Author: "Feroci, M." / Topic: astrophysics (astro-ph) - Searchworks@Jio Institute Digital Library Search Results

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56 results on '"Feroci, M."'

1. The AGILE Mission

Author: Tavani M, Barbiellini G, Argan A, Boffelli F, Bulgarelli A, Caraveo P, Cattaneo PW, Chen AW, Cocco V, Costa E, Del Monte E, De Paris G, Di Cocco G, Di Persio G, Donnarumma I, Evangelista Y, Feroci M, Ferrari A, Fiorini M, Fornari F, Fuschino F, Froysland T, Frutti M, Galli M, Gianotti F, Giuliani A, Labanti C, Lapshov I, Lazzarotto F, Liello F, Lipari P, Longo F, Mattaini E, Marisaldi M, Mastropietro M, Mauri A, Mauri F, Mereghetti S, Morelli E, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Piano G, Picozza P, Pontoni C, Porrovecchio G, Prest M, Pucella G, Rapisarda M, Rappoldi A, Rossi E, Rubini A, Soffitta P, Traci A, Trifoglio M, Trois A, Vallazza E, Vercellone S, Vittorini V, Zambra A, Zanello D, Pittori C, Preger B, Santolamazza P, Verrecchia F, Giommi P, Colafrancesco S, Antonelli A, Cutini S, Gasparrini D, Stellato S, Fanari G, Primavera R, Tamburelli F, Viola F, Guarrera G, Salotti L, D'Amico F, Marchetti E, Crisconio M, Sabatini P, Annoni G, Alia S, Longoni A, Sanquerin R, Battilana M, Concari P, Dessimone E, Grossi R, Parise A, Monzani F, Artina E, Pavesi R, Marseguerra G, Nicolini L, Scandelli L, Soli L, Vettorello V, Zardetto E, Bonati A, Maltecca L, D'Alba E, Patane M, Babini G, Onorati F, Acquaroli L, Angelucci M, Morelli B, Agostara C, Cerone M, Michetti A, Tempesta P, D'Eramo S, Rocca F, Giannini F, Borghi G, Garavelli B, Conte M, Balasini M, Ferrario I, Vanotti M, Collavo E, Giacomazzo M., D'AMMANDO, FILIPPO, M., Tavani, G., Barbiellini, A., Argan, F., Boffelli, A., Bulgarelli, P., Caraveo, P. W., Cattaneo, A. W., Chen, V., Cocco, E., Costa, F., D'Ammando, E. D., Monte, G. D., Pari, G. D., Cocco, G. D., Persio, I., Donnarumma, Y., Evangelista, M., Feroci, A., Ferrari, M., Fiorini, F., Fornari, F., Fuschino, T., Froysland, M., Frutti, M., Galli, F., Gianotti, A., Giuliani, C., Labanti, I., Lapshov, F., Lazzarotto, F., Liello, P., Lipari, Longo, Francesco, E., Mattaini, M., Marisaldi, M., Mastropietro, A., Mauri, F., Mauri, S., Mereghetti, E., Morelli, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, G., Piano, P., Picozza, C., Pontoni, G., Porrovecchio, M., Prest, G., Pucella, M., Rapisarda, A., Rappoldi, E., Rossi, A., Rubini, P., Soffitta, A., Traci, M., Trifoglio, A., Troi, E., Vallazza, S., Vercellone, V., Vittorini, A., Zambra, D., Zanello, C., Pittori, B., Preger, P., Santolamazza, F., Verrecchia, P., Giommi, S., Colafrancesco, A., Antonelli, S., Cutini, D., Gasparrini, S., Stellato, G., Fanari, R., Primavera, F., Tamburelli, F., Viola, G., Guarrera, L., Salotti, F., D'Amico, E., Marchetti, M., Crisconio, P., Sabatini, G., Annoni, S., Alia, A., Longoni, R., Sanquerin, M., Battilana, P., Concari, E., Dessimone, R., Grossi, A., Parise, F., Monzani, E., Artina, R., Pavesi, G., Marseguerra, L., Nicolini, L., Scandelli, L., Soli, V., Vettorello, E., Zardetto, A., Bonati, L., Maltecca, E., D'Alba, M., Patane, G., Babini, F., Onorati, L., Acquaroli, M., Angelucci, B., Morelli, C., Agostara, M., Cerone, A., Michetti, P., Tempesta, S., D'Eramo, F., Rocca, F., Giannini, G., Borghi, B., Garavelli, M., Conte, M., Balasini, I., Ferrario, M., Vanotti, E., Collavo, M., Giacomazzo, Tavani M, Barbiellini G, Argan A, Boffelli F, Bulgarelli A, Caraveo P, Cattaneo PW, Chen AW, Cocco V, Costa E, DAmmando F, Del Monte E, De Paris G, Di Cocco G, Di Persio G, Donnarumma I, Evangelista Y, Feroci M, Ferrari A, Fiorini M, Fornari F, Fuschino F, Froysland T, Frutti M, Galli M, Gianotti F, Giuliani A, Labanti C, Lapshov I, Lazzarotto F, Liello F, Lipari P, Longo F, Mattaini E, Marisaldi M, Mastropietro M, Mauri A, Mauri F, Mereghetti S, Morelli E, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Piano G, Picozza P, Pontoni C, Porrovecchio G, Prest M, Pucella G, Rapisarda M, Rappoldi A, Rossi E, Rubini A, Soffitta P, Traci A, Trifoglio M, Trois A, Vallazza E, Vercellone S, Vittorini V, Zambra A, Zanello D, Pittori C, Preger B, Santolamazza P, Verrecchia F, Giommi P, Colafrancesco S, Antonelli A, Cutini S, Gasparrini D, Stellato S, Fanari G, Primavera R, Tamburelli F, Viola F, Guarrera G, Salotti L, D'Amico F, Marchetti E, Crisconio M, Sabatini P, Annoni G, Alia S, Longoni A, Sanquerin R, Battilana M, Concari P, Dessimone E, Grossi R, Parise A, Monzani F, Artina E, Pavesi R, Marseguerra G, Nicolini L, Scandelli L, Soli L, Vettorello V, Zardetto E, Bonati A, Maltecca L, D'Alba E, Patane M, Babini G, Onorati F, Acquaroli L, Angelucci M, Morelli B, Agostara C, Cerone M, Michetti A, Tempesta P, D'Eramo S, Rocca F, Giannini F, Borghi G, Garavelli B, Conte M, Balasini M, Ferrario I, Vanotti M, Collavo E, and Giacomazzo M
Subjects: Agile, Active galactic nucleus, gamma and X ray detection, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, satellite, FOS: Physical sciences, Astrophysics, High Energy Gamma-ray Astronomy, Pulsar, astro-ph, Angular resolution, media_common, Physics, Calorimeter (particle physics), Astrophysics (astro-ph), Detector, AGILE satellite, Detectors, Astronomy and Astrophysics, Universe, Supernova, Space and Planetary Science, Orbit (dynamics), instrumentation: detectors – techniques: high angular resolution – techniques: image processing – gamma rays: observations – X-rays: general
Abstract: AGILE is an Italian Space Agency mission dedicated to the observation of the gamma-ray Universe. The AGILE very innovative instrumentation combines for the first time a gamma-ray imager (sensitive in the energy range 30 MeV - 50 GeV), a hard X-ray imager (sensitive in the range 18-60 keV) together with a Calorimeter (sensitive in the range 300 keV - 100 MeV) and an anticoincidence system. AGILE was successfully launched on April 23, 2007 from the Indian base of Sriharikota and was inserted in an equatorial orbit with a very low particle background. AGILE provides crucial data for the study of Active Galactic Nuclei, Gamma-Ray Bursts, pulsars, unidentified gamma-ray sources, Galactic compact objects, supernova remnants, TeV sources, and fundamental physics by microsecond timing. An optimal angular resolution (reaching 0.1-0.2 degrees in gamma-rays, 1-2 arcminutes in hard X-rays) and very large fields of view (2.5 sr and 1 sr, respectively) are obtained by the use of Silicon detectors integrated in a very compact instrument. The paper describes the AGILE Mission and its space and ground segments., 20 pages, 26 figures. submitted to Astron. & Astrophys
Published: 2009

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. Inner accretion disk disappearance during a radio flare in GRS 1915+105

Author: Feroci, M., Matt, G., Pooley, G., Enrico Costa, Tavani, M., Belloni, T., Feroci, M, Matt, Giorgio, Pooley, G, Costa, E, Tavani, M, and Belloni, T.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: Simultaneous X-ray (BeppoSAX, 0.1-300 keV) and radio (Ryle Telescope, 15 GHz) observations of the superluminal galactic source GRS 1915+105 in high flux state were carried out starting October 1996. Here we present the simultaneous radio/X-ray light curves of the flare event and the spectral and timing analysis of the relevant BeppoSAX data. We obtain evidence for a temporary disappearance and subsequent restoring of the inner portion of the accretion disk during the flare from the spectral analysis of the X-ray data. We find a variable power law photon index positively correlated to the variability of the exponential cut-off energy. In addition, frequency and intensity variations of a $\sim$4-5~Hz quasi-periodic oscillation (QPO) are detected during the same time interval. The centroid frequency of the QPO is found to be correlated to the spectral power law photon index, and to the X-ray flux from the disk and the high energy flux from the power law. These observational results are discussed in the framework of the disk-instability model proposed for this source., 10 pages, 9 figures; A&A Main Journal in press
Published: 1999

4. The search for Muon neutrinos from northern hemisphere gamma-ray bursts with AMANDA

Author: Achterberg, A, Ackermann, M, Adams, J, Ahrens, J, Andeen, K, Auffenberg, J, Bahcall, JN, Bai, X, Baret, B, Barwick, SW, Bay, R, Beattie, K, Becka, T, Becker, JK, Becker, K-H, Berghaus, P, Berley, D, Bernardini, E, Bertrand, D, Besson, DZ, Blaufuss, E, Boersma, DJ, Bohm, C, Bolmont, J, Boeser, S, Botner, O, Bouchta, A, Braun, J, Burgess, C, Burgess, T, Castermans, T, Chirkin, D, Christy, B, Clem, J, Cowen, DF, D'Agostino, MV, Davour, A, Day, CT, De Clercq, C, Demiroeres, L, Descamps, F, Desiati, P, DeYoung, T, Diaz-Velez, JC, Dreyer, J, Dumm, JP, Duvoort, MR, Edwards, WR, Ehrlich, R, Eisch, J, Ellsworth, RW, Evenson, PA, Fadiran, O, Fazely, AR, Filimonov, K, Foerster, MM, Fox, BD, Franckowiak, A, Gaisser, TK, Gallagher, J, Ganugapati, R, Geenen, H, Gerhardt, L, Goldschmidt, A, Goodman, JA, Gozzini, R, Griesel, T, Gross, A, Grullon, S, Gunasingha, RM, Gurtner, M, Hallgren, A, Halzen, F, Han, K, Hanson, K, Hardtke, D, Hardtke, R, Hart, JE, Hasegawa, Y, Hauschildt, T, Hays, D, Heise, J, Helbing, K, Hellwig, M, Herquet, P, Hill, GC, Hodges, J, Hoffman, KD, Hommez, B, Hoshina, K, Hubert, D, Hughey, B, Hulth, PO, Huess, J-P, Hultqvist, K, Hundertmark, S, Inaba, M, Ishihara, A, Jacobsen, J, Japaridze, GS, Johansson, H, Jones, A, Joseph, JM, Kampert, K-H, Kappes, A, Karg, T, Karle, A, Kawai, H, Kelley, JL, Kitamura, N, Klein, SR, Klepser, S, Kohnen, G, Kolanoski, H, Pke, LK, Kowalski, M, Kowarik, T, Krasberg, M, Kuehn, K, Labare, M, Landsman, H, Leich, H, Leier, D, Liubarsky, I, Lundberg, J, Luenemann, J, Madsen, J, Mase, K, Matis, HS, McCauley, T, McParland, CP, Meli, A, Messarius, T, Meszaros, P, Miyamoto, H, Mokhtarani, A, Montaruli, T, Morey, A, Morse, R, Movit, SM, Muenich, K, Nahnhauer, R, Nam, JW, Niessen, P, Nygren, DR, Oegelman, H, Olivas, A, Patton, S, Pena-Garay, C, De Los Heros, CP, Piegsa, A, Pieloth, D, Pohl, AC, Porrata, R, Pretz, J, Price, PB, Przybylski, GT, Rawlins, K, Razzaque, S, Resconi, E, Rhode, W, Ribordy, M, Rizzo, A, Robbins, S, Roth, P, Rott, C, Rutledge, D, Ryckbosch, D, Sander, H-G, Sarkar, S, Schlenstedt, S, Schmidt, T, Schneider, D, Seckel, D, Semburg, B, Seo, SH, Seunarine, S, Silvestri, A, Smith, AJ, Solarz, M, Song, C, Sopher, JE, Spiczak, GM, Spiering, C, Stamatikos, M, Stanev, T, Steffen, P, Stezelberger, T, Stokstad, RG, Stoufer, MC, Stoyanov, S, Strahler, EA, Straszheim, T, Sulanke, K-H, Sullivan, GW, Sumner, TJ, Taboada, I, Tarasova, O, Tepe, A, Thollander, L, Tilav, S, Tluczykont, M, Toale, PA, Turcan, D, Van Eijndhoven, N, Vandenbroucke, J, Van Overloop, A, Viscomi, V, Voigt, B, Wagner, W, Walck, C, Waldmann, H, Walter, M, Wang, Y-R, Wendt, C, Wiebusch, CH, Wikstroem, G, Williams, DR, Wischnewski, R, Wissing, H, Woschnagg, K, Xu, XW, Yodh, G, Yoshida, S, Zornoza, JD, Boer, M, Cline, T, Crew, G, Feroci, M, Frontera, F, Hurley, K, Lamb, D, Rau, A, Rossi, F, Ricker, G, and Von Kienlin, A
Subjects: Antarctic Muon And Neutrino Detector Array, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Astrophysics, 01 natural sciences, Gamma rays: bursts, Neutrinos, 0103 physical sciences, Muon neutrino, 010306 general physics, 010303 astronomy & astrophysics, Physics, Muon, Astrophysics (astro-ph), Order (ring theory), Astronomy and Astrophysics, Space and Planetary Science, Astronomia, High Energy Physics::Experiment, Neutrino, Gamma-ray burst, Energy (signal processing)
Abstract: We present the results of the analysis of neutrino observations by the Antarctic Muon and Neutrino Detector Array (AMANDA) correlated with photon observations of more than 400 gamma-ray bursts (GRBs) in the Northern Hemisphere from 1997 to 2003. During this time period, AMANDA's effective collection area for muon neutrinos was larger than that of any other existing detector. Based on our observations of zero neutrinos during and immediately prior to the GRBs in the dataset, we set the most stringent upper limit on muon neutrino emission correlated with gamma-ray bursts. Assuming a Waxman-Bahcall spectrum and incorporating all systematic uncertainties, our flux upper limit has a normalization at 1 PeV of E^2{\Phi}_{\nu} {\leq} 6.0 \times 10^{-9} GeV cm^{-2} s^{-1} sr^{-1}, with 90% of the events expected within the energy range of ~10 TeV to ~3 PeV. The impact of this limit on several theoretical models of GRBs is discussed, as well as the future potential for detection of GRBs by next generation neutrino telescopes. Finally, we briefly describe several modifications to this analysis in order to apply it to other types of transient point sources., Comment: 44 pages, 10 figures; submitted to Astrophysical Journal
Published: 2008

5. 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

6. A XMM-Newton View of the Soft Gamma-ray Repeater SGR 1806--20: Long Term Variability in the pre-Super Giant Flare Epoch

Author: Mereghetti, S., Tiengo, A., Esposito, P., Gotz, D., Stella, L., Israel, G. L., Rea, N., Feroci, M., Turolla, R., and Zane, S .
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: The low energy (, Revised version (several changes in text, figures and tables). Accepted for publication on The Astrophysical Journal
Published: 2005

7. The INTEGRAL view of the Soft Gamma-ray Repeater SGR 1806-20

Author: Gotz, D., Mereghetti, S., Mirabel, I. F., Hurley, K., Brandt, S., Lund, N., Ubertini, P., Del Santo, M., Costa, E., Feroci, M., Castro-Tirado, A., Gimenez, A., Atteia, J. -L., Boer, M., Cline, T., Frontera, F., Pizzichini, G., von Kienlin, A., Gougus, E., Kouveliotou, C., Finger, M., Thompson, C., Pedersen, H., and van der Klis, M.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: We present the results obtained by INTEGRAL on the Soft-Gamma Ray Repeater SGR 1806-20. In particular we report on the temporal and spectral properties of the bursts detected during a moderately active period of the source in September and October 2003 and on the search for quiescent emission., Comment: To appear in the proceedings (ESA-SP) of the 5th INTEGRAL Workshop, "The INTEGRAL UNIVERSE", Munich, 16-20 February 2004
Published: 2004
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8. X/gamma-ray measurements of the faint GRB 020321

