703 research outputs found
Chandra Observation of the Magellanic Cloud Supernova Remnant 0454-672 in N9
A Chandra observation has defined the extent of the SNR B 0454-692 in the LMC
H II region N9. The remnant has dimension 2.3" x 3.6" and is elongated in the
NS direction. The brightest emission comes from a NS central ridge which
includes three bright patches. There is good agreement between X-ray and [O
III] and [S II] morphology. The remnant is old enough so that optical data give
more information about dynamics than do the X-ray data. The SN energy release
was >= 4 x 10^50 ergs and the age is ~3 x 10^4 years. There are several
unresolved sources nearby but none are clearly associated with the remnant. The
X-ray spectrum is soft and indicates enhanced Fe abundance in the central
region, consistent with a Type Ia SN origin, but a Type II origin cannot be
ruled out.Comment: AASTeX, 20 pages including 5 figures. Accepted for publication in The
Astrophysical Journal. Figures have been reduced in resolution for space
requirements; full-resolution figures may be requested by email to
[email protected]
X-Ray Light Curves of Gamma-ray Bursts Detected with the All-Sky Monitor on RXTE
We present X-ray light curves (1.5-12 keV) for fifteen gamma-ray bursts
(GRBs) detected by the All-Sky Monitor on the Rossi X-ray Timing Explorer. We
compare these soft X-ray light curves with count rate histories obtained by the
high-energy (>12 keV) experiments BATSE, Konus-Wind, the BeppoSAX Gamma-Ray
Burst Monitor, and the burst monitor on Ulysses. We discuss these light curves
within the context of a simple relativistic fireball and synchrotron shock
paradigm, and we address the possibility of having observed the transition
between a GRB and its afterglow. The light curves show diverse morphologies,
with striking differences between energy bands. In several bursts, intervals of
significant emission are evident in the ASM energy range with little or no
corresponding emission apparent in the high-energy light curves. For example,
the final peak of GRB 970815 as recorded by the ASM is only detected in the
softest BATSE energy bands. We also study the duration of bursts as a function
of energy. Simple, singly-peaked bursts seem consistent with the E^{-0.5} power
law expected from an origin in synchrotron radiation, but durations of bursts
that exhibit complex temporal structure are not consistent with this
prediction. Bursts such as GRB 970828 that show many short spikes of emission
at high energies last significantly longer at low energies than the synchrotron
cooling law would predict.Comment: 15 pages with 20 figures and 2 tables. In emulateapj format. Accepted
by ApJ
Supernova Remnants in the Magellanic Clouds. V. The Complex Interior Structure of the N206 SNR
The N206 supernova remnant (SNR) in the Large Magellanic Cloud (LMC) has long
been considered a prototypical "mixed morphology" SNR. Recent observations,
however, have added a new twist to this familiar plot: an elongated,
radially-oriented radio feature seen in projection against the SNR face.
Utilizing the high resolution and sensitivity available with the Hubble Space
Telescope, Chandra, and XMM-Newton, we have obtained optical emission-line
images and spatially resolved X-ray spectral maps for this intriguing SNR. Our
findings present the SNR itself as a remnant in the mid to late stages of its
evolution. X-ray emission associated with the radio "linear feature" strongly
suggests it to be a pulsar-wind nebula (PWN). A small X-ray knot is discovered
at the outer tip of this feature. The feature's elongated morphology and the
surrounding wedge-shaped X-ray enhancement strongly suggest a bow-shock PWN
structure.Comment: 41 pages including 7 figures, accepted for publication by the
Astrophysical Journa
X-ray Spectroscopy of Candidate Ultracompact X-ray Binaries
We present high-resolution spectroscopy of the neutron star/low-mass X-ray
binaries (LMXBs) 4U 1850-087 and 4U 0513-40 as part of our continuing study of
known and candidate ultracompact binaries. The LMXB 4U 1850-087 is one of four
systems in which we had previously inferred an unusual Ne/O ratio in the
absorption along the line of sight, most likely from material local to the
binaries. However, our recent Chandra X-ray Observatory LETGS spectrum of 4U
