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1. ASTENA: an innovative mission concept for broadband high-energy astrophysics

Author: Enrico Virgilli, Filippo Frontera, Lisa Ferro, Miguel Moita, Leo Cavazzini, Piero Rosati, Cristiano Guidorzi, Mauro Orlandini, Claudio Labanti, Ezio Caroli, Natalia Auricchio, John B. Stephen, Stefano del Sordo, and Lorenzo Amati
Published: 2022

2. The X/Gamma-ray Imaging Spectrometer (XGIS) for THESEUS and other mission opportunities

Author: Lorenzo Amati, Claudio Labanti, Sandro Mereghetti, Filippo Frontera, Riccardo Campana, Natalia Auricchio, Giuseppe Baldazzi, Pierluigi Bellutti, Giuseppe Bertuccio, Marica Branchesi, Reginald C. Butler, Maria D. Caballero-Garcia, Anna E. Camisasca, Alberto J. Castro-Tirado, Leo Cavazzini, Riccardo Ciolfi, Adriano De Rosa, Federico Evangelisti, Ruben Farinelli, Lisa Ferro, Francesco Ficorella, Mauro Fiorini, Fabio Fuschino, José L. Gasent-Blesa, Giancarlo Ghirlanda, Marco Grassi, Cristiano Guidorzi, Paul Hedderman, Irfan Kuvvetli, Giovanni La Rosa, Paolo Lorenzi, Piero Malcovati, Ezequiel Marchesini, Martino Marisaldi, Michele Melchiorri, Filippo Mele, Malgorzata Mikhalska, Mauro Orlandini, Piotr Orleanski, Soren M. Pedersen, Raffaele Pizzolla, Alexandre Rachevski, Irina Rashevskaya, Piero Rosati, Victor Reglero, Samuele Ronchini, Andrea Santangelo, Ruben Salvaterra, Paolo Sarra, Francesca Sortino, Giuseppe Sottile, Giulia Stratta, Stefano Squerzanti, John B. Stephen, Chris Tenzer, Luca Terenzi, Alessio Trois, Andrea Vacchi, Enrico Virgilli, Angela Volpe, Marek Winkler, Gianluigi Zampa, Nicola Zampa, Andrzej Zdziarski, Ministerio de Ciencia e Innovación (España), den Herder, Jan-Willem A., Nikzad, Shouleh, and Nakazawa, Kazuhiro
Subjects: bursts [Gamma-ray], future missions [High-energy astrophysics], Space astrophysics: X and gamma-ray detectors, High-energy astrophysics: future missions, Gamma-ray:bursts, X and gamma-ray detectors [Space astrophysics], Time-domain astronomy, X-rays: transients, Gamma-ray bursts, transients [X-rays], Multi-messenger astrophysics
Abstract: Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray (2022), Montreal, Jul 17-22, 2022.--Proceedings of SPIE - The International Society for Optical Engineering vol. 12181 Article number 1218126.-- Full list of authors: Amati, Lorenzo; Labanti, Claudio; Mereghetti, Sandro; Frontera, Filippo; Campana, Riccardo; Auricchio, Natalia; Baldazzi, Giuseppe; Bellutti, Pierluigi; Bertuccio, Giuseppe; Branchesi, Marica; Butler, Reginald C.; Caballero-Garcia, Maria D.; Camisasca, Anna E.; Castro-Tirado, Alberto J.; Cavazzini, Leo; Ciolfi, Riccardo; De Rosa, Adriano; Evangelisti, Federico; Farinelli, Ruben; Ferro, Lisa; Ficorella, Francesco; Fiorini, Mauro; Fuschino, Fabio; Gasent-Blesa, Jose L.; Ghirlanda, Giancarlo; Grassi, Marco; Guidorzi, Cristiano; Hedderman, Paul; Kuvvetli, Irfan; La Rosa, Giovanni; Lorenzi, Paolo; Malcovati, Piero; Marchesini, Ezequiel; Marisaldi, Martino; Melchiorri, Michele; Mele, Filippo; Mikhalska, Malgorzata; Orlandini, Mauro; Orleanski, Piotr; Pedersen, Soren M.; Pizzolla, Raffaele; Rachevski, Alexandre; Rashevskaya, Irina; Rosati, Piero; Reglero, Victor; Ronchini, Samuele; Santangelo, Andrea; Salvaterra, Ruben; Sarra, Paolo; Sortino, Francesca; Sottile, Giuseppe; Stratta, Giulia; Squerzanti, Stefano; Stephen, John B.; Tenzer, Chris; Terenzi, Luca; Trois, Alessio; Vacchi, Andrea; Virgilli, Enrico; Volpe, Angela; Winkler, Marek; Zampa, Gianluigi; Zampa, Nicola; Zdziarski, Andrzej, We describe the science case, design and expected performances of the X/Gamma-ray Imaging Spectrometer (XGIS), a GRB and transients monitor developed and studied for the THESEUS mission project, capable of covering an exceptionally wide energy band (2 keV – 10 MeV), with imaging capabilities and location accuracy, With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709
Published: 2022

3. Phase-dependent Evolution within the Large Luminosity Range of 1A 0535+262 Observed by Insight-HXMT during 2020 Giant Outburst

Author: Ling-Da Kong, Shu Zhang, Long Ji, Victor Doroshenko, Andrea Santangelo, Mauro Orlandini, Filippo Frontera, Jian Li, Yu-Peng Chen, Peng-Ju Wang, Zhi Chang, Jin-Lu Qu, Shuang-Nan Zhang, ITA, DEU, and CHN
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 have performed phase-resolved spectral analysis of the accreting pulsar 1A 0535+262 based on observations of Insight-HXMT during the 2020 type II outburst of the source. We focus on the two-dimensional dependence of the cyclotron resonance scattering features (CRSFs) along the outburst time and at different phases. The fundamental CRSF line (f-CRSF) shows different time- and phase-dependent behaviors. At higher luminosity, the phase profile of the f-CRSF energy changes from a single peak to double peaks, with the transition occurring at MJD 59185. On the contrary, the first harmonic CRSF (first CRSF) at ∼100 keV is only detected within a narrow phase range (0.8−1.0) accompanied by a shallow f-CRSF line. Based on these results, we speculate that when the source enters the supercritical regime, the higher accretion column height can significantly enhance the harmonic line at a narrow phase through an “anti-pencil” beam at a higher energy band. At the same time, it will also affect the behavior of the fundamental line.
Published: 2022

4. A deep study of the high–energy transient sky

Author: R. M. Curado da Silva, Raffaella Margutti, Søren Brandt, Elena Pian, F. Fuschino, Ezio Caroli, Lorenzo Amati, Luciano Burderi, C. G. Mundell, R. Mochkovitch, F. Frontera, Piero Rosati, Enrico Bozzo, C. Guidorzi, G. Ghirlanda, Chris L. Fryer, T. Di Salvo, Shiho Kobayashi, Mauro Orlandini, Riccardo Campana, M. Della Valle, Riccardo Ciolfi, John B. Stephen, Claudio Labanti, P. Laurent, Gabriele Ghisellini, R. Martone, M. Marongiu, Enrico Virgilli, G. Stratta, Università degli Studi di Ferrara, Ministerio de Economía y Competitividad (España), European Commission, Agenzia Spaziale Italiana, 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 d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Guidorzi C., Frontera F., Ghirlanda G., Stratta G., Mundell C.G., Virgilli E., Rosati P., Caroli E., Amati L., Pian E., Kobayashi S., Ghisellini G., Fryer C., Valle M.D., Margutti R., Marongiu M., Martone R., Campana R., Fuschino F., Labanti C., Orlandini M., Stephen J.B., Brandt S., Silva R.C., Laurent P., Mochkovitch R., Bozzo E., Ciolfi R., Burderi L., and Di Salvo T.
Subjects: Electromagnetic spectrum, ESA voyage 2050, High-energy transient sky, Multi-messenger astrophysics, Space mission concept, X–/γ–ray polarimetry, X–/γ–ray telescopes, 01 natural sciences, 7. Clean energy, law.invention, Settore FIS/05 - Astronomia E Astrofisica, law, Nuclear astrophysics, optical, 010303 astronomy & astrophysics, media_common, Physics, density, Strong gravity, Astrophysics::Instrumentation and Methods for Astrophysics, nucleosynthesis, imaging, Particle acceleration, Neutrino, burst, particle, lens, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, interferometer, Telescope, 0103 physical sciences, TeV, equation of state, polarization, 010308 nuclear & particles physics, Gravitational wave, nucleus, gravitational radiation, Ambientale, Astronomy, Astronomy and Astrophysics, acceleration, sensitivity, Universe, monitoring, electromagnetic, angular resolution, [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, gamma ray, gravitation, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: This is an open access article. This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article's Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article's Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder., The coming decades will establish the exploration of the gravitational wave (GW) Universe over a broad frequency range by ground and space interferometers. Meanwhile, wide-field, high-cadence and sensitive surveys will span the electromagnetic spectrum from radio all the way up to TeV, as well as the high-energy neutrino window. Among the numerous classes of transients, γ–ray bursts (GRBs) have direct links with most of the hot topics that will be addressed, such as the strong gravity regime, relativistic shocks, particle acceleration processes, equation of state of matter at nuclear density, and nucleosynthesis of heavy elements, just to mention a few. Other recently discovered classes of transients that are observed throughout cosmological distances include fast radio bursts (FRBs), fast blue optical transients (FBOTs), and other unidentified high-energy transients. Here we discuss how these topics can be addressed by a mission called ASTENA (Advanced Surveyor of Transient Events and Nuclear Astrophysics, see Frontera et al. 18). Its payload combines two instruments: (i) an array of wide-field monitors with imaging, spectroscopic, and polarimetric capabilities (WFM-IS); (ii) a narrow field telescope (NFT) based on a Laue lens operating in the 50–600 keV range with unprecedented angular resolution, polarimetric capabilities, and sensitivity. © 2021, The Author(s)., The ASTENA mission concept is the result of several development activities. We wish to acknowledge the support by the Italian Space Agency (ASI) and that by the AHEAD European program. Open access funding provided by Universita degli Studi di Ferrara within the CRUI-CARE Agreement., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.
Published: 2021

5. Disk vs wind accretion in X-ray pulsar GX 301-2

Author: Andrea Santangelo, Xiaobo Li, P. A. Jenke, Shu Zhang, Jiren Liu, Mauro Orlandini, Shuang-Nan Zhang, Ming-Yu Ge, Zhenxuan Liao, Long Ji, and Victor Doroshenko
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Accretion (meteorology), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Absorption column, 01 natural sciences, Pulse (physics), Luminosity, Space and Planetary Science, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Event (particle physics), Astrophysics::Galaxy Astrophysics, X-ray pulsar, Fermi Gamma-ray Space Telescope
Abstract: GX 301-2 provides a rare opportunity to study both disk and wind accretion in a same target. We report Insight-HXMT observations of the spin-up event of GX 301-2 happened in 2019 and compare with those of wind-fed state. The pulse profiles of the initial rapid spin-up period are dominated by one main peak, while those of the later slow spin-up period are composed of two similar peaks, as those of wind-fed state. These behaviors are confirmed by Fermi/GBM data, which also show that during the rapid spin-up period, the main peak increases with luminosity up to $8\times10^{37}$ erg s$^{-1}$, but the faint peak keeps almost constant. The absorption column densities during the spin-up period are $\sim1.5\times10^{23}$ cm$^{-2}$, much less than those of wind-fed state at similar luminosity ($\sim9\times10^{23}$ cm$^{-2}$), supporting the scenario that most of material is condensed into a disk during the spin-up period. We discuss possible differences between disk and wind accretion that may explain the observed different trend of pulse profiles., 9 pages, 6 figs, to appear in MNRAS
Published: 2021

6. Comptonization as an origin of the continuum in Intermediate Polars

Author: Mauro Orlandini, W. Wang, Lev Titarchuk, T. Maiolino, and F. Frontera
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Photon, 010504 meteorology & atmospheric sciences, Continuum (design consultancy), X-ray binary, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Electron, 01 natural sciences, Spectral line, Luminosity, Space and Planetary Science, 0103 physical sciences, Optical depth (astrophysics), Black-body radiation, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: In this paper we test if the ∼0.3–15 keV XMM-Newton EPIC pn spectral continuum of IPs can be described by the thermal Comptonization compTT model. We used publicly observations of 12 IPs (AE Aqr, EX Hya, V1025 Cen, V2731 Oph, RX J2133.7+5107, PQ Gem, NY Lup, V2400 Oph, IGR J00234+6141, IGR J17195-4100, V1223 Sgr, and XY Ari). We find that our modeling is capable of fitting well the average spectral continuum of these sources. In this framework, UV/soft X-ray seed photons (with 〈kT s〉 of 0.096 ± 0.013 keV) coming presumably from the star surface are scattered off by electrons present in an optically thick plasma (with 〈kT e〉 of 3.05 ± 0.16 keV and optical depth 〈τ〉 of 9.5 ± 0.6 for plane geometry) located nearby (on top) to the more central seed photon emission regions. A soft blackbody (bbody) component is observed in 5 out of the 13 observations analyzed, with a mean temperature 〈kT bb 〉 of 0.095 ± 0.004 keV. We observed that the spectra of IPs show in general two photon indices Γ, which are driven by the source luminosity and optical depth. Low luminosity IPs show 〈Γ〉 of 1.83 ± 0.19, whereas high luminosity IPs show lower 〈Γ〉 of 1.34 ± 0.02. Moreover, the good spectral fits of PQ Gem and V2400 Oph indicate that the polar subclass of CVs may be successfully described by the thermal Comptonization as well.
Published: 2021

7. Understanding the origin of the positron annihilation line and the physics of supernova explosions

Author: Natalia Auricchio, Chris L. Fryer, R. M. Curado da Silva, Roland Diehl, M. Della Valle, Lorenzo Amati, Søren Brandt, Irfan Kuvvetli, Piero Rosati, Thomas Siegert, Enrico Bozzo, Carl Budtz-Jørgensen, Paolo A. Mazzali, Elena Pian, Claudio Labanti, Enrico Virgilli, Ezio Caroli, Mauro Orlandini, S. Del Sordo, C. Guidorzi, Riccardo Campana, F. Fuschino, F. Frontera, John B. Stephen, P. Laurent, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay
Subjects: Origin of positron annihilation line from Galactic bulge region, Astrophysics::High Energy Astrophysical Phenomena, Space mission concept, Population, Dark matter, Socio-culturale, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, Nucleosynthesis, 0103 physical sciences, Nuclear astrophysics, Nuclear fusion, education, 010303 astronomy & astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Dark matter from the Galactic Center region, ESA voyage 2050, Nuclear line distribution across supernova remnants, Nucleosynthesis study in novae, Physical origin of the Phillips law, type I and core-collapse supernovae, X–/γ–ray telescopes, Galaxy, Neutron star, Supernova, Space and Planetary Science, Type I and core-collapse supernovae, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Nuclear astrophysics, and particularly nuclear emission line diagnostics from a variety of cosmic sites, has remained one of the least developed fields in experimental astronomy, despite its central role in addressing a number of outstanding questions in modern astrophysics. Radioactive isotopes are co-produced with stable isotopes in the fusion reactions of nucleosynthesis in supernova explosions and other violent events, such as neutron star mergers. The origin of the 511 keV positron annihilation line observed in the direction of the Galactic Center is a 50-year-long mystery. In fact, we still do not understand whether its diffuse large-scale emission is entirely due to a population of discrete sources, which are unresolved with current poor angular resolution instruments at these energies, or whether dark matter annihilation could contribute to it. From the results obtained in the pioneering decades of this experimentally-challenging window, it has become clear that some of the most pressing issues in high-energy astrophysics and astro-particle physics would greatly benefit from significant progress in the observational capabilities in the keV-to-MeV energy band. Current instrumentation is in fact not sensitive enough to detect radioactive and annihilation lines from a wide variety of phenomena in our and nearby galaxies, let alone study the spatial distribution of their emission. In this White Paper (WP), we discuss how unprecedented studies in this field will become possible with a new low-energy gamma-ray space experiment, called ASTENA (Advanced Surveyor of Transient Events and Nuclear Astrophysics), which combines new imaging, spectroscopic and polarization capabilities. In a separate WP (Guidorzi et al. 39), we discuss how the same mission concept will enable new groundbreaking studies of the physics of Gamma–Ray Bursts and other high-energy transient phenomena over the next decades.
Published: 2021

8. 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

9. Testing Comptonization as the Origin of the Continuum in Nonmagnetic Cataclysmic Variables: The Photon Index of X-Ray Emission

Author: Lev Titarchuk, Flavio D'Amico, W. Wang, Filippo Frontera, Mauro Orlandini, Zhongqun Cheng, T. Maiolino, ITA, and CHN
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Photon, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Continuum (design consultancy), X-ray binary, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Plasma, Cooling flow, 01 natural sciences, Spectral line, Atmospheric radiative transfer codes, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Optical depth, 0105 earth and related environmental sciences
Abstract: X-ray spectra of nonmagnetic cataclysmic variables (nmCVs) in the ~ 0.3$-$15 keV energy band have been described either by one or several optically thin thermal plasma components, or by cooling flow models. We tested if the spectral continuum in nmCVs could be successfully described by Comptonization of soft photons off hot electrons presented in a cloud surrounding the source [the transition layer, (TL)]. We used publicly XMM-Newton Epic-pn, Chandra HETG/ACIS and LETG/HRC, and RXTE PCA and HEXTE observations of four Dwarf Novae (U~Gem, SS~Cyg, VW~Hyi and SS~Aur) observed in the quiescence and outburst states. In total, we analyzed 18 observations, including a simultaneous 0.4$-$150 keV Chandra/RXTE spectrum of SS~Cyg in quiescence. We fitted the spectral continuum with up to two thermal Comptonization components (compTT or compTB models in XSPEC), using only one thermal plasma temperature and one optical depth. In this framework the two seed photon components are coming presumably from the innermost and outer parts of the TL (or innermost part of the disk). We obtained that the thermal Comptonization can successfully describe the spectral continuum of these nmCV in the ~ 0.4$-$150 keV energy band. Moreover, we present the first principal radiative transfer model which explains the quasi-constancy of the spectral photon index observed around 1.8, which strongly supports the Comptonization framework in nmCVs., Comment: 34 pages, 8 figures
Published: 2020

