scholarly journals Inferring the dark matter velocity anisotropy to the cluster edge

2020 ◽  
Vol 500 (3) ◽  
pp. 3151-3161
Author(s):  
Jacob Svensmark ◽  
Steen H Hansen ◽  
Davide Martizzi ◽  
Ben Moore ◽  
Romaine Tessier
Keyword(s):  
Dark Matter ◽  
Numerical Simulations ◽  
Galaxy Cluster ◽  
Dynamical Property ◽  
Large Error ◽  
New Method ◽  
Bright Galaxy ◽  
X Ray ◽  
Velocity Anisotropy ◽  
Error Bars

ABSTRACT Dark matter (DM) dominates the properties of large cosmological structures such as galaxy clusters, and the mass profiles of the DM have been inferred for these equilibrated structures for years by using cluster X-ray surface brightnesses and temperatures. A new method has been proposed, which should allow us to infer a dynamical property of the DM, namely the velocity anisotropy. For the gas, a similar velocity anisotropy is zero due to frequent collisions; however, the collisionless nature of DM allows it to be non-trivial. Numerical simulations have for years found non-zero and radially varying DM velocity anisotropies. Here we employ the method proposed by Hansen & Piffaretti, and developed by Høst et al. to infer the DM velocity anisotropy in the bright galaxy cluster Perseus, to near five times the radii previously obtained. We find the DM velocity anisotropy to be consistent with the results of numerical simulations, however, still with large error bars. At half the virial radius, we find the DM velocity anisotropy to be non-zero at 1.7$\, \sigma$, lending support to the collisionless nature of DM.

The new fundamental plane dictating galaxy cluster evolution

2019 ◽  
Vol 15 (S341) ◽  
pp. 271-272
Author(s):  
Yutaka Fujita ◽  
Keiichi Umetsu ◽  
Elena Rasia ◽  
Massimo Meneghetti ◽  
Megan Donahue ◽  
...  
Keyword(s):  
Numerical Simulations ◽  
Structure Formation ◽  
Similarity Solution ◽  
Cluster Structure ◽  
Galaxy Cluster ◽  
Fundamental Plane ◽  
X Ray ◽  
Cluster Evolution ◽  
Characteristic Radius ◽  
Tight Correlation

AbstractIn this study, we show that the characteristic radius rs, mass Ms, and the X-ray temperature, TX, of galaxy clusters form a thin plane in the space of (log rs, log Ms, log TX). This tight correlation indicates that the cluster structure including the temperature is affected by the formation time of individual clusters. Numerical simulations show that clusters move along the fundamental plane as they evolve. The plane and the cluster evolution within the plane can be explained by a similarity solution of structure formation. The angle of the plane shows that clusters have not achieved “virial equilibrium”. The details of this study are written in Fujita et al. (2018a,b).

scholarly journals Constraints on the Self‐Interaction Cross Section of Dark Matter from Numerical Simulations of the Merging Galaxy Cluster 1E 0657−56

2008 ◽  
Vol 679 (2) ◽  
pp. 1173-1180 ◽  
Author(s):  
Scott W. Randall ◽  
Maxim Markevitch ◽  
Douglas Clowe ◽  
Anthony H. Gonzalez ◽  
Marusa Bradač
Keyword(s):  
Dark Matter ◽  
Numerical Simulations ◽  
Cross Section ◽  
Galaxy Cluster ◽  
The Self ◽  
Interaction Cross Section

scholarly journals Investigating the Relationship Between the Hot Gas and the Dark Matter Components of Galaxy Clusters.

2007 ◽  
Vol 3 (S244) ◽  
pp. 374-375
Author(s):  
Leila C. Powell ◽  
Scott T. Kay ◽  
Arif Babul ◽  
Andisheh Mahdavi
Keyword(s):  
Dark Matter ◽  
Total Mass ◽  
Surface Brightness ◽  
Galaxy Cluster ◽  
Weak Lensing ◽  
X Ray ◽  
Hot Gas ◽  
Cluster Properties ◽  
The Impact ◽  
The Relationship

AbstractVarious differences in galaxy cluster properties derived from X-ray and weak lensing observations have been highlighted in the literature. One such difference is the observation of mass concentrations in lensing maps which have no X-ray counterparts (e.g. Jee, White, Ford et al. 2005). We investigate this issue by identifying substructures in maps of projected total mass (analogous to weak lensing mass reconstructions) and maps of projected X-ray surface brightness for three simulated clusters. We then compare the 2D mass substructures with both 3D subhalo data and the 2D X-ray substructures. Here we present preliminary results from the first comparison, where we have assessed the impact of projecting the data on subhalo identification.

scholarly journals Dark Matter and Baryons in the X‐Ray Luminous Merging Galaxy Cluster RX J1347.5−1145

2008 ◽  
Vol 681 (1) ◽  
pp. 187-196 ◽  
Author(s):  
Maruša Bradač ◽  
Tim Schrabback ◽  
Thomas Erben ◽  
Michael McCourt ◽  
Evan Million ◽  
...  
Keyword(s):  
Dark Matter ◽  
Galaxy Cluster ◽  
X Ray

scholarly journals PRECESSING JETS AND X-RAY BUBBLES FROM NGC 1275 (3C 84) IN THE PERSEUS GALAXY CLUSTER: A VIEW FROM THREE-DIMENSIONAL NUMERICAL SIMULATIONS

