2,371 research outputs found
Observational Tests of the Mass-Temperature Relation for Galaxy Clusters
We examine the relationship between the mass and x-ray gas temperature of
galaxy clusters using data drawn from the literature. Simple theoretical
arguments suggest that the mass of a cluster is related to the x-ray
temperature as . Virial theorem mass estimates based on
cluster galaxy velocity dispersions seem to be accurately described by this
scaling with a normalization consistent with that predicted by the simulations
of Evrard, Metzler, & Navarro (1996). X-ray mass estimates which employ
spatially resolved temperature profiles also follow a scaling
although with a normalization about 40% lower than that of the fit to the
virial masses. However, the isothermal -model and x-ray surface
brightness deprojection masses follow a steeper
scaling. The steepness of the isothermal estimates is due to their implicitly
assumed dark matter density profile of at large radii
while observations and simulations suggest that clusters follow steeper
profiles (e.g., ).Comment: 25 pages, 10 figures, accepted by Ap
Detection of the Entropy of the Intergalactic Medium: Accretion Shocks in Clusters, Adiabatic Cores in Groups
The thermodynamics of the diffuse, X-ray emitting gas in clusters of galaxies
is linked to the entropy level of the intra cluster medium. In particular,
models that successfully reproduce the properties of local X-ray clusters and
groups require the presence of a minimum value for the entropy in the center of
X-ray halos. Such a minimum entropy is most likely generated by
non-gravitational processes, in order to produce the observed break in
self-similarity of the scaling relations of X-ray halos. At present there is no
consensus on the level, the source or the time evolution of this excess
entropy. In this paper we describe a strategy to investigate the physics of the
heating processes acting in groups and clusters. We show that the best way to
extract information from the local data is the observation of the entropy
profile at large radii in nearby X-ray halos (z~0.1), both at the upper and
lower extremes of the cluster mass scale. The spatially and spectrally resolved
observation of such X-ray halos provides information on the mechanism of the
heating. We demonstrate how measurements of the size of constant entropy
(adiabatic) cores in clusters and groups can directly constrain heating models,
and the minimum entropy value. We also consider two specific experiments: the
detection of the shock fronts expected at the virial boundary of rich clusters,
and the detection of the isentropic, low surface-brightness emission extending
to radii larger than the virial ones in low mass clusters and groups. Such
observations will be a crucial probe of both the physics of clusters and the
relationship of non-gravitational processes to the thermodynamics of the
intergalactic medium.Comment: ApJ accepted, 31 pages including 8 figures. Important material added;
references update
HST/Acs Weak-Lensing and Chandra X-Ray Studies of the High-Redshift Cluster MS 1054-0321
We present Hubble Space Telescope/Advanced Camera for Surveys (ACS)
weak-lensing and Chandra X-ray analyses of MS 1054-0321 at z=0.83, the most
distant and X-ray luminous cluster in the Einstein Extended Medium-Sensitivity
Survey (EMSS). The high-resolution mass reconstruction through ACS weak-lensing
reveals the complicated dark matter substructure in unprecedented detail,
characterized by the three dominant mass clumps with the four or more minor
satellite groups within the current ACS field. The direct comparison of the
mass map with the Chandra X-ray image shows that the eastern weak-lensing
substructure is not present in the X-ray image and, more interestingly, the two
X-ray peaks are displaced away from the hypothesized merging direction with
respect to the corresponding central and western mass clumps, possibly because
of ram pressure. In addition, as observed in our previous weak-lensing study of
another high-redshift cluster CL 0152-1357 at z=0.84, the two dark matter
clumps of MS 1054-0321 seem to be offset from the galaxy counterparts. We
examine the significance of these offsets and discuss a possible scenario,
wherein the dark matter clumps might be moving ahead of the cluster galaxies.
