scholarly journals Unifying X-ray scaling relations from galaxies to clusters

2015 ◽  
Vol 449 (4) ◽  
pp. 3806-3826 ◽  
Author(s):  
M. E. Anderson ◽  
M. Gaspari ◽  
S. D. M. White ◽  
W. Wang ◽  
X. Dai
Keyword(s):  
Scaling Relations ◽  
X Ray

Supermassive Black Hole feedback in early type galaxies

2020 ◽  
Vol 15 (S359) ◽  
pp. 119-125
Author(s):  
W. Forman ◽  
C. Jones ◽  
A. Bogdan ◽  
R. Kraft ◽  
E. Churazov ◽  
...  
Keyword(s):  
Dark Matter Halo ◽  
Scaling Relations ◽  
Radio Sources ◽  
Early Type ◽  
X Ray ◽  
Galaxy Groups ◽  
Sufficient Energy ◽  
The Galaxy ◽  
Simple Scaling ◽  
Halo Masses

AbstractOptically luminous early type galaxies host X-ray luminous, hot atmospheres. These hot atmospheres, which we refer to as coronae, undergo the same cooling and feedback processes as are commonly found in their more massive cousins, the gas rich atmospheres of galaxy groups and galaxy clusters. In particular, the hot coronae around galaxies radiatively cool and show cavities in X-ray images that are filled with relativistic plasma originating from jets powered by supermassive black holes (SMBH) at the galaxy centers. We discuss the SMBH feedback using an X-ray survey of early type galaxies carried out using Chandra X-ray Observatory observations. Early type galaxies with coronae very commonly have weak X-ray active nuclei and have associated radio sources. Based on the enthalpy of observed cavities in the coronae, there is sufficient energy to “balance” the observed radiative cooling. There are a very few remarkable examples of optically faint galaxies that are 1) unusually X-ray luminous, 2) have large dark matter halo masses, and 3) have large SMBHs (e.g., NGC4342 and NGC4291). These properties suggest that, in some galaxies, star formation may have been truncated at early times, breaking the simple scaling relations.

scholarly journals LoCuSS: comparison of observed X-ray and lensing galaxy cluster scaling relations with simulations

2008 ◽  
Vol 482 (2) ◽  
pp. 451-472 ◽  
Author(s):  
Y.-Y. Zhang ◽  
A. Finoguenov ◽  
H. Böhringer ◽  
J.-P. Kneib ◽  
G. P. Smith ◽  
...  
Keyword(s):  
Galaxy Cluster ◽  
Scaling Relations ◽  
X Ray

scholarly journals Cluster Physics & Evolution

2015 ◽  
Vol 11 (A29B) ◽  
pp. 70-78
Author(s):  
Daisuke Nagai ◽  
Monique Arnaud ◽  
Sarthak Dasadia ◽  
Michael McDonald ◽  
Ikuyuki Mitsuishi ◽  
...  
Keyword(s):  
Galaxy Clusters ◽  
Statistical Power ◽  
Scaling Relations ◽  
Intracluster Medium ◽  
Physical Processes ◽  
X Ray ◽  
Cosmological Constraints ◽  
Recent Advances

AbstractRecent advances in X-ray and microwave observations have provided unprecedented insights into the structure and evolution of the hot X-ray emitting plasma from their cores to the virialization region in outskirts of galaxy clusters. Recent Sunyaev-Zel'dovich (SZ) surveys (ACT, Planck, SPT) have provided new cluster catalogs, significantly expanding coverage of the mass-redshift plane, whileChandraandXMM-NewtonX-ray follow-up programs have improved our understanding of cluster physics and evolution as well as the surveys themselves. However, the current cluster-based cosmological constraints are still limited by uncertainties in cluster astrophysics. In order to exploit the statistical power of the current and upcoming X-ray and microwave cluster surveys, it is critical to improve our understanding of the structure and evolution of the hot X-ray emitting intracluster medium (ICM). In this session, we discussed recent advances in observations and simulations of galaxy clusters, with highlights on (i) the evolution of ICM profiles and scaling relations, (ii) physical processes operating in the outskirts of galaxy clusters, and (iii) impact of mergers on the ICM structure in groups and clusters.

