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Detection of Pulsed X-ray Emission from PSR B1706-44
We report the first detection of pulsed X-ray emission from the young,
energetic radio and Gamma-ray pulsar PSR B1706-44. We find a periodic signal at
a frequency of f = 9.7588088 +/- 0.0000026 Hz (at epoch 51585.34104 MJD),
consistent with the radio ephemeris, using data obtained with the High
Resolution Camera on-board the Chandra X-ray Observatory}. The probability that
this detection is a chance occurrence is 3.5E-5 as judged by the Rayleigh test.
The folded light curve has a broad, single-peaked profile with a pulsed
fraction of 23% +/- 6%. This result is consistent the ROSAT PSPC upper limit of
< 18% after allowing for the ability of Chandra to resolve the pulsar from a
surrounding synchrotron nebula. We also fitted Chandra spectroscopic data on
PSR B1706-44, which require at least two components, e.g., a blackbody of
temperature T(infinity) between 1.51E6 K and 1.83E6 K and a power-law of Gamma
= 2.0 +/- 0.5. The blackbody radius at the nominal 2.5 kpc distance is only
R(infinity) = 3.6 +/- 0.9 km, indicating either a hot region on a cooler
surface, or the need for a realistic atmosphere model that would allow a lower
temperature and larger area. Because the power-law and blackbody spectra each
contribute more than 23% of the observed flux, it is not possible to decide
which component is responsible for the modulation in the spectrally unresolved
light curve.Comment: 6 pages, 4 figures, Latex, emulateapj. Published version. Includes an
updated radio ephemeris and presents the absolute radio/X-ray phase alignmen
Relative astrometry of the J=1-0, v=1 and v=2 SiO masers towards R Leonis Minoris using VERA
Oxygen-rich Asymptotic Giant Branch (AGB) stars are intense emitters of SiO
and HO maser lines at 43 (J=1-0, v=1 and 2) and 22 GHz, respectively. VLBI
observations of the maser emission provides a unique tool to sample the
innermost layers of the circumstellar envelopes in AGB stars. Nevertheless, the
difficulties in achieving astrometrically aligned v=1 and v=2 SiO maser maps
have traditionally prevented a unique interpretation of the observations in
terms of physical underlying conditions, which depend on the nature of the SiO
pumping mechanism.
We have carried out observations of the SiO and HO maser emission towards
RLMi, using the astrometric capabilities of VERA. Due to the too-weak emission
of the reference calibrator we had to develop a special method to accurately
relate the coordinates for both transitions. We present relative
astrometrically aligned v=1 and v=2 J=1-0 SiO maser maps, at multiple epochs,
and discuss the astrophysical results. The incorporation of astrometric
information into the maps of SiO masers challenges the weak points in the
current theoretical models, which will need further refinements to address the
observations results.Comment: 17 pages, 8 figure
Professor Ugo Carraro and BAM: two friends for life
Not available
Slow gait speed and cardiac rehabilitation participation in older adults after acute myocardial infarction
Background
Lack of participation in cardiac rehabilitation (
CR
) and slow gait speed have both been associated with poor longâterm outcomes in older adults after acute myocardial infarction (
AMI
). Whether the effect of
CR
participation on outcomes after
AMI
differs by gait speed is unknown.
Methods and Results
We examined the association between gait speed and
CR
participation at 1Â month after discharge after
AMI
, and death and disability at 1Â year, in 329 patients aged â„65Â years enrolled in the
TRIUMPH
(Translational Research Investigating Underlying Disparities in Recovery From Acute Myocardial Infarction: Patients' Health Status) registry. Among these patients, 177 (53.7%) had slow gait speed (<0.8Â m/s) and 109 (33.1%) participated in
CR
. Patients with slow gait speed were less likely to participate in
CR
compared with patients with normal gait speed (27.1% versus 40.1%;
P
=0.012). In unadjusted analysis,
CR
participants with normal gait speed had the lowest rate of death or disability at 1Â year (9.3%), compared with those with slow gait speed and no
CR
participation (43.2%). After adjustment for cardiovascular risk factors and cognitive impairment, both slow gait speed (odds ratio, 2.30; 95% confidence interval, 1.30â4.06) and nonâ
CR
participation (odds ratio, 2.34; 95 confidence interval, 1.22â4.48) were independently associated with death or disability at 1Â year. The effect of
CR
on the primary outcome did not differ by gait speed (
P
=0.70).
Conclusions
CR
participation is associated with reduced risk for death or disability after
AMI
. The beneficial effect of
CR
participation does not differ by gait speed, suggesting that slow gait speed alone should not preclude referral to
CR
for older adults after
AMI
.
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X-ray Spectrum and Pulsations of the Vela Pulsar
We report the results of the spectral and timing analysis of observations of
the Vela pulsar with the Chandra X-ray Observatory. The spectrum shows no
statistically significant spectral lines in the observed 0.25--8.0 keV band. It
consists of two distinct continuum components. The softer component can be
modeled as either a magnetic hydrogen atmosphere spectrum with kT = 59 +- 3 eV,
R = 15.5 +- 1.5 km, or a standard blackbody with kT = 129 +- 4 eV, R = 2.1 +-
0.2 km (the radii are for a distance of 250 pc). The harder component, modeled
as a power-law spectrum, gives photon indices depending on the model adopted
for the soft component: gamma = 1.5 +- 0.3 for the magnetic atmosphere soft
component, and gamma = 2.7 +- 0.4 for the blackbody soft component. Timing
analysis shows three peaks in the pulse profile, separated by about 0.3 in
phase. Energy-resolved timing provides evidence for pulse profile variation
with energy. The higher energy (E > 1.8 keV) profile shows significantly higher
pulsed fraction.Comment: 4 pages, 2 figures, To appear in "Neutron Stars in Supernova
Remnants" (ASP Conference Proceedings), eds P. O. Slane and B. M. Gaensler
Corrected TYPO
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