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1. Evidence of a New Population of Weak Terrestrial Gamma‐Ray Flashes Observed From Aircraft Altitude

Author

I. Bjørge‐Engeland, N. Østgaard, D. Sarria, M. Marisaldi, A. Mezentsev, A. Fuglestad, N. Lehtinen, J. E. Grove, D. Shy, T. Lang, M. Quick, H. Christian, C. Schultz, R. Blakeslee, I. Adams, R. Kroodsma, G. Heymsfield, K. Ullaland, S. Yang, B. Hasan Qureshi, J. Søndergaard, B. Husa, D. Walker, M. Bateman, D. Mach, P. Bitzer, M. Fullekrug, M. Cohen, M. Stanley, S. Cummer, J. Montanya, M. Pazos, C. Velosa, O. van derVelde, Y. Pu, P. Krehbiel, J. A. Roncancio, J. A. Lopez, M. Urbani, A. Santos, T. Neubert, and F. Gordillo‐Vazquez

Subjects
terrestrial gamma‐ray flashes, lightning, ALOFT, aircraft campaign, ASIM, Geophysics. Cosmic physics, QC801-809
Abstract

Abstract Terrestrial Gamma‐ray Flashes (TGFs) are ten‐to‐hundreds of microsecond bursts of gamma‐rays produced when electrons in strong electric fields in thunderclouds are accelerated to relativistic energies. Space instruments have observed TGFs with source photon brightness down to ∼1017–1016. Based on space and aircraft observations, TGFs have been considered rare phenomena produced in association with very few lightning discharges. Space observations associated with lightning ground observations in the radio band have indicated that there exists a population of dimmer TGFs. Here we show observations of TGFs from aircraft altitude that were not detected by a space instrument viewing the same area. The TGFs were found through Monte Carlo modeling to be associated with 1015–1012 photons at source, which is several orders of magnitude below what can be seen from space. Our results suggest that there exists a significant population of TGFs that are too weak to be observed from space.

Published
2024
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2. Possible effects on avionics induced by terrestrial gamma-ray flashes

Author

M. Tavani, A. Argan, A. Paccagnella, A. Pesoli, F. Palma, S. Gerardin, M. Bagatin, A. Trois, P. Picozza, P. Benvenuti, E. Flamini, M. Marisaldi, C. Pittori, and P. Giommi

Subjects
Environmental technology. Sanitary engineering, TD1-1066, Geography. Anthropology. Recreation, Environmental sciences, GE1-350, Geology, QE1-996.5
Abstract

Terrestrial gamma-ray flashes (TGFs) are impulsive (intrinsically sub-millisecond) events associated with lightning in powerful thunderstorms. TGFs turn out to be very powerful natural accelerators known to accelerate particles and generate radiation up to hundreds of MeV energies. The number ratio of TGFs over normal lightning has been measured in tropical regions to be near 10−4. We address in this Article the issue of the possible susceptibility of typical aircraft electronics exposed to TGF particle, gamma ray and neutron irradiation. We consider possible scenarios regarding the intensity, the duration, and geometry of TGFs influencing nearby aircraft, and study their effects on electronic equipment. We calculate, for different assumptions, the total dose and the dose-rate, and estimate single-event-effects. We find that in addition to the electromagnetic component (electrons/positrons, gamma rays) also secondary neutrons produced by gamma-ray photo production in the aircraft structure substantially contribute to single-event effects in critical semiconductors components. Depending on the physical characteristics and geometry, TGFs may deliver a large flux of neutrons within a few milliseconds in an aircraft. This flux is calculated to be orders of magnitude larger than the natural cosmic-ray background, and may constitute a serious hazard to aircraft electronic equipment. We present a series of numerical simulations supporting our conclusions. Our results suggest the necessity of dedicated measurement campaigns addressing the radiative and particle environment of aircraft near or within thunderstorms.

Published
2013
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3. Flickering Gamma Flashes, the Missing Link Between Gamma Glows and TGFs

Author

N Østgaard, A Mezentsev, M Marisaldi, J E Grove, M Quick, H Christian, S Cummer, M Pazos, Y Pu, M Stanley, D Sarria, T Lang, C Schultz, R Blakeslee, I Adams, R Kroodsma, G Heymsfield, N Lehtinen, K Ullaland, S Yang, B Hasan Qureshi, J Søndergaard, B Husa, D Walker, D Shy, M Bateman, P Bitzer, M Fullekrug, M Cohen, J Montanya, C Younes, O van der Velde, P Krehbiel, J A Roncancio, J A Lopez, M Urbani, A Santos, and D Mach

Subjects
Meteorology and Climatology, Space Radiation
Abstract

Two different hard radiation phenomena are known to originate from thunderclouds: Terrestrial Gamma-ray Flashes (TGFs) and gamma-ray glows. Both involve avalanche of electrons accelerated to relativistic energies but are different phenomena. Glows are known to last for one-to-hundreds of seconds, have moderate intensities and originate from quasi-stationary thundercloud fields. TGFs exhibit high intensities and have characteristic durations of tens-to-hundreds of microseconds. TGFs often show close association with emission of strong radio signals and optical pulses indicating involvement of lightning leaders in their generation. Here we report unique observations of a different phenomenon, which we call Flickering Gamma-ray Flashes (FGFs). FGFs resemble usual multi-pulse TGFs, but with larger number of pulses and each pulse has a longer duration than ordinary TGFs. FGF durations span from 20 to 250 milliseconds, which reaches the lower boundary of the gamma-ray glow duration. FGFs are radio and optically silent, which makes them distinct from normal TGFs. An FGF starts as an ordinary gamma-ray glow, then suddenly increases exponentially in intensity, and turns into an unstable, “flickering” mode with a sequence of pulses. FGFs could be the missing link between the gamma-ray glows and conventional TGFs, whose absence has been puzzling atmospheric electricity community for two decades.

Published
2024

4. Highly Dynamic Gamma-Ray Emissions Are Common in Tropical Thunderclouds

Author

M Marisaldi, N Østgaard, A Mezentsev, T Lang, J E Grove, D Shy, G M Heymsfield, P Krehbiel, R J Thomas, M Stanley, D Sarria, C Schultz, R Blakeslee, M G Quick, H Christian, I Adams, R Kroodsma, N Lehtinen, K Ullaland, S Yang, B Hasan Qureshi, J Søndergaard, B Husa, D Walker, M Bateman, D Mach, S Cummer, M Pazos, Y Pu, P Bitzer, M Fullekrug, M Cohen, J Montanya, C Younes, O van der Velde, J A Roncancio, J A Lopez, M Urbani, and A Santos

Subjects
Meteorology and Climatology
Abstract

Thunderstorms emit fluxes of gamma rays known as gamma-ray glows, sporadically observed by aircraft, balloons and from ground. Glows are observed as increased gamma-ray emissions by tens of percent up to two orders of magnitude above the background, sometimes abruptly terminated by lightning discharges. Glows are produced by the acceleration of energetic electrons in high electric field regions within thunderclouds, and contribute to charge dissipation. Glows are considered as quasi�-stationary phenomena, with durations up to a few tens of seconds and spatial scales up to 10-20 kilometers. No measurement of the full extension in space and time of a gamma� ray glow region and their occurring frequency has been reported so far. Here we show that tropical thunderclouds over ocean and coastal regions commonly emit gamma rays for hours over areas up to a few thousands of square kilometers. Emission is associated with deep convective cores; it is not uniform and continuous but shows characteristic timescales of 1-10 seconds and even sub-second for individual glows. The dynamics of gamma-glowing thunderclouds starkly contradicts the quasi-stationary picture of glows, but rather resembles that of a huge gamma-glowing «boiling pot» both in pattern and behavior.

Published
2024

5. AGILE detection of GeV gamma-ray emission from the SNR W28

Author

Giuliani, A., Tavani, M., Bulgarelli, A., Striani, E., Sabatini, S., Cardillo, M., Fukui, Y., Kawamura, A., Ohama, A., Furukawa, N., Torii, K., Aharonian, F. A., Verrecchia, F., Argan, A., Barbiellini, G., Caraveo, P. A., Cattaneo, P. W., Chen, A. W., Cocco, V., Costa, E., D'Ammando, F., Del Monte, E., De Paris, G., Di Cocco, G., Donnarumma, I., Evangelista, Y., Feroci, M., Fiorini, M., Froysland, T., Fuschino, F., Galli, M., Gianotti, F., Labanti, C., Lapshov, Y., Lazzarotto, F., Lipari, P., Longo, F., Mereghetti, M. Marisaldi., Morselli, A., Moretti, E., Pacciani, L., Pellizzoni, A., Perotti, F., Picozza, P., Pilia, M., Prest, M., Pucella, G., Rapisarda, M., Rappoldi, A., Soffitta, P., Trifoglio, M., Trois, A., Vallazza, E., Vercellone, S., Vittorini, V., Zambra, A., Zanello, D., Pittori, C., Santolamazza, P., Giommi, P., Colafrancesco, S., and Salotti, L.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Supernova remnants (SNRs) are believed to be the main sources of Galactic cosmic rays. Molecular clouds associated with SNRs can produce gamma-ray emission through the interaction of accelerated particles with the concentrated gas. The middle aged SNR W28, for its associated system of dense molecular clouds, provides an excellent opportunity to test this hypothesis. We present the AGILE/GRID observations of SNR W28, and compare them with observations at other wavelengths (TeV and 12CO J=1-->0 molecular line emission). The gamma-ray flux detected by AGILE from the dominant source associated with W28 is (14 +- 5) 10^-8 ph cm^-2 s^-1 for E > 400 MeV. This source is positionally well correlated with the TeV emission observed by the HESS telescope. The local variations of the GeV to TeV flux ratio suggest a difference between the CR spectra of the north-west and south molecular cloud complexes. A model based on a hadronic-induced interaction and diffusion with two molecular clouds at different distances from the W28 shell can explain both the morphological and spectral features observed by AGILE in the MeV-GeV energy range and by the HESS telescope in the TeV energy range. The combined set of AGILE and H.E.S.S. data strongly support a hadronic model for the gamma-ray production in W28., Comment: Accepted for publication in Astronomy & Astrophysics Letters

Published
2010
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6. Multiwavelength study of the luminous GRB 210619B observed with Fermi and ASIM

Author

M D Caballero-García, Rahul Gupta, S B Pandey, S R Oates, M Marisaldi, A Ramsli, Y-D Hu, A J Castro-Tirado, R Sánchez-Ramírez, P H Connell, F Christiansen, A Kumar Ror, A Aryan, J-M Bai, M A Castro-Tirado, Y-F Fan, E Fernández-García, A Kumar, A Lindanger, A Mezentsev, J Navarro-González, T Neubert, N Østgaard, I Pérez-García, V Reglero, D Sarria, T R Sun, D-R Xiong, J Yang, Y-H Yang, and B-B Zhang

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, data analysis [Methods], Astrophysics - High Energy Astrophysical Phenomena, individual: GRB 210619B [Gamma-ray burst], Astrophysics::Galaxy Astrophysics, general [Gamma-ray burst]
Abstract

We report on detailed multi-wavelength observations and analysis of the very bright and long GRB 210619B, detected by the Atmosphere-Space Interactions Monitor (ASIM) installed on the International Space Station (ISS) and the Gamma-ray Burst Monitor (GBM) on-board the Fermi mission. Our main goal is to understand the radiation mechanisms and jet composition of GRB 210619B. With a measured redshift of $z$ = 1.937, we find that GRB 210619B falls within the 10 most luminous bursts observed by Fermi so far. The energy-resolved prompt emission light curve of GRB 210619B exhibits an extremely bright hard emission pulse followed by softer/longer emission pulses. The low-energy photon indices ($\alpha_{\rm pt}$) values obtained using the time-resolved spectral analysis of the burst suggest a transition between the thermal (during harder pulse) to non-thermal (during softer pulse) outflow. We examine the correlation between spectral parameters and find that both peak energy and $\alpha_{\rm pt}$ exhibit the flux tracking pattern. The late time broadband photometric dataset can be explained within the framework of the external forward shock model with $\nu_m$ $< \nu_c$ $< \nu_{x}$ (where $\nu_m$, $\nu_c$, and $\nu_{x}$ are the synchrotron peak, cooling-break, and X-ray frequencies, respectively) spectral regime supporting a rarely observed hard electron energy index ($p, Comment: 24 pages, 18 figures, 10 tables, accepted for publication in MNRAS

Published
2022
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8. Ultra high energy cosmic rays The intersection of the Cosmic and Energy Frontiers

Author

A. Coleman, J. Eser, E. Mayotte, F. Sarazin, F.G. Schröder, D. Soldin, T.M. Venters, R. Aloisio, J. Alvarez-Muñiz, R. Alves Batista, D. Bergman, M. Bertaina, L. Caccianiga, O. Deligny, H.P. Dembinski, P.B. Denton, A. di Matteo, N. Globus, J. Glombitza, G. Golup, A. Haungs, J.R. Hörandel, T.R. Jaffe, J.L. Kelley, J.F. Krizmanic, L. Lu, J.N. Matthews, I. Mariş, R. Mussa, F. Oikonomou, T. Pierog, E. Santos, P. Tinyakov, Y. Tsunesada, M. Unger, A. Yushkov, M.G. Albrow, L.A. Anchordoqui, K. Andeen, E. Arnone, D. Barghini, E. Bechtol, J.A. Bellido, M. Casolino, A. Castellina, L. Cazon, R. Conceição, R. Cremonini, H. Dujmovic, R. Engel, G. Farrar, F. Fenu, S. Ferrarese, T. Fujii, D. Gardiol, M. Gritsevich, P. Homola, T. Huege, K.-H. Kampert, D. Kang, E. Kido, P. Klimov, K. Kotera, B. Kozelov, A. Leszczyńska, J. Madsen, L. Marcelli, M. Marisaldi, O. Martineau-Huynh, S. Mayotte, K. Mulrey, K. Murase, M.S. Muzio, S. Ogio, A.V. Olinto, Y. Onel, T. Paul, L. Piotrowski, M. Plum, B. Pont, M. Reininghaus, B. Riedel, F. Riehn, M. Roth, T. Sako, F. Schlüter, D.H. Shoemaker, J. Sidhu, I. Sidelnik, C. Timmermans, O. Tkachenko, D. Veberic, S. Verpoest, V. Verzi, J. Vícha, D. Winn, E. Zas, and M. Zotov

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Energy Frontier, Astronomy, Particle physics, FOS: Physical sciences, Astronomy and Astrophysics, Cosmic Frontier, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), Astroparticle Physics, Ultra High Energy Cosmic Rays, Snowmass White Paper, Experimental High Energy Physics, High Energy Physics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

The present white paper is submitted as part of the "Snowmass" process to help inform the long-term plans of the United States Department of Energy and the National Science Foundation for high-energy physics. It summarizes the science questions driving the Ultra-High-Energy Cosmic-Ray (UHECR) community and provides recommendations on the strategy to answer them in the next two decades., Comment: Prepared as a solicited white paper for the 2021 Snowmass process. To be published in the Journal of High Energy Astrophysics. v2: fixed typos in author list. v3: included all community feedback received by July 1st 2022 and added the list of endorsers. v4 is the post-reviewer preprint accepted to Astroparticle Physics vol. 149

Published
2023

9. The Second Catalog of Interplanetary Network Localizations of Konus Short Duration Gamma-Ray Bursts

Author

D. S. Svinkin, K. Hurley, A. V. Ridnaia, A. L. Lysenko, D. D. Frederiks, S. V. Golenetskii, A. E. Tsvetkova, M. V. Ulanov, A. Kokomov, T. L. Cline, I. Mitrofanov, D. Golovin, A. Kozyrev, M. Litvak, A. Sanin, A. Goldstein, M. S. Briggs, C. Wilson-Hodge, E. Burns, A. von Kienlin, X.-L. Zhang, A. Rau, V. Savchenko, E. Bozzo, C. Ferrigno, S. Barthelmy, J. Cummings, H. Krimm, D. M. Palmer, A. Tohuvavohu, K. Yamaoka, M. Ohno, Y. Fukazawa, Y. Hanabata, T. Takahashi, M. Tashiro, Y. Terada, T. Murakami, K. Makishima, W. Boynton, C. W. Fellows, K. P. Harshman, H. Enos, R. Starr, J. Goldsten, R. Gold, A. Ursi, M. Tavani, A. Bulgarelli, C. Casentini, E. Del Monte, Y. Evangelista, M. Galli, F. Longo, M. Marisaldi, N. Parmiggiani, C. Pittori, M. Romani, F. Verrecchia, D. M. Smith, W. Hajdas, S. Xiao, C. Cai, Q. B. Yi, Y. Q. Zhang, S. L. Xiong, X. B. Li, Y. Huang, C. K. Li, S. N. Zhang, L. M. Song, C. Z. Liu, X. Q. Li, W. X. Peng, and I. Martinez-Castellanos

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present the catalog of Interplanetary Network (IPN) localizations for 199 short-duration gamma-ray bursts (sGRBs) detected by the Konus-Wind (KW) experiment between 2011 January 1 and 2021 August 31, which extends the initial sample of IPN localized KW sGRBs (arXiv:1301.3740) to 495 events. We present the most comprehensive IPN localization data on these events, including probability sky maps in HEALPix format., Published in ApJS

Published
2022

10. Production of Terrestrial Gamma-Ray Flashes During the Early Stages of Lightning Flashes

Author

A. Lindanger, C. A. Skeie, M. Marisaldi, I. Bjørge‐Engeland, N. Østgaard, A. Mezentsev, D. Sarria, N. Lehtinen, V. Reglero, O. Chanrion, and T. Neubert

Subjects
Atmospheric Science, Geophysics, Space and Planetary Science, Earth and Planetary Sciences (miscellaneous)
Abstract

Terrestrial Gamma-ray Flashes (TGFs) are short emissions of high energy photons associated with thunderstorms. It has been known since the discovery of TGFs that they are associated with lightning, and several case studies have shown that the TGFs are produced at the initial phase of the lightning flash. However, it has not been tested whether this is true in general. By using the largest TGF sample up to date, combined with ground-based radio lightning detection data, we perform a statistical study to test this. One of the TGF missions is the Atmosphere-Space Interactions Monitor (ASIM) consisting of the innovative combination of X- and gamma-ray detectors, optical photometers and cameras. This allows us to investigate the temporal relation between gamma-rays produced by TGFs and the optical signal produced by lightning discharges. Based on stacking analysis of the TGF sample and ground-based measurements of associated lightning activity, together with the high temporal resolution of the optical signal from the ASIM photometers, it is shown that TGFs are produced in the beginning of the lightning flashes. In addition, for a significant fraction of the TGFs, the lightning activity detected in radio is enhanced in an interval between 150 and 750 ms following the TGFs, and is co-located with the lightning associated with the TGFs. The enhanced lightning activity is not evident in a randomly selected sample of flashes. This indicates that the activity between 150 and 750 ms is a characteristic property of a significant fraction of flashes that start with a TGF. publishedVersion

Published
2022
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11. The temporal relationship between Terrestrial Gamma‐ray flashes and associated optical pulses from lightning

Author

C. A. Skeie, N. Østgaard, A. Mezentsev, I. Bjørge‐Engeland, M. Marisaldi, N. Lehtinen, V. Reglero, and T. Neubert

Subjects
Atmospheric Science, Geophysics, Space and Planetary Science, Earth and Planetary Sciences (miscellaneous)
Abstract

