836 results on '"A. Marisaldi"'
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2. Flickering gamma-ray flashes, the missing link between gamma glows and TGFs
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Østgaard, N., Mezentsev, A., Marisaldi, M., Grove, J. E., Quick, M., Christian, H., Cummer, S., Pazos, M., Pu, Y., Stanley, M., Sarria, D., Lang, T., Schultz, C., Blakeslee, R., Adams, I., Kroodsma, R., Heymsfield, G., Lehtinen, N., Ullaland, K., Yang, S., Qureshi, B. Hasan, Søndergaard, J., Husa, B., Walker, D., Shy, D., Bateman, M., Bitzer, P., Fullekrug, M., Cohen, M., Montanya, J., Younes, C., van der Velde, O., Krehbiel, P., Roncancio, J. A., Lopez, J. A., Urbani, M., Santos, A., and Mach, D.
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- 2024
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3. AGILE gamma-ray detection of the exceptional GRB 221009A
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Tavani, M., Piano, G., Bulgarelli, A., Foffano, L., Ursi, A., Verrecchia, F., Pittori, C., Casentini, C., Giuliani, A., Longo, F., Panebianco, G., Di Piano, A., Baroncelli, L., Fioretti, V., Parmiggiani, N., Argan, A., Trois, A., Vercellone, S., Cardillo, M., Antonelli, L. A., Barbiellini, G., Caraveo, P., Cattaneo, P. W., Chen, A. W., Costa, E., Del Monte, E., Di Cocco, G., Donnarumma, I., Evangelista, Y., Feroci, M., Gianotti, F., Labanti, C., Lazzarotto, F., Lipari, P., Lucarelli, F., Marisaldi, M., Mereghetti, S., Morselli, A., Pacciani, L., Pellizzoni, A., Perotti, F., Picozza, P., Pilia, M., Rapisarda, M., Rappoldi, A., Rubini, A., Soffitta, P., Trifoglio, M., Vittorini, V., and D'Amico, F.
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
Gamma-ray emission in the MeV-GeV range from explosive cosmic events is of invaluable relevance to understanding physical processes related to the formation of neutron stars and black holes. Here we report on the detection by the AGILE satellite in the MeV-GeV energy range of the remarkable long-duration gamma-ray burst GRB 221009A. The AGILE onboard detectors have good exposure to GRB 221009A during its initial crucial phases. Hard X-ray/MeV emission in the prompt phase lasted hundreds of seconds, with the brightest radiation being emitted between 200 and 300 seconds after the initial trigger. Very intense GeV gamma-ray emission is detected by AGILE in the prompt and early afterglow phase up to 10,000 seconds. Time-resolved spectral analysis shows time-variable MeV-peaked emission simultaneous with intense power-law GeV radiation that persists in the afterglow phase. The coexistence during the prompt phase of very intense MeV emission together with highly nonthermal and hardening GeV radiation is a remarkable feature of GRB 221009A. During the prompt phase, the event shows spectrally different MeV and GeV emissions that are most likely generated by physical mechanisms occurring in different locations. AGILE observations provide crucial flux and spectral gamma-ray information regarding the early phases of GRB 221009A during which emission in the TeV range was reported., Comment: Accepted for publication in ApJL on September 19, 2023. Published online on October 17, 2023. Revised Figure 5 (June 13, 2024)
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- 2023
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4. Evidence of a New Population of Weak Terrestrial Gamma‐Ray Flashes Observed From Aircraft Altitude
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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
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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.
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- 2024
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5. AGILE Observations of GRB 220101A: A 'New Year's Burst' with an Exceptionally Huge Energy Release
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Ursi, Alessandro, Romani, Marco, Piano, Giovanni, Verrecchia, Francesco, Longo, Francesco, Pittori, Carlotta, Tavani, Marco, Bulgarelli, Andrea, Cardillo, Martina, Casentini, Claudio, Cattaneo, Paolo Walter, Costa, Enrico, Feroci, Marco, Fioretti, Valentina, Foffano, Luca, Lucarelli, Fabrizio, Marisaldi, Martino, Morselli, Aldo, Pacciani, Luigi, Parmiggiani, Nicolò, Tempesta, Patrizio, Trois, Alessio, and Vercellone, Stefano
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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
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- 2022
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6. Multi-wavelength study of the luminous GRB 210619B observed with Fermi and ASIM
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Caballero-García, M. D., Gupta, Rahul, Pandey, S. B., Oates, S. R., Marisaldi, M., Ramsli, A., Hu, Y. -D., Castro-Tirado, A. J., Sánchez-Ramírez, R., Connell, P. H., Christiansen, F., Ror, A. Kumar, Aryan, A., Bai, J. -M., Castro-Tirado, M. A., Fan, Y. -F., Fernández-García, E., Kumar, A., Lindanger, A., Mezentsev, A., Navarro-González, J., Neubert, T., Østgaard, N., Pérez-García, I., Reglero, V., Sarria, D., Sun, T. R., Xiong, D. -R., Yang, J., Yang, Y. -H., and Zhang, B. -B.
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Astrophysics - High Energy Astrophysical Phenomena - 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 ($p<$ 2). We find moderate values of host extinction of E(B-V) = 0.14 $\pm$ 0.01 mag for the Small Magellanic Cloud (SMC) extinction law. In addition, we also report late-time optical observations with the 10.4 m GTC placing deep upper limits for the host galaxy ($z$=1.937), favouring a faint, dwarf host for the burst., Comment: 24 pages, 18 figures, 10 tables, accepted for publication in MNRAS
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- 2022
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7. Ultra-High-Energy Cosmic Rays: The Intersection of the Cosmic and Energy Frontiers
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Coleman, A., Eser, J., Mayotte, E., Sarazin, F., Schröder, F. G., Soldin, D., Venters, T. M., Aloisio, R., Alvarez-Muñiz, J., Batista, R. Alves, Bergman, D., Bertaina, M., Caccianiga, L., Deligny, O., Dembinski, H. P., Denton, P. B., di Matteo, A., Globus, N., Glombitza, J., Golup, G., Haungs, A., Hörandel, J. R., Jaffe, T. R., Kelley, J. L., Krizmanic, J. F., Lu, L., Matthews, J. N., Mariş, I., Mussa, R., Oikonomou, F., Pierog, T., Santos, E., Tinyakov, P., Tsunesada, Y., Unger, M., Yushkov, A., Albrow, M. G., Anchordoqui, L. A., Andeen, K., Arnone, E., Barghini, D., Bechtol, E., Bellido, J. A., Casolino, M., Castellina, A., Cazon, L., Conceição, R., Cremonini, R., Dujmovic, H., Engel, R., Farrar, G., Fenu, F., Ferrarese, S., Fujii, T., Gardiol, D., Gritsevich, M., Homola, P., Huege, T., Kampert, K. -H., Kang, D., Kido, E., Klimov, P., Kotera, K., Kozelov, B., Leszczyńska, A., Madsen, J., Marcelli, L., Marisaldi, M., Martineau-Huynh, O., Mayotte, S., Mulrey, K., Murase, K., Muzio, M. S., Ogio, S., Olinto, A. V., Onel, Y., Paul, T., Piotrowski, L., Plum, M., Pont, B., Reininghaus, M., Riedel, B., Riehn, F., Roth, M., Sako, T., Schlüter, F., Shoemaker, D., Sidhu, J., Sidelnik, I., Timmermans, C., Tkachenko, O., Veberič, D., Verpoest, S., Verzi, V., Vícha, J., Winn, D., Zas, E., and Zotov, M.
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Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Instrumentation and Methods for Astrophysics ,High Energy Physics - Experiment - 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
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- 2022
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8. The Second Catalog of Interplanetary Network Localizations of Konus Short Duration Gamma-Ray Bursts
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Svinkin, D., Hurley, K., Ridnaia, A., Lysenko, A., Frederiks, D., Golenetskii, S., Tsvetkova, A., Ulanov, M., Kokomov, A., Cline, T. L., Mitrofanov, I., Golovin, D., Kozyrev, A., Litvak, M., Sanin, A., Goldstein, A., Briggs, M. S., Wilson-Hodge, C., Burns, E., von Kienlin, A., Zhang, X. -L., Rau, A., Savchenko, V., Bozzo, E., Ferrigno, C., Barthelmy, S., Cummings, J., Krimm, H., Palmer, D. M., Tohuvavohu, A., Yamaoka, K., Ohno, M., Fukazawa, Y., Hanabata, Y., Takahashi, T., Tashiro, M., Terada, Y., Murakami, T., Makishima, K., Boynton, W., Fellows, C. W., Harshman, K. P., Enos, H., Starr, R., Goldsten, J., Gold, R., Ursi, A., Tavani, M., Bulgarelli, A., Casentini, C., Del Monte, E., Evangelista, Y., Galli, M., Longo, F., Marisaldi, M., Parmiggiani, N., Pittori, C., Romani, M., Verrecchia, F., Smith, D. M., Hajdas, W., Xiao, S., Cai, C., Yi, Q. B., Zhang, Y. Q., Xiong, S. L., Li, X. B., Huang, Y., Li, C. K., Zhang, S. N., Song, L. M., Liu, C. Z., Li, X. Q., Peng, W. X., and Martinez-Castellanos, I.
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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., Comment: Published in ApJS
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- 2022
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9. Flickering Gamma Flashes, the Missing Link Between Gamma Glows and TGFs
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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
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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.
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- 2024
10. Highly Dynamic Gamma-Ray Emissions Are Common in Tropical Thunderclouds
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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
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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.
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- 2024
11. Detection of terrestrial gamma-ray flashes with the AGILE/MCAL
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Ursi, Alessandro, Marisaldi, Martino, and Tavani, Marco
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Physics - Space Physics ,Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
AGILE is one of the satellites currently detecting terrestrial gamma-ray flashes (TGFs). In particular, the AGILE Mini-CALorimeter detected more than 2000 events in 8 years activity, by exploiting a unique sub-millisecond timescale trigger logic and high-energy range. A change in the onboard configuration enhanced the trigger capabilities for the detection of these events, overcoming dead time issues and enlarging the detection rate of these events up to $>$50 TGFs/month, allowing to reveal shorter duration flashes. The quasi-equatorial low-inclination ( 2.5$^{\circ}$) orbit of AGILE allows for the detection of repeated TGFs coming from the same storms, at the same orbital passage and throughout successive orbital overpasses, over the same geographic region. All TGFs detected by AGILE are fulfilling a database that can be used for offline analysis and forthcoming studies. The limited number of missions currently detecting these brief terrestrial flashes makes the understanding of this phenomenon very challenging and, in this perspective, the AGILE satellite played and still plays a major role, helping shedding light to many aspects of TGF science
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- 2021
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12. On the High-Energy Spectral Component and Fine Time Structure of Terrestrial Gamma Ray Flashes
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Marisaldi, M., Galli, M., Labanti, C., Østgaard, N., Sarria, D., Cummer, S. A., Lyu, F., Lindanger, A., Campana, R., Ursi, A., Tavani, M., Fuschino, F., Argan, A., Trois, A., Pittori, C., and Verrecchia, F.
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Physics - Space Physics ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
Terrestrial gamma ray flashes (TGFs) are very short bursts of gamma radiation associated to thunderstorm activity and are the manifestation of the highest-energy natural particle acceleration phenomena occurring on Earth. Photon energies up to several tens of megaelectronvolts are expected, but the actual upper limit and high-energy spectral shape are still open questions. Results published in 2011 by the AGILE team proposed a high-energy component in TGF spectra extended up to $\approx$100 MeV, which is difficult to reconcile with the predictions from the Relativistic Runaway Electron Avalanche (RREA) mechanism at the basis of many TGF production models. Here we present a new set of TGFs detected by the AGILE satellite and associated to lightning measurements capable to solve this controversy. Detailed end-to-end Monte Carlo simulations and an improved understanding of the instrument performance under high-flux conditions show that it is possible to explain the observed high-energy counts by a standard RREA spectrum at the source, provided that the TGF is sufficiently bright and short. We investigate the possibility that single high-energy counts may be the signature of a fine-pulsed time structure of TGFs on time scales $\approx$4 {\mu}s, but we find no clear evidence for this. The presented data set and modeling results allow also for explaining the observed TGF distribution in the (Fluence x duration) parameter space and suggest that the AGILE TGF detection rate can almost be doubled. Terrestrial gamma ray flashes (TGFs) are very short bursts of gamma radiation associated to thunderstorm activity and are the manifestation of the highest-energy natural particle acceleration phenomena occurring on Earth. (...continues)
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- 2021
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13. Gamma Ray Glow Observations at 20-km Altitude
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Østgaard, N., Christian, H. J., Grove, J. E., Sarria, D., Mezentsev, A., Kochkin, P., Lehtinen, N., Quick, M., Al-Nussirat, S., Wulf, E., Genov, G., Ullaland, K., Marisaldi, M., Yang, S., and Blakeslee, R. J.
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Physics - Space Physics - Abstract
In the spring of 2017 an ER-2 aircraft campaign was undertaken over continental United States to observe energetic radiation from thunderstorms and lightning. The payload consisted of a suite of instruments designed to detect optical signals, electric fields, and gamma rays from lightning. Starting from Georgia, USA, 16 flights were performed, for a total of about 70 flight hours at a cruise altitude of 20 km. Of these, 45 flight hours were over thunderstorm regions. An analysis of two gamma ray glow events that were observed over Colorado at 21:47 UT on 8May 2017 is presented.We explore the charge structure of the cloud system, as well as possible mechanisms that can produce the gamma ray glows. The thundercloud system we passed during the gamma ray glow observation had strong convection in the core of the cloud system. Electric field measurements combined with radar and radio measurements suggest an inverted charge structure, with an upper negative charge layer and a lower positive charge layer. Based on modeling results, we were not able to unambiguously determine the production mechanism. Possible mechanisms are either an enhancement of cosmic background locally (above or below 20 km) by an electric field below the local threshold or an enhancement of the cosmic background inside the cloud but then with normal polarity and an electric field well above the Relativistic Runaway Electron Avalanche threshold
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- 2021
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14. AGILESim: Monte Carlo simulation of the AGILE gamma-ray telescope
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Fioretti, V., Bulgarelli, A., Tavani, M., Sabatini, S., Aboudan, A., Argan, A., Cattaneo, P. W., Chen, A. W., Donnarumma, I., Longo, F., Galli, M., Giuliani, A., Marisaldi, M., Parmiggiani, N., and Rappoldi, A.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
The accuracy of Monte Carlo simulations in reproducing the scientific performance of space telescopes (e.g. angular resolution) is mandatory for a correct design of the mission. A brand-new Monte Carlo simulator of the Astrorivelatore Gamma ad Immagini LEggero (AGILE)/Gamma-Ray Imaging Detector (GRID) space telescope, AGILESim, is built using the customizable Bologna Geant4 Multi-Mission Simulator (BoGEMMS) architecture and the latest Geant4 library to reproduce the instrument performance of the AGILE/GRID instrument. The Monte Carlo simulation output is digitized in the BoGEMMS postprocessing pipeline, according to the instrument electronic read-out logic, then converted into the onboard data handling format, and finally analyzed by the standard mission on-ground reconstruction pipeline, including the Kalman filter, as a real observation in space. In this paper we focus on the scientific validation of AGILESim, performed by reproducing (i) the conversion efficiency of the tracker planes, (ii) the tracker charge readout distribution measured by the on-ground assembly, integration, and verification activity, and (iii) the point-spread function of in-flight observations of the Vela pulsar in the 100 MeV - 1 GeV energy range. We measure an in-flight angular resolution (FWHM) for Vela-like point sources of $2.0^{+0.2}_{-0.3}$ and $0.8^{+0.1}_{-0.1}$ degrees in the 100 - 300 and 300 - 1000 MeV energy bands, respectively. The successful cross-comparison of the simulation results with the AGILE on-ground and in-space performance validates the BoGEMMS framework for its application to future gamma-ray trackers (e.g. e-ASTROGAM and AMEGO).
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- 2020
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15. An X-Ray Burst from a Magnetar Enlightening the Mechanism of Fast Radio Bursts
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Tavani, M., Casentini, C., Ursi, A., Verrecchia, F., Addis, A., Antonelli, L. A., Argan, A., Barbiellini, G., Baroncelli, L., Bernardi, G., Bianchi, G., Bulgarelli, A., Caraveo, P., Cardillo, M., Cattaneo, P. W., Chen, A. W., Costa, E., Del Monte, E., Di Cocco, G., Di Persio, G., Donnarumma, I., Evangelista, Y., Feroci, M., Ferrari, A., Fioretti, V., Fuschino, F., Galli, M., Gianotti, F., Giuliani, A., Labanti, C., Lazzarotto, F., Lipari, P., Longo, F., Lucarelli, F., Magro, A., Marisaldi, M., Mereghetti, S., Morelli, E., Morselli, A., Naldi, G., Pacciani, L., Parmiggiani, N., Paoletti, F., Pellizzoni, A., Perri, M., Perotti, F., Piano, G., Picozza, P., Pilia, M., Pittori, C., Puccetti, S., Pupillo, G., Rapisarda, M., Rappoldi, A., Rubini, A., Setti, G., Soffitta, P., Trifoglio, M., Trois, A., Vercellone, S., Vittorini, V., Giommi, P., and Amico, F. D'
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
Fast radio bursts (FRBs) are short (millisecond) radio pulses originating from enigmatic sources at extragalactic distances so far lacking a detection in other energy bands. Magnetized neutron stars (magnetars) have been considered as the sources powering the FRBs, but the connection is controversial because of differing energetics and the lack of radio and X-ray detections with similar characteristics in the two classes. We report here the detection by the AGILE satellite on April 28, 2020 of an X-ray burst in coincidence with the very bright radio burst from the Galactic magnetar SGR 1935+2154. The burst detected by AGILE in the hard X-ray band (18-60 keV) lasts about 0.5 seconds, it is spectrally cutoff above 80 keV, and implies an isotropically emitted energy ~ $10^{40}$ erg. This event is remarkable in many ways: it shows for the first time that a magnetar can produce X-ray bursts in coincidence with FRB-like radio bursts; it also suggests that FRBs associated with magnetars may emit X-ray bursts of both magnetospheric and radio-pulse types that may be discovered in nearby sources. Guided by this detection, we discuss SGR 1935+2154 in the context of FRBs, and especially focus on the class of repeating-FRBs. Based on energetics, magnetars with fields B ~ $10^{15}$ G may power the majority of repeating-FRBs. Nearby repeating-FRBs offer a unique occasion to consolidate the FRB-magnetar connection, and we present new data on the X-ray monitoring of nearby FRBs. Our detection enlightens and constrains the physical process leading to FRBs: contrary to previous expectations, high-brightness temperature radio emission coexists with spectrally-cutoff X-ray radiation., Comment: Submitted to Nature Astronomy, May 18, 2020
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- 2020
16. AGILE Observations of Two Repeating Fast Radio Bursts with Small Intrinsic Dispersion Measures
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Casentini, C., Verrecchia, F., Tavani, M., Ursi, A., Antonelli, L. A., Argan, A., Barbiellini, G., Bulgarelli, A., Caraveo, P., Cardillo, M., Cattaneo, P. W., Chen, A., Costa, E., Donnarumma, I., Feroci, M., Ferrari, A., Fuschino, F., Galli, M., Giuliani, A., Labanti, C., Lazzarotto, F., Lipari, P., Longo, F., Lucarelli, F., Marisaldi, M., Morselli, A., Paoletti, F., Parmiggiani, N., Pellizzoni, A., Piano, G., Pilia, M., Pittori, C., and Vercellone, S.
