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1. Measurement of the Ce 140 (n,y) cross section at n_TOF and its astrophysical implications for the chemical evolution of the universe

Author: Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. ANT - Advanced Nuclear Technologies Research Group, Amaducci, Simone, Colonna, Nicola, Cosentino, Luigi, Cristallo, Sergio, Finocchiaro, Paolo, Krticka, Milan, Massimi, Cristian, Mastromarco, Mario, Mazzone, Annamaria, Maugeri, Emilio Andrea, Mengoni, Alberto, Roederer, Ian U., Straniero, Oscar, Calviño Tavares, Francisco, Casanovas Hoste, Adrià, Cortés Rossell, Guillem Pere, Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. ANT - Advanced Nuclear Technologies Research Group, Amaducci, Simone, Colonna, Nicola, Cosentino, Luigi, Cristallo, Sergio, Finocchiaro, Paolo, Krticka, Milan, Massimi, Cristian, Mastromarco, Mario, Mazzone, Annamaria, Maugeri, Emilio Andrea, Mengoni, Alberto, Roederer, Ian U., Straniero, Oscar, Calviño Tavares, Francisco, Casanovas Hoste, Adrià, and Cortés Rossell, Guillem Pere
Abstract: 140 Ce (n, y) is a key reaction for slow neutron-capture (s-process) nucleosynthesis due to being a bottleneck in the reaction flow. For this reason, it was measured with high accuracy (uncertainty˜5%) at the n_TOF facility, with an unprecedented combination of a high purity sample and low neutron-sensitivity detectors. The measured Maxwellian averaged cross section is up to 40% higher than previously accepted values. Stellar model calculations indicate a reduction around 20% of the s-process contribution to the Galactic cerium abundance and smaller sizeable differences for most of the heavier elements. No variations are found in the nucleosynthesis from massive stars., I.U.R. acknowledges support from the U.S. National Science Foundation (Grants No. AST 1613536, No. AST 1815403/1815767, No. AST 2205847, and No. PHY1430152—Joint Institute for Nuclear Astrophysics—Chemical Evolution of the Elements). S.C. acknowledges funding by the European Union—NextGenerationEU RFFM4C2 1.1 PRIN 2022 project “2022RJLWHN URKA” and by INAF Theory Grant “Understanding R-process & Kilonovae Aspects (URKA).” The authors acknowledge support from the MSMT of the Czech Republic, the Charles University UNCE/SCI/013 project, and by the funding agencies of the participating institutes. The authors declare that they have no known competing financial interests or personal relationships that could have appeared to influence the work reported in this Letter., Article signat per 141 autors/es: S. Amaducci, N. Colonna, L. Cosentino, S. Cristallo, P. Finocchiaro, M. Krtička, C. Massimi, M. Mastromarco, A. Mazzone, E. A. Maugeri, A. Mengoni, I. U. Roederer, O. Straniero, S. Valenta, D. Vescovi, O. Aberle, V. Alcayne, J. Andrzejewski, L. Audouin, V. Babiano-Suarez, M. Bacak, M. Barbagallo, S. Bennett, E. Berthoumieux, J. Billowes, D. Bosnar, A. Brown, M. Busso, M. Caamaño, L. Caballero-Ontanaya, F. Calviño, M. Calviani, D. Cano-Ott, A. Casanovas, F. Cerutti, E. Chiaveri, G. Cortés, M. A. Cortés-Giraldo, L. A. Damone, P. J. Davies, M. Diakaki, M. Dietz, C. Domingo-Pardo, R. Dressler, Q. Ducasse, E. Dupont, I. Durán, Z. Eleme, B. Fernández-Domínguez, A. Ferrari, V. Furman, K. Göbel, R. Garg, A. Gawlik-Ramięga, S. Gilardoni, I. F. Gonçalves, E. González-Romero, C. Guerrero, F. Gunsing, H. Harada, S. Heinitz, J. Heyse, D. G. Jenkins, A. Junghans, F. Käppeler, Y. Kadi, A. Kimura, I. Knapová, M. Kokkoris, Y. Kopatch, D. Kurtulgil, I. Ladarescu, C. Lederer-Woods, H. Leeb, J. Lerendegui-Marco, S. J. Lonsdale, D. Macina, A. Manna, T. Martínez, A. Masi, P. Mastinu, E. Mendoza, V. Michalopoulou, P. M. Milazzo, F. Mingrone, J. Moreno-Soto, A. Musumarra, A. Negret, R. Nolte, F. Ogállar, A. Oprea, N. Patronis, A. Pavlik, J. Perkowski, C. Petrone, L. Piersanti, E. Pirovano, I. Porras, J. Praena, J. M. Quesada, D. Ramos-Doval, T. Rauscher, R. Reifarth, D. Rochman, C. Rubbia, M. Sabat ́e-Gilarte, A. Saxena, P. Schillebeeckx, D. Schumann, A. Sekhar, A. G. Smith, N. V. Sosnin, P. Sprung, A. Stamatopoulos, G. Tagliente, J. L. Tain, A. Tarifeño-Saldivia, L. Tassan-Got, Th. Thomas, P. Torres-Sánchez, A. Tsinganis, J. Ulrich, S. Urlass, G. Vannini, V. Variale, P. Vaz, A. Ventura, V. Vlachoudis, R. Vlastou, A. Wallner, P. J. Woods, T. Wright, P.Žugec, Postprint (published version)
Published: 2024

2. Prospects for combined analyses of hadronic emission from gamma-ray sources in the Milky Way with CTA and KM3NeT

Author: Universitat Politècnica de Catalunya. Departament de Física, KM3NeT Collaboration, CTA Consortium, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, Unbehaun, Tim, Mohrmann, Lars, Funk, Stefan, Aiello, Sebastiano, Albert, Arnauld, Alves Garre, Sergio, Aly, Zineb, Ambrosone, Antonio, Ameli, Fabrizio, André, Michel, Androutsou, E., Anghinolfi, Marco, Anguita, M., Aphecetche, Laurent, Ardid Ramírez, Miguel, Universitat Politècnica de Catalunya. Departament de Física, KM3NeT Collaboration, CTA Consortium, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, Unbehaun, Tim, Mohrmann, Lars, Funk, Stefan, Aiello, Sebastiano, Albert, Arnauld, Alves Garre, Sergio, Aly, Zineb, Ambrosone, Antonio, Ameli, Fabrizio, André, Michel, Androutsou, E., Anghinolfi, Marco, Anguita, M., Aphecetche, Laurent, and Ardid Ramírez, Miguel
Abstract: The Cherenkov Telescope Array and the KM3NeT neutrino telescopes are major upcoming facilities in the fields of gamma-ray and neutrino astronomy, respectively. Possible simultaneous production of rays and neutrinos in astrophysical accelerators of cosmic gamma-ray nuclei motivates a combination of their data. We assess the potential of a combined analysis of CTA and KM3NeT data to determine the contribution of hadronic emission processes in known Galactic gamma-ray emitters, comparing this result to the cases of two separate analyses. In doing so, we demonstrate the capability of GAMMAPY, an open-source software package for the analysis of gamma-ray data, to also process data from neutrino telescopes. For a selection of prototypical gamma-ray sources within our Galaxy, we obtain models for primary proton and electron spectra in the hadronic and leptonic emission scenario, respectively, by fitting published gamma-ray spectra. Using these models and instrument response functions for both detectors, we employ the GAMMAPY package to generate pseudo data sets, where we assume 200 h of CTA observations and 10 years of KM3NeT detector operation. We then apply a three-dimensional binned likelihood analysis to these data sets, separately for each instrument and jointly for both. We find that the largest benefit of the combined analysis lies in the possibility of a consistent modelling of the gamma-ray and neutrino emission. Assuming a purely leptonic scenario as input, we obtain, for the most favourable source, an average expected 68% credible interval that constrains the contribution of hadronic processes to the observed gamma-ray emission to below 15%., The KM3NeT Collaboration acknowledges the financial support of the funding agencies: Agence Nationale de la Recherche (contract ANR-15-CE31-0020), Centre National de la Recherche Scientifique (CNRS), Commission Européenne (FEDER fund and Marie Curie Program), LabEx UnivEarthS (ANR-10-LABX-0023 and ANR-18-IDEX-0001), Paris Île-de-France Region, France; Shota Rustaveli National Science Foundation of Georgia (SRNSFG, FR-22-13708), Georgia; The General Secretariat of Research and Innovation (GSRI), Greece; Istituto Nazionale di Fisica Nucleare (INFN), Ministero dell’Università e della Ricerca (MIUR), PRIN 2017 program (Grant NAT-NET 2017W4HA7S) Italy; Ministry of Higher Education, Scientific Research and Innovation, Morocco, and the Arab Fund for Economic and Social Development, Kuwait; Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO), the Netherlands; The National Science Centre, Poland (2021/41/N/ST2/01177); National Authority for Scientific Research (ANCS), Romania; Grants PID2021-124591NB-C41, -C42, -C43 funded by MCIN/AEI/ 10.13039/501100011033 and, as appropriate, by “ERDF A way of making Europe”, by the “European Union” or by the “European Union NextGenerationEU/PRTR”, Programa de Planes Complementarios I+D+I (refs. ASFAE/2022/023, ASFAE/2022/014), Programa Prometeo (PROMETEO/2020/019) and GenT (refs. CIDEGENT/2018/034, /2019/043, /2020/049, /2021/23) of the Generalitat Valenciana, Junta de Andalucía (ref. SOMM17/6104/UGR, P18-FR-5057), EU: MSC program (ref. 101025085), Programa María Zambrano (Spanish Ministry of Universities, funded by the European Union, NextGenerationEU), Spain; The European Union’s Horizon 2020 Research and Innovation Programme (ChETEC-INFRA – Project no. 101008324). T. Unbehaun, L. Mohrmann, and S. Funk are members of the CTA Consortium. The paper has been reviewed by the CTA Consortium Speakers and Publications Office. This research has made use of the “Prod 5” CTA instrument response functions provided by the CTA Consortium a, Peer Reviewed, Article signat per 274 autors: T. Unbehaun, L. Mohrmann, S. Funk, i membres del "KM3NeT Collaboration": S. Aiello, A. Albert, S. Alves Garre, Z. Aly, A. Ambrosone, F. Ameli, M. Andre, E. Androutsou, M. Anghinolfi, M. Anguita, L. Aphecetche, M. Ardid, S. Ardid, H. Atmani, J. Aublin, C. Bagatelas, L. Bailly-Salins, B. Baret, S. Basegmez du Pree, Y. Becherini, M. Bendahman, F. Benfenati, M. Benhassi, D. M. Benoit, E. Berbee, V. Bertin, S. Biagi, M. Boettcher, M. Bou Cabo, J. Boumaaza, M. Bouta, M. Bouwhuis, C. Bozza, R. M. Bozza, H. Brânzaş, F. Bretaudeau, R. Bruijn, J. Brunner, R. Bruno, E. Buis, R. Buompane, J. Busto, B. Caiffi, D. Calvo, S. Campion, A. Capone, F. Carenini, V. Carretero, T. Cartraud, P. Castaldi, V. Cecchini, S. Celli, L. Cerisy, M. Chabab, M. Chadolias, A. Chen, S. Cherubini, T. Chiarusi, M. Circella, R. Cocimano, J. A. B. Coelho, A. Coleiro, R. Coniglione, P. Coyle, A. Creusot, A. Cruz, G. Cuttone, R. Dallier, Y. Darras, A. De Benedittis, B. De Martino, V. Decoene, R. Del Burgo, L. S. Di Mauro, I. Di Palma, A. F. Díaz, D. Diego-Tortosa, C. Distefano, A. Domi, C. Donzaud, D. Dornic, M. Dörr, E. Drakopoulou, D. Drouhin, R. Dvornický, T. Eberl, A. Eddymaoui, T. van Eeden, M. Eff, D. van Eijk, I. El Bojaddaini, S. El Hedri, A. Enzenhöfer, G. Ferrara, M. D. Filipović, F. Filippini, L. A. Fusco, J. Gabriel, T. Gal, J. García Méndez, A. Garcia Soto, C. Gatius Oliver, N. Geißelbrecht, H. Ghaddari, L. Gialanella, B. K. Gibson, E. Giorgio, A. Girardi, I. Goos, S. R. Gozzini, R. Gracia, K. Graf, D. Guderian, C. Guidi, B. Guillon, M. Gutiérrez, H. van Haren, A. Heijboer, A. Hekalo, L. Hennig, J. J. Hernández-Rey, F. Huang, W. Idrissi Ibnsalih, G. Illuminati, C. W. James, M. de Jong, P. de Jong, B. J. Jung, P. Kalaczyński, O. Kalekin, U. F. Katz, N. R. Khan Chowdhury, A. Khatun, G. Kistauri, F. van der Knaap, A. Kouchner, V. Kulikovskiy, R. Kvatadze, M. Labalme, R. Lahmann, G. Larosa, C. Lastoria, A. Lazo, S. Le Stum, G. Lehaut, E. Leonora, N. Lessing, G. Levi, Membres del KM3Net: S. Aiello, A. Albert, S. Alves Garre, Z. Aly, A. Ambrosone, F. Ameli, M. Andre, E. Androutsou, M. Anghinolfi, M. Anguita, L. Aphecetche, M. Ardid, S. Ardid, H. Atmani, J. Aublin, C. Bagatelas, L. Bailly-Salins, B. Baret, S. Basegmez du Pree, Y. Becherini, M. Bendahman, F. Benfenati, M. Benhassi, D. M. Benoit, E. Berbee, V. Bertin, S. Biagi, M. Boettcher, M. Bou Cabo, J. Boumaaza, M. Bouta, M. Bouwhuis, C. Bozza, R. M. Bozza, H. Brânzaş, F. Bretaudeau, R. Bruijn, J. Brunner, R. Bruno, E. Buis, R. Buompane, J. Busto, B. Caiffi, D. Calvo, S. Campion, A. Capone, F. Carenini, V. Carretero, T. Cartraud, P. Castaldi, V. Cecchini, S. Celli, L. Cerisy, M. Chabab, M. Chadolias, A. Chen, S. Cherubini, T. Chiarusi, M. Circella, R. Cocimano, J. A. B. Coelho, A. Coleiro, R. Coniglione, P. Coyle, A. Creusot, A. Cruz, G. Cuttone, R. Dallier, Y. Darras, A. De Benedittis, B. De Martino, V. Decoene, R. Del Burgo, L. S. Di Mauro, I. Di Palma, A. F. Díaz, D. Diego-Tortosa, C. Distefano, A. Domi, C. Donzaud, D. Dornic, M. Dörr, E. Drakopoulou, D. Drouhin, R. Dvornický, T. Eberl, A. Eddymaoui, T. van Eeden, M. Eff, D. van Eijk, I. El Bojaddaini, S. El Hedri, A. Enzenhöfer, G. Ferrara, M. D. Filipović, F. Filippini, L. A. Fusco, J. Gabriel, T. Gal, J. García Méndez, A. Garcia Soto, C. Gatius Oliver, N. Geißelbrecht, H. Ghaddari, L. Gialanella, B. K. Gibson, E. Giorgio, A. Girardi, I. Goos, S. R. Gozzini, R. Gracia, K. Graf, D. Guderian, C. Guidi, B. Guillon, M. Gutiérrez, H. van Haren, A. Heijboer, A. Hekalo, L. Hennig, J. J. Hernández-Rey, F. Huang, W. Idrissi Ibnsalih, G. Illuminati, C. W. James, M. de Jong, P. de Jong, B. J. Jung, P. Kalaczyński, O. Kalekin, U. F. Katz, N. R. Khan Chowdhury, A. Khatun, G. Kistauri, F. van der Knaap, A. Kouchner, V. Kulikovskiy, R. Kvatadze, M. Labalme, R. Lahmann, G. Larosa, C. Lastoria, A. Lazo, S. Le Stum, G. Lehaut, E. Leonora, N. Lessing, G. Levi, M. Lindsey Clark, F. Longhitano, J. Majumdar, L. Malerba, J. Mańczak, A. Manfreda, Postprint (published version)
Published: 2024