We present 221 Terrestrial Gamma-ray Flashes (TGFs) and associated optical pulses observed by the Atmosphere-Space Interactions Monitor (ASIM) on board the International Space Station. The events were detected between the end of March 2019 and November 2020 and consist of X- and gamma-ray energy detections, as well as photometer data (180–230, 337, and 777 nm) and optical camera data (337 and 777 nm). Using the available ASIM data and applying a consistency check based on TGF characteristics and lightning detections from lightning radio atmospherics close in time, we determine the most likely position of the TGFs in relation to the photometer field of view (FoV), and the association to the observed optical pulses. Out of the 221 events we find 72 events where the TGF and optical data are determined to be associated and inside the photometer FoV. Using the measured TGF durations and the time between the onsets of the TGFs and optical pulses we find: (a) That the TGF onsets are always before or at the same time as the optical pulse onsets (taking into account cloud scattering). (b) A tendency for longer duration TGFs to have longer delays between onsets. (c) Two groups of events: (a) where there is a possible overlap between the TGFs and the optical emissions, as the TGFs last longer than the delay between onsets and (b) where the TGFs and optical emissions do not overlap, as there are long delays between the onsets, which cannot be explained by cloud scattering. publishedVersion

Published
2022
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12. AGILE Observations of GRB 220101A: A 'New Year's Burst' with an Exceptionally Huge Energy Release

Author

A. Ursi, M. Romani, G. Piano, F. Verrecchia, F. Longo, C. Pittori, M. Tavani, A. Bulgarelli, M. Cardillo, C. Casentini, P. W. Cattaneo, E. Costa, M. Feroci, V. Fioretti, L. Foffano, F. Lucarelli, M. Marisaldi, A. Morselli, L. Pacciani, N. Parmiggiani, P. Tempesta, A. Trois, and S. Vercellone

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We report the AGILE observations of GRB 220101A, which took place at the beginning of 1st January 2022 and was recognized as one of the most energetic gamma-ray bursts (GRBs) ever detected since their discovery. The AGILE satellite acquired interesting data concerning the prompt phase of this burst, providing an overall temporal and spectral description of the event in a wide energy range, from tens of keV to tens of MeV. Dividing the prompt emission into three main intervals, we notice an interesting spectral evolution, featuring a notable hardening of the spectrum in the central part of the burst. The average fluxes encountered in the different time intervals are relatively moderate, with respect to those of other remarkable bursts, and the overall fluence exhibits a quite ordinary value among the GRBs detected by MCAL. However, GRB 220101A is the second farthest event detected by AGILE, and the burst with the highest isotropic equivalent energy of the whole MCAL GRB sample, releasing E_iso=2.54x10^54 erg and exhibiting an isotropic luminosity of L_iso=2.34x10^52 erg/s (both in the 400 keV - 10 MeV energy range). We also analyzed the first 10^6 s of the afterglow phase, using the publicly available Swift XRT data, carrying out a theoretical analysis of the afterglow, based on the forward shock model. We notice that GRB 220101A is with high probability surrounded with a wind-like density medium, and that the energy carried by the initial shock shall be a fraction of the total E_iso, presumably near 50%., Comment: 16 pages, 9 figures, 4 tables

Published
2022
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13. Very-high-frequency oscillations in the main peak of a magnetar giant flare

Author

A. J. Castro-Tirado, N. Østgaard, E. Göǧüş, C. Sánchez-Gil, J. Pascual-Granado, V. Reglero, A. Mezentsev, M. Gabler, M. Marisaldi, T. Neubert, C. Budtz-Jørgensen, A. Lindanger, D. Sarria, I. Kuvvetli, P. Cerdá-Durán, J. Navarro-González, J. A. Font, B.-B. Zhang, N. Lund, C. A. Oxborrow, S. Brandt, M. D. Caballero-García, I. M. Carrasco-García, A. Castellón, M. A. Castro Tirado, F. Christiansen, C. J. Eyles, E. Fernández-García, G. Genov, S. Guziy, Y.-D. Hu, A. Nicuesa Guelbenzu, S. B. Pandey, Z.-K. Peng, C. Pérez del Pulgar, A. J. Reina Terol, E. Rodríguez, R. Sánchez-Ramírez, T. Sun, K. Ullaland, S. Yang, European Space Agency, European Research Council, European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), and Generalitat Valenciana

Subjects
Multidisciplinary, Stars, Celestial, Atmosphere
Abstract

Full list of authors: Castro-Tirado, A. J.; Østgaard, N.; Göǧüş, E.; Sánchez-Gil, C.; Pascual-Granado, J.; Reglero, V.; Mezentsev, A.; Gabler, M.; Marisaldi, M.; Neubert, T.; Budtz-Jørgensen, C.; Lindanger, A. Sarria, D.; Kuvvetli, I.; Cerdá-Durán, P.; Navarro-González, J.; Font, J. A.; Zhang, B. -B.; Lund, N.; Oxborrow, C. A.; Brandt, S.; Caballero-García, M. D.; Carrasco-García, I. M.; Castellón, A.; Castro Tirado, M. A.; Christiansen, F.; Eyles, C. J.; Fernández-García, E.; Genov, G.; Guziy, S.; Hu, Y. -D.; Nicuesa Guelbenzu, A.; Pandey, S. B.; Peng, Z. -K.; Pérez del Pulgar, C.; Reina Terol, A. J.; Rodríguez, E.; Sánchez-Ramírez, R.; Sun, T.; Ullaland, K.; Yang, S., Magnetars are strongly magnetized, isolated neutron stars1–3 with magnetic fields up to around 1015 gauss, luminosities of approximately 1031–1036 ergs per second and rotation periods of about 0.3–12.0 s. Very energetic giant flares from galactic magnetars (peak luminosities of 1044–1047 ergs per second, lasting approximately 0.1 s) have been detected in hard X-rays and soft γ-rays4, and only one has been detected from outside our galaxy5. During such giant flares, quasi-periodic oscillations (QPOs) with low (less than 150 hertz) and high (greater than 500 hertz) frequencies have been observed6–9, but their statistical significance has been questioned10. High-frequency QPOs have been seen only during the tail phase of the flare9. Here we report the observation of two broad QPOs at approximately 2,132 hertz and 4,250 hertz in the main peak of a giant γ-ray flare11 in the direction of the NGC 253 galaxy12–17, disappearing after 3.5 milliseconds. The flare was detected on 15 April 2020 by the Atmosphere–Space Interactions Monitor instrument18,19 aboard the International Space Station, which was the only instrument that recorded the main burst phase (0.8–3.2 milliseconds) in the full energy range (50 × 103 to 40 × 106 electronvolts) without suffering from saturation effects such as deadtime and pile-up. Along with sudden spectral variations, these extremely high-frequency oscillations in the burst peak are a crucial component that will aid our understanding of magnetar giant flares. © 2021, The Author(s), under exclusive licence to Springer Nature Limited., This work made use of data from ASIM. ASIM is an international experiment aboard the International Space Station. ASIM is a mission of the European Space Agency (ESA), funded by ESA and national grants from Denmark, Norway and Spain. ESA PRODEX contracts C 4000115884 (DTU) and 4000123438 (Bergen) support the ASIM Science Data Centre. The science analysis is supported by ESA Topical Team contract 4200019920/06/NL/VJ; European Research Council grant AdG-FP7/2007-2013: n 320839; Research Council of Norway contract 223252/F50 (CoE/BCSS); and Ministerio de Ciencia, Innovación y Universidades grants ESP 2017-86263-C4 and ESP2017-87676-C5-5-R. J.A.F. and P.C.-D. acknowledge support by the Spanish Agencia Estatal de Investigación (grant PGC2018-095984-B-I00) and by the Generalitat Valenciana (PROMETEO/2019/071). P.C.-D. acknowledges the Ramon y Cajal funding (RYC-2015-19074) for supporting his research. M.G. acknowledges support through the Generalitat Valenciana via the grant CIDEGENT/2019/031. A.J.C.-T., J.P.-G., M.D.C.-G. and E.R. acknowledge financial support from the State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). This work is partly based on observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, on the island of La Palma. We thank J. D. Scargle for his help with the preliminary time-series analysis and his comments. J.P.-G. also acknowledges funding support from Spanish public funds for research from project PID2019-107061GB-C63 from the ‘Programas Estatales de Generación de Conocimiento y Fortalecimiento Científico y Tecnológico del Sistema de I+D+i y de I+D+i Orientada a los Retos de la Sociedad’ from the Spanish Ministry of Science, Innovation and Universities (MCIU).

Published
2021
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14. THE INTERPLANETARY NETWORK

Author

K. Hurley, I. G. Mitrofanov, D. Golovin, M. L. Litvak, A. B. Sanin, W. Boynton, C. Fellows, K. Harshman, R. Starr, S. Golenetskii, R. Aptekar, E. Mazets, V. Palshin, D. Frederiks, D. Svinkin, D. M. Smith, W. Hajdas, A. von Kienlin, X. Zhang, A. Rau, K. Yamaoka, T. Takahashi, M. Ohno, Y. Hanabata, Y. Fukazawa, M. Tashiro, Y. Terada, T. Murakami, K. Makishima, T. Cline, S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, D. Palmer, J. Goldsten, E. Del Monte, M. Feroci, M. Marisaldi, V. Connaughton, M. S. Briggs, and C. Meegan

Published
2020
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15. The Second AGILE MCAL Gamma-Ray Burst Catalog: 13 yr of Observations

Author

A. Ursi, M. Romani, F. Verrecchia, C. Pittori, M. Tavani, M. Marisaldi, M. Galli, C. Labanti, N. Parmiggiani, A. Bulgarelli, A. Addis, L. Baroncelli, M. Cardillo, C. Casentini, P. W. Cattaneo, A. Chen, A. Di Piano, F. Fuschino, F. Longo, F. Lucarelli, A. Morselli, G. Piano, and S. Vercellone

Subjects
Space and Planetary Science, Astronomy and Astrophysics
Abstract

We present the results of a systematic search and analysis of GRBs detected by the Astrorivelatore Gamma ad Immagini LEggero (AGILE) MiniCALorimeter (MCAL; 0.4–100 MeV) over a time frame of 13 yr, from 2007 to 2020 November. The MCAL GRB sample consists of 503 bursts triggered by MCAL, 394 of which were fully detected onboard with high time resolution. The sample consists of about 44% short GRBs and 56% long GRBs. In addition, 109 bursts triggered partial MCAL onboard data acquisitions, providing further detections that can be used for joint analyses or triangulations. More than 90% of these GRBs were also detected by the AGILE Scientific RateMeters (RMs), providing simultaneous observations between 20 keV and 100 MeV. We performed spectral analysis of these events in the 0.4–50 MeV energy range. We could fit the time-integrated spectrum of 258 GRBs with a single power-law model, resulting in a mean photon index 〈β〉of−2.3. Among them, 43 bursts could also be fitted with a Band model, with peak energy above 400 keV, resulting in a mean low-energy photon index 〈α〉 = −0.6, a mean high-energy photon index 〈β〉 = −2.5, and a mean peak energy 〈E p 〉 = 640 keV. The AGILE MCAL GRB sample mostly consists of hard-spectrum GRBs, with a large fraction of short-duration events. We discuss properties and features of the MCAL bursts, whose detections can be used to perform joint broad-band analysis with other missions, and to provide insights on the high-energy component of the prompt emission in the tens of mega electron volt energy range.

Published
2022
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16. The InterPlanetary Network Supplement to the Second Fermi GBM Catalog of Cosmic Gamma-Ray Bursts

Author

K. Hurley, R. L. Aptekar, S. V. Golenetskii, D. D. Frederiks, D. S. Svinkin, V. D. Pal’shin, M. S. Briggs, C. Meegan, V. Connaughton, J. Goldsten, W. Boynton, C. Fellows, K. Harshman, I. G. Mitrofanov, D. V. Golovin, A. S. Kozyrev, M. L. Litvak, A. B. Sanin, A. Rau, A. von Kienlin, X. Zhang, K. Yamaoka, Y. Fukazawa, M. Ohno, M. Tashiro, Y. Terada, S. Barthelmy, T. Cline, N. Gehrels, J. Cummings, H. A. Krimm, D. M. Smith, E. Del Monte, M. Feroci, M. Marisaldi, ITA, USA, DEU, JPN, NOR, and RUS

Subjects
Space and Planetary Science, Astronomy and Astrophysics
Abstract

InterPlanetary Network (IPN) data are presented for the gamma-ray bursts in the second Fermi Gamma-Ray Burst Monitor (GBM) catalog. Of the 462 bursts in that catalog between 2010 July 12 and 2012 July 11, 428, or 93%, were observed by at least 1 other instrument in the 9-spacecraft IPN. Of the 428, the localizations of 165 could be improved by triangulation. For these bursts, triangulation gives one or more annuli whose half-widths vary between about 2.′3° and 16°, depending on the peak flux, fluence, time history, arrival direction, and the distance between the spacecraft. We compare the IPN localizations with the GBM 1σ, 2σ, and 3σ error contours and find good agreement between them. The IPN 3σ error boxes have areas between about 8 square arcminutes and 380 square degrees, and are an average of 2500 times smaller than the corresponding GBM 3σ localizations. We identify four bursts in the IPN/GBM sample whose origins were given as “uncertain,” but may in fact be cosmic. This leads to an estimate of over 99% completeness for the GBM catalog.

Published
2017

17. The large area detector of LOFT: the Large Observatory for X-ray TimingSpace Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray

Author

Tadayuki Takahashi, Jan Willem A. den Herder, Mark Bautz, S. Zane, D. Walton, T. Kennedy, M. Feroci, J. W. Den Herder, M. Ahangarianabhari, A. Argan, P. Azzarello, M. Barbera, D. Barret, G. Bertuccio, P. Bodin, E. Bozzo, L. Bradley, F. Cadoux, P. Cais, R. Campana, J. Coker, A. Cros, E. Del Monte, A. De Rosa, S. Di Cosimo, I. Donnarumma, Y. Evangelista, Y. Favre, C. Feldman, G. Fraser, F. Fuschino, M. Grassi, M. R. Hailey, R. Hudec, C. Labanti, P. Malcovati, D. Macera, M. Marisaldi, A. Martindale, T. Mineo, F. Muleri, M. Nowak, M. Orlandini, L. Pacciani, E. Perinati, V. Petracek, M. Pohl, A. Rachevski, P. Smith, A. Santangelo, J. Y. Seyler, C. Schmid, P. Soffitta, S. Suchy, C. Tenzer, P. Uttley, A. Vacchi, G. Zampa, N. Zampa, J. Wilms, B. Winter, BALDAZZI, GIUSEPPE, Tadayuki Takahashi, Jan-Willem A. den Herder, Mark Bautz, S. Zane, D. Walton, T. Kennedy, M. Feroci, J.-W Den Herder, M. Ahangarianabhari, A. Argan, P. Azzarello, G. Baldazzi, M. Barbera, D. Barret, G. Bertuccio, P. Bodin, E. Bozzo, L. Bradley, F. Cadoux, P Cai, R. Campana, J. Coker, A. Cro, E. Del Monte, A. De Rosa, S. Di Cosimo, I. Donnarumma, Y. Evangelista, Y. Favre, C. Feldman, G. Fraser, F. Fuschino, M. Grassi, M. R. Hailey, R. Hudec, C. Labanti, P. Malcovati, D. Macera, M. Marisaldi, A. Martindale, T. Mineo, F. Muleri, M. Nowak, M. Orlandini, L. Pacciani, E. Perinati, V. Petracek, M. Pohl, A. Rachevski, P. Smith, A. Santangelo, J.-Y. Seyler, C. Schmid, P. Soffitta, S. Suchy, C. Tenzer, P. Uttley, A. Vacchi, G. Zampa, N. Zampa, J. Wilm, and B. Winter

Subjects
SPACE MISSIONS, large area position-sensitive detector, x-rays, SILICON DRIFT DETECTORS
Abstract

LOFT (Large Observatory for X-ray Timing) is one of the five candidates that were considered by ESA as an M3 mission (with launch in 2022-2024) and has been studied during an extensive assessment phase. It is specifically designed to perform fast X-ray timing and probe the status of the matter near black holes and neutron stars. Its pointed instrument is the Large Area Detector (LAD), a 10 m2-class instrument operating in the 2-30keV range, which holds the capability to revolutionise studies of variability from X-ray sources on the millisecond time scales. The LAD instrument has now completed the assessment phase but was not down-selected for launch. However, during the assessment, most of the trade-offs have been closed leading to a robust and well documented design that will be reproposed in future ESA calls. In this talk, we will summarize the characteristics of the LAD design and give an overview of the expectations for the instrument capabilities. © (2014) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.

Published
2014

19. Detection of multiple terrestrial gamma-ray flashes from thunderstorm systems

Author

A. Ursi, M. Marisaldi, M. Tavani, D. Casella, P. Sanò, and S. Dietrich

Subjects
AGILE, TGF, thunderstorm
Abstract

Since their discovery, Terrestrial Gamma ray Flashes (TGFs) exhibited an evident correlationwith thunderstorms and lightning activity. The fleeting nature of these events and the heavy absorptionof gamma rays in the lowest atmospheric layers severely hamper the observation of this phenomenon,making us reveal just a small fraction of a probably much wider population. As each thunderstorm producesa large amount of lightning discharges during its lifetime, it is reasonable that even a large amount of TGFsare produced during the same event. However, detection of multiple TGFs coming from the same stormis difficult to perform, as it requires the constant monitoring of a spatially limited geographic region:this is not an easy task to perform for satellites on high-inclination orbits that make them experiencenonnegligible latitudinal shifts at each orbital passage over a certain region, preventing the monitoringof a limited geographic region throughout successive overpasses. In this perspective, the quasi-equatorial(2.5?) orbit of the Astrorivelatore Gamma ad Immagini LEggero (AGILE) satellite ensures a minimal latitudinalshift when flying over the same region at successive passages, allowing for the follow-up of thunderstormsin time. We exploit this feature of the AGILE satellite to search for multiple TGFs coming from the samegeographic region and, in particular, from the same thunderstorm. We carry out this search on the AGILETGF database (2009-2016), ending up with a sample of 79 systems producing more than one TGF, bothduring the same overpass and up to four overpasses after. Data acquired by geostationary meteorologicalsatellites and cross correlation with radio sferics detected by World Wide Lightning Location Network areused to support this investigation. The AGILE satellite for the first time clearly establishes the multipleoccurrences of TGFs from convective thunderstorms, both on timescales of minutes to several hours.

Published
2016
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20. FLARES: A flexible scintillation light apparatus for rare event searches

Author

M. Sisti, G. Baldazzi, V. Bonvicini, R. Campana, S. Capelli, Y. Evangelista, M. Feroci, F. Fuschino, L. Gironi, C. Labanti, M. Marisaldi, E. Previtali, L. Rignanese, A. Rachevsky, A. Vacchi, G. Zampa, N. Zampa, M. Zuffa, Sisti, M, Baldazzi, Giuseppe, Bonvicini, V., Campana, Riccardo, Capelli, S., Evangelista, Y., Feroci, M., Fuschino, Fabio, Gironi, L., Labanti, C., Marisaldi, Martino, Previtali, E., Rignanese, LUIGI PIO, Rachevsky, A., Vacchi, A., Zampa, G., Zampa, N., Zuffa, M., Baldazzi, G, Bonvicini, V, Campana, R, Capelli, S, Evangelista, Y, Feroci, M, Fuschino, F, Gironi, L, Labanti, C, Marisaldi, M, Previtali, E, Rignanese, L, Rachevsky, A, Vacchi, A, Zampa, G, Zampa, N, and Zuffa, M

Subjects
Nuclear and High Energy Physics, 010308 nuclear & particles physics, Physics::Instrumentation and Detectors, Detector techniques for cosmology, Astroparticle and general physics, 01 natural sciences, Double beta decay, Scintillation detector, Silicon drift detectors, 0103 physical sciences, Astroparticle and general physic, Scintillation detectors, High Energy Physics::Experiment, 010306 general physics, Instrumentation, Silicon drift detector, Nuclear and High Energy Physic
Abstract

FLARES 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. The performances of a first production of matrices of Silicon Drift Detectors are presented and discussed in this paper.

