Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://hea.iki.rssi.ru/integral06/fregistration.bib_~ Äàòà èçìåíåíèÿ: Wed Mar 21 23:31:55 2007 Äàòà èíäåêñèðîâàíèÿ: Mon Oct 1 21:49:13 2012 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: total solar eclipse

@inproceedings {Sergei_Grebenev,
email={sergei@hea.iki.rssi.ru},
first_name={Sergei},
last_name={Grebenev},
affiliation={Space Research Institute, Russian Academy of Sciences},
address={Profsoyuznaya st., 84/32, Moscow, 117997},
presentation_type={oral},
presentation_number={1},
presentation_panel={E9},
title={Fast X-ray transients observed with INTEGRAL},
authors={S.A.Grebenev, R.A.Sunyaev},
abstract={During three and a half years of operation INTEGRAL discovered more than 100 new hard X-ray sources that significantly (by 40-50 percents) enlarges the amount of such sources detected in previous experiments. Although sources of different types are obviously present in this sample, two source populations certainly escape: the strongly absorbed sources (with a very low flux in the standard X-ray band that made them unobservable in X-ray surveys) and the short-living transients appearing on the sky for only a few hours (that made them again very difficult for observations). Outbursts of the latter sources are shorter than the viscous time scale ($>1.4$ days) characterizing the transfer of matter in the standard accretion disk (if the disk gets matter through the inner Lagrangian point). However, the viscous time scale could be shorter if the disk is formed from the companion stellar wind or if it is not formed at all. Recent optical identification of several fast transients with OB-supergiants supports such point of view. In this report we describe properties of several fast transients discovered or detected during outbursts by INTEGRAL in course of its ultra-deep Open Program observations of the Galactic center field. We consider conditions for the accretion disk formation in these systems in sight of constraints following from the observations. We discuss mechanisms responsible for the outbursts, in particular, unsteady accretion from the clumpy stellar wind, and propose as well a new reliable mechanism.},
persons_number={0},
date={01Mar06 21:16:50},
date={19Apr06 16:53:18}
}

@inproceedings {Sergey_Tsygankov,
email={st@hea.iki.rssi.ru},
first_name={Sergey},
last_name={Tsygankov},
affiliation={Space Research Institute RAS},
address={Profsoyuznaya 84/32, Moscow, 117997 Russia},
presentation_type={poster},
presentation_number={1},
presentation_panel={G6},
title={Pulse profiles and cyclotron line energy dependence on X-ray pulsars luminosity},
authors={S. Tsygankov, A. Lutovinov, E. Churazov, R. Sunyaev},
abstract={We present the results of a broad band (3-100 keV) observations of X-ray pulsars with the INTEGRAL and RXTE observatories. We concentrate on the luminosity and energy dependence of the pulse profile and on the variations of the cyclotron line energy. In V0332+53 the line energy varies linearly with the source luminosity, while in 4U0115+63 the behavior is more complicated. Strong variations of the pulse profile shape with energy and the source intensity were found for several pulsars, including V0332+53 and 4U0115+63. In V0332+53 the changes of the pulse profile near the cyclotron line are especially drastic. We discuss these results and possible emission mechanisms in terms of the theoretical models of accreting pulsars.},
persons_number={0},
pdate={28Feb06 20:12:12},
date={19Apr06 17:51:49}
}

@inproceedings {Patrick_Sizun,
email={sizun@cea.fr},
first_name={Patrick},
last_name={Sizun},
affiliation={CEA/SAp},
address={Orme des Merisiers, 91191 Gif-sur-Yvette Cedex, France},
presentation_type={poster},
presentation_number={1},
presentation_panel={A0},
title={On the injection energies of positrons at the Galactic centre},
authors={P. Sizun, M. Cass\'e, S. Schanne},
abstract={The positron annihilation line at 511 keV in the Galaxy has been observed by INTEGRAL/SPI for more than 3 years. The spectrometer confirmed this annihilation takes place mainly in the Galactic bulge with an extension of 8 degrees FWHM and a line flux of $10^3$ ph cm$^{-2}$ s$^{-1}$, corresponding to about $10^{43}$ positrons annihilating every second. None of the classic astrophysical scenarii -- supernovae, black holes, hypernovae -- has yet been able to qualify as the source of the annihilating positrons, as they failed to account either for the flux or for the morphology of the emission. Though new considerations about the transport of positrons between their production and their annihilation (Prantzos 2005) recently revived some of those hypotheses, more exotic sources of positrons such as those involving dark matter remain topical. Before 2004, heavy dark matter particles had been excluded from the list of candidate sources of positrons because of the direct or indirect radiations incidental to the decay of the dark matter particle and to the positron production. Such radiations were incompatible with observations. Boehm et al. (2004) suggested a new dark matter candidate in the form of a light particle (1-100 MeV), whose decay would not be accompanied by the emission of any radiation or particles other than positrons and electrons. Since then, some authors tried to disallow this light dark matter scenario by modelling indirect radiations, such as internal bremsstrahlung (Beacom et al. 2005) and in-flight annihilation (Beacom \& Y\"uksel 2005) and by comparing them to observations. In this contribution, we will review the various observational constraints relative to energy losses by a positron during its thermalization phase through the ionisation, inverse Compton, bremsstrahlung, synchrotron, in-flight annihilation channels. We will discuss the detectability of these effects by INTEGRAL and other experiments, and their consequences on the possible injection energies of the positrons responsible for the 511 keV line and thus on the mass range of a potential dark matter candidate. },
persons_number={0},
pdate={28Feb06 18:39:05},
date={19Apr06 17:52:51}
}

@inproceedings {Mikhail_Revnivtsev,
email={mikej@hea.iki.rssi.ru},
first_name={Mikhail},
last_name={Revnivtsev},
affiliation={IKI, Moscow; MPA, Garching},
address={},
presentation_type={oral},
presentation_number={1},
presentation_panel={C2},
title={Origin of the Galactic ridge X-ray emission: puzzle solved?},
authors={},
abstract={Origin of the Galactic ridge X-ray emission (GRXE) was a long standing problem of X-ray astronomy. Explainations of the ridge emission by emission of a hot thermal plasma or by interaction of cosmic rays with interstellar matter were connected with serious problems. Latest studies of the ridge emission with highest sensitivity X-ray telescopes (like CHANDRA) have not provided conclusive answer. We have studied the morphology of the Galactic ridge X-ray emission with Rossi Explorer and showed that the GRXE contains both disk and bulge/bar components, which parameters very well agree with those of known stellar Galactic components. We have showed that the GRXE volume emissivity well traces the stellar mass density in the Galaxy. Average Galactic unit stellar mass emissivity of the GRXE can be easily explained by average unit stellar mass X-ray emissivity in the Solar neighbourhood. Dominant contributors to the GRXE are accreting white dwarfs and coronally active stars. Weighted spectrum of known types of sources well agree with the spectrum of GRXE in the energy band 3-100 keV.},
persons_number={0},
pdate={17.02.06 16:23:57},
date={19Apr06 18:03:07}
}

@inproceedings {Ivan_Chelovekov,
email={chelovekov@hea.iki.rssi.ru},
first_name={Ivan},
last_name={Chelovekov},
affiliation={Space Research Institute, Moscow, Russia},
address={Profsoyuznaya 84/32, Moscow 117997 Russia},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={Hard X-ray bursts detected by the IBIS/INTEGRAL telescope in 2003-2004},
authors={I.V. Chelovekov, S.A. Grebenev, R.A. Sunyaev},
abstract={We present the results of our search for X-ray bursts in the data of the first one and a half years of IBIS/INTEGRAL work on the orbit (10.02.2003 --- 02.07.2004). Scaning of the 15-25 keV lightcurves measured with the IBIS/ISGRI detector has revealed 1077 bursts with durations ranging from $\sim5$ to $\sim500$ s. All the events passed quite a high statistical criterion, allowing only a 20\% chance for a false burst to be detected as a true one in the whole time series. In total 115 bursts were localized and all of them but one were identified with known persistant or transient X-ray sources (96 --- with known X-ray bursters). Among the rest of detected events some were related to cosmic $\gamma$-ray bursts and solar flares passing through a telescope cover. One of the localized bursts was related to none of the known sources, but originated from a new burster with a very low persistent luminosity. We named it \mbox{IGR J17364-2711}. All the information on the localized bursts observed from X-ray bursters is collected in a burst catalogue. It is worth mentioning that 61 of the observed bursts originated from one X-ray burster --- \mbox{GX354-0}. This fact allowed us to build and investigate statistical distributions of bursts from this source on its duration, peak flux and reccurence period. Some of the identified bursts were also observed with the JEM-X/INTEGRAL X-ray monitor allowing lightcurves in the standard X-ray band (3--20 keV) to be built.},
persons_number={0},
pdate={28Feb06 17:28:23},
date={19Apr06 18:13:19}
}

@inproceedings {Sandrine_Deluit,
email={Sandrine.Deluit@cesr.fr},
first_name={Sandrine},
last_name={Deluit},
affiliation={Centre d'Etude Spatiale des Rayonnements (C.E.S.R)},
address={9 av. du Colonel Roche, 31028 Toulouse, France},
presentation_type={poster},
presentation_number={2},
presentation_panel={D0},
title={INTEGRAL contribution to the AGNs study},
authors={S. Deluit, E. Jourdain, J. Malzac et al.},
abstract={Through the study of several Active Galactic Nuclei (AGN) observed by INTEGRAL, we present a view of the IBIS and SPI contribution to the understanding of such extragalactic compact objects. ISGRI allows spectral (primary continuum, reflection, cutoff) and temporal (variability over short and long timescales) analyses of their high energy emission. The spectrometer SPI gives a continuous view of the X to gamma ray emission in order to investigate the presence of spectral signatures (such cutoff or break) above 200 keV. The ISGRI and SPI complementarity thus provides us a powerful tool to study the characteristics and the processes related to the hard X/gamma ray emission of a sample of AGN, we review the results obtained. },
persons_number={0},
pdate={28Feb06 17:10:36},
date={19Apr06 18:20:03}
}

@inproceedings {Olivia_Tsang,
email={olivia.tsang@mpi-hd.mpg.de},
first_name={Olivia},
last_name={Tsang},
affiliation={Max Planck Institute for Nuclear Physics},
address={Saupfercheckweg 1, 69117 Heidelberg, Germany},
presentation_type={poster},
presentation_number={1},
presentation_panel={D0},
title={Brightness temperature and circular polarisation in extra-galactic radio sources},
authors={J. G. Kirk and O. Tsang},
abstract={Many extra galactic radio sources show rapid variability, which implies very high brightness temperatures (TB) well over $10^{12}$ K, and high degrees of circular polarisation (CP) at the percent level. These results are well over the limits imposed by standard synchrotron models that assume a power law electron distribution. We examined the synchrotron and inverse Compton radiation from a mono-energetic electron distribution. The model gives TB of $10^{13}$ to $10^{14}$ K for moderate ($\sim10$) Doppler boosting factors, together with intrinsic degrees of CP of 1 to a few percent. I will present the constraints on TB and degree of CP of this model, and the synchrotron and inverse Compton emission predicted by this model, which gives a spectrum proportional to frequency to the 1/3rd power between radio and infra-red frequencies, and in gamma-ray between MeV to GeV. I will show that an estimate of the gamma-ray flux using published observations is above the detection threshold of the instruments on board INTEGRAL.},
persons_number={0},
pdate={28Feb06 13:18:52},
date={19Apr06 18:38:45}
}

@inproceedings {Pierre_Jean,
email={pierre.jean@cesr.fr},
first_name={Pierre},
last_name={Jean},
affiliation={Centre d'Etude Spatiale des Rayonnements - Toulouse},
address={CESR, CNRS/UPS, B.P. 4346, 31028 Toulouse Cedex 4, France},
presentation_type={poster},
presentation_number={1},
presentation_panel={A0},
title={Positron annihilation radiation fluxes, light curves, and spectra from misaligned microquasars},
authors={},
abstract={We consider nearby `misaligned'´ microquasars, where the jets are inclined substantially enough toward the plane of orbit to make them occasionally hit the atmosphere of the companion star. Assuming that microquasar jets do eject substantial quantities of positrons (see Guessoum, Jean, and Prantzos, this workshop), these systems would represent interesting annihilation point sources, for which we determine the resulting flux and the corresponding light curve, as well as the line's spectral profile. For these calculations, a detailed treatment of the physical processes undergone by the positrons in the atmosphere of the companion star is performed. We discuss the possibility of detection of such point sources by future instruments.},
persons_number={0},
pdate={28Feb06 07:54:35},
date={19Apr06 19:35:15}
}

@inproceedings {Julien_Malzac,
email={malzac@cesr.fr},
first_name={Julien},
last_name={Malzac},
affiliation={CESR (CNRS/UPS/OMP)},
address={9 av du colonel Roche, BP4346, 31028 Toulouse, France BP4346 Cedex 4},
presentation_type={poster},
presentation_number={1},
presentation_panel={F0},
title={A mini-state transition in Cygnus X-1},
authors={},
abstract={I will present the results of an INTEGRAL observation of Cygnus X-1 in an intermediate state. During our 4 days long observation, the source exhibited a strong variability. A principal component analysis demonstrates that most of this variability occurs through 2 independent modes. The first mode consists in changes in the overall luminosity on time scales of hours with almost constant spectra. We associate this mode to variations of the dissipation rate in the corona, possibly associated with magnetic flares. The second variability mode consists in a pivoting of the spectrum around 10 keV. It acts on a longer time-scale: initially soft, the spectrum hardens in the first part of the observation and then softens again. This pivoting pattern is strongly correlated with the radio (15 GHz) emission: radio fluxes are stronger when the INTEGRAL spectrum is harder. We propose that the pivoting mode represents a mini state transition from a nearly soft state to a nearly hard state, and back. This mini-transition would be caused by changes in the soft cooling photons flux in the hot comptonising plasma, associated with an increase of the temperature of the geometrical thin disc. This interpretation suggests that during state transitions the radio jet power anti-correlates with thermal disc emission while the comptonised hard X-ray flux seems to vary independently. Our results also indicate a radiatively inefficient accretion flow in the hard state. },
persons_number={0},
pdate={01Mar06 20:37:47},
date={19Apr06 19:37:36}
}

@inproceedings {Askar_Ibragimov,
email={askar.ibragimov@oulu.fi},
first_name={Askar},
last_name={Ibragimov},
affiliation={Kazan State University, Russia; University of Oulu, Finland},
address={Astronomy Division, PO Box 3000, FIN-90014 University of Oulu, Finland},
presentation_type={poster},
presentation_number={1},
presentation_panel={F0},
title={Superorbital variability in Cyg X-1 galactic black hole source},
authors={A. Ibragimov, A. Zdziarski and J. Poutanen },
abstract={The well-known black hole source Cyg X-1 has been continiously observed by the RXTE satellite during last 10 years, that leads to very large amount of observed data. One of the particular observation properties of the source is the superorbital variability with the period of 152 days. This periodicity is believed to be caused by the disk precession, and our work aims to investigate this hypothesis. Using both phenomenological and physical approaches, we determin the physical and geometrical parameters (inclination and precession angles, the emission pattern) that reproduce the observed flux variations. Our main finding is that the orbital modulation amplitude apparently has a connection with the superorbital phase. This fact provides a strong support in favour of explanation of superorbital variations with changes in the source geometry. },
persons_number={0},
pdate={28Feb06 20:06:05},
date={19Apr06 19:38:45}
}

@inproceedings {Pierre_Jean,
email={jean@cesr.fr},
first_name={Pierre},
last_name={Jean},
affiliation={C.E.S.R.},
address={9 av colonel Roche, 31028 Toulouse, France },
presentation_type={oral},
presentation_number={2},
presentation_panel={A4},
title={Spectral analysis of the Galactic positron-electron annihilation emission measured with SPI/INTEGRAL},
authors={},
abstract={We present a spectral analysis of the Galactic positron-electron annihilation emission. This analysis is based on $\sim2.5$ years of measurements made with the spectrometer SPI of the INTEGRAL mission. The Galactic bulge annihilation emission can be modelled by the sum of a narrow and a broad 511 keV line plus an ortho-positronium continuum. The 511 keV line and the ortho-positronium continuum emissions from the Galactic disk are significantly detected. Their characteristics are presented and discussed. },
persons_number={0},
pdate={28Feb06 23:01:07},
date={19Apr06 19:39:54}
}

@inproceedings {Nidhal_Guessoum,
email={nguessoum@aus.edu},
first_name={Nidhal},
last_name={Guessoum},
affiliation={American University of Sharjah},
address={Physics Dept, PO Box 26666, Sharjah, UAE},
presentation_type={oral},
presentation_number={1},
presentation_panel={A8},
title={Microquasars' contribution to the galactic positron annihilation radiation},
authors={},
abstract={Microquasars are by definition compact objects that frequently eject matter through their jets. Whether the jet content is leptonic or hadronic or a combination of both is, at present, uncertain and model-dependent. Assuming the jets are not purely hadronic, various models and methods allow one to estimate either the `typical´ microquasar' or the global galactic microquasar population's positron emissivity and thus see whether such a population (currently estimated at $\sim100$ in the Galaxy, Paredes 2005) would constitute a substantial contribution to the 511 keV annihilation flux measured by INTEGRAL/SPI and other instruments. Furthermore, one can attempt to compare the spatial distribution of Galactic microquasars (based on the scarce available data on the two dozen sources known today) and the spatial distribution of the annihilation flux as inferred by INTEGRAL/SPI. We estimate the production rate of positrons in microquasars, both by simple energy considerations and in the framework of various proposed models. We find that the collective emissivity of the annihilation radiation produced by Galactic microquasars might constitute a substantial contribution to the annihilation flux measured by INTEGRAL/SPI. The spatial distribution of microquasars leads to a Bulge/Disk ratio that is somewhat smaller than the lower limit inferred from INTEGRAL/SPI data. We stress that these results, although encouraging, suffer from significant uncertainties in our present knowledge of microquasar properties and jet physics.},
persons_number={0},
pdate={28Feb06 07:52:11},
date={19Apr06 19:40:25}
}

@inproceedings {Vincent_Lonjou,
email={lonjou@cesr.fr},
first_name={Vincent},
last_name={Lonjou},
affiliation={Centre d'Etude Spatiale des Rayonnements},
address={9 avenue du Colonel Roche 31028 Toulouse, France},
presentation_type={poster},
presentation_number={1},
presentation_panel={A0},
title={Status of the INTEGRAL/IBIS 511 keV line analysis},
authors={},
abstract={We report on the study of the 511 keV annihilation line with the imager IBIS onboard INTEGRAL after about 2 years of observations. In particular, we make a systematic analysis of IBIS data using the standard pipeline. At the same time, we use a ``light bucket analysis'' to detect the Galactic Centre extended emission and to optimise the background modelling. The status of the two methods are reported.},
persons_number={4},
pdate={01Mar06 18:51:24},
date={19Apr06 19:44:15}
}

@inproceedings {Carlo_Ferrigno,
email={ferrigno@ifc.inaf.it},
first_name={Carlo},
last_name={Ferrigno},
affiliation={IASF-INAF Palermo},
address={via Ugo la Malfa 153 I-90146 Palermo, Italy},
presentation_type={poster},
presentation_number={2},
presentation_panel={G0},
title={Similarities and differences in high mass X-ray binary pulsar pulse profiles},
authors={},
abstract={We present the timing analysis of several high mass X-ray binary pulsars observed with INTEGRAL. We show the background subtracted pulse profiles in several energy ranges and make a comparative study of their evolution with energy. We also study the evolution of the spectra with phase, comparing the results for the different sources.},
persons_number={1},
pdate={01Mar06 15:01:02},
date={19Apr06 19:47:25}
}

@inproceedings {Carlo_Ferrigno,
email={ferrigno@ifc.inaf.it},
first_name={Carlo},
last_name={Ferrigno},
affiliation={IASF-INAF Palermo},
address={via Ugo la Malfa 153},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={INTEGRAL observation of 4U~0115+634 in outburst},
authors={},
abstract={We present the phase resolved spectroscopy of the X-ray binary pulsar 4U~0115+634 observed by INTEGRAL during the outburst occured in September 2004. Combining JEM-X and ISGRI spectra we obtain a broad band continuum from 3~keV to 100~keV in which four Cyclotron resonant scattering absorption features are present. We perform analysis of both the continuum and the cyclotron lines prameter as function of phase and interpret the results under the theory of radiation transfer in highly magnetized plasma.},
persons_number={1},
pdate={01Mar06 14:58:45},
date={19Apr06 19:48:19}
}

@inproceedings {Ilfan_Bikmaev,
email={Ilfan.Bikmaev@ksu.ru},
first_name={Ilfan},
last_name={Bikmaev, Nail Sakhibullin},
affiliation={Dept. of Astronomy, Kazan State University},
address={Kremlevskaya Str., 18, Kazan, Russia},
presentation_type={poster},
presentation_number={1},
presentation_panel={D0},
title={Optical identifications of INTEGRAL/RXTE sources with 1.5-m optical telescope RTT150},
authors={I.Bikmaev, R.Sunyaev, M.Revnivtsev, R.Burenin, N.Sakhibullin},
abstract={We present the first results of a campaign to optically identify X-Ray sources discovered in the all-sky surveys of the INTEGRAL and RXTE observatories. Optical observations have been made with 1.5-m Russian-Turkish telescope equipped with CCD-photometer and TFOSC instrument. Among dozen fields with unidenfied sources we have found six earlier unknown nearby active galactic nuclei ($z < 0.1$) and two close binary systems - intermediate polars. Main spectral parameters and physical properties of the new discovered sources are discussed.},
persons_number={0},
pdate={28Feb06 20:10:48},
date={19Apr06 19:58:09}
}

@inproceedings {Diego_Gotz,
email={diego.gotz@cea.fr},
first_name={Diego},
last_name={Gotz},
affiliation={SAP/CEA},
address={Orme des Merisiers, Bat. 709, 91191 Gif sur Yvette, France},
presentation_type={oral},
presentation_number={1},
presentation_panel={I2},
title={INTEGRAL and magnetars},
authors={D. G\"otz, S. Mereghetti, K. Hurley, I.F. Mirabel, G. Weidenspointner, A. von Kienlin, A. Rau, A. Tiengo, P. Esposito},
abstract={Thanks to INTEGRAL long exposures of the Galactic Plane, the two brightest Soft Gamma-Ray Repeaters, SGR 1806-20 and SGR 1900+14, have been monitored and studied in detail for the first time at hard-X/soft-gamma rays. SGR 1806-20, lying close to the Galactic Centre, and being very active in the past two years, has provided a wealth of new INTEGRAL results, which we will review here: more than 300 short bursts have been observed from this source and their characteristics have been studied with unprecedented sensitivity in the 15-200 keV range. A hardness-intensity anticorrelation within the bursts has been discovered and the overall Number-Intensity distribution of the bursts has been determined. The increase of its explosive activity eventually led to the December 2004 Giant Flare for which a possible soft gamma-ray ($>80$ keV) early afterglow has been detected with INTEGRAL. The deep observations allowed us to discover the persistent emission in hard X-rays (20-150 keV) from 1806-20 and 1900+14, the latter being in quiescent state, and to directly compare the spectral characteristics of all Magnetars (two SGRs and three Anomalous X-ray Pulsars) detected with INTEGRAL.},
persons_number={0},
pdate={17.02.06 17:12:26},
date={19Apr06 20:01:27}
}

@inproceedings {Nail_Sakhibullin,
email={Nail.Sakhibullin@ksu.ru},
first_name={Nail},
last_name={Sakhibullin},
affiliation={Dept. of Astronomy, Kazan State University},
address={Kremlevskaya Str., 18, Kazan, Russia},
presentation_type={none},
presentation_number={1},
presentation_panel={D0},
title={Optical identifications of INTEGRAL/RXTE sources with 1.5-m optical telescope RTT150},
authors={I.Bikmaev, R.Sunyaev, M.Revnivtsev, R.Burenin, N.Sakhibullin},
abstract={We present the first results of a campaign to optically identify X-Ray sources discovered in the all-sky surveys of the INTEGRAL and RXTE observatories. Optical observations have been made with 1.5-m Russian-Turkish telescope equipped with CCD-photometer and TFOSC instrument. Among dozen fields with unidenfied sources we have found six earlier unknown nearby active galactic nuclei ($z < 0.1$) and two close binary systems - intermediate polars. Main spectral parameters and physical properties of the new discovered sources are discussed. },
persons_number={0},
pdate={28Feb06 20:13:30},
date={19Apr06 20:07:42}
}

@inproceedings {Cornelia_Wunderer,
email={wunderer@ssl.berkeley.edu},
first_name={Cornelia},
last_name={Wunderer},
affiliation={Space Sciences Laboratory / UC Berkeley},
address={7 Gauss Way, Berkeley, CA 94720},
presentation_type={poster},
presentation_number={1},
presentation_panel={I0},
title={Searching for millisecond flares in INTEGRAL GRBs},
authors={C.B. Wunderer, S.E. Boggs, W. Coburn, K. Hurley},
abstract={Since the discovery of the cosmological origin of GRBs there has been growing interest in using these transient events to probe the Quantum Gravity energy scale in the range $10^{16}-10^{19}$ GeV, up to the Planck mass scale. This energy scale can manifest itself through a modification in the electromagnetic radiation dispersion relation, specifically, an energy-dependence of the velocity of light. To impose stringent limits on a possible modification of the dispersion relation, a flare within a GRB must be both short, and significant over a wide energy band to provide a sufficient baseline for determining $dt/dE$, the difference in the arrival times of photons of different energies. We have searched INTEGRAL-observed GRBs for suitable flares, requiring a $5\sigma$ trigger on a 2 ms, 10 ms, or 100 ms time scale using only photons above 1 MeV. This search has been made more difficult by false triggers from the SPI electronic noise component evident in single-event spectra at 1.4-1.6 MeV. We report on the status of our work.},
persons_number={0},
pdate={01Mar06 21:08:23},
date={19Apr06 20:16:24}
}

@inproceedings {Peter_Kretschmar,
email={Peter.Kretschmar@esa.int},
first_name={Peter},
last_name={Kretschmar},
affiliation={ESA},
address={ESAC, Urb. Villafranca del Castillo, Madrid, Spain},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={Pulse phase resolved spectroscopy of INTEGRAL observations of Vela X-1},
authors={P. Kretschmar (ESA), G. Sch\"onherr (IAAT), J. Wilms (Warwick), I. Kreykenbohm (ISDC/IAAT), A. Santangelo, R. Staubert (IAAT)},
abstract={The archetypical wind-accreting X-ray binary pulsar Vela X-1 has been known as a cyclotron line source for many years but with continuing discussions about the true fundamental line and thus the strength of its magnetic field. We present the results of pulse phase resolved analysis of INTEGRAL spectra from a long observation in summer 2003, concentrating on the line features and their variations with pulse phase. },
persons_number={0},
pdate={28Feb06 16:17:12},
date={19Apr06 20:26:00}
}

@inproceedings {Maria_Dolores_Caballero-Garcia,
email={mcaballe@laeff.inta.es},
first_name={Maria Dolores},
last_name={Caballero-Garcia},
affiliation={LAEFF-INTA \& ESAC},
address={Villafranca del Castillo, Villanueva de la Canada E-28691. Madrid, Spain},
presentation_type={poster},
presentation_number={1},
presentation_panel={F0},
title={ToO observations of GRO J1655-40 in outburst},
authors={M. D. Caballero-Garcia, E. Kuulkers, P. Kretschmar, A. Domingo, D. RÌsquez, J. M. Miller, J. M. Mas-Hesse},
abstract={We present the results of four ToO INTEGRAL observations of GRO J1655-40 spread from February to April of 2005, just after it started its outburst (27th February 2005). First results regarding the spectra, light curves and variability using ISGRI, JEM-X, SPI and OMC are presented. These results are also compared with previous high-energy observations of this source during its outbursts. },
persons_number={0},
pdate={01Mar06 18:46:03},
date={19Apr06 20:41:26}
}

@inproceedings {Daniel_Risquez,
email={risquez@laeff.inta.es},
first_name={Daniel},
last_name={Risquez},
affiliation={LAEFF},
address={LAEFF, Estacion de Seguimiento de Satelites - ESA, E-28691 Villanueva de la Caßada, Madrid (Spain) },
presentation_type={poster},
presentation_number={1},
presentation_panel={E0},
title={Optical observations of high energy sources},
authors={D. Risquez, A. Domingo, J.M. Mas-Hesse},
abstract={The INTEGRAL Optical Monitor Camera, OMC, has detected many high energy sources. We have obtained V-band fluxes and light-curves for their counterparts. In the cases of previously unknown counterparts, we have searched for characteristic variations in optical sources around the high-energy target position. Results about Galactic Bulge Monitoring, IGRs, and many other high energy sources will be presented. We will also discuss the implications of the correlation/non-correlation between the optical and high energy emissions in different kind of objects.},
persons_number={0},
pdate={28Feb06 20:17:54},
date={19Apr06 20:41:57}
}