3. Gamma-ray observations of MAXI J1820+070 during the 2018 outburst

Author: Abe, H., Abe, S., Acciari, V. A., Aniello, T., Ansoldi, S., Antonelli, L. A., Engels, A. Arbet, Arcaro, C., Artero, M., Asano, K., Baack, D., Babić, A., Baquero, A., de Almeida, U. Barres, Barrio, J. A., Batković, I., Baxter, J., González, J. Becerra, Bednarek, W., Bernardini, E., Bernardos, M., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Bošnjak, Ž., Burelli, I., Busetto, G., Carosi, R., Carretero-Castrillo, M., Ceribella, G., Chai, Y., Chilingarian, A., Cikota, S., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D'Amico, G., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Del Popolo, A., Delfino, M., Delgado, J., Mendez, C. Delgado, Depaoli, D., Di Pierro, F., Di Venere, L., Dominis Prester, D., Donini, A., Dorner, D., Doro, M., Elsaesser, D., Emery, G., Fallah Ramazani, V., Fariña, L., Fattorini, A., Font, L., Fruck, C., Fukami, S., Fukazawa, Y., López, R. J. García, Garczarczyk, M., Gasparyan, S., Gaug, M., Paiva, J. G. Giesbrecht, Giglietto, N., Giordano, F., Gliwny, P., Godinović, N., Grau, R., Green, D., Green, J. G., Hadasch, D., Hahn, A., Hassan, T., Heckmann, L., Herrera, J., Hoang, J., Hrupec, D., Hütten, M., Imazawa, R., Inada, T., Iotov, R., Ishio, K., Martínez, I. Jiménez, Jormanainen, J., Kerszberg, D., Kobayashi, Y., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Linhoff, L., Lombardi, S., Longo, F., López-Coto, R., López-Moya, M., López-Oramas, A., Loporchio, S., Lorini, A., Lyard, E., de Oliveira Fraga, B. Machado, Majumdar, P., Makariev, M., Maneva, G., Mang, N., Manganaro, M., Mangano, S., Mannheim, K., Mariotti, M., Martínez, M., Aguilar, A. Mas, Mazin, D., Menchiari, S., Mender, S., Mićanović, S., Miceli, D., Miener, T., Miranda, J. M., Mirzoyan, R., Molina, E., Mondal, H. A., Moralejo, A., Morcuende, D., Moreno, V., Nakamori, T., Nanci, C., Nava, L., Neustroev, V., Nievas Rosillo, M., Nigro, C., Nilsson, K., Nishijima, K., Ekoume, T. Njoh, Noda, K., Nozaki, S., Ohtani, Y., Oka, T., Okumura, A., Otero-Santos, J., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Pavletić, L., Persic, M., Pihet, M., Pirola, G., Podobnik, F., Prada Moroni, P. G., Prandini, E., Principe, G., Priyadarshi, C., Puljak, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Saturni, F. G., Schleicher, B., Schmidt, K., Schmuckermaier, F., Schubert, J. L., Schweizer, T., Sitarek, J., Sliusar, V., Sobczynska, D., Spolon, A., Stamerra, A., Strišković, J., Strom, D., Strzys, M., Suda, Y., Surić, T., Tajima, H., Takahashi, M., Takeishi, R., Tavecchio, F., Temnikov, P., Terauchi, K., Terzić, T., Teshima, M., Tosti, L., Truzzi, S., Tutone, A., Ubach, S., van Scherpenberg, J., Vazquez Acosta, M., Ventura, S., Verguilov, V., Viale, I., Vigorito, C. F., Vitale, V., Vovk, I., Walter, R., Will, M., Wunderlich, C., Yamamoto, T., Zarić, D., Abdalla, H., Aharonian, F., Benkhali, F. Ait, Angüner, E. O., Ashkar, H., Backes, M., Baghmanyan, V., Barbosa Martins, V., Batzofin, R., Becherini, Y., Berge, D., Bernlöhr, K., Böttcher, M., Boisson, C., Bolmont, J., de Bony de Lavergne, M., Bradascio, F., Breuhaus, M., Brose, R., Brun, F., Bulik, T., Bylund, T., Cangemi, F., Caroff, S., Casanova, S., Cerruti, M., Chand, T., Chandra, S., Chen, A., Chibueze, O. U., Cotter, G., Cristofari, P., Mbarubucyeye, J. Damascene, Devin, J., Djannati-Ataï, A., Dmytriiev, A., Egberts, K., Ernenwein, J.-P., Fiasson, A., Fichet de Clairfontaine, G., Fontaine, G., Füßling, M., Funk, S., Gabici, S., Ghafourizadeh, S., Giavitto, G., Glawion, D., Glicenstein, J. F., Goswami, P., Grolleron, G., Hinton, J. A., Hörbe, M., Hoischen, C., Holch, T. L., Holler, M., Horns, D., Huang, Zhiqiu, Jamrozy, M., Jankowsky, F., Joshi, V., Jung-Richardt, I., Kasai, E., Katarzyński, K., Katz, U., Khélifi, B., Kluźniak, W., Komin, Nu., Kosack, K., Kostunin, D., Lang, R. G., Le Stum, S., Lemière, A., Lemoine-Goumard, M., Lenain, J.-P., Leuschner, F., Lohse, T., Luashvili, A., Lypova, I., Mackey, J., Majumdar, J., Malyshev, D., Marandon, V., Marchegiani, P., Martí-Devesa, G., Marx, R., Maurin, G., Meyer, M., Mitchell, A., Moderski, R., Mohrmann, L., Montanari, A., Moulin, E., Muller, J., Murach, T., Nakashima, K., de Naurois, M., Nayerhoda, A., Niemiec, J., Noel, A. Priyana, O'Brien, P., Ohm, S., Olivera-Nieto, L., de Ona Wilhelmi, E., Ostrowski, M., Panny, S., Panter, M., Parsons, R. D., Poireau, V., Prokhorov, D. A., Prokoph, H., Pühlhofer, G., Punch, M., Quirrenbach, A., Reichherzer, P., Reimer, A., Reimer, O., Renaud, M., Rieger, F., Rowell, G., Rudak, B., Ricarte, H. Rueda, Ruiz-Velasco, E., Sahakian, V., Salzmann, H., Santangelo, A., Sasaki, M., Schäfer, J., Schüssler, F., Schutte, H. M., Schwanke, U., Shapopi, J. N. S., Sol, H., Specovius, A., Spencer, S., Stawarz, Ł., Steenkamp, R., Steinmassl, S., Steppa, C., Sushch, I., Suzuki, H., Takahashi, T., Tanaka, T., Thorpe-Morgan, C., Tluczykont, M., Tomankova, L., Tsuji, N., Uchiyama, Y., van Eldik, C., van Soelen, B., Vecchi, M., Veh, J., Venter, C., Vink, J., Wagner, S. J., White, R., Wierzcholska, A., Wong, Yu Wun, Yusafzai, A., Zacharias, M., Zanin, R., Zargaryan, D., Zdziarski, A. A., Zech, A., Zhu, S. J., Zouari, S., Żywucka, N., Acharyya, A., Adams, C. B., Batista, P., Benbow, W., Capasso, M., Christiansen, J. L., Chromey, A. J., Errando, M., Falcone, A., Feng, Q., Finley, J. P., Foote, G. M., Fortson, L., Furniss, A., Gent, A., Hanlon, W. F., Hervet, O., Holder, J., Hona, B., Humensky, T. B., Jin, W., Kaaret, P., Kertzman, M., Kherlakian, M., Kleiner, T. K., Kumar, S., Lang, M. J., Lundy, M., Maier, G., McGrath, C. E., Millis, J., Moriarty, P., Mukherjee, R., O'Brien, S., Ong, R. A., Park, N., Patel, S. R., Pfrang, K., Pohl, M., Pueschel, E., Quinn, J., Ragan, K., Reynolds, P. T., Ribeiro, D., Roache, E., Ryan, J. L., Sadeh, I., Saha, L., Santander, M., Sembroski, G. H., Shang, R., Splettstoesser, M., Tak, D., Tucci, J. V., Weinstein, A., Williams, D. A., Williamson, T. J., Bosch-Ramon, V., Celma, C., Linares, M., Russell, D. M., Sala, G., VERITAS Collaboration, H. E. S. S. Collaboration, MAGIC Collaboration, Astronomy, 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 Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de Physique des Deux Infinis Bordeaux (LP2I - Bordeaux), Université de Bordeaux (UB)-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), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM), MAGIC, H.E.S.S., VERITAS, Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, Federal Ministry of Education and Research (Germany), Istituto Nazionale di Astrofisica, Department of Atomic Energy (India), University of Tokyo, Ministry of Education and Science (Bulgaria), High Energy Astrophys. & Astropart. Phys (API, FNWI), and Gravitation and Astroparticle Physics Amsterdam
Subjects: individual: MAXI J1820+070 [stars], FOS: Physical sciences, X-rays: binaries, Raigs gamma, black holes [stars], gamma rays: general, stars: black holes, stars: individual: MAXI J1820+070, Estels binaris de raigs X, High Energy Astrophysical Phenomena (astro-ph.HE), Stars: individual: MAXI J1820+070 – gamma rays: general – stars: black holes – X-rays: binaries, Gamma rays, Astronomy and Astrophysics, X-ray binaries, Space and Planetary Science, HESS - Abteilung Hinton, ddc:520, binaries [X-rays], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, general [gamma rays]
Abstract: Full list of authors: Abe, H.; Abe, S.; Acciari, V. A.; Aniello, T.; Ansoldi, S.; Antonelli, L. A.; Engels, A. Arbet; Arcaro, C.; Artero, M.; Asano, K.; Baack, D.; Babic, A.; Baquero, A.; de Almeida, U. Barres; Barrio, J. A.; Batkovic, I; Baxter, J.; Gonzalez, J. Becerra; Bednarek, W.; Bernardini, E.; Bernardos, M.; Berti, A.; Besenrieder, J.; Bhattacharyya, W.; Bigongiari, C.; Biland, A.; Blanch, O.; Bonnoli, G.; Bosnjak, Z.; Burelli, I; Busetto, G.; Carosi, R.; Carretero-Castrillo, M.; Ceribella, G.; Chai, Y.; Chilingarian, A.; Cikota, S.; Colombo, E.; Contreras, J. L.; Cortina, J.; Covino, S.; D'Amico, G.; D'Elia, V; Da Vela, P.; Dazzi, F.; De Angelis, A.; De Lotto, B.; Del Popolo, A.; Delfino, M.; Delgado, J.; Mendez, C. Delgado; Depaoli, D.; Di Pierro, F.; Di Venere, L.; Prester, D. Dominis; Donini, A.; Dorner, D.; Doro, M.; Elsaesser, D.; Emery, G.; Ramazani, V. Fallah; Farina, L.; Fattorini, A.; Font, L.; Fruck, C.; Fukami, S.; Fukazawa, Y.; Lopez, R. J. Garcia; Garczarczyk, M.; Gasparyan, S.; Gaug, M.; Paiva, J. G. Giesbrecht; Giglietto, N.; Giordano, F.; Gliwny, P.; Godinovic, N.; Grau, R.; Green, D.; Green, J. G.; Hadasch, D.; Hahn, A.; Hassan, T.; Heckmann, L.; Herrera, J.; Hoang, J.; Hrupec, D.; Hutten, M.; Imazawa, R.; Inada, T.; Iotov, R.; Ishio, K.; Martinez, I. Jimenez; Jormanainen, J.; Kerszberg, D.; Kobayashi, Y.; Kubo, H.; Kushida, J.; Lamastra, A.; Lelas, D.; Leone, F.; Lindfors, E.; Linhoff, L.; Lombardi, S.; Longo, F.; Lopez-Coto, R.; Lopez-Moya, M.; Lopez-Oramas, A.; Loporchio, S.; Lorini, A.; Lyard, E.; Fraga, B. Machado de Oliveira; Majumdar, P.; Makariev, M.; Maneva, G.; Mang, N.; Manganaro, M.; Mangano, S.; Mannheim, K.; Mariotti, M.; Martinez, M.; Aguilar, A. Mas; Mazin, D.; Menchiari, S.; Mender, S.; Micanovic, S.; Miceli, D.; Miener, T.; Miranda, J. M.; Mirzoyan, R.; Molina, E.; Mondal, H. A.; Moralejo, A.; Morcuende, D.; Moreno, V; Nakamori, T.; Nanci, C.; Nava, L.; Neustroev, V; Rosillo, M. Nievas; Nigro, C.; Nilsson, K.; Nishijima, K.; Ekoume, T. Njoh; Noda, K.; Nozaki, S.; Ohtani, Y.; Oka, T.; Okumura, A.; Otero-Santos, J.; Paiano, S.; Palatiello, M.; Paneque, D.; Paoletti, R.; Paredes, J. M.; Pavletic, L.; Persic, M.; Pihet, M.; Pirola, G.; Podobnik, F.; Moroni, P. G. Prada; Prandini, E.; Principe, G.; Priyadarshi, C.; Puljak, I; Rhode, W.; Ribo, M.; Rico, J.; Righi, C.; Rugliancich, A.; Sahakyan, N.; Saito, T.; Sakurai, S.; Satalecka, K.; Saturni, F. G.; Schleicher, B.; Schmidt, K.; Schmuckermaier, F.; Schubert, J. L.; Schweizer, T.; Sitarek, J.; Sliusar, V; Sobczynska, D.; Spolon, A.; Stamerra, A.; Striskovic, J.; Strom, D.; Strzys, M.; Suda, Y.; Suric, T.; Tajima, H.; Takahashi, M.; Takeishi, R.; Tavecchio, F.; Temnikov, P.; Terauchi, K.; Terzic, T.; Teshima, M.; Tosti, L.; Truzzi, S.; Tutone, A.; Ubach, S.; van Scherpenberg, J.; Acosta, M. Vazquez; Ventura, S.; Verguilov, V.; Viale, I; Vigorito, C. F.; Vitale, V.; Vovk, I; Walter, R.; Will, M.; Wunderlich, C.; Yamamoto, T.; Zaric, D.; Abdalla, H.; Aharonian, F.; Benkhali, F. Ait; Anguner, E. O.; Ashkar, H.; Backes, M.; Baghmanyan, V; Martins, V. Barbosa; Batzofin, R.; Becherini, Y.; Berge, D.; Bernloehr, K.; Bottcher, M.; Boisson, C.; Bolmont, J.; de Lavergne, M. de Bony; Bradascio, F.; Breuhaus, M.; Brose, R.; Brun, F.; Bulik, T.; Bylund, T.; Cangemi, F.; Caroff, S.; Casanova, S.; Cerruti, M.; Chand, T.; Chandra, S.; Chen, A.; Chibueze, O. U.; Cotter, G.; Cristofari, P.; Mbarubucyeye, J. Damascene; Devin, J.; Djannati-Atai, A.; Dmytriiev, A.; Egberts, K.; Ernenwein, J-P; Fiasson, A.; de Clairfontaine, G. Fichet; Fontaine, G.; Fuessling, M.; Funk, S.; Gabici, S.; Ghafourizadeh, S.; Giavitto, G.; Glawion, D.; Glicenstein, J. F.; Goswami, P.; Grolleron, G.; Hinton, J. A.; Horbe, M.; Hoischen, C.; Holch, T. L.; Holler, M.; Horns, D.; Huang, Zhiqiu; Jamrozy, M.; Jankowsky, F.; Joshi, V; Jung-Richardt, I; Kasai, E.; Katarzynski, K.; Katz, U.; Khelifi, B.; Kluzniak, W.; Komin, Nu; Kosack, K.; Kostunin, D.; Lang, R. G.; Le Stum, S.; Lemiere, A.; Lemoine-Goumard, M.; Lenain, J-P; Leuschner, F.; Lohse, T.; Luashvili, A.; Lypova, I; Mackey, J.; Majumdar, J.; Malyshev, D.; Malyshev, D.; Marandon, V; Marchegiani, P.; Marti-Devesa, G.; Marx, R.; Maurin, G.; Meyer, M.; Mitchell, A.; Moderski, R.; Mohrmann, L.; Montanari, A.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, K.; de Naurois, M.; Nayerhoda, A.; Niemiec, J.; Noel, A. Pniyana; O'Brien, P.; Ohm, S.; Olivera-Nieto, L.; Wilhelmi, E. de Ona; Ostrowski, M.; Panny, S.; Panter, M.; Parsons, R. D.; Poireau, V; Prokhorov, D. A.; Prokoph, H.; Puehlhofer, G.; Punch, M.; Quirrenbach, A.; Reichherzer, P.; Reimer, A.; Reimer, O.; Renaud, M.; Rieger, F.; Rowell, G.; Rudak, B.; Ricarte, H. Rueda; Ruiz-Velasco, E.; Sahakian, V; Salzmann, H.; Santangelo, A.; Sasaki, M.; Schaefer, J.; Schussler, F.; Schutte, H. M.; Schwanke, U.; Shapopi, J. N. S.; Sol, H.; Specovius, A.; Spencer, S.; Stawarz, L.; Steenkamp, R.; Steinmassl, S.; Steppa, C.; Sushch, I; Suzuki, H.; Takahashi, T.; Tanaka, T.; Thorpe-Morgan, C.; Tluczykont, M.; Tomankova, L.; Tsuji, N.; Uchiyama, Y.; van Eldik, C.; van Soelen, B.; Vecchi, M.; Veh, J.; Venter, C.; Vink, J.; Wagner, S. J.; White, R.; Wierzcholska, A.; Wong, Yu Wun; Yusafzai, A.; Zacharias, M.; Zanin, R.; Zargaryan, D.; Zdziarski, A. A.; Zech, A.; Zhu, S. J.; Zouari, S.; Zywucka, N.; Acharyya, A.; Adams, C. B.; Batista, P.; Benbow, W.; Capasso, M.; Christiansen, J. L.; Chromey, A. J.; Errando, M.; Falcone, A.; Feng, Q.; Finley, J. P.; Foote, G. M.; Fortson, L.; Furniss, A.; Gent, A.; Hanlon, W. E.; Hervet, O.; Holder, J.; Hona, B.; Humensky, T. B.; Jin, W.; Kaaret, P.; Kertzman, M.; Kherlakian, M.; Kleiner, T. K.; Kumar, S.; Lang, M. J.; Lundy, M.; Maier, G.; McGrath, C. E.; Millis, J.; Moriarty, P.; Mukherjee, R.; O'Brien, S.; Ong, R. A.; Park, N.; Patel, S. R.; Pfrang, K.; Pohl, M.; Pueschel, E.; Quinn, J.; Ragan, K.; Reynolds, P. T.; Ribeiro, D.; Roache, E.; Ryan, J. L.; Sadeh, I; Saha, L.; Santander, M.; Sembroski, G. H.; Shang, R.; Splettstoesser, M.; Tak, D.; Tucci, J., V; Weinstein, A.; Williams, D. A.; Williamson, T. J.; Bosch-Ramon, V; Celma, C.; Linares, M.; Russell, D. M.; Sala, G.; MAGIC Collaboration; H E S S Collaboration; VERITAS Collaboration., MAXI J1820+070 is a low-mass X-ray binary with a black hole (BH) as a compact object. This binary underwent an exceptionally bright X-ray outburst from 2018 March to October, showing evidence of a non-thermal particle population through its radio emission during this whole period. The combined results of 59.5 h of observations of the MAXI J1820+070 outburst with the H.E.S.S., MAGIC and VERITAS experiments at energies above 200 GeV are presented, together with Fermi-LAT data between 0.1 and 500 GeV, and multiwavelength observations from radio to X-rays. Gamma-ray emission is not detected from MAXI J1820+070, but the obtained upper limits and the multiwavelength data allow us to put meaningful constraints on the source properties under reasonable assumptions regarding the non-thermal particle population and the jet synchrotron spectrum. In particular, it is possible to show that, if a high-energy (HE) gamma-ray emitting region is present during the hard state of the source, its predicted flux should be at most a factor of 20 below the obtained Fermi-LAT upper limits, and closer to them for magnetic fields significantly below equipartition. During the state transitions, under the plausible assumption that electrons are accelerated up to ∼500 GeV, the multiwavelength data and the gamma-ray upper limits lead consistently to the conclusion that a potential HE and very-HE gamma-ray emitting region should be located at a distance from the BH ranging between 1011 and 1013 cm. Similar outbursts from low-mass X-ray binaries might be detectable in the near future with upcoming instruments such as CTA. © 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society., MAGIC acknowledgements: MAGIC would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF, MPG, and HGF; the Italian INFN and INAF; the Swiss National Fund SNF; the grants PID2019-104114RB-C31, PID2019-104114RB-C32, PID2019-104114RB-C33, PID2019-105510GB-C31, PID2019-107847RB-C41, PID2019-107847RB-C42, PID2019-107847RB-C44, PID2019-107988GB-C22 funded by MCIN/AEI/ 10.13039/501100011033; the Indian Department of Atomic Energy; the Japanese ICRR, the University of Tokyo, JSPS, and MEXT; the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-400/18.12.2020 and the Academy of Finland grant nr. 320045 is gratefully acknowledged. This work was also been supported by Centros de Excelencia ‘Severo Ochoa’ y Unidades ‘María de Maeztu’ program of the MCIN/AEI/ 10.13039/501100011033 (SEV-2016-0588, SEV-2017-0709, CEX2019-000920-S, CEX2019-000918-M, MDM-2015-0509-18-2) and by the CERCA institution of the Generalitat de Catalunya; by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project uniri-prirod-18-48; by the DFG Collaborative Research Centers SFB1491 and SFB876/C3; the Polish Ministry Of Education and Science grant No. 2021/WK/08; and by the Brazilian MCTIC, CNPq and FAPERJ. H.E.S.S. acknowledgements: the support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the German Research Foundation (DFG), the Helmholtz Association, the Alexander von Humboldt Foundation, the French Ministry of Higher Education, Research and Innovation, the Centre National de la Recherche Scientifique (CNRS/IN2P3 and CNRS/INSU), the Commissariat à l’énergie atomique et aux énergies alternatives (CEA), the U.K. Science and Technology Facilities Council (STFC), the Irish Research Council (IRC) and the Science Foundation Ireland (SFI), the Knut and Alice Wallenberg Foundation, the Polish Ministry of Education and Science, agreement no. 2021/WK/06, the South African Department of Science and Technology and National Research Foundation, the University of Namibia, the National Commission on Research, Science & Technology of Namibia (NCRST), the Austrian Federal Ministry of Education, Science and Research and the Austrian Science Fund (FWF), the Australian Research Council (ARC), the Japan Society for the Promotion of Science, the University of Amsterdam and the Science Committee of Armenia grant 21AG-1C085. We appreciate the excellent work of the technical support staff in Berlin, Zeuthen, Heidelberg, Palaiseau, Paris, Saclay, Tübingen and in Namibia in the construction and operation of the equipment. This work benefited from services provided by the H.E.S.S. Virtual Organisation, supported by the national resource providers of the EGI Federation. VERITAS acknowledgements: VERITAS is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, and by the Helmholtz Association in Germany. This research used resources provided by the Open Science Grid, which is supported by the National Science Foundation and the U.S. Department of Energy’s Office of Science, and resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under Contract No. DE-AC02-05CH11231. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. E. Molina acknowledges support from MCIN through grant BES-2016-076342. V. Bosch-Ramon acknowledges financial support from the State Agency for Research of the Spanish Ministry of Science and Innovation under grant PID2019-105510GB-C31 and through the ‘Unit of Excellence María de Maeztu 2020-2023 award to the Institute of Cosmos Sciences (CEX2019-000918-M). V. Bosch-Ramon is Correspondent Researcher of CONICET, Argentina, at the IAR. M. Linares has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 101002352). G. Sala acknowledges support from the Spanish MINECO grant PID2020-117252GB-I00.
Published: 2022