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
We focus on two repeating fast radio bursts (FRBs) recently detected by the CHIME/FRB experiment in 2018--2019 (Source 1: 180916.J0158+65, and Source 2: 181030.J1054+73). These sources have low excess dispersion measures (DMs) ($ < 100 \rm \, pc \, cm^{-3}$ and $ < 20 \rm \, pc \, cm^{-3}$, respectively), implying relatively small maximal distances. They were repeatedly observed by AGILE in the MeV--GeV energy range. We do not detect prompt emission simultaneously with these repeating events. This search is particularly significant for the submillisecond and millisecond integrations obtainable by AGILE. The sources are constrained to emit a MeV-fluence in the millisecond range below $F'_{MeV} = 10^{-8} \, \rm erg \, cm^{-2}$ corresponding to an isotropic energy near $E_{MeV,UL} \simeq 2 \times 10^{46}\,$erg for a distance of 150 Mpc (applicable to Source 1). We also searched for $\gamma$-ray emission for time intervals up to 100 days, obtaining 3$\,\sigma$ upper limits (ULs) for the average isotropic luminosity above 50 MeV, $L_{\gamma,UL} \simeq \,$(5-10)$\,\times 10^{43} \rm \, erg \, s^{-1}$. For a source distance near 100 kpc (possibly applicable to Source 2), our ULs imply $E_{MeV,UL}\simeq10^{40} \rm erg$, and $L_{\gamma,UL} \simeq \,$2$\,\times 10^{37} \rm \, erg \, s^{-1}$. Our results are significant in constraining the high-energy emission of underlying sources such as magnetars, or other phenomena related to extragalactic compact objects, and show the prompt emission to be lower than the peak of the 2004 magnetar outburst of SGR 1806-20 for source distances less than about 100 Mpc., Comment: to be published in ApJL
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- 2019
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17. New WMO Certifi ed Megaflash Lightning Extremes for Flash Distance and Duration Recorded from Space
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Peterson, Michael J., Lang, Timothy J., Logan, Timothy, Kiong, Cheong Wee, Gijben, Morne, Holle, Ron, Kolmasova, Ivana, Marisaldi, Martino, Montanya, Joan, Pawar, Sunil D., Zhang, Daile, Brunet, Manola, and Cerveny, Randall S.
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- 2022
18. Decreasing pH impairs sexual reproduction in a Mediterranean coral transplanted at a CO₂ vent
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Marchini, Chiara, Gizzi, Francesca, Pondrelli, Thomas, Moreddu, Lisa, Marisaldi, Luca, Montori, Francesco, Lazzari, Valentina, Airi, Valentina, Caroselli, Erik, Prada, Fiorella, Falini, Giuseppe, Dubinsky, Zvy, and Goffredo, Stefano
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- 2021
19. Calibration of AGILE-GRID with on-ground data and Monte Carlo simulations
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Cattaneo, P. W., Rappoldi, A., Argan, A., Barbiellini, G., Boffelli, F., Bulgarelli, A., Buonomo, B., Cardillo, M., Chen, A. W., Cocco, V., Colafrancesco, S., D'Ammando, F., Donnarumma, I., Ferrari, A., Fioretti, V., Foggetta, L., Froysland, T., Fuschino, F., Galli, M., Gianotti, F., Giuliani, A., Longo, F., Lucarelli, F., Marisaldi, M., Mazzitelli, G., Morselli, A., Paoletti, F., Parmigiani, N., Pellizzoni, A., Piano, G., Pilia, M., Pittori, C., Prest, M., Pucella, G., Quintieri, L., Sabatini, S., Tavani, M., Trifoglio, M., Trois, A., Valente, P., Vallazza, E., Vercellone, S., Verrecchia, F., and Zambra, A.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
AGILE is a mission of the Italian Space Agency (ASI) Scientific Program dedicated to gamma-ray astrophysics, operating in a low Earth orbit since April 23, 2007. It is designed to be a very light and compact instrument, capable of simultaneously detecting and imaging photons in the 18 keV to 60 keV X-ray energy band and in the 30 MeV{50 GeV gamma-ray energy with a good angular resolution (< 1 deg at 1 GeV). The core of the instrument is the Silicon Tracker complemented with a CsI calorimeter and a AntiCoincidence system forming the Gamma Ray Imaging Detector (GRID). Before launch, the GRID needed on-ground calibration with a tagged gamma-ray beam to estimate its performance and validate the Monte Carlo simulation. The GRID was calibrated using a tagged gamma-ray beam with energy up to 500 MeV at the Beam Test Facilities at the INFN Laboratori Nazionali di Frascati. These data are used to validate a GEANT3 based simulation by comparing the data and the Monte Carlo simulation by measuring the angular and energy resolutions. The GRID angular and energy resolutions obtained using the beam agree well with the Monte Carlo simulation. Therefore the simulation can be used to simulate the same performance on-light with high reliability., Comment: 19 page 12 figures
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- 2018
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20. The e-ASTROGAM gamma-ray space observatory for the multimessenger astronomy of the 2030s
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Tatischeff, V., De Angelis, A., Tavani, M., Grenier, I., Oberlack, U., Hanlon, L., Walter, R., Argan, A., von Ballmoos, P., Bulgarelli, A., Donnarumma, I., Hernanz, M., Kuvvetli, I., Mallamaci, M., Pearce, M., Zdziarski, A., Aboudan, A., Ajello, M., Ambrosi, G., Bernard, D., Bernardini, E., Bonvicini, V., Brogna, A., Branchesi, M., Budtz-Jorgensen, C., Bykov, A., Campana, R., Cardillo, M., Ciprini, S., Coppi, P., Cumani, P., da Silva, R. M. Curado, De Martino, D., Diehl, R., Doro, M., Fioretti, V., Funk, S., Ghisellini, G., Giordano, F., Grove, J. E., Hamadache, C., Hartmann, D. H., Hayashida, M., Isern, J., Kanbach, G., Kiener, J., Knödlseder, J., Labanti, C., Laurent, P., Leising, M., Limousin, O., Longo, F., Mannheim, K., Marisaldi, M., Martinez, M., Mazziotta, M. N., McEnery, J. E., Mereghetti, S., Minervini, G., Moiseev, A., Morselli, A., Nakazawa, K., Orleanski, P., Paredes, J. M., Patricelli, B., Peyré, J., Piano, G., Pohl, M., Rando, R., Roncadelli, M., Tavecchio, F., Thompson, D. J., Turolla, R., Ulyanov, A., Vacchi, A., Wu, X., and Zoglauer, A.
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
e-ASTROGAM is a concept for a breakthrough observatory space mission carrying a gamma-ray telescope dedicated to the study of the non-thermal Universe in the photon energy range from 0.15 MeV to 3 GeV. The lower energy limit can be pushed down to energies as low as 30 keV for gamma-ray burst detection with the calorimeter. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with remarkable polarimetric capability. Thanks to its performance in the MeV-GeV domain, substantially improving its predecessors, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on the surroundings. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous and current generation instruments, e-ASTROGAM will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will be a major player of the multiwavelength, multimessenger time-domain astronomy of the 2030s, and provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LISA, LIGO, Virgo, KAGRA, the Einstein Telescope and the Cosmic Explorer, IceCube-Gen2 and KM3NeT, SKA, ALMA, JWST, E-ELT, LSST, Athena, and the Cherenkov Telescope Array., Comment: 15 pages, 7 figures. Submitted to the proceedings of the conference SPIE Astronomical Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray. v2: corrections of authors' affiliations
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- 2018
21. Monte Carlo simulations of Gamma-ray space telescopes: a BoGEMMS multi-purpose application
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Fioretti, Valentina, Bulgarelli, Andrea, Tavani, Marco, Marisaldi, Martino, Sabatini, Sabina, Malaguti, Giuseppe, Trifoglio, Massimo, and Gianotti, Fulvio
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
After the development of a BoGEMMS (Bologna Geant4 Multi-Mission Simulator) template for the back- ground study of X-ray telescopes, a new extension is built for the simulation of a Gamma-ray space mission (e.g. AGILE, Fermi), conceived to work as a common, multi-purpose framework for the present and future electron tracking gamma-ray space telescopes. The Gamma-ray extension involves the Geant4 mass model, the physics list and, more important, the production and treatment of the simulation output. From the user point of view, the simulation set-up follows a tree structure, with the main level being the selection of the simulation framework (the general, X-ray or gamma-ray application) and the secondary levels being the detailed configuration of the geometry and the output format. The BoGEMMS application to Gamma-ray missions has been used to evaluate the instrument performances of a new generation of Gamma-ray tele- scopes (e.g. Gamma-Light), and a full simulation of the AGILE mission is currently under construction, to scientifically validate and calibrate the simulator with real in-space data sets. A complete description of the BoGEMMS Gamma-ray framework is presented here, with an overview of the achieved results for the potential application to present and future experiments (e.g., GAMMA-400 and Gamma-Light). The evaluation of the photon conversion efficiency to beta particle pairs and the comparison to tabulated data allows the preliminary physical validation of the overall architecture. The Gamma-ray module application for the study of the Gamma-Light instrument performances is reported as reference test case.
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- 2018
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22. The X-Gamma Imaging Spectrometer (XGIS) onboard THESEUS
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Campana, R., Fuschino, F., Labanti, C., Amati, L., Mereghetti, S., Fiorini, M., Frontera, F., Baldazzi, G., Bellutti, P., Borghi, G., Elmi, I., Evangelista, Y., Feroci, M., Ficorella, F., Orlandini, M., Picciotto, A., Marisaldi, M., Rachevski, A., Uslenghi, M., Vacchi, A., Zampa, G., Zampa, N., and Zorzi, N.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
A compact and modular X and gamma-ray imaging spectrometer (XGIS) has been designed as one of the instruments foreseen on-board the THESEUS mission proposed in response to the ESA M5 call. The experiment envisages the use of CsI scintillator bars read out at both ends by single-cell 25 mm 2 Silicon Drift Detectors. Events absorbed in the Silicon layer (lower energy X rays) and events absorbed in the scintillator crystal (higher energy X rays and Gamma-rays) are discriminated using the on-board electronics. A coded mask provides imaging capabilities at low energies, thus allowing a compact and sensitive instrument in a wide energy band (~2 keV up to ~20 MeV). The instrument design, expected performance and the characterization performed on a series of laboratory prototypes are discussed., Comment: To be published in the Proceedings of the THESEUS Workshop 2017 (http://www.isdc.unige.ch/theseus/workshop2017.html), Journal of the Italian Astronomical Society (Mem.SAIt), Editors L. Amati, E. Bozzo, M. Della Valle, D. Gotz, P. O'Brien. Details on the THESEUS mission concept can be found in the white paper Amati et al. 2017 (arXiv:171004638) and Stratta et al. 2017 (arXiv:1712.08153)
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- 2018
23. Science with e-ASTROGAM (A space mission for MeV-GeV gamma-ray astrophysics)
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De Angelis, A., Tatischeff, V., Grenier, I. A., McEnery, J., Mallamaci, M., Tavani, M., Oberlack, U., Hanlon, L., Walter, R., Argan, A., Von Ballmoos, P., Bulgarelli, A., Bykov, A., Hernanz, M., Kanbach, G., Kuvvetli, I., Pearce, M., Zdziarski, A., Conrad, J., Ghisellini, G., Harding, A., Isern, J., Leising, M., Longo, F., Madejski, G., Martinez, M., Mazziotta, M. N., Paredes, J. M., Pohl, M., Rando, R., Razzano, M., Aboudan, A., Ackermann, M., Addazi, A., Ajello, M., Albertus, C., Alvarez, J. M., Ambrosi, G., Anton, S., Antonelli, L. A., Babic, A., Baibussinov, B., Balbo, M., Baldini, L., Balman, S., Bambi, C., de Almeida, U. Barres, Barrio, J. A., Bartels, R., Bastieri, D., Bednarek, W., Bernard, D., Bernardini, E., Bernasconi, T., Bertucci, B., Biland, A., Bissaldi, E., Boettcher, M., Bonvicini, V., Ramon, V. Bosch, Bottacini, E., Bozhilov, V., Bretz, T., Branchesi, M., Brdar, V., Bringmann, T., Brogna, A., Jorgensen, C. Budtz, Busetto, G., Buson, S., Busso, M., Caccianiga, A., Camera, S., Campana, R., Caraveo, P., Cardillo, M., Carlson, P., Celestin, S., Cermeno, M., Chen, A., Cheung, C. C, Churazov, E., Ciprini, S., Coc, A., Colafrancesco, S., Coleiro, A., Collmar, W., Coppi, P., da Silva, R. Curado, Cutini, S., DAmmando, F., De Lotto, B., de Martino, D., De Rosa, A., Del Santo, M., Delgado, L., Diehl, R., Dietrich, S., Dolgov, A. D., Dominguez, A., Prester, D. Dominis, Donnarumma, I., Dorner, D., Doro, M., Dutra, M., Elsaesser, D., Fabrizio, M., FernandezBarral, A., Fioretti, V., Foffano, L., Formato, V., Fornengo, N., Foschini, L., Franceschini, A., Franckowiak, A., Funk, S., Fuschino, F., Gaggero, D., Galanti, G., Gargano, F., Gasparrini, D., Gehrz, R., Giammaria, P., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Ghirlanda, G., Godinovic, N., Gouiffes, C., Grove, J. E., Hamadache, C., Hartmann, D. H., Hayashida, M., Hryczuk, A., Jean, P., Johnson, T., Jose, J., Kaufmann, S., Khelifi, B., Kiener, J., Knodlseder, J., Kole, M., Kopp, J., Kozhuharov, V., Labanti, C., Lalkovski, S., Laurent, P., Limousin, O., Linares, M., Lindfors, E., Lindner, M., Liu, J., Lombardi, S., Loparco, F., LopezCoto, R., Moya, M. Lopez, Lott, B., Lubrano, P., Malyshev, D., Mankuzhiyil, N., Mannheim, K., Marcha, M. J., Marciano, A., Marcote, B., Mariotti, M., Marisaldi, M., McBreen, S., Mereghetti, S., Merle, A., Mignani, R., Minervini, G., Moiseev, A., Morselli, A., Moura, F., Nakazawa, K., Nava, L., Nieto, D., Orienti, M., Orio, M., Orlando, E., Orleanski, P., Paiano, S., Paoletti, R., Papitto, A., Pasquato, M., Patricelli, B., PerezGarcia, M. A., Persic, M., Piano, G., Pichel, A., Pimenta, M., Pittori, C., Porter, T., Poutanen, J., Prandini, E., Prantzos, N., Produit, N., Profumo, S., Queiroz, F. S., Raino, S., Raklev, A., Regis, M., Reichardt, I., Rephaeli, Y., Rico, J., Rodejohann, W., Fernandez, G. Rodriguez, Roncadelli, M., Roso, L., Rovero, A., Ruffini, R., Sala, G., SanchezConde, M. A., Santangelo, A., Parkinson, P. Saz, Sbarrato, T., Shearer, A., Shellard, R., Short, K., Siegert, T., Siqueira, C., Spinelli, P., Stamerra, A., Starrfield, S., Strong, A., Strumke, I., Tavecchio, F., Taverna, R., Terzic, T., Thompson, D. J., Tibolla, O., Torres, D. F., Turolla, R., Ulyanov, A., Ursi, A., Vacchi, A., Abeele, J. Van den, Kirilovai, G. Vankova, Venter, C., Verrecchia, F., Vincent, P., Wang, X., Weniger, C., Wu, X., Zaharijas, G., Zampieri, L., Zane, S., Zimmer, S., Zoglauer, A., and collaboration, the eASTROGAM
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Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Solar and Stellar Astrophysics ,High Energy Physics - Experiment - Abstract
e-ASTROGAM (enhanced ASTROGAM) is a breakthrough Observatory space mission, with a detector composed by a Silicon tracker, a calorimeter, and an anticoincidence system, dedicated to the study of the non-thermal Universe in the photon energy range from 0.3 MeV to 3 GeV - the lower energy limit can be pushed to energies as low as 150 keV for the tracker, and to 30 keV for calorimetric detection. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with polarimetric capability. Thanks to its performance in the MeV-GeV domain, substantially improving its predecessors, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on the surroundings. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous generation instruments, e-ASTROGAM will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LIGO-Virgo-GEO600-KAGRA, SKA, ALMA, E-ELT, TMT, LSST, JWST, Athena, CTA, IceCube, KM3NeT, and LISA., Comment: Published on Journal of High Energy Astrophysics (Elsevier)
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- 2017
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24. AGILE Observations of the Gravitational-wave Source GW170817: Constraining Gamma-Ray Emission from a NS-NS Coalescence
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Verrecchia, F., Tavani, M., Donnarumma, I., Bulgarelli, A., Evangelista, Y., Pacciani, L., Ursi, A., Piano, G., Pilia, M., Cardillo, M., Parmiggiani, N., Giuliani, A., Pittori, C., Longo, F., Lucarelli, F., Minervini, G., Feroci, M., Argan, A., Fuschino, F., Labanti, C., Marisaldi, M., Fioretti, V., Trois, A., Del Monte, E., Antonelli, L. A., Barbiellini, G., Caraveo, P., Cattaneo, P. W., Colafrancesco, S., Costa, E., D'Amico, F., Ferrari, A., Giommi, P., Morselli, A., Paoletti, F., Pellizzoni, A., Picozza, P., Rappoldi, A., Soffitta, P., Vercellone, S., Baroncelli, L., and Zollino, G.
