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9 results on '"ASI-Science Data Center, Rome"'

1. Lyman continuum leakage in faint star-forming galaxies at redshift $z=3-3.5$ probed by gamma-ray bursts

Author

A. de Ugarte Postigo, J. B. Vielfaure, Tanmoy Laskar, Andrea Rossi, Nial R. Tanvir, Johan P. U. Fynbo, Sergio Campana, Stefano Covino, Valerio D'Elia, Dieter H. Hartmann, Chryssa Kouveliotou, Francois Hammer, Max Gronke, Patrick Petitjean, Andrew J. Levan, David Alexander Kann, S. D. Vergani, Ruben Salvaterra, Klaas Wiersema, M. de Pasquale, M. Arabsalmani, D. B. Malesani, J. T. Palmerio, Kasper E. Heintz, Pall Jakobsson, J. Japelj, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), HEP, INSPIRE, 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), Faculty of Mathematics and Physics [Ljubljana] (FMF), University of Ljubljana, Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), ASI-Science Data Center, Rome, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), INAF-IASF Milano, Istituto Nazionale di Astrofisica (INAF), Department of Physics and Astronomy [Leicester], University of Leicester, University of Siena, Department of History and Cultural Heritage, Universitá degli Studi dell’Insubria, NUCLEOVIR, Centre International de Recherche en Infectiologie - UMR (CIRI), Institut National de la Santé et de la Recherche Médicale (INSERM)-École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM)-École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Equipe virus AAV et vecteurs AAV (INSERM U758/ ENS de Lyon), Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre de génétique et de physiologie moléculaire et cellulaire (CGPhiMC), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Agence Nationale de la Recherche (France), National Aeronautics and Space Administration (US), Carlsberg Foundation, Villum Fonden, Science and Technology Facilities Council (UK), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, National Science Foundation (US), API Other Research (FNWI), Low Energy Astrophysics (API, FNWI), Faculty of Science, University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Università degli Studi di Siena = University of Siena (UNISI), Universitá degli Studi dell’Insubria = University of Insubria [Varese] (Uninsubria), Centre de génétique et de physiologie moléculaire et cellulaire (CGPhiMC), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Centre International de Recherche en Infectiologie (CIRI), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Université Jean Monnet - Saint-Étienne (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure de Lyon (ENS de Lyon)-Université Jean Monnet - Saint-Étienne (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Equipe virus AAV et vecteurs AAV (INSERM U758/ ENS de Lyon), Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut National de la Santé et de la Recherche Médicale (INSERM), ANR-16-CE31-0003,BEaPro,Using the most powerful explosion as probes of the high-redshift Universe(2016), 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), Raunvísindastofnun (HÍ), Science Institute (UI), Verkfræði- og náttúruvísindasvið (HÍ), School of Engineering and Natural Sciences (UI), Háskóli Íslands, and University of Iceland

