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1. Probing the emission physics and weak/soft population of Gamma-Ray Bursts with LOFT

Author

Amati, L., Stratta, G., Atteia, J. -L, Pasquale, M., Del Monte, E., Gendre, B., Götz, D., Guidorzi, C., Izzo, L., Kouveliotou, C., Osborne, J., Penacchioni, A. V., Romano, P., Sakamoto, T., Salvaterra, R., Schanne, S., In T Zand, J. J. M., Lucio Angelo Antonelli, Braga, J., Brandt, S., Bucciantini, N., Castro-Tirado, A., D Elia, V., Feroci, M., Fuschino, F., Guetta, D., Longo, F., Lyutikov, M., Maccarone, T., Mangano, V., Marisaldi, M., Mereghetti, S., O Brien, P., Rossi, E. M., Ryde, F., Soffitta, P., Troja, E., Wijers, R. A. M. J., and Zhang, B.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract

This is a White Paper in support of the mission concept of the Large Observatory for X-ray Timing (LOFT), proposed as a medium-sized ESA mission. We discuss the potential of LOFT for the study of gamma-ray bursts. For a summary, we refer to the paper., White Paper in Support of the Mission Concept of the Large Observatory for X-ray Timing

Published
2015

2. The rapid decay of the optical emission from GRB 980326 and its possible implications

Author

Groot, P. J., Galama, T. J., Vreeswijk, P. M., Wijers, R. A. M. J., Pian, E., Palazzi, E., Paradijs, J., Kouveliotou, C., In T Zand, J. J. M., Heise, J., Robinson, C., Tanvir, N., Lidman, C., C.G. Tinney, Keane, M., Briggs, M., Hurley, K., Gonzalez, J. -F, Hall, P., Smith, M. G., Covarrubias, R., Jonker, P. G., Casares, J., Masetti, N., Frontera, F., Feroci, M., Piro, L., Costa, E., Smith, R., Jones, B., Windridge, D., Bland-Hawthorn, J., Veilleux, S., Garcia, M., Brown, W. R., Stanek, K. Z., Castro-Tirado, A. J., Gorosabel, J., Greiner, J., Jäger, K., Böhm, A., Fricke, K. J., Artificial intelligence, Economics, Tinbergen Institute, (Astro)-Particles Physics, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Physics, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Optical decay, Power law, Space and Planetary Science, Spectral slope, Exponent, Optical emission spectroscopy, Gamma-ray burst, Constant (mathematics)
Abstract

We report the discovery of the optical counterpart to GRB 980326. Its rapid optical decay can be characterized by a power law with exponent -2.10 +/- 0.13 and a constant underlying source at R_c=25.5 +/- 0.5. Its optical colours 2.1 days after the burst imply a spectral slope of -0.66 +/- 0.70. The gamma-ray spectrum as observed with BATSE shows that it is among the 4% softest bursts ever recorded. We argue that the rapid optical decay may be a reason for the non-detection of some low-energy afterglows of GRBs., 13 pages, 3 Postscipt figures, Astrophysical Journal Letters, accepted May 29, 1998

