arXiv subjects

Didier Barret

Publications and source records attributed to Didier Barret.

126 records · Page 7Linked to original sources

arXiv2004

Faint X-ray sources in globular clusters in the XMM-Newton and Chandra era

X-ray imaging and spectroscopy can be used to probe the binary content of globular clusters. Binaries are thought to play a key role in the dynamical evolution of the clusters by serving as an internal source of energy which counters the tendency of their cores to collapse. Various kinds of binaries are found in clusters in X-rays, including BY Dra or RS CVn systems, Cataclysmic Variables and low mass X-ray binaries as well as millisecond pulsars. In this review, we will present the most recent X-ray observations of globular clusters as performed with XMM-Newton and Chandra. We will illustrate the power of X-ray observations to separate the different X-ray source populations, and emphasize how the results are important in understanding the binary formation processes.

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arXiv2004

Accretion flows around stellar mass black holes and neutron stars

In this review, I summarize the main X-ray/hard X-ray properties of the accretion flows around black holes and neutron stars based on recent broad-band spectral and timing observations performed by the BeppoSAX and Rossi X-ray Timing Explorer satellites. Emphasizing the spectral and timing similarities observed between black holes and neutron stars, I discuss on the most likely accretion geometry and emission processes associated with hard and soft spectral states. For black holes, in the hard state, the accretion geometry is more likely made of a truncated disk and a hot inner flow, in which thermal Comptonization takes place. The truncated disk is likely to be the dominant source of seed photons, and the site for the production of the reflection component observed. In soft states, the disk now extends closer to the compact object and is brighter in X-rays. The hard X-ray emission occurs through Comptonization of disk photons on a thermal/non-thermal electron distribution, generated in magnetic flares above the accretion disk. For neutron stars, similar accretion geometry and emission mechanisms may apply but the unavoidable radiation from the neutron star surface adds yet another component in the X-ray spectrum. It also acts as an additional source of cooling for the Comptonizing cloud, leading to softer spectra in neutron stars than in black holes.

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arXiv2004

XTRA: The fast X-ray timing detector on XEUS

The Rossi X-ray Timing Explorer (RXTE) has demonstrated that the dynamical variation of the X-ray emission from accreting neutron stars and stellar mass black holes is a powerful probe of their strong gravitational fields. At the same time, the X-ray burst oscillations at the neutron star spin frequency have been used to set important constraints on the mass and radius of neutron stars, hence on the equation of state of their high density cores. The X-ray Evolving Universe Spectroscopy mission (XEUS), the potential follow-on mission to XMM-Newton, will have a mirror aperture more than ten times larger than the effective area of the RXTE proportional counter array (PCA). Combined with a small dedicated fast X-ray timing detector in the focal plane (XTRA: XEUS Timing for Relativistic Astrophysics), this collecting area will provide a leap in timing sensitivity by more than one order of magnitude over the PCA for bright sources, and will open a brand new window on faint X-ray sources, owing to the negligible detector background. The use of advanced Silicon drift chambers will further improve the energy resolution by a factor of ~6 over the PCA, so that spectroscopic diagnostics of the strong field region, such as the relativistically broadened Iron line, will become exploitable. By combining fast X-ray timing and spectroscopy, XTRA will thus provide the first real opportunity to test general relativity in the strong gravity field regime and to constrain with unprecedented accuracy the equation of state of matter at supranuclear density.

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arXiv2003

Discovery of a quiescent neutron star binary in the globular cluster M13

We have discovered with XMM-Newton an X-ray source in the core of the globular cluster M13, whose X-ray spectral properties suggest that it is a quiescent neutron star X-ray binary. The spectrum can be well fitted with a pure hydrogen atmosphere model, with T=76 +/- 3 eV, R=12.8 +/- 0.4 km and an X-ray luminosity of 7.3 +/- 0.6 x 10^{32} erg/s. In the light of this result, we have discovered a strong correlation between the stellar encounter rate and the number of quiescent neutron stars found in the ten globular clusters observed so far by either XMM-Newton or Chandra. This result lends strong support to the idea that these systems are primarily produced by stellar encounters in the core of globular clusters.