Subjects
Astronomy, gamma-ray burst: general, Astrophysics, 01 natural sciences, 7. Clean energy, high-redshift [Galaxies], Reionization, galaxies: high-redshift, ABSORPTION, Emission spectrum, GRB AFTERGLOW SPECTRA, dark ages, 010303 astronomy & astrophysics, QC, ESCAPE FRACTION, QB, BRIGHT, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, [PHYS]Physics [physics], Balmer series, Vetrarbrautir, general [Gamma-ray burst], Dark ages, Dark Ages, symbols, reionization, intergalactic medium, Astrophysics - High Energy Astrophysical Phenomena, galaxies: evolution, Astrophysics::High Energy Astrophysical Phenomena, first stars, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, BD, symbols.namesake, LY-ALPHA, 0103 physical sciences, Astrophysics::Galaxy Astrophysics, First stars, Intergalactic medium, 010308 nuclear & particles physics, CONSTRAINTS, Astronomy and Astrophysics, Stjarneðlisfræði, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, EVOLUTION, Afterglow, HOST GALAXIES, STELLAR, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Gamma-ray burst, EMISSION, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited., Context. The identification of the sources that reionized the Universe and their specific contribution to this process are key missing pieces of our knowledge of the early Universe. Faint star-forming galaxies may be the main contributors to the ionizing photon budget during the epoch of reionization, but their escaping photons cannot be detected directly due to inter-galactic medium opacity. Hence, it is essential to characterize the properties of faint galaxies with significant Lyman continuum (LyC) photon leakage up to z ∼ 4 to define indirect indicators allowing analogs to be found at the highest redshift. Aims. Long gamma-ray bursts (LGRBs) typically explode in star-forming regions of faint, star-forming galaxies. Through LGRB afterglow spectroscopy it is possible to detect directly LyC photons. Our aim is to use LGRBs as tools to study LyC leakage from faint, star-forming galaxies at high redshift. Methods. Here we present the observations of LyC emission in the afterglow spectra of GRB 191004B at z = 3.5055, together with those of the other two previously known LyC-leaking LGRB host galaxies (GRB 050908 at z = 3.3467, and GRB 060607A at z = 3.0749), to determine their LyC escape fraction and compare their properties. Results. From the afterglow spectrum of GRB 191004B we determine a neutral hydrogen column density at the LGRB redshift of log(NH I/cm−2) = 17.2 ± 0.15, and negligible extinction (AV = 0.03 ± 0.02 mag). The only metal absorption lines detected are C IV and Si IV. In contrast to GRB 050908 and GRB 060607A, the host galaxy of GRB 191004B displays significant Lyman-alpha (Lyα) emission. From its Lyα emission and the non-detection of Balmer emission lines we constrain its star-formation rate (SFR) to 1 ≤ SFR ≤ 4.7 M⊙ yr−1. We fit the Lyα emission with a shell model and find parameters values consistent with the observed ones. The absolute (relative) LyC escape fractions we find for GRB 191004B, GRB 050908 and GRB 060607A are of 0.35−0.11+0.10 (0.43−0.13+0.12), 0.08−0.04+0.05 (0.08−0.04+0.05) and 0.20−0.05+0.05 (0.45−0.15+0.15), respectively. We compare the LyC escape fraction of LGRBs to the values of other LyC emitters found from the literature, showing that LGRB afterglows can be powerful tools to study LyC escape for faint high-redshift star-forming galaxies. Indeed we could push LyC leakage studies to much higher absolute magnitudes. The host galaxies of the three LGRBs presented here have all M1600 > −19.5 mag, with the GRB 060607A host at M1600 > −16 mag. LGRB hosts may therefore be particularly suitable for exploring the ionizing escape fraction in galaxies that are too faint or distant for conventional techniques. Furthermore, the time involved is minimal compared to galaxy studies. © J.-B. Vielfaure et al. 2020, This work is part of the BEaPro project (PI: S.D. Vergani) funded by the French Agence Nationale de la Recherche (ANR-16-CE31-0003). We thank Giancarlo Ghirlanda for providing useful information. JBV and SDV thank Anne Verhamme for useful discussions. SDV acknowledges financial support from the French Space Agency (CNES). MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409 and acknowledges support from HST grants HST-GO-15643.017-A, HST-AR-15039.003-A, and XSEDE grant TG-AST180036. The Cosmic DAWN center is funded by the DNRF. JPUF thanks the Carlsberg foundation for support. DBM acknowledges support from VILLUM FONDEN research grant 19054. NRT acknowledges support from STFC via grant ST/N000757/1. DAK acknowledges support from Spanish research project RTI2018-098104-J-I00 (GRBPhot). The PanSTARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project O ffice, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation Grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium).Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The NumPy (van der Walt et al. 2011), SciPy (Virtanen et al. 2020) and matplotlib (Hunter 2007) packages have been extensively used for the preparation and presentation of this work.