1850-087 finds a Ne/O ratio by number of 0.22+/-0.05, smaller than previously
measured and consistent with the expected interstellar value. We propose that
variations in the Ne/O ratio due to source variability, as previously observed
in these sources, can explain the difference between the low- and
high-resolution spectral results for 4U 1850-087. Our XMM-Newton RGS
observation of 4U 0513-40 also shows no unusual abundance ratios in the
absorption along the line of sight. We also present spectral results from a
third candidate ultracompact binary, 4U 1822-000, whose spectrum is well fit by
an absorbed power-law + blackbody model with absorption consistent with the
expected interstellar value. Finally, we present the non-detection of a fourth
candidate ultracompact binary, 4U 1905+000, with an upper limit on the source
luminosity of < 1 x 10^{32} erg s^{-1}. Using archival data, we show that the
source has entered an extended quiescent state.Comment: 8 pages, 3 figures, accepted for publication to the Astrophysical
Journa
Chandra Observation of Luminous and Ultraluminous X-ray Binaries in M101
X-ray binaries in the Milky Way are among the brightest objects on the X-ray
sky. With the increasing sensitivity of recent missions, it is now possible to
study X-ray binaries in nearby galaxies. We present data on six luminous
sources in the nearby spiral galaxy, M101, obtained with the Chandra ACIS-S. Of
these, five appear to be similar to ultraluminous sources in other galaxies,
while the brightest source, P098, shows some unique characteristics. We present
our interpretation of the data in terms of an optically thick outflow, and
discuss implications.Comment: Accepted for publication in Astrophysical Journal (16 pages including
4 figures
An X-ray survey of low-mass stars in Trumpler 16 with Chandra
We identify and characterize low-mass stars in the ~3 Myr old Trumpler 16
(Tr16) region by means of a deep Chandra X-ray observation, and study their
optical and near-IR properties. We compare X-ray activity of Tr16 stars with
known characteristics of Orion and Cygnus OB2 stars. We analyzed a 88.4 ksec
Chandra ACIS-I observation pointed at the center of Tr16. Because of diffuse
X-ray emission, source detection was performed using the PWDetect code for two
different energy ranges: 0.5-8.0 keV and 0.9-8.0 keV. Results were merged into
a single final list. We positionally correlate X-ray sources with optical and
2MASS catalogues. Source events were extracted with the IDL-based routine
ACIS-Extract. X-ray variability was characterized using the Kolmogorov-Smirnov
test and spectra were fitted by using XSPEC. X-ray spectra of early-type,
massive stars were analyzed individually. Our list of X-ray sources consists of
1035 entries, 660 of which have near-IR counterparts and are probably
associated with Tr16 members. From near-IR color-color and color-magnitudes
diagrams we compute individual masses of stars and their Av values. About 15%
of the near-IR counterparts show disk-induced excesses. X-ray variability is
found in 77 sources. X-ray emission from OB stars appear softer than the
low-mass stars. The Tr16 region has a very rich population of low-mass X-ray
emitting stars. An important fraction of its circumstellar disks survive the
intense radiation field of its massive stars. Stars with masses 1.5-2.5 Mo
display X-ray activity similar to that of stars in Cyg OB2 but much less
intense than observed for Orion Nebula Cluster members.Comment: 19 pages, 3 ellectronic tables and 19 figures. Accepted for
publication at the A&
DEM L241, a Supernova Remnant containing a High-Mass X-ray Binary
A Chandra observation of the Large Magellanic Cloud supernova remnant DEM
L241 reveals an interior unresolved source which is probably an
accretion-powered binary. The optical counterpart is an O5III(f) star making
this a High-Mass X-ray Binary (HMXB) with orbital period likely to be of order
tens of days. Emission from the remnant interior is thermal and spectral
information is used to derive density and mass of the hot material. Elongation
of the remnant is unusual and possible causes of this are discussed. The
precursor star probably had mass > 25 solar masse
Cardiomyocyte Deletion of \u3ci\u3eBmal1\u3c/i\u3e Exacerbates QT- and RR-Interval Prolongation in \u3ci\u3eScn5a\u3c/i\u3e\u3csup\u3e+/ΔKPQ\u3c/sup\u3e Mice