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
The LIGO-Virgo Collaboration (LVC) detected, on 2017 August 17, an exceptional gravitational-wave (GW) event temporally consistent within $\sim\,1.7 \, \rm s$ with the GRB 1708117A observed by Fermi-GBM and INTEGRAL. The event turns out to be compatible with a neutron star-neutron star (NS-NS) coalescence that subsequently produced a radio/optical/X-ray transient detected at later times. We report the main results of the observations by the AGILE satellite of the GW170817 localization region (LR) and its electromagnetic (e.m.) counterpart. At the LVC detection time $T_0$, the GW170817 LR was occulted by the Earth. The AGILE instrument collected useful data before and after the GW-GRB event because in its spinning observation mode it can scan a given source many times per hour. The earliest exposure of the GW170817 LR by the gamma-ray imaging detector (GRID) started about 935 s after $T_0$. No significant X-ray or gamma-ray emission was detected from the LR that was repeatedly exposed over timescales of minutes, hours, and days before and after GW170817, also considering Mini-calorimeter and Super-AGILE data. Our measurements are among the earliest ones obtained by space satellites on GW170817 and provide useful constraints on the precursor and delayed emission properties of the NS-NS coalescence event. We can exclude with high confidence the existence of an X-ray/gamma-ray emitting magnetar-like object with a large magnetic field of $10^{15} \, \rm G$. Our data are particularly significant during the early stage of evolution of the e.m. remnant., Comment: Submitted to Astrophysical Journal Letters on October 13, 2017; LVC; revised October 25, 2017; accepted October 25, 2017
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- 2017
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25. The THESEUS space mission concept: science case, design and expected performances
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Amati, L., O'Brien, P., Goetz, D., Bozzo, E., Tenzer, C., Frontera, F., Ghirlanda, G., Labanti, C., Osborne, J. P., Stratta, G., Tanvir, N., Willingale, R., Attina, P., Campana, R., Castro-Tirado, A. J., Contini, C., Fuschino, F., Gomboc, A., Hudec, R., Orleanski, P., Renotte, E., Rodic, T., Bagoly, Z., Blain, A., Callanan, P., Covino, S., Ferrara, A., Floch, E. Le, Marisaldi, M., Mereghetti, S., Rosati, P., Vacchi, A., D'Avanzo, P., Giommi, P., Piranomonte, S., Piro, L., Reglero, V., Rossi, A., Santangelo, A., Salvaterra, R., Tagliaferri, G., Vergani, S., Vinciguerra, S., Briggs, M., Campolongo, E., Ciolfi, R., Connaughton, V., Cordier, B., Morelli, B., Orlandini, M., Adami, C., Argan, A., Atteia, J. -L., Auricchio, N., Balazs, L., Baldazzi, G., Basa, S., Basak, R., Bellutti, P., Bernardini, M. G., Bertuccio, G., Braga, J., Branchesi, M., Brandt, S., Brocato, E., Budtz-Jorgensen, C., Bulgarelli, A., Burderi, L., Camp, J., Capozziello, S., Caruana, J., Casella, P., Cenko, B., Chardonnet, P., Ciardi, B., Colafrancesco, S., Dainotti, M. G., D'Elia, V., De Martino, D., De Pasquale, M., Del Monte, E., Della Valle, M., Drago, A., Evangelista, Y., Feroci, M., Finelli, F., Fiorini, M., Fynbo, J., Gal-Yam, A., Gendre, B., Ghisellini, G., Grado, A., Guidorzi, C., Hafizi, M., Hanlon, L., Hjorth, J., Izzo, L., Kiss, L., Kumar, P., Kuvvetli, I., Lavagna, M., Li, T., Longo, F., Lyutikov, M., Maio, U., Maiorano, E., Malcovati, P., Malesani, D., Margutti, R., Martin-Carrillo, A., Masetti, N., McBreen, S., Mignani, R., Morgante, G., Mundell, C., Nargaard-Nielsen, H. U., Nicastro, L., Palazzi, E., Paltani, S., Panessa, F., Pareschi, G., Pe'er, A., Penacchioni, A. V., Pian, E., Piedipalumbo, E., Piran, T., Rauw, G., Razzano, M., Read, A., Rezzolla, L., Romano, P., Ruffini, R., Savaglio, S., Sguera, V., Schady, P., Skidmore, W., Song, L., Stanway, E., Starling, R., Topinka, M., Troja, E., van Putten, M., Vanzella, E., Vercellone, S., Wilson-Hodge, C., Yonetoku, D., Zampa, G., Zampa, N., Zhang, B., Zhang, B. B., Zhang, S., Zhang, S. -N., Antonelli, A., Bianco, F., Boci, S., Boer, M., Botticella, M. T., Boulade, O., Butler, C., Campana, S., Capitanio, F., Celotti, A., Chen, Y., Colpi, M., Comastri, A., Cuby, J. -G., Dadina, M., De Luca, A., Dong, Y. -W., Ettori, S., Gandhi, P., Geza, E., Greiner, J., Guiriec, S., Harms, J., Hernanz, M., Hornstrup, A., Hutchinson, I., Israel, G., Jonker, P., Kaneko, Y., Kawai, N., Wiersema, K., Korpela, S., Lebrun, V., Lu, F., MacFadyen, A., Malaguti, G., Maraschi, L., Melandri, A., Modjaz, M., Morris, D., Omodei, N., Paizis, A., Pata, P., Petrosian, V., Rachevski, A., Rhoads, J., Ryde, F., Sabau-Graziati, L., Shigehiro, N., Sims, M., Soomin, J., Szecsi, D., Urata, Y., Uslenghi, M., Valenziano, L., Vianello, G., Vojtech, S., Watson, D., and Zicha, J.
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Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
THESEUS is a space mission concept aimed at exploiting Gamma-Ray Bursts for investigating the early Universe and at providing a substantial advancement of multi-messenger and time-domain astrophysics. These goals will be achieved through a unique combination of instruments allowing GRB and X-ray transient detection over a broad field of view (more than 1sr) with 0.5-1 arcmin localization, an energy band extending from several MeV down to 0.3 keV and high sensitivity to transient sources in the soft X-ray domain, as well as on-board prompt (few minutes) follow-up with a 0.7 m class IR telescope with both imaging and spectroscopic capabilities. THESEUS will be perfectly suited for addressing the main open issues in cosmology such as, e.g., star formation rate and metallicity evolution of the inter-stellar and intra-galactic medium up to redshift $\sim$10, signatures of Pop III stars, sources and physics of re-ionization, and the faint end of the galaxy luminosity function. In addition, it will provide unprecedented capability to monitor the X-ray variable sky, thus detecting, localizing, and identifying the electromagnetic counterparts to sources of gravitational radiation, which may be routinely detected in the late '20s / early '30s by next generation facilities like aLIGO/ aVirgo, eLISA, KAGRA, and Einstein Telescope. THESEUS will also provide powerful synergies with the next generation of multi-wavelength observatories (e.g., LSST, ELT, SKA, CTA, ATHENA)., Comment: Accepted for publication in Advances in Space Research. Partly based on the proposal submitted on October 2016 in response to the ESA Call for next M5 mission, with expanded and updated science sections
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- 2017
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26. Cherenkov Telescope Array Contributions to the 35th International Cosmic Ray Conference (ICRC2017)
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Acero, F., Acharya, B. S., Portella, V. Acín, Adams, C., Agudo, I., Aharonian, F., Samarai, I. Al, Alberdi, A., Alcubierre, M., Alfaro, R., Alfaro, J., Alispach, C., Aloisio, R., Batista, R. Alves, Amans, J. -P., Amato, E., Ambrogi, L., Ambrosi, G., Ambrosio, M., Anderson, J., Anduze, M., Angüner, E. O., Antolini, E., Antonelli, L. A., Antonuccio, V., Antoranz, P., Aramo, C., Araya, M., Arcaro, C., Armstrong, T., Arqueros, F., Arrabito, L., Arrieta, M., Asano, K., Asano, A., Ashley, M., Aubert, P., Singh, C. B., Babic, A., Backes, M., Bajtlik, S., Balazs, C., Balbo, M., Ballester, O., Ballet, J., Ballo, L., Balzer, A., Bamba, A., Bandiera, R., Barai, P., Barbier, C., Barcelo, M., Barkov, M., de Almeida, U. Barres, Barrio, J. A., Bastieri, D., Bauer, C., Becciani, U., Becherini, Y., Tjus, J. Becker, Bednarek, W., Belfiore, A., Benbow, W., Benito, M., Berge, D., Bernardini, E., Bernardini, M. G., Bernardos, M., Bernhard, S., Bernlöhr, K., Salucci, C. Bertinelli, Bertucci, B., Besel, M. -A., Beshley, V., Bettane, J., Bhatt, N., Bhattacharyya, W., Bhattachryya, S., Biasuzzi, B., Bicknell, G., Bigongiari, C., Biland, A., Bilinsky, A., Bird, R., Bissaldi, E., Biteau, J., Bitossi, M., Blanch, O., Blasi, P., Blazek, J., Boccato, C., Bockermann, C., Boehm, C., Bohacova, M., Boisson, C., Bolmont, J., Bonanno, G., Bonardi, A., Bonavolontà, C., Bonnoli, G., Borkowski, J., Bose, R., Bosnjak, Z., Böttcher, M., Boutonnet, C., Bouyjou, F., Bowman, L., Bozhilov, V., Braiding, C., Brau-Nogué, S., Bregeon, J., Briggs, M., Brill, A., Brisken, W., Bristow, D., Britto, R., Brocato, E., Brown, A. M., Brown, S., Brügge, K., Brun, P., Brun, F., Brunetti, L., Brunetti, G., Bruno, P., Bryan, M., Buckley, J., Bugaev, V., Bühler, R., Bulgarelli, A., Bulik, T., Burton, M., Burtovoi, A., Busetto, G., Buson, S., Buss, J., Byrum, K., Caccianiga, A., Cameron, R., Canelli, F., Canestrari, R., Capalbi, M., Capasso, M., Capitanio, F., Caproni, A., Capuzzo-Dolcetta, R., Caraveo, P., Cárdenas, V., Cardenzana, J., Cardillo, M., Carlile, C., Caroff, S., Carosi, R., Carosi, A., Carquín, E., Carr, J., Casandjian, J. -M., Casanova, S., Cascone, E., Castro-Tirado, A. J., Mora, J. Castroviejo, Catalani, F., Catalano, O., Cauz, D., Silva, C. Celestino, Celli, S., Cerruti, M., Chabanne, E., Chadwick, P., Chakraborty, N., Champion, C., Chatterjee, A., Chaty, S., Chaves, R., Chen, A., Chen, X., Cheng, K., Chernyakova, M., Chikawa, M., Chitnis, V. R., Christov, A., Chudoba, J., Cieślar, M., Clark, P., Coco, V., Colafrancesco, S., Colin, P., Colombo, E., Colome, J., Colonges, S., Conforti, V., Connaughton, V., Conrad, J., Contreras, J. L., Cornat, R., Cortina, J., Costa, A., Costantini, H., Cotter, G., Courty, B., Covino, S., Covone, G., Cristofari, P., Criswell, S. J., Crocker, R., Croston, J., Crovari, C., Cuadra, J., Cuevas, O., Cui, X., Cumani, P., Cusumano, G., D'Aì, A., D'Ammando, F., D'Avanzo, P., D'Urso, D., Da Vela, P., Dale, Ø., Dang, V. T., Dangeon, L., Daniel, M., Davids, I., Dawson, B., Dazzi, F., De Angelis, A., De Caprio, V., Anjos, R. de Cássia dos, De Cesare, G., De Franco, A., De Frondat, F., Pino, E. M. de Gouveia Dal, de la Calle, I., De Lisio, C., Lopez, R. de los Reyes, De Lotto, B., De Luca, A., De Lucia, M., Neto, J. R. T. de Mello, de Naurois, M., Wilhelmi, E. de Oña, De Palma, F., De Persio, F., de Souza, V., Decock, J., Deil, C., Deiml, P., Del Santo, M., Delagnes, E., Deleglise, G., Reznicek, M. Delfino, Delgado, C., Mengual, J. Delgado, Della Ceca, R., della Volpe, D., Detournay, M., Devin, J., Di Girolamo, T., Di Giulio, C., Di Pierro, F., Di Venere, L., Diaz, L., Díaz, C., Dib, C., Dickinson, H., Diebold, S., Digel, S., Djannati-Ataï, A., Doert, M., Domínguez, A., Prester, D. Dominis, Donnarumma, I., Dorner, D., Doro, M., Dournaux, J. -L., Downes, T., Drake, G., Drappeau, S., Drass, H., Dravins, D., Drury, L., Dubus, G., Morå, K. Dundas, Durkalec, A., Dwarkadas, V., Ebr, J., Eckner, C., Edy, E., Egberts, K., Einecke, S., Eisch, J., Eisenkolb, F., Ekoume, T. R. N., Eleftheriadis, C., Elsässer, D., Emmanoulopoulos, D., Ernenwein, J. -P., Escarate, P., Eschbach, S., Espinoza, C., Evans, P., Evoli, C., Fairbairn, M., Falceta-Goncalves, D., Falcone, A., Ramazani, V. 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J., Hassan, T., Haubold, T., Haupt, A., Hayashi, K., Hayashida, M., He, H., Heller, M., Helo, J. C., Henault, F., Henri, G., Hermann, G., Hermel, R., Llorente, J. Herrera, Herrero, A., Hervet, O., Hidaka, N., Hinton, J., Hiroshima, N., Hirotani, K., Hnatyk, B., Hoang, J. K., Hoffmann, D., Hofmann, W., Holder, J., Horan, D., Hörandel, J., Hörbe, M., Horns, D., Horvath, P., Houles, J., Hovatta, T., Hrabovsky, M., Hrupec, D., Huet, J. -M., Hughes, G., Hui, D., Hull, G., Humensky, T. B., Hussein, M., Hütten, M., Iarlori, M., Ikeno, Y., Illa, J. M., Impiombato, D., Inada, T., Ingallinera, A., Inome, Y., Inoue, S., Inoue, T., Inoue, Y., Iocco, F., Ioka, K., Ionica, M., Iori, M., Iriarte, A., Ishio, K., Israel, G. L., Iwamura, Y., Jablonski, C., Jacholkowska, A., Jacquemier, J., Jamrozy, M., Janecek, P., Jankowsky, F., Jankowsky, D., Jansweijer, P., Jarnot, C., Jean, P., Johnson, C. 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Mc, McHardy, I., Medina, C., Melandri, A., Melioli, C., Melkumyan, D., Mereghetti, S., Meunier, J. -L., Meures, T., Meyer, M., Micanovic, S., Michael, T., Michałowski, J., Mievre, I., Miller, J., Minaya, I. A., Mineo, T., Mirabel, F., Miranda, J. M., Mirzoyan, R., Mitchell, A., Mizuno, T., Moderski, R., Mohammed, M., Mohrmann, L., Molijn, C., Molinari, E., Moncada, R., Montaruli, T., Monteiro, I., Mooney, D., Moore, P., Moralejo, A., Morcuende-Parrilla, D., Moretti, E., Mori, K., Morlino, G., Morris, P., Morselli, A., Moscato, F., Motohashi, D., Moulin, E., Mueller, S., Mukherjee, R., Munar, P., Mundell, C., Mundet, J., Murach, T., Muraishi, H., Murase, K., Murphy, A., Nagai, A., Nagar, N., Nagataki, S., Nagayoshi, T., Nagesh, B. K., Naito, T., Nakajima, D., Nakamori, T., Nakamura, Y., Nakayama, K., Naumann, D., Nayman, P., Neise, D., Nellen, L., Nemmen, R., Neronov, A., Neyroud, N., Nguyen, T., Nguyen, T. T., Trung, T. 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J., Webb, N., Wegner, P., Weiner, O., Weinstein, A., Weniger, C., Werner, F., Wetteskind, H., White, M., White, R., Wierzcholska, A., Wiesand, S., Wijers, R., Wilcox, P., Wilhelm, A., Wilkinson, M., Will, M., Williams, D. A., Winter, M., Wojcik, P., Wolf, D., Wood, M., Wörnlein, A., Wu, T., Yadav, K. K., Yaguna, C., Yamamoto, T., Yamamoto, H., Yamane, N., Yamazaki, R., Yanagita, S., Yang, L., Yelos, D., Yoshida, T., Yoshida, M., Yoshiike, S., Yoshikoshi, T., Yu, P., Zaborov, D., Zacharias, M., Zaharijas, G., Zajczyk, A., Zampieri, L., Zandanel, F., Zanin, R., Sanchez, R. Zanmar, Zaric, D., Zavrtanik, M., Zavrtanik, D., Zdziarski, A. A., Zech, A., Zechlin, H., Zhdanov, V. I., Ziegler, A., Ziemann, J., Ziętara, K., Zink, A., Ziółkowski, J., Zitelli, V., Zoli, A., and Zorn, J.
