74 research outputs found
The Chandra ACIS Survey of M33 (ChASeM33): Transient X-ray Sources Discovered in M33
The Chandra ACIS Survey of M33 (ChASeM33) has acquired 7 fields of ACIS data
covering M33 with 200 ks of exposure in each field. A catalog from the first 10
months of data, along with archival Chandra observations dating back to the
year 2000, is currently available. We have searched these data for transient
sources that are measured to have a 0.35-8.0 keV unabsorbed luminosity of at
least 4 erg s in one epoch and are not detected in
another epoch. This set of the survey data has yielded seven such sources,
including one previously-known supersoft source. We analyzed XMM-Newton data
from the archive distributed over the years 2000 to 2003 to search for
recurrent outbursts and to get a spectrum for the supersoft transient. We find
only one recurrent transient in our sample. The X-ray spectra, light curves,
and optical counterpart candidates of two of the other sources suggest that
they are high-mass X-ray binaries. Archival Spitzer photometry and high X-ray
absorption suggest that one of the sources is a highly variable background
active galactic nucleus. The other three sources are more difficult to
classify. The bright transient population of M33 appears to contain a large
fraction of high-mass X-ray binaries compared with the transient populations of
M31 and the Galaxy, reflecting the later morphology of M33.Comment: 33 pages, 2 tables, 10 figures, accepted for publication in Ap
SXP214, an X-ray Pulsar in the Small Magellanic Cloud, Crossing the Circumstellar Disk of the Companion
Located in the Small Magellanic Cloud (SMC), SXP214 is an X-ray pulsar in a
high mass X-ray binary system with a Be-star companion. A recent survey of the
SMC under a Chandra X-ray Visionary program found the source in a transition
when the X-ray flux was on a steady rise. The Lomb-Scargle periodogram revealed
a pulse period of 211.49 +/- 0.42 s, which is significantly (>5sigma) shorter
than the previous measurements with XMM-Newton and RXTE. This implies that the
system has gone through sudden spin-up episodes recently. The pulse profile
shows a sharp eclipse-like feature with a modulation amplitude of >95%. The
linear rise of the observed X-ray luminosity from <~2x to 7x10^35 erg s^-1 is
correlated with steady softening of the X-ray spectrum, which can be described
by the changes in the local absorption from N_H ~ 10^24 to <~10^20 cm^-2 for an
absorbed power-law model. The soft X-ray emission below 2 keV was absent in the
early part of the observation when only the pulsating hard X-ray component was
observed, whereas at later times both soft and hard X-ray components were
observed pulsating. A likely explanation is that the neutron star was initially
hidden in the circumstellar disk of the companion, and later came out of the
disk with the accreted material that continued fueling the observed pulsation.Comment: 8 pages, 4 figures, 1 table, accepted for publication in Ap
A Deep XMM-Newton Survey of M33: Point Source Catalog, Source Detection and Characterization of Overlapping Fields
We have obtained a deep 8-field XMM-Newton mosaic of M33 covering the galaxy
out to the D isophote and beyond to a limiting 0.2--4.5 keV unabsorbed
flux of 510 erg cm s (L410
erg s at the distance of M33). These data allow complete coverage of the
galaxy with high sensitivity to soft sources such as diffuse hot gas and
supernova remnants. Here we describe the methods we used to identify and
characterize 1296 point sources in the 8 fields. We compare our resulting
source catalog to the literature, note variable sources, construct hardness
ratios, classify soft sources, analyze the source density profile, and measure
the X-ray luminosity function. As a result of the large effective area of
XMM-Newton below 1 keV, the survey contains many new soft X-ray sources. The
radial source density profile and X-ray luminosity function for the sources
suggests that only 15% of the 391 bright sources with
L3.610 erg s are likely to be associated with M33,
and more than a third of these are known supernova remnants. The log(N)--log(S)
distribution, when corrected for background contamination, is a relatively flat
power-law with a differential index of 1.5, which suggests many of the other
M33 sources may be high-mass X-ray binaries. Finally, we note the discovery of
an interesting new transient X-ray source, which we are unable to classify.Comment: 26 pages, 6 tables, 13 figures, accepted for publication in ApJ
Chandra ACIS Survey of M33 (ChASeM33): X-ray Imaging Spectroscopy of M33SNR21, the Brightest X-ray Supernova Remnant in M33
We present and interpret new X-ray data for M33SNR21, the brightest X-ray
supernova remnant (SNR) in M33. The SNR is in seen projection against (and
appears to be interacting with) the bright HII region NGC592. Data for this
source were obtained as part of the Chandra ACIS Survey of M33 (ChASeM33) Very
Large Project. The nearly on-axis Chandra data resolve the SNR into a ~5"
diameter (20 pc at our assumed M33 distance of 817+/-58 kpc) slightly