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arXiv2003

Simultaneous BeppoSAX and Rossi X-ray Timing Explorer observations of 4U1812-12

4U1812-12 is a faint persistent and weakly variable neutron star X-ray binary. It was observed by BeppoSAX between April 20th and 21st, 2000 in a hard spectral state with a bolometric luminosity of ~2x10^36 ergs/s. Its broad band energy spectrum is characterized by the presence of a hard X-ray tail extending above ~100 keV. It can be represented as the sum of a dominant hard Comptonized component (electron temperature of ~36 keV and optical depth ~3) and a weak soft component. The latter component which can be fitted with a blackbody of about 0.6 keV and equivalent radius of ~2 km is likely to originate from the neutron star surface. We also report on the first measurement of the power density spectrum of the source rapid X-ray variability, as recorded during a simultaneous snapshot observation performed by the Rossi X-ray Timing Explorer. As expected for a neutron star system in such hard spectral state, its power density spectrum is characterized by the presence of a ~0.7 Hz low frequency quasi-periodic oscillation together with three broad noise components, one of which extends above ~200 Hz.

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arXiv2002

An XMM-Newton observation of the globular cluster Omega Centauri

We report on a deep XMM-Newton EPIC observation of the globular cluster Omega Cen performed on August 13th, 2001. We have detected 11 and 27 faint X-ray sources in the core and half mass radii, searching down to a luminosity of 1.3 x 10^{31} erg s^{-1} in the 0.5-5 keV range. Most sources have bolometric X-ray luminosities between ~ 10^{31}-10^{32} erg s^{-1}. We present the color-color and hardness-intensity diagrams of the source sample, as well as high-quality EPIC spectra of the brightest objects of the field; including the two candidate Cataclysmic Variables (CVs) in the core and the quiescent neutron star low-mass X-ray binary candidate. The spectra of the latter objects fully support their previous classification. We show that the bulk of sources are hard and spectrally similar to CVs. The lack of soft faint sources might be related to the absence of millisecond pulsars in the cluster. The XMM-Newton observations reveal the presence of an excess of sources well outside the core of the cluster where several RS CVn binaries have already been found. We have also analyzed a publicly available Chandra ACIS-I observation performed on January 24-25th, 2000, to improve the XMM-Newton source positions and to search for source intensity variations between the two data sets. 63 XMM-Newton sources have a Chandra counterpart, and 15 sources within the half-mass radius have shown time variability. Overall, the general properties of the faint X-ray sources in Omega Cen suggest that they are predominantly CVs and active binaries (RS CVn or BY Dra).

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arXiv2002

ECLAIRs: A microsatellite to observe the prompt optical and X-ray emission of Gamma-Ray Bursts

ECLAIRs is a French microsatellite devoted to the observation of the prompt optical and X-ray emission of GRBs. For about 100 GRBs/yr, independent of their duration, ECLAIRs will provide high time resolution high sensitivity spectral coverage from a few eV up to ~50 keV and localization to ~5 arcsec in near real time. This capability is achieved by combining wide field optical and X-ray cameras sharing a common field of view (~1/6th of the sky) with the coded-mask imaging telescopes providing the triggers and the coarse localizations of the bursts. Given the delays to start ground-based observations in response to a GRB trigger, ECLAIRs is unique in its ability to observe the early phases (the first ~20 sec) of all GRBs at optical wavelengths. Furthermore, with its mode of operation, ECLAIRs will enable to search for optical and X-ray precursors expected from theoretical grounds. Finally ECLAIRs is proposed to operate simultaneously with GLAST on a synchronous orbit. This combination will ensure broad band spectral coverage from eV to GeV energies for the GRBs detected by the two satellites, ECLAIRs further providing their accurate localization to enable follow-up studies.

