288 research outputs found
Spectral variability in Swift and Chandra observations of the Ultraluminous source NGC 55 ULX1
NGC 55 ULX1 is a bright Ultraluminous X-ray source located 1.78 Mpc away. We
analysed a sample of 20 Swift observations, taken between 2013 April and
August, and two Chandra observations taken in 2001 September and 2004 June. We
found only marginal hints of a limited number of dips in the light curve,
previously reported to occur in this source, although the uncertainties due to
the low counting statistics of the data are large. The Chandra and Swift
spectra showed clearly spectral variability which resembles those observed in
other ULXs. We can account for this spectral variability in terms of changes in
both the normalization and intrinsic column density of a two-components model
consisting of a blackbody (for the soft component) and a multicolour accretion
disc (for the hard component). We discuss the possibility that strong outflows
ejected by the disc are in part responsible for such spectral changes.Comment: 9 pages, 6 figure; accepted to be published on MNRA
Spectral analysis of SXP59.0 during its 2017 outburst and properties of the soft excess in X-ray binary pulsars
We report the results provided by the XMM-Newton observation of the X-ray
binary pulsar SXP59.0 during its most recent outburst in April 2017. The source
was detected at (0.2-12 keV) = 8 erg cm
s, one of its highest flux levels reported to date. The measured pulse
period was = 58.949(1) s, very similar to the periods measured
in most of the previous observations. The pulsed emission was clearly detected
over the whole energy range between 0.2 and 12 keV, but the pulse profile is
energy dependent and the pulsed fraction increases as the energy increases.
Although the time-averaged EPIC spectrum is dominated by a power-law component
(with photon index ), the data show an evident soft
excess, which can be described with the sum of a black-body and a hot thermal
plasma component (with temperatures eV and
keV, respectively). Moreover, the EPIC
and RGS spectra show narrow emission lines due to N, O, Ne, Mg, and Fe. The
phase-resolved spectral analysis of the EPIC data shows that the flux of the
black-body component varies with the pulse phase, while the plasma component is
almost constant. We show that the black-body component can be attributed to the
reprocessing of the primary emission by the optically thick material at the
inner edge of the accretion disc, while the hot plasma component is due to a
diffuse gas far from the accretion region and the narrow emission lines of the
RGS spectrum are most probably due to photoionized matter around the accreting
source.Comment: 11 pages, 9 figures, 5 tables. Accepted for publication by Astronomy
and Astrophysic
Spectral analysis of IGR J01572-7259 during its 2016 outburst
We report on the results of the observation of IGR J01572-7259
during its most recent outburst in 2016 May, the first since 2008. The source
reached a flux erg cm s, which allowed us to
perform a detailed analysis of its timing and spectral properties. We obtained
a pulse period = 11.58208(2) s. The pulse profile is double
peaked and strongly energy dependent, as the second peak is prominent only at
low energies and the pulsed fraction increases with energy. The main spectral
component is a power-law model, but at low energies we also detected a soft
thermal component, which can be described with either a blackbody or a hot
plasma model. Both the EPIC and RGS spectra show several emission lines, which
can be identified with the transition lines of ionized N, O, Ne, and Fe and
cannot be described with a thermal emission model. The phase-resolved spectral
analysis showed that the flux of both the soft excess and the emission lines
vary with the pulse phase: the soft excess disappears in the first pulse and
becomes significant only in the second, where also the Fe line is stronger.
This variability is difficult to explain with emission from a hot plasma, while
the reprocessing of the primary X-ray emission at the inner edge of the
accretion disk provides a realiable scenario. On the other hand, the narrow
emission lines can be due to the presence of photoionized matter around the
accreting source.Comment: 10 pages, 7 figures, 5 tables. Accepted for publication by Monthly
Notices of the Royal Astronomical Societ
Il progetto TN-1
Descrione hardware e software della scheda Transmission Node 1 (modulo della stazione sismica GAIA1), sua installazione ed utilizzo
Spectral analysis of SMC X-2 during its 2015 outburst
We report on the results of Swift and XMM-Newton observations of SMC X-2
during its last outburst in 2015 October, the first one since 2000. The source
reached a very high luminosity ( erg s), which allowed
us to perform a detailed analysis of its timing and spectral properties. We
obtained a pulse period = 2.372267(5) s and a characterization
of the pulse profile also at low energies. The main spectral component is a
hard () power-law model with an exponential cut-off, but at
low energies we detected also a soft (with kT 0.15 keV) thermal
component. Several emission lines can be observed at various energies. The
identification of these features with the transition lines of highly ionized N,
O, Ne, Si, and Fe suggests the presence of photoionized matter around the
accreting source.Comment: 5 pages, 3 figures, 2 tables. Accepted for publication in Monthly
Notices of the Royal Astronomical Society Letter
Enforcing Dirichlet boundary conditions in physics-informed neural networks and variational physics-informed neural networks
In this paper, we present and compare four methods to enforce Dirichlet
boundary conditions in Physics-Informed Neural Networks (PINNs) and Variational
Physics-Informed Neural Networks (VPINNs). Such conditions are usually imposed
by adding penalization terms in the loss function and properly choosing the
corresponding scaling coefficients; however, in practice, this requires an
expensive tuning phase. We show through several numerical tests that modifying
the output of the neural network to exactly match the prescribed values leads
to more efficient and accurate solvers. The best results are achieved by
exactly enforcing the Dirichlet boundary conditions by means of an approximate
distance function. We also show that variationally imposing the Dirichlet
boundary conditions via Nitsche's method leads to suboptimal solvers.Comment: 22 pages, 45 figure
Behind the dust curtain: the spectacular case of GRB 160623A
We report on the X-ray dust-scattering features observed around the afterglow
of the gamma ray burst GRB 160623A. With an XMM-Newton observation carried out
~2 days after the burst, we found evidence of at least six rings, with angular
size expanding between ~2 and 9 arcmin, as expected for X-ray scattering of the
prompt GRB emission by dust clouds in our Galaxy. From the expansion rate of
the rings, we measured the distances of the dust layers with extraordinary
precision: 528.1 +\- 1.2 pc, 679.2 +\- 1.9 pc, 789.0 +\- 2.8 pc, 952 +\- 5 pc,
1539 +\- 20 pc and 5079 +\- 64 pc. A spectral analysis of the ring spectra,
based on an appropriate dust-scattering model (BARE-GR-B from Zubko et al.
2004}) and the estimated burst fluence, allowed us to derive the column density
of the individual dust layers, which are in the range 7x10^20-1.5x10^22 cm^-2.
The farthest dust-layer (i.e. the one responsible for the smallest ring) is
also the one with the lowest column density and it is possibly very extended,
indicating a diffuse dust region. The properties derived for the six
dust-layers (distance, thickness, and optical depth) are generally in good
agreement with independent information on the reddening along this line of
sight and on the distribution of molecular and atomic gas.Comment: 9 pages, 10 figures, 1 table; accepted for publication in MNRA
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