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1. The 100-month Swift catalogue of supergiant fast X-ray transients II. SFXT diagnostics from outburst properties

Author: P., Romano, A., Evans P., E., Bozzo, V., Mangano, S., Vercellone, C., Guidorzi, L., Ducci, A., Kennea J., D., Barthelmy S., M., Palmer D., A., Krimm H., and B., Cenko
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Supergiant Fast X-ray Transients (SFXT) are High Mass X-ray Binaries displaying X-ray outbursts reaching peak luminosities of 10$^{38}$ erg/s and spend most of their life in more quiescent states with luminosities as low as 10$^{32}$-10$^{33}$ erg/s. The main goal of our comprehensive and uniform analysis of the SFXT Swift triggers is to provide tools to predict whether a transient which has no known X-ray counterpart may be an SFXT candidate. These tools can be exploited for the development of future missions exploring the variable X-ray sky through large FoV instruments. We examined all available data on outbursts of SFXTs that triggered the Swift/BAT collected between 2005-08-30 and 2014-12-31, in particular those for which broad-band data, including the Swift/XRT ones, are also available. We processed all BAT and XRT data uniformly with the Swift Burst Analyser to produce spectral evolution dependent flux light curves for each outburst. The BAT data allowed us to infer useful diagnostics to set SFXT triggers apart from the general GRB population, showing that SFXTs give rise uniquely to image triggers and are simultaneously very long, faint, and `soft' hard-X-ray transients. The BAT data alone can discriminate very well the SFXTs from other fast transients such as anomalous X-ray pulsars and soft gamma repeaters. However, to distinguish SFXTs from, for instance, accreting millisecond X-ray pulsars and jetted tidal disruption events, the XRT data collected around the time of the BAT triggers are decisive. The XRT observations of 35/52 SFXT BAT triggers show that in the soft X-ray energy band, SFXTs display a decay in flux from the peak of the outburst of at least 3 orders of magnitude within a day and rarely undergo large re-brightening episodes, favouring in most cases a rapid decay down to the quiescent level within 3-5 days (at most). [Abridged], Comment: Accepted for publication in Astronomy and Astrophysics. 18 pages, 11 figures
Published: 2022
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2. The ASTRI Mini-Array of Cherenkov Telescopes at the Observatorio del Teide

Author: S., Scuderi, A., Giuliani, G., Pareschi, G., Tosti, O., Catalano, E., Amato, A., Antonelli L., J., Becerra Gonzáles, G., Bellassai, Bigongiari, B., Biondo, M., Böttcher, G., Bonanno, G., Bonnoli, P., Bruno, A., Bulgarelli, R., Canestrari, M., Capalbi, P., Caraveo, M., Cardillo, V., Conforti, G., Contino, M., Corpora, A., Costa, G., Cusumano, A., D'Aí, E., de Gouveia Dal Pino, R., Della Ceca, D., Escribano Rodriguez E. Falceta Gonçalves, C., Fermino, M., Fiori, V., Fioretti, M., Fiorini, S., Gallozzi, C., Gargano, S., Garozzo, S., Germani, A., Ghedina, F., Gianotti, S., Giarrusso, R., Gimenes, V., Giordano, A., Grillo, C., Grivel Gelly, D., Impiombato, F., Incardona, S., Incorvaia, S., Iovenitti, A., La Barbera, N., La Palombara, V., La Parola, A., Lamastra, L., Lessio, G., Leto, F., Lo Gerfo, M., Lodi, S., Lombardi, F., Longo, F., Lucarelli, C., Maccarone M., D., Marano, E., Martinetti, S., Mereghetti, A., Micciché, R., Millul, T., Mineo, D., Mollica, G., Morlino, A., Morselli, G., Naletto, G., Nicotra, A., Pagliaro, N., Parmiggiani, G., Piano, F., Pintore, E., Poretti, B., Olmi, G., Rodeghiero, G., Rodriguez Fernandez, P., Romano, G., Romeo, F., Russo, P., Sangiorgi, G., Saturni F., H., Schwarz J., Sciacca, G., Sironi, G., Sottile, A., Stamerra, G., Tagliaferri, V., Testa, G., Umana, M., Uslenghi, S., Vercellone, L., Zampieri, and R, Zanmar Sanchez
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The ASTRI Mini-Array (MA) is an INAF project to build and operate a facility to study astronomical sources emitting at very high-energy in the TeV spectral band. The ASTRI MA consists of a group of nine innovative Imaging Atmospheric Cherenkov telescopes. The telescopes will be installed at the Teide Astronomical Observatory of the Instituto de Astrofisica de Canarias (IAC) in Tenerife (Canary Islands, Spain) on the basis of a host agreement with INAF. Thanks to its expected overall performance, better than those of current Cherenkov telescopes' arrays for energies above \sim 5 TeV and up to 100 TeV and beyond, the ASTRI MA will represent an important instrument to perform deep observations of the Galactic and extra-Galactic sky at these energies., Comment: 19 pages, 22 figures
Published: 2022
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3. Prospects for γ-ray observations of narrow-line Seyfert 1 galaxies with the Cherenkov Telescope Array – II. γ–γ absorption in the broad-line region radiation fields

Author: P Romano, M Böttcher, L Foschini, C Boisson, S Vercellone, and M Landoni
Published: 2020
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4. The beamed jet and quasar core of the distant blazar 4C 71.07

Author: C M Raiteri, M Villata, M I Carnerero, J A Acosta-Pulido, D O Mirzaqulov, V M Larionov, P Romano, S Vercellone, I Agudo, A A Arkharov, U Bach, R Bachev, S Baitieri, G A Borman, W Boschin, V Bozhilov, M S Butuzova, P Calcidese, D Carosati, C Casadio, W-P Chen, G Damljanovic, A Di Paola, V T Doroshenko, N V Efimova, Sh A Ehgamberdiev, M Giroletti, J L Gómez, T S Grishina, S Ibryamov, H Jermak, S G Jorstad, G N Kimeridze, S A Klimanov, E N Kopatskaya, O M Kurtanidze, S O Kurtanidze, A Lähteenmäki, E G Larionova, A P Marscher, B Mihov, M Minev, S N Molina, J W Moody, D A Morozova, S V Nazarov, A A Nikiforova, M G Nikolashvili, E Ovcharov, S Peneva, S Righini, N Rizzi, A C Sadun, M R Samal, S S Savchenko, E Semkov, L A Sigua, L Slavcheva-Mihova, I A Steele, A Strigachev, M Tornikoski, Yu V Troitskaya, I S Troitsky, and O Vince
Published: 2019
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5. Putting thehadron beamscenario for extreme blazars to the test with the Cherenkov Telescope Array

Author: F Tavecchio, P Romano, M Landoni, and S Vercellone
Published: 2018
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6. Prospects for gamma-ray observations of narrow-line Seyfert 1 galaxies with the Cherenkov Telescope Array

Author: P Romano, S Vercellone, L Foschini, F Tavecchio, M Landoni, and J Knödlseder
Published: 2018
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7. Extragalactic observatory science with the ASTRI mini-array at the Observatorio del Teide

Author: F.G. Saturni, C.H.E. Arcaro, B. Balmaverde, J. Becerra González, A. Caccianiga, M. Capalbi, A. Lamastra, S. Lombardi, F. Lucarelli, R. Alves Batista, L.A. Antonelli, E.M. de Gouveia Dal Pino, R. Della Ceca, J.G. Green, A. Pagliaro, C. Righi, F. Tavecchio, S. Vercellone, A. Wolter, E. Amato, C. Bigongiari, M. Böttcher, G. Brunetti, P. Bruno, A. Bulgarelli, M. Cardillo, V. Conforti, A. Costa, G. Cusumano, V. Fioretti, S. Germani, A. Ghedina, F. Gianotti, V. Giordano, A. Giuliani, F. Incardona, A. La Barbera, G. Leto, F. Longo, G. Morlino, B. Olmi, N. Parmiggiani, P. Romano, G. Romeo, A. Stamerra, G. Tagliaferri, V. Testa, G. Tosti, P.A. Caraveo, and G. Pareschi
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Gamma ray, FOS: Physical sciences, Cherenkov, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, ASTRI Mini Array, Instrumentation and Methods for Astrophysics (astro-ph.IM), Cherenkov, Extragalactic, Gamma ray, ASTRI Mini Array, Extragalactic
Abstract: The ASTRI Mini-Array is a next-generation system of nine imaging atmospheric Cherenkov telescopes that is going to be built at the Observatorio del Teide site. After a first phase, in which the instrument will be operated as an experiment prioritizing a schedule of primary science cases, an observatory phase is foreseen in which other significant targets will be pointed. We focus on the observational feasibility of extragalactic sources and on astrophysical processes that best complement and expand the ASTRI Mini-Array core science, presenting the most relevant examples that are at reach of detection over long-term time scales and whose observation can provide breakthrough achievements in the very-high energy extragalactic science. Such examples cover a wide range of $\gamma$-ray emitters, including the study of AGN low states in the multi-TeV energy range, the possible detection of Seyfert galaxies with long exposures and the searches of dark matter lines above 10 TeV. Simulations of the presented objects show that the instrument performance will be competitive at multi-TeV energies with respect to current arrays of Cherenkov telescopes., Comment: 27 pages, 10 figures, 7 tables, published on JHEAp
Published: 2022
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8. Long-term Swift and Mets\'ahovi monitoring of SDSS J164100.10+345452.7 reveals multi-wavelength correlated variability

Author: P. Romano, A. Lähteenmäki, S. Vercellone, L. Foschini, M. Berton, C. M. Raiteri, V. Braito, S. Ciroi, E. Järvelä, S. Baitieri, I. Varglund, M. Tornikoski, S. Suutarinen, Osservatorio Astronomico di Brera, Department of Electronics and Nanoengineering, European Southern Observatory Santiago, National Institute for Astrophysics, University of Padova, Urbanización Villafranca Del Castillo, Metsähovi Radio Observatory, Aalto-yliopisto, and Aalto University
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), individual: SDSS J164100.10+345452.7 [Galaxies], Seyfert [Galaxies], active [Galaxies], Space and Planetary Science, FOS: Physical sciences, individuals: SDSS J164100.10+345452.7 [X-rays], Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report on the first multi-wavelength Swift monitoring campaign performed on SDSS J164100.10+345452.7, a nearby narrow-line Seyfert 1 galaxy formerly known as radio quiet which was recently detected both in the radio (at 37 GHz) and in the $\gamma$-rays, which hints at the presence of a relativistic jet. During our 20-month Swift campaign, while pursuing the primary goal of assessing the baseline optical/UV and X-ray properties of J1641, we caught two radio flaring episodes, one each year. Our strictly simultaneous multi-wavelength data closely match the radio flare and allow us to unambiguously link the jetted radio emission of J1641. Indeed, for the X-ray spectra preceding and following the radio flare a simple absorbed power-law model is not an adequate description, and an extra absorption component is required. The average spectrum of J1641 can be best described by an absorbed power law model with a photon index $\Gamma=1.93\pm0.12$, modified by a partially covering neutral absorber with a covering fraction $f=0.91_{-0.03}^{+0.02}$. On the contrary, the X-ray spectrum closest to the radio flare does not require such extra absorber and is much harder ($\Gamma_{\rm flare} \sim 0.7\pm0.4$), thus implying the emergence of a further, harder spectral component. We interpret this as the jet emission emerging from a gap in the absorber. The fractional variability we derive in the optical/UV and X-ray bands are found to be lower than the typical values reported in the literature, since our observations of J1641 are dominated by the source being in a low state. Under the assumption that the origin of the 37 GHz radio flare is the emergence of a jet from an obscuring screen also observed in the X-rays, the derived total jet power is $P^{\rm tot}_{\rm jet}=3.5\times10^{42}$ erg s$^{-1}$, comparable to the lowest measured in the literature. [Abridged], Comment: Accepted for publication in Astronomy and Astrophysics (13 pages, 4 figures, 8 tables)
Published: 2023

9. Long-term Swift and multiwavelength observations of two TeV-detected blazars with unknown redshifts

Author: B. Kapanadze, A. Gurchumelia, S. Vercellone, P. Romano, S. Kapanadze, and O. Kharshiladze
Subjects: Space and Planetary Science, Astronomy and Astrophysics
Published: 2023
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10. Sensitivity of the Cherenkov Telescope Array to TeV photon emission from the Large Magellanic Cloud

Author: A Acharyya, R Adam, A Aguasca-Cabot, I Agudo, A Aguirre-Santaella, J Alfaro, R Aloisio, R Alves Batista, E Amato, E O Angüner, C Aramo, C Arcaro, K Asano, J Aschersleben, H Ashkar, M Backes, A Baktash, C Balazs, M Balbo, J Ballet, A Bamba, A Baquero Larriva, V Barbosa Martins, U Barres de Almeida, J A Barrio, D Bastieri, P Batista, I Batkovic, J R Baxter, J Becerra González, J Becker Tjus, W Benbow, E Bernardini, M I Bernardos Martín, J Bernete Medrano, A Berti, B Bertucci, V Beshley, P Bhattacharjee, S Bhattacharyya, C Bigongiari, A Biland, E Bissaldi, F Bocchino, P Bordas, J Borkowski, E Bottacini, M Böttcher, F Bradascio, A M Brown, A Bulgarelli, L Burmistrov, S Caroff, A Carosi, E Carquín, S Casanova, E Cascone, F Cassol, M Cerruti, P Chadwick, S Chaty, A Chen, A Chiavassa, L Chytka, V Conforti, J Cortina, A Costa, H Costantini, G Cotter, S Crestan, P Cristofari, F D’Ammando, M Dalchenko, F Dazzi, A De Angelis, V De Caprio, E M de Gouveia Dal Pino, D De Martino, M de Naurois, V de Souza, M V del Valle, A G Delgado Giler, C Delgado, D della Volpe, D Depaoli, T Di Girolamo, A Di Piano, F Di Pierro, R Di Tria, L Di Venere, S Diebold, M Doro, D Dumora, V V Dwarkadas, C Eckner, K Egberts, G Emery, J Escudero, D Falceta-Goncalves, E Fedorova, S Fegan, Q Feng, D Ferenc, G Ferrand, E Fiandrini, M Filipovic, V Fioretti, L Foffano, G Fontaine, Y Fukui, D Gaggero, G Galanti, G Galaz, S Gallozzi, V Gammaldi, M Garczarczyk, C Gasbarra, D Gasparrini, A Ghalumyan, M Giarrusso, G Giavitto, N Giglietto, F Giordano, A Giuliani, J-F Glicenstein, P Goldoni, J Goulart Coelho, J Granot, D Green, J G Green, M-H Grondin, O Gueta, D Hadasch, P Hamal, T Hassan, K Hayashi, M Heller, S Hernández Cadena, N Hiroshima, B Hnatyk, R Hnatyk, W Hofmann, J Holder, M Holler, D Horan, P Horvath, M Hrabovsky, M Hütten, M Iarlori, T Inada, F Incardona, S Inoue, F Iocco, M Jamrozy, W Jin, I Jung-Richardt, J Juryšek, D Kantzas, V Karas, H Katagiri, D Kerszberg, J Knödlseder, N Komin, P Kornecki, K Kosack, G Kowal, H Kubo, A Lamastra, J Lapington, M Lemoine-Goumard, J-P Lenain, F Leone, G Leto, F Leuschner, E Lindfors, T Lohse, S Lombardi, F Longo, R López-Coto, A López-Oramas, S Loporchio, P L Luque-Escamilla, O Macias, P Majumdar, D Mandat, S Mangano, G Manicò, M Mariotti, P Marquez, G Marsella, J Martí, P Martin, M Martínez, D Mazin, S Menchiari, D M-A Meyer, D Miceli, M Miceli, J Michałowski, A Mitchell, R Moderski, L Mohrmann, M Molero, E Molina, T Montaruli, A Moralejo, D Morcuende, A Morselli, E Moulin, V Moya, R Mukherjee, K Munari, A Muraczewski, S Nagataki, T Nakamori, A Nayak, J Niemiec, M Nievas, M Nikołajuk, K Nishijima, K Noda, D Nosek, B Novosyadlyj, S Nozaki, M Ohishi, S Ohm, A Okumura, B Olmi, R A Ong, M Orienti, R Orito, M Orlandini, E Orlando, S Orlando, M Ostrowski, I Oya, A Pagliaro, M Palatka, F R Pantaleo, R Paoletti, J M Paredes, N Parmiggiani, B Patricelli, M Pech, M Pecimotika, M Persic, O Petruk, E Pierre, E Pietropaolo, G Pirola, M Pohl, E Prandini, C Priyadarshi, G Pühlhofer, M L Pumo, M Punch, F S Queiroz, A Quirrenbach, S Rainò, R Rando, S Razzaque, A Reimer, O Reimer, T Reposeur, M Ribó, T Richtler, J Rico, F Rieger, M Rigoselli, V Rizi, E Roache, G Rodriguez Fernandez, P Romano, G Romeo, J Rosado, A Rosales de Leon, B Rudak, C Rulten, I Sadeh, T Saito, M Sánchez-Conde, H Sano, A Santangelo, R Santos-Lima, S Sarkar, F G Saturni, A Scherer, P Schovanek, F Schussler, U Schwanke, O Sergijenko, M Servillat, H Siejkowski, C Siqueira, S Spencer, A Stamerra, S Stanič, C Steppa, T Stolarczyk, Y Suda, T Tavernier, M Teshima, L Tibaldo, D F Torres, N Tothill, M Vacula, B Vallage, P Vallania, C van Eldik, M Vázquez Acosta, M Vecchi, S Ventura, S Vercellone, A Viana, C F Vigorito, J Vink, V Vitale, V Vodeb, S Vorobiov, T Vuillaume, S J Wagner, R Walter, M White, A Wierzcholska, M Will, R Yamazaki, L Yang, T Yoshikoshi, M Zacharias, G Zaharijas, D Zavrtanik, M Zavrtanik, A A Zdziarski, V I Zhdanov, K Ziętara, M Živec, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and Cherenkov Telescope Array
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), photon, emission, acceleration, efficiency, Cherenkov Telescope Array, WIMP, diffusion, FOS: Physical sciences, Astronomy and Astrophysics, suppression, sensitivity, Navarro-Frenk-White profile, dark matter, photon, energy, flux, cosmic radiation, spectrum, energy, high, Space and Planetary Science, cloud, TeV, spectral, galaxy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], nucleus, cosmic radiation
Abstract: A deep survey of the Large Magellanic Cloud at ~0.1-100TeV photon energies with the Cherenkov Telescope Array is planned. We assess the detection prospects based on a model for the emission of the galaxy, comprising the four known TeV emitters, mock populations of sources, and interstellar emission on galactic scales. We also assess the detectability of 30 Doradus and SN 1987A, and the constraints that can be derived on the nature of dark matter. The survey will allow for fine spectral studies of N157B, N132D, LMC P3, and 30 Doradus C, and half a dozen other sources should be revealed, mainly pulsar-powered objects. The remnant from SN 1987A could be detected if it produces cosmic-ray nuclei with a flat power-law spectrum at high energies, or with a steeper index 2.3-2.4 pending a flux increase by a factor >3-4 over ~2015-2035. Large-scale interstellar emission remains mostly out of reach of the survey if its >10GeV spectrum has a soft photon index ~2.7, but degree-scale 0.1-10TeV pion-decay emission could be detected if the cosmic-ray spectrum hardens above >100GeV. The 30 Doradus star-forming region is detectable if acceleration efficiency is on the order of 1-10% of the mechanical luminosity and diffusion is suppressed by two orders of magnitude within, Accepted for publication in MNRAS. Corresponding authors: Pierrick Martin, Maria Isabel Bernardos Martin, Fabio Iocco
Published: 2023
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11. The 100-month Swift catalogue of supergiant fast X–ray transients

Author: P. Romano, P. A. Evans, E. Bozzo, V. Mangano, S. Vercellone, C. Guidorzi, L. Ducci, J. A. Kennea, S. D. Barthelmy, D. M. Palmer, H. A. Krimm, and S. B. Cenko
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Supergiant Fast X-ray Transients (SFXT) are High Mass X-ray Binaries displaying X-ray outbursts reaching peak luminosities of 10$^{38}$ erg/s and spend most of their life in more quiescent states with luminosities as low as 10$^{32}$-10$^{33}$ erg/s. The main goal of our comprehensive and uniform analysis of the SFXT Swift triggers is to provide tools to predict whether a transient which has no known X-ray counterpart may be an SFXT candidate. These tools can be exploited for the development of future missions exploring the variable X-ray sky through large FoV instruments. We examined all available data on outbursts of SFXTs that triggered the Swift/BAT collected between 2005-08-30 and 2014-12-31, in particular those for which broad-band data, including the Swift/XRT ones, are also available. We processed all BAT and XRT data uniformly with the Swift Burst Analyser to produce spectral evolution dependent flux light curves for each outburst. The BAT data allowed us to infer useful diagnostics to set SFXT triggers apart from the general GRB population, showing that SFXTs give rise uniquely to image triggers and are simultaneously very long, faint, and `soft' hard-X-ray transients. The BAT data alone can discriminate very well the SFXTs from other fast transients such as anomalous X-ray pulsars and soft gamma repeaters. However, to distinguish SFXTs from, for instance, accreting millisecond X-ray pulsars and jetted tidal disruption events, the XRT data collected around the time of the BAT triggers are decisive. The XRT observations of 35/52 SFXT BAT triggers show that in the soft X-ray energy band, SFXTs display a decay in flux from the peak of the outburst of at least 3 orders of magnitude within a day and rarely undergo large re-brightening episodes, favouring in most cases a rapid decay down to the quiescent level within 3-5 days (at most). [Abridged], Accepted for publication in Astronomy and Astrophysics. 18 pages, 11 figures
Published: 2023
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12. Cherenkov Telescope Array : the World’s largest VHE gamma-ray observatory