@inproceedings {Albert_Domingo,
email={albert@laeff.inta.es},
first_name={Albert},
last_name={Domingo},
affiliation={Laboratorio de AstrofÌsica Espacial y FÌsica Fundamental (LAEFF-INTA)},
address={POB 50727, E-28080 Madrid, Spain},
presentation_type={poster},
presentation_number={1},
presentation_panel={F0},
title={ToO observations of GRO J1655-40 in outburst},
authors={M.D. Caballero-Garcia, E. Kuulkers, P. Kretschmar, A. Domingo, D. RÌsquez, J.M. Miller, J.M. Mas-Hesse},
abstract={We present the results of four ToO INTEGRAL observations of GRO J1655-40 spread from February to April of 2005, just after it started its outburst (27th February 2005). First results regarding the spectra, light curves and variability using ISGRI, JEM-X, SPI and OMC are presented. These results are also compared with previous high-energy observations of this source during its outbursts.},
persons_number={0},
pdate={28Feb06 21:26:17},
date={19Apr06 20:49:30}
}

@inproceedings {Ingo_Kreykenbohm,
email={kpottschmidt@ucsd.edu},
first_name={Ingo},
last_name={Kreykenbohm},
affiliation={IAA T\"ubingen / ISDC},
address={Sand 1, 72076 T\"ubingen},
presentation_type={poster},
presentation_number={1},
presentation_panel={E0},
title={Monitoring Supergiant Fast X-ray Transient candidates with INTEGRAL and RXTE},
authors={K. Pottschmidt, D.M. Smith, I. Kreykenbohm, I. Negueruela, C. Markwardt},
abstract={Recently the existence of a class of Supergiant Fast X-ray Transients (SFXTs) has been revealed through observations of their characteristic fast outbursts with rise times of a few minutes and durations of 3-8 hours. The few established members of this group have OB supergiant companions and show high and variable absorption columns. The best studied of these systems is XTE J1739-302 (see contributions by Smith et al. and Negueruela et al. for new results from X-ray and optical analyses). In addition several SFXT candidates have been identified, especially by monitoring programs of the Galactic Plane with RXTE and INTEGRAL. Considering the low source duty cycle, these detections might indicate that SFXTs are a dominant class of high mass X-ray binaries. Here we present a study of three new candidate SFXTs that have been identified by classifying light curves obtained from regular RXTE PCA scans of the Galactic Center. All three sources have also been extensively monitored with INTEGRAL, especially within the Galactic Center Deep Exposure (GCDE) program. A companion study concentrates on their precise localization and soft X-ray components (see contribution by Smith et al.).},
persons_number={0},
pdate={01Mar06 06:20:14},
date={19Apr06 21:19:28}
}

@inproceedings {Arash_Bodaghee,
email={arash.bodaghee@obs.unige.ch},
first_name={Arash},
last_name={Bodaghee},
affiliation={INTEGRAL Science Data Centre, Geneva Observatory},
address={16 Chemin d'Ecogia, 1290 Versoix, Switzerland},
presentation_type={oral},
presentation_number={1},
presentation_panel={E8},
title={Population studies of INTEGRAL sources},
authors={Arash Bodaghee, Thierry J.-L. Courvoisier, Jerome Rodriguez, Volker Beckmann},
abstract={Thus far, INTEGRAL/ISGRI has detected over 300 objects above 20 keV. Although the majority of them were known before INTEGRAL, many of the newly-discovered sources were found to feature high intrinsic absorptions that might have helped prevent past detection by softer X-ray missions. We present the distributions of parameters (e.g. column density, pulse and orbital periods, and distances) available in the literature for sources seen with ISGRI. These trends are discussed in relation to source classifications and corresponding evolutionary scenarios.},
persons_number={0},
pdate={01Mar06 17:12:16},
date={19Apr06 21:56:39}
}

@inproceedings {Sirin_Caliskan,
email={scaliskan@sabanciuniv.edu},
first_name={Sirin},
last_name={Caliskan},
affiliation={Sabanci University},
address={Orhanli-Tuzla, Istanbul, 34956, Turkey},
presentation_type={poster},
presentation_number={1},
presentation_panel={B0},
title={Search for redshifted 2.2 MeV line from 4U 1820-30},
authors={},
abstract={Accretion onto a neutron star surface results in very high temperatures. Collisions of nuclei under these conditions can free neutrons, and these free neutrons can potentially be captured by hydrogen nuclei, producing 2.223 MeV photons ([H(n,$\gamma$)D]). In a binary system, the 2.223 MeV photons can produce narrow or broadened lines depending on the position of interactions. If the capture is on the neutron star surface, it will produce a redshifted and broadened line. We searched for such a line from the accreting neturon star system 4U 1820-30 to determine the gravitational red-shift. This information can constrain the equation of state of the neutron star directly. In this poster, we summarize our preliminary results on this search. },
persons_number={0},
pdate={28Feb06 13:29:08},
date={19Apr06 22:46:31}
}

@inproceedings {Emrah_Kalemci,
email={ekalemci@sabanciuniv.edu},
first_name={Emrah},
last_name={Kalemci},
affiliation={Sabanci University},
address={Orhanli-Tuzla, Istanbul, 34956, Turkey},
presentation_type={poster},
presentation_number={1},
presentation_panel={I0},
title={Polarization measurement of GRB 041219 with SPI},
authors={},
abstract={Measuring the polarization of the prompt gamma-ray emission from GRBs can significantly improve our understanding of both the GRB emission mechanisms, as well as the underlying engine driving the explosion. We searched for polarization in the prompt gamma-ray emission of GRB 041219 with the SPI instrument on INTEGRAL. Using multiple-detector coincidence events in the 100-500 keV energy band, our analysis yields a polarization fraction from this GRB of $66\pm21$\%. While statistically this measurement suggests a non-zero polarization, we cannot strongly rule out the possibility that the measured modulation is dominated by instrumental systematics. Even though SPI observations of GRB 041219 do not significantly constrain GRB models, the measurement demonstrates the capability of SPI to measure polarization.},
persons_number={0},
pdate={28Feb06 16:40:29},
date={19Apr06 22:50:17}
}

@inproceedings {Emrah_Kalemci,
email={ekalemci@sabanciuniv.edu},
first_name={Emrah},
last_name={Kalemci},
affiliation={Sabanci University},
address={Orhanli-Tuzla, Istanbul, 34956, Turkey},
presentation_type={poster},
presentation_number={2},
presentation_panel={B0},
title={SN 1006 with INTEGRAL},
authors={},
abstract={The remnant of the supernova of 1006 AD, the remnant first showing evidence for the presence of X-ray synchrotron emission from shock-accelerated electrons, was observed for $\sim3500$ ksec with INTEGRAL for the study of electron acceleration to very high energies as well as the search for the 511 keV positron annihilation line. In this poster, we will show the results of the analysis of the first million seconds of the observations from all three instruments, JEM-X, ISGRI and SPI. We will also include as much preliminary results as possible from the recently taken new set of observations (2.5 Ms). },
persons_number={0},
pdate={28Feb06 16:53:33},
date={19Apr06 22:51:16}
}

@inproceedings {Volker_Beckmann,
email={beckmann@milkyway.gsfc.nasa.gov},
first_name={Volker},
last_name={Beckmann},
affiliation={NASA Goddard Space Flight Center},
address={Code 661, Exploration of the Universe Division, Greenbelt, MD 20770, USA},
presentation_type={oral},
presentation_number={1},
presentation_panel={D3},
title={The hard X-ray luminosity function of INTEGRAL detected AGN},
authors={},
abstract={We have compiled a complete, significance limited sample based on $\sim25,000$ square degrees to a limiting flux of $3\times10^{-11}$ ergs cm$^{-2}$ s$^{-1}$ ($\sim7,000$ square degrees to a flux limit of $1\times10^{-11}$ ergs cm$^{-2}$ s$^{-1}$) in the 20-40 keV band with INTEGRAL. We have constructed a detailed exposure map to compensate for effects of non-uniform exposure. The flux-number relation is best described by a power-law with a slope of $1.66\pm0.11$. We present the first luminosity function of AGN in the 20-40 keV energy range, based on 68 extragalactic objects detected by the imager IBIS/ISGRI on-board INTEGRAL. The luminosity function shows a smoothly connected two power-law form, with an index of $\gamma_1 = 0.9$ below, and $\gamma_2 = 2.2$ above the turn-over luminosity of $L_x = 4.6\times10^{43}$ ergs/s. The emissivity of all INTEGRAL AGNs per unit volume is $W(> 1\times10^{41}$ ergs/s)$ = 2.8\times10^{38}$ ergs s$^{-1}$ Mpc$^{-3}$. These results are consistent with those derived in the 2-20 keV energy band and do not show a significant contribution by Compton-thick objects. Because the sample used in this study is truly local ($z = 0.022$), only limited conclusions can be drawn for the evolution of AGNs in this energy band. But the objects explaining the peak in the cosmic X-ray background are likely to be either low luminosity AGN ($L_x < 1\times10^{41}$ ergs/s) or of other type, such as intermediate mass black holes, clusters, and star forming regions. },
persons_number={0},
pdate={25.02.06 01:10:08},
date={19Apr06 23:11:06}
}

@inproceedings {Lev_Titarchuk,
email={ltitarchuk@ssd5.nrl.navy.mil},
first_name={Lev},
last_name={Titarchuk},
affiliation={George Mason and Naval Research Laboratory},
address={US Naval Research Laboratory Washington, D.C. 20375},
presentation_type={oral},
presentation_number={1},
presentation_panel={F6},
title={Power spectra of black holes and neutron stars as a probe of accretion hydrodynamics. Diffusion theory and its application to INTEGRAL and RXTE observations of Cyg X-1},
authors={Lev Titarchuk, Nickolai Shaposhnikov and Vadim Arefiev},
abstract={We present a model of Fourier Power Density Spectrum (PDS) formation in accretion powered X-ray binary systems derived from the first principles of the diffusion theory. Timing properties are defined by diffusion propagation in a bounded medium. The PDS continuum consists of two major components, presumably coming from an extended accretion disk and from the innermost part of the source (Compton cloud). The disk PDS component has a power law shape with index $\sim-1.5$ and dominated during the soft states of the system, while coronal component is roughly described by a zero-centered Lorentzian. The PDS spectral components have their corresponding components in energy spectrum, namely, thermal (directly observed accretion disk) and power law (disk emission Comptonized by the corona) components. We apply the model to the Integral and RXTE data from Cygnus X-1, which describes the data adequately throughout all spectral states of the source. We argue that timing properties of neutron star systems are dictated by the same physics and the same model can be applicable to these systems as well.},
persons_number={0},
pdate={28Feb06 22:56:10},
date={19Apr06 23:17:59}
}

@inproceedings {Angelique_Joinet,
email={Angelique.Joinet@cesr.fr},
first_name={Angelique},
last_name={Joinet},
affiliation={CESR},
address={9, Avenue du Colonel Roche, 31028 Toulouse Cedex 4},
presentation_type={poster},
presentation_number={1},
presentation_panel={F0},
title={GX339-4 and H1743-322 observed by SPI/INTEGRAL during a state transition},
authors={},
abstract={GX339-4 and H1743-322 are transient Galactic Black Hole (GBH) which harbor a complex X, Gamma and radio activity. We studied the spectro-temporal evolution of these sources during theri outburst covering the period of 2002-2004 using SPI/INTEGRAL and PCA,HEXTE/RXTE data. A relativistic radio jet emission was observed for both sources. After this ejection occuring two weeks before the maximum of X-ray luminosity, H1743-322 exhibited correlated X and Gamma flare events within a timescale of one day. Moreover a high energy excess has been observed fo GX339-4 during the low/hard state and will be described using non thermal models. These observations allow us to investigate the role of jet during a state transition.},
persons_number={0},
pdate={01Mar06 19:24:49},
date={19Apr06 23:28:28}
}

@inproceedings {Alberto_Segreto,
email={segreto@ifc.inaf.it},
first_name={Alberto},
last_name={Segreto},
affiliation={INAF-IASF Palermo},
address={Via Ugo La Malfa, 153},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={A tool for phase resolved spectroscopy of sources observed with ISGRI},
authors={A. Segreto, C. Ferrigno},
abstract={INTEGRAL observations provide a large amount of data regarding accreting binary systems. The interpretation of the spectral emission of these sources needs timing analysis and phase resolved spectroscopy, which are really cumbersome tasks if performed with tools based on the imaging extraction methods usually used for coded mask instruments. Here we present a software we have developed for the ISGRI instrument which allows to generate in a fast way light curves, pulse profiles and phase resolved spectra, thus making data reduction an easy task. After presenting the tool, we show some examples of its application on pulsating sources.},
persons_number={0},
pdate={01Mar06 01:49:46},
date={20Apr06 00:24:03}
}

@inproceedings {Yukikatsu_Terada,
email={terada@riken.jp},
first_name={Yukikatsu},
last_name={Terada},
affiliation={RIKEN, Japan},
address={2-1 Hirosawa, Wako-si, Saitama, Japan},
presentation_type={poster},
presentation_number={1},
presentation_panel={H0},
title={A high-sensitive Suzaku observation of possible non-thermal emission from a white dwarf},
authors={Y. Terada, M. Ishida, K. Mukai, T. Dotani, K. Makishima, L. Gallo, S. Naik, T. Enoto},
abstract={As a similar system of a rotating neutron star, a strongly-magnetized white dwarf (WD) may be a moderate particle acceleration site. At the best case, the induced electric field is expected to reach $10^{13}$ to $10^{14}$ eV. A trial to detect non-thermal emission from a best candidate among WDs, AE Aquarii, was performed with the hard X-ray detector (HXD) on-board the fifth Japaneses X-ray satellite, Suzaku. Although the HXD has non imaging capability, the sensitivity in 10 -- 70 keV band reaches about $5 \times 10^{-6}$ -- $10^{-5}$ photons s$^{-1}$ cm$^{-2}$ keV$^{-1}$ level with only 100 ksec exposure. A marginal detection has been achieved with the HXD, and was separated from the thermal emission. If it is real, this must be a first case of a detection of non-thermal emission from WDs.},
persons_number={0},
pdate={01Mar06 16:09:30},
date={20Apr06 06:25:40}
}

@inproceedings {Vitaliy_Bogomolov,
email={vit_bogom@nm.ru},
first_name={Vitaliy},
last_name={Bogomolov},
affiliation={Skobeltsyn Institute of Nuclear Physics, Moscow State University},
address={},
presentation_type={poster},
presentation_number={1},
presentation_panel={J0},
title={The image reconstruction modeling in the space experiment with Wide-field gamma-ray telescope with the use of INTEGRAL sky maps},
authors={Kudryavtsev, M.I., Bogomolov, V.V., Morozov, O.V., Svertilov, S.I.},
abstract={The INTEGRAL sky maps were used for the simulations of the image reconstruction in the space experiment with a wide field (up to $\sim2\pi$ sr) coding mask telescope elaborated for the all-sky monitoring in gamma-rays (0.05-1.0 MeV). The experiment with such telescope will have angular resolution about 2-3 degrees. Such resolution is enough for the study of the galactic and extragalactic variable sources, transients and gamma-ray bursts in soft gamma rays. The sky maps calculated with the use of INTEGRAL sky maps allow us to estimate the final capabilities of the proposed experiment. One can also consider the expected observation conditions for each of the known galactic and extragalactic sources.},
persons_number={0},
pdate={27Feb06 19:54:54},
date={20Apr06 08:44:48}
}

@inproceedings {Motohide_Kokubun,
email={kokubun@phys.s.u-tokyo.ac.jp},
first_name={Motohide},
last_name={Kokubun},
affiliation={University of Tokyo},
address={7-3-1 Hongo Bunkyo Tokyo, 113-0033, Japan},
presentation_type={oral},
presentation_number={1},
presentation_panel={E2},
title={Hard X-ray view of the Milky Way galaxy obtained with the HXD onboard Suzaku},
authors={M.Kokubun, K.Makishima, and T.Takahashi on behalf of the HXD team},
abstract={With Suzaku, which is the fifth Japanese X-ray astronomical satellite launched on July 10, 2005, we have observed selected regions of the Milky Way Galaxy in the performance verification phase, and obtained the non-thermal view of our Galaxy by fully utilizing the unprecedented high sensitivity of the Hard X-ray Detector (HXD). We have been developing the detector for about 10 years based upon a quite originative concept, ``compound-eye configuration of well-type phoswich counters'', and just have finished in-flight calibrations. Main scientific results from the initial observations will be summarized, together with the issue of extensive study for the in-orbit detector background. },
persons_number={0},
pdate={28Feb06 08:50:32},
date={20Apr06 08:59:22}
}

@inproceedings {Jerome_Rodriguez,
email={jrodriguez@cea.fr},
first_name={Jerome},
last_name={Rodriguez},
affiliation={CEA Saclay, SAp},
address={CEA Saclay, DSM/DAPNIA/SAp, Orme des Merisiers Bat 709, F-91191 Gif Sur Yvette Cedex, FRANCE},
presentation_type={oral},
presentation_number={1},
presentation_panel={F2},
title={An integral monitoring of GRS 1915+105: simultaneous observations with INTEGRAL, RXTE, The Ryle},
authors={},
abstract={Since the launch of INTEGRAL in late 2002 we monitor the Galactic microquasar GRS 1915+105 with long exposure ($\sim100$ ks) pointings. All the observations have been conducted simultaneously with other instruments, in particular RXTE, the Ryle telescope and GMRT, but in some cases also with others (Spitzer, Nan?Ãay, Suzaku,...). We report here the main results of these three years of monitoring focusing\begin{enumerate}\item on the X-ray behaviour of the source as seen by INTEGRAL and RXTE: \begin{quote}
-class of variability\\

-long term evolution\\

-spectral and temporal properties,\end{quote} focusing on some particularly interesting observations
\item on the radio-X-ray connection: \begin{quote}
-occurence of ejection of material\\

-correlation with the X-ray behaviour.\end{quote}\end{enumerate} Our monitoring shows the importance of long uninterrupted exposures accompanied by multiwavelength coverage. We discuss our findings in the context of accretion-ejection models.},
persons_number={0},
pdate={13.02.06 18:49:29},
date={20Apr06 09:49:24}
}

@inproceedings {Peter_Predehl,
email={prp@mpe.mpg.de},
first_name={Peter},
last_name={Predehl},
affiliation={MPE Garching},
address={Giessenbachstrasse},
presentation_type={poster},
presentation_number={1},
presentation_panel={J0},
title={The eROSITA instrument aboard SRG},
authors={Hasinger, Friedrich, et al.},
abstract={eROSITA is an X-ray telescope consisting of seven 54-fold nested Wolter-1 mirrors with a focal length of 160 cm and a diameter of 35 cm. Each telescopes is equipped with a new generation pn-CCD detector specifically developed in the MPI semiconductor lab. We plan an all-sky survey and expect to detect $\sim1$ Mio AGN and $\sim100000$ clusters of galaxies, providing strong constraints on the nature of Dark Energy. },
persons_number={0},
pdate={01Mar06 16:56:47},
date={20Apr06 10:22:44}
}

@inproceedings {Dmitry_Klochkov,
email={klochkov@astro.uni-tuebingen.de},
first_name={Dmitry},
last_name={Klochkov},
affiliation={Institut fuer Astronomie und Astrophysik T\"ubingen (IAAT)},
address={Sand 1, D-72076 T\"ubingen, Germany},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={INTEGRAL observations of Her X-1},
authors={},
abstract={First results of observations of the low mass X-ray binary Her X-1/HZ Her performed by the INTEGRAL satellite in July-August 2005 are presented. A significant part of one 35 day main-on state was covered. The cyclotron line in the X-ray spectrum is well observed and its position and shape, as well as its variability with time and phase of the 1.24 s pulsation are explored. X-ray pulse profiles for different energy bands are studied throughout the observation. The pulse period is found to vary on short time scales revealing a dynamical spin-up/spin-down behavior. Results of simultaneous optical observations of HZ Her are also discussed.},
persons_number={0},
pdate={28Feb06 17:35:44},
date={20Apr06 11:04:44}
}

@inproceedings {Radoslaw_Marcinkowski,
email={radek@cbk.waw.pl},
first_name={Radoslaw},
last_name={Marcinkowski},
affiliation={Institute for Nuclear Studies},
address={05-400 Swierk/Otwock, Poland},
presentation_type={poster},
presentation_number={2},
presentation_panel={I0},
title={First catalogue of the INTEGRAL off-axis gamma-ray burts},
authors={R.Marcinkowski, M.Denis, T.Bulik, Ph.Laurent, P.Goldoni, A.Rau},
abstract={We will present the catalogue of the bursts taking place outside the field of view of the INTEGRAL telescopes, so called off-axis GRBs. Basing on the SPI/INTEGRAL (spectrometer) anticoincidence system data and data from the IBIS/INTEGRAL (imager), with the help of detailed Monte Carlo simulation we will show the summary of bursts detected since the INTEGRAL start in October 2002 up to the beginning of 2004. Localization maps of the sky, light curves and spectra will be presented.},
persons_number={0},
pdate={01Mar06 00:20:13},
date={20Apr06 11:07:02}
}

@inproceedings {Radoslaw_Marcinkowski,
email={radek@cbk.waw.pl},
first_name={Radoslaw},
last_name={Marcinkowski},
affiliation={Institute for Nuclear Studies},
address={05-400 Swierk/Otwock, Poland},
presentation_type={poster},
presentation_number={1},
presentation_panel={I0},
title={Extremely hard gamma-ray spectra of the GRBs detected with INTEGRAL},
authors={R.Marcinkowski, M.Denis, T.Bulik, Ph.Laurent, P.Goldoni, A.Rau},
abstract={The anticoincidence shield of the SPI/INTEGRAL can detect about 100 GRBs a year. About 10\% of these GRBs are detected by the two-layer detector plane of IBIS/INTEGRAL. We present methods of the data processing allowing for localization of the GRBs and spectral analyzing of the above-mentioned outside-filed-of-view cases. These methods use data coming from the so-called Compton mode. We will show results of our methods applied to the 2 year of the INTEGRAL data containing 5 successful localization and several dozen of extracted spectra in the energy range 50 keV - 3 MeV. },
persons_number={0},
pdate={01Mar06 00:17:00},
date={20Apr06 11:08:15}
}

@inproceedings {Solen_Balman,
email={sbalman@rssd.esa.int},
first_name={Solen},
last_name={Balman},
affiliation={ESA/ESTEC},
address={Astrophysics Missions Division, Research and Sceintific Support Department of ESA, ESTEC, Postbus 299, Keplerlaan 1 2201 AZ Noordwijk ZH, Netherlands},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={The time average broadband spectra of LMXB dippers observed with INTEGRAL},
authors={A.N. Parmar, L. Sidoli, M. Diaz Trigo, A. Paizis, T. Oosterbroek},
abstract={The X-ray observations have revealed that many microquasars and low-mass X-ray binaries (LMXBs) exhibit narrow absorption features identified with resonant absorption from and iron and other abundant ions. XMM-Newton observations have shown that at moderate spectral resolution, these features blend together modifying the observed 1--10 keV continuum (also yielding the Fe xxv and Fe xxvi absorption lines). We present the time-averaged INTEGRAL broadband spectra of the LMXB dipping sources 4U 1916-053, 4U 1323-62, 4U 1624-49 and 4U 1746-37. We discuss the nature of the comptonizing regions in these systems. We find that the broadband spectra can be modeled if the effects of a highly photo-ionized plasma are also included. },
persons_number={0},
pdate={01Mar06 18:51:33},
date={20Apr06 11:17:37}
}

@inproceedings {Pavel_Shtykovskiy,
email={pav_sht@hea.iki.rssi.ru},
first_name={Pavel},
last_name={Shtykovskiy},
affiliation={IKI},
address={},
presentation_type={poster},
presentation_number={1},
presentation_panel={E0},
title={High mass X-ray binaries and recent star formation history of the host galaxy},
authors={P.Shtykovskiy, M.Gilfanov},
abstract={We consider the dependence of population of high mass X-ray binaries on the star formation activity in the host galaxy. Based on the XMM-Newton observations of Magellanic Clouds we demonstrate various observational consequences of this dependence. We show that simple $N_{HMXB}\propto SFR$ linear relation fails to explain the spatial distribution of HMXBs over star formation complexes in these galaxies. A successful explanation of the observed distribution is offered by a model taking into account the dependence $N(t)$ of the number of high mass X-ray binaries on time elapsed after the star formation event. Using archival optical observations of the Magellanic Clouds we reconstruct their star-formation histories. Combining these with the X-ray data we determine the $N(t)$ dependence and compare our results with the predictions of populations synthesis models. },
persons_number={0},
pdate={28Feb06 15:15:47},
date={20Apr06 11:19:16}
}

@inproceedings {Vadim_Arefiev,
email={gita@hea.iki.rssi.ru},
first_name={Vadim},
last_name={Arefiev},
affiliation={IKI RAN},
address={Moscow, Russia},
presentation_type={oral},
presentation_number={1},
presentation_panel={G4},
title={X-ray variability and viscous time scale at X-ray binaries},
authors={Marat Gilfanov},
abstract={Based on data of several X-ray missions we have studied X-ray variability of set of quasi-persistent X-ray binaries on wide frequency range. The power density spectra of most of the sources have displayed prominent feature near the frequency associated with the viscos time scale of the accretion disk. We present experimental data and give brief theoretical description of observed results.},
persons_number={0},
pdate={28Feb06 12:00:24},
date={20Apr06 11:25:58}
}

@inproceedings {Gabriele_Schoenherr,
email={gschoen@astro.uni-tuebingen.de},
first_name={Gabriele},
last_name={Schoenherr},
affiliation={IAAT, University of T\"ubingen},
address={Sand 1, 72076 T\"ubingen, Germany},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={Cyclotron line features of magnetized accreting neutron stars},
authors={},
abstract={Providing the only known direct estimate of the magnetic field strength of an accreting neutron star, the study of ``Cyclotron Resonance Scattering Features'' (often abbreviated CRSF or cyclotron lines) is fundamental to a better understanding of the physics of those powerful X- and Gamma-ray sources. During the last 3 decades cyclotron lines have been detected as absorption features in many accreting neutron star binaries. The excellent energy resolution of todays' instruments flying on observatories like INTEGRAL allows not only for the detection of cyclotron lines but also for a good resolution of their non-trivial line shapes. Using a revised version of the Monte Carlo code by R. Araya (Araya \& Harding 1999, 2000), we set up a preliminary model for cyclotron line formation and compare its predictions to observational data.},
persons_number={0},
pdate={28Feb06 13:30:58},
date={20Apr06 11:32:19}
}

@inproceedings {Nikolai_von_Krusenstiern,
email={krusenstiern@astro.uni-tuebingen.de},
first_name={Nikolai von},
last_name={Krusenstiern},
affiliation={Institute for Astronomy and Astrophysics (IAAT)},
address={Sand 1, D 72076 T\"ubingen, Germany},
presentation_type={none},
presentation_number={1},
presentation_panel={},
title={},
authors={},
abstract={},
persons_number={0},
pdate={28Feb06 19:07:27},
date={20Apr06 12:07:12}
}

@inproceedings {Maria_Chernyakova,
email={Masha.Chernyakova@obs.unige.ch},
first_name={Maria},
last_name={Chernyakova},
affiliation={ISDC},
address={16, Chemin d'Ecogia, CH-1290 Versoix},
presentation_type={poster},
presentation_number={1},
presentation_panel={D0},
title={3C273 at its lowest: X-ray, gamma ray and multiwavelength observations between 2003 and 2005},
authors={M.Chernyakova, A.Neronov, T.J.-L.Courvoisier, M.Turler},
abstract={3C 273 is a radio loud quasar, with a jet showing superluminal motion, discovered at the very beginning of quasar research. Being one of the brightest and nearest quasars, 3C 273 was intensively studied at different wavelengths. In this work we present the results of quasi simultaneous INTEGRAL and XMM-Newton monitoring of the quasar during the period of 2003 -- 2005, and test with its help different theoretical models. During the time period under discussion 3C 273 had the lowest flux ever observed in the mm domain. Coordinated multi-wavelength observations in June 2004 in X-rays, optical, infrared, millimeter and radio domains were used to identify and study spectral features usually hidden by the strong synchrotron emission. },
persons_number={0},
pdate={01Mar06 13:52:51},
date={20Apr06 12:26:58}
}