elliptical shell. The shell is brighter in the east, which suggests that it is
encountering higher density material in that direction. The optical emission is
coextensive with the X-ray shell in the north, but extends well beyond the
X-ray rim in the southwest. Modeling the X-ray spectrum with an absorbed sedov
model yields a shock temperature of 0.46(+0.01,-0.02) keV, an ionization
timescale of n_e t = cm s, and
half-solar abundances (0.45 (+0.12, -0.09)). Assuming Sedov dynamics gives an
average preshock H density of 1.7 +/- 0.3 cm. The dynamical age estimate
is 6500 +/- 600 yr, while the best fit value and derived gives
8200 +/- 1700 yr; the weighted mean of the age estimates is 7600 +/- 600 yr. We
estimate an X-ray luminosity (0.25-4.5 keV) of (1.2 +/- 0.2) times
ergs s (absorbed), and (1.7 +/- 0.3) times ergs s
(unabsorbed), in good agreement with the recent XMM-Newton determination. No
significant excess hard emission was detected; the luminosity ergs s (2-8 keV) for any hard point source.Comment: 27 pages, 6 figures (3 color). ApJ (in press
Serum proteins and paraproteins in women with silicone implants and connective tissue disease: a case–control study
Prior studies have suggested abnormalities of serum proteins, including paraproteins, in women with silicone implants but did not control for the presence of connective-tissue disease (CTD). This retrospective case–control study, performed in tertiary-care academic centers, assessed possible alterations of serum proteins, including paraproteins, in such a population. Seventy-four women with silicone implants who subsequently developed CTD, and 74 age-matched and CTD-matched women without silicone implants, were assessed in the primary study; other groups were used for additional comparisons. Routine serum protein determinations and high-sensitivity protein electrophoresis and immunofixation electrophoresis were performed for detection of paraproteins. Women with silicone implants, either with or without CTD, had significantly lower serum total protein and α1-globulin, α2-globulin, β-globulin, γ-globulin, and IgG levels compared with those without silicone implants. There was no significant difference, however, in the frequency of paraproteinemia between women with silicone implants and CTD (9.5%) and age-matched and CTD-matched women without silicone implants (5.4%) (odds ratio, 1.82; 95% confidence interval, 0.51–6.45). Paraprotein isotypes were similar in the two groups, and the clinical characteristics of the 13 women with paraproteinemia were comparable with an independent population of 10 women with silicone breast implants, CTD, and previously diagnosed monoclonal gammopathies. In summary, this first comprehensive study of serum proteins in women with silicone implants and CTD found no substantially increased risk of monoclonal gammopathy. Women with silicone implants, however, had unexpectedly low serum globulin and immunoglobulin levels, with or without the subsequent development of CTD. The causes and clinical implications of these findings require further investigation
Chandra ACIS Survey of M33 (ChASeM33): The enigmatic X-ray emission from IC131
We present the first X-ray analysis of the diffuse hot ionized gas and the
point sources in IC131, after NGC604 the second most X-ray luminous giant HII
region in M33. The X-ray emission is detected only in the south eastern part of
IC131 (named IC131-se) and is limited to an elliptical region of ~200pc in
extent. This region appears to be confined towards the west by a hemispherical
shell of warm ionized gas and only fills about half that volume. Although the
corresponding X-ray spectrum has 1215 counts, it cannot conclusively be told
whether the extended X-ray emission is thermal, non-thermal, or a combination
of both. A thermal plasma model of kT_e=4.3keV or a single power law of
Gamma=2.1 fit the spectrum equally well. If the spectrum is purely thermal
(non-thermal), the total unabsorbed X-ray luminosity in the 0.35-8keV energy
band amounts to L_X = 6.8(8.7)x10^35erg/s. Among other known HII regions
IC131-se seems to be extreme regarding the combination of its large extent of
the X-ray plasma, the lack of massive O stars, its unusually high electron
temperature (if thermal), and the large fraction of L_X emitted above 2keV
(~40-53%). A thermal plasma of ~4keV poses serious challenges to theoretical
models, as it is not clear how high electron temperatures can be produced in
HII regions in view of mass-proportional and collisionless heating. If the gas
is non-thermal or has non-thermal contributions, synchrotron emission would
clearly dominate over inverse Compton emission. It is not clear if the same
mechanisms which create non-thermal X-rays or accelerate CRs in SNRs can be
applied to much larger scales of 200pc. In both cases the existing theoretical
models for giant HII regions and superbubbles do not explain the hardness and
extent of the X-ray emission in IC131-se.Comment: 28 pages, 7 figures and 2 tables. Accepted for publication in ApJ.
