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101. Analysis of global Terrestrial Gamma Ray Flashes distribution and special focus on AGILE detections over South America

Author

F. Fuschino, Oscar van der Velde, Joan Montanyà, Ferran Fabró, Martino Marisaldi, Universitat Politècnica de Catalunya. Departament d'Enginyeria Elèctrica, and Universitat Politècnica de Catalunya. LRG - Lightning Research Group

Subjects
Atmospheric Science, 010504 meteorology & atmospheric sciences, Atmospheric physics, FOS: Physical sciences, Atmospheric sciences, 01 natural sciences, Lightning, Altitude, Meteorology, Physics - Space Physics, Diurnal cycle, 0103 physical sciences, BURSTS, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, ITCZ, Intertropical Convergence Zone, Cloud top, High energy radiation, AIR, Terrestrial Gamma ray Flashes, Thunderstorms, CAPE, Space Physics (physics.space-ph), Convective available potential energy, Energies::Energia elèctrica [Àrees temàtiques de la UPC], Geophysics, 13. Climate action, Space and Planetary Science, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], Física atmosfèrica, Thunderstorm, Environmental science, Tropopause
Abstract

Global distribution of the Terrestrial Gamma-ray Flashes (TGFs) detected by AGILE and RHESSI for the period from March 2009 to July 2012 has been analysed. A fourth TGF production region has been distinguished over the Pacific. It is confirmed that TGF occurrence follows the Intertropical Convergence Zone (ITCZ) seasonal migration and prefers afternoons. TGF/lightning ratio appears to be lower over America than other regions suggesting that meteorological regional differences are important for the TGF production. Diurnal cycle of TGFs peaks in the afternoon suggesting that Convective Available Potential Energy (CAPE) and convection are important for TGF production. Moreover all AGILE passages over South America in the same period have been analysed to find meteorological preferences for TGF occurrence. In each passage the analysis of Cloud Top Altitude (CfA), CAPE, number of strokes, number of storms and coverage area of clouds with temperatures below 70 degrees C (Cloud Top Coverage area, CTC) are computed. On average, AGILE has been exposed to 19,100 strokes between each TGF representing similar to 68 h of exposure over active storms. High CAPE values, high cloud tops and high stroke occurrence suggest that meteorological conditions conducive to vigorous and electrically active storms are important for TGF production. It is shown that a high number of thunderstorms is preferable for TGF production which may be explained by a greater chance of the presence of a thunderstorm in the best development stage for TGF production. High tropopause altitude seems to be important but not primordial for TGF production. (C) 2015 Elsevier Ltd. All rights reserved.

Published
2015

102. Detection of multiple TGFs produced by the same thunderstorm system

Author

Alessandro Ursi, Martino Marisaldi, Marco Tavani, Stefano Dietrich, Daniele Casella, and Paolo Sanò

Subjects
satellite, TGF, convection
Abstract

The new on-board configuration of the AGILE satellite enhanced the detection of Terrestrial Gamma-ray Flashes (TGFs) of about one order of magnitude (up to ~100 TGFs/month), making the MiniCALorimeter more sensitive to events, especially on shorter time scales. As a direct consequence of the increased statistics, we observe several cases of more TGFs produced by the same thunderstorm system. Among the 179 TGFs detected in the period 23/03/2015 - 23/06/2015 we identify 15 pairs of consecutive TGFs occurring

Published
2015

103. Silicon drift detectors coupled to CsI(Tl) scintillators for spaceborne gamma-ray detectors

Author

F. Perotti, Martino Marisaldi, Antonio Francesco Longoni, Heike Soltau, Claudio Labanti, Carlo Fiorini, and E. Rossi

Subjects
Physics, Nuclear and High Energy Physics, Scintillation, Photon, sezele, Physics::Instrumentation and Detectors, business.industry, Compton telescope, Detector, Photodetector, Scintillator, Atomic and Molecular Physics, and Optics, Anger Camera, Optics, Optoelectronics, business, Image resolution
Abstract

Silicon Drift Detectors (SDDs), thanks to their peculiar low noise characteristics, have proven to be excellent photodetectors for CsI(Tl) scintillation light detection. Two basic detector configurations have been developed: either a single SDD or a monolithic array of SDDs coupled to a single CsI(Tl) crystal. A 16 independent detectors prototype is under construction, designed to work in conjunction with the MEGA Compton telescope prototype under development at MPE, Garching, Germany. A single SDD coupled to a CsI(Tl) crystal has also been tested as a monolithic detector with an extended energy range between 1.5 keV and 1 MeV. The SDD is used as a direct X-ray detector for low energy photons interacting in silicon and as a scintillation light photodetector for photons interacting in the crystal. The type of interaction is identified by means of pulse shape discrimination technique. Detectors based on an array of SDDs coupled to a single CsI(Tl) crystal have also been built. The readout of these detectors is based on the Anger camera technique, and submillimeter spatial resolution can be achieved. The two detectors' approaches and their applications will be described.

Published
2006

104. The Mini-Calorimeter detector for the AGILE mission

Author

Marco Tavani, Martino Marisaldi, A. Argan, M. Trifoglio, Andrea Bulgarelli, E. Rossi, A. Mauri, Alessandro Traci, G. Di Cocco, Claudio Labanti, and Fulvio Gianotti

Subjects
Physics, Nuclear and High Energy Physics, Calorimeter (particle physics), Physics::Instrumentation and Detectors, business.industry, High-energy astronomy, Astrophysics::High Energy Astrophysical Phenomena, Detector, Gamma ray, Scintillator, Atomic and Molecular Physics, and Optics, Photodiode, law.invention, Optics, law, Optoelectronics, Angular resolution, business, Gamma-ray burst
Abstract

AGILE is an ASI space mission for high energy astrophysics in the gamma ray energy range 30MeV-50GeV, and in the X-ray band (10keV-40keV). AGILE is composed of three detecting systems: a Tungsten-Silicon Tracker, a Csl Mini-Calorimeter and a Silicon based X-ray detector (Super-Agile), plus an anticoincidence system for background rejection. The satellite will have good imaging performances (with angular resolution of a few arc-minutes in the gamma ray band), good timing resolution and a large field of view (about 1/5 of the sky). AGILE high energy detector is composed of a Silicon Tracker, a Mini-Calorimeter, the Anticoincidence and the Data Handling system The Mini-Calorimeter can also work as a stand-alone gamma ray detector in the energy range 250keV-250MeV, with no imaging capabilities, for the detection of transients and gamma ray burst events and for the evaluation of gamma ray background fluctuations. The Mini-Calorimeter is made of 30 independent elements of 37.5 × 2.3 × 1.5 cm stacked in two layers. Each detector scintillator signal is read out via two photodiodes glued on the small surfaces of the bar. The characteristics of the engineering model detectors has been deeply investigated and will be reported.

Published
2006

105. Cosmic rays tracks in the PICsIT instrument onboard the INTEGRAL satellite

Author

Martino Marisaldi, Claudio Labanti, and A. Segreto

Subjects
Physics, Nuclear and High Energy Physics, High energy, Physics::Instrumentation and Detectors, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Cosmic ray, Scintillator, Atomic and Molecular Physics, and Optics, law.invention, Photodiode, Telescope, Optics, law, Satellite, business, Energy (signal processing)
Abstract

The PICsIT (PIxelated CsI Telescope) instrument is the high energy plane of the IBIS imager onboard the INTEGRAL satellite, launched on October 2002 and currently fully operative. PICsIT consists of a 64 × 64 detectors array, each composed of a CsI(Tl) scintillating crystal with p-i-n photodiode readout. Since its first in-orbit activation, several count rate spikes have been detected. The tracks in the detector corresponding to those spikes clearly indicate that their origin is the interaction of cosmic rays with the detector or the satellite structure. Several extended elliptical tracks have been detected, indicating the presence of electromagnetic and hadronic showers initiated by primary cosmic rays interacting with the satellite structure. The tracks morphology and statistics is presented. There is strong evidence that tracks events are due to phosphorescence states excited in the CsI(Tl) crystals by a high energy deposit. Since events due to cosmic rays tracks account for a significant fraction of the instrument background, their rejection is important to improve the instrument sensitivity. Tracks rejection is especially important in those instruments, based on large quantities of alkali halide scintillators, designed to trigger on count rate increases, such as gamma-ray burst monitors. In the PICsIT detector operated in photon-by-photon mode, tracks events rejection can be easily accomplished thanks to the tracks peculiar geometrical and timing characteristics.

Published
2006

106. A pulse shape discrimination gamma-ray detector based on a silicon drift chamber coupled to a CsI(Tl) scintillator: prospects for a 1 keV-1 MeV monolithic detector

Author

Heike Soltau, Claudio Labanti, and Martino Marisaldi

Subjects
Physics, Nuclear and High Energy Physics, Range (particle radiation), Photon, Silicon drift detector, Silicon, Physics::Instrumentation and Detectors, business.industry, Detector, chemistry.chemical_element, Scintillator, Pulse shaping, Semiconductor detector, Optics, Nuclear Energy and Engineering, chemistry, High Energy Physics::Experiment, Electrical and Electronic Engineering, business
Abstract

In this paper, an X- and gamma-ray detector based on a silicon drift detector (SDD) coupled to a CsI(Tl) scintillating crystal is presented. The SDD is operated both as a direct X-ray detector for photons interacting in silicon and as an indirect detector for photons interacting in the scintillator. As interactions in silicon and in CsI yield different amounts of charge per unit energy deposited, discrimination of the place of interaction is necessary to obtain the correct energy. Discrimination of the interaction type is carried out by means of pulse shape discrimination performed with two parallel processing chains with different shaping times. The performance of the detectors are described and discussed. Pulse shape discrimination is possible throughout the detector energy range.

Published
2004

107. Calorimeter prototype based on silicon drift detectors coupled to scintillators for Compton telescopes application

Author

Martino Marisaldi, G. Di Cocco, Claudio Labanti, Elena M. Rossi, Andrea Bulgarelli, M. Trifoglio, A. Mauri, Alessandro Traci, E. Celesti, and Fulvio Gianotti

Subjects
Physics, Calorimeter (particle physics), Physics::Instrumentation and Detectors, business.industry, Detector, Photodetector, Astronomy and Astrophysics, Scintillator, Noise (electronics), Capacitance, Photodiode, law.invention, Optics, Application-specific integrated circuit, Space and Planetary Science, law, business
Abstract

The project of a new calorimeter module for Compton telescopes based on an array of silicon drift detectors (SDD) coupled to thallium activated cesium iodide (CsI(Tl)) scintillating crystals is presented. Because of their low output capacitance and the possibility to have the first amplifying stage directly integrated on chip, SDDs show better noise performances than traditional p-intrinsic-n (PIN) photodiodes. For this reason, SDDs coupled to scintillators show a higher energy resolution than similar systems based on PIN photodiodes. The detectors will be integrated in an array with read-out based on custom made ASIC’s built to match with the SDDs electrical properties. Shaped signals are digitally converted by a Digital Front-End Electronic Board which also takes care of ASICs handshaking. The system architecture is based on the PICsIT instrument on board the INTEGRAL satellite, at present fully operative. In this paper an overview of the instrument will be given and the status of the project will be reported.

Published
2004

108. AGILE, a satellite for high energy γ-ray astrophysics: prospects for the Mini-Calorimeter

Author

G. Di Cocco, A. Mauri, M. Tavani, Fulvio Gianotti, Claudio Labanti, E. Celesti, Elena M. Rossi, A. Argan, Andrea Bulgarelli, M. Galli, Alessandro Traci, M. Trifoglio, and Martino Marisaldi

Subjects
Physics, Photon, Calorimeter (particle physics), Physics::Instrumentation and Detectors, High-energy astronomy, Astrophysics::High Energy Astrophysical Phenomena, Detector, Gamma ray, Astronomy, Astronomy and Astrophysics, Astrophysics, Radiation, Space and Planetary Science, Angular resolution, Gamma-ray burst
Abstract

AGILE is an ASI (Italian Space Agency) small space mission for high energy astrophysics in the gamma ray energy range 30MeV–50GeV, and in the X-ray band 10keV–40keV. AGILE is composed of three scientific detectors: a TungstenSilicon Tracker, a CsI Mini-Calorimeter and a Silicon based X-ray detector (Super-Agile), moreover an anticoincidence system carries out background rejection. The satellite’s payload will have good imaging performances (with angular resolution of a few arc-minutes in the gamma ray band), good timing resolution and a large field of view (about 1/5 of the sky). AGILE detection principle is based on the pair production process that arises from the interaction between high energy photons and the Tungsten layers of the Silicon Tracker. The Silicon Tracker is designed to determine the direction of the incoming radiation, while the Mini-Calorimeter evaluates the energy of the interacting photons. The Mini-Calorimeter can also work as a stand-alone gamma ray detector in the energy range 250keV–250MeV, with no imaging capabilities, for the detection of transients and gamma ray burst events (in cooperation with Super-Agile) and for the evaluation of gamma ray background fluctuations. In this paper a description of the Mini-Calorimeter is done.

Published
2004

109. X-ray imaging and spectroscopy performance of a large area silicon drift chamber for wide-field x-ray astronomy applications

Author

Andrea Vacchi, Alexander Rashevsky, G. Zampa, A. Rubini, Francesco Lazzarotto, Riccardo Campana, Fabio Muleri, F. Fuschino, Piero Malcovati, Ettore Del Monte, M. Feroci, Massimo Rapisarda, Marco Grassi, Enrico Costa, Martino Marisaldi, Claudio Labanti, L. Pacciani, N. Zampa, Giuseppe Baldazzi, V. Bonvicini, Paolo Soffitta, I. Donnarumma, Y. Evangelista, E. Morelli, Marcello Mastropietro, L. Picolli, Gianluigi Zampa, Andrea Vacchi, Marco Feroci, Claudio Labanti, Valter Bonvicini, Alexander Rashevsky, Nicola Zampa, Riccardo Campana, Ettore Del Monte, Yuri Evangelista, Fabio Muleri, Luigi Pacciani, Alda Rubini, Paolo Soffitta, Enrico Costa, Immacolata Donnarumma, Francesco Lazzarotto, Marcello Mastropietro, Ennio Morelli, Massimo Rapisarda, Fabio Fuschino, Martino Marisaldi, Giuseppe Baldazzi, Luca Picolli, Marco Grassi, and and Piero Malcovati

Subjects
Silicon, Physics::Instrumentation and Detectors, High-energy astronomy, Astrophysics::High Energy Astrophysical Phenomena, Silicon Drift Chambers, chemistry.chemical_element, Context (language use), Collimated light, Imaging, law.invention, Optics, law, X-rays, Electronic, Optical and Magnetic Materials, Electrical and Electronic Engineering, SILICON DRIFT DETECTORS, Spectroscopy, X-RAY IMAGING, Room temperature, Physics, X-ray astronomy, High energy astrophysics, Electronic, Optical and Magnetic Materials, Condensed Matter Physics, Computer Science Applications1707 Computer Vision and Pattern Recognition, Applied Mathematics, business.industry, Detector, Particle accelerator, X-RAY ASTRONOMY, chemistry, business
Abstract

In the context of the design of wide-field of view experiments for X-ray astronomy, we studied the response to X-rays in the range between 2 and 60 keV of a large area Silicon Drift Chamber originally designed for particle tracking in high energy physics. We demonstrated excellent imaging and spectroscopy performance of monolithic 53 cm 2 detectors, with position resolution as good as 30 μm and energy resolution in the range 300-570 eV FWHM obtainable at room temperature (20 °C). In this paper we show the results of test campaigns at the X-ray facility at INAF/IASF Rome, aimed at characterizing the detector performance by scanning the detector area with highly collimated spots of monochromatic X-rays. In these tests we used a detector prototype equipped with discrete read-out front-end electronics.

Published
2010

110. On the highest photon energy of Terrestrial Gamma-ray Flashes

Author

Martino Marisaldi (1, Fabio Fuschino (1), Marco Tavani (3), Stefano Dietrich (4), Colin Price (5), Andrea Argan (3), Claudio Labanti (1), Marcello Galli (6), Francesco Longo (7), Ettore Del Monte (3), Guido Barbiellini (7), Andrea Giuliani (8), Andrea Bulgarelli (1), Fulvio Gianotti (1), Massimo Trifoglio (1), Alessio Trois (9), Carlotta Pittori (10), Francesco Verrecchia (10), and Paolo Giommi (10)

Subjects
Astrophysics::High Energy Astrophysical Phenomena
Abstract

TGFs are known to include photons of energy up to several tens of MeV. Results by the AGILE satellite have shown that the cumulative spectrum of TGFs is significantly above background up to about 100 MeV and that the spectral shape deviates from a cutoff power law at high energy suggesting a production mechanism different from canonical Relativistic Runaway Electron Avalanche (RREA). Subsequent analysis of AGILE data have shown that about 15% of TGFs exhibit photon energies above 30 MeV and that these events have different properties than lower energy TGFs. From the theoretical point of view, it has been shown that a production model based on electron acceleration in strong electric fields at lightning leader tips may account for the high energies observed by AGILE. In this presentation we report on the detection of high-energy photons in TGFs for five years of AGILE observation. Possible sources of error such as energy calibration, background and cosmic rays contamination are discussed as well.