@inproceedings {Anatoli_Iyudin,
email={aiyudin@srd.sinp.msu.ru},
first_name={Anatoli},
last_name={Iyudin},
affiliation={Skobeltsyn Institute of Nuclear Physics, Moscow State University},
address={Vorob'evy Gory, 119992 Moscow, Russia},
presentation_type={oral},
presentation_number={1},
presentation_panel={B6},
title={Multiwavelength appearance of Vela Jr.: Is it up to expectations?},
authors={A.F. Iyudin, B. Aschenbach, V. Burwitz, C. Dennerl, M. Filipovic, M. Freyberg},
abstract={Vela Jr. is one of the youngest and likely nearest among the known galactic supernova remnants. Discovered in 1997 it has been studied since the discovery at many energy ranges and wavelengths, that cover almost 20 decades in energy. We will present and discuss Vela Jr. properties revealed via multiwavelength observations. The observationally revealed properties of this intriguing SNR will be confronted with the SNR model expectations.},
persons_number={0},
pdate={28Feb06 12:41:44},
date={20Apr06 12:48:01}
}

@inproceedings {Guillaume_Belanger,
email={belanger@cea.fr},
first_name={Guillaume},
last_name={Belanger},
affiliation={Service d'Astrophysique, DAPNIA/DSM/CEA-Saclay},
address={91191 Gif-sur-Yvette Cedex, France},
presentation_type={oral},
presentation_number={1},
presentation_panel={E1},
title={What we have learnt about the GC in two years of INTEGRAL observations},
authors={G.Belanger, A.Goldwurm, M.Renaud, R.Terrier, F.Melia, N.Lund, J.Paul, G.Skinner, F.Yusef-Zadeh},
abstract={The nuclear region of our Galaxy, has been observed repeatedly and on several occasions in the two years since the launch of the INTEGRAL soft gamma-ray observatory in October 2002. We have analysed more than 10 Ms of observations accumulated on the Galactic nucleus and amounting to $\sim7$ Ms of effective exposure at the position of Sgr A$^*$. Here, I present a synopsis of the analysis, the results and their implications on our view of the nuclear region and central molecular zone.},
persons_number={0},
pdate={01Mar06 17:07:31},
date={20Apr06 12:57:36}
}

@inproceedings {Ekaterina_Filippova,
email={kate@hea.iki.rssi.ru},
first_name={Ekaterina},
last_name={Filippova},
affiliation={Space Research Institute (RAS)},
address={},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={Hard spectra of X-ray pulsars from INTEGRAL data},
authors={S.S. Tsygankov, A.A. Lutovinov, R.A. Sunyaev},
abstract={We present spectra for 34 accretion-powered X-ray and one millisecond pulsars that were within the field of view of the INTEGRAL observatory over two years (December 2002--January 2005) of its in-orbit operation and that were detected by its instruments at a statistically significant level ($> 8\sigma$ in the energy range 18--60 keV). There are seven recently discovered objects of this class among the pulsars studied: 2RXP~J130159.6-635806, IGR/AX~J16320-4751, IGR~J16358-4726, AX~J163904-4642, IGR~J16465-4507, SAX/IGR~J18027-2017 and AX~J1841.0-0535. We analyze the evolution of spectral parameters as a function of the intensity of the sources and compare these with the results of previous studies. },
persons_number={0},
pdate={01Mar06 19:44:55},
date={20Apr06 13:08:43}
}

@inproceedings {Maurizio_Falanga,
email={mfalanga@cea.fr},
first_name={Maurizio},
last_name={Falanga},
affiliation={Service d'Astrophysique, CEA Saclay, France},
address={Orme des Merisiers - B�Át. 709},
presentation_type={oral},
presentation_number={1},
presentation_panel={G7},
title={Accreting X-ray millisecond pulsars observed with INTEGRAL},
authors={},
abstract={Accreting X-ray millisecond pulsars (XMSP) are key systems to understand the spin and accretion history of the neutron stars. Out of the seven recently found XMSP, three were extensively observed with the INTEGRAL satellite in the high energy range and one of this has also been discovered by INTEGRAL. Detailed timing and spectral results will be presented, including data obtained during the most recent outburst of the pulsar HETE J1900.1-2455.},
persons_number={0},
pdate={04Mar06 22:12:28},
date={20Apr06 13:24:34}
}

@inproceedings {Andreas_von_Kienlin,
email={azk@mpe.mpg.de},
first_name={Andreas},
last_name={von Kienlin},
affiliation={Max-Planck-Institut f\"ur extraterrestrische Physik},
address={Giessenbachstrasse, D-85748 Garching, Germany },
presentation_type={poster},
presentation_number={1},
presentation_panel={B0},
title={The nature of SNR RX J0852-4622 / GRO J0852-4642},
authors={},
abstract={The confirmation and clarification of the gamma-ray line emission from the radioactive decay of $^{44}$Ti nuclei (half-life 63 years) discovered by COMPTEL (GRO J0852-4642) and located at the ROSAT X-ray supernova remnant (SNR) RX J0852-4622, is crucial for its interpretation as a young and nearby SNR. The detection and determination of the $^{44}$Ti line flux and the measurement of the line shape will help to settle the issues raised by this exciting potential correlation. If true, this would make this object the nearest SNR. INTEGRAL observed the Vela region twice, during the first-year core program for about 1.2 Ms and in November-December 2005 in the frame of the AO-3 open-time observation for about 1.7 Ms. Among other nucleosynthesis studies one of the most important scientific goals of these observations is the detection of $^{44}$Ti gamma-ray lines expected at 68 keV, 78 keV and 1157 keV. For this purpose the INTEGRAL Spectrometer (SPI), with its exceptional high-energy resolution thanks to its Ge-detector camera is the key instrument for this observation, permitting a precise determination of gamma-ray line intensities and profiles. In this paper, we present first results of our $^{44}$Ti gamma-ray line analysis with SPI.},
persons_number={0},
pdate={27Mar06 15:55:43},
date={20Apr06 13:32:15}
}

@inproceedings {Stefano_Bianchi,
email={Stefano.Bianchi@sciops.esa.int},
first_name={Stefano},
last_name={Bianchi},
affiliation={European Space Astronomy Center - ESA},
address={},
presentation_type={none},
presentation_number={1},
presentation_panel={},
title={},
authors={},
abstract={},
persons_number={0},
pdate={23Mar06 15:01:50},
date={20Apr06 13:42:25}
}

@inproceedings {Brian_McBreen,
email={brian.mcbreen@ucd.ie},
first_name={Brian},
last_name={McBreen},
affiliation={University College Dublin},
address={School of Physics, Belfield, Dublin 4, Ireland},
presentation_type={oral},
presentation_number={1},
presentation_panel={I8},
title={Spectral and polarisation properties of GRB041219A},
authors={},
abstract={GRB 041219A was the brightest burst localised by INTEGRAL to date and was detected simultaneously at optical frequencies. The peak flux of 43 photons cm$^{-2}$ s$^{-1}$ over 1 s integration time (20-8000 keV) was higher than 98\% of the bursts detected by BATSE. The results of analysis of the prompt gamma ray emission from the spectrometer SPI on board INTEGRAL will be presented. GRB 041219A had a multi-peaked lightcurve with an initial weak pulse followed by a 200 s period of quiescence, before the main emission interval consisting of 2 minute-long strong pulses. The main periods of emission and the overall burst were well fit by the Band model, with some evolution of the low energy photon index after the quiescent period. Due to the brightness of the burst, it was possible to obtain a limit on the percentage polarisation of the prompt emission detected by SPI. },
persons_number={0},
pdate={28Feb06 19:54:15},
date={20Apr06 14:12:12}
}

@inproceedings {Guram_Kakhidze,
email={guram@ipu.rssi.ru},
first_name={Guram},
last_name={Kakhidze},
affiliation={ICS RAS},
address={Moscow,117997, 65 Profsoyuznya, rum 343},
presentation_type={none},
presentation_number={1},
presentation_panel={},
title={},
authors={},
abstract={},
persons_number={0},
pdate={05Apr06 15:46:36},
date={20Apr06 14:15:14}
}

@inproceedings {Christoph_Winkler,
email={Christoph.Winkler@rssd.esa.int},
first_name={Christoph},
last_name={Winkler},
affiliation={ESA-ESTEC, RSSD},
address={Keplerlaan 1, NL-2201 AZ Noordwijk, The Netherlands},
presentation_type={oral},
presentation_number={1},
presentation_panel={X1},
title={INTEGRAL --- overview and current status},
authors={},
abstract={INTEGRAL, ESA's gamma-ray observatory mission, in collaboration with Russia and NASA, was launched on 17 October 2002 and is performing very well since then. The mission duration has been extended until late 2010. Thanks to its unprecedented imaging performance and unique gamma-ray spectroscopy capabilities, the scientific community using INTEGRAL has - during the past 3.5 years - achieved important scientific results in the field of high energy astrophysics. Examples include the detection of a new class of Galactic compact sources; resolution of the Galactic diffuse continuum emission at hard X-ray energies into point sources; imaging and spectroscopy of the 511 keV annihilation line and the 1.8 MeV radioactive emission of $^{26}$Al. I will present an overview and the current status of this exciting gamma-ray mission.},
persons_number={0},
pdate={13.02.06 16:34:51},
date={20Apr06 14:48:22}
}

@inproceedings {Willem_Hermsen,
email={W.Hermsen@sron.nl},
first_name={Willem},
last_name={Hermsen},
affiliation={SRON Netherlands Institute for Space Research},
address={Sorbonnelaan 2, 3584 CA Utecht, The Netherlands},
presentation_type={none},
presentation_number={1},
presentation_panel={},
title={},
authors={},
abstract={},
persons_number={0},
pdate={28Mar06 14:08:41},
date={20Apr06 15:14:34}
}

@inproceedings {Flavio_D\'Amico,
email={damico@das.inpe.br},
first_name={Flavio},
last_name={D'Amico},
affiliation={Instituto Nacional de Pesquisas Espaciais - INPE},
address={Av. dos Astronautas 1758 12227-010 S.J.dos Campos-SP, Brazil},
presentation_type={poster},
presentation_number={1},
presentation_panel={E0},
title={Infrared observations of IGR J16320-4751 and IGR J16358-4756},
authors={},
abstract={The search for infrared counterparts of newly discovered INTEGRAL sources is a subject of an ongoing project carrying out in Brazil. We will show here our results on two of these sources, IGR J16320-4751 and IGR J16358-4756. },
persons_number={0},
pdate={31Mar06 16:22:30},
date={20Apr06 15:16:22}
}

@inproceedings {Sergei_Trushkin,
email={satr@sao.ru},
first_name={Sergei},
last_name={Trushkin},
affiliation={SAO RAS },
address={Nizhnij Arkhyz, KCHR, 369167},
presentation_type={poster},
presentation_number={1},
presentation_panel={F0},
title={Recent radio monitoring of microquasars with RATAN-600 radio telescope},
authors={Bursov N. N., Kotani T., Nizhelskij N.A., Namiki M., Tsuboi M., Voitsik P. A.},
abstract={We report about the multi-frequency (1-30 GHz) daily monitoring of the radio flux variability of the three microquasars: SS433, GRS1915+105 and Cyg X-3 during the set from September 2005 to March 2006. We detected remarkable correlation of the flaring fluxes and RXTE ASM X-rays emission from GRS1915+105 during eight bright ($\sim200$-600 mJy) radio flares in October 2005. After 100 days of the quiescent radio emission at level of 100-150 mJy we detected a dramatic drop down of the fluxes ($\sim20$ mJy) from Cyg X-3. That is a sign of the following bright flare. Indeed such a 1Jy-flare was detected in February 2006 after 18 days of the quenched radio emission. The daily spectra of the flare in the maximum was flat from 1 to 100 GHz, using the quasi-simultaneous observations at $\sim100$ GHz with RT45m telescope and millimeter array (NMA) of Nobeyama Radio Observatiory in Japan (Tsuboi at al ATEL.\#727). The several bright radio flaring events (1-5 Jy) followed during this state of very variable and intensive X-ray emission ($\sim0.5$ Crab) as detected in RXTE ASM. We discussed the various spectral and temporal characteristics of the detected 180-day light curves from three microquasars in comparison with Rossi XTE ASM data.},
persons_number={0},
pdate={06Apr06 17:27:55},
date={20Apr06 15:19:37}
}

@inproceedings {Volker_Springel,
email={volker@mpa-garching.mpg.de},
first_name={Volker},
last_name={Springel},
affiliation={Max-Planck-Institute for Astrophysics},
address={Karl-Schwarzschild-Str. 1, 85740 Garching},
presentation_type={oral},
presentation_number={1},
presentation_panel={C3},
title={Cosmic rays in simulations of structure formation},
authors={},
abstract={Cosmic rays contribute significantly to the pressure of the interstellar medium in our own Galaxy, and may be produced abundantly by diffusive shock acceleration at large-scale structure shock waves. Despite this, they have been largely neglected thus far in theoretical efforts to model galaxy formation in the Universe. In my talk, I will discuss results from a new hydrodynamical simulation framework that for the first time allows simulations that self-consistently follow the dynamics of cosmic rays during structure growth. In particular, I show that the star formation efficiencies of small galaxies can be reduced substantially by cosmic ray feedback. I will also discuss some results from the Millennium Simulation that are of interest to the topics of the meeting.},
persons_number={1},
pdate={31Mar06 19:28:34},
date={20Apr06 15:35:57}
}

@inproceedings {Alexey_Lukomskiy,
email={lucomsky@iki.rssi.ru},
first_name={Alexey},
last_name={Lukomskiy},
affiliation={Space Research Institute},
address={},
presentation_type={poster},
presentation_number={1},
presentation_panel={J0},
title={Improved logarithmic counter description for intensive flows},
authors={V.F. Babkin, A.K. Lukomskiy},
abstract={A new design of particles (or quanta) flows counter is offering having large dynamic range, which relative registration error slightly vary depending on input flow intesity. Such counters belong to logarithmic class. Unlike wide known structure of logarithmic counters based on rising binary recount coefficient, presented recount concept is defined by integer-valued recurring expression that is colligates recurring Fibonacci expression. That is why mentioned counter can be called ``Fibonacci counter''. Analysis of relative Fibonacci counter precision have done in comparison with counter based on binary recount. It was shown that under count rates greater than 900 Fibonacci counter have more preferred characteristics, specifically for an ordinary binary counter example that approximate logarithmic counter by piecewise linear one using the same input impules count range 10 Giga counts. We offer simple hardware design for Fibonacci counter made of basic logic elements.},
persons_number={0},
pdate={01Mar06 15:42:46},
date={20Apr06 16:10:01}
}

@inproceedings {Isabel_Caballero,
email={isabel@astro.uni-tuebingen.de},
first_name={Isabel},
last_name={Caballero},
affiliation={Institut f\"ur Astronomie und Astrophysik T\"ubingen (IAAT)},
address={Sand 1, D-72076 T\"ubingen, Germany},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={Pulse period history of A 0535+26},
authors={I.Caballero, P.Kretschmar, A.Segreto, A.Santangelo},
abstract={The Be/X-ray binary A 0535+26 was discovered in 1975 during a giant outburst. Afterwards it has shown periods of quiescence (flux below 10 mCrab), normal outbursts (10 mCrab-1 Crab) and occasionally giant outbursts (several Crab). Ending 11 years of quiescence, the last giant outburst took place in May/June 2005, but the source was too close to the Sun to be observed by most satellites. A subsequent normal outburst took place in August 2005, which was observed in INTEGRAL and RXTE TOO observations. We will present timing properties of the source, and a long term pulse period history, as well as phase averaged spectra and phase resolved spectroscopy.},
persons_number={0},
pdate={28Feb06 20:53:55},
date={20Apr06 16:13:20}
}

@inproceedings {Hans-Thomas_Janka,
email={thj@mpa-garching.mpg.de},
first_name={Hans-Thomas},
last_name={Janka},
affiliation={MPA, Max Planck Institute for Astrophysics},
address={Karl-Schwarzschild-Str. 1},
presentation_type={oral},
presentation_number={1},
presentation_panel={B1},
title={Stellar explosions and compact object mergers as sources of heavy elements and gamma-ray bursts supernovae},
authors={},
abstract={I will review the status of modeling stellar explosions and gamma-ray burst sources, focussing on thei physics of the central engine and the conditions for the creation of heavy elements. While our understanding of the events that determine stellar core collapse and explosions has made significant progress, in particular also by numerical modeling, the detailed conditions and processes are still a matter of debate. Observational constraints, e.g. by measuring neutrino and gravitational wave signals or nucleosynthetic products in situ would yield extremely valuable insights.},
persons_number={0},
pdate={10Apr06 00:00:00},
date={20Apr06 16:14:10}
}

@inproceedings {Roman_Krivonos,
email={kris@hea.iki.rssi.ru},
first_name={Roman},
last_name={Krivonos},
affiliation={IKI, Moscow, Russia; MPA, Garching, Germany},
address={},
presentation_type={oral},
presentation_number={1},
presentation_panel={C3},
title={INTEGRAL/IBIS observation of the Galactic ridge X-ray emission},
authors={R.Krivonos, M.Revnivtsev, E. Churazov, S. Sazonov, S. Grebenev and R. Sunyaev},
abstract={We present results of study of the Galactic ridge X-ray emission (GRXE) in hard X-rays performed with IBIS telescope aboard INTEGRAL. Imaging capabilities of coding aperture telescope make it possible to account for flux from bright Galactic point sources and wide field of view permits to collect large flux from underlying GRXE emission. Extensive study of the IBIS/ISGRI detector background allowed us to construct the model which predicts the detector count rate with $\sim1$\% accuracy in the energy band 17-60 keV. Derived longitude and latitude profiles of the ridge emission are in good agreement with Galactic distribution of stars obtained from infrared observations. This, along with obtained hard X-ray spectrum of the Galactic ridge emission strongly indicates its stellar origin which support findings of Revnivtsev et al. 2005. Derived unit stellar mass emissivity of the ridge in the energy band 17-60 keV $\sim1.0\times10^{27}$ agrees with that obtained for accreting magnetic white dwarf binaries - dominant contributors to the GRXE at these energies. At energies higher than 70--80 keV no additional contribution to the total emission of the Galaxy apart from detected point sources is detected.},
persons_number={0},
pdate={01Mar06 21:27:29},
date={20Apr06 16:17:10}
}

@inproceedings {Ingo_Kreykenbohm,
email={Ingo.Kreykenbohm@obs.unige.ch},
first_name={Ingo},
last_name={Kreykenbohm},
affiliation={IAA T\"ubingen / ISDC},
address={Sand 1, 72076 T\"ubingen},
presentation_type={oral},
presentation_number={1},
presentation_panel={G5},
title={Accreting X-ray pulsars observed with INTEGRAL},
authors={J. Wilms, P. Kretschmar, N. Mowlavi, S. Fritz, J. Torrejon, D. Klochkov, C. Ferrigno, A. Santangelo, R. Staubert},
abstract={We present an observational review of the transient and persistent accreting X-ray pulsars observed with INTEGRAL. Accreting X-ray pulsars are among the brightest sources in the X-ray sky and are observed frequently by INTEGRAL and other X-ray missions. Nevertheless they are still very enigmatic sources as fundamental questions on the X-ray production mechanism still remain largely unanswered. These questions are addressed by performing detailed temporal and spectral studies on a large sample of objects over a long time range. Of vital importance is the study of cyclotron lines as they provide the only direct link to the magnetic field of the pulsar. While some objects show cyclotron lines which are extremely stable with time and pulse phase, in other objects the lines depend strongly either on the pulse, the luminosity of the source, or both. Of special interest in any case are transient sources where it is possible to study the evolution of the cyclotron line, the temporal behavior, and the source in general from the onset until the end of the outburst through a wide range of different luminosity states. },
persons_number={0},
pdate={28Feb06 21:07:07},
date={20Apr06 16:45:06}
}

@inproceedings {Hiromitsu_Takahashi,
email={hirotaka@amalthea.phys.s.u-tokyo.ac.jp},
first_name={Hiromitsu},
last_name={Takahashi},
affiliation={Hiroshima University},
address={1-3-1 Kagamiyama Higashi-Hiroshima 739-8526 Japan},
presentation_type={oral},
presentation_number={1},
presentation_panel={F5},
title={Suzaku broadband observations of Galactic black hole binaries},
authors={Suzaku team},
abstract={Suzaku, the 5th Japanese X-ray satellite, has observed 4 black hole binaries, Cyg X-1, GRO J1655-40, GRS 1915+105, and 4U 1630-47, since the launch on July 10, 2005. The former two were observed in their low/hard state, while the others are in high/soft ones. Utilizing the capability of the X-ray Imaging Spectrometer (XIS) and the Hard X-ray Detector (HXD), we obtained broadband energy spectra from sub keV to several 100 keV with the exposures of several 10 ks. We will present these results, with particular emphasis on GRO J1655-40, which was observed at the end of the outburst and displayed a decreasing luminosity ($6\times10^{36}$ erg s$^{-1}$) even during the Suzaku observation. },
persons_number={0},
pdate={02Mar06 01:02:48},
date={20Apr06 16:51:56}
}

@inproceedings {Sonja_Fritz,
email={fritz@astro.uni-tuebingen.de},
first_name={Sonja},
last_name={Fritz},
affiliation={IAAT},
address={Sand 1, 72076 T\"ubingen, Germany},
presentation_type={poster},
presentation_number={1},
presentation_panel={F0},
title={The broad band spectrum of Cygnus X-1},
authors={S. Fritz, J. Wilms, K. Pottschmidt, M.A. Nowak, E. Kendziorra, M. Kirsch, A. Santangelo},
abstract={The black hole binary Cygnus X-1 has been observed simultaneously by INTEGRAL, RXTE, and XMM-Newton for four times in November and December 2004, when Cyg X-1 became first observable with XMM-Newton. During this observations the source was found in one of its transitional states between the hard and the soft state. We obtained a high signal to noise spectrum of Cyg X-1 from 2.5 keV to 1 MeV which allows us to put constrains on the nature of the comptonizing plasma by modeling the continuum with Comptonization models (compTT or eqpair) as well as on the structure of the Fe line. },
persons_number={0},
pdate={28Feb06 21:07:47},
date={20Apr06 17:09:55}
}

@inproceedings {Roman_Rafikov,
email={rrr@cita.utoronto.ca},
first_name={Roman},
last_name={Rafikov},
affiliation={Canadian Institute for Theoretical Astrophysics (CITA)},
address={},
presentation_type={oral},
presentation_number={1},
presentation_panel={H3},
title={Double pulsar: high and low energy emission puzzles},
authors={},
abstract={Recently discovered unique double pulsar system J0737-3039 provides us with unprecedented tests of general relativity and magnetospheric effects. After a general overview of the system properties I will focus on the high-energy emission detected from the double pulsar. I will describe observations of X-ray emission from the double neutron star systems and discuss some mechanisms of its production. Finally, a description of some puzzling phenomena at low energies (in the radio), such as magnetospheric eclipse and modulation of the pulsar radio emission at the rotational frequency of its companion, will be given.},
persons_number={0},
pdate={05Apr06 19:44:54},
date={20Apr06 17:31:57}
}

@inproceedings {Josh_Grindlay,
email={josh@cfa.harvard.edu},
first_name={Josh},
last_name={Grindlay},
affiliation={Harvard},
address={CfA, 60 Garden St., Cambridge, MA 02138, USA},
presentation_type={oral},
presentation_number={1},
presentation_panel={D5},
title={Initial results from the BAT Slew Survey},
authors={J. Grindlay, A. Copete, J. Hong (CfA), N. Gehrels, C. Markwardt and J. Tueller (GSFC)},
abstract={We describe the implementation and initial results of the BAT Slew Survey (BATSS) to derive BAT images for sky coverage in slews to GRBs and pointed targets. Some $\sim40$ slews ($\sim2-3$ min each) per day are obtained which significantly increase the BAT sky coverage and allow an ASM-like capability for bright transients as well as extend sky coverage for GRBs. The imaging software is nearly developed and production processing of slew data, which have been acquired since February, 2006, should be possible beginning in April. Initial sky survey results will be reported, along with implications of BATSS as a testbed for the scanning coded aperture survey proposed for EXIST as the Black Hole Finder Probe.},
persons_number={1},
pdate={02Mar06 07:00:50},
date={20Apr06 17:33:26}
}

@inproceedings {William_Gillard,
email={gillard@cesr.fr},
first_name={William},
last_name={Gillard},
affiliation={C.E.S.R},
address={9, avenue du Colonel Roche - 31028 Toulouse},
presentation_type={poster},
presentation_number={1},
presentation_panel={A0},
title={Transport of positrons in the interstellar medium},
authors={W. Gillard, A. Marcowith, K. FerriÕre, P. Jean},
abstract={The spectral analysis of the positron-electron annihilation, based on measurements made with the spectrometer SPI of the INTEGRAL observatory, indicates that positrons annihilate mainly in the warm medium, including the warm ionized and the warm neutral medium (Churazov et al. 2005 ; Jean et al. 2006). In contrast, the high filling factor of the hot medium, in the central regions of the Galaxy, suggests an e$^+$/e$^-$ annihilation taking place mainly in the hot medium. This difference can be explained if positrons propagate in the interstellar medium and can escape the hot medium (Jean et al. 2006). The transport of positrons is also comforted by the production processes producing high-energy positrons ($>1$ MeV) with long-lived times before annihilation, favorable to their diffusion. We then present the possible processes of transport for both cosmic-ray positrons, at high energy ($E \gg 1$ MeV), and positrons produced by the beta$+$ decay of radioactive nuclei at lower energy ($E \sim 1$ MeV). We also describe the diffusive processes of positrons during their cooling phase and during their thermalized phase before they annihilate with electrons.},
persons_number={0},
pdate={23.02.06 18:56:06},
date={20Apr06 17:58:04}
}

@inproceedings {Michael_Schmidt,
email={Michael.Schmidt@esa.int},
first_name={Michael},
last_name={Schmidt},
affiliation={ESA-ESOC / OPS-OFI},
address={},
presentation_type={none},
presentation_number={1},
presentation_panel={},
title={S/C Operations Manager},
authors={},
abstract={},
persons_number={0},
pdate={06Apr06 17:52:22},
date={20Apr06 18:09:28}
}

@inproceedings {Konstantin_V._Krasnobaev,
email={kvk-kras@list.ru},
first_name={Konstantin V.},
last_name={Krasnobaev},
affiliation={Lomonosov Moscow State University, Department of Mechanics and Matematics},
address={},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={Luminosity response of an X-ray source on variations of the stellar wind parameters},
authors={},
abstract={We present numerical simulations of the 2-dimensional nonsteady flow of nonuniform stellar wind around an X-ray source. Nonuniformity of the flow's parameters is assumed to be connected with the presence of sound and entropy perturbations. In the computations, both amplitude and typical scale of the nonuniformities have varied significantly. As a result we determine the changes with time of accretion rate and luminosity of the X-ray source caused by these perturbations.},
persons_number={0},
pdate={21Mar06 18:11:33},
date={20Apr06 19:03:41}
}

@inproceedings {Fiamma_Capitanio,
email={fiamma.capitanio@iasf-roma.inaf.it},
first_name={Fiamma},
last_name={Capitanio},
affiliation={IASF-Roma INAF; School of Physics and Astronomy, University of Southampton, UK.},
address={},
presentation_type={poster},
presentation_number={1},
presentation_panel={F0},
title={Monitoring of transient black hole candidates observed in the INTEGRAL survey},
authors={},
abstract={The INTEGRAL/IBIS survey is realised collecting all the GPS and GCDE data together with all the public data available. The second catalogue, published in 2005, is dominated by detection of 113 X-ray binaries, with 38 high--mass and 67 low--mass. In most cases the compact object is a neutron star, but the sample also contains 4 confirmed Black Holes and 6 LMXB black hole candidates (BHC). There are also an additional 6 tentative associations as BHCs based simply on spectral and timing properties. In the sample of 12 sources (BHC and tentatively associated BHC) there are 8 transient sources that went in outburst during the INTEGRAL survey observations. We present here the monitoring of the temporal and spectral evolution of these 8 outbursts. },
persons_number={0},
pdate={01Mar06 21:31:35},
date={20Apr06 19:21:12}
}