4. Uncertainties in the 18F(p, α)15O reaction rate in classical novae

Author: D. Kahl, Philip Woods, Jordi José, Universitat Politècnica de Catalunya. Departament de Física, and Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica
Subjects: Thermonuclear fusion, Nuclear Theory, Abundance (chemistry), cataclysmic variables [Novae], Context (language use), Astrophysics, Novae: cataclysmic variables, Reaction rate, white dwarfs [Stars], Gamma rays: stars, Raigs gamma, Nuclear astrophysics, Novae, Physics, Range (particle radiation), cataclysmic variables, Física [Àrees temàtiques de la UPC], Gamma rays, stars [Gamma rays], Stars: abundances, White dwarf, White dwarfs, Astronomy and Astrophysics, Nova (laser), Stars, New, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, abundances [Stars], Astrophysics - High Energy Astrophysical Phenomena, White dwarf stars
Abstract: Context. Direct observation of gamma-ray emission from the decay of $^{18}$F ejected in classical nova outbursts remains a major focus of the nuclear astrophysics community. However, modeling the abundance of ejected $^{18}$F, and thus the predicted detectability distance of a gamma-ray signal near 511 keV emitted from these transient thermonuclear episodes, is hampered by significant uncertainties in our knowledge of the key $^{18}$F(p,$\alpha$) reaction rate. Aims. We analyze uncertainties in the most recent nuclear physics experimental results employed to calculate the $^{18}$F(p,$\alpha$) reaction rate. Our goal is to determine which uncertainties have the most profound influence on the predicted abundance of $^{18}$F ejected from novae, in order to guide future experimental works. Methods. We calculated a wide range of $^{18}$F(p,$\alpha$) reaction rates using R-Matrix formalism, allowing us to take into account all interference effects. Using a selection of 16 evenly-spaced rates over the full range, we performed 16 new hydrodynamic nova simulations. Results. We performed one of the most thorough theoretical studies of the impact of the $^{18}$F(p,$\alpha$) reaction in classical novae to date. The $^{18}$F(p,$\alpha$) rate remains highly uncertain at nova temperatures, resulting in a factor ~10 uncertainty in the predicted abundance of $^{18}$F ejected from nova explosions. We also found that the abundance of $^{18}$F may be strongly correlated with that of $^{19}$F. Conclusions. Despite numerous nuclear physics uncertainties affecting the $^{18}$F(p,$\alpha$) reaction rate, which are dominated by unknown interference signs between 1/2$^+$ and 3/2$^+$ resonances, future experimental work should focus on firmly and precisely determining the directly measurable quantum properties of the subthreshold states in the compound nucleus $^{19}$Ne near 6.13 and 6.29 MeV., Comment: Accepted for publication in Astronomy & Astrophysics 4 June 2021 as manuscript no. AA/2021/40339
Published: 2021

5. Tropical TGF paradox: a perspective from TRMM precipitation radar

Author: Universitat Politècnica de Catalunya. Departament d'Enginyeria Elèctrica, Universitat Politècnica de Catalunya. LRG - Lightning Research Group, Morales Rodríguez, Carlos Augusto, Montanya Puig, Joan, Van der Velde, Oscar Arnoud, Fabró Tàpia, Ferran, López Trujillo, Jesús Alberto, Universitat Politècnica de Catalunya. Departament d'Enginyeria Elèctrica, Universitat Politècnica de Catalunya. LRG - Lightning Research Group, Morales Rodríguez, Carlos Augusto, Montanya Puig, Joan, Van der Velde, Oscar Arnoud, Fabró Tàpia, Ferran, and López Trujillo, Jesús Alberto
Abstract: The Terrestrial Gamma-ray Flash (TGF) to lightning ratio, computed over the three tropical chimneys, presents a paradox: African thunderstorms produce the most lightning but yield the lowest fraction of TGFs when compared to American and Southeast Asian thunderstorms. To understand the physical insights into this asymmetry, Tropical Rainfall Measuring Mission Precipitation Radar measurements are used to depict the vertical precipitation structure and infer the vertical electrical charge fraction distribution of the observed thunderstorms in the three regions and the thunderstorms during TGF occurrences detected by the AGILE, Fermi-GBM, and RHESSI sensors. Regional differences show that African thunderstorms are taller, smaller, and have a higher concentration of denser ice particles (graupel and or hail) above the freezing level in addition to having more lightning flashes per thunderstorm. The overall TGF-related thunderstorms are taller, more intense (0.5–1.5 dBZ) and present similar radar reflectivity decay with height independent of the region. The two dimensional precipitation vertical distribution diagrams indicate that TGF thunderstorms develop to a mature stage. Independent of the region, thunderstorms show a midlevel negative charge center varying from 4.6 to 8.1 km in height and an upper level positive charge center ranging from 7.4 to 14.6 km. TGF thunderstorms have thicker positive inferred charge layer and present larger vertical distances between the opposite charging layers in comparison with the overall thunderstorm population, here defined as Climatology. African TGF thunderstorms have higher fraction of positive charges near the negative layer, helping to produce more and shorter lightning discharges., Peer Reviewed, Postprint (author's final draft)
Published: 2021

6. ANTARES upper limits on the multi-TeV neutrino emission from the GRBs detected by IACTs

Author: Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, Albert, A., André, Michel, Anghinolfi, Marco, Anton, Gisela, Ardid Ramírez, Miguel, Aubert, J.-J., Aublin, J., Baret, B., Basa, Stéphane, Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, Albert, A., André, Michel, Anghinolfi, Marco, Anton, Gisela, Ardid Ramírez, Miguel, Aubert, J.-J., Aublin, J., Baret, B., and Basa, Stéphane
Abstract: The first gamma-ray burst detections by Imaging Atmospheric Cherenkov Telescopes have been recently announced: GRB 190114C, detected by MAGIC, GRB 180720B and GRB 190829A, observed by H.E.S.S. A dedicated search for neutrinos in space and time coincidence with the gammaray emission observed by IACTs has been performed using ANTARES data. The search covers both the prompt and afterglow phases, yielding no neutrinos in coincidence with the three GRBs studied. Upper limits on the energetics of the neutrino emission are inferred. The resulting upper limits are several orders of magnitude above the observed gamma-ray emission, and they do not allow to constrain the available models., Peer Reviewed, Postprint (author's final draft)
Published: 2021

7. Constraining the contribution of gamma-ray bursts to the high-energy diffuse neutrino flux with 10 yr of ANTARES data

Author: Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, Albert, A., André, Michel, Anghinolfi, Marco, Anton, Gisela, Ardid Ramírez, Miguel, Aubert, J.-J., Aublin, J., Baret, Bruny, Basa, S., Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, Albert, A., André, Michel, Anghinolfi, Marco, Anton, Gisela, Ardid Ramírez, Miguel, Aubert, J.-J., Aublin, J., Baret, Bruny, and Basa, S.
Abstract: Addressing the origin of the astrophysical neutrino flux observed by IceCube is of paramount importance. Gamma-Ray Bursts (GRBs) are among the few astrophysical sources capable of achieving the required energy to contribute to such neutrino flux through p¿ interactions. In this work, ANTARES data have been used to search for upward going muon neutrinos in spatial and temporal coincidence with 784 GRBs occurred from 2007 to 2017. For each GRB, the expected neutrino flux has been calculated in the framework of the internal shock model and the impact of the lack of knowledge on the majority of source redshifts and on other intrinsic parameters of the emission mechanism has been quantified. It is found that the model parameters that set the radial distance where shock collisions occur have the largest impact on neutrino flux expectations. In particular, the bulk Lorentz factor of the source ejecta and the minimum variability timescale are found to contribute significantly to the GRB-neutrino flux uncertainty. For the selected sources, ANTARES data have been analysed, by maximising the discovery probability of the stacking sample through an extended maximum-likelihood strategy. Since no neutrino event passed the quality cuts set by the optimisation procedure, 90 % confidence level upper limits (with their uncertainty) on the total expected diffuse neutrino flux have been derived, according to the model. The GRB contribution to the observed diffuse astrophysical neutrino flux around 100 TeV is constrained to be less than 10 %., Peer Reviewed, Postprint (author's final draft)
Published: 2021

8. Search for correlations between high-energy gamma rays and neutrinos with the HAWC and ANTARES detectors

Author: Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, Alves Garre, Sergio, André, Michel, Anghinolfi, Marco, Anton, Gisela, Ardid Ramírez, Miguel, Aublin, J., Belhorma, Bouchra, Bendahman, Meriem, Bertin, Vincent, Bissinger, Matthias, Boumaaza, Jihad, Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, Alves Garre, Sergio, André, Michel, Anghinolfi, Marco, Anton, Gisela, Ardid Ramírez, Miguel, Aublin, J., Belhorma, Bouchra, Bendahman, Meriem, Bertin, Vincent, Bissinger, Matthias, and Boumaaza, Jihad
Abstract: ANTARES is an underwater neutrino detector in the Mediterranean Sea. Its location, reconstruction accuracy for all-flavor neutrino interactions, and low energy threshold, make it the most sensitive neutrino observatory for searches below 100 TeV over large parts of the sky. The HAWC experiment is a water Cherenkov gamma-ray detector located in Mexico. Thanks to its large field of view it is an excellent instrument to observe the very-high energy gamma-ray sky and perform high-sensitivity surveys of the Galactic Plane. The 10-year ANTARES data set and 3-year HAWC point source surveys are used to search for all-flavor neutrino emission in correlation with the highly-significant observations by HAWC in the gamma-ray sky by means of a maximumlikelihood template search. No significant observation for a correlation has been identified and upper limits on the neutrino flux from the HAWC observations have been set., Article signat per 276 autors/es: A. Albert, S. Alves, M. André, M. Anghinolfi, G. Anton, M. Ardid, S. Ardid, J.-J. Aubert, J. Aublin, B. Baret, S. Basa,B. Belhorma, B. Belhorma, M. Bendahman, V. Bertin, S. Biagi, M. Bissinger, J. Boumaaza, M. Bouta, M.C. Bouwhuis, H. Brânzas, R. Bruijn, J. Brunner, J. Busto, B. Caiffi, A. Capone, L. Caramete, J. Carr, V. Carretero, S. Celli, M. Chabab,T. N. Chau, R. Cherkaoui El Moursli, T. Chiarusi, M. Circella, A. Coleiro, M. Colomer-Molla, R. Coniglione, P. Coyle, A. Creusot, A. F. Díaz, G. de Wasseige, A. Deschamps, C. Distefano, I. Di Palma, A. Domi, C. Donzaud, D. Dornic, D. Drouhin, T. Eberl, T. van Eeden, D. van Eijk, N. El Khayati, A. Enzenhöfer, P. Fermani, G. Ferrara, F. Filippini, L.A. Fusco, Y. Gatelet, P. Gay, H. Glotin, R. Gozzini, R. Gracia Ruiz, K. Graf, C. Guidi, S. Hallmann, H. van Haren, A.J. Heijboer, Y. Hello, J.J. Hernández-Rey, J. Hößl, J. Hofestädt, F. Huang, G. Illuminati, C.W James, B. Jisse-Jung, M. de Jong, P. de Jong, M. Kadler, O. Kalekin, U. Katz, N.R. Khan Chowdhury, A. Kouchner, I. Kreykenbohm, V. Kulikovskiy, R. Lahmann, R. Le Breton, D. Lefèvre, E. Leonora, G. Levi, M. Lincetto, D. Lopez-Coto, S. Loucatos, L. Maderer, J. Manczak, M. Marcelin, A. Margiotta, A. Marinelli, J.A. Martínez-Mora, K. Melis, P. Migliozzi, A. Moussa, R. Muller, L.Nauta, S.Navas, E.Nezri, B. O’Fearraigh, A. Paun, G.E. Pavalas, C. Pellegrino, M. Perrin-Terrin,V. Pestel, P. Piattelli, C. Pieterse, C. Poirè,V. Popa, T. Pradier,N. Randazzo, S.Reck, G. Riccobene, A. Romanov, A. Sánchez-Losa, F. Salesa Greus, D. F. E. Samtleben, M. Sanguineti, P. Sapienza, J. Schnabel, J. Schumann, F. Schüssler, M. Spurio, Th. Stolarczyk, M. Taiuti, Y. Tayalati, S.J. Tingay, B. Vallage, V. Van Elewyck, F. Versari, S. Viola, D. Vivolo, J. Wilms, S. Zavatarelli5, A. Zegarelli, J.D. Zornoza, and J. Zúñiga. A.U. Abeysekara, A. Albert, R. Alfaro, C. Alvarez, J.D. Álvarez, J.R. Angeles Camacho, J.C. Arteaga-Velázquez, K. P. Arunbabu, D. Avila Rojas, H., Postprint (published version)
Published: 2021

9. Uncertainties in the 18F(p, a)15O reaction rate in classical novae

Author: Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica, Kahl, D., José Pont, Jordi, Woods, Phil J., Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica, Kahl, D., José Pont, Jordi, and Woods, Phil J.
Abstract: Context. Direct observation of ¿-ray emission from the decay of 18F ejected in classical nova outbursts remains a major focus of the nuclear astrophysics community. However, modeling the abundance of ejected 18F, and thus the predicted detectability distance of a ¿-ray signal near 511 keV emitted from these transient thermonuclear episodes, is hampered by significant uncertainties in our knowledge of the key 18F(p, a) reaction rate. Aims. We analyze uncertainties in the most recent nuclear physics experimental results employed to calculate the 18F(p, a) reaction rate. Our goal is to determine which uncertainties have the most profound influence on the predicted abundance of 18F ejected from novae in order to guide future experimental works. Methods. We calculated a wide range of 18F(p, a) reaction rates using the R-Matrix formalism, which allowed us to take all interference effects into account. Using a selection of 16 evenly spaced rates over the full range, we performed 16 new hydrodynamic nova simulations. Results. We have performed one of the most thorough theoretical studies of the impact of the 18F(p, a) reaction in classical novae to date. The 18F(p, a) rate remains highly uncertain at nova temperatures, resulting in a factor of ~10 uncertainty in the predicted abundance of 18F ejected from nova explosions. We also found that the abundance of 18F may be strongly correlated with that of 19F. Conclusions. Despite numerous nuclear physics uncertainties affecting the determination of the 18F(p, a) reaction rate, dominated by unknown interference signs between 1/2+ and 3/2+ resonances, future experimental work should focus on firmly and precisely determining the directly measurable quantum properties of the subthreshold states in the compound nucleus 19Ne near 6.13 and 6.29 MeV., Postprint (author's final draft)
Published: 2021

10. Determining the probability of locating peaks using computerized peak-location methods in gamma-ray spectra as a function of the relative peak-area uncertainty

Author: Universitat Politècnica de Catalunya. Institut de Tècniques Energètiques, Universitat Politècnica de Catalunya. DRM - Dosimetria i Radiofísica Mèdica, Ali Santoro, María Del Carmen, Boshkova, Tatiana, Anagnostakis, Mario J., Camacho García, Antonia, Fornaciari Iljadica, Marra C., Collins, Sean M., Ubiratan Delgado, José, Universitat Politècnica de Catalunya. Institut de Tècniques Energètiques, Universitat Politècnica de Catalunya. DRM - Dosimetria i Radiofísica Mèdica, Ali Santoro, María Del Carmen, Boshkova, Tatiana, Anagnostakis, Mario J., Camacho García, Antonia, Fornaciari Iljadica, Marra C., Collins, Sean M., and Ubiratan Delgado, José
Abstract: The probabilities of locating peaks with a high relative peak-area uncertainty were determined empirically with nine types of peak-location software used in laboratories engaged in gamma-ray spectrometry measurements. It was found that it is not possible to locate peaks with a probability of 0.95, when they have a relative peak-area uncertainty in excess of 50%. Locating peaks at these relatively high peak-area uncertainties with a probability greater than 0.95 is only possible in the library-driven mode, where the peak positions are supposed a-priori. The deficiencies of the library-driven mode and the possibilities to improve the probabilities of locating peaks are briefly discussed., Postprint (author's final draft)
Published: 2020

11. Tropical TGF Paradox: A Perspective From TRMM Precipitation Radar

Author: Jesús López, Ferran Fabró, Oscar van der Velde, Joan Montanyà, Carlos Augusto Morales Rodriguez, Universitat Politècnica de Catalunya. Departament d'Enginyeria Elèctrica, and Universitat Politècnica de Catalunya. LRG - Lightning Research Group
Subjects: Atmospheric Science, Enginyeria elèctrica [Àrees temàtiques de la UPC], Gamma rays, Geofísica, Lightning, law.invention, Geophysics, Raigs gamma, Space and Planetary Science, law, Climatology, Earth and Planetary Sciences (miscellaneous), Thunderstorm, Environmental science, Precipitation, Radar
Abstract: The Terrestrial Gamma-ray Flash (TGF) to lightning ratio, computed over the three tropical chimneys, presents a paradox: African thunderstorms produce the most lightning but yield the lowest fraction of TGFs when compared to American and Southeast Asian thunderstorms. To understand the physical insights into this asymmetry, Tropical Rainfall Measuring Mission Precipitation Radar measurements are used to depict the vertical precipitation structure and infer the vertical electrical charge fraction distribution of the observed thunderstorms in the three regions and the thunderstorms during TGF occurrences detected by the AGILE, Fermi-GBM, and RHESSI sensors. Regional differences show that African thunderstorms are taller, smaller, and have a higher concentration of denser ice particles (graupel and or hail) above the freezing level in addition to having more lightning flashes per thunderstorm. The overall TGF-related thunderstorms are taller, more intense (0.5–1.5 dBZ) and present similar radar reflectivity decay with height independent of the region. The two dimensional precipitation vertical distribution diagrams indicate that TGF thunderstorms develop to a mature stage. Independent of the region, thunderstorms show a midlevel negative charge center varying from 4.6 to 8.1 km in height and an upper level positive charge center ranging from 7.4 to 14.6 km. TGF thunderstorms have thicker positive inferred charge layer and present larger vertical distances between the opposite charging layers in comparison with the overall thunderstorm population, here defined as Climatology. African TGF thunderstorms have higher fraction of positive charges near the negative layer, helping to produce more and shorter lightning discharges.
Published: 2021