Author: Zand, J. J. M. in 't, Kuiper, L., Heise, J., Amati, L., Costa, E., Feroci, M., Frontera, F., Gandolfi, G., Nicastro, L., Piro, L., Rodriguez-Pascual, P., Santos-Lleo, M., and Schartel, N.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: GRB 020321 is a faint GRB that received wide follow-up attention in X-rays (BeppoSAX/NFI, Chandra/ACIS-S, XMM-Newton), radio (ATCA) and optical (ESO, HST). We identify a weak X-ray afterglow by a combined study of the Chandra and XMM-Newton observations. Its decay index of 1.2 is typical for GRB afterglows. Inside the 4"-accurate error box there is a weak optical counterpart candidate with a much shallower decay index., 5 pages, 3 figures, to be published in Proc. "GRBs in the afterglow era: 3rd Rome workshop (2002)", eds. L. Piro, F. Frontera, N. Masetti, M. Feroci
Published: 2003

9. X-ray Astronomical Polarimetry in the XEUS Era

Author: Costa, E., Soffitta, P., Di Persio, G., Feroci, M., Pacciani, L., Rubini, A., Bellazzini, R., Brez, A., Baldini, L., Latronico, L., Omodei, N., and Spandre, G.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: X-ray Polarimetry is almost as old as X-ray Astronomy. Since the first discovery of X-ray sources theoretical analysis suggested that a high degree of linear polarization could be expected due either to the, extremely non thermal, emission mechanism or to the transfer of radiation in highly asymmetric systems. The actual implementation of this subtopic was, conversely, relatively deceiving. This is mainly due to the limitation of the conventional techniques based on the Bragg diffraction at 45deg, or on Thomson scattering around 90deg. Acually no X-ray Polarimeter has been launched since 25 years. Nevertheless the expectations from such measurement on several astrophysical targets including High and Low Mass X-Ray Binaries, isolated neutron Stars, Galactic and Extragalactic Black Holes is extremely attractive. We developed a new technique to measure the linear polarization of X-ray sources. It is based on the visualization of photoelectron tracks in a, finely subdivided, gas filled detector (micropattern). The initial direction of the photoelectron is derived and from the angular distribution of the tracks the amount and angle of polarization is computed. This technique can find an optimal exploitation in the focus of XEUS-1. Even in a very conservative configuration (basically the already existing prototype) the photoelectric polarimeter could perform polarimetry at % level on many AGNs. Further significant improvements can be expected from a technological development on the detector and with the use of XEUS-2 telescope., 6 pages, 7 pdf figures, Proceedindg of the Workshop: "XEUS - studying the evolution of the hot universe" held in Garching, March 11-13, 2002, eds. G. Hasinger, Th. Boller and A. Parmar, MPE report
Published: 2003

10. Study of the largest multiwavelength campaign of the microquasar GRS 1915+105

Author: Sanchez-Fernandez, C., Dhawan, V., Chaty, S., Grove, J. E., McCollough, M., Castro-Tirado, A. J., Mirabel, F., Kohno, K., Feroci, M., Casella, P., Trushkin, S. A., Castaneda, H., Rodriguez, J., Durouchoux, P., Swank, J., Ueda, Yoshihiro, Yamaoka, K., Ebisawa, Ken, Kotani, T., Inoue, Hajime, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-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), Pôle Astronomie du LESIA, and 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 Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris
Subjects: Physics, geography, Plateau, geography.geographical_feature_category, Photon, Infrared, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Flux, Astronomy and Astrophysics, Astrophysics, Power law, Space and Planetary Science, Magnitude (astronomy), Cutoff, Electronic band structure, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: 著者人数：20名, Accepted: 2002-02-06, 資料番号: SA1002392000
Published: 2002

11. A comparative study of the X-ray afterglow properties of optically bright and dark GRBs

Author: De Pasquale, M., Piro, L., Perna, R., Costa, E., Feroci, M., Gandolfi, G., Zand, J. in 't, Nicastro, L., Frontera, F., Antonelli, L. A., Fiore, F., and Stratta, G.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: We have examined the complete set of X-ray afterglow observations of dark and optically bright GRBs performed by BeppoSAX until February 2001. X-ray afterglows are detected in 90% of the cases. We do not find significant differences in the X-ray spectral shape, in particular no higher X-ray absorption in GRBs without optical transient (dark GRBs) compared to GRBs with optical transient (OTGRBs). Rather, we find that the 1.6-10 keV flux of OTGRBs is on average about 5 times larger than that of the dark GRBs. A K-S test shows that this difference is significant at 99.8% probability. Under the assumption that dark and OTGRB have similar spectra, this could suggest that the first are uncaught in the optical band because they are just faint sources. In order to test this hypothesis, we have determined the optical-to-X ray flux ratios of the sample. OTGRBs show a remarkably narrow distribution of flux ratios, which corresponds to an average optical-to-x spectral index 0.794\pm 0.054. We find that, while 75% of dark GRBs have flux ratio upper limits still consistent with those of OT GRBs, the remaining 25% are 4 - 10 times weaker in optical than in X-rays. The significance of this result is equal to or higher than 2.6 sigma. If this sub-population of dark GRBs were constituted by objects assimilable to OTGRBs, they should have shown optical fluxes higher than upper limits actually found. We discuss the possible causes of their behaviour, including a possible occurrence in high density clouds or origin at very high redshift and a connection with ancient, Population III stars., Comment: 19 pages, 5 figures. To be published in The Astrophysical Journal
Published: 2002
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12. The BeppoSAX View on the 2001 Reactivation of SGR 1900+14

Author: Feroci, M., Mereghetti, S., Costa, E., Zand, J. J. M. in 't, Soffitta, P., Cline, T., Duncan, R., Finger, M., Golenetskii, S. V., Hurley, K., Kouveliotou, C., Li, P., Mazets, E., Tavani, M., Thompson, C., and Woods, P.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: After a couple of years of quiescence, the soft gamma repeater SGR 1900+14 suddenly reactivated on 18 April 2001, with the emission of a very intense, long and modulated flare, only second in intensity and duration to the 27 August 1998 giant flare. BeppoSAX caught the large flare with its Gamma Ray Burst Monitor and with one of the Wide Field Cameras. The Wide Field Cameras also detected X-ray bursting activity shortly before the giant flare. A target of opportunity observation was started only 8 hours after the large flare with the Narrow Field Instruments, composed of two 60-ks long pointings. These two observations show an X-ray afterglow of the persistent SGR 1900+14 source, decaying with time according to a power law of index -0.6., 4 pages. To appear in "Neutron Stars in Supernova Remnants" (ASP Conference Proceedings), eds P. O. Slane and B. M. Gaensler
Published: 2001

13. GRB000615 in X-rays

Author: Nicastro, L., Cusumano, G., Antonelli, A., Amati, L., Frontera, F., Palazzi, E., Pian, E., Costa, E., Feroci, M., Piro, L., Zand, J. in 't, and Heise, J.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences
Abstract: GRB000615 was detected simultaneously by the BeppoSAX GRBM and WFC 1 with a localization uncertainty of 2' (error circle radius). X-ray emission was detected only in the 0.1-4 keV range during a NFI observation started about 10 hours after the trigger time. The positional and temporal analysis shows the presence of two sources, one of which may be related to the GRB., 3 pages, LaTeX, 4 PS figures, to appear in Procs. of the 2nd Workshop "Gamma-Ray Bursts in the Afterglow Era"
Published: 2001
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14. BeppoSAX Observations of the Soft Gamma-Ray Repeater SGR 1806-20

Author: Mereghetti, S., Cremonesi, D., Feroci, M., and Tavani, M.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: We have observed with the BeppoSAX satellite the quiescent counterpart of the Soft Gamma-ray Repeater SGR 1806-20. Observations performed in October 1998 and in March 1999 showed that this pulsar continued its long term spin-down trend at an average rate of ~8 10e-11 s/s while its flux and spectrum remained remarkably constant between the two observations, despite the soft gamma-ray bursting activity that occurred in this period. We also reanalyzed archival ASCA data, that when compared with the new BeppoSAX observations, show evidence for a long term variation in luminosity., 5 pages, latex, 2 figures, Accepted for publication on Astronomy and Astrophysics
Published: 2000

15. ISO detection of a 60micron source near GRB970508

Author: Hanlon, L., Laureijs, R. J., Metcalfe, L., McBreen, B., Altieri, B., Castro-Tirado, A., Claret, A., Costa, E., Delaney, M., Feroci, M., Frontera, F., Galama, T., Gorosabel, J., Groot, P., Heise, J., Kessler, M., Kouveliotou, C., Palazzi, E., van Paradijs, J., Piro, L., and Smith, N.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The Infrared Space Observatory observed the field of the $\gamma$--ray burst GRB 970508 with the CAM and PHT instruments on May 21 and 24, 1997 and with PHT in three filters in November 1997. A source at 60 $\mu$m (flux in May of $66\pm 10$ mJy) was detected near the position of the host galaxy of this $\gamma$--ray burst. The source was detected again in November 1997, at a marginally lower flux ($43\pm 13$ mJy). A Galactic cirrus origin and a stellar origin for the emission can be ruled out on the basis of the infrared colours. The marginal evidence for variability in the 60 $\mu$m flux between May and November is not sufficient to warrant interpretation of the source as transient fireball emission. However, the infrared colours are physically reasonable if attributed to conventional dust emission from a single blackbody source. The probability of detecting a 60 $\mu$m by chance in a PHT beam down to a detection limit of 50 mJy is $\sim 5\times 10^{-3}$. If the source is at the redshift of the host galaxy of the $\gamma$--ray burst the fluxes and upper limits at wavelengths from 12 $\mu$m to 170 $\mu$m indicate it is an ultraluminous infrared galaxy (L$_{\rm ir} \sim 2\times 10^{12}$ L$_{\sun}$). The star formation rate is estimated to be several hundred solar masses per year, depending significantly on model-dependent parameters. If this source is associated with the host galaxy of GRB 970508, progenitor models which associate GRBs with star-forming regions are favoured., Comment: Accepted for publication in Astronomy & Astrophysics
Published: 2000

16. Integrating the BeppoSAX Gamma-Ray Burst Monitor into the 3rd Interplanetary Network

Author: Hurley, K., Feroci, M., Cinti, M. -N., Costa, E., Preger, B., Frontera, F., Fiume, D. Dal, Orlandini, M., Amati, Nicastro, L., Heise, J., Zand, J. J. M. in 't, and Cline, T.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: We have added the BeppoSAX Gamma-Ray Burst Monitor to the 3rd Interplanetary Network of burst detectors. We analyze 16 bursts whose positions are known to good accuracy from measurements at other wavelengths. We show that there is excellent agreement between the Ulysses/BeppoSAX triangulation annuli and the known positions of these events, and that these annuli can in many cases provide useful constraints on the positions of bursts detected by the BeppoSAX Wide Field Camera and Narrow Field Instruments., 16 pages, 18 figures, submitted to the Astrophysical Journal
Published: 1999

17. The afterglow, the redshift, and the extreme energetics of the gamma-ray burst 990123

Author: Kulkarni, S. R., Djorgovski, S. G., Odewahn, S. C., Bloom, J. S., Gal, R. R., Koresko, C. D., Harrison, F. A., Lubin, L. M., Armus, L., Sari, R., Illingworth, G. D., Kelson, D. D., Magee, D. K, van Dokkum, P. G., Frail, D. A., Mulchaey, J. S., Malkan, M. A., McLean, I. S., Teplitz, H. I., Koerner, D., Kirkpatrick, D., Kobayashi, N., Yadigaroglu, I. A., Halpern, J., Piran, T., Goodrich, R., Chaffee, F., Feroci, M., and Costa, E.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Afterglow, or long-lived emission, has now been detected from about a dozen well-positioned gamma-ray bursts. Distance determinations made by measuring optical emission lines from the host galaxy, or absorption lines in the afterglow spectrum, place the burst sources at significant cosmological distances, with redshifts ranging from ~1--3. The energy required to produce the bright gamma-ray flashes is enormous: up to ~10^{53} erg or 10 percent of the rest mass energy of a neutron star, if the emission is isotropic. Here we present the discovery of the optical afterglow and the redshift of GRB 990123, the brightest well-localized GRB to date. With our measured redshift of >1.6, the inferred isotropic energy release exceeds the rest mass of a neutron star thereby challenging current theoretical models for the origin of GRBs. We argue that the optical and IR afterglow measurements reported here may provide the first observational evidence of beaming in a GRB, thereby reducing the required energetics to a level where stellar death models are still tenable., Revised version (27 Feb 99). 19 pages, 3 figures. Original version submitted to Nature 2/11/99. Uses macros reforder.sty and citmac.sty (supplied)
Published: 1999

18. The X-ray afterglow of the Gamma-ray burst of May 8, 1997: spectral variability and possible evidence of an iron line

Author: Piro, L., Costa, E., Feroci, M., Frontera, F., Amati, L., Fiume, D. Dal, Antonelli, L. A., Heise, J., Zand, J. in 't, Owens, A., Parmar, A. N., Cusumano, G., Vietri, M., and Perola, G. C.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: We report the possible detection (99.3% of statistical significance) of redshifted Fe iron line emission in the X-ray afterglow of Gamma-ray burst GRB970508 observed by BeppoSAX. Its energy is consistent with the redshift of the putative host galaxy determined from optical spectroscopy. The line disappeared about 1 day after the burst. We have also analyzed the spectral variability during the outburst event that characterizes the X-ray afterglow of this GRB. The spectrum gets harder during the flare, turning to steep when the flux decreases. The variability, intensity and width of the line indicate that the emitting region should have a mass approximately greater than 0.5 solar masses (assuming the iron abundance similar to its solar value), a size of about 3 times 10^15 cm, be distributed anisotropically, and be moving with sub-relativistic speed. In contrast to the fairly clean environment expected in the merging of two neutron stars, the observed line properties would imply that the site of the burst is embedded in a large mass of material, consistent with pre-explosion ejecta of a very massive star. This material could be related with the outburst observed in the afterglow 1 day after the GRB and with the spectral variations measured during this phase., Comment: To appear in The Astrophysical Journal Letters, AASTEX LateX, 2 PostScript figures
Published: 1999
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19. A Giant Outburst from SGR 1900+14 Observed with the BeppoSAX Gamma Ray Burst Monitor

Author: Feroci, M., Frontera, F., Costa, E., Amati, L., Tavani, M., Rapisarda, M., and Orlandini, M.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: We report the detection by the Gamma Ray Burst Monitor onboard BeppoSAX of the strongest and longest ever detected outburst from SGR 1900+14. Oscillations are detectable with a period of ~5.16 s for the entire duration of the event ~300 s. The temporal analysis reveals also a remarkable periodic substructure: after about 35 s from the event onset each 5.16-s pulse shows a pattern of four subpulses and a dip, each separated by ~1 s. Significant spectral variation is detected during the event and for each individual oscillation. The first and most intense part of the outburst is quite hard, and similar to what previously detected from the `March 5th event'. A hard non-thermal spectral component persists for ~200 s. SGR 1900+14 was proposed to be a strongly magnetized neutron star (B>10^14 G) undergoing violent instabilities by internal magnetic/crustal stresses. However, the onset of an apparent 1-s periodicity within the 5.16-s pulsations and the observed spectral properties show a complex behaviour that is not satisfactorily modelled yet., 16 pages, 3 figures, TeX uses aasms4.sty; ApJ Letters in press
Published: 1999
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20. The unusual afterglow of GRB 980326: evidence for the gamma-ray burst/supernova connection

Author: Bloom, J. S., Kulkarni, S. R., Djorgovski, S. G., Eichelberger, A. C., Cote, P., Blakeslee, J. P., Odewahn, S. C., Harrison, F. A., Frail, D. A., Filippenko, A. V., Leonard, D. C., Riess, A. G., Spinrad, H., Stern, D., Bunker, A., Dey, A., Stanford, S. A., Grossan, B., Perlmutter, S., Knop, R. A., Hook, I. M., and Feroci, M.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Cosmic gamma-ray bursts (GRBs) have been firmly established as one of the most powerful phenomena in the Universe, releasing electromagnetic energy approaching the rest-mass energy of a neutron star in a few seconds. The two currently popular models for GRB progenitors are the coalescence of two compact objects (such as neutron stars or black holes) or collapse of a massive star. An unavoidable consequence of the latter model is that a bright supernovae should accompany the GRB. The emission from this supernova competes with the much brighter afterglow produced by the relativistic shock that gives rise to the GRB itself. Here we present evidence for an unusual light curve for GRB 980326 based on new optical observations. The transient brightened ~3 weeks after the burst to a flux sixty times larger than that extrapolated from the rapid decay seen at early time. Furthermore, the spectrum changed dramatically and became extremely red. We argue that the new source is the underlying supernova. If our hypothesis is true then this would be the first evidence for a supernova connection with GRBs at cosmological distances. We suggest that GRBs with long durations are associated with death of massive stars., Comment: Submitted to Nature (restricted embargo). Sixteen pages of TeX. Uses macros reforder.tex, citmac.tex and psfig.sty (included). Three Postscript figures
Published: 1999
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21. BeppoSAX observations of GRB970402

