arXiv subjects

F. Haardt

Publications and source records attributed to F. Haardt.

At least 73 records · Page 4Linked to original sources

arXiv2003

The X-ray spectrum of the black hole candidate GX339-4 in a low state

We report on four observations of the black hole candidate GX 339-4 collected in the spectral range 0.4-140 keV with the BeppoSAX satellite during 1997. All our spectra are typical of a black hole candidate in its low-hard state, i.e. are dominated by the hard tail of the emission from the corona. Although the direct emission from the accretion disk in the soft X-ray range is weak, spectra are well described only with models that take into consideration the Compton reflection of hard X-rays from the corona onto the surface of an accretion disk of non negligible extent.

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arXiv2002

A rapidly variable narrow X-ray iron line in Mkn 841

We report on the detection of a rapidly variable narrow Fe K$α$ line in Mkn 841. The source has been observed two times by XMM-Newton and simultaneously with BeppoSAX. The two observations, of about 10ks long each, were separated by $\sim$ 15 hours. The line flux reaches a maximum during the first observation and is significantly reduced in the second one. The continuum shape and flux, instead, keep roughly constant between the two pointings. Such rapid variability of a narrow (unresolved by the XMM-pn instrument) line has never been reported in the past. These results are not easily explained in the standard cold reflection model where the narrow line component is supposed to be produced far from the primary X-ray source (e.g. from the torus) and is thus not expected to vary rapidly. Different interpretations are discussed.

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arXiv2002

Long Term Spectral Variability of Seyfert Galaxies from RXTE Color-Flux Diagrams

We present results from RXTE data obtained during a systematic monitoring program of four Seyfert galaxies (NGC5548, NGC5506, MCG-6-30-15 and NGC4051). We studied the variability of three hardness ratios derived from the light curves in four energy bands. All the objects show similar spectral variations in all ratios. In order to interpret the results we computed the hardness ratios corresponding to a simple spectral model of a power law plus iron line plus reflection component, considering two possibilities: a)variations with constant line equivalent width and reflection parameter R and b) variations with constant line and reflection flux. The overall, mean observed trends can be explained by spectral slope variations and a constant flux Fe line and reflection component, although the existence of a line component which is variable on short time scales cannot be excluded. Finally, we find that the data are not consistent with an increase of R with flux for individual sources, indicating that, as a single source varies, softer spectra do not correspond to larger R values.

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arXiv2001

The optical afterglow of GRB 000911: evidence for an associated supernova?

We present photometric and spectroscopic observations of the late afterglow of GRB 000911, starting ~1 day after the burst event and lasting ~8 weeks. We detect a moderately significant re-brightening in the R, I and J lightcurves, associated with a sizable reddening of the spectrum. This can be explained through the presence of an underlying supernova, outshining the afterglow ~30 days after the burst event. Alternative explanations are discussed.

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arXiv2001

The effects of a comptonizing corona on the appearance of the reflection components in accreting black hole spectra

We discuss the effects of a comptonizing corona on the appearance of the reflection components, and in particular of the reflection hump, in the X-rays spectra of accreting black holes. Indeed, in the framework of a thermal corona model, we expect that part (or even all, depending on the coronal covering factor) of the reflection features should cross the hot plasma, and thus suffer Compton scattering, before being observed. We have studied in detail the dependence of these effects on the physical (i.e. temperature and optical depth) and geometrical (i.e. inclination angle) parameters of the corona, concentrating on the slab geometry . Due to the smoothing and shifting towards high energies of the comptonized reflection hump, the main effects on the emerging spectra appear above 100 keV. We have also investigated the importance of such effects on the interpretation of the results obtained with the standard fitting procedures. We found that fitting Comptonization models, taking into account comptonized reflection, by the usual cut-off power law + uncomptonized reflection model, may lead to an underestimation of the reflection normalization and an overestimation of the high energy cut-off. We discuss and illustrate the importance of these effects by analysing recent observational results as those of the galaxy NGC 4258. We also find that the comptonizing corona can produce and/or emphasize correlations between the reflection features characteristics (like the iron line equivalent width or the covering fraction) and the X-ray spectral index similar to those recently reported in the literature. We also underline the importance of these effects when dealing with accurate spectral fitting of the X-ray background.

