A Complete Sample of 12 Very X-Ray Luminous Galaxy Clusters at z > 0.5

2007 ◽  
Vol 661 (1) ◽  
pp. L33-L36 ◽  
Author(s):  
H. Ebeling ◽  
E. Barrett ◽  
D. Donovan ◽  
C.-J. Ma ◽  
A. C. Edge ◽  
...  
Keyword(s):  
Galaxy Clusters ◽  
Complete Sample ◽  
X Ray

scholarly journals Chandrameasurements of a complete sample of X-ray luminous galaxy clusters: the luminosity–mass relation

2016 ◽  
Vol 465 (1) ◽  
pp. 858-884 ◽  
Author(s):  
P. A. Giles ◽  
B. J. Maughan ◽  
H. Dahle ◽  
M. Bonamente ◽  
D. Landry ◽  
...  
Keyword(s):  
Galaxy Clusters ◽  
Mass Relation ◽  
Complete Sample ◽  
X Ray

scholarly journals The X-ray luminosity–temperature relation of a complete sample of low-mass galaxy clusters

2016 ◽  
Vol 463 (1) ◽  
pp. 820-831 ◽  
Author(s):  
S. Zou ◽  
B. J. Maughan ◽  
P. A. Giles ◽  
A. Vikhlinin ◽  
F. Pacaud ◽  
...  
Keyword(s):  
Galaxy Clusters ◽  
Complete Sample ◽  
Temperature Relation ◽  
X Ray ◽  
Low Mass

scholarly journals The NEP ROSAT Survey

1998 ◽  
Vol 188 ◽  
pp. 473-474 ◽  
Author(s):  
C.R. Mullis ◽  
I.M. Gioia ◽  
J.P. Henry
Keyword(s):  
Galaxy Clusters ◽  
Luminosity Function ◽  
Survey Area ◽  
Complete Sample ◽  
X Ray ◽  
Preliminary Results ◽  
The North ◽  
Sky Survey

The Rosat All-Sky Survey (Trümper 1991, Adv. Spce Res., 2, 241) has its largest exposure times, approaching 10 ks, at the ecliptic poles where the scan circles overlap. The North Ecliptic Pole (NEP) region covers a 9° X 9° field, and contains a total of 465 X-ray sources detected at > 4σ in the 0.1-2.4 keV. We are identifying all sources in the field. The principal derivative is a statistically complete sample of galaxy clusters appropriate for more fully characterizing X-ray Luminosity Function (XLF) evolution. We report preliminary results for two subregions which are identified to the 95% level. These subregions are observed to approximately the median NEP survey exposure. They enclose 16% of the survey area and contain 96 X-ray sources representing 21% of the total NEP. The typical mix of sources is consistent with the Einstein Extended Medium Sensisitivity Survey (EMSS; Gioia et al., 1990a, ApJS, 72, 567). In particular there are 56% AGN/ELG (59% in the EMSS), 25% stars (27% in the EMSS) and 14% clusters against 13% clusters in the EMSS.

scholarly journals Chandra measurements of a complete sample of X-ray luminous galaxy clusters: the gas mass fraction

2013 ◽  
Vol 433 (4) ◽  
pp. 2790-2811 ◽  
Author(s):  
D. Landry ◽  
M. Bonamente ◽  
P. Giles ◽  
B. Maughan ◽  
M. Joy ◽  
...  
Keyword(s):  
Galaxy Clusters ◽  
Mass Fraction ◽  
Complete Sample ◽  
X Ray

scholarly journals Diffuse radio sources in a statistically complete sample of high-redshift galaxy clusters

2020 ◽  
Vol 640 ◽  
pp. A108 ◽  
Author(s):  
G. Giovannini ◽  
M. Cau ◽  
A. Bonafede ◽  
H. Ebeling ◽  
L. Feretti ◽  
...  
Keyword(s):  
Radio Emission ◽  
Galaxy Clusters ◽  
High Redshift ◽  
Complete Sample ◽  
Cluster Emission ◽  
X Ray ◽  
Cluster Galaxies ◽  
Diffuse Sources ◽  
Radio Halo ◽  
Radio Halos