Published
2020

2. THESEUS: A key space mission concept for Multi-Messenger Astrophysics

Author

F. Fuschino, Ruben Salvaterra, F. Frontera, M. Branchesi, Bruce Gendre, U. Maio, Stefano Covino, Tomaz Rodic, Giancarlo Ghirlanda, Serena Vinciguerra, D. Mereghetti, Andrea Rossi, Lorenzo Amati, Diego Götz, M. H. P. M. van Putten, Monica Colpi, Roberto Mignani, P. D'Avanzo, Riccardo Campana, Eliana Palazzi, Andrea Bulgarelli, M. G. Bernardini, Valerio D'Elia, Jochen Greiner, Elisabetta Maiorano, Enzo Brocato, Joseph Caruana, Piero Rosati, R. L. C. Starling, Nial Tanvir, Riccardo Ciolfi, G. Stratta, S. D. Vergani, S. Colafrancesco, Claudio Labanti, Bing Zhang, Dorottya Szécsi, M. Razzano, Enrico Bozzo, Antonio Stamerra, D. Malesani, René Hudec, Francesco Longo, Luciano Rezzolla, S. Piranomonte, M. de Pasquale, Richard Willingale, B. Patricelli, J. P. Osborne, P. T. O'Brien, Peter G. Jonker, Luciano Nicastro, C. Guidorzi, Aniello Grado, M. Boer, Alessandro Drago, Maria Giovanna Dainotti, Carole Mundell, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Istituto Nazionale di Astrofisica (INAF), ISDC Data Centre for Astrophysics, University of Geneva [Switzerland], INAF - Osservatorio Astronomico di Brera (OAB), University of Ferrara [Ferrara], Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Department of Physics and Astronomy [Leicester], University of Leicester, Max-Planck-Institut für Extraterrestrische Physik (MPE), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), INAF - Osservatorio Astronomico di Roma (OAR), INAF-IASF Milano, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), ASI-Science Data Center, Rome, Laboratori Nazionali di Frascati (LNF), National Institute for Nuclear Physics (INFN), Laboratoire d'Astrophysique de Marseille (LAM), 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), Astronomical Institute of the Czech Academy of Sciences, Czech Academy of Sciences [Prague] (ASCR), Department of Astrophysics [Nijmegen], Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud university [Nijmegen]-Radboud university [Nijmegen], Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), CNR Institute of Atmospheric Sciences and Climate (ISAC), Consiglio Nazionale delle Ricerche (CNR), Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), 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 de Genève = University of Geneva (UNIGE), Università degli Studi di Ferrara = University of Ferrara (UniFE), Istituto Nazionale di Fisica Nucleare (INFN), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), Radboud University [Nijmegen]-Radboud University [Nijmegen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) (DAP), 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, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 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, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-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), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), THESEUS, Stratta, G., Ciolfi, R., Amati, L., Bozzo, E., Ghirlanda, G., Maiorano, E., Nicastro, L., Rossi, A., Vinciguerra, S., Frontera, F., Götz, D., Guidorzi, C., O'Brien, P., Osborne, J. P., Tanvir, N., Branchesi, M., Brocato, E., Dainotti, M. G., De Pasquale, M., Grado, A., Greiner, J., Longo, F., Maio, U., Mereghetti, D., Mignani, R., Piranomonte, S., Rezzolla, L., Salvaterra, R., Starling, R., Willingale, R., Böer, M., Bulgarelli, A., Caruana, J., Colafrancesco, S., Colpi, M., Covino, S., D'Avanzo, P., D'Elia, V., Drago, A., Fuschino, F., Gendre, B., Hudec, R., Jonker, P., Labanti, C., Malesani, D., Mundell, C. G., Palazzi, E., Patricelli, B., Razzano, M., Campana, R., Rosati, P., Rodic, T., Szécsi, D., Stamerra, A., van Putten, M., Vergani, S., Zhang, B., Bernardini, M., 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Università degli Studi di Ferrara (UniFE), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Stratta, G, Ciolfi, R, Amati, L, Bozzo, E, Ghirlanda, G, Maiorano, E, Nicastro, L, Rossi, A, Vinciguerra, S, Frontera, F, Götz, D, Guidorzi, C, O'Brien, P, Osborne, J, Tanvir, N, Branchesi, M, Brocato, E, Dainotti, M, De Pasquale, M, Grado, A, Greiner, J, Longo, F, Maio, U, Mereghetti, D, Mignani, R, Piranomonte, S, Rezzolla, L, Salvaterra, R, Starling, R, Willingale, R, Böer, M, Bulgarelli, A, Caruana, J, Colafrancesco, S, Colpi, M, Covino, S, D'Avanzo, P, D'Elia, V, Drago, A, Fuschino, F, Gendre, B, Hudec, R, Jonker, P, Labanti, C, Malesani, D, Mundell, C, Palazzi, E, Patricelli, B, Razzano, M, Campana, R, Rosati, P, Rodic, T, Szécsi, D, Stamerra, A, van Putten, M, Vergani, S, Zhang, B, and Bernardini, M

Subjects
Atmospheric Science, Computer science, Astronomy, Astronomical and space-research instrumentation, Gamma-ray bursts, Gamma-ray sources, X-ray bursts, X-ray sources, Aerospace Engineering, Space and Planetary Science, Astrophysics, 01 natural sciences, Economica, astronomical and space-research instrumentation, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), [PHYS]Physics [physics], energy: high, gamma-ray bursts, Gamma-ray source, neutrino: detector, Geophysics, Upgrade, Neutrino detector, upgrade, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Cosmic Vision, media_common.quotation_subject, FOS: Physical sciences, Context (language use), frequency: high, X-ray source, 0103 physical sciences, gravitational radiation: frequency, Gamma-ray burst, X-ray burst, gamma-ray sources, 010308 nuclear & particles physics, Gravitational wave, family: 3, Astronomy and Astrophysics, gravitational radiation detector, Universe, messenger, electromagnetic, General Earth and Planetary Sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The recent discovery of the electromagnetic counterpart of the gravitational wave source GW170817, has demonstrated the huge informative power of multi-messenger observations. During the next decade the nascent field of multi-messenger astronomy will mature significantly. Around 2030, third generation gravitational wave detectors will be roughly ten times more sensitive than the current ones. At the same time, neutrino detectors currently upgrading to multi km^3 telescopes, will include a 10 km^3 facility in the Southern hemisphere that is expected to be operational around 2030. In this review, we describe the most promising high frequency gravitational wave and neutrino sources that will be detected in the next two decades. In this context, we show the important role of the Transient High Energy Sky and Early Universe Surveyor (THESEUS), a mission concept proposed to ESA by a large international collaboration in response to the call for the Cosmic Vision Programme M5 missions. THESEUS aims at providing a substantial advancement in early Universe science as well as playing a fundamental role in multi-messenger and time-domain astrophysics, operating in strong synergy with future gravitational wave and neutrino detectors as well as major ground- and space-based telescopes. This review is an extension of the THESEUS white paper (Amati et al. 2017), also in light of the discovery of GW170817/GRB170817A that was announced on October 16th, 2017., Comment: 25 pages, 13 figures, accepted to Advances in Space Research with minor revisions. Details on the THESEUS instrumentation, science case and expected performances can also be found in Amati et al. 2017 (arXiv:1710.04638) and in the presentations of the THESEUS Workshop 2017 (http://www.isdc.unige.ch/theseus/workshop2017-programme.html). v2 few typos corrected