Published
2016

21. Characterization of a tagged gamma-ray beam line at the DAPhNE Beam Test Facility

Author

P. W. Cattaneo, A. Argan, F. Boffelli, A. Bulgarelli, B. Buonomo, A. W. Chen, F. D'Ammando, L. Foggetta, T. Froysland, F. Fuschino, M. Galli, F. Gianotti, A. Giuliani, M. Marisaldi, G. Mazzitelli, A. Pellizzoni, M. Prest, G. Pucella, L. Quintieri, A. Rappoldi, M. Tavani, M. Trifoglio, A. Trois, P. Valente, E. Vallazza, S. Vercellone, A. Zambra, G. Barbiellini, P. Caraveo, V. Cocco, E. Costa, G. . Paris, E. . Monte, G. . Cocco, I. Donnarumma, Y. Evangelista, M. Feroci, A. Ferrari, M. Fiorini, C. Labanti, I. Lapshov, F. Lazzarotto, P. Lipari, M. Mastropietro, S. Mereghetti, E. Morelli, E. Moretti, A. Morselli, L. Pacciani, F. Perotti, G. Piano, P. Picozza, M. Pilia, G. Porrovecchio, M. Rapisarda, A. Rubini, S. Sabatini, P. Soffitta, E. Striani, V. Vittorini, D. Zanello, S. Colafrancesco, P. Giommi, C. Pittori, P. Santolamazza, F. Verrecchia, L. Salotti, LONGO, FRANCESCO, P. W., Cattaneo, A., Argan, F., Boffelli, A., Bulgarelli, B., Buonomo, A. W., Chen, F., D'Ammando, L., Foggetta, T., Froysland, F., Fuschino, M., Galli, F., Gianotti, A., Giuliani, Longo, Francesco, M., Marisaldi, G., Mazzitelli, A., Pellizzoni, M., Prest, G., Pucella, L., Quintieri, A., Rappoldi, M., Tavani, M., Trifoglio, A., Troi, P., Valente, E., Vallazza, S., Vercellone, A., Zambra, G., Barbiellini, P., Caraveo, V., Cocco, E., Costa, Paris, G., Monte, E., Cocco, G., I., Donnarumma, Y., Evangelista, M., Feroci, A., Ferrari, M., Fiorini, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, M., Mastropietro, S., Mereghetti, E., Morelli, E., Moretti, A., Morselli, L., Pacciani, F., Perotti, G., Piano, P., Picozza, M., Pilia, G., Porrovecchio, 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
MonteCarlo Simulations, Gamma-ray Satellites, Calibrations, Gamma-ray Satellites, Calibrations, MonteCarlo Simulations
Published
2012

22. The Extraordinary Gamma-Ray Flare Of The Blazar 3c 454.3

Author

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

Subjects
Agile, Cosmology and Nongalactic Astrophysics (astro-ph.CO), blazar, gamma detection, Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Astrophysics, Type (model theory), Vela, High Energy Gamma-ray Astronomy, AGILE satellite, Active Galactic Nuclei, law.invention, Pulsar, law, Blazar, Physics, gamma rays: galaxies – quasars: individual (3C 454.3), Gamma ray, Astronomy and Astrophysics, Quasar, Space and Planetary Science, Astrophysics - Cosmology and Nongalactic Astrophysics, Flare
Abstract

We present the gamma-ray data of the extraordinary flaring activity above 100 MeV from the flat spectrum radio quasar 3C 454.3 detected by AGILE during the month of December 2009. 3C 454.3, that has been among the most active blazars of the FSRQ type since 2007, was detected in the gamma-ray range with a progressively rising flux since November 10, 2009. The gamma-ray flux reached a value comparable with that of the Vela pulsar on December 2, 2009. Remarkably, between December 2 and 3, 2009 the source more than doubled its gamma-ray emission and became the brightest gamma-ray source in the sky with a peak flux of F_{\gamma,p} = (2000 \pm 400) x 10^-8 ph cm^-2 s^-1 for a 1-day integration above 100 MeV. The gamma-ray intensity decreased in the following days with the source flux remaining at large values near F \simeq (1000 \pm 200) x 10^-8 ph cm^-2 s^-1 for more than a week. This exceptional gamma-ray flare dissipated among the largest ever detected intrinsic radiated power in gamma-rays above 100 MeV (L_{\gamma, source, peak} \simeq 3 x 10^46 erg s^-1, for a relativistic Doppler factor of {\delta} \simeq 30). The total isotropic irradiated energy of the month-long episode in the range 100 MeV - 3 GeV is E_{\gamma,iso} \simeq 10^56 erg. We report the intensity and spectral evolution of the gamma-ray emission across the flaring episode. We briefly discuss the important theoretical implications of our detection., Comment: 17 pages, 3 figures, ApJ accepted

Published
2010

23. Enhanced detection of terrestrial gamma-ray flashes by AGILE

Author

M. Marisaldi, A. Argan, A. Ursi, T. Gjesteland, F. Fuschino, C. Labanti, M. Galli, M. Tavani, C. Pittori, F. Verrecchia, F. D'Amico, N. Østgaard, S. Mereghetti, R. Campana, P. W. Cattaneo, A. Bulgarelli, S. Colafrancesco, S. Dietrich, F. Longo, F. Gianotti, P. Giommi, A. Rappoldi, M. Trifoglio, A. Trois, Marisaldi, M., Argan, A., Ursi, A., Gjesteland, T., Fuschino, F., Labanti, C., Galli, M., Tavani, M., Pittori, C., Verrecchia, F., D'Amico, F., Ostgaard, N., Mereghetti, S., Campana, R., Cattaneo, P. W., Bulgarelli, A., Colafrancesco, S., Dietrich, S., Longo, F., Gianotti, F., Giommi, P., Rappoldi, A., Trifoglio, M., and Trois, A.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Solar Physics, Astrophysics, and Astronomy, Atmospheric Science, FOS: Physical sciences, terrestrial gamma-ray flashes, terrestrial gamma‐ray flashes, atmospheric electricity, TGF, Space Physics (physics.space-ph), Lightning, Research Letters, Physics - Space Physics, Atmospheric Processes, Research Letter, Matematikk og Naturvitenskap: 400 [VDP], Instruments and Techniques, AGILE TGF, Astrophysics - High Energy Astrophysical Phenomena
Abstract

At the end of March 2015 the onboard software configuration of the Astrorivelatore Gamma a Immagini Leggero (AGILE) satellite was modified in order to disable the veto signal of the anticoincidence shield for the minicalorimeter instrument. The motivation for such a change was the understanding that the dead time induced by the anticoincidence prevented the detection of a large fraction of Terrestrial Gamma‐Ray Flashes (TGFs). The configuration change was highly successful resulting in an increase of one order of magnitude in TGF detection rate. As expected, the largest fraction of the new events has short duration (, Key Points Tenfold improvement in TGF detection rate by AGILE is obtained after a major configuration changeThe sample is dead time‐free, with TGF durations as short as 20 μsThe relationship between TGF duration and likelihood of association with lightning is confirmed

Published
2015
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24. THE JUNE 2008 FLARE OF MARKARIAN 421 FROM OPTICAL TO TeV ENERGIES

Author

I. Donnarumma, V. Vittorini, S. Vercellone, E. Del Monte, M. Feroci, F. D'Ammando, L. Pacciani, A. W. Chen, M. Tavani, A. Bulgarelli, A. Giuliani, F. Longo, G. Pucella, A. Argan, G. Barbiellini, F. Boffelli, P. Caraveo, P. W. Cattaneo, V. Cocco, E. Costa, G. De Paris, G. Di Cocco, Y. Evangelista, M. Fiorini, T. Froysland, M. Frutti, F. Fuschino, M. Galli, F. Gianotti, C. Labanti, I. Lapshov, F. Lazzarotto, P. Lipari, M. Marisaldi, M. Mastropietro, S. Mereghetti, E. Morelli, A. Morselli, A. Pellizzoni, F. Perotti, P. Picozza, G. Porrovecchio, M. Prest, M. Rapisarda, A. Rappoldi, A. Rubini, P. Soffitta, M. Trifoglio, A. Trois, E. Vallazza, A. Zambra, D. Zanello, C. Pittori, P. Santolamazza, F. Verrecchia, P. Giommi, S. Colafrancesco, L. Salotti, M. Villata, C. M. Raiteri, W. P. Chen, N. V. Efimova, B. Jordan, T. S. Konstantinova, E. Koptelova, O. M. Kurtanidze, V. M. Larionov, J. A. Ros, A. C. Sadun, H. Anderhub, L. A. Antonelli, P. Antoranz, M. Backes, C. Baixeras, S. Balestra, J. A. Barrio, H. Bartko, D. Bastieri, J. Becerra González, J. K. Becker, W. Bednarek, K. Berger, E. Bernardini, A. Biland, R. K. Bock, G. Bonnoli, P. Bordas, D. Borla Tridon, V. Bosch-Ramon, T. Bretz, I. Britvitch, M. Camara, E. Carmona, A. Chilingarian, S. Commichau, J. L. Contreras, J. Cortina, M. T. Costado, S. Covino, V. Curtef, F. Dazzi, A. De Angelis, E. De Cea del Pozo, R. de los Reyes, B. De Lotto, M. De Maria, F. De Sabata, C. Delgado Mendez, A. Dominguez, D. Dorner, M. Doro, D. Elsaesser, M. Errando, D. Ferenc, E. Fernández, R. Firpo, M. V. Fonseca, L. Font, N. Galante, R. J. García López, M. Garczarczyk, M. Gaug, F. Goebel, D. Hadasch, M. Hayashida, A. Herrero, D. Höhne-Mönch, J. Hose, C. C. Hsu, S. Huber, T. Jogler, D. Kranich, A. La Barbera, A. Laille, E. Leonardo, E. Lindfors, S. Lombardi, M. López, E. Lorenz, P. Majumdar, G. Maneva, N. Mankuzhiyil, K. Mannheim, L. Maraschi, M. Mariotti, M. Martínez, D. Mazin, M. Meucci, M. Meyer, J. M. Miranda, R. Mirzoyan, J. Moldón, M. Moles, A. Moralejo, D. Nieto, K. Nilsson, J. Ninkovic, I. Oya, R. Paoletti, J. M. Paredes, M. Pasanen, D. Pascoli, F. Pauss, R. G. Pegna, M. A. Perez-Torres, M. Persic, L. Peruzzo, F. Prada, E. Prandini, N. Puchades, A. Raymers, W. Rhode, M. Ribó, J. Rico, M. Rissi, A. Robert, S. Rügamer, A. Saggion, T. Y. Saito, M. Salvati, M. Sanchez-Conde, P. Sartori, K. Satalecka, V. Scalzotto, V. Scapin, T. Schweizer, M. Shayduk, K. Shinozaki, S. N. Shore, N. Sidro, A. Sierpowska-Bartosik, A. Sillanpää, J. Sitarek, D. Sobczynska, F. Spanier, A. Stamerra, L. S. Stark, L. Takalo, F. Tavecchio, P. Temnikov, D. Tescaro, M. Teshima, M. Tluczykont, D. F. Torres, N. Turini, H. Vankov, A. Venturini, V. Vitale, R. M. Wagner, W. Wittek, V. Zabalza, F. Zandanel, R. Zanin, J. Zapatero, V. Acciari, E. Aliu, T. Arlen, M. Beilicke, W. Benbow, S. M. Bradbury, J. H. Buckley, V. Bugaev, Y. Butt, K. Byrum, A. Cannon, A. Cesarini, Y. C. Chow, L. Ciupik, P. Cogan, P. Colin, W. Cui, M. K. Daniel, R. Dickherber, C. Duke, T. Ergin, S. J. Fegan, J. P. Finley, G. Finnegan, P. Fortin, A. Furniss, D. Gall, G. H. Gillanders, R. Guenette, G. Gyuk, J. Grube, D. Hanna, J. Holder, D. Horan, C. M. Hui, T. Brian Humensky, A. Imran, P. Kaaret, N. Karlsson, M. Kertzman, D. Kieda, J. Kildea, A. Konopelko, H. Krawczynski, F. Krennrich, M. J. Lang, S. LeBohec, G. Maier, A. McCann, M. McCutcheon, A. Milovanovic, P. Moriarty, T. Nagai, R. A. Ong, A. N. Otte, D. Pandel, J. S. Perkins, A. Pichel, M. Pohl, K. Ragan, L. C. Reyes, P. T. Reynolds, E. Roache, H. J. Rose, M. Schroedter, G. H. Sembroski, A. W. Smith, D. Steele, S. P. Swordy, M. Theiling, J. A. Toner, L. Valcarcel, A. Varlotta, S. P. Wakely, J. E. Ward, T. C. Weekes, A. Weinstein, D. A. Williams, S. Wissel, M. Wood, B. Zitzer, I., Donnarumma, V., Vittorini, S., Vercellone, E. D., Monte, M., Feroci, F., D'Ammando, L., Pacciani, A. W., Chen, M., Tavani, A., Bulgarelli, A., Giuliani, Longo, Francesco, G., Pucella, A., Argan, G., Barbiellini, F., Boffelli, P., Caraveo, P. W., Cattaneo, V., Cocco, E., Costa, G. D., Pari, G. D., Cocco, Y., Evangelista, M., Fiorini, T., Froysland, M., Frutti, F., Fuschino, M., Galli, F., Gianotti, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, M., Marisaldi, M., Mastropietro, S., Mereghetti, E., Morelli, A., Morselli, A., Pellizzoni, F., Perotti, P., Picozza, G., Porrovecchio, M., Prest, M., Rapisarda, A., Rappoldi, A., Rubini, P., Soffitta, M., Trifoglio, A., Troi, E., Vallazza, A., Zambra, D., Zanello, C., Pittori, P., Santolamazza, F., Verrecchia, P., Giommi, S., Colafrancesco, L., Salotti, M., Villata, C. M., Raiteri, W. P., Chen, N. V., Efimova, B., Jordan, T. S., Konstantinova, E., Koptelova, O. M., Kurtanidze, V. M., Larionov, J. A., Ro, A. C., Sadun, H., Anderhub, L. A., Antonelli, P., Antoranz, M., Backe, C., Baixera, S., Balestra, J. A., Barrio, H., Bartko, D., Bastieri, J. B., Gonzalez, J. K., Becker, W., Bednarek, K., Berger, E., Bernardini, A., Biland, R. K., Bock, G., Bonnoli, P., Borda, D. B., Tridon, V., Bosch Ramon, T., Bretz, I., Britvitch, M., Camara, E., Carmona, A., Chilingarian, S., Commichau, J. L., Contrera, J., Cortina, M. T., Costado, S., Covino, V., Curtef, F., Dazzi, A. D., Angeli, E. D., Del Pozo, R. D., Reye, B. D., Lotto, M. D., Maria, F. D., Sabata, C. D., Mendez, A., Dominguez, D., Dorner, M., Doro, D., Elsaesser, M., Errando, D., Ferenc, E., Fernandez, R., Firpo, M. V., Fonseca, L., Font, N., Galante, R. J. G., Lopez, M., Garczarczyk, M., Gaug, F., Goebel, D., Hadasch, M., Hayashida, A., Herrero, D., Hohne Monch, J., Hose, C. C., Hsu, S., Huber, T., Jogler, D., Kranich, A. L., Barbera, A., Laille, E., Leonardo, E., Lindfor, S., Lombardi, M., Lopez, E., Lorenz, P., Majumdar, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, M., Mariotti, M., Martinez, D., Mazin, M., Meucci, M., Meyer, J. M., Miranda, R., Mirzoyan, J., Moldon, M., Mole, A., Moralejo, D., Nieto, K., Nilsson, J., Ninkovic, I., Oya, R., Paoletti, J. M., Parede, M., Pasanen, D., Pascoli, F., Pau, R. G., Pegna, M. A., Perez Torre, M., Persic, L., Peruzzo, F., Prada, E., Prandini, N., Puchade, A., Raymer, W., Rhode, M., Ribo, J., Rico, M., Rissi, A., Robert, S., Rugamer, A., Saggion, T. Y., Saito, M., Salvati, M., Sanchez Conde, P., Sartori, K., Satalecka, V., Scalzotto, V., Scapin, T., Schweizer, M., Shayduk, K., Shinozaki, S. N., Shore, N., Sidro, A., Sierpowska Bartosik, A., Sillanpaa, J., Sitarek, D., Sobczynska, F., Spanier, A., Stamerra, L. S., Stark, L., Takalo, F., Tavecchio, P., Temnikov, D., Tescaro, M., Teshima, M., Tluczykont, D. F., Torre, N., Turini, H., Vankov, A., Venturini, V., Vitale, R. M., Wagner, W., Wittek, V., Zabalza, F., Zandanel, R., Zanin, J., Zapatero, V., Acciari, E., Aliu, T., Arlen, M., Beilicke, W., Benbow, S. M., Bradbury, J. H., Buckley, V., Bugaev, Y., Butt, K., Byrum, A., Cannon, A., Cesarini, Y. C., Chow, L., Ciupik, P., Cogan, P., Colin, W., Cui, M. K., Daniel, R., Dickherber, C., Duke, T., Ergin, S. J., Fegan, J. P., Finley, G., Finnegan, P., Fortin, A., Furni, D., Gall, G. H., Gillander, R., Guenette, G., Gyuk, J., Grube, D., Hanna, J., Holder, D., Horan, C. M., Hui, T. B., Humensky, A., Imran, P., Kaaret, N., Karlsson, M., Kertzman, D., Kieda, J., Kildea, A., Konopelko, H., Krawczynski, F., Krennrich, M. J., Lang, S., Lebohec, G., Maier, A., Mccann, M., Mccutcheon, A., Milovanovic, P., Moriarty, T., Nagai, R. A., Ong, A. N., Otte, D., Pandel, J. S., Perkin, A., Pichel, M., Pohl, K., Ragan, L. C., Reye, P. T., Reynold, E., Roache, H. J., Rose, M., Schroedter, G. H., Sembroski, A. W., Smith, D., Steele, S. P., Swordy, M., Theiling, J. A., Toner, L., Valcarcel, A., Varlotta, S. P., Wakely, J. E., Ward, T. C., Weeke, A., Weinstein, D. A., William, S., Wissel, M., Wood, B., Zitzer, Donnarumma I, Vittorini V, Vercellone S, del Monte E, Feroci M, DAmmando F, Pacciani L, Chen A W, Tavani M, Bulgarelli A, Giuliani A, Longo F, Pucella G, Argan A, Barbiellini G, Boffelli F, Caraveo P, Cattaneo P W, Cocco V, Costa E, DeParis G, Di Cocco G, Evangelista Y, Fiorini M, Froysland T, Frutti M, Fuschino F, Galli M, Gianotti F, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Marisaldi M, Mastropietro M, Mereghetti S, Morelli E, Morselli A, Pellizzoni A, Perotti F, Picozza P, Porrovecchio G, Prest M, Rapisarda M, Rappoldi A, Rubini A, Soffitta P, Trifoglio M, Trois A, Vallazza E, Zambra A, Zanello D, Pittori C, Santolamazza P, Verrecchia F, Giommi P, Colafrancesco S, Salotti L, Villata M, Raiteri C M, Chen W P, Efimova N V, Jordan B, Konstantinova T S, Koptelova E, Kurtanidze O M, Larionov V M, Ros J A, Sadun A C, Anderhub H, Antonelli L A, Antoranz P, Backes M, Baixeras C, Balestra S, Barrio J A, Bartko H, Bastieri D, González J Becerra, Becker J K, Bednarek W, Berger K, Bernardini E, Biland A, Bock R K, Bonnoli G, Bordas P, Tridon D Borla, Bosch-Ramon V, Bretz T, Britvitch I, Camara M, Carmona E, Chilingarian A, Commichau S, Contreras J L, Cortina J, Costado M T, Covino S, Curtef V, Dazzi F, DeAngelis A, DeCea del Pozo E, de los Reyes R, DeLotto B, DeMaria M, DeSabata F, Mendez C Delgado, Dominguez A, Dorner D, Doro M, Elsaesser D, Errando M, Ferenc D, Fernández E, Firpo R, Fonseca M V, Font L, Galante N, García López R J, Garczarczyk M, Gaug M, Goebel F, Hadasch D, Hayashida M, Herrero A, Höhne-Mönch D, Hose J, Hsu C C, Huber S, Jogler T, Kranich D, La Barbera A, Laille A, Leonardo E, Lindfors E, Lombardi S, López M, Lorenz E, Majumdar P, Maneva G, Mankuzhiyil N, Mannheim K, Maraschi L, Mariotti M, Martínez M, Mazin D, Meucci M, Meyer M, Miranda J M, Mirzoyan R, Moldón J, Moles M, Moralejo A, Nieto D, Nilsson K, Ninkovic J, Oya I, Paoletti R, Paredes J M, Pasanen M, Pascoli D, Pauss F, Pegna R G, Perez-Torres M A, Persic M, Peruzzo L, Prada F, Prandini E, Puchades N, Raymers A, Rhode W, Ribó M, Rico J, Rissi M, Robert A, Rügamer S, Saggion A, Saito T Y, Salvati M, Sanchez-Conde M, Sartori P, Satalecka K, Scalzotto V, Scapin V, Schweizer T, Shayduk M, Shinozaki K, Shore S N, Sidro N, Sierpowska-Bartosik A, Sillanpää A, Sitarek J, Sobczynska D, Spanier F, Stamerra A, Stark L S, Takalo L, Tavecchio F, Temnikov P, Tescaro D, Teshima M, Tluczykont M, Torres D F, Turini N, Vankov H, Venturini A, Vitale V, Wagner R M, Wittek W, Zabalza V, Zandanel F, Zanin R, Zapatero J, Acciari V, Aliu E, Arlen T, Beilicke M, Benbow W, Bradbury S M, Buckley J H, Bugaev V, Butt Y, Byrum K, Cannon A, Cesarini A, Chow Y C, Ciupik L, Cogan P, Colin P, Cui W, Daniel M K, Dickherber R, Duke C, Ergin T, Fegan S J, Finley J P, Finnegan G, Fortin P, Furniss A, Gall D, Gillanders G H, Guenette R, Gyuk G, Grube J, Hanna D, Holder J, Horan D, Hui C M, Humensky T Brian, Imran A, Kaaret P, Karlsson N, Kertzman M, Kieda D, Kildea J, Konopelko A, Krawczynski H, Krennrich F, Lang M J, LeBohec S, Maier G, McCann A, McCutcheon M, Milovanovic A, Moriarty P, Nagai T, Ong R A, Otte A N, Pandel D, Perkins J S, Pichel A, Pohl M, Ragan K, Reyes L C, Reynolds P T, Roache E, Rose H J, Schroedter M, Sembroski G H, Smith A W, Steele D, Swordy S P, Theiling M, Toner J A, Valcarcel L, Varlotta A, Wakely S P, Ward J E, Weekes T C, Weinstein A, Williams D A, Wissel S, Wood M, and Zitzer B