Published
1998

3. The Large Observatory for X-ray Timing (LOFT)

Author

Feroci, M., Stella, L., Klis, M., Courvoisier, T. J. -L, Hernanz, M., Hudec, R., Santangelo, A., Walton, D., Zdziarski, A., Barret, D., Belloni, T., Braga, José, Brandt, S., Budtz-Jørgensen, C., Campana, S., Den Herder, J. -W, Huovelin, J., Israel, G. L., Pohl, M., Ray, P., Vacchi, A., Zane, S., Argan, A., Primo Attinà, Bertuccio, G., Bozzo, E., Campana, R., Chakrabarty, D., Costa, E., Rosa, A., Del Monte, E., Di Cosimo, S., Donnarumma, I., Evangelista, Y., Haas, D., Jonker, P., Korpela, S., Labanti, C., Malcovati, P., Mignani, R., Muleri, F., Rapisarda, M., Rashevsky, A., Rea, N., Rubini, A., Tenzer, C., Wilson-Hodge, C., Winter, B., Wood, K., Zampa, G., Zampa, N., Abramowicz, M. A., Alpar, M. A., Altamirano, D., Alvarez, J. M., Amati, L., Amoros, C., Antonelli, L. A., Artigue, R., Azzarello, P., Bachetti, M., Baldazzi, G., Barbera, M., Barbieri, C., Basa, S., Baykal, A., Belmont, R., Boirin, L., Bonvicini, V., Burderi, L., Bursa, M., Cabanac, C., Cackett, E., Caliandro, G. A., Casella, P., Chaty, S., Chenevez, J., Coe, M. J., Collura, A., Corongiu, A., Covino, S., Cusumano, G., D Amico, Frank, Dall Osso, S., Martino, D., Paris, G., Di Persio, G., Di Salvo, T., Done, C., Dovčiak, M., Drago, A., Ertan, U., Fabiani, S., Falanga, M., Fender, R., Ferrando, P., Della Monica Ferreira, D., Fraser, G., Frontera, F., Fuschino, F., Galvez, J. L., Gandhi, P., Giommi, P., Godet, O., Göǧüş, E., Goldwurm, A., Götz, D., Grassi, M., Guttridge, P., Hakala, P., Henri, G., Hermsen, W., Horak, J., Hornstrup, A., In T Zand, J. J. M., Isern, J., Kalemci, E., Kanbach, G., Karas, V., Kataria, D., Kennedy, T., Klochkov, D., Kluźniak, W., Kokkotas, K., Kreykenbohm, I., Krolik, J., Kuiper, L., Kuvvetli, I., Kylafis, N., Lattimer, J. M., Lazzarotto, F., Leahy, D., Lebrun, F., Lin, D., Lund, N., Maccarone, T., Malzac, J., Marisaldi, M., Martindale, A., Mastropietro, M., Mcclintock, J., Mchardy, I., Mendez, M., Mereghetti, S., Miller, M. C., Mineo, T., Morelli, E., Morsink, S., Motch, C., Motta, S., Muñoz-Darias, T., Naletto, G., Neustroev, V., Nevalainen, J., Olive, J. F., Orio, M., Orlandini, M., Orleanski, P., Ozel, F., Pacciani, L., Paltani, S., Papadakis, I., Papitto, A., Patruno, A., Pellizzoni, A., Petráček, V., Petri, J., Petrucci, P. O., Phlips, B., Picolli, L., Possenti, A., Psaltis, D., Rambaud, D., Reig, P., Remillard, R., Rodriguez, J., Romano, P., Romanova, M., Schanz, T., Schmid, C., Segreto, A., Shearer, A., Smith, A., Smith, P. J., Soffitta, P., Stergioulas, N., Stolarski, M., Stuchlik, Z., Tiengo, A., Torres, D., Török, G., Turolla, R., Uttley, P., Vaughan, S., Vercellone, S., Waters, R., Watts, A., Wawrzaszek, R., Webb, N., Wilms, J., Zampieri, L., Zezas, A., Ziolkowski, J., Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), APC - Astrophysique des Hautes Energies (APC - AHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Astronomy, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), M. Feroci, L. Stella, M. v. der, T. Courvoisier, M. Hernanz, R. Hudec, A. Santangelo, D. Walton, A. Zdziarski, D. Barret, T. Belloni, J. Braga, S. Brandt, C. Budtz-Jorgensen, S. Campana, J. d. Herder, J. Huovelin, G. Israel, M. Pohl, P. Ray, A. Vacchi, S. Zane, A. Argan, P. Attina, G. Bertuccio, E. Bozzo, R. Campana, D. Chakrabarty, E. Costa, A. D. Rosa, E. D. Monte, S. D. Cosimo, I. Donnarumma, Y. Evangelista, D. Haa, P. Jonker, S. Korpela, C. Labanti, P. Malcovati, R. Mignani, F. Muleri, M. Rapisarda, A. Rashevsky, N. Rea, A. Rubini, C. Tenzer, C. Wilson-Hodge, B. Winter, K. Wood, G. Zampa, N. Zampa, M. Abramowicz, M. Alpar, D. Altamirano, J. Alvarez, L. Amati, C. Amoro, L. Antonelli, R. Artigue, P. Azzarello, M. Bachetti, G. Baldazzi, M. Barbera, C. Barbieri, S. Basa, A. Baykal, R. Belmont, L. Boirin, V. Bonvicini, L. Burderi, M. Bursa, C. Cabanac, E. Cackett, G. Caliandro, P. Casella, S. Chaty, J. Chenevez, M. Coe, A. Collura, A. Corongiu, S. Covino, G. Cusumano, F. D'Amico, S. Dall'Osso, D. D. Martino, G. D. Pari, G. D. Persio, T. D. Salvo, C. Done, M. Dovciak, A. Drago, U. Ertan, S. Fabiani, M. Falanga, R. Fender, P. Ferrando, D. Ferreira, G. Fraser, F. Frontera, F. Fuschino, J. Galvez, P. Gandhi, P. Giommi, O. Godet, E. Gogu, A. Goldwurm, D. Gotz, M. Grassi, P. Guttridge, P. Hakala, G. Henri, W. Hermsen, J. Horak, A. Hornstrup, J. i. Zand, J. Isern, E. Kalemci, G. Kanbach, V. Kara, D. Kataria, T. Kennedy, D. Klochkov, W. Kluzniak, K. Kokkota, I. Kreykenbohm, J. Krolik, L. Kuiper, I. Kuvvetli, N. Kylafi, J. Lattimer, F. Lazzarotto, D. Leahy, F. Lebrun, D. Lin, N. Lund, T. Maccarone, J. Malzac, M. Marisaldi, A. Martindale, M. Mastropietro, J. McClintock, I. McHardy, M. Mendez, S. Mereghetti, M. Miller, T. Mineo, E. Morelli, S. Morsink, C. Motch, S. Motta, T. Munoz-Daria, G. Naletto, V. Neustroev, J. Nevalainen, J. Olive, M. Orio, M. Orlandini, P. Orleanski, F. Ozel, L. Pacciani, S. Paltani, I. Papadaki, A. Papitto, A. Patruno, A. Pellizzoni, V. Petracek, J. Petri, P. Petrucci, B. Phlip, L. Picolli, A. Possenti, D. Psalti, D. Rambaud, P. Reig, R. Remillard, J. Rodriguez, P. Romano, M. Romanova, T. Schanz, C. Schmid, A. Segreto, A. Shearer, A. Smith, P. Smith, P. Soffitta, N. Stergioula, M. Stolarski, Z. Stuchlik, A. Tiengo, D. Torre, G. Torok, R. Turolla, P. Uttley, S. Vaughan, S. Vercellone, R. Water, A. Watt, R. Wawrzaszek, N. Webb, J. Wilm, L. Zampieri, A. Zeza, J. Ziolkowski, High Energy Astrophys. & Astropart. Phys (API, FNWI), Feroci, M., Stella, L., van der Klis, M., Courvoisier, T. J.-L., Hernanz, M., Hudec, R., Santangelo, A., Walton, D., Zdziarski, A., Barret, D., Belloni, T., Braga, J., Brandt, S., Budtz-Jørgensen, C., Campana, S., den Herder, J.-W., Huovelin, J., Israel, G. L., Pohl, M., Ray, P., Vacchi, A., Zane, S., Argan, A., Attinà, P., Bertuccio, G., Bozzo, E., Campana, R., Chakrabarty, D., Costa, E., De Rosa, A., Del Monte, E., Di Cosimo, S., Donnarumma, I., Evangelista, Y., Haas, D., Jonker, P., Korpela, S., Labanti, C., Malcovati, P., Mignani, R., Muleri, F., Rapisarda, M., Rashevsky, A., Rea, N., Rubini, A., Tenzer, C., Wilson-Hodge, C., Winter, B., Wood, K., Zampa, G., Zampa, N., Abramowicz, M. A., Alpar, M. A., Altamirano, D., Alvarez, J. M., Amati, L., Amoros, C., Antonelli, L. A., Artigue, R., Azzarello, P., Bachetti, M., Baldazzi, G., Barbera, M., Barbieri, C., Basa, S., Baykal, A., Belmont, R., Boirin, L., Bonvicini, V., Burderi, L., Bursa, M., Cabanac, C., Cackett, E., Caliandro, G. A., Casella, P., Chaty, S., Chenevez, J., Coe, M. J., Collura, A., Corongiu, A., Covino, S., Cusumano, G., D'Amico, F., Dall'Osso, S., De Martino, D., De Paris, G., Di Persio, G., Di Salvo, T., Done, C., Dovčiak, M., Drago, A., Ertan, U., Fabiani, S., Falanga, M., Fender, R., Ferrando, P., Della Monica Ferreira, D., Fraser, G., Frontera, F., Fuschino, F., Galvez, J. L., Gandhi, P., Giommi, P., Godet, O., Göǧüş, E., Goldwurm, A., Götz, D., Grassi, M., Guttridge, P., Hakala, P., Henri, G., Hermsen, W., Horak, J., Hornstrup, A., in't Zand, J. J. M., Isern, J., Kalemci, E., Kanbach, G., Karas, V., Kataria, D., Kennedy, T., Klochkov, D., Kluźniak, W., Kokkotas, K., Kreykenbohm, I., Krolik, J., Kuiper, L., Kuvvetli, I., Kylafis, N., Lattimer, J. M., Lazzarotto, F., Leahy, D., Lebrun, F., Lin, D., Lund, N., Maccarone, T., Malzac, J., Marisaldi, M., Martindale, A., Mastropietro, M., McClintock, J., McHardy, I., Mendez, M., Mereghetti, S., Miller, M. C., Mineo, T., Morelli, E., Morsink, S., Motch, C., Motta, S., Muñoz-Darias, T., Naletto, G., Neustroev, V., Nevalainen, J., Olive, J. F., Orio, M., Orlandini, M., Orleanski, P., Ozel, F., Pacciani, L., Paltani, S., Papadakis, I., Papitto, A., Patruno, A., Pellizzoni, A., Petráček, V., Petri, J., Petrucci, P. O., Phlips, B., Picolli, L., Possenti, A., Psaltis, D., Rambaud, D., Reig, P., Remillard, R., Rodriguez, J., Romano, P., Romanova, M., Schanz, T., Schmid, C., Segreto, A., Shearer, A., Smith, A., Smith, P. J., Soffitta, P., Stergioulas, N., Stolarski, M., Stuchlik, Z., Tiengo, A., Torres, D., Török, G., Turolla, R., Uttley, P., Vaughan, S., Vercellone, S., Waters, R., Watts, A., Wawrzaszek, R., Webb, N., Wilms, J., Zampieri, L., Zezas, A., Ziolkowski, J., Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, and Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO)