Author: Roberta Zanin, H. Abdalla, H. Abe, S. Abe, A. Abusleme, F. Acero, A. Acharyya, V. Acin Portella, K. Ackley, R. Adam, C. Adams, S.S. Adhikari, I. Aguado Ruesga, I. Agudo, R. Aguilera, A. Aguirre Santaella, F. Aharonian, A. Alberdi, R. Alfaro, J. Alfaro, C. Alispach, R. Aloisio, R. Alves Batista, J.P. Amans, L. Amati, E. Amato, L. Ambrogi, G. Ambrosi, M. Ambrosio, R. Ammendola, J. Anderson, M. Anduze, E.O. Anguner, L.A. Antonelli, V. Antonuccio, P. Antoranz, R. Anutarawiramkul, J. Aragunde Gutierrez, C. Aramo, A. Araudo, M. Araya, A. Arbet Engels, C. Arcaro, V. Arendt, C. Armand, T. Armstrong, F. Arqueros, L. Arrabito, B. Arsioli, M. Artero, K. Asano, Y. Ascasibar, J. Aschersleben, M. Ashley, P. Attina, P. Aubert, C. B. Singh, D. Baack, A. Babic, M. Backes, V. Baena, S. Bajtlik, A. Baktash, C. Balazs, M. Balbo, O. Ballester, J. Ballet, B. Balmaverde, A. Bamba, R. Bandiera, A. Baquero Larriva, P. Barai, C. Barbier, V. Barbosa Martins, M. Barcelo, M. Barkov, M. Barnard, L. Baroncelli, U. Barres de Almeida, J.A. Barrio, D. Bastieri, P.I. Batista, I. Batkovic, C. Bauer, R. Bautista González, J. Baxter, U. Becciani, J. Becerra González, Y. Becherini, G. Beck, J. Becker Tjus, W. Bednarek, A. Belfiore, L. Bellizzi, R. Belmont, W. Benbow, D. Berge, E. Bernardini, M.I. Bernardos, K. Bernlöhr, A. Berti, M. Berton, B. Bertucci, V. Beshley, N. Bhatt, S. Bhattacharyya, W. Bhattacharyya, B. Y. Bi, G. Bicknell, N. Biederbeck, C. Bigongiari, A. Biland, R. Bird, E. Bissaldi, J. Biteau, M. Bitossi, O. Blanch, M. Blank, J. Blazek, J. Bobin, C. Boccato, F. Bocchino, C. Boehm, M. Bohacova, C. Boisson, J. Boix, J.P. Bolle, J. Bolmont, G. Bonanno, C. Bonavolontà, L. Bonneau Arbeletche, G. Bonnoli, P. Bordas, J. Borkowski, R. Bose, D. Bose, Z. Bosnjak, E. Bottacini, Markus Böttcher, M.T. Botticella, C. Boutonnet, F. Bouyjou, V. Bozhilov, E. Bozzo, L. Brahimi, C. Braiding, S. Brau Nogue, S. Breen, J. Bregeon, M. Breuhaus, A. Brill, W. Brisken, E. Brocato, A.M. Brown, K. Brügge, P. Brun, F. Brun, L. Brunetti, G. Brunetti, P. Bruno, A. Bruno, A. Bruzzese, N. Bucciantini, J. H. Buckley, R. Bühler, A. Bulgarelli, T. Bulik, M. Bünning, M. Bunse, M. Burton, A. Burtovoi, M. Buscemi, S. Buschjager, G. Busetto, J. Buss, K. Byrum, A. Caccianiga, F. Cadoux, A. Calanducci, C. Calderon, J. Calvo Tovar, R. A. Cameron, P. Campana, R. Canestrari, F. Cangemi, B. Cantlay, M. Capalbi, M. Capasso, M. Cappi, A. Caproni, R. Capuzzo Dolcetta, P. Caraveo, V. Cárdenas, L. Cardiel, M. Cardillo, C. Carlile, S. Caroff, R. Carosi, A. Carosi, E. Carquin, M. Carrere, J.M. Casandjian, S. Casanova, F. Cassol, F. Catalani, O. Catalano, D. Cauz, A. Ceccanti, C. Celestino Silva, K. Cerny, M. Cerruti, E. Chabanne, P. Chadwick, Y. Chai, P. Chambery, C. Champion, S. Chaty, A. Chen, K. Cheng, M. Chernyakova, G. Chiaro, A. Chiavassa, M. Chikawa, V.R. Chitnis, J. Chudoba, L. Chytka, S. Cikota, A. Circiello, P. Clark, M. Colak, E. Colombo, S. Colonges, A. Comastri, A. Compagnino, V. Conforti, E. Congiu, R. Coniglione, J. Conrad, F. Conte, J.L. Contreras, P. Coppi, R. Cornat, J. Coronado Blazquez, J. Cortina, A. Costa, H. Costantini, G. Cotter, B. Courty, S. Covino, S. Crestan, P. Cristofari, R. Crocker, J. Croston, K. Cubuk, O. Cuevas, X. Cui, G. Cusumano, S. Cutini, G. D'Amico, F. D'Ammando, P. D'Avanzo, P. Da Vela, M. Dadina, S. Dai, M. Dalchenko, M. Dall'Ora, M.K. Daniel, J. Dauguet, I. Davids, J. Davies, B. Dawson, A. De Angelis, A.E. de Araujo Carvalho, M. de Bony de Lavergne, G. De Cesare, F. de Frondat, I. de la Calle, E. de Gouveia Dal Pino, B. De Lotto, A. De Luca, D. De Martino, M. de Naurois, E. de Ona Wilhelmi, F. De Palma Persio, N. De Simone, V. de Souza Valle, E. Delagnes, G. Deleglise Reznicek, C. Delgado, A.G. Delgado Giler, J. Delgado Mengual Valle, Domenico Della Volpe, D. Depaoli, J. Devin, T. Di Girolamo, C. Di Giulio Pierro, L. Di Venere, C. Díaz, C. Dib, S. Diebold, S. Digel, A. Djannati Atai, J. Djuvsland, A. Dmytriiev, K. Docher, A. Domínguez, D. Dominis Prester, A. Donini, D. Dorner, M. Doro, Rita Cassia dos Anjos, J.L. Dournaux, T. Downes, G. Drake, H. Drass, D. Dravins, C. Duangchan, A. Duara, G. Dubus, L. Ducci, C. Duffy, D. Dumora, K. Dundas Mora, A. Durkalec, V.V. Dwarkadas, J. Ebr, C. Eckner, J. Eder, E. Edy, K. Egberts, S. Einecke, C. Eleftheriadis, D. Elsässer, G. Emery, D. Emmanoulopoulos, J.P. Ernenwein, M. Errando, P. Escarate, J. Escudero, C. Espinoza, S. Ettori, A. Eungwanichayapant, P. Evans, C. Evoli, M. Fairbairn, D. Falceta Goncalves, A. Falcone, V. Fallah Ramazanı, R. Falomo, K. Farakos, G. Fasola, A. Fattorini, Y. Favre, R. Fedora, E. Fedorova, K. Feijen, Q. Feng, G. Ferrand, G. Ferrara, O. Ferreira, M. Fesquet, E. Fiandrini, A. Fiasson, M. Filipovic, D. Fink, J.P. Finley, V. Fioretti, D.F.G. Fiorillo, M. Fiorini, S. Flis, H. Flores, L. Foffano, C. Fohr, M.V. Fonseca, L. Font, G. Fontaine, O. Fornieri, P. Fortin, L. Fortson, N. Fouque, B. Fraga, A. Franceschini, F.J. Franco, L. Freixas Coromina, L. Fresnillo, D. Fugazza, Y. Fujita, S. Fukami, Y. Fukazawa, D. Fulla, S. Funk, A. Furniss, S. Gabici, D. Gaggero, G. Galanti, P. Galdemard, Y. A. Gallant, D. Galloway, S. Gallozzi, V. Gammaldi, R. Garcia, L. E. García-Muñoz, E. Garcia Lopez, F. Gargano, C. Gargano, S. Garozzo, D. Gascon, T. Gasparetto, D. Gasparrini, H. Gasparyan, M. Gaug, N. Geffroy, A. Gent, S. Germani, A. Ghalumyan, A. Ghedina, G. Ghirlanda, F. Gianotti, S. Giarrusso, M. Giarrusso, G. Giavitto, B. Giebels, N. Giglietto, V. Gika, F. Gillardo, R. Gimenes, F. Giordano, E. Giro, M. Giroletti, Andrea Giuliani, M. Gjaja, J.F. Glicenstein, P. Gliwny, H. Goksu, P. Goldoni, J.L. Gomez, M.M. Gonzalez, Juan Manuel Gonzalez, K.S. Gothe, D. Gotz Coelho, T. Grabarczyk, R. Graciani, P. Grandi, G. Grasseau, D. Grasso, D. Green, J. Green, T. Greenshaw, P. Grespan, A. Grillo, M.H. Grondin, J. Grube, V. Guarino, B. Guest, O. Gueta, M. Günduz, S. Gunji, G. Gyuk, J. Hackfeld, D. Hadasch, L. Hagge, A. Hahn, J.E. Hajlaoui, A. Halim, P. Hamal, W. Hanlon, Y. Harada, M.J. Hardcastle, M. Harvey Collado, T. Haubold, A. Haupt, M. Havelka, K. Hayashi, M. Hayashida, H. He, L. Heckmann, M. Heller, F. Henault, Gilles Henri, G. Hermann, S. Hernández Cadena, J. Herrera Llorente, O. Hervet, J. Hinton, A. Hiramatsu, K. Hirotani, B. Hnatyk, R. Hnatyk, J.K. Hoang, D. H.H. Hoffmann, C. Hoischen, J. Holder, M. Holler, B. Hona, D. Horan, Dieter Horns, P. Horvath, J. Houles, M. Hrabovsky, D. Hrupec, Y. Huang, J.‑M. Huet, G. Hughes, G. Hull, T.B. Humensky, M. Hütten, M. Iarlori, J.M. Illa, R. Imazawa, T. Inada, F. Incardona, A. Ingallinera, S. Inoue, T. Inoue, Y. Inoue, F. Iocco, K. Ioka, M. Ionica, S. Iovenitti, A. Iriarte, K. Ishio, W. Ishizaki, Y. Iwamura, J. Jacquemier, M. Jacquemont, M. Jamrozy, P. Janecek, F. Jankowsky, A. JardinBlicq, C. Jarnot, P. Jean Martínez, L. Jocou, N. Jordana, M. Josselin, I. JungRichardt, F.J.P.A. Junqueira, C. Juramy Gilles, P. Kaaret, L.H.S. Kadowaki, M. Kagaya, R. Kankanyan, D. Kantzas, V. Karas, A. Karastergiou, S. Karkar, J. Kasperek, H. Katagiri, J. Kataoka, K. Katarzynski, S. Katsuda, N. Kawanaka, D. Kazanas, D. Kerszberg, B. Khélifi, M.C. Kherlakian, T.P. Kian, D.B. Kieda, T. Kihm, S. Kim, S. Kisaka, R. Kissmann, R. Kleijwegt, G. Kluge, W. Kluźniak, J. Knapp, A. Kobakhidze, Y. Kobayashi, B. Koch, J. Kocot, K. Kohri, N. Komin, A. Kong, K. Kosack, F. Krack, M. Krause, F. Krennrich, H. Kubo, V. N. Kudryavtsev, S. Kunwar, J. Kushida, P. Kushwaha, Barbera Parola, G. La Rosa, R. Lahmann, A. Lamastra, M. Landoni, D. Landriu, R.G. Lang, J. Lapington, P. Laporte, P. Lason, J. Lasuik, J. Lazendic Galloway, T. Le Flour, P. Le Sidaner, S. Leach, S.H. Lee, W.H. Lee, S. Lee Oliveira, A. Lemiere, M. Lemoine Goumard, J.P. Lenain, F. Leone, V. Leray, G. Leto, F. Leuschner, R. Lindemann, E. Lindfors, L. Linhoff, I. Liodakis, A. Lipniacka, M. Lobo, Thomas Lohse, S. Lombardi, A. Lopez, M. Lopez, R. Lopez Coto, F. Louis, M. Louys, F. Lucarelli, H. Ludwig Boudi, P.L. Luque Escamilla, M.C. Maccarone, E. Mach, A.J. Maciejewski, J. Mackey, P. Maeght, C. Maggio, G. Maier, P. Majumdar, M. Makariev, M. Mallamaci, R. Malta Nunes de Almeida, D. Malyshev, D. Mandat, G. Maneva, M. Manganaro, P. Manigot, K. Mannheim, N. Maragos, D. Marano, M. Marconi, A. Marcowith, M. Marculewicz, B. Marcun, J. Marin, N. Marinello, P. Marinos, S. Markoff, P. Marquez, G. Marsella, J. M. Martin, P. G. Martin, M. Martinez, G. Martinez, O. Martinez, H. Martinez Huerta, C. Marty, R. Marx, N. Masetti, P. Massimino, H. Matsumoto, N. Matthews, G. Maurin, W. Max Moerbeck, N. Maxted, M.N. Mazziotta, S.M. Mazzola, J.D. Mbarubucyeye, L. Mc Comb, I. McHardy, S. McKeague, S. McMuldroch, E. Medina, D. Medina Miranda, A. Melandri, C. Melioli, D. Melkumyan, S. Menchiari, S. Mereghetti, G. Merino Arevalo, E. Mestre, J.L. Meunier, T. Meures, S. Micanovic, M. Miceli, M. Michailidis, J. Michalowski, T. Miener, I. Mievre, J. D. Miller, T. Mineo, M. Minev, J.M. Miranda, A. Mitchell, T. Mizuno, B. A. Mode, R. Moderski, L. Mohrmann, E. Molinari, T. Montaruli, I. Monteiro, C. Moore, A. Moralejo, D. Morcuende Parrilla, E. Moretti, K. Mori, P. Moriarty, K. Morik, P. Morris, A. Morselli, K. Mosshammer, R. Mukherjee, J. Muller, C. Mundell, J. Mundet, T. Murach, A. Muraczewski, H. Muraishi, I. Musella, A. Musumarra, A. Nagai, S. Nagataki, T. Naito, T. Nakamori, K. Nakashima, K. Nakayama, N. Nakhjiri, G. Naletto, D. Naumann, L. Nava, M.A. Nawaz, H. Ndiyavala, D. Neise, L. Nellen, R. Nemmen, N. Neyroud, K. Ngernphat, T. Nguyen Trung, L. Nicastro, L. Nickel, J. Niemiec, D. Nieto, C. Nigro, M. Nikołajuk, D. Ninci, K. Noda, Y. Nogami, S. Nolan, R. P. Norris, D. Nosek, M. Nöthe, V. Novotny, S. Nozaki, F. Nunio, P. O'Brien, K. Obara, Y. Ohira, M. Ohishi, S. Ohm, T. Oka, N. Okazaki, A. Okumura, C. Oliver, G. Olivera, B. Olmi, M. Orienti, R. Orito, M. Orlandini, E. Orlando, J.P. Osborne, M. Ostrowski, N. Otte, E. Ovcharov, E. Owen, I. Oya, A. Ozieblo, M. Padovani, A. Pagliaro, A. Paizis, M. Palatiello, M. Palatka, E. Palazzi, J.‑L. Panazol, D. Paneque, S. Panny, Francesca Romana Pantaleo, M. Panter, M. Paolillo, A. Papitto, A. Paravac, J.M. Paredes, G. Pareschi, N. Parmiggiani, R.D. Parsons, P. Paśko, S. R. Patel, B. Patricelli, L. Pavletic, S. Pavy, A. Peer, M. Pecimotika, M.G. Pellegriti, P. Peñil Del Campo, A. Pepato, S. Perard, C. Perennes, M. Peresano, A. Perez Aguilera, J. Perez Romero, M.A. Perez Torres, M. Persic, P. O. Petrucci, O. Petruk, B. Peyaud, K. Pfrang, E. Pian, P. Piatteli, E. Pietropaolo, R. Pillera, D. Pimentel, F. Pintore, C. Pio Garcia, G. Pirola, F. Piron, S. Pita, M. Pohl, V. Poireau, A. Pollo, M. Polo, C. Pongkitivanichkul, J. Porthault, J. Powell, D. Pozo, R.R. Prado, E. Prandini, J. Prast, K. Pressard, G. Principe, N. Produit, D. Prokhorov, H. Prokoph, H. Przybilski, E. Pueschel, G. Pühlhofer, I. Puljak, M.L. Pumo, M. Punch, F. Queiroz, J. Quinn, A. Quirrenbach, P.J. Rajda, R. Rando, S. Razzaque, S. Recchia, P. Reichherzer, O. Reimer, A. Reisenegger, Q. Remy, M. Renaud, T. Reposeur, B. Reville, J.M. Reymond, J. Reynolds, D. Ribeiro, M. Ribo, G. Richards, J. Rico, F. Rieger, L. Riitano, M. Riquelme, D. Riquelme, S. Rivoire, V. Rizi, E. Roache, M. Roche, J. Rodriguez, G. Rodriguez Fernandez, J.C. Rodriguez Ramirez, J.J. Rodriguez Vazquez, G. Rojas, P. Romano, G. Romeo Lobato, C. Romoli, M. Roncadelli, J. Rosado, A. Rosales de Leon, G. Rowell, A. Rugliancich, J.E. Ruiz del Mazo, C. Rulten, C. Russell, F. Russo Hatlen, S. Safi Harb, L. Saha, V. Sahakian, S. Sailer, T. Saito, N. Sakaki, S. Sakurai, G. Salina, H. Salzmann, D. Sanchez, H. Sandaker, A. Sandoval, P. Sangiorgi, M. Sanguillon, H. Sano, M. Santander, A. Santangelo, R. Santos Lima, A. Sanuy, L. Sapozhnikov, T. Saric, S. Sarkar, H. Sasaki, N. Sasaki, Y. Sato, F.G. Saturni, M. Sawada, J. Schaefer, A. Scherer, J. Scherpenberg, P. Schipani, B. Schleicher, J. Schmoll, M. Schneider, H. Schoorlemmer, P. Schovanek, F. Schussler, B. Schwab, U. Schwanke, J. Schwarz, E. Sciacca, S. Scuderi, M. Seglar Arroyo, I. Seitenzahl, D. Semikoz, O. Sergijenko, J.E. Serna Franco, Karol Seweryn, V. Sguera, A. Shalchi, R.Y. Shang, P. Sharma, L. Sidoli, J. Sieiro, H. Siejkowski, A. Sillanpaa, B.B. Singh, K.K. Singh, A. Sinha, C. Siqueira, J. Sitarek, P. Sizun, V. Sliusar, D. Sobczynska, R.W. Sobrinho, H. Sol, G. Sottile, H. Spackman, S. Spencer, G. Spengler, D. Spiga, W. Springer, A. Stamerra, S. Stanic, R. Starling, Ł. Stawarz, Stanislav Stefanik, C. Stegmann, A. Steiner, S. Steinmassl, C. Stella, R. Sternberger, M. Sterzel, C. Stevens, B. Stevenson, T. Stolarczyk, G. Stratta, U. Straumann, J. Striskovic, M. Strzys, R. Stuik, M. Suchenek, Y. Sunada, Tiina Suomijarvi, T. Suric, H. Suzuki, P. Swierk, T. Szepieniec, K. Tachihara, G. Tagliaferri, H. Tajima, N. Tajima, D. Tak, H. Takahashi, M. Takahashi, J. Takata, R. Takeishi, T. Tam, M. Tanaka, T. Tanaka, S. Tanaka, M. Tavani, F. Tavecchio, T. Tavernier, A. Russ Taylor, L.A. Tejedor, P. Temnikov, K. Terauchi, J.C. Terrazas, R. Terrier, T. Terzic, M. Teshima, D. Thibaut, F. Thocquenne, W. Tian, L. Tibaldo, A. Tiengo, M. Tluczykont, C.J. Todero Peixoto, K. Toma, L. Tomankova, J. Tomastik, M. Tornikoski, D.F. Torres, E. Torresi, G. Tosti, L. Tosti, N. Tothill, F. Toussenel, G. Tovmassian, C. Trichard, M. Trifoglio, A. Trois, S. Truzzi, A. Tsiahina, B. Turk, A. Tutone, Y. Uchiyama, P. Utayarat, L. Vaclavek, M. Vacula, V. Vagelli, F. Vagnetti, J.A. Valdivia, M. Valentino, A. Valio, B. Vallage, P. Vallania Quispe, A.M. van den Berg, W. van Driel, C. van Eldik, C. van Rensburg, Brian van Soelen, J. Vandenbroucke, G. Vasileiadis, V. Vassiliev, M. Vazquez Acosta, M. Vecchi, A. Vega, J. Veh, P. Veitch, C. Venter, S. Ventura, S. Vercellone, V. Verguilov, G. Verna, S. Vernetto, V. Verzi, G.P. Vettolani, C. Veyssiere, I. Viale, A. Viana, N. Viaux, J. Vignatti, C.F. Vigorito, J. Villanueva, V. Vitale, V. Vittorini, V. Vodeb, N. Vogel, V. Voisin, S. Vorobiov, M. Vrastil, T. Vuillaume, S.J. Wagner, P. Wagner, K. Wakazono, S.P. Wakely, M. Ward, D. Warren, J. Watson, M. Wechakama, P. Wegner, A. Weinstein, C. Weniger, F. Werner, H. Wetteskind, M. L. White, A. Wierzcholska, S. Wiesand, R. Wijers, M. Wilkinson, M. Will, J. Williams, T. J. Williamson, A. Wolter, Y.W. Wong, M. Wood, T. Yamamoto, H. Yamamoto, Y. Yamane, R. Yamazaki, S. Yanagita, L. Yang, S. Yoo, T. Yoshida, T. Yoshikoshi, P. Yu, A. Yusafzai, Michael Zacharias, B. Zaldivar, L. Zampieri, R. Zanin, R. Zanmar Sanchez, D. Zaric, M. Zavrtanik, D. Zavrtanik, Andrzej Zdziarski, A. Zech, H. Zechlin, A. Zenin, A. Zerwekh, K. Ziętara, A. Zink, J. Ziolkowski, M. Zivec, A. Zmija, Współautorami artykułu są członkowie CTA Observatory, CTA Consortium i LST Collaboration w liczbie 1139, Astronomy, Research unit Nuclear & Hadron Physics, and Research unit Astroparticle Physics
Subjects: Physics, Observatory, Gamma ray, Astronomy
Abstract: Very-high Energy (VHE) gamma-ray astroparticle physics is a relatively young field, and observations over the past decade have surprisingly revealed almost two hundred VHE emitters which appear to act as cosmic particle accelerators. These sources are an important component of the Universe, influencing the evolution of stars and galaxies. At the same time, they also act as a probe of physics in the most extreme environments known - such as in supernova explosions, and around or after the merging of black holes and neutron stars. However, the existing experiments have provided exciting glimpses, but often falling short of supplying the full answer. A deeper understanding of the TeV sky requires a significant improvement in sensitivity at TeV energies, a wider energy coverage from tens of GeV to hundreds of TeV and a much better angular and energy resolution with respect to the currently running facilities. The next generation gamma-ray observatory, the Cherenkov Telescope Array Observatory (CTAO), is the answer to this need. In this talk I will present this upcoming observatory from its design to the construction, and its potential science exploitation. CTAO will allow the entire astronomical community to explore a new discovery space that will likely lead to paradigm-changing breakthroughs. In particular, CTA has an unprecedented sensitivity to short (sub-minute) timescale phenomena, placing it as a key instrument in the future of multi-messenger and multi-wavelength time domain astronomy. I will conclude the talk presenting the first scientific results obtained by the LST-1, the prototype of one CTAO telescope type - the Large-Sized Telescope, that is currently under commission., PoS: Proceedings of Science, 395, ISSN:1824-8039, Proceedings of 37th International Cosmic Ray Conference (ICRC2021)
Published: 2022

13. Galactic Observatory Science with the ASTRI Mini-Array at the Observatorio del Teide

Author: A. D'Aì, E. Amato, A. Burtovoi, A.A. Compagnino, M. Fiori, A. Giuliani, N. La Palombara, A. Paizis, G. Piano, F.G. Saturni, A. Tutone, A. Belfiore, M. Cardillo, S. Crestan, G. Cusumano, M. Della Valle, M. Del Santo, A. La Barbera, V. La Parola, S. Lombardi, S. Mereghetti, G. Morlino, F. Pintore, P. Romano, S. Vercellone, A. Antonelli, C. Arcaro, C. Bigongiari, M. Böettcher, P. Bruno, A. Bulgarelli, V. Conforti, A. Costa, E. de Gouveia Dal Pino, V. Fioretti, S. Germani, A. Ghedina, F. Gianotti, V. Giordano, F. Incardona, G. Leto, F. Longo, A. López Oramas, F. Lucarelli, B. Olmi, A. Pagliaro, N. Parmiggiani, G. Romeo, A. Stamerra, V. Testa, G. Tosti, G. Umana, L. Zampieri, P. Caraveo, and G. Pareschi
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: The ASTRI (Astrofisica con Specchi a Tecnologia Replicante Italiana) Mini-Array will be composed of nine imaging atmospheric Cherenkov telescopes at the Observatorio del Teide site. The array will be best suited for astrophysical observations in the 0.3-200 TeV range with an angular resolution of few arc-minutes and an energy resolution of 10-15\%. A core-science programme in the first four years will be devoted to a limited number of key targets, addressing the most important open scientific questions in the very-high energy domain. At the same time, thanks to a wide field of view of about 10 degrees, ASTRI Mini-Array will observe many additional field sources, which will constitute the basis for the long-term observatory programme that will eventually cover all the accessible sky. In this paper, we review different astrophysical Galactic environments, e.g. pulsar wind nebulae, supernova remnants, and gamma-ray binaries, and show the results from a set of ASTRI Mini-Array simulations of some of these field sources made to highlight the expected performance of the array (even at large offset angles) and the important additional observatory science that will complement the core-science program., Comment: Accepted for publication in Journal of High-Energy Astrophysics
Published: 2022
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14. ASTRI Mini-Array Core Science at the Observatorio del Teide

Author: S. Vercellone, C. Bigongiari, A. Burtovoi, M. Cardillo, O. Catalano, A. Franceschini, S. Lombardi, L. Nava, F. Pintore, A. Stamerra, F. Tavecchio, L. Zampieri, R. Alves Batista, E. Amato, L.A. Antonelli, C. Arcaro, J. Becerra González, G. Bonnoli, M. Böttcher, G. Brunetti, A.A. Compagnino, S. Crestan, A. D'Aì, M. Fiori, G. Galanti, A. Giuliani, E.M. de Gouveia Dal Pino, J.G. Green, A. Lamastra, M. Landoni, F. Lucarelli, G. Morlino, B. Olmi, E. Peretti, G. Piano, G. Ponti, E. Poretti, P. Romano, F.G. Saturni, S. Scuderi, A. Tutone, G. Umana, J.A. Acosta-Pulido, P. Barai, A. Bonanno, G. Bonanno, P. Bruno, A. Bulgarelli, V. Conforti, A. Costa, G. Cusumano, M. Del Santo, M.V. del Valle, R. Della Ceca, D.A. Falceta-Gonçalves, V. Fioretti, S. Germani, R.J. García-López, A. Ghedina, F. Gianotti, V. Giordano, M. Kreter, F. Incardona, S. Iovenitti, A. La Barbera, N. La Palombara, V. La Parola, G. Leto, F. Longo, A. López-Oramas, M.C. Maccarone, S. Mereghetti, R. Millul, G. Naletto, A. Pagliaro, N. Parmiggiani, C. Righi, J.C. Rodríguez-Ramírez, G. Romeo, P. Sangiorgi, R. Santos de Lima, G. Tagliaferri, V. Testa, G. Tosti, M. Vázquez Acosta, N. Żywucka, P.A. Caraveo, and G. Pareschi
Subjects: ASTRI, Imaging atmospheric Cherenkov arrays, Very high-energy gamma ray astrophysics, Astroparticle, High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: The ASTRI (Astrofisica con Specchi a Tecnologia Replicante Italiana) Project led by the Italian National Institute for Astrophysics (INAF) is developing and will deploy at the Observatorio del Teide a mini-array (ASTRI Mini-Array) composed of nine telescopes similar to the small-size dual-mirror Schwarzschild-Couder telescope (ASTRI-Horn) currently operating on the slopes of Mt. Etna in Sicily. The ASTRI Mini-Array will surpass the current Cherenkov telescope array differential sensitivity above a few tera-electronvolt (TeV), extending the energy band well above hundreds of TeV. This will allow us to explore a new window of the electromagnetic spectrum, by convolving the sensitivity performance with excellent angular and energy resolution figures. In this paper we describe the Core Science that we will address during the first four years of operation, providing examples of the breakthrough results that we will obtain when dealing with current open questions, such as the acceleration of cosmic rays, cosmology and fundamental physics and the new window, for the TeV energy band, of the time-domain astrophysics., Comment: Published in Journal of High Energy Astrophysics. 46 Figures, 7 Tables
Published: 2022
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15. AGILE Observations of GRB 220101A: A 'New Year's Burst' with an Exceptionally Huge Energy Release

Author: A. Ursi, M. Romani, G. Piano, F. Verrecchia, F. Longo, C. Pittori, M. Tavani, A. Bulgarelli, M. Cardillo, C. Casentini, P. W. Cattaneo, E. Costa, M. Feroci, V. Fioretti, L. Foffano, F. Lucarelli, M. Marisaldi, A. Morselli, L. Pacciani, N. Parmiggiani, P. Tempesta, A. Trois, and S. Vercellone
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report the AGILE observations of GRB 220101A, which took place at the beginning of 1st January 2022 and was recognized as one of the most energetic gamma-ray bursts (GRBs) ever detected since their discovery. The AGILE satellite acquired interesting data concerning the prompt phase of this burst, providing an overall temporal and spectral description of the event in a wide energy range, from tens of keV to tens of MeV. Dividing the prompt emission into three main intervals, we notice an interesting spectral evolution, featuring a notable hardening of the spectrum in the central part of the burst. The average fluxes encountered in the different time intervals are relatively moderate, with respect to those of other remarkable bursts, and the overall fluence exhibits a quite ordinary value among the GRBs detected by MCAL. However, GRB 220101A is the second farthest event detected by AGILE, and the burst with the highest isotropic equivalent energy of the whole MCAL GRB sample, releasing E_iso=2.54x10^54 erg and exhibiting an isotropic luminosity of L_iso=2.34x10^52 erg/s (both in the 400 keV - 10 MeV energy range). We also analyzed the first 10^6 s of the afterglow phase, using the publicly available Swift XRT data, carrying out a theoretical analysis of the afterglow, based on the forward shock model. We notice that GRB 220101A is with high probability surrounded with a wind-like density medium, and that the energy carried by the initial shock shall be a fraction of the total E_iso, presumably near 50%., Comment: 16 pages, 9 figures, 4 tables
Published: 2022
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16. Perspectives of blazar studies with future space missions

Author: I. Donnarumma, S. Vercellone, and ITA
Subjects: 0303 health sciences, business.industry, Computer science, Astrophysics::High Energy Astrophysical Phenomena, Space (commercial competition), 01 natural sciences, Space exploration, 03 medical and health sciences, 030301 anatomy & morphology, 0103 physical sciences, Systems engineering, General Earth and Planetary Sciences, General Agricultural and Biological Sciences, Blazar, business, 010303 astronomy & astrophysics, General Environmental Science, Fermi Gamma-ray Space Telescope, Agile software development
Abstract: Since the AGILE and Fermi launch, the synergy between gamma-ray experiments and other space- and ground-based observatories has been the key to carry out multi-wavelength campaign aimed at understanding the physical mechanisms responsible for the observed gamma-ray emission in astrophysical sources. Blazars are the best examples of astrophysical sources where this strategy has been applied. The big efforts put in place for blazars to obtain coordinated observations with a broad coverage of the electromagnetic spectrum are providing new diagnostics of the physical processes at work in these sources, raising a lot of challenges for the theoretical interpretation. These could be partially solved through further observations with ground- and space-based facilities, therefore requiring new advances in technology and mission profile design. We will discuss how the lessons learned from current $$\gamma$$-ray observatories represent an important heritage for future missions expected to play a crucial role in the understanding of extreme phenomena in the high-energy domain.
Published: 2019
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17. Unveiling the origin of the gamma-ray emission in NGC 1068 with the Cherenkov Telescope Array

Author: Alessandra Lamastra, Fabrizio Tavecchio, Marco Landoni, P. Romano, S. Vercellone, and ITA
Subjects: Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Relativistic particle, Spitzer Space Telescope, Observatory, gamma rays: galaxies, 0103 physical sciences, galaxies: Seyfert: individual: NGC 1068, AGN, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, galaxies, 010308 nuclear & particles physics, Gamma ray, Active Galactic Nuclei, Astronomy and Astrophysics, Cherenkov Telescope Array, Galaxy, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope
Abstract: Several observations are revealing the widespread occurrence of mildly relativistic wide-angle AGN winds strongly interacting with the gas of their host galaxy. Such winds are potential cosmic-ray accelerators, as supported by gamma-ray observations of the nearby Seyfert galaxy NGC 1068 with the Fermi gamma-ray space telescope. The non-thermal emission produced by relativistic particles accelerated by the AGN-driven wind observed in the circum-nuclear molecular disk of such galaxy is invoked to produce the gamma-ray spectrum. The AGN wind model predicts a hard spectrum that extend in the very high energy band which differs significantly from those corresponding to other models discussed in the literature, like starburst or AGN jet. We present dedicated simulations of observations through the Cherenkov Telescope Array (CTA), the next-generation ground based gamma-ray observatory, of the very high energy spectrum of the Seyfert galaxy NGC 1068 assuming the AGN wind and the AGN jet models. We demonstrate that, considering 50 hours of observations, CTA can be effectively used to constrain the two different emission models, providing important insight into the physics governing the acceleration of particles in non-relativistic AGN-driven outflows. This analysis strongly motivates observations of Seyfert and starburst galaxies with CTA in order to test source population models of the extragalactic gamma-ray and neutrino backgrounds., 29 pages, 4 figures, accepted for publication in Astroparticle Physics
Published: 2019
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18. Multi-messenger astronomy with the γ-ray satellite AGILE: gravitational wave events and ultra-high energy astrophysical neutrinos