Subjects
campaign, Raigs còsmics, BL Lacertae: individual: Mrk421, galaxies: jets, X-Rays: Galaxies, gamma rays: observations, radiation mechanisms: nonthermal, bl-lacertae objects, blazars, Flux, Astrophysics, 01 natural sciences, 7. Clean energy, High Energy Gamma-ray Astronomy, law.invention, Raigs gamma, law, optical, MAGIC (telescope), Agile, blazr, X-ray, gamma, high energy observation, 010303 astronomy & astrophysics, webt, Physics, x-ray-spectra, Astrophysics (astro-ph), gamma-rays, lac objects, xmm-newton, Spectral energy distribution, Electrónica, Física nuclear, Raigs X, Electricidad, Flare, outburst, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, 0103 physical sciences, X-rays, BL Lacertae objects: individual (Mrk 421) – gamma rays: observations – galaxies: jets – radiation mechanisms: non-thermal – X-rays: galaxies, Blazar, Cosmic rays, 010308 nuclear & particles physics, Gamma rays, Astronomy and Astrophysics, Active Galactic Nuclei, radiation mechanisms: non-thermal, Light curve, Galaxies, Galàxies, MAGIC telescope, Space and Planetary Science, Very High Energy Gamma-ray Astronomy, ddc:520, AGILE satellite, bl lacertae objects: individual (mrk 421), Energy (signal processing), Lepton
Abstract

We present optical, X-ray, high energy ($\lessapprox 30$ GeV) and very high energy ($\gtrapprox 100$ GeV; VHE) observations of the high-frequency peaked blazar Mrk 421 taken between 2008 May 24 and June 23. A high energy $\gamma$-ray signal was detected by AGILE with \sqrt{TS}=4.5 on June 9--15, with $F(E>100 \mathrm{MeV})= 42^{+14}_{-12}\times 10^{-8}$ photons cm$^{-2}$ s$^{-1}$. This flaring state is brighter than the average flux observed by EGRET by a factor of $\sim$3, but still consistent with the highest EGRET flux. In hard X-rays (20-60 keV) SuperAGILE resolved a 5-day flare (June 9-15) peaking at $\sim$ 55 mCrab. SuperAGILE, RXTE/ASM and Swift/BAT data show a correlated flaring structure between soft and hard X-rays. Hints of the same flaring behavior are also detected in the simultaneous optical data provided by the GASP-WEBT. A Swift/XRT observation near the flaring maximum revealed the highest 2-10 keV flux ever observed from this source, of 2.6 $\times 10^{-9}$ erg cm$^{-2}$ s$^{-1}$ (i.e. > 100 mCrab). A peak synchrotron energy of $\sim$3 keV was derived, higher than typical values of $\sim$0.5-1 keV. VHE observations with MAGIC and VERITAS on June 6-8 show the flux peaking in a bright state, well correlated with the X-rays. This extraordinary set of simultaneous data, covering a twelve-decade spectral range, allowed for a deep analysis of the spectral energy distribution as well as of correlated light curves. The $\gamma$-ray flare can be interpreted within the framework of the synchrotron self-Compton model in terms of a rapid acceleration of leptons in the jet., Comment: accepted for publication in ApJL, 7 pages, 2 figures, 1 table

Published
2009
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25. Multiwavelength Observations Of 3c 454.3. Ii. The Agile 2007 December Campaign

Author

I. Donnarumma, G. Pucella, V. Vittorini, F. D'Ammando, S. Vercellone, C. M. Raiteri, M. Villata, M. Perri, W. P. Chen, R. L. Smart, J. Kataoka, N. Kawai, Y. Mori, G. Tosti, D. Impiombato, T. Takahashi, R. Sato, M. Tavani, A. Bulgarelli, A. W. Chen, A. Giuliani, F. Longo, L. Pacciani, A. Argan, G. Barbiellini, F. Boffelli, P. Caraveo, P. W. Cattaneo, V. Cocco, T. Contessi, E. Costa, E. Del Monte, G. De Paris, G. Di Cocco, Y. Evangelista, M. Feroci, A. Ferrari, M. Fiorini, T. Froysland, M. Frutti, F. Fuschino, M. Galli, F. Gianotti, C. Labanti, I. Lapshov, F. Lazzarotto, P. Lipari, M. Marisaldi, M. Mastropietro, S. Mereghetti, E. Morelli, 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, E. Scalise, P. Soffitta, E. Striani, M. Trifoglio, A. Trois, E. Vallazza, A. Zambra, D. Zanello, C. Pittori, P. Santolamazza, F. Verrecchia, P. Giommi, L. A. Antonelli, S. Colafrancesco, L. Salotti, Donnarumma I, Pucella G, Vittorini V, DAmmando F, Vercellone S, Raiteri CM, Villata M, Perri M, Chen WP, Smart RL, Kataoka J, Kawai N, Mori Y, Tosti G, Impiombato D, Takahashi T, Sato R, Tavani M, Bulgarelli A, Chen AW, Giuliani A, Longo F, Pacciani L, Argan A, Barbiellini G, Boffelli F, Caraveo P, Cattaneo PW, Cocco V, Contessi T, Costa E, Del Monte E, De Paris G, Di Cocco G, Evangelista Y, Feroci M, Ferrari A, Fiorini M, Froysland T, Frutti M, Fuschino F, Galli M, Gianotti F, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Marisaldi M, Mastropietro M, Mereghetti S, Morelli E, 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, Scalise E, Soffitta P, Striani E, Trifoglio M, Trois A, Vallazza E, Zambra A, Zanello D, Pittori C, Santolamazza P, Verrecchia F, Giommi P, Antonelli A, Colafrancesco S, Salotti L, I., Donnarumma, G., Pucella, V., Vittorini, F., D'Ammando, S., Vercellone, C. M., Raiteri, M., Villata, M., Perri, W. P., Chen, R. L., Smart, J., Kataoka, N., Kawai, Y., Mori, G., Tosti, D., Impiombato, T., Takahashi, R., Sato, 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, T., Contessi, E., Costa, E. D., Monte, G. D., Pari, G. D., Cocco, Y., Evangelista, M., Feroci, A., Ferrari, M., Fiorini, T., Froysland, M., Frutti, F., Fuschino, M., Galli, F., Gianotti, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, M., Marisaldi, M., Mastropietro, S., Mereghetti, E., Morelli, 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, E., Scalise, P., Soffitta, E., Striani, M., Trifoglio, A., Troi, E., Vallazza, A., Zambra, D., Zanello, C., Pittori, P., Santolamazza, F., Verrecchia, P., Giommi, A., Antonelli, S., Colafrancesco, and L., Salotti

Subjects
Agile, Photon, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Flux, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, High Energy Gamma-ray Astronomy, AGILE satellite, Active Galactic Nuclei, blazar, law.invention, law, Target of opportunity, quasars: general, multiwavelength campaign, Blazar, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), We report on the second Astrorivelatore Gamma a Immagini Leggero (AGILE) multiwavelength campaign of the blazar 3C 454.3 during the first half of 2007 December. This campaign involved AGILE, Spitzer, Swift, Suzaku, the Whole Earth Blazar Telescope (WEBT) consortium, the Rapid Eye Mount (REM), and the Multicolor Imaging Telescopes for Survey and Monstrous Explosions (MITSuME) telescopes, offering a broadband coverage that allowed for a simultaneous sampling of the synchrotron and inverse Compton (IC) emissions. The two-week AGILE monitoring was accompanied by radio to optical monitoring by WEBT and REM, and by sparse observations in mid-infrared and soft/hard X-ray energy bands performed by means of Target of Opportunity observations by Spitzer, Swift, and Suzaku, respectively. The source was detected with an average flux of ~250 × 10^-8 photons cm^-2 s^-1 above 100 MeV, typical of its flaring states. The simultaneous optical and γ-ray monitoring allowed us to study the time lag associated with the variability in the two energy bands, resulting in a possible lsimone-day delay of the γ-ray emission with respect to the optical one. From the simultaneous optical and γ-ray fast flare detected on December 12, we can constrain the delay between the γ-ray and optical emissions within 12 hr. Moreover, we obtain three spectral energy distributions (SEDs) with simultaneous data for 2007 December 5, 13, and 15, characterized by the widest multifrequency coverage. We found that a model with an external Compton on seed photons by a standard disk and reprocessed by the broad-line regions does not describe in a satisfactory way the SEDs of 2007 December 5, 13, and 15. An additional contribution, possibly from the hot corona with T = 106 K surrounding the jet, is required to account simultaneously for the softness of the synchrotron and the hardness of the IC emissions during those epochs, Astronomy and Astrophysics, galaxies: jets, radiation mechanisms: non-thermal, Corona, Synchrotron, Space and Planetary Science, galaxies: individual: 3C 454.3, Astrophysics - High Energy Astrophysical Phenomena, gamma rays: observations, Astrophysics - Cosmology and Nongalactic Astrophysics, Flare
Abstract

著者人数：79名, Accepted: 2009-10-29, 資料番号: SA1000754000

Published
2009

26. The X-Ray Spectroscopic Performance of a Very Large Area Silicon Drift Detector

Author

G. Zampa, R. Campana, 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, E. Costa, I. Donnarumma, M. Grassi, F. Lazzarotto, P. Malcovati, M. Mastropietro, E. Morelli, L. Picolli, BALDAZZI, GIUSEPPE, G. Zampa, R. Campana, 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, Silicon drift detector, Silicon, Square Centimeter, business.industry, Physics::Instrumentation and Detectors, Detector, X-ray detector, chemistry.chemical_element, X-RAY SPECTROSCOPY, ROOM TEMPERATURE, Noise (electronics), Nuclear Energy and Engineering, chemistry, Optoelectronics, Electrical and Electronic Engineering, Square Millimeter, business, Spectroscopy, SILICON DRIFT DETECTORS
Abstract

Silicon drift detectors (SDDs), due to their collection electrode geometry, have excellent noise performance and are well suited for low-energy X-ray spectroscopy applications. On the other hand these detectors, when dedicated to low energy X-ray spectroscopy, have a small sensitive area (from few square millimeters up to one square centimeter) to reduce the leakage current and its impact on the energy resolution. Because of this limitation they are rarely used in applications where large sensitive surfaces are required. We present the characterization of the spectroscopic performance of a very large sensitive area SDD (about 53 cm2) that has been realized in the frame of the LHC-ALICE experiment. We studied the energy resolution of the detector analyzing its dependence on both biasing conditions and temperature to evaluate the contribution of the different noise sources exploiting their relation with the shaping time. The experimental results obtained with 241 Am and 55 Fe sources show that the goal of a high energy resolution combined with large sensitive areas can be achieved.

Published
2009

27. Properties of terrestrial gamma ray flashes detected by AGILE MCAL below 30\u2009MeV

Author

M. Marisaldi, F. Fuschino, M. Tavani, S. Dietrich, C. Price, M. Galli, C. Pittori, F. Verrecchia, S. Mereghetti, P. W. Cattaneo, S. Colafrancesco, A. Argan, C. Labanti, F. Longo, E. Del Monte, G. Barbiellini, A. Giuliani, A. Bulgarelli, R. Campana, A. Chen, F. Gianotti, P. Giommi, F. Lazzarotto, A. Morselli, M. Rapisarda, A. Rappoldi, M. Trifoglio, A. Trois, and S. Vercellone

Published
2014

28. Science with the new generation high energy gamma- ray experiments

Author

Alvarez, M., D'Armiento, D., Agnetta, G., Alberdi, A., Antonelli, A., Argan, A., Assis, P., Baltz, E. A., Bambi, C., Barbiellini, G., Bartko, H., Basset, M., Bastieri, D., Belli, P., Benford, G., Bergstrom, L., Bernabei, R., Bertone, G., Biland, A., Biondo, B., Bocchino, F., Brigida, M., Bringmann, T., Brogueira, P., Bulgarelli, A., Caballero, J. A., Caliandro, G. A., Camarri, P., Cappella, F., Caraveo, P., Carbone, R., Carvajal, M., Casanova, S., Castro Tirado, A. J. , Catalano, O. , Catena, R. , Celi, F. , Celotti, A. , Cerulli, R. , Chen, A. , Clay, R. , Cocco, V. , Conrad, J. , Costa, E. , Cuoco, A. , Cusumano, G. , Dai, C. J. , Dawson, De Lotto, De Paris, de Ugarte Postigo, Del Monte, E. , Delgado, Di Ciaccio, Di Cocco, Di Falco, Di Persio, G. , Dingus, B. L. , Dominguez, A. , Donato, F. , Donnarumma, I. , Doro, M. , Edsjo, Espino Navas, J. M., Espirito Santo, M. C. , Evangelista, Y. , Evoli, C. , Fargion, D. , Favuzzi, C. , Feroci, M. , Fiorini, M. , Foggetta, L. , Fornengo, N. , Froysland, T. , Frutti, M. , Fuschino, F. , Gomez, J. L. , Gomez, M. , Gaggero, D. , Galante, N. , Gallardo, M. I. , Galli, M. , Garcia, J. E. , Garczarczyk, M. , Gargano, F. , Gaug, M. , Gianotti, F. , Giarrusso, S. , Giebels, B. , Giglietto, N. , Giommi, P. , Giordano, F. , Giuliani, A. , Glicenstein, J. , Goncalves, P. , Grasso, D. , Guerriero, M. , He, H. L. , Incicchitti, A. , Kirk, J. , Kuang, H. H., La Barbera, La Rosa, G. , Labanti, C. , Lamanna, G. , Lapshov, I. , Lazzarotto, F. , Liberati, S. , Liello, F. , Lipari, P. , Longo, F. , Loparco, F. , Lozano, Lucentini De Sanctis, P. G. , Ma, J. M. , Maccarone, M. C. , Maccione, L. , Malvezzi, V. , Mangano, A. , Mariotti, M. , Marisaldi, M. , Martel, I. , Masiero, A. , Massaro, E. , Mastropietro, M. , Mattaini, E. , Mauri, F. , Mazziotta, M. N. , Mereghetti, S. , Mineo, T. , Mizobuchi, S. , Moiseev, A. , Moles, M. , Monte, C. , Montecchia, F. , Morelli, E. , Morselli, A. , Moskalenko, I. , Nozzoli, F. , Ormes, J. F., Peres Torres, M. A. , Pacciani, L. , Pellizzoni, Perez Bernal, F. , Perotti, F. , Picozza, P. , Pieri, L. , Pietroni, M. , Pimenta, M. , Pina, A. , Pittori, C. , Pontoni, C. , Porrovecchio, G. , Prada, F. , Prest, M. , Prosperi, D. , Protheroe, R. , Pucella, G. , Quesada, J. M. , Quintana, J. M. , Quintero, J. R. , Raino, S. , Rapisarda, M. , Rissi, M. , Rodriguez, J. , Rossi, E. , Rowell, G. , Rubini, A. , Russo, Sanchez Conde, M. , Sacco, B. , Scapin, V. , Schelke, M. , Segreto, A. , Sellerholm, A. , Sheng, X. D. , Smith, A. , Soffitta, P. , Sparvoli, R. , Spinelli, P. , Stamatescu, V. , Stark, L. S. , Tavani, M. , Thornton, G. , Titarchuk, L. G. , Tome, B. , Traci, A. , Trifoglio, M. , Trois, A. , Vallania, P. , Vallazza, E. , Vercellone, S. , Vernetto, S. , Vitale, V. , Wild, N. , Ye, Z. P. , Zambra, A. , Zandanel, F. , Zanello, BRANCHINI, ENZO FRANCO, A.Lionetto, A.Morselli, Alvarez, M., D'Armiento, D., Agnetta, G., Alberdi, A., Antonelli, A., Argan, A., Assis, P., Baltz, E. A., Bambi, C., Barbiellini, G., Bartko, H., Basset, M., Bastieri, D., Belli, P., Benford, G., Bergstrom, L., Bernabei, R., Bertone, G., Biland, A., Biondo, B., Bocchino, F., Branchini, ENZO FRANCO, Brigida, M., Bringmann, T., Brogueira, P., Bulgarelli, A., Caballero, J. A., Caliandro, G. A., Camarri, P., Cappella, F., Caraveo, P., Carbone, R., Carvajal, M., Casanova, S., Castro, Tirado, A. J., Catalano, O., Catena, R., Celi, F., Celotti, A., Cerulli, R., Chen, A., Clay, R., Cocco, V., Conrad, J., Costa, E., Cuoco, A., Cusumano, G., Dai, C. J., Dawson, De, Lotto, De, Pari, de Ugarte, Postigo, Del, Monte, E., Delgado, Di, Ciaccio, Di, Cocco, Di, Falco, Di, Persio, G., Dingu, B. L., Dominguez, A., Donato, F., Donnarumma, I., Doro, M., Edsjo, Espino, Nava, J., M., Espirito, Santo, M. C., Evangelista, Y., Evoli, C., Fargion, D., Favuzzi, C., Feroci, M., Fiorini, M., Foggetta, L., Fornengo, N., Froysland, T., Frutti, M., Fuschino, F., Gomez, J. L., Gomez, M., Gaggero, D., Galante, N., Gallardo, M. I., Galli, M., Garcia, J. E., Garczarczyk, M., Gargano, F., Gaug, M., Gianotti, F., Giarrusso, S., Giebel, B., Giglietto, N., Giommi, P., Giordano, F., Giuliani, A., Glicenstein, J., Goncalve, P., Grasso, D., Guerriero, M., He, H. L., Incicchitti, A., Kirk, J., Kuang, H., H., La, Barbera, La, Rosa, G., Labanti, C., Lamanna, G., Lapshov, I., Lazzarotto, F., Liberati, S., Liello, F., Lipari, P., Longo, F., Loparco, F., Lozano, Lucentini De, Sancti, P. G., Ma, J. M., Maccarone, M. C., Maccione, L., Malvezzi, V., Mangano, A., Mariotti, M., Marisaldi, M., Martel, I., Masiero, A., Massaro, E., Mastropietro, M., Mattaini, E., Mauri, F., Mazziotta, M. N., Mereghetti, S., Mineo, T., Mizobuchi, S., Moiseev, A., Mole, M., Monte, C., Montecchia, F., Morelli, E., Morselli, A., Moskalenko, I., Nozzoli, F., Orme, J., F., Peres, Torre, M. A., Pacciani, L., Pellizzoni, Perez, Bernal, F., Perotti, F., Picozza, P., Pieri, L., Pietroni, M., Pimenta, M., Pina, A., Pittori, C., Pontoni, C., Porrovecchio, G., Prada, F., Prest, M., Prosperi, D., Protheroe, R., Pucella, G., Quesada, J. M., Quintana, J. M., Quintero, J. R., Raino, S., Rapisarda, M., Rissi, M., Rodriguez, J., Rossi, E., Rowell, G., Rubini, A., Russo, Sanchez, Conde, M., Sacco, B., Scapin, V., Schelke, M., Segreto, A., Sellerholm, A., Sheng, X. D., Smith, A., Soffitta, P., Sparvoli, R., Spinelli, P., Stamatescu, V., Stark, L. S., Tavani, M., Thornton, G., Titarchuk, L. G., Tome, B., Traci, A., Trifoglio, M., Troi, A., Vallania, P., Vallazza, E., Vercellone, S., Vernetto, S., Vitale, V., Wild, N., Ye, Z. P., Zambra, A., Zandanel, and F., Zanello