scholarly journals Do sub-galactic regions follow the galaxy-wide X-ray scaling relations? The example of NGC 3310 and NGC 2276

2018 ◽  
Vol 483 (1) ◽  
pp. 711-733 ◽  
Author(s):  
K Anastasopoulou ◽  
A Zezas ◽  
V Gkiokas ◽  
K Kovlakas
Keyword(s):  
Scaling Relations ◽  
X Ray ◽  
The Galaxy

scholarly journals The X-Ray Halo Scaling Relations of Supermassive Black Holes

2019 ◽  
Vol 884 (2) ◽  
pp. 169 ◽  
Author(s):  
M. Gaspari ◽  
D. Eckert ◽  
S. Ettori ◽  
P. Tozzi ◽  
L. Bassini ◽  
...  
Keyword(s):  
Black Holes ◽  
Supermassive Black Holes ◽  
Scaling Relations ◽  
X Ray

scholarly journals X-ray calibration of Sunyaev-Zel’dovich scaling relations with the ACCEPT catalogue of galaxy clusters observed by Chandra

2011 ◽  
Vol 418 (2) ◽  
pp. 1089-1101 ◽  
Author(s):  
B. Comis ◽  
M. De Petris ◽  
A. Conte ◽  
L. Lamagna ◽  
S. De Gregori
Keyword(s):  
Galaxy Clusters ◽  
Scaling Relations ◽  
X Ray

scholarly journals Probing cosmic isotropy with a new X-ray galaxy cluster sample through the LX–T scaling relation

2020 ◽  
Vol 636 ◽  
pp. A15 ◽  
Author(s):  
K. Migkas ◽  
G. Schellenberger ◽  
T. H. Reiprich ◽  
F. Pacaud ◽  
M. E. Ramos-Ceja ◽  
...  
Keyword(s):  
Galaxy Clusters ◽  
Statistical Significance ◽  
Cosmological Parameters ◽  
Galaxy Cluster ◽  
Temperature Measurements ◽  
Joint Analysis ◽  
Scaling Relations ◽  
Exact Nature ◽  
X Rays ◽  
X Ray

The isotropy of the late Universe and consequently of the X-ray galaxy cluster scaling relations is an assumption greatly used in astronomy. However, within the last decade, many studies have reported deviations from isotropy when using various cosmological probes; a definitive conclusion has yet to be made. New, effective and independent methods to robustly test the cosmic isotropy are of crucial importance. In this work, we use such a method. Specifically, we investigate the directional behavior of the X-ray luminosity-temperature (LX–T) relation of galaxy clusters. A tight correlation is known to exist between the luminosity and temperature of the X-ray-emitting intracluster medium of galaxy clusters. While the measured luminosity depends on the underlying cosmology through the luminosity distance DL, the temperature can be determined without any cosmological assumptions. By exploiting this property and the homogeneous sky coverage of X-ray galaxy cluster samples, one can effectively test the isotropy of cosmological parameters over the full extragalactic sky, which is perfectly mirrored in the behavior of the normalization A of the LX–T relation. To do so, we used 313 homogeneously selected X-ray galaxy clusters from the Meta-Catalogue of X-ray detected Clusters of galaxies. We thoroughly performed additional cleaning in the measured parameters and obtain core-excised temperature measurements for all of the 313 clusters. The behavior of the LX–T relation heavily depends on the direction of the sky, which is consistent with previous studies. Strong anisotropies are detected at a ≳4σ confidence level toward the Galactic coordinates (l, b) ∼ (280°, − 20°), which is roughly consistent with the results of other probes, such as Supernovae Ia. Several effects that could potentially explain these strong anisotropies were examined. Such effects are, for example, the X-ray absorption treatment, the effect of galaxy groups and low redshift clusters, core metallicities, and apparent correlations with other cluster properties, but none is able to explain the obtained results. Analyzing 105 bootstrap realizations confirms the large statistical significance of the anisotropic behavior of this sky region. Interestingly, the two cluster samples previously used in the literature for this test appear to have a similar behavior throughout the sky, while being fully independent of each other and of our sample. Combining all three samples results in 842 different galaxy clusters with luminosity and temperature measurements. Performing a joint analysis, the final anisotropy is further intensified (∼5σ), toward (l, b) ∼ (303°, − 27°), which is in very good agreement with other cosmological probes. The maximum variation of DL seems to be ∼16 ± 3% for different regions in the sky. This result demonstrates that X-ray studies that assume perfect isotropy in the properties of galaxy clusters and their scaling relations can produce strongly biased results whether the underlying reason is cosmological or related to X-rays. The identification of the exact nature of these anisotropies is therefore crucial for any statistical cluster physics or cosmology study.