10. Constraining the transient high-energy activity of FRB180916.J0158+65 with Insight-HXMT followup observations

Author: L. Chen, Yu-Dong Gu, Ya Fang Huang, R. J. Yang, Y. J. Yang, L. Wang, Junqiang Zhang, Wenhan Jiang, Qiu-Yi Luo, X. H. Liang, C. Z. Liu, G. C. Xiao, B. Y. Wu, Y. L. Tuo, Sisi Yang, He-Yang Liu, Wei Cui, W. S. Wang, Xiaobo Li, Wei Zhang, G. H. Gao, Ge Ou, Bing Li, B. B. Wu, Bin Meng, C. Guidorzi, F. Frontera, Yi Zhang, C. Cai, Luciano Nicastro, Lei Sun, Mauro Orlandini, M. Wu, J. Jin, Xin-Fu Zhao, H. S. Zhao, Y. Nang, Cheng-Cheng Guo, Y. P. Xu, Tao Luo, Yuan You, Qingcui Bu, S. Xiao, C. K. Li, Qi-Bin Yi, Shaolin Xiong, P. J. Wang, Wenxiong Li, Y. B. Chen, J. Y. Liao, H. M. Zhang, L. D. Kong, B. S. Liu, X. X. Li, H. Gao, H. W. Liu, N. Sai, Z. W. Li, W. C. Zhang, R. C. Ma, Min Gao, Fuqin Zhang, Y. F. Zhang, S. N. Zhang, D. K. Zhou, C. Wang, J. L. Qu, J. Guan, Lorenzo Amati, Y. G. Zheng, Y. S. Wang, Xin Ren, Tian-Xiang Chen, E. Virgilli, Lian Tao, Z. Chang, Da-Wei Han, Jia Huo, Y. H. Tan, X. Y. Song, X. F. Li, Gang Li, P. Zhang, Ming-Yu Ge, J. Y. Nie, Yuan-Yuan Du, F. J. Lu, XiangYang Wen, X. H. Ma, Li-Ming Song, Xue-Feng Lu, Tong Li, S. M. Jia, X. J. Liu, X. L. Cao, Q. Q. Yin, Y. P. Chen, S. J. Zheng, ITA, and CHN
Subjects: Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Socio-culturale, Context (language use), Astrophysics, Magnetar, 01 natural sciences, law.invention, Telescope, stars: magnetars, law, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Fast radio burst, Detector, Astronomy and Astrophysics, radiation mechanisms: non-thermal, stars: magnetars, radiation mechanisms: non-thermal, Wavelength, Space and Planetary Science, Phase space, Astrophysics - High Energy Astrophysical Phenomena, Energy (signal processing)
Abstract: A link between magnetars and fast radio burst (FRB) sources has finally been established. In this context, one of the open issues is whether/which sources of extra galactic FRBs exhibit X/gamma-ray outbursts and whether it is correlated with radio activity. We aim to constrain possible X/gamma-ray burst activity from one of the nearest extragalactic FRB sources currently known over a broad energy range, by looking for bursts over a range of timescales and energies that are compatible with being powerful flares from extragalactic magnetars. We followed up the as-yet nearest extragalactic FRB source at a mere 149 Mpc distance, the periodic repeater FRB180916.J0158+65, during the active phase on February 4-7, 2020, with the Insight-Hard X-ray Modulation Telescope (HXMT). Taking advantage of the combination of broad band, large effective area, and several independent detectors available, we searched for bursts over a set of timescales from 1 ms to 1.024 s with a sensitive algorithm, that had previously been characterised and optimised. Moreover, through simulations we studied the sensitivity of our technique in the released energy-duration phase space for a set of synthetic flares and assuming different energy spectra. We constrain the possible occurrence of flares in the 1-100 keV energy band to E, 10 pages, 3 figures, accepted by A&A
Published: 2020

11. X-ray reprocessing in accreting pulsar GX 301-2 observed with Insight-HXMT

Author: G. H. Gao, X. X. Li, M. Wu, S. J. Zheng, Y. G. Zheng, Y. Nang, Mauro Orlandini, J. Y. Liao, H. M. Zhang, Y. L. Tuo, Y. J. Yang, R. C. Ma, Y. F. Zhang, X. B. Li, B. S. Liu, Yuan You, X. Q. Ren, Yanji Yang, Armin Nabizadeh, C. Cai, L. Chen, Tian-Xiang Chen, Wenxiong Li, Wan-Chang Zhang, W. S. Wang, Yi Zhang, Ge Ou, Andrea Santangelo, R. J. Yang, Bo Li, Peng Zhang, Qiu-Yi Luo, B. B. Wu, Cunguo Wang, H. S. Zhao, Li-Ming Song, Ming-Yu Ge, C. K. Li, F. J. Lu, Xue-Feng Lu, Y. P. Chen, Shuinai Zhang, Tong Li, Y. H. Tan, P. J. Wang, J. Y. Zhang, Victor Doroshenko, Shaolin Xiong, S. M. Jia, XiangYang Wen, Ling-Jun Wang, H. Gao, Jiren Liu, X. H. Ma, Z. W. Li, Yuan-Yuan Du, C. Z. Liu, D. K. Zhou, Sisi Yang, Ya Fang Huang, J. Jin, Xin-Fu Zhao, G. Li, Tao Luo, S. Xiao, Yu-Dong Gu, X. J. Liu, D. Gavran, X. L. Cao, Q. Q. Yin, Q. B. Yi, B. Y. Wu, V. F. Suleimanov, L. D. Kong, Y. B. Chen, X. H. Liang, L. Sun, Fuqin Zhang, S. N. Zhang, Long Ji, Z. Chang, Y. H. Zhang, Y. P. Xu, Wenhan Jiang, H. W. Liu, N. Sai, Y. S. Wang, W. C. Zhang, Xuelong Li, J. Guan, Lian Tao, Cheng-Cheng Guo, X. Y. Song, Jia Huo, Lorenzo Ducci, J. Y. Nie, Bin Meng, Wei Cui, G. C. Xiao, Qingcui Bu, Da-Wei Han, J. L. Qu, Hongfei Liu, ITA, DEU, and CHN
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Accretion (meteorology), Astrophysics::High Energy Astrophysical Phenomena, X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radiation, 01 natural sciences, Neutron star, Pulsar, Space and Planetary Science, Ionization, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010306 general physics, Absorption (electromagnetic radiation), Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Equivalent width, Astrophysics::Galaxy Astrophysics
Abstract: We investigate the absorption and emission features in observations of GX 301-2 detected with Insight-HXMT/LE in 2017-2019. At different orbital phases, we found prominent Fe Kalpha, Kbeta and Ni Kalpha lines, as well as Compton shoulders and Fe K-shell absorption edges. These features are due to the X-ray reprocessing caused by the interaction between the radiation from the source and surrounding accretion material. According to the ratio of iron lines Kalpha and Kbeta, we infer the accretion material is in a low ionisation state. We find an orbital-dependent local absorption column density, which has a large value and strong variability around the periastron. We explain its variability as a result of inhomogeneities of the accretion environment and/or instabilities of accretion processes. In addition, the variable local column density is correlated with the equivalent width of the iron Kalpha lines throughout the orbit, which suggests that the accretion material near the neutron star is spherically distributed., Comment: 10 pages, 5 figures, 2 tables, accepted for publication in MNRAS
Published: 2020
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12. The X/Gamma-ray Imaging Spectrometer (XGIS) on-board THESEUS: Design, main characteristics, and concept of operation

Author: Sandro Mereghetti, Lorenzo Amati, J. L. Gasent-Blesa, Denis Tcherniak, Piero Malcovati, F. Fuschino, Piero Rosati, P. Bellutti, Natalia Auricchio, Giacomo Borghi, A. de Rosa, Irfan Kuvvetli, Francesco Ficorella, M. Fiorini, Andrea Santangelo, E. Demenev, Giuseppe Bertuccio, A. Picciotto, C. Guidorzi, G. Zampa, Giuseppe Sottile, Riccardo Campana, Raffaele Piazzolla, Søren Møller Pedersen, F. Evangelisti, Pedro Rodríguez-Martínez, Mauro Orlandini, Paolo Lorenzi, Luca Terenzi, Nadia Zorzi, M. Melchiorri, M. Winkler, Paolo Sarra, Filippo Frontera, E. Virgilli, I. Rashevskaya, C. Tenzer, P. H. Connell, J. Navarro-González, A. Vacchi, Miriam Grassi, V. Reglero, F. Mele, V. Da Ronco, J. B. Stephen, V. Zanini, Piotr Orleanski, A. Volpe, A. J. Castro-Tirado, N. Zampa, Paul Hedderman, A. Rachevski, Giuseppe Baldazzi, Alessio Trois, M. Gandola, Benjamin Pinazo-Herrero, R. C. Butler, Gianluca Morgante, G. La Rosa, Claudio Labanti, S. Squerzanti, den Herder, Jan-Willem A., Labanti C., Amati L., Frontera F., Mereghetti S., Gasent-Blesa J.L., Tenzer C., Orleanski P., Kuvvetli I., Campana R., Fuschino F., Terenzi L., Virgilli E., Morgante G., Orlandini M., Butler R.C., Stephen J.B., Auricchio N., de Rosa A., da Ronco V., Evangelisti F., Melchiorri M., Squerzanti S., Fiorini M., Bertuccio G., Mele F., Gandola M., Malcovati P., Grassi M., Bellutti P., Borghi G., Ficorella F., Picciotto A., Zanini V., Zorzi N., Demenev E., Rashevskaya I., Rachevski A., Zampa G., Vacchi A., Zampa N., Baldazzi G., la Rosa G., Sottile G., Volpe A., Winkler M., Reglero V., Connell P., Pinazo-Herrero B., Navarro-Gonzalez J., Rodriguez-Martinez P., Castro-Tirado A.J., Santangelo A., Hedderman P., Lorenzi P., Sarra P., Pedersen S.M., Tcherniak A.D., Guidorzi C., Rosati P., Trois A., Piazzolla R., Agenzia Spaziale Italiana, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, National Science Centre (Poland), Foundation for Polish Science, ITA, DEU, ESP, DNK, POL, Herder, Jan-Willem A. den, Nikzad, Shouleh, and Nakazawa, Kazuhiro
Subjects: Cosmic Vision, ESA Missions, Gamma-ray detectors, Astrophysics::High Energy Astrophysical Phenomena, Infrared telescope, Imaging spectrometer, X-ray detector, FOS: Physical sciences, Silicon Drift Detectors, Scintillator, 01 natural sciences, law.invention, Telescope, ESA Mission, Optics, law, Coded Mask Imaging, 0103 physical sciences, Gamma ray astronomy, XGIS, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Physics, Spectrometer, 010308 nuclear & particles physics, business.industry, Gamma Ray Bursts, Astrophysics::Instrumentation and Methods for Astrophysics, X-ray detectors, Gamma-ray astronomy, Gamma Ray Burst, THESEUS, Astrophysics - Instrumentation and Methods for Astrophysics, business, Gamma-ray Bursts
Abstract: Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray; Virtual, Online; United States; 14 December 2020 through 18 December 2020; Code 166330.--Proceedings of SPIE - The International Society for Optical Engineering Volume 11444, 2020, Article number 114442K.--Full list of authors: Labanti, C.; Amati, L.; Frontera, F.; Mereghetti, S.; Gasent-Blesa, J. L.; Tenzer, C.; Orleanski, P.; Kuvvetli, I.; Campana, R.; Fuschino, F.; Terenzi, L.; Virgilli, E.; Morgante, G.; Orlandini, M.; Butler, R. C.; Stephen, J. B.; Auricchio, N.; De Rosa, A.; Da Ronco, V.; Evangelisti, F. Melchiorri, M.; Squerzanti, S.; Fiorini, M.; Bertuccio, G.; Mele, F.; Gandola, M.; Malcovati, P.; Grassi, M.; Bellutti, P.; Borghi, G.; Ficorella, F.; Picciotto, A.; Zanini, V.; Zorzi, N.; Demenev, E.; Rashevskaya, I.; Rachevski, A.; Zampa, G.; Vacchi, A.; Zampa, N.; Baldazzi, G.; La Rosa, G.; Sottile, G.; Volpe, A.; Winkler, M.; Reglero, V.; Connell, P. H.; Pinazo-Herrero, B.; Navarro-González, J.; Rodríguez-Martínez, P.; Castro-Tirado, A. J.; Santangelo, A.; Hedderman, P.; Lorenzi, P.; Sarra, P.; Pedersen, S. M.; Tcherniak, D.; Guidorzi, C.; Rosati, P.; Trois, A.; Piazzolla, R., THESEUS (Transient High Energy Sky and Early Universe Surveyor) is one of the three missions selected by ESA as fifth medium class mission (M5) candidates in its Cosmic Vision science program, currently under assessment in a phase A study with a planned launch date in 2032. THESEUS is designed to carry on-board two wide and deep sky monitoring instruments for X/gamma-ray transients detection: a wide-field soft X-ray monitor with imaging capability (Soft X-ray Imager, SXI, 0.3 - 5 keV), a hard X-ray, partially-imaging spectroscopic instrument (X and Gamma Imaging Spectrometer, XGIS, 2 keV - 10 MeV), and an optical/near-IR telescope with both imaging and spectroscopic capability (InfraRed Telescope, IRT, 0.7 - 1.8 µm). The spacecraft will be capable of performing fast repointing of the IRT to the error region provided by the monitors, thus allowing it to detect and localize the transient sources down to a few arcsec accuracy, for immediate identification and redshift determination. The prime goal of the XGIS will be to detect transient sources, with monitoring timescales down to milliseconds, both independently of, or following up, SXI detections, and identify the sources performing localisation at, The Phase A study of the THESEUS/XGIS instrument is supported by ASI-INAF Agreement n. 2018-29-HH.0, OHB Italia/ - INAF-OASBo Agreement n.2331/2020/01, by the European Space Agency ESA through the M5/NPMC Programme and by the AHEAD2020 project funded by UE through H2020-INFRAIA-2018-2020. By the Spanish Ministerio de Ciencia e Innovación, PID2019-109269RB-C41. By Polish National Science Center, Project 2019/35/B/ST9/03944 and Foundation for Polish Science, Project POIR.04.04.00-00-5C65/17-00.
Published: 2020

13. The XGIS instrument on-board THESEUS: Monte Carlo simulations for response, background, and sensitivity

Author: Valentina Fioretti, Enrico Virgilli, Riccardo Campana, Mauro Orlandini, F. Fuschino, John B. Stephen, Claudio Labanti, Sandro Mereghetti, Lorenzo Amati, and ITA
Subjects: Physics, Photon, Cosmic Vision, Spectrometer, business.industry, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Monte Carlo method, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Albedo, Universe, Sky, Physics::Space Physics, Transient (oscillation), Astrophysics::Earth and Planetary Astrophysics, Aerospace engineering, business, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), media_common
Abstract: The response of the X and Gamma Imaging Spectrometer (XGIS) instrument onboard the Transient High Energy Sky and Early Universe Surveyor (THESEUS) mission, selected by ESA for an assessment phase in the framework of the Cosmic Vision M5 launch opportunity, has been extensively modeled with a Monte Carlo Geant-4 based software. In this paper, the expected sources of background in the Low Earth Orbit foreseen for THESEUS are described (e.g. diffuse photon backgrounds, cosmic-ray populations, Earth albedo emission) and the simulated on-board background environment and its effects on the instrumental performance is shown., Proceedings of the SPIE 2020, paper 11444-275. arXiv admin note: text overlap with arXiv:2101.03017
Published: 2020

14. The XGIS imaging system on board the THESEUS mission

Author: Lorenzo Amati, F. Fuschino, F. Evangelisti, Sandro Mereghetti, Luca Terenzi, M. D. Caballero-Garcia, Riccardo Campana, J. L. Gasent-Blesa, Victor Reglero, Pedro Rodríguez-Martínez, Mauro Orlandini, A. de Rosa, Filippo Frontera, J. Navarro-González, John B. Stephen, S. Squerzanti, Claudio Labanti, M. Melchiorri, P. Connell, Benjamin Pinazo-Herrero, A. J. Castro-Tirado, Gianluca Morgante, Istituto Nazionale di Astrofisica, European Space Agency, European Commission, Ministerio de Ciencia e Innovación (España), National Science Centre (Poland), and Foundation for Polish Science
Subjects: 010504 meteorology & atmospheric sciences, Computer science, Imaging techniques, X-ray transients, 01 natural sciences, Multiplexing, law.invention, X-ray astronomy, law, 0103 physical sciences, International Space Station, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, COSMIC cancer database, business.industry, Detector, Collimator, Upgrade, Signal multiplexing, Electromagnetic shielding, Gamma-ray bursts, Coded mask, business, Computer hardware
Abstract: Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray; Virtual, Online; United States; 14 December 2020 through 18 December 2020; Code 166330.--Proceedings of SPIE - The International Society for Optical Engineering Volume 11444, 2020, Article number 114448S.--Full list of authors: Gasent-Blesa, J. L.; Reglero, V.; Connell, P.; Pinazo-Herrero, B.; Navarro-González, J.; Rodríguez-Martínez, P.; Castro-Tirado, A. J.; Caballero-García, M. D.; Amati, L.; Labanti, C.; Mereghetti, S.; Frontera, F.; Campana, R.; Orlandini, M.; Stephen, J.; Terenzi, L.; Evangelisti, F.; Squerzanti, S.; Melchiorri, M.; Fuschino, F. De Rosa, A.; Morgante, G., Within the scientific goals of the THESEUS ESA/M5 candidate mission, a critical item is a fast (within a few s) and accurate (, THESEUS/XGIS instrument is supported by: the ASI-INAF Agreement n. 2018-29-HH.0; the OHB Italia/INAF-OASBo Agreement n.2331/2020/01; the European Space Agency ESA through the M5/NPMC Programme; the AHEAD2020 project funded by the UE through H2020-INFRAIA-2018-2020; the Spanish Ministerio de Ciencia e Innovaci?n, PID2019 109269RB-C41; the Polish National Science Centre, Project 2019/35/B/ST9/03944 and Foundation for Polish Science, Project POIR.04.04.00-00-5C65/17-00. The authors thank all the members of the THESEUS team involved in the development of XGIS instrument.
Published: 2020

