1,005 research outputs found
The Observable Thermal and Kinetic Sunyaev-Zel'dovich Effect in Merging Galaxy Clusters
The advent of high-resolution imaging of galaxy clusters using the
Sunyaev-Zel'dovich Effect (SZE) provides a unique probe of the astrophysics of
the intracluster medium (ICM) out to high redshifts. To investigate the effects
of cluster mergers on resolved SZE images, we present a high-resolution
cosmological simulation of a 1.5E15 M_sun adiabatic cluster using the TreeSPH
code ChaNGa. This massive cluster undergoes a 10:3:1 ratio triple merger
accompanied by a dramatic rise in its integrated Compton-Y, peaking at z =
0.05. By modeling the thermal SZE (tSZ) and kinetic SZE (kSZ) spectral
distortions of the Cosmic Microwave Background (CMB) at this redshift with
relativistic corrections, we produce various mock images of the cluster at
frequencies and resolutions achievable with current high-resolution SZE
instruments. The two gravitationally-bound merging subclusters account for 10%
and 1% of the main cluster's integrated Compton-Y, and have extended merger
shock features in the background ICM visible in our mock images. We show that
along certain projections and at specific frequencies, the kSZ CMB intensity
distortion can dominate over the tSZ due to the large line of sight velocities
of the subcluster gas and the unique frequency-dependence of these effects. We
estimate that a one-velocity assumption in estimation of line of sight
velocities of the merging subclusters from the kSZ induces a bias of ~10%. This
velocity bias is small relative to other sources of uncertainty in
observations, partially due to helpful bulk motions in the background ICM
induced by the merger. Our results show that high-resolution SZE observations,
which have recently detected strong kSZ signals in subclusters of merging
systems, can robustly probe the dynamical as well as the thermal state of the
ICM.Comment: MNRAS, accepted. 13 pages, 9 figure
Physics with Identified Particles at STAR
New physics results with identified particles at STAR are presented.
Measurements at low address bulk properties of the collision, while those
at high address jet energy loss in the bulk matter produced. Between
these extremes, measurements at intermediate address the interplay
between jets and the bulk. We highlight: measurements of fluctuations as
a new, sensitive probe of the initial conditions and the equation of state;
correlations involving multi-strange particles, along with ratios of identified
particles to test coalescence as a mechanism of particle production at
intermediate ; three particle azimuthal correlation to search for conical
emission; and the energy and particle-type dependence of hadron production at
high to study quark and gluon jet energy loss.Comment: 9 pages, 7 figures. To appear in the proceedings of the 19th
International Conference on Ultra-Relativistic Nucleus-Nucleus Collisions
(Quark Matter 2006), Shanghai, China, November 14-20, 200
and production from Au+Au collisions at GeV
The preliminary results of and spectra are
reported from Au+Au collisions at GeV. Particle
identification is from the Time Projection Chamber and Time-of-Flight system at
STAR. The nuclear modification factor for mesons () and baryons () will also be discussed.Comment: 5 pages, 4 figures, Contributed to 8th International Conference on
Strangeness in Quark Matter (SQM 2004),to be published in Journal of Physics
SDSSJ14584479+3720215: A Benchmark JHK Blazar Light Curve from the 2MASS Calibration Scans
Active galactic nuclei (AGNs) are well-known to exhibit flux variability
across a wide range of wavelength regimes, but the precise origin of the
variability at different wavelengths remains unclear. To investigate the
relatively unexplored near-IR variability of the most luminous AGNs, we conduct
a search for variability using well sampled JHKs-band light curves from the
2MASS survey calibration fields. Our sample includes 27 known quasars with an
average of 924 epochs of observation over three years, as well as one
spectroscopically confirmed blazar (SDSSJ14584479+3720215) with 1972 epochs of
data. This is the best-sampled NIR photometric blazar light curve to date, and
it exhibits correlated, stochastic variability that we characterize with
continuous auto-regressive moving average (CARMA) models. None of the other 26
known quasars had detectable variability in the 2MASS bands above the
photometric uncertainty. A blind search of the 2MASS calibration field light
curves for AGN candidates based on fitting CARMA(1,0) models (damped-random
walk) uncovered only 7 candidates. All 7 were young stellar objects within the
{\rho} Ophiuchus star forming region, five with previous X-ray detections. A
significant {\gamma}-ray detection (5{\sigma}) for the known blazar using 4.5
years of Fermi photon data is also found. We suggest that strong NIR
variability of blazars, such as seen for SDSSJ14584479+3720215, can be used as
an efficient method of identifying previously-unidentified {\gamma}-ray
blazars, with low contamination from other AGN.Comment: 6 pages, 3 figures, ApJ Accepte
Signatures of Massive Black Hole Merger Host Galaxies from Cosmological Simulations I: Unique Galaxy Morphologies in Imaging
Low-frequency gravitational wave experiments such as the Laser Interferometer
Space Antenna and pulsar timing arrays are expected to detect individual
massive black hole (MBH) binaries and mergers. However, secure methods of
identifying the exact host galaxy of each MBH merger amongst the large number
of galaxies in the gravitational wave localization region are currently
lacking. We investigate the distinct morphological signatures of MBH merger
host galaxies, using the Romulus25 cosmological simulation. We produce mock
telescope images of 201 simulated galaxies in Romulus25 hosting recent MBH
mergers, through stellar population synthesis and dust radiative transfer.
Based on comparisons to mass- and redshift-matched control samples, we show
that combining multiple morphological statistics via a linear discriminant
analysis enables identification of the host galaxies of MBH mergers, with
accuracies that increase with chirp mass and mass ratio. For mergers with high
chirp masses (>10^8.2 Msun) and high mass ratios (>0.5), the accuracy of this
approach reaches >80%, and does not decline for at least >1 Gyr after numerical
merger. We argue that these trends arise because the most distinctive
morphological characteristics of MBH merger and binary host galaxies are
prominent classical bulges, rather than relatively short-lived morphological
disturbances from their preceding galaxy mergers. Since these bulges are formed
though major mergers of massive galaxies, they lead to (and become permanent
signposts for) MBH binaries and mergers that have high chirp masses and mass
ratios. Our results suggest that galaxy morphology can aid in identifying the
host galaxies of future MBH binaries and mergers.Comment: 19 pages, 10 figures. Submitted to Ap
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