For a high resolution version of the paper see
http://hea-www.harvard.edu/vlp_m33_public/publications.htm
Chandra ACIS Survey of M33 (ChASeM33): A First Look
We present an overview of the Chandra ACIS Survey of M33 (ChASeM33): A Deep
Survey of the Nearest Face-on Spiral Galaxy. The 1.4 Ms survey covers the
galaxy out to R \approx 18\arcmin (\approx 4 kpc). These data provide the
most intensive, high spatial resolution assessment of the X-ray source
populations available for the confused inner regions of M33. Mosaic images of
the ChASeM33 observations show several hundred individual X-ray sources as well
as soft diffuse emission from the hot interstellar medium. Bright, extended
emission surrounds the nucleus and is also seen from the giant \hii regions NGC
604 and IC 131. Fainter extended emission and numerous individual sources
appear to trace the inner spiral structure. The initial source catalog, arising
from ~2/3 of the expected survey data, includes 394 sources significant
at the confidence level or greater, down to a limiting luminosity
(absorbed) of 1.6\ergs{35} (0.35 -- 8.0 keV). The hardness ratios of the
sources separate those with soft, thermal spectra such as supernova remnants
from those with hard, non-thermal spectra such as X-ray binaries and background
active galactic nuclei. Emission extended beyond the Chandra point spread
function is evident in 23 of the 394 sources. Cross-correlation of the ChASeM33
sources against previous catalogs of X-ray sources in M33 results in matches
for the vast majority of the brighter sources and shows 28 ChASeM33 sources
within 10\arcsec of supernova remnants identified by prior optical and radio
searches. This brings the total number of such associations to 31 out of 100
known supernova remnants in M33.Comment: accepted for publication ApJS, full resolution images and complete
tables available at http://hea-www.harvard.edu/vlp_m33_public
Evaluating the American Heart Association/American College of Cardiology Guideline—Recommended and Contemporary Pretest Probability Models in a Mixed Asian Cohort: The Contribution of Coronary Artery Calcium
BACKGROUND: Most pretest probability (PTP) tools for obstructive coronary artery disease (CAD) were Western -developed. The most appropriate PTP models and the contribution of coronary artery calcium score (CACS) in Asian populations remain unknown. In a mixed Asian cohort, we compare 5 PTP models: local assessment of the heart (LAH), CAD Consortium (CAD2), risk factor-weighted clinical likelihood, the American Heart Association/American College of Cardiology and the European Society of Cardiology PTP and 3 extended versions of these models that incorporated CACS: LAH (CACS), CAD2 (CACS), and the CACS-clinical likelihood. METHODS AND RESULTS: The study cohort included 771 patients referred for stable chest pain. Obstructive CAD prevalence was 27.5%. Calibration, area under the receiver-operating characteristic curves (AUC) and net reclassification index were evaluated. LAH clinical had the best calibration (χ 2 5.8; P=0.12). For CACS models, LAH (CACS) showed least deviation between observed and expected cases (χ 2 37.5; P<0.001). There was no difference in AUCs between the LAH clinical (AUC, 0.73 [95% CI, 0.69-0.77]), CAD2 clinical (AUC, 0.72 [95% CI, 0.68-0.76]), risk factor-weighted clinical likelihood (AUC, 0.73 [95% CI: 0.69-0.76) and European Society of Cardiology PTP (AUC, 0.71 [95% CI, 0.67-0.75]). CACS improved discrimination and reclassification of the LAH (CACS) (AUC, 0.88; net reclassification index, 0.46), CAD2 (CACS) (AUC, 0.87; net reclassification index, 0.29) and CACS-CL (AUC, 0.87; net reclassification index, 0.25). CONCLUSIONS: In a mixed Asian cohort, Asian-derived LAH models had similar discriminatory performance but better calibration and risk categorization for clinically relevant PTP cutoffs. Incorporating CACS improved discrimination and reclassification. These results support the use of population-matched, CACS-inclusive PTP tools for the prediction of obstructive CAD.</p
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