Cosmology with Clusters of Galaxies

Borgani, S.

doi:10.1007/978-1-4020-6941-3_9

Cited by 22 publications

(21 citation statements)

References 163 publications

(212 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…), and so is the L X − M with respect to the simplest gravitational model. These processes are modeled in up-to-date numerical simulations that combine the gravitational evolution of dark matter structures with the hydrodynamical behavior of the intracluster gas (Borgani et al 2004;Kay 2004;Borgani 2008). These simulations also seem to favor a slope of the L X − M relation that is steeper than the canonical one.…”

Section: X-ray Scaling Lawsmentioning

confidence: 99%

The dark matter distribution inz ~ 0.5 clusters of galaxies

Foëx¹,

Soucail²,

Pointecouteau³

et al. 2012

A&A

View full text Add to dashboard Cite

The total mass of clusters of galaxies is a key parameter for studing massive halos. It relates to numerous gravitational and baryonic processes at play in the framework of large-scale structure formation, thus rendering its determination both important and challenging. From a sample of the 11 X-ray bright clusters selected from the EXCPRES sample, we investigate the optical and X-ray properties of clusters with respect to their total mass derived from weak gravitational lensing. From multicolor, wide-field imaging obtained with MegaCam at CFHT, we derive the shear profile of each individual cluster of galaxies. We carefully investigate all systematic sources related to the weak lensing mass determination. The weak lensing masses are then compared to the X-ray masses obtained from the analysis of XMM-Newton observations assuming hydrostatic equilibrium. We find good agreement between the two mass proxies although a few outliers with either perturbed morphology or poor quality data prevent deriving robust mass estimates. The weak lensing mass is also correlated with the optical richness and the total optical luminosity, as well as with the X-ray luminosity, to provide scaling relations within the redshift range 0.4 < z < 0.6. These relations are in good agreement with previous works at lower redshifts. For the L X − M relation we combine our sample with two other cluster and group samples from the literature, thus covering two decades in mass and X-ray luminosity, with a regular and coherent correlation between the two physical quantities.

show abstract

Section: X-ray Scaling Lawsmentioning

confidence: 99%

The dark matter distribution inz ~ 0.5 clusters of galaxies

Foëx¹,

Soucail²,

Pointecouteau³

et al. 2012

A&A

View full text Add to dashboard Cite

show abstract

“…They contain from a few tens to a few thousands of galaxies. The frequency distribution of cluster masses, the mass function, and its evolution have been recognized as a very important cosmological probe that can constrain the current cosmological model (eg., Borgani 2008, Reddick et al 2014, Sartoris et al 2014. Consequently, the accurate calculation of cluster masses is of uttermost importance and a powerful means to cosmological studies.…”

Section: Introductionmentioning

confidence: 99%

Galaxy cluster's rotation

Manolopoulou

Plionis

2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We study the possible rotation of cluster galaxies, developing, testing and applying a novel algorithm which identifies rotation, if such does exist, as well as its rotational centre, its axis orientation, rotational velocity amplitude and, finally, the clockwise or counterclockwise direction of rotation on the plane of the sky. To validate our algorithms we construct realistic Monte Carlo mock rotating clusters and confirm that our method provides robust indications of rotation. We then apply our methodology on a sample of Abell clusters with z 0.1 with member galaxies selected from the Sloan Digital Sky Survey (SDSS) DR10 spectroscopic data base. After excluding a number of substructured clusters, which could provide erroneous indications of rotation, and taking into account the expected fraction of misidentified coherent substructure velocities for rotation, provided by our Monte-Carlo simulation analysis, we find that ∼ 23% of our clusters are rotating under a set of strict criteria. Loosening the strictness of the criteria, on the expense of introducing spurious rotation indications, we find this fraction increasing to ∼ 28%. We correlate our rotation indicators with the cluster dynamical state, provided either by their Bautz-Morgan type or by their Xray isophotal shape and find for those clusters showing rotation within 1.5 h −1 70 Mpc that the significance of their rotation is related to the dynamically younger phases of cluster formation but after the initial anisotropic accretion and merging has been completed. Finally, finding rotational modes in galaxy clusters could lead to the necessity of correcting the dynamical cluster mass calculations.

show abstract

“…The member galaxy and relativistic particle properties of cluster outskirts have been reviewed, e.g., in the Proceedings to the IAU colloquium "Outskirts of Galaxy Clusters: Intense Life in the Suburbs" (Diaferio 2004) and Brüggen et al (2011), respectively. Other useful reviews mostly about the ICM properties of clusters include, e.g., Sarazin (1986); Borgani & Guzzo (2001); Rosati et al (2002); Voit (2005); Arnaud (2005); Norman (2005); Borgani (2008); Borgani & Kravtsov (2011); Allen et al (2011).…”

Section: Introductionmentioning

confidence: 99%

Outskirts of Galaxy Clusters

et al. 2013

View full text Add to dashboard Cite

Until recently, only about 10% of the total intracluster gas volume had been studied with high accuracy, leaving a vast region essentially unexplored. This is now changing and a wide area of hot gas physics and chemistry awaits discovery in galaxy cluster outskirts. Also, robust large-scale total mass profiles and maps are within reach. First observational and theoretical results in this emerging field have been achieved in recent years with sometimes surprising findings. Here, we summarize and illustrate the relevant underlying physical and chemical processes and review the recent progress in X-ray, Sunyaev-Zel'dovich, and weak gravitational lensing observations of cluster outskirts, including also brief discussions of technical challenges and possible future improvements.Keywords Galaxy clusters · large-scale structure of the Universe · intracluster matter

show abstract

Cosmology with Clusters of Galaxies

Cited by 22 publications

References 163 publications

The dark matter distribution inz ~ 0.5 clusters of galaxies

The dark matter distribution inz ~ 0.5 clusters of galaxies

Galaxy cluster's rotation

Outskirts of Galaxy Clusters

Contact Info

Product

Resources

About