Subjects
Event horizon, X-ray timing, Mission, 7. Clean energy, 01 natural sciences, neutron stars, T175 Industrial research. Research and development, BINARIES, Settore FIS/05 - Astronomia E Astrofisica, ALICE, SILICON DRIFT DETECTOR, Observatory, EQUATION, neutron star, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::Instrumentation and Methods for Astrophysics, Missions, X-ray timing, compact objects, black holes, neutron stars, compact objects, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, PROPORTIONAL COUNTER, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Active galactic nucleus, Cosmic Vision, X-ray astronomy, high time variability, Astrophysics::High Energy Astrophysical Phenomena, black holes, Missions, FOS: Physical sciences, 0103 physical sciences, OSCILLATIONS, Instrumentation and Methods for Astrophysics (astro-ph.IM), Supermassive black hole, 010308 nuclear & particles physics, Astronomy, CONSTRAINTS, Astronomy and Astrophysics, Galaxy, Black hole, Neutron star, Space and Planetary Science, QB460-466 Astrophysics, DISCOVERY, BLACK-HOLE, SUPERAGILE
Abstract

High-time-resolution X-ray observations of compact objects provide direct access to strong-field gravity, to the equation of state of ultra-dense matter and to black hole masses and spins. A 10 m^2-class instrument in combination with good spectral resolution is required to exploit the relevant diagnostics and answer two of the fundamental questions of the European Space Agency (ESA) Cosmic Vision Theme "Matter under extreme conditions", namely: does matter orbiting close to the event horizon follow the predictions of general relativity? What is the equation of state of matter in neutron stars? The Large Observatory For X-ray Timing (LOFT), selected by ESA as one of the four Cosmic Vision M3 candidate missions to undergo an assessment phase, will revolutionise the study of collapsed objects in our galaxy and of the brightest supermassive black holes in active galactic nuclei. Thanks to an innovative design and the development of large-area monolithic Silicon Drift Detectors, the Large Area Detector (LAD) on board LOFT will achieve an effective area of ~12 m^2 (more than an order of magnitude larger than any spaceborne predecessor) in the 2-30 keV range (up to 50 keV in expanded mode), yet still fits a conventional platform and small/medium-class launcher. With this large area and a spectral resolution of, 29 pages, 10 figures. Accepted for publication in Experimental Astronomy

Published
2012

4. GRB990123: multiwavelength afterglow study

Author

Maiorano, E., Masetti, N., Palazzi, E., Frontera, F., Grandi, P., Pian, E., Amati, L., Nicastro, L., Paolo Soffitta, Corsi, A., Piro, L., Antonelli, L. A., Costa, E., Feroci, M., Heise, J., and In T Zand, J. J. M.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract

We report on the BeppoSAX and multiwavelength data analysis of the afterglow of Gamma-Ray Burst (GRB) 990123. Mainly due to its exceptional brightness, this is the only source for which the Wide Field Cameras have allowed an early detection of the X-ray afterglow between about 20 and 60 min after the GRB trigger. Besides, again for the first time, high-energy emission from the afterglow was detected up to 60 keV. The backwards extrapolation of the afterglow decay smoothly reconnects with the late GRB emission, thus indicating that both are consistent with being produced by the same phenomenon. For the X-ray afterglow we found a power-law decay with index alpha_X = 1.46 +/- 0.04; the spectrum has a power-law shape with photon index Gamma about 2. An extensive set of multiwavelength observations on the afterglow, collected from the literature and made during the BeppoSAX pointing, allowed constructing a Spectral Flux Distribution. We performed an analysis of the GRB afterglow emission in the context of the "fireball" model., 4 pages, 2 figures, 1 table. Poster presented at the 4th Workshop Gamma-Ray Bursts in the Afterglow Era, Rome,18-22 October 2004. Editors: L. Piro, L. Amati, S. Covino, and B. Gendre. Il Nuovo Cimento, in press

Published
2005

7. Discovery of type-I X-ray bursts from GRS 1741.9-2853

Author

Cocchi, M., Angela Bazzano, Natalucci, L., Ubertini, P., Heise, J., Muller, J. M., and In T Zand, J. J. M.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

For the first time X-ray bursts have been detected from a sky position consistent with the one of GRS 1741.9-2853, a GRANAT transient source located only ~10' from the Galactic Centre. A total of 3 bursts have been observed by the Wide Field Cameras telescopes on board BeppoSAX during a monitoring observation of the Sgr A region in August-September 1996. The characteristics of the events are consistent with type-I bursts, thus identifying the source as a likely low-mass X-ray binary containing a neutron star. Evidence of photospheric radius expansion due to super-Eddington luminosity is present in one of the observed bursts, thus leading to an estimate og the source distance (~8 kpc)., 4 pages, 3 figures. Accepted for publication in A&A Letters

Published
1999

8. Long term BeppoSAX-WFC monitoring of GRS 1758-258

Author

Cocchi, M., Smith, J. M. S., Muller, J. M., Angela Bazzano, Natalucci, L., Ubertini, P., Heise, J., and In T Zand, J. J. M.