The non-parametric weak-lensing mass modeling gives a projected mass of M(r<1
Mpc)=(1.02+-0.15)x 10^{15} solar mass, where the uncertainty reflects both the
statistical error and the cosmic shear effects. Our temperature measurement of
T=8.9_{-0.8}^{+1.0} keV utilizing the newest available low-energy quantum
efficiency degradation prescription for the Chandra instrument, together with
the isothermal beta description of the cluster (r_c=16"+-15" and
beta=0.78+-0.08), yields a projected mass of M(r<1 Mpc)=(1.2+-0.2) x 10^{15}
solar mass, consistent with the weak-lensing result.Comment: Accepted for publication in apj. Full-resolution version can be
downloaded from http://acs.pha.jhu.edu/~mkjee/ms1054.pd
The WARPS Survey: VI. Galaxy Cluster and Source Identifications from Phase I
We present in catalog form the optical identifications for objects from the
first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a
serendipitous survey of relatively deep, pointed ROSAT observations for
clusters of galaxies. The X-ray source detection algorithm used by WARPS is
Voronoi Tessellation and Percolation (VTP), a technique which is equally
sensitive to point sources and extended sources of low surface brightness.
WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an
area of 16.2 square degrees. We describe here the X-ray source screening and
optical identification process for WARPS-I, which yielded 34 clusters at
0.06<z<0.75. Twenty-two of these clusters form a complete, statistically well
defined sample drawn from 75 of these 86 fields, covering an area of 14.1
square degrees, with a flux limit of F (0.5-2.0 keV) = 6.5 \times 10^{-14} erg
cm^{-2} s^{-1}}. This sample can be used to study the properties and evolution
of the gas, galaxy and dark matter content of clusters, and to constrain
cosmological parameters. We compare in detail the identification process and
findings of WARPS to those from other recently published X-ray surveys for
clusters, including RDCS, SHARC-Bright, SHARC-south and the CfA 160 deg
survey.Comment: v3 reflects minor updates to tables 2 and
Delta-Function Bose Gas Picture of S=1 Antiferromagnetic Quantum Spin Chains Near Critical Fields
We study the zero-temperature magnetization curve (M-H curve) of the S=1
bilinear-biquadratic spin chain, whose Hamiltonian is given by 0 \leq \beta <1H_sH_cH_scH_c\beta\beta_c(\approx 0.41)0<\beta<\beta_cccM\sim \sqrt{H-H_c}\beta \to \beta_c-0M\sim (H-H_c)^{1/4}\beta_c<\beta <1c$ becomes negative.Comment: 6 pages, RevTeX, 8 ps figure
Cross-correlation between the soft X-ray background and SZ Sky
While both X-ray emission and Sunyaev-Zel'dovich (SZ) temperature
fluctuations are generated by the warm-hot gas in dark matter halos, the two
observables have different dependence on the underlying physical properties,
including the gas distribution. A cross-correlation between the soft X-ray
background (SXRB) and the SZ sky may allow an additional probe on the
distribution of warm-hot gas at intermediate angular scales and redshifts
complementing studies involving clustering within SXRB and SZ separately. Using
a halo approach, we investigate this cross-correlation analytically. The two
contributions are correlated mildly with a correlation coefficient of
, and this relatively low correlation presents a significant challenge
for its detection. The correlation, at small angular scales, is affected by the
presence of radiative cooling or preheating and provides a probe on the thermal
history of the hot gas in dark halos. While the correlation remains
undetectable with CMB data from the WMAP satellite and X-ray background data
from existing catalogs, upcoming observations with CMB missions such as Planck,
for the SZ side, and an improved X-ray map of the large scale structure, such
as the one planned with DUET mission, may provide a first opportunity for a
reliable detection of this cross-correlation.Comment: 8 pages, 6 figures, accepted for publication in A&
DANSR: A tool for the detection of annotated and novel small RNAs