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, General Relativity and Quantum Cosmology, dark matter, Space Physics (physics.space-ph), High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Physics - Space Physics, gamma ray astronomy
Abstract

This Conference is the fifth of a series of Workshops on High Energy Gamma- ray Experiments, following the Conferences held in Perugia 2003, Bari 2004, Cividale del Friuli 2005, Elba Island 2006. This year the focus was on the use of gamma-ray to study the Dark Matter component of the Universe, the origin and propagation of Cosmic Rays, Extra Large Spatial Dimensions and Tests of Lorentz Invariance., Comment: 328 pages, 7.8Mb, Proceedings of the 5th SCINEGHE Workshop, June 18-20, 2007 http://www.roma2.infn.it/SciNeGHE07/

Published
2007
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29. The observation of GRBs with AGILE and the interesting cases of GRB 090618 and GRB 100724B

Author

E. Del Monte, G. Barbiellini, F. Fuschino, A. Giuliani, F. Longo, M. Marisaldi, E. Moretti, M. Trifoglio, A. Argan, A. Bulgarelli, P. Caraveo, P. W. Cattaneo, A. Chen, E. Costa, G. Di Cocco, I. Donnarumma, Y. Evangelista, M. Feroci, M. Galli, F. Gianotti, C. Labanti, I. Lapshov, F. Lazzarotto, P. Lipari, S. Mereghetti, A. Morselli, L. Pacciani, A. Pellizzoni, F. Perotti, P. Picozza, M. Pilia, M. Prest, G. Pucella, M. Rapisarda, A. Rappoldi, P. Soffitta, M. Tavani, A. Trois, E. Vallazza, S. Vercellone, V. Vittorini, C. Pittori, L. Salotti, J. E. McEnery, J. L. Racusin, and N. Gehrels

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Delayed onset, Gamma ray, Astronomy, Spectral analysis, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Gamma-ray burst, Redshift
Abstract

The AGILE satellite, in orbit since 2007, is localizing about 0.5 GRBs per month with the hard X‐ray imager SuperAGILE (18–60 keV) and is detecting around 1 GRB per week with the non‐imaging Minicalorimeter (0.35–100 MeV). Up to now the AGILE Gamma Ray Imaging Detector firmly detected four GRBs in the energy band between 20 MeV and few GeV. In this presentation we review the status of the GRBs observation with AGILE, we discuss the upper limits in the gamma‐ray band of the non‐detected events and we show some interesting bursts, especially GRB 090618 (bright in soft and hard‐X rays, optical and radio but lacking GeV emission) and GRB 100724B (with a bright GeV emission simultaneous to hard‐X rays without delayed onset).

Published
2011
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30. The Third Interplanetary Network

Author

K. Hurley, S. Golenetskii, R. Aptekar, E. Mazets, V. Pal’shin, D. Frederiks, I. G. Mitrofanov, D. Golovin, A. Kozyrev, M. Litvak, A. B. Sanin, W. Boynton, C. Fellows, K. Harshman, R. Starr, A. von Kienlin, A. Rau, K. Yamaoka, M. Ohno, Y. Fukazawa, T. Takahashi, M. Tashiro, Y. Terada, T. Murakami, K. Makishima, S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, T. Cline, J. Goldsten, E. Del Monte, M. Feroci, M. Marisaldi, M. Briggs, V. Connaughton, C. Meegan, D. M. Smith, C. Wigger, W. Hajdas, J. E. McEnery, and J. L. Racusin

Published
2011
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31. A concept for a lightweight, low-power and sensitive silicon-based all sky monitor for transient sources and gamma ray bursts

Author

R. Campana, L. Pacciani, M. Feroci, E. Costa, E. Del Monte, I. Donnarumma, Y. Evangelista, F. Lazzarotto, M. Mastropietro, F. Muleri, A. Rubini, M. Rapisarda, L. Amati, F. Fuschino, C. Labanti, M. Marisaldi, M. Orlandini, F. Perotti, V. Bonvicini, A. Rashevsky, A. Vacchi, G. Zampa, N. Zampa, L. A. Antonelli, F. Fiore, G. L. Israel, F. Nicastro, A. Comastri, L. Angelini, and M. Cappi

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Antenna aperture, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Steradian, Field of view, Astrophysics, Physics and Astronomy (all), Sky, Instrumentation:detectors, X-rays:general, Angular resolution, Transient (oscillation), Gamma-ray burst, media_common
Abstract

We present a concept for a coded‐mask All Sky Monitor based on Silicon Drift Detectors. The current design has a high level of readiness, minimizes the total weight ( 2 steradians and an on‐axis sensitivity of ∼3 mCrab (5σ, 50 ks). The intrinsic modularity of the detector allows to envisage experiments with different configurations, in terms of field of view, angular resolution or effective area. We show the expected scientific performances of such an experiment, with emphasis on the observations of X‐ray Galactic transients and gamma‐ray bursts.

Published
2010

32. The Status and Future of the Third Interplanetary Network

Author

K. Hurley, T. Cline, I. G. Mitrofanov, D. Golovin, M. L. Litvak, A. B. Sanin, W. Boynton, C. Fellows, K. Harshman, R. Starr, S. Golenetskii, R. Aptekar, E. Mazets, V. Pal’shin, D. Frederiks, D. M. Smith, C. Wigger, W. Hajdas, A. Zehnder, A. von Kienlin, G. G. Lichti, A. Rau, K. Yamaoka, M. Ohno, Y. Fukazawa, T. Takahashi, M. Tashiro, Y. Terada, T. Murakami, K. Makishima, S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, J. Goldsten, E. Del Monte, M. Feroci, M. Marisaldi, Charles Meegan, Chryssa Kouveliotou, Neil Gehrels, Meagan, Charles, Kouveliotou, Chryssa, and Gehrels, Neil

Subjects
Physics, Earth's orbit, COSMIC cancer database, Spacecraft, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Cosmic ray, Astrophysics, Mars Exploration Program, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Interplanetary spaceflight, business, Gamma-ray burst, Fermi Gamma-ray Space Telescope
Abstract

The 3rd interplanetary network (IPN), which has been in operation since 1990, presently consists of 9 spacecraft: AGILE, RHESSI, Suzaku, and Swift, in low Earth orbit; INTEGRAL, in eccentric Earth orbit with apogee 0.5 light‐seconds; Wind, up to ∼7 light‐seconds from Earth; MESSENGER, en route to Mercury; and Mars Odyssey, in orbit around Mars. Ulysses and HETE have ceased operations, and the Fermi GBM is being incorporated into the network. The IPN operates as a full‐time, all‐sky monitor for transients down to a threshold of about 6 × 10^(−7) erg cm^(−2) or 1 photon cm^(−2) s^(−1). It detects about 275 cosmic gamma‐ray bursts per year. These events are generally not the same ones detected by narrower field of view imaging instruments such as Swift, INTEGRAL IBIS, and SuperAGILE; the localization accuracy is in the several arcminute and above range.

Published
2009

33. AGILE View of TGFs

Author

F. Fuschino, F. Longo, M. Marisaldi, C. Labanti, M. Galli, A. Bulgarelli, F. Gianotti, M. Trifoglio, G. Di Cocco, A. Argan, G. Barbiellini, M. Basset, F. Boffelli, P. Caraveo, P. W. Cattaneo, A. W. Chen, V. Cocco, E. Costa, F. D’Ammando, E. Del Monte, G. De Paris, G. Di Persio, I. Donnarumma, Y. Evangelista, M. Feroci, A. Ferrari, M. Fiorini, L. Foggetta, T. Froysland, M. Frutti, A. Giuliani, I. Lapshov, F. Lazzarotto, F. Liello, P. Lipari, M. Mastropietro, E. Mattaini, F. Mauri, S. Mereghetti, A. Morselli, E. Moretti, L. Pacciani, A. Pellizzoni, F. Perotti, P. Picozza, C. Pontoni, G. Porrovecchio, M. Prest, G. Pucella, M. Rapisarda, A. Rappoldi, A. Rubini, P. Soffitta, M. Tavani, A. Trois, E. Vallazza, S. Vercellone, V. Vittorini, A. Zambra, D. Zanello, C. Pittori, F. Verrecchia, S. Cutini, D. Gasparrini, G. Fanari, B. Preger, P. Santolamazza, P. Giommi, L. A. Antonelli, S. Colafrancesco, L. Salotti, Norma B. Crosby, Tai-Yin Huang, and Michael J. Rycroft

Subjects
Physics, COSMIC cancer database, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Astronomy, Astrophysics, Lightning, Sky, Observatory, Thunderstorm, Satellite, Gamma-ray burst, media_common
Abstract

The AGILE Satellite [8] [9], launched the 23rd April 2007, is an italian mission devoted to high energy gamma‐ray astrophysics in the 30 MeV–50 GeV range, with a window in the hard‐X domain 18–60 keV. One of the on‐board detectors, the Mini‐Calorimeter (MCAL), was also designed to work as all sky transient monitor in the energy range 0.33–100 MeV. Though the main purpose of MCAL is the detection of cosmological Gamma‐Ray‐Bursts (GRB), MCAL detected transient events with a very brief duration, few msec, that does not match timing and spectral features of known cosmic GRB. These events more likely agree with the features of typical Terrestrial Gamma‐Ray Flashes as described in the literature and previously detected by the BATSE instrument onboard the Compton Gamma Ray Observatory and the RHESSI satellite. The characteristics of the detected TGF candidate events, as well as their geographical distribution will be presented and discussed.

Published
2009
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34. A Light and Effective Wide Field Monitor for Gamma Ray Bursts and Transient Sources

Author

M. Feroci, L. Amati, L. A. Antonelli, V. Bonvicini, R. Campana, E. Costa, E. Del Monte, I. Donnarumma, Y. Evangelista, F. Fiore, F. Fuschino, G. L. Israel, C. Labanti, I. Lapshov, F. Lazzarotto, M. Marisaldi, M. Mastropietro, E. Morelli, F. Muleri, F. Nicastro, M. Orlandini, L. Pacciani, F. Perotti, M. Rapisarda, A. Rashevsky, A. Rubini, P. Soffitta, A. Vacchi, G. Zampa, N. Zampa, Charles Meegan, Chryssa Kouveliotou, and Neil Gehrels

Subjects
Physics, business.industry, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, X-ray detectors, Modular design, All sky monitoring, Gamma ray bursts, Physics and Astronomy (all), Optics, Sky, Scintillation counter, Angular resolution, Transient (oscillation), Gamma-ray burst, business, Event (particle physics), media_common
Abstract

We present here a concept for a light and low‐power wide field monitor working in the X‐ray range, suitable for simultaneous imaging of large portions of the sky and GRB localizations. Our concept evolves from and improves on the design of the 5‐kg SuperAGILE experiment, flying on the AGILE mission and currently delivering arcmin‐localizations of GRBs at a rate of about 1/month. Similar to SuperAGILE, our concept is based on position sensitive silicon detectors equipped with one‐dimensional coded masks. Different options are available for the detector, whose properties, combined with the scientific requirements, drive the design of the experiment. Our approach is based on a modular detector. The experiment design can then be tailored to specific scientific goals of the experiment or the mission (e.g., to cite GRBs only: the brightest GRBs/XRFs on a large field of view—FoV, or many low‐fluence GRBs/XRFs on a smaller FoV, or the low energy spectrum of the prompt event, or the detection of high‐z GRBs). In this paper we describe the concept, the main detector properties and outline some possible experiment configurations, with examples of their expected performance. Different experiment configurations in terms of area, FoV, angular resolution may be designed starting from the same detectors. Instead, the band‐pass is mostly related to the detector properties. A key point of our project is the high degree of readiness of the detectors that are at production level and may be immediately proposed for a future experiment onboard missions with high readiness requirements.

Published
2009
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35. AGILE and the Gamma-Ray Bursts

Author

M. Tavani, A. Argan, G. Barbiellini, A. Bulgarelli, P. Cattaneo, P. Caraveo, A. Chen, E. Costa, G. De Paris, E. Del Monte, G. Di Cocco, I. Donnarumma, Y. Evangelista, M. Feroci, F. Fuschino, M. Galli, F. Gianotti, A. Giuliani, C. Labanti, I. Lapshov, F. Lazzarotto, P. Lipari, F. Longo, M. Marisaldi, S. Mereghetti, A. Morselli, A. Pellizzoni, F. Perotti, P. Picozza, M. Prest, G. Pucella, M. Rapisarda, P. Soffitta, M. Trifoglio, A. Trois, E. Vallazza, S. Vercellone, V. Vittorini, A. Zambra, P. Giommi, C. Pittori, B. Preger, F. Verrecchia, L. A. Antonelli, L. Salotti, M. Galassi, David Palmer, and Ed Fenimore

Subjects
Physics, Calorimeter (particle physics), Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Astronomy, Field of view, Gamma-ray astronomy, Astrophysics, Universe, Orbit (dynamics), Angular resolution, Satellite, Gamma-ray burst, media_common
Abstract

AGILE is an ASI high‐energy astrophysics mission dedicated to the observation of the Universe. The satellite was successfully launched on April 23, 2007 to a quasi equatorial low‐background orbit. The AGILE instrument is very compact and light (∼100 kg): a gamma‐ray imager (sensitive in the energy band 30 MeV–50 GeV) is the central part of the instrument that includes also a light hard X‐ray imager (18–60 keV) positioned on top of the instrument, and an omnidirectional Calorimeter (350 keV–100 MeV). AGILE is aimed at the study of the most energetic phenomena of our Universe including AGNs, GRBs, Galactic sources and transients. For the first time in gamma‐ray astrophysics, AGILE reaches a field of view of about 3 sr with excellent angular resolution and good sensitivity. The unique combination of a hard X‐ray imager and a gamma‐ray imager is ideal for GRB and transient studies that constitute a crucial part of the AGILE scientific program. We summarize here the main characteristics of the GRB broad‐band d...

Published
2008
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38. The status of the AGILE GRB observations and the noticeable case of GRB 080514B

Author

E. Del Monte, E. Costa, I. Donnarumma, Y. Evangelista, F. Fornari, F. Fuschino, M. Galli, A. Giuliani, I. Lapshov, F. Lazzarotto, P. Lipari, F. Longo, M. Marisaldi, S. Mereghetti, E. Moretti, L. Pacciani, M. Rapisarda, P. Soffitta, S. Vercellone, A. Argan, G. Barbiellini, A. Bulgarelli, P. Caraveo, P. W. Cattaneo, A. Chen, G. Di Cocco, M. Feroci, F. Gianotti, C. Labanti, A. Morselli, A. Pellizzoni, F. Perotti, G. Piano, P. Picozza, M. Prest, G. Pucella, A. Rappoldi, S. Sabatini, M. Tavani, M. Trifoglio, A. Trois, E. Vallazza, V. Vittorini, B. Preger, C. Pittori, L. Salotti, Charles Meegan, Chryssa Kouveliotou, and Neil Gehrels

Subjects
Physics, Scintillation, Astrophysics::High Energy Astrophysical Phenomena, Scintillation counter, Detector, Gamma ray, Astronomy, Field of view, Context (language use), Astrophysics, Gamma-ray burst, Afterglow
Abstract

Since Summer 2007, the AGILE mission is successfully detecting and localizing Gamma Ray Bursts by using its wide‐field hard X‐ray monitor SuperAGILE (17–60 keV) and its CsI Minicalorimeter (0.3–20 MeV). Moreover, all the events with a known localization in the field of view of the Gamma Ray Imaging Detector are searched for in the 30 MeV–50 GeV energy range. Among the several bursts occurred in the field of view of the Gamma Ray Imaging Detector during more than one year of operations, at the time of writing the remarkable GRB 080514B is detected at high significance and GRB 080721 and GRB 081001 are detected at low significance. GRB 080514B is the first Gamma Ray Burst showing a significant emission above 20 MeV after EGRET, and the first ever associated with an afterglow, measured at X‐rays and in the IR/Optical/UV. Significant upper limits are derived for the other GRBs. In this paper we report about the status and the scientific performances of the AGILE instrumentation in the study of GRBs and we discuss the properties of GRB 080514B in the context of the long Gamma Ray Bursts.