@inproceedings {Nicola_Masetti,
email={masetti@iasfbo.inaf.it},
first_name={Nicola},
last_name={Masetti},
affiliation={INAF/IASF, Bologna, Italy},
address={via Gobetti, 101},
presentation_type={poster},
presentation_number={1},
presentation_panel={E0},
title={New results on optical identification of INTEGRAL sources},
authors={},
abstract={We report on results concerning our ongoing program on optical spectroscopic observations of unknown INTEGRAL sources using various telescopes.},
persons_number={0},
pdate={01Mar06 18:14:18},
date={20Apr06 19:45:05}
}

@inproceedings {Arvind_Parmar,
email={aparmar@rssd.esa.int},
first_name={Arvind},
last_name={Parmar},
affiliation={ESA},
address={ESTEC},
presentation_type={none},
presentation_number={1},
presentation_panel={},
title={},
authors={},
abstract={},
persons_number={0},
pdate={13Apr06 21:26:11},
date={20Apr06 20:07:03}
}

@inproceedings {Petr_Kubanek,
email={pkubanek@asu.cas.cz},
first_name={Petr},
last_name={Kubanek},
affiliation={AI Ondrejov Czech Republic \& ISDC, Versoix},
address={Fricova, CZ - 251 65 Ondrejov},
presentation_type={poster},
presentation_number={1},
presentation_panel={I0},
title={Bright optical flash from GRB 060117 --- an example of event detected Bright optical flash from GRB 060117 - an example of event detectedwith OMC class camera},
authors={Petr Kubanek, Martin Jelinke, Michael Prouza, Martin Nekola, Stanislav Vitek, Rene Hudec},
abstract={We will present observations of a very bright (magnitude 10) optical transient associated with GRB 060117. These observations were obtained with an OMC-class ground based device . The detected optical trigger will be presented and discussed, together with consequences for INTEGRAL OMC camera chance to detect analogous event.},
persons_number={0},
pdate={03Mar06 19:32:23},
date={20Apr06 20:12:44}
}

@inproceedings {Cornelia_Wunderer,
email={wunderer@ssl.berkeley.edu},
first_name={Cornelia},
last_name={Wunderer},
affiliation={Space Sciences Laboratory / UC Berkeley},
address={7 Gauss Way, Berkeley, CA 94720},
presentation_type={poster},
presentation_number={2},
presentation_panel={J0},
title={Adding hard X-ray imaging capabilities to a Compton Telescope},
authors={C.B. Wunderer, M. Bandstra, S.E. Boggs, J.D. Bowen, W. Coburn},
abstract={The efficiency of a Compton telescope operating in its ``imaging mode'', as well as its angular resolution, decrease rapidly with energy below a few hundred keV. The efficiency decrease is mainly due to the increasing photoabsorption cross sections at these energies. The average distance between interaction sites for Compton events decreases with photon energy; this, together with the increasing impact of Doppler broadening, results in the instrument's angular resolution rapidly deteriorating. These limitations of efficiency and angular resolution constitute essentially ``fundamental'' limits on the energy regime accessible to imaging Compton telescopes. At the same time, a Compton Telescope at balloon altitudes or in space is exposed to Cosmic diffuse and atmospheric photon backgrounds. The intensity of both of these components increases rapidly with decreasing energy, making photons $< 100$ keV a possibly significant contributor to random coincident events or instrument dead time. Thus shielding of low- energy photon components is desirable. For the first balloon flight of the Nuclear Compton Telescope (NCT) we have simultaneously addressed these two concerns by enshrouding the top of the instrument in a tin shield (bottom had BGO shielding), with part of the shield having strategically placed holes - a 10\% open coded aperture mask working up to several tens of keV in conjunction with the finely pixellated double-sided Ge strip detectors. We present pre-flight calibration results.},
persons_number={0},
pdate={01Mar06 21:39:06},
date={20Apr06 21:10:23}
}

@inproceedings {Cornelia_Wunderer,
email={wunderer@ssl.berkeley.edu},
first_name={Cornelia},
last_name={Wunderer},
affiliation={Space Sciences Laboratory / UC Berkeley},
address={7 Gauss Way, Berkeley, CA 94720},
presentation_type={poster},
presentation_number={3},
presentation_panel={J0},
title={The Advanced Compton Telescope Mission},
authors={C.B. Wunderer, for the ACT Collaboration},
abstract={The Advanced Compton Telescpe (ACT), the next major step in gamma-ray astronomy, will probe the fires where chemical elements are formed by enabling high resolution spectroscopy of nuclear emission from supernova explosions. During the past two years, our collaboration has been undertaking a NASA mission concept study for ACT. This study was designed to (1) transform the key scientific objectives into specific instrument requirements, (2) to identify the most promising technologies to meet those requirements, and (3) to design a viable mission concept for this instrument. We will present the results of this study, including scientific goals and expected performance, mission design, and technology recommendations. },
persons_number={0},
pdate={03Mar06 01:12:28},
date={20Apr06 21:13:02}
}

@inproceedings {David_Smith,
email={dsmith@scipp.ucsc.edu},
first_name={David},
last_name={Smith},
affiliation={University of California, Santa Cruz},
address={Physics Dept., UCSC, 1156 High St, Santa Cruz, CA 95064 USA},
presentation_type={poster},
presentation_number={2},
presentation_panel={E0},
title={X-ray observations of Supergiant Fast X-ray Transients},
authors={D. M. Smith, I. Negueruela, N. Bezayiff, K. Pottschmidt},
abstract={The supergiant fast x-ray transients (SFXTs) are a recently-recognized class of x-ray binary characterized by a late O- or very early B-type supergiant companion, extremely faint quiescent emission, and rare outbursts at moderate luminosities lasting on the order of hours. Due to the difficulty in detecting these systems, they may actually make up the majority of HMXBs, and may be the most common progenitors of NS/NS or NS/BH mergers. The most certain members of this class are XTE J1739-302, IGR J17544-2619, IGR J16465-4507, and AX J1841.0-0536. We will discuss the X-ray properties of these objects, which have been observed by INTEGRAL, RXTE, ASCA, Chandra, and Newton, discuss the status of several additional candidates for the class, and review the properties of three luminous supergiant X-ray binaries which show very bright outbursts at a similar timescale: Cyg X-1, Vela X-1, and 1E 1145.1-6141.},
persons_number={0},
pdate={01Mar06 01:52:10},
date={20Apr06 21:51:21}
}

@inproceedings {Alexander_Zakharov,
email={zakharov@itep.ru},
first_name={Alexander},
last_name={Zakharov},
affiliation={Institute of Theoretical and Experimental Physics},
address={B. Cheremushkinskaya, 25, Moscow, Russia},
presentation_type={poster},
presentation_number={1},
presentation_panel={D0},
title={Measuring parameters of supermassive black holes with space missions},
authors={},
abstract={A number of X-ray space missions like, ASCA, XMM-Newton, Chandra got a lot of information about Fe $K_\alpha$ lines and other X-ray lines. Recent X-ray observations of microquasars and Seyfert galaxies reveal broad emission lines in their spectra, which can arise in the innermost parts of accretion disks. Simulations indicate that at low inclination angle the line is measured by a distant observer as characteristic two-peak profile. However, at high inclination angles ($> 85^0$) two additional peaks arise. This phenomenon was discovered by Matt et al. (1993) using the Schwarzschild black hole metric to analyze such effect. They assumed that the effect is applicable to a Kerr metric far beyond the range of parameters that they exploited. We check and confirm their hypothesis about such a structure of the spectral line shape for the Kerr metric case. We use no astrophysical assumptions about the physical structure of the emission region except the assumption that the region should be narrow enough. Positions and heights of these extra peaks drastically depend on both the radial coordinate of the emitting region (annuli) and the inclination angle. It was found that these extra peaks arise due to gravitational lens effect in the strong gravitational field, namely they are formed by photons with some number of revolutions around black hole. This conclusion is based only on relativistic calculations without any assumption about physical parameters of the accretion disc like X-ray surface emissivity etc. We discuss how analysis of the iron spectral line shapes could give an information about an upper limit of magnetic field near black hole horizon. Based on results of numerical simulations we discussed origins of double peaked and double horned profiles and clarified the M\"uller and Camenzind hypothesis (2003). In 2007 Radioastron mission will be launched and it will be a generalization of VLBI technique using space base. This instrument will have the extraordinary angular resolution. We could measure parameters of the black hole in the Galactic Center. We discuss glories (mirages) formed near rapidly rotating Kerr black hole horizons and propose a procedure to measure masses and rotation parameters analyzing these forms of mirages. In some sense that is a manifestation of gravitational lens effect in the strong gravitational field near black hole horizon and a generalization of the retro-gravitational lens phenomenon. We analyze the case of a Kerr black hole rotating at arbitrary speed for some selected positions of a distant observer with respect to the equatorial plane of a Kerr black hole. We also propose to use future radio interferometer RADIOASTRON facilities to measure shapes of mirages (glories) and to evaluate the black hole spin as a function of the position angle of a distant observer. },
persons_number={0},
pdate={08Apr06 13:24:34},
date={20Apr06 22:07:00}
}

@inproceedings {Francois_Lebrun,
email={flebrun@discovery.saclay.cea.fr},
first_name={Francois},
last_name={Lebrun},
affiliation={CEA-Saclay, APC},
address={91191 Gif sur Yvette Cedex},
presentation_type={none},
presentation_number={1},
presentation_panel={},
title={},
authors={},
abstract={},
persons_number={0},
pdate={19Apr06 19:59:38},
date={20Apr06 22:34:27}
}

@inproceedings {Matthieu_Renaud,
email={mrenaud@cea.fr},
first_name={Matthieu},
last_name={Renaud},
affiliation={CEA/DSM/DAPNIA/SAp},
address={L'Orme des Merisiers, 91191 Gif-sur-Yvette, France},
presentation_type={oral},
presentation_number={1},
presentation_panel={B5},
title={INTEGRAL observations of young Galactic supernova remnants},
authors={Vink, J., Decourchelle A., Lebrun, F., Terrier R.},
abstract={We will present results based on INTEGRAL IBIS/ISGRI observations on young Galactic Supernova remnants in the line emission of $^{44}$Ti at 68 and 78 keV as well as in the hard X-ray / soft gamma-ray nonthermal continuum emission. $^{44}$Ti is a radioactive nucleus exclusively produced in SNe during the first stages of the explosion. It has a lifetime of about 85 y and is then the best indicator of (very) young SNe, as examplified by the detection of $^{44}$Ti in the youngest galactic SNR Cas A with COMPTEL and latter with BeppoSAX. In addition, the study of the nonthermal continuum emission in the gamma-ray domain combined with multi-wavelength observations (Radio, X-ray, TeV energies) may help us to better understand the mechanisms of particle acceleration at work in young SNRs.},
persons_number={0},
pdate={01Mar06 17:14:45},
date={20Apr06 22:35:32}
}

@inproceedings {Joseph_Dolan,
email={Joseph.F.Dolan@nasa.gov},
first_name={Joseph},
last_name={Dolan},
affiliation={NASA Goddard Space Flight Center},
address={Mail Code 662, Greenbelt, MD 20771 USA},
presentation_type={poster},
presentation_number={1},
presentation_panel={H0},
title={1-8 MeV photometry of pulsars},
authors={},
abstract={Maximum liklihood fits to SPI data produce a biased flux estimate when the number of energy channels fit to the spectrum is small (cf. Carson 2006). We find that the bias is consistent when one energy channel is used, and so can do photometry by calibrating the results using sources with known spectra. We present 1-8 MeV photometry of pulsars using SPI. Other than the calibration sources (Crab and Vela pulsars), the results are stated as upper limits.},
persons_number={0},
pdate={11Mar06 01:59:44},
date={20Apr06 22:42:12}
}

@inproceedings {M._Ali_Alpar,
email={alpar@sabanciuniv.edu},
first_name={M. Ali},
last_name={Alpar},
affiliation={Sabanci University},
address={Orhanli-Tuzla, 34956 Istanbul, Turkey},
presentation_type={oral},
presentation_number={1},
presentation_panel={I4},
title={A review on fallback disks and magnetars},
authors={},
abstract={Some bound matter in the form of a fallback disk may be an initial parameter of isolated neutron stars at birth, which, along with the initial rotation rate and dipole (and higher multipole) magnetic moments, determines the evolution of neutron stars and the categories into which they fall. This talk reviews the strengths and difficulties of fallback disk models in explaining properties of isolated neutron stars of different categories. Evidence for and observational limits on fallback disks will also be discussed. High energy magnetospheric emission with or without the presence of a disk will also be discussed.},
persons_number={},
pdate={01Mar06 15:33:21},
date={20Apr06 23:49:53}
}

@inproceedings {Nail_Gehrels,
email={gehrels@milkyway.gsfc.nasa.gov},
first_name={Nail},
last_name={Gehrels},
affiliation={GSFC},
address={Code 661, NASA-GSFC, Greenbelt, MD 20771},
presentation_type={oral},
presentation_number={1},
presentation_panel={I1},
title={Highlights from SWIFT},
authors={N. Gehrels},
abstract={Swift was launched in November 2004 and is performing successfully on orbit. It has a primary objective to study gamma-ray bursts and secondary objectives covering many areas of high energy astrophysics. A new-technology wide-field gamma-ray camera detects about a hundred bursts per year. Sensitive narrow-field X-ray and UV/optical telescopes, built in collaboration with UK and Italian partners, are pointed at the burst location in $\sim1$ minute by an autonomously controlled Swift spacecraft. For each burst, arcsec positions are determined and optical/UV/X-ray/gamma-ray spectrophotometry performed. Information is also rapidly sent to the ground to a team of more than 50 observers at telescopes around the world. The observatory is also valuable for transient source studies. In addition, the on-board instruments are performing surveys and source observations in the optical, X-ray and hard X-ray bands. An all-sky hard X-ray survey by the wide-field gamma-ray camera is complementary to the galactic plane survey by INTEGRAL. Results from the first 1.5 years of operation will be presented. The many synergies between Swift and INTEGRAL will be discussed.},
persons_number={0},
pdate={10Apr06 00:00:00},
date={21Apr06 01:52:43}
}

@inproceedings {Teruaki_Enoto,
email={enoto@amalthea.phys.s.u-tokyo.ac.jp},
first_name={Teruaki},
last_name={Enoto},
affiliation={The University of Tokyo},
address={Makishima group, Physics department of science, The University of Tokyo, Hongo 7-3-1, Bunkyo-ku, Tokyo, Japan},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={Wide-band study of X-ray pulsars with Suzaku},
authors={T.Enoto, T.Mihara, Y.Terada, M.Nakajima, M.Suzuki, K.Makishima, H.Takahashi, S.Naik, F.Nagase, S.Kitamoto, K.Sudoh, A.Yoshida, Y.Nakagawa, S.Sugita, T.Kohmura, T.Kotani, D.Yonetoku, M.Kokubun, A.Bamba, K.Tamura, K.Mori},
abstract={Carrying onboard the XIS (X-ray Imaging Spectrometer) and the HXD (Hard X-ray Detector), Suzaku allows high-sensitivity studies of X-ray pulsars over a wide energy band (0.4-600 keV). We have so far observed several X-ray pulsars, such as the Crab pulsar, PSR 1509-58, Her X-1, and A0535-26, partially for the purpose of calibrating the HXD timing accuracy and the HXD energy scale. We will report some first results, both technical and scientific, including the cyclotron resonance line of A0535+26 which was successfully detected even when the object was in a very low (about $4\times10^{35}$ erg s$^{-1}$) luminosity state.},
persons_number={0},
pdate={01Mar06 05:48:03},
date={21Apr06 07:13:30}
}

@inproceedings {XiaoLing_Zhang,
email={zhangx@mpe.mpg.de},
first_name={XiaoLing},
last_name={Zhang},
affiliation={MPE},
address={Giessenbach Strasse 1},
presentation_type={none},
presentation_number={1},
presentation_panel={},
title={},
authors={},
abstract={},
persons_number={0},
pdate={03Apr06 11:55:00},
date={21Apr06 11:44:11}
}

@inproceedings {Ignacio_Negueruela,
email={ignacio@dfists.ua.es},
first_name={Ignacio},
last_name={Negueruela},
affiliation={University of Alicante},
address={DFISTS,EPSA, Universidad de Alicante, PO Box 99, E03080 Alicante, Spain},
presentation_type={oral},
presentation_number={1},
presentation_panel={e0},
title={Characterization of Supergiant Fast X-ray Transients as a class},
authors={D.M. Smith, P.Reig, J.M. Torrej\'on},
abstract={INTEGRAL is finding large numbers of fast transients. We have shown that, at least, a significant fraction of them are associated with OB supergiants (SFXTs). Our ongoing observational campaign on SFXTs with a range of space and ground telescopes, including the VLT, has allowed us to identify new counterparts and derive their astrophysical parameters. We will present new data on the counterparts to SFXT and derive their distances and X-ray luminosities. With these new data we will be ready to start characterizing the class of SFXTs.},
persons_number={1},
pdate={24.02.06 01:00:18},
date={21Apr06 12:33:37}
}

@inproceedings {Ascension_Camero-Arranz,
email={ascension.camero@uv.es},
first_name={Ascension},
last_name={Camero-Arranz},
affiliation={GACE, Instituto de Ciencias de los Materiales, Universidad de Valencia},
address={PO Box 20085, 46071-Valencia, Spain},
presentation_type={poster},
presentation_number={2},
presentation_panel={G0},
title={Long-term frequency history of the Be/X-binary system SAX J2103.5+4545},
authors={Colleen Wilson, Mark Finger, Ascension Camero-Arranz},
abstract={We have carried out a long-term pulse-timing analysis of the transient X-ray pulsar SAX J2103.5+4545 using data from the INTEGRAL and the RXTE missions. This X-ray binary system was observed from 1999 to 2004 by the RXTE Proportional Counter Array (PCA), and by INTEGRAL, from 2002 to 2005, during the Performance and Verification (PV) phase and the Galactic Plane Scan (GPS) survey. We will present the long-term flux, frequency, and spin-up rate histories. Moreover, an analysis of the correlation between the flux and spin-up rate will be shown. A new set of orbital parameters has been determined from the analysis, which is more precise than those that have been previously published.},
persons_number={0},
pdate={01Mar06 22:09:04},
date={21Apr06 12:44:26}
}

@inproceedings {Ascension_Camero-Arranz,
email={ascension.camero@uv.es},
first_name={Ascension},
last_name={Camero-Arranz},
affiliation={GACE, Instituto de Ciencias de los Materiales, Universidad de Valencia},
address={PO Box 20085, 46071-Valencia, Spain},
presentation_type={poster},
presentation_number={1},
presentation_panel={E0},
title={The Scutum Galactic Arm survey},
authors={Ascension Camero-Arranz, Anthony Bird, Paul H. Connell, Silvia Martinez-Nußez},
abstract={The Scutum Galactic arm has been proposed to be the site of vigorous recent star formation. We will present imaging, spectral and timing results of the Scutum survey performed by the three high-energy instruments on board INTEGRAL. In addition, data from the GPS and GCDE of the same region have been used. The aim of the present work is to detect for the first time the transient sources embedded in this dense molecular cloud, as well as those fainter persistent supergiant ones. A proof of the existence of such a population of highly absorbed X-ray sources is the detection of four INTEGRAL sources (IGR J19140+0951, IGR J18450-0435, IGR J18483-0311, IGR J18027-2016) in the 20 to 40 keV band by ISGRI. Moreover, preliminary analysis of the data suggests the presence of several new sources. },
persons_number={0},
pdate={01Mar06 15:35:09},
date={21Apr06 12:45:19}
}

@inproceedings {Lorraine_Hanlon,
email={lorraine.hanlon@ucd.ie},
first_name={Lorraine},
last_name={Hanlon},
affiliation={University College Dublin},
address={School of Physics, UCD, Belfield, Dublin 4, Ireland},
presentation_type={oral},
presentation_number={1},
presentation_panel={I5},
title={Gamma-ray bursts detected by INTEGRAL},
authors={},
abstract={The INTEGRAL satellite's Burst Alert System (IBAS) has detected and localised over 35 GRBs to date. We discuss the global characteristics of this GRB sample, using data obtained from the imager, IBIS, and spectrometer, SPI, on board INTEGRAL. Spectral, spatial and temporal characteristics of the prompt gamma-ray emission will be presented for a selection of GRBs. Particular emphasis will be placed on the characteristics of a subset of weak, long bursts which tend to be X-ray rich. A small number of INTEGRAL GRBs have also been detected by the BAT on board Swift. Spectral analyses of these GRBs will be presented. In the region where the instruments overlap in energy a relative calibration may be performed to verify the absolute efficiency of either instrument.},
persons_number={0},
pdate={01Mar06 12:59:03},
date={21Apr06 13:51:38}
}

@inproceedings {Irek_Khamitov,
email={irekk@tug.tug.tubitak.gov.tr},
first_name={Irek},
last_name={Khamitov},
affiliation={TUBITAK National Observatory},
address={TUG, 07052, Akdeniz Universitesi Yerleskesy, Antalya, Turkey},
presentation_type={poster},
presentation_number={1},
presentation_panel={D0},
title={Photometry and spectroscopy of IGR J21247+5058 radiogalaxy with RTT150},
authors={I.Khamitov, I.Bikmaev, Z.Aslan, N.Sakhibullin, M.Revnivtsev, R.Sunyaev },
abstract={We present results of photometry and spectroscopy of IGR J21247+5058 made by using 1.5-m optical telescope RTT150 with Andor CCD and TFOSC instrument. R-band images obtained at 0.8 arcsec seeing conditions have allowed us to separate foreground star from point-like extragalactic source and estimate their brightness separately. Low-resolution but high $S/N$ ratio spectra of this optically combined source is confirming the presence of red-shifted H$_{\alpha}$ emission line of extragalactic nature. Physical properties of radio-galaxy are briefly discussed.},
persons_number={0},
pdate={28Feb06 09:17:22},
date={21Apr06 14:26:26}
}

@inproceedings {Ruben_Farinelli,
email={farinelli@fe.infn.it},
first_name={Ruben},
last_name={Farinelli},
affiliation={Physics Departement, Ferrara University},
address={via Saragat 1 44100 Ferrara},
presentation_type={oral},
presentation_number={1},
presentation_panel={G2},
title={Average hard X-ray emission from neutron star LMXBs: a view with INTEGRAL},
authors={},
abstract={We present the results of 2 years of INTEGRAL monitoring on LMXBs hosting a neutron star. Our sample comprises all the six known bright sources belonging to the Z class and four bright sources of the atoll class which share several spectral properties with Z sources. We focus on the average spectral properties of these sources, in particular above 30 keV, where we investigate for the presence of power-law like hard X-ray tails.},
persons_number={0},
pdate={28Feb06 21:38:23},
date={21Apr06 14:52:51}
}

@inproceedings {Linnea_Hjalmarsdotter,
email={nea@astro.helsinki.fi},
first_name={Linnea},
last_name={Hjalmarsdotter},
affiliation={Observatory, University of Helsinki},
address={P.O Box 14, 00014 Helsinki, Finland},
presentation_type={poster},
presentation_number={1},
presentation_panel={F0},
title={The nature of the hard state of Cygnus X-3},
authors={L. Hjalmarsdotter, A. A. Zdziarski, S. Larsson, A. Paizis, V. Beckmann},
abstract={TBA},
persons_number={0},
pdate={28Feb06 18:53:56},
date={21Apr06 15:01:07}
}

@inproceedings {Wei_Wang,
email={wwang@mpe.mpg.de},
first_name={Wei},
last_name={Wang},
affiliation={Max-Planck Institute for Extraterrestrial Physics},
address={Giessenbachstrasse 1, 85741 Garching, Germany},
presentation_type={oral},
presentation_number={1},
presentation_panel={B3},
title={SPI observations of $^{60}$Fe lines in the Galaxy},
authors={W. Wang, M.J.Harris, R. Diehl, H. Halloin, C. Ciemiuk, A.W. Strong},
abstract={Following its detection of the gamma-ray lines at 1173 and 1333 keV from 60Fe in data obtained during its first year, the SPI on board INTEGRAL has accumulated two further years' worth of data. We have analyzed these data, obtaining a more precise measurement of the flux in both two lines ($4\pm 1.6 \times 10^{-5}$ ph cm$^{-2}$ s$^{-1}$ per line) which is in agreement with our earlier result. We discuss the implications of these results for the widely-held hypothesis that $^{60}$Fe is synthesized in core-collapse supernovae, and for the closely-related question of the precise origin of $^{26}$Al in massive stars.},
persons_number={0},
pdate={17.02.06 12:33:08},
date={21Apr06 15:09:40}
}

@inproceedings {Elisabeth_Jourdain,
email={jourdain@cesr.fr},
first_name={Elisabeth},
last_name={Jourdain},
affiliation={CESR},
address={9 avue du Colonel Roche, 31028 TOULOUSE, FRANCE},
presentation_type={none},
presentation_number={1},
presentation_panel={},
title={},
authors={},
abstract={},
persons_number={0},
pdate={20Apr06 19:33:38},
date={21Apr06 16:27:03}
}

@inproceedings {John_Stephen,
email={stephen@iasfbo.inaf.it},
first_name={John},
last_name={Stephen},
affiliation={IASF-INAF},
address={Via Gobetti 101, 40129 Bologna, ITALY},
presentation_type={poster},
presentation_number={1},
presentation_panel={E0},
title={Using the correlation between ISGRI survey results and other catalogues to help in source identification},
authors={},
abstract={We have developed a tool with which to easily perform correlations between sources in various catalogues. It has already been used with the ROSAT all-sky catalogues resulting in the identification of a number of sources and leading to optical follow-up observations. We demonstrate the capability with several other catalogues.},
persons_number={1},
pdate={01Mar06 20:08:25},
date={21Apr06 16:53:29}
}

@inproceedings {Jerome_Chenevez,
email={jerome@dnsc.dk},
first_name={Jerome},
last_name={Chenevez},
affiliation={Danish National Space Center},
address={Juliane Maries Vej 30, DK 2100 Copenhagen, Denmark},
presentation_type={poster},
presentation_number={1},
presentation_panel={E0},
title={A JEM-X catalog of X-ray Sources},
authors={Niels J. Westergaard, Jerome Chenevez, Niels Lund, S$\o$ren Brandt, Carl Budtz-J$\o$rgensen},
abstract={Based on public data from the first 259 revolutions of INTEGRAL and the survey program data (Galactic Plane Scans and Galactic Center Exposures) all found sources have been combined into a single catalog. About 110 sources have been identified and in some cases improved position determinations have been obtained. The sources are searched both in the single Science Windows and in mosaic sky images. For selected sources spectra and lightcurves are presented.},
persons_number={0},
pdate={01Mar06 18:43:35},
date={21Apr06 17:10:30}
}

@inproceedings {S$\o$ren_Brandt,
email={sb@spacecenter.dk},
first_name={S$\o$ren},
last_name={Brandt},
affiliation={Danish National Space Center},
address={Juliane Mariesvej 30, DK-2100, Copehagen, Denmark},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={X-ray bursts observed with JEM-X},
authors={},
abstract={We report on the search for X-ray bursts, X-ray flashes, soft gamma repeater events, and untriggered gamma-ray bursts in the JEM-X ray monitor on INTEGRAL during the first two years of operations. },
persons_number={0},
pdate={01Mar06 19:16:12},
date={21Apr06 17:13:20}
}

@inproceedings {J._Miguel_Mas-Hesse,
email={mm@laeff.inta.es},
first_name={J. Miguel},
last_name={Mas-Hesse},
affiliation={Centro de Astrobiologia (CSIC-INTA)},
address={POB 50727 28080 Madrid Spain},
presentation_type={poster},
presentation_number={1},
presentation_panel={J0},
title={The Optical Monitoring Camera onboard INTEGRAL},
authors={},
abstract={The Optical Monitoring Camera (OMC) is observing the optical emission from the prime targets of the gamma-ray instruments onboard the ESA mission INTEGRAL, with the support of the JEM-X monitor in the X-ray domain. This capability provides invaluable diagnostic information on the nature and the physics of the sources over a broad wavelength range. Its main scientific objectives are: (1) to monitor the optical emission from the sources observed by the gamma- and X-ray instruments, measuring the time and intensity structure of the optical emission for comparison with variability at high energies, and (2) to provide the brightness and position of the optical counterpart of any gamma- or X-ray transient taking place within its field of view. The OMC is based on a refractive optics with an aperture of 50 mm focused onto a large format CCD (1024 X 2048 pixels) working in frame transfer mode (1024 X 1024 pixels imaging area). With a field of view of 5 deg X 5 deg OMC is able to monitor sources down to magnitude $V=17$. Typical observations are performing a sequence of different integration times, allowing for photometric uncertainties below 0.1 magnitude for objects with $V<16$.},
persons_number={0},
pdate={28Feb06 19:50:31},
date={21Apr06 17:35:37}
}