12. The Major Role of Eccentricity in the Evolution of Colliding Pulsar-Stellar Winds

Author: Valentí Bosch-Ramon, Maxim V. Barkov, and Ministerio de Ciencia, Innovación y Universidades (España)
Subjects: 010504 meteorology & atmospheric sciences, media_common.quotation_subject, stars [Gamma-rays], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, General Physics and Astronomy, Binary number, Scale (descriptive set theory), Outflows, QC793-793.5, Astrophysics, Star (graph theory), 01 natural sciences, X-rays: binaries, Raigs gamma, Pulsar, 0103 physical sciences, X-rays, Eccentricity (behavior), Temporal scales, winds [Stars], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Hidrodinàmica, Gamma-rays: stars, Gamma rays, Elementary particle physics, Stars: winds, Orbit (dynamics), Hydrodynamics, Outflow, binaries [X-rays], Astrophysics::Earth and Planetary Astrophysics, Raigs X, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Binary systems that host a massive star and a non-accreting pulsar can be powerful non-thermal emitters. The relativistic pulsar wind and the non-relativistic stellar outflows interact along the orbit, producing ultrarelativistic particles that radiate from radio to gamma rays. To properly characterize the physics of these sources, and better understand their emission and impact on the environment, careful modelling of the outflow interactions, spanning a broad range of spatial and temporal scales, is needed. Full 3-dimensional approaches are very computationally expensive, but simpler approximate approaches, while still realistic at the semi-quantitative level, are available. We present here the results of calculations done with a quasi 3-dimensional scheme to compute the evolution of the interacting flows in a region spanning in size up to a thousand times the size of the binary. In particular, we analyze for the first time the role of different eccentricities in the large scale evolution of the shocked flows. We find that the higher the eccentricity, the closer the flows behave like a one-side outflow, which becomes rather collimated for eccentricity values $\gtrsim 0.75$. The simulations also unveil that the pulsar and the stellar winds become fully mixed within the grid for low eccentricity systems, presenting a more stochastic behavior at large scales than in the highly eccentric systems., 18 pages, 11 figures
Published: 2021

13. Search for correlations between high-energy gamma rays and neutrinos with the HAWC and ANTARES detectors

Author: Alves Garre, Sergio, André, Michel, Anghinolfi, Marco, Anton, Gisela, Ardid Ramírez, Miguel, Aublin, J., Belhorma, Bouchra, Bendahman, Meriem, Bertin, Vincent, Bissinger, Matthias, Boumaaza, Jihad, Centre Tecnològic de Vilanova i la Geltrú, and Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques
Subjects: Astrofísica, Raigs gamma, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], Gamma ray astronomy, Neutrins, Astrophysics, Neutrino astrophysics
Abstract: ANTARES is an underwater neutrino detector in the Mediterranean Sea. Its location, reconstruction accuracy for all-flavor neutrino interactions, and low energy threshold, make it the most sensitive neutrino observatory for searches below 100 TeV over large parts of the sky. The HAWC experiment is a water Cherenkov gamma-ray detector located in Mexico. Thanks to its large field of view it is an excellent instrument to observe the very-high energy gamma-ray sky and perform high-sensitivity surveys of the Galactic Plane. The 10-year ANTARES data set and 3-year HAWC point source surveys are used to search for all-flavor neutrino emission in correlation with the highly-significant observations by HAWC in the gamma-ray sky by means of a maximumlikelihood template search. No significant observation for a correlation has been identified and upper limits on the neutrino flux from the HAWC observations have been set. Article signat per 276 autors/es: A. Albert, S. Alves, M. André, M. Anghinolfi, G. Anton, M. Ardid, S. Ardid, J.-J. Aubert, J. Aublin, B. Baret, S. Basa,B. Belhorma, B. Belhorma, M. Bendahman, V. Bertin, S. Biagi, M. Bissinger, J. Boumaaza, M. Bouta, M.C. Bouwhuis, H. Brânzas, R. Bruijn, J. Brunner, J. Busto, B. Caiffi, A. Capone, L. Caramete, J. Carr, V. Carretero, S. Celli, M. Chabab,T. N. Chau, R. Cherkaoui El Moursli, T. Chiarusi, M. Circella, A. Coleiro, M. Colomer-Molla, R. Coniglione, P. Coyle, A. Creusot, A. F. Díaz, G. de Wasseige, A. Deschamps, C. Distefano, I. Di Palma, A. Domi, C. Donzaud, D. Dornic, D. Drouhin, T. Eberl, T. van Eeden, D. van Eijk, N. El Khayati, A. Enzenhöfer, P. Fermani, G. Ferrara, F. Filippini, L.A. Fusco, Y. Gatelet, P. Gay, H. Glotin, R. Gozzini, R. Gracia Ruiz, K. Graf, C. Guidi, S. Hallmann, H. van Haren, A.J. Heijboer, Y. Hello, J.J. Hernández-Rey, J. Hößl, J. Hofestädt, F. Huang, G. Illuminati, C.W James, B. Jisse-Jung, M. de Jong, P. de Jong, M. Kadler, O. Kalekin, U. Katz, N.R. Khan Chowdhury, A. Kouchner, I. Kreykenbohm, V. Kulikovskiy, R. Lahmann, R. Le Breton, D. Lefèvre, E. Leonora, G. Levi, M. Lincetto, D. Lopez-Coto, S. Loucatos, L. Maderer, J. Manczak, M. Marcelin, A. Margiotta, A. Marinelli, J.A. Martínez-Mora, K. Melis, P. Migliozzi, A. Moussa, R. Muller, L.Nauta, S.Navas, E.Nezri, B. O’Fearraigh, A. Paun, G.E. Pavalas, C. Pellegrino, M. Perrin-Terrin,V. Pestel, P. Piattelli, C. Pieterse, C. Poirè,V. Popa, T. Pradier,N. Randazzo, S.Reck, G. Riccobene, A. Romanov, A. Sánchez-Losa, F. Salesa Greus, D. F. E. Samtleben, M. Sanguineti, P. Sapienza, J. Schnabel, J. Schumann, F. Schüssler, M. Spurio, Th. Stolarczyk, M. Taiuti, Y. Tayalati, S.J. Tingay, B. Vallage, V. Van Elewyck, F. Versari, S. Viola, D. Vivolo, J. Wilms, S. Zavatarelli5, A. Zegarelli, J.D. Zornoza, and J. Zúñiga. A.U. Abeysekara, A. Albert, R. Alfaro, C. Alvarez, J.D. Álvarez, J.R. Angeles Camacho, J.C. Arteaga-Velázquez, K. P. Arunbabu, D. Avila Rojas, H.A. Ayala Solares, R. Babu, V. Baghmanyan, A.S. Barber, J. Becerra Gonzalez, E. BelmontMoreno, S.Y. BenZvi, D. Berley, C. Brisbois, K.S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, O. Chaparro-Amaro, U. Cotti, J. Cotzomi, S. Coutiño de León, E. De la Fuente, C. de León, L. Diaz-Cruz, R. Diaz Hernandez, J.C. Díaz-Vélez, B.L. Dingus, M. Durocher, M.A. DuVernois, R.W. Ellsworth, K. Engel, C. Espinoza, K.L. Fan, K. Fang, M. Fernández Alonso, B. Fick, H. Fleischhack, J.L. Flores, N.I. Fraĳa, D. Garcia, J.A. García-González, J. L. García-Luna, G. García-Torales, F. Garfias, G. Giacinti, H. Goksu, M.M. González, J.A. Goodman, J.P. Harding, S. Hernandez, I. Herzog, J. Hinton, B. Hona, D. Huang, F. Hueyotl-Zahuantitla, C.M. Hui, B. Humensky, P. Hüntemeyer, A. Iriarte, A. Jardin-Blicq, H. Jhee, V. Joshi, D. Kieda, G J. Kunde, S. Kunwar, A. Lara, J. Lee, W.H. Lee, D. Lennarz, H. León Vargas, J. Linnemann, A.L. Longinotti, R. López-Coto, G. Luis-Raya, J. Lundeen, K. Malone, V. Marandon, O. Martinez, I. Martinez-Castellanos, H. Martínez-Huerta, J. Martínez-Castro, J.A.J. Matthews, J. McEnery, P. Miranda-Romagnoli, J.A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M.U. Nisa, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, A. Peisker, Y. Pérez Araujo, E.G. Pérez-Pérez, C.D. Rho, C. Rivière, D. Rosa-Gonzalez, E. Ruiz-Velasco, J. Ryan, H. Salazar, F. Salesa Greus, A. Sandoval, M. Schneider, H. Schoorlemmer, J. Serna-Franco, G. Sinnis, A.J. Smith, R.W. Springer, P. Surajbali, I. Taboada, M. Tanner, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, L. Villaseñor, X. Wang, I.J. Watson, T. Weisgarber, F. Werner, E. Willox, J. Wood, G.B. Yodh, A. Zepeda, H. Zhou
Published: 2021

14. A dynamical and radiation semi-Analytical model of pulsar-star colliding winds along the orbit: Application to LS 5039

Author: E. Molina, Valentí Bosch-Ramon, Ministerio de Economía y Competitividad (España), European Commission, and Generalitat de Catalunya
Subjects: Radiation mechanisms: non-thermal, Astrophysics::High Energy Astrophysical Phenomena, Stars: individual: LS 5039, FOS: Physical sciences, Context (language use), Outflows, Astrophysics, Radiation, 01 natural sciences, individual: LS 5039 [Stars], law.invention, Gamma rays: stars, Raigs gamma, Pulsar, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, winds [Stars], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Estels binaris de raigs X, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), non-thermal [Radiation mechanisms], 010308 nuclear & particles physics, Gamma rays, stars [Gamma rays], Astronomy and Astrophysics, Particle accelerator, Stars: winds, Particle acceleration, Orbit, X-ray binaries, Space and Planetary Science, Orbital motion, Astrophysics - High Energy Astrophysical Phenomena, Phenomenology (particle physics)
Abstract: [Context]: Gamma-ray binaries are systems that emit nonthermal radiation peaking at energies above 1 MeV. One proposed scenario to explain their emission consists of a pulsar orbiting a massive star, with particle acceleration taking place in shocks produced by the interaction of the stellar and pulsar winds. [Aims]: We develop a semi-Analytical model of the nonthermal emission of the colliding-wind structure, which includes the dynamical effects of orbital motion. We apply the model to a general case and to LS 5039. [Methods]: The model consists of a one-dimensional emitter, the geometry of which is affected by Coriolis forces owing to orbital motion. Two particle accelerators are considered: one at the two-wind standoff location and the other one at the turnover produced by the Coriolis force. Synchrotron and inverse Compton emission is studied taking into account Doppler boosting and absorption processes associated to the massive star. [Results]: If both accelerators are provided with the same energy budget, most of the radiation comes from the region of the Coriolis turnover and beyond, up to a few orbital separations from the binary system. Significant orbital changes of the nonthermal emission are predicted in all energy bands. The model allows us to reproduce some of the LS 5039 emission features, but not all of them. In particular, the MeV radiation is probably too high to be explained by our model alone, the GeV flux is recovered but not its modulation, and the radio emission beyond the Coriolis turnover is too low. The predicted system inclination is consistent with the presence of a pulsar in the binary. [Conclusions]: The model is quite successful in reproducing the overall nonthermal behavior of LS 5039. Some improvements are suggested to better explain the phenomenology observed in this source, such as accounting for particle reacceleration beyond the Coriolis turnover, unshocked pulsar wind emission, and the three-dimensional extension of the emitter., We acknowledge support by the Spanish Ministerio de Economía y Competitividad (MINECO/FEDER, UE) under grant AYA2016-76012-C3-1-P, with partial support by the European Regional Development Fund (ERDF/FEDER), and from the Catalan DEC grant 2017 SGR 643. EM acknowledges support from MINECO through grant BES-2016-076342.
Published: 2020

15. The high-energy emission from HD 93129A near periastron

Author: J. M. Paredes, M. De Becker, Valentí Bosch-Ramon, P. Munar Adrover, Kenji Hamaguchi, Michael F. Corcoran, Marco Tavani, Rodolfo H. Barbá, Asif ud-Doula, S. del Palacio, Diego Altamirano, J. Maíz Apellániz, Gustavo E. Romero, Hugues Sana, Federico García, Unidad de Excelencia Científica María de Maeztu Instituto de Ciencias del Cosmos (ICCUB), MDM-2014-0369, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, García, F. [0000-0001-9072-4069], Altamirano, D. [0000-0002-3422-0074], Barbá, R. [0000-0003-1086-1579], Corcoran, M. [0000-0002-7762-3172], Del Palacio, S. [0000-0002-5761-2417], Agencia Estatal de Investigación (AEI), Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET), Dutch Research Council (NWO), Unidad de Excelencia Científica María de Maeztu del Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2014-0369, and Astronomy
Subjects: High energy, Acceleration of particles, Ciencias Físicas, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Non-thermal mechanisms, Kinetic energy, 01 natural sciences, Relativistic particle, purl.org/becyt/ford/1 [https], Raigs gamma, Coincident, 0103 physical sciences, Radiative transfer, Radiation mechanisms, 010303 astronomy & astrophysics, Estels binaris de raigs X, stars [X-rays], High Energy Astrophysical Phenomena (astro-ph.HE), Physics, X rays, 010308 nuclear & particles physics, Acceleradors de partícules, Gamma rays, stars [Gamma rays], non thermal [Radiation mechanisms], Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], Galaxy, Particle accelerators, Magnetic field, Astronomía, X-ray binaries, Space and Planetary Science, Satellite, Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS
Abstract: We conducted an observational campaign towards one of the most massive and luminous colliding wind binaries in the Galaxy, HD~93129A, close to its periastron passage in 2018. During this time the source was predicted to be in its maximum of high-energy emission. Here we present our data analysis from the X-ray satellites \textit{Chandra} and \textit{NuSTAR} and the $\gamma$-ray satellite \textit{AGILE}. High-energy emission coincident with HD~93129A was detected in the X-ray band up to $\sim$18~keV, whereas in the $\gamma$-ray band only upper limits were obtained. We interpret the derived fluxes using a non-thermal radiative model for the wind-collision region. We establish a conservative upper limit for the fraction of the wind kinetic power that is converted into relativistic electron acceleration, $f_\mathrm{NT,e} < 0.02$. In addition, we set a lower limit for the magnetic field in the wind-collision region as $B_\mathrm{WCR} > 0.3$~G. We also argue a putative interpretation of the emission from which we estimate $f_\mathrm{NT,e} \approx 0.006$ and $B_\mathrm{WCR} \approx 0.5$~G. We conclude that multi-wavelength, dedicated observing campaigns during carefully selected epochs are a powerful tool for characterising the relativistic particle content and magnetic field intensity in colliding wind binaries., Comment: 11 pages, 10 figures, accepted for publication in MNRAS
Published: 2020

16. Determining the probability of locating peaks using computerized peak-location methods in gamma-ray spectra as a function of the relative peak-area uncertainty

Author: S Hurtado Bermudez, Leen Verheyen, M.A. Duch, Sandra Siri, T Boshkova, José Ubiratan Delgado, V H Elvira, Romul Margineanu, Branko Vodenik, Arunas Gudelis, A Pantelica, Aleksandar Kandić, Leticia S. Pibida, Jelena Krneta Nikolić, I. Mitsios, S.A. Long, A. Camacho, Sean Collins, M. C. Fornaciari Iljadica, Matjaž Korun, Bojan Šešlak, Dani Mulas, H. Wiedner, Aleksandar M. Jevremović, R Diaz Perez, K Karfopolous, D. Gurau, V Peyres Medina, Ivana Vukanac, Constantinos Potiriadis, M. C. Alí Santoro, Ronaldo Lins da Silva, Raquel Idoeta, Benjamin Zorko, M. J. Anagnostakis, Regio dos Santos Gomes, M Đurašavić, Matthias Laubenstein, Universitat Politècnica de Catalunya. Institut de Tècniques Energètiques, Universitat Politècnica de Catalunya. DRM - Dosimetria i Radiofísica Mèdica, Universidad de Sevilla. Departamento de Física Aplicada II, and Universidad de Sevilla. RNM138: Física Nuclear Aplicada
Subjects: Gamma ray spectra, 010403 inorganic & nuclear chemistry, Mass spectrometry, 01 natural sciences, 030218 nuclear medicine & medical imaging, 03 medical and health sciences, 0302 clinical medicine, Raigs gamma, Relative peak-area uncertainty, Gamma ray spectrometry, Peak area, Physics, Radiation, Física [Àrees temàtiques de la UPC], Gamma rays, Espectrometria de raigs gamma, Mode (statistics), Function (mathematics), Gamma-ray spectrometry, 0104 chemical sciences, Computational physics, Decision threshold, Peak location
Abstract: The probabilities of locating peaks with a high relative peak-area uncertainty were determined empirically with nine types of peak-location software used in laboratories engaged in gamma-ray spectrometry measurements. It was found that it is not possible to locate peaks with a probability of 0.95, when they have a relative peak-area uncertainty in excess of 50%. Locating peaks at these relatively high peak-area uncertainties with a probability greater than 0.95 is only possible in the library-driven mode, where the peak positions are supposed a-priori. The deficiencies of the library-driven mode and the possibilities to improve the probabilities of locating peaks are briefly discussed. © 2019 Elsevier Ltd
Published: 2020