15. Red-skewed Kα iron lines in GX 13+1

Author: T. Maiolino, F. Frontera, Mauro Orlandini, P. Laurent, Lev Titarchuk, Università degli Studi di Ferrara (UniFE), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Erasmus Mundus Joint Doctorate Program by Grants Number 2013-1471 from the agency EACEA of the European CommissionCNES/INTEGRALCNR/INAF-IASF Bologna, ITA, FRA, University of Ferrara [Ferrara], 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), Università degli Studi di Ferrara = University of Ferrara (UniFE), 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, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Continuum (design consultancy), Astronomy and Astrophysics, Context (language use), line: profiles, Astrophysics, Compact star, 01 natural sciences, Spectral line, outflows, Neutron star, X-rays: binaries, stars: neutron, Space and Planetary Science, stars: winds, 0103 physical sciences, Emission spectrum, line: formation, Relativistic quantum chemistry, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Line (formation)
Abstract: Context. Broad, asymmetric, and red-skewed Fe Kα emission lines have been observed in the spectra of low-mass X-ray binaries hosting neutron stars (NSs) as a compact object. Because more than one model is able to describe these features, the explanation of where and how the red-skewed Fe lines are produced is still a matter of discussion. It is broadly accepted that the shape of the Fe Kα line is strongly determined by the special and general relativistic effects occurring in the innermost part of the accretion disk. In this relativistic framework, the Fe fluorescent lines are produced in the innermost part of the accretion disk by reflection of hard X-ray photons coming from the central source (corona and/or NS surface). We developed an alternative and nonrelativistic model, called the WINDLINE model, that is capable to describe the Fe line features. In this nonrelativistic framework, the line photons are produced at the bottom of a partly ionized outflow (wind) shell as a result of illumination by the continuum photons coming from the central source. In this model the red-skewness of the line profile is explained by repeated electron scattering of the photons in a diverging outflow. Aims. Examining the asymmetry of the fluorescent Fe K emission line evident in the XMM-Newton EPIC-pn spectra of the NS source GX 13+1, we aim to distinguish between the two line models. Because GX 13+1 is a well-known disk-wind source, it is a perfect target for testing the WINDLINE model and compare the spectral fits between the relativistic and nonrelativistic line models. Methods. We used two XMM-Newton EPIC-pn observations in which the Fe line profiles were previously reported in the literature. These observations are not strongly affected by pile-up, and the Fe emission lines appear very strong and red-skewed. In order to access the goodness of the fit and distinguish between the two line models, we used the run-test statistical method in addition to the canonical χ2 statistical method. Results. The DISKLINE and WINDLINE models both fit the asymmetric Fe line well that is present in the XMM-Newton energy spectra of GX 13+1. From a statistical point of view, for the two observations we analyzed, the run-test was not able to distinguish between the two Fe line models, at 5% significance level.
Published: 2019

16. Physics and astrophysics of strong magnetic field systems with eXTP

Author: Can Güngör, Francesco Coti Zelati, Lin Lin, Nanda Rea, Cristina Baglio, Sandro Mereghetti, G. L. Israel, George Younes, Biswajit Paul, Silvia Zane, Shuang-Nan Zhan, Roberto Turolla, Renxin Xu, Fangjun Lu, Roberto Taverna, Jeremy S. Heyl, Antonios Manousakis, Ilaria Caiazzo, Chanda Prescod-Weinstein, Victor Doroshenko, Marco Feroci, Mauro Orlandini, Yupeng Xu, Hao Tong, Enrico Bozzo, Ersin Gogus, Long Ji, Shu Zhang, Anna L. Watts, Andrea Tiengo, Paolo Esposito, Romana Mikusincova, Federico Bernardini, Roberto Mignani, Zhaosheng Li, Niccolò Bucciantini, Denis González-Caniulef, Hua Feng, Felix Fürst, Daniela Huppenkothen, Andrea Santangelo, High Energy Astrophys. & Astropart. Phys (API, FNWI), ITA, USA, DEU, ESP, CAN, ARE, IND, OMN, NLD, POL, CHN, CHE, and TUR
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, Polarimetry, Astrophysics::Instrumentation and Methods for Astrophysics, General Physics and Astronomy, FOS: Physical sciences, Astrophysics, Rotation, Magnetar, 01 natural sciences, 7. Clean energy, Chinese academy of sciences, Magnetic field, Pulsar, 0103 physical sciences, 010306 general physics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract: In this paper we present the science potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies of strongly magnetized objects. We will focus on the physics and astrophysics of strongly magnetized objects, namely magnetars, accreting X-ray pulsars, and rotation powered pulsars. We also discuss the science potential of eXTP for QED studies. Developed by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Sciences, the eXTP mission is expected to be launched in the mid 2020s., Accepted for publication on Sci. China Phys. Mech. Astron. (2019)
Published: 2019

17. A Search for Gamma-Ray Prompt Emission Associated with the Lorimer Burst FRB 010724

Author: Enrico Virgilli, Luciano Nicastro, F. Frontera, M. Marongiu, C. Guidorzi, Lorenzo Amati, Raffaella Margutti, R. Martone, Mauro Orlandini, ITA, and USA
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Space and Planetary Science, Radiation mechanisms: Non-thermal-stars: Individual (frb 010724), Gamma ray, FOS: Physical sciences, Socio-culturale, Astronomy and Astrophysics, Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: No transient electromagnetic emission has yet been found in association to fast radio bursts (FRBs), the only possible exception (3sigma confidence) being the putative gamma-ray signal detected in Swift/BAT data in the energy band 15-150 keV at the time and position of FRB131104. Systematic searches for hard X/gamma-ray counterparts to other FRBs ended up with just lower limits on the radio/gamma-ray fluence ratios. In 2001, at the time of the earliest discovered FRBs, the BeppoSAX Gamma-Ray Burst Monitor (GRBM) was one of the most sensitive open sky gamma-ray monitors in the 40-700~keV energy band. During its lifetime, one of the FRBs with the highest radio fluence ever recorded, FRB010724 (800 +- 400 Jy ms), also known as the Lorimer burst, was promptly visible to the GRBM. Upon an accurate modeling of the GRBM background, eased by its equatorial orbit, we searched for a possible gamma-ray signal in the first 400 s following the FRB, similar to that claimed for FRB131104 and found no significant emission down to a 5-sigma limit in the range (0.24-4.7)x10^-6 erg cm^-2 (corresponding to 1 and 400 s integration time, respectively), in the energy band 40-700 keV. This corresponds to eta = F_radio/F_gamma>10^{8-9} Jy ms erg^-1 cm^2, i.e. the deepest limit on the ratio between radio and gamma-ray fluence, which rules out a gamma-ray counterpart similar to that of FRB131104. We discuss the implications on the possible mechanisms and progenitors that have been proposed in the literature, also taking into account its relatively low dispersion measure (375 +- 3 pc cm^-3) and an inferred redshift limit of z, 7 pages, 4 figures, accepted by ApJ
Published: 2019

18. A cumulative search for hard X/ γ -ray emission associated with fast radio bursts in Fermi /GBM data

Author: Raffaella Margutti, Mauro Orlandini, Enrico Virgilli, M. Marongiu, C. Guidorzi, Lorenzo Amati, Luciano Nicastro, R. Martone, F. Frontera, and ITA
Subjects: Time delay and integration, Physics, Sample average, 010308 nuclear & particles physics, Gamma rays: general, Socio-culturale, Gamma-ray burst: general, Astronomy and Astrophysics, Context (language use), Astrophysics, Magnetar, 01 natural sciences, Fluence, Radio continuum: general, Space and Planetary Science, 0103 physical sciences, Radio frequency, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Fermi Gamma-ray Space Telescope
Abstract: Context. Fast Radio Bursts (FRBs) are millisecond-long bursts uniquely detected at radio frequencies. FRB 131104 is the only case for which a $\gamma$-ray transient positionally and temporally consistent was claimed. This high-energy transient had a duration of $\sim400$~s and a 15-150~keV fluence $S_{\gamma}\sim4\times10^{-6}$ erg $\mathrm{cm}^{-2}$. However, the association with the FRB is still debated. Aims. We aim at testing the systematic presence of an associated transient high-energy counterpart throughout a sample of the FRB population. Methods. We used an approach like that used in machine learning methodologies to accurately model the highly-variable Fermi/GBM instrumental background on a time interval comparable to the duration of the proposed $\gamma$-ray counterpart of FRB 131104. A possible $\gamma$-ray signal is then constrained considering sample average lightcurves. Results. We constrain the fluence of the possible $\gamma$-ray signal in the 8-1000 keV band down to $6.4 \times 10^{-7}$ ($7.1 \times 10^{-8}$) erg cm$^{-2}$ for a 200-s (1-s) integration time. Furthermore, we found the radio-to-gamma fluence ratio to be $\eta>10^{8}$ Jy ms erg$^{-1}$ cm$^2$. Conclusions. Our fluence limits exclude $\sim 94\%$ of Fermi/GBM detected long gamma-ray bursts and $\sim 96\%$ of Fermi/GBM detected short gamma-ray bursts. In addition, our limits on the radio-to-gamma fluence ratio point to a different emission mechanism from that of magnetar giant flares. Finally, we exclude a $\gamma$-ray counterpart as fluent as the one possibly associated with FRB 131104 to be a common feature of FRBs., Comment: 8 pages, 6 figures, Accepted on A&A
Published: 2019

19. The wide field monitor and spectrometer instrument on board the ASTENA satellite mission concept

Author: Lorenzo Amati, F. Fuschino, Claudio Labanti, G. De Cesare, Ezio Caroli, Filippo Frontera, E. Virgili, Mauro Orlandini, Piero Rosati, Riccardo Campana, and ITA
Subjects: Physics, Photon, Spectrometer, Physics::Instrumentation and Detectors, business.industry, High-energy astronomy, Astrophysics::High Energy Astrophysical Phenomena, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Polarimetry, Scintillator, law.invention, Telescope, Optics, law, Satellite, business
Abstract: The ASTENA mission concept under study in the framework of the H2020 AHEAD project includes a wide field monitor and spectrometer (WFM/S), mainly dedicated to GRBs. The instrument, composed by different units, is sensitive in the range 1 keV – 20 MeV. The total isotropic detection area will be ~3.0 m2 with a FOV of about 1.35 sr. The WFM will allow the detection and spectroscopic and polarimetric characterization of all classes of GRBs. Each module is a coded mask telescope that will allow the source localization within few arcmin up to 50–100 keV. The detector core is based on the coupling of low-noise, solid-state Silicon Drift Detectors (SDDs) with CsI(Tl) scintillator bars. Low-energy and highenergy photons are discriminated using the on-board electronics. The instrument design and preliminary experimental characterizations are reported and discussed.
Published: 2018

20. The Narrow Field telescope on board the ASTENA mission (Conference Presentation)

Author: Lorenzo Amati, Irfan Kuvvetli, Angela Malizia, Loredana Bassani, Filippo Frontera, Enrico Virgilli, S. Silvestri, Natalia Auricchio, C. Guidorzi, Rui M. Curado da Silva, Piero Rosati, Riccardo Campana, Mauro Orlandini, A. Basili, Claudio Labanti, F. Fuschino, Søren Brandt, John B. Stephen, Ezio Caroli, and Carl Budtz-Jørgensen
Subjects: Telescope, On board, Presentation, Engineering, Field (physics), law, business.industry, media_common.quotation_subject, Astronomy, business, law.invention, media_common
Published: 2018

21. The advanced surveyor of transient events and nuclear astrophysics (ASTENA) mission within the AHEAD project (Conference Presentation)

Author: Mauro Orlandini, C. Guidorzi, Natalia Auricchio, Rui M. Curado da Silva, Piero Rosati, Lorenzo Amati, Filippo Frontera, Enrico Virgilli, Søren Brandt, Irfan Kuvvetli, Loredana Bassani, John B. Stephen, Claudio Labanti, Carl Budtz-Jørgensen, Giancarlo Ghirlanda, Angela Malizia, Riccardo Campana, Ezio Caroli, F. Fuschino, and Roberto Gilli
Subjects: Physics, Telescope, Photon, Spectrometer, law, Astrophysics::High Energy Astrophysical Phenomena, Nuclear astrophysics, Astrophysics, Blazar, Magnetar, Gamma-ray burst, Afterglow, law.invention
Abstract: Within the AHEAD consortium a mission concept named ASTENA (Advanced Surveyor of Transient Events and Nuclear Astrophysics) is proposed to address the top-priority themes identified by the AHEAD Science Advisory Group: Gamma-Ray Bursts and Nuclear Astrophysics. GRBs are among the most intriguing phenomena of the Universe, which thanks to their vast luminosities can be used to probe the first billion years of cosmic history, i.e. the era of first stars and black-holes. In spite of great advancements in the GRB astronomy since the BeppoSAX discovery of afterglows, several issues concerning both the prompt emission and the afterglow are still open. Concerning the prompt emission, for example, the emission mechanism of the radiation and the energy dissipation site (internal shocks? external shocks? photosphere?) are far from being understood. What is required is an accurate determination of the photon spectrum from few keV up to tens of MeV, and importantly, a measurement of the polarization of the radiation. The emission of the afterglow has been deeply investigated with Swift in the energy band from 0.5 to 10 keV, showing that an understanding of the origin of the emission mechanism requires spectral information extending to much higher energies, as already suggested by a few studies at < 60 keV (e.g., Kouveliotou et al. 2013, ApJ 779, L1). Landmark progress on this issue therefore requires polarization capabilities and a passband extending well beyond 60 keV. Concerning nuclear astrophysics, a fundamental issue concerns the origin of the 511 keV positron annihilation line discovered with INTEGRAL/SPI in the Galactic center. According to the INTEGRAL results the emission is diffuse, but the poor imaging capability of INTEGRAL (at the best with a resolution of 12 arcmin with ISGRI) does not allow one to establish whether what appears diffuse is indeed the superposition of the emission from point-like sources, such as micro-quasars. The important role played by micro-quasars as sources of positron annihilation line emission has also been established with INTEGRAL (Siegert et al. 2016, Nature 531, 341). Another open issue in nuclear astrophysics concerns the determination and understanding of the nuclear burning processes in Type-1a supernovae. This requires a study of the intensity and time behavior of the expected lines emitted by the heavy elements produced in supernova explosions. Instrument concept to address the IWG requirements. With the above considerations in mind, we propose to perform a feasibility study of a configuration of two instruments: a) a wide field monitor/spectrometer (WFM/S), with a passband from 1 keV to 20 MeV, made of a suitable number of detection modules, each consisting of an array of long bars of scintillator with very small cross section, and readout from both sides with solid state thin detectors (e.g. Silicon Drift Detectors, SDD). One of the SDD is used as soft X-ray Position Sensitive Detector. A possible crystal material is CsI(Tl), but also other faster crystals such as LSO(Ce) or CeBr3 should be examined. The detector modules are coupled to a light coded mask, for obtaining a GRB localization accuracy of order of ~1 arcmin between 1 and 30/50 keV. The number of modules, equipped with collimators, should be sufficient to achieve the required sensitivity to GRBs. The order of magnitude of the total detection area is 18000 cm2. The modules are slightly misaligned with each other tin order o achieve a wide FOV (> 1 sr). b) a narrow field telescope (NFT), made of a broad-band Laue lens (50 – 600/700 keV) of a 20 m focal length, based on the exploitation of bent crystals, like those under development in Ferrara (FOV= 3.5 arcmin, angular resolution ≈20”). The NFT is coupled to a high efficiency (>80% above 600 keV) focal plane position sensitive detector, with 3D spatial resolution of at least 300 µm in the (X,Y) plane, fine spectroscopic response (1% @511 keV) and with polarization sensitivity. With the WFM/S, we expect to accurately determine the energy spectrum of GRB prompt emission in the broadest band ever achieved with a single instrument, to measure the gamma-ray polarization of, at least, the brightest GRBs and to search for electromagnetic counterparts of Gravitational Wave events. In addition, with adequate scintillator bars and fast electronics, the Lorentz invariance for the brightest events can be tested. With the NFT, which is >~100 times more sensitive at a few hundred keV than any other past or planned mission, we can carry out for the first time a long-sought study of the afterglow spectrum of GRBs up to high energies (600/700 keV), including its polarization level. We can also establish, thanks to its high angular resolution (about 20”), whether the 511 keV positron annihilation line is due to the superposition of emission from point-like sources. In addition, we can address many Legacy Science topics mentioned in the Call, such as the origin of the high energy emission from magnetars, the first determination of the spectrum of blazars out to z~8 in between the two Synchrotron and Compton bumps, the determination of the sources that give rise to the gamma-ray diffuse background. For example, one could determine the high-energy cutoff from spectra of relatively bright AGN and study how this depends on the physics of the accretion (e.g. BH mass, Eddington ratio). We emphasize that the unprecedented sensitivity of the NFT and the combination with the WFM/S implies a large discovery space of this configuration. Moreover, such an instrument concept, thanks to the lightweight of the Laue lens and compactness of the wide field instrument, is expected to be within the limits imposed by an ESA Medium Size Mission.
Published: 2018

22. XV Convegno Annuale - 'Il linguaggio della Ricerca' - junior

Author: Giovanna Sotgiu (Chair), Mirko Seri (Chair), Eleonora Polo (speaker), Annalisa Aluigi, Luca Bellucci, Alessandra Degli Esposti, Laura Favaretto, Ilse Manet, Francesco Manoli, Franco Marabini, Mauro Orlandini, Ornella Russo, Armida Torreggiani, Alberto Zanelli, and Francesco Piazzi (Rotary) G. Balzani, T. Cremonini, S. Favaretto, G. Longino, M. Minghetti, F. Testi
Subjects: Ricerca, scuola, divulgazione
Abstract: "Il linguaggio della Ricerca (LdR)", progetto di divulgazione scientifica promosso dal Consiglio Nazionale delle Ricerche (CNR) e dall'Istituto Nazionale di Astrofisica (INAF).
Published: 2018

23. XV Convegno Annuale 'Il linguaggio della Ricerca'

Author: Armida Torreggiani (Chair), Greta Varchi (Chair), Eleonora Polo (speaker), Annalisa Aluigi, Luca Bellucci, Emilia Benvenuti, Alessandra Degli Esposti, Laura Favaretto, Francesco Manoli, Ilse Manet, Franco Marabini, Mauro Orlandini, Sara Ricciardi, Ornella Russo, Maura Sandri, Mirko Seri, Giovanna Sotgiu, Alberto Zanelli, and Francesco Piazzi (Rotary) G. Balzani, T. Cremonini, S. Favaretto, G. Longino, M. Minghetti, F. Testi
Subjects: Ricerca, scuola, divulgazione, progetto MIUR
Abstract: Organizzazione del XV Convegno de "Il linguaggio della Ricerca (LdR)", progetto di divulgazione scientifica promosso dal Consiglio Nazionale delle Ricerche (CNR) e dall'Istituto Nazionale di Astrofisica (INAF).
Published: 2018

