The X-ray luminous galaxy cluster XMMU J1007.4+1237 at<i>z</i>= 1.56

Fassbender, R.; Nastasi, A.; Böhringer, H.; Šuhada, R.; Santos, J. S.; Rosati, P.; Pierini, D.; Mühlegger, M.; Quintana, H.; Schwope, A. D.; Lamer, G.; Hoon, A. de; Kohnert, J.; Pratt, G. W.; Mohr, J. J.

doi:10.1051/0004-6361/201016169

Cited by 89 publications

(101 citation statements)

References 38 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…15 as well as the two spectroscopic members classified as elliptical galaxies (ID = 2 and ID = 15) at cluster-centric distances of 28 and 2.1 , respectively. Interestingly, there is evidence of sustained star-formation activity at the bright end of the galaxy luminosity function in the X-ray luminous cluster XMMU J1007.4+1237 at z = 1.555 (Fassbender et al 2011b) and in dense environments at z ∼ 1 (e.g., Elbaz et al 2007;Gerke et al 2007;Cooper et al 2008). Several [O II] line emitters are found in the luminous, red galaxy population of XMMU J0302.2−0001 at z = 1.185 with a total mass of a few times 10 14 M (Suhada et al 2011).…”

Section: Discussionmentioning

confidence: 99%

“…We opted to do this because there is independent evidence that the bright end of the galaxy luminosity function of a high-z cluster can be populated by [O II] line emitters (as for XMMU J0302.2−0001 at z = 1.186, Suhada et al 2011), sometimes with vigorous starburst activity (as for XMMU J1007.4+1237 at z = 1.555, Fassbender et al 2011b).…”

Section: Photometric-redshiftsmentioning

confidence: 99%

“…This strategy has already yielded more than 30 spectroscopically confirmed distant clusters since the discovery of XMMU J2235.3−2557 at z = 1.393 . They include XMMU J0338.8+0021 at z = 1.49 , XMMU J1007.4+1237 at z = 1.555 (Fassbender et al 2011b) and XMMU J0044.0−2033 at z = 1.579 (Santos et al 2011).…”

Section: Introductionmentioning

confidence: 99%

“…Among the main results from XDCP we quote the multiwavelength studies of XMMU J1229+0151 at z = 0.975 (Santos et al 2009) and XMMU J2235.3−2557 Strazzullo et al 2010); the weak-lensing estimate of the total mass of XMMU J2235.3−2557 (Jee et al 2009); the total mass estimate of XMMU J100750.5+125818 (z = 1.082) from strong lensing, optical spectroscopy and X-ray imaging (Schwope et al 2010); the pan-chromatic study of XMMU J1230.3+1339 at z = 0.975 (Fassbender et al 2011a) and its total mass estimate from weak-lensing analysis of ground-based imaging (Lerchster et al 2010); the evidence of starburst activity in the core of XMMU J1007.4+1237 (Fassbender et al 2011b).…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

First simultaneous optical/near-infrared imaging of an X-ray selected, high-redshift cluster of galaxies with GROND

Pierini

Šuhada

Fassbender

et al. 2012

A&A

Self Cite

View full text Add to dashboard Cite

Context. The XMM-Newton Distant Cluster Project is a serendipitous survey for clusters of galaxies at redshifts z ≥ 0.8 based on deep archival XMM-Newton observations. X-ray sources identified as extended are screened against existing optical all-sky surveys for galaxies, in case of candidate high-z clusters followed up with imaging at 4 m-class telescopes and, ultimately, multi-object spectroscopy at 8 m-class telescopes. Low-significance candidate high-z clusters are followed up with the seven-channel imager GROND (Gamma-Ray Burst Optical and Near-Infrared Detector) that is mounted at a 2 m-class telescope. Its unique capability of simultaneous imaging in the g , r , i , z , J, H, Ks bands enables the use of the photometric redshift technique. Aims. Observing strategy, data reduction and analysis, depth and accuracy of the simultaneous multi-wavelength photometry are discussed with the goal of establishing GROND as a useful instrument to confirm X-ray selected (high-z) clusters. Methods. The test case is XMMU J0338.7+0030, suggested to be at z ∼ 1.45 ± 0.15 (1σ) from the analysis of the z − H vs. H colour−magnitude diagram obtained from the follow-up imaging. Later VLT-FORS2 spectroscopy enabled us to identify four members, which set this cluster at z = 1.097 ± 0.002 (1σ). To reach a better knowledge of its galaxy population, we observed XMMU J0338.7+0030 with GROND for about 6 h. The publicly available photo-z code le Phare was used. Results. The Ks-band number counts of the non-stellar sources out of the 832 detected down to z ∼ 26 AB mag (1σ) in the 3.9×4.3 arcmin 2 region of XMMU J0338.7+0030 imaged at all GROND bands clearly exceed those computed in deep fields/survey areas at ∼20.5-22.5 AB mag. The photo-z's of the three imaged spectroscopic members yield z = 1.12 ± 0.09 (1σ). The spatial distribution and the properties of the GROND sources with a photo-z in the range 1.01-1.23 confirm the correspondence of the X-ray source with a galaxy over-density at a significance of at least 4.3σ. Candidate members that are spectro-photometrically classified as elliptical galaxies define a red locus in the i −z vs. z colour−magnitude diagram that is consistent with the red sequence of the cluster RDCS J0910+5422 at z = 1.106. XMMU J0338.7+0030 hosts also a population of bluer late-type spirals and irregulars. The starbursts among the photometric members populate both loci, consistently with previous results. Conclusions. The analysis of the available data set indicates that XMMU J0338.7+0030 is a low-mass cluster (M 200 ∼ 10 14 M ) at z = 1.1. With the photometric accuracy yielded by the present unoptimized multi-band observations with GROND, we not only confirm the spectroscopic redshift of this cluster but also show that it hosts a galaxy population that can still undergo significant bursts of star-formation activity.

