828 research outputs found
Probing the dark matter profile of hot clusters and the M-T relation with XMM-Newton
We present results based on XMM-Newton observations of a small sample of hot
galaxy clusters. Making a full use of XMM-Newton's spectro-imaging
capabilities, we have extracted the radial temperature profile and gas density
profile, and with this information, calculated the total mass profile of each
cluster (under the assumption of hydrostatic equilibrium and spherical
symmetry). Comparing the individual scaled total mass profiles, we have probed
the Universality of rich cluster mass profiles over a wide range of radii (from
0.01 to 0.7 the virial radius). We have also tested the shape of cluster mass
profiles by comparing with the predicted profiles from numerical simulations of
hierarchical structure formation. We also derived the local mass-temperature
(M-T) scaling relation over a range of temperature going from 4 to 9 keV, that
we compare with theoretical predictions.Comment: 7 pages, 2 figures, Advances in Space Research in press (proceedings
of the COSPAR 2004 Assembly, Paris
Distances and Cosmology From Galaxy Cluster CMB Data
The measurement of angular diameter distance to galaxy clusters, through
combined Sunyaev-Zel'dovich (SZ) effect data with X-ray emission observations,
is now a well-known probe of cosmology. Using a combination of SZ data and a
map of the lensed CMB anisotropies by the galaxy cluster potential, we propose
an alternative geometric technique to measure distance information primarily
through cluster related multi-frequency CMB measurements. We discuss necessary
requirements to implement this measurement, potential errors including
systematic biases, and the extent to which cosmological parameters can be
extracted. While individual cluster distances are not likely to be precise,
with upcoming subarcminute resolution wide-area CMB observations, useful
information on certain cosmological parameters, such as the equation of state
of dark energy, can be obtained from a large sample of galaxy clusters.Comment: 4 pages, 2 figure
Calibration of the galaxy cluster M_500-Y_X relation with XMM-Newton
The quantity Y_ X, the product of the X-ray temperature T_ X and gas mass M_
g, has recently been proposed as a robust low-scatter mass indicator for galaxy
clusters. Using precise measurements from XMM-Newton data of a sample of 10
relaxed nearby clusters, spanning a Y_ X range of 10^13 -10^15 M_sun keV, we
investigate the M_500-Y_ X relation. The M_500 - Y_ X data exhibit a power law
relation with slope alpha=0.548 \pm 0.027, close to the self-similar value
(3/5) and independent of the mass range considered. However, the normalisation
is \sim 20% below the prediction from numerical simulations including cooling
and galaxy feedback. We discuss two effects that could contribute to the
normalisation offset: an underestimate of the true mass due to the HE
assumption used in X-ray mass estimates, and an underestimate of the hot gas
mass fraction in the simulations. A comparison of the functional form and
scatter of the relations between various observables and the mass suggest that
Y_ X may indeed be a better mass proxy than T_ X or M_g,500.Comment: 4 pages, 2 figures, accepted for publication in A&
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
Discovery of diffuse radio emission at the center of the most X-ray-luminous cluster RX J1347.5-1145
We report on new VLA radio observations of the distant cluster RX
J1347.5-1145, which is the most luminous in X-rays. We aim at investigating the
possible presence of diffuse and extended radio emission in this very peculiar
system which shows both a massive cooling flow and merging signatures. New low
resolution (~18 arcsec) VLA radio observations of this cluster are combined
with higher resolution (~2 arcsec) data available in the VLA archive. We
discover the presence of a diffuse and extended (~500 kpc) radio source
centered on the cluster, unrelated to the radio emission of the central AGN.
The properties of the radio source, in particular a) its occurrence at the
center of a massive cooling flow cluster, b) its total size comparable to that
of the cooling region, c) its agreement with the observational trend between
radio luminosity and cooling flow power, indicate that RX J1347.5-1145 hosts a
radio mini-halo. We suggest that the radio emission of this mini-halo, which is
the most distant object of its class discovered up to now, is due to electron
re-acceleration triggered by the central cooling flow. However, we also note
that the morphology of the diffuse radio emission shows an elongation
coincident with the position of a hot subclump detected in X-rays, thus
suggesting that additional energy for the electron re-acceleration might be
provided by the submerger event.Comment: 5 pages, 6 figures, accepted for publication in A&A Letter
Scaling relations for galaxy clusters: properties and evolution
Well-calibrated scaling relations between the observable properties and the
total masses of clusters of galaxies are important for understanding the
physical processes that give rise to these relations. They are also a critical
ingredient for studies that aim to constrain cosmological parameters using
galaxy clusters. For this reason much effort has been spent during the last
decade to better understand and interpret relations of the properties of the
intra-cluster medium. Improved X-ray data have expanded the mass range down to
galaxy groups, whereas SZ surveys have openened a new observational window on
the intracluster medium. In addition,continued progress in the performance of
cosmological simulations has allowed a better understanding of the physical
processes and selection effects affecting the observed scaling relations. Here
we review the recent literature on various scaling relations, focussing on the
latest observational measurements and the progress in our understanding of the
deviations from self similarity.Comment: 38 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
Weak Lensing of Galaxy Clusters in MOND
We study weak gravitational lensing of galaxy clusters in terms of the MOND
(MOdified Newtonian Dynamics) theory. We calculate shears and convergences of
background galaxies for three clusters (A1689, CL0024+1654, CL1358+6245) and
the mean profile of 42 SDSS (Sloan Digital Sky Survey) clusters and compare
them with observational data. The mass profile is modeled as a sum of X-ray
gas, galaxies and dark halo. For the shear as a function of the angular radius,
MOND predicts a shallower slope than the data irrespective of the critical
acceleration parameter . The dark halo is necessary to explain the data
for any and for three interpolation functions. If the dark halo is
composed of massive neutrinos, its mass should be heavier than 2 eV. However
the constraint still depends on the dark halo model and there are systematic
uncertainties, and hence the more careful study is necessary to put a stringent
constraint.Comment: 12 pages, 7 figures, references added, minor changes, accepted for
publication in Ap
The hot gas content of fossil galaxy clusters
We investigate the properties of the hot gas in four fossil galaxy systems
detected at high significance in the Planck Sunyaev-Zeldovich (SZ) survey.
XMM-Newton observations reveal overall temperatures of kT ~ 5-6 keV and yield
hydrostatic masses M500,HE > 3.5 x 10e14 Msun, confirming their nature as bona
fide massive clusters. We measure the thermodynamic properties of the hot gas
in X-rays (out to beyond R500 in three cases) and derive their individual
pressure profiles out to R ~ 2.5 R500 with the SZ data. We combine the X-ray
and SZ data to measure hydrostatic mass profiles and to examine the hot gas
content and its radial distribution. The average Navarro-Frenk-White (NFW)
concentration parameter, c500 = 3.2 +/- 0.4, is the same as that of relaxed
`normal' clusters. The gas mass fraction profiles exhibit striking variation in
the inner regions, but converge to approximately the cosmic baryon fraction
(corrected for depletion) at R500. Beyond R500 the gas mass fraction profiles
again diverge, which we interpret as being due to a difference in gas clumping
and/or a breakdown of hydrostatic equilibrium in the external regions. Overall
our observations point to considerable radial variation in the hot gas content
and in the gas clumping and/or hydrostatic equilibrium properties in these
fossil clusters, at odds with the interpretation of their being old, evolved
and undisturbed. At least some fossil objects appear to be dynamically young.Comment: 4 pages, 2 figures. Accepted for publication in A&
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