Author: Nicastro, L., Amati, L., Antonelli, L. A., Reginald Butler, Costa, E., Cusumano, G., Feroci, M., Frontera, F., Heise, J., Hurley, K., Muller, J. M., Owens, A., and Piro, L.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: GRB970402 is the fourth gamma-ray burst detected by BeppoSAX simultaneously in the Gamma Ray Burst Monitor (GRBM) and one of the two Wide Field Cameras (WFCs). A rapid pointing of the BeppoSAX Narrow Field Instruments (NFIs) 8 hours after the GRB led to the identification of an unknown weak X-ray source: 1SAX J1450.1-6920. Its position was approximately at the center of the 3 arcmin error circle derived from the WFC image. Both the Medium Energy (MECS, 2-10 keV) and Low Energy (LECS, 0.1-10 keV) concentrators detected the source. A follow-up observation performed 1.5 days later and lasting 54 ks showed that the source had faded almost to, but not below the detectability threshold. The flux decrease between the two observations was a factor ~= 2.5. 1SAX J1450.1-6920 was the second X-ray afterglow associated with a GRB. Searches promptly started at other wavelengths (optical, IR, radio) did not reveal any transient event within the 3 arcmin error circle., 4 pages, Latex, 3 PS figures, requires l-aa.sty, accepted for publication in Astronomy and Astrophysics Letters
Published: 1998

22. The Discovery of the Radio Afterglow From the Optically Dim Gamma-Ray Burst of March 29, 1998

Author: Taylor, G. B., Frail, D. A., Kulkarni, S. R., Shepherd, D. S., Feroci, M., and Frontera, F.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: We report on the discovery of a variable radio source, VLA J070238.0+385044, associated with the proposed x-ray counterpart, 1SAX J0702.6+3850 of GRB 980329. The source was monitored from one day after the burst to one month later at centimeter wavelengths (1.4, 4.9, 8.3 and 15 GHz; Very Large Array -- VLA), and in the 3-mm band (90 GHz; Owen Valley Radio Observatory -- OVRO). Based on its variability, compactness and spectrum, we identify VLA J070238.0+385044 as the afterglow from GRB 980329. We interpret the rapid flux density variations as interstellar scintillation and the sharp turnover in the radio spectrum below 13 GHz as arising from synchrotron self-absorption. This suggests that the angular diameter of the fireball from GRB 980329 was of order a few microarcseconds in the first two weeks. The absence of a readily detectable afterglow in the optical, but clear detections in both the radio and infrared, can be understood as the result of extinction by dust. In this context it is interesting to note that half of all well-localized gamma-ray bursts have no optical counterpart. Based on our study of GRB 980329 we suggest that the progenitors of a sizable fraction of gamma-ray bursts are associated with regions of moderate to high gas density., in press at ApJ Letters, 12 page LaTeX document includes 2 postscript figures
Published: 1998

23. BVRcIc photometry of GRB970508 optical remnant: May-August, 1997

Author: Sokolov, V. V., Kopylov, A. I., Zharikov, S. V., Feroci, M., Nicastro, L., and Palazzi, E.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: We present the results of photometric observations of the variable optical source associated to the remnant of the gamma-ray burst GRB970508 performed at SAO RAS (Russia) from May to August 1997. The observations were carried out with the standard (Johnson-Kron-Cousins) photometric BVRcIc system using the 1-meter and 6-meter telescopes. The brightness of the optical source increased from Rc=21.19 (May 9.75 UT) to Rc=19.70 (May 10.77 UT), whereupon it was decaying in all the four BVRcIc bands during about one month after the burst. Between the 3rd and the 6th night after the GRB970508 event, the flux decrease of the optical source follows an exponential law in all the four bands. In that period the broad-band spectrum of the object does not change and can be approximately described by a power with index -1.1. The subsequent observations showed a reduction of the source brightness decrease rate in all bands. The source flux decay after the maximum in the Rc band is well described by a single power-law with index -1.171 for the whole set of observations during 86 days. In the other bands the decay seems to slow down from the 31th day onwards. In particular, in the Ic band the source magnitude is about 23.1 from the 36th day after the GRB to the end of the observations (August 4, 1997)., 8 pages, Latex, 5 PS figures, requires l-aa.sty, accepted for publication in Astronomy and Astrophysics
Published: 1998

24. 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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25. Spectral Properties of the Prompt X-ray emission and Afterglow from the Gamma-Ray Burst of 28 February 1997

Author: Frontera, F., Costa, E., Piro, L., Muller, J. M., Amati, L., Feroci, M., Fiore, F., Pizzichini, G., Tavani, M., Castro-Tirado, A., Cusumano, G., Fiume, D. Dal, Heise, J., Hurley, K., Nicastro, L., Orlandini, M., Owens, A., Palazzi, E., Parmar, A. N., Zand, J. in 't, and Zavattini, G.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We report high-energy spectral data of the prompt emission of GRB970228 and its X-ray afterglow. We establish that the nature of the X-ray afterglow emission is non-thermal and similar to the later portion of GRB970228. Our data can be used to discriminate different emission models of GRB afterglows. While cooling of excited compact objects can be ruled out, fireball models are constrained in the physics of the radiation emission processes and their evolution., 12 pages, 4 figures Accepted for publication in ApJ Letters
Published: 1997

26. The broad-band (0.1-200 keV) spectrum of Her X-1 observed with BeppoSAX

Author: Dal Fiume, D., Orlandini, M., Cusumano, G., Del Sordo, S., Feroci, M., Frontera, F., Oosterbroek, T., Palazzi, E., Parmar, A. N., Santangelo, A., and Alberto Segreto
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: The X-ray pulsar Her X-1 was observed for more than two orbital cycles near the maximum of the 35 day X-ray intensity cycle by the Narrow Field Instruments on-board the BeppoSAX satellite. We present the first simultaneous measurement of the 0.1-200 keV spectrum. Three distinct continuum components are evident in the phase averaged spectrum: a low energy excess, modeled as a 0.1 keV blackbody; a power-law and a high energy cut-off. Superposed on this continuum are Fe L and K emission features at 1.0 and 6.5 keV, respectively, and a ~40 keV cyclotron absorption feature. The cyclotron feature can be clearly seen in raw count spectra. We present the properties of the cyclotron feature with unprecedented precision and discuss the indications given by this measurement on the physical properties of the emitting region., Comment: 5 pages, 2 figures, accepted for publication in A&A Letters
Published: 1997
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27. In-flight performances of the BeppoSAX Gamma-Ray Burst Monitor

Author: Feroci, M., Frontera, F., Costa, E., Fiume, D. Dal, Amati, L., Bruca, L., Cinti, M. N., Coletta, A., Collina, P., Guidorzi, C., Nicastro, L., Orlandini, M., Palazzi, E., Rapisarda, M., Zavattini, G., and Butler, R. C.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: The Italian-Dutch satellite for X-ray Astronomy BeppoSAX is successfully operating on a 600 km equatorial orbit since May 1996. We present here the in-flight performances of the Gamma Ray Burst Monitor experiment during its first year of operation. The GRBM is the secondary function of the four CsI(Na) slabs primarily operating as an active anticoincidence of the PDS hard X-ray experiment.. It has a geometric area of about 4000 cm2 but, due to its location in the core of the satellite its effective area is dependent on the energy and direction of the impinging photons. A dedicated electronics allows to trigger on cosmic gamma-ray bursts. When the trigger condition is satisfied the light curve of the event is recorded from 8 s before to 98 s after the trigger time, with a maximum time resolution of 0.48 ms, in an energy band of 40-700 keV., Comment: 12 pages, Postscript; Proc. SPIE Conference 3114 (San Diego, 1997)
Published: 1997
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28. Radio Monitoring of the January 11, 1997 Gamma-Ray Burst

Author: Frail, D. A., Kulkarni, S. R., Costa, E., Frontera, F., Heise, J., Feroci, M., Piro, L., Fiume, D. Dal, Nicastro, L., Palazzi, E., and Jager, R.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: We report on a comprehensive radio monitoring program of the bright gamma-ray burster GRB970111. These VLA observations were made at a frequency of 1.4 GHz and span a range of post-burst timescales between 28 hours and one month. Despite extensive sampling at sub-milliJansky sensitivities, no radio source was detected above 0.5 mJy in the current best error box (~14 arcmin^2) for GRB970111. A highly unusual radio source, VLA J1528.7+1945, was seen to drop in flux density by a factor of two in our monitoring period but it lies outside the error box and thus it is unlikely to be related to GRB970111. Cosmological fireball models of gamma-ray bursts make predictions of late-time emission occurring at longer wavelengths. The absence of a flaring or fading radio counterpart to GRB970111 provides strong constraints on these models., Comment: ApJ Let (accepted)
Published: 1997
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29. 3rd Interplanetary Network Localization, Time History, Fluence, Peak Flux, and Distance Lower Limit of the February 28, 1997 Gamma-Ray Burst

Author: Hurley, K., Costa, E., Feroci, M., Frontera, F., Cline, T., Fiume, D. Dal, Orlandini, M., Boer, M., Mazets, E., Aptekar, R., Golenetskii, S., and Terekhov, M.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: The gamma-ray burst of 1997 February 28 was localized using the arrival-time analysis method with the Ulysses, BeppoSAX, and WIND spacecraft. The result is a plus-or-minus 31.5 arcsec (3 sigma) wide annulus of possible arrival directions which intersects both the position of the burst determined independently by the SAX Wide Field Camera, and the position of a fading X-ray source detected by the SAX focussing X-ray telescopes, and reduces these source location areas by factors of 7 and 1.5 respectively. The combination of the annulus and the SAX locations, a 0.76 square arcminute error box, is consistent with that of an optical transient source and an extended object, possibly a galaxy. We also present the time history, peak flux, and fluence of this event, and derive a model-independent lower limit to the source distance of ~11000 AU., Comment: 11 pages, postscript, 2 figures. Accepted for publication in ApJ Letters
Published: 1997
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30. The GRB of 1999 January 23: Prompt emission and broad-band afterglow modeling

Author: Corsi, A., Piro, L., Kuulkers, E., Lorenzo Amati, Antonelli, L. A., Costa, E., Feroci, M., Frontera, F., Guidorzi, C., Heise, J., In T Zand, J., Maiorano, E., Montanari, E., Nicastro, L., Pian, E., and Soffitta, P.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: We report on BeppoSAX simultaneous X- and gamma-ray observations of the bright gamma-ray burst (GRB) 990123. We present the broad-band spectrum of the prompt emission, including optical, X- and gamma-rays, confirming the suggestion that the emission mechanisms at low and high frequencies must have different physical origins. We discuss the X-ray afterglow observed by the Narrow Field Instruments (NFIs) on board BeppoSAX and its hard X-ray emission up to 60 keV several hours after the burst, in the framework of the standard fireball model. The effects of including an important contribution of Inverse Compton scattering or modifying the hydrodynamics are studied., 4 pages, 3 figures, minor changes; accepted for publication in Il Nuovo Cimento, proceedings of the 4th Workshop on Gamma-Ray Bursts in the Afterglow Era, Rome,18-22 October 2004. For more details, see astro-ph/0504607 (accepted in A&A)

31. An optical study of the GRB 970111 field beginning 19 hours after the gamma-ray burst

Author: Gorosabel, J., Castro-Tirado, A. J., Wolf, C., Heidt, J., Seitz, T., Thommes, E., Bartolini, C., Guarnieri, A., Masetti, N., Piccioni, A., Larsen, S., Enrico Costa, Feroci, M., Frontera, F., Palazzi, E., and Lund, N.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: We present the results of the monitoring of the GRB 970111 field that started 19 hours after the event. This observation represents the fastest ground-based follow-up performed for GRB 970111 in all wavelengths. As soon as the detection of the possible GRB 970111 X-ray afterglow was reported by Feroci et al. (1998) we reanalyzed the optical data collected for the GRB 970111 field. Although we detect small magnitude variability in some objects, no convincing optical counterpart is found inside the WFC error box. Any change in brightness 19 hours after the GRB is less than 0.2 mag for objects with B < 21 and R < 20.8. The bluest object found in the field is coincident with 1SAXJ1528.8+1937. Spectroscopic observations revealed that this object is a Seyfert-1 galaxy with redshift z=0.657, which we propose as the optical counterpart of the X-ray source. Further observations allowed to perform multicolour photometry for objects in the GRB 970111 error box. The colour-colour diagrams do not show any object with unusual colours. We applied a photometric classification method to the objects inside the GRB error box, that can distinguish stars from galaxies and estimate redshifts. We were able to estimate photometric redshifts in the range 0.2 < z < 1.4 for several galaxies in this field and we did not find any conspicuous unusual object. We note that GRB 970111 and GRB 980329 could belong to the same class of GRBs, which may be related to nearby sources (z ~1) in which high intrinsic absorption leads to faint optical afterglows., 10 pages with 11 encapsulated PostScript figures included. Uses Astronomy & Astrophysics LaTeX macros. Accepted for publication in Astronomy & Astrophysics

32. BeppoSAX spectrum of GRB971214: evidence of a substantial energy output during afterglow

Author: Dal Fiume, D., Amati, L., Antonelli, L. A., Fiore, F., Muller, J. M., Parmar, A., Masetti, N., Pian, E., Costa, E., Frontera, F., Piro, L., Heise, J., Reginald Butler, Coletta, A., Feroci, M., Giommi, P., Nicastro, L., Orlandini, M., Palazzi, E., Pizzichini, G., and Tavani, M.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: We report the X/gamma-ray spectrum of GRB971214 and of its afterglow. The afterglow was measured few hours after the main event and for an elapsed time of more than two days. The measure of this GRB and afterglow is relevant due to its extreme, cosmological distance (z=3.42). The prompt event shows a hard photon spectrum, consistent with a broken power law with photon indices Gamma_X~0.1 below ~20 keV and Gamma_g~1.3 above 60 keV. The afterglow spectrum, measured with the MECS and LECS BeppoSAX telescopes, is consistent with a power law with spectral photon index Gamma=1.6. Within the statistical accuracy of our measure no spectral evolution is detected during the observation of the afterglow. When integrated during the time span covered by BeppoSAX observations, the power in the afterglow emission, even with very conservative assumptions, is at least comparable with the power in the main event. The IR-to-X rays broad band spectrum is also presented, collecting data from the literature and adding them to the BeppoSAX measure. It shows that the predictions from synchrotron emission models is qualitatively confirmed. The BeppoSAX measurement of the X and gamma ray spectrum of this GRB/afterglow is discussed in the framework of current theoretical models., Comment: 8 pages, 4 figures. To be published in Astronomy and Astrophysics. Uses aa, epsf and times LaTeX macros

33. 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)

34. Early detection of the optical counterpart to GRB 980329

Author: Gorasabel, J., A. J. Castro-Tirado, Pedrosa, A., Zapatero-Osorio, M. R., Fernades, A. J. L., Feroci, M., Costa, E., and Frontera, F.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: We report optical observations of the GRB 980329 error box which represent the second earliest detection of the GRB 980329 optical transient. We determine R = 23.7 $\pm$ 0.5 mag on 29.89 March, which is consistent with R = 23.6 $\pm$ 0.2 mag as reported by Palazzi et al. (1998) on 29.99 March. Based on extrapolations of the light curve we claim that the R-band magnitude of the GRB 980329 host galaxy should lie in the range 26.8 mag $, Comment: 4 pages with three encapsulated PostScript figure included. Accepted for publication as a letter in Astronomy & Astrophysics

35. What can BeppoSAX tell us about short GRBs: An update from the subsecond GRB project

Author: Muller, J., Smith, M., Feroci, M., Costa, E., Piro, L., Gandolfi, G., Frontera, F., Tassone, G., Tarei, G., Paolino, A., Di Ciolo, L., Celidonio, G., and Coletta, A.
Subjects: Physics, X-ray astronomy, Astrophysics (astro-ph), FOS: Physical sciences, Cosmic ray, Astrophysics, Gamma-ray astronomy, Gamma-ray burst, Wide field
Abstract: We present some statistical considerations on the BeppoSAX hunt for subsecond GRBs at the Scientific Operation Center. Archive analysis of a BATSE/SAX sub-sample of bursts indicates that the GRB Monitor is sensitive to short (< 2 sec) events, that are in fact about 22% of the total. The non-detection of corresponding prompt X-ray counterparts to short bursts in the Wide Field Cameras, in about 3 years of operations, is discussed: with present data no implications on the X-to-gamma-ray spectra of short vs long GRBs may be inferred. Finally, the status of searching procedures at SOC is reviewed., Proc. 5th Huntsville GRB Symposium

36. Early detection of the optical transient following the Gamma-Ray Burst GRB 970228

Author: Guarnieri, A., Bartolini, C., Nicola Masetti, Piccioni, A., Costa, E., Feroci, M., Frontera, F., Dal Fiume, D., Nicastro, L., Palazzi, E., Castro-Tirado, A. J., and Gorosabel, J.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: The optical counterpart of the Gamma-Ray Burst GRB 970228, discovered by Groot et al. (IAU Circ. 6584), is also detected in the B and R frames obtained about 4 hours earlier at the Bologna Observatory. Our observations indicate a very likely rise of the optical emission within these 4 hours. The R luminosity of the transient at maximum was about 15 times that of an underlying extended object. Follow-up data show that the maximum optical emission was delayed of not less than 0.7 days with respect to the gamma-ray peak and that no new big flares were seen after the main one. The optical transient became significantly redder once it has reverted to quiescence., 4 pages, no figures, LaTeX A&A style file L-AA version 3, accepted by Astronomy and Astrophysics Letters, also available at http://www.bo.astro.it/bap/BAPhome.html (file bap97-21-text.ps) or via anonymous ftp at boas3.bo.astro.it/bap/files/bap97-21-text.ps

