1,056 research outputs found
Chandra Measurements of a Complete Sample of X-ray Luminous Galaxy Clusters: The Luminosity-Mass Relation
We present the results of work involving a statistically complete sample of
34 galaxy clusters, in the redshift range 0.15z0.3 observed with
. We investigate the luminosity-mass () relation for the cluster
sample, with the masses obtained via a full hydrostatic mass analysis. We
utilise a method to fully account for selection biases when modeling the
relation, and find that the relation is significantly different than the
relation modelled when not account for selection effects. We find that the
luminosity of our clusters is 2.20.4 times higher (when accounting for
selection effects) than the average for a given mass, its mass is 30% lower
than the population average for a given luminosity. Equivalently, using the
relation measured from this sample without correcting for selection biases
would lead to the underestimation by 40% of the average mass of a cluster with
a given luminosity. Comparing the hydrostatic masses to mass estimates
determined from the parameter, we find that they are entirely
consistent, irrespective of the dynamical state of the cluster.Comment: 31 pages, 43 figures, accepted for publication in MNRA
Weak Lensing Mass Reconstruction of the Galaxy Cluster Abell 209
Weak lensing applied to deep optical images of clusters of galaxies provides
a powerful tool to reconstruct the distribution of the gravitating mass
associated to these structures. We use the shear signal extracted by an
analysis of deep exposures of a region centered around the galaxy cluster Abell
209, at redshift z=0.2, to derive both a map of the projected mass distribution
and an estimate of the total mass within a characteristic radius. We use a
series of deep archival R-band images from CFHT-12k, covering an area of 0.3
deg^2. We determine the shear of background galaxy images using a new
implementation of the modified Kaiser-Squires-Broadhurst pipeline for shear
determination, which we has been tested against the ``Shear TEsting Program 1
and 2'' simulations. We use mass aperture statistics to produce maps of the 2
dimensional density distribution, and parametric fits using both
Navarro-Frenk-White (NFW) and singular-isothermal-sphere profiles to constrain
the total mass. The projected mass distribution shows a pronounced asymmetry,
with an elongated structure extending from the SE to the NW. This is in general
agreement with the optical distribution previously found by other authors. A
similar elongation was previously detected in the X-ray emission map, and in
the distribution of galaxy colours. The circular NFW mass profile fit gives a
total mass of M_{200} = 7.7^{+4.3}_{-2.7} 10^{14} solar masses inside the
virial radius r_{200} = 1.8\pm 0.3 Mpc. The weak lensing profile reinforces the
evidence for an elongated structure of Abell 209, as previously suggested by
studies of the galaxy distribution and velocities.Comment: accepted by A&A, 15 pages, 11 figure
Lost dynamics and the dynamics of loss: Longitudinal compression of brain signal variability is coupled with declines in functional integration and cognitive performance
Spatially Resolved Outflows in a Seyfert Galaxy at z = 2.39
We present the first spatially resolved analysis of rest-frame optical and UV
imaging and spectroscopy for a lensed galaxy at z = 2.39 hosting a Seyfert
active galactic nucleus (AGN). Proximity to a natural guide star has enabled
high signal-to-noise VLT SINFONI + adaptive optics observations of rest-frame
optical diagnostic emission lines, which exhibit an underlying broad component
with FWHM ~ 700 km/s in both the Balmer and forbidden lines. Measured line
ratios place the outflow robustly in the region of the ionization diagnostic
diagrams associated with AGN. This unique opportunity - combining gravitational
lensing, AO guiding, redshift, and AGN activity - allows for a magnified view
of two main tracers of the physical conditions and structure of the
interstellar medium in a star-forming galaxy hosting a weak AGN at cosmic noon.
