1,133 research outputs found
The infrared counterpart to the magnetar 1RXS J170849.0-400910
We have analyzed both archival and new infrared imaging observations of the
field of the Anomalous X-ray Pulsar 1RXS J170849.0-400910, in search of the
infrared counterpart. This field has been previously investigated, and one of
the sources consistent with the position of the AXP suggested as the
counterpart. We, however, find that this object is more likely a background
star, while another object within the positional error circle has non-stellar
colors and shows evidence for variability. These two pieces of evidence, along
with a consistency argument for the X-ray-to-infrared flux ratio, point to the
second source being the more likely infrared counterpart to the AXP.Comment: 19 pages AASTEX, 4 figure. Accepted for publication in ApJ. Full
resolution figures at: http://www.astro.utoronto.ca/~durant/1708.ps.g
Discovery of a new pulsating X-ray source with a 1549.1-s period, AX J183220-0840
A new pulsating X-ray source, AX J183220-0840, with a 1549.1-s period was
discovered at R.A.= 18h32m20s and Dec.=-8d40'30'' (J2000,
uncertainty=0.6degree) during an ASCA observation on the Galactic plane. The
source was observed two times, in 1997 and in 1999. A phase-averaged X-ray flux
of 1.1E-11 ergs cm-2 s-1 and pulsation period of 1549.1+/-0.4 s were
consistently obtained from these two observations. The X-ray spectrum was
represented by a flat absorbed power-law with a photon-index of =~0.8 and an
absorption column density of =~1.3E22 cm-2. Also, a signature of iron K-shell
line emission with a centroid of 6.7 keV and an equivalent width of
approximately 450 eV was detected. From the pulsation period and the iron-line
feature, AX J183220-0840 is likely to be a magnetic white dwarf binary with a
complexly absorbed thermal spectrum with a temperature of about 10 keV.Comment: 13 pages, 4 figures, accepted for publication in ApJ Letter
Probing the stellar wind environment of Vela X-1 with MAXI
Vela X-1 is among the best studied and most luminous accreting X-ray pulsars.
The supergiant optical companion produces a strong radiatively-driven stellar
wind, which is accreted onto the neutron star producing highly variable X-ray
emission. A complex phenomenology, due to both gravitational and radiative
effects, needs to be taken into account in order to reproduce orbital spectral
variations. We have investigated the spectral and light curve properties of the
X-ray emission from Vela X-1 along the binary orbit. These studies allow to
constrain the stellar wind properties and its perturbations induced by the
compact object. We took advantage of the All Sky Monitor MAXI/GSC data to
analyze Vela X-1 spectra and light curves. By studying the orbital profiles in
the and keV energy bands, we extracted a sample of orbital light
curves (% of the total) showing a dip around the inferior
conjunction, i.e., a double-peaked shape. We analyzed orbital phase-averaged
and phase-resolved spectra of both the double-peaked and the standard sample.
The dip in the double-peaked sample needs cm to
be explained by absorption solely, which is not observed in our analysis. We
show how Thomson scattering from an extended and ionized accretion wake can
contribute to the observed dip. Fitted by a cutoff power-law model, the two
analyzed samples show orbital modulation of the photon index, hardening by
around the inferior conjunction, compared to earlier and later
phases, hinting a likely inadequacy of this model. On the contrary, including a
partial covering component at certain orbital phase bins allows a constant
photon index along the orbital phases, indicating a highly inhomogeneous
environment. We discuss our results in the framework of possible scenarios.Comment: 10 pages, 9 figures, accepted for publication in A&
Footprints in the wind of Vela X-1 traced with MAXI
The stellar wind around the compact object in luminous wind-accreting high
mass X-ray binaries is expected to be strongly ionized with the X-rays coming
from the compact object. The stellar wind of hot stars is mostly driven by
light absorption in lines of heavier elements, and X-ray photo-ionization
significantly reduces the radiative force within the so-called Stroemgren
region leading to wind stagnation around the compact object. In close binaries
like Vela X-1 this effect might alter the wind structure throughout the system.