37. The first X-ray localization of a gamma-ray burst by BeppoSAX and its fast spectral evolution

Author: Piro, L., Heise, J., Jager, R., Costa, E., Frontera, F., Feroci, M., Muller, J. M., Amati, L., Cinti, M. N., Dal Fiume, D., Luciano Nicastro, Orlandini, M., and Pizzichini, G.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: In this paper we present the observations performed by the BeppoSAX Gamma-Ray Burst Monitor (GRBM) and Wide Field Cameras (WFC) of GB960720. We derive a precise localization (3 arcmin radius) and fast broad band (2-700 keV) spectral evolution of the event. A search in the catalogues at all wavelengths in the error box yields a unique outstanding source: the bright radio quasar 4C 49.29. Although the probability of finding such a source by chance is very low (0.0002), the absence of similar counterparts in other small error boxes suggests a chance occurrence. We also find that the duration-energy relationship for bursts previously observed above 25keV (Fenimore et al. 1995) extends down to 1.5 keV. This result suggests that the same radiation mechanism is operating from X-rays to gamma-rays and is in agreement with radiative cooling by synchotron emission. A fast evolution of the spectrum is found, in which the ratio of X- to gamma-ray intensities varies over three orders of magnitude. Furthermore, the spectrum in the initial phase of the event betrays the presence of an optically thick source rapidly evolving in a thin configuration.No other class of sources in the universe shows such a fast and extreme evolution. These results pose new and tighter constraints on theoretical models for gamma-ray bursts., 5 pages, LaTeX, 5 postscript figures; A&A, Accepted 15 July 1997, updated reference Costa 1997b

38. The optical transient of GRB970228, 16 hours after the burst

Author: Pedichini, F., Di Paola, A., Stella, L., Buonanno, R., Boattini, A., Gandolfi, G., Costa, E., Feroci, M., Piro, L., Dal Fiume, D., Frontera, F., Nicastro, L., Eliana Palazzi, Heise, J., In T Zand, J., and Vietri, M.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: Until recently the positions of gamma ray bursts were not sufficiently well known within a short timescale to localize and identify them with known celestial sources. Following the historical detection of the X-ray afterglow of the burst GRB970228, extending from 30 s to 3 days after the main peak, by the Beppo-SAX satellite and that of an optical transient 21 hr after the burst, we report here the detection of the same optical transient, in images obtained only 16 hours after the burst., Accepted for publication in Astronomy and Astrophysics Letters, Springer LateX needed

39. Opening a new window to Fundamental Physics and astrophysics: X-ray Polarimetry

Author: Costa, E., Bellazzini, R., Soffltta, P., Di Persio, G., Feroci, M., Morelli, E., Muleri, F., Pacciani, L., Rubini, A., Luca Baldini, Bitti, F., Brez, A., Cavalca, F., Latronico, L., Massai, M. M., Omodei, N., Sgrò, C., Spandre, G., Matt, G., Perola, G. C., Santangelo, A., Celotti, A., Barret, D., Vilhu, O., Piro, L., Fraser, G., Courvoisier, T. J. -L, and Barcons, X.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics
Abstract: An extensive theoretical literature predicts that X-ray Polarimetry can directly determine relevant physical and geometrical parameters of astrophysical sources, and discriminate between models further than allowed by spectral and timing data only. X-ray Polarimetry can also provide tests of Fundamental Physics. A high sensitivity polarimeter in the focal plane of a New Generation X-ray telescope could open this new window in the High Energy Sky., Comment: 8 pages 1 table 14 figures

40. EDGE: explorer of diffuse emission and gamma-ray burst explosions

Author: Piro, L., den Herder, J. W. , Ohashi, T. , Amati, L. , Atteia, J. L. , Barthelmy, S. , Barbera, M. , Barret, D. , Basso, S. , Boer, M. , Borgani, S. , Boyarskiy, Branduardi Raymont, G. , Briggs, M. , Brunetti, Budtz Jorgensen, C. , Burrows, D. , Campana, S. , Caroli, E. , Chincarini, G. , Christensen, F. , Cocchi, M. , Comastri, A. , Corsi, A. , Cotroneo, V. , Conconi, P. , Colasanti, L. , Cusumano, de Rosa, Del Santo, M. , Ettori, S. , Ezoe, Y. , Ferrari, L. , Feroci, M. , Finger, M. , Fishman, G. , Fujimoto, R. , Galeazzi, M. , Galli, A. , Gatti, F. , Gehrels, N. , Gendre, B. , Ghirlanda, G. , Ghisellini, G. , Giommi, P. , Girardi, M. , Guzzo, L. , Haardt, F. , Hepburn, I. , Hermsen, W. , Hoevers, H. , Holland, in't Zand, J. , Ishisaki, Y. , Kawahara, H. , Kawai, N. , Kaastra, J. , Kippen, de Korte, P. A. J. , Kouveliotou, C. , Kusenko, A. , Labanti, C. , Lieu, R. , Macculi, C. , Makishima, K. , Matt, G. , Mazzotta, P. , McCammon, D. , Méndez, M. , Mineo, T. , Mitchell, S. , Mitsuda, K. , Molendi, S. , Moscardini, L. , Mushotzky, R. , Natalucci, L. , Nicastro, F. , O'Brien, P. , Osborne, J. , Paerels, F. , Page, M. , Paltani, S. , Pareschi, G. , Perinati, E. , Perola, C. , Ponman, T. , Rasmussen, A. , Roncarelli, M. , Rosati, P. , Ruchayskiy, O. , Quadrini, E. , Sakurai, I. , Salvaterra, R. , Sasaki, S. , Sato, G. , Schaye, J. , Schmitt, J. , Sciortino, S. , Shaposhnikov, M. , Shinozaki, K. , Spiga, D. , Suto, Y. , Tagliaferri, G. , Takahashi, T. , Takei, Y. , Tawara, Y. , Tozzi, P. , Tsunemi, H. , Tsuru, T. , Ubertini, P. , Ursino, E. , Viel, M. , Vink, J. , White, N. , Willingale, R. , Wijers, R. , Yoshikawa, K. , Yamasaki, BRANCHINI, ENZO FRANCO, Piro, L, den Herder, J W, Ohashi, T, Amati, L, Atteia, J L, Barthelmy, S, Barbera, M, Barret, D, Basso, S, Boer, M, Borgani, S, Boyarskiy, O, Branchini, E, Branduardi-Raymont, G, Briggs, M, Brunetti, G, Budtz-Jorgensen, C, Burrows, D, Campana, S, Caroli, E, Chincarini, G, Christensen, F, Cocchi, M, Comastri, A, Corsi, A, Cotroneo, V, Conconi, P, Colasanti, L, Cusumano, G, de Rosa, A, Del Santo, M, Ettori, S, Ezoe, Y, Ferrari, L, Feroci, M, Finger, M, Fishman, G, Fujimoto, R, Galeazzi, M, Galli, A, Gatti, F, Gehrels, N, Gendre, B, Ghirlanda, G, Ghisellini, G, Giommi, P, Girardi, M, Guzzo, L, Haardt, F, Hepburn, I, Hermsen, W, Hoevers, H, Holland, A, in't Zand, J, Ishisaki, Y, Kawahara, H, Kawai, N, Kaastra, J, Kippen, M, de Korte, P A J, Kouveliotou, C, Kusenko, A, Labanti, C, Lieu, R, Macculi, C, Makishima, K, Matt, G, Mazzotta, P, McCammon, D, Méndez, M, Mineo, T, Mitchell, S, Mitsuda, K, Molendi, S, Moscardini, L, Mushotzky, R, Natalucci, L, Nicastro, F, O'Brien, P, Osborne, J, Paerels, F, Page, M, Paltani, S, Pareschi, G, Perinati, E, Perola, C, Ponman, T, Rasmussen, A, Roncarelli, M, Rosati, P, Ruchayskiy, O, Quadrini, E, Sakurai, I, Salvaterra, R, Sasaki, S, Sato, G, Schaye, J, Schmitt, J, Sciortino, S, Shaposhnikov, M, Shinozaki, K, Spiga, D, Suto, Y, Tagliaferri, G, Takahashi, T, Takei, Y, Tawara, Y, Tozzi, P, Tsunemi, H, Tsuru, T, Ubertini, P, Ursino, E, Viel, M, Vink, J, White, N, Willingale, R, Wijers, R, Yoshikawa, K, Yamasaki, N, JW DEN HERDER, L PIRO, T OHASHI, L AMATI, J ATTEIA, S BARTHELMY, BARBERA M, D BARRET, S BASSO, M BOER, S BORGANI, O BOYARSKIY BRANCHINI, BRANDUARDI-RAYMONT, M BRIGGS, G BRUNETTI, C BUDTZ-JORGENSEN, D BURROWS, S CAMPANA, E CAROLI, F CHRISTENSEN, M COCCHI, A COMASTRI, A CORSI, V COTRONEO, P CONCONI, L COLASANTI, G CUSUMANO, A DE ROSA, M DEL SANTO, S ETTORI, Y EZOE, L FERRARI, M FEROCI, M FINGER, G FISHMAN, R FUJIMOTO, M GALEAZZI, A GALLI, F GATTI, N GEHRELS, B GENDRE, G GHIRLANDA, G GHISELLINI, P GIOMMI, M GIRARDI, L GUZZO, F HAARDT, I HEPBURN, W HERMSEN, H HOEVERS, A HOLLAND, J INT ZAND, Y ISHISAKI, H KAWAHARA, N KAWAI, J KAASTRA, M KIPPEN, PAJ DE KORTE, C KOUVELIOTOU, A KUSENKO, C LABANTI, R LIEU, C MACCULI, K MAKISHIMA, G MATT, P MAZOTTA, D MCCAMMON, M MNDEZ, T MINEO, S MITCHELL, K MITSUDA, S MOLENDI, L MOSCARDINI, R MUSHOTZKY, L NATALUCCI, F NICASTRO, P OBRIEN, J OSBORNE, F PAERELS, M PAGE, S PALTANI, G PARESCHI, E PERINATI, C PEROLA, T PONMAN, A RASMUSSEN, M RONCARELLI, P ROSATI, O RUCHAYSKIY, E QUADRINI, I SAKURAI, R SALVATERRA, S SASAKI, G SATO, J SCHAYE, J SCHMIDTT, S SCIORITINO, M SHAPOOSHNIKOV, K SHINOZAKI, D SPIGA, Y SUTO, G TAGLIAFERRI, T TAKAHASHI, Y TAKEI, Y TAWARA, P TOZZI, H TSUNEMI, T TSURU, P UBERTINI, E URSINO, M VIEL, J VINK, N WHITE, R WILLINGALE, R WIJERS, K YOSHIKAWA, N YAMASAKI, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), European Organization for Nuclear Research (CERN), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), L. Piro, J. W. den Herder, T. Ohashi, L. Amati, J. L. Atteia, S. Barthelmy, M. Barbera, D. Barret, S. Basso, M. Boer, S. Borgani, O. Boyarskiy, E. Branchini, G. Branduardi-Raymont, M. Brigg, G. Brunetti, C. Budtz-Jorgensen, D. Burrow, S. Campana, E. Caroli, G. Chincarini, F. Christensen, M. Cocchi, A. Comastri, A. Corsi, V. Cotroneo, P. Conconi, L. Colasanti, G. Cusumano, A. Rosa, M. Del Santo, S. Ettori, Y. Ezoe, L. Ferrari, M. Feroci, M. Finger, G. Fishman, R. Fujimoto, M. Galeazzi, A. Galli, F. Gatti, N. Gehrel, B. Gendre, G. Ghirlanda, G. Ghisellini, P. Giommi, M. Girardi, L. Guzzo, F. Haardt, I. Hepburn, W. Hermsen, H. Hoever, A. Holland, J. in’t Zand, Y. Ishisaki, H. Kawahara, N. Kawai, J. Kaastra, M. Kippen, P. A. J. Korte, C. Kouveliotou, A. Kusenko, C. Labanti, R. Lieu, C. Macculi, K. Makishima, G. Matt, P. Mazzotta, D. McCammon, M. Méndez, T. Mineo, S. Mitchell, K. Mitsuda, S. Molendi, L. Moscardini, R. Mushotzky, L. Natalucci, F. Nicastro, P. O’Brien, J. Osborne, F. Paerel, M. Page, S. Paltani, G. Pareschi, E. Perinati, C. Perola, T. Ponman, A. Rasmussen, M. Roncarelli, P. Rosati, O. Ruchayskiy, E. Quadrini, I. Sakurai, R. Salvaterra, S. Sasaki, G. Sato, J. Schaye, J. Schmitt, S. Sciortino, M. Shaposhnikov, K. Shinozaki, D. Spiga, Y. Suto, G. Tagliaferri, T. Takahashi, Y. Takei, Y. Tawara, P. Tozzi, H. Tsunemi, T. Tsuru, P. Ubertini, E. Ursino, M. Viel, J. Vink, N. White, R. Willingale, R. Wijer, K. Yoshikawa, N. Yamasaki, High Energy Astrophys. & Astropart. Phys (API, FNWI), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Osservatorio Astronomico di Brera, Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Astronomy, Stephen L. O'Dell, Giovanni Pareschi, den Herder, J. W., Piro, L., Ohashi, T., Amati, L., Atteia, J., Barthelmy, S., Barbera, M., Barret, D., Basso, S., Boer, M., Borgani, S., Boyarskiy, O., Branchini, E., Branduardi-Raymont, G., Briggs, M., Brunetti, G., Budtz-Jorgensenf, C., Burrows, D., Campana, S., Caroli, E., Chincarini, G., Christensen, F., Cocchi, M., Comastri, A., Corsi, A., Cotroneo, V., Conconi, P., Colasanti, L., Cusamano, G., de Rosa, A., Del Santo, M., Ettori, S., Ezoe, Y., Ferrari, L., Feroci, M., Finger, M., Fishman, G., Fujimoto, R., Galeazzi, M., Galli, A., Gatti, F., Gehrels, N., Gendre, B., Ghirlanda, G., Ghisellini, G., Giommi, P., Girardi, M., Guzzo, L., Haardt, F., Hepburn, I., Hermsen, W., Hoevers, H., Holland, A., In't Zand, J., Ishisaki, Y., Kawahara, H., Kawai, N., Kaastra, J., Kippen, M., de Korte, P. A. J., Kouveliotou, C., Kusenko, A., Labanti, C., Lieu, R., Macculi, C., Makishima, K., Matt, G., Mazotta, P., Mccammon, D., Méndez, M., Mineo, T., Mitchell, S., Mitsuda, K., Molendi, S., Moscardini, L., Mushotzky, R., Natalucci, L., Nicastro, F., O'Brien, P., Osborne, J., Paerels, F., Page, M., Paltani, S., Pareschi, G., Perinati, E., Perola, C., Ponman, T., Rasmussen, A., Roncarelli, M., Rosati, P., Ruchayskiy, O., Quadrini, E., Sakurai, I., Salvaterra, R., Sasaki, S., Sato, G., Schaye, J., Schmidtt, J., Scioritino, S., Shaposhnikov, M., Shinozaki, K., Spiga, D., Suto, Y., Tagliaferri, G., Takahashi, T., Takei, Y., Tawara, Y., Tozzi, P., Tsunemi, H., Tsuru, T., Ubertini, P., Ursino, E., Viel, M., Vink, J., White, N., Willingale, R., Wijers, R., Yoshikawa, K., Yamasaki, N., DEN HERDER, J. W. . OHASHI T., Atteia, J. L., Borgani, Stefano, Coauthors, Girardi, Marisa, Den, Herder, J. W., Ohashi, T., Amati, L., Atteia, J. L., Barthelmy, S., Barbera, M., Barret, D., Basso, S., Boer, M., Borgani, S., Boyarskiy, Branchini, ENZO FRANCO, Branduardi, Raymont, G., Brigg, M., Brunetti, Budtz, Jorgensen, C., Burrow, D., Campana, S., Caroli, E., Chincarini, G., Christensen, F., Cocchi, M., Comastri, A., Corsi, A., Cotroneo, V., Conconi, P., Colasanti, L., Cusumano, De, Rosa, Del, Santo, M., Ettori, S., Ezoe, Y., Ferrari, L., Feroci, M., Finger, M., Fishman, G., Fujimoto, R., Galeazzi, M., Galli, A., Gatti, F., Gehrel, N., Gendre, B., Ghirlanda, G., Ghisellini, G., Giommi, P., Girardi, M., Guzzo, L., Haardt, F., Hepburn, I., Hermsen, W., Hoever, H., Holland, In'T, Zand, J., Ishisaki, Y., Kawahara, H., Kawai, N., Kaastra, J., Kippen, De, Korte, P. A. J., Kouveliotou, C., Kusenko, A., Labanti, C., Lieu, R., Macculi, C., Makishima, K., Matt, G., Mazzotta, P., Mccammon, D., Méndez, M., Mineo, T., Mitchell, S., Mitsuda, K., Molendi, S., Moscardini, L., Mushotzky, R., Natalucci, L., Nicastro, F., O'Brien, P., Osborne, J., Paerel, F., Page, M., Paltani, S., Pareschi, G., Perinati, E., Perola, C., Ponman, T., Rasmussen, A., Roncarelli, M., Rosati, P., Ruchayskiy, O., Quadrini, E., Sakurai, I., Salvaterra, R., Sasaki, S., Sato, G., Schaye, J., Schmitt, J., Sciortino, S., Shaposhnikov, M., Shinozaki, K., Spiga, D., Suto, Y., Tagliaferri, G., Takahashi, T., Takei, Y., Tawara, Y., Tozzi, P., Tsunemi, H., Tsuru, T., Ubertini, P., Ursino, E., Viel, M., Vink, J., White, N., Willingale, R., Wijer, R., Yoshikawa, K., Yamasaki, Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3)
Subjects: Vision, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Warm–hot intergalactic medium, Astrophysics, 7. Clean energy, 01 natural sciences, Cosmology, Settore FIS/05 - Astronomia E Astrofisica, Intergalactic Medium, Warm-Hot Intergalactic Medium, X-rays, Cosmology, Clusters, Gamma-ray bursts, Warm-hot intergalactic medium, Missions, 010303 astronomy & astrophysics, X-ray telescopes, X-rays, Clusters, Gamma-ray bursts, Warm– hot intergalactic medium, Missions, Physics, Equipment and services, Satellite Mission, Spectrometers, Astrophysics (astro-ph), X-rays, Cosmology, Clusters, Gamma-ray bursts, Warm–, hot intergalactic medium, Missions, Temperature, Astrophysics::Instrumentation and Methods for Astrophysics, Cosmic Vision, Spectral resolution, Galaxy Clusters, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Warm&ndash, Astrophysics::Cosmology and Extragalactic Astrophysics, hot intergalactic medium, Absorption, NO, 010309 optics, X-ray, Galaxy groups and clusters, 0103 physical sciences, Imaging systems, 010306 general physics, Gamma-ray burst, Galaxy cluster, Spatial resolution, Sensors, Astronomy, X-rays, clusters, Gamma-Ray Bursts, Warm-Hot Intergalactic Medium, missions, Astronomy and Astrophysics, Galaxy, Redshift, Cluster, 13. Climate action, Space and Planetary Science
Abstract: How structures on various scales formed and evolved from the early Universe up to present time is a fundamental question of astrophysical cosmology. EDGE will trace the cosmic history of the baryons from the early generations of massive star by Gamma-Ray Burst (GRB) explosions, through the period of cluster formation, down to very low redshifts, when between a third and one half of the baryons are expected to reside in cosmic filaments undergoing gravitational collapse by dark matter (Warm Hot Intragalactic Medium: WHIM). In addition EDGE, with its unprecedented observational capabilities, will provide key results on several other topics. The science is feasible with a medium class mission using existing technology combined with innovative instrumental and observational capabilities on a single satellite by: a) observing with fast reaction Gamma-Ray Bursts with a high spectral resolution (R ~ 500). This enables the study of their (star-forming) environment from the Dark to the local Universe and the use of GRB as back light of large scale cosmological structures b) Observing and surveying extended sources (clusters, WHIM) with high sensitivity using two wide field of view X-ray telescopes (one with a high angular resolution and the other with a high spectral resolution)., This is a low resolution version of the proposal submitted to ESA in response to the Cosmic Vision Call. A high quality version is available at the web address reported in the cover page
Published: 2007