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
List of contributions from the Cherenkov Telescope Array Consortium presented at the 35th International Cosmic Ray Conference, July 12-20 2017, Busan, Korea., Comment: Index of Cherenkov Telescope Array conference proceedings at the ICRC2017, Busan, Korea
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27. AGILE Observations of the Gravitational Wave Source GW170104
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Verrecchia, F., Tavani, M., Ursi, A., Argan, A., Pittori, C., Donnarumma, I., Bulgarelli, A., Fuschino, F., Labanti, C., Marisaldi, M., Evangelista, Y., Minervini, G., Giuliani, A., Cardillo, M., Longo, F., Lucarelli, F., Munar-Adrover, P., Piano, G., Pilia, M., Fioretti, V., Parmiggiani, N., Trois, A., Del Monte, E., Antonelli, L. A., Barbiellini, G., Caraveo, P., Cattaneo, P. W., Colafrancesco, S., Costa, E., D'Amico, F., Feroci, M., Ferrari, A., Morselli, A., Pacciani, L., Paoletti, F., Pellizzoni, A., Picozza, P., Rappoldi, A., and Vercellone, S.
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
The LIGO/Virgo Collaboration (LVC) detected on 2017 January 4, a significant gravitational-wave (GW) event (now named GW170104). We report in this Letter the main results obtained from the analysis of hard X-ray and gamma-ray data of the AGILE mission that repeatedly observed the GW170104 localization region (LR). At the LVC detection time $T_0$ AGILE observed about 36% of the LR. The gamma-ray imaging detector did not reveal any significant emission in the energy range 50 MeV--30 GeV. Furthermore, no significant gamma-ray transients were detected in the LR that was repeatedly exposed over timescales of minutes, hours, and days. We also searched for transient emission using data near $T_0$ of the omnidirectional detector MCAL operating in the energy band 0.4--100 MeV. A refined analysis of MCAL data shows the existence of a weak event (that we call "E2") with a signal-to-noise ratio of $4.4\,\sigma$ lasting about 32 ms and occurring $0.46\,\pm\,0.05 \,\rm s$ before $T_0$. A study of the MCAL background and of the false-alarm rate of E2 leads to the determinination of a post-trial significance between $2.4\,\sigma$ and $2.7\,\sigma$ for a temporal coincidence with GW170104. We note that E2 has characteristics similar to those detected from the weak precursor of the short GRB 090510. The candidate event E2 is worth consideration for simultaneous detection by other satellites. If associated with GW170104, it shows emission in the MeV band of a short burst preceding the final coalescence by 0.46 sec and involving $\sim 10^{-7}$ of the total rest mass energy of the system., Comment: Submitted to Astrophysical Journal Letters on 2017 May 31; revised 2017 July 19; accepted 2017 July 20
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28. A compact and modular X and gamma-ray detector with a CsI scintillator and double-readout Silicon Drift Detectors
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Campana, R., Fuschino, F., Labanti, C., Marisaldi, M., Amati, L., Fiorini, M., Uslenghi, M., Baldazzi, G., Bellutti, P., Evangelista, Y., Elmi, I., Feroci, M., Ficorella, F., Frontera, F., Picciotto, A., Piemonte, C., Rachevski, A., Rashevskaya, I., Rignanese, L. P., Vacchi, A., Zampa, G., Zampa, N., and Zorzi, N.
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Astrophysics - Instrumentation and Methods for Astrophysics ,Physics - Instrumentation and Detectors - Abstract
A future compact and modular X and gamma-ray spectrometer (XGS) has been designed and a series of prototypes have been developed and tested. The experiment envisages the use of CsI scintillator bars read out at both ends by single-cell 25 mm2 Silicon Drift Detectors. Digital algorithms are used to discriminate between events absorbed in the Silicon layer (lower energy X rays) and events absorbed in the scintillator crystal (higher energy X rays and gamma-rays). The prototype characterization is shown and the modular design for future experiments with possible astrophysical applications (e.g. for the THESEUS mission proposed for the ESA M5 call) are discussed., Comment: 10 pages, 11 figures. Published in Proceeding of SPIE Astronomical Telescopes and Instrumentation 2016
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29. Discerning TGF and Leader Current Pulse in ASIM Observation.
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Mezentsev, A., Østgaard, N., Marisaldi, M., Sarria, D., Lehtinen, N., Neubert, T., Chanrion, O., and Gordillo‐Vazquez, F.
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RADIO waves ,GAMMA rays ,OPTICAL sensors ,LIGHTNING - Abstract
Terrestrial gamma ray flash (TGF) observations made by the Atmosphere‐Space Interaction Monitor (ASIM) have demonstrated that these TGFs are accompanied by a prominent optical pulse from a hot leader channel. It is hard to confidently resolve the true sequence of the events in the source region due to temporal proximity of the involved processes. Here we report a bright long duration TGF together with its associated optical recordings showing clear temporal separation between the TGF and the optical pulse. In this observation the optical pulse is clearly distinct and subsequent relative to the TGF. The corresponding lightning discharge occurred at the very end of the TGF. We conclude that the current surge inside the lightning leader channel cannot be responsible for generation of this TGF. The current surge that produced the associated optical pulse can itself be conditioned by the TGF and may be responsible for the TGF termination. Plain Language Summary: TGFs observed from space are found to be associated with current surges in lightning leader channels. These current surges emit radio waves and can be detected with lightning detection networks. They also produce optical pulses which can be observed by the optical sensors on board of the space satellites. The fact that TGFs have usually short duration does not allow to define the real sequence of events in the source region due to timing uncertainties. In this paper we report a unique observation of a rare coincidence of a long duration TGF accompanied by an optical pulse and a high peak current lightning detection. Duration of the TGF is one order of magnitude larger than the overall observational uncertainty, which allows us to reliably discern the TGF and the accompanying current pulse in the leader channel. We could confidently conclude that the TGF was generated first, in the very end of the TGF the current surge in the leader channel occurred, and the optical pulse was produced. The appearance of the current surge close to the end of the TGF can indicate that the current surge is conditioned by the TGF, and, reciprocally, it could condition the TGF termination. Key Points: Accompanying optical pulse is subsequent to TGFTGF precedes the current surge in the leader channel and cannot be generated by this current surgeTGF may be terminated by the current surge in the leader channel [ABSTRACT FROM AUTHOR]
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- 2024
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30. Reducing the Use of Antibiotics in European Aquaculture with Vaccines, Functional Feed Additives and Optimization of the Gut Microbiota
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Seyed Hossein Hoseinifar, Ghasem Ashouri, Luca Marisaldi, Michela Candelma, Danilo Basili, Andrea Zimbelli, Valentina Notarstefano, Lucrezia Salvini, Basilio Randazzo, Matheo Zarantoniello, Andrea Pessina, Jerry Maria Sojan, Arturo Vargas, and Oliana Carnevali
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fish health ,environmental sustainability ,antibiotic resistance in aquaculture ,gut microbiota ,feed additives ,Naval architecture. Shipbuilding. Marine engineering ,VM1-989 ,Oceanography ,GC1-1581 - Abstract
This review presents several alternatives to replace antibiotic therapy and make the European aquaculture industry more friendly and environmentally sustainable. The first part of this review highlights the growing importance of the aquaculture industry worldwide for its ability to supply low-cost proteins and lipids. The second part discusses different strategies for these replacements, from recombinant vaccines to diets with low environmental impact and rich in bioactive molecules that can benefit other species. Specifically, the beneficial effects of bioactive compounds present within insect meals are discussed. In addition, particular focus is placed on the importance of adopting sustainable protocols for fish farming, including supplements such as probiotics, prebiotics, and synbiotics capable of modulating the gut microbiota as the second brain. Those feed additives can stimulate European farmed species’ immunological systems, growth, and welfare.
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- 2024
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31. New WMO Certified Megaflash Lightning Extremes for Flash Distance and Duration Recorded from Space
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Peterson, Michael J., Lang, Timothy J., Logan, Timothy, Kiong, Cheong Wee, Gijben, Morne, Holle, Ron, Kolmasova, Ivana, Marisaldi, Martino, Montanya, Joan, Pawar, Sunil D., Zhang, Daile, Brunet, Manola, and Cerveny, Randall S.
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Business ,Earth sciences - Abstract
Initial global extremes in lightning duration and horizontal distance were established in 2017 (Lang et al. 2016) by an international panel of atmospheric lightning scientists and engineers assembled by the [...]
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- 2022
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32. AGILE Gamma-Ray Detection of the Exceptional GRB 221009A
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Marco Tavani, Giovanni Piano, Andrea Bulgarelli, Luca Foffano, Alessandro Ursi, Francesco Verrecchia, Carlotta Pittori, Claudio Casentini, Andrea Giuliani, Francesco Longo, Gabriele Panebianco, Ambra Di Piano, Leonardo Baroncelli, Valentina Fioretti, Nicolò Parmiggiani, Andrea Argan, Alessio Trois, Stefano Vercellone, Martina Cardillo, Lucio Angelo Antonelli, Guido Barbiellini, Patrizia Caraveo, Paolo W. Cattaneo, Andrew W. Chen, Enrico Costa, Ettore Del Monte, Guido Di Cocco, Immacolata Donnarumma, Yuri Evangelista, Marco Feroci, Fulvio Gianotti, Claudio Labanti, Francesco Lazzarotto, Paolo Lipari, Fabrizio Lucarelli, Martino Marisaldi, Sandro Mereghetti, Aldo Morselli, Luigi Pacciani, Alberto Pellizzoni, Francesco Perotti, Piergiorgio Picozza, Maura Pilia, Massimo Rapisarda, Andrea Rappoldi, Alda Rubini, Paolo Soffitta, Massimo Trifoglio, Valerio Vittorini, and Fabio D’Amico
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Gamma-ray bursts ,Gamma-ray astronomy ,Gamma-ray observatories ,Astrophysics ,QB460-466 - Abstract
Gamma-ray emission in the MeV–GeV range from explosive cosmic events is of invaluable relevance to understanding physical processes related to the formation of neutron stars and black holes. Here we report on the detection by the AGILE satellite in the MeV–GeV energy range of the remarkable long-duration gamma-ray burst GRB 221009A. The AGILE onboard detectors have good exposure to GRB 221009A during its initial crucial phases. Hard X-ray/MeV emission in the prompt phase lasted hundreds of seconds, with the brightest radiation being emitted between 200 and 300 s after the initial trigger. Very intense GeV gamma-ray emission is detected by AGILE in the prompt and early afterglow phase up to 10,000 s. Time-resolved spectral analysis shows time-variable MeV-peaked emission simultaneous with intense power-law GeV radiation that persists in the afterglow phase. The coexistence during the prompt phase of very intense MeV emission together with highly nonthermal and hardening GeV radiation is a remarkable feature of GRB 221009A. During the prompt phase, the event shows spectrally different MeV and GeV emissions that are most likely generated by physical mechanisms occurring in different locations. AGILE observations provide crucial flux and spectral gamma-ray information regarding the early phases of GRB 221009A during which emission in the TeV range was reported.
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- 2023
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33. Very-high-frequency oscillations in the main peak of a magnetar giant flare
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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., and Yang, S.
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- 2021
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34. The e-ASTROGAM mission (exploring the extreme Universe with gamma rays in the MeV-GeV range)
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De Angelis, Alessandro, Tatischeff, Vincent, Tavani, Marco, Oberlack, Uwe, Grenier, Isabelle A., Hanlon, Lorraine, Walter, Roland, Argan, Andrea, von Ballmoos, Peter, Bulgarelli, Andrea, Donnarumma, Immacolata, Hernanz, Margarita, Kuvvetli, Irfan, Pearce, Mark, Zdziarski, Andrzej, Aboudan, Alessio, Ajello, Marco, Ambrosi, Giovanni, Bernard, Denis, Bernardini, Elisa, Bonvicini, Valter, Brogna, Andrea, Branchesi, Marica, Budtz-Jorgensen, Carl, Bykov, Andrei, Campana, Riccardo, Cardillo, Martina, Coppi, Paolo, De Martino, Domitilla, Diehl, Roland, Doro, Michele, Fioretti, Valentina, Funk, Stefan, Ghisellini, Gabriele, Grove, J. Eric, Hamadache, Clarisse, Hartmann, Dieter H., Hayashida, Masaaki, Isern, Jordi, Kanbach, Gottfried, Kiener, Jurgen, Knodlseder, Jurgen, Labanti, Claudio, Laurent, Philippe, Limousin, Olivier, Longo, Francesco, Mannheim, Karl, Marisaldi, Martino, Martinez, Manel, Mazziotta, Mario N., McEnery, Julie, Mereghetti, Sandro, Minervini, Gabriele, Moiseev, Alexander, Morselli, Aldo, Nakazawa, Kazuhiro, Orleanski, Piotr, Paredes, Josep M., Patricelli, Barbara, Peyre, Jean, Piano, Giovanni, Pohl, Martin, Ramarijaona, Harald, Rando, Riccardo, Reichardt, Ignasi, Roncadelli, Marco, da Silva, Rui Curado, Tavecchio, Fabrizio, Thompson, David J., Turolla, Roberto, Ulyanov, Alexei, Vacchi, Andrea, Wu, Xin, and Zoglauer, Andreas
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Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Solar and Stellar Astrophysics ,Nuclear Experiment - Abstract
e-ASTROGAM (`enhanced ASTROGAM') is a breakthrough Observatory mission dedicated to the study of the non-thermal Universe in the photon energy range from 0.3 MeV to 3 GeV. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with polarimetric capability. In the largely unexplored MeV-GeV domain, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on Galactic ecosystems. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous generation instruments, will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LIGO-Virgo-GEO600-KAGRA, SKA, ALMA, E-ELT, TMT, LSST, JWST, Athena, CTA, IceCube, KM3NeT, and the promise of eLISA. Keywords: High-energy gamma-ray astronomy, High-energy astrophysics, Nuclear Astrophysics, Compton and Pair creation telescope, Gamma-ray bursts, Active Galactic Nuclei, Jets, Outflows, Multiwavelength observations of the Universe, Counterparts of gravitational waves, Fermi, Dark Matter, Nucleosynthesis, Early Universe, Supernovae, Cosmic Rays, Cosmic antimatter., Comment: Exp Astron (2017)
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- 2016
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35. Contributions of the Cherenkov Telescope Array (CTA) to the 6th International Symposium on High-Energy Gamma-Ray Astronomy (Gamma 2016)