Using the spectral data from Monitor of All-sky X-ray Image (MAXI), we study
the observed dependence of the photoelectric absorption as function of orbital
phase in Vela X-1, and find that it is inconsistent with expectations for a
spherically-symmetric smooth wind. Taking into account previous investigations
we develop a simple model for wind structure with a stream-like photoionization
wake region of slower and denser wind trailing the neutron star responsible for
the observed absorption curve.Comment: 5 pages, 3 figures, accepted in A&
Discovery of X-ray pulsations from IGR J16320-4751 = AX J1631.9-4752
We report a discovery of strong modulations of the X-ray flux detected from
IGR J16320-4751 = AX J1631.9-4752 with a period of P~1300 sec. We reanalyzed
the data of an XMM-Newton ToO performed soon after the discovery of the source
by INTEGRAL and found the modulation at a period of P=1309+/-40 sec with a high
significance. Modulations of the source flux with two possible periods of ~1300
and ~1500 sec were identified in the ASCA archival data. It is very likely that
the modulation can be interpreted as X-ray pulsations, favouring a pulsar as
the compact object in IGR/AX J16320-4752. Thus for the moment this source
became the fourth source from a new class of highly absorbed binary systems for
which the pulsations are observed.Comment: accepted for the publication in A&A Letters, 4 pages, 4 figure
Precision Timing of Two Anomalous X-Ray Pulsars
We report on long-term X-ray timing of two anomalous X-ray pulsars, 1RXS
J170849.0-400910 and 1E 2259+586, using the Rossi X-ray Timing Explorer. In
monthly observations made over 1.4 yr and 2.6 yr for the two pulsars,
respectively, we have obtained phase-coherent timing solutions which imply that
these objects have been rotating with great stability throughout the course of
our observations. For 1RXS J170849.0-400910, we find a rotation frequency of
0.0909169331(5) Hz and frequency derivative -15.687(4) x 10^(-14) Hz/s, for
epoch MJD 51215.931. For 1E 2259+586, we find a rotation frequency of
0.1432880613(2)Hz, and frequency derivative -1.0026(7) x 10^(-14) Hz/s, for
epoch MJD 51195.583. RMS phase residuals from these simple models are only
about 0.01 cycles for both sources. We show that the frequency derivative for
1E 2259+586 is inconsistent with that inferred from incoherent frequency
observations made over the last 20 yr. Our observations are consistent with the
magnetar hypothesis and make binary accretion scenarios appear unlikely.Comment: 12 pages including 3 figures. To appear in ApJ Letter
The dust-enshrouded microquasar candidate AX J1639.0-4642 = IGR J16393-4643
We present a multiwavelength study of the field containing the unidentified
X-ray source AX J1639.0-4642, discovered with the ASCA observatory and recently
detected with the IBIS telescope, onboard the INTEGRAL satellite, dubbed IGR
J16393-4643. The huge hydrogen column density towards the source, the hard
spectral index in the 0.7-10 keV band and its flux variability suggest that the
source is a High Mass X-ray Binary (HMXB) enshrouded by dust. Our search
reveals the presence of a non-thermal radio counterpart within the X-ray error
box. After a study of the broadband emission from X-rays to the radio domain,
we propose that AX J1639.0-4642 is a dust-enshrouded Microquasar (MQ)
candidate. In addition, the X-ray source is well within the 95% location
contour of the unidentified gamma-ray source 3EG J1639-4702. The main
properties of AX J1639.0-4642/3EG J1639-4702 are consistent with those of two
other MQs previously proposed to display high-energy gamma-ray emission.Comment: 7 pages, 5 figures. Accepted for publication in A&A. Title and
discussion on the possible NIR counterpart have been modifie
RESPIRATORY ACTIVITY OF ISOLATED MITOCHONDRIA FROM ORGANS AND TISSUES OF THE ANTARCTIC FISH Trematomus bernacchii, Trematomus newnesi, Lepidonotothen nudifrons, and Pagothenia hansoni
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