39. First GRB detections with the AGILE Minicalorimeter

Author

M. Marisaldi, C. Labanti, F. Fuschino, M. Galli, M. Tavani, A. Bulgarelli, F. Gianotti, M. Trifoglio, A. Argan, M. Galassi, David Palmer, and Ed Fenimore

Subjects
Physics, High energy, Physics::Instrumentation and Detectors, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Real-time computing, Detector, Astronomy, Time resolution, Scintillator, Energy spectrum, Gamma-ray burst, business, Burst mode (computing), Agile software development
Abstract

The Minicalorimeter (MCAL) onboard the AGILE satellite is a 1400 cm2 scintillation detector sensitive in the energy range 0.3–200 MeV. MCAL works both as a slave of the AGILE Silicon Tracker and as an autonomous detector for transient events (BURST mode). A dedicated onboard Burst Search logic scans BURST mode data in search of count rate increase. Peculiar characteristics of the detector are the high energy spectral coverage and a timing resolution of about 2 microseconds. Even if a trigger is not issued, BURST mode data are used to build a broad band energy spectrum (scientific ratemeters) organized in 11 bands for each of the two MCAL detection planes, with a time resolution of 1 second. After the first engineering commissioning phase, following the AGILE launch on 23rd April 2007, between 22nd June and 5th November 2007 eighteen GRBs were detected offline in the scientific ratemeters data, with a detection rate of about one per week. In this paper the capabilities of the detector will be described and...

40. GRB 070724B: the first Gamma Ray Burst localized by SuperAGILE

Author

E. Del Monte, E. Costa, I. Donnarumma, Y. Evangelista, M. Feroci, I. Lapshov, F. Lazzarotto, M. Rapisarda, P. Soffitta, A. Argan, G. Barbiellini, M. Basset, A. Bulgarelli, P. Caraveo, A. Chen, G. Di Cocco, L. Foggetta, F. Fuschino, M. Galli, F. Gianotti, A. Giuliani, C. Labanti, P. Lipari, F. Longo, M. Marisaldi, F. Mauri, S. Mereghetti, A. Morselli, A. Pellizzoni, F. Perotti, P. Picozza, M. Prest, G. Pucella, M. Tavani, M. Trifoglio, A. Trois, E. Vallazza, S. Vercellone, V. Vittorini, A. Zambra, P. Romano, D. N. Burrows, G. Chincarini, N. Gehrels, V. La Parola, P. T. O'Brien, J. P. Osborne, B. Preger, C. Pittori, L. A. Antonelli, F. Verrecchia, P. Giommi, L. Salotti, M. Galassi, David Palmer, and Ed Fenimore

Subjects
Physics, Swift Gamma-Ray Burst Mission, Astrophysics::High Energy Astrophysical Phenomena, Physics::Space Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Astronomy, Gamma ray spectra, Astrophysics, Gamma-ray burst, Gamma detection
Abstract

GRB070724B is the first Gamma Ray Burst localized by the SuperAGILE instrument aboard the AGILE space mission. The SuperAGILE localization has been confirmed after the after‐glow observation by the XRT aboard the Swift satellite. No significant gamma ray emission above 50 MeV has been detected for this GRB. In this paper we describe the SuperAGILE capabilities in detecting Gamma Ray Burst and the AGILE observation of GRB 070724B.

41. Search for Very Short Bursts with the AGILE Mini-Calorimeter

Author

M. Marisaldi, C. Labanti, F. Fuschino, M. Galli, A. Argan, G. Barbiellini, F. Boffelli, A. Bulgarelli, P. Caraveo, P. W. Cattaneo, A. Chen, E. Costa, F. D’Ammando, E. Del Monte, G. Di Cocco, I. Donnarumma, Y. Evangelista, M. Feroci, F. Fornari, F. Gianotti, A. Giuliani, I. Lapshov, F. Lazzarotto, P. Lipari, F. Longo, S. Mereghetti, E. Moretti, A. Morselli, L. Pacciani, A. Pellizzoni, F. Perotti, P. Picozza, M. Prest, G. Pucella, M. Rapisarda, A. Rappoldi, P. Soffitta, M. Tavani, M. Trifoglio, A. Trois, E. Vallazza, S. Vercellone, V. Vittorini, C. Pittori, L. A. Antonelli, S. Cutini, D. Gasparrini, P. Giommi, B. Preger, P. Santolamazza, F. Verrecchia, L. Salotti, Charles Meegan, Chryssa Kouveliotou, and Neil Gehrels

Subjects
Physics, business.industry, Time windows, Telemetry, Real-time computing, Astronomy, Geophysical Phenomena, Gamma-ray burst, Gamma detection, business, Calorimeter, Agile software development, Data transmission
Abstract

In this paper the results of the first months of burst search on very short time scales with the Mini‐Calorimeter (MCAL) on‐board the AGILE mission are presented. MCAL is equipped with a flexible on‐board trigger logic for autonomous GRB detection. In addition to standard trigger time windows, MCAL has been equipped with trigger capabilities on 16 ms, 1 ms and sub‐millisecond time windows. Since June 2008 burst search on these short time scales has been enabled, resulting in an average rate of 4 triggers/orbit, compliant with telemetry budget. An on‐ground rejection strategy is applied, allowing more sophisticated selection criteria than those allowed by the on‐board trigger logic. Triggers due to instrumental effects or geophysical phenomena can be spotted due to their photon‐by‐photon pattern; what remains after this cleaning is an almost unexplored territory and could shed light on the origin of very short bursts. The trigger criteria, as well as the on‐ground rejection strategy and the properties of the selected events will be described and discussed.

44. The XGS instrument on-board THESEUS.

Author

F. Fuschino, R. Campana, C. Labanti, M. Marisaldi, L. Amati, M. Fiorini, M. Uslenghi, G. Baldazzi, Y. Evangelista, I. Elmi, M. Feroci, F. Frontera, A. Rachevski, L. P. Rignanese, A. Vacchi, G. Zampa, N. Zampa, I. Rashevskaya, P. Bellutti, and C. Piemonte

Published
2016
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46. AGILE OBSERVATIONS OF THE GRAVITATIONAL-WAVE EVENT GW150914.

Author

M. Tavani, C. Pittori, F. Verrecchia, A. Bulgarelli, A. Giuliani, I. Donnarumma, A. Argan, A. Trois, F. Lucarelli, M. Marisaldi, E. Del Monte, Y. Evangelista, V. Fioretti, A. Zoli, G. Piano, P. Munar-Adrover, L. A. Antonelli, G. Barbiellini, P. Caraveo, and P. W. Cattaneo

Published
2016
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47. Analysis of Thunderstorms Producing Terrestrial Gamma Ray Flashes With the Meteosat Second Generation

Author

Stefano Dietrich, Federico Porcù, A. Ursi, Marco Tavani, Martino Marisaldi, Alessandra Tiberia, and A. Ursi, M. Marisaldi, S. Dietrich, M. Tavani, A. Tiberia, F. Porcù

Subjects
Atmospheric Science, Thesaurus (information retrieval), Meteorology, Gamma ray, TGF, lightning, thunderstorms, meteosat, geostationary, tgf, Geophysics, Space and Planetary Science, Earth and Planetary Sciences (miscellaneous), Geostationary orbit, Thunderstorm, Environmental science, gamma-ray, thunderstorm
Abstract

Up to now, only few works focused on the meteorological context leading to the production of Terrestrial Gamma ray Flashes (TGFs). In this study, we carry out, for the first time, an analysis on large scale of the meteorological scenario linked to 278 TGFs detected by RHESSI, AGILE, and Fermi, by using the Meteosat Second Generation geostationary satellites. These satellites are useful as they continuously monitor the same geographic region in time, allowing investigations on thunderstorms' development; moreover, they are endowed with channels and products that provide information about the meteorological context under analysis, such as the cloud top temperature and altitude, the cloud extension, the drop effective radius and the cloud phase. Our work confirms what previously found in other studies about the TGF‐associated thunderstorms, by using a different approach and by using for the first time the Meteosat satellites: we find TGFs mostly linked to the development phase of deep convective thunderstorm systems, exhibiting typical characteristics of tropical storms, and providing a first picture on large scale of the TGF‐associated thunderstorm systems. publishedVersion

Published
2019
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48. The LOFT mission concept: a status update