@inproceedings {Kazuhiro_Nakazawa,
email={nakazawa@astro.isas.jaxa.jp},
first_name={Kazuhiro},
last_name={Nakazawa},
affiliation={Institute of Space and Astronautical Science, Japan Aerospace Exploration Egency},
address={},
presentation_type={oral},
presentation_number={1},
presentation_panel={E3},
title={Hard X-ray view from initial half year observations of Suzaku},
authors={Kazuhiro Nakazawa, Kazuhisa Mitsuda, Tadayuki Takahashi (ISAS/JAXA), Hideyo Kunieda (Nagoya-U), Kazuo Makishima (Univ. Tokyo), Tuneyosi Kamae (SLAC) and the Suzaku-team},
abstract={Suzaku satellite, launched into orbit at 10th July 2005, is equipped with four X-ray CCD cameras (XISs) combined with X-ray mirror optics (XRTs) covering 0.3-12 keV, as well as a hard X-ray detector (HXD) covering 10-600 keV. The HXD is characterized with the lowest detector background ever achieved, e.g. several times $10^{-5}$ cts s$^{-1}$ cm$^{-2}$ keV$^{-1}$ at 10-50 keV and the XISs also show more stable and lower detector background in comparison with contemporary CCD detectors. Together with its wide band-pass from 0.3 to several hundred keV, Suzaku is a powerful tool to explore the high energy universe and its non thermal phenomena. Within the first half year, Suzaku has observed more than 100 sources, such as binaries, SNRs, Galactic center region, AGNs, galaxies and clusters of galaxies. Some of the major hard X-ray results are provided in other talks, while this talk will mainly present the in orbit performance and characteristics of Suzaku as a hard X-ray observatory. Brief summary of initial scientific results will also be presented.},
persons_number={0},
pdate={02Mar06 12:50:32},
date={21Apr06 17:41:35}
}

@inproceedings {Erik_Kuulkers,
email={ekuulker@rssd.esa.int},
first_name={Erik},
last_name={Kuulkers},
affiliation={ISOC, ESAC/ESA},
address={Apartado 50727},
presentation_type={oral},
presentation_number={1},
presentation_panel={E5},
title={An unshrouded view of our lively Galactic Bulge},
authors={et al.},
abstract={The Galactic Bulge region is a rich host of variable high-energy X-ray and gamma-ray point sources. These sources include bright and relatively faint X-ray transients, X-ray bursters, persistent neutron star and black-hole candidate binaries, high-mass X-ray binaries, etc.. We have a program to monitor the Galactic Bulge region regularly and frequently with the gamma-ray observatory INTEGRAL. As a service to the scientific community the high-energy light curves of sources present are made available through the WWW. We show the preliminary results of this exciting new program. },
persons_number={0},
pdate={23.02.06 12:18:57},
date={21Apr06 17:58:24}
}

@inproceedings {Loredana_Bassani,
email={bassani@iasfbo.ianf.it},
first_name={Loredana},
last_name={Bassani},
affiliation={IASF/INAF Bologna},
address={Via Gobetti 101,40129 Bologna Italy},
presentation_type={oral},
presentation_number={1},
presentation_panel={D2},
title={INTEGRAL/IBIS extragalactic survey: 20-100 keV selected AGN},
authors={},
abstract={Analysis of INTEGRAL Core Program and public Open Time observations provides a sample of extragalactic sources selected in the 20-100 keV band above a flux of $\sim10^{-11}$ erg cm$^{-2}$ s$^{-1}$; since this band probes heavily obscured regions/objects, i.e. those that could be missed in optical, UV, and even X-ray surveys, our sample offers the opportunity of studying the extragalactic sky from a different point of view with respect to surveys at lower energies. We present the results of our analysis, with particular emphasis on Active Galaxies, complemented by follow up oservations at optical and X-ray frequencies. We discuss the overall characteristics of individual objects as well as of the entire sample. We also present the AGN 20-100 keV Log$N$/Log$S$ distribution and luminosity function derived from our sample.},
persons_number={0},
pdate={01Mar06 18:46:52},
date={21Apr06 18:03:00}
}

@inproceedings {Viktor_Grafutin,
email={grafutin@itep.ru},
first_name={Viktor},
last_name={Grafutin, Eugene Svetlov-Prokop'ev},
affiliation={Institute for Theoretical and Experimental Physics, FSUF SSC},
address={B.Cheremushkinskaya 25, Moscow, Russia},
presentation_type={poster},
presentation_number={1},
presentation_panel={A0},
title={Research of positron states in space plasma},
authors={A.L. Suvorov, Yu.V. Funtikov, V.I. Grafutin, T.L. Razinkova, E.P. Svetlov-Prokop'ev, A.F. Zakharov, A.I. Alikhanov},
abstract={Features and some ways of researches of a problem of physics, chemistry and technology of antimatter are discussed in brief. Properties positron sources and positron states in galactic and extragalactic environments with low density are analyzed. We follow the standard assumption that the nature positron sources is possibly caused by SN explosions or activities of galactic black holes or supermassive black holes in the centers of galaxies (including our Galaxy). It is established, that by the basic positron states in space plasma are fast (including relativistic and ultra relativistic) positrons, slow and `termalized' positrons, positronium atoms and the bound states of positrons on hydrogen atoms, other atoms and molecules of the various nature and particle a dust (in galactic and extragalactic environments). Positron annihilation from positronium and the connected positron states in atoms of space plasma lead to change of spectra of annihilation radiations that corresponds to available experimental data on positron annihilation in various environments. It is indicated, that observations for 0.511 MeV annihilation line an extraterrestrial origin allow to receive the information on some properties of space environment in which has taken place positron annihilation, by example, on particle of dusty space plasma. },
persons_number={2},
pdate={13Apr06 11:43:32},
date={21Apr06 18:03:21}
}

@inproceedings {Eugene_Svetlov-Prokop'ev,
email={epprokopiev@mail.ru},
first_name={Eugene},
last_name={Svetlov-Prokop'ev},
affiliation={Institute for Theoretical and Experimental Physics, FSUF SSC},
address={B.Cheremushkinskaya 25, Moscow, Russia},
presentation_type={none},
presentation_number={1},
presentation_panel={A0},
title={Research of positron states in space plasma},
authors={A.L.Suvorov, Yu.V.Funtikov, V.I.Grafutin, T.L.Razinkova, E.P.Svetlov-Prokop'ev, A.F.Zakharov A.I.Alikhanov},
abstract={Features and some ways of researches of a problem of physics, chemistry and technology of antimatter are discussed in brief. Properties positron sources and positron states in galactic and extragalactic environments with low density are analyzed. We follow the standard assumption that the nature positron sources is possibly caused by SN explosions or activities of galactic black holes or supermassive black holes in the centers of galaxies (including our Galaxy). It is established, that by the basic positron states in space plasma are fast (including relativistic and ultra relativistic) positrons, slow and `termalized'´positrons, positronium atoms and the bound states of positrons on hydrogen atoms, other atoms and molecules of the various nature and particle a dust (in galactic and extragalactic environments). Positron annihilation from positronium and the connected positron states in atoms of space plasma lead to change of -spectra of annihilation radiations that corresponds to available experimental data on positron annihilation in various environments. It is indicated, that observations for 0.511 MeV annihilation line an extraterrestrial origin allow to receive the information on some properties of space environment in which has taken place positron annihilation, by example, on particle of dusty space plasma.},
persons_number={2},
pdate={13Apr06 11:43:32},
date={21Apr06 18:04:52}
}

@inproceedings {Antonella_Tarana,
email={antonella.tarana@iasf-roma.inaf.it},
first_name={Antonella},
last_name={Tarana},
affiliation={IASF-Roma INAF; Dip. di Fisica Universiti Tor Vergata di Roma},
address={},
presentation_type={poster},
presentation_number={2},
presentation_panel={G0},
title={High energy behaviour of the LMXB XB~1832-33},
authors={},
abstract={The Low Mass X-ray Binary XB 1832-33 is located in the globular cluster NGC 6652 and is a type I X-ray bursts source. We present the preliminary results about the temporal behaviuor of this source performed with IBIS and JEM-X instruments. We also present results on the spectral analysis.},
persons_number={0},
pdate={01Mar06 20:13:20},
date={21Apr06 18:12:14}
}

@inproceedings {Antonella_Tarana,
email={antonella.tarana@iasf-roma.inaf.it},
first_name={Antonella},
last_name={Tarana},
affiliation={IASF-Roma INAF; Dip. di Fisica Universiti Tor Vergata di Roma},
address={},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={INTEGRAL spectral variations study of the LMXB 4U~1820-30: first detection of hard X-ray emission},
authors={},
abstract={4U 1820-30 is a Low Mass X-ray Binary located in the Globular Cluster NGC 6624. This source is a burster classified as Atoll source. We present the temporal and spectral analysis and also the evolution in the Hardness-Intensity Diagram with the IBIS and JEM-X instruments on board INTEGRAL satellite. Spectral state variations are looked for during the long observing period, 2003 March 12th up to 2005 October 5th.},
persons_number={0},
pdate={01Mar06 20:07:34},
date={21Apr06 18:20:56}
}

@inproceedings {Pierrick_Martin,
email={martin@cesr.fr},
first_name={Pierrick},
last_name={Martin},
affiliation={CESR},
address={9, avenue du Colonel Roche - 31028 Toulouse - FRANCE},
presentation_type={poster},
presentation_number={1},
presentation_panel={B0},
title={Search for the $^{44}$Ti lines in Cas A with INTEGRAL/SPI},
authors={},
abstract={$^{44}$Ti has already become famous as one of the few radioisotopes accessibles to gamma-ray astronomy. It originates mostly from the depths of core-collapse supernovae, and decays with a mean lifetime of 86 yr, hence constituting a powerful tool to probe into the intimacies of the most recent supernovae, known or obscured. As a necessary first step in the study of supernova explosions from the $^{44}$Ti gamma-ray line emission, we present the results obtained on Cassiopea A from about 4Ms of observation with INTEGRAL/SPI. The analyses of two of the three lines of the decay chain (at 78.4 and 1157.0 keV) will be reported, and their outcomes discussed in terms of constraints on the explosion scenario, consistency with previous detections (by CGRO and BeppoSax),and prospects for the discovery of young SNR using $^{44}$Ti signals.},
persons_number={0},
pdate={01Mar06 14:35:42},
date={21Apr06 18:29:01}
}

@inproceedings {Michael_Forot,
email={mforot@cea.fr},
first_name={Michael},
last_name={Forot},
affiliation={Service d'Astrophysique CEA Saclay},
address={91191 Gif sur Yvette},
presentation_type={poster},
presentation_number={1},
presentation_panel={H0},
title={INTEGRAL observation of the pulsar wind nebula powered by the pulsar PSR B1509-58},
authors={},
abstract={We present observations with the INTEGRAL/IBIS telescope of the pulsar wind nebula powered by the young pulsar PSR B1509-58 and discuss spatial and spectroscopic properties in the energy range 20-300 keV. The spectra of the unpulsed component is fitted by a power law with a photon index of $\alpha = -2.12 \pm 0.05$ with an high energy spectral break seen closed to 120 keV. Joint results from INTEGRAL, HESS and BeppoSax observations allows us to constrain the electron maximum energy available which is not far from a few hundred Tev. Emission models are also discussed thanks to this multiwavelenght result.},
persons_number={0},
pdate={01Mar06 19:03:55},
date={21Apr06 18:42:26}
}

@inproceedings {Toru_Tamagawa,
email={tamagawa@riken.jp},
first_name={Toru},
last_name={Tamagawa},
affiliation={RIKEN, The Institute of Physical and Chemical Research},
address={2-1 Hirosawa, Wako, Saitama 351-0198, Japan},
presentation_type={oral},
presentation_number={1},
presentation_panel={i0},
title={GRB Observations with Suzaku Wideband All-sky Monitor},
authors={T. Tamagawa, K. Yamaoka, M. Ohno, Y. Terada, M. Tashiro, M. Kokubun, K. Makishima, Y. Fukazawa, K. Nakazawa, T. Takahashi and the Suzaku HXD-WAM team},
abstract={The shield counters of Hard X-ray Detector onboard Suzaku are designed to use as the Wideband All-sky Monitor (WAM). The WAM is a very powerful Gamma-ray Burst monitor which covers the energy range between 50 keV and 5 MeV with large effective area of $400$ cm$^2$ even at 1 MeV. The conjunctive observations with Swift Burst Alert Telescope, the WAM enable us to study the unbiased $E_{\rm peak}$ observation over the energy range of 15 keV to 5 MeV. The WAM has detected 45 GRBs coincident with the other satellites from 22 August 2005 through 15 January 2006. The detection rate is about 100 GRBs per year, which is consistent with our expectation before launch. So far, the WAM detected the gamma-ray emission up to 1 MeV from at least 8 GRBs including a bright and hard GRB 051008. In the conference, we present the new spectral properties of GRBs observed by the WAM.},
persons_number={0},
pdate={02Mar06 03:10:54},
date={21Apr06 18:58:37}
}

@inproceedings {Angela_Bazzano,
email={angela.bazzano@iasf-roma.inaf.it},
first_name={Angela},
last_name={Bazzano},
affiliation={IASF-Roma/INAF},
address={Area di Ricerca Tor Vergata, Via Fosso del Cavaliere 100, 00133 Roma, Italy},
presentation_type={oral},
presentation_number={1},
presentation_panel={G1},
title={An INTEGRAL view on X-ray bursters},
authors={},
abstract={A broald band spectral study of low mass X-ray binaries containing neutron star performed with INTEGAL will be presented. A sample consisting of about 40 sources has been monitored as part of the IBIS Survey to follow the high energy behaviour. New high energy characteristic have been detected for a sub-sample of sources and states transitions as well. INTEGRAL observations are compared to previous and current in orbit satellites data.},
persons_number={0},
pdate={01Mar06 19:23:05},
date={21Apr06 19:10:39}
}

@inproceedings {Melania_Del_Santo,
email={melania.delsanto@iasf-roma.inaf.it},
first_name={Melania},
last_name={Del Santo},
affiliation={INAF/IASF-Roma},
address={via del Fosso del Cavaliere 100, I-00133, Roma},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={First high energy study of the mysterious source 1E~1743.1-2843},
authors={},
abstract={In the last years, the persistent source 1E~1743.1-2843, lying at few arcminutes from the Galactic Centre, has been observed above 2 keV by all instruments with X-ray imaging capability. Neither type-I X-ray bursts nor pulsations providing indication on the nature of the compact object have ever been detected. Before the INTEGRAL satellite, the source was detected only up to 20 keV. In the framework of the IBIS telescope survey, the first detection at high energy (20-40 keV) was obtained. In previous works, it was stressed that a possible high energy emission could give further indications on the accreting object. We report on results obtained with the INTEGRAL/IBIS data collected during the period 2003-2005 and public XMM-Newton and Chandra X-ray observations. We present the temporal study in the 20-40 keV band showing a rather constant flux on few months time scale, as well as the first broad-band spectral study (2-70 keV) showing a steep power law ($\sim3$) as high energy component. Combining spectral parameters and discussion about the luminosity evaluations for different possible distances, our conclusions are in favour of a LMXB system with a neutron star at distance higher than the Galactic Centre, even though a firm conclusion can not be stated.},
persons_number={0},
pdate={01Mar06 23:28:06},
date={21Apr06 19:11:18}
}

@inproceedings {Melania_Del_Santo,
email={melania.delsanto@iasf-roma.inaf.it},
first_name={Melania},
last_name={Del Santo},
affiliation={INAF/IASF-Roma},
address={via del Fosso del Cavaliere 100, I-00133, Roma},
presentation_type={poster},
presentation_number={2},
presentation_panel={F0},
title={Long term monitoring of the BHC 1E 1740.7-2942},
authors={},
abstract={The microquasar 1E 1740.7-2942 is one of the most appealing source of the Galactic Centre region. The nature of the star companion is still unknown and, so far, the high energy feature detected once by SIGMA has been never observed again. Classified as a persistent source starting from February 2004 and for few months after, it showed an unusual quiescent-like state, since it was not detected either with X-ray and soft gamma-ray detectors. We present results of the long term monitoring of 1E 1740.7-2942 over 3 years of INTEGRAL observations, in order to look for flux modulations previously observed with RXTE in the X-rays, and possible spectral transitions.},
persons_number={0},
pdate={06Mar06 21:34:36},
date={21Apr06 19:11:45}
}

@inproceedings {J\"urgen_Kn\"odlseder,
email={knodlseder@cesr.fr},
first_name={J\"urgen},
last_name={Kn\"odlseder},
affiliation={Centre d'Etude Spatiale des Rayonnements},
address={9, avenue Colonel-Roche, 31000 Toulouse, FRANCE },
presentation_type={poster},
presentation_number={1},
presentation_panel={J0},
title={GRI: The Gamma-Ray Imager mission},
authors={},
abstract={Observations of the gamma-ray sky reveal the most powerful sources and the most violent events in the Universe. While at lower wavebands the observed emission is generally dominated by thermal processes, the gamma-ray sky provides us with a view on the non-thermal Universe. Here particles are accelerated to extreme relativistic energies by mechanisms which are still poorly understood, and nuclear reactions are synthesizing the basic constituents of our world. Cosmic accelerators and cosmic explosions are the major science themes that are addressed in the gamma-ray regime. With the INTEGRAL observatory, ESA has provided a unique tool to the astronomical community and has put Europe in the lead in the field of gamma-ray astronomy. INTEGRAL provides an unprecedented survey of the soft gamma-ray sky, revealing hundreds of sources, new classes of objects, extraordinary views of antimatter annihilation in our Galaxy, and fingerprints of recent nucleosynthesis processes. While INTEGRAL has provided the global overview over the soft gamma-ray sky, there is a growing need to perform deeper, more focused investigations of gamma-ray sources. In soft X-rays a comparable step was taken going from the Einstein satellite to the XMM/Newton observatory. Technological advances in the past years in the domain of gamma-ray focusing using Laue diffraction and multilayer-coated mirror techniques have paved the way towards a gamma-ray mission, providing major improvements compared to past missions regarding sensitivity and angular resolution. Such a future Gamma-Ray Imager will allow to study particle acceleration processes and explosion physics in unprecedented detail, providing essential clues on the innermost nature of the most violent and most energetic processes in the Universe. },
persons_number={0},
pdate={27Feb06 12:26:44},
date={21Apr06 19:34:30}
}

@inproceedings {J\"urgen_Kn\"odlseder,
email={knodlseder@cesr.fr},
first_name={J\"urgen},
last_name={Kn\"odlseder},
affiliation={Centre d'Etude Spatiale des Rayonnements},
address={9, avenue Colonel-Roche, 31000 Toulouse, FRANCE},
presentation_type={oral},
presentation_number={2},
presentation_panel={A1},
title={Imaging the gamma-ray sky with SPI},
authors={},
abstract={The spectrometer SPI on INTEGRAL allows for the first time simultaneous imaging of diffuse and point-like emission in the hard X-ray and soft gamma-ray regime. To fully exploit the capabilities of the instrument, we implemented the MREM image deconvolution algorithm, initially developed for COMPTEL data analysis, to SPI data analysis. We present the performances of the algorithm and apply it to produce allsky maps of continuum and gamma-ray line emission throughout the accessible energy range. },
persons_number={0},
pdate={27Feb06 13:56:12},
date={21Apr06 19:34:57}
}

@inproceedings {Takefumi_Mitani,
email={mitani@astro.isas.jaxa.jp},
first_name={Takefumi},
last_name={Mitani},
affiliation={ISAS/JAXA, Japan},
address={3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan},
presentation_type={oral},
presentation_number={1},
presentation_panel={G3},
title={Study of hard X-ray emission from accreting neutron star binaries with Swift BAT},
authors={T. Mitani, G. Sato, T. Takahashi, K. Nakazawa, M. Tashiro, C. Markwardt, J. Tueller, A. Parsons, S. Barthelmy, N. Gehrels},
abstract={The wide field of view of BAT detector onboard Swift Gamma-ray burst explorer, launched in November 2004, enables us to monitor almost any region of the sky in 15--150 keV band with quasi-daily frequency. Here, we show systematic study of hard X-ray emission from neutron star LMXBs, including luminous six ``Z-sources'' and less luminous sixteen ``Atoll sources'', based on one year observations with Swift. From the 300 days monitoring observation of Sco X-1, the brightest Z-source, we have firmly confirmed the existence of the power law hard tail extending up to at least 100 keV with a photon index of 2.8. We have discovered two distinct spectral states with and without hard tails on a hard X-ray intensity-intensity diagram. The same picture also is applicable to other Z-sources. In regard to atoll sources, soft and hard states are clearly observed with BAT. The spectrum in the hard states of the nearby atoll source 4U1608-522 is interpreted as an inverse Compton scattering by the distribution of hot electrons of about 20 keV. With the complete sample of neutron star LMXBs, we discuss the similarity with stellar black hole binaries in the point of view of very hot, up to 100 keV or even non-thermal population of high energy electrons and their dependency on the mass accretion rate. },
persons_number={0},
pdate={02Mar06 13:26:32},
date={21Apr06 19:58:50}
}

@inproceedings {Celia_Sanchez-Fernandez,
email={celia.sanchez@sciops.esa.int},
first_name={Celia},
last_name={Sanchez-Fernandez},
affiliation={ISOC/ESA},
address={},
presentation_type={poster},
presentation_number={1},
presentation_panel={E0},
title={X-ray bursting sources in the Galactic Bulge Region},
authors={Celia Sanchez-Fernandez, Erik Kuulers, et al.},
abstract={We present here a catalogue of the X-ray bursts detected during the AO-3 Galactic Bulge Observations carried out with INTEGRAL},
persons_number={0},
pdate={01Mar06 21:22:24},
date={21Apr06 20:11:45}
}

@inproceedings {Sheila_McBreen,
email={smcbreen@mpe.mpg.de},
first_name={Sheila},
last_name={McBreen},
affiliation={Max-Planck-Institut fuer extraterrestrische Physik},
address={Giessenbachstrasse, 85748 Garching, Germany.},
presentation_type={none},
presentation_number={1},
presentation_panel={A0},
title={},
authors={},
abstract={},
persons_number={0},
pdate={21Apr06 18:48:08},
date={21Apr06 21:52:28}
}

@inproceedings {Alexei_Pozanenko,
email={apozanen@iki.rssi.ru},
first_name={Alexei},
last_name={Pozanenko},
affiliation={Space Research Institute},
address={Profsoysnaya str., 84/32, Moscow},
presentation_type={poster},
presentation_number={1},
presentation_panel={I0},
title={Observation of optical GRB afterglow with CIS network in 2002-2005},
authors={},
abstract={We present observation of GRB in CIS network (Crimean astrophysical observatory, high altitude Maidank observatory, peak Terskol observatory and Ussurisk observatory). Statistics and main results of observations in 2002-2005 are presented. Based on our observation of GRB021004, GRB041006 and GRB050802 we discuss a range of possible color variation of early afterglow, and confirmed color variation of GRB030329 in the first day. We also discuss models of ``dark'' burst, in particular the most dark GRB051008 registered in our network.},
persons_number={0},
pdate={28Mar06 23:53:41},
date={21Apr06 23:28:43}
}

@inproceedings {St\'ephane_Schanne,
email={schanne@hep.saclay.cea.fr},
first_name={St\'ephane},
last_name={Schanne},
affiliation={DSM/DAPNIA/SAp},
address={CEA Saclay, 91191 Gif-sur-Yvette, France},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={INTEGRAL observations of the Vela region focussing on Vela X-1},
authors={St\'ephane Schanne, Diego G\"otz, Maurizio Falanga, Patrick Sizun, Michael Forot, Andreas von Kienlin, Bertrand Cordier},
abstract={The INTEGRAL satellite observed the Vela region in the X-ray and gamma-ray energy bands during 1.7 Ms between November and December 2005 in the context of an INTEGRAL open-time observation proposal. We present first results of the data analysis, including in particular a spectral and temporal study of the eclipsing high-mass X-ray binary Vela X-1. Thanks to this long-term observation we could update the system parameters and obtain new ephemeris. A precise orbital ephemeris is important for the study of this system, since it allows to determine detailed time-resolved spectra during the eclipse ingress and egress phases in different energy bands, and to monitor details of the companion wind. In addition we derived the time-averaged spectrum of the source, investigating the presence of cyclotron resonant scattering features (CRSF). Orbital and pulse-phase resolved spectroscopy have been performed to understand the underlying physics of the high-energy emission. We studied the variation of the pulse morphology with energy and time. At high energy the profile shows a primary and a secondary peak. Using a relativistic description of the polar-cap emission of the neutron star, we fitted the double-peaked pulse profile in order to model the pulsed flux in energy and constrain the system geometry.},
persons_number={0},
pdate={01Mar06 16:39:51},
date={22Apr06 00:33:12}
}

@inproceedings {St\'ephane_Schanne,
email={schanne@hep.saclay.cea.fr},
first_name={St\'ephane},
last_name={Schanne},
affiliation={DSM/DAPNIA/SAp},
address={CEA Saclay, 91191 Gif-sur-Yvette, France},
presentation_type={poster},
presentation_number={2},
presentation_panel={B0},
title={Search for 1809 keV gamma-ray emission from $^{26}$Al decays in the Vela region with INTEGRAL/SPI},
authors={St\'ephane Schanne, Patrick Sizun, David Maurin, Bertrand Cordier, Andreas von Kienlin},
abstract={The Vela region is a promising target for the detection of gamma-rays emitted by the decays of radioactive isotopes produced in hydrostatic and explosive stellar nucleosynthesis processes, such as $^{26}$Al (gamma-ray energy: 1809 keV), $^{60}$Fe (1173 and 1332 keV) and the associated positrons, detectable through e$^+$ e$^-$ annihilation (511 keV). The importance of the Vela region as a nucleosynthesis laboratory is underlined by the presence of potential nucleosynthesis sites (young Supernova Remnants, Wolf-Rayet stars) at distances as close as a few hundred parsec. COMPTEL observations have revealed 1.8 MeV gamma-ray emission from the Vela region at a level of $3.6\times 10^{-5}$ ph cm$^{-2}$ s$^{-1}$, yet the source of the emission has so far not been identified. In this paper, we present results of our search for $^{26}$Al gamma-ray emission in the Vela region with the spectrometer SPI aboard INTEGRAL, capable of resolving high-energy gamma-ray lines with good sensitivity with its Ge-detectors, using data acquired during 1.7 Ms in November-December 2005 in the frame of the AO-3 open-time observation.},
persons_number={0},
pdate={01Mar06 16:45:06},
date={22Apr06 00:34:52}
}

@inproceedings {St\'ephane_Schanne,
email={schanne@hep.saclay.cea.fr},
first_name={St\'ephane},
last_name={Schanne},
affiliation={DSM/DAPNIA/SAp},
address={CEA Saclay, 91191 Gif-sur-Yvette, France},
presentation_type={poster},
presentation_number={3},
presentation_panel={B0},
title={Type Ia Supernova rate in the Galactic bulge and central molecular zone},
authors={St\'ephane Schanne, Michel Cass\'e, Bertrand Cordier, Jacques Paul},
abstract={According to recent analyses of the type-Ia supernova rate as a function of redshift, prompt and late type-Ia supernovae should explode in the compact molecular zone, a gas rich structure with ongoing star formation, located in the central region of the Milky Way. In this paper we estimate the rate of type-Ia supernovae in the Galactic bulge and compact molecular zone. We show that this rate is insufficient to explain by positron escape from type-Ia supernovae envelopes alone the large positron injection rate into the Galactic central region indicated by the Spectrometer on INTEGRAL (about 1.5 10$^{43}$ s$^{-1}$ corresonding to about 0.7 SN Ia per century). We discuss the influence of the special star formation rate, initial mass function and binarity of the compact molecular zone on this result. },
persons_number={0},
pdate={01Mar06 20:38:25},
date={22Apr06 00:36:05}
}

@inproceedings {Janusz_Ziolkowski,
email={jz@camk.edu.pl},
first_name={Janusz},
last_name={Ziolkowski},
affiliation={Copernicus Astronomical Center},
address={ul. Bartycka 18, 00-716 Warsaw, Poland},
presentation_type={poster},
presentation_number={1},
presentation_panel={F0},
title={Photometric search for black holes in dormant X-ray transients},
authors={A. Sadowski, J. Ziolkowski, K. Belczynski},
abstract={Our calculations of stellar population synthesis indicate that the Galaxy contains some 15000-40000 dormant X-ray transients with black hole components. It means that there should be some 20-50 such systems within 0.5 kpc from the Sun. These objects do not emit X-rays, but their optical components should display ellipsoidal light variations, typical for Roche lobe filling components of close binaries. For a typical soft X-ray transient (mass of the optical component 0.5 to 1 $M_\odot$, mass of black hole 5 to 10 $M_\odot$), the amplitude of these variations (in V band) should be up to 0.5 magnitude (depending on the inclination of the system). Such variability should be easy to detect in mass photometric surveys (such as ASAS).},
persons_number={},
pdate={13Mar06 01:46:41},
date={22Apr06 01:14:43}
}