41. Long-term AGILE monitoring of the puzzling gamma-ray source 3EG J1835+5918

Author: G. De Paris, A. Zambra, F. D'Ammando, M. Feroci, M. Fiorini, Dario Gasparrini, L. Pacciani, F. Longo, A. Rappoldi, E. Vallazza, F. Boffelli, M. Rapisarda, P. Picozza, A. Argan, F. Perotti, E. Del Monte, G. Pucella, A. Trois, Andrea Bulgarelli, I. Donnarumma, T. Froysland, P. Soffitta, A. Pellizzoni, Guido Barbiellini, Enrico Costa, Y. Evangelista, F. Lazzarotto, V. Vittorini, V. Cocco, P. Santolamazza, M. Trifoglio, A. Giuliani, Paolo Lipari, A. W. Chen, P. Giommi, F. Fuschino, S. Vercellone, C. Pittoril, M. Galli, F. Verrecchia, Martino Marisaldi, Sandro Mereghetti, P. W. Cattaneo, P. A. Caraveo, I. Lapshov, M. Prest, S. Colafrancesco, Marco Tavani, G. Piano, A. Morselli, Claudio Labanti, L. Salotti, D. Zanello, M. Marelli, G. Di Cocco, S. Cutini, Fulvio Gianotti, Bulgarelli A, Tavani M, Caraveo P, Chen AW, Gianotti F, Trifoglio M, Marelli M, Argan A, Barbiellini G, Boffelli F, Cattaneo PW, Cocco V, Costa E, DAmmando F, Del Monte E, De Paris G, Di Cocco G, Donnarumma I, Evangelista Y, Feroci M, Fiorini M, Froysland T, Fuschino F, Galli M, Giuliani A, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Longo F, Marisaldi M, Mereghetti S, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Piano G, Picozza P, Prest M, Pucella G, Rapisarda M, Rappoldi A, Soffitta P, Trois A, Vallazza E, Vercellone S, Vittorini V, Zambra A, Zanello D, Giommi P, Pittori C, Verrecchia F, Santolamazza P, Gasparrini D, Cutini S, Colafrancesco S, Salotti L, A., Bulgarelli, M., Tavani, P., Caraveo, A. W., Chen, F., Gianotti, M., Trifoglio, M., Marelli, A., Argan, G., Barbiellini, F., Boffelli, P. W., Cattaneo, V., Cocco, E., Costa, F., D'Ammando, E. D., Monte, G. D., Pari, G. D., Cocco, I., Donnarumma, Y., Evangelista, M., Feroci, M., Fiorini, T., Froysland, F., Fuschino, M., Galli, A., Giuliani, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, Longo, Francesco, M., Marisaldi, S., Mereghetti, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, G., Piano, P., Picozza, M., Prest, G., Pucella, M., Rapisarda, A., Rappoldi, P., Soffitta, A., Troi, E., Vallazza, S., Vercellone, V., Vittorini, A., Zambra, D., Zanello, P., Giommi, C., Pittori, F., Verrecchia, P., Santolamazza, D., Gasparrini, S., Cutini, S., Colafrancesco, and L., Salotti
Subjects: Photon, Field (physics), FOS: Physical sciences, Flux, Field of view, Astrophysics, Unidentified Gamma-ray Source, Power law, High Energy Gamma-ray Astronomy, AGILE gamma ray satellite, 3EG J1835+5918, Egret, Physics, biology, Astrophysics (astro-ph), Gamma ray, Astronomy and Astrophysics, biology.organism_classification, Term (time), Space and Planetary Science, Unidentified Gamma-ray Sources, AGILE satellite, gamma rays: observations
Abstract: We present the AGILE gamma-ray observations of the field containing the puzzling gamma-ray source 3EG J1835+5918. This source is one of the most remarkable unidentified EGRET sources. An unprecedentedly long AGILE monitoring of this source yields important information on the positional error box, flux evolution, and spectrum. 3EG J1835+5918 has been in the AGILE field of view several times in 2007 and 2008 for a total observing time of 138 days from 2007 Sept 04 to 2008 June 30 encompassing several weeks of continuous coverage. With an exposure time approximately twice that of EGRET, AGILE confirms the existence of a prominent gamma-ray source (AGL J1836+5926) at a position consistent with that of EGRET, although with a remarkably lower average flux value for photon energies greater than 100 MeV. A 5-day bin temporal analysis of the whole data set of AGL J1836+5926 shows some evidence for variability of the gamma-ray flux. The source spectrum between 100 MeV and 1 GeV can be fitted with a power law with photon index in the range 1.6-1.7, fully consistent with the EGRET value. The faint X-ray source RX J1836.2+5925 that has been proposed as a possible counterpart of 3EG J1835+5918 is well within the AGILE error box. Future continuous monitoring (both by AGILE and GLAST) is needed to confirm the gamma-ray flux variability and to unveil the source origin, a subject that is currently being pursued through a multiwavelength search for counterparts., Comment: accepted for publication by Astron. & Astrophys, 4 pages, 2 figures, 2 tables
Published: 2008

42. AGILE Detection of a Strong Gamma-Ray Flare from the Blazar 3C 454.3

Author: T. Froysland, Martino Marisaldi, G. De Paris, Dario Gasparrini, Fulvio Gianotti, F. Perotti, F. Mauri, L. Salotti, A. Zambra, M. Prest, S. Cutini, Francesco Longo, G. Di Cocco, Paolo Giommi, Francesco Lazzarotto, M. Galli, Piergiorgio Picozza, Paolo Soffitta, F. Verrecchia, Marco Tavani, A. Pellizzoni, D. Zanello, Massimo Rapisarda, Claudio Labanti, Alessio Trois, Sergio Colafrancesco, L. A. Antonelli, P. A. Caraveo, Sandro Mereghetti, A. Giuliani, S. Vercellone, M. Fiorini, I. Donnarumma, Guido Barbiellini, A. Morselli, F. D'Ammando, Y. Evangelista, Marco Feroci, Luigi Pacciani, Paolo Lipari, E. Vallazza, F. Fuschino, V. Cocco, V. Vittorini, E. Del Monte, M. Trifoglio, G. Pucella, I. Lapshov, A. Argan, Andrea Bulgarelli, Enrico Costa, A. W. Chen, C. Pittori, S., Vercellone, A. W., Chen, A., Giuliani, A., Bulgarelli, I., Donnarumma, I., Lapshov, M., Tavani, A., Argan, G., Barbiellini, P., Caraveo, V., Cocco, E., Costa, F., D'Ammando, E. D., Monte, G. D., Pari, G. D., Cocco, Y., Evangelista, M., Feroci, M., Fiorini, T., Froysland, F., Fuschino, M., Galli, F., Gianotti, C., Labanti, F., Lazzarotto, P., Lipari, Longo, Francesco, M., Marisaldi, F., Mauri, S., Mereghetti, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, P., Picozza, M., Prest, G., Pucella, M., Rapisarda, P., Soffitta, M., Trifoglio, A., Troi, E., Vallazza, V., Vittorini, A., Zambra, D., Zanello, C., Pittori, F., Verrecchia, D., Gasparrini, S., Cutini, P., Giommi, L. A., Antonelli, S., Colafrancesco, L., Salotti, Vercellone S, Chen AW, Giuliani A, Bulgarelli A, Donnarumma I, Lapshov I, Tavani M, Argan A, Barbiellini G, Caraveo P, Cocco V, Costa E, DAmmando F, Del Monte E, De Paris G, Di Cocco G, Evangelista Y, Feroci M, Fiorini M, Froysland T, Fuschino F, Galli M, Gianotti F, Labanti C, Lazzarotto F, Lipari P, Longo F, Marisaldi M, Mauri F, Mereghetti S, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Picozza P, Prest M, Pucella G, Rapisarda M, Soffitta P, Trifoglio M, Trois A, Vallazza E, Vittorini V, Zambra A, Zanello D, Pittori C, Verrecchia F, Gasparrini D, Cutini S, Giommi P, Antonelli LA, Colafrancesco S, and Salotti L
Subjects: High Energy Gamma-ray Astronomy, Active Galactic Nuclei, AGILE satellite, Agile, Photon, blazar, gamma and X-ray detection, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, law.invention, astro-ph, law, Blazar, Physics, Range (particle radiation), Astrophysics (astro-ph), Detector, Gamma ray, Astronomy and Astrophysics, Quasar, Space and Planetary Science, gamma rays: observations — quasars: individual (3C 454.3), Energy (signal processing), Flare
Abstract: We report the first blazar detection by the AGILE satellite. AGILE detected 3C 454.3 during a period of strongly enhanced optical emission in July 2007. AGILE observed the source with a dedicated repointing during the period 2007 July 24-30 with its two co-aligned imagers, the Gamma-Ray Imaging Detector and the hard X-ray imager Super-AGILE sensitive in the 30 MeV-50 GeV and 18-60 keV, respectively. Over the entire period, AGILE detected gamma-ray emission from 3C 454.3 at a significance level of 13.8-$\sigma$ with an average flux (E$>$100 MeV) of $(280 \pm 40) \times 10^{-8}$ photons cm$^{-2}$ s$^{-1}$. The gamma-ray flux appears to be variable towards the end of the observation. No emission was detected by Super-AGILE in the energy range 20-60 keV, with a 3-$\sigma$ upper limit of $2.3 \times 10^{-3}$ photons cm$^{-2}$ s$^{-1}$. The gamma-ray flux level of 3C 454.3 detected by AGILE is the highest ever detected for this quasar and among the most intense gamma-ray fluxes ever detected from Flat Spectrum Radio Quasars., Comment: Accepted by Astrophysical Journal Letters; 14 pages, 3 EPS Figures, 1 Table
Published: 2008

43. GRB 070724B: the first gamma ray burst localized by SuperAGILE and its Swift X-ray afterglow

Author: F. Mauri, Marco Feroci, Luigi Pacciani, P. Lipari, M. Galli, Piergiorgio Picozza, Massimo Rapisarda, A. Argan, Andrea Bulgarelli, L. A. Antonelli, Claudio Labanti, Enrico Costa, F. Verrecchia, B. Preger, P. A. Caraveo, Neil Gehrels, V. Vittorini, E. Vallazza, M. Trifoglio, E. Del Monte, C. Pittori, A. Pellizzoni, P. Romano, S. Vercellone, F. Perotti, A. Giuliani, G. Di Cocco, L. Salotti, A. Zambra, J. P. Osborne, David N. Burrows, L. Foggetta, M. Prest, I. Lapshov, Alessio Trois, Paolo Soffitta, M. Basset, Sandro Mereghetti, Francesco Lazzarotto, Y. Evangelista, V. La Parola, Martino Marisaldi, P. T. O'Brien, G. Chincarini, Marco Tavani, I. Donnarumma, A. W. Chen, Fulvio Gianotti, F. Fuschino, A. Morselli, G. Barbiellini, Paolo Giommi, Francesco Longo, G. Pucella, DEL MONTE, E, Feroci, M, Pacciani, L, Evangelista, Y, Donnarumma, I, Soffitta, P, Costa, E, Lapshov, I, Lazzarotto, F, Rapisarda, M, Argan, A, BARBIELLINI AMIDEI, Guido, Basset, M, Bulgarelli, A, Caraveo, P, Chen, A, DI COCCO, G, Foggetta, L, Fuschino, F, Galli, M, Gianotti, F, Giuliani, A, Labanti, C, Lipari, P, Longo, Francesco, Marisaldi, M, Mauri, F, Mereghetti, S, Morselli, A, Pellizzoni, A, Perotti, F, Picozza, P, Prest, M, Pucella, G, Tavani, M, Trifoglio, M, Trois, A, Vallazza, E, Vercellone, S, Vittorini, V, Zambra, A, Romano, P, BURROWS D., N, Chincarini, G, Gehrels, N, LA PAROLA, V, O'BRIEN P., T, OSBORNE J., P, Preger, B, Pittori, C, ANTONELLI L., A, Verrecchia, F, Giommi, P, and Salotti, L.
Subjects: Physics, Swift, Very large array, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), X-ray, Gamma ray, FOS: Physical sciences, AGILE satellite, GRB 070724B, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, law.invention, Afterglow, Telescope, Space and Planetary Science, law, Gamma-ray burst, computer, computer.programming_language
Abstract: GRB 070724B is the first Gamma Ray Burst localized by SuperAGILE, the hard X-ray monitor aboard the AGILE satellite. The coordinates of the event were published $\sim 19$ hours after the trigger. The Swift X-Ray Telescope pointed at the SuperAGILE location and detected the X-ray afterglow inside the SuperAGILE error circle. The AGILE gamma-ray Tracker and Minicalorimeter did not detect any significant gamma ray emission associated with GRB 070724B in the MeV and GeV range, neither prompt nor delayed. Searches of the optical afterglow were performed by the Swift UVOT and the Palomar automated 60-inch telescopes without any significant detection. Similarly the Very Large Array did not detect a radio afterglow. This is the first GRB event with a firm upper limit in the 100 MeV -- 30 GeV energy range, associated with an X-ray afterglow., Comment: 7 pages, 4 figures (of which 2 in color), contains online material. Accepted for publication by Astronomy & Astrophysics Letters
Published: 2007