Published
2014

111. Search for Gravitational Waves Associated with gamma-ray Bursts Detected by the Interplanetary Network

Author

Robert Stone, A. Di Virgilio, A. R. Williamson, R. P. Croce, Namjun Kim, Xing-Jiang Zhu, S. T. Countryman, V. Necula, I. Santiago-Prieto, Hee-Suk Cho, Heinz-Bernd Eggenstein, A. K. Poteomkin, Tania Regimbau, Chiara M. F. Mingarelli, V. V. Frolov, Riccardo Bassiri, J. B. Kanner, Oscar Reula, F. Carbognani, M. M. Hanke, W. Ortega, H. Fehrmann, S. B. Anderson, C. Maglione, Ruslan Vaulin, E. O. Lebigot, E. Katsavounidis, Ludovico Carbone, P. Couvares, Benno Willke, Jean-Luc Atteia, E. Maros, Stanislav Babak, M. Constancio, Duncan A. Brown, Hans A. Krimm, David B. Tanner, F. Jiménez-Forteza, H. Radkins, Christian Gräf, S. Walsh, Alessandra Buonanno, M. R. Smith, N. Letendre, Jeonghoon Ha, S. P. Vyachanin, T. P. Downes, E. Dominguez, F. Brückner, M. Edwards, B. J. J. Slagmolen, D. Fazi, M. Brinkmann, T. Etzel, H. P. Daveloza, H. Dereli, K. Siellez, N. Mangini, P. Thomas, Benjamin William Allen, Karsten Danzmann, C. Aulbert, R. Cavalieri, M. Pedraza, Stefaan Franco, Maria Alessandra Papa, F. Cavalier, G. Vedovato, D. B. Kozak, C. Vorvick, T. Williams, David Coward, L. Bonelli, C. S. Unnikrishnan, S. H. Huttner, Piotr Jaranowski, Florent Robinet, M. Colombini, Roy Williams, C. J. Guido, Jonathan F. Stebbins, A. Basti, R. Bonnand, Collin Capano, D. Hoske, G. Kang, Karoline Wiesner, Sourav Ghosh, Imre Bartos, A. Rocchi, G. Endroczi, Andrew Melatos, M. Lorenzini, A. Masserot, M. J. Lubinski, M. Punturo, Shane L. Larson, Leopoldo Milano, Slawomir Gras, G. Mazzolo, D. S. Rabeling, M. Factourovich, Ryan DeRosa, Valerie Connaughton, B. M. Levine, V. Quetschke, Bangalore Suryanarayana Sathyaprakash, E. Black, J.-P. Coulon, Martin M. Fejer, J. R. Smith, R. Bork, Z. Frei, S. M. Scott, G. Mendell, S. G. Gaonkar, Mark Hannam, C. Buy, Maik Frede, A. Di Lieto, D. B. Kelley, Jordan Camp, Zhihui Du, C. Osthelder, M. Ducrot, D. O. Bridges, Rebecca Fisher, Prayush Kumar, K. E. Gushwa, G. P. Newton, M. Fyffe, Gabriela Gonzalez, D. Feldbaum, F. Cleva, T. B. Edo, V. D. Pal'Shin, M. A. Bizouard, V. Sequino, J. Betzwieser, Antoine Heidmann, C. C. Yancey, Haixing Miao, S. L. Danilishin, I. Kowalska, Rocco Romano, Markus A. Wimmer, John D. Scott, P. Leaci, A. Colla, Rajesh Kumar, Vladimir B. Braginsky, H. Vahlbruch, G. Bogaert, M. Shaltev, Rosa Poggiani, O. Bock, P. J. Sutton, C. C. Wipf, Alex B. Nielsen, J. H. Romie, J.-D. Fournier, Philip F. Hopkins, A. Mytidis, M. Born, K. Mailand, D. L. Kinzel, R. A. Mercer, W. G. Anderson, G. Cella, Peter Fritschel, Denis Martynov, Howard Pan, Aaron Buikema, R. Mittleman, István Rácz, K. L. Dooley, K. Riles, J. Y. Vinet, F. Frasconi, H. Overmier, Giacomo Ciani, A. Mullavey, D. Nolting, G. Manca, M. Weinert, S. J. Chamberlin, M. Vasúth, L. Cunningham, C. R. Ramet, R. Flaminio, S. Farinon, Lisa Barsotti, E. J. King, I. Fiori, M. Agathos, S. R. Morriss, N. A. Robertson, Q. Chu, B. P. Abbott, E. K. Gustafson, D. E. Clark, Kipp Cannon, M. Steinke, A. Staley, Nelson Christensen, L. Pinard, I. M. Pinto, F. Fidecaro, G. M. Guidi, M. J. Cowart, K. Loew, P. Raffai, R. Douglas, F. J. Raab, M. Pickenpack, J. Hanks, A. Pele, Sanichiro Yoshida, E. Lopez, D. Sellers, A. Kumar, Kevin M. Ryan, A. Moggi, H. J. Bulten, Nergis Mavalvala, M. Boer, Matthew Evans, Yukikatsu Terada, R. S. Ottens, Jerome Degallaix, R. J. G. Jonker, J. Meidam, David Jonathan Hofman, D. Hammer, A. von Kienlin, P. J. Lee, S. Vass, R. Vincent-Finley, Jesper Munch, M. Pichot, Federico Ferrini, Enrico Calloni, G. Traylor, Thomas Corbitt, W. Z. Korth, C. A. Costa, R. Inta, S. Klimenko, A. F. Brooks, Fabrice Matichard, Fumiko Kawazoe, Bala R. Iyer, Riccardo Sturani, L. R. Cominsky, C. Palomba, S. Privitera, S. S. Y. Chua, Roman Schnabel, J. E. Brau, A. A. van Veggel, L. Martinelli, B. Moe, Odylio D. Aguiar, I. W. Martin, B. C. Barish, M. S. Shahriar, S. Mitra, Scott Koranda, E. Saracco, C. Tomlinson, László Gondán, W. Kells, G. Vajente, Kevin Hurley, Graham Woan, H. Augustus, S. Ast, C. M. Reed, W. D. Vousden, C. I. Torrie, R. Gustafson, M. P. Thirugnanasambandam, D. Schuette, D. D. Frederiks, Katrin Dahl, Soma Mukherjee, Drew Keppel, C. Belczynski, Alberto Vecchio, M. A. Barton, Stuart Reid, G. Rajalakshmi, L. Matone, C-H. Lee, D. Barker, Efim A. Khazanov, G. Ballardin, Moritz Mehmet, M. Phelps, M. Branchesi, S. Kim, L. Prokhorov, H. R. Paris, Will M. Farr, J. Dickson, D. Hoak, D. Sentenac, C. L. Mueller, Patrick Brady, Peter Kalmus, Sebastien Biscans, S. Kaufer, Sascha Husa, N. Straniero, Rainer Weiss, D. R. Ingram, David Palmer, Nancy Aggarwal, Tobias Westphal, R. Aptekar, J. C. Batch, Jan Harms, A. S. Sengupta, J. Eichholz, Tobias Eberle, Meng Wang, D.B. DeBra, F. Ricci, R. W. P. Drever, W. W. Johnson, John A. Clark, Ben Farr, I. Yakushin, Jacob Scheuer, Viswanath Bavigadda, Christophe Collette, Ho-Gyu Lee, R. J. S. Greenhalgh, Gavin Davies, M. C. Araya, T. Prestegard, Bernard F. Schutz, Kip S. Thorne, T. Chalermsongsak, Alessandro Bertolini, P. Puppo, David Jones, D. Bersanetti, J. V. van Heijningen, K. A. Hodge, S. Sankar, P. G. Murray, D. Passuello, Thanh Vinh Nguyen, David Blair, S. Roddy, Eric Thrane, T. Kaur, L. Sammut, Tristan Briant, F. Clara, S. Recchia, A. Idrisy, Kevin M. McLin, V. Dolique, C. Baune, D. Ugolini, Sung-Po Chao, J. R. Leong, Fabien Kéfélian, J. H. Hough, C. Lazzaro, B. Hughey, E. C. Ferreira, Anton B. Ivanov, J. Bauchrowitz, M. Razzano, R. M. Magee, Patricia Schmidt, V. Brisson, Marilyne Andersen, S. Raja, S. E. Strigin, Marco Cavaglia, M. Lormand, C. Michel, A. Nitz, M. Tonelli, Larry R. Price, Sarah Caudill, R. De Rosa, Hyun Lee, N. Gehrels, T. Vo, J. Slutsky, R. Quitzow-James, R. Day, Jeffery Kline, Xuan Wang, J. S. Areeda, I. Leonor, V. Loriette, J. D. Lough, D. J. Stops, M. Prijatelj, Douglas R. Cook, R. Coyne, K. A. Thorne, C. Bradaschia, Li Ju, Daniel A. Shaddock, Michele Zanolin, T. Dal Canton, T. J. Massinger, R. Passaquieti, M. Huynh, V. Kalogera, J. Hanson, M. Damjanic, P. Oppermann, Marco Aurelio Diaz, Samaya Nissanke, Michele Vallisneri, M. Leonardi, R. Goetz, C. Bogan, E. Macdonald, G. A. Prodi, I. Nardecchia, F. Ohme, Martino Marisaldi, Laura Cadonati, F. Martelli, Carlos Cepeda, Ik Siong Heng, S. Steplewski, Evan Ochsner, Francesco Salemi, A. J. Weinstein, D. Buskulic, S. E. Zuraw, C. Padilla, Robert J. McCarthy, E. Cuoco, M. Kasprzack, Charlotte Bond, Alessandra Corsi, R. DeSalvo, S. A. Usman, G. D. Hammond, O. V. Palashov, F. Piergiovanni, Linqing Wen, C. Messenger, David Tshilumba, Tarun Souradeep, V. P. Mitrofanov, N. A. Gordon, P. J. Veitch, E. A. Huerta, G. M. Keiser, A. M. Sintes, Lee Samuel Finn, H. Tuennermann, Guido Mueller, Gijs Nelemans, Chandra Kant Mishra, M. V. van der Sluys, S. Golenetskii, Jinhyoung Lee, E. D. Hall, A. L. Stuver, S. Grunewald, J. Zweizig, S. E. Gossan, M. Davier, O. Puncken, S. Meshkov, Seog Oh, D. Moraru, A. W. Heptonstall, Vivien Raymond, Peter R. Saulson, B. Sassolas, E. J. Daw, F. Travasso, Michał Bejger, P. Astone, F. Marion, W. Del Pozzo, N. Leroy, Trevor Sidery, H. Heitmann, Rana X. Adhikari, Chad Hanna, R. Abbott, G. Tellez, K. Williams, C. Wilkinson, Andrew Lundgren, B. Machenschalk, F. Donovan, S. Caride, M. Landry, Lindy Blackburn, V. Kondrashov, L. Di Fiore, D. Amariutei, K. Holt, Andreas Freise, Vincenzo Pierro, Jessica McIver, Chunglee Kim, Paul D. Lasky, Gianpietro Cagnoli, S. D'Antonio, Sebastian Steinlechner, L. Kuo, H. Yamamoto, A. Effler, Paolo Addesso, K. D. Giardina, I. Di Palma, A. Cumming, A. Alemic, Y. Minenkov, F. Garufi, R. Burman, David Murphy, D. Lodhia, E. Genin, Joshua Yablon, G. May, M. Barsuglia, S. Chung, A. Conte, V. Sandberg, Ping Koy Lam, G. Debreczeni, Alexander Khalaidovski, F. Nocera, D. J. White, C. Zhao, H. Wittel, Kenneth G. Libbrecht, Chris Pankow, B. Mours, M. E. Normandin, Joshua L. Willis, J. Prasad, F. Vetrano, R. L. Savage, A. S. Bell, S. E. Dwyer, David Keitel, Matthew Pitkin, A. Perreca, G. Gemme, Elizabeth Harstad, A. K. Zadrożny, V. Boschi, E. Schreiber, P. T. Baker, A. Grant, J. Aasi, Jade Powell, V. Mangano, Sunil Susmithan, A. Chiummo, Matthew Heintze, L. Zhang, A. L. Lombardi, B. Lantz, Steven Bloemen, Philip Graff, Jonathan R. Gair, T. Isogai, C. J. Bell, N. A. Lockerbie, M. van Beuzekom, F. Y. Khalili, N. Mazumder, G. McIntyre, Leo Singer, M. Drago, Guenakh Mitselmakher, W. O. Hamilton, T. M. C. Abbott, M. Wade, M. J. Hart, A. M. Gretarsson, L. Naticchioni, Salvatore Vitale, K. Haris, Luca Gammaitoni, David H. Reitze, J. C. Driggers, Tyson Littenberg, Nicolás Wolovick, A. Allocca, Michael Thomas, Walter Winkler, Thomas Dent, Vladimir Dergachev, A. S. Markosyan, Yi-Ming Hu, Suvadeep Bose, J. D. E. Creighton, L. K. Nuttall, K. Mason, Matthew Abernathy, Harald Lück, Z. Márka, G. Valdes, B. C. Stephens, J. P. Zendri, James Whelan, P. Ajith, A. M. Sergeev, M. Granata, A. L. Urban, Huan Yang, Kasem Mossavi, Pierre-François Cohadon, J. K. Blackburn, E. Chassande-Mottin, Badri Krishnan, Sweta Shah, H. Kaufer, Koji Arai, G. Islas, Sheila Rowan, Sanjeev Dhurandhar, M. Cho, M. Pürrer, T. T. Fricke, S. C. McGuire, A. Giazotto, R. M. S. Schofield, A. R. Wade, G. Kuehn, C. M. Mow-Lowry, J. Logue, M. Was, Xin Chen, R. M. Martin, Christopher M. Biwer, S. Frasca, P. Shawhan, I. Ferrante, Ilya Mandel, Todd Adams, H. Vocca, Benjamin J. Owen, J. F. J. van den Brand, B. F. Whiting, Eugeniy E. Mikhailov, Xavier Siemens, Stephen S. Eikenberry, Máté Nagy, I. Maksimovic, J. Marque, P. Charlton, R. L. Ward, G. Hemming, C. Van Den Broeck, M. Tacca, Martin Hendry, K. V. Tokmakov, A. Viceré, D. Simakov, Yi Chen, I. A. Bilenko, C. Affeldt, S. M. Koehlenbeck, Martin Hewitson, S. Doravari, E. Goetz, Junwei Cao, David J. Ottaway, Igor Neri, S. Penn, Gleb Romanov, Stephen Fairhurst, A. C. Lin, G. L. Mansell, P. Fulda, V. Dattilo, Edwin J. Son, Archana Pai, Tjonnie G. F. Li, F. Paoletti, R. Taylor, Stefan Hild, Y. Ma, Eric Howell, S. Leavey, M. Schilman, Adam A. Libson, Jon M. Miller, A. Brillet, G. Billingsley, Matthew West, L. Bosi, Travis Horrom, P. Ruggi, M. Jacobson, M. G. Beker, Dmitry S. Svinkin, T. P. Bodiya, Qi Fang, Robinjeet Singh, Richard O'Shaughnessy, B. Barr, Malik Rakhmanov, M. Yvert, J. Worden, Peter Wessels, J. Tao, Kieran Craig, L. Williams, A. Rüdiger, A. Le Roux, A. Gennai, Curt Cutler, V. Lockett, William Yam, L. Wallace, J. Poeld, A. Królak, R. Frey, Mark S. Meyer, Duncan Meacher, V. Predoi, R. Riesen, Roland Schilling, J. O'Dell, T. Dayanga, P. J. King, B. Shapiro, Virginio Sannibale, David E. McClelland, Xi-Long Fan, A. G. Wiseman, Y. Ji, S. P. Tarabrin, Samuel Deléglise, Benjamin Canuel, J. C. Barayoga, D. C. Coyne, K. Grover, K. Izumi, P. M. Meyers, Paul J. Groot, John Veitch, M. MacInnis, P. Rapagnani, C. C. Arceneaux, J. Karlen, T. Huynh-Dinh, J. S. Kissel, Marc Favata, L. E. Wade, Roger Jones, D. D. Brown, S. S. Premachandra, K. Kawabe, S. M. Aston, Michael W. Coughlin, M. Mageswaran, V. Malvezzi, Timothy MacDonald, Giuseppe Castaldi, E. Rhoades, Carl-Johan Haster, N. Morgado, L. Rolland, Fabrizio Barone, M. Mohan, N. Man, H. J. Jang, K. Haughian, Nam-Gyu Kim, D. Talukder, C. V. Torres, I. W. Harry, T. L. Cline, R. Gouaty, Fausto Acernese, C. Gray, M. Mantovani, Vaibhav Tiwari, S. Omar, H. Zhu, David H. Shoemaker, D. Verkindt, Albert Lazzarini, M. T. Hartman, V. Kringel, S. Goßler, Tomasz Bulik, Richard J. Oram, François Bondu, K. Kokeyama, N. D. Smith-Lefebvre, J. Calderón Bustillo, J. Birch, D. J. Hosken, E. Coccia, K. E. Ramirez, M. E. Zucker, B. A. Weaver, J. G. Rollins, L.-W. Wei, Michael L. Gorodetsky, Simon Stevenson, E. A. Quintero, Joseph Gleason, Hartmut Grote, V. Fafone, Farhan Feroz, T. Denker, G. Losurdo, Kendall Ackley, R. K. Nayak, F. Magaña-Sandoval, Neil J. Cornish, Peter Aufmuth, Jiayi Qin, A. Singer, J. N. Marx, R. Chakraborty, B. E. Aylott, C. Celerier, V. Re, Bruce Gendre, Saps Buchman, J. H. Clayton, Vuk Mandic, Th. S. Bauer, M. Neri, J. A. Giaime, S. G. Crowder, Satya Mohapatra, Yu-Ning Wu, Y. M. Kim, J. R. Sanders, E. Cesarini, F. Mezzani, S. Márka, Kenneth A. Strain, Fabio Marchesoni, P. Hello, Kyungmin Kim, B. O'Reilly, Eric Oelker, Yi Pan, Jong H. Chow, A. Pasqualetti, M. Tse, D. M. Macleod, M. Barbet, M. Meinders, B. L. Swinkels, Timothy A Welborn, Grant David Meadors, W. Katzman, Ettore Majorana, P. Ehrens, J. B. Lewis, Z. Shao, M. Bitossi, G. Bergmann, K. Wette, John J. Oh, Timothy Evans, Rory Smith, C. Adams, D. Sigg, S. W. Ballmer, P. Campsie, Michelle E. Walker, G. Moreno, D. Rosińska, Fan Zhang, D. Nanda Kumar, Ruth A. Anderson, Jessica Steinlechner, M. Heurs, Reed Essick, S. Kandhasamy, B. Sorazu, A. Kutynia, Andrea Chincarini, T. Z. Summerscales, B. Behnke, G. M. Harry, K. Venkateswara, Yuri Levin, (Astro)-Particles Physics, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire des matériaux avancés (LMA), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Aasi, J., Abbott, B. P., Abbott, R., Abbott, T., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Affeldt, C., Agathos, M., Aggarwal, N., Aguiar, O. D., Ajith, P., Alemic, A., Allen, B., Allocca, A., Amariutei, D., Andersen, M., Anderson, R. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C., Areeda, J. S., Ast, S., Aston, S. M., Astone, P., Aufmuth, P., Augustus, H., Aulbert, C., Aylott, B. E., Babak, S., Baker, P. T., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barbet, M., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barton, M. A., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bauchrowitz, J., Bauer, T. h. S., Baune, C., Bavigadda, V., Behnke, B., Bejger, M., Beker, M. G., Belczynski, C., Bell, A. S., Bell, C., Bergmann, G., Bersanetti, D., Bertolini, A., Betzwieser, J., Bilenko, I. A., Billingsley, G., Birch, J., Biscans, S., Bitossi, M., Biwer, C., Bizouard, M. A., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bond, C., Bondu, F., Bonelli, L., Bonnand, R., Bork, R., Born, M., Boschi, V., Sukanta, Bose, Bosi, L., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Bridges, D. O., Brillet, A., Brinkmann, M., Brisson, V., Brooks, A. F., Brown, D. A., Brown, D. D., Brckner, F., Buchman, S., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Burman, R., Buskulic, D., Buy, C., Cadonati, L., Cagnoli, G., Caldern Bustillo, J., Calloni, Enrico, Camp, J. B., Campsie, P., Cannon, K. C., Canuel, B., Cao, J., Capano, C. D., Carbognani, F., Carbone, L., Caride, S., Castaldi, G., Caudill, S., Cavagli, M., Cavalier, F., Cavalieri, R., Celerier, C., Cella, G., Cepeda, C., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chao, S., Charlton, P., Chassande Mottin, E., Chen, X., Chen, Y., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S. S. Y., Chung, S., Ciani, G., Clara, F., Clark, D. E., Clark, J. A., Clayton, J. H., Cleva, F., Coccia, E., Cohadon, P. F., Colla, A., Collette, C., Colombini, M., Cominsky, L., Constancio, M., Conte, A., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Costa, C. A., Coughlin, M. W., Coulon, J. P., Countryman, S., Couvares, P., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Croce, R. P., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Cutler, C., Dahl, K., Dal Canton, T., Damjanic, M., Danilishin, S. L., Dantonio, S., Danzmann, K., Dattilo, V., Daveloza, H., Davier, M., Davies, G. S., Daw, E. J., Day, R., Dayanga, T., Debra, D., Debreczeni, G., Degallaix, J., Delglise, S., Del Pozzo, W., Denker, T., Dent, T., Dereli, H., Dergachev, V., DE ROSA, Rosario, Derosa, R. T., Desalvo, R., Dhurandhar, S., Daz, M., Dickson, J., Di Fiore, L., Di Lieto, A., Di Palma, I., Di Virgilio, A., Dolique, V., Dominguez, E., Donovan, F., Dooley, K. L., Doravari, S., Douglas, R., Downes, T. P., Drago, M., Drever, R. W. P., Driggers, J. C., Du, Z., Ducrot, M., Dwyer, S., Eberle, T., Edo, T., Edwards, M., Effler, A., Eggenstein, H. B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Endrczi, G., Essick, R., Etzel, T., Evans, M., Evans, T., Factourovich, M., Fafone, V., Fairhurst, S., Fan, X., Fang, Q., Farinon, S., Farr, B., Farr, W. M., Favata, M., Fazi, D., Fehrmann, H., Fejer, M. M., Feldbaum, D., Feroz, F., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Finn, L. S., Fiori, I., Fisher, R. P., Flaminio, R., Fournier, J. D., Franco, S., Frasca, S., Frasconi, F., Frede, M., Frei, Z., Freise, A., Frey, R., Fricke, T. T., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gair, J. R., Gammaitoni, L., Gaonkar, S., Garufi, Fabio, Gehrels, N., Gemme, G., Gendre, B., Genin, E., Gennai, A., Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gleason, J., Goetz, E., Goetz, R., Gondan, L., Gonzlez, G., Gordon, N., Gorodetsky, M. L., Gossan, S., Goler, S., Gouaty, R., Grf, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Greenhalgh, R. J. S., Gretarsson, A. M., Groot, P., Grote, H., Grover, K., Grunewald, S., Guidi, G. M., Guido, C. J., Gushwa, K., Gustafson, E. K., Gustafson, R., Ha, J., Hall, E. D., Hamilton, W., Hammer, D., Hammond, G., Hanke, M., Hanks, J., Hanna, C., Hannam, M. D., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Hart, M., Hartman, M. T., Haster, C. J., Haughian, K., Heidmann, A., Heintze, M., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Heptonstall, A. W., Heurs, M., Hewitson, M., Hild, S., Hoak, D., Hodge, K. A., Hofman, D., Holt, K., Hopkins, P., Horrom, T., Hoske, D., Hosken, D. J., Hough, J., Howell, E. J., Hu, Y., Huerta, E., Hughey, B., Husa, S., Huttner, S. H., Huynh, M., Huynh Dinh, T., Idrisy, A., Ingram, D. R., Inta, R., Islas, G., Isogai, T., Ivanov, A., Iyer, B. R., Izumi, K., Jacobson, M., Jang, H., Jaranowski, P., Ji, Y., Jimnez Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Haris, K., Kalmus, P., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Karlen, J., Kasprzack, M., Katsavounidis, E., Katzman, W., Kaufer, H., Kaufer, S., Kaur, T., Kawabe, K., Kawazoe, F., Kflian, F., Keiser, G. M., Keitel, D., Kelley, D. B., Kells, W., Keppel, D. G., Khalaidovski, A., Khalili, F. Y., Khazanov, E. A., Kim, C., Kim, K., Kim, N. G., Kim, N., Kim, S., Kim, Y. M., King, E. J., King, P. J., Kinzel, D. L., Kissel, J. S., Klimenko, S., Kline, J., Koehlenbeck, S., Kokeyama, K., Kondrashov, V., Koranda, S., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Krishnan, B., Krlak, A., Kuehn, G., Kumar, A., Nanda Kumar, D., Kumar, P., Kumar, R., Kuo, L., Kutynia, A., Lam, P. K., Landry, M., Lantz, B., Larson, S., Lasky, P. D., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lebigot, E. O., Lee, C. H., Lee, H. K., Lee, H. M., Lee, J., Lee, P. J., Leonardi, M., Leong, J. R., Leonor, I., Le Roux, A., Leroy, N., Letendre, N., Levin, Y., Levine, B., Lewis, J., T. G. F., Li, Libbrecht, K., Libson, A., Lin, A. C., Littenberg, T. B., Lockerbie, N. A., Lockett, V., Lodhia, D., Loew, K., Logue, J., Lombardi, A. L., Lopez, E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J., Lubinski, M. J., Lck, H., Lundgren, A. P., Ma, Y., Macdonald, E. P., Macdonald, T., Machenschalk, B., Macinnis, M., Macleod, D. M., Magaa Sandoval, F., Magee, R., Mageswaran, M., Maglione, C., Mailand, K., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Manca, G. M., Mandel, I., Mandic, V., Mangano, V., Mangini, N. M., Mansell, G., Mantovani, M., Marchesoni, F., Marion, F., Mrka, S., Mrka, Z., Markosyan, A., Maros, E., Marque, J., Martelli, F., Martin, I. W., Martin, R. M., Martinelli, L., Martynov, D., Marx, J. N., Mason, K., Masserot, A., Massinger, T. J., Matichard, F., Matone, L., Mavalvala, N., May, G., Mazumder, N., Mazzolo, G., Mccarthy, R., Mcclelland, D. E., Mcguire, S. C., Mcintyre, G., Mciver, J., Mclin, K., Meacher, D., Meadors, G. D., Mehmet, M., Meidam, J., Meinders, M., Melatos, A., Mendell, G., Mercer, R. A., Meshkov, S., Messenger, C., Meyer, M. S., Meyers, P. M., Mezzani, F., Miao, H., Michel, C., Mikhailov, E. E., Milano, Leopoldo, Miller, J., Minenkov, Y., Mingarelli, C. M. F., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moe, B., Moggi, A., Mohan, M., Mohapatra, S. R. P., Moraru, D., Moreno, G., Morgado, N., Morriss, S. R., Mossavi, K., Mours, B., Mow Lowry, C. M., Mueller, C. L., Mueller, G., Mukherjee, S., Mullavey, A., Munch, J., Murphy, D., Murray, P. G., Mytidis, A., Nagy, M. F., Nardecchia, I., Naticchioni, L., Nayak, R. K., Necula, V., Nelemans, G., Neri, I., Neri, M., Newton, G., Nguyen, T., Nielsen, A. B., Nissanke, S., Nitz, A. H., Nocera, F., Nolting, D., Normandin, M. E. N., Nuttall, L. K., Ochsner, E., Odell, J., Oelker, E., J. J., Oh, S. H., Oh, Ohme, F., Omar, S., Oppermann, P., Oram, R., Oreilly, B., Ortega, W., Oshaughnessy, R., Osthelder, C., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Padilla, C., Pai, A., Palashov, O., Palomba, C., Pan, H., Pan, Y., Pankow, C., Paoletti, F., Papa, M. A., Paris, H., Pasqualetti, A., Passaquieti, R., Passuello, D., Pedraza, M., Pele, A., Penn, S., Perreca, A., Phelps, M., Pichot, M., Pickenpack, M., Piergiovanni, F., Pierro, V., Pinard, L., Pinto, I. M., Pitkin, M., Poeld, J., Poggiani, R., Poteomkin, A., Powell, J., Prasad, J., Predoi, V., Premachandra, S., Prestegard, T., Price, L. 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I., Travasso, F., Traylor, G., Tse, M., Tshilumba, D., Tuennermann, H., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., Vallisneri, M., van Beuzekom, M., van den Brand, J. F. J., Van Den Broeck, C., van der Sluys, M. V., van Heijningen, J., van Veggel, A. A., Vass, S., Vasth, M., Vaulin, R., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Verkindt, D., Vetrano, F., Vicer, A., Vincent Finley, R., Vinet, J. Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Vousden, W. D., Vyachanin, S. P., Wade, A. R., Wade, L., Wade, M., Walker, M., Wallace, L., Walsh, S., Wang, M., Wang, X., Ward, R. L., Was, M., Weaver, B., Wei, L. W., Weinert, M., Weinstein, A. J., Weiss, R., Welborn, T., Wen, L., Wessels, P., West, M., Westphal, T., Wette, K., Whelan, J. T., White, D. J., Whiting, B. F., Wiesner, K., Wilkinson, C., Williams, K., Williams, L., Williams, R., Williams, T. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M., Winkler, W., Wipf, C. C., Wiseman, A. G., Wittel, H., Woan, G., Wolovick, N., Worden, J., Wu, Y., Yablon, J., Yakushin, I., Yam, W., Yamamoto, H., Yancey, C. C., Yang, H., Yoshida, S., Yvert, M., Zadrony, A., Zanolin, M., Zendri, J. P., Fan, Zhang, Zhang, L., Zhao, C., Zhu, H., Zhu, X. J., Zucker, M. E., Zuraw, S., Zweizig, J., Aptekar, R. L., Atteia, J. L., Cline, T., Connaughton, V., Frederiks, D. D., Golenetskii, S. V., Hurley, K., Krimm, H. A., Marisaldi, M., Palshin, V. D., Palmer, D., Svinkin, D. 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Subjects
Gamma ray burst, Astronomy, Interplanetary network, General Physics and Astronomy, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Pacs number: 04.80.Nn, Pacs number: 07.05.Kf, gravitational wave, 010303 astronomy & astrophysics, QC, QB, LIGO Scientific Collaboration, REPEATER, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, ORIGIN, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Settore FIS/01 - Fisica Sperimentale, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational waves, GRB, Interferometers, SDG 10 - Reduced Inequalities, 3. Good health, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - High Energy Astrophysical Phenomena, GIANT FLARE, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Population, REDSHIFT, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational waves, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Physics and Astronomy (all), Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Binary star, education, SHORT-DURATION, UNUSUAL SUPERNOVA, 010308 nuclear & particles physics, Gravitational wave, 5TH, [ PHYS.ASTR.HE ] Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Redshift, LIGO, Neutron star, [ SDU.ASTR.HE ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Gamma-ray burst, GRB 051103
Abstract

We present the results of a search for gravitational waves associated with 223 gamma-ray bursts (GRBs) detected by the InterPlanetary Network (IPN) in 2005-2010 during LIGO's fifth and sixth science runs and Virgo's first, second and third science runs. The IPN satellites provide accurate times of the bursts and sky localizations that vary significantly from degree scale to hundreds of square degrees. We search for both a well-modeled binary coalescence signal, the favored progenitor model for short GRBs, and for generic, unmodeled gravitational wave bursts. Both searches use the event time and sky localization to improve the gravitational-wave search sensitivity as compared to corresponding all-time, all-sky searches. We find no evidence of a gravitational-wave signal associated with any of the IPN GRBs in the sample, nor do we find evidence for a population of weak gravitational-wave signals associated with the GRBs. For all IPN-detected GRBs, for which a sufficient duration of quality gravitational-wave data is available, we place lower bounds on the distance to the source in accordance with an optimistic assumption of gravitational-wave emission energy of $10^{-2}M_{\odot}c^2$ at 150 Hz, and find a median of 13 Mpc. For the 27 short-hard GRBs we place 90% confidence exclusion distances to two source models: a binary neutron star coalescence, with a median distance of 12Mpc, or the coalescence of a neutron star and black hole, with a median distance of 22 Mpc. Finally, we combine this search with previously published results to provide a population statement for GRB searches in first-generation LIGO and Virgo gravitational-wave detectors, and a resulting examination of prospects for the advanced gravitational-wave detectors., 15 pages, 8 figures, 2 tables; for the science summary, see http://www.ligo.org/science/Publication-IPNS56VSR123grb/index.php

Published
2014

112. Characterization of the VEGA ASIC coupled to large area position-sensitive Silicon Drift Detectors

Author

D. Macera, N. Zampa, A. Vacchi, E. Del Monte, F. Ficorella, Gabriele Giacomini, Giuseppe Bertuccio, Marco Grassi, Lucia Andreani, Fabio Muleri, Gianluigi Zampa, A. Rachevski, Marco Feroci, Antonino Picciotto, Y. Evangelista, C. Labanti, Giuseppe Baldazzi, M. Zuffa, Yannick Favre, Martino Marisaldi, M. Ahangarianabhari, Piero Malcovati, I. Rashevskaya, F. Fuschino, Riccardo Campana, R Campana, Y Evangelista, F Fuschino, M Ahangarianabhari, D Macera, G Bertuccio, M Grassi, C Labanti, M Marisaldi, P Malcovati, A Rachevski, G Zampa, N Zampa, L Andreani, G Baldazzi, E Del Monte, Y Favre, M Feroci, F Muleri, I Rashevskaya, A Vacchi, F Ficorella, G Giacomini, A Picciotto, and M Zuffa

Subjects
X-ray detector, Physics - Instrumentation and Detectors, Physics::Instrumentation and Detectors, Computer science, Instrumentation, Detector, Front-end electronics for detector readout, X-ray detectors, Mathematical Physics, Vega, FOS: Physical sciences, Instrumentation and Detectors (physics.ins-det), Noise (electronics), Space exploration, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), Application-specific integrated circuit, Electronic engineering, Hardware_INTEGRATEDCIRCUITS, Electronics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

Low-noise, position-sensitive Silicon Drift Detectors (SDDs) are particularly useful for experiments in which a good energy resolution combined with a large sensitive area is required, as in the case of X-ray astronomy space missions and medical applications. This paper presents the experimental characterization of VEGA, a custom Application Specific Integrated Circuit (ASIC) used as the front-end electronics for XDXL-2, a large-area (30.5 cm^2) SDD prototype. The ASICs were integrated on a specifically developed PCB hosting also the detector. Results on the ASIC noise performances, both stand-alone and bonded to the large area SDD, are presented and discussed., Comment: 15 pages, 11 figures. Accepted for publication in Journal of Instrumentation (JINST)