Author: C. Pittori, A. Rappoldi, A. Morselli, A. W. Chen, Andrea Bulgarelli, Agile Team, M. Tavani, N. Parmiggiani, F. Verrecchia, Paolo W. Cattaneo, S. Vercellone, Fabrizio Lucarelli, ITA, and ZAF
Subjects: Physics, Nuclear and High Energy Physics, High energy, 010308 nuclear & particles physics, business.industry, Gravitational wave, media_common.quotation_subject, Astronomy, 01 natural sciences, LIGO, Sky, 0103 physical sciences, Satellite, Neutrino, 010306 general physics, business, Agile software development, media_common
Abstract: We report the results of an extensive search through the AGILE data for γ-ray counterparts to the LIGO gravitational-wave (GW) events detected in the O1 run corresponding to the period from September 12 2015 to January 19, 2016 and in the O2 run corresponding to the period from November 30, 2016 to August 25, 2017. We report as well the results of a search through the AGILE data for γ-ray counterparts to the IceCube neutrino events. Currently in spinning mode, AGILE has the potential of covering about 80% of the whole sky with its γ-ray instrument, with more than 100 useful passes every day for any accessible sky region and is ready to be operative during the incoming LIGO/VIRGO O3 run.
Published: 2019
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19. AGILE and blazars: the unexpected, the unprecedented, and the uncut

Author: S. Vercellone and ITA
Subjects: 0303 health sciences, Active galactic nucleus, Scope (project management), business.industry, Computer science, Interpretation (philosophy), Astronomy, 01 natural sciences, 03 medical and health sciences, 030301 anatomy & morphology, 0103 physical sciences, General Earth and Planetary Sciences, General Agricultural and Biological Sciences, Set (psychology), business, Blazar, 010303 astronomy & astrophysics, General Environmental Science, Agile software development
Abstract: AGILE has been coordinating multi-wavelength campaigns on active galactic nuclei with several major observing facilities since its launch in 2007. This effort allowed us to investigate some remarkable sources both on short and on long time-scales, deriving information on the physical mechanisms responsible for the emission in different energy bands. A complete review of the whole set of AGILE results on extra-galactic sources and their theoretical interpretation is well beyond the scope of this paper, therefore I will present an overview on an handful of outstanding objects and describe the most recent observations.
Published: 2019
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20. The Small-Sized Telescopes for the Southern Site of the Cherenkov Telescope Array

Author: Richard White, J.P. Amans, D. Berge, G. Bonanno, R.B. Bose, A.M Brown, J.H. Buckley, P.M. Chadwick, F. Conte, G. Cotter, F. de Frondat, N. De Simone, J.L. Dournaux, C.A. Duffy, S. Einecke, G. Fasola, S. Funk, G. Giavitto, J.A. Hinton, J.M. Huet, N. La Palombara, J.S. Lapington, P. Laporte, S.A. Leach, G. Leto, S. Lloyd, S. Lombardi, A. Nayak, A. Okumura, G. Pareschi, H. Prokoph, E. Rébert, D. Ross, G. Rowell, S. Scuderi, H. Sol, S. Spencer, H. Tajima, A. Trois, S. Vercellone, J. Vink, J.J. Watson, A. Zech, and for the CTA SST Collaboration
Subjects: Physics, COSMIC cancer database, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, FOS: Physical sciences, Astronomy, Field of view, Cherenkov Telescope Array, law.invention, Telescope, Silicon photomultiplier, Observatory, law, CTA - Abteilung Hinton, Angular resolution, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: The Cherenkov Telescope Array (CTA) will use three telescope sizes to efficiently detect cosmic gamma rays in the energy range from several tens of GeV to hundreds of TeV. The Small-Sized Telescopes (SSTs) will form the largest section of the array, covering an area of many square kilometres on the CTA southern site in Paranal, Chile. Up to 70 SSTs will be implemented by an international consortium of institutes and teams as an in-kind contribution to the CTA Observatory. The SSTs will provide unprecedented sensitivity to gamma rays above 1 TeV and the highest angular resolution of any instrument above the hard X-ray band. CTA has recently finalised the technology that will be used for the SSTs: the telescopes will be a dual-reflector design with a primary reflector of ~4 m diameter, equipped with an SiPM-based camera with full waveform readout from $\sim$2000 channels covering a $\sim$9$^\circ$ field of view. The Schwarzschild-Couder optical configuration leads to a small plate-scale, and consequently a compact, cost-efficient camera. In this contribution, we describe the experience gained operating telescope and camera prototypes during the CTA preparatory phase, and the development of the final SST design., Comment: Proceedings of the 37th International Cosmic Ray Conference (ICRC2021), Berlin, Germany; PoS (ICRC2021) 728
Published: 2021
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21. An X-ray burst from a magnetar enlightening the mechanism of fast radio bursts

Author: F. Perotti, M. Cardillo, Paolo Lipari, F. Lucarelli, Giancarlo Setti, F. Fuschino, N. Parmiggiani, P. Giommi, Francesco Lazzarotto, Arnaud Ferrari, F. Paoletti, P. Picozza, Guido Barbiellini, I. Donnarumma, Y. Evangelista, V. Vittorini, M. Trifoglio, Germano Bianchi, Simonetta Puccetti, Francesco Longo, Giovanni Naldi, A. Rappoldi, Alda Rubini, P. W. Cattaneo, M. Rapisarda, P. Caraveo, A. Addis, Valentina Fioretti, C. Casentini, A. W. Chen, S. Vercellone, G. Di Persio, Paolo Soffitta, M. Galli, A. Argan, F. Verrecchia, Gianni Bernardi, Alessio Magro, Andrea Bulgarelli, Enrico Costa, A. Ursi, Giuseppe Pupillo, L. Baroncelli, E. Del Monte, Martino Marisaldi, Marco Feroci, Luigi Pacciani, Sandro Mereghetti, L. A. Antonelli, C. Pittori, Maura Pilia, Alessio Trois, Marco Tavani, Fulvio Gianotti, Ennio Morelli, F. D'Amico, G. Piano, A. Pellizzoni, A. Morselli, A. Giuliani, Claudio Labanti, G. Di Cocco, M. Perri, ITA, USA, ZAF, 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 D???amico, F.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Magnetar, 01 natural sciences, Magnetic field, Neutron star, 0103 physical sciences, Fast radio bursts, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Event (particle physics), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
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., Submitted to Nature Astronomy, May 18, 2020
Published: 2021

22. A New Sample of Gamma-Ray Emitting Jetted Active Galactic Nuclei—Preliminary Results

Author: Emilia Järvelä, Elena Dalla Bontà, Merja Tornikoski, Sonia Antón, Stefano Ciroi, Matthew L. Lister, P. Romano, M. Berton, S. Vercellone, Maria J. M. Marchã, Luigi Foschini, INAF—Osservatorio Astronomico di Brera, Purdue University, Universidade de Coimbra, Metsähovi Radio Observatory, University of Padova, University College London, European Space Agency - ESA, Aalto-yliopisto, and Aalto University
Subjects: Astrophysics::High Energy Astrophysical Phenomena, quasars, General Physics and Astronomy, Library science, QC793-793.5, Astrophysics::Cosmology and Extragalactic Astrophysics, law.invention, Telescope, law, BL Lac objects, BL lac objects, Quasars, Relativistic jets, Seyfert galaxies, Fermilab, Astrophysics::Galaxy Astrophysics, relativistic jets, Web site, Physics, United States Naval Observatory, SIMBAD, Elementary particle physics, LAMOST, National development, National laboratory
Abstract: Funding Information: Acknowledgments: LF thanks Alessandro Caccianiga for a useful and valuable exchange of ideas on the classification of misaligned AGN. Funding for the Sloan Digital Sky Survey (SDSS) was provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the U.S. Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is http://www.sdss.org/, accessed on 9 September 2021. The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are the University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, University of Pittsburgh, Princeton University, the United States Naval Observatory, and the University of Washington. Guoshoujing Telescope (the Large Sky Area Multi-Object Fiber Spectroscopic Telescope LAMOST) is a National Major Scientific Project built by the Chinese Academy of Sciences. Funding for the project has been provided by the National Development and Reform Commission. LAMOST is operated and managed by the National Astronomical Observatories, Chinese Academy of Sciences. This research made use of the SIMBAD database, operated at CDS, Strasbourg, France (2000, A&AS, 143, 9, “The SIMBAD astronomical database”, Wenger et al.). This research made use of the NASA/IPAC Extragalactic Database (NED), which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology. This research made use of NASA’s Astrophysics Data System Bibliographic Services. Funding Information: LF thanks Alessandro Caccianiga for a useful and valuable exchange of ideas on the classification of misaligned AGN. Funding for the Sloan Digital Sky Survey (SDSS) was provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the U.S. Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is http://www.sdss.org/, accessed on 9 September 2021. The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are the University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, University of Pittsburgh, Princeton University, the United States Naval Observatory, and the University of Washington. Guoshoujing Telescope (the Large Sky Area Multi-Object Fiber Spectroscopic Telescope LAMOST) is a National Major Scientific Project built by the Chinese Academy of Sciences. Funding for the project has been provided by the National Development and Reform Commission. LAMOST is operated and managed by the National Astronomical Observatories, Chinese Academy of Sciences. This research made use of the SIMBAD database, operated at CDS, Strasbourg, France (2000, A&AS, 143, 9, ?The SIMBAD astronomical database?, Wenger et al.). This research made use of the NASA/IPAC Extragalactic Database (NED), which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology. This research made use of NASA?s Astrophysics Data System Bibliographic Services. Publisher Copyright: © 2021 by the authors. Licensee MDPI, Basel, Switzerland. We are compiling a new list of gamma-ray jetted active galactic nuclei (AGN), starting from the fourth catalog of point sources of the Fermi Large Area Telescope (LAT). Our aim is to prepare a list of jetted AGN with known redshifts and classifications to be used to calibrate jet power. We searched in the available literature for all the published optical spectra and multiwavelength studies useful to characterize the sources. We found new, missed, or even forgotten information leading to a substantial change in the redshift values and classification of many sources. We present here the preliminary results of this analysis and some statistics based on the gamma-ray sources with right ascension within the interval 0h–12h (J2000). Although flat-spectrum radio quasars and BL Lac objects are still the dominant populations, there is a significant increase in the number of other objects, such as misaligned AGN, narrow-line Seyfert 1 galaxies, and Seyfert galaxies. We also introduced two new classes of objects: changing-look AGN and ambiguous sources. About one third of the sources remain unclassified.
Published: 2021

23. Hunting for the nature of the enigmatic narrow-line Seyfert 1 galaxy PKS 2004-447

Author: Emilia Järvelä, A. Kreikenbohm, Stefano Ciroi, Luigi Foschini, Nidia Morrell, Marco Berton, Giacomo Terreran, E. Sani, Sina Chen, A. Vietri, Stefanie Komossa, F. Di Mille, Paola Marziani, P. Romano, L. Crepaldi, Jari Kotilainen, I. Björklund, S. Vercellone, Luigi C. Gallo, Enrico Congiu, Merja Tornikoski, G. Peluso, Metsähovi Radio Observatory, INAF - Osservatorio Astronomico di Padova, Max Planck Institute for Radio Astronomy, Osservatorio Astronomico di Brera, University of Padova, Universidad de Chile, Saint Mary's University Halifax, Department of Electronics and Nanoengineering, Carnegie Institution of Washington, European Space Agency - ESA, University of Turku, Friedrich-Alexander University Erlangen-Nürnberg, European Southern Observatory Santiago, Northwestern University, Aalto-yliopisto, and Aalto University
Subjects: Active galactic nucleus, active [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, law.invention, Astrophysical jet, law, 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astronomy and Astrophysics, Galaxy, Black hole, Space and Planetary Science, jets [Galaxies], Astrophysics - High Energy Astrophysical Phenomena, supermassive black holes [Quasars], Flare
Abstract: Narrow-line Seyfert 1 (NLS1) galaxies are a class of active galactic nuclei (AGN) that, in some cases, can harbor powerful relativistic jets. One of them, PKS 2004-447, shows gamma-ray emission, and underwent its first recorded multifrequency flare in 2019. However, past studies revealed that in radio this source can be classified as a compact steep-spectrum source (CSS), suggesting that, unlike other gamma-ray sources, the relativistic jets of PKS 2004-447 have a large inclination with respect to the line of sight. We present here a set of spectroscopic observations of this object, aimed at carefully measuring its black hole mass and Eddington ratio, determining the properties of its emission lines, and characterizing its long term variability. We find that the black hole mass is $(1.5\pm0.2)\times10^7$ M$_\odot$, and the Eddington ratio is 0.08. Both values are within the typical range of NLS1s. The spectra also suggest that the 2019 flare was caused mainly by the relativistic jet, while the accretion disk played a minor role during the event. In conclusion, we confirm that PKS 2004-447 is one of the rare examples of gamma-ray emitting CSS/NLS1s hybrid, and that these two classes of objects are likely connected in the framework of AGN evolution., Comment: 14 pages, 8 figures, 4 tables, resubmitted to A&A after minor comments from the referee
Published: 2021
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24. AGILE Observations of Fast Radio Bursts

Author: S. Vercellone, L. Baroncelli, Guido Barbiellini, F. Verrecchia, A. Di Piano, C. Pittori, G. Piano, M. Cardillo, A. Ursi, N. Parmiggiani, Marco Tavani, A. W. Chen, A. Addis, Sandro Mereghetti, P. W. Cattaneo, Valentina Fioretti, Fabrizio Lucarelli, A. Rappoldi, Arnaud Ferrari, E. Del Monte, Maura Pilia, Andrea Bulgarelli, Enrico Costa, Francesco Longo, C. Casentini, Verrecchia, F., Casentini, C., Tavani, M., Ursi, A., Mereghetti, S., Pilia, M., Cardillo, M., Addis, A., Barbiellini, G., Baroncelli, L., Bulgarelli, A., Cattaneo, P. W., Chen, A., Costa, E., Del Monte, E., Di Piano, A., Ferrari, A., Fioretti, V., Longo, F., Lucarelli, F., Parmiggiani, N., Piano, G., Pittori, C., Rappoldi, A., Vercellone, S., ITA, and ZAF
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Detector, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Magnetar, Coincidence, law.invention, Space and Planetary Science, Sky, law, Satellite, Fast radio bursts, Astrophysics - High Energy Astrophysical Phenomena, Systematic search, media_common, Flare
Abstract: We report on a systematic search for hard X-ray and gamma-ray emission in coincidence with fast radio bursts (FRBs) observed by the AGILE satellite. We used 13 years of AGILE archival data searching for time coincidences between exposed FRBs and events detectable by the MCAL (0.4-100 MeV) and GRID (50 MeV-30 GeV) detectors at timescales ranging from milliseconds to days/weeks. The current AGILE sky coverage allowed us to extend the search for high-energy emission preceding and following the FRB occurrence. We considered all FRBs sources currently included in catalogues, and identified a sub-sample (15 events) for which a good AGILE exposure either with MCAL or GRID was obtained. In this paper we focus on non-repeating FRBs, compared to a few nearby repeating sources. We did not detect significant MeV or GeV emission from any event. Our hard X-ray upper limits (ULs) in the MeV energy range were obtained for timescales from sub-millisecond to seconds, and in the GeV range from minutes to weeks around event times. We focus on a sub-set of 5 non-repeating and 2 repeating FRB sources whose distances are most likely smaller than that of 180916.J0158+65 (150 Mpc). For these sources, our MeV ULs translate into ULs on the isotropically-emitted energy of about 3x10^46 erg, comparable to that observed in the 2004 giant flare from the Galactic magnetar SGR 1806-20. On average, these nearby FRBs emit radio pulses of energies significantly larger than the recently detected SGR 1935+2154 and are not yet associated with intense MeV flaring., Comment: ApJ, 915, 102
Published: 2021

25. Sensitivity of the Cherenkov Telescope Array for probing cosmology and fundamental physics with gamma-ray propagation