17. ANTARES upper limits on the multi-TeV neutrino emission from the GRBs detected by IACTs

Author: ANTARES Collaboration, Albert, A., Andr��, M., Anghinolfi, M., Anton, G., Ardid, M., Aubert, J. -J., Aublin, J., Baret, B., Basa, S., Belhorma, B., Bertin, V., Biagi, S., Bissinger, M., Boumaaza, J., Bouta, M., Bouwhuis, M. C., Br��nza��, H., Bruijn, R., Brunner, J., Busto, J., Capone, A., Caramete, L., Carr, J., Carretero, V., Celli, S., Chabab, M., Chau, T. N., Moursli, R. Cherkaoui El, Chiarusi, T., Circella, M., Coleiro, A., Colomer-Molla, M., Coniglione, R., Coyle, P., Creusot, A., D��az, A. F., de Wasseige, G., Deschamps, A., Distefano, C., Di Palma, I., Domi, A., Donzaud, C., Dornic, D., Drouhin, D., Eberl, T., Khayati, N. El, Enzenh��fer, A., Ettahiri, A., Fermani, P., Ferrara, G., Filippini, F., Fusco, L., Garc��a, R., Gay, P., Glotin, H., Gozzini, R., Graf, K., Guidi, C., Hallmann, S., van Haren, H., Heijboer, A. J., Hello, Y., Hern��ndez-Rey, J. J., H��l, J., Hofest��dt, J., Huang, F., Illuminati, G., James, C. W., Jisse-Jung, B., de Jong, M., de Jong, P., Jongen, M., Kadler, M., Kalekin, O., Katz, U., Khan-Chowdhury, N. R., Kouchner, A., Kreykenbohm, I., Kulikovskiy, V., Lahmann, R., Breton, R. Le, Lef��vre, D., Leonora, E., Levi, G., Lincetto, M., Lopez-Coto, D., Loucatos, S., Maderer, L., Manczak, J., Marcelin, M., Margiotta, A., Marinelli, A., Mart��nez-Mora, J. A., Mazzou, S., Melis, K., Migliozzi, P., Moser, M., Moussa, A., Muller, R., Nauta, L., Navas, S., Nezri, E., Nu��ez-Casti��eyra, A., O'Fearraigh, B., Organokov, M., P��v��la��, G. E., Pellegrino, C., Perrin-Terrin, M., Piattelli, P., Pieterse, C., Poir��, C., Popa, V., Pradier, T., Randazzo, N., Reck, S., Riccobene, G., S��nchez-Losa, A., Samtleben, D. F. E., Sanguineti, M., Sapienza, P., Schnabel, J., Sch��ssler, F., Spurio, M., Stolarczyk, Th., Taiuti, M., Tayalati, Y., Thakore, T., Tingay, S. J., Vallage, B., Van Elewyck, V., Versari, F., Viola, S., Vivolo, D., Wilms, J., Zegarelli, A., Zornoza, J. D., Z��iga, J., Institut Pluridisciplinaire Hubert Curien (IPHC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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), Géoazur (GEOAZUR 7329), 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)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Université Paris-Sud - Paris 11 (UP11), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Laboratoire d'Informatique et Systèmes (LIS), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Institut méditerranéen d'océanologie (MIO), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Toulon (UTLN)-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, ANTARES, KM3NeT (IHEF, IoP, FNWI), ATLAS (IHEF, IoP, FNWI), IHEF (IoP, FNWI), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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), Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, Albert A., Andre M., Anghinolfi M., Anton G., Ardid M., Aubert J.-J., Aublin J., Baret B., Basa S., Belhorma B., Bertin V., Biagi S., Bissinger M., Boumaaza J., Bouta M., Bouwhuis M.C., Br nzas H., Bruijn R., Brunner J., Busto J., Capone A., Caramete L., Carr J., Carretero V., Celli S., Chabab M., Chau T.N., Cherkaoui El Moursli R., Chiarusi T., Circella M., Coleiro A., Colomer-Molla M., Coniglione R., Coyle P., Creusot A., Diaz A.F., De Wasseige G., Deschamps A., Distefano C., Di Palma I., Domi A., Donzaud C., Dornic D., Drouhin D., Eberl T., El Khayati N., Enzenhofer A., Ettahiri A., Fermani P., Ferrara G., Filippini F., Fusco L., Garcia R., Gay P., Glotin H., Gozzini R., Graf K., Guidi C., Hallmann S., Van Haren H., Heijboer A.J., Hello Y., Hernandez-Rey J.J., Hossl J., Hofest dt J., Huang F., Illuminati G., James C.W., Jisse-Jung B., De Jong M., De Jong P., Jongen M., Kadler M., Kalekin O., Katz U., Khan-Chowdhury N.R., Kouchner A., Kreykenbohm I., Kulikovskiy V., Lahmann R., Le Breton R., Lef vre D., Leonora E., Levi G., Lincetto M., Lopez-Coto D., Loucatos S., Maderer L., Manczak J., Marcelin M., Margiotta A., Marinelli A., Martinez-Mora J.A., Mazzou S., Melis K., Migliozzi P., Moser M., Moussa A., Muller R., Nauta L., Navas S., Nezri E., Nuez-Castieyra A., O'Fearraigh B., Organokov M., Pavalas G.E., Pellegrino C., Perrin-Terrin M., Piattelli P., Pieterse C., Poir C., Popa V., Pradier T., Randazzo N., Reck S., Riccobene G., Sanchez-Losa A., Samtleben D.F.E., Sanguineti M., Sapienza P., Schnabel J., Schussler F., Spurio M., Stolarczyk T., Taiuti M., Tayalati Y., Thakore T., Tingay S.J., Vallage B., Van Elewyck V., Versari F., Viola S., Vivolo D., Wilms J., Zegarelli A., Zornoza J.D., and Zuiga J.
Subjects: Astrofísica, electron, dimension: 3, Astrophysics, 01 natural sciences, neutrino: flux, IceCube, Raigs gamma, HESS, optical, MAGIC (telescope), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), photomultiplier, ultra high energy photons and neutrinos, Astrophysics::Instrumentation and Methods for Astrophysics, imaging, gamma ray: emission, neutrino: detector, Neutrino detector, Neutrino astronomy, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Photomultiplier, particle acceleration, Astrophysics::High Energy Astrophysical Phenomena, Particle acceleration, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, gamma ray: burst, GLAST, neutrino astronomy, X-ray, gamma ray bursts theory, 0103 physical sciences, Ultra high energy photons and neutrinos, Cherenkov radiation, ANTARES, Gamma ray bursts theory, Telescopis, 010308 nuclear & particles physics, Gamma rays, Astronomy and Astrophysics, MAGIC, Afterglow, Cherenkov counter, electromagnetic, gamma ray: VHE, 13. Climate action, FISICA APLICADA, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], correlation, ultra high energy photons and neutrino, Gamma-ray burst, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Telescopes
Abstract: [EN] The first gamma-ray burst detections by Imaging Atmospheric Cherenkov Telescopes have been recently announced: GRB 190114C, detected by MAGIC, GRB 180720B and GRB 190829A, observed by H.E.S.S. A dedicated search for neutrinos in space and time coincidence with the gamma-ray emission observed by IACTs has been performed using ANTARES data. The search covers both the prompt and afterglow phases, yielding no neutrinos in coincidence with the three GRBs studied. Upper limits on the energetics of the neutrino emission are inferred. The resulting upper limits are several orders of magnitude above the observed gamma-ray emission, and they do not allow to constrain the available models., The authors acknowledge the financial support of the funding agencies: Centre National de la Recherche Scientifique (CNRS), Commissariat a l'energie atomique et aux energies alternatives (CEA), Commission Europeenne (FEDER fund and Marie Curie Program), Institut Universitaire de France (IUF), LabEx UnivEarthS (ANR-10-LABX-0023 and ANR18-IDEX-0001), Region Ile-de-France (DIM-ACAV), Region Alsace (contrat CPER), Region Provence-Alpes-Cote d'Azur, Departement du Var and Ville de La Seyne-sur-Mer, France; Bundesministerium fur Bildung und Forschung (BMBF), Germany; Istituto Nazionale di Fisica Nucleare (INFN), Italy; Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO), the Netherlands; Council of the President of the Russian Federation for young scientists and leading scientific schools supporting grants, Russia; Executive Unit for Financing Higher Education, Research, Development and Innovation (UEFISCDI), Romania; Ministerio de Ciencia e Innovacion (MCI) and Agencia Estatal de Investigacion: Programa Estatal de Generacion de Conocimiento (refs. PGC2018-096663-B-C41, -A-C42, -B-C43, -BC44) (MCI/FEDER), Severo Ochoa Centre of Excellence and MultiDark Consolider, Junta de Andalucia (ref. SOMM17/6104/UGR and A-FQM-053-UGR18), Generalitat Valenciana: Grisolia (ref. GRISOLIA/2018/119), Spain; Ministry of Higher Education, Scientific Research and Professional Training, Morocco. We also acknowledge the technical support of Ifremer, AIM and Foselev Marine for the sea operation and the CC-IN2P3 for the computing facilities.
Published: 2020
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18. Gamma-ray emission from the microquasar Cygnus X-3

Author: Carrasco Brossa, Marta and Paredes i Poy, Josep Maria
Subjects: Microquasar, Bachelor's thesis, Raigs gamma, Microquàsars, Gamma rays, Bachelor's theses, Treballs de fi de grau
Abstract: Treballs Finals de Grau de Física, Facultat de Física, Universitat de Barcelona, Curs: 2020, Tutor: Josep Maria Paredes, Cygnus X-3 is a microquasar studied over the wide range of electromagnetic spectrum. It is believed to be a powerful source of cosmic rays particles in our galaxy. Gamma-ray emission has also been detected from it in several occasions. Studying gamma-ray emission from Cygnus X-3 will help to understand the process where charged particles are accelerated and gamma-rays formed. We have analyzed data from the NASA's Fermi satellite in two periods of time by performing lightcurves with the aperture photometry analysis. In the rst period, from 2008 to 2009, we compare our results with the ones already reported by Fermi LAT collaboration in 2009. In the second period, we analyse recent data from September 2018 to November 2019 following the same criteria and trying to find a period of high activity in gamma-ray emission. Our results corroborate the period of high activity in gamma-rays from June to August 2009 and they show hints of an active period from March to July 2019 where there is a large probability that the high energy gamma-ray emission detected is coming from the source
Published: 2020

19. H.E.S.S. detection of very high-energy γ-ray emission from the quasar PKS 0736+017

Author: Collaboration, H. E. S. S., Abdalla, H., Adam, R., Aharonian, F., Benkhali, F. Ait, Angüner, E. O., Arakawa, M., Arcaro, C., Armand, C., Ashkar, H., Backes, M., Martins, V. Barbosa, Barnard, M., Becherini, Y., Berge, D., Bernlöhr, K., Blackwell, R., Böttcher, M., Boisson, C., Bolmont, J., Bonnefoy, S., Bregeon, J., Breuhaus, M., Brun, F., Brun, P., Bryan, M., Büchele, M., Bulik, T., Bylund, T., Capasso, M., Caroff, S., Carosi, A., Casanova, S., Cerruti, M., Chand, T., Chandra, S., Chen, A., Colafrancesco, S., Curylo, M., Davids, I. D., Deil, C., Devin, J., deWilt, P., Dirson, L., Djannati-Ataï, A., Dmytriiev, A., Donath, A., Doroshenko, V., Drury, L. O'C., Dyks, J., Egberts, K., Emery, G., Ernenwein, J. -P., Eschbach, S., Feijen, K., Fegan, S., Fiasson, A., Fontaine, G., Funk, S., Füßling, M., Gabici, S., Gallant, Y. A., Gaté, F., Giavitto, G., Glawion, D., Glicenstein, J. F., Gottschall, D., Grondin, M. -H., Hahn, J., Haupt, M., Heinzelmann, G., Henri, G., Hermann, G., Hinton, J. A., Hofmann, W., Hoischen, C., Holch, T. L., Holler, M., Horns, D., Huber, D., Iwasaki, H., Jamrozy, M., Jankowsky, D., Jankowsky, F., Jardin-Blicq, A., Jung-Richardt, I., Kastendieck, M. A., Katarzynski, K., Katsuragawa, M., Katz, U., Khangulyan, D., Khélifi, B., King, J., Klepser, S., Kluzniak, W., Komin, Nu., Kosack, K., Kostunin, D., Kraus, M., Lamanna, G., Lau, J., Lemière, A., Lemoine-Goumard, M., Lenain, J. -P., Leser, E., Levy, C., Lohse, T., Lypova, I., Mackey, J., Majumdar, J., Malyshev, D., Marandon, V., Marcowith, A., Mares, A., Mariaud, C., Martí-Devesa, G., Marx, R., Maurin, G., Meintjes, P. J., Mitchell, A. M. W., Moderski, R., Mohamed, M., Mohrmann, L., Muller, J., Moore, C., Moulin, E., Murach, T., Nakashima, S., de Naurois, M., Ndiyavala, H., Niederwanger, F., Niemiec, J., Oakes, L., O'Brien, P., Odaka, H., Ohm, S., Wilhelmi, E. de Oña, Ostrowski, M., Oya, I., Panter, M., Parsons, R. D., Perennes, C., Petrucci, P. -O., Peyaud, B., Piel, Q., Pita, S., Poireau, V., Noel, A. Priyana, Prokhorov, D. A., Prokoph, H., Pühlhofer, G., Punch, M., Quirrenbach, A., Raab, S., Rauth, R., Reimer, A., Reimer, O., Remy, Q., Renaud, M., Rieger, F., Rinchiuso, L., Romoli, C., Rowell, G., Rudak, B., Ruiz-Velasco, E., Sahakian, V., Saito, S., Sanchez, D. A., Santangelo, A., Sasaki, M., Schlickeiser, R., Schüssler, F., Schulz, A., Schutte, H., Schwanke, U., Schwemmer, S., Seglar-Arroyo, M., Senniappan, M., Seyffert, A. S., Shafi, N., Shiningayamwe, K., Simoni, R., Sinha, A., Sol, H., Specovius, A., Spir-Jacob, M., Stawarz, L., Steenkamp, R., Stegmann, C., Steppa, C., Takahashi, T., Tavernier, T., Taylor, A. M., Terrier, R., Tiziani, D., Tluczykont, M., Trichard, C., Tsirou, M., Tsuji, N., Tuffs, R., Uchiyama, Y., van der Walt, D. J., van Eldik, C., van Rensburg, C., van Soelen, B., Vasileiadis, G., Veh, J., Venter, C., Vincent, P., Vink, J., Voisin, F., Völk, H. J., Vuillaume, T., Wadiasingh, Z., Wagner, S. J., White, R., Wierzcholska, A., Yang, R., Yoneda, H., Zacharias, M., Zanin, R., Zdziarski, A. A., Zech, A., Ziegler, A., Zorn, J., Zywucka, N., Smith, P. S., 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 d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Deutsches Elektronen-Synchrotron [Zeuthen] (DESY), Helmholtz-Gemeinschaft = Helmholtz Association, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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), 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), 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, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Institute for the Physics and Mathematics of the Universe (IPMU), The University of Tokyo (UTokyo), Max-Planck-Institut für Kernphysik (MPIK), Max-Planck-Gesellschaft, H.E.S.S. Collaboration, 26598973 - Abdalla, Hassan, 30588766 - Arcaro, Cornelia, 28644743 - Backes, Michael, 20574266 - Barnard, Monica, 24420530 - Böttcher, Markus, 30366755 - Chand, Tej B., 31125417 - Chandra, Sunil, 26403366 - Ndiyavala, Hambeleleni, 22799133 - Schutte, Hester M., 20126999 - Seyffert, Albertus Stefanus, 10060499 - Van der Walt, Diederick Johannes, 12006653 - Venter, Christo, 26594080 - Wadiasingh, Zorawar, 29092086 - Zacharias, Michael, 34208968 - Zywucka-Hejzner, Natalia, 21106266 - Van Rensburg, Carlo, H. E. S. S. Collaboration, University of Namibia, Federal Ministry of Education and Research (Germany), Max Planck Society, German Research Foundation, Helmholtz Association, Alexander von Humboldt Foundation, Ministre de l'Enseignement Supérieur, de la Recherche et de l'Innovation (France), Centre National de la Recherche Scientifique (France), Commissariat à l'Ènergie Atomique et aux Ènergies Alternatives (France), Science and Technology Facilities Council (UK), Knut and Alice Wallenberg Foundation, National Science Centre (Poland), Department of Science and Technology (South Africa), National Research Foundation (South Africa), National Commission on Research Science and Technology (Namibia), Federal Ministry of Education, Science and Research (Austria), Austrian Science Fund, Australian Research Council, Japan Society for the Promotion of Science, University of Amsterdam, La Caixa, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Helmholtz-Gemeinschaft, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), The University of Tokyo, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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 Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Faculty of Science, High Energy Astrophys. & Astropart. Phys (API, FNWI), Gravitation and Astroparticle Physics Amsterdam, PSL Research University (PSL)-PSL Research University (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)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), and 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)
Subjects: quasars: individual: PKS 0736+017, VHE [gamma ray], torus, Astrophysics, 01 natural sciences, law.invention, Raigs gamma, Observatory, law, HESS, optical, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, relativistic processes, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), photon, collimator, Relativistic processes, Gamma ray, Particle physics, observatory, Lorentz factor, astroparticle physics, symbols, Astrophysics - High Energy Astrophysical Phenomena, Lorentz, Flare, Astrophysics::High Energy Astrophysical Phenomena, general [Gamma rays], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, GLAST, Telescope, symbols.namesake, emission [gamma ray], 0103 physical sciences, quasar, Quasars, Cherenkov radiation, Quàsars, 010308 nuclear & particles physics, Gamma rays, opacity, Astronomy and Astrophysics, Quasar, gamma rays: general, doubling, individual: PKS 0736+017 [Quasars], flux, monitoring, Cherenkov counter, 13. Climate action, Space and Planetary Science, ddc:520, HESS - Abteilung Hinton, Astroparticle physics, Física de partícules, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope
Abstract: [Context] Flat-spectrum radio-quasars (FSRQs) are rarely detected at very high energies (E 100 GeV) due to their low-frequency-peaked spectral energy distributions. At present, only six FSRQs are known to emit very high-energy (VHE) photons, representing only 7% of the VHE extragalactic catalog, which is largely dominated by high-frequency-peaked BL Lacertae objects., [Aims] Following the detection of MeV–GeV γ-ray flaring activity from the FSRQ PKS 0736+017 (z = 0.189) with Fermi-LAT, the H.E.S.S. array of Cherenkov telescopes triggered target-of-opportunity (ToO) observations on February 18, 2015, with the goal of studying the γ-ray emission in the VHE band., [Methods] H.E.S.S. ToO observations were carried out during the nights of February 18, 19, 21, and 24, 2015. Together with Fermi-LAT, the multi-wavelength coverage of the flare includes Swift observations in soft X-ray and optical-UV bands, and optical monitoring (photometry and spectro-polarimetry) by the Steward Observatory, and the ATOM, the KAIT, and the ASAS-SN telescopes., [Results] VHE emission from PKS 0736+017 was detected with H.E.S.S. only during the night of February 19, 2015. Fermi-LAT data indicate the presence of a γ-ray flare, peaking at the time of the H.E.S.S. detection, with a flux doubling timescale of around six hours. The γ-ray flare was accompanied by at least a 1 mag brightening of the non-thermal optical continuum. No simultaneous observations at longer wavelengths are available for the night of the H.E.S.S. detection. The γ-ray observations with H.E.S.S. and Fermi-LAT are used to put constraints on the location of the γ-ray emitting region during the flare: it is constrained to be just outside the radius of the broad-line region rBLR with a bulk Lorentz factor Γ ≃ 20, or at the level of the radius of the dusty torus rtorus with Γ ≃ 60., [Conclusions] PKS 0736+017 is the seventh FSRQ known to emit VHE photons, and at z = 0.189 is the nearest so far. The location of the γ-ray emitting region during the flare can be tightly constrained thanks to opacity, variability, and collimation arguments., The support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the German Research Foundation (DFG), the Helmholtz Association, the Alexander von Humboldt Foundation, the French Ministry of Higher Education, Research and Innovation, the Centre National de la Recherche Scientifique (CNRS/IN2P3 and CNRS/INSU), the Commissariat à l’énergie atomique et aux énergies alternatives (CEA), the UK Science and Technology Facilities Council (STFC), the Knut and Alice Wallenberg Foundation, the National Science Centre, Poland grant no. 2016/22/M/ST9/00382, the South African Department of Science and Technology and National Research Foundation, the University of Namibia, the National Commission on Research, Science and Technology of Namibia (NCRST), the Austrian Federal Ministry of Education, Science and Research and the Austrian Science Fund (FWF), the Australian Research Council (ARC), the Japan Society for the Promotion of Science and by the University of Amsterdam. We appreciate the excellent work of the technical support staff in Berlin, Zeuthen, Heidelberg, Palaiseau, Paris, Saclay, Tübingen and in Namibia in the construction and operation of the equipment. This work benefited from services provided by the H.E.S.S. Virtual Organisation, supported by the national resource providers of the EGI Federation. The CC-IN2P3 (cc.in2p3.fr) is gratefully acknowledged for providing a significant amount of the computing resources and services needed for this work. Part of this work is based on archival data, software or online services provided by the Space Science Data Center – ASI. Blazar observations at Steward Observatory are funded though NASA/Fermi Guest Investigator Program grant NNX15AU81G. Matteo Cerruti has received financial support through the Postdoctoral Junior Leader Fellowship Programme from la Caixa Banking Foundation (LCF/BQ/PI18/11630012). The authors would like to thank the anonymous referee, whose constructive comments significantly improved the manuscript.
Published: 2020