2010 ◽  
Vol 713 (1) ◽  
pp. L74-L78 ◽  
Author(s):  
D. Falceta-Gonçalves ◽  
A. Caproni ◽  
Z. Abraham ◽  
D. M. Teixeira ◽  
E. M. de Gouveia Dal Pino
Keyword(s):  
Numerical Simulations ◽  
Three Dimensional ◽  
Galaxy Cluster ◽  
X Ray ◽  
Cluster A ◽  
Ngc 1275

scholarly journals Simulations of the merging galaxy cluster Abell 2034: what determines the level of separation between gas and dark matter

2020 ◽  
Vol 500 (2) ◽  
pp. 1858-1869 ◽  
Author(s):  
Micheli T Moura ◽  
Rubens E G Machado ◽  
Rogério Monteiro-Oliveira
Keyword(s):  
Dark Matter ◽  
Gravitational Lensing ◽  
Galaxy Cluster ◽  
X Rays ◽  
X Ray ◽  
History Of ◽  
Hydrodynamical Simulations ◽  
Cluster Mergers ◽  
Cluster Cores ◽  
Intracluster Gas

ABSTRACT Cluster mergers are an important laboratory for studying the behaviour of dark matter (DM) and intracluster gas. There are dissociative collisions that can separate the intracluster gas from the DM. Abell 2034 presents clear dissociative features observed by X-rays and gravitational lensing. The cluster, at z = 0.114, consists of two substructures with mass ratio of about 1:2.2, separated by ∼720 kpc. The X-ray emission peak is offcentred from the south DM peak by ∼350 kpc. Using N-body hydrodynamical simulations, we aim to reconstruct the dynamic history of the collision, reproducing the observed features, and also to explore the conditions that led to the dissociation. Our best model assuming that the collision is close to the plane of the sky, with a small impact parameter, observed 0.26 Gyr after central passage, reproduces the observed features of this cluster, such as the offset between X-ray and DM peaks, X-ray morphology, and temperatures. We explored several variations using different gas and DM concentrations for each cluster. The level of dissociation was quantified by the distances between X-ray and DM peaks, and also by the gas retention in the cluster cores. We found that the ratio of central gas densities is more important than the ratio of central DM densities in determining the level of dissociation.

scholarly journals Halo Occupation Distribution of AGNs throught Numerical Simulations

2013 ◽  
Vol 9 (S304) ◽  
pp. 335-336
Author(s):  
Liliana Altamirano-Dévora ◽  
Takamitsu Miyaji ◽  
Héctor Aceves
Keyword(s):  
Dark Matter ◽  
Numerical Simulations ◽  
Active Galactic Nuclei ◽  
Galactic Nuclei ◽  
Dark Matter Halos ◽  
X Ray ◽  
Major Merger ◽  
Halo Occupation Distribution

AbstractUsing a set of simulations in the ΛCDM cosmology, and the mass of intermediate X-Ray Active Galactic Nuclei (AGN) dark matter halos (DMH), we study the Halo Occupation Distribution (HOD) of their host DMH and compare with recent observations. We assume that intermediate X-Ray AGNs have been triggered by a major merger of sub-halos inside larger host halos. We find that the binary major merger HOD slope (α ≈ 0.8) do not seem to reproduce the observed HOD slope (α < 0.6) for these type of AGNs. Other mechanisms may be igniting these AGNs.

scholarly journals Galaxy cluster cosmology from X-ray surveys of the hot and energetic Universe

2015 ◽  
Vol 11 (A29B) ◽  
pp. 79-90
Author(s):  
Nicolas Clerc ◽  
Barbara Sartoris ◽  
Klaus Dolag ◽  
Rukmani Vijayaraghavan ◽  
Veronica Biffi
Keyword(s):  
Dark Energy ◽  
Numerical Simulations ◽  
Galaxy Clusters ◽  
Galaxy Cluster ◽  
X Ray ◽  
Recent Advances ◽  
Evolution With Time

AbstractWe discuss recent advances and prospects in our understanding of the formation of structures on cosmic scales based on surveys of galaxy clusters in the X-ray bands. We highlight the interaction between observations and numerical simulations of the X-ray sky. We show how future surveys will unveil the nature of the dark energy and study its evolution with time.

Mapping of accumulation of SeNPs in developing zebrafish embryos and larvae: a new method using SEM with energy dispersive X‐ray spectrometer

2017 ◽  
Vol 12 (7) ◽  
pp. 497-499
Author(s):  
Kalimuthu Kalishwaralal ◽  
Subhaschandrabose Jeyabharathi ◽  
Krishnan Sundar ◽  
Azhaguchamy Muthukumaran
Keyword(s):  
Energy Dispersive ◽  
New Method ◽  
Zebrafish Embryos ◽  
X Ray
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