Author: J.-P. Lenain, A. Domínguez, Jonathan Ivor Davies, T. Armstrong, A. A. Zdziarski, F. Gianotti, M. Balbo, E. O. Angüner, M. Marculewicz, Alasdair E. Gent, Alice Donini, Olivier Hervet, Henry Przybilski, Giacomo Principe, G. Leto, M. Peresano, Stefano Covino, P. A. Caraveo, Gianpiero Tagliaferri, D. de Martino, V. V. Vassiliev, D. Cauz, F. R. Pantaleo, U. Barres de Almeida, Pietro Bruno, E. Lindfors, M. Zavrtanik, G. Hughes, Miriam Lucio Martinez, P. Bordas, Y. Suda, G. S. Varner, R. Rando, K. Cerny, S. Pita, Csaba Balázs, E. Fiandrini, Michael Backes, Tomohiko Oka, Massimo Persic, Andrea Chiavassa, Johannes Veh, A. Stamerra, Fabrizio Tavecchio, B. Biasuzzi, Michael Punch, Soebur Razzaque, F. D'Ammando, P. I. Batista, Bruna Bertucci, F. Longo, Francesco Gabriele Saturni, Michael G. Burton, Bohdan Hnatyk, P. Sangiorgi, E. M. Santos, D. Nosek, Gagik Tovmassian, J. L. Dournaux, Pedro L. Luque-Escamilla, A. Aguirre-Santaella, M. Orienti, Lluis Font, Andreas Quirrenbach, Philippe Laporte, Ralf Kissmann, Francesco Lucarelli, K. Noda, I. Jiménez Martínez, G. Romeo, Wystan Benbow, P. Romano, B. Bi, J. Grube, H.-S. Zechlin, Giacomo Bonnoli, Martin White, J. P. Osborne, Enrico Cascone, Marek Jamrozy, C. Alispach, Miroslav Pech, O. Cuevas, Petr Schovanek, K. Hayashi, V. I. Zhdanov, Javier Coronado-Blázquez, D. Medina Miranda, Barbara Balmaverde, E. de Ona Wilhelmi, Frank M. Rieger, A. Shalchi, J. M. Paredes, Ruben Alfaro, N. Giglietto, Diego Falceta-Gonçalves, Helene Sol, Rodolfo Carosi, Ayan Acharyya, Dominik Elsässer, S. Vercellone, D. Pimentel, T. Mizuno, Alessandro Bruno, Juan Abel Barrio, K. Kosack, Mauro Orlandini, Rodrigo Guedes Lang, P. Marquez, Adrian Biland, Y. Kobayashi, Nicholas F. H Tothill, M. de Naurois, Daniele Spiga, Lili Yang, L. Tibaldo, Pavel Horvath, M. Lopez, I. Sadeh, Marek Nikolajuk, F. Schüssler, Reshmi Mukherjee, Gianpaolo Vettolani, Jürgen Knödlseder, Daniel Nieto, R. Hnatyk, German Martinez, Diego F. Torres, Farinaldo S. Queiroz, N. Parmiggiani, G. Lamanna, Marcos Santander, S. Fegan, I. Vovk, M. Sánchez-Conde, Wiphu Rujopakarn, Norita Kawanaka, R. C. Shellard, Michael C. B. Ashley, J. Jurysek, Francisco J. Franco, Samuel Timothy Spencer, E. Rebert, J. Morales Merino, M. Pecimotika, Marco Berton, Regis Terrier, G. A. Beck, Carlos Díaz, J. L. Contreras, G. Zaharijas, R. Moderski, José-María Martí, A. Insolia, D. Zavrtanik, K. Kohri, Ladislav Chytka, T. Grabarczyk, A. Zech, M. Garczarczyk, Anastasia Sokolenko, J. Lefaucheur, R. A. Cameron, Moritz Hütten, S. Karkar, K. Pfrang, V. Poireau, Asaf Pe'er, A. Reimer, Fabio Acero, L. Freixas Coromina, David Sánchez, Jonathan S. Lapington, Konstantinos N. Gourgouliatos, J.R. Hörandel, Mario Buscemi, Francesco Dazzi, Abelardo Moralejo, J. Bolmont, R. White, A. Rosales de Leon, J. Prast, Sabrina Einecke, Roberto Aloisio, Yvonne Becherini, Andreas Specovius, Shohei Yanagita, Juan Cortina, Miroslav Hrabovsky, Petr Janecek, D. Depaoli, Lucas Taylor, U. Schwanke, H. Abdalla, S. Recchia, Manuela Mallamaci, M. K. Daniel, Q. Feng, L. Baroncelli, Hiromitsu Takahashi, Susumu Inoue, U. Straumann, Masatoshi Ohishi, Roberto Capuzzo-Dolcetta, Nu. Komin, Federico Russo, R. de Cássia dos Anjos, Y. Ohira, Ferdinando Giordano, Nagisa Hiroshima, E. Garcia, Gavin Rowell, V. Bozhilov, Maxim V. Barkov, Dario Hrupec, I. Oya, F. Salesa Greus, Anna Wolter, M. Živec, R. Belmont, R. Adam, T. Reposeur, J. Rico, A. W. Chen, G. Pühlhofer, H. Prokoph, Stefan Wagner, F. Di Pierro, Fabrizio Bocchino, M. de Bony de Lavergne, A. Kong, Masha Chernyakova, M. Pohl, M. Vazquez Acosta, A. Nagai, A. Brill, Dusan Mandat, Jonathan Biteau, Martin Makariev, Catherine Boisson, E. Lyard, Gilles Maurin, H. Martínez-Huerta, Oscar Blanch, Bernd Schleicher, M. Minev, A. Berti, James E. M. Watson, Talvikki Hovatta, M. Valentino, Luis Ángel Tejedor, Elena Amato, M. V. Fonseca, Anderson Caproni, L. Mohrmann, P. Reichherzer, R. L. C. Starling, M. Seglar Arroyo, E. Orlando, B. Rudak, G. Emery, J. A. Green, Salvo Scuderi, M. Prouza, Tom Richtler, Bartłomiej Pilszyk, A. Carosi, Jacek Niemiec, Wolfgang Rhode, G. Ambrosi, D. Ribeiro, A. Wierzcholska, A. Ghalumyan, Eugenio Bottacini, Sylvain Chaty, A. Baquero Larriva, Olaf Reimer, D. Horan, Fabian Leuschner, T. Di Girolamo, Alessandro Caccianiga, Martin Will, Saverio Lombardi, A. Fiasson, Mitsunari Takahashi, J. J. Rodríguez Vázquez, B. De Lotto, V. De Caprio, Stefano Truzzi, Dirk L. Hoffmann, M. Vecchi, Antonio Pagliaro, Jose J. Gonzalez, Wenwu Tian, R. Della Ceca, J. Becerra González, S. Nozaki, T. Vuillaume, S. L. Lloyd, Maria Ionica, Elisabetta Bissaldi, Petr Travnicek, Y. Ascasibar, Carlo Vigorito, F. Tuossenel, Malcolm Fairbairn, O. Martinez, Marco Iarlori, Serena Loporchio, Alessandro Costa, R. Pillera, A. Morselli, M. Heller, Jaime Rosado, E. M. de Gouveia Dal Pino, V. Vitale, A. M. Brown, E. Molina, Takashi Saito, A. De Angelis, Thomas Murach, R. A. Ong, J. Bregeon, P. T. O'Brien, Mikael Jacquemont, P. Cristofari, Francesco Conte, Lab Saha, R. Walter, Vitalii Sliusar, W. Jin, Vito Conforti, N. Produit, H. Siejkowski, Lovro Pavletić, Carole Mundell, G. Rodriguez Fernandez, J. F. Glicenstein, Paresh Sharma, C. Delgado, Vladimír Karas, Luca Foffano, J. Granot, Manuel Meyer, Reiko Orito, G. Umana, G. Chiaro, D. Tonev, R. Wiemann, G. Manicò, J.C. Rodriguez Ramirez, Luca Tosti, Markus Böttcher, Andrea Bulgarelli, C. Díaz-Bahamondes, I. Jung-Richardt, Karol Seweryn, P. Piatteli, Agnieszka Slowikowska, Jan Ebr, M. Ostrowski, J. L. Rodriguez, D. della Volpe, Ermanno Pietropaolo, M. Caprai, T. Montaruli, A. Lopez, Rodrigo Nemmen, R. R. Prado, L. Arrabito, Atreyee Sinha, C. van Eldik, Serguei Vorobiov, Hidetoshi Sano, J. Alfaro, Sabrina Casanova, G. Maneva, B. Vallage, Valentina Fioretti, Carmelo Evoli, P. Kaaret, B. A. W. Mode, Agnieszka Majczyna, Sebastian Diebold, A. Scherer, F. de Palma, S. Hernández Cadena, V. Beshley, T.R.N. Ekoume, David A. Williams, M. Capasso, A. Halim, Alison Mitchell, Tomislav Terzić, Paola Grandi, Lorenzo Amati, Christopher Eckner, David Gascon, K. Nishijima, J. Becker Tjus, B. Khélifi, G. Galanti, Jamie Holder, Vincenzo Rizi, Orel Gueta, Daniele Gaggero, F. Pintore, Utane Sawangwit, Vassil Verguilov, Heide Costantini, F. Arqueros, Daniel Kerszberg, P. M. Chadwick, D. Zarić, Marc Ribó, Olga Sergijenko, Dario Grasso, Hidetoshi Kubo, Daniela Dorner, T. Stolarczyk, M. Gaug, R. Alves Batista, Elisa Bernardini, Vikram V. Dwarkadas, Jim Hinton, Jelena Strišković, Andreu Sanuy, M. Servillat, V. Barbosa Martins, Giovanni Bonanno, S. Gunji, R. Wischnewski, S. Sarkar, Gianluca Giavitto, Takeshi Nakamori, M. Palatka, Maria Letizia Pumo, Camilla Maggio, M. Zacharias, Katsuaki Asano, Valerio Vagelli, Anton Dmytriiev, Ryo Yamazaki, M. Vacula, P. Goldoni, Gilles Fontaine, Hiroshi Muraishi, D. Mazin, Samo Stanič, G. Ghirlanda, M. Polo, M. Nievas, M. Lemoine-Goumard, Oleh Petruk, Jose Miguel Miranda, M. Iori, A. Marcowith, Y. Renier, Satoshi Fukami, M. Roncadelli, F. Leone, Takanori Yoshikoshi, Ana Luiza d'Ávila Viana, Y. Fukui, Max Harvey, Sera Markoff, I. Agudo, P. Temnikov, Vincenzo Testa, R. López-Coto, J.D. Mbarubucyeye, Tjark Miener, David Paneque, V. Gammaldi, T. Hassan Collado, H. Abe, L. Bonneau Arbeletche, S. D. Vergani, Sasa Micanovic, P. Vallania, Marina Manganaro, Elena Torresi, M. Giarrusso, G. Ferrand, Paweł Świerk, B. Patricelli, Matteo Cerruti, N. La Palombara, D. Morcuende-Parrilla, V. de Souza, Toshiaki Inada, Yasushi Fukazawa, Werner Hofmann, Michele Doro, E. Pueschel, A. Araudo, E. Sciacca, Thomas Lohse, A. Djannati-Ataï, Abdalla, H., Abe, H., Acero, F., Acharyya, A., Adam, R., Agudo, I., Aguirre-Santaella, A., Alfaro, R., Alfaro, J., Alispach, C., Aloisio, R., Alves Batista, R., Amati, L., Amato, E., Ambrosi, G., Ang??ner, E. O., Araudo, A., Armstrong, T., Arqueros, F., Arrabito, L., Asano, K., Ascas??bar, Y., Ashley, M., Backes, M., Balazs, C., Balbo, M., Balmaverde, B., Baquero Larriva, A., Barbosa Martins, V., Barkov, M., Baroncelli, L., Barres de Almeida, U., Barrio, J. A., Batista, P. -I., Becerra Gonz??lez, J., Becherini, Y., Beck, G., Becker Tjus, J., Belmont, R., Benbow, W., Bernardini, E., Berti, A., Berton, M., Bertucci, B., Beshley, V., Bi, B., Biasuzzi, B., Biland, A., Bissaldi, E., Biteau, J., Blanch, O., Bocchino, F., Boisson, C., Bolmont, J., Bonanno, G., Bonneau Arbeletche, L., Bonnoli, G., Bordas, P., Bottacini, E., B??ttcher, M., Bozhilov, V., Bregeon, J., Brill, A., Brown, A. M., Bruno, P., Bruno, A., Bulgarelli, A., Burton, M., Buscemi, M., Caccianiga, A., Cameron, R., Capasso, M., Caprai, M., Caproni, A., Capuzzo-Dolcetta, R., Caraveo, P., Carosi, R., Carosi, A., Casanova, S., Cascone, E., Cauz, D., Cerny, K., Cerruti, M., Chadwick, P., Chaty, S., Chen, A., Chernyakova, M., Chiaro, G., Chiavassa, A., Chytka, L., Conforti, V., Conte, F., Contreras, J. L., Coronado-Blazquez, J., Cortina, J., Costa, A., Costantini, H., Covino, S., Cristofari, P., Cuevas, O., D'Ammando, F., Daniel, M. K., Davies, J., Dazzi, F., De Angelis, A., de Bony de Lavergne, M., De Caprio, V., de C??ssia dos Anjos, R., de Gouveia Dal Pino, E. M., De Lotto, B., De Martino, D., de Naurois, M., de O??a Wilhelmi, E., De Palma, F., de Souza, V., Delgado, C., Della Ceca, R., della Volpe, D., Depaoli, D., Di Girolamo, T., Di Pierro, F., D??az, C., D??az-Bahamondes, C., Diebold, S., Djannati-Ata??, A., Dmytriiev, A., Dom??nguez, A., Donini, A., Dorner, D., Doro, M., Dournaux, J., Dwarkadas, V. V., Ebr, J., Eckner, C., Einecke, S., Ekoume, T. R. N., Els??sser, D., Emery, G., Evoli, C., Fairbairn, M., Falceta-Goncalves, D., Fegan, S., Feng, Q., Ferrand, G., Fiandrini, E., Fiasson, A., Fioretti, V., Foffano, L., Fonseca, M. V., Font, L., Fontaine, G., Franco, F. J., Freixas Coromina, L., Fukami, S., Fukazawa, Y., Fukui, Y., Gaggero, D., Galanti, G., Gammaldi, V., Garcia, E., Garczarczyk, M., Gascon, D., Gaug, M., Gent, A., Ghalumyan, A., Ghirlanda, G., Gianotti, F., Giarrusso, M., Giavitto, G., Giglietto, N., Giordano, F., Glicenstein, J., Goldoni, P., Gonz??lez, J. M., Gourgouliatos, K., Grabarczyk, T., Grandi, P., Granot, J., Grasso, D., Green, J., Grube, J., Gueta, O., Gunji, S., Halim, A., Harvey, M., Hassan Collado, T., Hayashi, K., Heller, M., Hern??ndez Cadena, S., Hervet, O., Hinton, J., Hiroshima, N., Hnatyk, B., Hnatyk, R., Hoffmann, D., Hofmann, W., Holder, J., Horan, D., H??randel, J., Horvath, P., Hovatta, T., Hrabovsky, M., Hrupec, D., Hughes, G., H??tten, M., Iarlori, M., Inada, T., Inoue, S., Insolia, A., Ionica, M., Iori, M., Jacquemont, M., Jamrozy, M., Janecek, P., Jim??nez Mart??nez, I., Jin, W., Jung-Richardt, I., Jurysek, J., Kaaret, P., Karas, V., Karkar, S., Kawanaka, N., Kerszberg, D., Kh??lifi, B., Kissmann, R., Kn??dlseder, J., Kobayashi, Y., Kohri, K., Komin, N., Kong, A., Kosack, K., Kubo, H., La Palombara, N., Lamanna, G., Lang, R. G., Lapington, J., Laporte, P., Lefaucheur, J., Lemoine-Goumard, M., Lenain, J., Leone, F., Leto, G., Leuschner, F., Lindfors, E., Lloyd, S., Lohse, T., Lombardi, S., Longo, F., Lopez, A., L??pez, M., L??pez-Coto, R., Loporchio, S., Lucarelli, F., Luque-Escamilla, P. L., Lyard, E., Maggio, C., Majczyna, A., Makariev, M., Mallamaci, M., Mandat, D., Maneva, G., Manganaro, M., Manic??, G., Marcowith, A., Marculewicz, M., Markoff, S., Marquez, P., Mart??, J., Martinez, O., Mart??nez, M., Mart??nez, G., Mart??nez-Huerta, H., Maurin, G., Mazin, D., Mbarubucyeye, J. D., Medina Miranda, D., Meyer, M., Micanovic, S., Miener, T., Minev, M., Miranda, J. M., Mitchell, A., Mizuno, T., Mode, B., Moderski, R., Mohrmann, L., Molina, E., Montaruli, T., Moralejo, A., Morales Merino, J., Morcuende-Parrilla, D., Morselli, A., Mukherjee, R., Mundell, C., Murach, T., Muraishi, H., Nagai, A., Nakamori, T., Nemmen, R., Niemiec, J., Nieto, D., Nievas, M., Nikolajuk, M., Nishijima, K., Noda, K., Nosek, D., Nozaki, S., O'Brien, P., Ohira, Y., Ohishi, M., Oka, T., Ong, R. A., Orienti, M., Orito, R., Orlandini, M., Orlando, E., Osborne, J. P., Ostrowski, M., Oya, I., Pagliaro, A., Palatka, M., Paneque, D., Pantaleo, F. R., Paredes, J. M., Parmiggiani, N., Patricelli, B., Pavleti??, L., Pe'Er, A., Pech, M., Pecimotika, M., Peresano, M., Persic, M., Petruk, O., Pfrang, K., Piatteli, P., Pietropaolo, E., Pillera, R., Pilszyk, B., Pimentel, D., Pintore, F., Pita, S., Pohl, M., Poireau, V., Polo, M., Prado, R. R., Prast, J., Principe, G., Produit, N., Prokoph, H., Prouza, M., Przybilski, H., Pueschel, E., P??hlhofer, G., Pumo, M. L., Punch, M., Queiroz, F., Quirrenbach, A., Rando, R., Razzaque, S., Rebert, E., Recchia, S., Reichherzer, P., Reimer, O., Reimer, A., Renier, Y., Reposeur, T., Rhode, W., Ribeiro, D., Rib??, M., Richtler, T., Rico, J., Rieger, F., Rizi, V., Rodriguez, J., Rodriguez Fernandez, G., Rodriguez Ramirez, J. C., Rodr??guez V??zquez, J. J., Romano, P., Romeo, G., Roncadelli, M., Rosado, J., Rosales de Leon, A., Rowell, G., Rudak, B., Rujopakarn, W., Russo, F., Sadeh, I., Saha, L., Saito, T., Salesa Greus, F., Sanchez, D., S??nchez-Conde, M., Sangiorgi, P., Sano, H., Santander, M., Santos, E. M., Sanuy, A., Sarkar, S., Saturni, F. G., Sawangwit, U., Scherer, A., Schleicher, B., Schovanek, P., Schussler, F., Schwanke, U., Sciacca, E., Scuderi, S., Seglar Arroyo, M., Sergijenko, O., Servillat, M., Seweryn, K., Shalchi, A., Sharma, P., Shellard, R. C., Siejkowski, H., Sinha, A., Sliusar, V., Slowikowska, A., Sokolenko, A., Sol, H., Specovius, A., Spencer, S., Spiga, D., Stamerra, A., Stani??, S., Starling, R., Stolarczyk, T., Straumann, U., Stri??kovi??, J., Suda, Y., wierk, P., Tagliaferri, G., Takahashi, H., Takahashi, M., Tavecchio, F., Taylor, L., Tejedor, L. A., Temnikov, P., Terrier, R., Terzic, T., Testa, V., Tian, W., Tibaldo, L., Tonev, D., Torres, D. F., Torresi, E., Tosti, L., Tothill, N., Tovmassian, G., Travnicek, P., Truzzi, S., Tuossenel, F., Umana, G., Vacula, M., Vagelli, V., Valentino, M., Vallage, B., Vallania, P., van Eldik, C., Varner, G. S., Vassiliev, V., V??zquez Acosta, M., Vecchi, M., Veh, J., Vercellone, S., Vergani, S., Verguilov, V., Vettolani, G. P., Viana, A., Vigorito, C. F., Vitale, V., Vorobiov, S., Vovk, I., Vuillaume, T., Wagner, S. J., Walter, R., Watson, J., White, M., White, R., Wiemann, R., Wierzcholska, A., Will, M., Williams, D. A., Wischnewski, R., Wolter, A., Yamazaki, R., Yanagita, S., Yang, L., Yoshikoshi, T., Zacharias, M., Zaharijas, G., Zaric, D., Zavrtanik, M., Zavrtanik, D., Zdziarski, A. A., Zech, A., Zechlin, H., Zhdanov, V. I., ivec, M., Comisión Nacional de Investigación Científica y Tecnológica (Chile), Ministry of Education, Youth and Sports (Czech Republic), Academy of Finland, Istituto Nazionale di Astrofisica, National Science Centre (Poland), Slovenian Research Agency, European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia e Innovación (España), Junta de Andalucía, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), CTA, UAM. Departamento de Física Teórica, Batista, R. A., Anguner, E. O., Ascasibar, Y., Larriva, A. B., Martins, V. B., De Almeida, U. B., Gonzalez, J. B., Tjus, J. B., Arbeletche, L. B., Bottcher, M., Angelis, A. D., De Lavergne, M. D. B., Caprio, V. D., De Dos Anjos, R. C., De Gouveia Dal Pino, E. M., Lotto, B. D., Martino, D. D., De Naurois, M., Wilhelmi, E. D. O., DE PALMA, F., De Souza, V., Ceca, R. D., Volpe, D. D., Girolamo, T. D., Pierro, F. D., Diaz, C., Diaz-Bahamondes, C., Djannati-Atai, A., Dominguez, A., Elsasser, D., Coromina, L. F., Gonzalez, J. M., Collado, T. H., Cadena, S. H., Horandel, J., Hutten, M., Martinez, I. J., Khelifi, B., Knodlseder, J., Palombara, N. L., Lopez, M., Lopez-Coto, R., Manico, G., Marti, J., Martinez, M., Martinez, G., Martinez-Huerta, H., Miranda, D. M., Merino, J. M., Pavletic, L., Puhlhofer, G., Ribo, M., Fernandez, G. R., Ramirez, J. C. R., Vazquez, J. J. R., De Leon, A. R., Greus, F. S., Sanchez-Conde, M., Arroyo, M. S., Stanic, S., Striskovic, J., Swierk, P., Eldik, C. V., Acosta, M. V., Zivec, M., Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Abdalla H., Abe H., Acero F., Acharyya A., Adam R., Agudo I., Aguirre-Santaella A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Batista R.A., Amati L., Amato E., Ambrosi G., Anguner E.O., Araudo A., Armstrong T., Arqueros F., Arrabito L., Asano K., Ascasibar Y., Ashley M., Backes M., Balazs C., Balbo M., Balmaverde B., Larriva A.B., Martins V.B., Barkov M., Baroncelli L., De Almeida U.B., Barrio J.A., Batista P.-I., Gonzalez J.B., Becherini Y., Beck G., Tjus J.B., Belmont R., Benbow W., Bernardini E., Berti A., Berton M., Bertucci B., Beshley V., Bi B., Biasuzzi B., Biland A., Bissaldi E., Biteau J., Blanch O., Bocchino F., Boisson C., Bolmont J., Bonanno G., Arbeletche L.B., Bonnoli G., Bordas P., Bottacini E., Bottcher M., Bozhilov V., Bregeon J., Brill A., Brown A.M., Bruno P., Bruno A., Bulgarelli A., Burton M., Buscemi M., Caccianiga A., Cameron R., Capasso M., Caprai M., Caproni A., Capuzzo-Dolcetta R., Caraveo P., Carosi R., Carosi A., Casanova S., Cascone E., Cauz D., Cerny K., Cerruti M., Chadwick P., Chaty S., Chen A., Chernyakova M., Chiaro G., Chiavassa A., Chytka L., Conforti V., Conte F., Contreras J.L., Coronado-Blazquez J., Cortina J., Costa A., Costantini H., Covino S., Cristofari P., Cuevas O., D'Ammando F., Daniel M.K., Davies J., Dazzi F., Angelis A.D., De Lavergne M.D.B., Caprio V.D., De Dos Anjos R.C., De Gouveia Dal Pino E.M., Lotto B.D., Martino D.D., De Naurois M., Wilhelmi E.D.O., Palma F.D., De Souza V., Delgado C., Ceca R.D., Volpe D.D., Depaoli D., Girolamo T.D., Pierro F.D., Diaz C., Diaz-Bahamondes C., Diebold S., Djannati-Atai A., Dmytriiev A., Dominguez A., Donini A., Dorner D., Doro M., Dournaux J., Dwarkadas V.V., Ebr J., Eckner C., Einecke S., Ekoume T.R.N., Elsasser D., Emery G., Evoli C., Fairbairn M., Falceta-Goncalves D., Fegan S., Feng Q., Ferrand G., Fiandrini E., Fiasson A., Fioretti V., Foffano L., Fonseca M.V., Font L., Fontaine G., Franco F.J., Coromina L.F., Fukami S., Fukazawa Y., Fukui Y., Gaggero D., Galanti G., Gammaldi V., Garcia E., Garczarczyk M., Gascon D., Gaug M., Gent A., Ghalumyan A., Ghirlanda G., Gianotti F., Giarrusso M., Giavitto G., Giglietto N., Giordano F., Glicenstein J., Goldoni P., Gonzalez J.M., Gourgouliatos K., Grabarczyk T., Grandi P., Granot J., Grasso D., Green J., Grube J., Gueta O., Gunji S., Halim A., Harvey M., Collado T.H., Hayashi K., Heller M., Cadena S.H., Hervet O., Hinton J., Hiroshima N., Hnatyk B., Hnatyk R., Hoffmann D., Hofmann W., Holder J., Horan D., Horandel J., Horvath P., Hovatta T., Hrabovsky M., Hrupec D., Hughes G., Hutten M., Iarlori M., Inada T., Inoue S., Insolia A., Ionica M., Iori M., Jacquemont M., Jamrozy M., Janecek P., Martinez I.J., Jin W., Jung-Richardt I., Jurysek J., Kaaret P., Karas V., Karkar S., Kawanaka N., Kerszberg D., Khelifi B., Kissmann R., Knodlseder J., Kobayashi Y., Kohri K., Komin N., Kong A., Kosack K., Kubo H., Palombara N.L., Lamanna G., Lang R.G., Lapington J., Laporte P., Lefaucheur J., Lemoine-Goumard M., Lenain J., Leone F., Leto G., Leuschner F., Lindfors E., Lloyd S., Lohse T., Lombardi S., Longo F., Lopez A., Lopez M., Lopez-Coto R., Loporchio S., Lucarelli F., Luque-Escamilla P.L., Lyard E., Maggio C., Majczyna A., Makariev M., Mallamaci M., Mandat D., Maneva G., Manganaro M., Manico G., Marcowith A., Marculewicz M., Markoff S., Marquez P., Marti J., Martinez O., Martinez M., Martinez G., Martinez-Huerta H., Maurin G., Mazin D., Mbarubucyeye J.D., Miranda D.M., Meyer M., Micanovic S., Miener T., Minev M., Miranda J.M., Mitchell A., Mizuno T., Mode B., Moderski R., Mohrmann L., Molina E., Montaruli T., Moralejo A., Merino J.M., Morcuende-Parrilla D., Morselli A., Mukherjee R., Mundell C., Murach T., Muraishi H., Nagai A., Nakamori T., Nemmen R., Niemiec J., Nieto D., Nievas M., Nikolajuk M., Nishijima K., Noda K., Nosek D., Nozaki S., O'Brien P., Ohira Y., Ohishi M., Oka T., Ong R.A., Orienti M., Orito R., Orlandini M., Orlando E., Osborne J.P., Ostrowski M., Oya I., Pagliaro A., Palatka M., Paneque D., Pantaleo F.R., Paredes J.M., Parmiggiani N., Patricelli B., Pavletic L., Pe'Er A., Pech M., Pecimotika M., Peresano M., Persic M., Petruk O., Pfrang K., Piatteli P., Pietropaolo E., Pillera R., Pilszyk B., Pimentel D., Pintore F., Pita S., Pohl M., Poireau V., Polo M., Prado R.R., Prast J., Principe G., Produit N., Prokoph H., Prouza M., Przybilski H., Pueschel E., Puhlhofer G., Pumo M.L., Punch M., Queiroz F., Quirrenbach A., Rando R., Razzaque S., Rebert E., Recchia S., Reichherzer P., Reimer O., Reimer A., Renier Y., Reposeur T., Rhode W., Ribeiro D., Ribo M., Richtler T., Rico J., Rieger F., Rizi V., Rodriguez J., Fernandez G.R., Ramirez J.C.R., Vazquez J.J.R., Romano P., Romeo G., Roncadelli M., Rosado J., De Leon A.R., Rowell G., Rudak B., Rujopakarn W., Russo F., Sadeh I., Saha L., Saito T., Greus F.S., Sanchez D., Sanchez-Conde M., Sangiorgi P., Sano H., Santander M., Santos E.M., Sanuy A., Sarkar S., Saturni F.G., Sawangwit U., Scherer A., Schleicher B., Schovanek P., Schussler F., Schwanke U., Sciacca E., Scuderi S., Arroyo M.S., Sergijenko O., Servillat M., Seweryn K., Shalchi A., Sharma P., Shellard R.C., Siejkowski H., Sinha A., Sliusar V., Slowikowska A., Sokolenko A., Sol H., Specovius A., Spencer S., Spiga D., Stamerra A., Stanic S., Starling R., Stolarczyk T., Straumann U., Striskovic J., Suda Y., Swierk P., Tagliaferri G., Takahashi H., Takahashi M., Tavecchio F., Taylor L., Tejedor L.A., Temnikov P., Terrier R., Terzic T., Testa V., Tian W., Tibaldo L., Tonev D., Torres D.F., Torresi E., Tosti L., Tothill N., Tovmassian G., Travnicek P., Truzzi S., Tuossenel F., Umana G., Vacula M., Vagelli V., Valentino M., Vallage B., Vallania P., Eldik C.V., Varner G.S., Vassiliev V., Acosta M.V., Vecchi M., Veh J., Vercellone S., Vergani S., Verguilov V., Vettolani G.P., Viana A., Vigorito C.F., Vitale V., Vorobiov S., Vovk I., Vuillaume T., Wagner S.J., Walter R., Watson J., White M., White R., Wiemann R., Wierzcholska A., Will M., Williams D.A., Wischnewski R., Wolter A., Yamazaki R., Yanagita S., Yang L., Yoshikoshi T., Zacharias M., Zaharijas G., Zaric D., Zavrtanik M., Zavrtanik D., Zdziarski A.A., Zech A., Zechlin H., Zhdanov V.I., Zivec M., ITA, USA, GBR, FRA, DEU, ESP, AUS, BRA, BGR, CHL, HRV, FIN, JPN, IRL, MEX, NAM, NLD, POL, CZE, SVN, SWE, CHE, UKR, Astronomy, High Energy Astrophys. & Astropart. Phys (API, FNWI), and Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Gamma ray Astronomy, Cherenkov Telescope Array, axions, MATÉRIA ESCURA, redshift: dependence, Astronomy, Gamma ray experiments, gamma ray experiments, Astrophysics, 01 natural sciences, Cosmology, Observatory, cosmological model: parameter space, gamma ray experiment, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Physics, Cherenkov telescopes, IACT technique, Gamma rays, Cosmic rays, new physics, 4. Education, Settore FIS/01 - Fisica Sperimentale, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma-ray astronomy, violation: Lorentz, 3. Good health, observatory, Extragalactic background light, astro-ph.CO, axion-like particles, Física nuclear, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, gamma ray: propagation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, Axions, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, invariance: Lorentz, jet: relativistic, dark matter: halo, 0103 physical sciences, active galactic nuclei, extragalactic magnetic fields, AGN, Blazar, background, 010308 nuclear & particles physics, Física, Astronomy and Astrophysics, sensitivity, axion, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], absorption, statistical, Blazars, Telescopes
Abstract: Full list of authors: Abdalla, H.; Abe, H.; Acero, F.; Acharyya, A.; Adam, R.; Agudo, I; Aguirre-Santaella, A.; Alfaro, R.; Alfaro, J.; Alispach, C.; Aloisio, R.; Batista, R. Alves; Amati, L.; Amato, E.; Ambrosi, G.; Anguner, E. O.; Araudo, A.; Armstrong, T.; Arqueros, F.; Arrabito, L.; Asano, K.; Ascasibar, Y.; Ashley, M.; Backes, M.; Balazs, C.; Balbo, M.; Balmaverde, B.; Baquero Larriva, A.; Martins, V. Barbosa; Barkov, M.; Baroncelli, L.; de Almeida, U. Barres; Barrio, J. A.; Batista, P-, I; Becerra Gonzalez, J.; Becherini, Y.; Beck, G.; Tjus, J. Becker; Belmont, R.; Benbow, W.; Bernardini, E.; Berti, A.; Berton, M.; Bertucci, B.; Beshley, V; Bi, B.; Biasuzzi, B.; Biland, A.; Bissaldi, E.; Biteau, J.; Blanch, O.; Bocchino, F.; Boisson, C.; Bolmont, J.; Bonanno, G.; Arbeletche, L. Bonneau; Bonnoli, G.; Bordas, P.; Bottacini, E.; Bottcher, M.; Bozhilov, V; Bregeon, J.; Brill, A.; Brown, A. M.; Bruno, P.; Bruno, A.; Bulgarelli, A.; Burton, M.; Buscemi, M.; Caccianiga, A.; Cameron, R.; Capasso, M.; Caprai, M.; Caproni, A.; Capuzzo-Dolcetta, R.; Caraveo, P.; Carosi, R.; Carosi, A.; Casanova, S.; Cascone, E.; Cauz, D.; Cerny, K.; Cerruti, M.; Chadwick, P.; Chaty, S.; Chen, A.; Chernyakova, M.; Chiaro, G.; Chiavassa, A.; Chytka, L.; Conforti, V; Conte, F.; Contreras, J. L.; Coronado-Blazquez, J.; Cortina, J.; Costa, A.; Costantini, H.; Covino, S.; Cristofari, P.; Cuevas, O.; D'Ammando, F.; Daniel, M. K.; Davies, J.; Dazzi, F.; De Angelis, A.; de Lavergne, M. de Bony; De Caprio, V; dos Anjos, R. de Cassia; Dal Pino, E. M. de Gouveia; De Lotto, B.; De Martino, D.; de Naurois, M.; Wilhelmi, E. de Ona; De Palma, F.; de Souza, V; Delgado, C.; Della Ceca, R.; della Volpe, D.; Depaoli, D.; Di Girolamo, T.; Di Pierro, F.; Diaz, C.; Diaz-Bahamondes, C.; Diebold, S.; Djannati-Atai, A.; Dmytriiev, A.; Dominguez, A.; Donini, A.; Dorner, D.; Doro, M.; Dournaux, J.; Dwarkadas, V. V.; Ebr, J.; Eckner, C.; Einecke, S.; Ekoume, T. R. N.; Elsaesser, D.; Emery, G.; Evoli, C.; Fairbairn, M.; Falceta-Goncalves, D.; Fegan, S.; Feng, Q.; Ferrand, G.; Fiandrini, E.; Fiasson, A.; Fioretti, V; Foffano, L.; Fonseca, M., V; Font, L.; Fontaine, G.; Franco, F. J.; Freixas Coromina, L.; Fukami, S.; Fukazawa, Y.; Fukui, Y.; Gaggero, D.; Galanti, G.; Gammaldi, V; Garcia, E.; Garczarczyk, M.; Gascon, D.; Gaug, M.; Gent, A.; Ghalumyan, A.; Ghirlanda, G.; Gianotti, F.; Giarrusso, M.; Giavitto, G.; Giglietto, N.; Giordano, F.; Glicenstein, J.; Goldoni, P.; Gonzalez, J. M.; Gourgouliatos, K.; Grabarczyk, T.; Grandi, P.; Granot, J.; Grasso, D.; Green, J.; Grube, J.; Gueta, O.; Gunji, S.; Halim, A.; Harvey, M.; Collado, T. Hassan; Hayashi, K.; Heller, M.; Cadena, S. Hernandez; Hervet, O.; Hinton, J.; Hiroshima, N.; Hnatyk, B.; Hnatyk, R.; Hoffmann, D.; Hofmann, W.; Holder, J.; Horan, D.; Horandel, J.; Horvath, P.; Hovatta, T.; Hrabovsky, M.; Hrupec, D.; Hughes, G.; Hutten, M.; Iarlori, M.; Inada, T.; Inoue, S.; Insolia, A.; Ionica, M.; Iori, M.; Jacquemont, M.; Jamrozy, M.; Janecek, P.; Jimenez Martinez, I; Jin, W.; Jung-Richardt, I; Jurysek, J.; Kaaret, P.; Karas, V; Karkar, S.; Kawanaka, N.; Kerszberg, D.; Khelifi, B.; Kissmann, R.; Knodlseder, J.; Kobayashi, Y.; Kohri, K.; Komin, N.; Kong, A.; Kosack, K.; Kubo, H.; La Palombara, N.; Lamanna, G.; Lang, R. G.; Lapington, J.; Laporte, P.; Lefaucheur, J.; Lemoine-Goumard, M.; Lenain, J.; Leone, F.; Leto, G.; Leuschner, F.; Lindfors, E.; Lloyd, S.; Lohse, T.; Lombardi, S.; Longo, F.; Lopez, A.; Lopez, M.; Lopez-Coto, R.; Loporchio, S.; Lucarelli, F.; Luque-Escamilla, P. L.; Lyard, E.; Maggio, C.; Majczyna, A.; Makariev, M.; Mallamaci, M.; Mandat, D.; Maneva, G.; Manganaro, M.; Manico, G.; Marcowith, A.; Marculewicz, M.; Markoff, S.; Marquez, P.; Marti, J.; Martinez, O.; Martinez, M.; Martinez, G.; Martinez-Huerta, H.; Maurin, G.; Mazin, D.; Mbarubucyeye, J. D.; Miranda, D. Medina; Meyer, M.; Micanovic, S.; Miener, T.; Minev, M.; Miranda, J. M.; Mitchell, A.; Mizuno, T.; Mode, B.; Moderski, R.; Mohrmann, L.; Molina, E.; Montaruli, T.; Moralejo, A.; Morales Merino, J.; Morcuende-Parrilla, D.; Morselli, A.; Mukherjee, R.; Mundell, C.; Murach, T.; Muraishi, H.; Nagai, A.; Nakamori, T.; Nemmen, R.; Niemiec, J.; Nieto, D.; Nievas, M.; Nikolajuk, M.; Nishijima, K.; Noda, K.; Nosek, D.; Nozaki, S.; Ohira, Y.; Ohishi, M.; Oka, T.; Ong, R. A.; Orienti, M.; Orito, R.; Orlandini, M.; Orlando, E.; Osborne, J. P.; Ostrowski, M.; Oya, I; Pagliaro, A.; Palatka, M.; Paneque, D.; Pantaleo, F. R.; Paredes, J. M.; Parmiggiani, N.; Patricelli, B.; Pavletic, L.; Pe'er, A.; Pech, M.; Pecimotika, M.; Peresano, M.; Persic, M.; Petruk, O.; Pfrang, K.; Piatteli, P.; Pietropaolo, E.; Pillera, R.; Pilszyk, B.; Pimentel, D.; Pintore, F.; Pita, S.; Pohl, M.; Poireau, V; Polo, M.; Prado, R. R.; Prast, J.; Principe, G.; Produit, N.; Prokoph, H.; Prouza, M.; Przybilski, H.; Pueschel, E.; Puehlhofer, G.; Pumo, M. L.; Punch, M.; Queiroz, F.; Quirrenbach, A.; Rando, R.; Razzaque, S.; Rebert, E.; Recchia, S.; Reichherzer, P.; Reimer, O.; Reimer, A.; Renier, Y.; Reposeur, T.; Rhode, W.; Ribeiro, D.; Ribo, M.; Richtler, T.; Rico, J.; Rieger, F.; Rizi, V; Rodriguez, J.; Fernandez, G. Rodriguez; Ramirez, J. C. Rodriguez; Rodriguez Vazquez, J. J.; Romano, P.; Romeo, G.; Roncadelli, M.; Rosado, J.; de Leon, A. Rosales; Rowell, G.; Rudak, B.; Rujopakarn, W.; Russo, F.; Sadeh, I; Saha, L.; Saito, T.; Greus, F. Salesa; Sanchez, D.; Sanchez-Conde, M.; Sangiorgi, P.; Sano, H.; Santander, M.; Santos, E. M.; Sanuy, A.; Sarkar, S.; Saturni, F. G.; Sawangwit, U.; Scherer, A.; Schleicher, B.; Schovanek, P.; Schussler, F.; Schwanke, U.; Sciacca, E.; Scuderi, S.; Arroyo, M. Seglar; Sergijenko, O.; Servillat, M.; Seweryn, K.; Shalchi, A.; Sharma, P.; Shellard, R. C.; Siejkowski, H.; Sinha, A.; Sliusar, V; Slowikowska, A.; Sokolenko, A.; Sol, H.; Specovius, A.; Spencer, S.; Spiga, D.; Stamerra, A.; Starling, R.; Stolarczyk, T.; Straumann, U.; Striskovic, J.; Suda, Y.; Tagliaferri, G.; Takahashi, H.; Takahashi, M.; Tavecchio, F.; Taylor, L.; Tejedor, L. A.; Temnikov, P.; Terrier, R.; Terzic, T.; Testa, V; Tian, W.; Tibaldo, L.; Tonev, D.; Torres, D. F.; Torresi, E.; Tosti, L.; Tothill, N.; Tovmassian, G.; Travnicek, P.; Truzzi, S.; Tuossenel, F.; Umana, G.; Vacula, M.; Vagelli, V.; Valentino, M.; Vallage, B.; Vallania, P.; van Eldik, C.; Varner, G. S.; Vassiliev, V.; Vazquez Acosta, M.; Vecchi, M.; Veh, J.; Vercellone, S.; Vergani, S.; Verguilov, V.; Vettolani, G. P.; Viana, A.; Vigorito, C. F.; Vitale, V.; Vorobiov, S.; Vovk, I; Vuillaume, T.; Wagner, S. J.; Walter, R.; Watson, J.; White, M.; White, R.; Wiemann, R.; Wierzcholska, A.; Will, M.; Williams, D. A.; Wischnewski, R.; Wolter, A.; Yamazaki, R.; Yanagita, S.; Yang, L.; Yoshikoshi, T.; Zacharias, M.; Zaharijas, G.; Zaric, D.; Zavrtanik, M.; Zavrtanik, D.; Zdziarski, A. A.; Zech, A.; Zechlin, H.; Zhdanov, V., I; Zivec, M., The Cherenkov Telescope Array (CTA), the new-generation ground-based observatory for γ astronomy, provides unique capabilities to address significant open questions in astrophysics, cosmology, and fundamental physics. We study some of the salient areas of γ cosmology that can be explored as part of the Key Science Projects of CTA, through simulated observations of active galactic nuclei (AGN) and of their relativistic jets. Observations of AGN with CTA will enable a measurement of γ absorption on the extragalactic background light with a statistical uncertainty below 15% up to a redshift z=2 and to constrain or detect γ halos up to intergalactic-magnetic-field strengths of at least 0.3 pG . Extragalactic observations with CTA also show promising potential to probe physics beyond the Standard Model. The best limits on Lorentz invariance violation from γ astronomy will be improved by a factor of at least two to three. CTA will also probe the parameter space in which axion-like particles could constitute a significant fraction, if not all, of dark matter. We conclude on the synergies between CTA and other upcoming facilities that will foster the growth of γ cosmology. © 2021 IOP Publishing Ltd and Sissa Medialab., We gratefully acknowledge financial support from the following agencies and organizations: State Committee of Science of Armenia, Armenia; The Australian Research Council, Astronomy Australia Ltd, The University of Adelaide, Australian National University, Monash University, The University of New South Wales, The University of Sydney, Western Sydney University, Australia; Federal Ministry of Education, Science and Research, and Innsbruck University, Austria; Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq), Fundação de Amparo à Pesquisa do Estado do Rio de Janeiro (FAPERJ), Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP), Ministry of Science, Technology, Innovations and Communications (MCTIC), Brasil; Ministry of Education and Science, National RI Roadmap Project DO1-153/28.08.2018, Bulgaria; The Natural Sciences and Engineering Research Council of Canada and the Canadian Space Agency, Canada; CONICYT-Chile grants CATA AFB 170002, ANID PIA/APOYO AFB 180002, ACT 1406, FONDECYT-Chile grants, 1161463, 1170171, 1190886, 1171421, 1170345, 1201582, Gemini-ANID 32180007, Chile; Croatian Science Foundation, Rudjer Boskovic Institute, University of Osijek, University of Rijeka, University of Split, Faculty of Electrical Engineering, Mechanical Engineering and Naval Architecture, University of Zagreb, Faculty of Electrical Engineering and Computing, Croa tia; Ministry of Education, Youth and Sports, MEYS M2015046, LM2018105, LTT17006, EU/MEYS CZ.02.1.01/0.0/0.0/16_013/0001403, CZ.02.1.01/0.0/0.0/18_046/0016007 and CZ.02.1.01/0.0/0.0/16_019/0000754, Czech Republic; Academy of Finland (grant nr.317636 and 320045), Finland; Ministry of Higher Education and Research, CNRS-INSU and CNRS-IN2P3, CEA-Irfu, ANR, Regional Council Ile de France, Labex ENIGMASS, OCEVU, OSUG2020 and P2IO, France; Max Planck Society, BMBF, DESY, Helmholtz Association, Germany; Department of Atomic Energy, Department of Science and Technology, India; Istituto Nazionale di Astrofisica (INAF), Istituto Nazionale di Fisica Nucleare (INFN), MIUR, Istituto Nazionale di Astrofisica (INAF-OABRERA) Grant Fondazione Cariplo/Regione Lombardia ID 2014-1980/RST_ERC, Italy; ICRR, University of Tokyo, JSPS, MEXT, Japan; Netherlands Research School for Astronomy (NOVA), Netherlands Organization for Scientific Research (NWO), Netherlands; University of Oslo, Norway; Ministry of Science and Higher Education, DIR/WK/2017/12, the National Centre for Research and Development and the National Science Centre, UMO-2016/22/M/ST9/00583, Poland; Slovenian Research Agency, grants P1-0031, P1-0385, I0-0033, J1-9146, J1-1700, N1-0111, and the Young Researcher program, Slovenia; South African Department of Science and Technology and National Research Foundation through the South African Gamma-Ray Astronomy Programme, South Africa; The Spanish groups acknowledge the Spanish Ministry of Science and Innovation and the Spanish Research State Agency (AEI) through grants AYA2016-79724-C4-1-P, AYA2016-80889-P, AYA2016-76012-C3-1-P, BES-2016-076342, FPA2017-82729-C6-1-R, FPA2017-82729-C6-2-R, FPA2017-82729-C6-3-R, FPA2017-82729-C6-4-R, FPA2017-82729-C6-5-R, FPA2017-82729-C6-6-R, PGC2018-095161-B-I00, PGC2018-095512-B-I00, PID2019-107988GB-C22; the “Centro de Excelencia Severo Ochoa” program through grants no. SEV-2016-0597, SEV-2016-0588, SEV-2017-0709, CEX2019-000920-S; the “Unidad de Excelencia María de Maeztu” program through grant no. MDM-2015-0509; the “Ramón y Cajal” programme through grants RYC-2013-14511, RYC-2017-22665; and the MultiDark Consolider Network FPA2017-90566-REDC. They also acknowledge the Atracción de Talento contract no. 2016-T1/TIC-1542 granted by the Comunidad de Madrid; the “Postdoctoral Junior Leader Fellowship” programme from La Caixa Bank ing Foundation, grants no. LCF/BQ/LI18/11630014 and LCF/BQ/PI18/11630012; the “Programa Operativo” FEDER 2014-2020, Consejería de Economía y Conocimiento de la Junta de Andalucía (Ref. 1257737), PAIDI 2020 (Ref. P18-FR-1580) and Universidad de Jaén; “Programa Operativo de Crecimiento Inteligente” FEDER 2014-2020 (Ref. ESFRI-2017-IAC-12), Ministerio de Ciencia e Innovación, 15% co-financed by Consejería de Economía, Industria, Comercio y Conocimiento del Gobierno de Canarias; the Spanish AEI EQC2018-005094-P FEDER 2014-2020; the European Union’s “Horizon 2020” research and innovation programme under Marie Skłodowska-Curie grant agreement no. 665919; and the ESCAPE project with grant no. GA:824064; Swedish Research Council, Royal Physiographic Society of Lund, Royal Swedish Academy of Sciences, The Swedish National Infrastructure for Computing (SNIC) at Lunarc (Lund), Sweden; State Secretariat for Education, Research and Innovation (SERI) and Swiss National Science Foundation (SNSF), Switzerland; Durham University, Leverhulme Trust, Liverpool University, University of Leicester, University of Oxford, Royal Soci ety, Science and Technology Facilities Council, UK; U.S. National Science Foundation, U.S. Department of Energy, Argonne National Laboratory, Barnard College, University of California, University of Chicago, Columbia University, Georgia Institute of Technology, Institute for Nuclear and Particle Astrophysics (INPAC-MRPI program), Iowa State University, the Smithsonian Institution, Washington University McDonnell Center for the Space Sciences, The University of Wisconsin and the Wisconsin Alumni Research Foundation, USA. The research leading to these results has received funding from the European Union’s Seventh Framework Programme (FP7/2007-2013) under grant agreements No 262053 and No 317446. This project is receiving funding from the European Union’s Horizon 2020 research and innovation programs under agreement No 676134. The research leading to these results has received funding from the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement GammaRayCascades No 843800. The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à l’Energie Atomique and the Centre National de la Recherche Scientifique / Institut National de Physique Nucléaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d’Études Spatiales in France. This work performed in part under DOE Contract DE-AC02-76SF00515.
Published: 2021
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26. Gamma-Ray and X-Ray Observations of the Periodic-Repeater FRB 180916 During Active Phases