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arXiv2002

A peculiar spectral state transition of 4U1705--44: when an Atoll looks like a Z

We report on a clear spectral state transition of the neutron star low-mass X-ray binary 4U1705-44 observed by the Rossi X-ray Timing Explorer. In the X-ray color-color diagram (CCD), the source, classified as an Atoll, samples the upper parts of a Z, starting from and returning to the left bottom of the Z. We follow the path of 4U1705-44 on its CCD, model its broad band X-ray/hard X-ray spectrum, and compute the Fourier power density spectrum of its X-ray variability. The spectral transitions of 4U1705-44 are shown to be primarily associated with changes in the temperature of the Comptonizing electrons. In the hard state (top branch of the Z), the source evolves from left to right on the CCD, while its luminosity smoothly increases. Our observations can be interpreted in the framework of a model made of a truncated accretion disk of varying inner radius and an inner flow merging smoothly with the neutron star boundary layer. The spectral evolution could be driven by changes in the truncation radius of the disk; e.g. the soft to hard transition could be caused by the disk moving outwards. If this model is correct, then our data show that the disk truncation radius is not set by the instantaneous mass accretion rate, as derived from the source bolometric luminosity. Comparing the power density spectra of 4U1705-44 and Z sources when they occupy similar branches of the Z, we show that the most significant difference is on the diagonal branch, on which the power density spectra of 4U1705-44 remain similar to the ones measured on the top branch of the Z (hard state).

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arXiv2001

Phase-resolved X-ray spectroscopy of the millisecond pulsar SAX J1808.4-3658

We present new results based on RXTE observations of SAX J1808.4-3658. The X-ray spectrum can be fitted by a two-component model. We interpret the soft component as blackbody emission from a heated spot on the neutron star, and the hard component as coming from Comptonization in plasma heated by the accretion shock as the material collimated by the magnetic field impacts onto the neutron star surface. The hotspot is probably the source of seed photons for Comptonization. The hard component illuminates the disc, giving rise to a reflected spectrum. The inferred evolution of the inner radius is not consistent with the magnetic field truncating the disc. Instead it seems more likely that the inner disc radius is set by some much longer time-scale process, most probably connected to the overall evolution of the accretion disc. This disc truncation mechanism would then have to be generic in all low mass accretion rate flows both in disc accreting neutron stars and black hole systems. The phase resolved spectra show clearly that the blackbody and hard Comptonized spectra pulse independently. This obviously gives an energy dependent phase lag. Full general relativistic effects are not required to explain this. We do not detect Compton reflection from the neutron star surface, though we predict that it should be present in the X-ray spectrum. This would give an unambiguous observational measure of M/R if there is any iron on the neutron star surface which is not completely ionized.

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arXiv2001

First XMM-Newton Observations of the Globular Cluster M22

We have examined preliminary data of the globular cluster, M22, from the EPIC MOS detectors on board XMM-Newton. We have detected 27 X-ray sources within the centre of the field of view, 24 of which are new detections. Three sources were found within the core of the cluster. From spectral analysis of the X-ray sources, it is possible that the object at the centre of the core is a quiescent X-ray transient and those lying further out are maybe cataclysmic variables.

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arXiv2001

ECLAIRs: A microsatellite for the prompt optical and X-ray emission of Gamma-Ray Bursts

