric errors of (0.16 ± 0.04) mag, we obtain a first order estimate of the intrinsic red-sequence scatter of δ int z−H ∼ (0.19 ± 0.04) mag.…”

Section: A Young Cluster In Formation?supporting

confidence: 80%

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: A Young Cluster In Formation?supporting

confidence: 80%

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 supplement this with four high redshift clusters (XMM1229 - Santos et al 2009, RDCS1252 -Rosati et al 2004, ISCS1434 -Eisenhardt et al 2008and XMM2235 -Rosati et al 2009) with suitable archival data at 0.98 < z < 1.40 as already discussed in Paper I. See Table 1 for basic information.…”

Section: Datasetmentioning

confidence: 99%

Morphological evolution of cluster red sequence galaxies in the past 9 Gyr

Propris¹,

Bremer²,

Phillipps³

2016

Mon. Not. R. Astron. Soc.

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Galaxies arrive on the red sequences of clusters at high redshift (z > 1) once their star formation is quenched and evolve passively thereafter. However, we have previously found that cluster red sequence galaxies (CRSGs) undergo significant morphological evolution subsequent to the cessation of star formation, at some point in the past 9-10 Gyr. Through a detailed study of a large sample of cluster red sequence galaxies spanning 0.2 < z < 1.4 we elucidate the details of this evolution. Below z ∼ 0.5 − 0.6 (in the last 5-6 Gyr) there is little or no morphological evolution in the population as a whole, unlike in the previous 4-5 Gyrs. Over this earlier time (i) disklike systems with Sérsic n < 2 progressively disappear, as (ii) the range of their axial ratios similarly decreases, removing the most elongated systems (those consistent with thin disks seen at an appreciable inclination angle), and (iii) radial colour gradients (bluer outwards) decrease in an absolute sense from significant age-related gradients to a residual level consistent with the metallicity-induced gradients seen in low redshift cluster members. The distribution of their effective radii shows some evidence of evolution, consistent with growth of at most a factor < 1.5 between z ∼ 1.4 and z ∼ 0.5, significantly less than for comparable field galaxies, while the distribution of their central (< 1kpc) bulge surface densities shows no evolution at least at z < 1. A simple model involving the fading and thickening of a disk component after comparatively recent quenching (after z ∼ 1.5) around an otherwise passively evolving older spheroid component is consistent with all of these findings.

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“…This generally allows stronger constraints to be obtained, by mitigating inherent degeneracies among stellar population parameters. The same technique was used in Santos et al (2009) to age date earlytype galaxies in a cluster at z 1. ACS imaging shows that all the galaxies have early-type morphologies, however we defer the morphological analysis to another paper (Strazzullo et al in prep.…”

Section: Star-formation Histories Of Passive Membersmentioning

confidence: 99%

Multi-wavelength study of XMMU J2235.3-2557: the most massive galaxy cluster at z > 1

Rosati¹,

Tozzi

Gobat

et al. 2009

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Context. The galaxy cluster XMMU J2235.3−2557 (hereafter XMM2235), spectroscopically confirmed at z = 1.39, is one of the most distant X-ray selected galaxy clusters. It has been at the center of a multi-wavelength observing campaign with ground and space facilities. Aims. We characterize the galaxy populations of passive members, the thermodynamical properties and metal abundance of the hot gas, and the total mass of the system using imaging data with HST/ACS (i 775 and z 850 bands) and VLT/ISAAC (J and K S bands), extensive spectroscopic data obtained with VLT/FORS2, and deep (196 ks) Chandra observations. Methods. Chandra data allow temperature and metallicity to be measured with good accuracy and the X-ray surface brightness profile to be traced out to 1 (or 500 kpc), thus allowing the mass to be reliably estimated. Out of a total sample of 34 spectroscopically confirmed cluster members, we selected 16 passive galaxies (without detectable [OII]) within the central 2 (or 1 Mpc) with ACS coverage, and inferred star formation histories for subsamples of galaxies inside and outside the core by modeling their spectrophotometric data with spectral synthesis models. Results. Chandra data show a regular elongated morphology, closely resembling the distribution of core galaxies, with a significant cool core. We measure a global X-ray temperature of kT = 8.6 +1.3 −1.2 keV (68% confidence), which we find to be robust against several systematics involved in the X-ray spectral analysis. By detecting the rest frame 6.7 keV Iron K line in the Chandra spectrum, we measure a metallicity Z = 0.26 +0.20 −0.16 Z . In the likely hypothesis of hydrostatic equilibrium, we obtain a total mass of M tot (< 1 Mpc) = (5.9 ± 1.3) × 10 14 M . By modeling both the composite spectral energy distributions and spectra of the passive galaxies in and outside the core, we find a strong mean age radial gradient. Core galaxies, with stellar masses in excess of 10 11 M , appear to have formed at an earlier epoch with a relatively short star formation phase (z = 5−6), whereas passive galaxies outside the core show spectral signatures suggesting a prolonged star formation phase to redshifts as low as z ≈ 2. Conclusions. Overall, our analysis implies that XMM2235 is the hottest and most massive bona-fide cluster discovered to date at z > 1, with a baryonic content, both its galaxy population and intracluster gas, in a significantly advanced evolutionary stage at 1/3 of the current age of the Universe.

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Multiwavelength observations of a rich galaxy cluster at z $\thicksim$ 1

Cited by 34 publications

References 63 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

Morphological evolution of cluster red sequence galaxies in the past 9 Gyr

Multi-wavelength study of XMMU J2235.3-2557: the most massive galaxy cluster at z > 1

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