Published
2014

113. The Large Observatory For x-ray Timing

Author

Antonios Manousakis, S. Boutloukos, F. Zwart, Jose M. Torrejon, C. Pittori, Alessandro Drago, Dieter H. Hartmann, Feryal Özel, T. J. L. Courvoisier, Tim Johannsen, Jordi José, M. Michalska, Christian Schmid, I. Rashevskaya, Gottfried Kanbach, V. Petracek, L. Bradley, Allan Hornstrup, M. H. Erkut, Sergio Campana, Rudy Wijnands, Andrew Cumming, Nils Andersson, Tomaso Belloni, M. C. Miller, Roman Wawrzaszek, Stefano Bianchi, Enrique García-Berro, Sandro Mereghetti, C. Guidorzi, C. Corral Van Damme, Søren Brandt, Francesco Tombesi, Felix Ryde, Didier Barret, Simon Vaughan, Marco Feroci, T. Di Salvo, C. van Baren, Angelo Antonelli, Marc Ribó, J. L. Atteia, P. Soleri, Alessio Trois, Silvia Zane, G. Mouret, Ersin Gogus, Emanuele Perinati, J. Coker, Piero Malcovati, V. Mangano, F. Jetter, P. Uter, P. Romano, M. Nowak, Roberto Turolla, Laura Tolos, Antonino D'Ai, Laura Alvarez, C. Amoros, Simone Scaringi, A. Possenti, David M. Smith, M. Falanga, A. Goldwurm, René Hudec, Ignacio Negueruela, M. van der Klis, Francesco Longo, José A. Pons, I. M. McHardy, R. Rohlfs, P. Cais, Luigi Stella, S. Di Cosimo, Antoine Rousseau, M. Ayre, M. Gschwender, D. Klochkov, Niels Lund, Chryssa Kouveliotou, P. Azzarello, F. Château, Michael Gabler, S. Vercellone, Martin Durant, I. Donnarumma, Giorgio Matt, Mauro Orlandini, P. Kaaret, Patrick Smith, P. T. O'Brien, A. Argan, M. Orienti, Marco Grassi, Claudio Labanti, Edward F. Brown, Christopher S. Reynolds, Gloria Sala, Y. Evangelista, Gabriel Török, José Braga, Riccardo Campana, Alan Smith, C. Gouiffes, Nevin N. Weinberg, Leonardo Gualtieri, Yannick Favre, P.G. Jonker, Gabriele Giovannini, D. de Martino, Irfan Kuvvetli, S. Motta, Teresa Mineo, Paul J. Groot, Pablo Reig, Martino Marisaldi, Andrea Sanna, Lorenzo Amati, G. L. Israel, D. Macera, K. S. Wood, Pablo Cerdá-Durán, F. Fuschino, Suvi Gezari, Mariano Mendez, Slawomir Suchy, Damien Rambaud, Nanda Rea, R. Artigue, J.-Y. Seyler, S. N. Shore, Frederick K. Lamb, Jörn Wilms, Mark G. Alford, Margarita Hernanz, Thomas M. Tauris, Luca Izzo, Tobias Boenke, J. J. M. in 't Zand, J. Mulačová, P. Binko, Daniel Maier, Jan Schee, Bruce Gendre, Enrico Bozzo, Paul S. Ray, Giuseppe Bertuccio, Simone Migliari, Ignazio Bombaci, Vladimir Karas, Nikolaos Stergioulas, P. P. Laubert, D. Karelin, A. C. Fabian, Giovanni Miniutti, Dacheng Lin, L. Guy, Martine Mouchet, Colleen A. Wilson-Hodge, Valeria Ferrari, Kai Hebeler, Mark H. Finger, Shigeto Watanabe, Pawel Haensel, H. Jacobs, Adrian Martindale, A. A. Zdziarski, Andrea Santangelo, Giuseppe Baldazzi, Piergiorgio Casella, Fabio Muleri, M. Hailey, Antonio Bianchini, Giuseppe Lodato, E. Del Monte, M. Rapisarda, Zdeněk Stuchlík, Alain Cros, V. Sochora, Laurens Keek, Jorge Casares, Andrew Melatos, Pere Blay, E. Rossi, A. P. Spencer, G. Stratta, Conrado Albertus, J. M. Paredes, M. Ahangarianabhari, Anna L. Watts, M. Del Santo, I. Kreykenbohm, Alessandro Patruno, G. A. Caliandro, C. Feldman, M. Pohl, Fabrizio Tamburini, G. Zampa, Marina Orio, Flemming Hansen, P. Ramon, Ruben Salvaterra, David H. Lumb, Edward M. Cackett, Andrew Shearer, Sharon M. Morsink, L. Pacciani, J.-M. Bonnet Bidaud, A. De Luca, Jérôme Chenevez, Sebastian Diebold, N. Zampa, Carole A. Haswell, Luciano Burderi, E. Cavazzuti, Adam Ingram, Dhiren Kataria, Berend Winter, A. Vacchi, W. Hermsen, P. Giommi, Dong Lai, N. A. Webb, P. Bodin, Dom Walton, Solen Balman, Benjamin Stappers, M. Burgay, Luca Zampieri, Carl Budtz-Jørgensen, Ralph A. M. J. Wijers, Giancarlo Cusumano, J. L. Galvez Sanchez, Raffaella Schneider, Luciano Rezzolla, Alexander Heger, S. Korpela, Dimitrios Emmanoulopoulos, Biswajit Paul, Diego Götz, B. Artigues, Paolo Soffitta, M. H. Finger, J. W. den Herder, Paolo Esposito, Kazushi Iwasawa, Poul Erik Holmdahl Olsen, J. Neilsen, Marco Barbera, Deepto Chakrabarty, R. A. Osten, M. Reina Aranda, A. J. Castro-Tirado, Andrea Tramacere, D. Haas, Johannes Dercksen, John A. Tomsick, A. V. Penacchioni, V. D'Elia, Alfonso Collura, Altan Baykal, P. Le Provost, S. Turriziani, Kostas D. Kokkotas, Duncan K. Galloway, Ron Remillard, Juhani Huovelin, Somak Bhattacharyya, Pavel Bakala, Phil Uttley, Richard E. Cole, Mahesh Prakash, L. Kuiper, T. Munoz-Darias, Diego F. Torres, S. Mahmoodifar, G. Ramsay, Andrew Norton, T. Kennedy, Achim Schwenk, L. Zdunik, A. B. Giles, Jerome Rodriguez, C. Motch, Ilya Mandel, Marcello Giroletti, Dimitrios Psaltis, J. Sandberg, Fiamma Capitanio, Remon Cornelisse, M. R. Gilfanov, Peggy Varniere, Franck Cadoux, Peter J. Wheatley, M. de Pasquale, Juri Poutanen, S. Maestre, A. Pellizzoni, Axel Schwope, Diego Altamirano, Piotr Orleanski, V. Vrba, Agata Różańska, Kateřina Goluchová, P. Rodríguez Gil, Niccolò Bucciantini, Stéphane Schanne, Carlo Ferrigno, Thomas J. Maccarone, H. Wende, Tod E. Strohmayer, Tadayuki Takahashi, Francois Lebrun, E. Kuulkers, Jeroen Homan, Maurizio Paolillo, M. A. Perez, J. P. Osborne, A. Alpar, Sanjay Reddy, G.W. Fraser, V. Sulemainov, D. Linder, L. Sabau-Graziati, A. Rachevski, Bing Zhang, Alessandro Papitto, C. Tenzer, Alex Markowitz, J. Portell, Roberto Mignani, Fabrizio Bocchino, Arnau Rios, R. de la Rie, M. Wille, A. de Rosa, Alessandro Riggio, M. Frericks, Andrew W. Steiner, Michal Bursa, Federico Bernardini, Jon M. Miller, W. Kluzniak, INAF - Osservatorio Astronomico di Roma ( OAR ), Istituto Nazionale di Astrofisica ( INAF ), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées ( LATT ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Variable Energy Cyclotron Centre, Institut Pasteur de Montevideo, Réseau International des Instituts Pasteur ( RIIP ) -Institut Pasteur de Montevideo, Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), FORMATION STELLAIRE 2014, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux ( L3AB ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire aquitain des sciences de l'univers ( OASU ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ), Instituto de Astrofísica de Andalucía ( IAA ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Interactions et dynamique des environnements de surface ( IDES ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Licryl Laboratory ( CNR-IPCF UOS Cosenza ), University of Calabria, Laboratori Nazionali di Frascati ( LNF ), National Institute for Nuclear Physics ( INFN ), PCAS, Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano ( IASF-MI ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), Canada's National Laboratory for Particle and Nuclear Physics ( TRIUMF ), NRC, Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] ( UNIBO ), Institut de recherches sur la catalyse et l'environnement de Lyon ( IRCELYON ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Univers et Théories ( LUTH ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Spectrochimie Infrarouge et Raman - UMR 8516 ( LASIR ), Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Dipartimento di Scienze Fisiche [Naples], Università degli studi di Napoli Federico II, Energétique, propulsion, espace, environnement ( EPEE ), Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Physics and Astronomy [Hanover], Dartmouth College [Hanover], Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d’Optique Atmosphérique - UMR 8518 ( LOA ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Institut de Biologie du Développement de Marseille ( IBDM ), Aix Marseille Université ( AMU ) -Institut National de la Santé et de la Recherche Médicale ( INSERM ) -Centre National de la Recherche Scientifique ( CNRS ), Universitat Politècnica de Catalunya [Barcelona] ( UPC ), INAF-IASF Milano, Climate and Environmental Physics [Bern], University of Bern, Centre National d'Etudes Spatiales ( CNES ), Institute of Geology, Eidgenössische Technische Hochschule [Zürich] ( ETH Zürich ), IEEC-CSIC, Universitat Autònoma de Barcelona [Barcelona] ( UAB ), MedisysResearch Lab ( Medisys ), Philips Research, European Space Astronomy Center ( ESAC ), European Space Agency ( ESA ), High Energy Astrophys. & Astropart. Phys (API, FNWI), INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (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), Réseau International des Instituts Pasteur (RIIP), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Interactions et dynamique des environnements de surface (IDES), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Licryl Laboratory (CNR-IPCF UOS Cosenza), Università della Calabria [Arcavacata di Rende] (Unical), Laboratori Nazionali di Frascati (LNF), Istituto Nazionale di Fisica Nucleare (INFN), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Canada's particle accelerator centre (TRIUMF), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut de recherches sur la catalyse et l'environnement de Lyon (IRCELYON), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Laboratoire Avancé de Spectroscopie pour les Intéractions la Réactivité et l'Environnement - UMR 8516 (LASIRE), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), University of Naples Federico II = Università degli studi di Napoli Federico II, Energétique, propulsion, espace, environnement (EPEE), Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Laboratoire d’Optique Atmosphérique - UMR 8518 (LOA), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Institut de Biologie du Développement de Marseille (IBDM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Universitat Politècnica de Catalunya [Barcelona] (UPC), Climate and Environmental Physics [Bern] (CEP), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE)-Universität Bern [Bern] (UNIBE), Centre National d'Études Spatiales [Toulouse] (CNES), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Universitat Autònoma de Barcelona (UAB), MedisysResearch Lab (Medisys), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), SPIE, Takahashi, Tadayuki, Feroci M., Den Herder J.W., Bozzo E., Barret D., Brandt S., Hernanz M., Van Der Klis M., Pohl M., Santangelo A., Stella L., Watts A., Wilms J., Zane S., Ahangarianabhari M., Albertus C., Alford M., Alpar A., Altamirano D., Alvarez L., Amati L., Amoros C., Andersson N., Antonelli A., Argan A., Artigue R., Artigues B., Atteia J.-L., Azzarello P., Bakala P., Baldazzi G., Balman S., Barbera M., Van Baren C., Bhattacharyya S., Baykal A., Belloni T., Bernardini F., Bertuccio G., Bianchi S., Bianchini A., Binko P., Blay P., Bocchino F., Bodin P., Bombaci I., Bonnet Bidaud J.-M., Boutloukos S., Bradley L., Braga J., Brown E., Bucciantini N., Burderi L., Burgay M., Bursa M., Budtz-Jorgensen C., Cackett E., Cadoux F.R., Cais P., Caliandro G.A., Campana R., Campana S., Capitanio F., Casares J., Casella P., Castro-Tirado A.J., Cavazzuti E., Cerda-Duran P., Chakrabarty D., Chateau F., Chenevez J., Coker J., Cole R., Collura A., Cornelisse R., Courvoisier T., Cros A., Cumming A., Cusumano G., D'ai A., D'elia V., Del Monte E., De Luca A., De Martino D., Dercksen J.P.C., De Pasquale M., De Rosa A., Del Santo M., Di Cosimo S., Diebold S., Di Salvo T., Donnarumma I., Drago A., Durant M., Emmanoulopoulos D., Erkut M.H., Esposito P., Evangelista Y., Fabian A., Falanga M., Favre Y., Feldman C., Ferrari V., Ferrigno C., Finger M., Finger M.H., Fraser G.W., Frericks M., Fuschino F., Gabler M., Galloway D.K., Galvez Sanchez J.L., Garcia-Berro E., Gendre B., Gezari S., Giles A.B., Gilfanov M., Giommi P., Giovannini G., Giroletti M., Gogus E., Goldwurm A., Goluchova K., Gotz D., Gouiffes C., Grassi M., Groot P., Gschwender M., Gualtieri L., Guidorzi C., Guy L., Haas D., Haensel P., Hailey M., Hansen F., Hartmann D.H., Haswell C.A., Hebeler K., Heger A., Hermsen W., Homan J., Hornstrup A., Hudec R., Huovelin J., Ingram A., In't Zand J.J.M., Israel G., Iwasawa K., Izzo L., Jacobs H.M., Jetter F., Johannsen T., Jonker P., Jose J., Kaaret P., Kanbach G., Karas V., Karelin D., Kataria D., Keek L., Kennedy T., Klochkov D., Kluzniak W., Kokkotas K., Korpela S., Kouveliotou C., Kreykenbohm I., Kuiper L.M., Kuvvetli I., Labanti C., Lai D., Lamb F.K., Laubert P.P., Lebrun F., Lin D., Linder D., Lodato G., Longo F., Lund N., Maccarone T.J., Macera D., Maestre S., Mahmoodifar S., Maier D., Malcovati P., Mandel I., Mangano V., Manousakis A., Marisaldi M., Markowitz A., Martindale A., Matt G., Mchardy I.M., Melatos A., Mendez M., Mereghetti S., Michalska M., Migliari S., Mignani R., Miller M.C., Miller J.M., Mineo T., Miniutti G., Morsink S., Motch C., Motta S., Mouchet M., Mouret G., Mulaova J., Muleri F., Munoz-Darias T., Negueruela I., Neilsen J., Norton A.J., Nowak M., O'brien P., Olsen P.E.H., Orienti M., Orio M., Orlandini M., Orleaaski P., Osborne J.P., Osten R., Ozel F., Pacciani L., Paolillo M., Papitto A., Paredes J.M., Patruno A., Paul B., Perinati E., Pellizzoni A., Penacchioni A.V., Perez M.A., Petracek V., Pittori C., Pons J., Portell J., Possenti A., Poutanen J., Prakash M., Le Provost P., Psaltis D., Rambaud D., Ramon P., Ramsay G., Rapisarda M., Rachevski A., Rashevskaya I., Ray P.S., Rea N., Reddy S., Reig P., Reina Aranda M., Remillard R., Reynolds C., Rezzolla L., Ribo M., De La Rie R., Riggio A., Rios A., Rodriguez-Gil P., Rodriguez J., Rohlfs R., Romano P., Rossi E.M.R., Rozanska A., Rousseau A., Ryde F., Sabau-Graziati L., Sala G., Salvaterra R., Sanna A., Sandberg J., Scaringi S., Schanne S., Schee J., Schmid C., Shore S., Schneider R., Schwenk A., Schwope A.D., Seyler J.-Y., Shearer A., Smith A., Smith D.M., Smith P.J., Sochora V., Soffitta P., Soleri P., Spencer A., Stappers B., Steiner A.W., Stergioulas N., Stratta G., Strohmayer T.E., Stuchlik Z., Suchy S., Sulemainov V., Takahashi T., Tamburini F., Tauris T., Tenzer C., Tolos L., Tombesi F., Tomsick J., Torok G., Torrejon J.M., Torres D.F., Tramacere A., Trois A., Turolla R., Turriziani S., Uter P., Uttley P., Vacchi A., Varniere P., Vaughan S., Vercellone S., Vrba V., Walton D., Watanabe S., Wawrzaszek R., Webb N., Weinberg N., Wende H., Wheatley P., Wijers R., Wijnands R., Wille M., Wilson-Hodge C.A., Winter B., Wood K., Zampa G., Zampa N., Zampieri L., Zdunik L., Zdziarski A., Zhang B., Zwart F., Ayre M., Boenke T., Corral Van Damme C., Kuulkers E., Lumb D., Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), 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)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Centrale Lille Institut (CLIL), 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-Observatoire Midi-Pyrénées (OMP), Universität Bern [Bern]-Universität Bern [Bern], European Space Agency (ESA), Feroci, M., den Herder, J., Bozzo, E., Barret, D., Brandt, S., Hernanz, M., van der Klis, M., Pohl, M., Santangelo, A., Stella, L., Watts, A., Wilms, J., Zane, S., Ahangarianabhari, M., Albertus, C., Alford, M., Alpar, A., Altamirano, D., Alvarez, L., Amati, L., Amoros, C., Andersson, N., Antonelli, A., Argan, A., Artigue, R., Artigues, B., Atteia, J., Azzarello, P., Bakala, P., Baldazzi, G., Balman, S., Barbera, M., van Baren, C., Bhattacharyya, S., Baykal, A., Belloni, T., Bernardini, F., Bertuccio, G., Bianchi, S., Bianchini, A., Binko, P., Blay, P., Bocchino, F., Bodin, P., Bombaci, I., Bonnet Bidaud, J., Boutloukos, S., Bradley, L., Braga, J., Brown, E., Bucciantini, N., Burderi, L., Burgay, M., Bursa, M., Budtz Jørgensen, C., Cackett, E., Cadoux, F., Caïs, P., Caliandro, G., Campana, R., Campana, S., Capitanio, F., Casares, J., Casella, P., Castro Tirado, A., Cavazzuti, E., Cerda Duran, P., Chakrabarty, D., Château, F., Chenevez, J., Coker, J., Cole, R., Collura, A., Cornelisse, R., Courvoisier, T., Cros, A., Cumming, A., Cusumano, G., D'Ai', A., D'Elia, V., Del Monte, E., de Luca, A., de Martino, D., Dercksen, J., de Pasquale, M., De Rosa, A., Del Santo, M., Di Cosimo, S., Diebold, S., DI SALVO, T., Donnarumma, I., Drago, A., Durant, M., Emmanoulopoulos, D., Erkut, M., Esposito, P., Evangelista, Y., Fabian, A., Falanga, M., Favre, Y., Feldman, C., Ferrari, V., Ferrigno, C., Finger, M., Fraser, G., Frericks, M., Fuschino, F., Gabler, M., Galloway, D., Galvez Sanchez, J., Garcia Berro, E., Gendre, B., Gezari, S., Giles, A., Gilfanov, M., Giommi, P., Giovannini, G., Giroletti, M., Gogus, E., Goldwurm, A., Goluchová, K., Götz, D., Gouiffes, C., Grassi, M., Groot, P., Gschwender, M., Gualtieri, L., Guidorzi, C., Guy, L., Haas, D., Haensel, P., Hailey, M., Hansen, F., Hartmann, D., Haswell, C., Hebeler, K., Heger, A., Hermsen, W., Homan, J., Hornstrup, A., Hudec, R., Huovelin, J., Ingram, A., In't Zand, J., Israel, G., Iwasawa, K., Izzo, L., Jacobs, H., Jetter, F., Johannsen, T., Jonker, P., Josè, J., Kaaret, P., Kanbach, G., Karas, V., Karelin, D., Kataria, D., Keek, L., Kennedy, T., Klochkov, D., Kluzniak, W., Kokkotas, K., Korpela, S., Kouveliotou, C., Kreykenbohm, I., Kuiper, L., Kuvvetli, I., Labanti, C., Lai, D., Lamb, F., Laubert, P., Lebrun, F., Lin, D., Linder, D., Lodato, G., Longo, F., Lund, N., Maccarone, T., Macera, D., Maestre, S., Mahmoodifar, S., Maier, D., Malcovati, P., Mandel, I., Mangano, V., Manousakis, A., Marisaldi, M., Markowitz, A., Martindale, A., Matt, G., Mchardy, I., Melatos, A., Mendez, M., Mereghetti, S., Michalska, M., Migliari, S., Mignani, R., Miller, M., Miller, J., Mineo, T., Miniutti, G., Morsink, S., Motch, C., Motta, S., Mouchet, M., Mouret, G., Mulačová, J., Muleri, F., Muñoz Darias, T., Negueruela, I., Neilsen, J., Norton, A., Nowak, M., O'Brien, P., Olsen, P., Orienti, M., Orio, M., Orlandini, M., Orleański, P., Osborne, J., Osten, R., Ozel, F., Pacciani, L., Paolillo, M., Papitto, A., Paredes, J., Patruno, A., Paul, B., Perinati, E., Pellizzoni, A., Penacchioni, A., Perez, M., Petracek, V., Pittori, C., Pons, J., Portell, J., Possenti, A., Poutanen, J., Prakash, M., Le Provost, P., Psaltis, D., Rambaud, D., Ramon, P., Ramsay, G., Rapisarda, M., Rachevski, A., Rashevskaya, I., Ray, P., Rea, N., Reddy, S., Reig, P., Reina Aranda, M., Remillard, R., Reynolds, C., Rezzolla, L., Ribo, M., de la Rie, R., Riggio, A., Rios, A., Rodríguez Gil, P., Rodriguez, J., Rohlfs, R., Romano, P., Rossi, E., Rozanska, A., Rousseau, A., Ryde, F., Sabau Graziati, L., Sala, G., Salvaterra, R., Sanna, A., Sandberg, J., Scaringi, S., Schanne, S., Schee, J., Schmid, C., Shore, S., Schneider, R., Schwenk, A., Schwope, A., Seyler, J., Shearer, A., Smith, A., Smith, D., Smith, P., Sochora, V., Soffitta, P., Soleri, P., Spencer, A., Stappers, B., Steiner, A., Stergioulas, N., Stratta, G., Strohmayer, T., Stuchlik, Z., Suchy, S., Sulemainov, V., Takahashi, T., Tamburini, F., Tauris, T., Tenzer, C., Tolos, L., Tombesi, F., Tomsick, J., Torok, G., Torrejon, J., Torres, D., Tramacere, A., Trois, A., Turolla, R., Turriziani, S., Uter, P., Uttley, P., Vacchi, A., Varniere, P., Vaughan, S., Vercellone, S., Vrba, V., Walton, D., Watanabe, S., Wawrzaszek, R., Webb, N., Weinberg, N., Wende, H., Wheatley, P., Wijers, R., Wijnands, R., Wille, M., Wilson Hodge, C., Winter, B., Wood, K., Zampa, G., Zampa, N., Zampieri, L., Zdunik, L., Zdziarski, A., Zhang, B., Zwart, F., Ayre, M., Boenke, T., Corral van Damme, C., Kuulkers, E., Lumb, D., Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), National Institute for Nuclear Physics (INFN), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Canada's National Laboratory for Particle and Nuclear Physics (TRIUMF), Università di Bologna [Bologna] (UNIBO), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Spectrochimie Infrarouge et Raman - UMR 8516 (LASIR), Centre National de la Recherche Scientifique (CNRS)-Université de Lille, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Lille, Aix Marseille Université (AMU)-Collège de France (CdF)-Centre National de la Recherche Scientifique (CNRS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Universitat Autònoma de Barcelona [Barcelona] (UAB), Astronomy, den Herder, J. W., Atteia, J. L., Bonnet Bidaud, J. M., Cadoux, F. R., Cais, P., Caliandro, G. A., Castro Tirado, A. J., D'Aì, A., De Luca, A., De Martino, D., Dercksen, J. P. C., De Pasquale, M., Di Salvo, T., Erkut, M. H., Finger, M. H., Fraser, G. W., Galloway, D. K., Galvez Sanchez, J. L., Giles, A. B., Hartmann, D. H., Haswell, C. A., in't Zand, J. J. M., Jacobs, H. M., Kuiper, L. M., Lamb, F. K., Laubert, P. P., Maccarone, T. J., Mchardy, I. M., Miller, M. C., Miller, J. M., Norton, A. J., Olsen, P. E. H., Orleanski, P., Osborne, J. P., Paolillo, Maurizio, Paredes, J. M., Penacchioni, A. V., Perez, M. A., Ray, P. S., Rossi, E. M. R., Schwope, A. D., Seyler, J. Y., Smith, D. M., Smith, P. J., Steiner, A. W., Strohmayer, T. E., Torrejon, J. M., Torres, D. F., and Wilson Hodge, C. A.

Subjects
x-ray and γ-ray instrumentation, compact objects, microchannel plates, X-ray detectors, X-ray imaging, X-ray spectroscopy, X-ray timing, Electronic, Optical and Magnetic Materials, Condensed Matter Physics, Computer Science Applications1707 Computer Vision and Pattern Recognition, Applied Mathematics, Electrical and Electronic Engineering, Vision, Observatories, Field of view, 01 natural sciences, 7. Clean energy, neutron stars, Observatory, 010303 astronomy & astrophysics, Physics, Equipment and services, Astrophysics::Instrumentation and Methods for Astrophysics, Steradian, [ SDU.ASTR.IM ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics - Instrumentation and Methods for Astrophysics, X-ray detector, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Cosmic Vision, Spectral resolution, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, NO, microchannel plate, Settore FIS/05 - Astronomia e Astrofisica, X-rays, compact object, 0103 physical sciences, Electronic, Optical and Magnetic Materials, Instrumentation and Methods for Astrophysics (astro-ph.IM), dense hadronic matter, Sensors, 010308 nuclear & particles physics, Astronomy, Accretion (astrophysics), [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Neutron star, 13. Climate action, [ PHYS.ASTR.IM ] Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Gamma-ray burst, astro-ph.IM
Abstract

The Large Observatory For x-ray Timing (LOFT) was studied within ESA M3 Cosmic Vision framework and participated in the final down-selection for a launch slot in 2022-2024. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument, LOFT will study the behaviour of matter under extreme conditions, such as the strong gravitational field in the innermost regions of accretion flows close to black holes and neutron stars, and the supra-nuclear densities in the interior of neutron stars. The science payload is based on a Large Area Detector (LAD, 10 m 2 effective area, 2-30 keV, 240 eV spectral resolution, 1 deg collimated field of view) and a WideField Monitor (WFM, 2-50 keV, 4 steradian field of view, 1 arcmin source location accuracy, 300 eV spectral resolution). The WFM is equipped with an on-board system for bright events (e.g. GRB) localization. The trigger time and position of these events are broadcast to the ground within 30 s from discovery. In this paper we present the status of the mission at the end of its Phase A study., Proc. SPIE 9144, Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray, 91442T

Published
2014

114. The first AGILE low-energy ( < 30 MeV) Terrestrial Gamma-ray Flashes catalog

Author

Martino Marisaldi (1, Fabio Fuschino (1), Carlotta Pittori (3), Francesco Verrecchia (3), Paolo Giommi (3), Marco Tavani (4), Stefano Dietrich (5), Colin Price (6), Andrea Argan (4), Claudio Labanti (1), Marcello Galli (7), Francesco Longo (8), Ettore Del Monte (4), Guido Barbiellini (8), Andrea Giuliani (9), Andrea Bulgarelli (1), Fulvio Gianotti (1), Massimo Trifoglio (1), and Alessio Trois (10)

Abstract

We present the first catalog of Terrestrial Gamma-ray Flashes (TGFs) detected by the Minicalorimeter (MCAL) instrument on-board the AGILE satellite. The catalog includes 308 TGFs detected during the period March 2009 - July 2012 in the +/- 2.5 latitude band and selected to have the maximum photon energy up to 30 MeV. The char- acteristics of the AGILE events are analysed and compared to the observational framework established by the two other currently active missions capable of detecting TGFs from space, RHESSI and Fermi. A detailed model of the MCAL dead time is presented, which is fundamental to properly interpret our observations, particularly concerning duration, intensity and correlation with lightning sferics detected by the World Wide Lightning Location Network. The TGFs cumulative spectrum supports a low production altitude, in agreement with previous measurements. The AGILE TGF catalog below 30 MeV is publicly accessible online at the website of the ASI Science Data Center (ASDC) http://www.asdc.asi.it/mcaltgfcat/ In addition to the TGF sample properties we also present the catalog website functionalities available to users.

Published
2014

115. A prototype for the Real-Time analysis of the Cherenkov Telescope Array

Author

Jose Luis Contreras, Juan José Rodríguez-Vázquez, Andrea Bulgarelli, Simon Rosen, Raquel de los Reyes, A. Aboudan, Paola Grandi, S. Buson, Gino Tosti, Andrea Zoli, Domenico Beneventano, Stefan Ohm, Gernot Maier, Sonia Bergamaschi, Vito Conforti, Catherine Boisson, Louis Antonelli, Phil Evans, Martino Marisaldi, Karl Kosack, Giovanni Lamanna, Jürgen Knödlseder, Adriano De Rosa, R. Graciani, Jim Hinton, Nadine Neyroud, Vincenzo Testa, Amanda Weinstein, Denis Bastieri, Alessandro Tacchini, Etienne Lyard, Giovanni De Cesare, Eleonora Torresi, Saverio Lombardi, J. P. Dumm, Lucy Fortson, J. P. Osborne, Giuseppe Malaguti, Matthias Fuessling, Jean Jacquemier, Fulvio Gianotti, Alessandro Carosi, Brian Humensky, Jerzy Burkowski, M. Trifoglio, Luciano Nicastro, Valentina Fioretti, and Matteo Interlandi

Subjects
Cherenkov Telescope Array, Pipeline (computing), Interface (computing), Real-time computing, Cherenkov telescopes, gamma-ray flares, GPU, Intel/Phi, real-time Analysis, science alert system, VHE gamma-ray astronomy, 01 natural sciences, 7. Clean energy, Software, Observatory, 0103 physical sciences, 11. Sustainability, 010303 astronomy & astrophysics, Throughput (business), Physics, 010308 nuclear & particles physics, business.industry, Astronomy, Computer data storage, Software design pattern, Física nuclear, DataBase, Atmospheric Cherenkov telescopes, Observatories, Algorithms, Telescopes, Computer hardware, Data storage, Gamma radiation, Interfaces, business
Abstract

The Cherenkov Telescope Array (CTA) observatory will be one of the biggest ground-based very-high-energy (VHE) gamma-ray observatory. CTA will achieve a factor of 10 improvement in sensitivity from some tens of GeV to beyond 100 TeV with respect to existing telescopes. The CTA observatory will be capable of issuing alerts on variable and transient sources to maximize the scientific return. To capture these phenomena during their evolution and for effective communication to the astrophysical community, speed is crucial. This requires a system with a reliable automated trigger that can issue alerts immediately upon detection of gamma-ray flares. This will be accomplished by means of a Real-Time Analysis (RTA) pipeline, a key system of the CTA observatory. The latency and sensitivity requirements of the alarm system impose a challenge because of the anticipated large data rate, between 0.5 and 8 GB/s. As a consequence, substantial efforts toward the optimization of high-throughput computing service are envisioned. For these reasons our working group has started the development of a prototype of the Real-Time Analysis pipeline. The main goals of this prototype are to test: (i) a set of frameworks and design patterns useful for the inter-process communication between software processes running on memory; (ii) the sustainability of the foreseen CTA data rate in terms of data throughput with different hardware (e.g. accelerators) and software configurations, (iii) the reuse of non-real-time algorithms or how much we need to simplify algorithms to be compliant with CTA requirements, (iv) interface issues between the different CTA systems. In this work we focus on goals (i) and (ii).

Published
2014

116. [Untitled]

Author

L. Dori, F. Corticelli, A. Tagliani, Martino Marisaldi, Gian Carlo Cardinali, Antonella Poggi, and R. Angelucci

Subjects
Materials science, Silicon, Mechanical Engineering, technology, industry, and agriculture, Oxide, chemistry.chemical_element, Permeation, Porous silicon, chemistry.chemical_compound, Membrane, chemistry, Chemical engineering, Mechanics of Materials, Specific surface area, Organic chemistry, General Materials Science, Layer (electronics), NOx
Abstract

To realise advanced microsensors for a reliable monitoring of very low concentrations of pollutant species such as NOx, SO2, CO, O3 and aromatic hydrocarbons, the use of porous silicon (PS) permeated with semiconducting oxides has been explored. To reduce the power consumption and to make feasible the device to operate in a fast pulsed temperature mode, a novel sensor architecture has been designed. The main feature of the device is represented by a permeated suspended macroporous Si membrane, few tens of microns thick. In this paper the porous silicon formation through a suspended silicon membrane and the morphological characterization of the PS layer are reported. Moreover, the performance of a C6H6 gas sensor based on the suspended macroporous Si membrane (≅30 μm thick), permeated with the chemical precursor of Sn oxide is presented. The results have demonstrated the feasibility to realize a macroporous silicon suspended membrane with high specific surface area, efficient electrical insulation and negligible warpage. Furthermore, the permeation of the oxidized macroporous silicon membrane with SnO2 has been proved to be a valuable approach to fabricate gas sensors suitable to detect aromatic hydrocarbons in a sub-ppm range.