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

Following a series of deep observations of the Galactic Bulge region performed with the Wide Field Cameras on board BeppoSAX, it has been possible to study throughout a long time period a number of persistent X-ray sources. We report on the behaviour of GRS 1758-258, an X-ray binary suggested as a black hole candidate on the basis of its timing and spectral characteristics. The source has been monitored for almost 2 years since August 1996; preliminary results of the data analysis are shown hereafter., 4 pages, 3 figures, proc. 3rd INTEGRAL Workshop - Taormina 1998

Published
1999

9. A new X-ray outburst in the globular cluster NGC 6440: SAX J1748.9-2021

Author

In T Zand, J. J. M., Verbunt, F., Strohmayer, T. E., Angela Bazzano, Cocchi, M., Heise, J., Kerkwijk, M. H., Muller, J. M., Natalucci, L., Smith, M. J. S., and Ubertini, P.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

For the second time in 27 years a bright transient X-ray source has been detected coincident with the globular cluster NGC 6440. It was found to be active in August, 1998, with the Wide Field Camera and the narrow field instruments on the BeppoSAX spacecraft, and with the All-Sky Monitor and the Proportional Counter Array on the RossiXTE spacecraft. Four X-ray bursts were detected, at least one of which shows the characteristics of a thermonuclear flash on a neutron star, in analogy with some ~20 optically identified low-mass X-ray binaries. The broad-band spectrum is hard as is common among low-mass X-ray binaries of lower luminosity (>~10^37 erg/s) and can be explained by a Comptonized model. During the burst the >30 keV emission brightened, consistent with part of the burst emission being Compton up scattered within ~10^11 cm., 10 pages, accepted for publication in A&A

Published
1999
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10. Broad-band X-ray measurements of GS 1826-238

Author

In T Zand, J. J. M., Heise, J., Kuulkers, E., Angela Bazzano, Cocchi, M., and Ubertini, P.

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

The broad band X-ray spectrum of the low-mass X-ray binary (LMXB) GS1826-238 was measured with the narrow-field instruments on BeppoSAX on April 6 and 7, 1997. The spectrum is consistent with the Comptonization of a 0.6 keV thermal spectrum by a hot cloud of temperature equivalent kT=20 keV. During the observation two type I X-ray bursts were detected. From the bursts an upper limit to the distance could be derived of 8 kpc. Combined with an elsewhere determined lower limit of 4 kpc this implies a persistent X-ray luminosity between 3.5 X 10^36 and 1.4 X 10^37 erg/s which is fairly typical for a LMXB X-ray burster. The accurate determination of the energetics of the two bursts and the persistent emission confirm results with the Wide Field Cameras on BeppoSAX in a narrower bandpass (Ubertini et al. 1999). Comparison with independent X-ray measurements taken at other times indicates that GS 1826-238 since its turn-on in 1988 is a rather stable accretor, which is in line with the strong regularity of type I X-ray bursts.

Published
1999
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11. BeppoSAX follow-up search for the X-ray afterglow of GRB970111

Author

Feroci, M., Antonelli, L. A., Guainazzi, M., Muller, J. M., Enrico Costa, Piro, L., Heise, J., In T Zand, J. J. M., Frontera, F., Dal Flume, D., Nicastro, L., Orlandini, M., Palazzi, E., Zavattini, G., Giommi, P., Parmar, A. N., Owens, A., Castro-Tirado, A. J., Maccarone, M. C., and Butler, R. C.

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

The BeppoSAX satellite has recently opened a new way towards the solution of the long standing gamma-ray bursts' (GRBs) enigma, providing accurate coordinates few hours after the event thus allowing for multiwavelength follow-up observational campaigns. The BeppoSAX Narrow Field Instruments observed the region of sky containing GRB970111 16 hours after the burst. In contrast to other GRBs observed by BeppoSAX no bright afterglow was unambiguously observed. A faint source (1SAXJ1528.1+1937) is detected in a position consistent with the BeppoSAX Wide Field Camera position, but unconsistent with the IPN annulus. Whether 1SAXJ1528.1+1937 is associated with GRB970111 or not, the X-ray intensity of the afterglow is significantly lower than expected, based on the properties of the other BeppoSAX GRB afterglows. Given that GRB970111 is one of the brightest GRBs observed, this implies that there is no obvious relation between the GRB gamma-ray peak flux and the intensity of the X-ray afterglow., Comment: 5 pages, LaTeX A&A style, 3 postscript figures; A&A Letters accepted

Published
1998
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12. Detection of X-ray bursts in the globular cluster NGC 6652

Author

In T Zand, J. J. M., Verbunt, F., Heise, J., Muller, J. M., Angela Bazzano, Cocchi, M., Natalucci, L., and Ubertini, P.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Two type I X-ray bursts were detected from a position consistent with the transient X-ray source in NGC 6652 with the Wide Field Camera of the BeppoSAX satellite, strongly suggesting that this transient is a neutron star. Our detection brings to ten the number of X-ray sources in globular clusters in which a type I X-ray burst has been seen, out of twelve known bright sources. The statistical evidence that the fraction of low-mass X-ray binaries which contain a black hole accretor is smaller in globular clusters than in the galactic disk is suggestive, but as yet not compelling., Comment: Published in A&A, 1998, vol. 329, L37; 5 pages, 3 figures

Published
1997
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14. Prompt and afterglow emission from the x-ray-rich GRB 981226 observed with bepposax

Author

Frontera, F., Antonelli, L. A., Amati, L., Montanari, E., Enrico Costa, Dal Fiume, D., Giommi, P., Feroci, M., Gennaro, G., Heise, J., Masetti, N., Muller, J. M., Nicastro, L., Orlandini, M., Palazzi, E., Pian, E., Piro, L., Soffitta, P., Stornelli, M., In T Zand, J. J. M., Frail, D. A., Kulkarni, S. R., and Vietri, M.

