65,597 research outputs found
Chandra observations of the galaxy cluster Abell 1835
We present the analysis of 30 ksec of Chandra observations of the galaxy
cluster Abell 1835. Overall, the X-ray image shows a relaxed morphology,
although we detect substructure in in the inner 30 kpc radius. Spectral
analysis shows a steep drop in the X-ray gas temperature from ~12 keV in the
outer regions of the cluster to ~4 keV in the core. The Chandra data provide
tight constraints on the gravitational potential of the cluster which can be
parameterized by a Navarro, Frenk & White (1997) model. The X-ray data allow us
to measure the X-ray gas mass fraction as a function of radius, leading to a
determination of the cosmic matter density of \Omega_m=0.40+-0.09 h_50^-0.5.
The projected mass within a radius of ~150 kpc implied by the presence of
gravitationally lensed arcs in the cluster is in good agreement with the mass
models preferred by the Chandra data. We find a radiative cooling time of the
X-ray gas in the centre of Abell 1835 of about 3x10^8 yr. Cooling flow model
fits to the Chandra spectrum and a deprojection analysis of the Chandra image
both indicate the presence of a young cooling flow (~6x10^8 yr) with an
integrated mass deposition rate of 230^+80_-50 M_o yr^-1 within a radius of 30
kpc. We discuss the implications of our results in the light of recent RGS
observations of Abell 1835 with XMM-Newton.Comment: 15 pages, 15 figures, accepted by MNRA
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Cosmological constraints from the X-ray gas mass fraction in relaxed lensing clusters observed with Chandra
We present precise measurements of the X-ray gas mass fraction for a sample
of luminous, relatively relaxed clusters of galaxies observed with the Chandra
Observatory, for which independent confirmation of the mass results is
available from gravitational lensing studies. Parameterizing the total
(luminous plus dark matter) mass profiles using the model of Navarro, Frenk &
White (1997), we show that the X-ray gas mass fractions in the clusters
asymptote towards an approximately constant value at a radius r_2500, where the
mean interior density is 2500 times the critical density of the Universe at the
redshifts of the clusters. Combining the Chandra results on the X-ray gas mass
fraction and its apparent redshift dependence with recent measurements of the
mean baryonic matter density in the Universe and the Hubble Constant determined
from the Hubble Key Project, we obtain a tight constraint on the mean total
matter density of the Universe, Omega_m = 0.30^{+0.04}_{-0.03}, and measure a
positive cosmological constant, Omega_Lambda = 0.95^{+0.48}_{-0.72}. Our
results are in good agreement with recent, independent findings based on
analyses of anisotropies in the cosmic microwave background radiation, the
properties of distant supernovae, and the large-scale distribution of galaxies.Comment: Accepted for publication in MNRAS Letters (6 pages, 3 figures
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