Author

Feroci, M, Bozzo, E, Brandt, S, Hernanz, M, Van Der Klis, M, Liu, L, Orleanski, P, Pohl, M, Santangelo, A, Schanne, S, Stella, L, Takahashi, T, Tamura, H, Watts, A, Wilms, J, Zane, S, Zhang, S, Bhattacharyya, S, Agudo, I, 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, Ballantyne, Dr, Baldazzi, G, Baldo, M, Balman, S, Barbera, M, Van Baren, C, Barret, D, Baykal, A, Begelman, M, Behar, E, Behar, O, Belloni, T, Bellutti, P, Bernardini, F, Bertuccio, G, Bianchi, S, Bianchini, A, Binko, P, Blay, P, Bocchino, F, Bode, M, Bodin, P, Bombaci, I, Bonnet Bidaud, J, Borghi, G, Boutloukos, S, Bouyjou, F, Bradley, L, Braga, J, Briggs, Ms, Brown, E, Buballa, M, Bucciantini, N, Burderi, L, Burgay, M, Bursa, M, Budtz-Jorgensen, C, Cackett, E, Cadoux, Fr, Cais, P, Caliandro, Ga, Campana, R, Campana, S, Cao, X, Capitanio, F, Casares, J, Casella, P, Castro-Tirado, Aj, Cavazzuti, E, Cavechi, Y, Celestin, S, Cerda-Duran, P, Chakrabarty, D, Chamel, N, Chateau, F, Chen, C, Chen, Y, Chenevez, J, Chernyakova, M, Coker, J, Cole, R, Collura, A, Coriat, M, Cornelisse, R, Costamante, L, Cros, A, Cui, W, Cumming, A, Cusumano, G, Czerny, B, D'Ai, A, D'Ammando, F, D'Elia, V, Dai, Z, Del Monte, E, De Luca, A, De Martino, D, Dercksen, Jpc, De Pasquale, M, De Rosa, A, Del Santo, M, Di Cosimo, S, Degenaar, N, Den Herder, Jw, Diebold, S, Di Salvo, T, Dong, Y, Donnarumma, I, Doroshenko, V, Doyle, G, Drake, Sa, Durant, M, Emmanoulopoulos, D, Enoto, T, Erkut, Mh, Esposito, P, Evangelista, Y, Fabian, A, Falanga, M, Favre, Y, Feldman, C, Fender, R, Feng, H, Ferrari, V, Ferrigno, C, Ficorella, F, Finger, M, Finger, Mh, Fraser, Gw, Frericks, M, Fullekrug, M, Fuschino, F, Gabler, M, Galloway, Dk, Galvez Sanchez, Jl, Gandhi, P, Gao, Z, Garcia-Berro, E, Gendre, B, Gevin, O, Gezari, S, Giles, Ab, Gilfanov, M, Giommi, P, Giovannini, G, Giroletti, M, Gogus, E, Goldwurm, A, Goluchova, K, Gotz, D, Gou, L, Gouiffes, C, Grandi, P, Grassi, M, Greiner, J, Grinberg, V, Groot, P, Gschwender, M, Gualtieri, L, Guedel, M, Guidorzi, C, Guy, L, Haas, D, Haensel, P, Hailey, M, Hamuguchi, K, Hansen, F, Hartmann, Dh, Haswell, Ca, Hebeler, K, Heger, A, Hempel, M, Hermsen, W, Homan, J, Hornstrup, A, Hudec, R, Huovelin, J, Huppenkothen, D, Inam, Sc, Ingram, A, In'Tzand, Jjm, Israel, G, Iwasawa, K, Izzo, L, Jacobs, Hm, Jetter, F, Johannsen, T, Jenke, Pa, Jonker, P, Jose, J, Kaaret, P, Kalamkar, M, Kalemci, E, Kanbach, G, Karas, V, Karelin, D, Kataria, D, Keek, L, Kennedy, T, Klochkov, D, Kluzniak, W, Koerding, E, Kokkotas, K, Komossa, S, Korpela, S, Kouveliotou, C, Kowalski, Af, Kreykenbohm, I, Kuiper, Lm, Kunneriath, D, Kurkela, A, Kuvvetli, I, La Franca, F, Labanti, C, Lai, D, Lamb, Fk, Lachaud, C, Laubert, Pp, Lebrun, F, Li, X, Liang, E, Limousin, O, Lin, D, Linares, M, Linder, D, Lodato, G, Longo, F, Lu, F, Lund, N, Maccarone, Tj, Macera, D, Maestre, S, Mahmoodifar, S, Maier, D, Malcovati, P, Malzac, J, Malone, C, Mandel, I, Mangano, V, Manousakis, A, Marelli, M, Margueron, J, Marisaldi, M, Markoff, Sb, Markowitz, A, Marinucci, A, Martindale, A, Martinez, G, Mchardy, Im, Medina-Tanco, G, Mehdipour, M, Melatos, A, Mendez, M, Mereghetti, S, Migliari, S, Mignani, R, Michalska, M, Mihara, T, Miller, Mc, Miller, Jm, Mineo, T, Miniutti, G, Morsink, S, Motch, C, Motta, S, Mouchet, M, Mouret, G, Mulacova, J, Muleri, F, Munoz-Darias, T, Negueruela, I, Neilsen, J, Neubert, T, Norton, Aj, Nowak, M, Nucita, A, O'Brien, P, Oertel, M, Olsen, Peh, Orienti, M, Orio, M, Orlandini, M, Osborne, Jp, Osten, R, Ozel, F, Pacciani, L, Paerels, F, Paltani, S, Paolillo, M, Papadakis, I, Papitto, A, Paragi, Z, Paredes, Jm, Patruno, A, Paul, B, Pederiva, F, Perinati, E, Pellizzoni, A, Penacchioni, Av, Peretz, U, Perez, Ma, Perez-Torres, M, Peterson, Bm, Petracek, V, Picciotto, A, Piemonte, C, Pittori, C, Pons, J, Portell, J, Possenti, A, Postnov, K, Poutanen, J, Prakash, M, Prandoni, I, Le Provost, H, Psaltis, D, Pye, J, Qu, J, Rambaud, D, Ramon, P, Ramsay, G, Rapisarda, M, Rachevski, A, Rashevskaya, I, Ray, Ps, 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, Rischke, Dh, Rodriguez-Gil, P, Rodriguez, J, Rohlfs, R, Romano, P, Rossi, Emr, Rozanska, A, Rousseau, A, Rudak, B, Russell, Dm, Ryde, F, Sabau-Graziati, L, Sakamoto, T, Sala, G, Salvaterra, R, Salvetti, D, Sanna, A, Sandberg, J, Savolainen, T, Scaringi, S, Schaffner-Bielich, J, Schatz, H, Schee, J, Schmid, C, Serino, M, Shakura, N, Shore, S, Schnittman, Jd, Schneider, R, Schwenk, A, Schwope, Ad, Sedrakian, A, Seyler, J, Shearer, A, Slowikowska, A, Sims, M, Smith, A, Smith, Dm, Smith, Pj, Sobolewska, M, Sochora, V, Soffitta, P, Soleri, P, Song, L, Spencer, A, Stamerra, A, Stappers, B, Staubert, R, Steiner, Aw, Stergioulas, N, Stevens, Al, Stratta, G, Strohmayer, Te, Stuchlik, Z, Suchy, S, Suleimanov, V, Tamburini, F, Tauris, T, Tavecchio, F, Tenzer, C, Thielemann, Fk, Tiengo, A, Tolos, L, Tombesi, F, Tomsick, J, Torok, G, Torrejon, Jm, Torres, Df, Torresi, E, Tramacere, A, Traulsen, I, Trois, A, Turolla, R, Turriziani, S, Typel, S, Uter, P, Uttley, P, Vacchi, A, Varniere, P, Vaughan, S, Vercellone, S, Vietri, M, Vincent, Fh, Vrba, V, Walton, D, Wang, J, Wang, Z, Watanabe, S, Wawrzaszek, R, Webb, N, Weinberg, N, Wende, H, Wheatley, P, Wijers, R, Wijnands, R, Wille, M, Wilson-Hodge, Ca, Winter, B, Walk, Sj, Wood, K, Woosley, Se, Wu, X, Xiao, L, Xu, R, Yu, W, Yuan, F, Yuan, W, Yuan, Y, Zampa, G, Zampa, N, Zampieri, L, Zdunik, L, Zdziarski, A, Zech, A, Zhang, B, Zhang, C, Zingale, M, Zorzi, N, Zwart, F, High Energy Astrophys. & Astropart. Phys (API, FNWI), ISDC Data Centre for Astrophysics, Université de Genève = University of Geneva (UNIGE), Icahn School of Medicine at Mount Sinai [New York] (MSSM), Rutgers, The State University of New Jersey [New Brunswick] (RU), Rutgers University System (Rutgers), Institut für Astronomie und Astrophysik [Tübingen] (IAAT), Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen, 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), Dipartimento di Scienze e Tecnologie Chimiche, Università degli Studi di Roma Tor Vergata [Roma], Graduate School of the Natural Science and Technology [Kanazawa], Kanazawa University (KU), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Centre Interdisciplinaire de Nanoscience de Marseille (CINaM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Tampere University of Technology [Tampere] (TUT), University of Maryland [College Park], University of Maryland System, Department of Biological Sciences [Mississippi], University of Southern Mississippi (USM), School of Physics and Astronomy [Southampton], University of Southampton, Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Istituto Nazionale di Astrofisica (INAF), Università di Roma La Sapienza, Università di Roma Tor Vergata, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), 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), Institut de recherche en astrophysique et planétologie (IRAP), Swedish Institute of Space Physics [Uppsala] (IRF), INAF - Osservatorio Astronomico di Brera (OAB), Department of Computer Sciences [Scheffield], University of Sheffield [Sheffield], Colgate University, Bibliothèque nationale de France (BnF), Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo (IASF-Pa), ARC Centre of Excellence for Environmental Decisions (ARC CEED), The University of Western Australia (UWA)-Australian National University (ANU)-University of Queensland [Brisbane]-Royal Melbourne Institute of Technology University (RMIT University)-School of BioSciences [Melbourne], Faculty of Science [Melbourne], University of Melbourne-University of Melbourne-Faculty of Science [Melbourne], University of Melbourne-University of Melbourne, ARC Centre of Excellence for Coral Reef Studies (CoralCoE), James Cook University (JCU), Lund University [Lund], Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Anthropologie Moléculaire et Imagerie de Synthèse (AMIS), Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de synthèse organique (DCSO), École polytechnique (X)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), University of Alabama at Birmingham [ Birmingham] (UAB), INAF - Osservatorio Astronomico di Cagliari (OAC), ELECTRONIQUE 2016, 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)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Modèles Statistiques (LPTMS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), School of Geosciences, Monash University [Clayton], Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), 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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université libre de Bruxelles (ULB), National Oceanography Centre [Southampton] (NOC), Dublin Institute for Advanced Studies (DIAS), Dublin City University [Dublin] (DCU), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Institut Parisien de Chimie Moléculaire (IPCM), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Chinese Academy of Sciences [Beijing] (CAS), Laboratoire Univers et Théories (LUTH (UMR_8102)), 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), China Information Technology Security Evaluation Center (CNITSEC), Department of Applied Mathematics and Computer Science [Lyngby] (DTU Compute), Danmarks Tekniske Universitet = Technical University of Denmark (DTU), PCAS, Anton Pannekoek Institute for Astronomy, Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), International Space Science Institute [Bern] (ISSI), Université Grenoble Alpes - UFR Médecine (UGA UFRM), Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), CALVIN research group [Edinburgh], Institute of Perception, Action and Behaviour (IPAB), University of Edinburgh-University of Edinburgh, Department of Electronics and Electrical Engineering [Bath], University of Bath [Bath], United States Geological Survey [Reston] (USGS), Sr. PLM Consultant, 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, Dept Ind Engn & Informat Techonolgy, Università degli studi di Trieste = University of Trieste, Max-Planck-Institut für Extraterrestrische Physik (MPE), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology (MIT), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Matériaux, ingénierie et science [Villeurbanne] (MATEIS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS), Wisconsin Regional Primate Research Center, University of Wisconsin-Madison, SRON Netherlands Institute for Space Research (SRON), Opole University of Technology, University of Technology (Opole), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Department of Astrophysics [Nijmegen], Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University [Nijmegen]-Radboud University [Nijmegen], Radboud University [Nijmegen], NASA Goddard Space Flight Center (GSFC), Dept Fis Aplicada, Universidad de Granada = University of Granada (UGR), Victoria University [Melbourne], The Hong Kong Polytechnic University [Hong Kong] (POLYU), Chinese Academy of Sciences [Changchun Branch] (CAS), Department of Physics, Chemistry and Biology [Linköping] (IFM), Linköping University (LIU), Institut de Chimie des Substances Naturelles (ICSN), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire de Lyon (IPNL), 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), Erlangen Centre for Astroparticle Physics (ECAP), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), Centre de recherche en Biologie cellulaire de Montpellier (CRBM), Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy, University of Zielona Góra, Department of Electronics and Computer Systems, Takushoku University, Instituto Nacional de Pesquisas da Amazônia (INPA), Università degli studi di Catania = University of Catania (Unict), Centre d'Ecologie et des Sciences de la COnservation (CESCO), Muséum national d'Histoire naturelle (MNHN)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Ecologie Alpine (LECA ), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Laboratoire de Physico-Chimie de l'Atmosphère (LPCA), Université du Littoral Côte d'Opale (ULCO)-Centre National de la Recherche Scientifique (CNRS), HEPL, Solar Physics, Stanford University, Institut des Sciences Moléculaires de Marseille (ISM2), Aix Marseille Université (AMU)-École Centrale de Marseille (ECM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Space Telescope Science Institute (STSci), Dipartimento di Scienze Fisiche [Naples], University of Naples Federico II = Università degli studi di Napoli Federico II, Columbia University [New York], Laboratoire de Biométrie et Biologie Evolutive - UMR 5558 (LBBE), Université de Lyon-Université de Lyon-Institut National de Recherche en Informatique et en Automatique (Inria)-VetAgro Sup - Institut national d'enseignement supérieur et de recherche en alimentation, santé animale, sciences agronomiques et de l'environnement (VAS)-Centre National de la Recherche Scientifique (CNRS), Department of Anthropology [University of Arkansas], University of Arkansas [Fayetteville], Hu county ventre for disease control and prevention of Shaanxi province, Istituto Nazionale di Fisica Nucleare, Sezione di Trieste (INFN, Sezione di Trieste), Istituto Nazionale di Fisica Nucleare (INFN), Institut Jean le Rond d'Alembert (DALEMBERT), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), University of Reading (UOR), Departamento de Matemática Aplicada, Universidade de Santiago de Compostela [Spain] (USC ), Osservatorio Astrofisico di Catania, Équipe Robotique et InteractionS (LAAS-RIS), Laboratoire d'analyse et d'architecture des systèmes (LAAS), Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT)-Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT), Centro Euro-Mediterraneo per i Cambiamenti Climatici [Bologna] (CMCC), Institut für Theoretische Physik, Universität Heidelberg [Heidelberg] = Heidelberg University, Augsburg Hospital, Leibniz-Institut für Astrophysik Potsdam (AIP), Daimler Chrysler AG (Daimler), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Montserrat Volcano Observatory (MVO), Institut Armand Frappier (INRS-IAF), Institut National de la Recherche Scientifique [Québec] (INRS)-Réseau International des Instituts Pasteur (RIIP), Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], FICLIT, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Max-Planck-Institut für Radioastronomie (MPIFR), Argelander-Institut für Astronomie (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Christian-Albrechts-Universität zu Kiel (CAU), Dipartimento di Fisica e Astronomia 'Galileo Galilei', Università degli Studi di Padova = University of Padua (Unipd), APC - Gravitation (APC-Gravitation), 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)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Cahill Center for Astronomy and Astrophysics, California Institute of Technology (CALTECH), Xinjiang Astronomical Observatory, Mitsubishi Electric Research Laboratories (MERL), Mitsubishi Research Institute, Inc., School of Urban and Regional Planning, University of Southern California (USC), National University of Defense Technology [China], Princeton University, Department of Microtechnology and Nanoscience (MC2), Chalmers University of Technology [Gothenburg, Sweden], Feroci, M., Bozzo, E., Brandt, S., Hernanz, M., van der Klis, M., Liu, L., Orleanski, P., Pohl, M., Santangelo, A., Schanne, S., Stella, L., Takahashi, T., Tamura, H., Watts, A., Wilms, J., Zane, S., Zhang, S., Bhattacharyya, S., Agudo, I., 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., Ballantyne, D., Baldazzi, G., Baldo, M., Balman, S., Barbera, M., van Baren, C., Barret, D., Baykal, A., Begelman, M., Behar, E., Behar, O., Belloni, T., Bernardini, F., Bertuccio, G., Bianchi, S., Bianchini, A., Binko, P., Blay, P., Bocchino, F., Bode, M., Bodin, P., Bombaci, I., Bonnet Bidaud, J., Boutloukos, S., Bouyjou, F., Bradley, L., Braga, J., Briggs, M., Brown, E., Buballa, M., Bucciantini, N., Burderi, L., Burgay, M., Bursa, M., Budtz Jørgensen, C., Cackett, E., Cadoux, F., Cais, P., Caliandro, G., Campana, R., Campana, S., Cao, X., Capitanio, F., Casares, J., Casella, P., Castro Tirado, A., Cavazzuti, E., Cavechi, Y., Celestin, S., Cerda Duran, P., Chakrabarty, D., Chamel, N., Château, F., Chen, C., Chen, Y., Chenevez, J., Chernyakova, M., Coker, J., Cole, R., Collura, A., Coriat, M., Cornelisse, R., Costamante, L., Cros, A., Cui, W., Cumming, A., Cusumano, G., Czerny, B., D'Aì, A., D'Ammando, F., D'Elia, V., Dai, Z., Del Monte, E., De Luca, A., De Martino, D., Dercksen, J., De Pasquale, M., De Rosa, A., Del Santo, M., Di Cosimo, S., Degenaar, N., den Herder, J., Diebold, S., DI SALVO, T., Dong, Y., Donnarumma, I., Doroshenko, V., Doyle, G., Drake, S., Durant, M., Emmanoulopoulos, D., Enoto, T., Erkut, M., Esposito, P., Evangelista, Y., Fabian, A., Falanga, M., Favre, Y., Feldman, C., Fender, R., Feng, H., Ferrari, V., Ferrigno, C., Finger, M., Fraser, G., Frericks, M., Fullekrug, M., Fuschino, F., Gabler, M., Galloway, D., Gálvez Sanchez, J., Gandhi, P., Gao, Z., Garcia Berro, E., Gendre, B., Gevin, O., Gezari, S., Giles, A., Gilfanov, M., Giommi, P., Giovannini, G., Giroletti, M., Gogus, E., Goldwurm, A., Goluchová, K., Götz, D., Gou, L., Gouiffes, C., Grandi, P., Grassi, M., Greiner, J., Grinberg, V., Groot, P., Gschwender, M., Gualtieri, L., Guedel, M., Guidorzi, C., Guy, L., Haas, D., Haensel, P., Hailey, M., Hamuguchi, K., Hansen, F., Hartmann, D., Haswell, C., Hebeler, K., Heger, A., Hempel, M., Hermsen, W., Homan, J., Hornstrup, A., Hudec, R., Huovelin, J., Huppenkothen, D., Inam, S., Ingram, A., In't Zand, J., Israel, G., Iwasawa, K., Izzo, L., Jacobs, H., Jetter, F., Johannsen, T., Jenke, P., Jonker, P., Josè, J., Kaaret, P., Kalamkar, K., Kalemci, E., Kanbach, G., Karas, V., Karelin, D., Kataria, D., Keek, L., Kennedy, T., Klochkov, D., Kluzniak, W., Koerding, E., Kokkotas, K., Komossa, S., Korpela, S., Kouveliotou, C., Kowalski, A., Kreykenbohm, I., Kuiper, L., Kunneriath, D., Kurkela, A., Kuvvetli, I., La Franca, F., Labanti, C., Lai, D., Lamb, F., Lachaud, C., Laubert, P., Lebrun, F., Li, X., Liang, E., Limousin, O., Lin, D., Linares, M., Linder, D., Lodato, G., Longo, F., Lu, F., Lund, N., Maccarone, T., Macera, D., Maestre, S., Mahmoodifar, S., Maier, D., Malcovati, P., Malzac, J., Malone, C., Mandel, I., Mangano, V., Manousakis, A., Marelli, M., Margueron, J., Marisaldi, M., Markoff, S., Markowitz, A., Marinucci, A., Martindale, A., Martínez, G., Mchardy, I., Medina Tanco, G., Mehdipour, M., Melatos, A., Mendez, M., Mereghetti, S., Migliari, S., Mignani, R., Michalska, M., Mihara, T., 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., Neubert, T., Norton, A., Nowak, M., Nucita, A., O'Brien, P., Oertel, M., Olsen, P., Orienti, M., Orio, M., Orlandini, M., Osborne, J., Osten, R., Ozel, F., Pacciani, L., Paerels, F., Paltani, S., Paolillo, M., Papadakis, I., Papitto, A., Paragi, Z., Paredes, J., Patruno, A., Paul, B., Pederiva, F., Perinati, E., Pellizzoni, A., Penacchioni, A., Peretz, U., Perez, M., Perez Torres, M., Peterson, B., Petracek, V., Pittori, C., Pons, J., Portell, J., Possenti, A., Postnov, K., Poutanen, J., Prakash, M., Prandoni, I., Le Provost, H., Psaltis, D., Pye, J., Qu, J., Rambaud, D., Ramon, P., Ramsay, G., Rapisarda, M., Rashevski, 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., Rischke, D., Rodríguez Gil, P., Rodriguez, J., Rohlfs, R., Romano, P., Rossi, E., Rozanska, A., Rousseau, A., Rudak, B., Russell, D., Ryde, F., Sabau Graziati, L., Sakamoto, T., Sala, G., Salvaterra, R., Salvetti, D., Sanna, A., Sandberg, J., Savolainen, T., Scaringi, S., Schaffner Bielich, J., Schatz, H., Schee, J., Schmid, C., Serino, M., Shakura, N., Shore, S., Schnittman, J., Schneider, R., Schwenk, A., Schwope, A., Sedrakian, A., Seyler, J., Shearer, A., Slowikowska, A., Sims, M., Smith, A., Smith, D., Smith, P., Sobolewska, M., Sochora, V., Soffitta, P., Soleri, P., Song, L., Spencer, A., Stamerra, A., Stappers, B., Staubert, R., Steiner, A., Stergioulas, N., Stevens, A., Stratta, G., Strohmayer, T., Stuchlik, Z., Suchy, S., Suleimanov, V., Tamburini, F., Tauris, T., Tavecchio, F., Tenzer, C., Thielemann, F., Tiengo, A., Tolos, L., Tombesi, F., Tomsick, J., Torok, G., Torrejon, J., Torres, D., Torresi, E., Tramacere, A., Traulsen, I., Trois, A., Turolla, R., Turriziani, S., Typel, S., Uter, P., Uttley, P., Vacchi, A., Varniere, P., Vaughan, S., Vercellone, S., Vietri, M., Vincent, F., Vrba, V., Walton, D., Wang, J., Wang, Z., Watanabe, S., Wawrzaszek, R., Webb, N., Weinberg, N., Wende, H., Wheatley, P., Wijers, R., Wijnands, R., Wille, M., Wilson Hodge, C., Winter, B., Walk, S., Wood, K., Woosley, S., Wu, X., Xu, R., Yu, W., Yuan, F., Yuan, W., Yuan, Y., Zampa, G., Zampa, N., Zampieri, L., Zdunik, L., Zdziarski, A., Zech, A., Zhang, B., Zhang, C., Zingale, M., Zwart, F., University of Geneva [Switzerland], Eberhard Karls Universität Tübingen, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Graduate School of the Natural Science and Technology, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), School of BioSciences [Melbourne], University of Melbourne-University of Melbourne-Royal Melbourne Institute of Technology University (RMIT University)-University of Queensland [Brisbane]-Australian National University (ANU)-The University of Western Australia (UWA), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Université Libre de Bruxelles [Bruxelles] (ULB), Dublin City University, Dublin 9, Ireland, Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), China Information Technology Security Evaluation Center, Technical University of Denmark [Lyngby] (DTU), Université Grenoble Alpes (UGA), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), University of Trieste, Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Institut de Biologie Intégrative de la Cellule (I2BC), Université Paris-Sud - Paris 11 (UP11)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA), Università degli Studi di Roma 'La Sapienza' [Rome], Radboud university [Nijmegen]-Radboud university [Nijmegen], Radboud university [Nijmegen], Universidad de Granada (UGR), Centre National de la Recherche Scientifique (CNRS), Centre de recherche en Biologie Cellulaire (CRBM), Université Montpellier 1 (UM1)-Université Montpellier 2 - Sciences et Techniques (UM2)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Università degli studi di Catania [Catania], Laboratoire d'Ecologie Alpine (LECA), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA), Centre National de la Recherche Scientifique (CNRS)-Université du Littoral Côte d'Opale, Stanford University [Stanford], Centre National de la Recherche Scientifique (CNRS)-École Centrale de Marseille (ECM)-Aix Marseille Université (AMU), Università degli studi di Napoli Federico II, IFP Energies nouvelles (IFPEN), National Institute for Nuclear Physics (INFN), Institut Jean Le Rond d'Alembert (DALEMBERT), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse 1 Capitole (UT1)-Université Toulouse - Jean Jaurès (UT2J)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse 1 Capitole (UT1)-Université Toulouse - Jean Jaurès (UT2J), Ingénierie des Matériaux Polymères (IMP), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet [Saint-Étienne] (UJM)-Centre National de la Recherche Scientifique (CNRS), Centro Euro-Mediterraneo per i Cambiamenti Climatici (CMCC), Universität Heidelberg [Heidelberg], Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Réseau International des Instituts Pasteur (RIIP)-Institut National de la Recherche Scientifique [Québec] (INRS), Università di Bologna [Bologna] (UNIBO), University of California [Berkeley], University of California-University of California, Universita degli Studi di Padova, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Chalmers University of Technology [Göteborg], Astronomy, Jan-Willem A. den Herder, Shouleh Nikzad, Kazuhiro Nakazawa, Van Der Klis, M., Liu, L. -P., Zhang, S. -N., Atteia, J. -L., Ballantyne, D. R., Van Baren, C., Bellutti, P., Bonnet Bidaud, J. -M., Borghi, G., Briggs, M. S., Budtz-Jorgensen, C., Cadoux, F. R., Caliandro, G. A., Castro-Tirado, A. J., Cerda-Duran, P., Chateau, F., D'Ai, A., Dercksen, J. P. C., Den Herder, J. W., Di Salvo, T., Drake, S. A., Erkut, M. H., Ficorella, F., Finger, M. H., Fraser, G. W., Galloway, D. K., Galvez Sanchez, J. L., Garcia-Berro, E., Giles, A. B., Goluchova, K., Gotz, D., Hartmann, D. H., Haswell, C. A., Inam, S. C., In'Tzand, J. J. M., Jacobs, H. M., Jenke, P. A., Jose, J., Kalamkar, M., Kowalski, A. F., Kuiper, L. M., Lamb, F. K., Laubert, P. P., Maccarone, T. J., Markoff, S. B., Martinez, G., Mchardy, I. M., Medina-Tanco, G., Miller, M. C., Miller, J. M., Mulacova, J., Munoz-Darias, T., Norton, A. J., Olsen, P. E. H., Osborne, J. P., Paredes, J. M., Penacchioni, A. V., Perez, M. A., Perez-Torres, M., Peterson, B. M., Picciotto, A., Piemonte, C., Rachevski, A., Ray, P. S., De La Rie, R., Rischke, D. H., Rodriguez-Gil, P., Rossi, E. M. R., Russell, D. M., Sabau-Graziati, L., Schaffner-Bielich, J., Schnittman, J. D., Schwope, A. D., Seyler, J. -Y., Smith, D. M., Smith, P. J., Steiner, A. W., Stevens, A. L., Strohmayer, T. E., Thielemann, F. K., Torrejon, J. M., Torres, D. F., Vincent, F. H., Wilson-Hodge, C. A., Walk, S. J., Woosley, S. E., Xiao, L., Zorzi, N., 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), Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Institut de Chimie du CNRS (INC)-Université Pierre et Marie Curie - Paris 6 (UPMC)-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), 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), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Montpellier 2 - Sciences et Techniques (UM2)-Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Université Montpellier 1 (UM1), Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Muséum national d'Histoire naturelle (MNHN), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-École Centrale de Marseille (ECM)-Institut de Chimie du CNRS (INC), Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées, 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)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Department of Psychiatry (Icahn School of Medicine at Mount Sinai) ( ISMMS ), Rutgers, The State University of New Jersey [New Brunswick] ( RUTGERS ), Institut fur Astronomie und Astrophysik, 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 ), Kanazawa University ( KU ), Department of Earth Sciences, University of Oxford [Oxford], Centre Interdisciplinaire de Nanoscience de Marseille ( CINaM ), Aix Marseille Université ( AMU ) -Centre National de la Recherche Scientifique ( CNRS ), Tampere University of Technology [Tampere] ( TUT ), University of Southern Mississippi ( USM ), University of Southampton [Southampton], Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano ( IASF-MI ), Istituto Nazionale di Astrofisica ( INAF ), Istituto di Astrofisica e Planetologia Spaziali ( IAPS ), 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 ), 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 ), Swedish Institute of Space Physics [Uppsala] ( IRF ), Osservatorio Astronomico di Brera ( INAF ), Bibliothèque nationale de France ( BnF ), Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo ( IASF-Pa ), ARC Centre of Excellence for Environmental Decisions ( ARC CEED ), The University of Western Australia ( UWA ) -Australian National University ( ANU ) -University of Queensland [Brisbane]-RMIT University [Melbourne]-University of Melbourne, ARC Centre of Excellence for Coral Reef Studies ( CoralCoE ), James Cook University ( JCU ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Anthropologie Moléculaire et Imagerie de Synthèse ( AMIS ), PRES Université de Toulouse-Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de synthèse organique ( DCSO ), École polytechnique ( X ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Pathology, University of Alabama at Birmingham, University of Alabama at Birmingham Comprehensive Cancer Center, Birmingham, Alabama, INAF-Osservatorio di Cagliari, 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 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Théorique et Modèles Statistiques ( LPTMS ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace ( LPC2E ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Université Libre de Bruxelles [Bruxelles] ( ULB ), Ocean and Earth Sciences, National Oceanography Centre Southampton, Dublin Institute for advanced studies, 31 Fitzwilliam Place, Dublin 2, Ireland, Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), Institut Parisien de Chimie Moléculaire ( IPCM ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Centre National de la Recherche Scientifique ( CNRS ), Chinese Academy of Sciences [Beijing] ( CAS ), 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 ), Department of Applied Mathematics and Computer Science [Lyngby] ( DTU Compute ), Technical University of Denmark [Lyngby] ( DTU ), Institut für Astronomie und Astrophysik ( IAAT ), Anton Pannekoek Institute for Astronomy, University of Amsterdam, University of Cambridge [UK] ( CAM ), International Space Science Institute ( ISSI ), Université Grenoble Alpes - UFR Médecine ( UGA UFRM ), Université Grenoble Alpes ( UGA ), Institute of Perception, Action and Behaviour ( IPAB ), United States Geological Survey [Reston] ( USGS ), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), 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 ), Max-Planck-Institut für Extraterrestrische Physik ( MPE ), Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology ( MIT ), Institut de Physique du Globe de Paris ( IPGP ), Institut national des sciences de l'Univers ( INSU - CNRS ) -IPG PARIS-Université Paris Diderot - Paris 7 ( UPD7 ) -Université de la Réunion ( UR ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Biologie Intégrative de la Cellule ( I2BC ), Université Paris-Sud - Paris 11 ( UP11 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Centre National de la Recherche Scientifique ( CNRS ), Matériaux, ingénierie et science [Villeurbanne] ( MATEIS ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique ( CNRS ) -Institut National des Sciences Appliquées de Lyon ( INSA Lyon ), Université de Lyon-Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ), University of Wisconsin-Madison [Madison], SRON Netherlands Institute for Space Research ( SRON ), University of Technology ( Opole ), Institute for Mathematics, Astrophysics and Particle Physics ( IMAPP ), Grp Fis Atmosfera, Ctr Andaluz Medio Ambiente CEAMA, Universidad de Granada ( UGR ), The Hong Kong Polytechnic University [Hong Kong] ( POLYU ), Chinese Academy of Sciences [Changchun Branch] ( CAS ), Department of Physics, Chemistry and Biology, Linköping University ( LIU ), Institut de Chimie des Substances Naturelles ( ICSN ), Centre National de la Recherche Scientifique ( CNRS ), Institut de Physique Nucléaire de Lyon ( IPNL ), 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 ), Astronomical Institute Anton Pannekoek ( AI PANNEKOEK ), University of Amsterdam [Amsterdam] ( UvA ), Erlangen Centre for Astroparticle Physics ( ECAP ), Friedrich-Alexander Universität Erlangen-Nürnberg ( FAU ), Centre de recherches de biochimie macromoléculaire ( CRBM ), Université Montpellier 1 ( UM1 ) -Université Montpellier 2 - Sciences et Techniques ( UM2 ) -Université de Montpellier ( UM ) -Centre National de la Recherche Scientifique ( CNRS ), Instituto Nacional de Pesquisas da Amazônia ( INPA ), Instituto Nacional de Pesquisas da Amazônia, Centre d'Ecologie et des Sciences de la COnservation ( CESCO ), Muséum National d'Histoire Naturelle ( MNHN ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Ecologie Alpine ( LECA ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physico-Chimie de l'Atmosphère ( LPCA ), Université du Littoral Côte d'Opale-Centre National de la Recherche Scientifique ( CNRS ), Institut des Sciences Moléculaires de Marseille ( ISM2 ), Aix Marseille Université ( AMU ) -Ecole Centrale de Marseille ( ECM ) -Centre National de la Recherche Scientifique ( CNRS ), Space Telescope Science Institute ( STSci ), IFP Energies nouvelles ( IFPEN ), Laboratoire de Biométrie et Biologie Evolutive ( LBBE ), Université de Lyon-Université de Lyon-Institut National de Recherche en Informatique et en Automatique ( Inria ) -Centre National de la Recherche Scientifique ( CNRS ), University of Arkansas, Istituto Nazionale di Fisica Nucleare, Sezione di Trieste ( INFN, Sezione di Trieste ), National Institute for Nuclear Physics ( INFN ), Institut Jean Le Rond d'Alembert ( DALEMBERT ), Institut de Ciencies de l'Espai [Barcelona] ( ICE-CSIC ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), University of Reading ( UOR ), Universidade de Santiago de Compostela, Équipe Robotique et InteractionS ( LAAS-RIS ), Laboratoire d'analyse et d'architecture des systèmes [Toulouse] ( LAAS ), Institut National Polytechnique [Toulouse] ( INP ) -Institut National des Sciences Appliquées - Toulouse ( INSA Toulouse ), Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ) -Université Paul Sabatier - Toulouse 3 ( UPS ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National Polytechnique [Toulouse] ( INP ) -Institut National des Sciences Appliquées - Toulouse ( INSA Toulouse ), Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ) -Université Paul Sabatier - Toulouse 3 ( UPS ) -Centre National de la Recherche Scientifique ( CNRS ), Ingénierie des Matériaux Polymères - Site INSA Lyon ( IMP ), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon ( INSA Lyon ), Université de Lyon-Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ) -Université Jean Monnet [Saint-Étienne] ( UJM ) -Centre National de la Recherche Scientifique ( CNRS ), Leibniz-Institut für Astrophysik Potsdam ( AIP ), Daimler Chrysler AG ( Daimler ), Centre d'Etudes Nucléaires de Bordeaux Gradignan ( CENBG ), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Montserrat Volcano Observatory ( MVO ), Institut Armand Frappier ( INRS-IAF ), Institut National de la Recherche Scientifique [Québec] ( INRS ) -Réseau International des Instituts Pasteur ( RIIP ) -Institut Armand Frappier, Università di Bologna [Bologna] ( UNIBO ), Max-Planck-Institut für Radioastronomie, Argelander Institut für Astronomie, Bonn Universität [Bonn], Space Sciences Laboratory [Berkeley] ( SSL ), Christian-Albrechts-Universität zu Kiel ( CAU ), Universita degli Studi di Padova = University of Padua = Université de Padoue, APC - Gravitation ( APC-Gravitation ), 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 ) -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 ) -Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Max-Planck-Institut-Max-Planck-Institut, California Institute of Technology ( CALTECH ), Mitsubishi Electric Research Laboratories ( MERL ), Mitsubishi Electric Research Laboratories, Institute for Astronomy, University of Amsterdam, The Netherland, University of Southern California ( USC ), National University of Defense Technology [Changsha], Department of Microtechnology and Nanoscience ( MC2 ), Université Chalmers, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Nice Sophia Antipolis (UNS), Université Paris-Sud - Paris 11 (UP11)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay, Aix Marseille Université (AMU)-École Centrale de Marseille (ECM)-Centre National de la Recherche Scientifique (CNRS), Den Herder, Jan-Willem A., Bautz, M., den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Jan-Willem A. den Herder, Tadayuki Takahashi, Marshall Bautz, Liu, L. P., Zhang, S. N., Atteia, J. L., Bonnet Bidaud, J. M., Castro Tirado, A. J., D'Aı, A., den Herder, J. W., Gálvez Sanchez, J. L., In't Zand, J. J. M., Nucita, Achille, Seyler, J. Y., Wilson Hodge, C. A., Baldazzi, Giuseppe, Fuschino, Fabio, Bianchi, Stefano, Casella, Piergiorgio, DE ROSA, Alessandra, Giovannini, Gabriele, LA FRANCA, Fabio, Marinucci, Andrea, Paredes, M. J., Schneider, Raffaella, Vietri, Mario, 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), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), 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)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), M., Feroci, E., Bozzo, S., Brandt, M., Hernanz, M., van der Kli, L. P., Liu, P., Orleanski, M., Pohl, A., Santangelo, S., Schanne, L., Stella, T., Takahashi, H., Tamura, A., Watt, J., Wilm, S., Zane, S. N., Zhang, S., Bhattacharyya, I., Agudo, M., Ahangarianabhari, C., Albertu, M., Alford, A., Alpar, D., Altamirano, L., Alvarez, L., Amati, C., Amoro, N., Andersson, A., Antonelli, A., Argan, R., Artigue, B., Artigue, J. L., Atteia, P., Azzarello, P., Bakala, D., Ballantyne, G., Baldazzi, M., Baldo, S., Balman, M., Barbera, C., van Baren, D., Barret, A., Baykal, M., Begelman, E., Behar, O., Behar, T., Belloni, F., Bernardini, G., Bertuccio, S., Bianchi, A., Bianchini, P., Binko, P., Blay, F., Bocchino, M., Bode, P., Bodin, I., Bombaci, J. M., Bonnet Bidaud, S., Boutlouko, F., Bouyjou, L., Bradley, J., Braga, M. S., Brigg, E., Brown, M., Buballa, N., Bucciantini, L., Burderi, M., Burgay, M., Bursa, C., Budtz Jørgensen, E., Cackett, F., Cadoux, P., Cai, G. A., Caliandro, R., Campana, S., Campana, X., Cao, F., Capitanio, J., Casare, P., Casella, A. J., Castro Tirado, E., Cavazzuti, Y., Cavechi, S., Celestin, P., Cerda Duran, D., Chakrabarty, N., Chamel, F., Château, C., Chen, Y., Chen, J., Chenevez, M., Chernyakova, J., Coker, R., Cole, A., Collura, M., Coriat, R., Cornelisse, L., Costamante, A., Cro, W., Cui, A., Cumming, G., Cusumano, B., Czerny, A., D'Aì, F., D'Ammando, V., D'Elia, Z., Dai, E., Del Monte, A., De Luca, D., De Martino, J. P. C., Dercksen, M., De Pasquale, A., De Rosa, M., Del Santo, S., Di Cosimo, N., Degenaar, J. W., den Herder, S., Diebold, T., Di Salvo, Y., Dong, I., Donnarumma, V., Doroshenko, G., Doyle, S. A., Drake, M., Durant, D., Emmanoulopoulo, T., Enoto, M. H., Erkut, P., Esposito, Y., Evangelista, A., Fabian, M., Falanga, Y., Favre, C., Feldman, R., Fender, H., Feng, V., Ferrari, C., Ferrigno, M., Finger, M. H., Finger, G. W., Fraser, M., Frerick, M., Fullekrug, F., Fuschino, M., Gabler, D. K., Galloway, J. L., Gálvez Sanchez, P., Gandhi, Z., Gao, E., Garcia Berro, B., Gendre, O., Gevin, S., Gezari, A. B., Gile, M., Gilfanov, P., Giommi, G., Giovannini, M., Giroletti, E., Gogu, A., Goldwurm, K., Goluchová, D., Götz, L., Gou, C., Gouiffe, P., Grandi, M., Grassi, J., Greiner, V., Grinberg, P., Groot, M., Gschwender, L., Gualtieri, M., Guedel, C., Guidorzi, L., Guy, D., Haa, P., Haensel, M., Hailey, K., Hamuguchi, F., Hansen, D. H., Hartmann, C. A., Haswell, K., Hebeler, A., Heger, M., Hempel, W., Hermsen, J., Homan, A., Hornstrup, R., Hudec, J., Huovelin, D., Huppenkothen, S. C., Inam, A., Ingram, J. J. M., In't Zand, G., Israel, K., Iwasawa, L., Izzo, H. M., Jacob, F., Jetter, T., Johannsen, P. A., Jenke, P., Jonker, J., Josè, P., Kaaret, K., Kalamkar, E., Kalemci, G., Kanbach, V., Kara, D., Karelin, D., Kataria, L., Keek, T., Kennedy, D., Klochkov, W., Kluzniak, E., Koerding, K., Kokkota, S., Komossa, S., Korpela, C., Kouveliotou, A. F., Kowalski, I., Kreykenbohm, L. M., Kuiper, D., Kunneriath, A., Kurkela, I., Kuvvetli, F., La Franca, C., Labanti, D., Lai, F. K., Lamb, C., Lachaud, P. P., Laubert, F., Lebrun, X., Li, E., Liang, O., Limousin, D., Lin, M., Linare, D., Linder, G., Lodato, F., Longo, F., Lu, N., Lund, T. J., Maccarone, D., Macera, S., Maestre, S., Mahmoodifar, D., Maier, P., Malcovati, J., Malzac, C., Malone, I., Mandel, V., Mangano, A., Manousaki, M., Marelli, J., Margueron, M., Marisaldi, S. B., Markoff, A., Markowitz, A., Marinucci, A., Martindale, G., Martínez, I. M., Mchardy, G., Medina Tanco, M., Mehdipour, A., Melato, M., Mendez, S., Mereghetti, S., Migliari, R., Mignani, M., Michalska, T., Mihara, M. C., Miller, J. M., Miller, T., Mineo, G., Miniutti, S., Morsink, C., Motch, S., Motta, M., Mouchet, G., Mouret, J., Mulačová, F., Muleri, T., Muñoz Daria, I., Negueruela, J., Neilsen, T., Neubert, A. J., Norton, M., Nowak, A., Nucita, P., O'Brien, M., Oertel, P. E. H., Olsen, M., Orienti, M., Orio, M., Orlandini, J. P., Osborne, R., Osten, F., Ozel, L., Pacciani, F., Paerel, S., Paltani, Paolillo, Maurizio, I., Papadaki, A., Papitto, Z., Paragi, J. M., Parede, A., Patruno, B., Paul, F., Pederiva, E., Perinati, A., Pellizzoni, A. V., Penacchioni, U., Peretz, M. A., Perez, M., Perez Torre, B. M., Peterson, V., Petracek, C., Pittori, J., Pon, J., Portell, A., Possenti, K., Postnov, J., Poutanen, M., Prakash, I., Prandoni, H., Le Provost, D., Psalti, J., Pye, J., Qu, D., Rambaud, P., Ramon, G., Ramsay, M., Rapisarda, A., Rashevski, I., Rashevskaya, P. S., Ray, N., Rea, S., Reddy, P., Reig, M., Reina Aranda, R., Remillard, C., Reynold, L., Rezzolla, M., Ribo, R., de la Rie, A., Riggio, A., Rio, D. H., Rischke, P., Rodríguez Gil, J., Rodriguez, R., Rohlf, P., Romano, E. M. R., Rossi, A., Rozanska, A., Rousseau, B., Rudak, D. M., Russell, F., Ryde, L., Sabau Graziati, T., Sakamoto, G., Sala, R., Salvaterra, D., Salvetti, A., Sanna, J., Sandberg, T., Savolainen, S., Scaringi, J., Schaffner Bielich, H., Schatz, J., Schee, C., Schmid, M., Serino, N., Shakura, S., Shore, J. D., Schnittman, R., Schneider, A., Schwenk, A. D., Schwope, A., Sedrakian, J. Y., Seyler, A., Shearer, A., Slowikowska, M., Sim, A., Smith, D. M., Smith, P. J., Smith, M., Sobolewska, V., Sochora, P., Soffitta, P., Soleri, L., Song, A., Spencer, A., Stamerra, B., Stapper, R., Staubert, A. W., Steiner, N., Stergioula, A. L., Steven, G., Stratta, T. E., Strohmayer, Z., Stuchlik, S., Suchy, V., Suleimanov, F., Tamburini, T., Tauri, F., Tavecchio, C., Tenzer, F. K., Thielemann, A., Tiengo, L., Tolo, F., Tombesi, J., Tomsick, G., Torok, J. M., Torrejon, D. F., Torre, E., Torresi, A., Tramacere, I., Traulsen, A., Troi, R., Turolla, S., Turriziani, S., Typel, P., Uter, P., Uttley, A., Vacchi, P., Varniere, S., Vaughan, S., Vercellone, M., Vietri, F. H., Vincent, V., Vrba, D., Walton, J., Wang, Z., Wang, S., Watanabe, R., Wawrzaszek, N., Webb, N., Weinberg, H., Wende, P., Wheatley, R., Wijer, R., Wijnand, M., Wille, C. A., Wilson Hodge, B., Winter, S. J., Walk, K., Wood, S. E., Woosley, X., Wu, R., Xu, W., Yu, F., Yuan, W., Yuan, Y., Yuan, G., Zampa, N., Zampa, L., Zampieri, L., Zdunik, A., Zdziarski, A., Zech, B., Zhang, C., Zhang, S., Zhang, M., Zingale, and F., Zwart