Published
2018

3. Solving the conundrum of intervening strong Mg II absorbers towards gamma-ray bursts and quasars

Author

Lex Kaper, A. de Ugarte Postigo, J. Japelj, Guido Cupani, P. Cortés-Zuleta, P. Petitjean, F. Hammer, R. Sanchez-Ramirez, Nial R. Tanvir, George D. Becker, Marianne Vestergaard, T. A. M. Berg, N. Annau, R. Cañameras, D. Passi, Johan P. U. Fynbo, Sara L. Ellison, Kasper E. Heintz, Stefano Covino, Sebastian Lopez, P. Jakobsson, Zach Cano, V. D'Elia, Christina C. Thöne, S. D. Vergani, K. Wiersema, V. Pugliese, Gabor Worseck, Palle Møller, Steve Schulze, A. Gomboc, V. D'Odorico, P. Goldoni, Lise Christensen, Jonatan Selsing, D. Malesani, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Weizmann Institute of Science [Rehovot, Israël], Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), 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), INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Roma (OAR), 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, Faculty of Mathematics and Physics [Ljubljana] (FMF), University of Ljubljana, University of Iceland [Reykjavik], Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Institut de pharmacologie et de biologie structurale (IPBS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Physics and Astronomy [Leicester], University of Leicester, Aarhus University [Aarhus], Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, ANR-16-CE31-0003,BEaPro,Using the most powerful explosion as probes of the high-redshift Universe(2016), ITA, USA, GBR, FRA, DEU, ESP, Agence Nationale de la Recherche (France), Comisión Nacional de Investigación Científica y Tecnológica (Chile), Ministerio de Economía y Competitividad (España), National Science Foundation (US), Icelandic Research Fund, Agenzia Spaziale Italiana, European Commission, Danish Council for Independent Research, API Other Research (FNWI), High Energy Astrophys. & Astropart. Phys (API, FNWI), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Weizmann Institute of Science, University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Université Paris-Sud - Paris 11 (UP11)-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), INAF-OAB, ASI-Science Data Center, Rome, APC - Astrophysique des Hautes Energies (APC - AHE), 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)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Aarhus University, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Sciences et Technologies - Bordeaux 1, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées, and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)

Subjects
absorption lines [Quasars], Astrophysics::High Energy Astrophysical Phenomena, general [Gamma rays], galaxies: halos, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, media_common.cataloged_instance, European union, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Independent research, media_common, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, gamma rays: general, quasars: absorption lines, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Christian ministry, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Humanities, halos [Galaxies]
Abstract