Aims. Non-thermal properties of galaxy clusters have been studied using detailed and deep radio images in comparison with X-ray data. While much progress has been made in this area, most of the studied clusters are at a relatively low redshift (z <  0.3). Here we investigate the evolutionary properties of the non-thermal cluster emission using two statistically complete samples at z >  0.3. Methods. We obtained short JVLA observations at the L-band of the statistically complete sample of very X-ray luminous clusters from the Massive Cluster Survey (MACS), namely 34 clusters in the redshift range of 0.3–0.5 and with nominal X-ray fluxes in excess of 2 × 10−12 erg s−1 cm−2 (0.1–2.4 keV) in the ROSAT Bright Source Catalogue. We add to this list the complete sample of the 12 most distant MACS clusters (z >  0.5). Results. Most clusters show evidence of emission in the radio regime. We present the radio properties of all clusters in our sample and show images of newly detected diffuse sources. A radio halo is detected in 19 clusters and five clusters contain a relic source. Most of the brightest cluster galaxies (BCG) in relaxed clusters show radio emission with powers typical of FRII radio galaxies and some are surrounded by a radio mini-halo. Conclusions. The high frequency of radio emission from the BCG in relaxed clusters suggests that BCG feedback mechanisms are already in place at z ∼ 0.6. The properties of radio halos and the small number of detected relics suggest redshift evolution in the properties of diffuse sources. The radio power (and size) of radio halos could be related to the number of past merger events in the history of the system. In this scenario, the presence of a giant and high-power radio halo is indicative of an evolved system with a large number of past major mergers, whereas small low-power halos are found in less evolved clusters.

scholarly journals High redshift X-ray galaxy clusters

2007 ◽  
Vol 472 (3) ◽  
pp. 739-748 ◽  
Author(s):  
M. Branchesi ◽  
I. M. Gioia ◽  
C. Fanti ◽  
R. Fanti
Keyword(s):  
Galaxy Clusters ◽  
High Redshift ◽  
X Ray

scholarly journals ON THE ORIGIN OF COOL CORE GALAXY CLUSTERS: COMPARING X-RAY OBSERVATIONS WITH NUMERICAL SIMULATIONS

2009 ◽  
Vol 697 (2) ◽  
pp. 1597-1620 ◽  
Author(s):  
Jason W. Henning ◽  
Brennan Gantner ◽  
Jack O. Burns ◽  
Eric J. Hallman
Keyword(s):  
Numerical Simulations ◽  
Galaxy Clusters ◽  
X Ray

scholarly journals X-ray mapping the outer regions of galaxy clusters at z = 0.23 and 0.45

2014 ◽  
Vol 439 (2) ◽  
pp. 1796-1806 ◽  
Author(s):  
Q. Daniel Wang ◽  
Stephen Walker
Keyword(s):  
Galaxy Clusters ◽  
X Ray

scholarly journals Anisotropy of the galaxy cluster X-ray luminosity–temperature relation

2018 ◽  
Vol 611 ◽  
pp. A50 ◽  
Author(s):  
Konstantinos Migkas ◽  
Thomas H. Reiprich
Keyword(s):  
Galaxy Clusters ◽  
Statistical Significance ◽  
Cosmological Parameters ◽  
Galaxy Cluster ◽  
Luminosity Distance ◽  
Temperature Relation ◽  
X Ray ◽  
Two Samples ◽  
The Galaxy ◽  
Group A

We introduce a new test to study the cosmological principle with galaxy clusters. Galaxy clusters exhibit a tight correlation between the luminosity and temperature of the X-ray-emitting intracluster medium. While the luminosity measurement depends on cosmological parameters through the luminosity distance, the temperature determination is cosmology-independent. We exploit this property to test the isotropy of the luminosity distance over the full extragalactic sky, through the normalization a of the LX–T scaling relation and the cosmological parameters Ωm and H0. To this end, we use two almost independent galaxy cluster samples: the ASCA Cluster Catalog (ACC) and the XMM Cluster Survey (XCS-DR1). Interestingly enough, these two samples appear to have the same pattern for a with respect to the Galactic longitude. More specifically, we identify one sky region within l ~ (−15°, 90°) (Group A) that shares very different best-fit values for the normalization of the LX–T relation for both ACC and XCS-DR1 samples. We use the Bootstrap and Jackknife methods to assess the statistical significance of these results. We find the deviation of Group A, compared to the rest of the sky in terms of a, to be ~2.7σ for ACC and ~3.1σ for XCS-DR1. This tension is not significantly relieved after excluding possible outliers and is not attributed to different redshift (z), temperature (T), or distributions of observable uncertainties. Moreover, a redshift conversion to the cosmic microwave background (CMB) frame does not have an important impact on our results. Using also the HIFLUGCS sample, we show that a possible excess of cool-core clusters in this region, is not able to explain the obtained deviations. Furthermore, we tested for a dependence of the results on supercluster environment, where the fraction of disturbed clusters might be enhanced, possibly affecting the LX–T relation. We indeed find a trend in the XCS-DR1 sample for supercluster members to be underluminous compared to field clusters. However, the fraction of supercluster members is similar in the different sky regions, so this cannot explain the observed differences, either. Constraining Ωm and H0 via the redshift evolution of LX–T and the luminosity distance via the flux–luminosity conversion, we obtain approximately the same deviation amplitudes as for a. It is interesting that the general observed behavior of Ωm for the sky regions that coincide with the CMB dipole is similar to what was found with other cosmological probes such as supernovae Ia. The reason for this behavior remains to be identified.

Sign in / Sign up

Export Citation Format

Share Document