The prompt gamma-ray emission of Gamma-Ray Bursts (GRBs) is currently interpreted in terms of radiation from electrons accelerated in internal shocks in a relativistic fireball. On the other hand, the origin of the prompt (and early afterglow) optical and X-ray emission is still debated, mostly because very few data exist for comparison with theoretical predictions. It is however commonly agreed that this emission hides important clues on the GRB physics and can be used to constrain the fireball parameters, the acceleration and emission processes and to probe the surroundings of the GRBs. ECLAIRs is a microsatellite devoted to the observation of the prompt optical and X-ray emission of GRBs. For about 150 GRBs/yr, independent of their duration, ECLAIRs will provide high time resolution high sensitivity spectral coverage from a few eV up to ~50 keV and localization to ~ 5'' in near real time. This capability is achieved by combining wide field optical and X-ray cameras sharing a common field of view (>~ 2.2 steradians) with the coded-mask imaging telescopes providing the triggers and the coarse localizations of the bursts. Given the delays to start ground-based observations in response to a GRB trigger, ECLAIRs is unique in its ability to observe the early phases (the first ~20 sec) of all GRBs at optical wavelengths. Furthermore, with its mode of operation, ECLAIRs will enable to search for optical and X-ray precursors expected from theoretical grounds. Finally ECLAIRsis proposed to operate simultaneously with GLAST on a similar orbit. This combination will both provide unprecedented spectral coverage from a few eV up to ~200 GeV for ~100 GRBs/yr, as well as accurate localization of the GLAST GRBs to enable follow-up studies.

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arXiv2001

Phase-resolved spectra of the millisecond pulsar SAX J1808.4-3658

We analyze the RXTE observations of the April 1998 outburst of SAX J1808.4-3658. We show that the soft blackbody component of the X-ray spectrum is from the hotspot on the neutron star surface, while the hard component is from Comptonization of these blackbody photons in the plasma heated by the accretion shock. The disc cannot provide enough seed photons for Comptonization. It is truncated into an optically thin flow at ~20-40 R_g by some generic mechanisms common for black holes and neutron stars. Only below the truncation radius the flow is disrupted by the magnetic field and collimated onto the surface. The pulse profiles of both spectral components imply several constraints on the geometry of the system: the inclination angle, location and size of the hotspot and the shock.

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arXiv2001

The broad band X-ray/hard X-ray spectra of accreting neutron stars

I review the energy spectra of low mass X-ray binaries (LMXBs) containing weakly magnetized accreting neutron stars (NS), emphasizing the most recent broad band (0.1-200 keV) spectral and timing observations performed by Beppo-SAX and RXTE. Drawing on the similarities between black hole candidate (BHC) and NS accretion, I discuss the accretion geometry and emission processes of NS LMXBs.

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arXiv1998

Evolution of AQL X-1 During the Rising Phase of its 1998 Outburst

We present results from 16 snapshots of Aql X-1 with RXTE during the rising phase of its recent outburst. The observations were carried out at a typical rate of once or twice per day. The source shows interesting spectral evolution during this period. Phenomenologically, it bears remarkable similarities to ``atoll'' sources. Shortly after the onset of the outburst, the source is seen to be in an ``island'' state, but with little X-ray variability. It then appears to have made a rapid spectral transition (on a time scale less than half a day) to another ``island'' state, where it evolves slightly and stays for 4 days. In this state, the observed X-ray flux becomes increasingly variable as the source brightens. Quasi-period oscillation (QPO) in the X-ray intensity is detected in the frequency range 670--870 Hz. The QPO frequency increases with the X-ray flux while its fractional rms decreases. The QPO becomes undetectable following a transition to a ``banana'' state, where the source continues its evolution by moving up and down the ``banana'' branch in the color-color diagram as the flux (presumably, the mass accretion rate) fluctuates around the peak of the outburst. Throughout the entire period, the power density spectrum is dominated by very-low frequency noises. Little power can be seen above ~1 Hz, which is different from typical ``atoll'' sources. In the ``banana'' state, the overall X-ray variability remains low (with fractional rms ~3--4%) but roughly constant. The observed X-ray spectrum is soft with few photons from above $\sim$25 keV, implying the thermal origin of the emission. The evolution of both spectral and temporal X-ray properties is discussed in the context of disk-instability models.

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arXiv1997

Simulations and Measurements of the Background Encountered by a High-Altitude Balloon-Borne Experiment for Hard X-ray Astronomy

We have modelled the hard X-ray background expected for a high-altitude balloon flight of the Energetic X-ray Telescope Experiment (EXITE2), an imaging phoswich detector/telescope for the 20--600 keV energy range. Photon and neutron-induced contributions to the background are considered. We describe the code and the results of a series of simulations with different shielding configurations. The simulated hard X-ray background for the actual flight configuration agrees reasonably well (within a factor of $\sim$ 2) with the results measured on the first flight of EXITE2 from Palestine, Texas. The measured background flux at 100 keV is $\sim$ 4 $\times$ 10$^{-4}$ counts cm$^{-2}$ s$^{-1}$ keV$^{-1}$.