Existing small noncoding RNA analysis tools are optimized for processing short sequencing reads (17-35 nucleotides) to monitor microRNA expression. However, these strategies under-represent many biologically relevant classes of small noncoding RNAs in the 36-200 nucleotides length range (tRNAs, snoRNAs, etc.). To address this, we developed DANSR, a tool for the detection of annotated and novel small RNAs using sequencing reads with variable lengths (ranging from 17-200 nt). While DANSR is broadly applicable to any small RNA dataset, we applied it to a cohort of matched normal, primary, and distant metastatic colorectal cancer specimens to demonstrate its ability to quantify annotated small RNAs, discover novel genes, and calculate differential expression. DANSR is available as an open source tool
Probing the cosmic web: inter-cluster filament detection using gravitational lensing
The problem of detecting dark matter filaments in the cosmic web is
considered. Weak lensing is an ideal probe of dark matter, and therefore forms
the basis of particularly promising detection methods. We consider and develop
a number of weak lensing techniques that could be used to detect filaments in
individual or stacked cluster fields, and apply them to synthetic lensing data
sets in the fields of clusters from the Millennium Simulation. These techniques
are multipole moments of the shear and convergence, mass reconstruction, and
parameterized fits to filament mass profiles using a Markov Chain Monte Carlo
approach. In particular, two new filament detection techniques are explored
(multipole shear filters and Markov Chain Monte Carlo mass profile fits), and
we outline the quality of data required to be able to identify and quantify
filament profiles. We also consider the effects of large scale structure on
filament detection. We conclude that using these techniques, there will be
realistic prospects of detecting filaments in data from future space-based
missions. The methods presented in this paper will be of great use in the
identification of dark matter filaments in future surveys.Comment: 12 pages, 4 figures, MNRAS accepted, (replacement due to corrupted
end of pdf file
Measuring our universe from galaxy redshift surveys
Galaxy redshift surveys have achieved significant progress over the last
couple of decades. Those surveys tell us in the most straightforward way what
our local universe looks like. While the galaxy distribution traces the bright
side of the universe, detailed quantitative analyses of the data have even
revealed the dark side of the universe dominated by non-baryonic dark matter as
well as more mysterious dark energy (or Einstein's cosmological constant). We
describe several methodologies of using galaxy redshift surveys as cosmological
probes, and then summarize the recent results from the existing surveys.
Finally we present our views on the future of redshift surveys in the era of
Precision Cosmology.Comment: 82 pages, 31 figures, invited review article published in Living
Reviews in Relativity, http://www.livingreviews.org/lrr-2004-
The dynamical state of the Coma cluster with XMM-Newton
We present in this paper a substructure and spectroimaging study of the Coma
cluster of galaxies based on XMM-Newton data. XMM-Newton performed a mosaic of
observations of Coma to ensure a large coverage of the cluster. We add the
different pointings together and fit elliptical beta-models to the data. We
subtract the cluster models from the data and look for residuals, which can be
interpreted as substructure. We find several significant structures: the
well-known subgroup connected to NGC4839 in the South-West of the cluster, and
another substructure located between NGC 4839 and the centre of the Coma
cluster. Constructing a hardness ratio image, which can be used as a
temperature map we see that in front of this new structure the temperature is
significantly increased (higher or equal 10 keV). We interpret this temperature
enhancement as the result of heating as this structure falls onto the Coma
cluster. We furthermore reconfirm the filament-like structure South-East of the
cluster centre. This region is significantly cooler than the mean cluster
temperature. We estimate the temperature of this structure to be equal or below
1keV. A possible scenario to explain the observed features is stripping caused
by the infall of a small group of galaxies located around the two galaxies
NGC4921 and NGC4911 into the Coma cluster with a non-zero impact parameter. We
also see significant X-ray depressions North and South-East of NGC4921, which
might either be linked to tidal forces due to the merger with the Western
structure or connected to an older cluster merger.Comment: 12 pages, 4 figures accepted for publication in A&
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