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Consortium, The CTA, Abchiche, A., Abeysekara, U., Abril, Ó., Acero, F., Acharya, B. S., Adams, C., Agnetta, G., Aharonian, F., Akhperjanian, A., Albert, A., Alcubierre, M., Alfaro, J., Alfaro, R., Allafort, A. J., Aloisio, R., Amans, J. -P., Amato, E., Ambrogi, L., Ambrosi, G., Ambrosio, M., Anderson, J., Anduze, M., Angüner, E. O., Antolini, E., Antonelli, L. A., Antonucci, M., Antonuccio, V., Antoranz, P., Aramo, C., Aravantinos, A., Araya, M., Arcaro, C., Arezki, B., Argan, A., Armstrong, T., Arqueros, F., Arrabito, L., Arrieta, M., Asano, K., Ashley, M., Aubert, P., Singh, C. B., Babic, A., Backes, M., Bais, A., Bajtlik, S., Balazs, C., Balbo, M., Balis, D., Balkowski, C., Ballester, O., Ballet, J., Balzer, A., Bamba, A., Bandiera, R., Barber, A., Barbier, C., Barcelo, M., Barkov, M., Barnacka, A., de Almeida, U. Barres, Barrio, J. A., Basso, S., Bastieri, D., Bauer, C., Becciani, U., Becherini, Y., Tjus, J. Becker, Beckmann, V., Bednarek, W., Benbow, W., Ventura, D. Benedico, Berdugo, J., Berge, D., Bernardini, E., Bernardini, M. G., Bernhard, S., Bernlöhr, K., Bertucci, B., Besel, M. -A., Beshley, V., Bhatt, N., Bhattacharjee, P., Bhattacharyya, W., Bhattachryya, S., Biasuzzi, B., Bicknell, G., Bigongiari, C., Biland, A., Bilinsky, A., Bilnik, W., Biondo, B., Bird, R., Bird, T., Bissaldi, E., Bitossi, M., Blanch, O., Blasi, P., Blazek, J., Bockermann, C., Boehm, C., Bogacz, L., Bogdan, M., Bohacova, M., Boisson, C., Boix, J., Bolmont, J., Bonanno, G., Bonardi, A., Bonavolontà, C., Bonifacio, P., Bonnarel, F., Bonnoli, G., Borkowski, J., Bose, R., Bosnjak, Z., Böttcher, M., Bousquet, J. -J., Boutonnet, C., Bouyjou, F., Bowman, L., Braiding, C., Brantseg, T., Brau-Nogué, S., Bregeon, J., Briggs, M., Brigida, M., Bringmann, T., Brisken, W., Bristow, D., Britto, R., Brocato, E., Bron, S., Brook, P., Brooks, W., Brown, A. M., Brügge, K., Brun, F., Brun, P., Brunetti, G., Brunetti, L., Bruno, P., Buanes, T., Bucciantini, N., Buchholtz, G., Buckley, J., Bugaev, V., Bühler, R., Bulgarelli, A., Bulik, T., Burton, M., Burtovoi, A., Busetto, G., Buson, S., Buss, J., Byrum, K., Cadoux, F., Tovar, J. Calvo, Cameron, R., Canelli, F., Canestrari, R., Capalbi, M., Capasso, M., Capobianco, G., Caproni, A., Caraveo, P., Cardenzana, J., Cardillo, M., Carius, S., Carlile, C., Carosi, A., Carosi, R., Carquín, E., Carr, J., Carroll, M., Carter, J., Carton, P. -H., Casandjian, J. -M., Casanova, S., Cascone, E., Casiraghi, M., Castellina, A., Mora, J. Castroviejo, Catalani, F., Catalano, O., Catalanotti, S., Cauz, D., Cavazzani, S., Cerchiara, P., Chabanne, E., Chadwick, P., Chaleil, T., Champion, C., Chatterjee, A., Chaty, S., Chaves, R., Chen, A., Chen, X., Cheng, K., Chernyakova, M., Chiappetti, L., Chikawa, M., Chinn, D., Chitnis, V. R., Cho, N., Christov, A., Chudoba, J., Cieślar, M., Ciocci, M. A., Clay, R., Colafrancesco, S., Colin, P., Colley, J. -M., Colombo, E., Colome, J., Colonges, S., Conforti, V., Connaughton, V., Connell, S., Conrad, J., Contreras, J. L., Coppi, P., Corbel, S., Coridian, J., Cornat, R., Corona, P., Corti, D., Cortina, J., Cossio, L., Costa, A., Costantini, H., Cotter, G., Courty, B., Covino, S., Covone, G., Crimi, G., Criswell, S. J., Crocker, R., Croston, J., Cuadra, J., Cumani, P., Cusumano, G., Da Vela, P., Dale, Ø., D'Ammando, F., Dang, D., Dang, V. T., Dangeon, L., Daniel, M., Davids, I., Dawson, B., Dazzi, F., Costa, B. de Aguiar, De Angelis, A., Cardoso, R. F. de Araujo, De Caprio, V., Anjos, R. de Cássia dos, De Cesare, G., De Franco, A., De Frondat, F., Pino, E. M. de Gouveia Dal, de la Calle, I., De Lisio, C., Lopez, R. de los Reyes, De Lotto, B., De Luca, A., Neto, J. R. T. de Mello, de Naurois, M., Wilhelmi, E. de Oña, De Palma, F., De Persio, F., de Souza, V., Decock, G., Decock, J., Deil, C., Del Santo, M., Delagnes, E., Deleglise, G., Delgado, C., Delgado, J., della Volpe, D., Deloye, P., Detournay, M., Dettlaff, A., Devin, J., Di Girolamo, T., Di Giulio, C., Di Paola, A., Di Pierro, F., Diaz, M. A., Díaz, C., Dib, C., Dick, J., Dickinson, H., Diebold, S., Digel, S., Dipold, J., Disset, G., Distefano, A., Djannati-Ataï, A., Doert, M., Dohmke, M., Domínguez, A., Dominik, N., Dominique, J. -L., Prester, D. Dominis, Donat, A., Donnarumma, I., Dorner, D., Doro, M., Dournaux, J. -L., Downes, T., Doyle, K., Drake, G., Drappeau, S., Drass, H., Dravins, D., Drury, L., Dubus, G., Ducci, L., Dumas, D., Morå, K. Dundas, Durand, D., D'Urso, D., Dwarkadas, V., Dyks, J., Dyrda, M., Ebr, J., Edy, E., Egberts, K., Eger, P., Egorov, A., Einecke, S., Eisch, J., Eisenkolb, F., Eleftheriadis, C., Elsaesser, D., Elsässer, D., Emmanoulopoulos, D., Engelbrecht, C., Engelhaupt, D., Ernenwein, J. -P., Escarate, P., Eschbach, S., Espinoza, C., Evans, P., Fairbairn, M., Falceta-Goncalves, D., Falcone, A., Ramazani, V. Fallah, Fantinel, D., Farakos, K., Farnier, C., Farrell, E., Fasola, G., Favre, Y., Fede, E., Fedora, R., Fedorova, E., Fegan, S., Ferenc, D., Fernandez-Alonso, M., Fernández-Barral, A., Ferrand, G., Ferreira, O., Fesquet, M., Fetfatzis, P., Fiandrini, E., Fiasson, A., Filipčič, A., Filipovic, M., Fink, D., Finley, C., Finley, J. P., Finoguenov, A., Fioretti, V., Fiorini, M., Fleischhack, H., Flores, H., Florin, D., Föhr, C., Fokitis, E., Fonseca, M. V., Font, L., Fontaine, G., Fontes, B., Fornasa, M., Förster, A., Fortin, P., Fortson, L., Fouque, N., Franckowiak, A., Franco, F. J., Albuquerque, I. Freire Mota, Coromina, L. Freixas, Fresnillo, L., Fruck, C., Fuessling, M., Fugazza, D., Fujita, Y., Fukami, S., Fukazawa, Y., Fukuda, T., Fukui, Y., Funk, S., Furniss, A., Gäbele, W., Gabici, S., Gadola, A., Galindo, D., Gall, D. D., Gallant, Y., Galloway, D., Gallozzi, S., Galvez, J. A., Gao, S., Garcia, A., Garcia, B., Gil, R. García, López, R. Garcia, Garczarczyk, M., Gardiol, D., Gargano, C., Gargano, F., Garozzo, S., Garrecht, F., Garrido, L., Garrido-Ruiz, M., Gascon, D., Gaskins, J., Gaudemard, J., Gaug, M., Gaweda, J., Gebhardt, B., Gebyehu, M., Geffroy, N., Genolini, B., Gerard, L., Ghalumyan, A., Ghedina, A., Ghislain, P., Giammaria, P., Giannakaki, E., Gianotti, F., Giarrusso, S., Giavitto, G., Giebels, B., Gieras, T., Giglietto, N., Gika, V., Gimenes, R., Giomi, M., Giommi, P., Giordano, F., Giovannini, G., Girardot, P., Giro, E., Giroletti, M., Gironnet, J., Giuliani, A., Glicenstein, J. -F., Gnatyk, R., Godinovic, N., Goldoni, P., Gomez, G., Gonzalez, M. M., González, A., Gora, D., Gothe, K. S., Gotz, D., Goullon, J., Grabarczyk, T., Graciani, R., Graham, J., Grandi, P., Granot, J., Grasseau, G., Gredig, R., Green, A. J., Green, A. M., Greenshaw, T., Grenier, I., Griffiths, S., Grillo, A., Grondin, M. -H., Grube, J., Grudzinska, M., Grygorczuk, J., Guarino, V., Guberman, D., Gunji, S., Gyuk, G., Hadasch, D., Hagedorn, A., Hagge, L., Hahn, J., Hakobyan, H., Hara, S., Hardcastle, M. J., Hassan, T., Hatanaka, K., Haubold, T., Haupt, A., Hayakawa, T., Hayashida, M., Heller, M., Heller, R., Helo, J. C., Henault, F., Henri, G., Hermann, G., Hermel, R., Llorente, J. Herrera, Herrero, A., Hervet, O., Hidaka, N., Hinton, J., Hirai, W., Hirotani, K., Hnatyk, B., Hoang, J., Hoffmann, D., Hofmann, W., Holch, T., Holder, J., Hooper, S., Horan, D., Hörandel, J., Hörbe, M., Horns, D., Horvath, P., Hose, J., Houles, J., Hovatta, T., Hrabovsky, M., Hrupec, D., Huet, J. -M., Huetten, M., Hughes, G., Hui, D., Humensky, T. B., Hussein, M., Iacovacci, M., Ibarra, A., Ikeno, Y., Illa, J. M., Impiombato, D., Inada, T., Incorvaia, S., Infante, L., Inome, Y., Inoue, S., Inoue, T., Inoue, Y., Iocco, F., Ioka, K., Iori, M., Ishio, K., Israel, G. L., Iwamura, Y., Jablonski, C., Jacholkowska, A., Jacquemier, J., Jamrozy, M., Janecek, P., Janiak, M., Jankowsky, D., Jankowsky, F., Jean, P., Jegouzo, I., Jenke, P., Jimenez, J. J., Jingo, M., Jocou, L., Jogler, T., Johnson, C. A., Jones, M., Josselin, M., Journet, L., Jung, I., Kaaret, P., Kagaya, M., Kakuwa, J., Kalekin, O., Kalkuhl, C., Kamon, H., Kankanyan, R., Karastergiou, A., Kärcher, K., Karczewski, M., Karkar, S., Karn, P., Kasperek, J., Katagiri, H., Kataoka, J., Katarzyński, K., Kato, S., Katz, U., Kawanaka, N., Kaye, L., Kazanas, D., Kelley-Hoskins, N., Kersten, J., Khélifi, B., Kieda, D. B., Kihm, T., Kimeswenger, S., Kisaka, S., Kishida, S., Kissmann, R., Klepser, S., Kluźniak, W., Knapen, J., Knapp, J., Knödlseder, J., Koch, B., Köck, F., Kocot, J., Kohri, K., Kokkotas, K., Kolitzus, D., Komin, N., Kominis, I., Kong, A., Konno, Y., Kosack, K., Koss, G., Kossatz, M., Kowal, G., Koyama, S., Kozioł, J., Kraus, M., Krause, J., Krause, M., Krawzcynski, H., Krennrich, F., Kretzschmann, A., Kruger, P., Kubo, H., Kudryavtsev, V., Mezek, G. Kukec, Kuklis, M., Kuroda, H., Kushida, J., La Barbera, A., La Palombara, N., La Parola, V., La Rosa, G., Laffon, H., Lahmann, R., Lakicevic, M., Lalik, K., Lamanna, G., Landriu, D., Landt, H., Lang, R. G., Lapington, J., Laporte, P., Fèvre, J. -P. Le, Flour, T. Le, Sidaner, P. Le, Lee, S. -H., Lee, W. H., Lees, J. -P., Lefaucheur, J., Leffhalm, K., Leich, H., de Oliveira, M. A. Leigui, Lelas, D., Lemière, A., Lemoine-Goumard, M., Lenain, J. -P., Leonard, R., Leoni, R., Lessio, L., Leto, G., Leveque, A., Lieunard, B., Limon, M., Lindemann, R., Lindfors, E., Linhoff, L., Liolios, A., Lipniacka, A., Lockart, H., Lohse, T., Łokas, E., Lombardi, S., Longo, F., Lopatin, A., Lopez, M., Loreggia, D., Louge, T., Louis, F., Louys, M., Lucarelli, F., Lucchesi, D., Lüdecke, H., Luigi, T., Luque-Escamilla, P. L., Lyard, E., Maccarone, M. C., Maccarone, T., Maccarone, T. J., Mach, E., Madejski, G. M., Madonna, A., Magniette, F., Magniez, A., Mahabir, M., Maier, G., Majumdar, P., Makariev, M., Malaguti, G., Malaspina, G., Mallot, A. K., Malouf, A., Maltezos, S., Malyshev, D., Mancilla, A., Mandat, D., Maneva, G., Manganaro, M., Mangano, S., Manigot, P., Mankushiyil, N., Mannheim, K., Maragos, N., Marano, D., Marchegiani, P., Marcomini, J. A., Marcowith, A., Mariotti, M., Marisaldi, M., Markoff, S., Martens, C., Martí, J., Martin, J. -M., Martin, L., Martin, P., Martínez, G., Martínez, M., Martínez, O., Martynyuk-Lototskyy, K., Marx, R., Masetti, N., Massimino, P., Mastichiadis, A., Mastroianni, S., Mastropietro, M., Masuda, S., Matsumoto, H., Matsuoka, S., Matthews, N., Mattiazzo, S., Maurin, G., Maxted, N., Maya, J., Mayer, M., Mazin, D., Mazziotta, M. N., Comb, L. Mc, McCubbin, N., McHardy, I., Medina, C., Mehrez, F., Melioli, C., Melkumyan, D., Melse, T., Mereghetti, S., Merk, M., Mertsch, P., Meunier, J. -L., Meures, T., Meyer, M., Meyrelles jr, J. L., Miccichè, A., Michael, T., Michałowski, J., Mientjes, P., Mievre, I., Mihailidis, A., Miller, J., Mineo, T., Minuti, M., Mirabal, N., Mirabel, F., Miranda, J. M., Mirzoyan, R., Mitchell, A., Mizuno, T., Moderski, R., Mognet, I., Mohammed, M., Moharana, R., Mohrmann, L., Molinari, E., Molyneux, P., Monmarthe, E., Monnier, G., Montaruli, T., Monte, C., Monteiro, I., Mooney, D., Moore, P., Moralejo, A., Morello, C., Moretti, E., Mori, K., Morris, P., Morselli, A., Moscato, F., Motohashi, D., Mottez, F., Moudden, Y., Moulin, E., Mueller, S., Mukherjee, R., Munar, P., Munari, M., Mundell, C., Mundet, J., Muraishi, H., Murase, K., Muronga, A., Murphy, A., Nagar, N., Nagataki, S., Nagayoshi, T., Nagesh, B. K., Naito, T., Nakajima, D., Nakamori, T., Nakayama, K., Nanni, J., Naumann, D., Nayman, P., Nellen, L., Nemmen, R., Neronov, A., Neyroud, N., Nguyen, T., Nguyen, T. T., Trung, T. Nguyen, Nicastro, L., Nicolau-Kukliński, J., Niederwanger, F., Niedźwiecki, A., Niemiec, J., Nieto, D., Nievas-Rosillo, M., Nikolaidis, A., Nikołajuk, M., Nishijima, K., Nishikawa, K. -I., Nishiyama, G., Noda, K., Nogues, L., Nolan, S., Northrop, R., Nosek, D., Nöthe, M., Novosyadlyj, B., Nozka, L., Nunio, F., Oakes, L., O'Brien, P., Ocampo, C., Occhipinti, G., Ochoa, J. P., de Bhroithe, A. OFaolain, Oger, R., Ohira, Y., Ohishi, M., Ohm, S., Ohoka, H., Okazaki, N., Okumura, A., Olive, J. -F., Olszowski, D., Ong, R. A., Ono, S., Orienti, M., Orito, R., Orlati, A., Osborne, J., Ostrowski, M., Ottaway, D., Otte, N., Öttl, S., Ovcharov, E., Oya, I., Ozieblo, A., Padovani, M., Pagano, I., Paiano, S., Paizis, A., Palacio, J., Palatka, M., Pallotta, J., Panagiotidis, K., Panazol, J. -L., Paneque, D., Panter, M., Panzera, M. R., Paoletti, R., Paolillo, M., Papayannis, A., Papyan, G., Paravac, A., Paredes, J. M., Pareschi, G., Park, N., Parsons, D., Paśko, P., Pavy, S., Pech, M., Peck, A., Pedaletti, G., Pe'er, A., Peet, S., Pelat, D., Pepato, A., Perez, M. d. C., Perri, L., Perri, M., Persic, M., Petrashyk, A., Petrucci, P. -O., Petruk, O., Peyaud, B., Pfeifer, M., Pfeiffer, G., Piano, G., Pieloth, D., Pierre, E., de Pinho, F. Pinto, García, C. Pio, Piret, Y., Pisarski, A., Pita, S., Platos, Ł., Platzer, R., Podkladkin, S., Pogosyan, L., Pohl, M., Poinsignon, P., Pollo, A., Porcelli, A., Porthault, J., Potter, W., Poulios, S., Poutanen, J., Prandini, E., Prast, J., Pressard, K., Principe, G., Profeti, F., Prokhorov, D., Prokoph, H., Prouza, M., Pruchniewicz, R., Pruteanu, G., Pueschel, E., Pühlhofer, G., Puljak, I., Punch, M., Pürckhauer, S., Pyzioł, R., Queiroz, F., Quel, E. J., Quinn, J., Quirrenbach, A., Rafighi, I., Rainò, S., Rajda, P. J., Rameez, M., Rando, R., Rannot, R. C., Rataj, M., Ravel, T., Razzaque, S., Reardon, P., Reichardt, I., Reimann, O., Reimer, A., Reimer, O., Reisenegger, A., Renaud, M., Renner, S., Reposeur, T., Reville, B., Rezaeian, A., Rhode, W., Ribeiro, D., Prado, R. Ribeiro, Ribó, M., Richards, G., Richer, M. G., Richtler, T., Rico, J., Ridky, J., Rieger, F., Riquelme, M., Ristori, P. R., Rivoire, S., Rizi, V., Roache, E., Rodriguez, J., Fernandez, G. Rodriguez, Vázquez, J. J. Rodríguez, Rojas, G., Romano, P., Romeo, G., Roncadelli, M., Rosado, J., Rose, J., Rosen, S., Lees, S. Rosier, Ross, D., Rouaix, G., Rousselle, J., Rovero, A. C., Rowell, G., Roy, F., Royer, S., Rubini, A., Rudak, B., Rugliancich, A., Rujopakarn, W., Rulten, C., Rupiński, M., Russo, F., Rutkowski, K., Saavedra, O., Sabatini, S., Sacco, B., Sadeh, I., Saemann, E. O., Safi-Harb, S., Saggion, A., Sahakian, V., Saito, T., Sakaki, N., Sakurai, S., Salamon, A., Salega, M., Salek, D., Greus, F. Salesa, Salgado, J., Salina, G., Salinas, L., Salini, A., Sanchez, D., Sanchez-Conde, M., Sandaker, H., Sandoval, A., Sangiorgi, P., Sanguillon, M., Sano, H., Santander, M., Santangelo, A., Santos, E. M., Santos-Lima, R., Sanuy, A., Sapozhnikov, L., Sarkar, S., Satalecka, K., Sato, Y., Savalle, R., Sawada, M., Sayède, F., Schanne, S., Schanz, T., Schioppa, E. J., Schlenstedt, S., Schmid, J., Schmidt, T., Schmoll, J., Schneider, M., Schoorlemmer, H., Schovanek, P., Schubert, A., Schullian, E. -M., Schultze, J., Schulz, A., Schulz, S., Schure, K., Schussler, F., Schwab, T., Schwanke, U., Schwarz, J., Schweizer, T., Schwemmer, S., Schwendicke, U., Schwerdt, C., Sciacca, E., Scuderi, S., Segreto, A., Seiradakis, J. -H., Sembroski, G. H., Semikoz, D., Sergijenko, O., Serre, N., Servillat, M., Seweryn, K., Shafi, N., Shalchi, A., Sharma, M., Shayduk, M., Shellard, R. C., Shibata, T., Shigenaka, A., Shilon, I., Shum, E., Sidoli, L., Sidz, M., Sieiro, J., Siejkowski, H., Silk, J., Sillanpää, A., Simone, D., Simpson, H., Singh, B. B., Sinha, A., Sironi, G., Sitarek, J., Sizun, P., Sliusar, V., Smith, A., Sobczyńska, D., Sol, H., Sottile, G., Sowiński, M., Spanier, F., Spengler, G., Spiga, R., Stadler, R., Stahl, O., Stamerra, A., Stanič, S., Starling, R., Staszak, D., Stawarz, Ł., Steenkamp, R., Stefanik, S., Stegmann, C., Steiner, S., Stella, C., Stephan, M., Stergioulas, N., Sternberger, R., Sterzel, M., Stevenson, B., Stinzing, F., Stodulska, M., Stodulski, M., Stolarczyk, T., Stratta, G., Straumann, U., Stringhetti, L., Strzys, M., Stuik, R., Sulanke, K. -H., Suomijärvi, T., Supanitsky, A. D., Suric, T., Sushch, I., Sutcliffe, P., Sykes, J., Szanecki, M., Szepieniec, T., Szwarnog, P., Tacchini, A., Tachihara, K., Tagliaferri, G., Tajima, H., Takahashi, H., Takahashi, K., Takahashi, M., Takalo, L., Takami, S., Takata, J., Takeda, J., Talbot, G., Tam, T., Tanaka, M., Tanaka, S., Tanaka, T., Tanaka, Y., Tanci, C., Tanigawa, S., Tavani, M., Tavecchio, F., Tavernet, J. -P., Tayabaly, K., Taylor, A., Tejedor, L. A., Telezhinsky, I., Temme, F., Temnikov, P., Tenzer, C., Terada, Y., Terrazas, J. C., Terrier, R., Terront, D., Terzic, T., Tescaro, D., Teshima, M., Testa, V., Tezier, D., Thayer, J., Thornhill, J., Thoudam, S., Thuermann, D., Tibaldo, L., Tiengo, A., Timpanaro, M. C., Tiziani, D., Tluczykont, M., Peixoto, C. J. Todero, Tokanai, F., Tokarz, M., Toma, K., Tomastik, J., Tomono, Y., Tonachini, A., Tonev, D., Torii, K., Tornikoski, M., Torres, D. F., Torres, M., Torresi, E., Toso, G., Tosti, G., Totani, T., Tothill, N., Toussenel, F., Tovmassian, G., Toyama, T., Travnicek, P., Trichard, C., Trifoglio, M., Pujadas, I. Troyano, Trzeciak, M., Tsinganos, K., Tsujimoto, S., Tsuru, T., Uchiyama, Y., Umana, G., Umetsu, Y., Upadhya, S. S., Uslenghi, M., Vagelli, V., Vagnetti, F., Valdes-Galicia, J., Valentino, M., Vallania, P., Valore, L., van