Full list of authors: Christensen, L.; Vergani, S. D.; Schulze, S.; Annau, N.; Selsing, J.; Fynbo, J. P. U.; de Ugarte Postigo, A.; Cañameras, R.; Lopez, S.; Passi, D.; Cortés-Zuleta, P.; Ellison, S. L.; D'Odorico, V.; Becker, G.; Berg, T. A. M.; Cano, Z.; Covino, S.; Cupani, G.; D'Elia, V.; Goldoni, P. Gomboc, A.; Hammer, F.; Heintz, K. E.; Jakobsson, P.; Japelj, J.; Kaper, L.; Malesani, D.; Møller, P.; Petitjean, P.; Pugliese, V.; Sánchez-Ramírez, R.; Tanvir, N. R.; Thöne, C. C.; Vestergaard, M.; Wiersema, K.; Worseck, G., Previous studies have shown that the incidence rate of intervening strong Mgii absorbers towards gamma-ray bursts (GRBs) were a factor of 2-4 higher than towards quasars. Exploring the similar sized and uniformly selected legacy data sets XQ-100 and XSGRB, each consisting of 100 quasar and 81 GRB afterglow spectra obtained with a single instrument (VLT/X-shooter), we demonstrate that there is no disagreement in the number density of strong Mgii absorbers with rest-frame equivalent widths W r > 1 Å towards GRBs and quasars in the redshift range 0:1 . z . 5. With large and similar sample sizes, and path length coverages of Δz = 57:8 and 254.4 for GRBs and quasars, respectively, the incidences of intervening absorbers are consistent within 1σ uncertainty levels at all redshifts. For absorbers at z < 2:3; the incidence towards GRBs is a factor of 1.5± 0.4 higher than the expected number of strong Mgii absorbers in Sloan Digital Sky Survey (SDSS) quasar spectra, while for quasar absorbers observed with X-shooter we find an excess factor of 1.4 ± 0.2 relative to SDSS quasars. Conversely, the incidence rates agree at all redshifts with reported high-spectralresolution quasar data, and no excess is found. The only remaining discrepancy in incidences is between SDSS Mgii catalogues and high-spectral-resolution studies. The rest-frame equivalent-width distribution also agrees to within 1σ uncertainty levels between the GRB and quasar samples. Intervening strong Mgii absorbers towards GRBs are therefore neither unusually frequent, nor unusually strong. © ESO 2017., L.C. and R.C. are supported by YDUN grant DFF 4090-00079. S.D.V. is supported by the French National Research Agency (ANR) under contract ANR-16-CE31-0003 BEaPro. S.L. has been supported by FONDECYT grant number 1140838 and partially by PFB-06 CATA. A.d.U.P. and C.T. acknowledge support from Ramon y Cajal fellowships, and with RSR a BBVA Foundation Grant for Researchers and Cultural Creators, and the Spanish Ministry of Economy and Competitiveness through project AYA2014-58381-P. G.B. acknowledges support from the National Science Foundation through grant AST-1615814. Z.C. acknowledges support from the Juan de la Cierva Incorporacion fellowship IJCI-2014-21669 and from the Spanish research project AYA2014-58381-P. P.J. and K.E.H. acknowledge support by a Project Grant (162948-051) from The Icelandic Research Fund. J.J. acknowledges support from NOVA and NWO-FAPESP grant for advanced instrumentation in astronomy. R.S.R. acknowledges support from ASI (Italian Space Agency) through the Contract No. 2015-046-R.0 and from European Union Horizon 2020 Programme under the AHEAD project (grant agreement No. 654215). M.V. gratefully acknowledges financial support from the Danish Council for Independent Research via grant no. DFF 4002-00275.

Published
2017

4. ULF/ELF ionospheric electric field and plasma perturbations related to Chile earthquakes

Author

Jiadong Qian, Roberto Battiston, Z. Zeren, Xuemin Zhang, Michel Parrot, Xuhui Shen, Institute of Earthquake Science [Beijing], China Earthquake Administration (CEA), Dipartimento di Fisica e Geologia [Perugia], Università degli Studi di Perugia = University of Perugia (UNIPG), Laboratoire de physique et chimie de l'environnement (LPCE), Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Trento (UNITN), ASI-Science Data Center, Rome, Laboratoire Réactions et Génie des Procédés (LRGP), Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'analyse et modélisation de systèmes pour l'aide à la décision (LAMSADE), Université Paris Dauphine-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), International Cooperation Project (2009DFA 21480) and the National Science and Technology Support Project (2008BAC35B01, 2008BAC35B05)., Università degli Studi di Perugia (UNIPG), and Université d'Orléans (UO)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Atmospheric Science, Electron density, 010504 meteorology & atmospheric sciences, Logarithm, Aerospace Engineering, Perturbation (astronomy), DEMETER, Ionospheric irregularity, 010502 geochemistry & geophysics, 01 natural sciences, Physics::Geophysics, Electric field, Space research, ULF/ELF electric field perturbation, 0105 earth and related environmental sciences, Remote sensing, Electron distribution, Physics, Chile earthquake, Astronomy and Astrophysics, Plasma, Geophysics, [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, Physics::Space Physics, General Earth and Planetary Sciences, Ionosphere
Abstract

International audience; LF/ELF electric field perturbations in the ionosphere have been widely observed by the satellites. In this paper, we develop a method of Logarithm Electric Field Intensity (LEFI) to automatically distinguish this kind of disturbances based on the spectrum intensity and its damping exponent with frequency in electromagnetic signals. This method is applied to DEMETER data processing around Chile earthquakes with magnitude larger than 6.0. It is found that 2/3 earthquakes have shown obvious ULF/ELF electric field perturbations in this region. The temporal and spatial distributions of electron density and temperature were compared with that of electric field, which proved the existence of irregularities above epicentral area. Finally, the coupling mechanism of earthquake-ionosphere is discussed based on multi-parameter analysis