Circadian rhythms are generated by cell autonomous circadian clocks that perform a ubiquitous cellular time-keeping function and cell type-specific functions important for normal physiology. Studies show inducing the deletion of the core circadian clock transcription factor Bmal1 in adult mouse cardiomyocytes disrupts cardiac circadian clock function, cardiac ion channel expression, slows heart rate, and prolongs the QT-interval at slow heart rates. This study determined how inducing the deletion of Bmal1 in adult cardiomyocytes impacted the in vivo electrophysiological phenotype of a knock-in mouse model for the arrhythmogenic long QT syndrome (Scn5a+/ΔKPQ). Electrocardiographic telemetry showed inducing the deletion of Bmal1 in the cardiomyocytes of mice with or without the ΔKPQ-Scn5a mutation increased the QT-interval at RR-intervals that were ≥130 ms. Inducing the deletion of Bmal1 in the cardiomyocytes of mice with or without the ΔKPQ-Scn5a mutation also increased the day/night rhythm-adjusted mean in the RR-interval, but it did not change the period, phase or amplitude. Compared to mice without the ΔKPQ-Scn5a mutation, mice with the ΔKPQ-Scn5a mutation had reduced heart rate variability (HRV) during the peak of the day/night rhythm in the RR-interval. Inducing the deletion of Bmal1 in cardiomyocytes did not affect HRV in mice without the ΔKPQ-Scn5a mutation, but it did increase HRV in mice with the ΔKPQ-Scn5a mutation. The data demonstrate that deleting Bmal1 in cardiomyocytes exacerbates QT- and RR-interval prolongation in mice with the ΔKPQ-Scn5a mutation
An XMM-Newton view of Planetary Nebulae in the Small Magellanic Cloud. The X-ray luminous central star of SMP SMC 22
During an X-ray survey of the Small Magellanic Cloud, carried out with the
XMM-Newton satellite, we detected significant soft X-ray emission from the
central star of the high-excitation planetary nebula SMP SMC 22. Its very soft
spectrum is well fit with a non local thermodynamical equilibrium model
atmosphere composed of H, He, C, N, and O, with abundances equal to those
inferred from studies of its nebular lines. The derived effective temperature
of 1.5x10^5 K is in good agreement with that found from the optical/UV data.
The unabsorbed flux in the 0.1-0.5 keV range is about 3x10^{-11} erg cm^-2
s^-1, corresponding to a luminosity of 1.2x10^37 erg/s at the distance of 60
kpc. We also searched for X-ray emission from a large number of SMC planetary
nebulae, confirming the previous detection of SMP SMC 25 with a luminosity of
(0.2-6)x10^35 erg/s (0.1-1 keV). For the remaining objects that were not
detected, we derived flux upper limits corresponding to luminosity values from
several tens to hundreds times smaller than that of SMP SMC 22. The
exceptionally high X-ray luminosity of SMP SMC 22 is probably due to the high
mass of its central star, quickly evolving toward the white dwarf's cooling
branch, and to a small intrinsic absorption in the nebula itself.Comment: Accepted for publication on Astronomy and Astrophysic
Discovery of luminous pulsed hard X-ray emission from anomalous X-ray pulsars 1RXS J1708-4009, 4U 0142+61 and 1E 2259+586 by INTEGRAL and RXTE
We report on the discovery of hard spectral tails for energies above 10 keV
in the total and pulsed spectra of anomalous X-ray pulsars 1RXS J1708-4009, 4U
0142+61 and 1E 2259+586 using RXTE PCA (2-60 keV) and HEXTE (15-250 keV) data
and INTEGRAL IBIS ISGRI (20-300 keV) data. Improved spectral information on 1E
1841-045 is presented. The pulsed and total spectra measured above 10 keV have
power-law shapes and there is so far no significant evidence for spectral
breaks or bends up to ~150 keV. The pulsed spectra are exceptionally hard with
indices measured for 4 AXPs approximately in the range -1.0 -- 1.0. We also
reanalyzed archival CGRO COMPTEL (0.75-30 MeV) data to search for signatures
from our set of AXPs. No detections can be claimed, but the obtained
upper-limits in the MeV band indicate that for 1RXS J1708-4009, 4U 0142+61 and
1E 1841-045 strong breaks must occur somewhere between 150 and 750 keV.Comment: Accepted for publication in ApJ; 19 pages; 4 Tables; 15 Figures (6
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