Driel, W., van Eldik, C., van Soelen, B., Vandenbroucke, J., Vanderwalt, J., Vasileiadis, G., Vassiliev, V., Vázquez, J. R., Acosta, M. L. Vázquez, Vecchi, M., Vega, A., Vegas, I., Veitch, P., Venault, P., Venema, L., Venter, C., Vercellone, S., Vergani, S., Verma, K., Verzi, V., Vettolani, G. P., Veyssiere, C., Viana, A., Viaux, N., Vicha, J., Vigorito, C., Vincent, P., Vincent, S., Vink, J., Vittorini, V., Vlahakis, N., Vlahos, L., Voelk, H., Voisin, V., Vollhardt, A., Volpicelli, A., von Brand, H., Vorobiov, S., Vovk, I., Vrastil, M., Vu, L. V., Vuillaume, T., Wagner, R., Wagner, S. J., Wakely, S. P., Walstra, T., Walter, R., Walther, T., Ward, J. E., Ward, M., Warda, K., Warren, D., Wassberg, S., Watson, J. J., Wawer, P., Wawrzaszek, R., Webb, N., Wegner, P., Weiner, O., Weinstein, A., Wells, R., Werner, F., Wetteskind, H., White, M., White, R., Więcek, M., Wierzcholska, A., Wiesand, S., Wijers, R., Wilcox, P., Wild, N., Wilhelm, A., Wilkinson, M., Will, M., Williams, D. A., Williams, J. T., Willingale, R., Wilson, N., Winde, M., Winiarski, K., Winkler, H., Winter, M., Wischnewski, R., Witt, E., Wojcik, P., Wolf, D., Wood, M., Wörnlein, A., Wu, E., Wu, T., Yadav, K. K., Yamamoto, H., Yamamoto, T., Yamane, N., Yamazaki, R., Yanagita, S., Yang, L., Yelos, D., Yoshida, A., Yoshida, M., Yoshida, T., Yoshiike, S., Yoshikoshi, T., Yu, P., Zabalza, V., Zaborov, D., Zacharias, M., Zaharijas, G., Zajczyk, A., Zampieri, L., Zandanel, F., Sanchez, R. Zanmar, Zaric, D., Zavrtanik, D., Zavrtanik, M., Zdziarski, A., Zech, A., Zechlin, H., Zhao, A., Zhdanov, V., Ziegler, A., Ziemann, J., Ziętara, K., Zink, A., Ziółkowski, J., Zitelli, V., Zoli, A., Zorn, J., and Żychowski, P.
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
List of contributions from the Cherenkov Telescope Array (CTA) Consortium presented at the 6th International Symposium on High-Energy Gamma-Ray Astronomy (Gamma 2016), July 11-15, 2016, in Heidelberg, Germany., Comment: Index of CTA conference proceedings for the Gamma 2016, Heidelberg, Germany
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36. The e-ASTROGAM gamma-ray space mission
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Tatischeff, V., Tavani, M., von Ballmoos, P., Hanlon, L., Oberlack, U., Aboudan, A., Argan, A., Bernard, D., Brogna, A., Bulgarelli, A., Bykov, A., Campana, R., Caraveo, P., Cardillo, M., Coppi, P., De Angelis, A., Diehl, R., Donnarumma, I., Fioretti, V., Giuliani, A., Grenier, I., Grove, J. E., Hamadache, C., Hartmann, D., Hernanz, M., Isern, J., Kanbach, G., Kiener, J., Knödlseder, J., Labanti, C., Laurent, P., Limousin, O., Longo, F., Marisaldi, M., McBreen, S., McEnery, J. E., Mereghetti, S., Mirabel, F., Morselli, A., Nakazawa, K., Peyré, J., Piano, G., Pittori, C., Sabatini, S., Stawarz, L., Thompson, D. J., Ulyanov, A., Walter, R., Wu, X., Zdziarski, A., and Zoglauer, A.
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Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
The e-ASTROGAM is a gamma-ray space mission to be proposed as the M5 Medium-size mission of the European Space Agency. It is dedicated to the observation of the Universe with unprecedented sensitivity in the energy range 0.2 - 100 MeV, extending up to GeV energies, together with a groundbreaking polarization capability. It is designed to substantially improve the COMPTEL and Fermi sensitivities in the MeV-GeV energy range and to open new windows of opportunity for astrophysical and fundamental physics space research. e-ASTROGAM will operate as an open astronomical observatory, with a core science focused on (1) the activity from extreme particle accelerators, including gamma-ray bursts and active galactic nuclei and the link of jet astrophysics to the new astronomy of gravitational waves, neutrinos, ultra-high energy cosmic rays, (2) the high-energy mysteries of the Galactic center and inner Galaxy, including the activity of the supermassive black hole, the Fermi Bubbles, the origin of the Galactic positrons, and the search for dark matter signatures in a new energy window; (3) nucleosynthesis and chemical evolution, including the life cycle of elements produced by supernovae in the Milky Way and the Local Group of galaxies. e-ASTROGAM will be ideal for the study of high-energy sources in general, including pulsars and pulsar wind nebulae, accreting neutron stars and black holes, novae, supernova remnants, and magnetars. And it will also provide important contributions to solar and terrestrial physics. The e-ASTROGAM telescope is optimized for the simultaneous detection of Compton and pair-producing gamma-ray events over a large spectral band. It is based on a very high technology readiness level for all subsystems and includes many innovative features for the detectors and associated electronics., Comment: 11 pages, 5 figures, published in the proceedings of SPIE Astronomical Telescopes and Instrumentation: Ultraviolet to Gamma Ray conference, Edinburgh 2016. Addition of an acknowledgment statement in version 2
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37. eXTP -- enhanced X-ray Timing and Polarimetry Mission
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Zhang, S. N., Feroci, M., Santangelo, A., Dong, Y. W., Feng, H., Lu, F. J., Nandra, K., Wang, Z. S., Zhang, S., Bozzo, E., Brandt, S., De Rosa, A., Gou, L. J., Hernanz, M., van der Klis, M., Li, X. D., Liu, Y., Orleanski, P., Pareschi, G., Pohl, M., Poutanen, J., Qu, J. L., Schanne, S., Stella, L., Uttley, P., Watts, A., Xu, R. X., Yu, W. F., Zand, J. J. M. in 't, Zane, S., Alvarez, L., Amati, L., Baldini, L., Bambi, C., Basso, S., Bhattacharyya, S., Bellazzini, R., Belloni, T., Bellutti, P., Bianchi, S., Brez, A., Bursa, M., Burwitz, V., Budtz-Jorgensen, C., Caiazzo, I., Campana, R., Cao, X. L., Casella, P., Chen, C. Y., Chen, L., Chen, T. X., Chen, Y., Chen, Y. P., Civitani, M., Zelati, F. Coti, Cui, W., Cui, W. W., Dai, Z. G., Del Monte, E., De Martino, D., Di Cosimo, S., Diebold, S., Dovciak, M., Donnarumma, I., Doroshenko, V., Esposito, P., Evangelista, Y., Favre, Y., Friedrich, P., Fuschino, F., Galvez, J. L., Gao, Z. L., Ge, M. Y., Gevin, O., Goetz, D., Han, D. W., Heyl, J., Horak, J., Hu, W., Huang, F., Huang, Q. S., Hudec, R., Huppenkothen, D., Israel, G. L., Ingram, A., Karas, V., Karelin, D., Jenke, P. A., Ji, L., Kennedy, T., Korpela, S., Kunneriath, D., Labanti, C., Li, G., Li, X., Li, Z. S., Liang, E. W., Limousin, O., Lin, L., Ling, Z. X., Liu, H. B., Liu, H. W., Liu, Z., Lu, B., Lund, N., Lai, D., Luo, B., Luo, T., Ma, B., Mahmoodifar, S., Marisaldi, M., Martindale, A., Meidinger, N., Men, Y. P., Michalska, M., Mignani, R., Minuti, M., Motta, S., Muleri, F., Neilsen, J., Orlandini, M., Pan, A T., Patruno, A., Perinati, E., Picciotto, A., Piemonte, C., Pinchera, M., Rachevski, A., Rapisarda, M., Rea, N., Rossi, E. M. R., Rubini, A., Sala, G., Shu, X. W., Sgro, C., Shen, Z. X., Soffitta, P., Song, L. M., Spandre, G., Stratta, G., Strohmayer, T. E., Sun, L., Svoboda, J., Tagliaferri, G., Tenzer, C., Tong, H., Taverna, R., Torok, G., Turolla, R., Vacchi, A., Wang, J., Wang, J. X., Walton, D., Wang, K., Wang, J. F., Wang, R. J., Wang, Y. F., Weng, S. S., Wilms, J., Winter, B., Wu, X., Wu, X. F., Xiong, S. L., Xu, Y. P., Xue, Y. Q., Yan, Z., Yang, S., Yang, X., Yang, Y. J., Yuan, F., Yuan, W. M., Yuan, Y. F., Zampa, G., Zampa, N., Zdziarski, A., Zhang, C., Zhang, C. L., Zhang, L., Zhang, X., Zhang, Z., Zhang, W. D., Zheng, S. J., Zhou, P., and Zhou, X. L.
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Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
eXTP is a science mission designed to study the state of matter under extreme conditions of density, gravity and magnetism. Primary targets include isolated and binary neutron stars, strong magnetic field systems like magnetars, and stellar-mass and supermassive black holes. The mission carries a unique and unprecedented suite of state-of-the-art scientific instruments enabling for the first time ever the simultaneous spectral-timing-polarimetry studies of cosmic sources in the energy range from 0.5-30 keV (and beyond). Key elements of the payload are: the Spectroscopic Focusing Array (SFA) - a set of 11 X-ray optics for a total effective area of about 0.9 m^2 and 0.6 m^2 at 2 keV and 6 keV respectively, equipped with Silicon Drift Detectors offering <180 eV spectral resolution; the Large Area Detector (LAD) - a deployable set of 640 Silicon Drift Detectors, for a total effective area of about 3.4 m^2, between 6 and 10 keV, and spectral resolution <250 eV; the Polarimetry Focusing Array (PFA) - a set of 2 X-ray telescope, for a total effective area of 250 cm^2 at 2 keV, equipped with imaging gas pixel photoelectric polarimeters; the Wide Field Monitor (WFM) - a set of 3 coded mask wide field units, equipped with position-sensitive Silicon Drift Detectors, each covering a 90 degrees x 90 degrees FoV. The eXTP international consortium includes mostly major institutions of the Chinese Academy of Sciences and Universities in China, as well as major institutions in several European countries and the United States. The predecessor of eXTP, the XTP mission concept, has been selected and funded as one of the so-called background missions in the Strategic Priority Space Science Program of the Chinese Academy of Sciences since 2011. The strong European participation has significantly enhanced the scientific capabilities of eXTP. The planned launch date of the mission is earlier than 2025., Comment: 16 pages, 16 figures. Oral talk presented at SPIE Astronomical Telescopes and Instrumentation, June 26 to July 1, 2016, Edingurgh, UK
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- 2016
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38. Radio emissions from double RHESSI TGFs
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Mezentsev, Andrew, Østgaard, Nikolai, Gjesteland, Thomas, Albrechtsen, Kjetil, Lehtinen, Nikolai, Marisaldi, Martino, Smith, David, and Cummer, Steven
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Physics - Space Physics ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
A detailed analysis of Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) terrestrial gamma ray flashes (TGFs) is performed in association with World Wide Lightning Location Network (WWLLN) sources and very low frequency (VLF) sferics recorded at Duke University. RHESSI clock offset is evaluated and found to experience changes on the 5 August 2005 and 21 October 2013, based on the analysis of TGF-WWLLN matches. The clock offsets were found for all three periods of observations with standard deviations less than 100 {\mu}s. This result opens the possibility for the precise comparative analyses of RHESSI TGFs with the other types of data (WWLLN, radio measurements, etc.) In case of multiple-peak TGFs, WWLLN detections are observed to be simultaneous with the last TGF peak for all 16 cases of multipeak RHESSI TGFs simultaneous with WWLLN sources. VLF magnetic field sferics were recorded for two of these 16 events at Duke University. These radio measurements also attribute VLF sferics to the second peak of the double TGFs, exhibiting no detectable radio emission during the first TGF peak. Possible scenarios explaining these observations are proposed. Double (multipeak) TGFs could help to distinguish between the VLF radio emission radiated by the recoil currents in the +IC leader channel and the VLF emission from the TGF producing electrons.
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39. Analysis of global Terrestrial Gamma Ray Flashes distribution and special focus on AGILE detections over South America
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Fabró, Ferran, Montanyà, Joan, Marisaldi, Martino, van der Velde, Oscar A., and Fuschino, Fabio
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Physics - Space Physics - Abstract
Global distribution of the Terrestrial Gamma-ray Flashes (TGFs) detected by AGILE and RHESSI for the period from March 2009 to July 2012 has been analysed. A fourth TGF production region has been distinguished over the Pacific. It is confirmed that TGF occurrence follows the Intertropical Convergence Zone(ITCZ) seasonal migration and prefers afternoons. TGF/lightning ratio appears to be lower over America than other regions suggesting that meteorological regional differences are important for the TGF production. Diurnal cycle of TGFs peaks in the afternoon suggesting that Convective Available Potential Energy (CAPE) and convection are important for TGF production. Moreover all AGILE passages over South America in the same period have been analysed to find meteorological preferences for TGF occurrence. In each passage the analysis of Cloud Top Altitude (CTA), CAPE, number of strokes, number of storms and coverage area of clouds with temperatures below $-70\,^{\circ}{\rm C}$ (Cloud Top Coverage area, CTC) are computed. On average, AGILE has been exposed to 19,100 strokes between each TGF representing $\sim$68 hours of exposure over active storms. High CAPE values, high cloud tops and high stroke occurrence suggests that meteorological conditions conducive to vigorous and electrically active storms are important for TGF production. It is shown that a high number of thunderstorms is preferable for TGF production which may be explained by a greater chance of the presence of a thunderstorm in the best development stage for TGF production. High tropopause altitude seems to be important but not primordial for TGF production.
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40. Enhanced detection of terrestrial gamma-ray flashes by AGILE
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Marisaldi, M., Argan, A., Ursi, A., Gjesteland, T., Fuschino, F., Labanti, C., Galli, M., Tavani, M., Pittori, C., Verrecchia, F., D'Amico, F., Østgaard, N., Mereghetti, S., Campana, R., Cattaneo, P. W., Bulgarelli, A., Colafrancesco, S., Dietrich, S., Longo, F., Gianotti, F., Giommi, P., Rappoldi, A., Trifoglio, M., and Trois, A.