Published
2011

5. Geospace perturbations induced by the Earth: The state of the art and future trends

Author

Loredana Perrone, Lucilla Alfonsi, Gianfranco Cianchini, Luca Spogli, Vito Vitale, Enkelejda Qamili, Stefano Salvi, Marco Tavani, Stephen Monna, P. Picozza, Michel Parrot, G. Piano, A. De Santis, Livio Conti, R. Di Giovambattista, W. Liu, G. De Franceschi, Georgios Balasis, D. Tao, E. Filippi, A. Argan, Jean-Louis Pinçon, Roberto Battiston, Fco. Javier Pavón-Carrasco, Mario Luigi Rainone, Alessandro Piscini, Istituto Nazionale di Geofisica e Vulcanologia, Università degli studi 'G. d'Annunzio' Chieti-Pescara [Chieti-Pescara] (Ud'A), Istituto Nazionale di Geofisica e Vulcanologia - Sezione di Roma (INGV), Università degli Studi di Trento (UNITN), ASI-Science Data Center, Rome, Laboratori Nazionali di Frascati (INFN), LABORATORY NAZIONALI DI FRASCATI, Department of Physiology and Pharmacology, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome]-Réseau International des Instituts Pasteur (RIIP)-Institut Pasteur, Fondation Cenci Bolognetti - Istituto Pasteur Italia, Fondazione Cenci Bolognetti, Réseau International des Instituts Pasteur (RIIP), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institute for Space Applications and Remote Sensing, National Observatory of Athens (NOA), GeoForschungsZentrum - Helmholtz-Zentrum Potsdam (GFZ), I.C.R.E, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Wuhan University [China], Beihang University (BUAA), project SAFE (Swarm For Earthquake study) funded by ESA., European Project: 316210,EC:FP7:REGPOT,FP7-REGPOT-2012-2013-1,BEYOND(2013), Institut Pasteur, Fondation Cenci Bolognetti - Istituto Pasteur Italia, Fondazione Cenci Bolognetti, and Réseau International des Instituts Pasteur (RIIP)-Réseau International des Instituts Pasteur (RIIP)-Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA)

Subjects
pulsars: individual: PSR J2043 + 2740, Process (engineering), Geophysics, gamma rays: stars, Natural (archaeology), Physics::Geophysics, Coupling (physics), Geochemistry and Petrology, [SDU]Sciences of the Universe [physics], Satellite data, Phenomenon, State (computer science), Geology, Anthropic principle
Abstract

International audience; A systematic multi-parameter and multi-platform approach to study the slow process of earthquake preparation is fundamental to gain some insights on this complex phenomenon. In particular, an important contribution is the integrated analysis between ground geophysical data and satellite data. In this paper we review some of the more recent results and suggest the next directions of this kind of research. Our intention is not to detect a particular precursor but to understand the physics underlying the various observations and to establish a reliable physical model of the preparation phase before an impending earthquake. In this way, future investigation will search for suitable fore-patterns, which the physical model of multi-layers coupling predicts and characterizes by quasi-synchronism in time and geo-consistency in space. We also present alternative explanations for some anomalies which are not actually related to earthquakes, rather to other natural or anthropic processes.