44. HIGH-RESOLUTION TIMING OBSERVATIONS OF SPIN-POWERED PULSARS WITH THE AGILE GAMMA-RAY TELESCOPE

Author: M. Galli, Piergiorgio Picozza, F. Verrecchia, Marco Feroci, Luigi Pacciani, Patrick Weltevrede, F. Mauri, B. Preger, A. Rappoldi, A. W. Chen, G. De Paris, Filippo D'Ammando, E. Vallazza, F. Fuschino, Paolo Esposito, A. Morselli, F. Perotti, Paolo Soffitta, Jules P. Halpern, P. Santolamazza, C. Pittori, T. Froysland, P. Lipari, Fulvio Gianotti, G. Pucella, Ismaël Cognard, A. Argan, A. Giuliani, A. Pellizzoni, Alice K. Harding, Andrea Bulgarelli, Enrico Costa, M. Prest, George Hobbs, M. Fiorini, Paolo Giommi, F. Boffelli, N. D'Amico, Michael Kramer, L. Salotti, I. Lapshov, A. Zambra, F. Fornari, V. Cocco, Maura Pilia, Francesco Longo, S. Vercellone, E. Del Monte, M. Burgay, Alessio Trois, Sandro Mereghetti, Francesco Lazzarotto, G. Barbiellini, Andrea Possenti, P. W. Cattaneo, V. Vittorini, P. A. Caraveo, M. Trifoglio, Simon Johnston, I. Donnarumma, Marco Tavani, Martino Marisaldi, Claudio Labanti, D. Zanello, Richard N. Manchester, G. Di Cocco, Massimo Rapisarda, Aidan Hotan, Y. Evangelista, J. Palfreyman, Pellizzoni A, Pilia M, Possenti A, Fornari F, Caraveo P, Del Monte E, Mereghetti S, Tavani M, Argan A, Trois A, Burgay M, Chen A, Cognard I, Costa E, D'Amico N, Esposito P, Evangelista Y, Feroci M, Fuschino F, Giuliani A, Halpern J, Hobbs G, Hotan A, Johnston S, Kramer M, Longo F, Manchester RN, Marisaldi M, Palfreyman J, Weltevrede P, Barbiellini G, Boffelli F, Bulgarelli A, Cattaneo PW, Cocco V, DAmmando F, De Paris G, Di Cocco G, Donnarumma I, Fiorini M, Froysland T, Galli M, Gianotti F, Harding A, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Mauri F, Morselli A, Pacciani L, Perotti F, Picozza P, Prest M, Pucella G, Rapisarda M, Rappoldi A, Soffitta P, Trifoglio M, Vallazza E, Vercellone S, Vittorini V, Zambra A, Zanello D, Pittori C, Verrecchia F, Preger B, Santolamazza P, Giommi P, Salotti L, A., Pellizzoni, M., Pilia, A., Possenti, F., Fornari, P., Caraveo, E. D., Monte, S., Mereghetti, M., Tavani, A., Argan, A., Troi, M., Burgay, A., Chen, I., Cognard, E., Costa, N., D'Amico, P., Esposito, Y., Evangelista, M., Feroci, F., Fuschino, A., Giuliani, J., Halpern, G., Hobb, A., Hotan, S., Johnston, M., Kramer, Longo, Francesco, R. N., Manchester, M., Marisaldi, J., Palfreyman, P., Weltevrede, G., Barbiellini, F., Boffelli, A., Bulgarelli, P. W., Cattaneo, V., Cocco, F., D'Ammando, G. D., Pari, G. D., Cocco, I., Donnarumma, M., Fiorini, T., Froysland, M., Galli, F., Gianotti, A., Harding, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, F., Mauri, A., Morselli, L., Pacciani, F., Perotti, P., Picozza, M., Prest, G., Pucella, M., Rapisarda, A., Rappoldi, P., Soffitta, M., Trifoglio, E., Vallazza, S., Vercellone, V., Vittorini, A., Zambra, D., Zanello, C., Pittori, F., Verrecchia, B., Preger, P., Santolamazza, P., Giommi, and L., Salotti
Subjects: Agile, Photon, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, High Energy Gamma-ray Astronomy, Pulsar, AGILE satellite, pulsar, Vela, X-ray and gamma detection, Spin-½, Physics, business.industry, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Phaser, Space and Planetary Science, Satellite, gamma rays: observations – pulsars: general – pulsars: individual (Vela, Crab, Geminga, PSR B 1706-44) – stars: neutron, business, Agile software development, Fermi Gamma-ray Space Telescope
Abstract: AGILE is a small gamma-ray astronomy satellite mission of the Italian Space Agency dedicated to high-energy astrophysics launched in 2007 April. Its 1 microsecond absolute time tagging capability coupled with a good sensitivity in the 30 MeV-30 GeV range, with simultaneous X-ray monitoring in the 18-60 keV band, makes it perfectly suited for the study of gamma-ray pulsars following up on the CGRO/EGRET heritage. In this paper we present the first AGILE timing results on the known gamma-ray pulsars Vela, Crab, Geminga and B 1706-44. The data were collected from 2007 July to 2008 April, exploiting the mission Science Verification Phase, the Instrument Timing Calibration and the early Observing Pointing Program. Thanks to its large field of view, AGILE collected a large number of gamma-ray photons from these pulsars (about 10,000 pulsed counts for Vela) in only few months of observations. The coupling of AGILE timing capabilities, simultaneous radio/X-ray monitoring and new tools aimed at precise photon phasing, exploiting also timing noise correction, unveiled new interesting features at sub-millisecond level in the pulsars' high-energy light-curves., Accepted for publication in The Astrophysical Journal. 14 pages in emulate-apj style, 2 tables, 9 figures (1 color). Replacement corrected Figure 6
Published: 2009

45. THE JUNE 2008 FLARE OF MARKARIAN 421 FROM OPTICAL TO TeV ENERGIES

Author: I. Donnarumma, V. Vittorini, S. Vercellone, E. Del Monte, M. Feroci, F. D'Ammando, L. Pacciani, A. W. Chen, M. Tavani, A. Bulgarelli, A. Giuliani, F. Longo, G. Pucella, A. Argan, G. Barbiellini, F. Boffelli, P. Caraveo, P. W. Cattaneo, V. Cocco, E. Costa, G. De Paris, G. Di Cocco, Y. Evangelista, M. Fiorini, T. Froysland, M. Frutti, F. Fuschino, M. Galli, F. Gianotti, C. Labanti, I. Lapshov, F. Lazzarotto, P. Lipari, M. Marisaldi, M. Mastropietro, S. Mereghetti, E. Morelli, A. Morselli, A. Pellizzoni, F. Perotti, P. Picozza, G. Porrovecchio, M. Prest, M. Rapisarda, A. Rappoldi, A. Rubini, P. Soffitta, M. Trifoglio, A. Trois, E. Vallazza, A. Zambra, D. Zanello, C. Pittori, P. Santolamazza, F. Verrecchia, P. Giommi, S. Colafrancesco, L. Salotti, M. Villata, C. M. Raiteri, W. P. Chen, N. V. Efimova, B. Jordan, T. S. Konstantinova, E. Koptelova, O. M. Kurtanidze, V. M. Larionov, J. A. Ros, A. C. Sadun, H. Anderhub, L. A. Antonelli, P. Antoranz, M. Backes, C. Baixeras, S. Balestra, J. A. Barrio, H. Bartko, D. Bastieri, J. Becerra González, J. K. Becker, W. Bednarek, K. Berger, E. Bernardini, A. Biland, R. K. Bock, G. Bonnoli, P. Bordas, D. Borla Tridon, V. Bosch-Ramon, T. Bretz, I. Britvitch, M. Camara, E. Carmona, A. Chilingarian, S. Commichau, J. L. Contreras, J. Cortina, M. T. Costado, S. Covino, V. Curtef, F. Dazzi, A. De Angelis, E. De Cea del Pozo, R. de los Reyes, B. De Lotto, M. De Maria, F. De Sabata, C. Delgado Mendez, A. Dominguez, D. Dorner, M. Doro, D. Elsaesser, M. Errando, D. Ferenc, E. Fernández, R. Firpo, M. V. Fonseca, L. Font, N. Galante, R. J. García López, M. Garczarczyk, M. Gaug, F. Goebel, D. Hadasch, M. Hayashida, A. Herrero, D. Höhne-Mönch, J. Hose, C. C. Hsu, S. Huber, T. Jogler, D. Kranich, A. La Barbera, A. Laille, E. Leonardo, E. Lindfors, S. Lombardi, M. López, E. Lorenz, P. Majumdar, G. Maneva, N. Mankuzhiyil, K. Mannheim, L. Maraschi, M. Mariotti, M. Martínez, D. Mazin, M. Meucci, M. Meyer, J. M. Miranda, R. Mirzoyan, J. Moldón, M. Moles, A. Moralejo, D. Nieto, K. Nilsson, J. Ninkovic, I. Oya, R. Paoletti, J. M. Paredes, M. Pasanen, D. Pascoli, F. Pauss, R. G. Pegna, M. A. Perez-Torres, M. Persic, L. Peruzzo, F. Prada, E. Prandini, N. Puchades, A. Raymers, W. Rhode, M. Ribó, J. Rico, M. Rissi, A. Robert, S. Rügamer, A. Saggion, T. Y. Saito, M. Salvati, M. Sanchez-Conde, P. Sartori, K. Satalecka, V. Scalzotto, V. Scapin, T. Schweizer, M. Shayduk, K. Shinozaki, S. N. Shore, N. Sidro, A. Sierpowska-Bartosik, A. Sillanpää, J. Sitarek, D. Sobczynska, F. Spanier, A. Stamerra, L. S. Stark, L. Takalo, F. Tavecchio, P. Temnikov, D. Tescaro, M. Teshima, M. Tluczykont, D. F. Torres, N. Turini, H. Vankov, A. Venturini, V. Vitale, R. M. Wagner, W. Wittek, V. Zabalza, F. Zandanel, R. Zanin, J. Zapatero, V. Acciari, E. Aliu, T. Arlen, M. Beilicke, W. Benbow, S. M. Bradbury, J. H. Buckley, V. Bugaev, Y. Butt, K. Byrum, A. Cannon, A. Cesarini, Y. C. Chow, L. Ciupik, P. Cogan, P. Colin, W. Cui, M. K. Daniel, R. Dickherber, C. Duke, T. Ergin, S. J. Fegan, J. P. Finley, G. Finnegan, P. Fortin, A. Furniss, D. Gall, G. H. Gillanders, R. Guenette, G. Gyuk, J. Grube, D. Hanna, J. Holder, D. Horan, C. M. Hui, T. Brian Humensky, A. Imran, P. Kaaret, N. Karlsson, M. Kertzman, D. Kieda, J. Kildea, A. Konopelko, H. Krawczynski, F. Krennrich, M. J. Lang, S. LeBohec, G. Maier, A. McCann, M. McCutcheon, A. Milovanovic, P. Moriarty, T. Nagai, R. A. Ong, A. N. Otte, D. Pandel, J. S. Perkins, A. Pichel, M. Pohl, K. Ragan, L. C. Reyes, P. T. Reynolds, E. Roache, H. J. Rose, M. Schroedter, G. H. Sembroski, A. W. Smith, D. Steele, S. P. Swordy, M. Theiling, J. A. Toner, L. Valcarcel, A. Varlotta, S. P. Wakely, J. E. Ward, T. C. Weekes, A. Weinstein, D. A. Williams, S. Wissel, M. Wood, B. Zitzer, I., Donnarumma, V., Vittorini, S., Vercellone, E. D., Monte, M., Feroci, F., D'Ammando, L., Pacciani, A. W., Chen, M., Tavani, A., Bulgarelli, A., Giuliani, Longo, Francesco, G., Pucella, A., Argan, G., Barbiellini, F., Boffelli, P., Caraveo, P. W., Cattaneo, V., Cocco, E., Costa, G. D., Pari, G. D., Cocco, Y., Evangelista, M., Fiorini, T., Froysland, M., Frutti, F., Fuschino, M., Galli, F., Gianotti, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, M., Marisaldi, M., Mastropietro, S., Mereghetti, E., Morelli, A., Morselli, A., Pellizzoni, F., Perotti, P., Picozza, G., Porrovecchio, M., Prest, M., Rapisarda, A., Rappoldi, A., Rubini, P., Soffitta, M., Trifoglio, A., Troi, E., Vallazza, A., Zambra, D., Zanello, C., Pittori, P., Santolamazza, F., Verrecchia, P., Giommi, S., Colafrancesco, L., Salotti, M., Villata, C. M., Raiteri, W. P., Chen, N. V., Efimova, B., Jordan, T. S., Konstantinova, E., Koptelova, O. M., Kurtanidze, V. M., Larionov, J. A., Ro, A. C., Sadun, H., Anderhub, L. A., Antonelli, P., Antoranz, M., Backe, C., Baixera, S., Balestra, J. A., Barrio, H., Bartko, D., Bastieri, J. B., Gonzalez, J. K., Becker, W., Bednarek, K., Berger, E., Bernardini, A., Biland, R. K., Bock, G., Bonnoli, P., Borda, D. B., Tridon, V., Bosch Ramon, T., Bretz, I., Britvitch, M., Camara, E., Carmona, A., Chilingarian, S., Commichau, J. L., Contrera, J., Cortina, M. T., Costado, S., Covino, V., Curtef, F., Dazzi, A. D., Angeli, E. D., Del Pozo, R. D., Reye, B. D., Lotto, M. D., Maria, F. D., Sabata, C. D., Mendez, A., Dominguez, D., Dorner, M., Doro, D., Elsaesser, M., Errando, D., Ferenc, E., Fernandez, R., Firpo, M. V., Fonseca, L., Font, N., Galante, R. J. G., Lopez, M., Garczarczyk, M., Gaug, F., Goebel, D., Hadasch, M., Hayashida, A., Herrero, D., Hohne Monch, J., Hose, C. C., Hsu, S., Huber, T., Jogler, D., Kranich, A. L., Barbera, A., Laille, E., Leonardo, E., Lindfor, S., Lombardi, M., Lopez, E., Lorenz, P., Majumdar, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, M., Mariotti, M., Martinez, D., Mazin, M., Meucci, M., Meyer, J. M., Miranda, R., Mirzoyan, J., Moldon, M., Mole, A., Moralejo, D., Nieto, K., Nilsson, J., Ninkovic, I., Oya, R., Paoletti, J. M., Parede, M., Pasanen, D., Pascoli, F., Pau, R. G., Pegna, M. A., Perez Torre, M., Persic, L., Peruzzo, F., Prada, E., Prandini, N., Puchade, A., Raymer, W., Rhode, M., Ribo, J., Rico, M., Rissi, A., Robert, S., Rugamer, A., Saggion, T. Y., Saito, M., Salvati, M., Sanchez Conde, P., Sartori, K., Satalecka, V., Scalzotto, V., Scapin, T., Schweizer, M., Shayduk, K., Shinozaki, S. N., Shore, N., Sidro, A., Sierpowska Bartosik, A., Sillanpaa, J., Sitarek, D., Sobczynska, F., Spanier, A., Stamerra, L. S., Stark, L., Takalo, F., Tavecchio, P., Temnikov, D., Tescaro, M., Teshima, M., Tluczykont, D. F., Torre, N., Turini, H., Vankov, A., Venturini, V., Vitale, R. M., Wagner, W., Wittek, V., Zabalza, F., Zandanel, R., Zanin, J., Zapatero, V., Acciari, E., Aliu, T., Arlen, M., Beilicke, W., Benbow, S. M., Bradbury, J. H., Buckley, V., Bugaev, Y., Butt, K., Byrum, A., Cannon, A., Cesarini, Y. C., Chow, L., Ciupik, P., Cogan, P., Colin, W., Cui, M. K., Daniel, R., Dickherber, C., Duke, T., Ergin, S. J., Fegan, J. P., Finley, G., Finnegan, P., Fortin, A., Furni, D., Gall, G. H., Gillander, R., Guenette, G., Gyuk, J., Grube, D., Hanna, J., Holder, D., Horan, C. M., Hui, T. B., Humensky, A., Imran, P., Kaaret, N., Karlsson, M., Kertzman, D., Kieda, J., Kildea, A., Konopelko, H., Krawczynski, F., Krennrich, M. J., Lang, S., Lebohec, G., Maier, A., Mccann, M., Mccutcheon, A., Milovanovic, P., Moriarty, T., Nagai, R. A., Ong, A. N., Otte, D., Pandel, J. S., Perkin, A., Pichel, M., Pohl, K., Ragan, L. C., Reye, P. T., Reynold, E., Roache, H. J., Rose, M., Schroedter, G. H., Sembroski, A. W., Smith, D., Steele, S. P., Swordy, M., Theiling, J. A., Toner, L., Valcarcel, A., Varlotta, S. P., Wakely, J. E., Ward, T. C., Weeke, A., Weinstein, D. A., William, S., Wissel, M., Wood, B., Zitzer, Donnarumma I, Vittorini V, Vercellone S, del Monte E, Feroci M, DAmmando F, Pacciani L, Chen A W, Tavani M, Bulgarelli A, Giuliani A, Longo F, Pucella G, Argan A, Barbiellini G, Boffelli F, Caraveo P, Cattaneo P W, Cocco V, Costa E, DeParis G, Di Cocco G, Evangelista Y, Fiorini M, Froysland T, Frutti M, Fuschino F, Galli M, Gianotti F, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Marisaldi M, Mastropietro M, Mereghetti S, Morelli E, Morselli A, Pellizzoni A, Perotti F, Picozza P, Porrovecchio G, Prest M, Rapisarda M, Rappoldi A, Rubini A, Soffitta P, Trifoglio M, Trois A, Vallazza E, Zambra A, Zanello D, Pittori C, Santolamazza P, Verrecchia F, Giommi P, Colafrancesco S, Salotti L, Villata M, Raiteri C M, Chen W P, Efimova N V, Jordan B, Konstantinova T S, Koptelova E, Kurtanidze O M, Larionov V M, Ros J A, Sadun A C, Anderhub H, Antonelli L A, Antoranz P, Backes M, Baixeras C, Balestra S, Barrio J A, Bartko H, Bastieri D, González J Becerra, Becker J K, Bednarek W, Berger K, Bernardini E, Biland A, Bock R K, Bonnoli G, Bordas P, Tridon D Borla, Bosch-Ramon V, Bretz T, Britvitch I, Camara M, Carmona E, Chilingarian A, Commichau S, Contreras J L, Cortina J, Costado M T, Covino S, Curtef V, Dazzi F, DeAngelis A, DeCea del Pozo E, de los Reyes R, DeLotto B, DeMaria M, DeSabata F, Mendez C Delgado, Dominguez A, Dorner D, Doro M, Elsaesser D, Errando M, Ferenc D, Fernández E, Firpo R, Fonseca M V, Font L, Galante N, García López R J, Garczarczyk M, Gaug M, Goebel F, Hadasch D, Hayashida M, Herrero A, Höhne-Mönch D, Hose J, Hsu C C, Huber S, Jogler T, Kranich D, La Barbera A, Laille A, Leonardo E, Lindfors E, Lombardi S, López M, Lorenz E, Majumdar P, Maneva G, Mankuzhiyil N, Mannheim K, Maraschi L, Mariotti M, Martínez M, Mazin D, Meucci M, Meyer M, Miranda J M, Mirzoyan R, Moldón J, Moles M, Moralejo A, Nieto D, Nilsson K, Ninkovic J, Oya I, Paoletti R, Paredes J M, Pasanen M, Pascoli D, Pauss F, Pegna R G, Perez-Torres M A, Persic M, Peruzzo L, Prada F, Prandini E, Puchades N, Raymers A, Rhode W, Ribó M, Rico J, Rissi M, Robert A, Rügamer S, Saggion A, Saito T Y, Salvati M, Sanchez-Conde M, Sartori P, Satalecka K, Scalzotto V, Scapin V, Schweizer T, Shayduk M, Shinozaki K, Shore S N, Sidro N, Sierpowska-Bartosik A, Sillanpää A, Sitarek J, Sobczynska D, Spanier F, Stamerra A, Stark L S, Takalo L, Tavecchio F, Temnikov P, Tescaro D, Teshima M, Tluczykont M, Torres D F, Turini N, Vankov H, Venturini A, Vitale V, Wagner R M, Wittek W, Zabalza V, Zandanel F, Zanin R, Zapatero J, Acciari V, Aliu E, Arlen T, Beilicke M, Benbow W, Bradbury S M, Buckley J H, Bugaev V, Butt Y, Byrum K, Cannon A, Cesarini A, Chow Y C, Ciupik L, Cogan P, Colin P, Cui W, Daniel M K, Dickherber R, Duke C, Ergin T, Fegan S J, Finley J P, Finnegan G, Fortin P, Furniss A, Gall D, Gillanders G H, Guenette R, Gyuk G, Grube J, Hanna D, Holder J, Horan D, Hui C M, Humensky T Brian, Imran A, Kaaret P, Karlsson N, Kertzman M, Kieda D, Kildea J, Konopelko A, Krawczynski H, Krennrich F, Lang M J, LeBohec S, Maier G, McCann A, McCutcheon M, Milovanovic A, Moriarty P, Nagai T, Ong R A, Otte A N, Pandel D, Perkins J S, Pichel A, Pohl M, Ragan K, Reyes L C, Reynolds P T, Roache E, Rose H J, Schroedter M, Sembroski G H, Smith A W, Steele D, Swordy S P, Theiling M, Toner J A, Valcarcel L, Varlotta A, Wakely S P, Ward J E, Weekes T C, Weinstein A, Williams D A, Wissel S, Wood M, and Zitzer B
Subjects: campaign, Raigs còsmics, BL Lacertae: individual: Mrk421, galaxies: jets, X-Rays: Galaxies, gamma rays: observations, radiation mechanisms: nonthermal, bl-lacertae objects, blazars, Flux, Astrophysics, 01 natural sciences, 7. Clean energy, High Energy Gamma-ray Astronomy, law.invention, Raigs gamma, law, optical, MAGIC (telescope), Agile, blazr, X-ray, gamma, high energy observation, 010303 astronomy & astrophysics, webt, Physics, x-ray-spectra, Astrophysics (astro-ph), gamma-rays, lac objects, xmm-newton, Spectral energy distribution, Electrónica, Física nuclear, Raigs X, Electricidad, Flare, outburst, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, 0103 physical sciences, X-rays, BL Lacertae objects: individual (Mrk 421) – gamma rays: observations – galaxies: jets – radiation mechanisms: non-thermal – X-rays: galaxies, Blazar, Cosmic rays, 010308 nuclear & particles physics, Gamma rays, Astronomy and Astrophysics, Active Galactic Nuclei, radiation mechanisms: non-thermal, Light curve, Galaxies, Galàxies, MAGIC telescope, Space and Planetary Science, Very High Energy Gamma-ray Astronomy, ddc:520, AGILE satellite, bl lacertae objects: individual (mrk 421), Energy (signal processing), Lepton
Abstract: We present optical, X-ray, high energy ($\lessapprox 30$ GeV) and very high energy ($\gtrapprox 100$ GeV; VHE) observations of the high-frequency peaked blazar Mrk 421 taken between 2008 May 24 and June 23. A high energy $\gamma$-ray signal was detected by AGILE with \sqrt{TS}=4.5 on June 9--15, with $F(E>100 \mathrm{MeV})= 42^{+14}_{-12}\times 10^{-8}$ photons cm$^{-2}$ s$^{-1}$. This flaring state is brighter than the average flux observed by EGRET by a factor of $\sim$3, but still consistent with the highest EGRET flux. In hard X-rays (20-60 keV) SuperAGILE resolved a 5-day flare (June 9-15) peaking at $\sim$ 55 mCrab. SuperAGILE, RXTE/ASM and Swift/BAT data show a correlated flaring structure between soft and hard X-rays. Hints of the same flaring behavior are also detected in the simultaneous optical data provided by the GASP-WEBT. A Swift/XRT observation near the flaring maximum revealed the highest 2-10 keV flux ever observed from this source, of 2.6 $\times 10^{-9}$ erg cm$^{-2}$ s$^{-1}$ (i.e. > 100 mCrab). A peak synchrotron energy of $\sim$3 keV was derived, higher than typical values of $\sim$0.5-1 keV. VHE observations with MAGIC and VERITAS on June 6-8 show the flux peaking in a bright state, well correlated with the X-rays. This extraordinary set of simultaneous data, covering a twelve-decade spectral range, allowed for a deep analysis of the spectral energy distribution as well as of correlated light curves. The $\gamma$-ray flare can be interpreted within the framework of the synchrotron self-Compton model in terms of a rapid acceleration of leptons in the jet., Comment: accepted for publication in ApJL, 7 pages, 2 figures, 1 table
Published: 2009