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Physics - Space Physics ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
At the end of March 2015 the onboard software configuration of the AGILE satellite was modified in order to disable the veto signal of the anticoincidence shield for the minicalorimeter instrument. The motivation for such a change was the understanding that the dead time induced by the anticoincidence prevented the detection of a large fraction of Terrestrial Gamma-Ray Flashes (TGFs). The configuration change was highly successful resulting in an increase of one order of magnitude in TGF detection rate. As expected, the largest fraction of the new events has short duration ($< 100 \mathrm {\mu s}$), and part of them has simultaneous association with lightning sferics detected by the World Wide Lightning Location Network (WWLLN). The new configuration provides the largest TGF detection rate surface density (TGFs/$\mathrm{km^2}$/year) to date, opening prospects for improved correlation studies with lightning and atmospheric parameters on short spatial and temporal scales along the equatorial region.
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41. Observation of intrinsically bright terrestrial gamma ray flashes from the Mediterranean basin
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Gjesteland, T., Østgaard, N., Laviola, S., Maglietta, M. M., Arnone, E., Marisaldi, M., Fuschino, F., Collier, A. B., Fabró, F., and Montanya, J.
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Physics - Space Physics ,Physics - Atmospheric and Oceanic Physics - Abstract
We present three terrestrial gamma ray flashes (TGFs) observed over the Mediterranean basin by the Reuven Ramaty High Energy Solar Spectroscope Imager (RHESSI) satellite. Since the occurrence of these events in the Mediterranean region is quite rare, the characterisation of the events was optimised by combining different approaches in order to better define the cloud of origin. The TGFs on 7 November 2004 and 16 October 2006 came from clouds with cloud top higher than 10-12 km where often a strong penetration into the stratosphere is found. This kind of cloud is usually associated with heavy precipitation and intense lightning activity. Nevertheless, the analysis of the cloud type based on satellite retrievals shows that the TGF on 27 May 2004 was produced by an unusual shallow convection. This result appears to be supported by the model simulation of the particle distribution and phase in the upper troposphere. The TGF on 7 November 2004 is among the brightest ever measured by RHESSI. The analysis of the energy spectrum of this event is consistent with a production altitude $\leq$12 km, which is in the upper part of the cloud, as found by the meteorological analysis of the TGF-producing thunderstorm. This event must be unusually bright at the source in order to produce such a strong signal in RHESSI. We estimate that this TGF must contain $\sim$3x10$\rm ^{18}$ initial photons with energy $>$1 MeV. This is 1 order of magnitude brighter than earlier estimations of an average RHESSI TGF.
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42. Relativistic electrons from sparks in the laboratory
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Østgaard, N., Carlson, B. E., Nisi, R. S., Gjesteland, T., Grøndahl, Ø., Skeltved, A., Lehtinen, N. G., Mezentsev, A., Marisaldi, M., and Kochkin, P.
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Physics - Space Physics ,Physics - Instrumentation and Detectors - Abstract
Discharge experiments were carried out at the Eindhoven University of Technology in 2013. The experimental setup was designed to search for electrons produced in meter-scale sparks using a 1 MV Marx generator. Negative voltage was applied to the high voltage (HV) electrode. Five thin (1 mm) plastic detectors (5 $\rm cm^2$ each) were distributed in various configurations close to the spark gap. Earlier studies have shown (for HV negative) that X-rays are produced when a cloud of streamers is developed 30-60 cm from the negative electrode. This indicates that the electrons producing the X-rays are also accelerated at this location, that could be in the strong electric field from counterstreamers of opposite polarity. Comparing our measurements with modeling results, we find that $\sim$300 keV electrons produced about 30-60 cm from the negative electrode are the most likely source of our measurements. A statistical analysis of expected detection of photon bursts by these fiber detectors indicates that only 20%-45% of the detected bursts could be from soft ($\sim$10 keV) photons, which further supports that the majority of detected bursts are produced by relativistic electrons.
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- 2016
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43. Steps towards the hyperfine splitting measurement of the muonic hydrogen ground state: pulsed muon beam and detection system characterization
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Adamczak, A., Baccolo, G., Bakalov, D., Baldazzi, G., Bertoni, R., Bonesini, M., Bonvicini, V., Campana, R., Carbone, R., Cervi, T., Chignoli, F., Clemenza, M., Colace, L., Curioni, A., Danailov, M., Danev, P., D'Antone, I., De, A., De, C., De, M., Furini, M., Fuschino, F., Gadejisso-Tossou, K., Guffanti, D., Iaciofano, A., Ishida, K., Iugovaz, D., Labanti, C., Maggi, V., Margotti, A., Marisaldi, M., Mazza, R., Meneghini, S., Menegolli, A., Mocchiutti, E., Moretti, M., Morgante, G., Nardò, R., Nastasi, M., Niemela, J., Previtali, E., Ramponi, R., Rachevski, A., P., L., Rossella, M., Rossi, P. L., Somma, F., Stoilov, M., Stoychev, L., Tomaselli, A., Tortora, L., Vacchi, A., Vallazza, E., Zampa, G., and Zuffa, M.
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Physics - Instrumentation and Detectors - Abstract
The high precision measurement of the hyperfine splitting of the muonic-hydrogen atom ground state with pulsed and intense muon beam requires careful technological choices both in the construction of a gas target and of the detectors. In June 2014, the pressurized gas target of the FAMU experiment was exposed to the low energy pulsed muon beam at the RIKEN RAL muon facility. The objectives of the test were the characterization of the target, the hodoscope and the X-ray detectors. The apparatus consisted of a beam hodoscope and X-rays detectors made with high purity Germanium and Lanthanum Bromide crystals. In this paper the experimental setup is described and the results of the detector characterization are presented., Comment: 22 pages, 14 figures, published and open access on JINST
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- 2016
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44. AGILE Observations of the Gravitational Wave Event GW150914
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Tavani, M., Pittori, C., Verrecchia, F., Bulgarelli, A., Giuliani, A., Donnarumma, I., Argan, A., Trois, A., Lucarelli, F., Marisaldi, M., Del Monte, E., Evangelista, Y., Fioretti, V., Zoli, A., Piano, G., Munar-Adrover, P., Antonelli, L. A., Barbiellini, G., Caraveo, P., Cattaneo, P. W., Costa, E., Feroci, M., Ferrari, A., Longo, F., Mereghetti, S., Minervini, G., Morselli, A., Pacciani, L., Pellizzoni, A., Picozza, P., Pilia, M., Rappoldi, A., Sabatini, S., Vercellone, S., Vittorini, V., Giommi, P., Colafrancesco, S., and Cardillo, M.
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
We report the results of an extensive search in the AGILE data for a gamma-ray counterpart of the LIGO gravitational wave event GW150914. Currently in spinning mode, AGILE has the potential of covering with its gamma-ray instrument 80 % of the sky more than 100 times a day. It turns out that AGILE came within a minute from the event time of observing the accessible GW150914 localization region. Interestingly, the gamma-ray detector exposed about 65 % of this region during the 100 s time intervals centered at -100 s and +300 s from the event time. We determine a 2-sigma flux upper limit in the band 50 MeV - 10 GeV, $UL = 1.9 \times 10^{-8} \rm \, erg \, cm^{-2} \, s^{-1}$ obtained about 300 s after the event. The timing of this measurement is the fastest ever obtained for GW150914, and significantly constrains the electromagnetic emission of a possible high-energy counterpart. We also carried out a search for a gamma-ray precursor and delayed emission over timescales ranging from minutes to days: in particular, we obtained an optimal exposure during the interval -150 / -30 s. In all these observations, we do not detect a significant signal associated with GW150914. We do not reveal the weak transient source reported by Fermi-GBM 0.4 s after the event time. However, even though a gamma-ray counterpart of the GW150914 event was not detected, the prospects for future AGILE observations of gravitational wave sources are decidedly promising., Comment: 20 pages, 6 figures. Submitted to the Astrophysical Journal Letters on April 1, 2016
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- 2016
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45. The On-Site Analysis of the Cherenkov Telescope Array
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Bulgarelli, Andrea, Fioretti, Valentina, Zoli, Andrea, Aboudan, Alessio, Rodríguez-Vázquez, Juan José, De Cesare, Giovanni, De Rosa, Adriano, Maier, Gernot, Lyard, Etienne, Bastieri, Denis, Lombardi, Saverio, Tosti, Gino, Bergamaschi, Sonia, Beneventano, Domenico, Lamanna, Giovanni, Jacquemier, Jean, Kosack, Karl, Antonelli, Lucio Angelo, Boisson, Catherine, Borkowski, Jerzy, Buson, Sara, Carosi, Alessandro, Conforti, Vito, Colomé, Pep, Reyes, Raquel de los, Dumm, Jon, Evans, Phil, Fortson, Lucy, Fuessling, Matthias, Gotz, Diego, Graciani, Ricardo, Gianotti, Fulvio, Grandi, Paola, Hinton, Jim, Humensky, Brian, Inoue, Susumu, Knödlseder, Jürgen, Flour, Thierry Le, Lindemann, Rico, Malaguti, Giuseppe, Markoff, Sera, Marisaldi, Martino, Neyroud, Nadine, Nicastro, Luciano, Ohm, Stefan, Osborne, Julian, Oya, Igor, Rodriguez, Jerome, Rosen, Simon, Ribo, Marc, Tacchini, Alessandro, Schüssler, Fabian, Stolarczyk, Thierry, Torresi, Eleonora, Testa, Vincenzo, Wegner, Peter, and Weinstein, Amanda
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
The Cherenkov Telescope Array (CTA) observatory will be one of the largest ground-based very high-energy gamma-ray observatories. The On-Site Analysis will be the first CTA scientific analysis of data acquired from the array of telescopes, in both northern and southern sites. The On-Site Analysis will have two pipelines: the Level-A pipeline (also known as Real-Time Analysis, RTA) and the level-B one. The RTA performs data quality monitoring and must be able to issue automated alerts on variable and transient astrophysical sources within 30 seconds from the last acquired Cherenkov event that contributes to the alert, with a sensitivity not worse than the one achieved by the final pipeline by more than a factor of 3. The Level-B Analysis has a better sensitivity (not be worse than the final one by a factor of 2) and the results should be available within 10 hours from the acquisition of the data: for this reason this analysis could be performed at the end of an observation or next morning. The latency (in particular for the RTA) and the sensitivity requirements are challenging because of the large data rate, a few GByte/s. The remote connection to the CTA candidate site with a rather limited network bandwidth makes the issue of the exported data size extremely critical and prevents any kind of processing in real-time of the data outside the site of the telescopes. For these reasons the analysis will be performed on-site with infrastructures co-located with the telescopes, with limited electrical power availability and with a reduced possibility of human intervention. This means, for example, that the on-site hardware infrastructure should have low-power consumption. A substantial effort towards the optimization of high-throughput computing service is envisioned to provide hardware and software solutions with high-throughput, low-power consumption at a low-cost., Comment: In Proceedings of the 34th International Cosmic Ray Conference (ICRC2015), The Hague, The Netherlands. All CTA contributions at arXiv:1508.05894
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- 2015
46. CTA Contributions to the 34th International Cosmic Ray Conference (ICRC2015)
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Consortium, The CTA, Abchiche, A., Abeysekara, U., Abril, Ó., Acero, F., Acharya, B. S., Actis, M., Agnetta, G., Aguilar, J. A., Aharonian, F., Akhperjanian, A., Albert, A., Alcubierre, M., Alfaro, R., Aliu, E., Allafort, A. J., Allan, D., Allekotte, I., Aloisio, R., Amans, J. -P., Amato, E., Ambrogi, L., Ambrosi, G., Ambrosio, M., Anderson, J., Anduze, M., Angüner, E. O., Antolini, E., Antonelli, L. A., Antonucci, M., Antonuccio, V., Antoranz, P., Aramo, C., Aravantinos, A., Argan, A., Armstrong, T., Arnaldi, H., Arnold, L., Arrabito, L., Arrieta, M., Asano, K., Asorey, H. G., Aune, T., Singh, C. B., Babic, A., Backes, M., Bais, A., Bajtlik, S., Balazs, C., Balbo, M., Balis, D., Balkowski, C., Ballester, O., Ballet, J., Balzer, A., Bamba, A., Bandiera, R., Barber, A., Barbier, C., Barceló, M., Barnacka, A., de Almeida, U. Barres, Barrio, J. A., Basso, S., Bastieri, D., Bauer, C., Baushev, A., Becciani, U., Becherini, Y., Tjus, J. Becker, Beckmann, V., Bednarek, W., Benbow, W., Ventura, D. Benedico, Berdugo, J., Berge, D., Bernardini, E., Bernhard, S., Bernlöhr, K., Bertucci, B., Besel, M. -A., Bhatt, N., Bhattacharjee, P., Bhattachryya, S., Biasuzzi, B., Bicknell, G., Bigongiari, C., Biland, A., Billotta, S., Bilnik, W., Biondo, B., Bird, T., Birsin, E., Bissaldi, E., Biteau, J., Bitossi, M., Bigas, O. Blanch, Blasi, P., Boehm, C., Bogacz, L., Bogdan, M., Bohacova, M., Boisson, C., Gargallo, J. Boix, Bolmont, J., Bonanno, G., Bonardi, A., Bonifacio, P., Bonnoli, G., Borkowski, J., Bose, R., Bosnjak, Z., Bottani, A., Böttcher, M., Bousquet, J. -J., Boutonnet, C., Bouyjou, F., Braiding, C., Brandt, L., Brau-Nogué, S., Bregeon, J., Bretz, T., Briggs, M., Brigida, M., Bringmann, T., Brisken, W., Brocato, E., Brook, P., Brown, A. M., Brun, P., Brunetti, G., Brunetti, L., Bruno, P., Bryan, M., Buanes, T., Bucciantini, N., Buchholtz, G., Buckley, J., Bugaev, V., Bühler, R., Bulgarelli, A., Bulik, T., Burton, M., Burtovoi, A., Busetto, G., Buson, S., Buss, J., Byrum, K., Cameron, R., Camprecios, J., Canelli, F., Canestrari, R., Cantu, S., Capalbi, M., Capasso, M., Capobianco, G., Caraveo, P., Cardenzana, J., Carius, S., Carlile, C., Carmona, E., Carosi, A., Carosi, R., Carr, J., Carroll, M., Carter, J., Carton, P. -H., Caruso, R., Casandjian, J. -M., Casanova, S., Cascone, E., Casiraghi, M., Castellina, A., Catalano, O., Catalanotti, S., Cavazzani, S., Cazaux, S., Cefalà, M., Cerchiara, P., Cereda, M., Cerruti, M., Chabanne, E., Chadwick, P., Champion, C., Chaty, S., Chaves, R., Cheimets, P., Chen, A., Chen, X., Chernyakova, M., Chiappetti, L., Chikawa, M., Chinn, D., Chitnis, V. R., Cho, N., Christov, A., Chudoba, J., Cieślar, M., Cillis, A., Ciocci, M. A., Clay, R., Cohen-Tanugi, J., Colafrancesco, S., Colin, P., Colombo, E., Colome, J., Colonges, S., Compin, M., Conforti, V., Connaughton, V., Connell, S., Conrad, J., Contreras, J. L., Coppi, P., Corbel, S., Coridian, J., Corona, P., Corti, D., Cortina, J., Cossio, L., Costa, A., Costantini, H., Cotter, G., Courty, B., Covino, S., Covone, G., Crimi, G., Criswell, S. J., Crocker, R., Croston, J., Cusumano, G., Da Vela, P., Dale, Ø., D'Ammando, F., Dang, D., Daniel, M., Davids, I., Dawson, B., Dazzi, F., Costa, B. de Aguiar, De Angelis, A., Cardoso, R. F. de Araujo, De Caprio, V., De