24. The THESEUS space mission concept: science case, design and expected performances

Author: Martino Marisaldi, Enrico Bozzo, Valerie Connaughton, Dorottya Szécsi, D. Malesani, L. Maraschi, B. Cordier, P. D'Avanzo, Salvatore Capozziello, Darach Watson, C. Contini, Maryam Modjaz, Pierluigi Bellutti, M. de Pasquale, C. Guidorzi, Colleen A. Wilson-Hodge, O. Boulade, C. Adami, Y. Evangelista, A. Argan, Johan P. U. Fynbo, Y.-W. Dong, Poshak Gandhi, Allan Hornstrup, Eliana Palazzi, Andrea Bulgarelli, Andrea Comastri, E. Geza, Luciano Burderi, Giuseppe Malaguti, D. de Martino, Irfan Kuvvetli, S.-N. Zhang, Claudio Labanti, Fiamma Capitanio, Luca Izzo, Bradley Cenko, A. Melandri, Umberto Maio, Nicola Omodei, Stefano Ettori, C. Butler, S. D. Vergani, S. Zhang, Lajos G. Balázs, Patricia Schady, Federica B. Bianco, M. Branchesi, Jens Hjorth, Jochen Greiner, Felix Ryde, Jean-Gabriel Cuby, Piero Malcovati, Lorraine Hanlon, Peter G. Jonker, M. Della Valle, Elena Pian, Piotr Orleanski, Etienne Renotte, W. Skidmore, L. Sabau-Graziati, Mauro Dadina, Carl Budtz-Jørgensen, Tomaz Rodic, Giancarlo Ghirlanda, Luigi Piro, Sheila McBreen, M. Fiorini, M. Topinka, Jan Harms, Riccardo Ciolfi, Yi Chen, Giacomo Vianello, Ester Piedipalumbo, Zsolt Bagoly, Aniello Grado, Yuki Kaneko, Vito Sguera, B. Morelli, E. Le Floc'h, Luciano Rezzolla, K. Wiersema, Remo Ruffini, E. Del Monte, J. P. Osborne, M. G. Bernardini, A. Gomboc, A. De Luca, Stefano Covino, Ian Hutchinson, A. Antonelli, Enzo Brocato, Mark R. Sims, M. Razzano, Elisabetta Maiorano, Jean-Luc Atteia, J. Zicha, S. Korpela, Eros Vanzella, V. D'Elia, M. H. P. M. van Putten, Marco Feroci, Carole Mundell, A. V. Penacchioni, J. Soomin, Gabriele Ghisellini, Sandra Savaglio, N. Shigehiro, Andrea Santangelo, Antonio Martin-Carrillo, Avishay Gal-Yam, A. M. Read, Piergiorgio Casella, Giuseppe Baldazzi, B. Ciardi, Pawan Kumar, Li Song, V. Lebrun, G. Zampa, Daisuke Yonetoku, S. Vojtech, Gregor Rauw, Piero Rosati, A. J. Castro-Tirado, Bruce Gendre, Tsvi Piran, A. Rachevski, S. Basa, T. Li, Michela Uslenghi, Gianluca Morgante, Michèle Lavagna, Pascal Chardonnet, Andrew MacFadyen, Asaf Pe'er, Sandro Mereghetti, Alessandro Drago, M. Hafizi, Richard Willingale, D. Morris, Bing Zhang, Paolo Giommi, Andrea Ferrara, Mauro Orlandini, Maria Giovanna Dainotti, N. Masetti, Yuji Urata, Maxim Lyutikov, A. Vacchi, László L. Kiss, E. Campolongo, M. Boer, Lorenzo Amati, Diego Götz, Andrew Blain, M. T. Botticella, C. Tenzer, Monica Colpi, Victor Reglero, Roberto Mignani, Michael S. Briggs, Joseph Caruana, Elizabeth R. Stanway, S. Colafrancesco, Francesca Panessa, H. U. Nargaard-Nielsen, F. Lu, Giuseppe Bertuccio, A. Paizis, P. Romano, S. Vercellone, Luciano Nicastro, S. Paltani, G. Pareschi, G. Stratta, V. Petrosian, João Braga, N. Zampa, Nial Tanvir, James E. Rhoads, Raffaella Margutti, Luca Valenziano, Søren Brandt, S. Boci, Andrea Rossi, Paul J. Callanan, Annalisa Celotti, N. Kawai, René Hudec, Francesco Longo, Primo Attina, G. L. Israel, F. Fuschino, Fabio Finelli, M. Hernanz, Ruben Salvaterra, F. Frontera, P. T. O'Brien, Sergio Campana, Rupal Basak, Riccardo Campana, Eleonora Troja, Jordan Camp, Petr Páta, S. Piranomonte, G. Tagliaferri, Sylvain Guiriec, R. L. C. Starling, B. B. Zhang, Natalia Auricchio, Serena Vinciguerra, Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), 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), 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), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Agenzia Spaziale Italiana, European Commission, Czech Grant Agency, ITA, 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), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), 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 de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), THESEUS, Amati, L, O'Brien, P, Götz, D, Bozzo, E, Tenzer, C, Frontera, F, Ghirlanda, G, Labanti, C, Osborne, J, Stratta, G, Tanvir, N, Willingale, R, Attina, P, Campana, R, Castro-Tirado, A, Contini, C, Fuschino, F, Gomboc, A, Hudec, R, Orleanski, P, Renotte, E, Rodic, T, Bagoly, Z, Blain, A, Callanan, P, Covino, S, Ferrara, A, Le Floch, E, Marisaldi, M, Mereghetti, S, Rosati, P, Vacchi, A, D'Avanzo, P, Giommi, P, Piranomonte, S, Piro, L, Reglero, V, Rossi, A, Santangelo, A, Salvaterra, R, Tagliaferri, G, Vergani, S, Vinciguerra, S, Briggs, M, Campolongo, E, Ciolfi, R, Connaughton, V, Cordier, B, Morelli, B, Orlandini, M, Adami, C, Argan, A, Atteia, J, Auricchio, N, Balazs, L, Baldazzi, G, Basa, S, Basak, R, Bellutti, P, Bernardini, M, Bertuccio, G, Braga, J, Branchesi, M, Brandt, S, Brocato, E, Budtz-Jorgensen, C, Bulgarelli, A, Burderi, L, Camp, J, Capozziello, S, Caruana, J, Casella, P, Cenko, B, Chardonnet, P, Ciardi, B, Colafrancesco, S, Dainotti, M, D'Elia, V, De Martino, D, De Pasquale, M, Del Monte, E, Della Valle, M, Drago, A, Evangelista, Y, Feroci, M, Finelli, F, Fiorini, M, Fynbo, J, Gal-Yam, A, Gendre, B, Ghisellini, G, Grado, A, Guidorzi, C, Hafizi, M, Hanlon, L, Hjorth, J, Izzo, L, Kiss, L, Kumar, P, Kuvvetli, I, Lavagna, M, Li, T, Longo, F, Lyutikov, M, Maio, U, Maiorano, E, Malcovati, P, Malesani, D, Margutti, R, Martin-Carrillo, A, Masetti, N, Mcbreen, S, Mignani, R, Morgante, G, Mundell, C, Nargaard-Nielsen, H, Nicastro, L, Palazzi, E, Paltani, S, Panessa, F, Pareschi, G, Pe'Er, A, Penacchioni, A, Pian, E, Piedipalumbo, E, Piran, T, Rauw, G, Razzano, M, Read, A, Rezzolla, L, Romano, P, Ruffini, R, Savaglio, S, Sguera, V, Schady, P, Skidmore, W, Song, L, Stanway, E, Starling, R, Topinka, M, Troja, E, van Putten, M, Vanzella, E, Vercellone, S, Wilson-Hodge, C, Yonetoku, D, Zampa, G, Zampa, N, Zhang, B, Zhang, S, Antonelli, A, Bianco, F, Boci, S, Boer, M, Botticella, M, Boulade, O, Butler, C, Campana, S, Capitanio, F, Celotti, A, Chen, Y, Colpi, M, Comastri, A, Cuby, J, Dadina, M, De Luca, A, Dong, Y, Ettori, S, Gandhi, P, Geza, E, Greiner, J, Guiriec, S, Harms, J, Hernanz, M, Hornstrup, A, Hutchinson, I, Israel, G, Jonker, P, Kaneko, Y, Kawai, N, Wiersema, K, Korpela, S, Lebrun, V, Lu, F, Macfadyen, A, Malaguti, G, Maraschi, L, Melandri, A, Modjaz, M, Morris, D, Omodei, N, Paizis, A, Páta, P, Petrosian, V, Rachevski, A, Rhoads, J, Ryde, F, Sabau-Graziati, L, Shigehiro, N, Sims, M, Soomin, J, Szécsi, D, Urata, Y, Uslenghi, M, Valenziano, L, Vianello, G, Vojtech, S, Watson, D, Zicha, J, Amati, L., O'Brien, P., Götz, D., Bozzo, E., Tenzer, C., Frontera, F., Ghirlanda, G., Labanti, C., Osborne, J. P., Stratta, G., Tanvir, N., Willingale, R., Attina, P., Campana, R., Castro-Tirado, A. J., Contini, C., Fuschino, F., Gomboc, A., Hudec, R., Orleanski, P., Renotte, E., Rodic, T., Bagoly, Z., Blain, A., Callanan, P., Covino, S., Ferrara, A., Le Floch, E., Marisaldi, M., Mereghetti, S., Rosati, P., Vacchi, A., D'Avanzo, P., Giommi, P., Piranomonte, S., Piro, L., Reglero, V., Rossi, A., Santangelo, A., Salvaterra, R., Tagliaferri, G., Vergani, S., Vinciguerra, S., Briggs, M., Campolongo, E., Ciolfi, R., Connaughton, V., Cordier, B., Morelli, B., Orlandini, M., Adami, C., Argan, A., Atteia, J. -L., Auricchio, N., Balazs, L., Baldazzi, G., Basa, S., Basak, R., Gian Luca, Israel, Bellutti, P., Bernardini, M. G., Bertuccio, G., Braga, J., Branchesi, M., Brandt, S., Brocato, E., Budtz-Jorgensen, C., Bulgarelli, A., Burderi, L., Camp, J., Capozziello, S., Caruana, J., Casella, P., Cenko, B., Chardonnet, P., Ciardi, B., Colafrancesco, S., Dainotti, M. G., D'Elia, V., De Martino, D., De Pasquale, M., Del Monte, E., Della Valle, M., Drago, A., Evangelista, Y., Feroci, M., Finelli, F., Fiorini, M., Fynbo, J., Gal-Yam, A., Gendre, B., Ghisellini, G., Grado, A., Guidorzi, C., Hafizi, M., Hanlon, L., Hjorth, J., Izzo, L., Kiss, L., Kumar, P., Kuvvetli, I., Lavagna, M., Li, T., Longo, F., Lyutikov, M., Maio, U., Maiorano, E., Malcovati, P., Malesani, D., Margutti, R., Martin-Carrillo, A., Masetti, N., Mcbreen, S., Mignani, R., Morgante, G., Mundell, C., Nargaard-Nielsen, H. U., Nicastro, L., Palazzi, E., Paltani, S., Panessa, F., Pareschi, G., Pe'Er, A., Penacchioni, A. V., Pian, E., Piedipalumbo, E., Piran, T., Rauw, G., Razzano, M., Read, A., Rezzolla, L., Romano, P., Ruffini, R., Savaglio, S., Sguera, V., Schady, P., Skidmore, W., Song, L., Stanway, E., Starling, R., Topinka, M., Troja, E., van Putten, M., Vanzella, E., Vercellone, S., Wilson-Hodge, C., Yonetoku, D., Zampa, G., Zampa, N., Zhang, B., Zhang, B. B., Zhang, S., Zhang, S. -N., Antonelli, A., Bianco, F., Boci, S., Boer, M., Botticella, M. T., Boulade, O., Butler, C., Campana, S., Capitanio, F., Celotti, A., Chen, Y., Colpi, M., Comastri, A., Cuby, J. -G., Dadina, M., De Luca, A., Dong, Y. -W., Ettori, S., Gandhi, P., Geza, E., Greiner, J., Guiriec, S., Harms, J., Hernanz, M., Hornstrup, A., Hutchinson, I., Israel, G., Jonker, P., Kaneko, Y., Kawai, N., Wiersema, K., Korpela, S., Lebrun, V., Lu, F., Macfadyen, A., Malaguti, G., Maraschi, L., Melandri, A., Modjaz, M., Morris, D., Omodei, N., Paizis, A., Páta, P., Petrosian, V., Rachevski, A., Rhoads, J., Ryde, F., Sabau-Graziati, L., Shigehiro, N., Sims, M., Soomin, J., Szécsi, D., Urata, Y., Uslenghi, M., Valenziano, L., Vianello, G., Vojtech, S., Watson, D., Zicha, J., 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 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), ANR-16-CE31-0003,BEaPro,Using the most powerful explosion as probes of the high-redshift Universe(2016), Galaxies, Etoiles, Physique, Instrumentation ( GEPI ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), 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 ), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Gotz, D., Pata, P., Szecsi, D., Department of Physics, and Amati, L. and O'Brien, P. and Götz, D. and Bozzo, E. and Tenzer, C. and Frontera, F. and Ghirlanda, G. and Labanti, C. and Osborne, J.P. and Stratta, G. and Tanvir, N. and Willingale, R. and Attina, P. and Campana, R. and Castro-Tirado, A.J. and Contini, C. and Fuschino, F. and Gomboc, A. and Hudec, R. and Orleanski, P. and Renotte, E. and Rodic, T. and Bagoly, Z. and Blain, A. and Callanan, P. and Covino, S. and Ferrara, A. and Le Floch, E. and Marisaldi, M. and Mereghetti, S. and Rosati, P. and Vacchi, A. and D'Avanzo, P. and Giommi, P. and Piranomonte, S. and Piro, L. and Reglero, V. and Rossi, A. and Santangelo, A. and Salvaterra, R. and Tagliaferri, G. and Vergani, S. and Vinciguerra, S. and Briggs, M. and Campolongo, E. and Ciolfi, R. and Connaughton, V. and Cordier, B. and Morelli, B. and Orlandini, M. and Adami, C. and Argan, A. and Atteia, J.-L. and Auricchio, N. and Balazs, L. and Baldazzi, G. and Basa, S. and Basak, R. and Bellutti, P. and Bernardini, M.G. and Bertuccio, G. and Braga, J. and Branchesi, M. and Brandt, S. and Brocato, E. and Budtz-Jorgensen, C. and Bulgarelli, A. and Burderi, L. and Camp, J. and Capozziello, S. and Caruana, J. and Casella, P. and Cenko, B. and Chardonnet, P. and Ciardi, B. and Colafrancesco, S. and Dainotti, M.G. and D'Elia, V. and De Martino, D. and De Pasquale, M. and Del Monte, E. and Della Valle, M. and Drago, A. and Evangelista, Y. and Feroci, M. and Finelli, F. and Fiorini, M. and Fynbo, J. and Gal-Yam, A. and Gendre, B. and Ghisellini, G. and Grado, A. and Guidorzi, C. and Hafizi, M. and Hanlon, L. and Hjorth, J. and Izzo, L. and Kiss, L. and Kumar, P. and Kuvvetli, I. and Lavagna, M. and Li, T. and Longo, F. and Lyutikov, M. and Maio, U. and Maiorano, E. and Malcovati, P. and Malesani, D. and Margutti, R. and Martin-Carrillo, A. and Masetti, N. and McBreen, S. and Mignani, R. and Morgante, G. and Mundell, C. and Nargaard-Nielsen, H.U. and Nicastro, L. and Palazzi, E. and Paltani, S. and Panessa, F. and Pareschi, G. and Pe'er, A. and Penacchioni, A.V. and Pian, E. and Piedipalumbo, E. and Piran, T. and Rauw, G. and Razzano, M. and Read, A. and Rezzolla, L. and Romano, P. and Ruffini, R. and Savaglio, S. and Sguera, V. and Schady, P. and Skidmore, W. and Song, L. and Stanway, E. and Starling, R. and Topinka, M. and Troja, E. and van Putten, M. and Vanzella, E. and Vercellone, S. and Wilson-Hodge, C. and Yonetoku, D. and Zampa, G. and Zampa, N. and Zhang, B. and Zhang, B.B. and Zhang, S. and Zhang, S.-N. and Antonelli, A. and Bianco, F. and Boci, S. and Boer, M. and Botticella, M.T. and Boulade, O. and Butler, C. and Campana, S. and Capitanio, F. and Celotti, A. and Chen, Y. and Colpi, M. and Comastri, A. and Cuby, J.-G. and Dadina, M. and De Luca, A. and Dong, Y.-W. and Ettori, S. and Gandhi, P. and Geza, E. and Greiner, J. and Guiriec, S. and Harms, J. and Hernanz, M. and Hornstrup, A. and Hutchinson, I. and Israel, G. and Jonker, P. and Kaneko, Y. and Kawai, N. and Wiersema, K. and Korpela, S. and Lebrun, V. and Lu, F. and MacFadyen, A. and Malaguti, G. and Maraschi, L. and Melandri, A. and Modjaz, M. and Morris, D. and Omodei, N. and Paizis, A. and Páta, P. and Petrosian, V. and Rachevski, A. and Rhoads, J. and Ryde, F. and Sabau-Graziati, L. and Shigehiro, N. and Sims, M. and Soomin, J. and Szécsi, D. and Urata, Y. and Uslenghi, M. and Valenziano, L. and Vianello, G. and Vojtech, S. and Watson, D. and Zicha, J.
Subjects: Ionization, Atmospheric Science, cosmological model, Cherenkov Telescope Array, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astronomy, Dark age, MASSIVE SINGLE STARS, Star formation rates, Gamma ray, 01 natural sciences, Cosmology: observation, localization, law.invention, Astrophysic, Einstein Telescope, observational cosmology, law, Observational cosmology, Re-ionization, Cosmology: observations, Dark ages, First stars, Gamma-ray: bursts, LIGO, observations [Cosmology], Telescope, 010303 astronomy & astrophysics, High sensitivity, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Multi-wavelength, energy: high, sezele, gamma-ray bursts, Aerospace Engineering, Space and Planetary Science, Astrophysics::Instrumentation and Methods for Astrophysics, imaging, star: formation, burst [Gamma-ray], observatory, Geophysics, X rays, Cosmology: observation, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, signature, Star, TIDAL DISRUPTION, Gamma-ray: burst, Astrophysics::High Energy Astrophysical Phenomena, SIMILAR-TO 6, Socio-culturale, FOS: Physical sciences, observation [Cosmology], galaxy: luminosity, X-ray astronomy: instrumentation, 7 CANDIDATE GALAXIES, Astrophysics::Cosmology and Extragalactic Astrophysics, gamma ray: burst, 114 Physical sciences, Settore FIS/03 - Fisica della Materia, X-ray, bursts [Gamma-ray], FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, First star, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], KAGRA, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, LIGHT CURVES, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation, Astronomy and Astrophysics, 115 Astronomy, Space science, redshift, sensitivity, Redshift, NEUTRON-STAR MERGER, messenger, VIRGO, electromagnetic, LUMINOSITY FUNCTION, BLACK-HOLE, General Earth and Planetary Sciences, Gamma-ray burst, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: THESEUS is a space mission concept aimed at exploiting Gamma-Ray Bursts for investigating the early Universe and at providing a substantial advancement of multi-messenger and time-domain astrophysics. These goals will be achieved through a unique combination of instruments allowing GRB and X-ray transient detection over a broad field of view (more than 1sr) with 0.5¿1 arcmin localization, an energy band extending from several MeV down to 0.3¿keV and high sensitivity to transient sources in the soft X-ray domain, as well as on-board prompt (few minutes) follow-up with a 0.7¿m class IR telescope with both imaging and spectroscopic capabilities. THESEUS will be perfectly suited for addressing the main open issues in cosmology such as, e.g., star formation rate and metallicity evolution of the inter-stellar and intra-galactic medium up to redshift 10, signatures of Pop III stars, sources and physics of re-ionization, and the faint end of the galaxy luminosity function. In addition, it will provide unprecedented capability to monitor the X-ray variable sky, thus detecting, localizing, and identifying the electromagnetic counterparts to sources of gravitational radiation, which may be routinely detected in the late ¿20s/early ¿30s by next generation facilities like aLIGO/ aVirgo, eLISA, KAGRA, and Einstein Telescope. THESEUS will also provide powerful synergies with the next generation of multi-wavelength observatories (e.g., LSST, ELT, SKA, CTA, ATHENA).© 2018 COSPAR, S.E. acknowledges the financial support from contracts ASI-INAF 1/009/10/0, NARO15 ASI-INAF 1/037/12/0 and ASI 2015-046-R.0. R.H. acknowledges GACR grant 13-33324S. S.V. research leading to these results has received funding from the European Union's Seventh Framework Programme for research, technological development and demonstration under grant agreement no 606176. D.S. was supported by the Czech grant 1601116S GA CR. Maria Giovanna Dainotti acknowledges funding from the European Union through the Marie Curie Action FP7-PEOPLE-2013-IOF, under grant agreement No. 626267 (>Cosmological Candles>).
Published: 2018