@inproceedings {Filip_Munz,
email={munz@asu.cas.cz},
first_name={Filip},
last_name={Munz},
affiliation={Astronomical Institute, Academy of Sciences of the Czech Republic},
address={Fricova 298, 25165 Ondrejov, Czech Republic},
presentation_type={poster},
presentation_number={1},
presentation_panel={E0},
title={Search for weak and transient sources in INTEGRAL archive},
authors={},
abstract={Only 6 blazars have been identified among AGNs in IBIS survey results. Though the exposure is rather limited for sources far from Galactic plane, suitable combination of energy bands and mid-scale exposure can reveal outbursts of some of these highly variable sources. The method was applied also on galactic sources varying on shorter time scales.},
persons_number={0},
pdate={02Mar06 01:40:59},
date={22Apr06 01:49:10}
}

@inproceedings {Mark_H._Finger,
email={mark.finger@nsstc.nasa.gov},
first_name={Mark H.},
last_name={Finger},
affiliation={National Space Science and Technology Center/USRA},
address={320 Sparkman Drive, Huntsville, Alabama 35803, USA},
presentation_type={poster},
presentation_number={1},
presentation_panel={I0},
title={A search for gamma-ray burst polarization using the IBIS Compton Mode data},
authors={},
abstract={The IBIS Compton mode data, which consists of events coincident between the ISGRI and PICsIT detector planes, is sensitive to gamma-ray polarization, due to the polarization dependence of the azimuthal distribution of Compton scatters. We present an analysis of the Compton mode data obtained during GRB041912, a bright gamma-ray burst which occurred within the IBIS fully-coded field of view. We discuss the impact of data losses and accidental coincidence events during the burst, and present limits on the burst polarization. },
persons_number={0},
pdate={02Mar06 00:05:15},
date={22Apr06 01:51:30}
}

@inproceedings {Deepto_Chakrabarty,
email={deepto@space.mit.edu},
first_name={Deepto},
last_name={Chakrabarty},
affiliation={MIT},
address={70 Vassar St, 37-626A, Cambridge, MA 02139, USA},
presentation_type={oral},
presentation_number={1},
presentation_panel={G8},
title={Intermediate-field `centisecond' pulsars: an obscured population awaiting discovery?},
authors={Deepto Chakrabarty},
abstract={Classical accretion-powered pulsars have strong ($\sim10^12$ G) surface magnetic fields and equilibrium spin periods of order a few seconds. Sustained accretion over very long ($\sim10^8$ yr) time scales evidently results in substantially weaker ($\sim10^8$ G) fields and millisecond periods, yielding millisecond pulsars in low-mass X-ray binaries (and, eventually, millisecond radio pulsars). Presumably, there should exist an intermediate population of accreting X-ray pulsars with fields of order $10^9$ G and periods between 10 and 100 milliseconds, but no such objects have been definitively identified yet. Detecting even a few would strongly constrain the physics of accretion-induced magnetic field decay. I will discuss the possibility of finding this population.},
persons_number={0},
pdate={10Apr06 19:46:57},
date={22Apr06 02:23:18}
}

@inproceedings {Sylvain_Chaty,
email={chaty@cea.fr},
first_name={Sylvain},
last_name={Chaty},
affiliation={Universit'e Paris 7/Service d'Astrophysique},
address={CEA Saclay, DSM/DAPNIA/SAp, FR-91191 Gif-sur-Yvette Cedex France},
presentation_type={oral},
presentation_number={1},
presentation_panel={E6},
title={Multi-wavelength observations revealing the obscured high-energy systems},
authors={},
abstract={I will describe how recent multi-wavelength observations, mainly in optical, near-infrared and mid-infrared wavelengths, can reveal the obscured high-energy binary systems discovered by INTEGRAL, focusing on high-mass X-ray binaries, and the newly discovered supergiant fast X-ray transients.},
persons_number={0},
pdate={01Mar06 03:56:02},
date={22Apr06 02:30:02}
}

@inproceedings {Igor_Moskalenko,
email={imos@stanford.edu},
first_name={Igor},
last_name={Moskalenko},
affiliation={Stanford University},
address={HEPL/Stanford University, Stanford, CA 94305, U.S.A.},
presentation_type={poster},
presentation_number={2},
presentation_panel={C0},
title={Attenuation of VHE gamma rays by the anisotropic Galactic radiation field},
authors={},
abstract={The attenuation of very high energy gamma rays by pair production on the Galactic interstellar radiation field has long been thought of as negligible. However, a new calculation of the interstellar radiation field consistent with multi-wavelength observations by DIRBE and FIRAS indicates that the Galactic interstellar radiation field is intense. We have made a calculation of the attenuation of very high energy gamma rays in the Galaxy using this new interstellar radiation field which takes into account its nonuniform spatial and angular distributions. We find that the maximum attenuation occurs around 100 TeV at the level of about 25\% for sources located at the Galactic center, within the energy range of the HESS instrument, and is important for both Galactic and extragalactic sources.},
persons_number={0},
pdate={28Feb06 22:13:16},
date={22Apr06 03:08:04}
}

@inproceedings {Anatoliy_Tugay,
email={tugay@univ.kiev.ua},
first_name={Anatoliy},
last_name={Tugay},
affiliation={Taras Shevchenko Kyiv University, Faculty of Physics, Astronomy and Space Physics Department},
address={03022, Ukraine, Kyiv, Glushkova avenue, 2},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={Researches of Centaurus X-3 pulsar in Kyiv},
authors={},
abstract={Within the work of recently open INTEGRAL data-processing centre, SPI spectra of X-ray pulsar Centaurus X-3 have been analysed. We searched for nuclear lines and dependence of spectrum parameters from the eclipse phase. The model of Cen X-3 MeV-range emission based on inverse compton scattering cascades is discussed.},
persons_number={0},
action={Remove me from the list},
pdate={23.02.06 14:57:34},
date={22Apr06 14:01:28}
}

@inproceedings {Dmitry_Yakovlev,
email={yak@astro.ioffe.ru},
first_name={Dmitry},
last_name={Yakovlev},
affiliation={Ioffe Physical Technical Institute},
address={Politekhnicheskaya 21, 194021, Saint-Petersburg, Russia},
presentation_type={oral},
presentation_number={1},
presentation_panel={H1},
title={Strange or even stranger stars},
authors={D.G. Yakovlev (1) and P. Haensel (2) (1) Ioffe Physical Technical Institute, Politekhnicheskaya 26, 194021, Saint-Petersburg, Russia (2) Copernicus Astronomical Center, Bartycka 18, PL-00-716, Warsaw, Poland},
abstract={We describe the basic physical principles underlying the hypotheses on the existence of strange quark matter or more exotic forms of matter in the cores of compact stars or even at the surfaces of these stars. We review then the main parameters of hypothetical compact stars such as strange stars or even stranger stars (particularly, Q-stars). We formulate observational tests which would enable one to confirm or reject the hypotheses on the existence of these objects and compare theoretical predictions with results of present observations.},
persons_number={0},
pdate={07.02.06 18:11:11},
date={22Apr06 19:16:23}
}

@inproceedings {Elena_V._Seifina,
email={seif11@mail.ru},
first_name={Elena V.},
last_name={Seifina},
affiliation={Sternberg Astronomical Institute},
address={Universitetsky pr.13, Moscow, 119992, Russia},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={INTEGRAL observations of X-ray transient GS1843+009 during 2003-2005 activity events},
authors={},
abstract={We report the detection of a hard X-ray outburst of the transient X-ray binary pulsar GS1843+009 with IBIS/ISGRI detector aboard INTEGRAL. The source was detected during October 27-November 2, 2005 with flux 7.2 mCrab in the 20-50 keV energy range at a S/N ratio of 5. This source outburst was much weaker than the three known previous ones (1988, 1997, 2003). We report here the analysis of INTEGRAL observations at different epochs. The long term behaviour of the source tend to indicate a high mass X-ray binary with Be companion. We explane the origin of X-ray of GS1843+009 in the colliding wind model in momemt periastron passage of pulsar around Be star companion. Physical parameters of the model have been evaluated.},
persons_number={0},
pdate={02Mar06 17:45:22},
date={23Apr06 01:02:38}
}

@inproceedings {Niels_Lund,
email={nl@spacecenter.dk},
first_name={Niels},
last_name={Lund},
affiliation={Danish National Space Centre},
address={Juliane Maries vej 30, DK-2100 Copenhagen, Denmark},
presentation_type={poster},
presentation_number={1},
presentation_panel={J0},
title={JEM-X status after 3 years in space},
authors={},
abstract={The X-ray monitor, JEM-X, on INTEGRAL is working well after three years in space. Shortly after launch there were concerns that the instrument lifetime would be limited to a few years, but changes in the operational conditions have improved the performance and put the concerns to rest. The scientific capabilities of JEM-X after three years in space will be discussed and illustrated.},
persons_number={0},
pdate={21Apr06 18:09:28},
date={23Apr06 09:55:05}
}

@inproceedings {Petr_Kubanek,
email={pkubanek@asu.cas.cz},
first_name={Petr},
last_name={Kubanek},
affiliation={AI Ondrejov \& ISDC Versoix},
address={Fricova, CZ 251 65 Ondrejov, Czech Republic},
presentation_type={poster},
presentation_number={2},
presentation_panel={J0},
title={Access to INTEGRAL data through Virtual Observatory: Scientific Motivation and Recent Status},
authors={},
abstract={Virtual Observatory (VO) is an international effort to create distributed database of all data taken of sky. It should enable quick and common access to all data products - ranging from images to light curves and spectra. Once created, scientists will have common interface to access multi-mission, multi-wavelengths data on few mouse-clicks. We will discuss motivations to create Virtual Observatory access to INTEGRAL data, challenges which we have to attack on creating it, and current status of development VO enabled interface to public INTEGRAL data.},
persons_number={0},
pdate={02Mar06 01:18:16},
date={24Apr06 12:54:06}
}

@inproceedings {Bertrand_Cordier,
email={bcordier@cea.fr},
first_name={Bertrand},
last_name={Cordier},
affiliation={CEA-Saclay Service d'Astrophysique},
address={Bat 709, 91191 Gif sur Yvette},
presentation_type={poster},
presentation_number={1},
presentation_panel={B0},
title={Search for MeV gamma-ray emission from the Galaxy with SPI},
authors={Bertrand Cordier, Clarisse Hamadache, St\'ephane Schanne and Patrick Sizun},
abstract={We report the search of gamma-ray emission from the Galaxy in the 3--7 MeV energy range with the Spectromer SPI of the INTEGRAL observatory. This energy range encompasses the 4.4 MeV and 6.1 MeV nuclear de-excitations lines of $^{12}$C* and $^{16}$O*, respectively, which are predicted to be the strongest lines originating from the interaction of energetic particles with ambient matter. After a description of the background model built at these energies, we present the preliminary results based on 2.5 years of SPI data.},
persons_number={0},
pdate={28Feb06 19:15:42},
date={24Apr06 14:09:10}
}

@inproceedings {Sergey_Sazonov,
email={sazonov@mpa-garching.mpg.de},
first_name={Sergey},
last_name={Sazonov},
affiliation={IKI},
address={},
presentation_type={oral},
presentation_number={1},
presentation_panel={D4},
title={Statistics of local, hard X-ray selected AGN: contribution of obscured accretion onto supermassive black holes},
authors={},
abstract={X-ray surveys are essential in studying the demography and cosmological evolution of AGN. Deep X-ray surveys have greatly improved our knowledge of AGN at $z>0.3$, but told us little about the low-$z$ AGN population. There is also evidence that most AGN are strongly obscured at optical and soft X-ray wavelengths. To have an unbiased picture of the local AGN population, very large-area hard X-ray surveys are needed. We recently made a serendipitous survey of the high Galactic latitude sky at 3-20 keV with RXTE and are close to a completion of an all-sky survey with INTEGRAL at energies above 20 keV. We will compare the main results of these two surveys, including the AGN luminosity function and NH distribution.},
persons_number={0},
pdate={01Mar06 22:39:25},
date={24Apr06 16:23:34}
}

@inproceedings {Vincent_Tatischeff,
email={tatische@csnsm.in2p3.fr},
first_name={Vincent},
last_name={Tatischeff},
affiliation={CSNSM},
address={F-91405 Orsay Campus, France},
presentation_type={poster},
presentation_number={1},
presentation_panel={B0},
title={Delayed X- and gamma-ray line emission from Solar flare radioactivity},
authors={},
abstract={We have studied the radioactive line emission expected from solar active regions after large flares, following the production of long-lived radioisotopes by nuclear interactions of flare-accelerated ions. This delayed X- and gamma-ray line emission can provide unique information on the accelerated particle composition and energy spectrum, as well as on mixing processes in the solar atmosphere. Total cross sections for the formation of the main radioisotopes by proton, $^{3}$He and $\alpha$-particle reactions are evaluated from available data combined with nuclear reaction theory. The brightest delayed line for days after the flare is found to be the 511 keV positron-electron annihilation line. After about 2 days however, its flux can become lower than that of the 846.8 keV line from the decay of $^{56}$Co. Our study has revealed other delayed gamma-ray lines that appear to be promising for detection, e.g. at 1434 keV from the radioactivity of both the isomer and the ground state of $^{52}$Mn. The strongest delayed X-ray line is found to be the Co K$_{\alpha}$ at 6.92 keV, which is produced from both the decay of the isomeric state of $^{58}$Co by the conversion of a K-shell electron and the decay of $^{57}$Ni by orbital electron capture. Prospects for observation of these lines are discussed. },
persons_number={0},
pdate={10Apr06 16:04:57},
date={24Apr06 16:47:19}
}

@inproceedings {Kathryn_Flanagan,
email={kaf@space.mit.edu},
first_name={Kathryn},
last_name={Flanagan},
affiliation={MIT Kavli Institute for Astrophysics and Space Research},
address={MIT NE80-6025, 77 Massachusetts Ave., Cambridge, MA 02139 USA},
presentation_type={oral},
presentation_number={1},
presentation_panel={B4},
title={A Chandra update: chemical composition and shock structure in supernova remnants},
authors={},
abstract={The combined high-resolution spatial and spectral characteristics of Chandra have given us new insights into the chemical composition and the shock structure of supernova remnants. We highlight recent Chandra results on Cas A, Puppis A, E0102-72 and other remnants, touching on nucleosynthesis and mixing, velocity structure and equilibration processes.},
persons_number={0},
pdate={10Apr06 00:00:00},
date={24Apr06 18:35:03}
}

@inproceedings {Stephen_S._Murray,
email={ssm@head.cfa.harvard.edu},
first_name={Stephen S.},
last_name={Murray},
affiliation={Harvard-Smithsonian Center for Astrophysics},
address={60 Garden Street MS-2, Cambridge MA 02138, USA},
presentation_type={oral},
presentation_number={1},
presentation_panel={D1},
title={Mapping the Cosmic Web with X-ray selected AGN from the Chandra XBootes survey},
authors={Murray, Forman, Hickox, Jones, Kenter, Kochanek and Eisenstein},
abstract={Chandra has surveyed a 9 square degree region in the NDWFS Bootes area. Over 4000 X-ray sources were detected. For about half, there are followup spectroscopic observations that provide accurate redshifts. For redshifts below $\sim0.7$, these X-ray slected AGN follow the same spatial distribution as the galaxies, mapping filaments and voids. For redshifts beyond $\sim0.7$ the X-ray sources show similar structure.},
persons_number={0},
pdate={10Apr06 00:00:00},
date={24Apr06 19:19:47}
}

@inproceedings {Alberto Javier_Castro-Tirado,
email={ajct@iaa.es},
first_name={Alberto Javier},
last_name={Castro-Tirado},
affiliation={IAA-CSIC},
address={P.O. Box 03004, E-18080 Granada, Spain},
presentation_type={oral},
presentation_number={1},
presentation_panel={I6},
title={Multiwavelength observations of GRBs detected by INTEGRAL},
authors={},
abstract={We will show the result of our ongoing programme since 2003 aimed at following up the gamma-ray bursts detected by INTEGRAL. Millimeter, near-IR, optical and evantually X-ray observations will be presented as well as the redshift distribution of the bursts for which a value of z is available.},
persons_number={0},
pdate={10Mar06 16:19:07},
date={24Apr06 19:34:31}
}

@inproceedings {Sergiy_Guziy,
email={gss_mai@mail.ru},
first_name={Sergiy},
last_name={Guziy},
affiliation={Kalinenkov Astronomical Observatory, Nikolaev State University},
address={Nikolska 24, Nikolaev, 54030, Ukraine},
presentation_type={poster},
presentation_number={1},
presentation_panel={I0},
title={Comparison of two hypernovae GRB 030329/SN 2003dh and GRB060218/SN 2006aj},
authors={S. Guziy, A.J. Castro-Tirado, J. Gorosabel, A. de Ugarton Postugo, M. Jelinek, O. Bogdanov on behalf of a larger collaboration.},
abstract={We present comparison of two hypernovae GRB 030329/SN 2003dh and GRB060218/SN 2006aj. We have obtained optical and near-IR monitoring at different observatories around the wold. We have detected supernovae bump for GRB 030329/SN 2003dh and GRB060218/SN 2006aj. Details of comparison will be present.},
persons_number={0},
pdate={10Mar06 16:51:34},
date={24Apr06 20:04:30}
}

@inproceedings {Dmitri_Karasev,
email={dkarasev@hea.iki.rssi.ru},
first_name={Dmitri},
last_name={Karasev},
affiliation={IKI RAN},
address={117997, 84/32 Profsoyuznaya Str, Moscow, Russia},
presentation_type={poster},
presentation_number={1},
presentation_panel={E0},
title={INTEGRAL and RXTE observation of the fast X-ray transient XTE1901+014},
authors={},
abstract={We present results of spectral and timing analysis of the fast X-ray transient XTE1901+014 based on the RXTE and INTEGRAL data. The source was detected by INTEGRAL with the persistent flux of 2.7 mCrab in a 17-100 keV energy band at a significance level of 20 sigma during long observations of the Sagittarius arm region in 2003-2004. We used RXTE/PCA (3-20 keV) and INTEGRAL/ISGRI data (17-80 keV) to build broadband energy spectrum of the source in a quite state and found that it can be well approximated by a simple powerlaw with a photon index of $\sim2$. The contamination of the Galactic ridge emission to the PCA data was took into account. From timing analysis we found short time scale aperiodic variations which can be connected with instabilities of the accretion process.},
persons_number={0},
pdate={13Mar06 18:51:17},
date={24Apr06 20:30:13}
}

@inproceedings {Miguel_Torrejon,
email={jmt@dfists.ua.es},
first_name={Miguel},
last_name={Torrejon},
affiliation={University of Alicante},
address={Ap correos 99},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={The optical counterpart to the High Mass X-ray Binary IGR J11435-6109},
authors={},
abstract={We present here a characterization of the optical counterpart to the High Mass X-ray Binary of the newly discovered source IGR J11435-6109. The star is a B3Ve star, which renders it the Galactic Be/X-ray binary with the latest spectral type known to date.},
persons_number={1},
pdate={27Feb06 16:05:43},
date={25Apr06 13:23:57}
}

@inproceedings {Roland_Diehl,
email={rod@mpe.mpg.de},
first_name={Roland},
last_name={Diehl},
affiliation={MPE Garching},
address={Giessenbachstr 1, D-85748 Garching, Germany},
presentation_type={oral},
presentation_number={1},
presentation_panel={B2},
title={$^{26}$Al in the Galaxy},
authors={},
abstract={Gamma-ray line emission from radioactive $^{26}$Al has been measured with INTEGRAL's SPI spectrometer. The integrated signal from the inner Galaxy reveals a narrow line s
hape, consistent with normal interstellar dynamics around the sources. The Doppler shifts from inner-Galaxy rotation are indicated in systematic shifts of the line center. The ma
p of $^{26}$Al emission appears compatible with previous measurements. We present the status of our $^{26}$Al line data analysis and its astrophysical implications.},
persons_number={1},
pdate={20Mar06 16:26:18},
date={25Apr06 18:33:49}
}


@inproceedings {Marat_Gilfanov,
email={gilfanov@hea.iki.rssi.ru},
first_name={Marat},
last_name={Gilfanov},
affiliation={IKI, MPA},
address={},
presentation_type={none},
presentation_number={1},
presentation_panel={},
title={},
authors={},
abstract={},
persons_number={0},
pdate={01Mar06 23:02:42},
date={26Apr06 14:46:11}
}

@inproceedings {Eugene_Churazov,
email={churazov@hea.iki.rssi.ru},
first_name={Eugene},
last_name={Churazov},
affiliation={IKI, MPA},
address={},
presentation_type={oral},
presentation_number={1},
presentation_panel={A3},
title={Electron-positron annihilation emission of the Galaxy},
authors={},
abstract={},
persons_number={0},
pdate={02Mar06 21:11:28},
date={26Apr06 15:05:03}
}

@inproceedings {Sergei_Grebenev,
email={sergei@hea.iki.rssi.ru},
first_name={Sergei},
last_name={Grebenev},
affiliation={Space Research Institute, Russian Academy of Sciences},
address={Profsoyuznaya st., 84/32, Moscow, 117997},
presentation_type={poster},
presentation_number={2},
presentation_panel={F0},
title={IGR J17098-3828: an X-ray Nova discovered by INTEGRAL},
authors={S.A. Grebenev, S.V. Molkov, M.G. Revnivtsev, R.A. Sunyaev},
abstract={We report on the discovery with INTEGRAL on March 24, 2005, and follow-up observations of this X-ray nova.},
persons_number={0},
pdate={01Mar06 21:16:52},
date={26Apr06 15:17:13}
}

@inproceedings {Alexander_Lutovinov,
email={aal@hea.iki.rssi.ru},
first_name={Alexander},
last_name={Lutovinov},
affiliation={Space Research Institute},
address={},
presentation_type={oral},
presentation_number={1},
presentation_panel={E7},
title={Population of HMXB in the Galaxy},
authors={M. Revnivtsev, M. Gilfanov, R. Sunyaev},
abstract={We study populations of High-Mass X-ray Binaries in the Galaxy using data of the INTEGRAL observatory in a hard X-ray energy band. About two hundreds of sources are located near the Galactic plane (|b|$ <5$ deg), most of them have a galactic origin and belong to X-ray binaries, high (HMXB) and low mass (LMXB). We investigated HMXB distribution and discussed it in a comparison with some model estimations of the density of different components of Galaxy. The high quality broadband energy spectra for several dozens of new sources were also obtained using the data of different orbital observatories
(INTEGRAL, RXTE, ASCA, XMM-Newton) and used, in line with optical and radio data from ground-based observatories, for the establishing of their nature.},
persons_number={0},
pdate={01Mar06 21:45:59},
date={26Apr06 20:54:20}
}

@inproceedings {Werner_Collmar,
email={wec@mpe.mpg.de},
first_name={Werner},
last_name={Collmar},
affiliation={MPE},
address={Giessenbachstr., 85748 Garching, Germany},
presentation_type={poster},
presentation_number={1},
presentation_panel={D0},
title={Multifrequency observations of the blazar 3C 279 centered on an INTEGRAL ToO pointing in 2006},
authors={W. Collmar, M. Ajello, E. Bottacini, V. Burwitz (MPE, Garching, Germany), M. Boettcher (Ohio Univ., Athens, USA), T. Courvoisier (ISDC, Geneva, Switzerland), T. Krichbaum (MPIfR, Bonn, Germany), P. Kretschmar (ESA, Villafranca, Spain), K. Pottschmidt (UCSD, San Diego, USA), A. Sillanpaeae (Tuorla Obs., Piikkioe, Finland), M. Tornikoski (Metsaehovi Radio Obs., Kylmaelae, Finland), M. Villata (Obs. of Torino, Torino, Italy)},
abstract={The prominent gamma-ray blazar 3C 279 was observed by INTEGRAL in a ToO observation, triggered by an optical high-state, for a total of 511 ksec between January 13 and 22, 2006 in several pointings. Centered on the INTEGRAL observations, a multifrequency campaign was organized, which yielded simultaneous measurements in radio and mm-bands (e.g. Effelsberg, Metsaehovi, IRAM), in near-IR and optical bands by a WEBT-campaign, and in X-rays by Chandra and Swift. The analysis of the multifrequency data is currently in progress. We will present first results of this campaign, focusing on the results of INTEGRAL in the hard X-ray band and on the observed multifrequency spectrum. These 2006 high-state results will be compared to the ones derived during an optical low-state of 3C 279 in June 2003 (Collmar et al., 2004). The implications on blazar physics will be discussed.},
persons_number={0},
pdate={27Feb06 14:21:27},
date={27Apr06 13:25:06}
}

@inproceedings {Guido_Di_Cocco,
email={dicocco@iasfbo.inaf.it},
first_name={Guido},
last_name={Di Cocco},
affiliation={INAF/IASF-Bologna},
address={Via Gobetti 101 - 40129 - Bologna (Italy)},
presentation_type={poster},
presentation_number={1},
presentation_panel={F0},
title={IBIS/PICSIT status and scientific highlights},
authors={G. Di Cocco, V. Bianchin, L. Foschini, P. Lubinski, G. Malaguti},
abstract={We report about the status of the PICsIT layer of the imager IBIS, both about the instrument and the software for the scientific analysis. Recent scientific results obtained by using PICsIT data are also summarized.},
persons_number={0},
pdate={05Apr06 16:26:09},
date={27Apr06 17:13:23}
}

@inproceedings {Rashid_Sunyaev,
email={sunyaev@mpa-garching.mpg.de},
first_name={Rashid},
last_name={Sunyaev},
affiliation={MPA, Garching; IKI, Moscow},
address={},
presentation_type={oral},
presentation_number={1},
presentation_panel={C5},
title={INTEGRAL measurement of the CXB. Earth observation},
authors={},
abstract={We study the spectrum of cosmic X-ray background (CXB) in
energy range 5--100 keV. Early 2006 the INTEGRAL observatory performed a
series of four 30 ksec observations with the Earth disk crossing the
field of view of the instruments. The modulation of the aperture flux
due to occultation of extragalactic objects by the Earth disk was used
to obtain the spectrum of the Cosmic X-ray Background (CXB). Various
sources of contamination were evaluated, including compact sources,
Galactic Ridge emission, CXB reflection by the Earth atmosphere, cosmic
ray induced emission by the Earth atmosphere and the Earth auroral
emission. ---- Spectrum of cosmic X-ray background in energy band 5-100
keV is obtained. The shape of the spectrum is consistent with that
obtained previously by HEAO-I observatory, while the normalization is
$\sim12$\% higher. This normalization is obtained under assumption that
the total Crab nebular spectrum (nebular itself plus the pulsar) is
described by a power law $dN/dE = 10 E^{-2.1}$ phot/s/cm$^2$/keV across
5-100 keV range. With the procedure adopted here the changes in the
assumed normalization of the Crab spectrum can be directly translated in
to the changes in the CXB normalization. The CXB spectrum obtained by
INTEGRAL agrees well with the measurements of RXTE/PCA, latest
recalculation of HEAO-I measurements, with results of ASCA and CHANDRA
observatories. Increase of the absolute flux of the CXB near the energy
of maximum luminosity (20-50 keV) has direct implications for the energy
release of the supermassive black holes in the Universe and their growth
at the epoch of the CXB origin.},
persons_number={0},
pdate={02Mar06 02:32:44},
date={27Apr06 18:09:35}
}

@inproceedings {Andrzej_Zdziarski,
email={aaz@camk.edu.pl},
first_name={Andrzej},
last_name={Zdziarski},
affiliation={N. Copernicus Astronomical Center},
address={},
presentation_type={oral},
presentation_number={1},
presentation_panel={G0},
title={New timing properties of 4U 1820-30},
authors={},
abstract={4U 1820-30 is a Galactic X-ray binary with an 11-min orbital period. This period is the second shortest known of any binary. The binary consists of a low-mass white dwarf and a neutron star, separated by only about 100 000 km. The system loses its angular momentum by emission of gravitational waves, which leads to a high rate of mass trasfer from the white dwarf onto the neutron star. This, in turn, leads to strong X-ray emission, which is modulated at the 11-min. period. There is also a very strong 170-d modulation, which is probably due to the presence of a 3rd, much more remote, star in the system. The third star modulates the eccentricity of the inner orbit, resulting in the variable rate of the mass transfer. I will report a discovery of a new property of the X-ray variability, which strongly depends on the phase of the 170-d modulation. The discovered effect can be explained by dynamics of the triple system.},
persons_number={0},
action={Remove me from the list},
pdate={22Mar06 20:42:00},
date={28Apr06 09:45:10}
}