Author: F. Verrecchia, Giuseppe Pupillo, A. W. Chen, Valentina Fioretti, Y. Evangelista, Marco Feroci, P. W. Cattaneo, Luigi Pacciani, Francesco Longo, Maura Pilia, Simonetta Puccetti, L. A. Antonelli, A. Argan, Gianni Bernardi, Alessio Trois, C. Casentini, Andrea Bulgarelli, Enrico Costa, A. Ursi, Francesco Lazzarotto, G. Piano, Marco Tavani, N. Parmiggiani, C. Pittori, F. Paoletti, I. Donnarumma, S. Vercellone, L. Baroncelli, G. Di Persio, A. Morselli, Giovanni Naldi, P. Caraveo, A. Addis, M. Perri, Attilio Ferrari, Germano Bianchi, Tavani, M., Verrecchia, F., Casentini, C., Perri, M., Ursi, A., Pacciani, L., Pittori, C., Bulgarelli, A., Piano, G., Pilia, M., Bernardi, G., Addis, A., Antonelli, L. A., Argan, A., Baroncelli, L., Caraveo, P., Cattaneo, P. W., Chen, A., Costa, E., Persio, G. D., Donnarumma, I., Evangelista, Y., Feroci, M., Ferrari, A., Fioretti, V., Lazzarotto, F., Longo, F., Morselli, A., Paoletti, F., Parmiggiani, N., Trois, A., Vercellone, S., Naldi, G., Pupillo, G., Bianchi, G., Puccetti, S., ITA, USA, and ZAF
Subjects: Radio transient sources, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Flux, Astrophysics, 01 natural sciences, Gamma-ray transient sources, Luminosity, X-ray astronomy, 0103 physical sciences, 010303 astronomy & astrophysics, Radio burst, 0105 earth and related environmental sciences, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Gamma-ray astronomy, Radio bursts, Magnetic energy, Gamma ray, Radio transient source, Astronomy and Astrophysics, Radius, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Order of magnitude
Abstract: FRB 180916 is a most intriguing source at 150 Mpc distance capable of producing repeating fast radio bursts with a periodic 16.35 day temporal pattern. We report on the X-ray and $\gamma$-ray observations of FRB 180916 obtained by AGILE and Swift. We focused on the recurrent 5-day time intervals of active radio bursting and present results obtained on Feb. 3 - 8; Feb. 25; Mar. 5 - 10; Mar. 22 - 28, 2020 during a multiwavelength campaign involving high-energy and radio observations. We also searched for temporal coincidences at millisecond timescales between all known radio bursts of FRB 180916 and X-ray and MeV events detectable by AGILE. We do not detect any simultaneous event or any extended X-ray and $\gamma$-ray emission on timescales of hours/days/weeks. Our cumulative X-ray (0.3-10 keV) flux upper limit of $5 \times\,10^{-14} \rm \, erg \, cm^{-2} s^{-1}$ (obtained during 5-day active intervals) translates into an isotropic luminosity upper limit of $L_{X,UL} \sim 1.5 \times\, 10^{41} \rm erg \, s^{-1}$. Observations above 100 MeV over a many-year timescale provide an average luminosity upper limit one order of magnitude larger. These results provide the so-far most stringent limits on high-energy emission from FRB 180916 and constrain the dissipation of magnetic energy from a magnetar-like source of radius $R_m$, internal magnetic field $B_m$ and dissipation timescale $\tau_d$ to satisfy the relation $R_{m,6}^3 B_{m,16}^2 \tau_{d,8}^{-1} \lesssim 1$, where $R_{m,6}$ is $R_m$ in units of $10^6$ cm, $B_{m,16}$ is $B_m$ in units of $10^{16}$ G, and $\tau_{d,8}$ in units of $10^8$ s., Comment: Accepted for publication by the Astrophysical Journal Letters on April 5, 2020
Published: 2020

27. The swift observations of distant high-energy peaked BL Lacertae objects

Author: Bidzina Kapanadze, S. Kapanadze, L. Neparidze, P. Romano, and S. Vercellone
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Flux, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Spectral line, Redshift, law.invention, Luminosity, Relativistic plasma, Space and Planetary Science, law, 0103 physical sciences, High Energy Physics::Experiment, Blazar, 010303 astronomy & astrophysics, Flare, Fermi Gamma-ray Space Telescope
Abstract: In this paper, we present the timing and spectral results for the seven distant and poorly investigated BL Lacertae sources with redshifts $z\gtrsim 0.5$, using the archival data obtained with the Swift and other multifrequency instruments during 2006 August–2015 July. Our timing study has revealed a number of the 0.3–10 keV flux changes from the fluctuations observed within one day to the variabilities on timescales of a few months. Namely, the relatively densely-sampled observations of BZB J1517+6525 showed a strong X-ray flare by a factor of ∼5 during 2014 September-December. While this instance can be explained by the propagation of shock wave though the blazar jet which causes a strong heat-up of the relativistic plasma, the lower-amplitude flux fluctuations observed in higher X-ray states could be related to the interaction between the shock front and jet inhomogeneities. The curved 0.3–10 keV spectra showed the ranges of the photon index at 1 keV $a=1.27$(0.10)–2.30(0.09), curvature parameter $b = 0.12$(0.08)–1.19(0.27), synchrotron SED peak position $E_{p} = 0.49$(0.09)–3.39(0.97) keV, while some spectra do not exhibit spectral curvature and fit well with a simple power law model yielding the 0.3–10 keV photon-index $\Gamma =1.48$(0.15)–2.32(0.08). Large spectral curvatures observed for the majority of the log-parabolic spectra hint at the importance of the second-order Fermi mechanism for our targets. Our targets show very high isotropic luminosity $L_{0.3\text{--}10~\text{keV}}\sim 10^{46}~\mbox{erg}\,\mbox{s}^{-1}$ compared to the nearby bright BL Lacertae objects.
Published: 2020
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28. The Second AGILE MCAL Gamma-Ray Burst Catalog: 13 yr of Observations

Author: A. Ursi, M. Romani, F. Verrecchia, C. Pittori, M. Tavani, M. Marisaldi, M. Galli, C. Labanti, N. Parmiggiani, A. Bulgarelli, A. Addis, L. Baroncelli, M. Cardillo, C. Casentini, P. W. Cattaneo, A. Chen, A. Di Piano, F. Fuschino, F. Longo, F. Lucarelli, A. Morselli, G. Piano, and S. Vercellone
Subjects: Space and Planetary Science, Astronomy and Astrophysics
Abstract: We present the results of a systematic search and analysis of GRBs detected by the Astrorivelatore Gamma ad Immagini LEggero (AGILE) MiniCALorimeter (MCAL; 0.4–100 MeV) over a time frame of 13 yr, from 2007 to 2020 November. The MCAL GRB sample consists of 503 bursts triggered by MCAL, 394 of which were fully detected onboard with high time resolution. The sample consists of about 44% short GRBs and 56% long GRBs. In addition, 109 bursts triggered partial MCAL onboard data acquisitions, providing further detections that can be used for joint analyses or triangulations. More than 90% of these GRBs were also detected by the AGILE Scientific RateMeters (RMs), providing simultaneous observations between 20 keV and 100 MeV. We performed spectral analysis of these events in the 0.4–50 MeV energy range. We could fit the time-integrated spectrum of 258 GRBs with a single power-law model, resulting in a mean photon index 〈β〉of−2.3. Among them, 43 bursts could also be fitted with a Band model, with peak energy above 400 keV, resulting in a mean low-energy photon index 〈α〉 = −0.6, a mean high-energy photon index 〈β〉 = −2.5, and a mean peak energy 〈E p 〉 = 640 keV. The AGILE MCAL GRB sample mostly consists of hard-spectrum GRBs, with a large fraction of short-duration events. We discuss properties and features of the MCAL bursts, whose detections can be used to perform joint broad-band analysis with other missions, and to provide insights on the high-energy component of the prompt emission in the tens of mega electron volt energy range.
Published: 2022
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29. A new technique for probing the internal structure of volcanoes using cosmic-ray muons

Author: Daniele Carbone, Teresa Mineo, M. C. Maccarone, V. La Parola, G. La Rosa, Osvaldo Catalano, Giuseppe Sottile, S. Vercellone, M. Del Santo, G. Pareschi, Luciano Zuccarello, and Giancarlo Cusumano
Subjects: Physics, Nuclear and High Energy Physics, Particle physics, Muon, 010504 meteorology & atmospheric sciences, Physics::Instrumentation and Detectors, business.industry, Attenuation, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Electron, Scintillator, 010502 geochemistry & geophysics, 01 natural sciences, law.invention, Telescope, Optics, law, business, Image resolution, Cherenkov radiation, 0105 earth and related environmental sciences
Abstract: Among the considerable number of studies that can be carried out using muons, we pay specific attention to the radiography of volcanoes based on the same principle of the X-ray radiography of human body. Thanks to their high penetration capability, cosmic-ray muons can be used to reconstruct the density distribution of the interior of huge structures by measuring the attenuation induced by the material on the muon flux. In particular, the quantitative understanding of the inner structure of volcanoes is a key-point to forecast the dangerous stages of activity and mitigate volcanic hazards. The instrumental approach is currently based on the detection of muons crossing hodoscopes made up of scintillator planes. Unfortunately, these detectors are affected by a strong background comprised by accidental coincidence of vertical shower particles, horizontal high-energy electrons and upward going particles. We propose an alternative technique based on the detection of the Cherenkov light produced by muons. This can be achieved with an imaging atmospheric Cherenkov telescope composed of a high reflectivity optical system that focus the Cherenkov light onto a multi-pixel focal camera with fast read-out electronics. The Cherenkov light emitted by a muon is imaged on the camera as an annular pattern which contains information to reconstruct the direction of the incident muon. We have estimated that using the Cherenkov imaging technique for muon radiography of volcanoes gives the advantage of a negligible background and improved spatial resolution, compared to the majority of the particle detectors. We present results of simulations based on a telescope with a positioning resolution of 13.5 m which corresponds to an acceptance of 9 cm2 sr. The telescope is located 1500 m far from a toy-model volcano, namely, a cone with a base diameter of 500 m and a height of 240 m. We test the feasibility of the proposed method by estimating the minimum number of observation nights needed to resolve inner empty conduits of different diameter.
Published: 2017
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30. Prospects for γ-ray observations of narrow-line Seyfert 1 galaxies with the Cherenkov Telescope Array – II. γ–γ Absorption in the broad-line region radiation fields

Author: Luigi Foschini, Markus Böttcher, S. Vercellone, P. Romano, Catherine Boisson, Marco Landoni, 24420530 - Böttcher, Markus, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: galaxies [Gamma rays], Cherenkov Telescope Array, IACT, Astrophysics, model: absorption, 01 natural sciences, Spectral line, accretion, galaxies: individual: PKS 1502+036, propagation, individual: PMN J0948+0022 [Galaxies], black hole, 010303 astronomy & astrophysics, Line (formation), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), galaxies: individual: SBS 0846+513, galaxies: individual: PMN J0948+0022, Astrophysics::Instrumentation and Methods for Astrophysics, imaging, galaxies: Seyfert, gamma ray: emission, Eddington luminosity, symbols, Astrophysics - High Energy Astrophysical Phenomena, Seyfert [Galaxies], individual: PKS 1502+036 [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Cherenkov counter: atmosphere, VHE, GLAST, symbols.namesake, 0103 physical sciences, gamma rays: galaxies, quasar, Cherenkov radiation, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, background, Astronomy and Astrophysics, Quasar, galaxies: jets, sensitivity, photon photon: absorption, Galaxy, Automatic Keywords, Space and Planetary Science, individual: SBS 0846+513 [Galaxies], jets [Galaxies], galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Gamma-ray emitting narrow-line Seyfert 1 ($\gamma$-NLS1) galaxies possibly harbour relatively low-mass black holes (10$^6$-10$^8$ M$_{\odot}$) accreting close to the Eddington limit, and share many characteristics with their sibling sources, flat-spectrum radio quasars. Although they have been detected in the MeV--GeV band with Fermi-LAT, they have never been seen in the very high energy band with current imaging atmospheric Cherenkov telescopes (IACTs). Thus, they are key targets for the next-generation IACT, the Cherenkov Telescope Array (CTA). In a previous work we selected, by means of extensive simulations, the best candidates for a prospective CTA detection (SBS 0846$+$513, PMN J0948$+$0022, and PKS 1502$+$036) taking into account the effects of both the intrinsic absorption (approximated with a cut-off at 30 GeV), and the extra-galactic background light on the propagation of $\gamma$-rays. In this work we simulate the spectra of these three sources by adopting more realistic broad-line region (BLR) absorption models. In particular, we consider the detailed treatment of $\gamma$-$\gamma$ absorption in the radiation fields of the BLR as a function of the location of the $\gamma$-ray emission region with parameters inferred from observational constraints. We find that, due to the energy range extent and its sensitivity, CTA is particularly well suited to locate the $\gamma$-ray emitting region in $\gamma$-NLS1. In particular CTA will be able not only to distinguish whether the $\gamma$-ray emitting region is located inside or outside the BLR, but also where inside the BLR it may be., Comment: Accepted for publication in Monthly Notices of the Royal Astronomical Society. 15 pages, 8 figures, 7 tables
Published: 2020
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31. AGILE Observations of Two Repeating Fast Radio Bursts with Low Intrinsic Dispersion Measures

Author: A. Pellizzoni, E. Costa, M. Tavani, A. Ursi, A. Giuliani, Martino Marisaldi, G. Piano, A. Morselli, M. Pilia, A. Ferrari, C. Casentini, F. Longo, F. Fuschino, A. Argan, P. W. Cattaneo, M. Feroci, Andrea Bulgarelli, L. A. Antonelli, G. Barbiellini, N. Parmiggiani, F. Paoletti, P. A. Caraveo, M. Cardillo, I. Donnarumma, F. Lazzarotto, A. W. Chen, Claudio Labanti, M. Galli, F. Verrecchia, Francesco Lucarelli, C. Pittori, S. Vercellone, P. Lipari, 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.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Radio transient sources, Millisecond, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Magnetar, Gamma-ray transient sources, Luminosity, X-ray transient, Fast radio bursts, Gamma-ray Astrophysics, Space and Planetary Science, Dispersion (optics), Magnetars, Astrophysics - High Energy Astrophysical Phenomena, Energy (signal processing), Isotropic energy, Fast radio burst
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
Published: 2020

32. First detection of the Crab Nebula at TeV energies with a Cherenkov telescope in dual-mirror Schwarzschild-Couder configuration: the ASTRI-Horn telescope

