79 research outputs found
The matter distribution in z ~ 0.5 redshift clusters of galaxies. II : The link between dark and visible matter
We present an optical analysis of a sample of 11 clusters built from the
EXCPRES sample of X-ray selected clusters at intermediate redshift (z ~ 0.5).
With a careful selection of the background galaxies we provide the mass maps
reconstructed from the weak lensing by the clusters. We compare them with the
light distribution traced by the early-type galaxies selected along the red
sequence for each cluster. The strong correlations between dark matter and
galaxy distributions are confirmed, although some discrepancies arise, mostly
for merging or perturbed clusters. The average M/L ratio of the clusters is
found to be: M/L_r = 160 +/- 60 in solar units (with no evolutionary
correction), in excellent agreement with similar previous studies. No strong
evolutionary effects are identified even if the small sample size reduces the
significance of the result. We also provide a individual analysis of each
cluster in the sample with a comparison between the dark matter, the galaxies
and the gas distributions. Some of the clusters are studied for the first time
in the optical.Comment: 25 pages, 9 figues + 11 figures in Annex, 4 tables. Accepted for
publication in A&A. 1 reference correcte
Investigating the turbulent hot gas in X-COP galaxy clusters
Turbulent processes at work in the intracluster medium perturb this
environment, displacing gas, and creating local density fluctuations that can
be quantified via X-ray surface brightness fluctuation analyses. Improved
knowledge of these phenomena would allow for a better determination of the mass
of galaxy clusters, as well as a better understanding of their dynamic
assembly. In this work, we aim to set constraints on the structure of
turbulence using X-ray surface brightness fluctuations. We seek to consider the
stochastic nature of this observable and to constrain the structure of the
underlying power spectrum. We propose a new Bayesian approach, relying on
simulation-based inference to account for the whole error budget. We used the
X-COP cluster sample to individually constrain the power spectrum in four
regions and within . We spread the analysis on the 12 systems to
alleviate the sample variance. We then interpreted the density fluctuations as
the result of either gas clumping or turbulence. For each cluster considered
individually, the normalisation of density fluctuations correlates positively
with the Zernike moment and centroid shift, but negatively with the
concentration and the Gini coefficient. The spectral index within and
evaluated over all clusters is consistent with a Kolmogorov cascade. The
normalisation of density fluctuations, when interpreted in terms of clumping,
is consistent within with the literature results and numerical
simulations; however, it is higher between 0.5 and . Conversely,
when interpreted on the basis of turbulence, we deduce a non-thermal pressure
profile that is lower than the predictions of the simulations within 0.5
, but still in agreement in the outer regions. We explain these
results by the presence of central structural residues that are remnants of the
dynamic assembly of the clusters.Comment: Accepted for publication in A&A. Abstract slightly abridged for arXi
Outskirts of Galaxy Clusters
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.Comment: 52 pages. Review paper. Accepted for publication in Space Science
Reviews (eds: S. Ettori, M. Meneghetti). This is a product of the work done
by an international team at the International Space Science Institute (ISSI)
in Bern on "Astrophysics and Cosmology with Galaxy Clusters: the X-ray and
Lensing View
Simulating the impact of dust cooling on the statistical properties of the intracluster medium
From the first stages of star and galaxy formation, non-gravitational
processes such as ram pressure stripping, SNs, galactic winds, AGNs,
galaxy-galaxy mergers, etc... lead to the enrichment of the IGM in stars,
metals as well as dust, via the ejection of galactic material into the IGM. We
know now that these processes shape, side by side with gravitation, the
formation and the evolution of structures. We present here hydrodynamic
simulations of structure formation implementing the effect of the cooling by
dust on large scale structure formation. We focus on the scale of galaxy
clusters and study the statistical properties of clusters. Here we present our
results on the and the scaling relations which exhibit changes
on both the slope and normalization when adding cooling by dust to the standard
radiative cooling model. For example, the normalization of the relation
changes only by a maximum of 2% at M whereas the
normalization of the changes by as much as 10% at keV for
models that including dust cooling. Our study shows that the dust is an added
non-gravitational process that contributes shaping the thermodynamical state of
the hot ICM gas.Comment: 11 pages, 4 figures, ASR in pres
New constraints on MOND from galaxy clusters
We revisit the application of Modified Newtonian Dynamics (MOND) to galaxy
clusters. We confront the high quality X-ray data for eight clusters of
galaxies observed by the \xmm satellite with the predictions of MOND. We obtain
a ratio of the MOND dynamical mass to the baryonic mass of in the outer parts (i.e ~ R), in the concordance
cosmological model where the predicted asymptotic ratio, if any baryons are
present, is (at ~ R). We confirm that
the MOND paradigm lowers the discrepancy between the binding mass and the
baryonic mass in clusters by a factor of at about half the virial
radius. However, at this radius about 80% of the mass is still missing, and as
pointed out by \citet{sanders03}, this necessitates a component of dark baryons
or neutrinos in the cluster core. Concerning the neutrino hypothesis,
application of the new data requires a minimum neutrino mass of eV to fill this gap. The corresponding 2 lower limit of
eV is marginally inconsistent with the current constraints from
the cluster number counts, and from the CMB and large scale structure data.
MOND must invoke neutrinos to represent the main component that account for the
missing mass problem in clusters.Comment: 5 pages, 1 figure, accepted for publication in MNRAS. A section on
the neutrino mass in the MOND framework was added to the discussio
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