@inproceedings {Filippo_Frontera,
email={frontera@fe.infn.it},
first_name={Filippo},
last_name={Frontera},
affiliation={Physics Department,, University of Ferrara, Italy},
address={Via Saragat,, 1 -44100 Ferrara, Italy },
presentation_type={oral},
presentation_number={1},
presentation_panel={C4},
title={The cosmic hard X-ray ($>15$ keV) background with the PDS instrument aboard BeppoSAX},
authors={},
abstract={After more than 20 years from the last measurement of the Cosmic hard X-ray Background (CXB) with HEAO-1, we report new results on the CXB spectrum and its intensity at energies above 15 keV. These results have been obtained by peforming a systematic analysis of all the pointings at Galactic latitudes $|b|>15$ deg of the PDS instrument aboard the BeppoSAX satellite. We discuss our results in the context of the open issues on CXB and its origin.},
persons_number={1},
pdate={01Mar06 19:11:33},
date={29Apr06 12:29:53}
}

@inproceedings {William_Forman,
email={wrf@cfa.harvard.edu},
first_name={William},
last_name={Forman},
affiliation={Smithsonian Astrophysical Observatory},
address={60 Garden St. Cambridge MA 02138 USA},
presentation_type={oral},
presentation_number={1},
presentation_panel={D6},
title={Shocks, bubbles, and filaments: the effects of supermassive black hole outbursts in M87},
authors={W. Forman, C. Jones, E. Churazov},
abstract={We present the first results from a 500~ksec Chandra observation of M87. At soft energies (0.5-1.0 keV), we detect a complex filamentary structure associated with the eastern and southwestern arms. Many filaments are spatially resolved and have widths of $\sim300$ pc. This filamentary structure is particularly striking in the eastern arm where we suggest the filaments are outer edges of a series of buoyant bubbles filled with relativistic plasma, produced by the central supermassive black hole, in a succession of small outbursts occurring every $\sim6\times10^6$~years. The X-ray structures may be influenced by magnetic filamentation. At hard energies (3.5-7.5 keV), we detect a nearly circular shell of outer radius $2.8^\prime$ (13 kpc). This ring of hard X-ray emission provides an unambiguous signature of a weak shock, driven by an outburst from the SMBH, traversing the M87 atmosphere. The observed spectral hardening corresponds to a temperature rise from 2.0 to 2.4 keV, which translates to a Mach number $M\sim1.2$ for monoatomic gas with gamma=5/3. In addition, we detect two additional surface brightness edges (at radii of $\sim0.6^\prime$ and $\sim1.2^\prime$). The $\sim0.6^\prime$ feature may be the gas just outside the ``piston'' driving the $2.8^\prime$ shock, while the $\sim1.2^\prime$ feature is probably produced by a secondary outburst. We compare the M87 outbursts to those from central galaxies in rich clusters with outbursts of energy up to $10^{62}$ ergs and from ``normal'' galaxies with outbursts as low as $10^{55}$ ergs. We discuss the implications of these outbursts for the growth of supermassive black holes.},
persons_number={0},
pdate={10Apr06 00:00:00},
date={01May06 07:35:59}
}

@inproceedings {Thierry_Courvoisier,
email={thierry.courvoisier@obs.unige.ch},
first_name={Thierry},
last_name={Courvoisier},
affiliation={ISDC},
address={},
presentation_type={poster},
presentation_number={1},
presentation_panel={E0},
title={The INTEGRAL Science Centre},
authors={},
abstract={will be presented, together with some of the results obtained there.},
persons_number={0},
pdate={28Feb06 12:46:12},
date={02May06 12:24:51}
}

@inproceedings {Pere_Blay,
email={pere.blay@uv.es},
first_name={Pere},
last_name={Blay},
affiliation={GACE - Universitat de Valencia},
address={PO BOX 22085, E-46071 Valencia, SPAIN},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={The nature of the system 4U 2206+54, a multiwavelenght approach},
authors={Pere Blay, Ignacio Negueruela, Pablo Reig, Marc Ribo, Jose-Miguel Torrejon, Ascension Camero, Victor Reglero},
abstract={4U 2206+54, a High Mass X-Ray Binary system discovered with UHURU data in 1972, was initially classified as a BeX system (with BD+53 2790 as the optical counterpart). After a long term monitoring campaign, a multiwavelength approach allowed us to unveil the real nature of this system. From radio wavelenghts to gamma-ray energies, we present a complete analysis of the system which includes the detemination of the nature of both, the optical and compact component, as well as the properties of the mass transfer mechanism and constraints for the orbital parameters of 4U 2206+54. From optical data (from on ground telescopes), the spectral type of the optical companion, O9.5Vp, is derived. From infrared and UV observations (from on ground telescopes and IUE, respectively), the nature of the expanding envelope of BD+53 2790 is analysed. From a combination of radio and high-energy observations (from NRAO/VLA, INTEGRAL and RXTE), the nature of the compact companion, a neutron star, is derived. Lately, using both high-energy light curves and optical spectroscopy, the orbital parameters of the system can be constrained.},
persons_number={0},
pdate={02Mar06 01:04:13},
date={03May06 16:32:53}
}

@inproceedings {Mikhail_Pavlinsky,
email={pavlinsky@hea.iki.rssi.ru},
first_name={Mikhail},
last_name={Pavlinsky},
affiliation={Space Research Institute, RAS},
address={Profsouznaya 84/32, Moscow, Russia},
presentation_type={poster},
presentation_number={1},
presentation_panel={J0},
title={Spectrum-RG/eROSITA/Lobster astrophysical mission},
authors={Pavlinsky Mikhail, Guenther Hasinger, Peter Predehl, Evgenii Churazov, Marat Gilfanov, Alexey Viklinin, George Fraser, Arvind Parmar, Luigi Piro, Vadim Arefiev, Rashid Sunyaev, Alexey Tkachenko},
abstract={High particle background on high apogee orbits severely affects the capabilities of X-ray telescopes to study diffuse emission. For new baseline configuration of the SRG mission a low earth orbit was selected to circumvent this limitation. A medium size satellite will be launched in the 2009-2010 timeframe into a 600 km equatorial ($<4$ deg) orbit from Kourou or into a 29 deg. orbit from Baikonur as a fallback option. The payload includes eROSITA (extended ROentgen Survey with an Imaging Telescope Array, MPE, Germany) with 7 Wolter-type telescopes, the wide field X-ray monitor Lobster (LU, UK), and ART telescopes (IKI, Russia). The mission will conduct the first all-sky survey with an imaging telescope in the 2-12 keV band to discover the hidden population of several hundred thousand obscured supermassive black holes and the first all-sky imaging X-ray time variability survey. In addition to the all-sky surveys it is foreseen to observe the extragalactic sky with high sensitivity to detect 50 to 100 thousand clusters of galaxies and thereafter to do follow-up pointed observations of selected sources, in order to investigate the nature of Dark Matter and Dark Energy. The new SRG mission would thus be a highly significant scientific and technological step beyond Chandra/XMM-Newton and would provide important and timely inputs for the next generation of giant X-ray observatories like XEUS/Con-X planned for the 2015-2025 horizon.},
persons_number={0},
pdate={21.02.06 15:23:32},
date={03May06 16:52:24}
}

@inproceedings {Pere_Blay,
email={pere.blay@uv.es},
first_name={Pere},
last_name={Blay},
affiliation={GACE - Universitat de Valencia},
address={PO BOX 22085, E-46071 Valencia, SPAIN},
presentation_type={poster},
presentation_number={2},
presentation_panel={G0},
title={SAX J2103.5+4545: bright and faint states characterized with INTEGRAL},
authors={P. Blay, P. Reig, I. Negueruela, A. Camero, S. Martinez, V. Reglero},
abstract={The BeX system SAX J2103.5+4545 shows a set of peculiarities which make it different than the rest of BeXs. With a short orbital period compared to other BeXs (12.67 days) and a pulsating period of $\sim350$ s, it does not follow the Corbet relationship between $P_{orb}$ and $P_{spin}$ for BeX systems. It shows alternate bright and faint states. Bright states are characterized by luminosities of the order of $10^{36}$ erg s$^{-1}$ and orbital modulation of the high energy emission. Faint states are characterized by low luminosities ($\sim10^{34}$ erg s$^{-1}$) and the absence of detectable orbital modulation. For the first time we present a detailed comparative analysis of the source in the bright and faint states with INTEGRAL data, showing clear evidence of different spectral behaviour of both states. The interactions of the Be star envelope and the compact companion in SAX J2103.5+4545 are briefly presented and a discussion about the possible explanation of the onset of bright and faint states is included.},
persons_number={0},
pdate={02Mar06 01:08:09},
date={03May06 17:23:04}
}

@inproceedings {Chris_Shrader,
email={Chris.R.Shrader@gsfc.nasa.gov},
first_name={Chris},
last_name={Shrader},
affiliation={NASA Goddard Space Flight Center},
address={Code 661, NASA/GSFC, Greenbelt MD 20771, USA},
presentation_type={poster},
presentation_number={1},
presentation_panel={I0},
title={SPI Spectral Analsyis of Bright Gamma-Ray Bursts},
authors={},
abstract={There have been a number of bright gamma-ray bursts that occurred within the SPI and IBIS FCFOV, which have sufficient counts for accurate spectral determination. Previous studies have utilized the IBIS/ISGRI detector almost exclusively, however, there are cases where the peak-energy (Epeak) may lie above the ~200 keV IBIS useful sensitivity range (e.g. GRB 031203) or the low-energy ISGRI count rates saturate (e.g. GRB 041219). There are also incidences where the GRB has occurred outside of the ISGRI FCFOV, limiting subsequent analysis. In several cases, e.g. GRB 031203 and GRB 050502, a determination of Epeak is of particular interest, as they have some apparently anomalous properties (such as being outliers on the lag-luminosity diagram). We were thus motivated to explore methods for SPI event extraction, which can be used in conjunction with the standard ISDC software, to form time-windowed burst spectra. The resulting spectra, consisting of pre- and post-burst backgrounds (within a single SCW) from which a net GRB spectrum is generated, anre then analyzed using the full SPI instrument response, i.e. including diagonal plus off-diagonal elements are included, for different degrees of mask shadowing. Model fitting can then be performed using the ususal forward-folding methods. We discuss present details of our method, and results on our analysis of a number of bright GRBs, such as GRB 021203, 041219, 050502, 021125, and 030131.},
persons_number={0},
pdate={01Mar06 23:15:43},
action={Remove me from the list},
date={03May06 17:41:21}
}

@inproceedings {Roland_Diehl,
email={aws@mpe.mpg.de},
first_name={Roland},
last_name={Diehl},
affiliation={MPE},
address={D-85748 Garching, Germany},
presentation_type={poster},
presentation_number={2},
presentation_panel={C0},
title={Imaging Galactic gamma-ray emission with SPI},
authors={Andrew Strong},
abstract={Maximum-entropy imaging has demonstrated its value from gamma-rays (e.g. CGRO/COMPTEL) through radioastronomy (e.g. WMAP). Its advantage is to impose well-controlled but minimum assumptions on the form of the image. We use multi-year SPI data to generate images of the low-energy gamma-ray emission from the Galaxy in several energy bands. These are compared with COMPTEL and EGRET maps to obtain clues as to the nature of the unresolved emission from the Galaxy.},
persons_number={0},
pdate={21Mar06 11:53:20},
date={03May06 19:00:14}
}

@inproceedings {Steven_Sturner,
email={sturner@swati.gsfc.nasa.gov},
first_name={Steven},
last_name={Sturner},
affiliation={USRA, NASA/GSFC},
address={NASA/GSFC, Code 661, Greenbelt, MD 20771-0001, USA},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={INTEGRAL Observations of the Be stars gamma Cassiopeiae and HD 110432},
authors={},
abstract={We present the results of hard X-ray observations of the Be stars gamma Cassiopeiae and HD 110432 made with the INTEGRAL observatory. Both these stars are known, low-to-moderate luminosity X-ray sources. Gamma Cas has recently been shown to be part of a binary system with a 203.59 day orbital period. The secondary was shown to have a mass of ~1 solar mass, consistent with a white dwarf, a neutron star, or a normal late-type dwarf, however no orbital modulation of the X-ray intensity has been identified. This result has fueled debate as to whether the X-ray emission is due to accretion onto a compact companion or magnetic activity near the surface of the Be star. HD 110432 has been shown to have similar spectral properties to gamma Cas and it has been suggested that it is also a good candidate for a Be+WD binary system. We present IBIS/ISGRI and SPI hard X-ray spectra of these systems. We also calculate light curves in an effort to search for flares and long timescale flux variations. The results are compared with those of previous hard X-ray missions such as BeppoSAX and ASCA and conclusions are drawn as to the origins of the hard X-ray emission.},
persons_number={0},
pdate={28Feb06 22:44:18},
action={Remove me from the list},
date={03May06 19:19:01}
}

@inproceedings {Igor_Moskalenko,
email={imos@stanford.edu},
first_name={Igor},
last_name={Moskalenko},
affiliation={Stanford University},
address={HEPL/Stanford University, Stanford, CA 94305, U.S.A.},
presentation_type={oral},
presentation_number={1},
presentation_panel={C1},
title={Modeling of the Galactic diffuse continuum gamma-ray emission},
authors={},
abstract={We present new results on the modelling of the diffuse Galactic gamma-ray emission in the MeV - TeV energy range. We show how it is possible to improve agreement in the energy range covered by INTEGRAL and COMPTEL.},
persons_number={0},
pdate={28Feb06 22:11:19},
date={03May06 19:43:16}
}

@inproceedings {Vladimir_Dogiel,
email={dogiel@lpi.ru},
first_name={Vladimir},
last_name={Dogiel},
affiliation={P.N.Lebedev Physical Institute},
address={Leninskii pr.53, 119991 Moscow},
presentation_type={oral},
presentation_number={1},
presentation_panel={A7},
title={On the origin of annihilation emission from the Galactic center},
authors={K.S.Cheng, D.O.Chernyshov},
abstract={Both diffuse high energy gamma-rays and a strong and extended electron-positron annihilation line emission have been observed in the Galactic Center (GC) region. Although X-ray observations indicate that the galactic black hole Sgr A is in inactive phase, we suggest that the Sgr A could still be the energy source of relativistic protons when it captures a star. We assume that relativistic protons are injected into the ambient material. In this way we are able to explain the current observed diffuse gamma-rays and the annihilation line spectrum. Annihilation line is produced by secondary positrons whose time of cooling by Coulomb collisions is so large the the intensity of the annihilation line reaches its peak value long after the peak of high energy gamma-ray flux. It takes about ten million years for the positrons to cool down to thermal temperatures so they can diffuse into a very large extended region around the Galactic center. The required injected amount of energy is consistent with the estimation of the tidal capture of a star by a massive black hole.},
persons_number={0},
pdate={31.01.06 13:03:58},
date={04May06 16:27:57}
}

@inproceedings {Ruediger_Staubert,
email={staubert@astro.uni-tuebingen.de},
first_name={Ruediger},
last_name={Staubert},
affiliation={Astronomisches Inst. Univ. Tuebingen, Astronomie},
address={Sand 1, D72076 Tuebingen, Germany},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={Long-term change of the cyclotron line energy in Her X-1},
authors={R. Staubert, J. Wilms, N. Shakura, K. Postnov, D. Klochkov, L. Rodina, W. Coburn, R. Rothchild},
abstract={Recent measurements of the cyclotron line in the hard X-ray spectrum of Her X-1 with RXTE and INTEGRAL have confirmed the suspected secular decrease of the cyclotron energy, suggesting a change in the strength of the magnetic field in the region of the X-ray emission. The long-term development of the cyclotron energy since the discovery of the line in 1975 (including a rather steep increase between 1991 and 1993) will be presented and the physical implications discussed.},
persons_number={0},
pdate={01Mar06 14:20:22},
date={05May06 13:53:23}
}

@inproceedings {Sandrine_Deluit,
email={sandrine.deluit@cesr.fr},
first_name={Sandrine},
last_name={Deluit},
affiliation={Centre d'Etude Spatiale des Rayonnements (C.E.S.R)},
address={9 av. du Colonel Roche, 31028 Toulouse, France},
presentation_type={poster},
presentation_number={1},
presentation_panel={E0},
title={INTEGRAL/SPI view of the hard X/gamma ray emission of a sample of X-ray Binaries: hard tail extension and emission processes associated},
authors={S. Deluit, L. Bouchet, E. Jourdain et al.},
abstract={We present the results of our analysis of a sample of X-ray Binaries (XRBs) observed by the Spectrometer SPI on board INTEGRAL. Most of X-ray binaries emits below 150-200 keV, the detection of a thermal cutoff suggesting a pure Thermal Comptonisation as the physical mecanism at the origin of their hard X ray emission. However, only few satellites enabled to extend the analysis above 200 keV. The large energy domain covered by SPI (20 keV-8 MeV) and its high spectral resolution allow us to perform deep analyses at higher energies. Through spectro-temporal studies of a sample of XRBs with SPI, we are able to investigate the presence of an hard tail above 150-200 keV and the emission processes associated to their hard X/gamma-ray emission. We then present a preliminary comparison with SPI of the X/gamma characteristics of XRBs hosting a neutron star or a black hole.},
persons_number={0},
pdate={28Feb06 17:10:36},
date={05May06 16:14:02}
}

@inproceedings {Dieter_Hartmann,
email={ken-ichi.nishikawa@nsstc.nasa.gov},
first_name={Dieter},
last_name={Hartmann},
affiliation={Clemson University, Dept. of Physics \& Astronomy,},
address={Clemson, SC 29634-0978, USA},
presentation_type={poster},
presentation_number={2},
presentation_panel={D0},
title={Particle acceleration, magnetic field generation and emission from relativistic jets and supernova remnants},
authors={D.H. Hartmann, K.-I. Nishikawa, P. Hardee, C. Hededal, Y. Mizuno, G.J. Fishman},
abstract={We have applied numerical simulations to the particle acceleration, magnetic field generation, and emission from shocks in order to understand the observed emission from relativistic jets and flows in supernova remnants. The investigation involves the study of collisionless shocks where the Weibel instability is responsible for particle acceleration and magnetic field generation. A 3-D relativistic electromagnetic particle (REMP) code has been used to investigate the shock processes in electron-ion and electron-positron plasmas. The simulation results show the jitter radiation from inhomogeneous magnetic fields generated by the Weibel instability which is different from the standard synchrotron emission in the homogeneous magnetic field. In particular we investigate spectra calculated from simulations self-consistently without any assumptions about plasma parameters.},
persons_number={0},
pdate={01Mar06 00:53:59},
date={05May06 17:03:01}
}

@inproceedings {Silvia_Mart\'{i}nez-N\'{u}\~{n}ez,
email={silvia.martinez@uv.es},
first_name={Silvia},
last_name={Mart\'{i}nez-N\'{u}\~{n}ez},
affiliation={Valencia University},
address={GACE-ICMUV P.O.Box 22085 E-46071 Valencia, Spain},
presentation_type={poster},
presentation_number={1},
presentation_panel={F0},
title={Cygnus X-3 INTEGRAL observations: understanding the high-energy nature of the system},
authors={S. Mart\'{i}nez-N\'{u}\~{n}ez$^*$, P. Kretschmar$^{**}$, P. Reig$^*$, A. Camero-Arranz$^*$, P. Blay$^*$, P.H. Connell$^*$, and V. Reglero$^*$ ($^*$ Valencia University, Valencia, Spain, $^{**}$ ESAC Madrid, Spain},
abstract={We will present the results of a detailed imaging, timing and spectral analysis from the soft to the hard X-rays of Cygnus X-3, using the three high-energy instruments on-board INTEGRAL. The INTEGRAL data cover about 100 orbital cycles (4.8 h) of the system. Cygnus X-3 has been observed from the early times of the X-ray astronomy, but its nature is still unknown. This work will give new clues to solve the mysterious nature of the system. The analysis reveals changes in the spectral state of the source from high/soft to low/hard states. Moreover, during the high/soft state, the source presents orbital phase variability. This variability is characterized by a hardening of the spectrum when the source luminosity decreases.},
persons_number={0},
pdate={02Mar06 22:15:17},
date={05May06 20:47:10}
}

@inproceedings {Vladimir_Kocharovsky,
email={kochar@appl.sci-nnov.ru},
first_name={Vladimir},
last_name={Kocharovsky},
affiliation={Institute of Applied Physics RAS},
address={46 Ulyanov st., Nizhny Novgorod, 603950, Russia},
presentation_type={oral},
presentation_number={1},
presentation_panel={D8},
title={The converter acceleration mechanism and accompanying radiation in relativistic shocks or shear flows},
authors={E.V.Derishev, V.V.Kocharovsky, Vl.V.Kocharovsky, F.A.Aharonian},
abstract={We review the problem of particle acceleration in relativistic shocks or shear flows. We compare different acceleration mechanisms and show that the converter mechanism, suggested recently, is the least sensitive to the geometry of the magnetic field in accelerators and can routinely operate up to cosmic-ray energies close to the fundamental limit. The converter mechanism utilizes multiple conversions of charged particles into neutral ones (protons to neutrons and electrons/positrons to photons) and back by means of photon-induced reactions or inelastic nucleon-nucleon collisions. It works most efficiently in relativistic shocks or shear flows under the conditions typical for Active Galactic Nuclei, Gamma-Ray Bursts, and microquasars, where it outperforms the standard diffusive shock acceleration. The main advantages of the converter mechanism in such environments are that it greatly diminishes particle losses downstream and avoids the reduction in the energy gain factor, which normally takes place due to highly collimated distribution of accelerated particles. We also analyze the properties of gamma-ray radiation, which accompanies acceleration of particles via the converter mechanism and can provide an evidence for the latter. In particular, we point out the fact that the opening angle of the radiation beam-pattern is different at different photon energies, which is relevant to the observability of the cosmic-ray sources as well as to their timing properties. Various consequences for observations are discussed.},
persons_number={0},
pdate={28Feb06 20:38:59},
date={05May06 22:42:33}
}

@inproceedings {Dieter_Hartmann,
email={Yosuke.Mizuno@msfc.nasa.gov},
first_name={Dieter},
last_name={Hartmann},
affiliation={Clemson University, Dept. of Physics \& Astronomy},
address={Clemson, SC 29634-0978, USA},
presentation_type={poster},
presentation_number={3},
presentation_panel={D0},
title={GRMHD simulations of jet formation by using a newly developed GRMHD Code},
authors={D.H. Hartmann, Y. Mizuno, K.-I. Nishikawa, S. Koide, P. Hardee, G.J. Fishman},
abstract={We have developed a new three dimensional general relativistic magnetohydrodynamic (GRMHD) code by using a conservative, high-resolution shock-capturing scheme. The numerical fluxes are calculated using the Harten, Lax \& van Leer scheme. The flux-interpolated constrained transport scheme is used to maintain a divergence-free magnetic field. We describe code performance on various one dimensional test problems in both special and general relativity. We show the jet formations from a geometrically thin accretion disk near a non-rotating and a rotating black hole. The simulation results show the jet formation in a same manner as previous simulations (magnetically-driven and gas pressure-driven). The jets propagate outward with strongly twisted magnetic field. The simulations continue longer than those in previous simulations. We conclude that the newly developed GRMHD code is more robust than our previous GRMHD code.},
persons_number={0},
pdate={01Mar06 22:56:08},
date={06May06 17:13:59}
}

@inproceedings {Michael_Harris,
email={harris@csnsm.in2p3.fr},
first_name={Michael},
last_name={Harris},
affiliation={CSNSM},
address={Univ. Paris Sud, Batiment 104, 91045 Orsay, France},
presentation_type={poster},
presentation_number={1},
presentation_panel={B0},
title={High resolution gamma line spectroscopy of flares on the east and west limbs of the Sun},
authors={},
abstract={A new generation of Ge-based high-resolution gamma-ray spectrometers has allowed accurate measurements to be made of the profiles, widths and energies of the gamma-ray lines emitted in the impulsive phases of solar flares. Here we present measurements in two flares of the energies of the de-excitation lines of $^{12}$C and $^{16}$O (4.4 and 6.1 MeV respectively) by the Ge spectrometer SPI on board INTEGRAL, from which Doppler shifts are derived and compared with those expected from the recoil of $^{12}$C and $^{16}$O nuclei which were excited by the impacts of flare-accelerated ions. An anomalous Doppler measurement (in terms of recoil theory) has been reported by the Ge spectrometer RHESSI in an east limb flare, which might be interpreted to imply a significant difference between the Doppler shifts on the east and west limbs. SPI observed both east and west limb flares and found no significant difference in Doppler shifts.},
persons_number={0},
pdate={10Apr06 16:46:02},
date={07May06 18:02:04}
}

@inproceedings {Linnea_Hjalmarsdotter,
email={osmi.vilhu@helsinki.fi},
first_name={Linnea},
last_name={Hjalmarsdotter},
affiliation={Stockholm Observatory, AlbaNova University Center},
address={Roslagstullbacken 21 SE-10691 Stockholm Sweden},
presentation_type={poster},
presentation_number={2},
presentation_panel={F0},
title={Modelling hard X-ray light curves of Cygnus X-3 by particle simulations},
authors={Osmi Vilhu, Pasi Hakala, Linnea Hjalmarsdotter, Diana Hannikainen, Ada Paizis},
abstract={We modelled ISGRI and BATSE light curves of Cygnus X-3 using particle simulations from the WR-companion wind in the binary potential. During a few binary orbits a stable co-rotating filled cocoon is formed for a range of mass ratios and wind velocities. For large inclinations, assuming electron scattering as the main opacity source, the observed light curves can be briefly understood. We discuss also other consequences of these simulations.},
persons_number={0},
pdate={01Mar06 18:47:20},
date={08May06 09:45:29}
}

@inproceedings {Linnea_Hjalmarsdotter,
email={osmi.vilhu@helsinki.fi},
first_name={Linnea},
last_name={Hjalmarsdotter},
affiliation={Stockholm Observatory, AlbaNova center},
address={Roslagstullbacken 21, SE-10691 Stockholm, Sweden},
presentation_type={poster},
presentation_number={3},
presentation_panel={G0},
title={The spreding (boundary) layer of GX 9+9},
authors={Osmi Vilhu, Ada Paizis, Diana Hannikainen, Juho Schultz, Volker beckmann, Thierry Courvoisier, Linnea Hjalmarsdotter, Bright LMXRB team},
abstract={The INTEGRAL core-programme data of the bright atoll GX 9+9 (4A 1728-169) were analysed together with the RXTE observations allocated to the core programme Bright LMXRB team. We concentrated on the off-set angles less than 3 degrees. The source was on the banana state and the individual scw-spectra could be fitted with two components: disc and spreading layer (SL) emission (diskbb + compbb). The results are in a qualitative agreement with the spreading layer models by Inogamov and Sunyaev (1999) and Suleimanov and Poutanen (2005) where the SL-belt area increases with the SL-luminosity and the temprerature remains close to the critical (Eddington) one ( about 2 keV) . At small accretion rate the SL-area drops while the observed temperature increases above the local critical temperature possibly due to the color correction effect (diluted BB).},
persons_number={0},
pdate={21Mar06 14:22:14},
date={08May06 10:04:55}
}

@inproceedings {Eugenio_Bottacini,
email={eub@mpe.mpg.de},
first_name={Eugenio},
last_name={Bottacini},
affiliation={MPE, Garching, Germany},
address={Giessenbachstrasse - 85748 Garching},
presentation_type={poster},
presentation_number={1},
presentation_panel={D0},
title={INTEGRAL Observations of the Blazar 3C 279 during the `Deep Extragalactic Survey'},
authors={E. Bottacini (MPE, Garching, Germany), W. Collmar (MPE, Garching, Germany), T. Courvoisier (ISDC, Geneva, Switzerland)},
abstract={The prominent Gamma-Ray blazar 3C 279, an optically violently variable (OVV) quasar, was observed by INTEGRAL during AO3 on several occasions: in the observations of the so-called ``Deep Extragalactic Survey'', pointing to the Virgo region of the sky. This survey was conducted during the summer 2005 and winter 2005/2006 visibility period of the field in AO-3, yielding a total exposure time of 1 Msec. Currently we are analysing these INTEGRAL survey data with respect to 3C 279. We will present the hard X-ray behaviour (lightcurves, spectra) of the blazar as observed by INTEGRAL. The results will be compared to other high-energy measurements of the source, put in multifrequency context, and finally discussed in the framework of current blazar models.},
persons_number={0},
pdate={01Mar06 12:49:16},
date={08May06 11:36:35}
}