15. The orbital period of the recurrent X-ray transient in Terzan 6

Author

In T Zand, J. J. M., Bazzano, A., Cocchi, M., Cornelisse, R., Heise, J., Kuiper, L., Kuulkers, E., Markwardt, C. B., Muller, J. M., Lorenzo Natalucci, Smith, M. J. S., Strohmayer, T. E., Ubertini, P., and Verbunt, F.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Four or five new outbursts were detected of the bright X-ray transient GRS 1747-312 in the globular cluster Terzan 6 between 1996 and 1999, through monitoring campaigns with the Wide Field Cameras (WFCs) on BeppoSAX and the Proportional Counter Array (PCA) on RossiXTE. This is the first time that the source is seen to exhibit recurrent outbursts after the discovery in September 1990 with ART-P on Granat. Three target-of-opportunity observations in 1998 and 1999, with the narrow-field instruments on BeppoSAX and the PCA, revealed one sharp drop in the flux which we identify as an eclipse of the compact X-ray source by the companion star. A detailed analysis of WFC data identifies further eclipses and we measure the orbital period at 12.360+/-0.009 hr. This is consistent with an identification as a low-mass X-ray binary, as suggested already by the association with a globular cluster. The eclipse duration is 0.72+/-0.06 hr. This implies that the inclination angle is larger than 74 deg. The 0.1-200 keV unabsorbed peak luminosity is 7X10^36 erg/s. The nature of the compact object is unclear., replaced with accepted version

18. X/gamma-ray measurements of the faint GRB 020321

Author

In T Zand, J. J. M., Kuiper, L., Heise, J., Amati, L., Costa, E., Feroci, M., Frontera, F., Gandolfi, G., Luciano Nicastro, Piro, L., Rodriguez-Pascual, P., Santos-Lleo, M., and Schartel, N.

21. BeppoSAX observations of the nearby low-mass X-ray binary and fast transient SAX J1819.3-2525

Author

In T Zand, J. J. M., Kuulkers, E., Angela Bazzano, Cornelisse, R., Cocchi, M., Heise, J., Muller, J. M., Natalucci, L., Smith, M. J. S., and Ubertini, P.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

SAX J1819.3-2525 is a nearby X-ray transient which exhibited a fast and large X-ray outburst on Sep. 15, 1999 (Smith et al. 1999). The Wide Field Cameras and the Narrow Field Instruments (NFI) on board BeppoSAX observed SAX J1819.3-2525 at various stages of its activity before that, in the spring and fall of 1999. The fluxes range between 0.012 and 0.3 Crab units (2-10 keV). The NFI observation is unique because it is the longest semi-continuous observation of SAX J1819.3-2525 so far, and it offers a study of the spectrum at a relatively high resolution of 8% full width at half maximum at 6 keV. We discuss the observations with emphasis on the X-ray spectrum. A strong Fe-K emission line was detected in SAX J1819.3-2525 with an equivalent width between 0.3 and 1 keV. The line energy is up to 6.85 +/- 0.02 keV and suggests the presence of highly ionized iron. We identify this as fluorescent emission from a photo-ionized plasma. The continuum spectrum is typical for a low-mass X-ray binary in which emission from an accretion disk corona plays an important role. There is no sign of an eclipse or periodic signal due to the binary orbit in this exposure, despite the fact that the twin jets seen at radio wavelengths suggest a high inclination angle., 8 pages, accepted for publication in A&A Main Journal

23. Observations of Eddington-limited type-I X-ray bursts from 4U 1812-12

Author

Cocchi, M., Angela Bazzano, Natalucci, L., Ubertini, P., Heise, J., Kuulkers, E., Muller, J. M., and In T Zand, J. J. M.

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

During more than 3 years (August 1996-October 1999) monitoring of a 40x40 degree sky region around the Galactic Centre by the Wide Field Cameras on board BeppoSAX, a total of 8 type-I bursts have been detected from a sky position consistent with that of 4U 1812-12, a likely neutron-star low-mass X-ray binary. We present the results of a detailed study of the bursts of 4U 1812-12, about 15 years after the last reported observations of X-ray bursts from this source (Murakami et al. 1983). Clear evidence for photospheric radius expansion due to Eddington-limited burst luminosity is present in most of the observed events, allowing an accurate estimate of the source distance (~4 kpc) and its burst parameters., Comment: 6 pages, 3 figures, accepted for publication in A&A main journal

24. The Chandra Galactic Bulge Survey

Author

Hynes, Robert I., Jonker, P. G., Bassa, C. G., Nelemans, G., Steeghs, D., Torres, M. A. P., Maccarone, T. J., Greiss, S., Clem, J., Dieball, A., Mikles, V. J., Britt, C. T., Gossen, L., Collazzi, A. C., Wijnands, R., In T Zand, J. J. M., Mendez, M., Rea, N., Kuulkers, E., Ratti, E. M., Haaften, L. M., Heinke, C., Ozel, F., Paul Groot, Verbunt, F., Kapteyn Astronomical Institute, and Astronomy

Abstract

The Chandra Galactic Bulge Survey (GBS) is a shallow but wide survey of two approximately 6x1 degree strips of the Galactic Bulge about a degree above and below the plane. The survey by design targets regions where extinction and crowding are manageable and optical counterparts are accessible to detailed follow-up. Our strategy is based on going deep enough to detect quiescent low-mass X-ray binaries (LMXBs), but no deeper in order to avoid an excess of cataclysmic variables (CVs), while covering a large area to maximize the numbers of recovered objects. The primary goals of the GBS are to test predictions of binary evolutionary models through number counts and period distributions of detected sources, and to greatly expand the sample of LMXBs suitable for detailed optical follow-up including mass determination. We have identified 1234 X-ray sources most with optical counterparts, and expect these to be divided evenly between quiescent LMXBs, magnetic CVs, and R CVn stars, with smaller numbers of other source types. We are actively pursuing multiwavelength follow-up including searches for optical, infrared, and ultraviolet counterparts, measurement of variability, and optical spectroscopy. I will summarize the goals of the project and highlight some of the results obtained so far. This work is supported by the National Science Foundation under Grant No. AST-0908789.

26. LOFT: A large observatory for x-ray timing

Author

Muleri, F., Feroci, M., Belloni, T., Braga, J., Campana, S., Courvousier, T., Hernanz, M., Hudec, R., Israel, G. L., Ray, P. S., Santangelo, A., Stella, L., Vacchi, A., Klis, M., Walton, D., Zdziarski, A., Alvarez, J. M., Argan, A., Baldazzi, G., Barbera, M., Bertuccio, G., Bonvicini, V., Bozzo, E., Campana, R., Collura, A., Cusumano, G., Del Monte, E., Den Herder, J. W., Di Cosimo, S., Di Persio, G., Evangelista, Y., Fuschino, F., Galvez, J. L., Giommi, P., Grassi, M., Guttridge, P., In ’t Zand, J. J. M., Kataria, D., Klochkov, D., Labanti, C., Lazzarotto, F., Malcovati, P., Marisaldi, M., Mastropietro, M., Mineo, T., Morelli, E., Orleanski, P., Phlips, B., Picolli, L., Rapisarda, M., Rashevski, A., Remillard, R., Rubini, A., Schanz, T., Segreto, A., Stolarski, M., Tenzer, C., Wawrzaszek, R., Wilson-Hodge, C., Winter, B., Zampa, G., Zampa, N., Alpar, A., Altamirano, D., Amati, L., Antonelli, L. A., Primo Attinà, Barbieri, C., Burderi, L., Bursa, M., Caliandro, G. A., Casella, P., Chakrabarty, D., Corongiu, A., Costa, E., Covino, S., Dall’osso, S., D’amico, F., Done, C., Di Salvo, T., Drago, A., Martino, D., Rosa, A., Donnarumma, I., Dovciak, M., Ertan, U., Falanga, M., Fender, R., Frontera, F., Ghandi, P., Gogus, E., Hermsen, W., Isern, J., Horak, J., Jonker, P., Kalemci, E., Kanbach, G., Karas, V., Kluzniak, W., Kokkotas, K., Krolik, J., Kylafis, N., Lattimer, J., Leahy, D., Maccarone, T., Mcclintock, J., Mendez, M., Mereghetti, S., Mignani, R., Miller, C., Mornick, S., Motta, S., Muñoz-Darias, T., Naletto, A., Orio, M., Orlandini, M., Ozel, F., Pacciani, L., Paltani, S., Papadakis, I., Papitto, A., Patruno, A., Pellizzoni, A., Possenti, A., Psaltis, D., Rea, N., Reig, P., Romano, P., Romanova, M., Shearer, A., Soffitta, P., Stergioulas, N., Stuchlik, Z., Tiengo, A., Torres, D., Turolla, R., Vercellone, S., Watts, A., Wood, K., Zampieri, L., Zane, S., Zezas, A., and Ziolkowski, J.