Published
2015

6. GRB 130427A: A nearby ordinary monster

Author

D. Bersier, T. A. Pritchard, B. Sbarufatti, P. D'Avanzo, Valerio D'Elia, A. Maselli, G. Calderone, Drejc Kopač, Paul Kuin, G. Tagliaferri, Phil Evans, J. A. Nousek, T. Sakamoto, H. Hanayama, Giacomo Vianello, Nobuyuki Kawai, J. P. Osborne, A. P. Beardmore, B. Wiegand, P. Romano, David N. Burrows, Neil Gehrels, A. Gomboc, M. Perri, Iain A. Steele, L. Nava, Taketoshi Yoshii, S. R. Oates, Nial R. Tanvir, S. D. Barthelmy, Chryssa Kouveliotou, C. Pagani, C. Guidorzi, Andrew J. Levan, Giancarlo Ghirlanda, J. A. Kennea, M. Capalbi, Shiho Kobayashi, M. de Pasquale, J. R. Cummings, Y. Yatsu, A. Melandri, M. G. Bernardini, R. Harrison, D. Malesani, V. La Parola, Giancarlo Cusumano, Klaas Wiersema, M. J. Page, P. T. O'Brien, Sergio Campana, B.-B. Zhang, V. Mangano, Y. Saito, James Chiang, F. E. Marshall, J. Japelj, K. L. Page, Stefano Covino, Carole Mundell, Fabio Virgili, Motoko Serino, Gabriele Ghisellini, Daisuke Kuroda, D. Fugazza, Ruben Salvaterra, INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), Racah Institute of Physics (Racah Institute of Physics), The Hebrew University of Jerusalem (HUJ)-Racah Institute of Physics, 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), RIKEN - Institute of Physical and Chemical Research [Japon] (RIKEN), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Kyoto University [Kyoto], Institut de médecine moléculaire de Rangueil (I2MR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-IFR150-Institut National de la Santé et de la Recherche Médicale (INSERM), Astrophysics Research Institute [Liverpool] (ARI), Liverpool John Moores University (LJMU), Chimie Et Interdisciplinarité : Synthèse, Analyse, Modélisation (CEISAM), Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), ASI-Science Data Center, Rome, NASA Goddard Space Flight Center (GSFC), Faculty of Mathematics and Physics [Ljubljana] (FMF), University of Ljubljana, Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Osservatorio Astrofisico di Catania, Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), INAF-IASF Milano, Department of Physics and Astronomy [Leicester], University of Leicester, Institute of Zoology, Universität Regensburg (UR), 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), Kyoto University, Université de Toulouse (UT)-Université de Toulouse (UT)- Institut Fédératif de Recherche Bio-médicale Institution (IFR150)-Institut National de la Santé et de la Recherche Médicale (INSERM), Université de Nantes (UN)-Université de Nantes (UN)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], and University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)

Subjects
media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, QB, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, [PHYS]Physics [physics], Multidisciplinary, Gamma ray, GRB 130427A, Light curve, Universe, Afterglow, Stars, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Long-duration Gamma-Ray Bursts (GRBs) are an extremely rare outcome of the collapse of massive stars, and are typically found in the distant Universe. Because of its intrinsic luminosity ($L\sim 3 \times 10^{53}$ erg s$^{-1}$) and its relative proximity ($z=0.34$), GRB 130427A was a unique event that reached the highest fluence observed in the gamma-ray band. Here we present a comprehensive multiwavelength view of GRB 130427A with Swift, the 2-m Liverpool and Faulkes telescopes and by other ground-based facilities, highlighting the evolution of the burst emission from the prompt to the afterglow phase. The properties of GRB 130427A are similar to those of the most luminous, high-redshift GRBs, suggesting that a common central engine is responsible for producing GRBs in both the contemporary and the early Universe and over the full range of GRB isotropic energies., 64 pages, 11 figures; published in Science. Update for a few references and correction of a typo in the name of one of the authors

Published
2014

7. GRB Orphan Afterglows in Present and Future Radio Transient Surveys

Author

Burlon, D., Tagliaferri, G., Vergani, S., Nava, L., Murphy, T., Melandri, A., D’Elia, V., D’Avanzo, P., Covino, S., Campana, S., Bernardini, M., Salvaterra, R., Ghisellini, G., Ghirlanda, G., DElia, V., DAvanzo, P., INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), INAF-IASF Milano, ASI-Science Data Center, Rome, Racah Institute of Physics (Racah Institute of Physics), The Hebrew University of Jerusalem (HUJ)-Racah Institute of Physics, 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), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and 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

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, [PHYS]Physics [physics], education.field_of_study, Count distribution, Population, Radio flux, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radio spectrum, 13. Climate action, Space and Planetary Science, Population synthesis, Transient (oscillation), Radio frequency, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, education, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

Orphan Afterglows (OA) are slow transients produced by Gamma Ray Bursts seen off-axis that become visible on timescales of days/years at optical/NIR and radio frequencies, when the prompt emission at high energies (X and gamma rays) has already ceased. Given the typically estimated jet opening angle of GRBs theta_jet ~ 3 deg, for each burst pointing to the Earth there should be a factor ~ 700 more GRBs pointing in other directions. Despite this, no secure OAs have been detected so far. Through a population synthesis code we study the emission properties of the population of OA at radio frequencies. OAs reach their emission peak on year-timescales and they last for a comparable amount of time. The typical peak fluxes (which depend on the observing frequency) are of few micro Jy in the radio band with only a few OA reaching the mJy level. These values are consistent with the upper limits on the radio flux of SN Ib/c observed at late times. We find that the OA radio number count distribution has a typical slope -1.7 at high fluxes and a flatter (-0.4) slope at low fluxes with a break at a frequency-dependent flux. Our predictions of the OA rates are consistent with the (upper) limits of recent radio surveys and archive searches for radio transients. Future radio surveys like VAST/ASKAP at 1.4 GHz should detect ~ 3x10^-3 OA deg^-2 yr-1, MeerKAT and EVLA at 8.4 GHz should see ~ 3x10^-1 OA deg-2 yr-1. The SKA, reaching the micro Jy flux limit, could see up to ~ 0.2-1.5 OA deg^-2 yr^-1. These rates also depend on the duration of the OA above a certain flux limit and we discuss this effect with respect to the survey cadence., (10 pages, 5 figures, 1 table) Accepted for publication by PASA