Published
2000

117. Introducing the CTA concept

Author

A. Mathieu, R. G. Wagner, K. Panagiotidis, S Rosier Lees, Julien Rousselle, M. Gómez Berisso, Michela Uslenghi, Stephen Maxfield, R. C. Shellard, Ivica Puljak, T. Le Flour, Thomas Schanz, Tobias C. Walther, Juanan Aguilar, Pierre Colin, M. Chikawa, N. Fouque, Mosè Mariotti, G. Fontaine, Merja Tornikoski, V. Diez-Blanco, Enrico Giro, A. Krepps, G. Koss, J. M. Martin, Sergio Billotta, E. de Oña Wilhelmi, Keitaro Takahashi, S. Buson, P. Brook, S. Steiner, M. Dyrda, Joseph Silk, Sera Markoff, P. Lubinski, U. Schwanke, Sauvik Bhattacharyya, J. Ripken, T. Haubold, C. Zurbach, H. Wetteskind, R. Hermel, J. Darling, J. Nicolau-Kukliński, Konstancja Satalecka, M. Videla, Stefan Funk, P. Conconi, S. Bajtlik, Lukasz Stawarz, J. M. Paredes, K. Reitberger, Stefan Wagner, Teresa Mineo, David Kieda, G. Pareschi, Shigeto Kabuki, Makoto Sawada, Antonio Stamerra, Rodolfo Canestrari, N. Baby, G. Crimi, P. Kostka, J. Grube, R. Zanin, I. K. Kominis, L. Mc Comb, R. Sternberger, M. Fesquet, M. Tokarz, David Fink, Daniela Dorner, N. Hamer Heras, A. Moralejo Olaizola, M. de Naurois, Diego F. Torres, Claes Fransson, K. Nishijima, Yutaka Fujita, L. Fresnillo, B. García, R. Kossakowski, A. Masserot, H. von Gunten, Alkiviadis F. Bais, Ciro Bigongiari, A. Saggion, G. Papyan, I. Mrusek, K. Farakos, J. Michałowski, A. Franckowiak, Fernando Martinez, M. Doert, R. Wawrzaszek, Michele Doro, L. Sapozhnikov, Claudia Lavalley, D. Thuermann, A.A. Zdziarski, Cristina Knapic, Karen Byrum, N. Neyroud, Petr Schovanek, W. Domainko, D. Kastana, E. Birsin, Adrian Biland, F. Sánchez, Alexandre Marcowith, M. Errando, R. L. C. Starling, J. Schultze, A. Weinstein, B. B. Singh, Yassir Moudden, Jelena Aleksić, C. L. Naumann, V. Waegebaert, M. Shayduk, U. F. Katz, Gianpiero Tagliaferri, M. Schroedter, A. Vollhardt, O. Reimann, Hideyuki Ohoka, Vincenzo Testa, C. Jablonski, Tsuguya Naito, J. Schäfer, Stavros Maltezos, A. Wierzcholska, P. Wawer, L. Nellen, F. Mirabel, Tatsuo Yoshida, P. H. Carton, Nina Nowak, L. Platos, Riccardo Rando, P. P. Krueger, R. Wischnewski, W. Romaszkan, E. Fede, Martino Marisaldi, Markus Gaug, Richard Willingale, J. H. Buckley, U. De AlmeidaBarres, J. Knapp, Saverio Lombardi, D. della Volpe, A. Herrero, A. Bottani, E. Delagnes, Martin J. Hardcastle, C. Morello, Anna Lipniacka, T. Greenshaw, M. Renaud, Giancarlo Cusumano, Jonathan Biteau, M. Sowiński, J. R. T. de Mello Neto, T. B. Humensky, Michael G. Richer, G. Parks, G. Grasseau, H. Baba, Gino Tosti, Damir Lelas, H. Krawzcynski, David Paneque, M. Barcelo, R. Dickherber, P. Ferrando, Shinji Hara, D. Florin, Hideaki Katagiri, T. Shibata, Fuyuki Tokanai, N. A. McCubbin, J. Gomez-Ortega, D. Nakajima, A. Liolios, P. Laporte, Orjan Dale, A. Sillanpää, Dainis Dravins, Timothée Grégoire, Nu. Komin, A. Mihailidis, L. Sidoli, Shiu-Hang Lee, A. W. Chen, J. M. Illa, A. Kuznetsov, P. Munar-Adrover, D. Dominis Prester, Marcos Daniel Actis, Abraham D. Falcone, L. Journet, D. Hadasch, N. Galante, A. Murphy, C. J. Todero Peixoto, S. Wiesand, A. Aravantinos, A. C. Rovero, J. L. Dournaux, P. Romano, M. Hrabovsky, R. de los Reyes Lopez, M. Ostrowski, J. Pallota, Geza Gyuk, Petar Temnikov, R. Dubois, Jan Ebr, R. Koul, David J. Smith, S. Schwarzburg, P. Manigot, Chad Finley, Tarek M. Hassan, Giuseppe Sottile, Evgeni Ovcharov, P. J. Rajda, F. Krennrich, Peter L. Moore, W. B. Focke, W. Bednarek, Elena Amato, Kazunori Kohri, J. Gamez-Garcia, I. Oya, A. Shibuya, German Hermann, William H. Lee, Dorota Sobczyńska, X. Zhou, C. Balkowski, G. Vallejo, M. Hayashida, M. Bitossi, Loukas Vlahos, H. Lockart, N. Geffroy, L. Tibaldo, Marek Jamrozy, Luke O'c. Drury, Pratik Majumdar, P. Sutcliffe, S. Schlenstedt, M. Palatka, Christophe Champion, H. Ueno, M. Rupiński, P. Giommi, J. Schwarz, G. Pühlhofer, Takashi Saito, W. van Driel, C. van Eldik, Q. Xiong, Yasuo Fukui, A. Donat, A. Ibarra, R. S. Warwick, Michiko Ohishi, A. W. Smith, J.-P. Lenain, Aion Viana, Terry Ashton, Guillaume Dubus, Jacek Niemiec, K. Kodani, Luis Ángel Tejedor, A. Wörnlein, Takanori Yoshikoshi, Masahiro Teshima, W. Gäbele, Ll. Font, Olaf Reimer, J. F. Valdés-Galicia, Lucy Fortson, J. P. Osborne, Mattia Fornasa, Keith Bechtol, Masayuki Tanaka, Shigehiro Nagataki, M. Rataj, M. Ribordy, Emmanuel Moulin, I. de la Calle, K. Winiarski, C. Jeanney, I. Mognet, I. Vegas, C. Juffroy, Yutaka Ohira, A. Jacholkowska, Matthew Wood, A. E. Suárez, J. Bähr, K. M. Schure, J. Maya, M. Dafonseca, J. Tasan, R. Sugawara, M. Bourgeat, A. Mancilla, D. Pelat, Olga Botner, D. Nedbal, G. Depaola, Robert Wagner, T. Okuda, H. Arnaldi, Josep Martí, P. Corona, T. Bonev, D. Yelos, J. Sieiro, V. Scalzotto, Jacco Vink, D. Languignon, Marco Ajello, J. Vandenbrouke, Philipp Mertsch, M. Mordalska, P. Wegner, P. Ziółkowski, P. T. O'Brien, A. Nozato, Robert D. Preece, B. Huber, Matteo Balbo, J.R. Bogart, R. Kankanyan, K. Mori, T. Jogler, Seth Digel, Claudio Vuerli, Hiromitsu Takahashi, Thomas Lohse, K. Saito, A. W. Borgland, Elisa Prandini, Helene Sol, Ryan Heller, M. Bogdan, D. Dumas, M. Stodulski, Y. Awane, Piercarlo Bonifacio, Pedro L. Luque-Escamilla, Judith H. Croston, Fabio Pizzolato, P. M. Chadwick, M. K. Daniel, Riccardo Paoletti, Reiko Orito, Katsuaki Asano, R. Frei, G. Disset, Valerie Connaughton, Juhani Huovelin, Hiroyasu Tajima, S. Vercellone, F. Feinstein, G. Decerprit, Riccardo Smareglia, S. Spyrou, Gustavo E. Romero, J. Shi, J. Carr, N. Girard, Dirk L. Hoffmann, Andreas Zech, Markus Boettcher, Osvaldo Catalano, Akira Okumura, M. Dohmke, C. Föhr, Sabrina Casanova, R. A. Cameron, Jan Conrad, K. Umehara, K. K. Yadav, A. Paizis, John L. Quinn, L. Pogosyan, C. Farnier, William J. Potter, Domenico Impiombato, Tadashi Kifune, Jonathan Granot, Gernot Maier, M. Cieślar, S. Palanque, G.W. Fraser, J. Prast, R. Bose, Heidi Sandaker, G. Lamanna, Dusan Mandat, J.F. Glicenstein, J. Harris, D. Naumann, J. 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A., Ong, R., Orito, M., Orr, J., Osborne, M., Ostrowski, L. A., Otero, N., Otte, E., Ovcharov, I., Oya, A., Ozieblo, L., Padilla, S., Paiano, D., Paillot, A., Paizi, S., Palanque, M., Palatka, J., Pallota, K., Panagiotidi, D., Paneque, M., Panter, R., Paoletti, A., Papayanni, G., Papyan, J. M., Parede, G., Pareschi, G., Park, D., Parson, M. P., Arriba, M., Pech, G., Pedaletti, V., Pelassa, D., Pelat, M. D., C., M., Persic, P. . ., O., B., Peyaud, A., Pichel, S., Pita, F., Pizzolato, L., Plato, R., Platzer, L., Pogosyan, M., Pohl, G., Pojmanski, J. D., Ponz, W., Potter, J., Poutanen, E., Prandini, J., Prast, R., Preece, F., Profeti, H., Prokoph, M., Prouza, M., Proyetti, I., Puerto Gimenez, G., Puehlhofer, I., Puljak, M., Punch, R., Pyziol, E. J., Quel, J., Quinn, A., Quirrenbach, E., Racero, P. J., Rajda, P., Ramon, R., Rando, R. C., Rannot, M., Rataj, M., Raue, P., Reardon, O., Reimann, A., Reimer, O., Reimer, K., Reitberger, M., Renaud, S., Renner, B., Reville, W., Rhode, M., Ribo, M., Ribordy, M. G., Richer, J., Rico, J., Ridky, F., Rieger, P., Ringegni, J., Ripken, P. R., Ristori, A., Riviere, S., Rivoire, L., Rob, U., Roeser, R., Rohlf, G., Roja, P., Romano, W., Romaszkan, G. E., Romero, S., Rosen, S. R., Lee, D., Ro, G., Rouaix, J., Rousselle, S., Rousselle, A. C., Rovero, F., Roy, S., Royer, B., Rudak, C., Rulten, M., Rupinski, F., Russo, F., Ryde, B., Sacco, E. O., Saemann, A., Saggion, V., Safiakian, K., Saito, T., Saito, Y., Saito, N., Sakaki, R., Sakonaka, A., Salini, F., Sanchez, M., Sanchez Conde, A., Sandoval, H., Sandaker, E., Sant'Ambrogio, A., Santangelo, E. M., Santo, A., Sanuy, L., Sapozhnikov, S., Sarkar, N., Sartore, H., Sasaki, K., Satalecka, M., Sawada, V., Scalzotto, V., Scapin, M., Scarcioffolo, J., Schafer, T., Schanz, S., Schlenstedt, R., Schlickeiser, T., Schmidt, J., Schmoll, P., Schovanek, M., Schroedter, C., Schultz, J., Schultze, A., Schulz, K., Schure, T., Schwab, U., Schwanke, J., Schwarz, S., Schwarzburg, T., Schweizer, S., Schwemmer, A., Segreto, G. H., Sembroski, K., Seweryn, M., Sharma, M., Shayduk, R. C., Shellard, J., Shi, T., Shibata, A., Shibuya, E., Shum, L., Sidoli, M., Sidz, J., Sieiro, M., Sikora, J., Silk, A., Sillanpaa, B. B., Singh, J., Sitarek, C., Skole, R., Smareglia, A., Smith, D., Smith, J., Smith, N., Smith, D., Sobczynska, H., Sol, G., Sottile, M., Sowinski, F., Spanier, D., Spiga, S., Spyrou, V., Stamatescu, A., Stamerra, R., Starling, L., Stawarz, R., Steenkamp, C., Stegmann, S., Steiner, N., Stergioula, R., Sternberger, M., Sterzel, F., Stinzing, M., Stodulski, U., Straumann, E., Strazzeri, L., Stringhetti, A., Suarez, M., Suchenek, R., Sugawara, K. . ., H., S., Sun, A. D., Supanitsky, T., Suric, P., Sutcliffe, J., Syke, M., Szanecki, T., Szepieniec, A., Szostek, G., Tagliaferri, H., Tajima, H., Takahashi, K., Takahashi, L., Takalo, H., Takami, C., Talbot, J., Tammi, M., Tanaka, S., Tanaka, J., Tasan, M., Tavani, L. A., Tejedor, I., Telezhinsky, P., Temnikov, C., Tenzer, Y., Terada, R., Terrier, M., Teshima, V., Testa, D., Tezier, D., Thuermann, L., Tibaldo, O., Tibolla, A., Tiengo, M., Tluczykont, C. J., Todero, F., Tokanai, M., Tokarz, K., Toma, K., Torii, M., Tornikoski, D. F., Torre, M., Torre, G., Tosti, T., Totani, C., Toussenel, G., Tovmassian, P., Travnicek, M., Trifoglio, I., Troyano, K., Tsingano, H., Ueno, K., Umehara, S. S., Upadhya, T., Usher, M., Uslenghi, J. F., Valdes Galicia, P., Vallania, G., Vallejo, W. v., Driel, C. v., Eldik, J., Vandenbrouke, J., Vanderwalt, H., Vankov, G., Vasileiadi, V., Vassiliev, D., Veberic, I., Vega, S., Vercellone, S., Vergani, C., Veyssiere, J. P., Vialle, A., Viana, M., Videla, P., Vincent, S., Vincent, J., Vink, N., Vlahaki, L., Vlaho, P., Vogler, A., Vollhardt, H. . ., P., S., Vorobiov, C., Vuerli, V., Waegebaert, R., Wagner, R. G., Wagner, S., Wagner, S. P., Wakely, R., Walter, T., Walther, K., Warda, R., Warwick, P., Wawer, R., Wawrzaszek, N., Webb, P., Wegner, A., Weinstein, Q., Weitzel, R., Welsing, M., Werner, H., Wetteskind, R., White, A., Wierzcholska, S., Wiesand, M., Wilkinson, D. A., William, R., Willingale, K., Winiarski, R., Wischnewski, L., Wisniewski, M., Wood, A., Woernlein, Q., Xiong, K. K., Yadav, H., Yamamoto, T., Yamamoto, R., Yamazaki, S., Yanagita, J. M., Yebra, D., Yelo, A., Yoshida, T., Yoshida, T., Yoshikoshi, V., Zabalza, M., Zacharia, A., Zajczyk, R., Zanin, A., Zdziarski, A., Zech, A., Zhao, X., Zhou, K., Zietara, J., Ziolkowski, P., Ziolkowski, V., Zitelli, C., Zurbach, P., Zychowski, Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), APC - Astrophysique des Hautes Energies (APC - AHE), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, CTA, Laboratoire Univers et Théories (LUTH (UMR_8102)), 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), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Laboratoire d'Annecy de Physique des Particules (LAPP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Next generation Cherenkov telescopes, Ciencias Físicas, 01 natural sciences, 7. Clean energy, TeV GAMMA-RAY ASTRONOMY, Observatory, Air showers, HESS, Cherenkov Telescopes, 010303 astronomy & astrophysics, MISSION, SUPERNOVA REMNANT W44, TELESCOPE, ASTRONOMY, EMISSION, Physics, ta213, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Settore FIS/01 - Fisica Sperimentale, Astrophysics::Instrumentation and Methods for Astrophysics, TeV gamma-ray astronomy, ddc:540, CIENCIAS NATURALES Y EXACTAS, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Air shower, AIR SHOWERS, Astrophysics::High Energy Astrophysical Phenomena, 0103 physical sciences, Preparatory phase, ta115, TeV gamma-ray astronomy Air showers Cherenkov Telescopes, 010308 nuclear & particles physics, business.industry, CHERENKOV TELESCOPES, Física, Astronomy, Institut für Physik und Astronomie, Astronomy and Astrophysics, ASTROFÍSICA, Cherenkov Telescope Array, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astronomía, Design study, Telecommunications, business
Abstract

The Cherenkov Telescope Array (CTA) is a new observatory for very high-energy (VHE) gamma rays. CTA has ambitions science goals, for which it is necessary to achieve full-sky coverage, to improve the sensitivity by about an order of magnitude, to span about four decades of energy, from a few tens of GeV to above 100 TeV with enhanced angular and energy resolutions over existing VHE gamma-ray observatories. An international collaboration has formed with more than 1000 members from 27 countries in Europe, Asia, Africa and North and South America. In 2010 the CTA Consortium completed a Design Study and started a three-year Preparatory Phase which leads to production readiness of CTA in 2014. In this paper we introduce the science goals and the concept of CTA, and provide an overview of the project., La lista completa de autores puede consultarse en el documento o en la página web de la revista., Facultad de Ingeniería

Published
2013

118. Calibration of AGILE-GRID with in-flight data and Monte Carlo simulations

Author

F. Perotti, Ennio Morelli, Massimiliano Fiorini, Sandro Mereghetti, G. Valentini, P. W. Cattaneo, E. Moretti, C. Pittori, A. Rappoldi, V. Vittorini, P. Santolamazza, T. Contessi, G. De Paris, E. Vallazza, Francesco Longo, Fulvio Gianotti, I. Donnarumma, M. Trifoglio, A. Pellizzoni, M. Galli, Piergiorgio Picozza, M. Giusti, Alda Rubini, G. Piano, Paolo Giommi, A. Morselli, Y. Evangelista, F. Verrecchia, G. Di Cocco, Francesco Lazzarotto, E. Striani, Attilio Ferrari, Valentina Fioretti, Marco Tavani, S. Sabatini, Paolo Lipari, A. Argan, Maura Pilia, I. Lapshov, F. Lucarelli, Sergio Colafrancesco, Guido Barbiellini, E. Del Monte, Martino Marisaldi, G. Pucella, Massimo Rapisarda, Alessio Trois, F. Fuschino, Andrea Bulgarelli, M. Prest, D. Zanello, Enrico Costa, C. Labanti, A. Giuliani, P. A. Caraveo, A. W. Chen, S. Vercellone, Marco Feroci, Luigi Pacciani, Paolo Soffitta, Rapisarda, M., Pucella, G., Tadayuki Takahashi, Stephen S. Murray, Jan-Willem A. den Herder, A. W., Chen, A., Argan, A., Bulgarelli, P. W., Cattaneo, A., Giuliani, C., Pittori, G., Pucella, M., Tavani, A., Troi, G., Barbiellini, P., Caraveo, S., Colafrancesco, E., Costa, Paris, G., Monte, E., Cocco, G., I., Donnarumma, Y., Evangelista, A., Ferrari, M., Feroci, M., Fiorini, F., Fuschino, M., Galli, F., Gianotti, P., Giommi, M., Giusti, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, Longo, Francesco, F., Lucarelli, M., Marisaldi, S., Mereghetti, E., Morelli, E., Moretti, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, G., Piano, P., Picozza, M., Pilia, M., Prest, M., Rapisarda, A., Rappoldi, A., Rubini, S., Sabatini, P., Santolamazza, P., Soffitta, E., Striani, M., Trifoglio, L., Salotti, E., Vallazza, S., Vercellone, F., Verrecchia, V., Vittorini, D., Zanello, T., Contessi, BARBIELLINI AMIDEI, Guido, G., De Pari, E., Del Monte, G., Di Cocco, V., Fioretti, Moretti, Elena, and G., Valentini

Subjects
Photon, Monte Carlo method, X-ray telescope, techniques: image processing, Astrophysics, telescope, Orbital mechanics, Vela, High Energy Gamma-ray Astronomy, law.invention, law, imaging detector, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Instrumentation: detector, image processing [techniques], detector [instrumentation], Detector, agile, Astrophysics::Instrumentation and Methods for Astrophysics, Calibrations, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Interpolation, Point spread function, gamma ray source, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Context (language use), Telescope, Optics, data analysis [methods], Calibration, instrumentation: detectors, gamma rays: general, telescopes, methods: data analysis, Instrumentation and Methods for Astrophysics (astro-ph.IM), business.industry, Astronomy and Astrophysics, Kalman filter, calibration, silicon tracker, Computational physics, Space and Planetary Science, Gamma rays: general, Instrumentation: detectors, Methods: data analysis, Techniques: image processing, Telescopes, Orbit (dynamics), AGILE satellite, business, general [gamma rays], Methods: data analysi
Abstract

Context: AGILE is a gamma-ray astrophysics mission which has been in orbit since 23 April 2007 and continues to operate reliably. The gamma-ray detector, AGILE-GRID, has observed Galactic and extragalactic sources, many of which were collected in the first AGILE Catalog. Aims: We present the calibration of the AGILE-GRID using in-flight data and Monte Carlo simulations, producing Instrument Response Functions (IRFs) for the effective area A_eff), Energy Dispersion Probability (EDP), and Point Spread Function (PSF), each as a function of incident direction in instrument coordinates and energy. Methods: We performed Monte Carlo simulations at different gamma-ray energies and incident angles, including background rejection filters and Kalman filter-based gamma-ray reconstruction. Long integrations of in-flight observations of the Vela, Crab and Geminga sources in broad and narrow energy bands were used to validate and improve the accuracy of the instrument response functions. Results: The weighted average PSFs as a function of spectra correspond well to the data for all sources and energy bands. Conclusions: Changes in the interpolation of the PSF from Monte Carlo data and in the procedure for construction of the energy-weighted effective areas have improved the correspondence between predicted and observed fluxes and spectra of celestial calibration sources, reducing false positives and obviating the need for post-hoc energy-dependent scaling factors. The new IRFs have been publicly available from the Agile Science Data Centre since November 25, 2011, while the changes in the analysis software will be distributed in an upcoming release.

Published
2013

119. Characterization of the VEGA ASIC dedicated to large area position-sensitive SDDs for space and medical applications

Author

Piero Malcovati, A. Rachevski, Riccardo Campana, F. Fuschino, Giuseppe Baldazzi, Martino Marisaldi, N. Zampa, Claudio Piemonte, Maurizio Boscardin, A. Picciotto, Giuseppe Bertuccio, M. Ahangarianabhari, E. Del Monte, A. Vacchi, I. Rashevskaya, Fabio Muleri, M. Zuffa, Yannick Favre, Gabriele Giacomini, Y. Evangelista, Marco Feroci, Marco Grassi, Lucia Andreani, Claudio Labanti, G. Zampa, IEEE, Fuschino F., Campana R., Evangelista Y., Ahangarianabhari M., Andreani L., Grassi M., Bertuccio G., Malcovati P., Favre Y., Zuffa M., Baldazzi G., Del Monte E., Feroci M., Labanti C., Marisaldi M., Muleri F., Rachevski A., Rashevskaya I., Vacchi A., Zampa G., Zampa N., Piemonte C., Giacomini G., Picciotto A., and Boscardin M.

Subjects
Engineering, Nuclear and High Energy Physics, Radiation, sezele, Noise measurement, Physics::Instrumentation and Detectors, business.industry, Detector, ComputingMethodologies_IMAGEPROCESSINGANDCOMPUTERVISION, Vega, Noise (electronics), Space exploration, Application-specific integrated circuit, Nuclear Medicine and Imaging, Electronic engineering, ASIC, Position Sensitive Silicon Drift Detector (PSSDD), Large area silicon detector, X-ray Astronomy, Electronics, business, Radiology, Nuclear Medicine and Imaging, Radiology, Energy (signal processing)
Abstract

An Application Specific Integrated Circuit (ASIC) designed as front-end electronics for large area monolithic Silicon Drift Detectors (SDD) read-out has been developed and tested. The challenging framework of this project is the read-out of the large-area SDD detectors to be used for X-ray astronomy space missions and medical applications. Due to the inherent low noise of the SDD, these detectors are able to find application in payloads where instruments capable of good energy resolution combined with position resolution and large area are needed. The ASIC has been tested with a SDD prototype having a sensitive area of 4.35×7.02 cm2. The SDD was designed to test both the spectroscopic and imaging performance with different anode pitches (967 μm and 147 μm, respectively) being able to fulfill stringent constraints on low-noise (< 19 e- rms and < 15 er. m.s., respectively) and low-power (< 0.65 mW/ch). The ASIC prototypes were integrated on specially developed high technology PCB hosting also the SDD. Results of the tests on the ASIC, both stand alone and when connected to the detector, are presented in this work. © 2013 IEEE.

Published
2013

120. Terrestrial gamma-ray flashes

Author

A. Argan, Guido Barbiellini, Andrea Bulgarelli, Fulvio Gianotti, A. Giuliani, Alessio Trois, Claudio Labanti, M. Trifoglio, F. Fuschino, Martino Marisaldi, Ettore Del Monte, Francesco Longo, Marco Tavani, M., Marisaldi, F., Fuschino, C., Labanti, M., Tavani, A., Argan, Monte, E., Longo, Francesco, BARBIELLINI AMIDEI, Guido, A., Giuliani, A., Troi, A., Bulgarelli, F., Gianotti, and M., Trifoglio

Subjects
Physics, Nuclear and High Energy Physics, Millisecond, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Astronomy, Particle accelerator, Astrophysics, Electron, Terrestrial Gamma-ray Flashes, Lightning, law.invention, law, Thunderstorm, Neutron, Instrumentation, Fermi Gamma-ray Space Telescope
Abstract

Lightning and thunderstorm systems in general have been recently recognized as powerful particle accelerators, capable of producing electrons, positrons, gamma-rays and neutrons with energies as high as several tens of MeV. In fact, these natural systems turn out to be the highest energy and most efficient natural particle accelerators on Earth. Terrestrial Gamma-ray Flashes (TGFs) are millisecond long, very intense bursts of gamma-rays and are one of the most intriguing manifestation of these natural accelerators. Only three currently operative missions are capable of detecting TGFs from space: the RHESSI, Fermi and AGILE satellites. In this paper we review the characteristics of TGFs, including energy spectrum, timing structure, beam geometry and correlation with lightning, and the basic principles of the associated production models. Then we focus on the recent AGILE discoveries concerning the high energy extension of the TGF spectrum up to 100 MeV, which is difficult to reconcile with current theoretical models.

Published
2013

121. AGILE mini-calorimeter gamma-ray burst catalog

Author

C. Pittori, Francesco Longo, Sandro Mereghetti, A. Pellizzoni, S. Vercellone, P. W. Cattaneo, A. Argan, A. Morselli, Andrea Bulgarelli, M. Galli, F. Fuschino, F. Verrecchia, Guido Barbiellini, Fulvio Gianotti, Massimo Rapisarda, C. Labanti, Martino Marisaldi, Marco Feroci, Luigi Pacciani, E. Del Monte, Marco Tavani, Sergio Colafrancesco, Alessio Trois, A. Giuliani, A. Rappoldi, M. Trifoglio, M., Galli, M., Marisaldi, F., Fuschino, C., Labanti, A., Argan, BARBIELLINI AMIDEI, Guido, A., Bulgarelli, P. W., Cattaneo, S., Colafrancesco, Monte, E., M., Feroci, F., Gianotti, A., Giuliani, Longo, Francesco, S., Mereghetti, A., Morselli, L., Pacciani, A., Pellizzoni, C., Pittori, M., Rapisarda, A., Rappoldi, M., Tavani, M., Trifoglio, A., Troi, S., Vercellone, F., Verrecchia, Rapisarda, M., and Galli, M.

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), catalog, Calorimeter (particle physics), business.industry, Astrophysics::High Energy Astrophysical Phenomena, Gamma rays: general, Timing data, Catalogs, X-rays: bursts, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Space and Planetary Science, Satellite, Catalog, burst [X-rays], catalogs, gamma rays: general, Spectral data, Gamma-ray burst, business, Astrophysics - High Energy Astrophysical Phenomena, general [gamma rays], Agile software development
Abstract

The Mini-Calorimeter of the AGILE satellite can observe the high-energy part of gamma-ray bursts with good timing capability. We present the data of the 85 hard gamma-ray bursts observed by the Mini-Calorimeter since the launch (April 2007) until October 2009. We report the timing data for 84 and spectral data for 21 bursts., Comment: Paper accepted by: Astronomy and Astrophysics, 11 pages, 7 figures. Detailed GRB data will be available from ASI-ASDC: http://www.asdc.asi.it/mcalgrbcat/ Some typo errors has been corrected in the last versions

Published
2013

122. AGILE OBSERVATIONS OF THE GRAVITATIONAL-WAVE EVENT GW150914

Author

Marco Tavani, C. Pittori, Sandro Mereghetti, E. Del Monte, G. Minervini, S. Colafrancesco, Arnaud Ferrari, Guido Barbiellini, Martino Marisaldi, V. Vittorini, Francesco Longo, P. Picozza, M. Galli, S. Sabatini, Andrea Zoli, A. Argan, P. W. Cattaneo, Andrea Bulgarelli, Paolo Giommi, F. Verrecchia, A. Rappoldi, Enrico Costa, Fabrizio Lucarelli, Marco Feroci, Luigi Pacciani, S. Vercellone, G. Piano, M. Cardillo, Louis Antonelli, A. Pellizzoni, Maura Pilia, P. Munar-Adrover, Alessio Trois, I. Donnarumma, Y. Evangelista, A. Giuliani, A. Morselli, Valentina Fioretti, P. A. Caraveo, F. Fuschino, Galli, M., Tavani, M., Pittori, C., Verrecchia, F., Bulgarelli, A., Giuliani, A., Donnarumma, I., Argan, A., Trois, A., Lucarelli, F., Marisaldi, M., Monte, E. Del, Evangelista, Y., Fioretti, V., Zoli, A., Piano, G., Munar Adrover, P., Antonelli, L. A., Barbiellini, G., Caraveo, P., Cattaneo, P. W., Costa, E., Feroci, M., Ferrari, A., Longo, Francesco, Mereghetti, S., Minervini, G., Morselli, A., Pacciani, L., Pellizzoni, A., Picozza, P., Pilia, M., Rappoldi, A., Sabatini, S., Vercellone, S., Vittorini, V., Giommi, P., Colafrancesco, S., Cardillo, M., Fuschino, F., and ITA

Subjects
gamma rays: general, gravitational waves, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Event (relativity), FOS: Physical sciences, 01 natural sciences, 0103 physical sciences, Gamma ray detectors, gravitational wave, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Gravitational wave, business.industry, Astronomy, Astronomy and Astrophysic, LIGO, Astrophysics - High Energy Astrophysical Phenomena, business, general [gamma rays], Agile software development
Abstract

We report the results of an extensive search in the AGILE data for a gamma-ray counterpart of the LIGO gravitational wave event GW150914. Currently in spinning mode, AGILE has the potential of covering with its gamma-ray instrument 80 % of the sky more than 100 times a day. It turns out that AGILE came within a minute from the event time of observing the accessible GW150914 localization region. Interestingly, the gamma-ray detector exposed about 65 % of this region during the 100 s time intervals centered at -100 s and +300 s from the event time. We determine a 2-sigma flux upper limit in the band 50 MeV - 10 GeV, $UL = 1.9 \times 10^{-8} \rm \, erg \, cm^{-2} \, s^{-1}$ obtained about 300 s after the event. The timing of this measurement is the fastest ever obtained for GW150914, and significantly constrains the electromagnetic emission of a possible high-energy counterpart. We also carried out a search for a gamma-ray precursor and delayed emission over timescales ranging from minutes to days: in particular, we obtained an optimal exposure during the interval -150 / -30 s. In all these observations, we do not detect a significant signal associated with GW150914. We do not reveal the weak transient source reported by Fermi-GBM 0.4 s after the event time. However, even though a gamma-ray counterpart of the GW150914 event was not detected, the prospects for future AGILE observations of gravitational wave sources are decidedly promising., Comment: 20 pages, 6 figures. Submitted to the Astrophysical Journal Letters on April 1, 2016

Published
2016

123. A flexible scintillation light apparatus for rare events searches

Author

Anna Vedda, Martino Marisaldi, N. Zampa, L. Riganese, F. Fuschino, Simone Capelli, Alexander Rashevsky, Mauro Fasoli, M. Zuffa, A. Vacchi, Monica Sisti, Marco Feroci, L. Gironi, Claudio Labanti, Riccardo Campana, Y. Evangelista, Ezio Previtali, G. Zampa, Giuseppe Baldazzi, V. Bonvicini, Gironi, L., Baldazzi, Giuseppe, Bonvicini, V., Campana, R., Capelli, S., Evangelista, Y., Fasoli, M., Feroci, M., Fuschino, Fabio, Labanti, C., Marisaldi, M., Previtali, E., Riganese, L., Rashevsky, A., Sisti, M., Vacchi, A., Vedda, A., Zampa, G., Zampa, N., Zuffa, M., Gironi, L, Baldazzi, G, Bonvicini, V, Campana, R, Capelli, S, Evangelista, Y, Fasoli, M, Feroci, M, Fuschino, F, Labanti, C, Marisaldi, M, Previtali, E, Riganese, L, Rashevsky, A, Sisti, M, Vacchi, A, Vedda, A, Zampa, G, Zampa, N, Zuffa, M, and ITA

Subjects
Physics, History, Scintillation, scintillating crystal, rare event searches, Physics::Instrumentation and Detectors, business.industry, Detector, Photodetector, Computer Science Applications, Education, Semiconductor detector, Physics and Astronomy (all), Optics, Double beta decay, Scalability, Rare events, High Energy Physics::Experiment, Neutrinoless double beta decay, business, Event (particle physics)
Abstract

FLARES (a Flexible scintillation Light Apparatus for Rare Event Searches) is a project for an innovative detector technology to be applied to rare event searches, and in particular to neutrinoless double beta decay experiments. Its novelty is the enhancement and optimization of the collection of the scintillation light emitted by ultra-pure crystals through the use of arrays of high performance silicon photodetectors cooled to 120 K. This would provide scintillation detectors with ~1% level energy resolution, with the advantages of a technology offering relatively simple low cost mass scalability and powerful background reduction handles, as requested by future neutrinoless double beta decay experimental programs.