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arXiv2001

A measurement of the broad-band spectrum of XTE J1118+480 with BeppoSAX and its astrophysical implications

We report on results of a target of opportunity observation of the X-ray transient XTE J1118+480 performed on 2000 April 14-15 with the Narrow Field Instruments (0.1-200 keV) of the SAX satellite. The measured spectrum is a power law with a photon index of ~1.7 modified by an ultrasoft X-ray excess and a high-energy cutoff above ~100 keV. The soft excess is consistent with a blackbody with temperature of ~40 eV and a low flux, while the cut-off power law is well fitted by thermal Comptonization in a plasma with an electron temperature of 100 keV and an optical depth of order of unity. Consistent with the weakness of the blackbody, Compton reflection is weak. Though the data are consistent with various geometries of the hot and cold phases of the accreting gas, we conclude that a hot accretion disk is the most plausible model. The Eddington ratio implied by recent estimates of the mass and the distance is about 10^{-3}, which may indicate that advection is probably not the dominant cooling mechanism. We finally suggest that the reflecting medium has a low metallicity, consistent with location of the system in the halo.

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arXiv2001

BeppoSAX observations of Mrk 841 and Mrk335

We present and discuss BeppoSAX observations of Mrk841 and Mrk335, two Seyfert 1 galaxies in which previous observations have established the presence of soft excesses. We confirm the soft excess in both sources, even if for Mrk~841 a warm absorber provides a fit almost as good as the one with a true excess. As far as the hard X-ray continuum is concerned, a Comptonization model provides a fit as good as a power law and a physically sound solution for Mrk841. For Mrk335, the Comptonization model gives a result which is somewhat better on statistical ground, but rather problematic on physical ground. The most interesting results regard the reprocessing components. For Mrk841 we find a very large reflection continuum but an almost normal iron line equivalent width even if, within the errors, a solution in which both components are a factor ~2 larger than expected for an accretion disc is still marginally acceptable. If this is the case, an anisotropy of the primary emission seems the best explanation. On the contrary, in Mrk335 we find a very large iron line EW but a reflection component not accordingly large. In this case, the best solution seems to be in terms of reflection from an ionized disc.

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arXiv2001

Testing Comptonisation models using BeppoSAX observations of Seyfert 1 galaxies

We have used realistic Comptonization models to fit high quality BeppoSAX data of 6 Seyfert galaxies. Our main effort was to adopt a Comptonization model taking into account the anisotropy of the soft photon field. The most important consequence is a reduction of the first scattering order, which produces a break (the so-called anisotropy break) in the outgoing spectra. The physical parameters of the hot corona (i.e. the temperature and optical depth) obtained fitting this class of models to broad band X-ray spectra are substantially different from those derived fitting the same data with the power law + cut-off model commonly used in the literature. In particular, our best fits with Comptonization models in slab geometry give a temperature generally much larger and an optical depth much smaller than derived from the power law + cut-off fits, using standard Comptonization formulae. The estimate of the reflection normalization is also larger with the slab corona model. For most objects of our sample, both models give Compton parameter values larger than expected in a slab corona geometry, suggesting a more ``photon starved'' X-ray source configuration. Finally, the two models provide different trends and correlation between the physical parameters which has major consequences for the physical interpretation of the data.

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arXiv2001

Constraints on the High Energy Continuum of Seyfert galaxies from RXTE Color-Color and Color-Flux Diagrams

We report on some results from a three-year program of RXTE observations of 4 Seyfert galaxies: NGC 4051, NGC 5548, MCG-6-30-15 and NGC 5506. We focus here on color-color and color-flux diagrams obtained using the count-rates of the PCA instrument in different energy ranges: 3--5, 5--7 and 7--10 keV. The data of the different sources show interesting trends in the different color-color and color-flux planes. These trends are quite similar from one source to the other, even in the case of the narrow line Seyfert 1 NGC 4051 which exhibits strong flux and spectral variability. We discuss these results in term of a simple spectral model: a power law with high energy cut-off + reflection + Iron line, with the scope of understanding the relations between the observed variations of different components and the physical causes of the variability.