Subjects
X-ray timing, [ SDU.ASTR.GA ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Field of view, Astrophysics, 01 natural sciences, law.invention, law, Observatory, timing, 010303 astronomy & astrophysics, QB, Physics, microchannel plates. PROPORTIONAL COUNTER ARRAY, CALIBRATION, X-ray astronomy, Electronic, Optical and Magnetic Material, Applied Mathematics, Astrophysics::Instrumentation and Methods for Astrophysics, Computer Science Applications1707 Computer Vision and Pattern Recognition, X-ray detectors, Condensed Matter Physics, compact objects, X-ray spectroscopy, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], spectroscopy, Cosmic Vision, [ INFO ] Computer Science [cs], Silicon detector, Astrophysics::High Energy Astrophysical Phenomena, Condensed Matter Physic, Telescope, X-ray, Silicon detectors, Electronic, Optical and Magnetic Materials, Electrical and Electronic Engineering, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Electronic, [INFO]Computer Science [cs], Optical and Magnetic Materials, Spectral resolution, DETECTOR, ta115, X-ray astronomy, Silicon detectors, timing, spectroscopy, 010308 nuclear & particles physics, X-ray imaging, Applied Mathematic, Neutron star, QB460-466 Astrophysics, Large Observatory For x-ray Timing (LOFT), Large Area Detector (LAD), Wide Field Monitor (WFM), Large Area Silicon Drift Detectors (SDD), Gamma-ray burst
Abstract

The Large Observatory For x-ray Timing (LOFT) is a mission concept which was proposed to ESA as M3 and M4 candidate in the framework of the Cosmic Vision 2015-2025 program. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument and the uniquely large field of view of its wide field monitor, LOFT will be able to study the behaviour of matter in extreme conditions such as the strong gravitational field in the innermost regions close to black holes and neutron stars and the supra-nuclear densities in the interiors of neutron stars. The science payload is based on a Large Area Detector (LAD, >8m2 effective area, 2-30 keV, 240 eV spectral resolution, 1 degree collimated field of view) and a Wide Field 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 current technical and programmatic status of the mission. © (2016) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.

Published
2016
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49. Room-temperature spectroscopic performance of a very-large area silicon drift detector

Author

Marco Feroci, Luigi Pacciani, Claudio Labanti, Martino Marisaldi, Fabio Muleri, Paolo Soffitta, Giuseppe Baldazzi, V. Bonvicini, A. Vacchi, Marco Grassi, Riccardo Campana, M. Mastropietro, E. Del Monte, F. Fuschino, Francesco Lazzarotto, Enrico Costa, Massimo Rapisarda, Piero Malcovati, Alexander Rashevsky, Alda Rubini, L. Picolli, Ennio Morelli, N. Zampa, I. Donnarumma, Y. Evangelista, G. Zampa, G. Zampa, R. Campana, 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, X-ray spectroscopy, Silicon, Silicon drift detector, Physics::Instrumentation and Detectors, business.industry, Detector, X-RAY SPECTROSCOPY, chemistry.chemical_element, ROOM TEMPERATURE, Signal, Anode, Full width at half maximum, Optics, chemistry, Optoelectronics, SILICON DRIFT DETECTORS, Spectroscopy, business, Instrumentation
Abstract

Silicon drift detectors (SDD) of small dimensions (up to 1 cm 2 ) have been successfully employed in X-ray spectroscopy due to their small anode geometry, which allows to minimize the electronic noise due to the readout device. Many applications, however, require large sensitive areas to be covered (e.g. X-ray astronomy), so that these detectors are effectively impractical. We present the spectroscopic performance of a 53 cm 2 sensitive area, multi-anode SDD, measured at room temperature using an eight-channel readout setup. The measurements, taken using 55 Fe and 241 Am sources, and X-ray tubes generating energies down to 2 keV, show energy resolutions in the range 290–570 eV FWHM, at 20 °C, depending on the number of anodes collecting the signal. Further developments we are carrying out could improve the detector characteristics and allow to approach the performance of small area SDDs.

Published
2011
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50. Preliminary results on TeV sources search with AGILE

Author

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

Subjects
Physics, Very High Energy Gamma-ray Astronomy, High Energy Gamma-ray Astronomy, Nuclear and High Energy Physics, business.industry, AGILe, gamma ray sky, TeV source, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics, Sky, Milagro, Satellite, MAGIC (telescope), business, Instrumentation, Agile software development, media_common
Abstract

During its first 2 years of operation, the gamma-ray AGILE satellite almost completed a full study of the gamma-ray sky. This paper presents the preliminary results of the systematic study performed on the AGILE data to search for GeV counterparts and to derive flux upper limits of the TeV sources detected by various instruments (MAGIC, HESS, VERITAS, Cangaroo, MILAGRO, ARGO, … .).

Published
2011
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