46. High energy variability of 3C 273 during the AGILE multiwavelength campaign of December 2007-January 2008

Author: F. Perotti, V. Vittorini, Y. Evangelista, Marco Feroci, M. Trifoglio, Luigi Pacciani, Mariateresa Fiocchi, A. W. Chen, E. Vallazza, L. A. Antonelli, D. Impiombato, Sandro Mereghetti, Paolo Lipari, P. W. Cattaneo, C. Pittori, V. Cocco, Claudio Labanti, T. Froysland, A. Pellizzoni, Dario Gasparrini, A. Argan, Gino Tosti, A. Giuliani, Andrea Bulgarelli, F. Boffelli, Enrico Costa, I. Donnarumma, L. Salotti, F. Fuschino, G. Di Cocco, I. Lapshov, Fulvio Gianotti, M. Galli, Piergiorgio Picozza, F. Verrecchia, D. Zanello, Francesco Lazzarotto, P. A. Caraveo, Marco Tavani, Massimo Rapisarda, Alessio Trois, M. Prest, Sergio Colafrancesco, Martino Marisaldi, Filippo D'Ammando, Paolo Soffitta, G. Stratta, Francesco Longo, S. Vercellone, A. Morselli, Paolo Giommi, Guido Barbiellini, S. Cutini, E. Del Monte, G. Pucella, L., Pacciani, I., Donnarumma, V., Vittorini, F., D'Ammando, M. T., Fiocchi, D., Impiombato, G., Stratta, F., Verrecchia, A., Bulgarelli, A. W., Chen, A., Giuliani, Longo, Francesco, G., Pucella, S., Vercellone, M., Tavani, A., Argan, G., Barbiellini, F., Boffelli, P. A., Caraveo, P. W., Cattaneo, V., Cocco, E., Costa, E. D., Monte, G. D., Cocco, Y., Evangelista, M., Feroci, T., Froysland, F., Fuschino, M., Galli, F., Gianotti, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, M., Marisaldi, S., Mereghetti, A., Morselli, A., Pellizzoni, F., Perotti, P., Picozza, M., Prest, M., Rapisarda, P., Soffitta, M., Trifoglio, G., Tosti, A., Troi, E., Vallazza, D., Zanello, L. A., Antonelli, S., Colafrancesco, S., Cutini, D., Gasparrini, P., Giommi, C., Pittori, L., Salotti, Pacciani L, Donnarumma I, Vittorini V, DAmmando F, Fiocchi MT, Impiombato D, Stratta G, Verrecchia F, Bulgarelli A, Chen AW, Giuliani A, Longo F, Pucella G, Vercellone S, Tavani M, Argan A, Barbiellini G, Boffelli F, Caraveo PA, Cattaneo PW, Cocco V, Costa E, Del Monte E, Di Cocco G, Evangelista Y, Feroci M, Froysland T, Fuschino F, Galli M, Gianotti F, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Marisaldi M, Mereghetti S, Morselli A, Pellizzoni A, Perotti F, Picozza P, Prest M, Rapisarda M, Soffitta P, Trifoglio M, Tosti G, Trois A, Vallazza E, Zanello D, Antonelli LA, Colafrancesco S, Cutini S, Gasparrini D, Giommi P, Pittori C, and Salotti L
Subjects: High Energy Gamma-ray Astronomy, Active Galactic Nuclei, AGILE satellite, Agile, Photon, multi-wavelength campaign, radio quasar, Astrophysics::High Energy Astrophysical Phenomena, Population, Flux, FOS: Physical sciences, Astrophysics, Electron, gamma rays: observations – galaxies: active – galaxies: quasar: general – galaxies: individual: 3C 273 – radiation mechanisms: non-thermal, Observatory, Egret, education, Physics, education.field_of_study, biology, Astrophysics (astro-ph), Astronomy and Astrophysics, Quasar, Light curve, biology.organism_classification, Space and Planetary Science
Abstract: We report the results of a 3-weeks multi-wavelength campaign on the flat spectrum radio quasar 3C 273 carried out with the AGILE gamma-ray mission, covering the 30 MeV -50 GeV and 18-60 keV, the REM observatory (covering the near-IR and optical), Swift (near-UV/Optical, 0.2-10 keV and 15-50 keV), INTEGRAL (3 - 200 keV) and Rossi XTE (2-12 keV). This is the first observational campaign including gamma-ray data, after the last EGRET observations, more than 8 years ago. Our study was carried out using simultaneous light curves of the source flux from all the involved instruments, in the different energy ranges, in search for correlated variability. Then a time-resolved SED was used for a detailed physical modelling of the emission mechanisms. The source was detected in gamma-rays only in the second week of our campaign. We found indication of a possible anti-correlation between the emission at gamma-rays and at soft and hard X-rays, supported by the complete set of instruments. Instead, optical data do not show short term variability. Only in two EGRET observations (in 1993 and 1997) 3C 273 showed intra-observation variability in gamma-rays. The SED with almost simultaneous data, partially covers the regions of the synchrotron emission, the big blue bump, and the inverse-Compton. The soft X-ray emission is consistent with combined SSC and EC mechanisms, while hard X and gamma-ray emissions are compatible with EC from thermal photons of the disk. The time evolution of the SED is well interpreted and modelled in terms of an acceleration episode of the electrons population, leading to a shift in the IC peak towards higher energies., Comment: Regular paper, Acceped by Astronomy & Astrophysics, 25 pages, 7 tables, 5 figures
Published: 2009

47. AGILE observation of a gamma-ray flare from the blazar 3C 279

Author: A. Morselli, A. W. Chen, P. Giommi, Sandro Mereghetti, P. W. Cattaneo, F. Perotti, I. Donnarumma, Y. Evangelista, A. Argan, A. Trois, Andrea Bulgarelli, S. Colafrancesco, Martino Marisaldi, F. Lazzarotto, Enrico Costa, G. De Paris, P. Picozza, M. Prest, F. Fornari, M. Rapisarda, P. Soffitta, Y. Lapshov, F. Longo, A. Pellizzoni, F. Fuschino, M. Galli, F. Verrecchia, L. Salotti, Marco Tavani, A. Giuliani, B. Preger, C. Pittori, T. Froysland, P. A. Caraveo, G. Tosti, Fulvio Gianotti, V. Cocco, M. Trifoglio, Paolo Lipari, E. Vallazza, A. Rappoldi, Dario Gasparrini, A. Zambra, F. D'Ammando, M. Feroci, M. Fiorini, E. Del Monte, G. Pucella, Domenico Impiombato, Guido Barbiellini, V. Vittorini, P. Santolamazza, Claudio Labanti, D. Zanello, G. Di Cocco, F. Boelli, S. Cutini, L. Pacciani, S. Vercellone, Giuliani A, DAmmando F, Vercellone S, Vittorini V, Chen AW, Donnarumma I, Pacciani L, Pucella G, Trois A, Bulgarelli A, Longo F, Tavani M, Tosti G, Impiombato D, Argan A, Barbiellini F, Boffelli F, Caraveo PA, Cattaneo PW, Cocco V, Costa E, Del Monte E, De Paris G, Di Cocco G, Evangelista Y, Feroci M, Fiorini M, Fornari F, Froysland T, Fuschino F, Galli M, Gianotti F, Labanti C, Lapshov Y, Lazzarotto F, Lipari P, Marisaldi M, Mereghetti S, Morselli A, Pellizzoni A, Perotti F, Picozza P, Prest M, Rapisarda M, Rappoldi A, Soffitta P, Trifoglio M, Vallazza E, Zambra A, Zanello D, Cutini S, Gasparrini D, Pittori C, Preger B, Santolamazza P, Verrecchia F, Giommi P, Colafrancesco S, Salotti L, A., Giuliani, F., D'Ammando, S., Vercellone, V., Vittorini, A. W., Chen, I., Donnarumma, L., Pacciani, G., Pucella, A., Troi, A., Bulgarelli, Longo, Francesco, M., Tavani, G., Tosti, D., Impiombato, A., Argan, F., Barbiellini, F., Boffelli, P. A., Caraveo, P. W., Cattaneo, V., Cocco, E., Costa, E. D., Monte, G. D., Pari, G. D., Cocco, Y., Evangelista, M., Feroci, M., Fiorini, F., Fornari, T., Froysland, F., Fuschino, M., Galli, F., Gianotti, C., Labanti, Y., Lapshov, F., Lazzarotto, P., Lipari, M., Marisaldi, S., Mereghetti, A., Morselli, A., Pellizzoni, F., Perotti, P., Picozza, M., Prest, M., Rapisarda, A., Rappoldi, P., Soffitta, M., Trifoglio, E., Vallazza, A., Zambra, D., Zanello, S., Cutini, D., Gasparrini, C., Pittori, B., Preger, P., Santolamazza, F., Verrecchia, P., Giommi, S., Colafrancesco, and L., Salotti
Subjects: High Energy Gamma-ray Astronomy, Active Galactic Nuclei, AGILE satellite, Agile, Photon, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, X and gamma emission, Astrophysics, gamma-ray flare, law.invention, Telescope, law, gamma rays: observations, galaxies: quasars: individual: 3C 279, quasar, Blazar, Physics, Astrophysics (astro-ph), Compton scattering, Gamma ray, Astronomy and Astrophysics, Quasar, Space and Planetary Science, Spectral energy distribution, Flare
Abstract: Context. We report the detection by the AGILE satellite of an intense gamma-ray flare from the gamma-ray source 3EG J1255-0549, associated to the Flat Spectrum Radio Quasar 3C 279, during the AGILE pointings towards the Virgo Region on 2007 July 9-13. Aims. The simultaneous optical, X-ray and gamma-ray covering allows us to study the spectral energy distribution (SED) and the theoretical models relative to the flaring episode of mid-July. Methods. AGILE observed the source during its Science Performance Verification Phase with its two co-aligned imagers: the Gamma- Ray Imaging Detector (GRID) and the hard X-ray imager (Super-AGILE) sensitive in the 30 MeV - 50 GeV and 18 - 60 keV respectively. During the AGILE observation the source was monitored simultaneously in optical band by the REM telescope and in the X-ray band by the Swift satellite through 4 ToO observations. Results. During 2007 July 9-13 July 2007, AGILE-GRID detected gamma-ray emission from 3C 279, with the source at ~2 deg from the center of the Field of View, with an average flux of (210+-38) 10^-8 ph cm^-2 s^-1 for energy above 100 MeV. No emission was detected by Super-AGILE, with a 3-sigma upper limit of 10 mCrab. During the observation lasted about 4 days no significative gamma-ray flux variation was observed. Conclusions. The Spectral Energy Distribution is modelled with a homogeneous one-zone Synchrotron Self Compton emission plus the contributions by external Compton scattering of direct disk radiation and, to a lesser extent, by external Compton scattering of photons from the Broad Line Region., Accepted for publication in Astronomy and Astrophysics
Published: 2009