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arXiv2001

Testing Comptonization models using BeppoSAX observations of Seyfert 1 galaxies

We used high quality BeppoSAX data of 6 Seyfert galaxies to test realistic thermal Comptonization models. Our main effort was to adopt a Comptonization model taking into account the anisotropy of the soft photon field. The best fit parameter values of the temperature and optical depth of the corona and of the reflection normalization obtained fitting this class of models to the data are substantially different from those derived fitting the same data with the power law + cut--off model commonly used. The two models also provide different trends and correlation between the physical parameters, which has major consequences for the physical interpretation of the data

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arXiv2000

Broad-band X-ray spectra of the persistent black hole candidates LMC X-1 and LMC X-3

We report on observations of the two persistent black hole candidates LMC X-3 and LMCX-1 performed with \BS in October 1997. The flux of LMC X-1 was possibly measured up to 60 keV, but there is a possible confusion with PSR 0540-69. Fits with an absorbed multicolor disk black body are not satisfactory, while the superposition of this model with a power law is acceptable. The sources showed little variations during the observations. However in LMC X-1 some X-ray color dependence on intensity is apparent, indicating a hardening of the spectrum in the second half of the observation. The inner disk radius and temperature change, featuring the same (anti)correlation found in {\it RXTE} data (Wilms et al. 2000). QPOs were searched for. In LMC X-3 none was detected; in LMCX-1 a 3 sigma upper (9% rms) limit is given at 0.07 Hz, the frequency of the QPO discovered with Ginga.

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arXiv2000

Broad band spectrum of Cygnus X-1 in two spectral states with BeppoSAX

We report on the 0.5--200 keV spectral properties of Cyg X-1 observed at different epochs with the Narrow Field Instruments of the BeppoSAX satellite. The source was in its soft state during the first observation of 1996 June. In the second observation of 1996 September, the source had parameters characteristic to its hard state. A soft X-ray excess, a broad Fe K$α$ line and Compton reflection are clearly detected in both states. The soft-state broad-band continuum is well modeled by a disk blackbody (accounting for the soft excess) and Compton upscattering of the disk photons by a hybrid, thermal/non-thermal, plasma, probably forming a corona above the disk (also giving rise to the Compton-reflection component). In the hard state, the primary hard X-ray spectrum can be well modeled by Compton upscattering of a weak blackbody emission by a thermal plasma at a temperature of $\sim 60$ keV. The soft excess is then explained by thermal Comptonization of the same blackbody emission by another hot plasma cloud characterized by a low value of its Compton parameter. Finally, we find the characteristic ratio of the bolometric flux in the soft state to that in the hard state to be about 3. This value is much more compatible with theories of state transitions than the previously reported (and likely underestimated) value of 1.5.

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arXiv2000

A Self-Consistent Test of Comptonisation Models Using Bepposax Observations of Seyfert Galaxies

We test accurate models of Comptonisation spectra over BeppoSAX observations of Seyfert galaxies focusing on the long look at NGC 5548. The hot plasma temperature derived with these models is significantly higher than that obtained fitting the same data with a power law plus high energy cut off model for the continuum. This is due to the fact that in anisotropic geometries Comptonisation spectra show "intrinsic" curvature which moves the fitted high energy cut-off to higher energies. We also show preliminary results of our analysis of a sample of 5 other Seyfert galaxies.

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arXiv2000

BeppoSAX observations of Mrk 509 and MCG+8-11-11

BeppoSAX observations of the Seyfert galaxies Mrk 509 and MCG+8-11-11 are presented. Earlier evidence of a soft excess in Mrk 509 is confirmed. This excess is found to be better represented by a power law than by a black body: with a photon slope of 2.5, its extrapolation matches the flux recorded in the far UV. An ASCA observation, which appeared to exclude the presence of the excess while showing instead evidence of a warm absorber, turns out to be compatible with the coexistence of the excess seen with BeppoSAX and of the warm absorber. The hard power law of Mrk 509 is seen for the first time to be affected by a cut-off at high energies, with an e-folding energy of about 70 keV. In MCG+8-11-11 the cut-off is found at about 170 keV, consistent within the combined errors with a previous estimate from a ASCA+OSSE/CGRO observation. In both objects the reflection component is clearly detected. In Mrk 509 its strength, together with that of the iron K line, indicates a solid angle Omega, subtended by the reprocessing gas in the accretion disk, much less than 2pi, but lacking a valid constraint on the inclination angle this evidence is not as convincing as that found with BeppoSAX in IC 4329A. In MCG+8-11-11 the same parameters are instead consistent with Omega=2pi, but the comparison with an ASCA observation, when the flux level was about 2.5 times weaker, suggests that a substantial fraction of the angle might be associated with gas farther out than the accretion disk.