By analyzing the spatial extent and morphology of the Ly-alpha and
dust-corrected H-alpha emission, disentangling the effects of star formation
and AGN ionization on each tracer, and comparing the AGN induced mass outflow
rate to the host star formation rate, we find that the AGN does not
significantly impact the star formation within its host galaxy.Comment: 16 pages, 5 figures, accepted for publication in Ap
A Thirty Kiloparsec Chain of "Beads on a String" Star Formation Between Two Merging Early Type Galaxies in the Core of a Strong-Lensing Galaxy Cluster
New Hubble Space Telescope ultraviolet and optical imaging of the
strong-lensing galaxy cluster SDSS J1531+3414 (z=0.335) reveals two centrally
dominant elliptical galaxies participating in an ongoing major merger. The
interaction is at least somewhat rich in cool gas, as the merger is associated
with a complex network of nineteen massive superclusters of young stars (or
small tidal dwarf galaxies) separated by ~1 kpc in projection from one another,
combining to an estimated total star formation rate of ~5 solar masses per
year. The resolved young stellar superclusters are threaded by narrow H-alpha,
[O II], and blue excess filaments arranged in a network spanning ~27 kpc across
the two merging galaxies. This morphology is strongly reminiscent of the
well-known "beads on a string" mode of star formation observed on kpc-scales in
the arms of spiral galaxies, resonance rings, and in tidal tails between
interacting galaxies. Nevertheless, the arrangement of this star formation
relative to the nuclei of the two galaxies is difficult to interpret in a
dynamical sense, as no known "beads on a string" systems associated with
kpc-scale tidal interactions exhibit such lopsided morphology relative to the
merger participants. In this Letter we present the images and follow-up
spectroscopy, and discuss possible physical interpretations for the unique
arrangement of the young stellar clusters. While we suggest that this
morphology is likely to be dynamically short-lived, a more quantitative
understanding awaits necessary multiwavelength follow-up, including optical
integral field spectroscopy, ALMA sub-mm interferometry, and Chandra X-ray
imaging.Comment: 7 pages, 4 figures, accepted for publication in ApJ Letters. High
resolution images of the cluster can be found at
http://hubblesite.org/news/2014/2
Using quality mapping to predict spatial variation in local properties and component performance in Mg alloy thin-walled high-pressure die castings: an ICME approach and case study
Weak Gravitational Lensing by a Sample of X-Ray Luminous Clusters of Galaxies -- II. Comparison with Virial Masses
Dynamic velocity dispersion and mass estimates are given for a sample of five
X-ray luminous rich clusters of galaxies at intermediate redshifts (z~0.3)
drawn from a sample of 39 clusters for which we have obtained gravitational
lens mass estimates. The velocity dispersions are determined from between 9 and
20 redshifts measured with the LDSS spectrograph of the William Herschel
Telescope, and virial radii are determined from imaging using the UH8K mosaic
CCD camera on the University of Hawaii 2.24m telescope.
Including clusters with velocity dispersions taken from the literature, we
have velocity dispersion estimates for 12 clusters in our gravitational lensing
sample. For this sample we compare the dynamical velocity dispersion estimates
with our estimates of the velocity dispersions made from gravitational lensing
by fitting a singular isothermal sphere profile to the observed tangential weak
lensing distortion as a function of radius. In all but two clusters, we find a
good agreement between the velocity dispersion estimates based on spectroscopy
and on weak lensing.Comment: 9 pages, 4 figures, accepted for publication in ApJ. Version in
emulateapj format with only minor change
Regional brain changes in aging healthy adults : General trends, individual differences and modifiers
Soluble urokinase plasminogen activator receptor (suPAR) levels predict damage accrual in patients with recent-onset systemic lupus erythematosus
© 2019 The Authors Objective: The soluble urokinase plasminogen activator receptor (suPAR) has potential as a prognosis and severity biomarker in several inflammatory and infectious diseases. In a previous cross-sectional study, suPAR levels were shown to reflect damage accrual in cases of systemic lupus erythematosus (SLE). Herein, we evaluated suPAR as a predictor of future organ damage in recent-onset SLE. Methods: Included were 344 patients from the Systemic Lupus International Collaborating Clinics (SLICC) Inception Cohort who met the 1997 American College of Rheumatology classification criteria with 5-years of follow-up data available. Baseline sera from patients and age- and sex-matched controls were assayed for suPAR. Organ damage was assessed annually using the SLICC/ACR damage index (SDI). Results: The levels of suPAR were higher in patients who accrued damage, particularly those with SDI≥2 at 5 years (N = 32, 46.8% increase, p = 0.004), as compared to patients without damage. Logistic regression analysis revealed a significant impact of suPAR on SDI outcome (SDI≥2; OR = 1.14; 95% CI 1.03–1.26), also after adjustment for confounding factors. In an optimized logistic regression to predict damage, suPAR persisted as a predictor, together with baseline disease activity (SLEDAI-2K), age, and non-Caucasian ethnicity (model AUC = 0.77). Dissecting SDI into organ systems revealed higher suPAR levels in patients who developed musculoskeletal damage (SDI≥1; p = 0.007). Conclusion: Prognostic biomarkers identify patients who are at risk of acquiring early damage and therefore need careful observation and targeted treatment strategies. Overall, suPAR constitutes an interesting biomarker for patient stratification and for identifying SLE patients who are at risk of acquiring organ damage during the first 5 years of disease
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