show abstract

Section: Discussionmentioning

confidence: 99%

Section: Photometric-redshiftsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

First simultaneous optical/near-infrared imaging of an X-ray selected, high-redshift cluster of galaxies with GROND

Pierini

Šuhada

Fassbender

et al. 2012

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…Several recent studies have claimed to find evidence of significant star formation even in central cluster regions at z 1.5 (e.g., Hilton et al 2010;Tran et al 2010;Hayashi et al 2010;Santos et al 2011;Fassbender et al 2011;Brodwin et al 2013), suggesting that we indeed are approaching the formation epoch of massive cluster galaxies. However, it is also noticeable that massive passive galaxies are often found, even in such most distant clusters, although in many cases sharing their environment with galaxies in a still active formation phase (e.g., Kurk et al 2009;Papovich et al 2010;Gobat et al 2011Gobat et al , 2013Tanaka et al 2013;Spitler et al 2012;Strazzullo et al 2013;Newman et al 2014;Andreon et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Passive galaxies as tracers of cluster environments atz~ 2

Strazzullo

Daddi

Gobat

et al. 2015

A&A

View full text Add to dashboard Cite

Even 10 billion years ago, the cores of the first galaxy clusters are often found to host a characteristic population of massive galaxies with already suppressed star formation. Here we search for distant cluster candidates at z ∼ 2 using massive passive galaxies as tracers. With a sample of ∼40 spectroscopically confirmed passive galaxies at 1.3 < z < 2.1, we tuned photometric redshifts of several thousand passive sources in the 2 sq. deg COSMOS field. This allowed us to map their density in redshift slices, probing the largescale structure in the COSMOS field as traced by passive sources. We report here on the three strongest passive galaxy overdensities that we identify in the range 1.5 < z < 2.5. While the actual nature of these concentrations still needs to be confirmed, we discuss their identification procedure and the arguments supporting them as candidate galaxy clusters (probably in the mid-10 13 M range). Although this search approach is probably biased toward more evolved structures, it has the potential of selecting still rare, clusterlike environments close to their epoch of first appearance, enabling new investigations of the evolution of galaxies in the context of structure growth.

show abstract

Detection and characterisation of the first Planck high‐z candidates

Flores-Cacho

2013

Astron Nachr

View full text Add to dashboard Cite

With its unprecedented ability to scrutinise the sub-millimetre (sub-mm) to centimetre full sky, the Planck satellite is uniquely suited to search for the progenitors of clusters of galaxies. The forming massive halos at z 1-2 are expected to host massive galaxies with high star formation rates. Clustered in the growing potential well that is being established, these galaxies are within Planck's reach via their sub-mm emission. We have applied a new colour-based method combining Planck and IRAS data to detect the rarest and brightest sub-mm cold sources on the sky. In this work, we describe the method and present the first confirmations of our high-z candidates, particularly focusing on 17p732, a newly discovered high-z (proto)cluster candidate at z 1.7 for which we carried a multi-wavelength follow-up.

show abstract

The X-ray luminous galaxy cluster XMMU J1007.4+1237 atz= 1.56

Cited by 89 publications

References 38 publications

First simultaneous optical/near-infrared imaging of an X-ray selected, high-redshift cluster of galaxies with GROND

First simultaneous optical/near-infrared imaging of an X-ray selected, high-redshift cluster of galaxies with GROND

Passive galaxies as tracers of cluster environments atz~ 2

Detection and characterisation of the first Planck high‐z candidates

Contact Info

Product

Resources

About