scholarly journals First Weak-lensing Results from “See Change”: Quantifying Dark Matter in the Twoz≳ 1.5 High-redshift Galaxy Clusters SPT-CL J2040–4451 and IDCS J1426+3508

2017 ◽  
Vol 847 (2) ◽  
pp. 117 ◽  
Author(s):  
M. James Jee ◽  
Jongwan Ko ◽  
Saul Perlmutter ◽  
Anthony Gonzalez ◽  
Mark Brodwin ◽  
...  
Keyword(s):  
Dark Matter ◽  
Galaxy Clusters ◽  
High Redshift ◽  
Weak Lensing ◽  
Redshift Galaxy

scholarly journals Precise weak lensing constraints from deep high-resolution Ks images: VLT/HAWK-I analysis of the super-massive galaxy cluster RCS2 J 232727.7−020437 at z = 0.70

2018 ◽  
Vol 610 ◽  
pp. A85 ◽  
Author(s):  
Tim Schrabback ◽  
Mischa Schirmer ◽  
Remco F. J. van der Burg ◽  
Henk Hoekstra ◽  
Axel Buddendiek ◽  
...  
Keyword(s):  
Galaxy Clusters ◽  
High Redshift ◽  
Galaxy Cluster ◽  
Weak Lensing ◽  
Data Sets ◽  
Redshift Distribution ◽  
Model And Simulation ◽  
Single Orbit ◽  
Redshift Galaxy ◽  
Massive Galaxy

We demonstrate that deep good-seeing VLT/HAWK-I Ks images complemented with g + z-band photometry can yield a sensitivity for weak lensing studies of massive galaxy clusters at redshifts 0.7 ≲ z ≲ 1.1, which is almost identical to the sensitivity of HST/ACS mosaics of single-orbit depth. Key reasons for this good performance are the excellent image quality frequently achievable for Ks imaging from the ground, a highly effective photometric selection of background galaxies, and a galaxy ellipticity dispersion that is noticeably lower than for optically observed high-redshift galaxy samples. Incorporating results from the 3D-HST and UltraVISTA surveys we also obtained a more accurate calibration of the source redshift distribution than previously achieved for similar optical weak lensing data sets. Here we studied the extremely massive galaxy cluster RCS2 J232727.7−020437 (z = 0.699), combining deep VLT/HAWK-I Ks images (point spread function with a 0.′′35 full width at half maximum) with LBT/LBC photometry. The resulting weak lensing mass reconstruction suggests that the cluster consists of a single overdensity, which is detected with a peak significance of 10.1σ. We constrained the cluster mass to M200c/(1015 M⊙) = 2.06−0.26+0.28(stat.) ± 0.12(sys.) assuming a spherical Navarro, Frenk & White model and simulation-based priors on the concentration, making it one of the most massive galaxy clusters known in the z ≳ 0.7 Universe. We also cross-checked the HAWK-I measurements through an analysis of overlapping HST/ACS images, yielding fully consistent estimates of the lensing signal.

scholarly journals Scaling Relations from Sunyaev‐Zel’dovich Effect andChandraX‐Ray Measurements of High‐Redshift Galaxy Clusters

2008 ◽  
Vol 675 (1) ◽  
pp. 106-114 ◽  
Author(s):  
Massimiliano Bonamente ◽  
Marshall Joy ◽  
Samuel J. LaRoque ◽  
John E. Carlstrom ◽  
Daisuke Nagai ◽  
...  
Keyword(s):  
Galaxy Clusters ◽  
High Redshift ◽  
Scaling Relations ◽  
Redshift Galaxy ◽  
Sunyaev Zel'dovich Effect

scholarly journals Implications of multiple high-redshift galaxy clusters

2011 ◽  
Vol 83 (10) ◽  
Author(s):  
Ben Hoyle ◽  
Raul Jimenez ◽  
Licia Verde
Keyword(s):  
Galaxy Clusters ◽  
High Redshift ◽  
Redshift Galaxy

scholarly journals What are protoclusters? – Defining high-redshift galaxy clusters and protoclusters

2015 ◽  
Vol 452 (3) ◽  
pp. 2528-2539 ◽  
Author(s):  
Stuart I. Muldrew ◽  
Nina A. Hatch ◽  
Elizabeth A. Cooke
Keyword(s):  
Galaxy Clusters ◽  
High Redshift ◽  
Redshift Galaxy

scholarly journals On the Gas Surrounding High-Redshift Galaxy Clusters

2001 ◽  
Vol 18 (1) ◽  
pp. 64-75 ◽  
Author(s):  
Paul J. Francis ◽  
Greg M. Wilson ◽  
Bruce E. Woodgate
Keyword(s):  
Galaxy Clusters ◽  
Hydrogen Absorption ◽  
High Redshift ◽  
Neutral Hydrogen ◽  
Neutral Gas ◽  
Cluster Of Galaxies ◽  
Galaxy Halos ◽  
Redshift Galaxy ◽  
High Redshift Universe