@inproceedings {Mariateresa_Fiocchi,
email={mariateresa.fiocchi@iasf-roma.inaf.it},
first_name={Mariateresa},
last_name={Fiocchi},
affiliation={IASF-Roma INAF},
address={},
presentation_type={poster},
presentation_number={2},
presentation_panel={G0},
title={First detection of Compton reflection in the low-mass X-ray binary 4U1705-44 with INTEGRAL},
authors={},
abstract={We will present data from INTEGRAL and BeppoSAX satellites showing a pronounced spectral state transition of the neutron-star, atoll-type, low-mass X-ray binary 4U1705-44. Its energy spectrum in both states can be described as the sum of a blackbody, a 6.4-keV Fe line and a component due to thermal Comptonization. For the first time in this source, we find a strong signature of Compton reflection in the INTEGRAL hard state, appearing presumably from the accretion disk surface illuminated by the primary Comptonized spectrum. The blackbody component originates in the optically thick accretion disk and the neutron-star surface, and the harder Comptonized component arises from a hot inner flow with the seed photons coming from the accretion disk and/or the neutron-star surface. The spectral transitions of 4U1705-44 are shown to be associated with changes in the accretion rate, changing in turn the temperature of the Comptonizing electrons and the strength of Compton reflection. This can be theoretically explained in a model with a truncated outer accretion disk surrounding a hot inner flow, with the accretion rate determining the truncation radius.},
persons_number={0},
pdate={01Mar06 19:17:09},
date={08May06 11:48:20}
}

@inproceedings {Mariateresa_Fiocchi,
email={mariateresa.fiocchi@iasf-roma.inaf.it},
first_name={Mariateresa},
last_name={Fiocchi},
affiliation={IASF-Roma INAF},
address={},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={Detection of a hard tail in the spectrum of the low mass X-ray binary 4U 1636-53 with INTEGRAL},
authors={},
abstract={We will present the spectral analysis results of the neutron star, atoll type, low mass X-ray Binary 4U 1636-53 observed by INTEGRAL and BeppoSAX satellites, covering the energy range 0.1-150 keV. We study the spectral behaviour separately in three epochs. 1st and 2rd epoch show a continuum well described by a soft blackbody and Comptonized spectrum with a spectral transition associated with changes in the Comptonizing electrons and black body temperature. In the 3rd epoch, a hard tail dominates the emission above 40 keV. This INTEGRAL spectrum can be fitted as the sum of a power law with photon index of 1.8, a blackbody and a Comptonized component. A comparison with hard tails detected in Z sources and some soft states of black hole binaries suggests that a similar mechanism could originate these components in black hole and neutron star systems.},
persons_number={0},
pdate={01Mar06 19:14:21},
date={08May06 11:48:46}
}

@inproceedings {Valentina_Bianchin,
email={bianchin@iasfbo.inaf.it},
first_name={Valentina},
last_name={Bianchin},
affiliation={INAF/IASF-Bologna},
address={via Gobetti 101, 40129 BOLOGNA (ITALY)},
presentation_type={none},
presentation_number={1},
presentation_panel={J0},
title={IBIS/PICSIT status and scientific highlights},
authors={},
abstract={Co-author of the poster by Di Cocco et al.},
persons_number={0},
pdate={27Apr06 19:03:16},
date={08May06 12:32:34}
}

@inproceedings {Vladimir_Kocharovsky,
email={hdjk1@mail.nnov.ru},
first_name={Vladimir},
last_name={Kocharovsky},
affiliation={Institute of Applied Physics RAS},
address={46 Ulyanov st., Nizhny Novgorod, 603950, Russia},
presentation_type={poster},
presentation_number={2},
presentation_panel={D0},
title={The self-consistent current sheets and filaments in relativistic astrophysical jets},
authors={V.Martyanov, E.Derishev, V.Kocharovsky, Vl.Kocharovsky},
abstract={We find analytically a continuous set of stationary current sheets and filaments in collisionless multi-component plasma using integrals of two-dimensional motion of particles in the self-consistent magnetic field. In our solutions, the magnetic energy density can be comparable to that of particles, and the spatial scale can be arbitrary compared to typical gyroradius of the particles. We consider the properties of newly found stationary solutions and their possible applications to analysis of magnetic field configurations emerging in relativistic astrophysical shocks and jets. We use our results for interpretation of recent observations and numerical simulations. By choosing particular dependence of particle distribution function on the integrals of motion we are able to obtain various profiles of magnetic field and self-consistent current, including non-monotone. The obtained solutions describe much more general class of equilibrium configurations as compared to known generalizations of Harris current sheets. On this basis, we suggest a way to describe slow dynamics and filamentation of collisionless current configurations in AGNs, microquasars and GRB sources.},
persons_number={0},
pdate={28Feb06 20:41:00},
date={08May06 12:46:15}
}

@inproceedings {Lorenzo_Natalucci,
email={Lorenzo.Natalucci@iasf-roma.inaf.it},
first_name={Lorenzo},
last_name={Natalucci},
affiliation={INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica},
address={Via del Fosso del Cavaliere, 100 - Roma (Italy)},
presentation_type={poster},
presentation_number={1},
presentation_panel={E0},
title={INTEGRAL observation of three compact sources in the Sagittarius Arm region},
authors={},
abstract={A sky region, located in the direction of the tangent of the Sagittarius Arm, has been observed during 2003 by the high energy observatory INTEGRAL. The field, centered on the position of the X-ray burster X1916-053 contains three interesting objects. One is the microquasar GRS 1915+105, clearly detected by IBIS on May 1, 2003 during an observation lasting $\sim14$ ks. The two other sources are the X-ray pulsars 4U 1901+03 and XTE J1855-026. The former, a recurrent transient, is bright in the May 1 observation at an intensity of $\sim110$ mCrab in the 20-40 keV energy range. XTE J1855-026, seen at the level of $\sim15$ mCrab was also detected. This source, an eclipsing system with an orbital period of $\sim6$ days, has been better studied during a long observation (200 ks) performed in November 2003.},
persons_number={0},
pdate={01Mar06 21:28:09},
date={08May06 15:11:19}
}

@inproceedings {Demosthenes_Kazanas,
email={kazanas@milkyway.gsfc.nasa.gov},
first_name={Demosthenes},
last_name={Kazanas},
affiliation={NASA/Goddard Space Flight Center},
address={NASA/GSFC, Code 663, Greenbelt MD, 20771},
presentation_type={oral},
presentation_number={1},
presentation_panel={I9},
title={The `Nuclear Pile' GRB model: spectro-temporal properties of prompt GRB emission},
authors={},
abstract={The `Nuclear Pile' is a GRB model that can provide the electrons necessary for the GRB emission as a result of a radiative instability effected through the proton-photon -- pair reaction. Under conditions similar to those of the criticality of a nuclear pile, the energy storred in relativistic protons can be released explosively to produce the prompt GRB emission. Because of the reaction threshold, the nuFnu spectra of the resulting radiation exhibit a peak at $\sim1$ MeV in the lab frame, in agreement with GRB observations. We provide detailed spectra of the prompt emission as a function of time from optical to 1 TeV energies, which are in general agreement with those observed. We also discuss the transition from the prompt emission to the afterglow.},
persons_number={1},
pdate={01Mar06 22:49:18},
date={08May06 17:35:21}
}

@inproceedings {Wojtek_Hajdas,
email={wojtek.hajdas@psi.ch},
first_name={Wojtek},
last_name={Hajdas},
affiliation={Paul Scherrer Institut},
address={PSI-Villigen, ODRA 120, CH-5232 Switzerland},
presentation_type={poster},
presentation_number={1},
presentation_panel={I0},
title={Observations of the initial spike from the SGR1806-20 Giant Flare with INTEGRAL and PROBA1 SREM instruments},
authors={},
abstract={Two identical radiation monitors (SREMs) onboard of INTEGRAL and PROBA satellites detected on 27 Dec 2004 a Giant Flare from SGR1806-20. Due to small dimensions and high counting rate ability two SREMs were able to provide clean, unsaturated data with a coarse energy resolution in the range from 70 keV to 1000 keV. We present spectral analysis performed with both instruments, compare results with measurements from other space missions and discuss implications from different types of spectral forms.},
persons_number={0},
pdate={28Feb06 17:14:02},
date={09May06 00:36:44}
}

@inproceedings {Wojtek_Hajdas,
email={wojtek.hajdas@psi.ch},
first_name={Wojtek},
last_name={Hajdas},
affiliation={Paul Scherrer Institut},
address={PSI-Villigen, ODRA 120, CH-5232 Switzerland},
presentation_type={poster},
presentation_number={2},
presentation_panel={I0},
title={RHESSI instrumental limits on measurements of linear photon polarization from GRBs, SGRs and Solar Flares.},
authors={},
abstract={The RHESSI spectrometer with its 9 large Ge detectors can be used as a rotating gamma ray polarimeter in the energy range from tens to hundreds keV. The polarization signal is extracted from the eventlist using Compton scattering technique in either single or coincidence mode. In an ideal case of low background levels and gamma source locations close to the satellite axis the modulation factor can be as high 50\%. In this paper we discuss more realistic polarimetric performance of RHESSI using the entire satellite computer mass model and Monte Carlo simulations of photons reaching detectors also after scattering in the Earth atmosphere. In the single mode it introduces an additional, strongly oscillating background signal depending on relative position between the source, RHESSI and Earth. In the coincidence mode an extra contamination comes out from a position dependent pattern of accidental and real coincidences. New limits and examples of the minimum detectable polarization are given for several sources like Solar Flares, Soft Gamma Repeaters and Gamma-Ray Bursts.},
persons_number={0},
pdate={02Mar06 01:09:42},
date={09May06 00:37:28}
}

@inproceedings {Linnea_Hjalmarsdotter,
email={diana@astro.helsinki.fi},
first_name={Linnea},
last_name={Hjalmarsdotter},
affiliation={Observatory, University of Helsinki},
address={},
presentation_type={poster},
presentation_number={4},
presentation_panel={F0},
title={INTEGRAL observes GRS 1915+105},
authors={Diana Hannikainen, Osmi Vilhu, Jerome Rodriguez, Andrzej Zdziarksi, Juri Poutanen, Harry Lehto, on behalf of a larger collaboration},
abstract={We have observed the microquasar GRS 1915+105 already several times with INTEGRAL (see talk by Jerome Rodriguez). Here we present results from Revolution 48 - when the source exhibited a new class of variability - and Revolution 193 - when the source was not only very variable, but we also observed a major radio flaring episode.},
persons_number={0},
pdate={01Mar06 18:32:04},
date={09May06 15:02:08}
}

@inproceedings {Peter_den_Hartog,
email={Hartog@sron.nl},
first_name={Peter},
last_name={den Hartog},
affiliation={Ph.D. Student},
address={Sorbonnelaan 2, 2587 CA, Utrecht, The Netherlands},
presentation_type={oral},
presentation_number={1},
presentation_panel={H2},
title={Lastest INTEGRAL results on hard X-ray characteristics of Anomalous X-ray Pulsars},
authors={Hermsen W., Kuiper L., Kaspi V., Dib R., van Kerkwijk M., Durant M., Stappers B., Rea N., Vink J.},
abstract={One of the breakthrough discoveries with INTEGRAL is the detection of hard X-ray emission from Anomalous X-ray Pulsars (AXPs). Before the INTEGRAL era AXPs were known as soft X-ray pulsars which could be studied up to $\sim10$ keV. This view has changed drastically since the discovery of hard X-ray emission ($>10$ keV) from three AXPs by INTEGRAL (Molkov et al. 2004, Revnivtsev et al. 2004 and den Hartog et al. 2004; 2006). Kuiper et al. (2004; 2006) discovered pulsed emission above 10 keV from four AXPs using RXTE (PCA and HEXTE) data. The power-law like spectra (20-150 keV) are very hard with photon indices $\leq1.0$ and the derived luminosities are 2-3 orders of magnitude above the rotational energy losses. The regular and long INTEGRAL observations of the Cassiopeia and Galactic-Center regions allow us to study the spectral and timing characteristics of several AXPs in these regions in great detail. In this talk we will present, 1) the most recent INTEGRAL results on the detected AXPs, 2) compare these with those from observations at radio, near infra red and optical wavelengths, and 3) confront proposed theoretical scenarios from the production of non-thermal emission in AXP magnetospheres with our observational results. },
persons_number={0},
pdate={28Feb06 18:40:37},
date={09May06 19:24:04}
}

@inproceedings {Georg_Weidenspointner,
email={Georg.Weidenspointner@cesr.fr},
first_name={Georg},
last_name={Weidenspointner},
affiliation={Centre d'Etude Spatiale des Rayonnements},
address={9, avenue du Colonel-Roche; BP 4346; 31028 Toulouse Cedex 4; France},
presentation_type={poster},
presentation_number={1},
presentation_panel={J0},
title={MGGPOD Version 1.1: a Monte Carlo Suite for Gamma Ray Astronomy},
authors={},
abstract={Intense and complex instrumental backgrounds, against which the much smaller signals from celestial sources have to be discerned, are a notorious problem for low and intermediate energy gamma-ray astronomy. Therefore a detailed qualitative and quantitative understanding of instrumental line and continuum backgrounds is crucial for most stages of gamma-ray astronomy missions, ranging from the design and development of new instrumentation through performance prediction to data reduction. We announce the public release of Version 1.1 of MGGPOD, a user-friendly suite of Monte Carlo codes built around the widely used GEANT (Version 3.21) package, to simulate ab initio the physical processes relevant for the production of instrumental backgrounds. These include the build-up and delayed decay of radioactive isotopes as well as the prompt de-excitation of excited nuclei, both of which give rise to a plethora of instrumental gamma-ray background lines in addition to continuum backgrounds. The MGGPOD package and documentation are publicly available for download from http://sigma-2.cesr.fr/spi/MGGPOD/. Improvements implemented in Version 1.1 of the proven MGGPOD Monte Carlo suite include: additional beam geometry and spectral options, capability of modelling polarized photons, additional output formats suitable for event reconstruction algorithms, and improved neutron interaction cross sections.},
persons_number={0},
pdate={01Mar06 12:13:14},
date={10May06 16:33:29}
}

@inproceedings {Georg_Weidenspointner,
email={Georg.Weidenspointner@cesr.fr},
first_name={Georg},
last_name={Weidenspointner},
affiliation={Centre d'Etude Spatiale des Rayonnements},
address={9, avenue du Colonel-Roche; BP 4346; 31028 Toulouse Cedex 4; France},
presentation_type={oral},
presentation_number={2},
presentation_panel={A2},
title={The sky distribution of 511 keV positron annihilation line emission as measured with INTEGRAL/SPI},
authors={},
abstract={We present the current status of our studies of the sky distribution of 511 keV positron annihilation line emission with now about 2.5 years of observations with the SPI imaging spectrometer onboard ESA's INTEGRAL observatory and further improved background modelling. In particular, we provide current constraints on the spatial distribution of 511 keV line emission from the Galactic bulge region and from the Galactic disk, and discuss its implications on the origin of Galactic positrons. We also update limits on 511 keV line emission from individual positron source candidates.},
persons_number={0},
pdate={01Mar06 12:55:54},
date={10May06 16:34:12}
}

@inproceedings {Barnstedt_Juergen,
email={barnstedt@astro.uni-tuebingen.de},
first_name={Barnstedt},
last_name={Juergen},
affiliation={University of Tuebingen, Institute for Astronomy and Astrophysics},
address={Sand 1, 72076 Tuebingen, Germany},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={INTEGRAL observations of OAO 1657-415},
authors={},
abstract={We present results of INTEGRAL observations of the high-mass X-ray binary pulsar OAO 1657-415. A total observation time of about 2 Ms was evaluated, mainly from the Galactic Plane Survey program, but also public data. We investigated spectra resolved in both the orbital period and the pulsar period. We will discuss the existance of an cyclotron absorption line which was formerly detected in BeppoSAX observations.},
persons_number={0},
pdate={28Feb06 19:08:00},
action={Remove me from the list},
date={11May06 13:51:31}
}

@inproceedings {Vyacheslav_Dokuchaev,
email={dokuchaev@inr.npd.ac.ru},
first_name={Vyacheslav},
last_name={Dokuchaev},
affiliation={Institute for Nuclear Research of the Russian Academy of Sciences},
address={Prospect 60-letiya Oktyabrya 7a, 117312 Moscow},
presentation_type={poster},
presentation_number={1},
presentation_panel={A0},
title={Dark matter annihilation in the Galaxy},
authors={V. Berezinsky, V. Dokuchaev and Yu. Eroshenko},
abstract={The annihilation of dark matter (DM) in the Galactic halo is enhanced due to the presence of small-scale DM clumps. It is shown that the resulting enhancement (boost factor) of annihilation signal due to the halo clumpiness strongly depends on the primordial perturbation spectrum and varies in the range ~10-100.},
persons_number={0},
pdate={22.02.06 11:17:24},
date={11May06 18:44:02}
}

@inproceedings {Yury_Eroshenko,
email={erosh@inr.npd.ac.ru},
first_name={Yury},
last_name={Eroshenko},
affiliation={Institute for Nuclear Research RAS},
address={60th Oktober Univ. prosp., 7A, Moscow, 117312, Russia },
presentation_type={poster},
presentation_number={1},
presentation_panel={A0},
title={Small-scale DM structures in the Galactic halo},
authors={Berezinsky V.S., Dokuchaev V.I., Eroshenko Yu.N. },
abstract={The tidal gravitational destruction of small-scale dark matter clumps in the Galactic halo is considered. We take into account the destruction of clumps by stars in the Galactic bulge and halo and by the Galactic disk. It is shown that the Galactic disc provides the dominant contribution to the tidal destruction of small-scale clumps outside the bulge. The results obtained are crucial for calculations of the dark matter annihilation signal in the Galaxy.},
persons_number={0},
pdate={28Feb06 14:59:56},
date={12May06 07:25:48}
}

@inproceedings {Anatol_Cherepashchuk,
email={cher@sai.msu.ru},
first_name={Anatol},
last_name={Cherepashchuk},
affiliation={Sternberg Astronomical Institute},
address={119992, Universitetskij pr. 13, Moscow},
presentation_type={oral},
presentation_number={1},
presentation_panel={F3},
title={INTEGRAL observations of SS433: Analysis of precessional and orbital hard X-ray periodicities.},
authors={},
abstract={Results of long-term monitoring of SS433 by INTEGRAL in 2003-2005 are presented. Several new features of the observed precessional and orbital light curves of SS433 are particulary discussed. The amplitude (maximum to minimum flux ratio) of the precessional light curve in 20-60 keV is found to be 4-8 (much higher than in the standard X-ray band 2-10 keV), with the secondary maximum present. An orbital eclipse observed around precessional phase 0 coincides with the optical one, while that observed at the phase 0.22 is found to be shifted with respect to the optical eclipse. These features are described by the geometrical model with thick supercritical accretion disk and jet from the central source. The analysis of the INTEGRAL data allows us to put constraints on the parameters of SS433 and lends further support that SS433 is a galactic microquasar with a black hole. },
persons_number={0},
pdate={27Feb06 15:23:47},
date={18May06 11:42:55}
}

@inproceedings {Stephane_Corbel,
email={corbel@discovery.saclay.cea.fr},
first_name={Stephane},
last_name={Corbel},
affiliation={Univ. Paris 7 & CEA Saclay},
address={Bat 709, Ormes des Merisiers, 91191 Gif sur Yvette Cedex, France},
presentation_type={poster},
presentation_number={1},
presentation_panel={F0},
title={Multiwavelength observations of GX 339-4 },
authors={},
abstract={GX 339-4 has been one of the key sources to unravel the accretion - ejection coupling around stellar mass black holes. We will present the results of our new campaigns during the recent outbursts of GX 3339-4 from 2002 to 2005. We will emphasize on the origin of the high energy emission in this black hole, as well as the general properties of the outflows in light of recent advances in this field.},
persons_number={ ?},
pdate={28Feb06 12:36:18},
action={Remove me from the list},
date={19May06 15:38:29}
}

@inproceedings {Yuri_Gnedin,
email={gnedin@gao.spb.ru},
first_name={Yuri},
last_name={Gnedin},
affiliation={Central Astronomical Observatory at Pulkovo, S-Petersburg, Russia.},
address={S-Petersburg, 196140, Pulkovskoe Shosse 65/1, GAO RAN.},
presentation_type={poster},
presentation_number={1},
presentation_panel={G0},
title={Near infrared and radio observations of relativistic objects at telescopes AZT-24 GAO RAS and RTF-32 IPA RAS},
authors={},
abstract={I present the review of the basic results of NIR and radio observations of some INTEGRAL targets made at telescopes of Pulkovo Observatory and Institute of Applied Astronomy RAS.},
persons_number={0},
pdate={19May06 14:17:10},
date={19May06 20:10:15}
}

@inproceedings {Jean-Pierre_Roques,
email={roques@cesr.fr},
first_name={Jean-Pierre},
last_name={Roques},
affiliation={CESR},
address={9 avenue du colonel Roche, 31028 Toulouse, France},
presentation_type={none},
presentation_number={1},
presentation_panel={},
title={},
authors={},
abstract={},
persons_number={0},
pdate={23May06 19:32:35},
date={25May06 19:16:31}
}

@inproceedings {Dieter_Hartmann,
email={hdieter@clemson.edu},
first_name={Dieter},
last_name={Hartmann},
affiliation={Clemson University},
address={Dept. of Physics & Astronomy, Clemson, SC 29634-0978},
presentation_type={oral},
presentation_number={1},
presentation_panel={B7},
title={Tracing Galactic star formation with radioactivities},
authors={},
abstract={We discuss methods for tracing the galactic supernova rate, and by implication the star formation rate. In particular, we highlight tracers involving radioactivities such as $^{26}$Al, $^{44}$Ti, and $^{60}$Fe. We discuss existing results obtained with INTEGRAL and RHESSI, and present an outlook on expected results that can be obtained with continued observations with these detectors and discuss expectations for a future Advanced Compton Telescope. },
persons_number={1},
pdate={01Mar06 07:36:15},
date={25May06 19:57:03}
}

@inproceedings {Edward_P.J._van_den_Heuvel,
email={edvdh@science.uva.nl},
first_name={Edward P.J.},
last_name={van den Heuvel},
affiliation={University of Amsterdam, Astronomy Department},
address={Kruislaan 403, 1098SJ Amsterdam, The Netherlands},
presentation_type={oral},
presentation_number={1},
presentation_panel={X2},
title={After dinner speech},
authors={},
abstract={None},
persons_number={0},
pdate={29May06 23:09:09},
date={30May06 19:29:13}
}

@inproceedings {Pietro_Ubertini,
email={pietro.ubertini@iasf-roma.inaf.it},
first_name={Pietro},
last_name={Ubertini},
affiliation={IASF-Roma/INAF},
address={Via Fosso del Cavaliere 100},
presentation_type={none},
presentation_number={1},
presentation_panel={A0},
title={},
authors={},
abstract={},
persons_number={0},
pdate={30May06 18:31:25},
date={30May06 19:30:03}
}

@inproceedings {Stern_Boris,
email={stern@bes.asc.rssi.ru},
first_name={Stern},
last_name={Boris},
affiliation={Astro Space Center of Lebedev Physical Institute},
address={Moscow, Profsoyuznaya 84/32 },
presentation_type={oral},
presentation_number={1},
presentation_panel={D7},
title={Runaway electromagnetic cascade in shear flows and high energy radi
ation of astrophysical jets},
authors={},
abstract={We propose a straightforward and efficient mechanism for the hig
h-energy emission of relativistic astrophysical jets associated with an ex
change of interacting high-energy photons between the jet and external env
ironment. Physical processes playing the main role in this mechanism are e
lectron-positron pair production by photons and the inverse Compton scatte
ring. This scenario has been studied with numerical simulations demonstrat
ing that under reasonable conditions it has a supercritical character: the
high-energy photons breed exponentially being fed directly by the bulk ki
netic energy of the jet. Eventually particles feed back on the fluid dynam
ics and the jet partially decelerates. As a result, a significant fraction
(at least 10--20 per cent) of the jet kinetic energy is converted into ra
diation.},
persons_number={0},
pdate={02Mar06 16:51:58},
date={01Jun06 19:53:23}
}

@inproceedings {Pascal_Chardonnet,
email={chardonnet@lapp.in2p3.fr},
first_name={Pascal},
last_name={Chardonnet},
affiliation={Universit\'e de Savoie},
address={LAPTH, BP 110, 74941 Annecy-le-vieux Cedex, France},
presentation_type={poster},
presentation_number={1},
presentation_panel={I0},
title={On the GRB 031203 spectra},
authors={},
abstract={The theoretical model we have been developing [M.G. Bernardini, C.L. Bianco, P. Chardonnet, F. Fraschetti, R. Ruffini, S.-S. Xue, ApJ 634 (2005) L29-L32] has a clear advantage of predicting the structure of the instantaneous spectrum of GRB 031203, showing a monotonic transition from hard to soft. Each instantaneous spectrum is obtained by an integration over the corresponding equitemporal surface (EQTS): it is itself a convolution, weighted by appropriate Lorentz and Doppler factors, of $\sim10^6$ thermal spectra with variable temperature. Therefore the time-integrated spectra are not plain convolutions of thermal spectra; they are convolutions of convolutions of thermal spectra. Such time-integrated spectra give rise to simple power-law shapes. },
persons_number={1},
pdate={03Apr06 13:52:12},
date={01Jun06 20:36:35}
}

@inproceedings {David_Smith,
email={dsmith@scipp.ucsc.edu},
first_name={David},
last_name={Smith},
affiliation={University of California, Santa Cruz},
address={Physics Dept., UCSC, 1156 High St, Santa Cruz, CA 95064 USA},
presentation_type={oral},
presentation_number={1},
presentation_panel={A5},
title={Highlights from RHESSI},
authors={},
abstract={The Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI), designed to study the Sun, has also provided important data on astrophysical targets in the Galaxy with its unshielded germanium detectors. I will review recent RHESSI results on Galactic nucleosynthesis, the enormous flare from SGR 1806-20 on 27 December 2004, the 2005 outburst of the Be/X-ray pulsar A0535+26, and other topics, including some solar results from gamma-ray lines (e.g. positron annihilation and nuclear de-excitation). I will also report on instrument status and future operations.},
persons_number={0},
pdate={28Feb06 22:58:23},
date={01Jun06 21:27:32}
}

@inproceedings {Valery_Zolotarev,
email={zolotasd@yandex.ru},
first_name={Valery},
last_name={Zolotarev},
affiliation={Space research institute RAS, Moscow},
address={RF, Moscow, ul.Profsouznaja,84/32},
presentation_type={poster},
presentation_number={1},
presentation_panel={J0},
title={The New Quick Decoders for Noisy Space channels},
authors={},
abstract={New kinds of decoding schemes are proposed for the Space and satellite channels. They are all very quick and can work near channel capacity. Soft and hard coding variants are discussed. Real devices will be shown. Comparison with other decoders will be done.},
persons_number={0},
pdate={01Mar06 16:40:56},
date={02Jun06 00:36:11}
}

@inproceedings {Nickolai_Shaposhnikov,
email={nikolai@milkyway.gsfc.nasa.gov},
first_name={Nickolai},
last_name={Shaposhnikov},
affiliation={Universities Space Research Association/GSFC},
address={GSFS, Bld 2, Code 662, W20J, Greenbelt, MD, 20770, USA},
presentation_type={poster},
presentation_number={1},
presentation_panel={F0},
title={GRO J1655-40: Early Stage of the 2005 Outburst},
authors={},
abstract={The black-hole X-ray binary transient GRO J1655-40 underwent an outburst beginning in early 2005. We present the results of our multiwavelenght observational campaign to study the early outburst spectral and temporal evolution, which combines a program of target of opportunity with the INTEGRAL, RXTE and NRAO. We model the broad-band high- energy spectrum in the context of empirical models, as well as more physically motivated thermal and bulk-motion Comptonization and Compton reflection models. We present an analysis of the multi-frequency light curves, identifying structures such as intensity dips, and inflections.We also consider radio/optical/X-ray connection in context of possible syncrotron origin of X-ray emission in Low/Hard state of BH sources. },
persons_number={0},
pdate={28Feb06 21:35:59},
action={Remove me from the list},
date={02Jun06 15:34:58}
}