Published
2014

8. The optical SN 2012bz associated with the long GRB 120422A

Author

Gabriele Ghisellini, A. J. Castro-Tirado, Filomena Bufano, D. Bersier, Gianni Marconi, M. Della Valle, Emma S. Walker, Alexei V. Filippenko, Masaomi Tanaka, Sergio Campana, Gianpiero Tagliaferri, Patrizia Ferrero, Jinsong Deng, Ferdinando Patat, Paolo A. Mazzali, R. L. C. Starling, Stefano Covino, Chryssa Kouveliotou, Keiichi Maeda, Ivo Saviane, Silvia Piranomonte, L. A. Antonelli, Lorenzo Amati, Elena Pian, S. D. Vergani, N. Masetti, Ruben Salvaterra, P. D'Avanzo, G. Ghirlanda, Eliana Palazzi, Dino Fugazza, Valerio D'Elia, C. Guidorzi, A. Melandri, Ken'ichi Nomoto, Maria Grazia Bernardini, G. Chincarini, INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), ASI-Science Data Center, Rome, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Hôpital Européen Georges Pompidou [APHP] (HEGP), Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Hôpitaux Universitaires Paris Ouest - Hôpitaux Universitaires Île de France Ouest (HUPO), Astrophysics Research Institute [Liverpool] (ARI), Liverpool John Moores University (LJMU), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Fudan University, School of Information Science and Engineering, Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), CNR Institute of Atmospheric Sciences and Climate (ISAC), Consiglio Nazionale delle Ricerche (CNR), Centre d’Investigation Clinique [Tours] CIC 1415 (CIC ), Centre Hospitalier Régional Universitaire de Tours (CHRU Tours)-Hôpital Bretonneau-Université de Tours-Institut National de la Santé et de la Recherche Médicale (INSERM), INAF - Osservatorio Astronomico di Roma (OAR), INAF-IASF Milano, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), and Centre Hospitalier Régional Universitaire de Tours (CHRU Tours)-Hôpital Bretonneau-Université de Tours (UT)-Institut National de la Santé et de la Recherche Médicale (INSERM)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), gamma-ray burst: general, FOS: Physical sciences, Astrophysics, 01 natural sciences, Lower limit, Spectral line, Luminosity, 0103 physical sciences, supernovae: individual: SN2012bz, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Astronomy and Astrophysics, Light curve, Redshift, Galaxy, Supernova, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The association of Type Ic SNe with long-duration GRBs is well established. We endeavor, through accurate ground-based observational campaigns, to characterize these SNe at increasingly high redshifts. We obtained a series of optical photometric and spectroscopic observations of the Type Ic SN2012bz associated with the Swift long-duration GRB120422A (z=0.283) using the 3.6-m TNG and the 8.2-m VLT telescopes. The peak times of the light curves of SN2012bz in various optical filters differ, with the B-band and i'-band light curves reaching maximum at ~9 and ~23 rest-frame days, respectively. The bolometric light curve has been derived from individual bands photometric measurements, but no correction for the unknown contribution in the near-infrared (probably around 10-15%) has been applied. Therefore, the present light curve should be considered as a lower limit to the actual UV-optical-IR bolometric light curve. This pseudo-bolometric curve reaches its maximum (Mbol = -18.56 +/- 0.06) at 13 +/- 1 rest-frame days; it is similar in shape and luminosity to the bolometric light curves of the SNe associated with z, 7 pages, 6 figures, 2 tables, accepted for publication in Astronomy & Astrophysics

Published
2012

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

Author

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

Abstract

At the end of March 2015 the onboard software configuration of the Astrorivelatore Gamma a Immagini Leggero (AGILE) satellite was modified in order to disable the veto signal of the anticoincidence shield for the minicalorimeter instrument. The motivation for such a change was the understanding that the dead time induced by the anticoincidence prevented the detection of a large fraction of Terrestrial Gamma-Ray Flashes (TGFs). The configuration change was highly successful resulting in an increase of one order of magnitude in TGF detection rate. As expected, the largest fraction of the new events has short duration (<100 μs), and part of them has simultaneous association with lightning sferics detected by the World Wide Lightning Location Network. The new configuration provides the largest TGF detection rate surface density (TGFs/km 2 /yr) to date, opening prospects for improved correlation studies with lightning and atmospheric parameters on short spatial and temporal scales along the equatorial region.

Published
2015
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