20. Constraining the contribution of Gamma-Ray Bursts to the high-energy diffuse neutrino flux with 10 years of ANTARES data

Author: J.D. Zornoza, U. Katz, F. Filippini, H. Brânzaş, Steven Tingay, Giuseppe Levi, Michel André, B. Strandberg, M. Perrin-Terrin, M. Anghinolfi, Michael Moser, J. Hößl, R. Cherkaoui El Moursli, Hervé Glotin, V. Van Elewyck, Dominique Lefèvre, Julien Aublin, G. Illuminati, P. de Jong, C. W. James, N.R. Khan-Chowdhury, Jutta Schnabel, M. Taiuti, Th. Stolarczyk, Silvia Celli, Alba Domi, Alessia Capone, A. Creusot, Emanuele Leonora, S. Sánchez Navas, N. Randazzo, J. Carr, S. Reck, C. Donzaud, Abdelilah Moussa, A. Trovato, D. Lopez-Coto, V. Popa, Thierry Pradier, B. Belhorma, G.E. Păvălaş, Mohamed Chabab, Steffen Hallmann, S. Viola, S.F. Biagi, B. O'Fearraigh, Massimiliano Lincetto, Thomas Eberl, M. Bissinger, A. Marinelli, T. N. Chau, R. Gozzini, F. Schüssler, Matthias Kadler, A. Sánchez-Losa, Robert Lahmann, M. Organokov, P. Coyle, R. Le Breton, R. Muller, O. Kalekin, Jörn Wilms, Kay Graf, Karel Melis, Daniele Vivolo, M.C. Bouwhuis, M. Jongen, Anne Deschamps, L. Nauta, Antoine Kouchner, C. Guidi, C. Distefano, D. F. E. Samtleben, B. Baret, Vladimir Kulikovskiy, C. Pellegrino, Damien Dornic, A. Zegarelli, M. de Jong, Matteo Sanguineti, A. Nuñez-Castiñeyra, Giovanna Ferrara, M. Circella, J. Manczak, J. Brunner, M. Colomer-Molla, E. Nezri, G. Maggi, G. Riccobene, B. Vallage, V. Bertin, P. Migliozzi, R. Bruijn, S. Loucatos, G. de Wasseige, I. Di Palma, Antonio F. Díaz, Maurizio Spurio, F. Huang, Arnauld Albert, A.J. Heijboer, Paolo Fermani, J. Zúñiga, Tommaso Chiarusi, N. E. l. Khayati, C. Poirè, P. Piattelli, J.A. Martínez-Mora, Alexis Coleiro, M. Marcelin, R. Coniglione, J. Hofestädt, L. Caramete, Jihad Boumaaza, Paolo Sapienza, M. Ardid, F. Versari, A. Enzenhöfer, Yann Hello, S. Mazzou, D. Drouhin, Gisela Anton, J.J. Hernández-Rey, Yahya Tayalati, S. Basa, L. Fusco, H. van Haren, M. Bouta, A. Ettahiri, Annarita Margiotta, Jose Busto, T. Thakore, I. Kreykenbohm, J-J. Aubert, Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), Géoazur (GEOAZUR 7329), 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)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Université Paris-Sud - Paris 11 (UP11), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Informatique et Systèmes (LIS), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Institut méditerranéen d'océanologie (MIO), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Toulon (UTLN)-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, ANTARES, ANR-18-IDEX-0001,Université de Paris,Université de Paris(2018), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-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 de Paris (UP), 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), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne (UCA)-Centre National de la Recherche Scientifique (CNRS), KM3NeT (IHEF, IoP, FNWI), IoP (FNWI), ATLAS (IHEF, IoP, FNWI), IHEF (IoP, FNWI), Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, Albert A., Andre M., Anghinolfi M., Anton G., Ardid M., Aubert J.-J., Aublin J., Baret B., Basa S., Belhorma B., Bertin V., Biagi S., Bissinger M., Boumaaza J., Bouta M., Bouwhuis M.C., Branzas H., Bruijn R., Brunner J., Busto J., Capone A., Caramete L., Carr J., Celli S., Chabab M., Chau T.N., Cherkaoui El Moursli R., Chiarusi T., Circella M., Coleiro A., Colomer-Molla M., Coniglione R., Coyle P., Creusot A., Diaz A.F., De Wasseige G., Deschamps A., Distefano C., Palma I.D., Domi A., Donzaud C., Dornic D., Drouhin D., Eberl T., Khayati N.E.L., Enzenhofer A., Ettahiri A., Fermani P., Ferrara G., Filippini F., Fusco L.A., Gay P., Glotin H., Gozzini R., Graf K., Guidi C., Hallmann S., Van Haren H., Heijboer A.J., Hello Y., Hernandez-Rey J.J., Hossl J., Hofestadt J., Huang F., Illuminati G., James C.W., De Jong M., De Jong P., Jongen M., Kadler M., Kalekin O., Katz U., Khan-Chowdhury N.R., Kouchner A., Kreykenbohm I., Kulikovskiy V., Lahmann R., Le Breton R., Lefevre D., Leonora E., Levi G., Lincetto M., Lopez-Coto D., Loucatos S., Maggi G., Manczak J., Marcelin M., Margiotta A., Marinelli A., Martinez-Mora J.A., Mazzou S., Melis K., Migliozzi P., Moser M., Moussa A., Muller R., Nauta L., Navas S., Nezri E., Nunez-Castineyra A., O'Fearraigh B., Organokov M., Pavalas G.E., Pellegrino C., Perrin-Terrin M., Piattelli P., Poire C., Popa V., Pradier T., Randazzo N., Reck S., Riccobene G., Sanchez-Losa A., Samtleben D.F.E., Sanguineti M., Sapienza P., Schnabel J., Schussler F., Spurio M., Stolarczyk T., Strandberg B., Taiuti M., Tayalati Y., Thakore T., Tingay S.J., Trovato A., Vallage B., Van Elewyck V., Versari F., Viola S., Vivolo D., Wilms J., Zegarelli A., Zornoza J.D., and Zuniga J.
Subjects: Astrofísica, Acceleration of particles, Flux, Astrophysics, 7. Clean energy, 01 natural sciences, neutrino: flux, IceCube, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), neutrino, Gamma rays bursts, Hadronic interactions, Raigs gamma, hal-03171355, transients: gamma-ray bursts, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], acceleration of particles, astroparticle physics, neutrinos, 010303 astronomy & astrophysics, acceleration of particle, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, astro-ph.HE, astro-ph.IM, Energy, astroparticle physic, shock waves, Cosmology, Lorentz factor, Physique [physics]/Astrophysique [astro-ph], Neutrino detector, Neutrino astronomy, quality, stacking, gamma-ray bursts [Transients], symbols, Gamma-ray bursts, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Central engines, Lorentz, Internal shocks, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Neutrino fluxes, gamma ray: burst, Physique [physics]/Physique [physics], Transients, symbols.namesake, muon, 0103 physical sciences, Neutrins, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Neutrinos, Instrumentation and Methods for Astrophysics (astro-ph.IM), Cosmic rays, Neutrons, Astroparticle physics, neutrino muon, Muon, ANTARES, 010308 nuclear & particles physics, Gamma rays, Diffuse flux, Astronomy and Astrophysics, Astrophysical sources, redshift, Stars, Physique [physics]/Physique des Hautes Energies - Expérience [hep-ex], Redshift, Space and Planetary Science, FISICA APLICADA, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], High Energy Physics::Experiment, Gamma-ray burst, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: [EN] Addressing the origin of the astrophysical neutrino flux observed by IceCube is of paramount importance. Gamma-Ray Bursts (GRBs) are among the few astrophysical sources capable of achieving the required energy to contribute to such neutrino flux through p¿ interactions. In this work, ANTARES data have been used to search for upward going muon neutrinos in spatial and temporal coincidence with 784 GRBs occurred from 2007 to 2017. For each GRB, the expected neutrino flux has been calculated in the framework of the internal shock model and the impact of the lack of knowledge on the majority of source redshifts and on other intrinsic parameters of the emission mechanism has been quantified. It is found that the model parameters that set the radial distance where shock collisions occur have the largest impact on neutrino flux expectations. In particular, the bulk Lorentz factor of the source ejecta and the minimum variability time-scale are found to contribute significantly to the GRB-neutrino flux uncertainty. For the selected sources, ANTARES data have been analysed by maximizing the discovery probability of the stacking sample through an extended maximum-likelihood strategy. Since no neutrino event passed the quality cuts set by the optimization procedure, 90 per cent confidence level upper limits (with their uncertainty) on the total expected diffuse neutrino flux have been derived, according to the model. The GRB contribution to the observed diffuse astrophysical neutrino flux around 100 TeV is constrained to be less than 10 per cent., The authors acknowledge the financial support of the funding agencies: Centre National de la Recherche Scientifique (CNRS), Commissariata l'energie atomique et auxenergies alternatives (CEA), Commission Europeenne (FEDER fund and Marie Curie Program), Institut Universitaire de France (IUF), LabEx UnivEarthS (ANR-10-LABX-0023 and ANR-18-IDEX-0001), Region Ile-de-France (DIM-ACAV), Region Alsace (contrat CPER), Region Provence-Alpes-Cote d'Azur, Departement du Var and Ville de La Seyne-sur-Mer, France; Bundesministerium fur Bildung und Forschung (BMBF), Germany; Istituto Nazionale di Fisica Nucleare (INFN), Italy; Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO), the Netherlands; Council of the President of the Russian Federation for young scientists and leading scientific schools supporting grants, Russia; Executive Unit for Financing Higher Education, Research, Development and Innovation (UEFISCDI), Romania; Ministerio de Ciencia, Innovacion, Investigacion y Universidades (MCIU): Programa Estatal de Generacion de Conocimiento (refs. PGC2018-096663-B-C41, -A-C42, -B-C43, -B-C44) (MCIU/FEDER), Severo Ochoa Centre of Excellence and MultiDark Consolider (MCIU), Junta de Andalucia (ref. SOMM17/6104/UGR and A-FQM-053-UGR18), Generalitat Valenciana: Grisolia (ref. GRISOLIA/2018/119), Spain; Ministry of Higher Education, Scientific Research and Professional Training, Morocco. We also acknowledge the technical support of Ifremer, AIM and Foselev Marine for the sea operation and the CC-IN2P3 for the computing facilities.
Published: 2020

21. A blazar as the likely counterpart to 4FGL J0647.7−4418 instead of a gamma-ray binary

Author: Josep Martí, E. Sánchez-Ayaso, Pedro L. Luque-Escamilla, Valentí Bosch-Ramon, Josep M. Paredes, Robin H. D. Corbet, Ministerio de Economía y Competitividad (España), Junta de Andalucía, Generalitat de Catalunya, National Aeronautics and Space Administration (US), Agencia Estatal de Investigación (España), and European Commission
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Gamma rays, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, language.human_language, X-ray binaries, Raigs gamma, Space and Planetary Science, 0103 physical sciences, language, Catalan, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Humanities, Estels binaris de raigs X
Abstract: The persistent gamma-ray source 4FGL J0647.7−4418 is tentatively associated in the latest Fermi catalogue with the subdwarf O-type X-ray binary HD 49798. However, an active galactic nucleus (AGN) candidate is also mentioned as an alternative identification in updated versions of the catalogue accompanying paper. If the first association were correct, this would add HD 49798 to the handful of currently known gamma-ray binaries, and therefore represent a significant breakthrough not only because of a new member addition, but also because of the apparent white dwarf companion in this system. Despite these perspectives, here, we show that the stellar association is likely wrong and that the proposed AGN object, well inside the Fermi 95 per cent confidence ellipse, is a more conceivable counterpart candidate to the Fermi source due to its strong blazar similarities., This work was supported by the Agencia Estatal de Investigación grants AYA2016-76012-C3-1-P and AYA2016-76012-C3-3-P from the Spanish Ministerio de Economía y Competitividad (MINECO), by Consejería de Economía, Innovación, Ciencia y Empleo, Junta de Andalucía under research group FQM-322, by grant MDM-2014-0369 of the Institute of Cosmos Sciences (ICCUB, Unidad de Excelencia ‘María de Maeztu’), and by the Catalan DEC grant 2017 SGR 643, as well as Fondo Europeo de Desarrollo Regional (FEDER) funds. RC acknowledges support from National Aeronautics and Space Administration (NASA) Fermi grant NNX15AU83G.
Published: 2020

22. Resolving the Crab pulsar wind nebula at teraelectronvolt energies

Author: Natalia Żywucka, M. de Naurois, T. Chand, Frank M. Rieger, J. Bolmont, S. Colafrancesco, Ruizhi Yang, W. Kluźniak, S. Eschbach, Jim Hinton, R. Simoni, Dmitry Khangulyan, Christopher J. Moore, G. Fontaine, M. Büchele, D. A. Sanchez, T. Tavernier, L. Mohrmann, Denys Malyshev, J. Veh, S. Klepser, B. Khélifi, H. M. Schutte, C. Perennes, D. Glawion, Christoph Deil, Mohanraj Senniappan, A.A. Zdziarski, A. Djannati-Ataï, Y.A. Gallant, Gavin Rowell, Stefan Funk, T. Takahashi, Gianluca Giavitto, Axel Donath, A. W. Chen, M. Bryan, J. Dyks, D. Zaborov, I. Oya, G. Heinzelmann, K. Shiningayamwe, T. Lohse, Yvonne Becherini, M. Renaud, H. Iwasaki, M. Holler, J.-P. Ernenwein, P. Vincent, R. D. Parsons, G. Emery, H. Odaka, Christo Venter, D. Huber, M. Arakawa, D. Berge, M. Capasso, Matteo Cerruti, Nachiketa Chakraborty, F. Niederwanger, A. Marcowith, A. Zech, E. Leser, Jacco Vink, R. Rauth, Sabrina Casanova, C. Arcaro, I. Jung-Richardt, T. Vuillaume, G. Hermann, D. Gottschall, Werner Hofmann, Regis Terrier, J. Becker Tjus, A. Schulz, Carlo Romoli, M. Panter, M. Seglar-Arroyo, H. Ndiyavala, B. van Soelen, Felix Aharonian, M. Haupt, Lukasz Stawarz, Michael Punch, V. Doroshenko, M. Spir-Jacob, R. Tuffs, R. C. G. Chaves, E. O. Angüner, A. Priyana Noel, L. O'c. Drury, S. Saito, J.F. Glicenstein, D. J. van der Walt, S. Raab, Andreas Quirrenbach, C. Steppa, J.-P. Lenain, N. Shafi, K. Egberts, Robert Wagner, K. Kosack, J. Hahn, Reinhard Schlickeiser, M. Tsirou, G. Vasileiadis, M. Kraus, S. Chandra, S. Nakashima, G. Martí-Devesa, M. Katsuragawa, Ruben Lopez-Coto, M.-H. Grondin, M. Böttcher, R. Blackwell, E. Ruiz-Velasco, L. Dirson, Stefan Ohm, Léa Jouvin, S. Pita, F. Schüssler, P. deWilt, J. King, F. Voisin, Julien Lefaucheur, A. Dmytriiev, R. Moderski, S. Gabici, A. Fiasson, J. Lau, L. Oakes, I.D. Davids, Alison Mitchell, L. Rinchiuso, P.J. Meintjes, Heike Prokoph, Zorawar Wadiasingh, R. J. White, S. Fegan, Dieter Horns, V. Poireau, Monica Barnard, P.-O. Petrucci, H. Abdalla, D. Jankowsky, Q. Piel, C. Stegmann, Nu. Komin, Marek Jamrozy, Catherine Boisson, Helene Sol, Pierre Brun, A.S. Seyffert, A. Carosi, M. Füßling, M.A. Kastendieck, S. Bonnefoy, N. Tsuji, F. Gaté, J. Devin, G. Henri, D. A. Prokhorov, D. Tiziani, C. Hoischen, Ullrich Schwanke, A. Specovius, R. Steenkamp, A. Reimer, J. Bregeon, Francois Brun, B. Condon, Michael Backes, H. Yoneda, Tim Holch, M. Tluczykont, E. Moulin, Tomasz Bulik, T. Bylund, A. Jacholkowska, S. Caroff, Celine Armand, F. Jankowsky, Stefan Wagner, Yasunobu Uchiyama, C. van Rensburg, M. Zacharias, C. Trichard, F. Ait Benkhali, Manami Sasaki, S. Schwemmer, Andrea Santangelo, A. Ziegler, G. Maurin, A. Wierzcholska, C. Mariaud, Jacek Niemiec, Olaf Reimer, Thomas Murach, A. Lemière, M. Lemoine-Goumard, I. Shilon, Heinrich J. Völk, R. Marx, P. Bordas, I. Lypova, G. Lamanna, J. Zorn, U. Katz, J.-P. Tavernet, B. Rudak, V. Marandon, K. Katarzyński, A.M. Taylor, V. Sahakian, M. Mohamed, M. Ostrowski, Konrad Bernlöhr, B. Peyaud, G. Pühlhofer, R. Zanin, P. T. O'Brien, Atreyee Sinha, C. van Eldik, 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 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), 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 Cité (UPCité), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, H.E.S.S., Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), PSL Research University (PSL)-PSL Research University (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)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), European Commission, 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 National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Armagh Observatory, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Faculty of Science, High Energy Astrophys. & Astropart. Phys (API, FNWI), Gravitation and Astroparticle Physics Amsterdam, 26598973 - Abdalla, Hassan, 30588766 - Arcaro, Cornelia, 28644743 - Backes, Michael, 20574266 - Barnard, Monica, 24420530 - Böttcher, Markus, 30366755 - Chand, Tej B., 31125417 - Chandra, Sunil, 26403366 - Ndiyavala, Hambeleleni, 10060499 - Van der Walt, Diederick Johannes, 12006653 - Venter, Christo, 26594080 - Wadiasingh, Zorawar, 22799133 - Schutte, Hester M., 20126999 - Seyffert, Albertus Stefanus, 29092086 - Zacharias, Michael, 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: 010504 meteorology & atmospheric sciences, Electromagnetic spectrum, electron: relativistic, magnetic field, Astrophysics, positron: energy, 01 natural sciences, 7. Clean energy, Pulsar wind nebula, particle: acceleration, Raigs gamma, Astrophysics::Solar and Stellar Astrophysics, HESS - Abteilung Hofmann, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, pulsar, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, [PHYS]Physics [physics], Nebula, radio wave, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 4. Education, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], photon, Gamma ray, Astrophysics::Instrumentation and Methods for Astrophysics, High-energy astrophysics, Particle astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Camps magnètics, accelerator, High-energy astronomy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, gap, X-ray, energy loss: rotation, Pulsar, 0103 physical sciences, synchrotron, Astrophysics::Galaxy Astrophysics, gamma ray: energy, 0105 earth and related environmental sciences, Crab Pulsar, Gamma rays, Astronomy and Astrophysics, Crab Nebula, electromagnetic, gamma ray: VHE, [SDU]Sciences of the Universe [physics], Magnetic fields, ddc:520, Physics::Accelerator Physics
Abstract: arXiv:1909.09494v2, H.E.S.S. Collaboration: et al., The support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the German Research Foundation (DFG), the Helmholtz Association, the Alexander von Humboldt Foundation, the French Ministry of Higher Education, Research and Innovation, the Centre National de la Recherche Scientifique (CNRS/IN2P3 and CNRS/INSU), the Commissariat à l’énergie atomique et aux énergies alternatives (CEA), the UK Science and Technology Facilities Council (STFC), the Knut and Alice Wallenberg Foundation, the National Science Centre, Poland (grant number 2016/22/M/ST9/00382), the South African Department of Science and Technology and the National Research Foundation, the University of Namibia, the National Commission on Research, Science and Technology of Namibia (NCRST), the Austrian Federal Ministry of Education, Science and Research and the Austrian Science Fund (FWF), the Australian Research Council (ARC), the Japan Society for the Promotion of Science and the University of Amsterdam. We appreciate the excellent work of the technical support staff in Berlin, Zeuthen, Heidelberg, Palaiseau, Paris, Saclay, Tübingen and Namibia in the construction and operation of the equipment. This work benefited from services provided by the H.E.S.S. Virtual Organisation, supported by the national resource providers of the EGI Federation. R.C.G.C. was funded by EU FP7 Marie Curie (grant agreement number PIEF-GA-2012-332350).
Published: 2020