Published
2016

124. Upper limits on the high-energy emission from gamma-ray bursts observed by AGILE-GRID

Author

Arnaud Ferrari, Paolo Lipari, M. Cardillo, F. Fuschino, I. Donnarumma, Y. Evangelista, A. Pellizzoni, Elena Moretti, Paolo Soffitta, A. Giuliani, Marco Tavani, L. Salotti, A. Rappoldi, G. Di Cocco, E. Del Monte, Francesco Longo, S. Sabatini, A. Argan, M. Galli, Andrea Bulgarelli, M. Olivo, C. Pittori, F. Verrecchia, F. Lucarelli, M. Fiorini, G. Pucella, Enrico Costa, M. Giusti, Sandro Mereghetti, E. Striani, Marco Feroci, P. Santolamazza, Luigi Pacciani, Francesco Lazzarotto, L. Nava, V. Vittorini, F. Perotti, A. W. Chen, I. Lapshov, M. Trifoglio, D. Zanello, P. Giommi, Alda Rubini, P. W. Cattaneo, S. Vercellone, Fulvio Gianotti, Filippo D'Ammando, Claudio Labanti, P. Picozza, S. Cutini, M. Rapisarda, S. Colafrancesco, Martino Marisaldi, Maura Pilia, L. A. Antonelli, Alessio Trois, M. Prest, G. Piano, P. A. Caraveo, R. Desiante, G. Barbiellini, A. Morselli, E. Vallazza, Università degli Studi di Udine - University of Udine [Italie], Max-Planck-Institut für Physik (Werner-Heisenberg-Institut) (MPI-P), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Istituto Nazionale di Fisica Nucleare, Sezione di Torino (INFN, Sezione di Torino), Istituto Nazionale di Fisica Nucleare (INFN), Department of Physics and Astronomy [Uppsala], Uppsala University, Universitat Politècnica de València (UPV), I.C.R.E, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Dept. of Physics, Università degli Studi di Roma Tor Vergata [Roma], Netherlands Institute for Radio Astronomy (ASTRON), Natl Res Council, Perugia Div, Institute of Plant Genetics, Istituto Nazionale di Fisica Nucleare, Sezione di Roma 3 (INFN, Sezione di Roma 3), INAF-Cagliari Astronomical Observatory, Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo (IASF-Pa), Universita degli studi di Napoli 'Parthenope' [Napoli], Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Napoli 'Parthenope' = University of Naples (PARTHENOPE), Longo, Francesco, E., Moretti, L., Nava, R., Desiante, M., Olivo, Monte, E., A., Rappoldi, F., Fuschino, M., Marisaldi, A., Giuliani, S., Cutini, M., Feroci, E., Costa, C., Pittori, M., Tavani, A., Argan, G., Barbiellini, A., Bulgarelli, P., Caraveo, M., Cardillo, P. W., Cattaneo, A. W., Chen, F., D'Ammando, Cocco, G., I., Donnarumma, Y., Evangelista, A., Ferrari, M., Fiorini, M., Galli, F., Gianotti, M., Giusti, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, S., Mereghetti, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, G., Piano, P., Picozza, M., Pilia, M., Prest, G., Pucella, M., Rapisarda, A., Rubini, S., Sabatini, P., Soffitta, E., Striani, M., Trifoglio, A., Troi, E., Vallazza, S., Vercellone, V., Vittorini, D., Zanello, L. A., Antonelli, S., Colafrancesco, P., Giommi, P., Santolamazza, F., Verrecchia, F., Lucarelli, L., Salotti, Longo F, Moretti E, Nava L, Desiante R, Olivo M, Del Monte E, Rappoldi A, Fuschino F, Marisaldi M, Giuliani A, Cutini S, Feroci M, Costa E, Pittori C, Tavani M, Argan A, Barbiellini G, Bulgarelli A, Caraveo P, Cardillo M, Cattaneo PW, Chen AW, DAmmando F, Di Cocco G, Donnarumma I, Evangelista Y, Ferrari A, Fiorini M, Galli M, Gianotti F, Giusti M, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Mereghetti S, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Piano G, Picozza P, Pilia M, Prest M, Pucella G, Rapisarda M, Rubini A, Sabatini S, Soffitta P, Striani E, Trifoglio M, Trois A, Vallazza E, Vercellone S, Vittorini V, Zanello D, Antonelli LA, Colafrancesco S, Giommi P, Santolamazza P, Verrecchia F, Lucarelli F, and Salotti L

Subjects
High energy, Astrophysics::High Energy Astrophysical Phenomena, gamma-ray burst: general, Context (language use), Astrophysics, general [gamma-ray burst], 01 natural sciences, 7. Clean energy, Bayesian data analysis, AGILE, gamma ray burst, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], Astronomy, Astronomy and Astrophysics, Grid, Space and Planetary Science, Gamma-ray burst, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Context. The detection and the characterization of the high energy emission component from individual gamma-ray bursts (GRBs) is one of the key science objectives of the currently operating gamma-ray satellite AGILE, launched in April 2007. In its first two years of operation AGILE detected three GRBs with photons of energy larger than 30 MeV. One more GRB was detected in AGILE third operation year, while operating in spinning mode. Aims. For the 64 other GRBs localized during the period July 2007 to October 2009 in the field of view of the AGILE Gamma-Ray Imaging Detector (GRID), but not detected by this instrument, we estimate the count and flux upper limits on the GRB high energy emission in the AGILE-GRID energy band (30 MeV-3 GeV). Methods. To calculate the count upper limits, we adopted a Bayesian approach. The flux upper limits are derived using several assumptions on the high-energy spectral behavior. For 28 GRBs with available prompt spectral information, a flux upper limit and the comparison with the expected flux estimated from spectral extrapolation of the Band spectrum to the 30 MeV-3 GeV band are provided. Moreover, upper limits on the flux under the assumption of an extra power law component dominating the 30 MeV-3 GeV band are calculated for all GRBs and considering four different values for the spectral photon index. Finally, we performed a likelihood upper limit on the possible delayed emission up to 1 h after the GRB. Results. The estimated flux upper limits range between 1 x 10(-4) and similar to 2 x 10(-2) photons cm(-2) s(-1) and generally lie above the flux estimated from the extrapolation of the prompt emission in the 30 MeV-3 GeV band. A notable case is GRB 080721, where the AGILE-GRID upper limit suggests a steeper spectral index or the presence of a cut-off in the high energy part of the Band prompt spectrum. The four GRBs detected by AGILE-GRID show high-energy (30 MeV-3 GeV) to low-energy (1 keV-10 MeV) fluence ratios similar to those estimated in this paper for the 64 GRBs without GRID detection, favoring the possibility that AGILE-GRID detected only high-fluence, hard GRBs. From the flux upper limits derived in this work we put some constraint on high-energy radiation from the afterglow emission and from synchrotron self Compton emission in internal shocks.

Published
2012

125. GRB 080407: an ultra-long burst discovered by the IPN

Author

N. Gehrels, Martino Marisaldi, John O. Goldsten, S. Golenetskii, D. M. Palmer, Arne Rau, Jay Cummings, I. G. Mitrofanov, D. Frederiks, Kevin Hurley, Marco Feroci, D. Svinkin, C. Fellows, M. L. Litvak, V. Pal'Shin, Scott Barthelmy, K. Harshman, Xiao-Ling Zhang, R. Aptekar, R. D. Starr, E. P. Mazets, E. Del Monte, A. von Kienlin, William V. Boynton, A. B. Sanin, V. G. Savchenko, D. Golovin, and Hans A. Krimm

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy, Context (language use), Astrophysics, Magnetar, Wind measurement, Long period, Emission spectrum, Astrophysics - High Energy Astrophysical Phenomena, Interplanetary spaceflight, Gamma-ray burst
Abstract

We present observations of the extremely long GRB 080704 obtained with the instruments of the Interplanetary Network (IPN). The observations reveal two distinct emission episodes, separated by a ~1500 s long period of quiescence. The total burst duration is about 2100 s. We compare the temporal and spectral characteristics of this burst with those obtained for other ultra-long GRBs and discuss these characteristics in the context of different models., 5 pages, 2 figures, 3 tables. Proceedings of the Gamma-Ray Bursts 2012 Conference (GRB 2012) held in Munich, Germany, May 7-11, 2012. Published online at http://pos.sissa.it/cgi-bin/reader/conf.cgi?confid=152

Published
2012

126. The Interplanetary Network Database

Author

David M. Smith, E. Del Monte, Y. Hanabata, E. P. Mazets, Yasushi Fukazawa, Hans A. Krimm, Kevin Hurley, Yukikatsu Terada, N. Gehrels, A. B. Sanin, Arne Rau, Michael S. Briggs, Kazuo Makishima, R. Starr, V. Pal'Shin, Kazutaka Yamaoka, Scott Barthelmy, D. Frederiks, W. Hajdas, Dmitry Golovin, Marco Feroci, T. L. Cline, Martino Marisaldi, Tadayuki Takahashi, I. G. Mitrofanov, John O. Goldsten, C. Fellows, D. Svinkin, S. Golenetskii, Toshio Murakami, Charles A. Meegan, Valerie Connaughton, K. Harshman, Masanori Ohno, J. Cummings, A. von Kienlin, Makoto Tashiro, David Palmer, R. Aptekar, William V. Boynton, Xiao-Ling Zhang, and M. L. Litvak

Subjects
Physics, business.industry, business, Interplanetary spaceflight, Computer network, Network model
Published
2012

127. Galactic Sources Science With Agile: The Case Of The Carina Region

Author

E. Moretti, Claudio Labanti, Marco Tavani, G. Barbiellini, V. Cocco, A. Pellizzoni, M. Trifoglio, F. Longo, Marco Feroci, Luigi Pacciani, G. Di Cocco, C. Pittori, I. Lapshov, Ennio Morelli, Sandro Mereghetti, T. Froysland, Geiland Porrovecchio, A. Giuliani, Elena Pian, F. Perotti, D. Zanello, Alessio Trois, S. Colafrancesco, Martino Marisaldi, Michael F. Corcoran, I. Donnarumma, G. De Paris, Y. Evangelista, A. Argan, P. Picozza, Fulvio Gianotti, L. Salotti, F. Boffelli, A. Zambra, Francesco Lazzarotto, Andrea Bulgarelli, A. Rappoldi, M. Fiorini, Enrico Costa, Massimo Rapisarda, A. W. Chen, P. Giommi, E. Del Monte, G. Pucella, P. A. Caraveo, E. Vallazza, M. Prest, M. Galli, F. Verrecchia, F. Fuschino, Roberto Viotti, Filippo D'Ammando, Paolo Lipari, Paolo Soffitta, S. Vercellone, P. Santolamazza, Alda Rubini, P. W. Cattaneo, M. Mastropietro, V. Vittorini, Arnaud Ferrari, S. Sabatini, A. Morselli, M. Pilia, L. A. Antonelli, G. Piano, S., Sabatini, M., Tavani, E., Pian, A., Bulgarelli, P., Caraveo, R., Viotti, M. F., Corcoran, A., Giuliani, C., Pittori, F., Verrecchia, S., Vercellone, S., Mereghetti, A., Argan, G., Barbiellini, F., Boffelli, P. W., Cattaneo, A. W., Chen, V., Cocco, F., D'Ammando, E., Costa, Paris, G., Monte, E., Cocco, G., I., Donnarumma, Y., Evangelista, A., Ferrari, M., Feroci, M., Fiorini, T., Froysland, F., Fuschino, M., Galli, F., Gianotti, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, Longo, Francesco, M., Marisaldi, M., Mastropietro, E., Morelli, E., Moretti, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, G., Piano, P., Picozza, M., Pilia, G., Porrovecchio, G., Pucella, M., Prest, M., Rapisarda, A., Rappoldi, A., Rubini, P., Soffitta, M., Trifoglio, A., Troi, E., Vallazza, V., Vittorini, A., Zambra, D., Zanello, P., Santolamazza, P., Giommi, S., Colafrancesco, L. A., Antonelli, L., Salotti, Sabatini S, Tavani M, Pian E, Bulgarelli A, Caraveo P, Viotti R, Corcoran MF, Giuliani A, Pittori C, Verrecchia F, Vercellone S, Mereghetti S, Argan A, Barbiellini G, Boffelli F, Cattaneo PW, Chen AW, Cocco V, DAmmando F, Costa E, De Paris G, Del Monte E, Di Cocco G, Donnarumma I, Evangelista Y, Ferrari A, Feroci M, Fiorini M, Froysland T, Fuschino F, Galli M, Gianotti F, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Longo F, Marisaldi M, Mastropietro M, Morelli E, Moretti E, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Piano G, Picozza P, Pilia M, Porrovecchio G, Pucella G, Prest M, Rapisarda M, Rappoldi A, Rubini A, Soffitta P, Trifoglio M, Trois A, Vallazza E, Vittorini V, Zambra A, Zanello D, Santolamazza P, Giommi P, Colafrancesco S, Antonelli LA, and Salotti L

Subjects
Nuclear and High Energy Physics, Astrophysics::High Energy Astrophysical Phenomena, colliding wind binary, FOS: Physical sciences, Carina, Astrophysics, galactic gamma ray sky, High Energy Gamma-ray Astronomy, AGILE, Astrophysics::Solar and Stellar Astrophysics, Gamma rays: observations, Individual stars (Eta Carinae), Stars: winds, Outflows, X-rays: bynaries, Surface brightness, Instrumentation, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Colliding-wind binary, Physics, Nebula, Star formation, Molecular cloud, Gamma ray, Astronomy, Galactic sources, Galactic plane, Star cluster, Galactic source, Astrophysics - High Energy Astrophysical Phenomena
Abstract

During its first 2 years of operation, the gamma-ray AGILE satellite accumulated an extensive dataset for the Galactic plane. The data have been monitored for transient sources and several gamma-ray sources were detected. Their variability and possible association were studied. In this talk we will focus on the results of extensive observations of the Carina Region during the time period 2007 July - 2009 January, for a total livetime of ~130 days. The region is extremely complex, hosting massive star formation, with the remarkable colliding wind binary Eta Carinae, massive star clusters and HII regions (e.g. NGC 3324, RCW49, Westerlund II) and a giant molecular cloud extending over 150 pc (between l=284.7 and l=289). The Carina Nebula itself is the largest and IR highest surface brightness nebula of the Southern emisphere. We monitored several gamma ray sources in the Carina Region. In particular we detect a gamma ray source (1AGL J1043-5931) consistent with the position of Eta Carinae and report a remarkable 2-days gamma-ray flaring episode from this source on 2008 Oct 11-13. If 1AGL J1043-5931 is associated with the Eta Car system, our data provides the long sought first detection above 100 MeV of a colliding wind binary., 5 pages, 5 figures, proceedings of RICAP 2009

Published
2012

128. Scintillating fibers readout by single photon avalanche diodes (SPAD) for space applications

Author

Davide Bolognini, Piera Maccagnani, Andrea Giudice, Angelo Gulinatti, Danielo Rubini, Martino Marisaldi, Francesco Moscatelli, Claudio Labanti, Massimo Ghioni, Ivan Rech, Alessandro Berra, M. Prest, Georg Simmerle, and F. Fuschino

Subjects
Physics, Photon, sezele, business.industry, Physics::Instrumentation and Detectors, Detector, Photodetector, Avalanche photodiode, Particle detector, gamma-ray detector, Optics, Single-photon avalanche diode, single photon avalanche diode, Optoelectronics, business, Radiation hardening, Diode, scintillating fiber
Abstract

We present the design and performances of a radiation detector based on plastic scintillating fibers with doubleside readout by means of large-area Single Photon Avalanche Diodes (SPAD). This can be the basic step toward the realization of a large-area, cost-effective position sensitive detector to be employed in future space gammaray observatories. SPADs are silicon devices operated above the junction breakdown voltage (with the typical overvoltage of 5V), for which a single photon interacting in the active region is sufficient to trigger a selfsustainable avalanche discharge. SPADs can thus be used for the detection of very low light levels with a fast time response around 50ps FWHM for single photon detection, without spectroscopic capabilities. Large-area SPAD (500 μm in diameter) have been designed and fabricated at the CNR-IMM facility, with an intrinsic noise lower than 10kHz at -15°C, and are optically coupled to both ends of 3-meter long scintillating fibers, with the same diameter. Double-side readout is required to operate the devices in coincidence (10ns coincidence window), in order to reduce the rate of false detections to the level of 1Hz. The detectors have been tested with minimum ionizing particles at CERN PS demonstrating a detection efficiency larger than 90% and a moderate position resolution along the fiber due to the difference in time of arrival between the two photodetectors. Radiation hardness tests on SPADs have also been carried out, showing that large-area SPADs can be safely employed in low-inclination low Earth orbits.

Published
2012

129. Single Photon Avalanche Diodes for space applications

Author

F. Fuschino, Andrea Candelori, Andrea Giudice, Angelo Gulinatti, Ivan Rech, Davide Bolognini, Danilo Rubini, Martino Marisaldi, Piera Maccagnani, Massimo Ghioni, Georg Simmerle, M. Prest, Francesco Moscatelli, Alessandro Berra, Serena Mattiazzo, and Claudio Labanti

Subjects
Physics, Photomultiplier, Photon, sezele, Physics::Instrumentation and Detectors, business.industry, Detector, Settore FIS/01 - Fisica Sperimentale, Optics, Silicon photomultiplier, Scintillation counter, Optoelectronics, Photonics, business, Radiation hardening, Diode
Abstract

We study the possibility to use Single Photon Avalanche Diodes (SPADs) optically coupled to scintillating fibers as a novel type of gamma-ray detector for space applications. SPADs are silicon devices operating under polarization conditions above the junction breakdown voltage (typical overvoltage of 5V), for which a single photon interacting in the active region is sufficient to trigger a self sustainable avalanche discharge. SPADs can thus be used for the detection of very low light levels with an absolute timing accuracy of about 30 ps for single photon detection, without spectroscopic capabilities. In this presentation we report the preliminary results on large area SPAD (actual results refers to SPADs having 200 µm diameter, with the aim to grow up to 500 µm SPADs) coupled to scintillating fibers as the basic module for a particle tracker for space application. Dark counts rate as low as few tens of kHz at room temperature, lowering down to few kHz at −10°C have been obtained for the 200 µm devices, in accordance with the basic requirements for the proposed application. Similar instruments based on silicon photomultiplier (SiPM) readout have already been studied, but none based on SPAD has been realized up to now. Moreover, since very few information is available on SPADs for the use in a space environment, we performed bulk damage and total dose radiation tests with protons and gamma-rays in order to evaluate their radiation hardness properties and their suitability for application in a Low Earth Orbit (LEO) space mission. With this aim the SPAD devices have be irradiated using up to 20 krad total dose with gamma-rays and 5 krad with protons.

Published
2012

130. A large area detector proposed for the Large Observatory for X-ray Timing (LOFT)

Author

I. Donnarumma, Y. Evangelista, Phil Uttley, Christian Schmid, D. Macera, L. Pacciani, Paul S. Smith, T. Kennedy, J.-Y. Seyler, J. W. den Herder, Martino Marisaldi, Michael A. Nowak, A. de Rosa, Berend Winter, Dom Walton, E. Bozzo, A. Argan, Miriam Grassi, C. Tenzer, M. Ahangarianabhari, G. Zampa, Andrea Santangelo, Jörn Wilms, A. Vacchi, P. Bodini, Riccardo Campana, Claudio Labanti, Slawomir Suchy, Silvia Zane, P. Soffitta, F. Fuschino, Fabio Muleri, M. Hailey, S. Di Cosimo, Adrian Martindale, V. Petracek, P. Cais, Giuseppe Baldazzi, Yannick Favre, Mauro Orlandini, E. Del Monte, Didier Barret, Alain Cros, Emanuele Perinati, C. Feldman, M. Pohl, Franck Cadoux, J. Coker, Piero Malcovati, M. Feroci, René Hudec, P. Azzarello, Teresa Mineo, A. Rachevski, G.W. Fraser, Giuseppe Bertuccio, N. Zampa, SPIE, Takahashi, Tadayuki, Zane S., Walton D., Kennedy T., Feroci M., Den Herder J.-W., Ahangarianabhari M., Argan A., Azzarello P., Baldazzi G., Barret D., Bertuccio G., Bodin P., Bozzo E., Cadoux F., Cais P., Campana R., Coker J., Cros A., Del Monte E., De Rosa A., Di Cosimo S., Donnarumma I., Evangelista Y., Favre Y., Feldman C., Fraser G., Fuschino F., Grassi M., Hailey M.R., Hudec R., Labanti C., Macera D., Malcovati P., Marisaldi M., Martindale A., Mineo T., Muleri F., Nowak M., Orlandini M., Pacciani L., Perinati E., Petracek V., Pohl M., Rachevski A., Smith P., Santangelo A., Seyler J.-Y., Schmid C., Soffitta P., Suchy S., Tenzer C., Uttley P., Vacchi A., Zampa G., Zampa N., Wilms J., Winter B., High Energy Astrophys. & Astropart. Phys (API, FNWI), FORMATION STELLAIRE 2012, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Mullard Space Science Laboratory (MSSL), and University College of London [London] (UCL)

Subjects
Silicon, Photon, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Observatories, Collimators, FOS: Physical sciences, ddc:500.2, Astrophysics, 7. Clean energy, 01 natural sciences, Optics, Observatory, 0103 physical sciences, X-rays, Electronic, Optical and Magnetic Materials, Electrical and Electronic Engineering, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Compact objects, Physics, Millisecond, Photons, Equipment and services, sezele, 010308 nuclear & particles physics, Payload, business.industry, Sensors, Applied Mathematics, Detector, Antenna aperture, Computer Science Applications1707 Computer Vision and Pattern Recognition, Condensed Matter Physics, Capillaries, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Neutron star, X-ray Timing, Electronic, Optical and Magnetic Materials, Instrumentation and Methods for Astrophysics, business, Astrophysics - Instrumentation and Methods for Astrophysics, Energy (signal processing), Compact object
Abstract

The Large Observatory for X-ray Timing (LOFT) is one of the four candidate ESA M3 missions considered for launch in the 2022 time-frame. It is specifically designed to perform fast X-ray timing and probe the status of the matter near black holes and neutron stars. The LOFT scientific payload is composed of a Large Area Detector (LAD) and a Wide Field Monitor (WFM). The LAD is a 10 m2-class pointed instrument with 20 times the collecting area of the best past timing missions (such as RXTE) over the 2-30 keV range, which holds the capability to revolutionize studies of X-ray variability down to the millisecond time scales. Its ground-breaking characteristic is a low mass per unit surface, enabling an effective area of ~10 m^2 (@10 keV) at a reasonable weight. The development of such large but light experiment, with low mass and power per unit area, is now made possible by the recent advancements in the field of large-area silicon detectors - able to time tag an X-ray photon with an accuracy, Proceedings of SPIE, Vo. 8443, Paper No. 8443-87

Published
2012

131. On-ground calibration of AGILE-GRID with a photon beam: results and lessons for the future

Author

Maura Pilia, Alda Rubini, Alessio Trois, D. Zanello, C. Pittori, L. Salotti, A. Pellizzoni, G. De Paris, A. Giuliani, Fulvio Gianotti, Elena Moretti, Massimo Rapisarda, F. Perotti, E. Del Monte, P. Picozza, M. Trifoglio, Marco Tavani, Paolo Lipari, V. Vittorini, A. Rappoldi, G. Pucella, E. Striani, Sandro Mereghetti, Lina Quintieri, Francesco Lazzarotto, E. Vallazza, I. Lapshov, Ennio Morelli, G. Mazzitelli, P. A. Caraveo, P. W. Cattaneo, M. Giusti, F. Fuschino, A. Argan, Andrea Bulgarelli, S. Colafrancesco, Martino Marisaldi, Enrico Costa, G. Barbiellini, L. Foggetta, M. Prest, I. Donnarumma, Y. Evangelista, A. W. Chen, P. Giommi, M. Fiorini, Bruno Buonomo, Marco Feroci, Luigi Pacciani, Arnaud Ferrari, M. Galli, F. Longo, S. Sabatini, F. Verrecchia, G. Piano, P. Valente, Filippo D'Ammando, Paolo Soffitta, A. Morselli, Fabrizio Lucarelli, Claudio Labanti, S. Vercellone, G. Di Cocco, P. Santolamazza, Tadayuki Takahashi, Stephen S. Murray, Jan-Willem A. den Herder, P. W., Cattaneo, A., Rappoldi, A., Argan, B., Buonomo, A., Bulgarelli, A. W., Chen, F., D'Ammando, L., Foggetta, F., Fuschino, M., Galli, F., Gianotti, A., Giuliani, Longo, Francesco, M., Marisaldi, G., Mazzitelli, A., Pellizzoni, M., Prest, G., Pucella, L., Quintieri, M., Tavani, M., Trifoglio, A., Troi, P., Valente, E., Vallazza, S., Vercellone, G., Barbiellini, P., Caraveo, E., Costa, Paris, G., Monte, E., Cocco, G., I., Donnarumma, Y., Evangelista, A., Ferrari, M., Feroci, M., Fiorini, M., Giusti, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, F., Lucarelli, S., Mereghetti, E., Morelli, E., Moretti, A., Morselli, L., Pacciani, F., Perotti, G., Piano, P., Picozza, M., Pilia, M., Rapisarda, A., Rubini, S., Sabatini, P., Soffitta, E., Striani, V., Vittorini, D., Zanello, S., Colafrancesco, P., Giommi, C., Pittori, P., Santolamazza, F., Verrecchia, and L., Salotti

Subjects
Physics, Photon, Spectrometer, Physics::Instrumentation and Detectors, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Detector, agile, Bremsstrahlung, tagged photon beam, Scintillator, Calibrations, silicon tracker, High Energy Gamma-ray Astronomy, Optics, Beamline, Dipole magnet, business, Beam (structure)
Abstract

At the core of the AGILE scientific instrument, designed to operate on a satellite, there is the Gamma Ray Imaging Detector (GRID) consisting of a Silicon Tracker (ST), a Cesium Iodide Mini-Calorimeter and an Anti-Coincidence system of plastic scintillator bars. The ST needs an on-ground calibration with a γ-ray beam to validate the simulation used to calculate the energy response function and the effective area versus the energy and the direction of the γ rays. A tagged γ-ray beam line was designed at the Beam Test Facility (BTF) of the INFN Laboratori Nazionali of Frascati (LNF), based on an electron beam generating γ rays through bremsstrahlung in a position-sensitive target. The γ-ray energy is deduced by the difference with the post-bremsstrahlung electron energy 1-.2 The electron energy is measured by a spectrometer consisting of a dipole magnet and an array of position sensitive silicon strip detectors, the Photon Tagging System (PTS). The use of the combined BTF-PTS system as tagged photon beam requires understanding the efficiency of γ-ray tagging, the probability of fake tagging, the energy resolution and the relation of the PTS hit position versus the γ-ray energy. This paper describes this study comparing data taken during the AGILE calibration occurred in 2005 with simulation.