25. XIV Convegno Annuale de 'Il linguaggio della Ricerca' (LdR)

Author: 09/11/2017 LdR - Chairs del Convegno: Armida Torreggiani e Greta Varchi 10/11/2017 LdR Junior - Chairs del Convegno: Giovanna Sotgiu e Mirko Seri Comitato Organizzatore: Annalisa Aluigi, Luca Bellucci, Marica Canino, Alessandra Degli Esposti, Laura Favaretto, Daria Guidetti, Ilse Manet, Francesco Manoli, Giancarlo Marconi, Mauro Orlandini, Sara Ricciardi, Ornella Russo, Emanuela Saracino, Mirko Seri, Giovanna Sotgiu, Armida Torreggiani, Greta Varchi, Alberto Zanelli, Francesco Piazzi. Supporto tecnico-organizzativo: Silvano Favaretto, Giorgio Longino, Maurizio Minghetti, Fabio Testi, Giovanna Balzani, and Tiziana Cremonini
Subjects: ricerca-scuola, divulgazione scientifica, alternanza scuola-lavoro
Abstract: Relazione sul XIV Convegno del progetto di divulgazione scientifica "Il linguaggio della Ricerca" (LdR).
Published: 2017

26. The radiation environment in a low earth orbit:the case of BeppoSAX

Author: Filippo Frontera, Ettore Del Monte, Mauro Orlandini, Riccardo Campana, and Marco Feroci
Subjects: Physics, Low altitude, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radiation, Geophysics (physics.geo-ph), South Atlantic Anomaly, Physics - Geophysics, symbols.namesake, Low earth orbit, Space and Planetary Science, Van Allen radiation belt, Physics::Space Physics, symbols, Satellite, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics::Atmospheric and Oceanic Physics, Geocentric orbit
Abstract: Low-inclination, low altitude Earth orbits (LEO) are of increasing importance for astrophysical satellites, due to their low background environment. Here, the South Atlantic Anomaly (SAA) is the region with the highest amount of radiation. We study the radiation environment in a LEO (500-600 km altitude, 4 degrees inclination) through the particle background measured by the Particle Monitor (PM) experiment onboard the BeppoSAX satellite, between 1996 and 2002. Using time series of particle count rates measured by PM we construct intensity maps and derive SAA passage times and fluences. The low-latitude SAA regions are found to have an intensity strongly decreasing with altitude and dependent on the magnetic rigidity. The SAA extent, westward drift and strength vs altitude is shown., Comment: 16 pages, 12 figures. Accepted for publication in Experimental Astronomy
Published: 2014

27. Spectral evolution of the X-ray nova XTE J1859+226 during its outburst observed by BeppoSAX and RXTE

Author: C. Lombardi, Mauro Orlandini, Ruben Farinelli, Lorenzo Amati, Raffaella Landi, Catherine Brocksopp, N. Shaposhnikov, F. Frontera, Eliana Palazzi, and N. Masetti
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Jet (fluid), Photon, Accretion (meteorology), Astrophysics::High Energy Astrophysical Phenomena, X-ray, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Nova (laser), Astrophysics, Luminosity, Root mean square, Space and Planetary Science, Radiative transfer, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report results of an extensive analysis of the X-ray nova XTE J1859+226 observed with BeppoSAX and RXTE during its 1999 outburst. We modelled the source spectrum with a multicolour blackbody-like feature plus the generic Comptonization model BMC which has the advantage of providing spectral description of the emitted-radiation properties without assumptions on the underlying physical process. The multicolour component is attributed to the geometrically thin accretion disk, while the Comptonization spectrum is claimed to originate in the innermost sub-Keplerian region of the system (transition layer). We find that XTE J1859+226 covers all the spectral states typical of black-hole sources during its evolution across the outburst, however during the very high state, when the disk contribution to the total luminosity is more than 70% and the root mean square variability > 5%, the high-energy photon index is closer to a hard state value (Gamma ~ 1.8). The BMC normalization and photon index Gamma well correlate with the radio emission, and we also observed a possible saturation effect of Gamma at the brightest radio emission levels. A strong positive correlation was found between the fraction of Comptonized seed photons and the observed integrated root mean square variability, which strengthens the idea that most of the fast variability in these systems is provided by the innermost Compton cloud, which may be also identified as a jet., 12 pages, 8 figures, accepted for publication in MNRAS
Published: 2012

28. Average power density spectrum of Swift long gamma-ray bursts in the observer and in the source-rest frames

Author: Raffaella Margutti, Lorenzo Amati, Mauro Orlandini, M. Stamatikos, Sergio Campana, Gianpiero Tagliaferri, C. Guidorzi, and P. Romano
Subjects: Physics, Rest (physics), Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Astrophysics, Observer (special relativity), Rest frame, Redshift, law.invention, Telescope, Space and Planetary Science, law, Gamma-ray burst, Energy (signal processing), Power density
Abstract: We calculate the average power density spectra (PDS) of 244 long gamma-ray bursts detected with the Swift Burst Alert Telescope in the 15-150 keV band from January 2005 to August 2011. For the first time we derived the average PDS in the source rest frame of 97 GRBs with known redshift. For 49 of them an average PDS was also obtained in a common source-frame energy band to account for the dependence of time profiles on energy. Previous results obtained on BATSE GRBs with unknown redshift showed that the average spectrum in the 25-2000 keV band could be modelled with a power-law with a 5/3 index over nearly two decades of frequency with a break at ~1 Hz. Depending on the normalisation and on the subset of GRBs considered, our results show analogous to steeper slopes (between 1.7 and 2.0) of the power-law. However, no clear evidence for the break at ~1 Hz was found, although the softer energy band of BAT compared with BATSE might account for that. We instead find a break at lower frequency corresponding to a typical source rest frame characteristic time of a few seconds. We furthermore find no significant differences between observer and source rest frames. Notably, no distinctive PDS features are found for GRBs with different intrinsic properties of the prompt emission either. Finally, the average PDS of GRBs at higher redshifts shows possibly shallower power-law indices than that of low-z GRBs. It is not clear whether this is due to an evolution with z of the average PDS.
Published: 2012

29. The Large Area Detector of LOFT: the Large Observatory for X-ray Timing

Author: Dom Walton, Claudio Labanti, J.-Y. Seyler, Philipp Azzarello, E. Del Monte, C. Feldman, G.W. Fraser, Giuseppe Bertuccio, Martino Marisaldi, Enrico Bozzo, Slawomir Suchy, A. Rachevski, C. Tenzer, M. Ahangarianabhari, Andrea Santangelo, Fabio Muleri, M. Hailey, P. Cais, Adrian Martindale, Silvia Zane, Mauro Orlandini, N. Zampa, A. Vacchi, S. Di Cosimo, G. Zampa, Marco Barbera, Martin Pohl, Phil Uttley, I. Donnarumma, Y. Evangelista, Berend Winter, L. Bradley, René Hudec, D. Macera, A. de Rosa, Marco Grassi, T. Kennedy, Teresa Mineo, Y. Favre, Christian Schmid, V. Petracek, P. Bodin, J. W. den Herder, Paul S. Smith, Alain Cros, A. Argan, Marco Feroci, Luigi Pacciani, J. Coker, Piero Malcovati, M. Nowak, Didier Barret, Emanuele Perinati, Paolo Soffitta, Franck Cadoux, F. Fuschino, Riccardo Campana, Jörn Wilms, Giuseppe Baldazzi, Zane, S., Walton, D., Kennedy, T., Feroci, M., Den Herder, J., Ahangarianabhari, M., Argan, A., Azzarello, P., Baldazzi, G., Barbera, M., Barret, D., Bertuccio, G., Bodin, P., Bozzo, E., Bradley, L., Cadoux, F., Cais, P., Campana, R., Coker, J., Cros, A., Del Monte, E., De Rosa, A., Di Cosimo, S., Donnarumma, I., Evangelista, Y., Favre, Y., Feldman, C., Fraser, G., Fuschino, F., Grassi, M., Hailey, M., Hudec, R., Labanti, C., Malcovati, P., Macera, D., Marisaldi, M., Martindale, A., Mineo, T., Muleri, F., Nowak, M., Orlandini, M., Pacciani, L., Perinati, E., Petracek, V., Pohl, M., Rachevski, A., Smith, P., Santangelo, A., Seyler, J., Schmid, C., Soffitta, P., Suchy, S., Tenzer, C., Uttley, P., Vacchi, A., Zampa, G., Zampa, N., Wilms, J., Winter, B., Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), FORMATION STELLAIRE 2014, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Interactions et dynamique des environnements de surface (IDES), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Observatories, Sensors, X-rays, Equipment and services, X-ray sources, Computer science, FOS: Physical sciences, 01 natural sciences, 7. Clean energy, X-ray, Loft, Observatory, Range (aeronautics), 0103 physical sciences, Electronic, Timing, Optical and Magnetic Materials, Electrical and Electronic Engineering, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Compact Objects, Electronic, Optical and Magnetic Materials, Condensed Matter Physics, Computer Science Applications1707 Computer Vision and Pattern Recognition, Applied Mathematics, Remote sensing, Millisecond, 010308 nuclear & particles physics, Large area detector, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Neutron star, Astrophysics - Instrumentation and Methods for Astrophysics, astro-ph.IM
Abstract: LOFT (Large Observatory for X-ray Timing) is one of the five candidates that were considered by ESA as an M3 mission (with launch in 2022-2024) and has been studied during an extensive assessment phase. It is specifically designed to perform fast X-ray timing and probe the status of the matter near black holes and neutron stars. Its pointed instrument is the Large Area Detector (LAD), a 10 m 2 -class instrument operating in the 2-30keV range, which holds the capability to revolutionise studies of variability from X-ray sources on the millisecond time scales. The LAD instrument has now completed the assessment phase but was not down-selected for launch. However, during the assessment, most of the trade-offs have been closed leading to a robust and well documented design that will be re- proposed in future ESA calls. In this talk, we will summarize the characteristics of the LAD design and give an overview of the expectations for the instrument capabilities., Proc. SPIE 9144, Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray, 91442W
Published: 2015

30. Temperature Measurement during Thermonuclear X-ray Bursts with BeppoSAX

Author: Aru Beri, Mauro Orlandini, Chandreyee Maitra, Biswajit Paul, ITA, and IND
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Thermonuclear fusion, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, X-ray, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radius, 01 natural sciences, Standard technique, Temperature measurement, Space and Planetary Science, 0103 physical sciences, Black-body radiation, Time-resolved spectroscopy, Absorption (electromagnetic radiation), Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Instrumentation, 0105 earth and related environmental sciences
Abstract: We have carried out a study of temperature evolution during thermonuclear bursts in LMXBs using broad band data from two instruments onboard BeppoSAX, the MECS and the PDS. However, instead of applying the standard technique of time resolved spectroscopy, we have determined the temperature in small time intervals using the ratio of count rates in the two instruments assuming a blackbody nature of burst emission and different interstellar absorption for different sources. Data from a total of twelve observations of six sources were analysed during which 22 bursts were detected. We have obtained temperatures as high as ~3.0 keV, even when there is no evidence of photospheric radius expansion. These high temperatures were observed in the sources within different broadband spectral states (soft and hard)., Comment: To appear in New Astronomy
Published: 2015
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31. Searching for serendipitous sources at high galactic latitudes with BeppoSAX/PDS

Author: Lorenzo Amati, Loredana Bassani, Angela Malizia, Raffaella Landi, and Mauro Orlandini
Subjects: Physics, Atmospheric Science, High energy, Active galactic nucleus, Aerospace Engineering, Astronomy, Broad band, Astronomy and Astrophysics, Field of view, Astrophysics, Latitude, Geophysics, Space and Planetary Science, General Earth and Planetary Sciences, Spectral analysis, Systematic search
Abstract: Performing a systematic search in the BeppoSAX archive for high energy (15–100 keV) serendipitous sources at high galactic latitudes (|b| ⩾ 13°), we defined a sample of 12 regions in which the PDS/MECS cross-calibration constant, resulting from the fit of the target source with a simple power law, is substantially higher than the nominal value of 0.75–0.95 estimated from instrument intercalibration. This is probably due to the presence of a serendipitous source in the PDS field of view which is contaminating the PDS spectrum of the pointed source. This approach allowed us to find new six hard X-ray emitting sources (PKS 2356-611, 2MASX J14585116-1652223, NGC 1566, NGC 7319, PKS 0101-649 and ESO 025-G002), which are the object of this work. In two fields, the likely candidate contaminating sources are present in the MECS field of view; for these sources we have performed a broad band (1.5–100 keV) spectral analysis. In the remaining four cases, the identification of the source likely to provide the emission detected by the PDS is based on the search in high energy catalogs.
Published: 2006

32. A study of an orbital cycle of GX 301–2 observed by BeppoSAX

Author: I. Kreykenbohm, A. La Barbera, Alberto Segreto, Andrea Santangelo, and Mauro Orlandini
Subjects: Physics, Scattering, Astrophysics::High Energy Astrophysical Phenomena, Cyclotron, Cyclotron resonance, X-ray binary, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Accretion (astrophysics), law.invention, Neutron star, Pulsar, Space and Planetary Science, law, Emission spectrum
Abstract: In this paper we report on the 4-80 keV wide-band X-ray spectrum of the High Mass X-ray Binary GX 301-2 observed by the BeppoSAX satellite during an extended monitoring campaign in 1998. The source was observed at 4 different orbital phases corresponding to diverse luminosity states. The 4-80 keV continuum is described well by the multi component partial-covering absorber model corrected by a high energy cutoff. In addition to the Kα (at ∼6.4 keV) iron emission fluorescence line, the Kβ (at ∼7 keV) was observed together with an absorption-like feature at hard energies that we interpret as a cyclotron resonance scattering feature (CRSF). Both the continuum and the CRSF show clear dependence on the orbital phase. This is likely to be caused by the variation in the luminosity with the orbit, even if the resulting relation between cyclotron energy and luminosity is difficult to interpret within the present one-dimensional models of accretion columns. In fact, when the neutron star is close to periastron and the system is in a low luminosity state (Lx ∼ 0.8 × 10 37 erg/s for an assumed distance of 1.8 kpc), the CRSF centroid energy is observed at ∼45 keV, while at orbital phase ∼0.9 (at a maximum luminosity of ∼2 × 10 37 erg/s) it is 53 keV in contrast with predictions. The cyclotron energy is also found to vary with the pulse phase, asymmetrically with respect to the pulse profile. Consequences for the geometry of the magnetic field are finally discussed.
Published: 2005

33. Confirmation of the Presence of Nonthermal Hard X-Ray Excess in the Cluster A2256 from Two Epoch Observations

Author: Mauro Orlandini, Raffaella Landi, and Roberto Fusco-Femiano
Subjects: Physics, Range (particle radiation), Space and Planetary Science, Epoch (astronomy), Coma Cluster, X-ray, Cluster (physics), Flux, Astronomy and Astrophysics, Thermal emission, Astrophysics, Spectral line
Abstract: After confirmation of the presence of a nonthermal hard X-ray excess with respect to the thermal emission in the Coma cluster from two independent observations, obtained using the Phoswich Detection System onboard BeppoSAX, we present in this Letter also for Abell 2256 the results of two observations performed with a time interval of about 2.5 yr. In both spectra a nonthermal excess is present at a confidence level of ~3.3sigma and ~3.7sigma, respectively. The combined spectrum obtained by adding up the two spectra allows to measure an excess at the level of ~4.8sigma in the 20-80 keV energy range. The nonthermal X-ray flux is in agreement with the published value of the first observation (Fusco-Femiano et al. 2000) and with that measured by a Rossi X-Ray Timing Explorer observation (Rephaeli & Gruber 2003).
Published: 2005