scholarly journals The evolution of galaxy cluster X-ray scaling relations

2010 ◽  
Vol 408 (4) ◽  
pp. 2213-2233 ◽  
Author(s):  
C. J. Short ◽  
P. A. Thomas ◽  
O. E. Young ◽  
F. R. Pearce ◽  
A. Jenkins ◽  
...  
Keyword(s):  
Galaxy Cluster ◽  
Scaling Relations ◽  
X Ray

scholarly journals The cosmological analysis of X-ray cluster surveys

2018 ◽  
Vol 614 ◽  
pp. A72 ◽  
Author(s):  
A. Valotti ◽  
M. Pierre ◽  
A. Farahi ◽  
A. Evrard ◽  
L. Faccioli ◽  
...  
Keyword(s):  
Cosmological Parameters ◽  
Scaling Relations ◽  
Temperature Relation ◽  
Local Scaling ◽  
X Ray ◽  
Mass Size ◽  
Final Error ◽  
Hydrodynamical Simulations ◽  
The Impact ◽  
Size Relation

Context. This paper is the fourth of a series evaluating the ASpiX cosmological method, based on X-ray diagrams, which are constructed from simple cluster observable quantities, namely: count rate (CR), hardness ratio (HR), core radius (rc), and redshift. Aims. Following extensive tests on analytical toy catalogues (Paper III), we present the results of a more realistic study over a 711 deg2 template-based maps derived from a cosmological simulation. Methods. Dark matter haloes from the Aardvark simulation have been ascribed luminosities, temperatures, and core radii, using local scaling relations and assuming self-similar evolution. The predicted X-ray sky-maps were converted into XMM event lists, using a detailed instrumental simulator. The XXL pipeline runs on the resulting sky images, produces an observed cluster catalogue over which the tests have been performed. This allowed us to investigate the relative power of various combinations of the CR, HR, rc, and redshift information. Two fitting methods were used: a traditional Markov chain Monte Carlo (MCMC) approach and a simple minimisation procedure (Amoeba) whose mean uncertainties are a posteriori evaluated by means of synthetic catalogues. The results were analysed and compared to the predictions from the Fisher analysis (FA). Results. For this particular catalogue realisation, assuming that the scaling relations are perfectly known, the CR-HR combination gives σ8 and Ωm at the 10% level, while CR-HR-rc-z improves this to ≤3%. Adding a second HR improves the results from the CR-HR1-rc combination, but to a lesser extent than when adding the redshift information. When all coefficients of the mass-temperature relation (M-T, including scatter) are also fitted, the cosmological parameters are constrained to within 5–10% and larger for the M-T coefficients (up to a factor of two for the scatter). The errors returned by the MCMC, those by Amoeba and the FA predictions are in most cases in excellent agreement and always within a factor of two. We also study the impact of the scatter of the mass-size relation (M-Rc) on the number of detected clusters: for the cluster typical sizes usually assumed, the larger the scatter, the lower the number of detected objects. Conclusions. The present study confirms and extends the trends outlined in our previous analyses, namely the power of X-ray observable diagrams to successfully and easily fit at the same time, the cosmological parameters, cluster physics, and the survey selection, by involving all detected clusters. The accuracy levels quoted should not be considered as definitive. A number of simplifying hypotheses were made for the testing purpose, but this should affect any method in the same way. The next publication will consider in greater detail the impact of cluster shapes (selection and measurements) and of cluster physics on the final error budget by means of hydrodynamical simulations.

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