Author: S. Lombardi, O. Catalano, S. Scuderi, L. A. Antonelli, G. Pareschi, E. Antolini, L. Arrabito, G. Bellassai, K. Bernlöhr, C. Bigongiari, B. Biondo, G. Bonanno, G. Bonnoli, G. M. Böttcher, J. Bregeon, P. Bruno, R. Canestrari, M. Capalbi, P. Caraveo, P. Conconi, V. Conforti, G. Contino, G. Cusumano, E. M. de Gouveia Dal Pino, A. Distefano, G. Farisato, C. Fermino, M. Fiorini, A. Frigo, S. Gallozzi, C. Gargano, S. Garozzo, F. Gianotti, S. Giarrusso, R. Gimenes, E. Giro, A. Grillo, D. Impiombato, S. Incorvaia, N. La Palombara, V. La Parola, G. La Rosa, G. Leto, F. Lucarelli, M. C. Maccarone, D. Marano, E. Martinetti, A. Miccichè, R. Millul, T. Mineo, G. Nicotra, G. Occhipinti, I. Pagano, M. Perri, G. Romeo, F. Russo, B. Sacco, P. Sangiorgi, F. G. Saturni, A. Segreto, G. Sironi, G. Sottile, A. Stamerra, L. Stringhetti, G. Tagliaferri, M. Tavani, V. Testa, M. C. Timpanaro, G. Toso, G. Tosti, M. Trifoglio, G. Umana, S. Vercellone, R. Zanmar Sanchez, C. Arcaro, A. Bulgarelli, M. Cardillo, E. Cascone, A. Costa, A. D’Aì, F. D’Ammando, M. Del Santo, V. Fioretti, A. Lamastra, S. Mereghetti, F. Pintore, G. Rodeghiero, P. Romano, J. Schwarz, E. Sciacca, F. R. Vitello, A. Wolter, Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), 24420530 - Böttcher, Markus, ITA, USA, FRA, Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), and Université Grenoble Alpes (UGA)
Subjects: Cherenkov Telescope Array, reflection: efficiency, Astrophysics, 7. Clean energy, 01 natural sciences, law.invention, energy: threshold, Observatory, law, hardware, Cherenkov, data analysis [Methods], mirror, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, electronics, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Schwarzschild, observatory, Cardinal point, supernovae: individual: Crab Nebula, gamma ray: emission, techniques: miscellaneous, individual: Crab Nebula [Supernovae], Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, technique: miscellaneous, Astrophysics and Astronomy, gamma rays: general, telescopes, methods: data analysis, Astrophysics::High Energy Astrophysical Phenomena, general [Gamma rays], miscellaneous [Techniques], FOS: Physical sciences, Context (language use), programming, VHE, Telescope, 0103 physical sciences, detector: pixel, photomultiplier: silicon, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Cherenkov radiation, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, calibration, supernovae: individual (Crab Nebula), Crab Nebula, Cherenkov counter, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], statistical, Telescopes, astro-ph.IM
Abstract: We report on the first detection of very high-energy (VHE) gamma-ray emission from the Crab Nebula by a Cherenkov telescope in dual-mirror Schwarzschild-Couder (SC) configuration. The result has been achieved by means of the 4 m size ASTRI-Horn telescope, operated on Mt. Etna (Italy) and developed in the context of the Cherenkov Telescope Array Observatory preparatory phase. The dual-mirror SC design is aplanatic and characterized by a small plate scale, allowing us to implement large field of view cameras with small-size pixel sensors and a high compactness. The curved focal plane of the ASTRI camera is covered by silicon photo-multipliers (SiPMs), managed by an unconventional front-end electronics based on a customized peak-sensing detector mode. The system includes internal and external calibration systems, hardware and software for control and acquisition, and the complete data archiving and processing chain. The observations of the Crab Nebula were carried out in December 2018, during the telescope verification phase, for a total observation time (after data selection) of 24.4 h, equally divided into on- and off-axis source exposure. The camera system was still under commissioning and its functionality was not yet completely exploited. Furthermore, due to recent eruptions of the Etna Volcano, the mirror reflection efficiency was reduced. Nevertheless, the observations led to the detection of the source with a statistical significance of 5.4 sigma above an energy threshold of ~3 TeV. This result provides an important step towards the use of dual-mirror systems in Cherenkov gamma-ray astronomy. A pathfinder mini-array based on nine large field-of-view ASTRI-like telescopes is under implementation., 6 pages, 2 figures
Published: 2020
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33. The beamed jet and quasar core of the distant blazar 4C 71.07

Author: A. Di Paola, Evgeni Ovcharov, Yu. V. Troitskaya, Sergey S. Savchenko, A. A. Arkharov, N. V. Efimova, V. Bozhilov, M. G. Nikolashvili, Sunay Ibryamov, Elena G. Larionova, Manash R. Samal, P. Calcidese, I. Agudo, Marcello Giroletti, Givi N. Kimeridze, J. L. Gomez, Carolina Casadio, Anne Lähteenmäki, C. M. Raiteri, Alan P. Marscher, Valeri M. Larionov, Uwe Bach, D. Carosati, P. Romano, M. Minev, G. A. Borman, A. C. Sadun, Lorand A. Sigua, E. N. Kopatskaya, S. Vercellone, Joseph Moody, Goran Damljanović, Evgeni Semkov, D. O. Mirzaqulov, S. Baitieri, M. Villata, A. Strigachev, O. M. Kurtanidze, Helen Jermak, S. A. Klimanov, R. Bachev, Stoyanka Peneva, Wen Ping Chen, Walter Boschin, S. G. Jorstad, Sol N. Molina, D. A. Morozova, Iain A. Steele, O. Vince, M. S. Butuzova, T. S. Grishina, V. T. Doroshenko, Sofia O. Kurtanidze, M. I. Carnerero, J. A. Acosta-Pulido, L. Slavcheva-Mihova, Simona Righini, N. Rizzi, S. V. Nazarov, Boyko Mihov, Ivan S. Troitsky, Sh. A. Ehgamberdiev, Merja Tornikoski, A. A. Nikiforova, Department of Electronics and Nanoengineering, Metsähovi Radio Observatory, Aalto-yliopisto, Aalto University, Istituto Nazionale di Astrofisica, Bulgarian National Science Fund, Ministry of Education, Youth and Science (Bulgaria), Ministry of Education, Science and Technological Development (Serbia), Russian Science Foundation, and Shota Rustaveli National Science Foundation
Subjects: ACTIVE GALACTIC NUCLEI, RADIO-SOURCES, Quasars: individual: 4C 71.07, Astrophysics::High Energy Astrophysical Phenomena, jets [galaxies], Library science, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, The Republic, Observatory, 0103 physical sciences, ABSORPTION, Astrophysics::Solar and Stellar Astrophysics, SPECTRA, Bulgarian, 010303 astronomy & astrophysics, BLACK-HOLES, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Government, 010308 nuclear & particles physics, St petersburg, Astronomy and Astrophysics, Galaxies: active, Astrophysics - Astrophysics of Galaxies, language.human_language, Joint research, VARIABILITY, Work (electrical), 13. Climate action, Space and Planetary Science, Galaxies: jets, WEBT CAMPAIGN, Astrophysics of Galaxies (astro-ph.GA), individual: 4C 71.07 [quasars], active [galaxies], language, LUMINOSITY, ROTATIONS, Christian ministry, COMPLETE SAMPLE, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The object 4C 71.07 is a high-redshift blazar whose spectral energy distribution shows a prominent big blue bump and a strong Compton dominance. We present the results of a 2- yr multiwavelength campaign led by the Whole Earth Blazar Telescope (WEBT) to study both the quasar core and the beamed jet of this source. The WEBT data are complemented by ultraviolet and X-ray data from Swift, and by γ-ray data by Fermi. The big blue bump is modelled by using optical and near-infrared mean spectra obtained during the campaign, together with optical and ultraviolet quasar templates. We give prescriptions to correct the source photometry in the various bands for the thermal contribution, in order to derive the non-thermal jet flux. The role of the intergalactic medium absorption is analysed in both the ultraviolet and X-ray bands.We provide opacity values to deabsorb ultraviolet data, and derive a best-guess value for the hydrogen column density of Nbest H = 6.3 × 10 cmthrough the analysis of X-ray spectra.We estimate the disc and jet bolometric luminosities, accretion rate, and black hole mass. Light curves do not show persistent correlations among flux changes at different frequencies. We study the polarimetric behaviour and find no correlation between polarization degree and flux, even when correcting for the dilution effect of the big blue bump. Similarly, wide rotations of the electric vector polarization angle do not seem to be connected with the source activity.© 2019 The Author(s)., We acknowledge financial contribution from the agreement ASI-INAF n.2017-14-H.0 and from the contract PRIN-SKA-CTA-INAF 2016. PR and SV acknowledge contract ASI-INAF I/004/11/0. We acknowledge support by Bulgarian National Science Programme 'Young Scientists and Postdoctoral Students 2019', Bulgarian National Science Fund under grant DN18-10/2017 and National RI Roadmap Projects DO1-157/28.08.2018 and DO1-153/28.08.2018 of the Ministry of Education and Science of the Republic of Bulgaria. GD and OV gratefully acknowledge the observing grant support from the Institute of Astronomy and Rozhen National Astronomical Observatory, Bulgarian Academy of Sciences via bilateral joint research project 'Study of ICRF radio-sources and fast variable astronomical objects' (head -G.Damljanovic). This work is a part of the Projects No. 176011 ('Dynamics and Kinematics of Celestial Bodies and Systems'), No. 176004 ('Stellar Physics'), and No. 176021 ('Visible and Invisible Matter in Nearby Galaxies: Theory and Observations') supported by the Ministry of Education, Science and Technological Development of the Republic of Serbia. This research was partially supported by the Bulgarian National Science Fund of theMinistry of Education and Science under grants DN 08-1/2016, DN 18-13/2017, and KP-06-H28/3 (2018). The Skinakas Observatory is a collaborative project of the University of Crete, the Foundation for Research and Technology -Hellas, and the Max-Planck-Institut fur Extraterrestrische Physik. The St Petersburg University team acknowledges support from Russian Science Foundation grant no. 17-12-01029. The Abastumani team acknowledges financial support by the Shota Rustaveli National Science Foundation under contract FR/217950/16. This work was partly supported by the National Science Fund of the Ministry of Education and Science of Bulgaria under grant DN 08-20/2016, and by funds of the project RD-08-37/2019 of the University of Shumen. The Astronomical Observatory of the Autonomous Region of the Aosta Valley (OAVdA) is managed by the Fondazione Clement Fillietroz-ONLUS, which is supported by the Regional Government of the Aosta Valley, the Town Municipality of Nus and the Unite des Communes valdotaines Mont-Emilius'. The research at the OAVdA was partially funded by two 'Research and Education' grants from Fondazione CRT
Published: 2019

34. A recent strong X-ray flaring activity of 1ES 1959+650 withpossiblyless efficient stochastic acceleration

Author: Bidzina Kapanadze, P. Romano, S. Kapanadze, S. Vercellone, Daniela Dorner, and T. Mdzinarishvili
Subjects: Physics, Acceleration, 010308 nuclear & particles physics, Space and Planetary Science, 0103 physical sciences, X-ray, Astronomy and Astrophysics, Astrophysics, 010303 astronomy & astrophysics, 01 natural sciences
Abstract: We present an X-ray flaring activity of 1ES 1959+650 in 2015 August-2016 January, which was the most powerful and prolonged during the 10.75 yr period since the start of its monitoring with X-ray Telescope onboard Swift. A new highest historical 0.3-10 keV count rate was recorded three times that makes this object the third BL Lacertae source exceeding the level of 20 counts s-1. Along with the overall variability by a factor of 5.7, this epoch was characterized by fast X-ray flares by a factor of 2.0-3.1, accompanied with an extreme spectral variability. The source also shows a simultaneous flaring activity in the optical - UV and 0.3-100 GeV bands, although a fast γ-ray flare without significant optical - X-ray counterparts is also found. In contrast to the X-ray flares in the previous years, the stochastic acceleration seems be less important for the electrons responsible for producing X-ray emission during this flare that challenges the earlier suggestion that the electrons in the jets of TeV-detected BL Lacertae objects should undergo an efficient stochastic acceleration resulting in a lower X-ray spectral curvature.
Published: 2016
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35. AGILE and Konus-Wind Observations of GRB 190114C: The Remarkable Prompt and Early Afterglow Phases

Author: R. Aptekar, Francesco Lucarelli, V. Vittorini, F. Paoletti, Dmitry S. Svinkin, M. Feroci, C. Pittori, I. Donnarumma, Y. Evangelista, M. Romani, D. Frederiks, P. A. Caraveo, F. Fuschino, P. W. Cattaneo, A. Tsvetkova, F. Lazzarotto, G. Piano, Martino Marisaldi, N. Parmiggiani, A. Morselli, F. Longo, M. Pilia, M. Cardillo, C. Casentini, E. Costa, Arnaud Ferrari, M. Tavani, A. Ursi, M. Galli, F. Verrecchia, A. Giuliani, G. Barbiellini, Claudio Labanti, A. Trois, L. A. Antonelli, A. W. Chen, A. Argan, Andrea Bulgarelli, S. Vercellone, Ursi, A., Tavani, M., Frederiks, D. D., Romani, M., Verrecchia, F., Marisaldi, M., Aptekar, R. L., Antonelli, L. A., Argan, A., Bulgarelli, A., Barbiellini, G., Caraveo, P., Cardillo, M., Casentini, C., Cattaneo, P. W., Chen, A., Costa, E., Donnarumma, I., Evangelista, Y., Feroci, M., Ferrari, A., Fuschino, F., Galli, M., Giuliani, A., Labanti, C., Lazzarotto, F., Longo, F., Lucarelli, F., Morselli, A., Paoletti, F., Parmiggiani, N., Piano, G., Pilia, M., Pittori, C., Svinkin, D. S., Trois, A., Tsvetkova, A. E., Vercellone, S., and Vittorini, V.
Subjects: 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Flux, Astrophysics, 01 natural sciences, Gamma-ray transient sources, 0103 physical sciences, Radiative transfer, Gamma-ray transient sources (1853), Adiabatic process, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Gamma-ray astronomy, Gamma-ray astronomy (628), Astronomy and Astrophysics, Spectral component, Afterglow, Space and Planetary Science, Gamma-ray bursts (629), Gamma-ray bursts, Gamma-ray burst, Fermi Gamma-ray Space Telescope
Abstract: GRB 190114C represents a breakthrough for the physics of gamma-ray bursts (GRBs), being the first GRB with delayed emission above 300 GeV, as reported by MAGIC. We present in this paper the sub-MeV/MeV data of the prompt and early afterglow emissions of GRB 190114C, as detected by AGILE and Konus-Wind, in the 20 keV-100 MeV energy range. The first stages of the burst exhibit multiple emission components, associated with an interesting spectral evolution. The first 2 s of the prompt emission can be described by a single "Band-like" spectral component. The successive 4 s show the presence of an additional high-energy spectral component, which quickly evolves into a "hard-flat" component of the νFν spectrum, extending up to 10-100 MeV and likely produced by inverse Compton radiation, whose onset and evolution are clearly shown in our data. After this phase, the νFν spectrum evolves into a "V shape," showing the persistence and spectral hardening of the additional high-energy component in substantial agreement with Fermi and Swift results. We also analyze the first ∼200 s of the early afterglow that show a reflaring episode near T0 + 15 s. We identify a new, so-far-unnoticed flux temporal break near T0 + 100 s, which is detected in hard X-rays by both Konus-Wind and INTEGRAL/SPI-ACS. We find this break incompatible with the commonly assumed adiabatic evolution of a fireball in a constant-density medium. We interpret this break as a consequence of radiative evolution of the early afterglow from a fireball expanding in a wind-like circumburst medium.
Published: 2020
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36. Stochastic acceleration in the relativistic jets of BL Lacertae objects

Author: P. Romano, S. Vercellone, and Bidzina Kapanadze
Subjects: Physics, Jet (fluid), Active galactic nucleus, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Synchrotron radiation, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Black hole, Acceleration, Astrophysical jet, Space and Planetary Science, 0103 physical sciences, Spectral energy distribution, 010303 astronomy & astrophysics, Instrumentation, Fermi Gamma-ray Space Telescope
Abstract: BL Lacertae objects (BL Lacs) constitute a rare class of active galactic nuclei (AGNs) with the extreme observational features attributed to the Doppler-boosted emission from the relativistic jets, closely aligned along our line-of-sight. The spectral energy distribution (SED), extending over 17–19 orders of the frequency from the radio to the TeV energy range, is of nonthermal origin and shows a typical two-component structure. The lower-energy component, which ranges from the radio to the X-ray frequencies, is widely accepted to be a synchrotron radiation emitted by relativistic electrons. The latter can be accelerated and collimated via the Blandford-Znajek mechanism or magneto-hydrodynamic processes in the vicinity of the central super-massive black hole. However, the accelerated particles should loose the energy, sufficient for the emission of the KeV-TeV photons, very quickly and they require an additional acceleration via the mechanisms operating locally in the jet. According to the different studies and simulations, particles can undergo a strong stochastic (second-order Fermi) acceleration due to the resonant scattering of the magnetohydrodynamic waves, representing the turbulent magnetic irregularities. On the other hand, the jet turbulence can be strongly amplified due to the interaction between the shock front and the density inhomogeneities in the pre-shock relativistic jet fluid. Our intense X-ray spectral study of TeV-detected, bright BL Lacs (Mrk 421, 1ES 1959 + 650, Mrk 501) often demonstrate the signatures of the efficient stochastic acceleration (a low spectral curvature and different correlations expected within the stochastic process). We have also detected the cases when these sources show the relation between the synchrotron SED peak location Ep and peak height Sp in the form Sp ∝ E p α with the values of the exponent close to 0.6. The latter is expected when the momentum-diffusion coefficient and the turbulence spectrum are variable during the stochastic acceleration process: there is a transition from the Kraichnan-type into the hard-sphere turbulence.
Published: 2020
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37. AGILE, Fermi, Swift, and GASP/WEBT multi-wavelength observations of the high-redshift blazar 4C +71.07 in outburst

Author: Andrea Bulgarelli, P. Romano, S. Vercellone, Carolina Casadio, Anne Lähteenmäki, Boyko Mihov, A. Strigachev, Emilia Järvelä, C. Pittori, G. A. Borman, F. Paoletti, Marco Tavani, José L. Gómez, Sergio Colafrancesco, U. Bach, V. Vittorini, I. Donnarumma, Valeri M. Larionov, Fabrizio Lucarelli, V. T. Doroshenko, J. A. Acosta-Pulido, Valentina Fioretti, L. Slavcheva-Mihova, Simona Righini, P. W. Cattaneo, E. N. Kopatskaya, O. M. Kurtanidze, C. M. Raiteri, S. A. Klimanov, M. Villata, Francesco Longo, M. S. Butuzova, F. D'Ammando, N. V. Efimova, F. Verrecchia, S. V. Nazarov, Evgeni Semkov, R. Bachev, M. I. Carnerero, D. O. Mirzaqulov, Sergey S. Savchenko, T. S. Grishina, G. Damljanovic, A. Morselli, A. Di Paola, M. Orienti, P. Munar-Adrover, L. V. Larionova, Marcello Giroletti, Sol N. Molina, Sh. A. Ehgamberdiev, D. A. Morozova, G. Piano, Merja Tornikoski, Arkady A. Arkharov, O. Vince, N. Parmiggiani, Yu. V. Troitskaya, I. Agudo, Vercellone, S., Romano, P., Piano, G., Vittorini, V., Donnarumma, I., Munar-Adrover, P., Raiteri, C. M., Villata, M., Verrecchia, F., Lucarelli, F., Pittori, C., Bulgarelli, A., Fioretti, V., Tavani, M., Acosta-Pulido, J. A., Agudo, I., Arkharov, A. A., Bach, U., Bachev, R., Borman, G. A., Butuzova, M. S., Carnerero, M. I., Casadio, C., Damljanovic, G., D'Ammando, F., Di Paola, A., Doroshenko, V. T., Efimova, N. V., Ehgamberdiev, S. A., Giroletti, M., Gómez, J. L., Grishina, T. S., Järvelä, E., Klimanov, S. A., Kopatskaya, E. N., Kurtanidze, O. M., Lähteenmäki, A., Larionov, V. M., Larionova, L. V., Mihov, B., Mirzaqulov, D. O., Molina, S. N., Morozova, D. A., Nazarov, S. V., Orienti, M., Righini, S., Savchenko, S. S., Semkov, E., Slavcheva-Mihova, L., Strigachev, A., Tornikoski, M., Troitskaya, Y. V., Vince, O., Cattaneo, P. W., Colafrancesco, S., Longo, F., Morselli, A., Paoletti, F., Parmiggiani, N., ITA, Academy of Sciences Republic of Uzbekistan, Russian Science Foundation, Bulgarian Academy of Sciences, Agenzia Spaziale Italiana, Ministerio de Economía y Competitividad (España), Ministry of Education, Science and Technological Development (Serbia), Osservatorio Astronomico di Brera, Osservatorio Astronomico Roma, ASI Science Data Center, Autonomous University of Barcelona, Osservatorio Astronomico di Torino, INAF/IASF Bologna, Università di Roma Tor Vergata, Instituto de Astrofísica de Canarias, CSIC, RAS - Pulkovo Astronomical Observatory, Max-Planck-Institut für Radioastronomie, Crimean Astrophysical Observatory, University of Belgrade, Universita di Bologna, Lomonosov Moscow State University, Academy of Sciences of the Republic of Uzbekistan, St. Petersburg State University, Metsähovi Radio Observatory, Georgian National Academy of Sciences, Istituto Nazionale di Fisica Nucleare (INFN), University of the Witwatersrand, Università Degli Studi di Trieste, Sapienza University of Rome, Department of Electronics and Nanoengineering, Aalto-yliopisto, and Aalto University
Subjects: Galaxies [Gamma rays], Acceleration of particles, Relativistic processe, Radiation mechanisms: non-thermal, Astrophysics::High Energy Astrophysical Phenomena, Supermassive black holes [Quasars], FOS: Physical sciences, Galaxie [Gamma rays], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 7. Clean energy, 01 natural sciences, law.invention, law, 0103 physical sciences, Gamma rays: Galaxies, Quasars: Individual: 4C +71.07, Quasars: Supermassive black holes, Relativistic processes, Astronomy and Astrophysics, Space and Planetary Science, Blazar, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, non-thermal [Radiation mechanisms], 010308 nuclear & particles physics, Order (ring theory), Quasar, Astronomy and Astrophysic, Acceleration of particle, Redshift, Supermassive black hole [Quasars], Spectral energy distribution, Individual: 4C +71.07 [Quasars], Astrophysics - High Energy Astrophysical Phenomena, Energy (signal processing), Flare, Fermi Gamma-ray Space Telescope
Abstract: Context. The flat-spectrum radio quasar 4C +71.07 is a high-redshift (z = 2.172), γ-loud blazar whose optical emission is dominated by thermal radiation from the accretion disc. Aims. 4C +71.07 has been detected in outburst twice by the AGILE γ-ray satellite during the period from the end of October to mid-November 2015, when it reached a γ-ray flux of the order of F(E > 100 MeV)=(1.2 ± 0.3)×10 photons cm s and F(E > 100 MeV)=(3.1 ± 0.6)×10 photons cm s, respectively, allowing us to investigate the properties of the jet and the emission region. Methods. We investigated its spectral energy distribution by means of almost-simultaneous observations covering the cm, mm, near-infrared, optical, ultraviolet, X-ray, and γ-ray energy bands obtained by the GASP-WEBT Consortium and the Swift, AGILE, and Fermi satellites. Results. The spectral energy distribution of the second γ-ray flare (whose energy coverage is more dense) can be modelled by means of a one-zone leptonic model, yielding a total jet power of about 4 × 10 erg s. Conclusions. During the most prominent γ-ray flaring period our model is consistent with a dissipation region within the broad-line region. Moreover, this class of high-redshift, flat-spectrum radio quasars with high-mass black holes might be good targets for future γ-ray satellites such as e-ASTROGAM. © ESO 2019., AGILE is an ASI space mission developed with programmatic support by INAF and INFN. We acknowledge partial support through the ASI grant no. I/028/12/0. SV and PR acknowledge contract ASI-INAF I/004/11/0 and INAF/IASF Palermo where most of the work was carried out. SV acknowledges financial contribution from the agreement ASI-INAF no. 2017-14-H.0. Part of this work is based on archival data, software, or online services provided by the ASI SPACE SCIENCE DATA CENTER (ASI-SSDC). SV and PR thank Leonardo Barzaghi and Sara Baitieri for useful discussions. The Osservatorio di Torino team acknowledges the financial contribution from the agreement ASI-INAF No. 2017-14-H.0 and from the contract PRIN-SKA-CTA-INAF 2016. OMK acknowledges financial support from the Shota Rustaveli National Science Foundation under contract FR/217950/16 and grants NSFC11733001, NSFCU1531245. IA acknowledges support from a Ramón y Cajal grant of the Ministerio de Economía y Compet-itividad (MINECO) of Spain. The research at the IAA–CSIC was supported in part by the MINECO through grants AYA2016–80889–P, AYA2013–40825–P, and AYA2010–14844, and by the regional government of Andalucía through grant P09–FQM–4784. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). Calar Alto Observatory is jointly operated by the MPIA and the IAA-CSIC. This research was partially supported by the Bulgarian National Science Fund of the Ministry of Education and Science under grant DN 08-1/2016. The St. Petersburg University team acknowledges support from Russian Science Foundation grant 17-12-01029. AZT-24 observations are made within an agreement among the Pulkovo, Rome, and Teramo observatories. GD and OV gratefully acknowledge the observing grant support from the Institute of Astronomy and Rozhen National Astronomical Observatory, Bulgaria Academy of Sciences, via bilateral joint research project “Observations of ICRF radio-sources visible in optical domain” (PI G. Damljanovic). This work is a part of Project No. 176011 (“Dynamics and kinematics of celestial bodies and systems”), No. 176004 (“Stellar physics”) and No. 176021 (“Visible and invisible matter in nearby galaxies: theory and observations”) supported by the Ministry of Education, Science, and Technological Development of the Republic of Serbia. The Maidanak Observatory team acknowledges support from Uzbekistan Academy of Sciences grants No. F2-FA-F027 and F.4-16.
Published: 2019

38. Second AGILE catalogue of gamma-ray sources

Author: Fulvio Gianotti, L. Baroncelli, N. Parmiggiani, Maura Pilia, Fabrizio Lucarelli, Alessio Trois, A. W. Chen, M. Giusti, A. Rappoldi, F. Verrecchia, I. Donnarumma, S. Vercellone, M. Trifoglio, A. Argan, A. Pellizzoni, Andrea Bulgarelli, A. Giuliani, M. Tavani, P. W. Cattaneo, Valentina Fioretti, Paolo Giommi, Louis Antonelli, M. Cardillo, Alessio Aboudan, G. Piano, Francesco Longo, Andrea Zoli, C. Pittori, ITA, Bulgarelli, A., Fioretti, V., Parmiggiani, N., Verrecchia, F., Pittori, C., Lucarelli, F., Tavani, M., Aboudan, A., Cardillo, M., Giuliani, A., Cattaneo, P. W., Chen, A. W., Piano, G., Rappoldi, A., Baroncelli, L., Argan, A., Antonelli, L. A., Donnarumma, I., Gianotti, F., Giommi, P., Giusti, M., Longo, F., Pellizzoni, A., Pilia, M., Trifoglio, M., Trois, A., Vercellone, S., and Zoli, A.
Subjects: Physics, Active galactic nucleus, 010504 meteorology & atmospheric sciences, Spectral properties, Gamma rays: general, general [Gamma rays], Gamma ray, Astronomy and Astrophysics, Astrophysics, Surveys, Light curve, 01 natural sciences, Supernova, Pulsar, Space and Planetary Science, 0103 physical sciences, Catalogs, Catalog, Blazar, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Event reconstruction
Abstract: Aims: We present the second AGILE-GRID catalogue (2AGL) of γ-ray sources in the energy range 100 MeV-10 GeV. Methods: With respect to previous AGILE-GRID catalogues, the current 2AGL catalogue is based on the first 2.3 years of science data from the AGILE mission (the so-called pointing mode) and incorporates more data and several analysis improvements, including better calibrations at the event reconstruction level, an updated model for the Galactic diffuse γ-ray emission, a refined procedure for point-like source detection, and the inclusion of a search for extended γ-ray sources. Results: The 2AGL catalogue includes 175 high-confidence sources (above 4σ significance) with their location regions and spectral properties and a variability analysis with four-day light curves for the most significant. Relying on the error region of each source position, including systematic uncertainties, 122 sources are considered as positionally associated with known counterparts at different wavelengths or detected by other γ-ray instruments. Among the identified or associated sources, 62 are active galactic nuclei (AGNs) of the blazar class. Pulsars represent the largest Galactic source class, with 41 associated pulsars, 7 of which have detected pulsation; 8 supernova remnants and 4 high-mass X-ray binaries have also been identified. A substantial number of 2AGL sources are unidentified: for 53 sources no known counterpart is found at different wavelengths. Among these sources, we discuss a subclass of 29 AGILE-GRID-only γ-ray sources that are not present in 1FGL, 2FGL, or 3FGL catalogues; the remaining sources are unidentified in both 2AGL and 3FGL catalogues. We also present an extension of the analysis of 2AGL sources detected in the energy range 50-100 MeV. Full Tables 10 and 11 (the catalog) are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/627/A13
Published: 2019