34. The Prompt X‐Ray Emission of GRB 011211: Possible Evidence of a Transient Absorption Feature

Author: E. Costa, J. J. M. in 't Zand, F. Frontera, M. Vietri, Mauro Orlandini, L. Piro, M. Feroci, Enrico Montanari, Arieh Königl, Davide Lazzati, Lorenzo Amati, C. Guidorzi, and Elena Pian
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift, Afterglow, Gamma Rays: Bursts, X-Rays: General, Space and Planetary Science, Feature (computer vision), Ultrafast laser spectroscopy, Emission spectrum, Gamma Rays: Observations, Gamma-ray burst, Event (particle physics), Equivalent width
Abstract: We report on observation results of the prompt X- and gamma-ray emission from GRB011211. This event was detected with the Gamma-Ray Burst Monitor and one of the Wide Field Cameras aboard the BeppoSAX satellite. The optical counterpart to the GRB was soon identified and its redshift determined (z = 2.140), while with the XMM-Newton satellite, the X-ray afterglow emission was detected. Evidence of soft X-ray emission lines was reported by Reeves et al. (2002), but not confirmed by other authors. In investigating the spectral evolution of the prompt emission we find the possible evidence of a transient absorption feature at 6.9^{+0.6}_{-0.5} keV during the rise of the primary event. The significance of the feature is derived with non parametric tests and numerical simulations, finding a chance probability which ranges from 3x10^{-3} down to 4x10^{-4}. The feature shows a Gaussian profile and an equivalent width of 1.2^{+0.5}_{-0.6} keV. We discuss our results and their possible interpretation., 23 pages, 3 Tables, 6 Figures. Accepted for publication in Astrophysical Journal
Published: 2004

35. Confirmation of Nonthermal Hard X-Ray Excess in the Coma Cluster from Two Epoch Observations

Author: Gianfranco Brunetti, Giancarlo Setti, Luigina Feretti, Gabriele Giovannini, Mauro Orlandini, Roberto Fusco-Femiano, Paola Grandi, FUSCOFEMIANO R., ORLANDINI M., BRUNETTI G., FERETTI L., GIOVANNINI G., GRANDI P., and SETTI G.
Subjects: Physics, Astrophysics (astro-ph), X-ray, FOS: Physical sciences, Sigma, Astronomy and Astrophysics, Astrophysics, Thermal emission, Spectral line, Space and Planetary Science, Thermal, Coma Cluster, BL Lac object
Abstract: We report the hard X-ray spectrum of the Coma cluster obtained using the PDS data of two independent BeppoSAX observations performed with a time interval of about three years. In both the spectra a non thermal excess with respect to the thermal emission is present at a confidence level of ~ 3.4 sigma. The combined spectrum obtained by adding up the two spectra allows a measurement of the excess at the level of ~ 4.8 sigma at energies above 20 keV. The analysis of the full BeppoSAX data set provides a revised non-thermal X-ray flux which is slightly lower than that previously estimated (Fusco-Femiano et al. 1999) and in agreement with that measured by two RXTE observations. The analysis of the offset fields in our Coma observations provides a possible flux determination of the BL Lac object 1ES 1255+244., Comment: 14 Pages, 1 figure. Accepted for publication on ApJ Letters
Published: 2004

36. The Large Observatory For x-ray Timing

Author: Antonios Manousakis, S. Boutloukos, F. Zwart, Jose M. Torrejon, C. Pittori, Alessandro Drago, Dieter H. Hartmann, Feryal Özel, T. J. L. Courvoisier, Tim Johannsen, Jordi José, M. Michalska, Christian Schmid, I. Rashevskaya, Gottfried Kanbach, V. Petracek, L. Bradley, Allan Hornstrup, M. H. Erkut, Sergio Campana, Rudy Wijnands, Andrew Cumming, Nils Andersson, Tomaso Belloni, M. C. Miller, Roman Wawrzaszek, Stefano Bianchi, Enrique García-Berro, Sandro Mereghetti, C. Guidorzi, C. Corral Van Damme, Søren Brandt, Francesco Tombesi, Felix Ryde, Didier Barret, Simon Vaughan, Marco Feroci, T. Di Salvo, C. van Baren, Angelo Antonelli, Marc Ribó, J. L. Atteia, P. Soleri, Alessio Trois, Silvia Zane, G. Mouret, Ersin Gogus, Emanuele Perinati, J. Coker, Piero Malcovati, V. Mangano, F. Jetter, P. Uter, P. Romano, M. Nowak, Roberto Turolla, Laura Tolos, Antonino D'Ai, Laura Alvarez, C. Amoros, Simone Scaringi, A. Possenti, David M. Smith, M. Falanga, A. Goldwurm, René Hudec, Ignacio Negueruela, M. van der Klis, Francesco Longo, José A. Pons, I. M. McHardy, R. Rohlfs, P. Cais, Luigi Stella, S. Di Cosimo, Antoine Rousseau, M. Ayre, M. Gschwender, D. Klochkov, Niels Lund, Chryssa Kouveliotou, P. Azzarello, F. Château, Michael Gabler, S. Vercellone, Martin Durant, I. Donnarumma, Giorgio Matt, Mauro Orlandini, P. Kaaret, Patrick Smith, P. T. O'Brien, A. Argan, M. Orienti, Marco Grassi, Claudio Labanti, Edward F. Brown, Christopher S. Reynolds, Gloria Sala, Y. Evangelista, Gabriel Török, José Braga, Riccardo Campana, Alan Smith, C. Gouiffes, Nevin N. Weinberg, Leonardo Gualtieri, Yannick Favre, P.G. Jonker, Gabriele Giovannini, D. de Martino, Irfan Kuvvetli, S. Motta, Teresa Mineo, Paul J. Groot, Pablo Reig, Martino Marisaldi, Andrea Sanna, Lorenzo Amati, G. L. Israel, D. Macera, K. S. Wood, Pablo Cerdá-Durán, F. Fuschino, Suvi Gezari, Mariano Mendez, Slawomir Suchy, Damien Rambaud, Nanda Rea, R. Artigue, J.-Y. Seyler, S. N. Shore, Frederick K. Lamb, Jörn Wilms, Mark G. Alford, Margarita Hernanz, Thomas M. Tauris, Luca Izzo, Tobias Boenke, J. J. M. in 't Zand, J. Mulačová, P. Binko, Daniel Maier, Jan Schee, Bruce Gendre, Enrico Bozzo, Paul S. Ray, Giuseppe Bertuccio, Simone Migliari, Ignazio Bombaci, Vladimir Karas, Nikolaos Stergioulas, P. P. Laubert, D. Karelin, A. C. Fabian, Giovanni Miniutti, Dacheng Lin, L. Guy, Martine Mouchet, Colleen A. Wilson-Hodge, Valeria Ferrari, Kai Hebeler, Mark H. Finger, Shigeto Watanabe, Pawel Haensel, H. Jacobs, Adrian Martindale, A. A. Zdziarski, Andrea Santangelo, Giuseppe Baldazzi, Piergiorgio Casella, Fabio Muleri, M. Hailey, Antonio Bianchini, Giuseppe Lodato, E. Del Monte, M. Rapisarda, Zdeněk Stuchlík, Alain Cros, V. Sochora, Laurens Keek, Jorge Casares, Andrew Melatos, Pere Blay, E. Rossi, A. P. Spencer, G. Stratta, Conrado Albertus, J. M. Paredes, M. Ahangarianabhari, Anna L. Watts, M. Del Santo, I. Kreykenbohm, Alessandro Patruno, G. A. Caliandro, C. Feldman, M. Pohl, Fabrizio Tamburini, G. Zampa, Marina Orio, Flemming Hansen, P. Ramon, Ruben Salvaterra, David H. Lumb, Edward M. Cackett, Andrew Shearer, Sharon M. Morsink, L. Pacciani, J.-M. Bonnet Bidaud, A. De Luca, Jérôme Chenevez, Sebastian Diebold, N. Zampa, Carole A. Haswell, Luciano Burderi, E. Cavazzuti, Adam Ingram, Dhiren Kataria, Berend Winter, A. Vacchi, W. Hermsen, P. Giommi, Dong Lai, N. A. Webb, P. Bodin, Dom Walton, Solen Balman, Benjamin Stappers, M. Burgay, Luca Zampieri, Carl Budtz-Jørgensen, Ralph A. M. J. Wijers, Giancarlo Cusumano, J. L. Galvez Sanchez, Raffaella Schneider, Luciano Rezzolla, Alexander Heger, S. Korpela, Dimitrios Emmanoulopoulos, Biswajit Paul, Diego Götz, B. Artigues, Paolo Soffitta, M. H. Finger, J. W. den Herder, Paolo Esposito, Kazushi Iwasawa, Poul Erik Holmdahl Olsen, J. Neilsen, Marco Barbera, Deepto Chakrabarty, R. A. Osten, M. Reina Aranda, A. J. Castro-Tirado, Andrea Tramacere, D. Haas, Johannes Dercksen, John A. Tomsick, A. V. Penacchioni, V. D'Elia, Alfonso Collura, Altan Baykal, P. Le Provost, S. Turriziani, Kostas D. Kokkotas, Duncan K. Galloway, Ron Remillard, Juhani Huovelin, Somak Bhattacharyya, Pavel Bakala, Phil Uttley, Richard E. Cole, Mahesh Prakash, L. Kuiper, T. Munoz-Darias, Diego F. Torres, S. Mahmoodifar, G. Ramsay, Andrew Norton, T. Kennedy, Achim Schwenk, L. Zdunik, A. B. Giles, Jerome Rodriguez, C. Motch, Ilya Mandel, Marcello Giroletti, Dimitrios Psaltis, J. Sandberg, Fiamma Capitanio, Remon Cornelisse, M. R. Gilfanov, Peggy Varniere, Franck Cadoux, Peter J. Wheatley, M. de Pasquale, Juri Poutanen, S. Maestre, A. Pellizzoni, Axel Schwope, Diego Altamirano, Piotr Orleanski, V. Vrba, Agata Różańska, Kateřina Goluchová, P. Rodríguez Gil, Niccolò Bucciantini, Stéphane Schanne, Carlo Ferrigno, Thomas J. Maccarone, H. Wende, Tod E. Strohmayer, Tadayuki Takahashi, Francois Lebrun, E. Kuulkers, Jeroen Homan, Maurizio Paolillo, M. A. Perez, J. P. Osborne, A. Alpar, Sanjay Reddy, G.W. Fraser, V. Sulemainov, D. Linder, L. Sabau-Graziati, A. Rachevski, Bing Zhang, Alessandro Papitto, C. Tenzer, Alex Markowitz, J. Portell, Roberto Mignani, Fabrizio Bocchino, Arnau Rios, R. de la Rie, M. Wille, A. de Rosa, Alessandro Riggio, M. Frericks, Andrew W. Steiner, Michal Bursa, Federico Bernardini, Jon M. Miller, W. Kluzniak, INAF - Osservatorio Astronomico di Roma ( OAR ), Istituto Nazionale di Astrofisica ( INAF ), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées ( LATT ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Variable Energy Cyclotron Centre, Institut Pasteur de Montevideo, Réseau International des Instituts Pasteur ( RIIP ) -Institut Pasteur de Montevideo, Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), FORMATION STELLAIRE 2014, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux ( L3AB ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire aquitain des sciences de l'univers ( OASU ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ), Instituto de Astrofísica de Andalucía ( IAA ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Interactions et dynamique des environnements de surface ( IDES ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Licryl Laboratory ( CNR-IPCF UOS Cosenza ), University of Calabria, Laboratori Nazionali di Frascati ( LNF ), National Institute for Nuclear Physics ( INFN ), PCAS, Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano ( IASF-MI ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), Canada's National Laboratory for Particle and Nuclear Physics ( TRIUMF ), NRC, Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] ( UNIBO ), Institut de recherches sur la catalyse et l'environnement de Lyon ( IRCELYON ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Univers et Théories ( LUTH ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Spectrochimie Infrarouge et Raman - UMR 8516 ( LASIR ), Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Dipartimento di Scienze Fisiche [Naples], Università degli studi di Napoli Federico II, Energétique, propulsion, espace, environnement ( EPEE ), Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Physics and Astronomy [Hanover], Dartmouth College [Hanover], Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d’Optique Atmosphérique - UMR 8518 ( LOA ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Institut de Biologie du Développement de Marseille ( IBDM ), Aix Marseille Université ( AMU ) -Institut National de la Santé et de la Recherche Médicale ( INSERM ) -Centre National de la Recherche Scientifique ( CNRS ), Universitat Politècnica de Catalunya [Barcelona] ( UPC ), INAF-IASF Milano, Climate and Environmental Physics [Bern], University of Bern, Centre National d'Etudes Spatiales ( CNES ), Institute of Geology, Eidgenössische Technische Hochschule [Zürich] ( ETH Zürich ), IEEC-CSIC, Universitat Autònoma de Barcelona [Barcelona] ( UAB ), MedisysResearch Lab ( Medisys ), Philips Research, European Space Astronomy Center ( ESAC ), European Space Agency ( ESA ), High Energy Astrophys. & Astropart. Phys (API, FNWI), INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Réseau International des Instituts Pasteur (RIIP), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Interactions et dynamique des environnements de surface (IDES), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Licryl Laboratory (CNR-IPCF UOS Cosenza), Università della Calabria [Arcavacata di Rende] (Unical), Laboratori Nazionali di Frascati (LNF), Istituto Nazionale di Fisica Nucleare (INFN), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Canada's particle accelerator centre (TRIUMF), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut de recherches sur la catalyse et l'environnement de Lyon (IRCELYON), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Laboratoire Avancé de Spectroscopie pour les Intéractions la Réactivité et l'Environnement - UMR 8516 (LASIRE), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), University of Naples Federico II = Università degli studi di Napoli Federico II, Energétique, propulsion, espace, environnement (EPEE), Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Laboratoire d’Optique Atmosphérique - UMR 8518 (LOA), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Institut de Biologie du Développement de Marseille (IBDM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Universitat Politècnica de Catalunya [Barcelona] (UPC), Climate and Environmental Physics [Bern] (CEP), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE)-Universität Bern [Bern] (UNIBE), Centre National d'Études Spatiales [Toulouse] (CNES), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Universitat Autònoma de Barcelona (UAB), MedisysResearch Lab (Medisys), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), SPIE, Takahashi, Tadayuki, Feroci M., Den Herder J.W., Bozzo E., Barret D., Brandt S., Hernanz M., Van Der Klis M., Pohl M., Santangelo A., Stella L., Watts A., Wilms J., Zane S., Ahangarianabhari M., Albertus C., Alford M., Alpar A., Altamirano D., Alvarez L., Amati L., Amoros C., Andersson N., Antonelli A., Argan A., Artigue R., Artigues B., Atteia J.-L., Azzarello P., Bakala P., Baldazzi G., Balman S., Barbera M., Van Baren C., Bhattacharyya S., Baykal A., Belloni T., Bernardini F., Bertuccio G., Bianchi S., Bianchini A., Binko P., Blay P., Bocchino F., Bodin P., Bombaci I., Bonnet Bidaud J.-M., Boutloukos S., Bradley L., Braga J., Brown E., Bucciantini N., Burderi L., Burgay M., Bursa M., Budtz-Jorgensen C., Cackett E., Cadoux F.R., Cais P., Caliandro G.A., Campana R., Campana S., Capitanio F., Casares J., Casella P., Castro-Tirado A.J., Cavazzuti E., Cerda-Duran P., Chakrabarty D., Chateau F., Chenevez J., Coker J., Cole R., Collura A., Cornelisse R., Courvoisier T., Cros A., Cumming A., Cusumano G., D'ai A., D'elia V., Del Monte E., De Luca A., De Martino D., Dercksen J.P.C., De Pasquale M., De Rosa A., Del Santo M., Di Cosimo S., Diebold S., Di Salvo T., Donnarumma I., Drago A., Durant M., Emmanoulopoulos D., Erkut M.H., Esposito P., Evangelista Y., Fabian A., Falanga M., Favre Y., Feldman C., Ferrari V., Ferrigno C., Finger M., Finger M.H., Fraser G.W., Frericks M., Fuschino F., Gabler M., Galloway D.K., Galvez Sanchez J.L., Garcia-Berro E., Gendre B., Gezari S., Giles A.B., Gilfanov M., Giommi P., Giovannini G., Giroletti M., Gogus E., Goldwurm A., Goluchova K., Gotz D., Gouiffes C., Grassi M., Groot P., Gschwender M., Gualtieri L., Guidorzi C., Guy L., Haas D., Haensel P., Hailey M., Hansen F., Hartmann D.H., Haswell C.A., Hebeler K., Heger A., Hermsen W., Homan J., Hornstrup A., Hudec R., Huovelin J., Ingram A., In't Zand J.J.M., Israel G., Iwasawa K., Izzo L., Jacobs H.M., Jetter F., Johannsen T., Jonker P., Jose J., Kaaret P., Kanbach G., Karas V., Karelin D., Kataria D., Keek L., Kennedy T., Klochkov D., Kluzniak W., Kokkotas K., Korpela S., Kouveliotou C., Kreykenbohm I., Kuiper L.M., Kuvvetli I., Labanti C., Lai D., Lamb F.K., Laubert P.P., Lebrun F., Lin D., Linder D., Lodato G., Longo F., Lund N., Maccarone T.J., Macera D., Maestre S., Mahmoodifar S., Maier D., Malcovati P., Mandel I., Mangano V., Manousakis A., Marisaldi M., Markowitz A., Martindale A., Matt G., Mchardy I.M., Melatos A., Mendez M., Mereghetti S., Michalska M., Migliari S., Mignani R., Miller M.C., Miller J.M., Mineo T., Miniutti G., Morsink S., Motch C., Motta S., Mouchet M., Mouret G., Mulaova J., Muleri F., Munoz-Darias T., Negueruela I., Neilsen J., Norton A.J., Nowak M., O'brien P., Olsen P.E.H., Orienti M., Orio M., Orlandini M., Orleaaski P., Osborne J.P., Osten R., Ozel F., Pacciani L., Paolillo M., Papitto A., Paredes J.M., Patruno A., Paul B., Perinati E., Pellizzoni A., Penacchioni A.V., Perez M.A., Petracek V., Pittori C., Pons J., Portell J., Possenti A., Poutanen J., Prakash M., Le Provost P., Psaltis D., Rambaud D., Ramon P., Ramsay G., Rapisarda M., Rachevski A., Rashevskaya I., Ray P.S., Rea N., Reddy S., Reig P., Reina Aranda M., Remillard R., Reynolds C., Rezzolla L., Ribo M., De La Rie R., Riggio A., Rios A., Rodriguez-Gil P., Rodriguez J., Rohlfs R., Romano P., Rossi E.M.R., Rozanska A., Rousseau A., Ryde F., Sabau-Graziati L., Sala G., Salvaterra R., Sanna A., Sandberg J., Scaringi S., Schanne S., Schee J., Schmid C., Shore S., Schneider R., Schwenk A., Schwope A.D., Seyler J.-Y., Shearer A., Smith A., Smith D.M., Smith P.J., Sochora V., Soffitta P., Soleri P., Spencer A., Stappers B., Steiner A.W., Stergioulas N., Stratta G., Strohmayer T.E., Stuchlik Z., Suchy S., Sulemainov V., Takahashi T., Tamburini F., Tauris T., Tenzer C., Tolos L., Tombesi F., Tomsick J., Torok G., Torrejon J.M., Torres D.F., Tramacere A., Trois A., Turolla R., Turriziani S., Uter P., Uttley P., Vacchi A., Varniere P., Vaughan S., Vercellone S., Vrba V., Walton D., Watanabe S., Wawrzaszek R., Webb N., Weinberg N., Wende H., Wheatley P., Wijers R., Wijnands R., Wille M., Wilson-Hodge C.A., Winter B., Wood K., Zampa G., Zampa N., Zampieri L., Zdunik L., Zdziarski A., Zhang B., Zwart F., Ayre M., Boenke T., Corral Van Damme C., Kuulkers E., Lumb D., Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Centrale Lille Institut (CLIL), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Universität Bern [Bern]-Universität Bern [Bern], European Space Agency (ESA), Feroci, M., den Herder, J., Bozzo, E., Barret, D., Brandt, S., Hernanz, M., van der Klis, M., Pohl, M., Santangelo, A., Stella, L., Watts, A., Wilms, J., Zane, S., Ahangarianabhari, M., Albertus, C., Alford, M., Alpar, A., Altamirano, D., Alvarez, L., Amati, L., Amoros, C., Andersson, N., Antonelli, A., Argan, A., Artigue, R., Artigues, B., Atteia, J., Azzarello, P., Bakala, P., Baldazzi, G., Balman, S., Barbera, M., van Baren, C., Bhattacharyya, S., Baykal, A., Belloni, T., Bernardini, F., Bertuccio, G., Bianchi, S., Bianchini, A., Binko, P., Blay, P., Bocchino, F., Bodin, P., Bombaci, I., Bonnet Bidaud, J., Boutloukos, S., Bradley, L., Braga, J., Brown, E., Bucciantini, N., Burderi, L., Burgay, M., Bursa, M., Budtz Jørgensen, C., Cackett, E., Cadoux, F., Caïs, P., Caliandro, G., Campana, R., Campana, S., Capitanio, F., Casares, J., Casella, P., Castro Tirado, A., Cavazzuti, E., Cerda Duran, P., Chakrabarty, D., Château, F., Chenevez, J., Coker, J., Cole, R., Collura, A., Cornelisse, R., Courvoisier, T., Cros, A., Cumming, A., Cusumano, G., D'Ai', A., D'Elia, V., Del Monte, E., de Luca, A., de Martino, D., Dercksen, J., de Pasquale, M., De Rosa, A., Del Santo, M., Di Cosimo, S., Diebold, S., DI SALVO, T., Donnarumma, I., Drago, A., Durant, M., Emmanoulopoulos, D., Erkut, M., Esposito, P., Evangelista, Y., Fabian, A., Falanga, M., Favre, Y., Feldman, C., Ferrari, V., Ferrigno, C., Finger, M., Fraser, G., Frericks, M., Fuschino, F., Gabler, M., Galloway, D., Galvez Sanchez, J., Garcia Berro, E., Gendre, B., Gezari, S., Giles, A., Gilfanov, M., Giommi, P., Giovannini, G., Giroletti, M., Gogus, E., Goldwurm, A., Goluchová, K., Götz, D., Gouiffes, C., Grassi, M., Groot, P., Gschwender, M., Gualtieri, L., Guidorzi, C., Guy, L., Haas, D., Haensel, P., Hailey, M., Hansen, F., Hartmann, D., Haswell, C., Hebeler, K., Heger, A., Hermsen, W., Homan, J., Hornstrup, A., Hudec, R., Huovelin, J., Ingram, A., In't Zand, J., Israel, G., Iwasawa, K., Izzo, L., Jacobs, H., Jetter, F., Johannsen, T., Jonker, P., Josè, J., Kaaret, P., Kanbach, G., Karas, V., Karelin, D., Kataria, D., Keek, L., Kennedy, T., Klochkov, D., Kluzniak, W., Kokkotas, K., Korpela, S., Kouveliotou, C., Kreykenbohm, I., Kuiper, L., Kuvvetli, I., Labanti, C., Lai, D., Lamb, F., Laubert, P., Lebrun, F., Lin, D., Linder, D., Lodato, G., Longo, F., Lund, N., Maccarone, T., Macera, D., Maestre, S., Mahmoodifar, S., Maier, D., Malcovati, P., Mandel, I., Mangano, V., Manousakis, A., Marisaldi, M., Markowitz, A., Martindale, A., Matt, G., Mchardy, I., Melatos, A., Mendez, M., Mereghetti, S., Michalska, M., Migliari, S., Mignani, R., Miller, M., Miller, J., Mineo, T., Miniutti, G., Morsink, S., Motch, C., Motta, S., Mouchet, M., Mouret, G., Mulačová, J., Muleri, F., Muñoz Darias, T., Negueruela, I., Neilsen, J., Norton, A., Nowak, M., O'Brien, P., Olsen, P., Orienti, M., Orio, M., Orlandini, M., Orleański, P., Osborne, J., Osten, R., Ozel, F., Pacciani, L., Paolillo, M., Papitto, A., Paredes, J., Patruno, A., Paul, B., Perinati, E., Pellizzoni, A., Penacchioni, A., Perez, M., Petracek, V., Pittori, C., Pons, J., Portell, J., Possenti, A., Poutanen, J., Prakash, M., Le Provost, P., Psaltis, D., Rambaud, D., Ramon, P., Ramsay, G., Rapisarda, M., Rachevski, A., Rashevskaya, I., Ray, P., Rea, N., Reddy, S., Reig, P., Reina Aranda, M., Remillard, R., Reynolds, C., Rezzolla, L., Ribo, M., de la Rie, R., Riggio, A., Rios, A., Rodríguez Gil, P., Rodriguez, J., Rohlfs, R., Romano, P., Rossi, E., Rozanska, A., Rousseau, A., Ryde, F., Sabau Graziati, L., Sala, G., Salvaterra, R., Sanna, A., Sandberg, J., Scaringi, S., Schanne, S., Schee, J., Schmid, C., Shore, S., Schneider, R., Schwenk, A., Schwope, A., Seyler, J., Shearer, A., Smith, A., Smith, D., Smith, P., Sochora, V., Soffitta, P., Soleri, P., Spencer, A., Stappers, B., Steiner, A., Stergioulas, N., Stratta, G., Strohmayer, T., Stuchlik, Z., Suchy, S., Sulemainov, V., Takahashi, T., Tamburini, F., Tauris, T., Tenzer, C., Tolos, L., Tombesi, F., Tomsick, J., Torok, G., Torrejon, J., Torres, D., Tramacere, A., Trois, A., Turolla, R., Turriziani, S., Uter, P., Uttley, P., Vacchi, A., Varniere, P., Vaughan, S., Vercellone, S., Vrba, V., Walton, D., Watanabe, S., Wawrzaszek, R., Webb, N., Weinberg, N., Wende, H., Wheatley, P., Wijers, R., Wijnands, R., Wille, M., Wilson Hodge, C., Winter, B., Wood, K., Zampa, G., Zampa, N., Zampieri, L., Zdunik, L., Zdziarski, A., Zhang, B., Zwart, F., Ayre, M., Boenke, T., Corral van Damme, C., Kuulkers, E., Lumb, D., Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), National Institute for Nuclear Physics (INFN), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Canada's National Laboratory for Particle and Nuclear Physics (TRIUMF), Università di Bologna [Bologna] (UNIBO), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Spectrochimie Infrarouge et Raman - UMR 8516 (LASIR), Centre National de la Recherche Scientifique (CNRS)-Université de Lille, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Lille, Aix Marseille Université (AMU)-Collège de France (CdF)-Centre National de la Recherche Scientifique (CNRS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Universitat Autònoma de Barcelona [Barcelona] (UAB), Astronomy, den Herder, J. W., Atteia, J. L., Bonnet Bidaud, J. M., Cadoux, F. R., Cais, P., Caliandro, G. A., Castro Tirado, A. J., D'Aì, A., De Luca, A., De Martino, D., Dercksen, J. P. C., De Pasquale, M., Di Salvo, T., Erkut, M. H., Finger, M. H., Fraser, G. W., Galloway, D. K., Galvez Sanchez, J. L., Giles, A. B., Hartmann, D. H., Haswell, C. A., in't Zand, J. J. M., Jacobs, H. M., Kuiper, L. M., Lamb, F. K., Laubert, P. P., Maccarone, T. J., Mchardy, I. M., Miller, M. C., Miller, J. M., Norton, A. J., Olsen, P. E. H., Orleanski, P., Osborne, J. P., Paolillo, Maurizio, Paredes, J. M., Penacchioni, A. V., Perez, M. A., Ray, P. S., Rossi, E. M. R., Schwope, A. D., Seyler, J. Y., Smith, D. M., Smith, P. J., Steiner, A. W., Strohmayer, T. E., Torrejon, J. M., Torres, D. F., and Wilson Hodge, C. A.
Subjects: x-ray and γ-ray instrumentation, compact objects, microchannel plates, X-ray detectors, X-ray imaging, X-ray spectroscopy, X-ray timing, Electronic, Optical and Magnetic Materials, Condensed Matter Physics, Computer Science Applications1707 Computer Vision and Pattern Recognition, Applied Mathematics, Electrical and Electronic Engineering, Vision, Observatories, Field of view, 01 natural sciences, 7. Clean energy, neutron stars, Observatory, 010303 astronomy & astrophysics, Physics, Equipment and services, Astrophysics::Instrumentation and Methods for Astrophysics, Steradian, [ SDU.ASTR.IM ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics - Instrumentation and Methods for Astrophysics, X-ray detector, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Cosmic Vision, Spectral resolution, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, NO, microchannel plate, Settore FIS/05 - Astronomia e Astrofisica, X-rays, compact object, 0103 physical sciences, Electronic, Optical and Magnetic Materials, Instrumentation and Methods for Astrophysics (astro-ph.IM), dense hadronic matter, Sensors, 010308 nuclear & particles physics, Astronomy, Accretion (astrophysics), [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Neutron star, 13. Climate action, [ PHYS.ASTR.IM ] Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Gamma-ray burst, astro-ph.IM
Abstract: The Large Observatory For x-ray Timing (LOFT) was studied within ESA M3 Cosmic Vision framework and participated in the final down-selection for a launch slot in 2022-2024. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument, LOFT will study the behaviour of matter under extreme conditions, such as the strong gravitational field in the innermost regions of accretion flows close to black holes and neutron stars, and the supra-nuclear densities in the interior of neutron stars. The science payload is based on a Large Area Detector (LAD, 10 m 2 effective area, 2-30 keV, 240 eV spectral resolution, 1 deg collimated field of view) and a WideField Monitor (WFM, 2-50 keV, 4 steradian field of view, 1 arcmin source location accuracy, 300 eV spectral resolution). The WFM is equipped with an on-board system for bright events (e.g. GRB) localization. The trigger time and position of these events are broadcast to the ground within 30 s from discovery. In this paper we present the status of the mission at the end of its Phase A study., Proc. SPIE 9144, Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray, 91442T
Published: 2014