AbstractFrancis & Hewett (1993) identified two 10 Mpc-scale regions of the high-redshift universe that were seemingly very overdense in neutral hydrogen. Subsequent observations showed that at least one of these gas-rich regions enveloped a cluster of galaxies at redshift 2 ·38. We present improved observations of the three background QSOs with sightlines passing within a few Mpc of this cluster of galaxies. All three QSOs show strong neutral hydrogen absorption at the cluster redshift, suggesting that this cluster (and perhaps all high-redshift clusters) may be surrounded by a ~5 Mpc-scale region containing ~10 12 Mʘ of neutral gas. We show that if most high-redshift clusters are surrounded by such regions, the gas must be in the form of many small (<1 kpc), dense (> 0·03 cm ˗3 ) clouds, each of mass <10 6 Mʘ . These clouds are themselves probably gathered into >20 kpc-sized clumps, which may be galaxy halos or protogalaxies. If this gas exists, it will be partially photoionised by the UV background. We predict the diffuse Lyα flux from this photoionisation, and place observational limits on its intensity.

scholarly journals The WARPS survey - IV. The X-ray luminosity-temperature relation of high-redshift galaxy clusters

2000 ◽  
Vol 315 (4) ◽  
pp. 669-678 ◽  
Author(s):  
B. W. Fairley ◽  
L. R. Jones ◽  
C. Scharf ◽  
H. Ebeling ◽  
E. Perlman ◽  
...  
Keyword(s):  
Galaxy Clusters ◽  
High Redshift ◽  
Temperature Relation ◽  
X Ray ◽  
Redshift Galaxy

scholarly journals The history of metal enrichment traced by X-ray observations of high redshift galaxy clusters

2021 ◽  
Author(s):  
Anthony M Flores ◽  
Adam B Mantz ◽  
Steven W Allen ◽  
R Glenn Morris ◽  
Rebecca E A Canning ◽  
...  
Keyword(s):  
Galaxy Clusters ◽  
High Redshift ◽  
Substantial Improvement ◽  
Metal Enrichment ◽  
X Ray ◽  
Redshift Galaxy ◽  
History Of ◽  
Mass Profile ◽  
Massive Clusters ◽  
Massive Galaxy

Abstract We present the analysis of deep X-ray observations of 10 massive galaxy clusters at redshifts 1.05 &lt; z &lt; 1.71, with the primary goal of measuring the metallicity of the intracluster medium (ICM) at intermediate radii, to better constrain models of the metal enrichment of the intergalactic medium. The targets were selected from X-ray and Sunyaev-Zel’dovich (SZ) effect surveys, and observed with both the XMM-Newton and Chandra satellites. For each cluster, a precise gas mass profile was extracted, from which the value of r500 could be estimated. This allows us to define consistent radial ranges over which the metallicity measurements can be compared. In general, the data are of sufficient quality to extract meaningful metallicity measurements in two radial bins, r &lt; 0.3r500 and 0.3 &lt; r/r500 &lt; 1.0. For the outer bin, the combined measurement for all ten clusters, Z/Z⊙ = 0.21 ± 0.09, represents a substantial improvement in precision over previous results. This measurement is consistent with, but slightly lower than, the average metallicity of 0.315 Solar measured at intermediate-to-large radii in low-redshift clusters. Combining our new high-redshift data with the previous low-redshift results allows us to place the tightest constraints to date on models of the evolution of cluster metallicity at intermediate radii. Adopting a power law model of the form Z∝(1 + z)γ, we measure a slope $\gamma = -0.5^{+0.4}_{-0.3}$, consistent with the majority of the enrichment of the ICM having occurred at very early times and before massive clusters formed, but leaving open the possibility that some additional enrichment in these regions may have occurred since a redshift of 2.

scholarly journals New spectroscopic confirmations of high-redshift galaxy clusters

2005 ◽  
Vol 442 (3) ◽  
pp. 841-849 ◽  
Author(s):  
L. F. Olsen ◽  
E. Zucca ◽  
S. Bardelli ◽  
C. Benoist ◽  
L. da Costa ◽  
...  
Keyword(s):  
Galaxy Clusters ◽  
High Redshift ◽  
Redshift Galaxy
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