39. A Cloud-based Architecture for the Cherenkov Telescope Array Observation Simulations: Optimization, Design, and Results

Author: A. Corina, P. Romano, Marco Landoni, Jürgen Knödlseder, S. Vercellone, Fabrizio Tavecchio, A. Bianco, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cherenkov Telescope Array, Workstation, Real-time computing, FOS: Physical sciences, costs, Context (language use), Cloud computing, Cherenkov telescopes, 01 natural sciences, Field (computer science), VHE, law.invention, methods: numerical, law, 0103 physical sciences, cloud, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Physics, methods: statistical, IACT techniques, 010308 nuclear & particles physics, business.industry, Astronomy and Astrophysics, methods: data analysis, Task (computing), Cloud computing architecture, Orders of magnitude (time), Space and Planetary Science, Astrophysics - Instrumentation and Methods for Astrophysics, business, on-line
Abstract: Simulating and analysing detailed observations of astrophysical sources for very high energy (VHE) experiments, like the Cherenkov Telescope Array (CTA), can be a demanding task especially in terms of CPU consumption and required storage. In this context, we propose an innovative cloud computing architecture based on Amazon Web Services (AWS) aiming to decrease the amount of time required to simulate and analyse a given field by distributing the workload and exploiting the large computational power offered by AWS. We detail how the various services offered by the Amazon online platform are jointly used in our architecture and we report a comparison of the execution times required for simulating observations of a test source with the CTA, by a single machine and the cloud-based approach. We find that, by using AWS, we can run our simulations more than 2 orders of magnitude faster than by using a general purpose workstation for the same cost. We suggest to consider this method when observations need to be simulated, analysed, and concluded within short timescales., Comment: Accepted for publication in Astrophysical Journal Supplement (ApJS)
Published: 2019
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40. Mapping the narrow-line Seyfert 1 galaxy 1H 0323+342

Author: Luigi Foschini, Marco Berton, V. Braito, P. Romano, S. Vercellone, Stefano Ciroi, ITA, INAF—Osservatorio Astronomico di Brera, University of Padova, Metsähovi Radio Observatory, Aalto-yliopisto, and Aalto University
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), lcsh:QC793-793.5, Seyfert galaxies, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, lcsh:Elementary particle physics, General Physics and Astronomy, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, TheoryofComputation_MATHEMATICALLOGICANDFORMALLANGUAGES, Astrophysical jet, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, relativistic jets, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract: Taking advantage of the most recent measurements by means of high-resolution radio observations and other multiwavelength campaigns, it is possible to elaborate a detailed map of the narrow-line Seyfert 1 Galaxy 1H 0323+342. This map will open the possibility of intriguing hypotheses about the generation of high-energy gamma rays in the narrow-line region., Comment: 13 pages, 2 figures, 3 tables. Accepted for publication on Universe (MDPI)
Published: 2019

41. Monte Carlo studies for the optimisation of the Cherenkov Telescope Array layout

Author: Katsuaki Asano, Rodrigo Guedes Lang, M. Cieślar, Nicholas F. H Tothill, Gianpiero Tagliaferri, O. Le Blanc, M. Vazquez Acosta, Nicola Giglietto, S. Mangano, Julien Lefaucheur, Tatsuo Yoshida, D. de Martino, Martin Pohl, A. Shalchi, Y. Renier, B. Biasuzzi, T. B. Humensky, E. Fiandrini, Andreas Quirrenbach, Abelardo Moralejo, Carla Aramo, Vincenzo Rizi, J. Knapp, A. Pagliaro, Andrea Santangelo, Michael Punch, Andreas Specovius, A. M. Lopez, P. Peñil Del Campo, Henry Przybilski, J.-P. Lenain, Agnieszka Slowikowska, Satoshi Fukami, M. H. Grondin, S. Schlenstedt, Marek Nikolajuk, F. Schüssler, Maria Concetta Maccarone, Michael Zacharias, Francesco Giordano, T. Suomijärvi, Lorenzo Amati, J. Becker Tjus, Maxim V. Barkov, H. Prokoph, F.G. Saturni, R. J. White, Nu. Komin, María Isabel Bernardos, M. Orienti, Denis Bastieri, Justin Vandenbroucke, P. Vallania, Diego Falceta-Gonçalves, L. Tibaldo, A. Burtovoi, A. Viana, Takanori Yoshikoshi, Roberto Aloisio, Soebur Razzaque, M. Valentino, P. Da Vela, Pol Bordas, Francesco Longo, N. Otte, V. La Parola, E. O. Angüner, Marco Berton, Elina Lindfors, Salvo Scuderi, Hiroyasu Tajima, M. Prouza, E. Mach, P. Goldoni, C. Alispach, M. I. Martínez, Miroslav Pech, Kai Brügge, G. Vasileiadis, A. Nagai, A. Brill, Dusan Mandat, Geoff Romeo, M. Marculewicz, Cameron B Rulten, Fuyuki Tokanai, Luis Ángel Tejedor, Thomas Lohse, Anderson Caproni, Karol Seweryn, G. Bonnoli, D. Ninci, G. Pareschi, Stefan Kimeswenger, I. Sadeh, Łukasz Stawarz, M. Nöthe, Daniel Mazin, Ruben Alfaro, G. Busetto, Massimo Persic, A. Berti, G. Sironi, Pavel Horvath, Włodek Kluźniak, Pietro Bruno, Petr Travnicek, Daniel Kerszberg, M. Hayashida, Tomasz Szepieniec, A. Rugliancich, Marina Manganaro, Y. Ohtani, Samuel Timothy Spencer, L. Di Venere, S. Karkar, M. Füßling, E. de Oña Wilhelmi, Louis Antonelli, M. Lemoine-Goumard, Benjamin Koch, P.-O. Petrucci, M. de Naurois, Felix Werner, S. Sakurai, J. J. Rodríguez Vázquez, Petr Janecek, L. Dangeon, G. Fontaine, Alison Mitchell, Maria Magdalena González, Francesco Dazzi, Philip Kaaret, Reinaldo Santos-Lima, F. Di Pierro, Tomislav Terzić, Grzegorz Kowal, Stefan Wagner, R. A. Cameron, G. S. Varner, M. Roncadelli, Wystan Benbow, C. Bonavolontà, David Kieda, M. A. Leigui de Oliveira, Ullrich Schwanke, Y. Iwamura, K. Sedlaczek, R. C. Shellard, Q. Feng, David A. Williams, A. De Angelis, T. Nagayoshi, P. Sangiorgi, I. A. Minaya, Etienne Lyard, Juan Abel Barrio, B. De Lotto, S. Nozaki, J. Gironnet, L. Mohrmann, Oscar Blanch, Marcello Giroletti, Jean-Luc Meunier, Valentina Fioretti, S. Masuda, V. Vagelli, Rodolfo Canestrari, L. Freixas Coromina, M. Palatka, T. Di Girolamo, Vincenzo Testa, Tsuguya Naito, J. Becerra González, R. Alves Batista, Samo Stanič, S. D. Vergani, Lorenzo Bellizzi, Catherine Boisson, Olivier Hervet, P. Cumani, Konstancja Satalecka, Stefan Funk, Michele Doro, Pedro L. Luque-Escamilla, P. Romano, E. Fedorova, Carlo Vigorito, M. Zavrtanik, Markus Gaug, Stanislav Stefanik, R. J. García López, F. de Palma, V. Beshley, T.R.N. Ekoume, Enrico Congiu, Pierre Brun, Manuela Mallamaci, Barbara Balmaverde, L. Valore, Gino Tosti, Enrico Cascone, Marek Jamrozy, V. I. Zhdanov, Gavin Rowell, Elisabetta Bissaldi, M. Fiori, M. Capalbi, J. Bregeon, Dario Hrupec, F. Toussenel, R. Paoletti, Fulvio Gianotti, Ayan Acharyya, G. Spengler, P. Majumdar, A.A. Zdziarski, A. López-Oramas, M. Mariotti, Juri Poutanen, G. Ferrand, Paweł Świerk, M. Garczarczyk, S. Rainò, Tsunefumi Mizuno, Diego F. Torres, Ciro Bigongiari, Matteo Cerruti, M. Polo, Csaba Balázs, A. Dmytriiev, T. Gasparetto, D. Dorner, A. W. Chen, Elisa Prandini, Vitalii Sliusar, Helene Sol, Rodolfo Carosi, Jonathan Biteau, Vito Conforti, G. Rodriguez Fernandez, Shanta M. Zimmer, J. M. Paredes, S. Vercellone, Jonathan Granot, Alice Donini, Antonio Stamerra, Jaime Rosado, Michael G. Burton, Bohdan Hnatyk, F. D'Ammando, D. Nosek, M. Heller, Gagik Tovmassian, N. Produit, Petr Schovanek, German Martinez, G. Pühlhofer, S. Fegan, A. Kong, G. Morlino, G. Emery, H.-S. Zechlin, Tomasz Bulik, Antonino D'Ai, Riccardo Rando, Rocco Lico, K. Pfrang, D. Hadasch, R. López-Coto, A. Vollhardt, Pankaj Kushwaha, Petar Temnikov, Emmanuel Moulin, Luca Zampieri, Michiko Ohishi, C. Maggio, V. de Souza, Q. Piel, Marc Ribó, Werner Hofmann, A. Wierzcholska, Luisa Arrabito, Gianpaolo Vettolani, J. Pérez-Romero, Paramita Barai, Sylvain Chaty, N. Parmiggiani, V. Vassiliev, K. Nishijima, D. Cauz, S. Caroff, Giuseppe Leto, J.F. Glicenstein, Maria Ionica, Eva Sciacca, A. Bonardi, Juan Carlos Rodríguez-Ramírez, Marcos Santander, H. Siejkowski, Daniela Maria Ribeiro, Ralph Bird, S. Mićanović, D. Zavrtanik, Carole Mundell, Jan Ebr, Koji Noda, Elisa Bernardini, R. Gnatyk, Pierre Jean, M. Nievas Rosillo, M. López, Olga Sergijenko, R. Walter, Oleh Petruk, M. Del Santo, D. Elsasser, Jakub Juryšek, H. Martínez-Huerta, Andreas Zech, Jose J. Gonzalez, Akira Okumura, M. Iori, A. Ghalumyan, Jacco Vink, David Gascon, Jürgen Knödlseder, Daniel Nieto, R. A. Ong, Sabrina Casanova, B. Khélifi, S. Flis, G. Galanti, H. J. Voelk, Jim Hinton, M. Will, David H. Green, Giuseppe Malaguti, B. Rudak, A. Pe'Er, J. L. Dournaux, Andrea Bulgarelli, Frank M. Rieger, A. Djannati-Ataï, F. De Frondat, Lenka Tomankova, Moritz Hütten, Osvaldo Catalano, Hidetoshi Kubo, Tarek M. Hassan, Tomohiro Inada, Farinaldo S. Queiroz, J. Kushida, Daniel Morcuende, Jose Luis Contreras, F. Salesa Greus, Juan Cortina, Andreu Sanuy, S. Vorobiov, G. Maneva, B. Vallage, N. Maxted, N. Renault-Tinacci, P. Munar, M. Seglar-Arroyo, Fabrizio Tavecchio, Z. Ou, Anatolii Zenin, T. Tam, Miroslav Hrabovsky, G. Ambrosi, Giovanni Bonanno, R. Millul, Anastasia Maria Barbano, T. Grabarczyk, J. Zorn, D. Dominis Prester, R. D. Parsons, Luis H. S. Kadowaki, Elena Amato, M. Lallena Arquillo, I. Oya, Jacek Niemiec, Gianluca Giavitto, Marita Krause, Olaf Reimer, Josep Martí, M. Perri, Maria Chernyakova, Takeshi Nakamori, E. M. de Gouveia Dal Pino, Thomas Murach, P. Cristofari, C. Delgado, Fernando Catalani, G. La Rosa, J. Alfaro, Thomas Armstrong, J. Kocot, Léa Jouvin, Markus Böttcher, Rodrigo Nemmen, J. P. Amans, Utane Sawangwit, Y. Kobayashi, Hidetoshi Sano, D. Jankowsky, Heide Costantini, F. Arqueros, B. Bertucci, Sebastian Diebold, L. P. Taylor, Konstantinos N. Gourgouliatos, A. Fiasson, Miroslav Filipovic, R. Moderski, T. Stolarczyk, B. Patricelli, H. Ashkar, Alessandro Costa, Jonathan Blazek, C. Trichard, M. Vecchi, T. Greenshaw, A. Morselli, V. Vitale, A. M. Brown, S. M. Colak, Lili Yang, C. Díaz, J. Rico, P. Caraveo, S. Loporchio, Orel Gueta, Daniele Gaggero, V. De Caprio, R. Wischnewski, A. Sillanpää, C. J. Todero Peixoto, Takashi Saito, I. Agudo, Yasuo Fukui, Roberto Capuzzo-Dolcetta, F. Cassol, Manuel Meyer, Reiko Orito, G. Umana, M. V. Fonseca, U. Barres de Almeida, Saverio Lombardi, D. della Volpe, Giancarlo Cusumano, M. Ostrowski, T. Montaruli, L. Tosti, Garret Cotter, Konrad Bernlöhr, Reshmi Mukherjee, Fabio Iocco, M. Palatiello, Jonathan S. Lapington, U. Straumann, R. de Cássia dos Anjos, Matteo Balbo, Lab Saha, N. Hiroshima, G. Chiaro, D. Tonev, Ermanno Pietropaolo, Atreyee Sinha, Ministerio de Ciencia e Innovación (España), European Commission, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Research unit Astroparticle Physics, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Acharyya, A., Agudo, I., Anguner, E. O., Alfaro, R., Alfaro, J., Alispach, C., Aloisio, R., Alves Batista, R., Amans, J. -P., Amati, L., Amato, E., Ambrosi, G., Antonelli, L. A., Aramo, C., Armstrong, T., Arqueros, F., Arrabito, L., Asano, K., Ashkar, H., Balazs, C., Balbo, M., Balmaverde, B., Barai, P., Barbano, A., Barkov, M., Barres de Almeida, U., Barrio, J. A., Bastieri, D., Becerra Gonzalez, J., Becker Tjus, J., Bellizzi, L., Benbow, W., Bernardini, E., Bernardos, M. I., Bernlohr, K., Berti, A., Berton, M., Bertucci, B., Beshley, V., Biasuzzi, B., Bigongiari, C., Bird, R., Bissaldi, E., Biteau, J., Blanch, O., Blazek, J., Boisson, C., Bonanno, G., Bonardi, A., Bonavolonta, C., Bonnoli, G., Bordas, P., Bottcher, M., Bregeon, J., Brill, A., Brown, A. M., Brugge, K., Brun, P., Bruno, P., Bulgarelli, A., Bulik, T., Burton, M., Burtovoi, A., Busetto, G., Cameron, R., Canestrari, R., Capalbi, M., Caproni, A., Capuzzo-Dolcetta, R., Caraveo, P., Caroff, S., Carosi, R., Casanova, S., Cascone, E., Cassol, F., Catalani, F., Catalano, O., Cauz, D., Cerruti, M., Chaty, S., Chen, A., Chernyakova, M., Chiaro, G., Cieslar, M., Colak, S. M., Conforti, V., Congiu, E., Contreras, J. L., Cortina, J., Costa, A., Costantini, H., Cotter, G., Cristofari, P., Cumani, P., Cusumano, G., D'Ai, A., D'Ammando, F., Dangeon, L., Da Vela, P., Dazzi, F., De Angelis, A., De Caprio, V., de Cassia dos Anjos, R., De Frondat, F., de Gouveia Dal Pino, E. M., De Lotto, B., De Martino, D., de Naurois, M., de Ona Wilhelmi, E., de Palma, F., de Souza, V., Del Santo, M., Delgado, C., della Volpe, D., Di Girolamo, T., Di Pierro, F., Di Venere, L., Diaz, C., Diebold, S., Djannati-Atai, A., Dmytriiev, A., Dominis Prester, D., Donini, A., Dorner, D., Doro, M., Dournaux, J. -L., Ebr, J., Ekoume, T. R. N., Elsasser, D., Emery, G., Falceta-Goncalves, D., Fedorova, E., Fegan, S., Feng, Q., Ferrand, G., Fiandrini, E., Fiasson, A., Filipovic, M., Fioretti, V., Fiori, M., Flis, S., Fonseca, M. V., Fontaine, G., Freixas Coromina, L., Fukami, S., Fukui, Y., Funk, S., Fussling, M., Gaggero, D., Galanti, G., Garcia Lopez, R. J., Garczarczyk, M., Gascon, D., Gasparetto, T., Gaug, M., Ghalumyan, A., Gianotti, F., Giavitto, G., Giglietto, N., Giordano, F., Giroletti, M., Gironnet, J., Glicenstein, J. -F., Gnatyk, R., Goldoni, P., Gonzalez, J. M., Gonzalez, M. M., Gourgouliatos, K. N., Grabarczyk, T., Granot, J., Green, D., Greenshaw, T., Grondin, M. -H., Gueta, O., Hadasch, D., Hassan, T., Hayashida, M., Heller, M., Hervet, O., Hinton, J., Hiroshima, N., Hnatyk, B., Hofmann, W., Horvath, P., Hrabovsky, M., Hrupec, D., Humensky, T. B., Hutten, M., Inada, T., Iocco, F., Ionica, M., Iori, M., Iwamura, Y., Jamrozy, M., Janecek, P., Jankowsky, D., Jean, P., Jouvin, L., Jurysek, J., Kaaret, P., Kadowaki, L. H. S., Karkar, S., Kerszberg, D., Khelifi, B., Kieda, D., Kimeswenger, S., Kluzniak, W., Knapp, J., Knodlseder, J., Kobayashi, Y., Koch, B., Kocot, J., Komin, N., Kong, A., Kowal, G., Krause, M., Kubo, H., Kushida, J., Kushwaha, P., La Parola, V., La Rosa, G., Lallena Arquillo, M., Lang, R. G., Lapington, J., Le Blanc, O., Lefaucheur, J., Leigui de Oliveira, M. A., Lemoine-Goumard, M., Lenain, J. -P., Leto, G., Lico, R., Lindfors, E., Lohse, T., Lombardi, S., Longo, F., Lopez, A., Lopez, M., Lopez-Oramas, A., Lopez-Coto, R., Loporchio, S., Luque-Escamilla, P. L., Lyard, E., Maccarone, M. C., Mach, E., Maggio, C., Majumdar, P., Malaguti, G., Mallamaci, M., Mandat, D., Maneva, G., Manganaro, M., Mangano, S., Marculewicz, M., Mariotti, M., Marti, J., Martinez, M., Martinez, G., Martinez-Huerta, H., Masuda, S., Maxted, N., Mazin, D., Meunier, J. -L., Meyer, M., Micanovic, S., Millul, R., Minaya, I. A., Mitchell, A., Mizuno, T., Moderski, R., Mohrmann, L., Montaruli, T., Moralejo, A., Morcuende, D., Morlino, G., Morselli, A., Moulin, E., Mukherjee, R., Munar, P., Mundell, C., Murach, T., Nagai, A., Nagayoshi, T., Naito, T., Nakamori, T., Nemmen, R., Niemiec, J., Nieto, D., Nievas Rosillo, M., Nikolajuk, M., Ninci, D., Nishijima, K., Noda, K., Nosek, D., Nothe, M., Nozaki, S., Ohishi, M., Ohtani, Y., Okumura, A., Ong, R. A., Orienti, M., Orito, R., Ostrowski, M., Otte, N., Ou, Z., Oya, I., Pagliaro, A., Palatiello, M., Palatka, M., Paoletti, R., Paredes, J. M., Pareschi, G., Parmiggiani, N., Parsons, R. D., Patricelli, B., Pe'Er, A., Pech, M., Penil Del Campo, P., Perez-Romero, J., Perri, M., Persic, M., Petrucci, P. -O., Petruk, O., Pfrang, K., Piel, Q., Pietropaolo, E., Pohl, M., Polo, M., Poutanen, J., Prandini, E., Produit, N., Prokoph, H., Prouza, M., Przybilski, H., Puhlhofer, G., Punch, M., Queiroz, F., Quirrenbach, A., Raino, S., Rando, R., Razzaque, S., Reimer, O., Renault-Tinacci, N., Renier, Y., Ribeiro, D., Ribo, M., Rico, J., Rieger, F., Rizi, V., Rodriguez Fernandez, G., Rodriguez-Ramirez, J. C., Rodri-guez Vazquez, J. J., Romano, P., Romeo, G., Roncadelli, M., Rosado, J., Rowell, G., Rudak, B., Rugliancich, A., Rulten, C., Sadeh, I., Saha, L., Saito, T., Sakurai, S., Salesa Greus, F., Sangiorgi, P., Sano, H., Santander, M., Santangelo, A., Santos-Lima, R., Sanuy, A., Satalecka, K., Saturni, F. G., Sawangwit, U., Schlenstedt, S., Schovanek, P., Schussler, F., Schwanke, U., Sciacca, E., Scuderi, S., Sedlaczek, K., Seglar-Arroyo, M., Sergijenko, O., Seweryn, K., Shalchi, A., Shellard, R. C., Siejkowski, H., Sillanpaa, A., Sinha, A., Sironi, G., Sliusar, V., Slowikowska, A., Sol, H., Specovius, A., Spencer, S., Spengler, G., Stamerra, A., Stanic, S., Stawarz, L., Stefanik, S., Stolarczyk, T., Straumann, U., Suomijarvi, T., Swierk, P., Szepieniec, T., Tagliaferri, G., Tajima, H., Tam, T., Tavecchio, F., Taylor, L., Tejedor, L. A., Temnikov, P., Terzic, T., Testa, V., Tibaldo, L., Todero Peixoto, C. J., Tokanai, F., Tomankova, L., Tonev, D., Torres, D. F., Tosti, G., Tosti, L., Tothill, N., Toussenel, F., Tovmassian, G., Travnicek, P., Trichard, C., Umana, G., Vagelli, V., Valentino, M., Vallage, B., Vallania, P., Valore, L., Vandenbroucke, J., Varner, G. S., Vasileiadis, G., Vassiliev, V., Vazquez Acosta, M., Vecchi, M., Vercellone, S., Vergani, S., Vettolani, G. P., Viana, A., Vigorito, C. F., Vink, J., Vitale, V., Voelk, H., Vollhardt, A., Vorobiov, S., Wagner, S. J., Walter, R., Werner, F., White, R., Wierzcholska, A., Will, M., Williams, D. A., Wischnewski, R., Yang, L., Yoshida, T., Yoshikoshi, T., Zacharias, M., Zampieri, L., Zavrtanik, M., Zavrtanik, D., Zdziarski, A. A., Zech, A., Zechlin, H., Zenin, A., Zhdanov, V. I., Zimmer, S., Zorn, J., Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Durham University, Glorieta de la Astronomía s/n, Delegación Coyoacán, Pontificia Universidad Católica de Chile, Département de physique nucléaire et corpusculaire, Università degli Studi dell'Aquila and Gran Sasso Science Institute, Universidade de São Paulo (USP), PSL Research University, INAF - Osservatorio di astrofisica e scienza dello spazio di Bologna, INAF - Osservatorio Astrofisico di Arcetri, INFN Sezione di Perugia, Universitá degli Studi di Perugia, INAF - Osservatorio Astronomico di Roma, INFN Sezione di Napoli, University of Oxford, Universidad Complutense de Madrid, CNRS/IN2P3, University of Tokyo, Monash University, University of Geneva, INAF - Osservatorio Astronomico di Brera, Institute of Physical and Chemical Research, Centro Brasileiro de Pesquisas Físicas, INFN Sezione di Padova and Universitá degli Studi di Padova, Universidad de La Laguna, Ruhr-Universität Bochum, Harvard-Smithsonian Center for Astrophysics, Max-Planck-Institut für Kernphysik, INFN Sezione di Torino, Pidstryhach Institute for Applied Problems in Mechanics and Mathematics NASU, Université Paris-Saclay, University of California, INFN Sezione di Bari and Politecnico di Bari, The Barcelona Institute of Science and Technology, Institute of Physics of the Czech Academy of Sciences, INAF - Osservatorio Astrofisico di Catania, Radboud University Nijmegen, Dipartimento di Scienze Fisiche, IEEC-UB, North-West University, Columbia University, TU Dortmund University, University of Warsaw, Armagh Observatory and Planetarium, Stanford University, INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo, Núcleo de Astrofísica Teórica (NAT/UCS), INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano, INFN Sezione di Pisa, Polish Academy of Sciences, INAF - Osservatorio Astronomico di Capodimonte, INFN Sezione di Trieste and Università degli Studi di Udine, University of the Witwatersrand, Dublin City University, CIEMAT, CPPM, INAF - Istituto di Radioastronomia, Cherenkov Telescope Array Observatory, Universidade Federal do Paraná (UFPR), Université Paris-Saclay), CSIC), Institut d'Estudis Espacials de Catalunya (IEEC), Institució Catalana de Recerca i Estudis Avançats (ICREA) Barcelona, INFN Sezione di Bari and Università degli Studi di Bari, Universität Tübingen, Obs de Paris, University of Rijeka, Universität Würzburg, LPNHE, Astronomical Observatory of Taras Shevchenko National University of Kyiv, Western Sydney University, INAF - Osservatorio Astronomico di Padova, Deutsches Elektronen-Synchrotron, Nagoya University, University of Amsterdam, Universidad Autónoma de Madrid, INFN Sezione di Trieste and Università degli Studi di Trieste, Universitat Autónoma de Barcelona, Yerevan Physics Institute, Universidad Andrés Bello UNAB, Academic Computer Centre CYFRONET AGH, The Open University of Israel, Max-Planck-Institut für Physik, Oliver Lodge Laboratory, UMR 5797, Konan University, KEK (High Energy Accelerator Research Organization), RCPTM, Josip Juraj Strossmayer University of Osijek, Universidade Estadual Paulista (Unesp), INFN Sezione di Roma, Jagiellonian University, Physikalisches Institut, Université Paul Sabatier, University of Iowa, Leopold-Franzens-Universität, Kyoto University, Tokai University, University of Leicester, Universidade Federal do ABC (UFABC), University of Turku, Humboldt University Berlin, Universidad de Jaén, Saha Institute of Nuclear Physics, Bulgarian Academy of Sciences, Faculty of Physics, University of New South Wales, Universität Zürich, Hiroshima University, INFN Sezione di Roma Tor Vergata, INAF - Istituto di Astrofisica e Planetologia Spaziali (IAPS), University of Bath, Saitama University, Yamanashi-Gakuin University, Yamagata University, Institute of Particle & Nuclear Physics, Tokushima University, Georgia Institute of Technology, Institut de Planétologie et d'Astrophysique de Grenoble, Univ. Savoie Mont Blanc, Universität Potsdam, Linnaeus University, Universität Heidelberg, University of Johannesburg, University of Adelaide, Tuscaloosa, National Astronomical Research Institute of Thailand, Dept of Physics and Astronomy, Nicolaus Copernicus University, University of Nova Gorica, University of Wisconsin, INAF - Osservatorio Astrofisico di Torino, University of Hawai'i at Manoa, Ibaraki University, KVI - Center for Advanced Radiation Technology, University of Utah, USA, GBR, FRA, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Angüner, E. O., Becerra González, J., Bernlöhr, K., Bonavolontá, C., Böttcher, M., Brügge, K., Cieślar, M., D’Aí, A., D’Ammando, F., de Cássia dos Anjos, R., de Oña Wilhelmi, E., Díaz, C., Djannati-Ataï, A., Elsässer, D., Füßling, M., Garcia López, R. J., González, J. M., González, M. M., Hütten, M., Khélifi, B., Kluźniak, W., Knödlseder, J., López, M., López-Coto, R., Martí, J., Martínez, M., Martínez, G., Martínez-Huerta, H., Nikołajuk, M., Nöthe, M., Pe’Er, A., Peñil Del Campo, P., Pérez-Romero, J., Pühlhofer, G., Rainò, S., Ribó, M., Rodrí-guez Vázquez, J. J., Sillanpää, A., Stanič, S., Stawarz, Ł., Świerk, P., Vázquez Acosta, M., GRAPPA (ITFA, IoP, FNWI), and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Cherenkov Telescope Array, Astronomy, Monte Carlo method, energy resolution, Monte Carlo simulations, Cherenkov telescopes, IACT technique, gamma rays, cosmic rays, 01 natural sciences, 7. Clean energy, law.invention, Observatory, law, site, Monte Carlo, 010303 astronomy & astrophysics, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, observatory, Cosmic rays, Gamma rays, Astronomy and Astrophysics, ddc:540, Física nuclear, Monte carlo studies, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, performance, FÍSICA DE ALTA ENERGIA, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, FOS: Physical sciences, energy dependence, Telescope, Optics, CTA - Abteilung Hofmann, 0103 physical sciences, Cherenkov counter: imaging, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Monte Carlo simulation, Cherenkov radiation, CTA, 010308 nuclear & particles physics, business.industry, sensitivity, Cosmic ray, Cherenkov telescope, gamma ray: VHE, business, Energy (signal processing), astro-ph.IM
Abstract: The Cherenkov Telescope Array (CTA) is the major next-generation observatory for ground-based very-high-energy gamma-ray astronomy. It will improve the sensitivity of current ground-based instruments by a factor of five to twenty, depending on the energy, greatly improving both their angular and energy resolutions over four decades in energy (from 20 GeV to 300 TeV). This achievement will be possible by using tens of imaging Cherenkov telescopes of three successive sizes. They will be arranged into two arrays, one per hemisphere, located on the La Palma island (Spain) and in Paranal (Chile). We present here the optimised and final telescope arrays for both CTA sites, as well as their foreseen performance, resulting from the analysis of three different large-scale Monte Carlo productions.© 2019, We gratefully acknowledge financial support from the following agencies and organizations: State Committee of Science of Armenia, Armenia; The Australian Research Council, Astronomy Australia Ltd, The University of Adelaide, Australian National University, Monash University, The University of New South Wales, The University of Sydney, Western Sydney University, Australia; Federal Ministry of Science, Research and Economy, and Innsbruck University, Austria; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq), Fundacao de Amparo a Pesquisa do Estado do Rio de Janeiro (FAPERJ), Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP), Ministry of Science, Technology, Innovations and Communications (MCTIC), Brasil; Ministry of Education and Science, National RI Roadmap Project D01-153/28.08.2018, Bulgaria; The Natural Sciences and Engineering Research Council of Canada and the Canadian Space Agency, Canada; CONICYT-Chile grants PFB-06, FB0821, ACT 1406, FONDECYT-Chile grants 3160153, 3150314, 1150411, 1161463, 1170171, Pontificia Universidad Catolica de Chile Vice-Rectory of Research internationalization grant under MINEDUC agreement PUC1566, Chile, Croatian Science Foundation, Rudjer Boskovic Institute, University of Osijek, University of Rijeka, University of Split, Faculty of Electrical Engineering, Mechanical Engineering and Naval Architecture, University of Zagreb, Faculty of Electrical Engineering and Computing, Croatia; Ministry of Education, Youth and Sports, MEYS LM2015046, LTT17006 and EU/MEYS CZ.02.1.01/0.0/0.0/16_013/0001403, CZ.02.1.01/0.0/0.0/17_049/0008422, Czech Republic; Ministry of Higher Education and Research, CNRS-INSU and CNRS-IN2P3, CEA-Irfu, ANR, Regional Council Ile-de France, Labex ENIGMASS, OSUG2020, P210 and OCEVU, France; Max Planck Society, BMBF, DESY, Helmholtz Association, Germany; Department of Atomic Energy, Department of Science and Technology, India; Istituto Nazionale di Astrofisica (INAF), Istituto Nazionale di Fisica Nucleare (INFN), MIUR, Istituto Nazionale di Astrofisica (INAF-OABRERA) Grant Fondazione Cariplo/Regione Lombardia ID 2014-1980/RST_ERC, Italy; ICRR, University of Tokyo, JSPS, MEXT, Japan; Netherlands Research School for Astronomy (NOVA), Netherlands Organization for Scientific Research (NWO), Netherlands; University of Oslo, Norway; Ministry of Science and Higher Education, DIR/WK/2017/12, the National Centre for Research and Development and the National Science Centre, UMO-2016/22/M/ST9/00583, Poland; Slovenian Research Agency, Slovenia, grants P1-0031, P1-0385, 10-0033, J1-9146; South African Department of Science and Technology and National Research Foundation through the South African Gamma-Ray Astronomy Programme, South Africa; MINECO National R+D+I, Severo Ochoa, Maria de Maeztu, CDTI, PAIDI, UJA, FPA2017-90566-REDC, Spain; Swedish Research Council, Royal Physiographic Society of Lund, Royal Swedish Academy of Sciences, The Swedish National Infrastructure for Computing (SNIC) at Lunarc (Lund), Sweden; Swiss National Science Foundation (SNSF), Ernest Boninchi Foundation, Switzerland; Durham University, Leverhulme Trust, Liverpool University, University of Leicester, University of Oxford, Royal Society, Science and Technology Facilities Council, UK; U.S. National Science Foundation, U.S.Department of Energy, Argonne National Laboratory, Barnard College, University of California, University of Chicago, Columbia University, Georgia Institute of Technology, Institute for Nuclear and Particle Astrophysics (INPAC-MRPI program), Iowa State University, the Smithsonian Institution, Washington University McDonnell Center for the Space Sciences, The University of Wisconsin and the Wisconsin Alumni Research Foundation, USA. The research leading to these results has received funding from the European Union's Seventh Framework Programme (FP7/2007-2013) under grant agreements no 262053 and no 317446. This project is receiving funding from the European Union's Horizon 2020 research and innovation programs under agreement no 676134.
Published: 2019
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42. Swift Observations of Mrk 421 in Selected Epochs. III. Extreme X-Ray Timing/Spectral Properties and Multiwavelength Lognormality during 2015 December–2018 April