23. MAGIC very large zenith angle observations of the Crab Nebula up to 100 TeV

Author: David Paneque, A. Biland, T. Schweizer, D. Ninci, Elina Lindfors, J. Besenrieder, D. Guberman, Masahiro Teshima, Chiara Righi, Daniel Mazin, A. De Angelis, J. Becerra González, A. Berti, S. Ansoldi, N. Godinović, S. Fukami, B. Machado de Oliveira Fraga, L. Bellizzi, Giacomo Bonnoli, D. Dominis Prester, K. Mannheim, N. Torres-Albà, J. Palacio, J. van Scherpenberg, P. Da Vela, A. Babić, D. Elsaesser, M. Ribó, D. Morcuende, P. Peñil, F. Leone, I. Šnidarić, A. Rugliancich, Marina Manganaro, V. Moreno, Dario Hrupec, Antonio Stamerra, P. G. Prada Moroni, G. Ceribella, Massimo Persic, Stefano Covino, Konstancja Satalecka, V. Fallah Ramazani, L. Nogués, P. Majumdar, Jose Carlos Herrera, Michele Doro, M. A. Lopez, G. Maneva, Elisa Prandini, D. Miceli, D. Fidalgo, Julian Sitarek, M. Mariotti, S. Cikota, M. I. Martínez, Razmik Mirzoyan, L. Saha, A. Chilingaryan, W. Rhode, G. Vanzo, M. Strzys, J. M. Paredes, Kyoshi Nishijima, U. Barres de Almeida, U. Colin, David A. Green, D. Hadasch, E. Do Souto Espiñeira, Tomislav Terzić, Ciro Bigongiari, D. Dorner, L. A. Antonelli, Petar Temnikov, M. Mallamaci, M. Minev, W. Bhattacharyya, Christian Fruck, S. Lombardi, D. Zarić, Jordi Delgado, John Hoang, Elisa Bernardini, G. Busetto, Y. Suda, Jose Luis Contreras, Dorota Sobczyńska, C. Maggio, Juan Cortina, R. López-Coto, Saša Mićanović, T. Surić, D. Lelas, Fabrizio Tavecchio, Y. Chai, Seiya Nozaki, S. Gasparyan, A. Lamastra, Eduardo Colombo, Ll. Font, S. M. Colak, D. Strom, J. Kushida, V. Vagelli, M. V. Fonseca, Auni Somero, M. Peresano, Kevin Schmidt, A. Arbet Engels, F. Di Pierro, M. Palatiello, Vitaly Neustroev, Luca Tosti, Juan Abel Barrio, M. Takahashi, I. Puljak, Narek Sahakyan, Carlo Vigorito, Laura Maraschi, Francesco Dazzi, Riccardo Paoletti, Markus Gaug, M. Vazquez Acosta, Nicola Giglietto, Valerio D'Elia, M. Delfino, A. López-Oramas, P. Munar-Adrover, G. Ferrara, Susumu Inoue, Abelardo Moralejo, E. Moretti, D. Depaoli, C. Nigro, V. A. Acciari, M. Makariev, Dominik Baack, R. J. García López, Luca Foffano, Francesco Giordano, Kari Nilsson, J. Rico, H. Kubo, Daniel Kerszberg, M. Will, Ž. Bošnjak, L. Jouvin, S. Loporchio, Simona Paiano, K. Noda, Jose Miguel Miranda, Edgar Molina, T. Saito, L. Di Venere, M. Hütten, B. Banerjee, Shunsuke Sakurai, Vincenzo Vitale, Ievgen Vovk, A. Hahn, Y. Iwamura, Markus Garczarczyk, Kazuma Ishio, B. De Lotto, W. Bednarek, Francesco Longo, Oscar Blanch, A. Fattorini, Roberto Carosi, Tomohiro Inada, A. Donini, Federal Ministry of Education and Research (Germany), Istituto Nazionale di Fisica Nucleare, Istituto Nazionale di Astrofisica, Swiss National Science Foundation, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Department of Atomic Energy (India), Ministry of Education, Youth and Science (Bulgaria), Academy of Finland, Universidad de Barcelona, Croatian Science Foundation, University of Rijeka, Ministério da Ciência, Tecnologia e Inovação (Brasil), Acciari, V. A., Ansoldi, S., Antonelli, L. A., Arbet Engels, A., Baack, D., Babic, A., Banerjee, B., Barres De Almeida, U., Barrio, J. A., Becerra Gonzalez, J., Bednarek, W., Bellizzi, L., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Bosnjak, Z., Busetto, G., Carosi, R., Ceribella, G., Chai, Y., Chilingaryan, A., Cikota, S., Colak, S. M., Colin, U., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Depaoli, D., Di Pierro, F., Di Venere, L., Do Souto Espineira, E., Dominis Prester, D., Donini, A., Dorner, D., Doro, M., Elsaesser, D., Fallah Ramazani, V., Fattorini, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Fukami, S., Garcia Lopez, R. J., Garczarczyk, M., Gasparyan, S., Gaug, M., Giglietto, N., Giordano, F., Godinovic, N., Green, D., Guberman, D., Hadasch, D., Hahn, A., Herrera, J., Hoang, J., Hrupec, D., Hutten, M., Inada, T., Inoue, S., Ishio, K., Iwamura, Y., Jouvin, L., Kerszberg, D., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., Lopez, M., Lopez-Coto, R., Lopez-Oramas, A., Loporchio, S., Machado De Oliveira Fraga, B., Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martinez, M., Mazin, D., Micanovic, S., Miceli, D., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Morcuende, D., Moreno, V., Moretti, E., Munar-Adrover, P., Neustroev, V., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogues, L., Nozaki, S., Paiano, S., Palacio, J., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Penil, P., Peresano, M., Persic, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Rhode, W., Ribo, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Schmidt, K., Schweizer, T., Sitarek, J., Snidaric, I., Sobczynska, D., Somero, A., Stamerra, A., Strom, D., Strzys, M., Suda, Y., Suric, T., Takahashi, M., Tavecchio, F., Temnikov, P., Terzic, T., Teshima, M., Torres-Alba, N., Tosti, L., Vagelli, V., Van Scherpenberg, J., Vanzo, G., Vazquez Acosta, M., Vigorito, C. F., Vitale, V., Vovk, I., Will, M., and Zaric, D.
Subjects: Gamma rays: general, ISM: supernova remnants, Methods: observational, Astronomy, gamma rays general, methods observational, ISM supernova remnants, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, model [emission], generalI [Gamma rays], Astrophysics, 01 natural sciences, Raigs gamma, optical, MAGIC (telescope), 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Supernoves, supernova remnants [ISM], Astrophysics::Instrumentation and Methods for Astrophysics, imaging, Supernovae, Gamma rays: generalI, high [energy], Spectral energy distribution, Física nuclear, Astrophysics::High Energy Astrophysical Phenomena, general [Gamma rays], FOS: Physical sciences, SM: supernova remnants, monitoring [atmosphere], emission [gamma ray], 0103 physical sciences, Calibration, observational [Methods], 14. Life underwater, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Cherenkov radiation, Zenith, Computer Science::Information Retrieval, Gamma rays, Astronomy and Astrophysics, calibration, supernova remnants [SM], MAGIC, Cherenkov counter, Crab Nebula, Space and Planetary Science, ddc:520, spectral, supernova remnant [ISM], Energy (signal processing), Fermi Gamma-ray Space Telescope
Abstract: Aims. We measure the Crab Nebula γ-ray spectral energy distribution in the ~100 TeV energy domain and test the validity of existing leptonic emission models at these high energies. Methods. We used the novel very large zenith angle observations with the MAGIC telescope system to increase the collection area above 10 TeV. We also developed an auxiliary procedure of monitoring atmospheric transmission in order to assure proper calibration of the accumulated data. This employs recording optical images of the stellar field next to the source position, which provides a better than 10% accuracy for the transmission measurements. Results. We demonstrate that MAGIC very large zenith angle observations yield a collection area larger than a square kilometer. In only ~ 56 h of observations, we detect the γ-ray emission from the Crab Nebula up to 100 TeV, thus providing the highest energy measurement of this source to date with Imaging Atmospheric Cherenkov Telescopes. Comparing accumulated and archival MAGIC and Fermi/LAT data with some of the existing emission models, we find that none of them provides an accurate description of the 1 GeV to 100 TeV γ-ray signal., The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, FPA2017-90566-REDC), the Indian Department of Atomic Energy, the Japanese JSPS and MEXT, the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-153/28.08.2018 and the Academy of Finland grant nr. 320045 is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia “Severo Ochoa” SEV-2016-0588 and SEV-2015-0548, and Unidad de Excelencia “María de Maeztu” MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382 and by the Brazilian MCTIC, CNPq and FAPERJ. This research has made use of the CTA instrument response functions provided by the CTA Consortium and Observatory, see http://www.cta-observatory.org/science/cta-performance/ (version prod3b-v1) for more details.
Published: 2020

24. Inverse Compton emission from relativistic jets in binary systems

Author: Valentí Bosch-Ramon, Dmitry Khangulyan, and Yasunobu Uchiyama
Subjects: Astrofísica, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Inverse, Binary number, Astrophysics, Electron, 01 natural sciences, Raigs gamma, Astrophysical jet, 0103 physical sciences, 010303 astronomy & astrophysics, Estels binaris de raigs X, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Jet (fluid), 010308 nuclear & particles physics, Attenuation, Gamma rays, Compton scattering, Astronomy and Astrophysics, X-ray binaries, Space and Planetary Science, Beta (plasma physics), Astrophysics - High Energy Astrophysical Phenomena
Abstract: The gamma-ray emission detected from several microquasars can be produced by relativistic electrons emitting through inverse Compton scattering. In particular, the GeV emission detected from Cygnus X-3, and its orbital phase dependence, strongly suggest that the emitting electrons are accelerated in a relativistic jet, and that the optical companion provides the dominant target. Here, we study the effects related to particle transport in the framework of the relativistic jet scenario. We find that even in the most compact binary systems, with parameters similar to Cygnus X-3, particle transport can have a substantial influence on the GeV lightcurve unless the jet is slow, $\beta < 0.7$. In more extended binary systems, strong impact of particle transport is nearly unavoidable. Thus, even for a very compact system such as Cygnus X-3, particle transport significantly affects the ability of one-zone models to infer the properties of the gamma-ray production site based on the shape on the GeV lightcurve. We conclude that a detailed study of the gamma-ray spectrum can further constrain the structure and other properties of the gamma-ray emitter in Cygnus X-3, although such a study should account for gamma-gamma attenuation, since it may strongly affect the spectrum above $5\rm\,GeV$., Comment: 15 pages, 12 figures, MNRAS in press
Published: 2018

25. Calibration of gamma radiation beams of a secondary standards dosimetry laboratory: Programme Feixos19

Author: Universitat Politècnica de Catalunya. Departament de Física, Institut de Tècniques Energètiques (INTE), Ginjaume Egido, Mercè, Costa Vargas, Daniel, Universitat Politècnica de Catalunya. Departament de Física, Institut de Tècniques Energètiques (INTE), Ginjaume Egido, Mercè, and Costa Vargas, Daniel
Abstract: In this project, a new software called “Feixos19” is developed to allow defining the experimental conditions to calibrate protection monitors or to irradiate passive dosemeters with gamma beams in the calibration and dosimetry laboratory of the “Institut de Tècniques Energètiques” (INTE) of UPC. At the beginning of this project, the metrology, especially metrology for ionizing radiation, is introduced with basic concepts of dosimetry and radiation protection. More ahead, this project describes the calibration and dosimetry laboratory of the INTE, as an example of a calibration laboratory, and how this laboratory calibrates the radiation protection monitors with gamma beams. Next, it is explained how to calibrate gamma beams with a practical example. Finally, it is described the basis, the subsequent development and the consequent elaboration of “Feixos19”.
Published: 2019

26. The search for high-energy neutrinos coincident with fast radio bursts with the ANTARES neutrino telescope

Author: Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, Albert, Arthur, André, Michel, Anghinolfi, Marco, Anton, Gisela, Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, Albert, Arthur, André, Michel, Anghinolfi, Marco, and Anton, Gisela
Abstract: In the past decade, a new class of bright transient radio sources with millisecond duration has been discovered. The origin of these so-called fast radio bursts (FRBs) is still a mystery, despite the growing observational efforts made by various multiwavelength and multimessenger facilities. To date, many models have been proposed to explain FRBs, but neither the progenitors nor the radiative and the particle acceleration processes at work have been clearly identified. In this paper, we assess whether hadronic processes may occur in the vicinity of the FRB source. If they do, FRBs may contribute to the high-energy cosmic-ray and neutrino fluxes. A search for these hadronic signatures was carried out using the ANTARES neutrino telescope. The analysis consists in looking for high-energy neutrinos, in the TeV–PeV regime, that are spatially and temporally coincident with the detected FRBs. Most of the FRBs discovered in the period 2013–2017 were in the field of view of the ANTARES detector, which is sensitive mostly to events originating from the Southern hemisphere. From this period, 12 FRBs were selected and no coincident neutrino candidate was observed. Upper limits on the per-burst neutrino fluence were derived using a power-law spectrum, dN/dE¿¿E-¿¿¿, for the incoming neutrino flux, assuming spectral indexes ¿ = 1.0, 2.0, 2.5. Finally, the neutrino energy was constrained by computing the total energy radiated in neutrinos, assuming different distances for the FRBs. Constraints on the neutrino fluence and on the energy released were derived from the associated null results, Peer Reviewed, Postprint (published version)
Published: 2019

27. SENTISIM: A hybrid training platform for SLNB in local melanoma staging

Author: Universitat Politècnica de Catalunya. Departament d'Enginyeria de Sistemes, Automàtica i Informàtica Industrial, Universitat Politècnica de Catalunya. GRINS - Grup de Recerca en Robòtica Intel·ligent i Sistemes, Hernansanz Prats, Alberto, Pieras Morell, Tomas, Ferrandiz Pulido, Lara, Moreno Ramirez, David, Casals Gelpí, Alicia, Universitat Politècnica de Catalunya. Departament d'Enginyeria de Sistemes, Automàtica i Informàtica Industrial, Universitat Politècnica de Catalunya. GRINS - Grup de Recerca en Robòtica Intel·ligent i Sistemes, Hernansanz Prats, Alberto, Pieras Morell, Tomas, Ferrandiz Pulido, Lara, Moreno Ramirez, David, and Casals Gelpí, Alicia
Abstract: Sentinel Lymph Node Biopsy (SLNB) has been established as an accurate procedure for regional melanoma staging. SNLB has a diagnostic significance as biopsy-based staging identifies patients with nodal metastases who may benefit from immediate complete lymphadenectomy and prolongs disease-free survival for all patients. This work presents a new training platform for SLNB in local melanoma staging, that solves the previous problemsmaintaining a realistic scenario, at the same time that measures a series of important parameters to determine the quality of the surgery., Peer Reviewed, Postprint (published version)
Published: 2019

28. Estudio de una galga de retrodispersión de radiación gamma

Author: Universitat Politècnica de Catalunya. Departament de Física, Blas del Hoyo, Alfredo de, Tello Guizado, Josué Eduardo, Universitat Politècnica de Catalunya. Departament de Física, Blas del Hoyo, Alfredo de, and Tello Guizado, Josué Eduardo
Abstract: El presente informe es un estudio sobre la optimización de la configuración de una galga inclinada de retrodispersión que es un sistema formado por un detector de centelleo 3”x3” de NaI, una fuente de radiación gamma, 60Co o 137Cs en este caso, para poder medir el espesor de diferentes muestras. Las simulaciones con PENELOPE, que es un código de simulación de transporte de radiaciones ionizantes como los rayos gamma que está basado en métodos Monte Carlo, permite estudiar cual es la mejor configuración de las galgas, para llegar a esta se han hecho muchas simulaciones y con el análisis de las primeras simulaciones se decide nuevas configuraciones para conseguir el objetivo de optimizar la galga. Para verificar que los resultados obtenidos con PENELOPE se asemejan a la realidad, primero se realiza una simulación básica de una fuente de 60Co y un detector de centelleo 3”x3” de NaI y posteriormente un experimento con los mismos elementos y configuración para verificar que el número de cuentas por segundo detectadas son iguales para ambas. Además de encontrar la mejor configuración, se determina diferentes curvas de retrodispersión para distintos materiales (Al y Fe) y fuentes (60Co o 137Cs) para distintos tipos de galgas, y sus respectivos espesores de saturación. También se comprueban la relación entre número atómico y el número de cuentas netas de las partículas gamma. Este trabajo contiene información sobre diferentes tipos de galgas (inclinadas y sin barrera), la teoría sobre la determinación de espesores de distintas muestras y como utilizar el programa PENELOPE. Finalmente se realiza un presupuesto orientativo y un estudio de impacto ambiental de este proyecto.
Published: 2019

