77 research outputs found
Repeated X-ray Flaring Activity in Sagittarius A*
Investigating the spectral and temporal characteristics of the X-rays coming
from Sagittarius A* (Sgr A*) is essential to our development of a more complete
understanding of the emission mechanisms in this supermassive black hole
located at the center of our Galaxy. Several X-ray flares with varying
durations and spectral features have already been observed from this object.
Here we present the results of two long XMM-Newton observations of the Galactic
nucleus carried out in 2004, for a total exposure time of nearly 500 ks. During
these observations we detected two flares from Sgr A* with peak 2-10 keV
luminosities about 40 times (L ~ 9x10^34 erg s−1) above the quiescent
luminosity: one on 2004 March 31 and another on 2004 August 31. The first flare
lasted about 2.5 ks and the second about 5 ks. The combined fit on the Epic
spectra yield photon indeces of about 1.5 and 1.9 for the first and second
flare respectively. This hard photon index strongly suggests the presence of an
important population of non-thermal electrons during the event and supports the
view that the majority of flaring events tend to be hard and not very luminous.Comment: 8 pages, 7 figures, Accepted for publication in the Astrophysical
Journa
Modulated X-ray Emissivity near the Stress Edge in Sgr A*
Sgr A* is thought to be the radiative manifestation of a ~3.6E6 Msun
supermassive black hole at the Galactic center. Its mm/sub-mm spectrum and its
flare emission at IR and X-ray wavelengths may be produced within the inner ten
Schwarzschild radii of a hot, magnetized Keplerian flow. The lightcurve
produced in this region may exhibit quasi-periodic variability. We present
ray-tracing simulations to determine the general-relativistically modulated
X-ray luminosity expected from plasma coupled magnetically to the rest of the
disk as it spirals inwards below the innermost stable circular orbit towards
the "stress edge" in the case of a Schwarzschild metric. The resulting
lightcurve exhibits a modulation similar to that observed during a recent X-ray
flare from Sgr A*.Comment: 4 pages, 3 figures, accepted for publication in ApJ
General Relativistic Flux Modulations from Disk Instabilities in Sagittarius A*
Near-IR and X-ray flares have been detected from the supermassive black hole
Sgr A* at the center of our Galaxy with a (quasi)-period of ~17-20 minutes,
suggesting an emission region only a few Schwarzschild radii above the event
horizon. The latest X-ray flare, detected with XMM-Newton, is notable for its
detailed lightcurve, yielding not only the highest quality period thus far, but
also important structure reflecting the geometry of the emitting region. Recent
MHD simulations of Sgr A*'s disk have demonstrated the growth of a Rossby wave
instability, that enhances the accretion rate for several hours, possibly
accounting for the observed flares. In this Letter, we carry out ray-tracing
calculations in a Schwarzschild metric to determine as accurately as possible
the lightcurve produced by general relativistic effects during such a
disruption. We find that the Rossby wave induced spiral pattern in the disk is
an excellent fit to the data, implying a disk inclination angle of ~77 deg.
Note, however, that if this association is correct, the observed period is not
due to the underlying Keplerian motion but, rather, to the pattern speed. The
favorable comparison between the observed and simulated lightcurves provides
important additional evidence that the flares are produced in Sgr A*'s inner
disk.Comment: 5 Pages, 3 Figures, accepted for publication in ApJ Lette
Contribution of point sources to the soft gamma-ray Galactic emission
The nature of the soft gamma-ray (20-200 keV) Galactic emission has been a
matter of debate for a long time. Previous experiments have tried to separate
the point source contribution from the real interstellar emission, but with a
rather poor spatial resolution, they concluded that the interstellar emission
could be a large fraction of the total Galactic emission. INTEGRAL, having both
high resolution and high sensitivity, is well suited to reassess more precisely
this problem. Using the INTEGRAL core program Galactic Center Deep Exposure
(GCDE), we estimate the contribution of detected point sources to the total
Galactic flux.Comment: Proceedings of the 5th INTEGRAL Workshop, Munich 16-20 February 2004.
ESA SP-55
Multiwavelength study of the fast rotating supergiant high-mass X-ray binary IGR J16465-4507
Since its launch, the X-ray and gamma-ray observatory INTEGRAL satellite has
revealed a new class of high-mass X-ray binaries (HMXB) displaying fast flares
and hosting supergiant companion stars. Optical and infrared (OIR) observations
in a multi-wavelength context are essential to understand the nature and
evolution of these newly discovered celestial objects. The goal of this
multiwavelength study (from ultraviolet to infrared) is to characterise the
properties of IGR J16465-4507, to confirm its HMXB nature and that it hosts a
supergiant star. We analysed all OIR, photometric and spectroscopic
observations taken on this source, carried out at ESO facilities. Using
spectroscopic data, we constrained the spectral type of the companion star
between B0.5 and B1 Ib, settling the debate on the true nature of this source.
We measured a high rotation velocity of v = 320 +/- 8 km/s from fitting
absorption and emission lines in a stellar spectral model. We then built a
spectral energy distribution from photometric observations to evaluate the
origin of the different components radiating at each energy range. We finally
show that, having accurately determined the spectral type of the early-B
supergiant in IGR J16465-4507, we firmly support its classification as an
intermediate supergiant fast X-ray transient (SFXT).Comment: A&A in press, 14 pages, 15 tables, 13 figure
On the evolution of the Gamma- and X-ray luminosities of Pulsar Wind Nebulae
Pulsar wind nebulae are a prominent class of very high energy (E > 0.1 TeV)
Galactic sources. Their Gamma-ray spectra are interpreted as due to inverse
Compton scattering of ultrarelativistic electrons on the ambient photons,
whereas the X-ray spectra are due to synchrotron emission. We investigate the
relation between the Gamma- and-X-ray emission and the pulsars' spin-down
luminosity and characteristic age. We find that the distance-independent Gamma-
to X-ray flux ratio of the nebulae is inversely proportional to the spin-down
luminosity, (\propto \dot{E}^-1.9), while it appears proportional to the
characteristic age, (\propto tau_c^2.2), of the parent pulsar. We interpret
these results as due to the evolution of the electron energy distribution and
the nebular dynamics, supporting the idea of so-called relic pulsar wind
nebulae. These empirical relations provide a new tool to classify unidentified
diffuse Gamma-ray sources and to estimate the spin-down luminosity and
characteristic age of rotation powered pulsars with no detected pulsation from
the X- and Gamma-ray properties of the associated pulsar wind nebulae. We apply
these relations to predict the spin-down luminosity and characteristic age of
four (so far unpulsing) candidate pulsars associated to wind nebulae.Comment: Accepted for publication in ApJ (6 pages, 2 figures
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