27. Optical and near-infrared follow-up observations of GRB980329

Author

Eliana Palazzi, Pian, E., Masetti, N., Nicastro, L., Vreeswijk, R., Galama, T. J., Groot, P., Frontera, F., Dellavalle, M., Lidman, C., Kouveliotou, C., Pizzichini, G., Paradijs, J., Pedersen, H., Mannucci, F., Di Martino, M., Diercks, A. H., Deutsch, E. W., Amati, L., Benetti, S., Castro-Tirado, A. J., Clasen, J., Costa, E., Dal Fiume, D., Falomo, R., Feroci, M., Fynbo, J., Heise, J., In T Zand, J. J. M., Piro, L., Robinson, C., Tornikoski, M., Valtaoja, E., Zapatero-Osorio, M. R., Lamb, D., Quashnock, J., and Den Berk, D.

29. The absorption properties of gamma-ray burst afterglows measured by BeppoSAX

Author

Owens, Alan, Guainazzi, M., Oosterbroek, T., Orr, A., Parmar, A. N., Costa, E., Feroci, M., Piro, L., Soffitta, P., Dal Fiume, D., Frontera, F., Eliana Palazzi, Pian, E., Heise, J., In T Zand, J. J. M., Maccarone, M. C., and Nicastro, L.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present an analysis of the X-ray absorption properties of 6 gamma-ray burst (GRB) afterglows measured with BeppoSAX. Between 8 hrs and 20 hrs after the initial GRB trigger, individual spectra can be described by a power-law with a photon index of ~2 and absorption marginally consistent with the galactic value. Taken collectively, the data are inconsistent with zero absorption at the >99.999 confidence level. The data are only marginally consistent with a distribution of column densities varying as the total galactic absorption in the direction of each of the bursts (chi^2 =9.6 for 6 degrees of freedom). The data are consistent with cosmological models in which GRB occur within host galaxies. By simultaneously fitting a power-law spectral model with absorption fixed at the galactic value and additional, redshifted, absorption to all 6 afterglow spectra, the best-fit average absorption within the host objects is found to be (1.01 ^0.28_0.51) 10^22 atom cm^-2. This value is compatible with the host galaxy column densities inferred from optical data for GRB970508, GRB971214 and GRB980329, supporting the hypothesis that GRB occur within heavily absorbed star forming regions of their host galaxies., 4 pages. 1 Figure. Accepted for publication in A&AL)

30. LOFT: A large observatory for x-ray timing

Author

Muleri, F., Feroci, M., Belloni, T., Braga, J., Campana, S., Courvousier, T., Hernanz, M., Hudec, R., Israel, G. L., Ray, P. S., Santangelo, A., Stella, L., Vacchi, A., Klis, M., Walton, D., Zdziarski, A., Alvarez, J. M., Argan, A., Baldazzi, G., Barbera, M., Bertuccio, G., Bonvicini, V., Bozzo, E., Campana, R., Collura, A., Cusumano, G., Del Monte, E., Den Herder, J. W., Di Cosimo, S., Di Persio, G., Evangelista, Y., Fuschino, F., Galvez, J. L., Giommi, P., Grassi, M., Guttridge, P., In T Zand, J. J. M., Kataria, D., Klochkov, D., Labanti, C., Lazzarotto, F., Malcovati, P., Marisaldi, M., Mastropietro, M., Mineo, T., Morelli, E., Orleanski, P., Phlips, B., Picolli, L., Rapisarda, M., Rashevski, A., Remillard, R., Rubini, A., Schanz, T., Segreto, A., Stolarski, M., Tenzer, C., Wawrzaszek, R., Wilson-Hodge, C., Winter, B., Zampa, G., Zampa, N., Alpar, A., Altamirano, D., Amati, L., Antonelli, L. A., Attinà, P., Barbieri, C., Burderi, L., Bursa, M., Caliandro, G. A., Casella, P., Chakrabarty, D., Corongiu, A., Costa, E., Covino, S., Dall Osso, S., D Amico, F., Done, C., Di Salvo, T., Drago, A., Martino, D., Rosa, A., Donnarumma, I., Dovciak, M., Ertan, U., Falanga, M., Fender, R., Frontera, F., Ghandi, P., Ersin Gogus, Hermsen, W., Isern, J., Horak, J., Jonker, P., Kalemci, E., Kanbach, G., Karas, V., Kluzniak, W., Kokkotas, K., Krolik, J., Kylafis, N., Lattimer, J., Leahy, D., Maccarone, T., Mcclintock, J., Mendez, M., Mereghetti, S., Mignani, R., Miller, C., Mornick, S., Motta, S., Muñoz-Darias, T., Naletto, A., Orio, M., Orlandini, M., Ozel, F., Pacciani, L., Paltani, S., Papadakis, I., Papitto, A., Patruno, A., Pellizzoni, A., Possenti, A., Psaltis, D., Rea, N., Reig, P., Romano, P., Romanova, M., Shearer, A., Soffitta, P., Stergioulas, N., Stuchlik, Z., Tiengo, A., Torres, D., Turolla, R., Vercellone, S., Watts, A., Wood, K., Zampieri, L., Zane, S., Zezas, A., Ziolkowski, J., Muleri, Fabio, Feroci, M., Belloni, T., Braga, J., Campana, S., Courvousier, T., Hernanz, M., Hudec, R., Israel, G. L., Ray, P. S., Santangelo, A., Stella, L., Vacchi, A., Van Der Klis, M., Walton, D., Zdziarski, A., Alvarez, J. M., Argan, A., Baldazzi, Giuseppe, Barbera, M., Bertuccio, G., Bonvicini, V., Bozzo, E., Campana, R., Collura, A., Cusumano, G., Del Monte, E., Den Herder, J. W., Di Cosimo, S., Di Persio, G., Evangelista, Y., Fuschino, F., Galvez, J. L., Giommi, P., Grassi, M., Guttridge, P., In'T Zand, J. J. M., Kataria, D., Klochkov, D., Labanti, C., Lazzarotto, F., Malcovati, P., Marisaldi, M., Mastropietro, M., Mineo, T., Morelli, E., Muleri, F., Orleanski, P., Phlips, B., Picolli, L., Rapisarda, M., Rashevski, A., Remillard, R., Rubini, A., Schanz, T., Segreto, A., Stolarski, M., Tenzer, C., Wawrzaszek, R., Wilson Hodge, C., Winter, B., Zampa, G., Zampa, N., Alpar, A., Altamirano, D., Amati, L., Antonelli, L. A., Attinà, P., Barbieri, C., Burderi, L., Bursa, M., Caliandro, G. A., Casella, P., Chakrabarty, D., Corongiu, A., Costa, E., Covino, S., Dall'Osso, S., D'Amico, F., Done, C., Di Salvo, T., Drago, A., De Martino, D., De Rosa, A., Donnarumma, I., Dovciak, M., Ertan, U., Falanga, M., Fender, R., Frontera, F., Ghandi, P., Gogus, E., Hermsen, W., Isern, J., Horak, J., Jonker, P., Kalemci, E., Kanbach, G., Karas, V., Kluzniak, W., Kokkotas, K., Krolik, J., Kylafis, N., Lattimer, J., Leahy, D., Maccarone, T., Mcclintock, J., Mendez, M., Mereghetti, S., Mignani, R., Miller, C., Mornick, S., Motta, S., Muñoz Darias, T., Naletto, A., Orio, M., Orlandini, M., Ozel, F., Pacciani, L., Paltani, S., Papadakis, I., Papitto, A., Patruno, A., Pellizzoni, A., Possenti, A., Psaltis, D., Rea, N., Reig, P., Romano, P., Romanova, M., Shearer, A., Soffitta, P., Stergioulas, N., Stuchlik, Z., Tiengo, A., Torres, D., Turolla, R., Vercellone, S., Watts, A., Wood, K., Zampieri, L., Zane, S., Zezas, A., and Ziolkowski, J.