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arXiv2000

A self-consistent test of Comptonization models using a long BeppoSAX observation of NGC 5548

We test accurate models of Comptonization spectra over the high quality data of the BeppoSAX long look at NGC 5548. The data are well represented by a plane parallel corona with an inclination angle of 30$^{\circ}$, a soft photon temperature of 5 eV and a hot plasma temperature and optical depth of $kT_{\rm e}\simeq$ 360 keV and $τ\simeq$ 0.1, respectively. If energy balance applies, such values suggest that a more ``photon-starved'' geometry (e.g. a hemispheric region) is necessary. The spectral softening detected during a flare, appears to be associated to a decrease of the heating-to-cooling ratio, indicating a geometric and/or energetic modification of the disk plus corona system. The hot plasma temperature derived with the models above is significantly higher than that obtained fitting the same data with a power law plus high energy cut off model for the continuum. This is due to the fact that in anisotropic geometries Comptonization spectra show "intrinsic" curvature which moves the fitted high energy cut-off to higher energies.

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arXiv2000

Testing Comptonizing coronae on a long BeppoSAX observation of the Seyfert 1 galaxy NGC 5548

We test accurate models of Comptonization spectra over the high quality data of the BeppoSAX long look at NGC 5548, allowing for different geometries of the scattering region, different temperatures of the input soft photon field and different viewing angles. We find that the BeppoSAX data are well represented by a plane parallel or hemispherical corona viewed at an inclination angle of 30$^{\circ}$. For both geometries the best fit temperature of the soft photons is close to 15$^{+3}_{-9}$ eV. The corresponding best fit values of the hot plasma temperature and optical depth are $kT_{\rm e}\simeq$ 250--260 keV and $τ\simeq$ 0.16--0.37 for the slab and hemisphere respectively. These values are substantially different from those derived fitting the data with a power-law + cut off approximation to the Comptonization component ($kT_{\rm e}\lta$ 60 keV, $τ\simeq$ 2.4). This is due to the fact that accurate Comptonization spectra in anisotropic geometries show "intrinsic" curvature which reduces the necessity of a high energy cut-off. The Comptonization parameter derived for the slab model {is} larger than predicted for a two phase plane parallel corona in energy balance, suggesting that a more ``photon-starved'' geometry is necessary. The spectral softening detected during a flare which occurred in the central part of the observation corresponds to a decrease of the Comptonization parameter, probably associated with an increase of the soft photon luminosity, the {hard} photon luminosity remaining constant.

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arXiv2000

Gamma-loud quasars: a view with BeppoSAX

We present $Beppo$SAX observations of the $γ$-ray emitting quasars 0836+710, 1510-089 and 2230+114. All the objects have been detected in the PDS up to 100 keV and have extremely flat power-law spectra above 2 keV ($α_x$=0.3--0.5). 0836+710 shows absorption higher than the galactic value and marginal evidence for the presence of the redshifted 6.4 keV Iron line. 1510-089 shows a spectral break around 1 keV, with the low energy spectrum steeper ($α_l$=1.6) than the high energy power-law ($α_h$=0.3). The data are discussed in the light of current Inverse Compton models for the high energy emission.

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arXiv2000

The X-ray spectrum of a disk illuminated by ions

The X-ray spectrum from a cool disk embedded in an ion supported torus is computed. The interaction of the hot ions with the disk increases the hard X-ray luminosity of the system}. A surface layer of the disk is heated by the protons from the torus. The Comptonized spectrum produced by this layer has a shape that depends only weakly on the incident energy flux and the distance from the accreting compact object. It consists of a `blue bump' of unComptonized soft photons and a flat high energy tail, reminiscent of the observed spectra. The hard tail becomes flatter as the thermalization depth in the cool disk is increased. Further evidence for ion illumination are the Li abundance in the secondaries of low mass X-ray binaries and the 450 keV lines sometimes seen in black-hole transient spectra.

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