Published
2012

132. AGILE detection of Cygnus X-3 {\gamma}-ray active states during the period mid-2009/mid-2010

Author

E. Moretti, Maura Pilia, Guy G. Pooley, V. Vittorini, G. De Paris, G. Di Cocco, M. Trifoglio, Alessio Trois, A. Rappoldi, E. Vallazza, L. Salotti, F. Perotti, Francesco Lazzarotto, Francesco Longo, C. Pittori, A. Zambra, Paolo Soffitta, A. Morselli, A. Giuliani, Danny Steeghs, A. Pellizzoni, Y. Evangelista, I. Donnarumma, V. Cocco, Marco Tavani, D. Zanello, T. Contessi, M. Galli, Piergiorgio Picozza, S. Vercellone, E. Striani, Fulvio Gianotti, G. Piano, Michael L. McCollough, S. Sabatini, Sergio Colafrancesco, F. Verrecchia, P. Santolamazza, I. Lapshov, Alda Rubini, N. A. Nizhelskij, E. Del Monte, Sandro Mereghetti, Paolo Giommi, P. W. Cattaneo, N. Lavonen, A. W. Chen, Anne Lähteenmäki, Alessio Aboudan, Massimo Rapisarda, S. A. Trushkin, Guido Barbiellini, Joni Tammi, M. Prest, D. Hannikainen, Marco Feroci, Luigi Pacciani, C. Labanti, Filippo D'Ammando, A. Argan, Andrea Bulgarelli, Martino Marisaldi, Enrico Costa, M. Giusti, Karri I. I. Koljonen, Ennio Morelli, Massimiliano Fiorini, P. A. Caraveo, G. Pucella, Paolo Lipari, F. Lucarelli, F. Fuschino, Riccardo Campana, A., Bulgarelli, M., Tavani, A. W., Chen, Y., Evangelista, M., Trifoglio, F., Gianotti, G., Piano, S., Sabatini, E., Striani, G., Pooley, S., Trushkin, N. A., Nizhelskij, M., Mccollough, K. I., I., D., Hannikainen, A., L\ahteenm\aki, J., Tammi, N., Lavonen, D., Steegh, A., Aboudan, A., Argan, G., Barbiellini, R., Campana, P., Caraveo, P. W., Cattaneo, V., Cocco, T., Contessi, E., Costa, F., D'Ammando, Monte, E., Paris, G., Cocco, G., I., Donnarumma, M., Feroci, M., Fiorini, F., Fuschino, M., Galli, A., Giuliani, M., Giusti, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, Longo, Francesco, M., Marisaldi, S., Mereghetti, E., Morelli, E., Moretti, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, P., Picozza, M., Pilia, M., Prest, G., Pucella, M., Rapisarda, A., Rappoldi, A., Rubini, P., Soffitta, A., Troi, E., Vallazza, S., Vercellone, V., Vittorini, A., Zambra, D., Zanello, P., Giommi, C., Pittori, F., Verrecchia, P., Santolamazza, F., Lucarelli, S., Colafrancesco, L., Salotti, Bulgarelli A, Tavani M, Chen AW, Evangelista Y, Trifoglio M, Gianotti F, Piano G, Sabatini S, Striani E, Pooley G, Trushkin S, Nizhelskij NA, McCollough M, Koljonen KII, Hannikainen D, Lahteenmaki A, Tammi J, Lavonen N, Steeghs D, Aboudan A, Argan A, Barbiellini G, Campana R, Caraveo P, Cattaneo PW, Cocco V, Contessi T, Costa E, DAmmando F, Del Monte E, De Paris G, Di Cocco G, Donnarumma I, Feroci M, Fiorini M, Fuschino F, Galli M, Giuliani A, Giusti M, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Longo F, Marisaldi M, Mereghetti S, Morelli E, Moretti E, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Picozza P, Pilia M, Prest M, Pucella G, Rapisarda M, Rappoldi A, Rubini A, Soffitta P, Trois A, Vallazza E, Vercellone S, Vittorini V, Zambra A, Zanello D, Giommi P, Pittori C, Verrecchia F, Santolamazza P, Lucarelli F, Colafrancesco S, Salotti L, Anne Lähteenmäki Group, Aalto-yliopisto, and Aalto University

Subjects
gamma-rays: stars, education, Flux, Astrophysics, 01 natural sciences, gamma-rays: stars – stars: individual: Cygnus X-3, stars [gamma-rays], Acceleration, Astrophysical jet, 0103 physical sciences, MAGIC (telescope), microquasar, Cygnus X-3, 010303 astronomy & astrophysics, QB, stars: individual: Cygnus X-3, Physics, star [gamma-rays], 010308 nuclear & particles physics, AGILE satellite, gamma rays, Gamma ray, Astronomy and Astrophysics, Particle acceleration, Wavelength, Space and Planetary Science, individual: Cygnus X-3 [stars], Production (computer science), Astrophysics - High Energy Astrophysical Phenomena
Abstract

Cygnus X-3 (Cyg X-3) is a well-known microquasar producing variable emission at all wavelengths. Cyg X-3 is a prominent X-ray binary producing relativistic jets, and studying its high energy emission is crucial for the understanding of the fundamental acceleration processes in accreting compact objects. Aims. Our goal is to study extreme particle acceleration and {\gamma}-ray production above 100 MeV during special spectral states of Cyg X- 3 usually characterized by a low hard X-ray flux and enhanced soft X-ray states. We observed Cyg X-3 with the AGILE satellite in extended time intervals from 2009 Jun.-Jul., and 2009 Nov.-2010 Jul. We report here the results of the AGILE {\gamma}-ray monitoring of Cyg X-3 as well as the results from extensive multiwavelength campaigns involving radio (RATAN-600, AMI-LA and Mets\"{a}hovi Radio Observatories) and X-ray monitoring data (XTE and Swift). We detect a series of repeated {\gamma}-ray flaring activity from Cyg X-3 that correlate with the soft X-ray states and episodes of decreasing or non-detectable hard X-ray emission. Furthermore, we detect {\gamma}-ray enhanced emission that tends to be associated with radio flares greater than 1 Jy at 15 GHz, confirming a trend already detected in previous observations. The source remained active above 100 MeV for an extended period of time (almost 1.5 months in 2009 Jun.-Jul. and 1 month in 2010 May). We study in detail the short timescale {\gamma}-ray flares that occurred before or near the radio peaks. Our results confirm the transient nature of the extreme particle acceleration from the microquasar Cyg X-3. A series of repeated {\gamma}-ray flares shows correlations with radio and X-ray emission confirming a well established trend of emission. We compare our results with Fermi-LAT and MAGIC TeV observations of Cyg X-3., Comment: 16 pages, 8 figures, 7 tables; A&A (2011)

Published
2011

133. The AGILE observations of the hard and bright GRB 100724B

Author

P. Santolamazza, M. Galli, Piergiorgio Picozza, S. Cutini, F. Verrecchia, V. Vittorini, Paolo Giommi, M. Trifoglio, F. Perotti, E. Striani, Sandro Mereghetti, I. Lapshov, P. W. Cattaneo, A. W. Chen, Elena Moretti, Fulvio Gianotti, M. Prest, E. Del Monte, Francesco Lazzarotto, A. Rappoldi, E. Vallazza, G. Di Cocco, Marco Feroci, Filippo D'Ammando, Paolo Soffitta, Luigi Pacciani, Guido Barbiellini, Paolo Lipari, I. Donnarumma, C. Labanti, Francesco Longo, A. Morselli, Maura Pilia, A. Argan, Andrea Bulgarelli, Alessio Trois, P. A. Caraveo, Enrico Costa, S. Vercellone, G. Piano, Marco Tavani, S. Sabatini, Martino Marisaldi, L. A. Antonelli, L. Salotti, Massimo Rapisarda, Y. Evangelista, A. Giuliani, C. Pittori, A. Pellizzoni, G. Pucella, F. Fuschino, Del Monte E, Barbiellini G, Donnarumma I, Fuschino F, Giuliani A, Longo F, Marisaldi M, Pucella G, Tavani M, Trifoglio M, Trois A, Argan A, Bulgarelli A, Caraveo P, Cattaneo PW, Chen AW, Costa E, DAmmando F, Di Cocco G, Evangelista Y, Feroci M, Galli M, Gianotti F, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Mereghetti S, Moretti E, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Piano G, Picozza P, Pilia M, Prest M, Rapisarda M, Rappoldi A, Sabatini S, Soffitta P, Striani E, Vallazza E, Vercellone S, Vittorini V, Antonelli LA, Cutini S, Pittori C, Santolamazza P, Verrecchia F, Giommi P, Salotti L, E., Del Monte, G., Barbiellini, I., Donnarumma, F., Fuschino, A., Giuliani, Longo, Francesco, M., Marisaldi, G., Pucella, M., Tavani, M., Trifoglio, A., Troi, A., Argan, A., Bulgarelli, P., Caraveo, P. W., Cattaneo, A. W., Chen, E., Costa, F., D'Ammando, Cocco, G., Y., Evangelista, M., Feroci, M., Galli, F., Gianotti, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, S., Mereghetti, E., Moretti, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, G., Piano, P., Picozza, M., Pilia, M., Prest, M., Rapisarda, A., Rappoldi, S., Sabatini, P., Soffitta, E., Striani, E., Vallazza, S., Vercellone, V., Vittorini, L. A., Antonelli, S., Cutini, C., Pittori, P., Santolamazza, F., Verrecchia, P., Giommi, and L., Salotti

Subjects
Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Context (language use), Astrophysics, gamma-ray burst: individual: GRB 100724B, individual: GRB 100724B [gamma-ray burst], emission at MeV and GeV, gamma ray burst, symbols.namesake, Observatory, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Cross-correlation, AGILE satellite, Astronomy and Astrophysics, gamma rays: general, gamma rays: general / gamma-ray burst: individual: GRB 100724B, Lorentz factor, Space and Planetary Science, symbols, Gamma-ray burst, Interplanetary spaceflight, Astrophysics - High Energy Astrophysical Phenomena, Event (particle physics), general [gamma rays], Fermi Gamma-ray Space Telescope
Abstract

The observation of Gamma Ray Bursts (GRBs) in the gamma-ray band has been advanced by the AGILE and Fermi satellites after the era of the Compton Gamma-Ray Observatory. AGILE and Fermi are showing that the GeV-bright GRBs share a set of common features, particularly the high fluence from the keV up to the GeV energy bands, the high value of the minimum Lorentz factor, the presence of an extended emission of gamma-rays, often delayed with respect to lower energies, and finally the possible presence of multiple spectral components. GRB 100724B, localised in a joint effort by Fermi and the InterPlanetary Newtork, is the brightest burst detected in gamma-rays so far by AGILE. Characteristic features of GRB 100724B are the simultaneous emissions at MeV and GeV, without delayed onset nor time lag as shown by the analysis of the cross correlation function, and the significant spectral evolution in hard X-rays over the event duration. In this paper we show the analysis of the AGILE data of GRB 100724B and we discuss its features in the context of the bursts observed so far in gamma-rays and the recently proposed models., 8 pages, 5 figures. Accepted for publication by A&A. Final version after the correction by the language editor

Published
2011

134. High spatial resolution correlation of AGILE TGFs and global lightning activity above the equatorial belt

Author

A. Zambra, F. Fuschino, C. Pittori, Marco Feroci, Luigi Pacciani, M. Fiorini, P. Santolamazza, Claudio Labanti, A. W. Chen, Alda Rubini, E. Vallazza, S. Vercellone, P. W. Cattaneo, P. Giommi, G. Pucella, G. De Paris, G. Di Persio, Paolo Lipari, Arnaud Ferrari, A. Pellizzoni, Francesco Lazzarotto, F. Perotti, L. Salotti, L. A. Antonelli, Filippo D'Ammando, Paolo Soffitta, Elena Moretti, S. Sabatini, Massimo Rapisarda, A. Rappoldi, M. Prest, I. Donnarumma, Y. Evangelista, D. Zanello, Guido Barbiellini, V. Vittorini, E. Striani, P. Picozza, A. Giuliani, M. Trifoglio, Fabrizio Lucarelli, I. Lapshov, A. Argan, Andrea Bulgarelli, E. Del Monte, G. Di Cocco, P. A. Caraveo, S. Cutini, Enrico Costa, M. Galli, Maura Pilia, F. Verrecchia, Alessio Trois, Francesco Longo, Fulvio Gianotti, Martino Marisaldi, A. Morselli, G. Piano, Marco Tavani, Sandro Mereghetti, and S. Colafrancesco

Subjects
Physics, Correlation, Geophysics, Meteorology, Equator, High spatial resolution, General Earth and Planetary Sciences, Satellite, Radio atmospheric, Lightning, Latitude, Terrestrial gamma-ray flash
Abstract

[1] The AGILE satellite detects Terrestrial Gamma-ray Flashes (TGFs) in the 0.35–100 MeV energy range using its Mini-Calorimeter (MCAL) instrument with an average detection rate of 10 TGFs/month. Thanks to its Low Earth Orbit with only 2.5 degree of inclination, AGILE guarantees an unprecedented exposure above the equator, where both lightning activity and TGF detection peak. Here we report the comparison between the AGILE TGFs detected between March 2009 and February 2010 and full climatology lightning worldwide distribution based on satellite optical observations from LIS (Lightning Imaging Sensor) and OTD (Optical Transient Detector) instruments. This approach is complementary to the one-to-one TGF/lightning correlations by ground-based sferics measurements. Based on mono and bi-dimensional Kolmogorov-Smirnov tests, we show that the AGILE TGFs and time-averaged global lightning in the equatorial area are not drawn from the same distribution. However, we find significant regional differences in the degree of correlation as well as in the TGF/lightning ratio. In the case of south east Asia we find a 87% probability for the TGF and lightning being samples of the same distribution. This result supports the idea that the physical conditions at play in TGF generation can have strong geographical and climatological modulation. Based on the assumption that the observed range of TGF/flash ratio holds at all latitudes we can estimate a global rate of ≃ 220 ÷ 570 TGFs per day. The observed TGF/flash geographical modulation as well as the TGF global rate estimate are in agreement with previous observations.

Published
2011

135. Characterization of an ASIC front-end electronics dedicated to the silicon drift detectors

Author

Marco Grassi, Paolo Rossi, Alexander Rashevsky, A. Rubini, I. Donnarumma, Y. Evangelista, Piero Malcovati, F. Lazzarotto, F. Fuschino, Giuseppe Bertuccio, Martino Marisaldi, Stefano Cappelli, M. Feroci, L. Picolli, Claudio Labanti, Francesco Navarria, L. Pacciani, F. Muleri, Enrico Costa, Ennio Morelli, N. Zampa, Giuseppe Baldazzi, E. Del Monte, A. Vacchi, Riccardo Campana, M. Rapisarda, G. Zampa, P. Soffitta, Labanti, C, Baldazzi, G., Malcovati, P., Bertuccio, G., Feroci, M., Zampa, G., Grassi, M., Picolli, L., Evangelista, Y., Fuschino, F., Marisaldi, M., Morelli, E., Campana, R., Del Monte, E., Pacciani, L., Muleri, F., Costa, E., Donnarumma, I., Lazzarotto, F., Rapisarda, M., Rubini, A., Soffitta, P., Zampa, N., Rashevsky, A., Vacchi, A., Cappelli, S., Navarria, F., and Rossi, P.

Subjects
Physics, Coupling, Radiology, Nuclear Medicine and Imaging, Nuclear and High Energy Physics, Photon, Radiation, sezele, business.industry, Physics::Instrumentation and Detectors, Detector, ComputingMethodologies_IMAGEPROCESSINGANDCOMPUTERVISION, Noise (electronics), Characterization (materials science), Optics, Application-specific integrated circuit, Nuclear Medicine and Imaging, Electronic engineering, Point (geometry), business, Radiology, Energy (signal processing), Nuclear and High Energy Physic
Abstract

Large-area multi-anode Silicon Drift Detectors (SDDs) have X-ray imaging and spectroscopic characteristics that make them extremely attractive in the perspective of their applications to the field of space astrophysics and in instruments for medical diagnostic imaging. We describe here, in a few words, two developing applications concerning both these application fields. Nevertheless, the aim of this paper is to describe the characterisation of an ASIC suitably developed for coupling with SDDs. Notwithstanding the 1D nature of the SDD when the event time is not known, an algorithm that exploits the charge diffusion to reconstruct the position of the photon absorption point also along the drift direction (that is, the one formally not position-sensitive) was developed. So the SDD has the actual 2D imaging capability with both the spatial and energy resolution. The ASIC was developed specifically to account for these detector characteristics and to improve them. The structure of the ASIC and the 2D imaging method will be described and the characterization of the first prototypes of the ASIC will be exposed in terms of the energy resolution and noise. Finally preliminary tests of the ASIC will be shown. © 2011 IEEE.

Published
2011

136. Neutral Pion Emission from Accelerated Protons in the Supernova Remnant W44

Author

Yasuo Fukui, E. Striani, Y. Evangelista, E. Del Monte, C. Pittori, Guido Barbiellini, F. Lucarelli, A. Pellizzoni, Kazufumi Torii, Paolo Soffitta, Giovanni F. Bignami, M. Cardillo, Massimo Rapisarda, Satoshi Yoshiike, Gloria Mabel Dubner, Francesco Longo, G. Castelletti, I. Donnarumma, Andrea Bulgarelli, Enrico Costa, S. Vercellone, G. Pucella, P. Picozza, A. Rappoldi, A. Giuliani, V. Vittorini, Paolo Giommi, M. Trifoglio, A. W. Chen, Marco Feroci, Luigi Pacciani, P. A. Caraveo, Francesco Lazzarotto, Alessio Trois, F. Verrecchia, Fulvio Gianotti, Martino Marisaldi, Marco Tavani, S. Sabatini, Sergio Colafrancesco, Sandro Mereghetti, T. Contessi, P. W. Cattaneo, G. Piano, A., Giuliani, M., Cardillo, M., Tavani, Y., Fukui, S., Yoshiike, K., Torii, G., Dubner, G., Castelletti, G., Barbiellini, A., Bulgarelli, P., Caraveo, E., Costa, P. W., Cattaneo, A., Chen, T., Contessi, Monte, E., I., Donnarumma, Y., Evangelista, M., Feroci, F., Gianotti, F., Lazzarotto, F., Lucarelli, Longo, Francesco, M., Marisaldi, S., Mereghetti, L., Pacciani, A., Pellizzoni, G., Piano, P., Picozza, C., Pittori, G., Pucella, M., Rapisarda, A., Rappoldi, S., Sabatini, P., Soffitta, E., Striani, M., Trifoglio, A., Troi, S., Vercellone, F., Verrecchia, V., Vittorini, S., Colafrancesco, P., Giommi, and G., Bignami

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Hadron, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Radiation, Spectral line, Pion, acceleration of particles, cosmic rays, gamma rays: general, ISM: supernova remnants, Ejecta, Supernova remnant, acceleration of particle, cosmic ray, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Range (particle radiation), Molecular cloud, supernova remnants [ISM], Astronomy and Astrophysics, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, general [gamma rays]
Abstract

We present the AGILE gamma-ray observations in the energy range 50 MeV - 10 GeV of the supernova remnant (SNR) W44, one of the most interesting systems for studying cosmic-ray production. W44 is an intermediate-age SNR (20, 000 years) and its ejecta expand in a dense medium as shown by a prominent radio shell, nearby molecular clouds, and bright [SII] emitting regions. We extend our gamma-ray analysis to energies substantially lower than previous measurements which could not conclusively establish the nature of the radiation. We find that gamma-ray emission matches remarkably well both the position and shape of the inner SNR shocked plasma. Furthermore, the gamma-ray spectrum shows a prominent peak near 1 GeV with a clear decrement at energies below a few hundreds of MeV as expected from neutral pion decay. Here we demonstrate that: (1) hadron-dominated models are consistent with all W44 multiwavelength constraints derived from radio, optical, X-ray, and gamma-ray observations; (2) ad hoc lepton-dominated models fail to explain simultaneously the well-constrained gamma-ray and radio spectra, and require a circumstellar density much larger than the value derived from observations; (3) the hadron energy spectrum is well described by a power-law (with index s = 3.0 \pm 0.1) and a low-energy cut-off at Ec = 6 \pm 1 GeV. Direct evidence for pion emission is then established in an SNR for the first time., accepted for publication on ApJL

Published
2011

137. The flaring blazars of the first 1.5 years of the AGILE mission

Author

E. Moretti, A. Argan, Andrea Bulgarelli, Geiland Porrovecchio, Enrico Costa, A. W. Chen, P. Giommi, E. Vallazza, F. Longo, G. De Paris, G. Barbiellini, P. Santolamazza, P. Picozza, D. Zanello, Arnaud Ferrari, F. Perotti, M. Galli, Ennio Morelli, Alda Rubini, P. W. Cattaneo, A. Morselli, F. Verrecchia, S. Sabatini, F. Fuschino, Filippo D'Ammando, Paolo Soffitta, Massimo Rapisarda, Francesco Lazzarotto, M. Pilia, Paolo Lipari, S. Vercellone, I. Lapshov, M. Mastropietro, V. Vittorini, L. A. Antonelli, G. Piano, M. Prest, C. Pittori, I. Donnarumma, Y. Evangelista, T. Froysland, G. Di Cocco, Marco Feroci, E. Del Monte, Luigi Pacciani, Marco Tavani, A. Zambra, Alessio Trois, A. Pellizzoni, P. A. Caraveo, Sandro Mereghetti, M. Fiorini, Fulvio Gianotti, A. Giuliani, S. Colafrancesco, Martino Marisaldi, Claudio Labanti, M. Trifoglio, F. Boffelli, V. Cocco, L. Salotti, A. Rappoldi, G. Pucella, L., Pacciani, A., Bulgarelli, A. W., Chen, F., D'Ammando, I., Donnarumma, A., Giuliani, Longo, Francesco, G., Pucella, M., Tavani, S., Vercellone, V., Vittorini, A., Argan, G., Barbiellini, F., Boffelli, P., Caraveo, P. W., Cattaneo, V., Cocco, E., Costa, Paris, G., Monte, E., Cocco, G., Y., Evangelista, A., Ferrari, M., Feroci, M., Fiorini, T., Froysland, F., Fuschino, M., Galli, F., Gianotti, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, M., Marisaldi, M., Mastropietro, S., Mereghetti, E., Morelli, E., Moretti, A., Morselli, A., Pellizzoni, F., Perotti, G., Piano, P., Picozza, M., Pilia, G., Porrovecchio, M., Prest, M., Rapisarda, A., Rappoldi, A., Rubini, S., Sabatini, P., Soffitta, M., Trifoglio, A., Troi, E., Vallazza, A., Zambra, D., Zanello, L. A., Antonelli, S., Colafrancesco, P., Giommi, C., Pittori, F., Verrecchia, P., Santolamazza, L., Salotti, Pacciani L, Bulgarelli A, Chen AW, DAmmando F, Donnarumma I, Giuliani A, Longo F, Pucella G, Tavani M, Vercellone S, Vittorini V, Argan A, Barbiellini G, Boffelli F, Caraveo P, Cattaneo PW, Cocco V, Costa E, De Paris G, Del Monte E, Di Cocco G, Evangelista Y, Ferrari A, Feroci M, Fiorini M, Froysland T, Fuschino F, Galli M, Gianotti F, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Marisaldi M, Mastropietro M, Mereghetti S, Morelli E, Moretti E, Morselli A, Pellizzoni A, Perotti F, Piano G, Picozza P, Pilia M, Porrovecchio G, Prest M, Rapisarda M, Rappoldi A, Rubini A, Sabatini S, Soffitta P, Trifoglio M, Trois A, Vallazza E, Zambra A, Zanello D, Antonelli LA, Colafrancesco S, Giommi P, Pittori C, Verrecchia F, Santolamazza P, and Salotti L

Subjects
Nuclear and High Energy Physics, Active galactic nucleus, Galaxies: active, Galaxies: quasars: general, Galaxies: jets, Radiation mechanisms: non-thermal, Flux, FOS: Physical sciences, Astrophysics, blazar, law.invention, AGILE, Telescope, law, Egret, gamma-ray, Blazar, Instrumentation, Large fov, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), biology, Astronomy, Quasar, Active Galactic Nuclei, biology.organism_classification, multiwavelength campaign, Astrophysics - High Energy Astrophysical Phenomena, BL Lac object
Abstract

We report the AGILE γ -ray observations and the results of the multiwavelength campaigns on seven flaring blazars detected by the mission: During two multiwavelength campaigns, we observed γ -ray activity from two Flat Spectrum Radio Quasars of the Virgo region, e.g. 3C 279 and 3C 273 (the latter being the first extragalactic source simultaneously observed with the γ -ray telescope and the hard X ray imager of the mission). Due to the large FOV of the AGILE/GRID instrument, we achieved an almost continuous coverage of the FSRQ 3C 454.3. The source showed flux above 10 −6 photons/cm 2 /s ( E > 100 MeV ) and showed day by day variability during all the AGILE observing periods. In the EGRET era, the source was found in high γ -ray activity only once. An other blazar, PKS 1510-089 was frequently found in high γ -ray activity. S5 0716+71, an intermediate BL Lac object, exhibited a very high γ -ray activity and fast γ -ray variability during a period of intense optical activity. We observed high γ -ray activity from W Comae, a BL Lac object, and Mrk 421, a high energy peaked BL Lac object. For this source, a multiwavelength campaign from optical to TeV has been performed.

Published
2011

138. Imaging performance of a large-area Silicon Drift Detector for X-ray astronomy

Author

Marco Grassi, L. Picolli, E. Del Monte, Piero Malcovati, Fabio Muleri, M. Mastropietro, Francesco Lazzarotto, Enrico Costa, Paolo Soffitta, Marco Feroci, Luigi Pacciani, Claudio Labanti, Alda Rubini, Ennio Morelli, G. Zampa, I. Donnarumma, Giuseppe Baldazzi, Y. Evangelista, V. Bonvicini, Martino Marisaldi, Massimo Rapisarda, N. Zampa, Alexander Rashevsky, F. Fuschino, Riccardo Campana, A. Vacchi, R. Campana, G. Zampa, M. Feroci, A. Vacchi, V. Bonvicini, E. Del Monte, Y. Evangelista, F. Fuschino, C. Labanti, M. Marisaldi, F. Muleri, L. Pacciani, M. Rapisarda, A. Rashevsky, A. Rubini, P. Soffitta, N. Zampa, G. Baldazzi, E. Costa, I. Donnarumma, M. Grassi, F. Lazzarotto, P. Malcovati, M. Mastropietro, E. Morelli, and L. Picolli

Subjects
Physics, Nuclear and High Energy Physics, Large Hadron Collider, Photon, Silicon drift detector, High-energy astronomy, business.industry, Physics::Instrumentation and Detectors, X-RAYS, Detector, Monte Carlo method, Tracking (particle physics), HIGH ENERGY ASTROPHYSICS, Anode, Optics, business, SILICON DRIFT DETECTORS, Instrumentation
Abstract

Large-area multi-anode Silicon Drift Detectors (SDDs) have X-ray imaging and spectroscopic characteristics that make them extremely attractive in the perspective of their applications to the field of space astrophysics. We describe here the imaging performance of such a detector, originally developed for particle tracking in the ALICE experiment at LHC, as derived by laboratory measurements and Monte Carlo simulations. Despite an anode pitch of View the MathML source, we measured a position resolution as high as View the MathML source by charge weighting in the anode direction, for photon energies in the range 2–10 keV. These results are comparable to those obtained with the same detectors in particle tracking. Notwithstanding the 1-D nature of the devices, as far as their read-out is concerned, we envisaged an algorithm that exploits the charge diffusion to reconstruct the position of the photon absorption point also along the drift direction (that is, the one formally not position-sensitive). With the current set-up, the position resolution was measured as View the MathML source in the same energy range as above. Such 2-D imaging capability in a 1-D detector, although asymmetric, is highly useful in space applications, where the power and the complexity requested by a 2-D read-out system is sometimes unaffordable. Keywords: High Energy Astrophysics; Silicon Drift Detectors; X-rays

Published
2011

139. AGILE detection of extreme \gamma-ray activity from the blazar PKS 1510-089 during March 2009. Multifrequency analysis

Author

A. Di Paola, Mark Gurwell, L. Fuhrmann, Jochen Heidt, C. Pittori, T. Froysland, G. De Paris, M. Pasanen, Elena Pian, Tatiana S. Konstantinova, A. Rubini, Sofia O. Kurtanidze, I. M. McHardy, F. Fuschino, L. Pacciani, Sandro Mereghetti, D. A. Morozova, A. A. Arkharov, Uwe Bach, Corrado Trigilio, I. Donnarumma, P. Lipari, A. Zambra, Geiland Porrovecchio, I. Agudo, M. F. Aller, M. Feroci, Merja Tornikoski, G. Piano, Y. Evangelista, Claudio Labanti, G. Umana, Filippo D'Ammando, Carla Buemi, H. A. Krimm, S. Colafrancesco, M. Fiorini, F. Perotti, Stefano Covino, Fulvio Gianotti, E. Del Monte, G. Pucella, A. Rappoldi, Andrei Berdyugin, D. Zanello, Svetlana G. Jorstad, P. Caraveo, B. McBreen, I. S. Troitsky, Paolo Leto, A. Argan, E. Forné, F. Boffelli, Talvikki Hovatta, Erika Benítez, A. Sillanpää, P. Picozza, Arnaud Ferrari, L. Salotti, V. Vittorini, Kari Nilsson, A. Morselli, E. Striani, L. A. Antonelli, Andrea Bulgarelli, Wen Ping Chen, B. Jordan, P. Santolamazza, G. Di Cocco, Givi N. Kimeridze, M. Rapisarda, Massimo Frutti, S. Sabatini, I. Lapshov, F. Lazzarotto, A. Pellizzoni, E. Costa, Martino Marisaldi, M. Tavani, E. Vallazza, C. M. Raiteri, A. Trois, M. Pilia, H. Y. Hsiao, Omar M. Kurtanidze, Valeri M. Larionov, M. Prest, M. Roca-Sogorb, A. W. Chen, P. W. Cattaneo, P. Soffitta, Hugh D. Aller, V. Cocco, A. Giuliani, M. Orienti, M. Villata, Mauro Dolci, M. Trifoglio, Elina Lindfors, J. L. Gomez, P. Romano, Alan P. Marscher, P. Giommi, Anne Lähteenmäki, David Hiriart, G. Barbiellini, Ekaterina Koptelova, G. Giovannini, F. Longo, S. Vercellone, L. O. Takalo, E. N. Kopatskaya, M. Galli, F. Verrecchia, D. Blinov, F., D'Ammando, C. M., Raiteri, M., Villata, P., Romano, G., Pucella, H. A., Krimm, S., Covino, M., Orienti, G., Giovannini, S., Vercellone, E., Pian, I., Donnarumma, V., Vittorini, M., Tavani, A., Argan, G., Barbiellini, F., Boffelli, A., Bulgarelli, P., Caraveo, P. W., Cattaneo, A. W., Chen, V., Cocco, E., Costa, Monte, E., Paris, G., Cocco, G., Y., Evangelista, M., Feroci, A., Ferrari, M., Fiorini, T., Froysland, M., Frutti, 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, G., Piano, P., Picozza, M., Pilia, G., Porrovecchio, M., Prest, M., Rapisarda, A., Rappoldi, A., Rubini, S., Sabatini, P., Soffitta, E., Striani, M., Trifoglio, A., Troi, E., Vallazza, A., Zambra, D., Zanello, I., Agudo, H. D., Aller, M. F., Aller, A. A., Arkharov, U., Bach, E., Benitez, A., Berdyugin, D. A., Blinov, C. S., Buemi, W. P., Chen, Paola, A., M., Dolci, E., Forne, L., Fuhrmann, J. L., Gomez, M. A., Gurwell, B., Jordan, S. G., Jorstad, J., Heidt, D., Hiriart, T., Hovatta, H. Y., Hsiao, G., Kimeridze, T. S., Konstantinova, E. N., Kopatskaya, E., Koptelova, O. M., Kurtanidze, S. O., Kurtanidze, V. M., Larionov, A., L\ahteenm\aki, P., Leto, E., Lindfor, A. P., Marscher, B., Mcbreen, I. M., Mchardy, D. A., Morozova, K., Nilsson, M., Pasanen, M., Roca Sogorb, A., Sillanp\a\a, L. O., Takalo, M., Tornikoski, C., Trigilio, I. S., Troitsky, G., Umana, L. A., Antonelli, S., Colafrancesco, C., Pittori, P., Santolamazza, F., Verrecchia, P., Giommi, L., Salotti, Anne Lähteenmäki Group, Aalto-yliopisto, and Aalto University

