86 research outputs found
Dynamics of Intracluster Gas and Bulk Motions in Clusters
In this paper I briefly discuss progress in recent lines of research on the internal dynamics of clusters of galaxies that have been made possible thanks to improvements in current e-ray spectrometers that enable them to perform detailed spatially resolved spectroscopy. In particular, I focus on the study of bulk motion in intracluster gas and the nature of features called cold fronts.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/73040/1/annals.1350.022.pd
Detecting Intracluster Gas Motion in Galaxy Clusters: Mock Astro-E2 Observations
We explore the detectability of bulk motions in the X-ray emitting
intracluster medium (ICM) using a catalog of 1,836 mock Astro-E2 observations
of simulated clusters of galaxies. We generate high resolution mock spectra for
two observing strategies: a four-pointing mosaic and a single central pointing.
Normalizing to 200 (400) photons in the iron K-alpha region for the mosaic
(central) study, we fit Poisson realizations of each simulated spectrum to a
velocity broadened isothermal plasma emission model. We confirm that the
velocity characteristics (mean and dispersion) returned by the spectral
fittings are unbiased measures of the emission-weighted values within the
observed region, with scatter 55 km/s. The maximum velocity difference between
mosaic element pairs has ~ 6% likelihood of being
transonic (), and the likelihood falls steeply,
p \spropto (\Delta v_{\rm max}/c_s)^{-4}, at high Mach number. The velocity
broadening parameter from the central pointing fit exceeds the
thermal value in 49% of the cases, with again a tail at large
dispersion. We present as case studies the clusters that yield the strongest
signal for each observing strategy.Comment: 13 pages, 20 figures. Submitted to ApJ. Version with postscript
figures embedded in the text available at
http://www.umich.edu/~apawl/astroe2/. Version 2 includes changes in response
to referee report and corrects an error in optical depth estimate
Cosmic Filaments in Superclusters
Large-scale structure calculations show that modest overdensity filaments
will connect clusters of galaxies and these filaments are reservoirs of
baryons, mainly in gaseous form. To determine whether such filaments exist, we
have examined the UV absorption line properties of three AGNs projected behind
possible filaments in superclusters of galaxies; the AGNs lie within 3 Mpc of
the centerlines of loci connecting clusters. All three lines of sight show
absorption in Ly\alpha, Ly\beta, or/and OVI at redshifts within about 1300 km/s
of the nearby galaxy clusters that would define the closest filaments. For one
AGN, the absorption line redshifts are close to the emission line redshift of
the AGN, so we cannot rule out self-absorption for this object. These
absorption line associations with superclusters are unlikely to have occurred
by chance, a result consistent with the presence of cosmic filaments within
superclusters.Comment: 16 pages, 7 eps figures, Accepted for publication in Ap
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