Cesare, G., De Franco, A., De Frondat, F., Pino, E. M. de Gouveia Dal, de la Calle, I., De La Vega, G. A., Lopez, R. de los Reyes, De Lotto, B., De Luca, A., Neto, J. R. T. de Mello, de Naurois, M., Wilhelmi, E. de Oña, De Palma, F., de Souza, V., Decock, G., Deil, C., Del Santo, M., Delagnes, E., Deleglise, G., Delgado, C., della Volpe, D., Deloye, P., Depaola, G., Detournay, M., Dettlaff, A., Di Girolamo, T., Di Giulio, C., Di Paola, A., Di Pierro, F., Di Sciascio, G., Díaz, C., Dick, J., Dickinson, H., Diebold, S., Diez, V., Digel, S., Dipold, J., Disset, G., Distefano, A., Djannati-Ataï, A., Doert, M., Dohmke, M., Domainko, W., Dominik, N., Prester, D. Dominis, Donat, A., Donnarumma, I., Dorner, D., Doro, M., Dournaux, J. -L., Doyle, K., Drake, G., Dravins, D., Drury, L., Dubus, G., Dumas, D., Dumm, J., Durand, D., D'Urso, D., Dwarkadas, V., Dyks, J., Dyrda, M., Ebr, J., Echaniz, J. C., Edy, E., Egberts, K., Eger, P., Einecke, S., Eisch, J., Eisenkolb, F., Eleftheriadis, C., Elsässer, D., Emmanoulopoulos, D., Engelbrecht, C., Engelhaupt, D., Ernenwein, J. -P., Errando, M., Eschbach, S., Etchegoyen, A., Evans, P., Fairbairn, M., Falcone, A., Fantinel, D., Farakos, K., Farnier, C., Farrell, E., Farrell, S., Fasola, G., Fegan, S., Feinstein, F., Ferenc, D., Fernandez, A., Fernandez-Alonso, M., Ferreira, O., Fesquet, M., Fetfatzis, P., Fiasson, A., Filipčič, A., Filipovic, M., Fink, D., Finley, C., Finley, J. P., Finoguenov, A., Fioretti, V., Fiorini, M., Curcoll, R. Firpo, Fleischhack, H., Flores, H., Florin, D., Föhr, C., Fokitis, E., Font, L., Fontaine, G., Fontes, B., Forest, F., Fornasa, M., Förster, A., Fortin, P., Fortson, L., Fouque, N., Franckowiak, A., Franco, F. J., Frankowski, A., Frega, N., Albuquerque, I. Freire Mota, Coromina, L. Freixas, Fresnillo, L., Fruck, C., Fuessling, M., Fugazza, D., Fujita, Y., Fukami, S., Fukazawa, Y., Fukuda, T., Fukui, Y., Funk, S., Gäbele, W., Gabici, S., Gadola, A., Galante, N., Gall, D. D., Gallant, Y., Galloway, D., Gallozzi, S., Gao, S., Garcia, B., Gil, R. García, López, R. Garcia, Garczarczyk, M., Gardiol, D., Gargano, C., Gargano, F., Garozzo, S., Garrecht, F., Garrido, D., Garrido, L., Gascon, D., Gaskins, J., Gaudemard, J., Gaug, M., Gaweda, J., Geffroy, N., Gérard, L., Ghalumyan, A., Ghedina, A., Ghigo, M., Ghislain, P., Giannakaki, E., Gianotti, F., Giarrusso, S., Giavitto, G., Giebels, B., Giglietto, N., Gika, V., Gimenes, R., Giomi, M., Giommi, P., Giordano, F., Giovannini, G., Giro, E., Giroletti, M., Giuliani, A., Glicenstein, J. -F., Godinovic, N., Goldoni, P., Berisso, M. Gomez, Vargas, G. A. Gomez, Gonzalez, M. M., González, A., González, F., Muñoz, A. González, Gothe, K. S., Gotz, D., Grabarczyk, T., Graciani, R., Grandi, P., Grañena, F., Granot, J., Grasseau, G., Gredig, R., Green, A. J., Green, A. M., Greenshaw, T., Grenier, I., Grillo, A., Grondin, M. -H., Grube, J., Grudzinska, M., Grygorczuk, J., Guarino, V., Guberman, D., Gunji, S., Gyuk, G., Hadasch, D., Hagedorn, A., Hahn, J., Hakansson, N., Heras, N. Hamer, Hanabata, Y., Hara, S., Hardcastle, M. J., Harris, J., Hassan, T., Hatanaka, K., Haubold, T., Haupt, A., Hayakawa, T., Hayashida, M., Heller, M., Heller, R., Henault, F., Henri, G., Hermann, G., Hermel, R., Llorente, J. Herrera, Herrero, A., Hervet, O., Hidaka, N., Hinton, J., Hirai, W., Hirotani, K., Hoard, D., Hoffmann, D., Hofmann, W., Hofverberg, P., Holch, T., Holder, J., Hooper, S., Horan, D., Hörandel, J. R., Hormigos, S., Horns, D., Hose, J., Houles, J., Hovatta, T., Hrabovsky, M., Hrupec, D., Huet, J. -M., Hütten, M., Humensky, T. B., Huovelin, J., Huppert, J. -F., Iacovacci, M., Ibarra, A., Idźkowski, B., Ikawa, D., Illa, J. M., Impiombato, D., Incorvaia, S., Inome, Y., Inoue, S., Inoue, T., Inoue, Y., Iocco, F., Ioka, K., Iori, M., Ishio, K., Israel, G. L., Jablonski, C., Jacholkowska, A., Jacquemier, J., Jamrozy, M., Janecek, P., Janiak, M., Jankowsky, F., Jean, P., Jeanney, C., Jegouzo, I., Jenke, P., Jimenez, J. J., Jingo, M., Jocou, L., Jogler, T., Johnson, C. A., Journet, L., Juffroy, C., Jung, I., Kaaret, P. E., Kagaya, M., Kakuwa, J., Kalekin, O., Kalkuhl, C., Kankanyan, R., Karastergiou, A., Kärcher, K., Karczewski, M., Karkar, S., Karn, P., Kasperek, J., Katagiri, H., Kataoka, J., Katarzyński, K., Katz, U., Kaufmann, S., Kawanaka, N., Kawashima, T., Kazanas, D., Kelley-Hoskins, N., Kellner-Leidel, B., Kendziorra, E., Kersten, J., Khélifi, B., Kieda, D. B., Kihm, T., Kisaka, S., Kissmann, R., Klepser, S., Kluźniak, W., Knapen, J., Knapp, J., Knödlseder, J., Köck, F., Kocot, J., Kodakkadan, A., Kodani, K., Kohri, K., Kojima, T., Kokkotas, K., Kolitzus, D., Komin, N., Kominis, I., Konno, Y., Kosack, K., Koss, G., Koul, R., Kowal, G., Koyama, S., Kozioł, J., Kraus, M., Krause, J., Krause, M., Krawzcynski, H., Krennrich, F., Kretzschmann, A., Kruger, P., Kubo, H., Kudryavtsev, V., Mezek, G. Kukec, Kushida, J., Kuznetsov, A., La Barbera, A., La Palombara, N., La Parola, V., La Rosa, G., Laffon, H., Lagadec, T., Lahmann, R., Lalik, K., Lamanna, G., Landriu, D., Landt, H., Lang, R. G., Languignon, D., Lapington, J., Laporte, P., Latovski, N., Law-Green, D., Fèvre, J. -P. Le, Flour, T. Le, Sidaner, P. Le, Lee, S. -H., Lee, W. H., Leffhalm, K., Leich, H., de Oliveira, M. A. Leigui, Lelas, D., Lemière, A., Lemoine-Goumard, M., Lenain, J. -P., Leonard, R., Leoni, R., Lessio, L., Leto, G., Leveque, A., Lieunard, B., Limon, M., Lindemann, R., Lindfors, E., Liolios, A., Lipniacka, A., Lockart, H., Lohse, T., Loiseau, D., Łokas, E., Lombardi, S., Longo, F., Longo, G., Lopatin, A., Lopez, M., López-Coto, R., López-Oramas, A., Loreggia, D., Louge, T., Louis, F., Lu, C. -C., Lucarelli, F., Lucchesi, D., Lüdecke, H., Luque-Escamilla, P. L., Luz, O., Lyard, E., Maccarone, M. C., Maccarone, T. J., Mach, E., Madejski, G. M., Madonna, A., Mahabir, M., Maier, G., Majumdar, P., Makariev, M., Malaguti, G., Malaspina, G., Mallot, A. K., Maltezos, S., Mancilla, A., Mandat, D., Maneva, G., Manigot, P., Mankushiyil, N., Mannheim, K., Maragos, N., Marano, D., Marchegiani, P., Marcomini, J. A., Marcowith, A., Mariotti, M., Marisaldi, M., Markoff, S., Marszałek, A., Martens, C., Martí, J., Martin, J. -M., Martin, P., Martínez, G., Martínez, M., Martínez, O., Marx, R., Massimino, P., Mastichiadis, A., Mastroianni, S., Mastropietro, M., Masuda, S., Matsumoto, H., Matsuoka, S., Mattiazzo, S., Maurin, G., Maxted, N., Maya, J., Mayer, M., Mazin, D., Mazureau, E., Mazziotta, M. N., Comb, L. Mc, McCann, A., McCubbin, N., McHardy, I., McKay, R., McKinney, K., Meagher, K., Medina, C., Mehrez, F., Melioli, C., Melkumyan, D., Melo, D., Melse, T., Mereghetti, S., Mertsch, P., Meyer, M., Meyrelles jr, J. L., Miccichè, A., Michałowski, J., Micolon, P., Mientjes, P., Mignot, S., Mihailidis, A., Mineo, T., Minuti, M., Mirabal, N., Mirabel, F., Miranda, J. M., Mirzoyan, R., Mistò, A., Mitchell, A., Mizuno, T., Moderski, R., Mognet, I., Mohammed, M., Moharana, R., Molinari, E., Monmarthe, E., Monnier, G., Montaruli, T., Monte, C., Monteiro, I., Moore, P., Olaizola, A. Moralejo, Morello, C., Moretti, E., Mori, K., Morlino, G., Morselli, A., Mottez, F., Moudden, Y., Moulin, E., Mrusek, I., Mueller, S., Mukherjee, R., Munar-Adrover, P., Mundell, C., Muraishi, H., Murase, K., Muronga, A., Murphy, A., Nagataki, S., Nagayoshi, T., Nagesh, B. K., Naito, T., Nakajima, D., Nakamori, T., Nakayama, K., Naumann, D., Nayman, P., Nellen, L., Nemmen, R., Neronov, A., Neustroev, V., Neyroud, N., Nguyen, T., Nicastro, L., Nicolau-Kukliński, J., Niederwanger, F., Niedźwiecki, A., Niemiec, J., Nieto, D., Nievas, M., Nikolaidis, A., Nishijima, K., Nishikawa, K. -I., Noda, K., Nogues, L., Nolan, S., Northrop, R., Nosek, D., Nozka, L., Nunio, F., Oakes, L., O'Brien, P., Occhipinti, G., de Bhroithe, A. O'Faolain, Ogino, M., Ohira, Y., Ohishi, M., Ohm, S., Ohoka, H., Okumura, A., Olive, J. -F., Olszowski, D., Ong, R. A., Ono, S., Orienti, M., Orito, R., Orlati, A., Osborne, J., Ostrowski, M., Otero, L. A., Ottaway, D., Otte, N., Oya, I., Ozieblo, A., Padovani, M., Pagano, I., Paiano, S., Paizis, A., Palacio, J., Palatka, M., Pallotta, J., Panagiotidis, K., Panazol, J. -L., Paneque, D., Panter, M., Panzera, M. R., Paoletti, R., Paolillo, M., Papayannis, A., Papyan, G., Paravac, A., Paredes, J. M., Pareschi, G., Park, N., Parsons, D., Paśko, P., Pavy, S., Arribas, M. Paz, Pech, M., Peck, A., Pedaletti, G., Peet, S., Pelassa, V., Pelat, D., Peres, C., Perez, M. d. C., Perri, L., Persic, M., Petrashyk, A., Petrucci, P. -O., Peyaud, B., Pfeifer, M., Pfeiffer, G., Piano, G., Pichel, A., Pieloth, D., Pierbattista, M., Pierre, E., de Pinho, F. Pinto, García, C. Pio, Piret, Y., Pita, S., Planes, A., Platino, M., Platos, Ł., Platzer, R., Podkladkin, S., Pogosyan, L., Pohl, M., Poinsignon, P., Ponz, J. D., Porcelli, A., Potter, W., Poulios, S., Poutanen, J., Prandini, E., Prast, J., Preece, R., Profeti, F., Prokhorov, D., Prokoph, H., Prouza, M., Proyetti, M., Pruchniewicz, R., Pueschel, E., Pühlhofer, G., Puljak, I., Punch, M., Pyzioł, R., Queiroz, F., Quel, E. J., Quinn, J., Quirrenbach, A., Racero, E., Räck, T., Rafalski, J., Rafighi, I., Rainò, S., Rajda, P. J., Rameez, M., Rando, R., Rannot, R. C., Rataj, M., Rateau, S., Ravel, T., Ravignani, D., Razzaque, S., Reardon, P., Reimann, O., Reimer, A., Reimer, O., Reitberger, K., Renaud, M., Renner, S., Reposeur, T., Rettig, R., Reville, B., Rhode, W., Ribeiro, D., Ribó, M., Richards, G., Richer, M. G., Rico, J., Ridky, J., Rieger, F., Ringegni, P., Ristori, P. R., Rivière, A., Rivoire, S., Roache, E., Rodeghiero, G., Rodriguez, J., Fernandez, G. Rodriguez, Vázquez, J. J. Rodríguez, Rogers, T., Rojas, G., Romano, P., Rodriguez, M. P. Romay, Romeo, G., Romero, G. E., Roncadelli, M., Rose, J., Rosen, S., Lees, S. 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K., Yamamoto, H., Yamamoto, T., Yamazaki, R., Yanagita, S., Yang, L., Yebras, J. M., Yelos, D., Yeung, W., Yoshida, A., Yoshida, T., Yoshiike, S., Yoshikoshi, T., Yu, P., Zabalza, V., Zacharias, M., Zaharijas, G., Zajczyk, A., Zampieri, L., Zandanel, F., Zanin, R., Sanchez, R. Zanmar, Zavrtanik, D., Zavrtanik, M., Zdziarski, A., Zech, A., Zechlin, H., Zhao, A., Ziegler, A., Ziemann, J., Ziętara, K., Ziółkowski, J., Zitelli, V., Zoli, A., Zurbach, C., and Żychowski, P.
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
List of contributions from the CTA Consortium presented at the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands., Comment: Index of CTA conference proceedings at the ICRC2015, The Hague (The Netherlands). v1: placeholder with no arXiv links yet, to be replaced once individual contributions have been all submitted; v2: final with arXiv links to all CTA contributions and full author list
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- 2015
47. Evidence of a New Population of Weak Terrestrial Gamma‐Ray Flashes Observed From Aircraft Altitude.
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Bjørge‐Engeland, I., Østgaard, N., Sarria, D., Marisaldi, M., Mezentsev, A., Fuglestad, A., Lehtinen, N., Grove, J. E., Shy, D., Lang, T., Quick, M., Christian, H., Schultz, C., Blakeslee, R., Adams, I., Kroodsma, R., Heymsfield, G., Ullaland, K., Yang, S., and Qureshi, B. Hasan
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RELATIVISTIC energy ,ELECTRIC fields ,LIGHTNING ,ALTITUDES ,PHOTONS - 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. Plain Language Summary: Terrestrial Gamma‐ray Flashes (TGFs) are short bursts of gamma‐rays produced in the strong electric fields in thunderclouds. Based on space and aircraft observations, TGFs have been considered a rare phenomena. In this paper, we present observations of TGFs from an aircraft campaign that were not detected by a space instrument viewing the same area. Our results reveal that these TGFs were too weak to be observed from space, indicating a significant population of TGFs that are undetectable by space instruments. Key Points: The ALOFT flight campaign detected six TGFs within a few minutes during an ISS overpass, and none were detected by the ASIM instrumentWe show that there must be a population of TGFs that are too weak to be observed from spaceThe fluence at 15 km of this population is 2–5 orders of magnitude lower than the TGFs observed from space [ABSTRACT FROM AUTHOR]
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- 2024
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48. High-energy radiation from thunderstorms and lightning with LOFT
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Marisaldi, M., Smith, D. M., Brandt, S., Briggs, M. S., Budtz-Jørgensen, C., Campana, R., Carlson, B. E., Celestin, S., Connaughton, V., Cummer, S. A., Dwyer, J. R., Fishman, G. J., Fullekrug, M., Fuschino, F., Gjesteland, T., Neubert, T., Østgaard, N., and Tavani, M.
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
This is a White Paper in support of the mission concept of the Large Observatory for X-ray Timing (LOFT), proposed as a medium-sized ESA mission. We discuss the potential of LOFT for the study of high-energy radiation from thunderstorms and lightning. For a summary, we refer to the paper., Comment: White Paper in Support of the Mission Concept of the Large Observatory for X-ray Timing
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- 2015
49. Probing the emission physics and weak/soft population of Gamma-Ray Bursts with LOFT
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Amati, L., Stratta, G., Atteia, J. -L., De Pasquale, M., Del Monte, E., Gendre, B., Götz, D., Guidorzi, C., Izzo, L., Kouveliotou, C., Osborne, J., Penacchioni, A. V., Romano, P., Sakamoto, T., Salvaterra, R., Schanne, S., Zand, J. J. M. in 't, Antonelli, L. A., Braga, J., Brandt, S., Bucciantini, N., Castro-Tirado, A., D'Elia, V., Feroci, M., Fuschino, F., Guetta, D., Longo, F., Lyutikov, M., Maccarone, T., Mangano, V., Marisaldi, M., Mereghetti, S., O'Brien, P., Rossi, E. M., Ryde, F., Soffitta, P., Troja, E., Wijers, R. A. M. J., and Zhang, B.
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
This is a White Paper in support of the mission concept of the Large Observatory for X-ray Timing (LOFT), proposed as a medium-sized ESA mission. We discuss the potential of LOFT for the study of gamma-ray bursts. For a summary, we refer to the paper., Comment: White Paper in Support of the Mission Concept of the Large Observatory for X-ray Timing
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- 2015
50. The Large Area Detector of LOFT: the Large Observatory for X-ray Timing
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Zane, S., Walton, D., Kennedy, T., Feroci, M., Herder, J. -W. Den, Ahangarianabhari, M., Argan, A., Azzarello, P., Baldazzi, G., Barbera, M., Barret, D., Bertuccio, G., Bodin, P., Bozzo, E., Bradley, L., Cadoux, F., Cais, P., Campana, R., Coker, J., Cros, A., Del Monte, E., De Rosa, A., Di Cosimo, S., Donnarumma, I., Evangelista, Y., Favre, Y., Feldman, C., Fraser, G., Fuschino, F., Grassi, M., Hailey, M. R., Hudec, R., Labanti, C., Macera, D., Malcovati, P., Marisaldi, M., Martindale, A., Mineo, T., Muleri, F., Nowak, M., Orlandini, M., Pacciani, L., Perinati, E., Petracek, V., Pohl, M., Rachevski, A., Smith, P., Santangelo, A., Seyler, J. -Y., Schmid, C., Soffitta, P., Suchy, S., Tenzer, C., Uttley, P., Vacchi, A., Zampa, G., Zampa, N., Wilms, J., and Winter, B.
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Astrophysics - Instrumentation and Methods for Astrophysics - 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 m 2 -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 re- proposed 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., Comment: Proc. SPIE 9144, Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray, 91442W
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- 2014
- Full Text
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