Author: Bidzina Kapanadze, A. Gurchumelia, M. F. Aller, Oleg Kharshiladze, Hugh D. Aller, Philip A. Hughes, P. Romano, S. Vercellone, and Daniela Dorner
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Swift, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Spectral properties, X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, computer, computer.programming_language
Abstract: We present the results from the timing and spectral study of Mrk\,421 based mainly on the \emph{Swift} data in the X-ray energy range obtained during the time interval 2015\,December--2018\,April. The most extreme X-ray flaring activity on the long-term, daily and intraday timescales was observed during the 2-month period which started in 2017\,December when the 0.3--10\,keV flux exceeded a level of 5$\times$10$^{-9}$erg\,cm$^{-2}$s$^{-1}$, recorded only twice previously. While the TeV-band and X-ray variabilities mostly were correlated, the source often varied in a complex manner in the MeV--GeV and radio--UV energy ranges, indicating that the multifrequency emission of Mrk\,421 could not be always generated in a single zone. The longer-term flares at X-rays and $\gamma$-rays showed a lognormal character, possibly indicating a variability imprint of the accretion disk onto the jet. A vast majority of the 0.3--10\,keV spectra were consistent with the log-parabolic model, showing relatively low spectral curvature and correlations between the different spectral parameters, predicted in the case of the first and second-order Fermi processes. The position of the synchrotron spectral energy distribution (SED) peak showed an extreme variability on diverse timescales between the energies $E_{\rm p}$$$15\,keV, with 15\% of the spectra peaking at hard X-rays and was related to the peak height as $S_{\rm p}$$\varpropto$$E^{\alpha}_{\rm p}$ with $\alpha$$\sim$0.6, which is expected for the transition from Kraichnan-type turbulence into the \textquotedblleft hard-sphere\textquotedblright~ one. The 0.3--300\,GeV spectra showed the features of the hadronic contribution, jet-star interaction and upscatter in the Klein-Nishina regime in different time intervals., Comment: Accept
Published: 2020
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43. The TeV blazar 1ES 1959+650 - a short review

Author: D. Dorner, L. Tabagari, Bidzina Kapanadze, P. Romano, and S. Vercellone
Subjects: Physics, Astrophysics, Blazar
Published: 2018
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44. Simulations of gamma-ray narrow-line Seyfert 1 galaxies with the Cherenkov Telescope Array

Author: Jurgen Knoedlseder, P. Romano, S. Vercellone, Fabrizio Tavecchio, Luigi Foschini, Marco Landoni, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), CTA Consortium, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Cherenkov Telescope Array, Galaxy, law.invention, Black hole, Telescope, symbols.namesake, Observatory, law, Eddington luminosity, symbols, Blazar, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Cherenkov radiation
Abstract: International audience; Gamma-ray emitting narrow-line Seyfert 1 ($\gamma$-NLSy1) galaxies are jetted sources hosting a relatively low-mass black hole (10$^6$--10$^8$ $M_{\odot}$) which accretes close to the Eddington limit. $\gamma$-NLSy1 galaxies show flux and spectral variability in the gamma-ray energy band and radio properties similar to those of blazars, which indicate the presence of a relativistic jet. These properties make them interesting to investigate with the Cherenkov Telescope Array (CTA), the next-generation ground-based gamma-ray observatory. CTA will cover the 20 GeV--300 TeV energy range, with an improvement in average differential sensitivity by a factor 5--20 with respect to the current imaging atmospheric Cherenkov telescope arrays. For transients/flaring events (timescales of $\sim 1$ day or shorter) CTA will be about two orders of magnitude more sensitive with respect to Fermi-LAT at the overlapping energy of 25 GeV, allowing an unprecedented opportunity to investigate flaring $\gamma$-NLSy1 galaxies. We present preliminary results obtained by simulating the prototypical $\gamma$-NLSy1 galaxy, PMN~J0948$+$0022, by means of the CTA public {\tt ctools} software and the public instrument response files,investigating its possible detection and spectral properties, taking into account the effect of both the extra-galactic background light and intrinsic absorption components.
Published: 2018
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45. Gamma-ray blazars: The view from AGILE

Author: Filippo D'Ammando, F. Longo, P. Romano, Marco Tavani, Andrea Bulgarelli, S. Vercellone, Luigi Pacciani, C. M. Raiteri, Stefano Covino, V. Vittorini, E. Striani, Hans A. Krimm, A. W. Chen, M. Villata, G. Pucella, I. Donnarumma, A. Giuliani, F., D'Ammando, A., Bulgarelli, A. W., Chen, I., Donnarumma, A., Giuliani, Longo, Francesco, L., Pacciani, G., Pucella, E., Striani, M., Tavani, S., Vercellone, V., Vittorini, S., Covino, H. A., Krimm, C. M., Raiteri, P., Romano, M., Villata, DAmmando F, Bulgarelli A, Chen AW, Donnarumma I, Giuliani A, Longo F, Pacciani L, Pucella G, Striani E, Tavani M, Vercellone S, Vittorini V, Covino S, Krimm HA, Raiteri CM, Romano P, and Villata M
Subjects: Atmospheric Science, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, FOS: Physical sciences, Aerospace Engineering, Astrophysics, High Energy Gamma-ray Astronomy, law.invention, Telescope, Gamma-ray sources, Quasars, Active galactic nuclei, BL Lac objects, Blazars, law, MAGIC (telescope), Blazar, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Detector, Gamma ray, Astronomy, Active Galactic Nuclei, Astronomy and Astrophysics, Quasar, Geophysics, Space and Planetary Science, General Earth and Planetary Sciences, Satellite, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: During the first 3 years of operation the Gamma-Ray Imaging Detector onboard the AGILE satellite detected several blazars in a high gamma-ray activity: 3C 279, 3C 454.3, PKS 1510-089, S5 0716+714, 3C 273, W Comae, Mrk 421, PKS 0537-441 and 4C +21.35. Thanks to the rapid dissemination of our alerts, we were able to obtain multiwavelength data from other observatories such as Spitzer, Swift, RXTE, Suzaku, INTEGRAL, MAGIC, VERITAS, and ARGO as well as radio-to-optical coverage by means of the GASP Project of the WEBT and the REM Telescope. This large multifrequency coverage gave us the opportunity to study the variability correlations between the emission at different frequencies and to obtain simultaneous spectral energy distributions of these sources from radio to gamma-ray energy bands, investigating the different mechanisms responsible for their emission and uncovering in some cases a more complex behaviour with respect to the standard models. We present a review of the most interesting AGILE results on these gamma-ray blazars and their multifrequency data., Comment: 25 pages, 10 figures, accepted for publication on Advances in Space Research. Talk presented at the 38th COSPAR Scientific Assembly (Bremen, Germany; July 18-25, 2010)
Published: 2011
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46. Preliminary results on TeV sources search with AGILE

Author: F. Perotti, E. Striani, Claudio Labanti, Sandro Mereghetti, C. Pittori, M. Trifoglio, Marco Feroci, Luigi Pacciani, A. Argan, Andrea Bulgarelli, L. Salotti, Enrico Costa, Elena Moretti, G. De Paris, Francesco Lazzarotto, S. Colafrancesco, A. Rappoldi, Francesco Longo, Geiland Porrovecchio, Ennio Morelli, P. Picozza, V. Cocco, A. W. Chen, Massimo Rapisarda, A. Pellizzoni, S. Vercellone, P. Giommi, Arnaud Ferrari, G. Di Cocco, Marco Tavani, D. Zanello, E. Del Monte, I. Donnarumma, S. Sabatini, V. Vittorini, Y. Evangelista, M. Prest, Martino Marisaldi, A. Zambra, E. Vallazza, A. Giuliani, F. Boffelli, T. Froysland, M. Fiorini, Paolo Soffitta, P. A. Caraveo, M. Mastropietro, Guido Barbiellini, P. Santolamazza, M. Galli, F. Verrecchia, Alda Rubini, P. W. Cattaneo, I. Lapshov, F. Fuschino, Paolo Lipari, A. Morselli, F. D’ Ammando, G. Piano, M. Pilia, G. Pucella, Fulvio Gianotti, Alessio Trois, A., Rappoldi, Longo, Francesco, A., Argan, G., Barbiellini, F., Boffelli, A., Bulgarelli, P., Caraveo, P. W., Cattaneo, A. W., Chen, V., Cocco, S., Colafrancesco, E., Costa, Ammando, F., Paris, G., Monte, E., Cocco, G., I., Donnarumma, Y., Evangelista, A., Ferrari, M., Feroci, M., Fiorini, T., Froysland, F., Fuschino, M., Galli, F., Gianotti, P., Giommi, A., Giuliani, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, M., Marisaldi, M., Mastropietro, S., Mereghetti, E., Morelli, E., Moretti, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, G., Piano, P., Picozza, M., Pilia, C., Pittori, G., Porrovecchio, M., Prest, G., Pucella, M., Rapisarda, A., Rubini, S., Sabatini, L., Salotti, P., Santolamazza, P., Soffitta, E., Striani, M., Tavani, M., Trifoglio, A., Troi, E., Vallazza, F., Verrecchia, S., Vercellone, V., Vittorini, A., Zambra, and D., Zanello
Subjects: Physics, Very High Energy Gamma-ray Astronomy, High Energy Gamma-ray Astronomy, Nuclear and High Energy Physics, business.industry, AGILe, gamma ray sky, TeV source, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics, Sky, Milagro, Satellite, MAGIC (telescope), business, Instrumentation, Agile software development, media_common
Abstract: During its first 2 years of operation, the gamma-ray AGILE satellite almost completed a full study of the gamma-ray sky. This paper presents the preliminary results of the systematic study performed on the AGILE data to search for GeV counterparts and to derive flux upper limits of the TeV sources detected by various instruments (MAGIC, HESS, VERITAS, Cangaroo, MILAGRO, ARGO, … .).
Published: 2011
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47. The observation of gamma ray bursts and terrestrial gamma-ray flashes with AGILE

Author: Paolo Lipari, B. Preger, Francesco Longo, S. Sabatini, C. Pittori, Fulvio Gianotti, E. Vallazza, Andrea Bulgarelli, F. Fuschino, Enrico Costa, F. Verrecchia, P. Picozza, Maura Pilia, G. Piano, M. Trifoglio, S. Vercellone, I. Donnarumma, M. Prest, Alessio Trois, G. Pucella, G. Di Cocco, F. Boffelli, S. Cutini, A. W. Chen, Paolo Soffitta, M. Gallil, E. Striani, P. A. Caraveo, Y. Evangelista, Francesco Lazzarotto, P. Santolamazza, Massimo Rapisarda, F. Perotti, I. Lapshov, Giacomo Vianello, Claudio Labanti, A. Morselli, Marco Feroci, Luigi Pacciani, L. Salotti, P. W. Cattaneo, Paolo Giommi, Elena Moretti, A. Pellizzoni, Sandro Mereghetti, A. Rappoldi, A. Giuliani, Guido Barbiellini, V. Vittorini, Martino Marisaldi, L. A. Antonelli, Marco Tavani, E. Del Monte, E., Del Monte, G., Barbiellini, F., Fuschino, A., Giuliani, Longo, Francesco, M., Marisaldi, S., Mereghetti, E., Moretti, M., Trifoglio, G., Vianello, E., Costa, I., Donnarumma, Y., Evangelista, M., Feroci, M., Gallil, I., Lapshov, F., Lazzarotto, P., Lipari, L., Pacciani, M., Rapisarda, P., Soffitta, M., Tavani, S., Vercellone, S., Cutini, F., Boffelli, A., Bulgarelli, P., Caraveo, P. W., Cattaneo, A., Chen, Cocco, G., F., Gianotti, C., Labanti, A., Morselli, A., Pellizzoni, F., Perotti, G., Piano, P., Picozza, M., Pilia, M., Prest, G., Pucella, A., Rappoldi, S., Sabatini, E., Striani, A., Troi, E., Vallazza, V., Vittorini, L. A., Antonelli, C., Pittori, B., Preger, P., Santolamazza, F., Verrecchia, P., Giommi, and L., Salotti
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Nuclear and High Energy Physics, Terrestrial Gamma Ray Flashes, High-energy astronomy, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, FOS: Physical sciences, Astronomy, Field of view, AGILE, gamma ray bursts, short gamma transient, silicon tracker, Astrophysics, Statistical Confidence, Gamma-ray Bursts, Gamma-ray Burst, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, Instrumentation, Silicon microstrip detectors, Fermi Gamma-ray Space Telescope
Abstract: Since its early phases of operation, the AGILE mission is successfully observing Gamma Ray Bursts (GRBs) in the hard X-ray band with the SuperAGILE imager and in the MeV range with the Mini-Calorimeter. Up to now, three firm GRB detections were obtained above 25 MeV and some bursts were detected with lower statistical confidence in the same energy band. When a GRB is localized, either by SuperAGILE or Swift/BAT or INTEGRAL/IBIS or Fermi/GBM or IPN, inside the field of view of the Gamma Ray Imager of AGILE, a detection is searched for in the gamma ray band or an upper limit is provided. A promising result of AGILE is the detection of very short gamma ray transients, a few ms in duration and possibly identified with Terrestrial Gamma-ray Flashes. In this paper we show the current status of the observation of Gamma Ray Bursts and Terrestrial Gamma-ray Flashes with AGILE., Four pages and four figures
Published: 2011
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48. Swift Observations of Mrk 421 in Selected Epochs. I. The Spectral and Flux Variability in 2005-2008

Author: S. Kapanadze, Bidzina Kapanadze, P. Romano, S. Vercellone, Oleg Kharshiladze, Hugh D. Aller, M. F. Aller, Philip A. Hughes, L. Tabagari, and ITA
Subjects: Swift, Physics, 010308 nuclear & particles physics, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, 0103 physical sciences, Flux, Astronomy and Astrophysics, Astrophysics, 010303 astronomy & astrophysics, 01 natural sciences, computer, computer.programming_language
Abstract: We present detailed results of Swift observations of the nearby TeV-detected blazar Mrk 421, based on the rich archival data obtained during 2005 March-2008 June. The best fits of the 0.3-10 keV spectra were mainly obtained using the log-parabolic model, yielding low spectral curvatures expected in the case of the efficient stochastic acceleration of particles. During strong X-ray flares, the position of the synchrotron spectral energy distribution peak {E}{{p}} was beyond 8 keV for 41 spectra, while it sometimes was situated at the UV frequencies in quiescent states. The photon index at 1 keV exhibited a broad range, and the values a< 1.70 were observed during the strong flares, hinting at the possible presence of a jet hadronic component. The spectral parameters were correlated in some periods, expected in the framework of the first- and second-order Fermi accelerations of X-ray emitting particles, as well as in the case of turbulence spectrum. The 0.3-10 keV flux and spectral parameters sometimes showed very fast variability down to the fluctuations by 6-20% in 180-960 s, possibly related to the small-scale turbulent areas containing strongest magnetic fields. X-ray and very high-energy fluxes often showed correlated variability, although several occurrences of more complicated variability patterns are also revealed, indicating that the multifrequency emission of Mrk 421 could not be generated in a single zone.
Published: 2018

49. The Bright γ-ray Flare of 3C 279 in 2015 June: AGILE Detection and Multifrequency Follow-up Observations

Author: Alan P. Marscher, F. Verrecchia, E. N. Kopatskaya, Lorand A. Sigua, O. M. Kurtanidze, A. Morselli, Andrea Bulgarelli, M. Villata, F. Paoletti, P. W. Cattaneo, I. Donnarumma, Paolo Giommi, H. Y. Hsiao, C. Pittori, M. I. Carnerero, D. O. Mirzaqulov, Valeri M. Larionov, J. A. Acosta-Pulido, C. M. Raiteri, Sh. A. Ehgamberdiev, David Hiriart, L. V. Larionova, F. Longo, L. O. Takalo, Fabrizio Lucarelli, S. Vercellone, A. Strigachev, T. S. Grishina, V. Vittorini, Manash R. Samal, D. Carosati, Sofia O. Kurtanidze, G. A. Borman, Kari Nilsson, Givi N. Kimeridze, A. Goded, Marco Tavani, Wen Ping Chen, B. Spassov, M. Perri, S. Colafrancesco, Erika Benítez, Louis Antonelli, Svetlana G. Jorstad, D. A. Morozova, Simonetta Puccetti, Rumen Bachev, ITA, Pittori, C., Lucarelli, F., Verrecchia, F., Raiteri, C. M., Villata, M., Vittorini, V., Tavani, M., Puccetti, S., Perri, M., Donnarumma, I., Vercellone, S., Acosta-Pulido, J. A., Bachev, R., Benítez, E., Borman, G. A., Carnerero, M. I., Carosati, D., Chen, W. P., Ehgamberdiev, Sh. A., Goded, A., Grishina, T. S., Hiriart, D., Hsiao, H. Y., Jorstad, S. G., Kimeridze, G. N., Kopatskaya, E. N., Kurtanidze, O. M., Kurtanidze, S. O., Larionov, V. M., Larionova, L. V., Marscher, A. P., Mirzaqulov, D. O., Morozova, D. A., Nilsson, K., Samal, M. R., Sigua, L. A., Spassov, B., Strigachev, A., Takalo, L. O., Antonelli, L. A., Bulgarelli, A., Cattaneo, P., Colafrancesco, S., Giommi, P., Longo, F., Morselli, A., and Paoletti, and F.
Subjects: Physics, polarization, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Library science, Astronomy and Astrophysics, radiation mechanisms: non-thermal, non-thermal [radiation mechanisms], X-rays: general, 01 natural sciences, quasars: individual (3C 279), gamma rays: galaxies, Space and Planetary Science, Observatory, general [X-rays], active [galaxies], 0103 physical sciences, individual (3C 279) [quasars], Astrophysics::Solar and Stellar Astrophysics, galaxie [gamma rays], Christian ministry, 010303 astronomy & astrophysics
Abstract: We would like to acknowledge the financial support of ASI under contract to INAF:ASI 2014-049-R.0 dedicated to SSDC. Part of this work is based on archival data, software, or online services provided by the ASI SSDC. The research at Boston University was supported by National Science Foundation grant AST-1615796 and NASA Swift Guest Investigator grant 80NSSC17K0309. This research was partially supported by the Bulgarian National Science Fund of the Ministry of Education and Science under grant DN 08-1/2016. The Skinakas Observatory is a collaborative project of the University of Crete, the Foundation for Research and Technology-Hellas, and the Max-Planck-Institut fur Extraterrestrische Physik. The St. Petersburg University team acknowledges support from Russian Science Foundation grant 17-12-01029. This article is partly based on observations made with the telescope IAC80 operated by the Instituto de Astrofisica de Canarias in the Spanish Observatorio del Teide on the island of Tenerife. The IAC team acknowledges the support from the group of support astronomers and telescope operators of the Observatorio del Teide. Based (partly) on data obtained with the STELLA robotic telescopes in Tenerife, an AIP facility jointly operated by AIP and IAC. This work is partially based upon observations carried out at the Observatorio Astronomico Nacional on the Sierra San Pedro Martir (OAN-SPM), Baja California, Mexico. C.P., V.V. and M. T. also thank Professor A. Cavaliere for the insightful discussion. (INAF:ASI 2014-049-R.0 - ASI; AST-1615796 - National Science Foundation; 80NSSC17K0309 - NASA Swift Guest Investigator grant; DN 08-1/2016 - Bulgarian National Science Fund of the Ministry of Education and Science; 17-12-01029 - Russian Science Foundation)
Published: 2018

50. Calibration of AGILE-GRID with On-ground Data and Monte Carlo Simulations

Author: A. Argan, Francesco Lucarelli, Lina Quintieri, Andrea Bulgarelli, V. Cocco, M. Trifoglio, P. W. Cattaneo, L. Foggetta, M. Prest, A. Pellizzoni, A. Giuliani, F. Boffelli, N. Parmigiani, Valentina Fioretti, A. Zambra, F. D'Ammando, A. Morselli, M. Pilia, S. Sabatini, P. Valente, A. Rappoldi, C. Pittori, T. Froysland, M. Tavani, A. W. Chen, S. Vercellone, F. Longo, Bruno Buonomo, A. Trois, G. Pucella, M. Galli, F. Verrecchia, M. Cardillo, G. Mazzitelli, E. Vallazza, G. Barbiellini, S. Colafrancesco, Arnaud Ferrari, G. Piano, F. Fuschino, F. Gianotti, F. Paoletti, I. Donnarumma, Martino Marisaldi, ITA, USA, Pucella, G., Galli, M., 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., 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., Quintieri, L., Sabatini, S., Tavani, M., Trifoglio, M., Trois, A., Valente, P., Vallazza, E., Vercellone, S., Verrecchia, F., and Zambra, A.
Subjects: Physics::Instrumentation and Detectors, Calibration (statistics), astroparticle physics, instrumentation: detectors, Astrophysics::High Energy Astrophysical Phenomena, Monte Carlo method, FOS: Physical sciences, 01 natural sciences, 0103 physical sciences, Aerospace engineering, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astroparticle physics, Physics, 010308 nuclear & particles physics, business.industry, detector [instrumentation], astroparticle physic, Astronomy and Astrophysics, Astronomy and Astrophysic, Grid, Space and Planetary Science, Astrophysics - Instrumentation and Methods for Astrophysics, business, Agile software development
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., 19 page 12 figures
Published: 2018

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