Subjects
Multidisciplinary
Abstract

LOFT (Large area Observatory For x-ray Timing) is an innovative mission submitted in response to the Cosmic Vision "Call for a Medium-size mission opportunity for a launch in 2022" recently issued by ESA. LOFT is an ideal candidate for the next generation of (extremely) large experiments for X-ray timing dedicated to the study of the physics of compact objects and to the understanding of the behavior of matter in strong gravitational fields. Recent developments in the field of large area monolithic silicon detectors allowed us to reach an effective area ∼12 m2 (15 m2 goal), more than a order of magnitude larger that RXTE/PCA, in the energy range 2-30 keV (1-40 keV goal). This Large Area Detector (LAD) will have both high timing resolution (

31. Spectral states and transient behaviour of a sample of X-ray bursters observed by BeppoSAX

Author

Lorenzo Natalucci, Bazzano, A., Capitanio, F., Cocchi, M., Ubertini, P., and In T Zand, J. J. M.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

During observation campaigns of the Galactic Bulge region, BeppoSAX detected a total of 21 new X-ray bursters in about 6 years of operation. These sources are mostly transient and often feature a hard X-ray spectrum, extending up to ~ 200 keV. A hard spectrum is generally found in weak, relatively short outbursts. On the other hand two sources, SAX J1747.0-2853 and SAX J1750.8-2900, have been seen with soft X-ray transient behaviour. In both low/hard and high/soft state, a thermal component is observed at energies below \~10 keV and the spectra are compatible with the same model consisting of a blackbody or disk blackbody plus a hard or Comptonized component. Light curves are characterized by either weak, short flares or longer, high luminosity eruptions with exponential decay., 4 pages, 6 figures, to appear in Proceedings of the 5th INTEGRAL Workshop 'The INTEGRAL Universe', Munich, 16-20 February 2004. Accepted for publication in ESA SP-552

32. Turmoil on the accretion disk of GRO J1655-40

Author

Kuulkers, E., In T Zand, J. J. M., Cornelisse, R., Heise, J., Kong, A. K. H., Charles, P. A., Angela Bazzano, Cocchi, M., Natalucci, L., and Ubertini, P.

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

During the 1996/1997 outburst of the X-ray transient GRO J1655-40 the Wide Field Cameras onboard BeppoSAX observed the system with nearly continuous coverage during some stages of this outburst. On two occasions we find clear evidence for frequent dipping behaviour, characterized by several absorption dips occurring within one binary orbit. However, during preceding and following binary orbits there is no sign of such dips at the same range of orbital phases. We also collected light curves of absorption dips as seen with other X-ray instruments. Although the 65 dips that were collected occur preferably between orbital phases 0.68 and 0.92, there is evidence that the morphology of the material causing the dips is changing over just one binary orbit. The short duration (~minutes) and phasing of the dips are discussed in the framework of models where the stream from the companion star encounters a hot outer rim on the accretion disk., Comment: 15 pages, 10 figures, accepted for A&A, Main Journal

33. The LOFT perspective on neutron star thermonuclear bursts

Author

In T Zand, J. J. M., Altamirano, D., Ballantyne, D. R., Bhattacharyya, S., Brown, E. F., Cavecchi, Y., Chakrabarty, D., Chenevez, J., Cumming, A., Degenaar, N., Falanga, M., Galloway, D. K., Heger, A., José, J., Keek, L., Linares, M., Mahmoodifar, S., Malone, C. M., Méndez, M., Miller, M. C., Paerels, F. B. S., Juri Poutanen, Rózanska, A., Schatz, H., Serino, M., Strohmayer, T. E., Suleimanov, V. F., Thielemann, F. -K, Watts, A. L., Weinberg, N. N., Woosley, S. E., Yu, W., Zhang, S., Zingale, M., and Astronomy

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, Physics::Space Physics, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

This is a White Paper in support of the mission concept of the Large Observatory for X-ray Timing (LOFT), proposed as a medium-sized ESA mission. We discuss the potential of LOFT for the study of thermonuclear X-ray bursts on accreting neutron stars. For a summary, we refer to the paper., Comment: White Paper in Support of the Mission Concept of the Large Observatory for X-ray Timing

34. BeppoSAX detection and follow-up of GRB 980425

Author

Pian, E., Amati, L., Antonelli, L. A., Butler, R. C., Costa, E., Cusumano, G., Danziger, J., Feroci, M., Fiore, F., Frontera, F., Giommi, P., Masetti, N., Muller, J. M., Oosterbroek, T., Owens, A., Palazzi, E., Piro, L., Castro-Tirado, A., Coletta, A., Dal Fiume, D., Del Sordo, S., Heise, J., Nicastro, L., Mauro Orlandini, Parmar, A., Soffitta, P., Torroni, V., and In T Zand, J. J. M.