48. AGILE detection of variable gamma-ray activity from the blazar S5 0716+714 in September-October 2007

Author: F. Perotti, A. W. Chen, P. Giommi, Dario Gasparrini, Paolo Lipari, L. A. Antonelli, F. Boffelli, Arnaud Ferrari, Sandro Mereghetti, P. W. Cattaneo, Marco Feroci, Luigi Pacciani, D. Carosati, D. Zanello, C. Labanti, Francesco Lazzarotto, C. Pittori, Martino Marisaldi, T. Froysland, A. Argan, M. Pasanen, Valeri M. Larionov, A. Pellizzoni, Andrea Bulgarelli, Enrico Costa, Massimo Frutti, I. Donnarumma, S. Vercellone, G. De Paris, I. Lapshov, F. Fuschino, Massimo Rapisarda, Marco Tavani, Marcello Mastropietro, Fulvio Gianotti, A. Morselli, P. Caraveo, Sergio Colafrancesco, M. Prest, M. Villata, E. Del Monte, Paolo Soffitta, A. Giuliani, Geiland Porrovecchio, M. Galli, Piergiorgio Picozza, Alessio Trois, Ennio Morelli, F. Verrecchia, Massimiliano Fiorini, S. Cutini, P. Santolamazza, G. Pucella, Alda Rubini, Omar M. Kurtanidze, Guido Barbiellini, Y. Evangelista, V. Vittorini, M. Trifoglio, L. Salotti, A. Zambra, Filippo D'Ammando, C. M. Raiteri, Francesco Longo, V. Cocco, A. Rappoldi, E. Vallazza, G. Di Cocco, Chen AW, DAmmando F, Villata M, Raiteri CM, Tavani M, Vittorini V, Bulgarelli A, Donnarumma I, Ferrari A, Giuliani A, Longo F, Pacciani L, Pucella G, Vercellone S, Argan A, Barbiellini G, Boffelli F, Caraveo P, Carosati D, Cattaneo PW, Cocco V, Costa E, Del Monte E, De Paris G, Di Cocco G, Evangelista Y, Feroci M, Fiorini M, Froysland T, Frutti M, Fuschino F, Galli M, Gianotti F, Kurtanidze OM, Labanti C, Lapshov I, Larionov VM, Lazzarotto F, Lipari P, Marisaldi M, Mastropietro M, Mereghetti S, Morelli E, Morselli A, Pasanen M, Pellizzoni A, Perotti F, Picozza P, Porrovecchio G, Prest M, Rapisarda M, Rappoldi A, Rubini A, Soffitta P, Trifoglio M, Trois A, Vallazza E, Zambra A, Zanello D, Cutini S, Gasparrini D, Pittori C, Santolamazza P, Verrecchia F, Giommi P, Antonelli LA, Colafrancesco S, Salotti L, A. W., Chen, F., D'Ammando, M., Villata, C. M., Raiteri, M., Tavani, V., Vittorini, A., Bulgarelli, I., Donnarumma, A., Ferrari, A., Giuliani, Longo, Francesco, L., Pacciani, G., Pucella, S., Vercellone, A., Argan, G., Barbiellini, F., Boffelli, P., Caraveo, D., Carosati, P. W., Cattaneo, V., Cocco, E., Costa, E. D., Monte, G. D., Pari, G. D., Cocco, Y., Evangelista, M., Feroci, M., Fiorini, T., Froysland, M., Frutti, F., Fuschino, M., Galli, F., Gianotti, O. M., Kurtanidze, C., Labanti, I., Lapshov, V. M., Larionov, F., Lazzarotto, P., Lipari, M., Marisaldi, M., Mastropietro, S., Mereghetti, E., Morelli, A., Morselli, M., Pasanen, A., Pellizzoni, F., Perotti, P., Picozza, G., Porrovecchio, M., Prest, M., Rapisarda, A., Rappoldi, A., Rubini, P., Soffitta, M., Trifoglio, A., Troi, E., Vallazza, A., Zambra, D., Zanello, S., Cutini, D., Gasparrini, C., Pittori, P., Santolamazza, F., Verrecchia, P., Giommi, L. A., Antonelli, S., Colafrancesco, and L., Salotti
Subjects: Physics, High Energy Gamma-ray Astronomy, Active Galactic Nuclei, AGILE satellite, Photon, Astrophysics (astro-ph), Gamma ray, Spectral density, FOS: Physical sciences, Astronomy and Astrophysics, BL Lac S5 0716+714, Astrophysics, Light curve, law.invention, Space and Planetary Science, law, gamma rays: observations – galaxies: BL Lacertae objects: general – galaxies: BL Lacertae objects: individual: S5 0716+714, Blazar, Energy (signal processing), Flare, BL Lac object
Abstract: We report the gamma-ray activity from the intermediate BL Lac S5 0716+714 during observations acquired by the AGILE satellite in September and October 2007. These detections of activity were contemporaneous with a period of intense optical activity, which was monitored by GASP-WEBT. This simultaneous optical and gamma-ray coverage allows us to study in detail the light curves, time lags, gamma-ray photon spectrum, and Spectral Energy Distributions (SEDs) during different states of activity. AGILE observed the source with its two co-aligned imagers, the Gamma-Ray Imaging Detector (GRID) and the hard X-ray imager (Super-AGILE), which are sensitive to the 30 MeV-50 GeV and 18-60 keV energy ranges, respectively. Observations were completed in two different periods, the first between 2007 September 4-23, and the second between 2007 October 24-November 1. Over the period 2007 September 7-12, AGILE detected gamma-ray emission from the source at a significance level of 9.6-sigma with an average flux (E>100 MeV) of (97 +/- 15) x 10^{-8} photons cm^{-2} s^{-1}, which increased by a factor of at least four within three days. No emission was detected by Super-AGILE for the energy range 18-60 keV to a 3-sigma upper limit of 10 mCrab in 335 ksec. In October 2007, AGILE repointed toward S5 0716+714 following an intense optical flare, measuring an average flux of (47 +/- 11) x 10^{-8} photons cm^{-2} s^{-1} at a significance level of 6.0-sigma. The gamma-ray flux of S5 0716+714 detected by AGILE is the highest ever detected for this blazar and one of the most intense gamma-ray fluxes detected from a BL Lac object. The SED of mid-September appears to be consistent with the synchrotron self-Compton (SSC) emission model, but only by including two SSC components of different variabilities., 5 pages, 5 figures, accepted by A&A Letters 18/8/2008
Published: 2008

49. AGILE detection of delayed gamma-ray emission from GRB 080514B

Author: Paolo Soffitta, Martino Marisaldi, A. Giuliani, A. Rappoldi, E. Vallazza, Francesco Longo, S. Cutini, Y. Evangelista, Andrea Rossi, I. G. Mitrofanov, K. L. Page, I. Donnarumma, A. W. Chen, C. Pittori, F. Perotti, Marco Feroci, Marco Tavani, Luigi Pacciani, Fulvio Gianotti, A. Pellizzoni, Sandro Mereghetti, P. W. Cattaneo, F. Fuschino, S. Vercellone, William V. Boynton, Kevin Hurley, E. Del Monte, Francesco Lazzarotto, A. Argan, Alessio Trois, Andrea Bulgarelli, Enrico Costa, P. A. Caraveo, P. Lipari, B. Preger, Paolo Esposito, Filippo D'Ammando, D. Zanello, G. Piano, M. Trifoglio, Guido Barbiellini, F. Fornari, M. Prest, G. Pucella, M. Fiorini, P. Santolamazza, Neil Gehrels, Massimo Rapisarda, M. Galli, Piergiorgio Picozza, F. Verrecchia, I. Lapshov, F. Boffelli, A. Morselli, David N. Burrows, L. Salotti, Claudio Labanti, G. Di Cocco, Giuliani A, Mereghetti S, Fornari F, Del Monte E, Feroci M, Marisaldi M, Esposito P, Perotti F, Tavani M, Argan A, Barbiellini G, Boffelli F, Bulgarelli A, Caraveo P, Cattaneo PW, Chen AW, Costa E, DAmmando F, Di Cocco G, Donnarumma I, Evangelista Y, Fiorini M, Fuschino F, Galli M, Gianotti F, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Longo F, Morselli A, Pacciani L, Pellizzoni A, Piano G, Picozza P, Prest M, Pucella G, Rapisarda M, Rappoldi A, Soffitta P, Trifoglio M, Trois A, Vallazza E, Vercellone S, Zanello D, Salotti L, Cutini S, Pittori C, Preger B, Santolamazza P, Verrecchia F, Gehrels N, Page K, Burrows D, Rossi A, Hurley K, Mitrofanov I, Boynton W, A., Giuliani, S., Mereghetti, F., Fornari, E. D., Monte, M., Feroci, M., Marisaldi, P., Esposito, F., Perotti, M., Tavani, A., Argan, G., Barbiellini, F., Boffelli, A., Bulgarelli, P., Caraveo, P. W., Cattaneo, A. W., Chen, E., Costa, F., D'Ammando, G. D., Cocco, I., Donnarumma, Y., Evangelista, M., Fiorini, F., Fuschino, M., Galli, F., Gianotti, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, Longo, Francesco, A., Morselli, L., Pacciani, A., Pellizzoni, G., Piano, P., Picozza, M., Prest, G., Pucella, M., Rapisarda, A., Rappoldi, P., Soffitta, M., Trifoglio, A., Troi, E., Vallazza, S., Vercellone, D., Zanello, L., Salotti, S., Cutini, C., Pittori, B., Preger, P., Santolamazza, F., Verrecchia, N., Gehrel, K., Page, D., Burrow, A., Rossi, K., Hurley, I., Mitrofanov, and W., Boynton
Subjects: Photon, gamma rays: bursts, Astrophysics::High Energy Astrophysical Phenomena, AGILE, satellite, GRB 080514B, X and gamma ray, Phase (waves), FOS: Physical sciences, Astrophysics, High Energy Gamma-ray Astronomy, law.invention, Telescope, law, Egret, Physics, biology, Astrophysics (astro-ph), Gamma ray, Astronomy and Astrophysics, Dead time, biology.organism_classification, Gamma-ray Bursts, AGILE satellite, Space and Planetary Science, Gamma-ray Burst, Interplanetary spaceflight, Gamma-ray burst
Abstract: GRB 080514B is the first gamma ray burst (GRB), since the time of EGRET, for which individual photons of energy above several tens of MeV have been detected with a pair-conversion tracker telescope. This burst was discovered with the Italian AGILE gamma-ray satellite. The GRB was localized with a cooperation by AGILE and the interplanetary network (IPN). The gamma-ray imager (GRID) estimate of the position, obtained before the SuperAGILE-IPN localization, is found to be consistent with the burst position. The hard X-ray emission observed by SuperAGILE lasted about 7 s, while there is evidence that the emission above 30 MeV extends for a longer duration (at least ~13 s). Similar behavior was seen in the past from a few other GRBs observed with EGRET. However, the latter measurements were affected, during the brightest phases, by instrumental dead time effects, resulting in only lower limits to the burst intensity. Thanks to the small dead time of the AGILE/GRID we could assess that in the case of GRB 080514B the gamma-ray to X-ray flux ratio changes significantly between the prompt and extended emission phase., Comment: A&A letters, in press
Published: 2008

50. AGILE detection of intense gamma-ray emission from the blazar PKS 1510-089

Author: C. Pittori, T. Froysland, A. Pellizzoni, Alessio Trois, Margo F. Aller, H. D. Aller, F. Boffelli, Filippo D'Ammando, Marco Feroci, D. Zanello, Luigi Pacciani, G. Pucella, F. Perotti, Fulvio Gianotti, C. M. Raiteri, A. Rappoldi, E. Vallazza, E. Del Monte, Francesco Longo, A. W. Chen, G. De Paris, V. Cocco, Francesco Lazzarotto, Y. Evangelista, Marco Tavani, S. Cutini, G. Di Cocco, M. Prest, Sergio Colafrancesco, M. Villata, L. A. Antonelli, Sandro Mereghetti, P. W. Cattaneo, I. Donnarumma, A. Argan, M. Fiorini, Massimo Rapisarda, D. Carosati, P. Lipari, Andrea Bulgarelli, Dario Gasparrini, F. Fuschino, Enrico Costa, Martino Marisaldi, V. Vittorini, Valeri M. Larionov, M. Trifoglio, A. Giuliani, I. Lapshov, A. Morselli, P. A. Caraveo, Claudio Labanti, M. Galli, Piergiorgio Picozza, F. Verrecchia, L. Salotti, A. Zambra, Guido Barbiellini, R. Ligustri, Paolo Giommi, S. Vercellone, Paolo Soffitta, G., Pucella, V., Vittorini, F., D'Ammando, M., Tavani, C. M., Raiteri, M., Villata, A., Argan, G., Barbiellini, F., Boffelli, A., Bulgarelli, P., Caraveo, P. W., Cattaneo, A. W., Chen, V., Cocco, E., Costa, E., Delmonte, G. D., Pari, G. D., Cocco, I., Donnarumma, Y., Evangelista, M., Feroci, M., Fiorini, T., Froysland, F., Fuschino, M., Galli, F., Gianotti, A., Giuliani, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, Longo, Francesco, M., Marisaldi, S., Mereghetti, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, P., Picozza, M., Prest, M., Rapisarda, A., Rappoldi, P., Soffitta, M., Trifoglio, A., Troi, E., Vallazza, S., Vercellone, A., Zambra, D., Zanello, L. A., Antonelli, S., Colafrancesco, S., Cutini, D., Gasparrini, P., Giommi, C., Pittori, F., Verrecchia, L., Salotti, M. F., Aller, H. D., Aller, D., Carosati, V. M., Larionov, R., Ligustri, Pucella G, Vittorini V, DAmmando F, Tavani M, Raiteri CM, Villata M, Argan A, Barbiellini G, Boffelli F, Bulgarelli A, Caraveo P, Cattaneo PW, Chen AW, Cocco V, Costa E, DelMonte E, De Paris G, Di Cocco G, Donnarumma I, Evangelista Y, Feroci M, Fiorini M, Froysland T, Fuschino F, Galli M, Gianotti F, Giuliani A, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Longo F, Marisaldi M, Mereghetti S, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Picozza P, Prest M, Rapisarda M, Rappoldi A, Soffitta P, Trifoglio M, Trois A, Vallazza E, Vercellone S, Zambra A, Zanello D, Antonelli LA, Colafrancesco S, Cutini S, Gasparrini D, Giommi P, Pittori C, Verrecchia F, Salotti L, Aller MF, Aller HD, Carosati D, Larionov VM, and Ligustri R
Subjects: High Energy Gamma-ray Astronomy, Active Galactic Nuclei, AGILE satellite, Photon, Astrophysics::High Energy Astrophysical Phenomena, satellite, FOS: Physical sciences, Astrophysics, Photon energy, law.invention, Telescope, AGILE, law, gamma ray satellite, quasar, Blazar, Physics, Astrophysics (astro-ph), Gamma ray, Astronomy and Astrophysics, Quasar, gamma rays: observations -- radiation mechanisms: non-thermal -- quasars: individual: PKS 1510-089, Space and Planetary Science, Spectral energy distribution, Flare
Abstract: We report the detection by the AGILE (Astro-rivelatore Gamma a Immagini LEggero) satellite of an intense gamma-ray flare from the source AGL J1511-0909, associated with the powerful quasar PKS 1510-089, during ten days of observations from 23 August to 1 September 2007. During the observation period, the source was in optical decrease following a flaring event monitored by the GLAST-AGILE Support Program (GASP) of the Whole Earth Blazar Telescope (WEBT). The simultaneous gamma-ray, optical, and radio coverage allows us to study the spectral energy distribution and the theoretical models based on the synchrotron and inverse Compton (IC) emission mechanisms. AGILE observed the source with its two co-aligned imagers, the Gamma-Ray Imaging Detector and the hard X-ray imager Super-AGILE sensitive in the 30 MeV - 50 GeV and 18 - 60 keV bands, respectively. Between 23 and 27 August 2007, AGILE detected gamma-ray emission from PKS 1510-089 when this source was located about 50 degrees off-axis, with an average flux of (270 +/- 65) x 10^{-8} photons cm^{-2} s^{-1} for photon energy above 100 MeV. In the following period, 28 August - 1 September, after a satellite re-pointing, AGILE detected the source at about 35 degrees off-axis, with an average flux (E > 100 MeV) of (195 +/- 30) x 10^{-8} photons cm^{-2} s^{-1}. No emission was detected by Super-AGILE, with a 3-sigma upper limit of 45 mCrab in 200 ksec. The spectral energy distribution is modelled with a homogeneous one-zone synchrotron self Compton (SSC) emission plus contributions by external photons: the SSC emission contributes primarily to the X-ray band, whereas the contribution of the IC from the external disc and the broad line region match the hard gamma-ray spectrum observed., 5 pages, 5 figures, accepted for publication in A&A
Published: 2008
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