37. A Measurement of the Broadband Spectrum of XTE J1118+480 withBeppoSAXand Its Astrophysical Implications

Author: A. N. Parmar, Francesco Haardt, Mauro Orlandini, E. Kuulkers, T. M. Belloni, A. A. Zdziarski, Andrea Santangelo, Ron Remillard, E. Palazzi, Lorenzo Amati, J. Mikolajewska, S. Del Sordo, Luigi Stella, N. Masetti, F. Frontera, Astrophysics, Universiteit Utrecht, and Dep Natuurkunde
Subjects: Physics, Accretion, Accretion, accretion disks, Binaries: general, Black hole physics, X-rays: stars, Photon, accretion disks, Astrophysics::High Energy Astrophysical Phenomena, Metallicity, Astrophysics (astro-ph), FOS: Physical sciences, Flux, Astronomy and Astrophysics, Astrophysics, Power law, Space and Planetary Science, Optical depth (astrophysics), Electron temperature, Black-body radiation, Halo
Abstract: We report on results of a target of opportunity observation of the X-ray transient XTE J1118+480 performed on 2000 April 14-15 with the Narrow Field Instruments (0.1-200 keV) of the SAX satellite. The measured spectrum is a power law with a photon index of ~1.7 modified by an ultrasoft X-ray excess and a high-energy cutoff above ~100 keV. The soft excess is consistent with a blackbody with temperature of ~40 eV and a low flux, while the cut-off power law is well fitted by thermal Comptonization in a plasma with an electron temperature of 100 keV and an optical depth of order of unity. Consistent with the weakness of the blackbody, Compton reflection is weak. Though the data are consistent with various geometries of the hot and cold phases of the accreting gas, we conclude that a hot accretion disk is the most plausible model. The Eddington ratio implied by recent estimates of the mass and the distance is about 10^{-3}, which may indicate that advection is probably not the dominant cooling mechanism. We finally suggest that the reflecting medium has a low metallicity, consistent with location of the system in the halo., 14 pages, 8 figures, accepted for publication in The Astrophysical Journal
Published: 2001

38. The Prompt Emission of GRB 990712 with [ITAL]B[/ITAL][CSC][ITAL]eppo[/ITAL][/CSC][ITAL]SAX[/ITAL]: Evidence of a Transient X-Ray Emission Feature

Author: N. Masetti, Lorenzo Amati, Elena Pian, Enrico Costa, Mauro Orlandini, Luciano Nicastro, J. J. M. in 't Zand, John Heise, F. Frontera, Paolo Soffitta, Luigi Piro, M. Feroci, Eliana Palazzi, and Mario Vietri
Subjects: Physics, Field (physics), Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Black-body radiation, Astrophysics, Transient (oscillation), Light curve, Event (particle physics), Passband, Energy (signal processing), Pulse (physics)
Abstract: We report on the prompt X- and gamma-ray observations of GRB990712 with the BeppoSAX Gamma-Ray Burst Monitor and Wide Field Camera No. 2. Due to Sun constraints, we could not perform a follow-up observation with the BeppoSAX Narrow Field Instruments. The light curve of the prompt emission shows two pulses and a total duration of about 40s in X-rays. In gamma-rays the event is even shorter. The 2-700 keV spectral emission with time shows a discontinuity in the peak energy Ep of the E F(E) spectrum: Ep is above our energy passband during the first pulse and goes down to ~10 keV during the second pulse. Another peculiarity is noted in this event for the first time: the possible evidence of a 2s duration emission feature during the tail of the first pulse. The feature is consistent with either a Gaussian profile with centroid energy of 4.5 keV or a blackbody spectrum with kTbb ~1.3 keV. We discuss the possible origin of the feature. The most attractive possibility is that we are observing the thermal emission of a baryon-loaded expanding fireball, when it becomes optically thin.
Published: 2001

39. X-ray emission in the direction of the SNR G318.2+0.1

Author: Arvind Parmar, Fabrizio Bocchino, Andrea Santangelo, Sandro Mereghetti, Mauro Orlandini, and Lorella Angelini
Subjects: Physics, Young stellar object, Astrophysics (astro-ph), Shell (structure), X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Galactic plane, Star (graph theory), Electron acceleration, Space and Planetary Science, Coincident, Thermal
Abstract: We report the discovery of three X-ray sources within the radio shell G318.2+0.1, one of which may be extended. Two of the sources were detected during the \sax Galactic Plane Survey and one was found in archival \ros data. The fainter \sax source is coincident with an ultra-compact galactic H {\sc ii} region, and we discuss the possibility that it can be a flaring young stellar object, while the other \sax source has no obvious counterpart. The PSPC source is consistent with emission from a foreground star. The hard spectrum of the brighter \sax source is consistent with a non-thermal origin, although a thermal nature cannot be formally excluded. If this source is associated with G318.2+0.1, then its hard spectrum suggests that it may be site of non-thermal electron acceleration., Comment: 7 pages, 4 figures, accepted for publication in A&A, abstract was hidden, now it is OK
Published: 2001

40. Broadband Spectrum of Cygnus X‐1 in Two Spectral States withBeppoSAX

Author: A. A. Zdziarski, Andrea Santangelo, A. N. Parmar, S. Del Sordo, Mauro Orlandini, G. Cusumano, G. C. Perola, L. Piro, F. Frontera, Francesco Haardt, D. Dal Fiume, A. Segreto, Aldo Treves, L. Chiappetti, M. Trifoglio, and E. Palazzi
Subjects: Physics, Accretion, Photon, accretion disks, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Bolometer, FOS: Physical sciences, Broad band, X-rays: stars, Astronomy and Astrophysics, Astrophysics, Plasma, Black hole physics, law.invention, Accretion, accretion disks, Binaries: general, Stars: individual (Cygnus X-1), Soft state, Space and Planetary Science, law, Thermal, Black-body radiation, Plasma cloud
Abstract: We report on the 0.5--200 keV spectral properties of Cyg X-1 observed at different epochs with the Narrow Field Instruments of the BeppoSAX satellite. The source was in its soft state during the first observation of 1996 June. In the second observation of 1996 September, the source had parameters characteristic to its hard state. A soft X-ray excess, a broad Fe K$\alpha$ line and Compton reflection are clearly detected in both states. The soft-state broad-band continuum is well modeled by a disk blackbody (accounting for the soft excess) and Compton upscattering of the disk photons by a hybrid, thermal/non-thermal, plasma, probably forming a corona above the disk (also giving rise to the Compton-reflection component). In the hard state, the primary hard X-ray spectrum can be well modeled by Compton upscattering of a weak blackbody emission by a thermal plasma at a temperature of $\sim 60$ keV. The soft excess is then explained by thermal Comptonization of the same blackbody emission by another hot plasma cloud characterized by a low value of its Compton parameter. Finally, we find the characteristic ratio of the bolometric flux in the soft state to that in the hard state to be about 3. This value is much more compatible with theories of state transitions than the previously reported (and likely underestimated) value of 1.5., Comment: 15 pages, 5 figures. Accepted for publication in ApJ
Published: 2001