35. The Chandra Galactic Bulge Survey

Author

Hynes, Robert I., Jonker, P. G., Bassa, C. G., Dieball, A., Greiss, S., Maccarone, T. J., Gijs Nelemans, Steeghs, D., Torres, M. A. P., Britt, C. T., Clem, J. L., Gossen, L., Grindlay, J. E., Groot, P. J., Kuiper, L., Kuulkers, E., Mendez, M., Mikles, V. J., Ratti, E. M., Rea, N., Haaften, L. M., Wijnands, R., In T Zand, J. J. M., Astronomy, and Kapteyn Astronomical Institute

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The Chandra Galactic Bulge Survey (CGBS) is a shallow but wide survey of two approximately 6x1 degree strips of the Galactic Bulge about a degree above and below the plane. The survey by design targets regions where extinction and crowding are manageable and optical counterparts are accessible to detailed follow-up. Our strategy is based on going deep enough to detect quiescent low-mass X-ray binaries (LMXBs), but no deeper in order to avoid an excess of cataclysmic variables (CVs), while covering a large area to maximize the numbers of recovered objects. The primary goals of the CGBS are to test predictions of binary evolutionary models through number counts and period distributions of detected sources, and to greatly expand the sample of LMXBs suitable for detailed optical follow-up including mass determination. We have recovered over a thousand X-ray sources most with optical counterparts, and expect these to be divided evenly between quiescent LMXBs, magnetic CVs, and R CVn stars, with smaller numbers of other source types. We are actively pursuing multiwavelength follow-up including searches for optical, infrared, and ultraviolet counterparts, measurement of variability, and optical spectroscopy. So far we have identified about ten candidate LMXBs and CVs and a few other unusual objects such as X-ray selected sdO and carbon stars, both likely products of binary evolution. This work is supported by the National Science Foundation under Grant No. AST-0908789.

36. Discovery of the X-ray transient SAX J1808.4-3658, a likely low-mass X-ray binary

Author

In T Zand, J. J. M., Heise, J., Muller, J. M., Angela Bazzano, Cocchi, M., Natalucci, L., and Ubertini, P.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract

We report the discovery of a fairly bright transient during observations with the Wide Field Cameras on board the BeppoSAX satellite in September 1996. It was detected at a peak intensity of 0.1 Crab (2 to 10 keV) and lasted between 6 and 40 days above a detection threshold of 2 mCrab. Two very bright type I X-ray bursts were detected from this transient in the same observations. These almost certainly identify this X-ray transient as a low-mass X-ray binary with a neutron star as compact component. The double-peaked time history of both bursts at high energies suggests a peak luminosity close to the Eddington limit. Assuming this to be true implies a distance to this object of 4 kpc., Comment: 4 pages, 4 figures, published in A&A March II 1998 issue

37. Multiwavelength study of GRB 020410

Author

Nicastro, L., In T Zand, J. J. M., Heise, J., Mazets, E., Castro-Tirado, A., Gorosabel, J., Lorenzo Amati, Frontera, F., Costa, E., Feroci, M., Piro, L., and Pian, E.

39. Radio localization of IGR J16597-3704, a candidate neutron star X-ray binary undergoing an outburst in NGC 6256

Author

Tetarenko, A. J., Bahramian, A., Sivakoff, G. R., Heinke, C. O., Shaw, A. W., Wijnands, R., Degenaar, N., Russell, T. D., Miller-Jones, J. C. A., Plotkin, R. M., Tudor, V., Homan, J., Kuulkers, E., Chakrabarty, D., Chomiuk, L., Strader, J., Evangelia Tremou, Kennea, J. A., Altamirano, D., In T Zand, J. J. M., Deller, A., Maccarone, T. J., Rivera-Sandoval, L., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Abstract

We report follow-up VLA radio observations of NGC 6256, the globular cluster hosting the newly detected X-ray transient IGR J16597-3704 (ATel #10880, #10881).

40. BeppoSAX follow-up search for the X-ray afterglow of GRB970111

Author

Feroci, M., Antonelli, L. A., Guainazzi, M., Muller, J. M., Costa, E., Piro, L., In T Zand, J. J. M., Frontera, F., Dal Fiume, D., Nicastro, L., Orlandini, M., Palazzi, E., Zavattini, G., Giommi, P., Parmar, A. N., Owens, A., Castro-Tirado, A. J., Maccarone, M. C., and Reginald Butler

41. SAX J1810.8-2609: AN X-Ray Bursting Transient

Author

Cocchi, M., Bazzano, A., Lorenzo Natalucci, Ubertini, P., Heise, J., Muller, J. M., Smith, M. J., and In T Zand, J. J. M.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We report on the BeppoSAX/WFC observation of a strong type-I X-ray burst from the recently discovered transient source SAX J1810.8-2609. The observed event showed evidence of photospheric radius expansion due to super-Eddington burst luminosity. Burst detection identifies the source as a probable low-mass X-ray binary harbouring a neutron star., 4 pages, 3 figures, proc. 3rd INTEGRAL Workshop - Taormina 1998

43. On the enhanced X-ray emission from SGR 1900+14 after the August 27th giant flare

Author

Ünal Ertan, M. A. Alpar, Van den Heuvel, E. P. J., Wijers, R. A. M. J., and In 't Zand, J. J. M.

Subjects
Physics, Nuclear and High Energy Physics, Photon, Gamma ray, Astronomy, Cosmic ray, Astrophysics, Electromagnetic radiation, Atomic and Molecular Physics, and Optics, law.invention, Massless particle, QC Physics, Radiation pressure, law, Relaxation (physics), Flare
Abstract

We show that the giant flares of soft gamma ray repeaters ( E ∼10 44 erg) can push the inner regions of a fall-back disk out to larger radii by radiation pressure, while matter remains bound to the system for plausible parameters. The subsequent relaxation of this pushed-back matter can account for the observed enhanced X-ray emission after the August 27 th giant flare of SGR 1900+14.

Published
2004
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