Subjects
Photon, Astrophysics::High Energy Astrophysical Phenomena, education, galaxies: active, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, law.invention, law, quasars: general, 0103 physical sciences, individual: PKS 1510-089 [quasars], Electronic band structure, Blazar, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, general [quasars], 010308 nuclear & particles physics, Gamma ray, Astronomy and Astrophysics, gamma rays: general, quasars: individual: PKS 1510-089, radiation mechanisms: non-thermal, non-thermal [radiation mechanisms], Synchrotron, Space and Planetary Science, active [galaxies], Peak level, Astrophysics - High Energy Astrophysical Phenomena, general [gamma rays], Flare
Abstract

We report on the extreme gamma-ray activity from the FSRQ PKS 1510-089 observed by AGILE in March 2009. In the same period a radio-to-optical monitoring of the source was provided by the GASP-WEBT and REM. Moreover, several Swift ToO observations were triggered, adding important information on the source behaviour from optical/UV to hard X-rays. We paid particular attention to the calibration of the Swift/UVOT data to make it suitable to the blazars spectra. Simultaneous observations from radio to gamma rays allowed us to study in detail the correlation among the emission variability at different frequencies and to investigate the mechanisms at work. In the period 9-30 March 2009, AGILE detected an average gamma-ray flux of (311+/-21)x10^-8 ph cm^-2 s^-1 for E>100 MeV, and a peak level of (702+/-131)x10^-8 ph cm^-2 s^-1 on daily integration. The gamma-ray activity occurred during a period of increasing activity from near-IR to UV, with a flaring episode detected on 26-27 March 2009, suggesting that a single mechanism is responsible for the flux enhancement observed from near-IR to UV. By contrast, Swift/XRT observations seem to show no clear correlation of the X-ray fluxes with the optical and gamma-ray ones. However, the X-ray observations show a harder photon index (1.3-1.6) with respect to most FSRQs and a hint of harder-when-brighter behaviour, indicating the possible presence of a second emission component at soft X-ray energies. Moreover, the broad band spectrum from radio-to-UV confirmed the evidence of thermal features in the optical/UV spectrum of PKS 1510-089 also during high gamma-ray state. On the other hand, during 25-26 March 2009 a flat spectrum in the optical/UV energy band was observed, suggesting an important contribution of the synchrotron emission in this part of the spectrum during the brightest gamma-ray flare, therefore a significant shift of the synchrotron peak., 13 pages, 7 figures, 3 tables. Accepted for publication in Astronomy and Astrophysics

Published
2011

140. Study of the γ-ray source 1AGL J2022+4032 in the Cygnus region

Author

F. Longo, Elsa Beatriz Giacani, G. Piano, Arnaud Ferrari, A. Zambra, F. D'Ammando, C. Pittori, M. Feroci, M. Fiorini, P. Picozza, M. Rapisarda, G. De Paris, Gloria Mabel Dubner, A. Pellizzoni, E. Costa, E. Del Monte, G. Pucella, V. Vittorini, F. Perotti, A. Trois, M. Trifoglio, A. Morselli, M. Tavani, E. Vallazza, F. Gianotti, P. A. Caraveo, A. Argan, M. Pilia, A. Giuliani, Francesco Lucarelli, P. Soffitta, Andrea Bulgarelli, F. Lazzarotto, F. Fuschino, S. Vercellone, P. Lipari, P. Santolamazza, A. Rappoldi, E. Scalise, E. Striani, M. Giusti, L. Pacciani, P. W. Cattaneo, A. W. Chen, L. A. Antonelli, M. Galli, F. Verrecchia, M. Prest, S. Sabatini, P. Giommi, E. Moretti, Claudio Labanti, L. Salotti, D. Zanello, G. Di Cocco, Sandro Mereghetti, I. Donnarumma, Y. Evangelista, S. Colafrancesco, Martino Marisaldi, G. Barbiellini, A. W., Chen, G., Piano, M., Tavani, A., Troi, G., Dubner, E., Giacani, A., Argan, G., Barbiellini, A., Bulgarelli, P., Caraveo, P. W., Cattaneo, E., Costa, F., D'Ammando, Paris, G., Monte, E., Cocco, G., I., Donnarumma, Y., Evangelista, M., Feroci, A., Ferrari, M., Fiorini, F., Fuschino, M., Galli, F., Gianotti, A., Giuliani, M., Giusti, C., Labanti, F., Lazzarotto, P., Lipari, Longo, Francesco, M., Marisaldi, S., Mereghetti, E., Moretti, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, P., Picozza, M., Pilia, M., Prest, G., Pucella, M., Rapisarda, A., Rappoldi, S., Sabatini, E., Scalise, P., Soffitta, E., Striani, M., Trifoglio, E., Vallazza, S., Vercellone, V., Vittorini, A., Zambra, D., Zanello, C., Pittori, P., Giommi, F., Verrecchia, F., Lucarelli, P., Santolamazza, S., Colafrancesco, L. A., Antonelli, L., Salotti, Chen AW, Piano G, Tavani M, Trois A, Dubner G, Giacani E, Argan A, Barbiellini G, Bulgarelli A, Caraveo P, Cattaneo PW, Costa E, DAmmando F, De Paris G, Del Monte E, Di Cocco G, Donnarumma I, Evangelista Y, Feroci M, Ferrari A, Fiorini M, Fuschino F, Galli M, Gianotti F, Giuliani A, Giusti M, Labanti C, Lazzarotto F, Lipari P, Longo F, Marisaldi M, Mereghetti S, Moretti E, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Picozza P, Pilia M, Prest M, Pucella G, Rapisarda M, Rappoldi A, Sabatini S, Scalise E, Soffitta P, Striani E, Trifoglio M, Vallazza E, Vercellone S, Vittorini V, Zambra A, Zanello D, Pittori C, Giommi P, Verrecchia F, Lucarelli F, Santolamazza P, Colafrancesco S, Antonelli LA, and Salotti L

Subjects
pulsars: individual: 1FGL J2021.5+4026, Astrophysics::High Energy Astrophysical Phenomena, Ciencias Físicas, pulsars: individual: 1AGL J2022+4032, gamma rays: stars, pulsars: individual: LAT PSR J2021+4026, pulsars: individual: 3EG J2020+4017, individual: LAT PSR J2021+4026 [pulsars], Flux, FOS: Physical sciences, Astrophysics, star [gamma rays], law.invention, Telescope, purl.org/becyt/ford/1 [https], Pulsar, law, Blazar, Supernova remnant, individual: 1FGL J2021.5+4026 [pulsars], Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Gamma ray, Astronomy and Astrophysics, individual: 3EG J2020+4017 [pulsars], purl.org/becyt/ford/1.3 [https], Light curve, stars [gamma rays], Astronomía, gamma ray, Space and Planetary Science, AGILE satellite, galactic source, supernova remnant Gamma Cygni, individual: 1AGL J2022+4032 [pulsars], pulsars: individual: 1AGL J2022+4032 / gamma rays: stars / pulsars: individual: 1FGL J2021.5+4026 / pulsars: individual: LAT PSR J2021+4026 / pulsars: individual: 3EG J2020+4017, Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS, Fermi Gamma-ray Space Telescope
Abstract

Identification of gamma-ray-emitting Galactic sources is a long-standing problem in astrophysics. One such source, 1AGL J2022+4032, coincident with the interior of the radio shell of the supernova remnant Gamma Cygni (SNR G78.2+2.1) in the Cygnus Region, has recently been identified by Fermi as a gamma-ray pulsar, LAT PSR J2021+4026. We present long-term observations of 1AGL J2022+4032 with the AGILE gamma-ray telescope, measuring its flux and light curve. We compare the light curve of 1AGL J2022+4032 with that of 1AGL J2021+3652 (PSR J2021+3651), showing that the flux variability of 1AGL J2022+4032 appears to be greater than the level predicted from statistical and systematic effects and producing detailed simulations to estimate the probability of the apparent observed variability. We evaluate the possibility that the gamma-ray emission may be due to the superposition of two or more point sources, some of which may be variable, considering a number of possible counterparts. We consider the possibility of a nearby X-ray quiet microquasar contributing to the flux of 1AGL J2022+4032 to be more likely than the hypotheses of a background blazar or intrinsic gamma-ray variabilty of LAT PSR J2021+4026., 7 pages, 7 figures, accepted for publication in Astronomy & Astrophysics

Published
2010

141. Concept for an innovative wide-field camera for x-ray astronomy

Author

G. Zampa, L. Pacciani, Martino Marisaldi, Lorenzo Amati, Alexander Rashevsky, Miriam Grassi, Paolo Soffitta, G. L. Israel, Fabio Muleri, I. Donnarumma, Mauro Orlandini, L. A. Antonelli, Fabrizio Nicastro, F. Fuschino, A. Vacchi, Y. Evangelista, Enrico Costa, E. Morelli, Francesco Lazzarotto, Piero Malcovati, F. Perotti, M. Rapisarda, M. Feroci, E. Del Monte, M. Mastropietro, Filippo Frontera, Fabrizio Fiore, N. Zampa, Riccardo Campana, L. Picolli, Giuseppe Baldazzi, A. Rubini, V. Bonvicini, Claudio Labanti, R. Campana, M. Feroci, A. Vacchi, C. Labanti, G. Zampa, E. Del Monte, Y. Evangelista, F. Muleri, L. Pacciani, A. Rubini, P. Soffitta, E. Costa, I. Donnarumma, F. Lazzarotto, M. Mastropietro, E. Morelli, M. Rapisarda, F. Fuschino, M. Marisaldi, V. Bonvicini, A. Rashevsky, N. Zampa, F. Perotti, L. Amati, F. Frontera, L. A. Antonelli, F. Fiore, G. L. Israel, F. Nicastro, M. Orlandini, G. Baldazzi, L. Picolli, M. Grassi, and and P. Malcovati

Subjects
Detectors - X-rays, Silicon, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Instrumentation, chemistry.chemical_element, General, Electronic, Optical and Magnetic Materials, Condensed Matter Physics, Computer Science Applications1707 Computer Vision and Pattern Recognition, Applied Mathematics, Electrical and Electronic Engineering, X-ray astronomy, Optics, Electronic, Angular resolution, Optical and Magnetic Materials, Image resolution, Physics, business.industry, large-area, Detector, fine-pitch Silicon detector, Power (physics), chemistry, business, Energy (signal processing)
Abstract

The use of large-area, “ne-pitch Silicon detectors has demonstrated the feasibility of wide “eld imaging experi-ments requesting very low resources in terms of weight, volume, power and costs. The ”ying SuperAGILE instru-ment is the “rst such experiment, adopting large-area Silicon microstrip detectors coupled to one-dimensionalcoded masks. With less than 10 kg, 12 watt and 0.04 m 3 it provides 6-arcmin angular resolution over > 1 sr “eldof view. Due to odd operational conditions, SuperAGILE works in the unfavourable energy range 18 60 keV. Inthis paper we show that the use of innovative large-area Silicon Drift Detectors allows to design experiments witharcmin-imaging performance over steradian-wide “elds of view, in the energy range 2 50 keV, with spectroscopicresolution in the range of 300 570 eV (FWHM) at room temperature. We will show the concept, design andreadiness of such an experiment, supported by laboratory tests on large-area prototypes. We will quantify theexpected performance in potential applications on X-ray astronomy missions for the observation and long-termmonitoring of Galactic and extragalactic transient and persistent sources, as well as localization and “ne studyof the prompt emission of Gamma-Ray Bursts in soft X-rays.Keywords: Instrumentation:detectors „ X-rays:general

Published
2010

142. Detection of terrestrial gamma ray flashes up to 40 MeV by the AGILE satellite

Author

Martino Marisaldi, A. Zambra, E. Striani, I. Donnarumma, M. Trifoglio, C. Pittori, Claudio Labanti, I. Lapshov, T. Froysland, M. Fiorini, D. Zanello, Marco Tavani, F. Fuschino, A. Argan, P. A. Caraveo, M. Pilia, M. Galli, Marco Feroci, Luigi Pacciani, Andrea Bulgarelli, M. Prest, L. Salotti, F. Verrecchia, F. Boffelli, G. Di Persio, Sandro Mereghetti, F. Perotti, E. Del Monte, Enrico Costa, G. Pucella, Elena Moretti, Paolo Soffitta, L. A. Antonelli, Francesco Lazzarotto, Arnaud Ferrari, A. Rappoldi, E. Vallazza, Dario Gasparrini, G. Di Cocco, S. Cutini, G. De Paris, S. Sabatini, S. Colafrancesco, A. Morselli, S. Vercellone, V. Cocco, P. Santolamazza, A. W. Chen, Paolo Lipari, Alda Rubini, P. Picozza, P. Giommi, P. W. Cattaneo, G. Piano, Massimo Rapisarda, Guido Barbiellini, V. Vittorini, Y. Evangelista, A. Pellizzoni, A. Giuliani, B. Preger, Filippo D'Ammando, Francesco Longo, Alessio Trois, and Fulvio Gianotti

Subjects
Physics, Atmospheric Science, Ecology, Detector, Bremsstrahlung, Gamma ray, Paleontology, Soil Science, Astronomy, Forestry, Aquatic Science, Oceanography, Geographic distribution, Geophysics, Relativistic runaway electron avalanche, Space and Planetary Science, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Gamma ray detectors, Satellite, Earth-Surface Processes, Water Science and Technology, Remote sensing, Terrestrial gamma-ray flash
Abstract

We report the detection by the Astrorivelatore Gamma a Immagini Leggero (AGILE) satellite of terrestrial gamma ray flashes (TGFs) obtained with the minicalorimeter (MCAL) detector operating in the ...

Published
2010

143. Direct Evidence for Hadronic Cosmic-Ray Acceleration in the Supernova Renmant IC 443

Author

C. Pittori, Marco Feroci, F. Fuschino, Luigi Pacciani, Paolo Soffitta, G. De Paris, A. Giuliani, E. Scalise, Filippo D'Ammando, V. Cocco, M. Mastropietro, E. Del Monte, V. Vittorini, Arnaud Ferrari, Paolo Lipari, M. Trifoglio, Y. Evangelista, S. Vercellone, F. Perotti, Francesco Lazzarotto, P. Santolamazza, A. Zambra, A. Pellizzoni, G. Di Cocco, E. Striani, I. Lapshov, Fulvio Gianotti, I. Donnarumma, Martino Marisaldi, L. Salotti, Elena Moretti, Alda Rubini, P. W. Cattaneo, A. Rappoldi, A. W. Chen, P. Picozza, P. Giommi, Massimo Rapisarda, G. Pucella, F. Longo, D. Zanello, A. Argan, Andrea Bulgarelli, T. Contessi, Enrico Costa, Claudio Labanti, L. A. Antonelli, G. Piano, P. A. Caraveo, M. Galli, F. Verrecchia, Sandro Mereghetti, A. Morselli, S. Colafrancesco, M. Prest, Alessio Trois, M. Pilia, Marco Tavani, S. Sabatini, Ennio Morelli, G. Barbiellini, E. Vallazza, M., Tavani, A., Giuliani, A. W., Chen, A., Argan, G., Barbiellini, A., Bulgarelli, P., Caraveo, P. W., Cattaneo, V., Cocco, T., Contessi, F., D'Ammando, E., Costa, G. D., Pari, E. D., Monte, G. D., Cocco, I., Donnarumma, Y., Evangelista, A., Ferrari, M., Feroci, F., Fuschino, M., Galli, F., Gianotti, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, Longo, Francesco, M., Marisaldi, M., Mastropietro, S., Mereghetti, E., Morelli, E., Moretti, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, G., Piano, P., Picozza, M., Pilia, G., Pucella, M., Prest, M., Rapisarda, A., Rappoldi, E., Scalise, A., Rubini, S., Sabatini, E., Striani, P., Soffitta, M., Trifoglio, A., Troi, E., Vallazza, S., Vercellone, V., Vittorini, A., Zambra, D., Zanello, C., Pittori, F., Verrecchia, P., Santolamazza, P., Giommi, S., Colafrancesco, L. A., Antonelli, L., Salotti, Tavani M, Giuliani A, Chen AW, Argan A, Barbiellini G, Bulgarelli A, Caraveo P, Cattaneo PW, Cocco V, Contessi T, DAmmando F, Costa E, De Paris G, Del Monte E, Di Cocco G, Donnarumma I, Evangelista Y, Ferrari A, Feroci M, Fuschino F, Galli M, Gianotti F, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Longo F, Marisaldi M, Mastropietro M, Mereghetti S, Morelli E, Moretti E, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Piano G, Picozza P, Pilia M, Pucella G, Prest M, Rapisarda M, Rappoldi A, Scalise E, Rubini A, Sabatini S, Striani E, Soffitta P, Trifoglio M, Trois A, Vallazza E, Vercellone S, Vittorini V, Zambra A, Zanello D, Pittori C, Verrecchia F, Santolamazza P, Giommi P, Colafrancesco S, Antonelli LA, and Salotti L

Subjects
Agile, Photon, Supernova Remnants, Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Cosmic ray, Electron, Astrophysics, High Energy Gamma-ray Astronomy, gamma ray production, supernova, Supernova remnant, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Molecular cloud, AGILE satellite, Gamma ray, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Supernova, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, cosmic rays – gamma rays: general – ISM: supernova remnants – supernovae: general – supernovae: individual (IC 443)
Abstract

The Supernova Remnant (SNR) IC 443 is an intermediate-age remnant well known for its radio, optical, X-ray and gamma-ray energy emissions. In this Letter we study the gamma-ray emission above 100 MeV from IC 443 as obtained by the AGILE satellite. A distinct pattern of diffuse emission in the energy range 100 MeV-3 GeV is detected across the SNR with its prominent maximum (source "A") localized in the Northeastern shell with a flux F = (47 \pm 10) 10^{-8} photons cm^{-2} s^{-1} above 100 MeV. This location is the site of the strongest shock interaction between the SNR blast wave and the dense circumstellar medium. Source "A" is not coincident with the TeV source located 0.4 degree away and associated with a dense molecular cloud complex in the SNR central region. From our observations, and from the lack of detectable diffuse TeV emission from its Northeastern rim, we demonstrate that electrons cannot be the main emitters of gamma-rays in the range 0.1-10 GeV at the site of the strongest SNR shock. The intensity, spectral characteristics, and location of the most prominent gamma-ray emission together with the absence of co-spatial detectable TeV emission are consistent only with a hadronic model of cosmic-ray acceleration in the SNR. A high-density molecular cloud (cloud "E") provides a remarkable "target" for nucleonic interactions of accelerated hadrons: our results show enhanced gamma-ray production near the molecular cloud/shocked shell interaction site. IC 443 provides the first unambiguous evidence of cosmic-ray acceleration by SNRs., Comment: 5 pages, 2 figures; accepted by ApJLetters on Jan 21, 2010

Published
2010
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144. A year-long AGILE observation of Cygnus X-1 in hard spectral state

Author

A. W. Chen, Francesco Lazzarotto, A. Morselli, Marco Feroci, Luigi Pacciani, E. Striani, S. Vercellone, M. Prest, C. Pittori, I. Lapshov, I. Donnarumma, E. Del Monte, Sandro Mereghetti, A. Argan, M. Galli, P. W. Cattaneo, Piergiorgio Picozza, Massimo Rapisarda, F. Fuschino, Andrea Bulgarelli, F. Perotti, A. Pellizzoni, G. Di Cocco, F. Verrecchia, Enrico Costa, Elena Moretti, Filippo D'Ammando, G. Piano, A. Rappoldi, E. Vallazza, S. Cutini, A. Giuliani, P. A. Caraveo, L. Salotti, Paolo Soffitta, Claudio Labanti, A. Zambra, Francesco Longo, L. A. Antonelli, Guido Barbiellini, Martino Marisaldi, Paolo Lipari, P. Santolamazza, Paolo Giommi, Marco Tavani, S. Sabatini, V. Vittorini, M. Trifoglio, Maura Pilia, Alessio Trois, Fulvio Gianotti, B. Preger, F. Boffelli, Y. Evangelista, G. Pucella, Del Monte E, Feroci M, Evangelista Y, Costa E, Donnarumma I, Lapshov I, Lazzarotto F, Pacciani L, Rapisarda M, Soffitta P, Argan A, Barbiellini G, Boffelli F, Bulgarelli A, Caraveo P, Cattaneo PW, Chen A, DAmmando F, Di Cocco G, Fuschino F, Galli M, Gianotti F, Giuliani A, Labanti C, Lipari P, Longo F, Marisaldi M, Mereghetti S, Moretti E, Morselli A, Pellizzoni A, Perotti F, Piano G, Picozza P, Pilia M, Prest M, Pucella G, Rappoldi A, Sabatini S, Striani E, Tavani M, Trifoglio M, Trois A, Vallazza E, Vercellone S, Vittorini V, Zambra A, Antonelli LA, Cutini S, Pittori C, Preger B, Santolamazza P, Verrecchia F, Giommi P, Salotti L, E. D., Monte, M., Feroci, Y., Evangelista, E., Costa, I., Donnarumma, I., Lapshov, F., Lazzarotto, L., Pacciani, M., Rapisarda, P., Soffitta, A., Argan, G., Barbiellini, F., Boffelli, A., Bulgarelli, P., Caraveo, P. W., Cattaneo, A., Chen, F., D'Ammando, G. D., Cocco, F., Fuschino, M., Galli, F., Gianotti, A., Giuliani, C., Labanti, P., Lipari, Longo, Francesco, M., Marisaldi, S., Mereghetti, E., Moretti, A., Morselli, A., Pellizzoni, F., Perotti, G., Piano, P., Picozza, M., Pilia, M., Prest, G., Pucella, A., Rappoldi, S., Sabatini, E., Striani, M., Tavani, M., Trifoglio, A., Troi, E., Vallazza, S., Vercellone, V., Vittorini, A., Zambra, L. A., Antonelli, S., Cutini, C., Pittori, B., Preger, P., Santolamazza, F., Verrecchia, P., Giommi, and L., Salotti

Subjects
Agile, Black Holes, Astrophysics::High Energy Astrophysical Phenomena, Hadron, Phase (waves), Flux, FOS: Physical sciences, Astrophysics, cignus, High Energy Gamma-ray Astronomy, X-ray, binaries, silicon detector, Range (statistics), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Autocorrelation, Gamma ray, Static timing analysis, Astronomy and Astrophysics, stars: individual: Cyg X-1, gamma rays: observations, X-rays: binaries, X-rays: general, Space and Planetary Science, AGILE satellite, Astrophysics - High Energy Astrophysical Phenomena, Energy (signal processing)
Abstract

We present the observation of Cyg X-1 in hard spectral state performed during the AGILE Science Verification Phase and Observing Cycle 1 in hard X-rays (with SuperAGILE) and gamma rays (with the GRID) and lasting for about 160 days with a live time of $\sim 6$ Ms. We investigate the variability of Cyg X-1 in hard X-rays at different timescales, from $\sim 300$ s up to one day, and we apply different tools of timing analysis, such as the autocorrelation function, the first order structure function and the Lomb-Scargle periodogram, to our data (from SuperAGILE) and to the simultaneous data in soft X-rays (from RXTE/ASM). We conclude our investigation with a search for emission in the energy range above 100 MeV with the maximum likelihood technique. In the hard X-ray band the flux of Cyg X-1 shows its typical erratic fluctuations at all timescales with variations of about a factor of two that do not affect significantly the shape of the energy spectrum. From the first order structure function we find that the X-ray emission of Cyg X-1 is characterized by \textit{antipersistence}, indication of a negative feedback mechanism at work. In the gamma ray data a statistically significant point-like source at the position of Cyg X-1 is not found and the upper limit on the flux is $\mathrm{5 \times 10^{-8} \; ph \; cm^{-2} \; s^{-1}}$, over the whole observation (160 days). Finally we compare our upper limit in gamma rays with the expectation of various models of the Cyg X-1 emission, of both hadronic and leptonic origin, in the GeV -- TeV band. The time history of Cyg X-1 in the hard X-ray band over 13 months (not continuous) is shown. Different tools of analysis do not provide fully converging results of the characteristic timescales in the system, suggesting that the timescales found in the structure function are not intrinsic to the physics of the source., Comment: 15 pages and 11 figures (with subfigures). Accepted for publication by A&A.

Published
2010

145. AGILE OBSERVATIONS OF THE 'SOFT' GAMMA-RAY PULSAR PSR B1509-58

Author

A. Argan, Andrea Bulgarelli, Enrico Costa, G. De Paris, F. Perotti, Patrick Weltevrede, Simon Johnston, A. Giuliani, A. Morselli, I. Donnarumma, A. Rappoldi, E. Vallazza, G. Pucella, V. Cocco, Claudio Labanti, A. W. Chen, C. Pittori, T. Froysland, E. Del Monte, A. Pellizzoni, Francesco Lazzarotto, Massimiliano Fiorini, N. D'Amico, S. Sabatini, Y. Evangelista, Francesco Longo, Andrea Possenti, G. Di Cocco, Paolo Lipari, F. Lucarelli, Giovanni F. Bignami, Marco Feroci, L. Salotti, F. Fuschino, Luigi Pacciani, D. Zanello, A. Zambra, S. Vercellone, M. Burgay, V. Vittorini, Filippo D'Ammando, Paolo Soffitta, M. Trifoglio, Massimo Rapisarda, Guido Barbiellini, P. Santolamazza, Maura Pilia, Alessio Trois, Paolo Giommi, I. Lapshov, Paolo Esposito, Fulvio Gianotti, M. Prest, A. De Luca, P. A. Caraveo, M. Galli, Piergiorgio Picozza, F. Verrecchia, G. Piano, Marco Tavani, Martino Marisaldi, Sandro Mereghetti, P. W. Cattaneo, Pilia M, Pellizzoni A, Trois A, Verrecchia F, Esposito P, Weltevrede P, Johnston S, Burgay M, Possenti A, Del Monte E, Fuschino F, Santolamazza P, Chen A, Giuliani A, Caraveo P, Mereghetti S, Tavani M, Argan A, Costa E, D'Amico N, De Luca A, Evangelista Y, Feroci M, Longo F, Marisaldi M, Barbiellini G, Bulgarelli A, Cattaneo PW, Cocco V, DAmmando F, De Paris G, Di Cocco G, Donnarumma I, Fiorini M, Froysland T, Galli M, Gianotti F, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Morselli A, Pacciani L, Perotti F, Piano G, Picozza P, Prest M, Pucella G, Rapisarda M, Rappoldi A, Sabatini S, Soffitta P, Trifoglio M, Vallazza E, Vercellone S, Vittorini V, Zambra A, Zanello D, Pittori C, Lucarelli F, Giommi P, Salotti L, Bignami GF, M., Pilia, A., Pellizzoni, A., Troi, F., Verrecchia, P., Esposito, P., Weltevrede, S., Johnston, M., Burgay, A., Possenti, E. D., Monte, F., Fuschino, P., Santolamazza, A., Chen, A., Giuliani, P., Caraveo, S., Mereghetti, M., Tavani, A., Argan, E., Costa, N., D'Amico, A. D., Luca, Y., Evangelista, M., Feroci, Longo, Francesco, M., Marisaldi, G., Barbiellini, 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, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, A., Morselli, L., Pacciani, F., Perotti, G., Piano, P., Picozza, M., Prest, G., Pucella, M., Rapisarda, A., Rappoldi, S., Sabatini, P., Soffitta, M., Trifoglio, E., Vallazza, S., Vercellone, V., Vittorini, A., Zambra, D., Zanello, C., Pittori, F., Lucarelli, P., Giommi, L., Salotti, and G. F., Bignami

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Agile, pulsar, gamma ray, High Energy Gamma-ray Astronomy, AGILE satellite, Pulsar, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, FOS: Physical sciences, gamma rays: stars – pulsars: general – pulsars: individual (PSR J1513–5908 (B1509–58)) – stars: neutron, Astronomy and Astrophysics, Astrophysics, Light curve, Electromagnetic radiation, Spectral line, Neutron star, Pair production, Space and Planetary Science, Spectral energy distribution, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present the results of new Agile observations of PSR B1509-58 performed over a period of 2.5 years following the detection obtained with a subset of the present data. The modulation significance of the lightcurve above 30 MeV is at a 5$\sigma$ confidence level and the lightcurve is similar to those found earlier by Comptel up to 30 MeV: a broad asymmetric first peak reaching its maximum 0.39 +/- 0.02 cycles after the radio peak plus a second peak at 0.94 +/- 0.03. The gamma-ray spectral energy distribution of the pulsed flux detected by Comptel and Agile is well described by a power-law (photon index alpha=1.87+/-0.09) with a remarkable cutoff at E_c=81 +/- 20 MeV, representing the softest spectrum observed among gamma-ray pulsars so far. The pulsar luminosity at E > 1 MeV is $L_{\gamma}=4.2^{+0.5}_{-0.2} \times10^{35}$ erg/s, assuming a distance of 5.2 kpc, which implies a spin-down conversion efficiency to gamma-rays of $\sim 0.03$. The unusual soft break in the spectrum of PSR B1509-58 has been interpreted in the framework of polar cap models as a signature of the exotic photon splitting process in the strong magnetic field of this pulsar. In this interpretation our spectrum constrains the magnetic altitude of the emission point(s) at 3 km above the neutron star surface, implying that the attenuation may not be as strong as formerly suggested because pair production can substitute photon splitting in regions of the magnetosphere where the magnetic field becomes too low to sustain photon splitting. In the case of an outer-gap scenario, or the two pole caustic model, better constraints on the geometry of the emission would be needed from the radio band in order to establish whether the conditions required by the models to reproduce Agile lightcurves and spectra match the polarization measurements., Comment: 17 pages, 2 figures, accepted for publication in ApJ

