G. Malaguti

The XMM-Newton and BeppoSAX view of the Ultra Luminous Infrared Galaxy MKN 231

We discuss XMM-Newton and BeppoSAX observations of MKN 231, the lowest-redshift Broad Absorption Line (BAL) QSO known so far and one of the best-studied Ultra Luminous Infrared Galaxies. By combining the XMM-Newton spectral resolution and the high-energy bandpass of BeppoSAX we have been able to study in more detail than previ- ously possible its 0.2-50 keV spectral properties. The BeppoSAX PDS data unveiled, for the first time, a highly absorbed (NH ∼ 2 × 10 24 cm −2 ) power-law component. We find that: a) below 10 keV we are seeing only reprocessed radiation through reflection and/or scattering; b) the intrinsic 2-10 keV luminosity of MKN 231 is 1 +1.0 −0.5 × 10

BeppoSAX View of Radio-loud Active Galactic Nuclei

A systematic analysis of a large sample of radio-loud active galactic nuclei (AGNs) available in the BeppoSAX public archive has been performed. The sample includes 3 narrow-line radio galaxies (NLRGs), 10 broad-line radio galaxies (BLRGs), 6 steep-spectrum radio quasars (SSRQs), and 16 flat-spectrum radio quasars (FSRQs). According to the unified models, these classes correspond to objects with increasing viewing angles. As expected, the presence of a nonthermal beamed component emerges clearly in FSRQs. This class shows in fact a featureless continuum (with the exception of 3C 273) and a significantly flatter average spectral slope. However, traces of a nonthermal Doppler-enhanced radiation are elusive in the other classes. We find that the iron line equivalent widths (EWs) are generally weaker in radio-loud AGNs than in Seyfert 1 galaxies, and we confirm the presence of an X-ray Baldwin effect; that is, a decrease of EW with the 2-10 keV luminosity from Seyfert galaxies to BLRGs and quasars. Since the EW-L2-10 keV anticorrelation is present also in radio-quiet AGNs alone, this effect cannot be ascribed entirely to a strongly beamed jet component. Possible alternative interpretations are explored.

IBIS/PICsIT in-flight performances

PICsIT (Pixellated Imaging CaeSium Iodide Telescope) is the high energy detector of the IBIS telescope on-board the INTEGRAL satellite. PICsIT operates in the gamma-ray energy range between 175 keV and 10 MeV, with a typical energy resolution of 10% at 1 MeV, and an angular resolution of 12 arcmin within a100 square degree field of view, with the possibility to locate intense point sources in the MeV region at the few arcmin level. PICsIT is based upon a modular array of 4096 independent CsI(Tl) pixels,0.70 cm 2 in cross-section and 3 cm thick. In this work, the PICsIT on-board data handling and science operative modes are described. This work presents the in-flight performances in terms of background count spectra, sensitivity limit, and imaging capabilities.

X-ray evidence for a mildly relativistic and variable outflow in the luminous Seyfert 1 galaxy Mrk 509

Context. There is growing evidence for the presence of blueshifted Fe K absorption lines in a number of radio-quiet AGNs and QSOs. These may be fundamental to probe flow dynamics near supermassive black holes. Aims. Here we aim to verify and better characterise the existence of such Fe K absorption at ∼8–10 keV in the luminous Seyfert 1 galaxy Mrk 509, one of the most promising target for these studies. Methods. We present a comprehensive spectral analysis of the six XMM-Newton observations of the source (for a total of ∼200 ks), focusing on a detailed and systematic search for absorption features in the high-energy data. Results. We detect several absorption features at rest-frame energies ∼8–8.5 keV and ∼9.7 keV. The lines are consistent with being produced by H-like iron Kα and Kβ shell absorptions associated with an outflow with a mildly relativistic velocity of ∼0.14–0.2 c. The lines are found to be variable in energy and, marginally, in intensity, implying variations in either the column density, geometry and/or ionization structure of the outflow are common.

X-Ray/UV/Optical Follow-up of the Blazar PKS 2155–304 after the Giant TeV Flares of 2006 July

We present all the publicly available data, from optical/UV wavelengths (UVOT) to X-rays (XRT, BAT), obtained from Swift observations of the blazar PKS 2155-304, performed in response to the rapid alert sent out after the strong TeV activity (up to 17 crab flux level at E > 200 GeV) at the end of 2006 July. The X-ray flux increased by a factor of 5 in the 0.3-10 keV energy band and by a factor of 1.5 at optical/UV wavelengths, with roughly 1 day of delay. The comparison of the spectral energy distribution built with data quasi-simultaneous to the TeV detections shows an increase of the overall normalization with respect to archival data but only a small shift of the frequency of the synchrotron peak that remains consistent with the values reported in past observations when the TeV activity was much weaker.

Simbol-X: mission overview

Simbol-X is a hard X-ray mission, operating in the ~ 0.5-80 keV range, proposed as a collaboration between the French and Italian space agencies with participation of German laboratories for a launch in 2013. Relying on two spacecraft in a formation flying configuration, Simbol-X uses for the first time a 20-30 m focal length X-ray mirror to focus X-rays with energy above 10 keV, resulting in over two orders of magnitude improvement in angular resolution and sensitivity in the hard X-ray range with respect to non-focusing techniques. The Simbol-X revolutionary instrumental capabilities will allow us to elucidate outstanding questions in high energy astrophysics such as those related to black-holes accretion physics and census, and to particle acceleration mechanisms, which are the prime science objectives of the mission. After having undergone a thorough assessment study performed by CNES in the context of a selection of a formation flight scientific mission, Simbol-X has been selected for a phase A study to be jointly conducted by CNES and ASI. The mission science objectives, the current status of the instrumentation and mission design are presented in this paper.

XMM–Newton observations of the ultraluminous nuclear X-ray source in M 33

We present observations with XMM-Newton of M 33 X-8, the ultraluminous X-ray source (L0.5−10 keV ≈ 2×10 39 erg/s) closest to the centre of the galaxy. The best-fit model is similar to the typical model of Galactic black holes in very high state. Comparison with previous observations indicates that the source is still in a very high state after about 20 years of observations. No state transition has been observed even during the present set of XMM-Newton observations. We estimate the lower limit of the mass of the black hole >6 M� , but with proper parameters taking into account different effects, the best estimate becomes 12 M� . Our analysis favours the hypothesis that M 33 X-8 is a stellar mass black hole candidate, in agreement with the findings of other authors. In addition, we propose a different model where the high luminosity of the source is likely to be due to orientation effects of the accretion disc and anisotropies in the Comptonized emission.

In flight calibration of the ISGRI camera

ISGRI, the IBIS low energy camera (15 keV - 1 MeV) on board INTEGRAL, is the first large CdTe gamma-ray imager in orbit. We present here an overview of the ISGRI in-flight calibrations performed during the first months after launch. We discuss the stability of the camera as well as the CdTe pixels response under cosmic radiation. The energy calibrations were done using lead and tungsten fluorescence lines and the

IRAS 13197-1627 has them all : compton-thin absorption, photoionized gas, thermal plasmas and a broad Fe line

\mathrm{^{22}Na}

INTEGRAL and XMM-Newton observations of the X-ray pulsar IGR J16320-4751/AX J1631.9-4752

calibration unit. Thermal effects and charge correction algorithm are discussed, and the resulting energy resolution is presented. The ISGRI background spatial and spectral non-uniformity is also described, and some image correction results are presented.