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arXiv1997

Energy Spectra and High Frequency Oscillations in 4U 0614+091

We investigate the behavior of the high frequency quasi-periodic oscillations (QPOs) in 4U 0614+091, combining timing and spectral analysis of RXTE observations. The energy spectra of the source can be described by a power law (alpha ~ 2.8) and a blackbody (kT ~ 1.5), with the blackbody accounting for 10 - 20% of the total energy flux. We find a robust correlation of the frequency, nu, of the higher frequency QPO near 1 kHz with the flux of the blackbody, F_BB. The slope of this correlation, dlog(nu)/dlog(F_BB), is 0.27 to 0.37. The source follows the same relation even in observations separated by several months. The QPO frequency does not have a similarly unique correlation with the total flux or the flux of the power law component. The RMS fraction of the higher frequency QPO rises with energy from 6.8 +- 1.5 % (3-5 keV) to 21.3 +- 4.0 % (10-12 keV). For the lower frequency QPO, however, it is consistent with a constant value of 5.4 +- 0.9 %. The results may be interpreted in terms of a beat frequency model for the production of the high frequency QPOs.

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arXiv1997

Advection-Dominated Accretion Model of the Black Hole V404 Cyg in Quiescence

We have analyzed archival ASCA data on the soft X-ray transient source V404 Cyg in quiescence. We find that in the energy range 0.7 to 8.5 keV the spectrum is a hard power-law with a photon spectral index between 1.8 and 2.6 (90% confidence limits). We present a model of V404 Cyg in which the accretion flow has two components: (1) an outer thin disk with a small annular extent, and (2) a large interior region where the flow is advection-dominated. Nearly all the radiation in the infrared, optical, UV and X-ray bands is from the advection-dominated zone; the thin disk radiates primarily in the infrared where it contributes about ten percent of the observed flux. The spectrum we calculate with this model is in excellent agreement with the ASCA X-ray data presented here, as well as with previous optical data. Moreover, the fit is very insensitive to the choice of parameters such as black hole mass, orbital inclination, viscosity coefficient $α$, and magnetic field strength. We consider the success of the model to be strong support for the advection-dominated accretion paradigm, and further evidence of the black hole nature of V404 Cyg. We discuss strategies whereby systems with advection-dominated accretion could be used to prove the reality of event horizons in black holes.

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arXiv1995

Models of Quiescent Black Hole Neutron Star Soft X-Ray Transients

When the mass accretion rate onto a black hole (BH) falls below a critical rate, ${\dot M}_{crit}\sim α^2 {\dot M}_{Edd}$, accretion can occur via a hot optically thin flow where most of the dissipated energy is advected inward. We present such an advection-dominated model for the soft X-ray transient (SXT) A0620-00. This source has a puzzlingly low X-ray luminosity in quiescence, $\sim 6\times 10^{30} ~{\rm erg\,s^{-1}}$, despite a relatively high mass accretion rate $\sim10^{-10} ~M_{\odot}{\rm yr^{-1}}$ deduced from its optical flux. The accreting gas makes a transition from a standard thin disc at large radii to an advection-dominated flow at small radii. The transition occurs when the effective temperature of the thin disc is $\sim 10^4$ K. Because of the very low accretion efficiency, $\sim 10^{-3}-10^{-4}$, in the inner flow, the model fits both the optical and X-ray data. We also present models for V404 Cyg and Nova Mus 1991 in quiescence. Quiescent neutron star (NS) transients are expected to appear very different from BH systems because the advected energy is re-radiated from the NS surface whereas a BH swallows the advected energy. We discuss models for NS SXTs.

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