41. Integrating theBeppoSAXGamma‐Ray Burst Monitor into the Third Interplanetary Network

Author: M. Feroci, Mauro Orlandini, Luciano Nicastro, D. Dal Fiume, Enrico Costa, Maria Nerina Cinti, Kevin Hurley, J. J. M. in 't Zand, F. Frontera, Lorenzo Amati, T. L. Cline, B. Preger, and John Heise
Subjects: Physics, Space and Planetary Science, Detector, Gamma ray, Astronomy and Astrophysics, Triangulation (computer vision), Astrophysics, Gamma-ray burst, Interplanetary spaceflight
Abstract: We have added the BeppoSAX Gamma-Ray Burst Monitor to the third Interplanetary Network (IPN3) of burst detectors. We analyze 16 bursts whose positions are known to good accuracy from mea- surements at other wavelengths. We show that there is excellent agreement between the Ulysses/ BeppoSAX triangulation annuli and the known positions of these events and that these annuli can in many cases provide useful constraints on the positions of bursts detected by the BeppoSAX Wide-Field Camera and Narrow-Field Instruments. Subject heading: gamma rays: bursts
Published: 2000

42. [CSC][ITAL]BeppoSAX[/ITAL][/CSC] and [ITAL]Chandra[/ITAL] Observations of SAX J0103.2−7209 = 2E 0101.5−7225: A New Persistent 345 Second X-Ray Pulsar in the Small Magellanic Cloud

Author: D. Ricci, Stefano Covino, Sergio Campana, D. Dal Fiume, G. L. Israel, T. Oosterbroek, Sandro Mereghetti, Mauro Orlandini, Luigi Stella, Terrance J. Gaetz, and A. N. Parmar
Subjects: Physics, Photon, Pulsar, Space and Planetary Science, ROSAT, Flux, Astronomy and Astrophysics, Astrophysics, Type (model theory), X-ray pulsar, Luminosity
Abstract: We report the results of a 1998 July BeppoSAX observation of a field in the SMC which led to the discovery of 345s pulsations in the X-ray flux of SAXJ0103.2-7209. The BeppoSAX X-ray spectrum is well fit by an absorbed power-law with photon index 1.0 plus a black body component with kT=0.1keV. The unabsorbed luminosity in the 2-10 keV energy range is 1.2x10^{36} erg/s. In a very recent Chandra observation the 345s pulsations are also detected. The available period measurements provide a constant period derivative of -1.7s/yr over the last three years making SAXJ0103.2-7209 one of the most rapidly spinning-up X-ray pulsars known. The BeppoSAX position is consistent with that of the Einstein source 2E0101.5-7225 and the ROSAT source RXJ0103.2-7209. This source was detected at a luminosity level of few 10^{35}-10^{36} erg/s in all datasets of past X-ray missions since 1979. The ROSAT HRI and Chandra positions are consistent with that of a m_V=14.8 Be spectral type star already proposed as the likely optical counterpart of 2E0101.5-7225. We conclude that SAXJ0103.2-7209 and 2E0101.5-7225 are the same source, a relatively young and persistent X-ray pulsar in the SMC.
Published: 2000

43. A [CSC][ITAL]BeppoSAX[/ITAL][/CSC] Study of the Pulsating Transient X0115+63: The First X-Ray Spectrum with Four Cyclotron Harmonic Features

Author: Sergio Campana, Mauro Orlandini, S. Giarrusso, D. Dal Fiume, G. L. Israel, A. Segreto, Tatehiro Mihara, Luigi Stella, T. Oosterbroek, Arvind Parmar, Andrea Santangelo, and Tomasz Bulik
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Cyclotron, Phase (waves), Astronomy and Astrophysics, Astrophysics, Pulse (physics), law.invention, Magnetic field, Pulsar, Space and Planetary Science, law, Harmonics, Harmonic, Atomic physics, Relativistic quantum chemistry
Abstract: The recurrent hard pulsating X-ray transient X0115+63 was observed with BeppoSAX on 1999 March 19, when the source was at a 2-10 keV flux level of ~310 mcrab. We report on the high-energy spectrum of the source, concentrating on cyclotron resonant scattering features. The spectrum is strongly pulse phase dependent, and absorption features are detected at virtually all phases. In particular, four absorption-like features at 12.74, 24.16, 35.74, and 49.5 keV are observed in the descending edge of the main peak of the pulse profile. The ratios between the centroid energies of the lines with respect to the first are 1 : (1.9) : (2.8) : (3.9). These values are close to the harmonic relation expected from cyclotron resonant scattering in a strong magnetic field when relativistic effects are taken into account. The equivalent widths of the second, third, and fourth harmonics are found to be larger than that of the first harmonic, confirming the key role of two-photon processes in the spectral formation. These results provide the first evidence for four harmonically spaced lines in the spectrum of an accreting X-ray pulsar, yielding the clearest confirmation to date of their magnetic origin.
Published: 1999

44. A Giant Outburst from SGR 1900+14 Observed with the [ITAL]BeppoSAX[/ITAL] Gamma-Ray Burst Monitor

Author: Marco Feroci, Mauro Orlandini, F. Frontera, Massimo Rapisarda, Lorenzo Amati, Marco Tavani, and Enrico Costa
Subjects: Physics, Neutron star, Space and Planetary Science, Oscillation, Spectral properties, Spectral variation, Substructure, Astronomy and Astrophysics, Astrophysics, Spectral component, Gamma-ray burst, Event (particle physics)
Abstract: We report the detection by the Gamma Ray Burst Monitor onboard BeppoSAX of the strongest and longest ever detected outburst from SGR 1900+14. Oscillations are detectable with a period of ~5.16 s for the entire duration of the event ~300 s. The temporal analysis reveals also a remarkable periodic substructure: after about 35 s from the event onset each 5.16-s pulse shows a pattern of four subpulses and a dip, each separated by ~1 s. Significant spectral variation is detected during the event and for each individual oscillation. The first and most intense part of the outburst is quite hard, and similar to what previously detected from the `March 5th event'. A hard non-thermal spectral component persists for ~200 s. SGR 1900+14 was proposed to be a strongly magnetized neutron star (B>10^14 G) undergoing violent instabilities by internal magnetic/crustal stresses. However, the onset of an apparent 1-s periodicity within the 5.16-s pulsations and the observed spectral properties show a complex behaviour that is not satisfactorily modelled yet.
Published: 1999

45. SAX and XTE observations of GX1+4, SMC X-1, RX J0146.9+6121 and 4U 0142+614, a sample of X-ray pulsators with extreme properties

Author: Sandro Mereghetti, Luciano Burderi, Mauro Orlandini, A. N. Parmar, J. van Paradijs, D. Ricci, Sergio Campana, Lorella Angelini, M. Vietri, D. Dal Fiume, Andrea Santangelo, G. L. Israel, N. E. White, Luigi Stella, F. Frontera, and Santina Piraino
Subjects: Physics, Nuclear and High Energy Physics, Astrophysics::High Energy Astrophysical Phenomena, X-ray, Astronomy, Astrophysics, Atomic and Molecular Physics, and Optics, Neutron star, Stars, Pulsar, Millisecond pulsar, Binary star, Stellar evolution, X-ray pulsar
Abstract: We report and discuss preliminary results obtained from the analysis of a sample of X-ray pulsars observed by SAX and XTE. The sample includes GX1+4, a ∼125 s period low-mass X-ray pulsar which shows extreme properties and spin-up/down behaviour, 4U0142+614, a member of the recently identified class of “Anomalous” X-ray pulsars, SMC X-1, a short period (∼0.71 s) X-ray pulsar in a high-mass binary, and RX J0146.9+6121, the slowest spinning accreting neutron star currently known (∼ 25 min period).
Published: 1999

46. BeppoSAX observation of the transient X-ray pulsar GS 1843+009

Author: S. Del Sordo, N. R. Robba, G. Cusumano, Mauro Orlandini, Luciano Burderi, Andrea Santangelo, Arvind Parmar, D. Dal Fiume, T. Oosterbroek, S. Giarrusso, and Santina Piraino
Subjects: Physics, Nuclear and High Energy Physics, Radiation flux, Pulsar, Astronomy, Flux, Satellite, Transient (oscillation), Astrophysics, Atomic and Molecular Physics, and Optics, Particle detector, Spectral line, X-ray pulsar
Abstract: The transient X-ray pulsar GS 1843+009 was observed by BeppoSAX satellite on 1997 April 4, while it was at flux level of 50 mCrab in the 20–200 keV energy band. Using the MECS and LECS concentrators, the source position was measured with unprecedented accuracy of 30. In this poster we present results on both spectral and temporal analysis.
Published: 1999

47. Wide band pulse phase resolved spectroscopy with BeppoSax

Author: G. Cusumano, Mauro Orlandini, D. Dal Fiume, S. Del Sordo, Santina Piraino, A. Segreto, Andrea Santangelo, and Arvind Parmar
Subjects: Physics, Nuclear and High Energy Physics, Pulsar, Astrophysics::High Energy Astrophysical Phenomena, Phase (waves), Binary number, Astronomy, Wide band, Astrophysics, Spectroscopy, Atomic and Molecular Physics, and Optics, Spectral line, Pulse (physics)
Abstract: Broad-band observation of galactic X-ray binary pulsars is one of the main scientific goal of the BeppoSAX mission. In this framework a key role is played by Pulse Phase Resolved Spectroscopy. In the paper we present some preliminary results on both phase-resolved spectra and pulse profile evolution with energy on two sources of this class, Cen X-3 and Her X-1.
Published: 1999

48. Scientific prospects in soft gamma-ray astronomy enabled by the LAUE project

Author: V. Carassiti, Mauro Orlandini, Lev Titarchuk, Piero Rosati, S. Mottini, Angela Malizia, Natalia Auricchio, Filippo Frontera, L. Recanatesi, V. Valsan, Vincenzo Liccardo, Riccardo Campana, B. Negri, Ruben Farinelli, Enrico Virgilli, M. Pecora, C. Labanti, F. Cassese, L. Bassani, C. Guidorzi, John B. Stephen, Claudio Ferrari, Vincenzo Guidi, Lorenzo Amati, V. Sguera, Ezio Caroli, and R. Landi
Subjects: Physics, Point spread function, Photon, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics, focusing telescopes, gamma-rays, Laue lenses, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Gamma-ray astronomy, NO, law.invention, Lens (optics), Optics, law, Satellite, Astrophysics - Instrumentation and Methods for Astrophysics, business, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: This paper summarizes the development of a successful project, LAUE, supported by the Italian Space Agency (ASI) and devoted to the development of long focal length (up to 100 m) Laue lenses for hard X--/soft gamma--ray astronomy (80-600 keV). The apparatus is ready and the assembling of a prototype lens petal is ongoing. The great achievement of this project is the use of bent crystals. From measurements obtained on single crystals and from simulations, we have estimated the expected Point Spread Function and thus the sensitivity of a lens made of petals. The expected sensitivity is a few $\times10^{-8}$ photons cm$^{-2}$ s$^{-1}$ keV$^{-1}$. We discuss a number of open astrophysical questions that can settled with such an instrument aboard a free-flying satellite., 17 pages, 18 figures, published in Proceedings of the SPIE, Volume 8861, id. 886106 17 pp. (2013)
Published: 2013

49. BeppoSAX observations of the X-ray pulsar MAXI J1409-619 in low state: DISCOVERY of cyclotron resonance features

Author: N. Masetti, Vito Sguera, Lara Sidoli, Filippo Frontera, and Mauro Orlandini
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Photon, Astrophysics::High Energy Astrophysical Phenomena, Cyclotron, Cyclotron resonance, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galactic plane, stars: individual (IGR J14043-6148, law.invention, MAXI J1409-619), Neutron star, X-rays: binaries, Pulsar, Space and Planetary Science, law, Astrophysics - High Energy Astrophysical Phenomena, X-ray pulsar, Gravitational redshift, stars: individual (IGR J14043-6148, MAXI J1409-619)
Abstract: The transient 500 s X-ray pulsar MAXI J1409-619 was discovered by the slit cameras aboard MAXI on October 17, 2010, and soon after accurately localized by Swift. We found that the source position was serendipitously observed in 2000 during BeppoSAX observations of the Galactic plane. Two sources are clearly detected in the MECS: one is consistent with the position of IGR J14043-6148 and the other one with that of MAXI J1409-619. We report on the analysis of this archival BeppoSAX/MECS observation integrated with newly analyzed observation from ASCA and a set of high-energy observations obtained from the offset fields of the BeppoSAX/PDS instrument. For the ON-source observation, the 1.8-100 keV spectrum is fit by an absorbed power law with a photon index Gamma = 0.87_{-0.19}^{+0.29}, corresponding to 2-10 and 15-100 keV unabsorbed fluxes of 2.7E-12 and 4E-11 erg/cm2/s, respectively, and a 2-10 keV luminosity of 7E+34 erg/s for a 15 kpc distance. For a PDS offset field observation, performed about one year later and showing a 15-100 keV flux of 7E-11 erg/cm2/s, we clearly pinpoint three spectral absorption features at 44, 73, and 128 keV, resolved both in the spectral fit and in the Crab ratio. We interpret these not harmonically spaced features as due to cyclotron resonances. The fundamental energy of 44 +/- 3 keV corresponds to a magnetic field strength at the neutron star surface of 3.8E12 (1+z) G, where z is the gravitational redshift. We discuss the nature of the source in the light of its possible counterpart., Comment: 10 pages, 9 figures. Expanded and revised version accepted for publication in ApJ Main Journal
Published: 2012

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

Author: I. Donnarumma, Y. Evangelista, Phil Uttley, Christian Schmid, D. Macera, L. Pacciani, Paul S. Smith, T. Kennedy, J.-Y. Seyler, J. W. den Herder, Martino Marisaldi, Michael A. Nowak, A. de Rosa, Berend Winter, Dom Walton, E. Bozzo, A. Argan, Miriam Grassi, C. Tenzer, M. Ahangarianabhari, G. Zampa, Andrea Santangelo, Jörn Wilms, A. Vacchi, P. Bodini, Riccardo Campana, Claudio Labanti, Slawomir Suchy, Silvia Zane, P. Soffitta, F. Fuschino, Fabio Muleri, M. Hailey, S. Di Cosimo, Adrian Martindale, V. Petracek, P. Cais, Giuseppe Baldazzi, Yannick Favre, Mauro Orlandini, E. Del Monte, Didier Barret, Alain Cros, Emanuele Perinati, C. Feldman, M. Pohl, Franck Cadoux, J. Coker, Piero Malcovati, M. Feroci, René Hudec, P. Azzarello, Teresa Mineo, A. Rachevski, G.W. Fraser, Giuseppe Bertuccio, N. Zampa, SPIE, Takahashi, Tadayuki, Zane S., Walton D., Kennedy T., Feroci M., Den Herder J.-W., Ahangarianabhari M., Argan A., Azzarello P., Baldazzi G., Barret D., Bertuccio G., Bodin P., Bozzo E., Cadoux F., Cais P., Campana R., Coker J., Cros A., Del Monte E., De Rosa A., Di Cosimo S., Donnarumma I., Evangelista Y., Favre Y., Feldman C., Fraser G., Fuschino F., Grassi M., Hailey M.R., Hudec R., Labanti C., Macera D., Malcovati P., Marisaldi M., Martindale A., Mineo T., Muleri F., Nowak M., Orlandini M., Pacciani L., Perinati E., Petracek V., Pohl M., Rachevski A., Smith P., Santangelo A., Seyler J.-Y., Schmid C., Soffitta P., Suchy S., Tenzer C., Uttley P., Vacchi A., Zampa G., Zampa N., Wilms J., Winter B., High Energy Astrophys. & Astropart. Phys (API, FNWI), FORMATION STELLAIRE 2012, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Mullard Space Science Laboratory (MSSL), and University College of London [London] (UCL)
Subjects: Silicon, Photon, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Observatories, Collimators, FOS: Physical sciences, ddc:500.2, Astrophysics, 7. Clean energy, 01 natural sciences, Optics, Observatory, 0103 physical sciences, X-rays, Electronic, Optical and Magnetic Materials, Electrical and Electronic Engineering, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Compact objects, Physics, Millisecond, Photons, Equipment and services, sezele, 010308 nuclear & particles physics, Payload, business.industry, Sensors, Applied Mathematics, Detector, Antenna aperture, Computer Science Applications1707 Computer Vision and Pattern Recognition, Condensed Matter Physics, Capillaries, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Neutron star, X-ray Timing, Electronic, Optical and Magnetic Materials, Instrumentation and Methods for Astrophysics, business, Astrophysics - Instrumentation and Methods for Astrophysics, Energy (signal processing), Compact object
Abstract: The Large Observatory for X-ray Timing (LOFT) is one of the four candidate ESA M3 missions considered for launch in the 2022 time-frame. It is specifically designed to perform fast X-ray timing and probe the status of the matter near black holes and neutron stars. The LOFT scientific payload is composed of a Large Area Detector (LAD) and a Wide Field Monitor (WFM). The LAD is a 10 m2-class pointed instrument with 20 times the collecting area of the best past timing missions (such as RXTE) over the 2-30 keV range, which holds the capability to revolutionize studies of X-ray variability down to the millisecond time scales. Its ground-breaking characteristic is a low mass per unit surface, enabling an effective area of ~10 m^2 (@10 keV) at a reasonable weight. The development of such large but light experiment, with low mass and power per unit area, is now made possible by the recent advancements in the field of large-area silicon detectors - able to time tag an X-ray photon with an accuracy, Proceedings of SPIE, Vo. 8443, Paper No. 8443-87
Published: 2012

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