Published
2010

146. TEMPORAL PROPERTIES OF GX 301-2 OVER A YEAR-LONG OBSERVATION WITH SuperAGILE

Author

A. Pellizzoni, F. Fuschino, L. A. Antonelli, A. W. Chen, S. Cutini, Paolo Soffitta, G. Pucella, Marco Feroci, Luigi Pacciani, F. Perotti, P. Santolamazza, M. Prest, E. Striani, M. Galli, A. Argan, Piergiorgio Picozza, Paolo Lipari, Francesco Lazzarotto, I. Lapshov, Andrea Bulgarelli, F. Verrecchia, Filippo D'Ammando, Enrico Costa, Marco Tavani, G. Di Cocco, G. Piano, S. Sabatini, Massimo Rapisarda, Paolo Giommi, A. Morselli, Francesco Longo, Sandro Mereghetti, F. Boffelli, P. W. Cattaneo, Y. Evangelista, A. Giuliani, Guido Barbiellini, E. Del Monte, Martino Marisaldi, S. Vercellone, L. Salotti, A. Zambra, I. Donnarumma, P. A. Caraveo, Claudio Labanti, Elena Moretti, A. Rappoldi, E. Vallazza, Fulvio Gianotti, V. Vittorini, M. Trifoglio, Maura Pilia, Alessio Trois, B. Preger, C. Pittori, Y., Evangelista, M., Feroci, E., Costa, E. D., Monte, I., Donnarumma, I., Lapshov, F., Lazzarotto, L., Pacciani, M., Rapisarda, P., Soffitta, A., Argan, G., Barbiellini, F., Boffelli, A., Bulgarelli, P., Caraveo, P. W., Cattaneo, A., Chen, F., D'Ammando, G. D., Cocco, F., Fuschino, M., Galli, F., Gianotti, A., Giuliani, C., Labanti, P., Lipari, Longo, Francesco, M., Marisaldi, S., Mereghetti, E., Moretti, A., Morselli, A., Pellizzoni, F., Perotti, G., Piano, P., Picozza, M., Pilia, M., Prest, G., Pucella, A., Rappoldi, S., Sabatini, E., Striani, M., Tavani, M., Trifoglio, A., Troi, E., Vallazza, S., Vercellone, V., Vittorini, A., Zambra, L. A., Antonelli, S., Cutini, C., Pittori, B., Preger, P., Santolamazza, F., Verrecchia, P., Giommi, L., Salotti, Evangelista Y, Feroci M, Costa E, Del Monte E, Donnarumma I, Lapshov I, Lazzarotto F, Pacciani L, Rapisarda M, Soffitta P, Argan A, Barbiellini G, Boffelli F, Bulgarelli A, Caraveo P, Cattaneo PW, Chen A, DAmmando F, Di Cocco G, Fuschino F, Galli M, Gianotti F, Giuliani A, Labanti C, Lipari P, Longo F, Marisaldi M, Mereghetti S, Moretti E, Morselli A, Pellizzoni A, Perotti F, Piano G, Picozza P, Pilia M, Prest M, Pucella G, Rappoldi A, Sabatini S, Striani E, Tavani M, Trifoglio M, Trois A, Vallazza E, Vercellone S, Vittorini V, Zambra A, Antonelli LA, Cutini S, Pittori C, Preger B, Santolamazza P, Verrecchia F, Giommi P, and Salotti L

Subjects
Agile, SuperAGILE, Astrophysics::High Energy Astrophysical Phenomena, Phase (waves), Flux, FOS: Physical sciences, X-ray binary GX 301-2, pulsar, Astrophysics, High Mass X-ray Binaries, High Energy Gamma-ray Astronomy, law.invention, stars: neutron, X-rays: binaries, Pulsar, law, pulsars: individual (GX 3012), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Accretion (meteorology), Astronomy and Astrophysics, AGILE satellite, Light curve, Orbital period, Secular variation, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Flare
Abstract

We present the long-term monitoring of the High Mass X-ray Binary GX 301-2 performed with the SuperAGILE instrument on-board the AGILE mission. The source was monitored in the 20-60 keV energy band during the first year of the mission from 2007 July 17 to 2008 August 31, covering about one whole orbital period and three more pre-periastron passages for a total net observation time of about 3.7 Ms. The SuperAGILE dataset represents one of the most continuous and complete monitoring at hard X-ray energies of the 41.5 day long binary period available to date. The source behavior was characterized at all orbital phases in terms of hard X-ray flux, spectral hardness, spin period history, pulsed fraction and pulse shape profile. We also complemented the SuperAGILE observations with the soft X-ray data of the RossiXTE/ASM. Our analysis shows a clear orbital modulation of the spectral hardness, with peaks in correspondence with the pre-periastron flare and near phase 0.25. The hardness peaks we found could be related with the wind-plus-stream accretion model proposed in order to explain the orbital light curve modulation of GX 301-2. Timing analysis of the pulsar spin period shows that the secular trend of the about 680 s pulse period is consistent with the previous observations, although there is evidence of a slight decrease in the spin-down rate. The analysis of the hard X-ray pulsed emission also showed a variable pulse shape profile as a function of the orbital phase, with substructures detected near the passage at the periastron, and a clear modulation of the pulsed fraction, which appears in turn strongly anti-correlated with the source intensity., 10 pages, 7 figures, 3 tables, accepted for publication in ApJ

Published
2010

147. AGILE detection of intense gamma-ray activity from the blazar PKS 0537-441 in October 2008

Author

Marco Feroci, Luigi Pacciani, F. Boffelli, G. De Paris, E. Vallazza, Martino Marisaldi, Claudio Labanti, C. Pittori, T. Froysland, Domenico Impiombato, Ennio Morelli, A. Zambra, A. Morselli, F. Longo, A. Treves, Fulvio Gianotti, A. W. Chen, P. Caraveo, M. Fiorini, L. Salotti, G. Di Cocco, Francesco Lazzarotto, F. Perotti, E. Del Monte, G. Pucella, M. Perri, Filippo D'Ammando, G. Barbiellini, V. Vittorini, M. Prest, P. Santolamazza, M. Galli, G. Piano, F. Verrecchia, Marco Tavani, P. Giommi, P. W. Cattaneo, A. Argan, I. Donnarumma, Y. Evangelista, Andrea Bulgarelli, A. Pellizzoni, Sandro Mereghetti, Enrico Costa, Maura Pilia, Elena Pian, E. Striani, Alessio Trois, P. Picozza, I. Lapshov, S. Colafrancesco, M. Trifoglio, S. Sabatini, A. Giuliani, D. Zanello, Hans A. Krimm, Massimo Rapisarda, L. A. Antonelli, V. Cocco, A. Rappoldi, Paolo Lipari, F. Fuschino, D. Fugazza, Paolo Soffitta, P. Romano, S. Vercellone, Pucella G, DAmmando F, Romano P, Treves A, Pian E, Vercellone S, Vittorini V, Piano G, Impiombato D, Fugazza D, Verrecchia F, Krimm HA, Donnarumma I, Tavani M, Bulgarelli A, Chen AW, Giuliani A, Longo F, Pacciani L, Argan A, Barbiellini G, Boffelli F, Caraveo P, Cattaneo PW, Cocco V, Costa E, 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, Lapshov I, Lazzarotto F, Lipari P, Marisaldi M, Mereghetti S, Morelli E, Morselli A, Pellizzoni A, Perotti F, Picozza P, Pilia M, Prest M, Rapisarda M, Rappoldi A, Sabatini S, Soffitta P, Striani E, Trifoglio M, Trois A, Vallazza E, Zambra A, Zanello D, Perri M, Pittori C, Santolamazza P, Giommi P, Antonelli LA, Colafrancesco S, Salotti L, G., Pucella, F., D'Ammando, P., Romano, A., Treve, E., Pian, S., Vercellone, V., Vittorini, G., Piano, D., Impiombato, D., Fugazza, F., Verrecchia, H. A., Krimm, I., Donnarumma, M., Tavani, A., Bulgarelli, A. W., Chen, A., Giuliani, Longo, Francesco, L., Pacciani, A., Argan, G., Barbiellini, F., Boffelli, P., Caraveo, P. W., Cattaneo, V., Cocco, E., Costa, 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, I., Lapshov, F., Lazzarotto, P., Lipari, M., Marisaldi, S., Mereghetti, E., Morelli, A., Morselli, A., Pellizzoni, F., Perotti, P., Picozza, M., Pilia, M., Prest, M., Rapisarda, A., Rappoldi, S., Sabatini, P., Soffitta, E., Striani, M., Trifoglio, A., Troi, E., Vallazza, A., Zambra, D., Zanello, M., Perri, C., Pittori, P., Santolamazza, P., Giommi, L. A., Antonelli, S., Colafrancesco, and L., Salotti

Subjects
Swift Gamma-Ray Burst Mission, gamma-ray activity, Astrophysics::High Energy Astrophysical Phenomena, Flux, Context (language use), Astrophysics, High Energy Gamma-ray Astronomy, AGILE satellite, Active Galactic Nuclei, law.invention, Luminosity, Telescope, AGILE, X-ray, law, Target of opportunity, gamma rays: general – BL Lacertae objects: individual: PKS 0537-441 – radiation mechanisms: non-thermal, Blazar, Physics, Astronomy, Astronomy and Astrophysics, Gamma-Ray Imaging Detector, Space and Planetary Science, Spectral energy distribution
Abstract

Context. We report the detection by the AGILE satellite of intense gamma-ray activity from the source 1AGL J0538-4424, associated with the low-energy-peaked BL Lac PKS 0537-441, during a target of opportunity (ToO) observation performed on 2008 October 10-17, triggered by a Fermi-LAT alert, together with REM and Swift observations. Aims. The quasi-simultaneous near-infrared, optical, UV, X-ray, and gamma-ray coverage allowed us to investigate the behaviour of the source in different energy bands and study the spectral energy distribution and a theoretical model that can describe the gamma-ray state observed in mid-October. Methods. AGILE observed the source with its two co-aligned imagers: the Gamma-Ray Imaging Detector (GRID) and the hard X-ray imager (SuperAGILE), sensitive in the 30 MeV-30 GeV and 18-60 keV ranges, respectively. During the AGILE observation, the source was monitored simultaneously in the UV and X-ray bands by the Swift satellite through 6 ToO observations carried out between 2008 October 8 and 17. Moreover, the source was observed in the near-infrared and optical bands by the REM telescope on 2008 October 7, 8, and 9. Results. During 2008 October 10-17, AGILE-GRID detected gamma-ray emission from PKS 0537-441 at a significance level of 5.3-sigma with an average flux of (42 +/- 11) x 10(-8) photons cm(-2) s(-1) for energies higher than 100 MeV. A significant increase in the gamma-ray activity was detected between the first and the second halves of the observing period. REM and Swift/XRT detected the source in near-infrared/optical and X-rays during a relatively low and intermediate activity state, respectively, with no signs of evident variability in the different observations. However, Swift/UVOT detected an increase between the first and the second parts of the observing period, smaller than in the gamma-rays. Conclusions. The average gamma-ray flux of PKS 0537-441 detected by AGILE is close to the average flux observed for this source by the EGRET and Fermi-LAT instruments, with an increase of a factor 3 throughout the observation period up to a flux level slightly lower than the highest flux observed by Fermi-LAT during the first 11 months of operation. The spectral energy distribution of PKS 0537-441 in mid-October 2008 seems to require two synchrotron self-Compton components to be modelled, to account for both the near-infrared/optical bump and the X-ray data, together with the information on the gamma-ray flux level observed by AGILE. An alternative model based on the external Compton radiation, which requires an accretion disk with a relatively high luminosity, is also proposed.

Published
2010

148. Episodic Transient Gamma-Ray Emission From The Microquasar Cygnus X-1

Author

E. Moretti, V. Vittorini, Claudio Labanti, A. Giuliani, M. Trifoglio, C. Pittori, Francesco Lazzarotto, Paolo Lipari, Martino Marisaldi, Attilio Ferrari, Guido Barbiellini, P. Santolamazza, A. Pellizzoni, F. Perotti, S. Vercellone, M. Galli, Piergiorgio Picozza, E. Striani, Y. Evangelista, M. Giusti, Francesco Longo, Alda Rubini, F. Verrecchia, Ennio Morelli, Paolo Giommi, G. De Paris, Massimiliano Fiorini, Marco Tavani, F. Fuschino, G. Di Cocco, A. Rappoldi, E. Vallazza, S. Sabatini, Sergio Colafrancesco, Fulvio Gianotti, A. Argan, Sandro Mereghetti, P. W. Cattaneo, Andrea Bulgarelli, A. Morselli, I. Donnarumma, Enrico Costa, Filippo D'Ammando, Marco Feroci, Luigi Pacciani, M. Prest, Paolo Soffitta, L. A. Antonelli, A. W. Chen, E. Del Monte, Massimo Rapisarda, G. Piano, P. A. Caraveo, Maura Pilia, D. Zanello, G. Pucella, Alessio Trois, E. Scalise, L. Salotti, A. Zambra, F. de Pasquale, Sabatini S, Tavani M, Striani E, Bulgarelli A, Vittorini V, Piano G, Del Monte E, Feroci M, de Pasquale F, Trifoglio M, Gianotti F, Argan A, Barbiellini G, Caraveo P, Cattaneo PW, Chen AW, DAmmando F, Costa E, De Paris G, Di Cocco G, Donnarumma I, Evangelista Y, Ferrari A, Fiorini M, Fuschino F, Galli M, Giuliani A, Giusti M, Labanti C, Lazzarotto F, Lipari P, Longo F, Marisaldi M, Mereghetti S, Morelli E, Moretti E, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Picozza P, Pilia M, Pucella G, Prest M, Rapisarda M, Rappoldi A, Rubini A, Scalise E, Soffitta P, Trois A, Vallazza E, Vercellone S, Zambra A, Zanello D, Pittori C, Verrecchia F, Santolamazza P, Giommi P, Colafrancesco S, Antonelli LA, Salotti L, S., Sabatini, M., Tavani, E., Striani, A., Bulgarelli, V., Vittorini, G., Piano, E. D., Monte, M., Feroci, F. d., Pasquale, M., Trifoglio, F., Gianotti, A., Argan, G., Barbiellini, P., Caraveo, P. W., Cattaneo, A. W., Chen, F., D'Ammando, E., Costa, G. D., Pari, G. D., Cocco, I., Donnarumma, Y., Evangelista, A., Ferrari, M., Fiorini, F., Fuschino, M., Galli, A., Giuliani, M., Giusti, C., Labanti, F., Lazzarotto, P., Lipari, Longo, Francesco, M., Marisaldi, S., Mereghetti, E., Morelli, E., Moretti, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, P., Picozza, M., Pilia, G., Pucella, M., Prest, M., Rapisarda, A., Rappoldi, A., Rubini, E., Scalise, P., Soffitta, A., Troi, E., Vallazza, S., Vercellone, A., Zambra, D., Zanello, C., Pittori, F., Verrecchia, P., Santolamazza, P., Giommi, S., Colafrancesco, L. A., Antonelli, and L., Salotti

Subjects
Agile, Black Holes, transient gamma-ray emission, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Astrophysics, High Energy Gamma-ray Astronomy, X-rays: binaries, Cutoff, Cygnus X-1, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Range (particle radiation), Gamma ray, Astronomy and Astrophysics, gamma rays: general, stars: individual (Cygnus X-1), Galaxy, Black hole, Space and Planetary Science, AGILE satellite, Transient (oscillation), Astrophysics - High Energy Astrophysical Phenomena, Energy (signal processing)
Abstract

Cygnus X-1 is the archetypal black hole (BH) binary system in our Galaxy. We report the main results of an extensive search for transient gamma-ray emission from Cygnus X-1 carried out in the energy range 100 MeV - 3 GeV by the AGILE satellite, during the period 2007 July - 2009 October. The total exposure time is about 300 days, during which the source was in the "hard" X-ray spectral state. We divided the observing intervals in 2 or 4 week periods, and searched for transient and persistent emission. We report an episode of significant transient gamma-ray emission detected on 2009, October 16 in a position compatible with Cygnus X-1 optical position. This episode, occurred during a hard spectral state of Cygnus X-1, shows that a 1-2 day time variable emission above 100 MeV can be produced during hard spectral states, having important theoretical implications for current Comptonization models for Cygnus X-1 and other microquasars. Except for this one short timescale episode, no significant gamma-ray emission was detected by AGILE. By integrating all available data we obtain a 2$\sigma$ upper limit for the total integrated flux of $F_{\gamma,U.L.} = 3 \times 10^{-8} \rm ph cm^{-2} s^{-1}$ in the energy range 100 MeV - 3 GeV. We then clearly establish the existence of a spectral cutoff in the energy range 1-100 MeV that applies to the typical hard state outside the flaring period and that confirms the historically known spectral cutoff above 1 MeV., Comment: Accepted for publication by ApJ on the 9th of Feb 2010, 5 pages, 3 figures

Published
2010

149. AGILE detection of a rapid gamma-ray flare from the blazar PKS 1510-089 during the GASP-WEBT monitoring

Author

Dario Gasparrini, A. W. Chen, Alan P. Marscher, P. Giommi, C. Pittori, Filippo D'Ammando, T. Froysland, A. Argan, Andrea Bulgarelli, Enrico Costa, M. Sorcia, Carla Buemi, F. Fuschino, Svetlana G. Jorstad, Massimo Rapisarda, Marco Feroci, Arnaud Ferrari, Luigi Pacciani, Uwe Bach, Corrado Trigilio, F. Boffelli, G. De Paris, Jochen Heidt, L. A. Antonelli, Deborah Dultzin, F. Perotti, Raúl Mújica, C. M. Raiteri, Lars Fuhrmann, G. Umana, D. Zanello, A. Zambra, A. Morselli, Mark Gurwell, Paolo Soffitta, Margo F. Aller, Kari Nilsson, Marco Tavani, E. Vallazza, Wen Ping Chen, Tatiana S. Konstantinova, S. Sabatini, I. M. McHardy, Ekaterina Koptelova, A. Rappoldi, M. Fiorini, Ivan Agudo, Martino Marisaldi, José L. Gómez, V. Cocco, J. M. Lopez, Valeri M. Larionov, S. Vercellone, Elina Lindfors, A. Pellizzoni, E. Del Monte, H. Y. Hsiao, G. Pucella, F. Longo, I. Lapshov, L. Salotti, Ivan S. Troitsky, A. Giuliani, Sandro Mereghetti, Paolo Lipari, L. O. Takalo, Mar Roca-Sogorb, P. W. Cattaneo, Omar M. Kurtanidze, Brian W. Taylor, G. Di Rico, M. Trifoglio, David Hiriart, S. Colafrancesco, P. Picozza, G. Barbiellini, G. Piano, Hugh D. Aller, Fulvio Gianotti, Maura Pilia, Alessio Trois, A. A. Arkharov, B. Preger, G. Di Cocco, Givi N. Kimeridze, S. Cutini, Claudio Labanti, Erika Benítez, P. Santolamazza, I. Donnarumma, Y. Evangelista, A. Di Paola, M. Galli, E. N. Kopatskaya, P. A. Caraveo, Paolo Leto, F. Verrecchia, Michael Mommert, Francesco Lazzarotto, Andrei Berdyugin, M. Pasanen, D. A. Melnichuk, M. Prest, M. Villata, D. Blinov, V. Vittorini, DAmmando F, Pucella G, Raiteri CM, Villata M, Vittorini V, Vercellone S, Donnarumma I, Longo F, Tavani M, Argan A, Barbiellini G, Boffelli F, Bulgarelli A, Caraveo P, Cattaneo PW, Chen AW, Cocco V, Costa E, Del Monte E, De Paris G, Di Cocco G, Evangelista Y, Feroci M, Ferrari A, Fiorini M, Froysland T, Fuschino F, Galli M, Gianotti F, Giuliani A, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Marisaldi M, Mereghetti S, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Piano G, Picozza P, Pilia M, Prest M, Rapisarda M, Rappoldi A, Sabatini S, Soffitta P, Trifoglio M, Trois A, Vallazza E, Zambra A, Zanello D, Agudo I, Aller MF, Aller HD, Arkharov AA, Bach U, Benitez E, Berdyugin A, Blinov DA, Buemi CS, Chen WP, Di Paola A, Di Rico G, Dultzin D, Fuhrmann L, Gomez JL, Gurwell MA, Jorstad SG, Heidt J, Hiriart D, Hsiao HY, Kimeridze G, Konstantinova TS, Kopatskaya EN, Koptelova E, Kurtanidze O, Larionov VM, Leto P, Lindfors E, Lopez JM, Marscher AP, McHardy IM, Melnichuk DA, Mommert M, Mujica R, Nilsson K, Pasanen M, Roca-Sogorb M, Sorcia M, Takalo LO, Taylor B, Trigilio C, Troitsky IS, Umana G, Antonelli LA, Colafrancesco S, Cutini S, Gasparrini D, Pittori C, Preger B, Santolamazza P, Verrecchia F, Giommi P, Salotti L, F., D'Ammando, G., Pucella, C. M., Raiteri, M., Villata, V., Vittorini, S., Vercellone, I., Donnarumma, Longo, Francesco, M., Tavani, A., Argan, G., Barbiellini, F., Boffelli, A., Bulgarelli, P., Caraveo, P. W., Cattaneo, A. W., Chen, V., Cocco, E., Costa, E. D., Monte, G. D., Pari, G. D., Cocco, Y., Evangelista, M., Feroci, A., Ferrari, M., Fiorini, T., Froysland, F., Fuschino, M., Galli, F., Gianotti, A., Giuliani, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, M., Marisaldi, S., Mereghetti, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, G., Piano, P., Picozza, M., Pilia, M., Prest, M., Rapisarda, A., Rappoldi, S., Sabatini, P., Soffitta, M., Trifoglio, A., Troi, E., Vallazza, A., Zambra, D., Zanello, I., Agudo, M. F., Aller, H. D., Aller, A. A., Arkharov, U., Bach, E., Benitez, A., Berdyugin, D. A., Blinov, C. S., Buemi, W. P., Chen, A. D., Paola, G. D., Rico, D., Dultzin, L., Fuhrmann, J. L., Gomez, M. A., Gurwell, S. G., Jorstad, J., Heidt, D., Hiriart, H. Y., Hsiao, G., Kimeridze, T. S., Konstantinova, E. N., Kopatskaya, E., Koptelova, O., Kurtanidze, V. M., Larionov, P., Leto, E., Lindfor, J. M., Lopez, A. P., Marscher, I. M., Mchardy, D. A., Melnichuk, M., Mommert, R., Mujica, K., Nilsson, M., Pasanen, M., Roca Sogorb, M., Sorcia, L. O., Takalo, B., Taylor, C., Trigilio, I. S., Troitsky, G., Umana, L. A., Antonelli, S., Colafrancesco, S., Cutini, D., Gasparrini, C., Pittori, B., Preger, P., Santolamazza, F., Verrecchia, P., Giommi, and L., Salotti

Subjects
Agile, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Radio spectrum, gamma-ray flare, High Energy Gamma-ray Astronomy, AGILE satellite, Active Galactic Nuclei, law.invention, law, quasar, Blazar, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Gamma ray, Compton scattering, Astronomy and Astrophysics, Quasar, Space and Planetary Science, gamma-rays: observations – mechanism: non-thermal – quasars: individual (PKS 1510-089), Spectral energy distribution, Astrophysics - High Energy Astrophysical Phenomena, Flare, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report the detection by the AGILE satellite of a rapid gamma-ray flare from the powerful gamma-ray quasar PKS 1510-089, during a pointing centered on the Galactic Center region from 1 March to 30 March 2008. This source has been continuosly monitored in the radio-to-optical bands by the GLAST-AGILE Support Program (GASP) of the Whole Earth Blazar Telescope (WEBT). Moreover, the gamma-ray flaring episode triggered three ToO observations by the Swift satellite in three consecutive days, starting from 20 March 2008. In the period 1-16 March 2008, AGILE detected gamma-ray emission from PKS 1510-089 at a significance level of 6.2-sigma with an average flux over the entire period of (84 +/- 17) x 10^{-8} photons cm^{-2} s^{-1} for photon energies above 100 MeV. After a predefined satellite re-pointing, between 17 and 21 March 2008, AGILE detected the source at a significance level of 7.3-sigma, with an average flux (E > 100 MeV) of (134 +/- 29) x 10^{-8} photons cm^{-2} s^{-1} and a peak level of (281 +/- 68) x 10^{-8} photons cm^{-2} s^{-1} with daily integration. During the observing period January-April 2008, the source also showed an intense and variable optical activity, with several flaring episodes and a significant increase of the flux was observed at millimetric frequencies. Moreover, in the X-ray band the Swift/XRT observations seem to show an harder-when-brighter behaviour of the source spectrum. The spectral energy distribution of mid-March 2008 is modelled with a homogeneous one-zone synchrotron self Compton emission plus contributions from inverse Compton scattering of external photons from both the accretion disc and the broad line region. Indeed, some features in the optical-UV spectrum seem to indicate the presence of Seyfert-like components, such as the little blue bump and the big blue bump., 10 pages, 4 figures and 2 tables, accepted for publication in A&A

Published
2009

150. Detection of Gamma-Ray Emission from the Eta-Carinae Region

Author

Massimo Rapisarda, C. Pittori, D. Zanello, Roberto Viotti, L. Salotti, Filippo D'Ammando, T. Froysland, Michael F. Corcoran, Claudio Labanti, Maura Pilia, Elena Pian, Paolo Soffitta, A. Zambra, F. Boffelli, Francesco Lazzarotto, Alessio Trois, Geiland Porrovecchio, A. Pellizzoni, F. Fuschino, A. Giuliani, Francesco Longo, Marco Feroci, Luigi Pacciani, L. A. Antonelli, Fulvio Gianotti, G. Piano, Y. Evangelista, G. Di Cocco, M. Prest, E. Del Monte, Marcello Mastropietro, I. Donnarumma, S. Vercellone, Paolo Lipari, I. Lapshov, E. Moretti, V. Vittorini, G. Pucella, G. De Paris, M. Trifoglio, P. A. Caraveo, V. Cocco, Marco Tavani, S. Sabatini, Sergio Colafrancesco, Ennio Morelli, M. Galli, Sandro Mereghetti, P. W. Cattaneo, Piergiorgio Picozza, Massimiliano Fiorini, F. Verrecchia, Martino Marisaldi, A. W. Chen, F. Perotti, A. Morselli, A. Argan, P. Santolamazza, Andrea Bulgarelli, Enrico Costa, Alda Rubini, Paolo Giommi, A. Rappoldi, E. Vallazza, Attilio Ferrari, Guido Barbiellini, Tavani M, Sabatini S, Pian E, Bulgarelli A, Caraveo P, Viotti R F, Corcoran M F, Giuliani A, Pittori C, Verrecchia F, Vercellone S, Mereghetti S, Argan A, Barbiellini G, Boffelli F, Cattaneo P W, Chen A W, Cocco V, DAmmando F, Costa E, DeParis G, Del Monte E, Di Cocco G, Donnarumma I, Evangelista Y, Ferrari A, Feroci M, Fiorini M, Froysland T, Fuschino F, Galli M, Gianotti F, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Longo F, Marisaldi M, Mastropietro M, Morelli E, Moretti E, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Piano G, Picozza P, Pilia M, Porrovecchio G, Pucella G, Prest M, Rapisarda M, Rappoldi A, Rubini A, Soffitta P, Trifoglio M, Trois A, Vallazza E, Vittorini V, Zambra A, Zanello D, Santolamazza P, Giommi P, Colafrancesco S, Antonelli L A, Salotti L, M., Tavani, S., Sabatini, E., Pian, A., Bulgarelli, P., Caraveo, R. F., Viotti, M. F., Corcoran, A., Giuliani, C., Pittori, F., Verrecchia, S., Vercellone, S., Mereghetti, A., Argan, G., Barbiellini, F., Boffelli, P. W., Cattaneo, A. W., Chen, V., Cocco, F., D'Ammando, E., Costa, G. D., Pari, E. D., Monte, G. D., Cocco, I., Donnarumma, Y., Evangelista, A., Ferrari, M., Feroci, M., Fiorini, T., Froysland, F., Fuschino, M., Galli, F., Gianotti, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, Longo, Francesco, M., Marisaldi, M., Mastropietro, E., Morelli, E., Moretti, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, G., Piano, P., Picozza, M., Pilia, G., Porrovecchio, G., Pucella, M., Prest, M., Rapisarda, A., Rappoldi, A., Rubini, P., Soffitta, M., Trifoglio, A., Troi, E., Vallazza, V., Vittorini, A., Zambra, D., Zanello, P., Santolamazza, P., Giommi, S., Colafrancesco, L. A., Antonelli, and L., Salotti

Subjects
Agile, Astrophysics::High Energy Astrophysical Phenomena, Carina Nebula, Flux, FOS: Physical sciences, Astrophysics, Radiation, High Energy Gamma-ray Astronomy, Luminosity, gamma rays: observations, stars: individual: Eta Carinae, stars: winds, outflows, X-rays: binaries, Astrophysics::Solar and Stellar Astrophysics, wind binary Eta Carinae, Astrophysics::Galaxy Astrophysics, Colliding-wind binary, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Nebula, Gamma ray, Galactic region, Astronomy and Astrophysics, AGILE satellite, Unidentified Gamma-ray Sources, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present the results of extensive observations by the gamma-ray AGILE satellite of the Galactic region hosting the Carina nebula and the remarkable colliding wind binary Eta Carinae (Eta Car) during the period 2007 July to 2009 January. We detect a gamma-ray source (1AGL J1043-5931) consistent with the position of Eta Car. If 1AGL J1043-5931 is associated with the Eta Car system our data provide the long sought first detection above 100 MeV of a colliding wind binary. The average gamma-ray flux above 100 MeV and integrated over the pre-periastron period 2007 July to 2008 October is F = (37 +/- 5) x 10-8 ph cm-2 s-1 corresponding to an average gamma-ray luminosity of L = 3.4 x 10^34 erg s-1 for a distance of 2.3 kpc. We also report a 2-day gamma-ray flaring episode of 1AGL J1043-5931 on 2008 Oct. 11-13 possibly related to a transient acceleration and radiation episode of the strongly variable shock in the system., Comment: 5 pages, 4 figure, accepted for publication in ApJ Letters

Published
2009

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