29. A model for high-mass microquasar jets under the influence of a strong stellar wind

Author: E. Molina, V. Bosch-Ramon, and Santiago del Palacio
Subjects: Ciencias Astronómicas, Photon, 010504 meteorology & atmospheric sciences, Ciencias Físicas, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Electron, Astrophysics, 01 natural sciences, purl.org/becyt/ford/1 [https], X-rays: binaries, Raigs gamma, massive [stars], Astrophysical jet, Microquasars, 0103 physical sciences, Adiabatic process, winds, outflows [stars], 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Estels binaris de raigs X, relativistic processes, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, stars: winds, outflows, Momentum transfer, Gamma rays, Gamma ray, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], radiation mechanisms: non-thermal, Light curve, non-thermal [radiation mechanisms], Astronomía, stars: massive, X-ray binaries, Space and Planetary Science, Orbital motion, High Energy Physics::Experiment, binaries [X-rays], Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS
Abstract: High-mass microquasars (HMMQs) are systems from which relativistic jets are launched. At the scales of several times the binary system size, the jets are expected to follow a helical path caused by the interaction with a strong stellar wind and orbital motion. Such a trajectory has its influence on the non-thermal emission of the jets, which also depends strongly on the observing angle due to Doppler boosting effects. We explore how the expected non-thermal emission of HMMQ jets at small scales is affected by the impact of the stellar wind and the orbital motion on the jet propagation. We studied the broadband non-thermal emission, from radio to gamma rays, produced in HMMQ jets up to a distance of several orbital separations, taking into account a realistic jet trajectory, different model parameters, and orbital modulation. The jet trajectory is computed by considering momentum transfer with the stellar wind. Electrons are injected at the position where a recollimation shock in the jets is expected due to the wind impact. Their distribution along the jet path is obtained assuming local acceleration at the recollimation shock, and cooling via adiabatic, synchrotron, and inverse Compton processes. The synchrotron and inverse Compton emission is calculated taking into account synchrotron self-absorption within the jet, free-free absorption with the stellar wind, and absorption by stellar photons via pair production. Asymmetric light curves are obtained owing to the helical trajectory of the jets. The presence of helical shaped jets could be inferred from asymmetries in the light curves, which become noticeable only for large jet Lorentz factors and low magnetic fields. Model parameters could be constrained if accurate phase-resolved light curves from GeV to TeV energies were available., Comment: 11 pages, 12 figures, published in Astronomy & Astrophysics. v2: Typo corrected in Eq. 2
Published: 2019

30. H.E.S.S. and Suzaku observations of the Vela X pulsar wind nebula

Author: P. deWilt, J. King, C. Mariaud, J. Zorn, J. Dyks, Matteo Cerruti, Nachiketa Chakraborty, Jacek Niemiec, D. J. van der Walt, Florian Gaté, R. C. G. Chaves, E. O. Angüner, G. Lamanna, S. Nakashima, Olaf Reimer, H. Yoneda, Werner Hofmann, J. Lau, Michelle Tsirou, N. Shafi, Natalia Żywucka, M. de Naurois, Michael Punch, L. Rinchiuso, Michael Backes, Sami Caroff, Thomas Murach, D. A. Prokhorov, K. Kosack, Konrad Bernlöhr, M.-H. Grondin, G. Emery, Stefan Ohm, S. Saito, Axel Donath, A. W. Chen, F. Niederwanger, Markus Böttcher, M. Seglar-Arroyo, S. Pita, G. Pühlhofer, Krzysztof Katarzynski, Tim Holch, Ramin Marx, M. Panter, U. Katz, Jacco Vink, Catherine Boisson, A. Reimer, Marek Jamrozy, Ruizhi Yang, Stefano Gabici, Naomi Tsuji, Emmanuel Moulin, Pierre Brun, V. Marandon, I. Oya, M. Kraus, Helene Sol, I. Shilon, Sabrina Casanova, M. Büchele, F. Ait Benkhali, Anton Dmytriiev, Jean-Pierre Ernenwein, A. Fiasson, Manami Sasaki, L. Oakes, C. Perennes, S. Schwemmer, Andrea Santangelo, J. Bolmont, S. J. Fegan, A. Djannati-Ataï, R. D. Parsons, V. Poireau, Dieter Horns, D. Jankowsky, Johannes Veh, M. Tluczykont, F. Schüssler, A. Schulz, S. Bonnefoy, H. Abdalla, M. A. Kastendieck, T. Chand, G. Vasileiadis, Constantin Steppa, E. de Oña Wilhelmi, Isak Delberth Davids, M. Mohamed, E. Leser, Włodek Kluźniak, Roberta Zanin, Y. A. Gallant, Clemens Hoischen, A. A. Zdziarski, Nu. Komin, Iryna Lypova, Gianluca Giavitto, Heinrich J. Völk, Yvonne Becherini, P. T. O'Brien, Ullrich Schwanke, M. Renaud, B. van Soelen, B. Condon, Riaan Steenkamp, B. Khélifi, G. Hermann, Regis Terrier, Rachel Simoni, Carlo Romoli, Christoph Deil, B. Rudak, D. Gottschall, Anne Lemiere, Justine Devin, Mohanraj Senniappan, A. Carosi, K. Egberts, Masanori Arakawa, Pascal Vincent, H. Odaka, Frank M. Rieger, R. Blackwell, E. Ruiz-Velasco, Thomas Bylund, S. Raab, I. Jung-Richardt, Tadayuki Takahashi, A. S. Seyffert, Atreyee Sinha, Kirsty Feijen, C. van Eldik, Victor Doroshenko, Markus Holler, G. Heinzelmann, Felix Jankowsky, D. Berge, M. Füßling, N. Maxted, R. J. Tuffs, Felix Aharonian, G. Martí-Devesa, H. Prokoph, Jim Hinton, Dmitry Khangulyan, Alison Mitchell, S. Eschbach, Thomas Lohse, H. Iwasaki, L. Tibaldo, J.-P. Tavernet, Kleopas Shiningayamwe, F. Voisin, Reinhard Schlickeiser, S. Colafrancesco, S. Chandra, M. Capasso, Michal Ostrowski, V. Sahakian, J.-P. Lenain, Dmitriy Kostunin, L. Dirson, R. J. White, R. Rauth, Gilles Maurin, Zorawar Wadiasingh, Stefan Funk, Alicja Wierzcholska, Domenico Tiziani, D. Malyshev, Monica Barnard, Thomas Tavernier, B. Peyaud, Maria Haupt, Hester Schutte, L. O'c. Drury, A.M. Taylor, Rafal Moderski, Andreas Specovius, Christo Venter, C. Trichard, P. J. Meintjes, A. Zech, David Sánchez, A. Ziegler, Léa Jouvin, Marion Spir-Jacob, D. Huber, C. Arcaro, Gavin Rowell, M. Bryan, D. Zaborov, C. Moore, Dorit Glawion, Tomasz Bulik, M. Katsuragawa, A. Jacholkowska, Andreas Quirrenbach, Michael Zacharias, Joachim Hahn, P.-O. Petrucci, Stefan Klepser, Łukasz Stawarz, Gilles Henri, Q. Piel, Christian Stegmann, Stefan Wagner, Yasunobu Uchiyama, L. Mohrmann, C. van Rensburg, T. Vuillaume, J. F. Glicenstein, A. Priyana Noel, Francois Brun, J. Bregeon, Celine Armand, Ruben Lopez-Coto, M. Lemoine-Goumard, Gilles Fontaine, A. Marcowith, Hambeleleni Ndiyavala, 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 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), 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)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), 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), 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), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), 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), H.E.S.S. Collaboration, 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)-Université de Montpellier (UM)-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), 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, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-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), API Other Research (FNWI), Faculty of Science, High Energy Astrophys. & Astropart. Phys (API, FNWI), 26598973 - Abdalla, Hassan, 30588766 - Arcaro, Cornelia, 28644743 - Backes, M., 20574266 - Barnard, Monica, 24420530 - Böttcher, Markus, 31125417 - Chandra, Sunil, 26403366 - Ndiyavala, Hambeleleni, 22799133 - Schutte, Hester M., 20126999 - Seyffert, Albertus Stefanus, 21106266 - Van Rensburg, Carlo, 12006653 - Venter, Christo, 26594080 - Wadiasingh, Zorawar, 29092086 - Zacharias, Michael, 30366755 - Chand, T.B., 34208968 - Zywucka-Hejzner, Natalia, 10060499 - Van der Walt, Diederick Johannes, 28644743 - Backes, Michael, 30366755 - Chand, Tej B., Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Camps magnètics, Astrophysics::High Energy Astrophysical Phenomena, Synchrotron radiation, FOS: Physical sciences, Cosmic ray, Astrophysics, Vela, gamma rays: stars, 01 natural sciences, 7. Clean energy, Pulsar wind nebula, outflows, Relativistic particle, Raigs gamma, Pulsar, 0103 physical sciences, ddc:530, winds, outflows [stars], 010303 astronomy & astrophysics, individual: PSR B0833-45 [pulsars], Astrophysics::Galaxy Astrophysics, acceleration of particles, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Computer Science::Information Retrieval, Gamma rays, Institut für Physik und Astronomie, Astronomy and Astrophysics, radiation mechanisms: non-thermal, non-thermal [radiation mechanisms], stars [gamma rays], pulsars: individual: PSR B0833-45, Crab Nebula, 13. Climate action, Space and Planetary Science, stars: winds, Magnetic fields, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Heliosphere
Abstract: Pulsar Wind Nebulae (PWNe) represent the most prominent population of Galactic very-high-energy gamma-ray sources and are thought to be an efficient source of leptonic cosmic rays. Vela X is a nearby middle-aged PWN, which shows bright X-ray and TeV gamma-ray emission toward an elongated structure called the cocoon. Since TeV emission is likely inverse-Compton emission of electrons while X-ray emission is synchrotron radiation of the same electrons, we aim to derive the properties of the relativistic particles and of magnetic fields with minimal modelling. We use data from the Suzaku XIS to derive the spectra from three compact regions in Vela X covering distances from 0.3 pc to 4 pc from the pulsar along the cocoon. We obtain gamma-ray spectra of the same regions from H.E.S.S. observations and fit a radiative model to the multi-wavelength spectra. The TeV electron spectra and magnetic field strengths are consistent within the uncertainties for the three regions, with energy densities of the order $10^{-12}\rm\,erg\,cm^{-3}$. The data indicate the presence of a cutoff in the electron spectrum at energies of $\sim$100 TeV and a magnetic field strength of $\sim$$6\,\rm\mu G$. Constraints on the presence of turbulent magnetic fields are weak. The pressure of TeV electrons and magnetic fields in the cocoon is dynamically negligible, requiring the presence of another dominant pressure component. Sub-TeV electrons cannot account completely for the missing pressure, that may be provided either by relativistic ions or from mixing of the ejecta with the pulsar wind. The electron spectra are consistent with expectations from transport scenarios dominated either by advection via the reverse shock or by diffusion. Constraints on turbulent magnetic fields and the shape of the electron cutoff can be improved by spectral measurements in the energy range $\gtrsim 10\rm\,keV$. (abridged), Comment: Accepted for publication in A&A
Published: 2019

31. Gamma rays from jets interacting with BLR clouds in blazars

Author: Gustavo E. Romero, Santiago del Palacio, and Valenti Bosch Ramon
Subjects: GALAXIES [GAMMA RAYS], Ciencias Físicas, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, NON-THERMAL [RADIATION MECHANISMS], 01 natural sciences, purl.org/becyt/ford/1 [https], Raigs gamma, 0103 physical sciences, Nucli galàctic actiu, Blazar, ACTIVE [GALAXIES], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Active galactic nuclei, 010308 nuclear & particles physics, Gamma rays, Gamma ray, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], Astronomía, Space and Planetary Science, Galàxies actives, Active galaxies, Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS
Abstract: The innermost parts of powerful jets in active galactic nuclei are surrounded by dense, high-velocity clouds from the broad-line region, which may penetrate into the jet and lead to the formation of a strong shock. Such jet-cloud interactions are expected to have measurable effects on the $\gamma$-ray emission from blazars. We characterise the dynamics of a typical cloud-jet interaction scenario, and the evolution of its radiative output in the 0.1-30~GeV energy range, to assess to what extent these interactions can contribute to the $\gamma$-ray emission in blazars. We use semi-analytical descriptions of the jet-cloud dynamics, taking into account the expansion of the cloud inside the jet and its acceleration. Assuming that electrons are accelerated in the interaction and making use of the hydrodynamical information, we then compute the high-energy radiation from the cloud, including the absorption of $\gamma$-rays in the ambient photon field through pair creation. Jet-cloud interactions can lead to significant $\gamma$-ray fluxes in blazars with a broad-line region, in particular when the cloud expansion and acceleration inside the jet are taken into account. This is caused by 1) the increased shocked area in the jet, which leads to an increase in the energy budget for the non-thermal emission; 2) a more efficient inverse Compton cooling with the boosted photon field of the broad-line region; and 3) an increased observer luminosity due to Doppler boosting effects. For typical broad-line region parameters, either (i) jet-cloud interactions contribute significantly to the persistent $\gamma$-ray emission from blazars or (ii) the broad-line region is far from spherical or the fraction of energy deposited in non-thermal electrons is small., Comment: 9 pages, 9 figures. Accepted for publication in A&A
Published: 2019

32. Gamma rays from red giant wind bubbles entering the jets of elliptical host blazars

Author: N. Torres-Albà and Valentí Bosch-Ramon
Subjects: Red giant, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Raigs gamma, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Nucli galàctic actiu, Blazar, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Jet (fluid), Active galactic nuclei, 010308 nuclear & particles physics, Gamma rays, Gamma ray, Astronomy and Astrophysics, Magnetic field, Stars, Space and Planetary Science, Galàxies actives, Elliptical galaxy, Active galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Blazars in elliptical hosts have a population of red giants surrounding their jet. These stars can carry large wind-blown bubbles into the jets, leading to gamma-ray emission through bubble-jet interactions. We study the interaction dynamics and the gamma-ray emission produced when the bubbles formed by red giant winds penetrate the jet of a blazar in an elliptical galaxy. First, we characterized the masses and penetration rates of the red giant wind bubbles that enter the jet. Then, the dynamical evolution of these bubbles under the jet impact was analysed analytically and numerically, and the radiation losses of the particles accelerated in the interaction were characterised. Finally, the synchrotron and the inverse Compton contributions above 100 MeV were estimated under different jet magnetic fields, powers, and Lorentz factors. We find that an analytical dynamical model is a reasonable approximation for the red giant wind bubble-jet interaction. The radiation produced by these wind bubbles interacting with a jet can have a duty cycle of up to 1. For realistic magnetic fields, gamma rays could be detectable from sources within the local universe, preferentially from those with high Lorentz factors (of about 10), and this could be a relatively common phenomenon for these sources. For magnetic fields in equipartition with the jet power, and high acceleration rates, synchrotron gamma rays may be detectable even for modest Lorentz factors (of about 3), but with a much lower duty cycle., 9 pages, 3 figures, 1 table, accepted for publication in A&A
Published: 2019

33. Calibration of gamma radiation beams of a secondary standards dosimetry laboratory: Programme Feixos19

Author: Costa Vargas, Daniel, Ginjaume Egido, Mercè, Universitat Politècnica de Catalunya. Departament de Física, and Institut de Tècniques Energètiques (INTE)
Subjects: Energies::Energia nuclear::Protecció radiològica [Àrees temàtiques de la UPC], Raigs gamma, Gamma rays, Radioactivitat -- Mesurament -- Programes d’ordinador, Radioactivity -- Measurement -- Computer programs
Abstract: In this project, a new software called “Feixos19” is developed to allow defining the experimental conditions to calibrate protection monitors or to irradiate passive dosemeters with gamma beams in the calibration and dosimetry laboratory of the “Institut de Tècniques Energètiques” (INTE) of UPC. At the beginning of this project, the metrology, especially metrology for ionizing radiation, is introduced with basic concepts of dosimetry and radiation protection. More ahead, this project describes the calibration and dosimetry laboratory of the INTE, as an example of a calibration laboratory, and how this laboratory calibrates the radiation protection monitors with gamma beams. Next, it is explained how to calibrate gamma beams with a practical example. Finally, it is described the basis, the subsequent development and the consequent elaboration of “Feixos19”.
Published: 2019

34. High Energy Processes in Active Galaxies

Author: Torres Albà, Núria, Bosch i Ramon, Valentí, Iwasawa, Kazushi, Manrique Oliva, Alberto, and Universitat de Barcelona. Departament de Física Quàntica i Astrofísica
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Gamma rays, Particle physics, Astrophysics::Cosmology and Extragalactic Astrophysics, Rayos gamma, Astronomía de rayos X, Ciències Experimentals i Matemàtiques, Cúasares, Astronomia de raigs X, X-ray astronomy, Raigs gamma, Física de partículas, Física de partícules, Quasars, Astrophysics::Galaxy Astrophysics, Quàsars
Abstract: [eng] This thesis has as an objective the study of very energetic phenomena in the central regions of active galaxies. Intense star formation is triggered by mergers of galaxies, and the funneling of large quantities of gas toward the inner regions is thought to also cause accretion onto the central black hole. Whether the two processes necessarily take place together as a step of galaxy evolution is still debated. Regardless of the origin of their connection, star formation and strong AGN activity often coexist in the nuclei of galaxies. Even after star formation is no longer ongoing, the nuclear starburst in a merger results in the formation of galactic bulges. Therefore, stellar densities in the inner kiloparsecs of a galaxy are typically high. As stars, or star forming regions, are close to the AGN, interaction between the two is expected to be frequent, and it can result in a multitude of phenomena worthy of study. The thesis thus focuses on high energy processes taking place in regions where AGN activity and stellar presence is likely important. In particular, the goal of the thesis is to study the emission produced by these phenomena, in the range of X-rays to gamma-rays, whether to disentangle their individual contributions or to detect emission resulting from their interaction. The thesis intends to provide data to continue the study of the starburst-AGN connection, and new models to explain the production of gamma rays in other galaxies. Part I focuses on the X-ray analysis of a local sample of LIRGs. The Great Observatories All-Sky LIRG survey (GOALS) is a project to study the brightest infrared galaxies at z < 0.1, in all possible wavelengths. In this part we analyze data for 63 LIRGs in the lower luminosity range of GOALS. We provide X-ray images, fluxes, luminosities and radial profiles for 84 individual galaxies, spanning a wide range of activity types and merger stages. We also provide information on AGN presence using X-ray and IR diagnostics, and compare the results to those derived for the brightest GOALS galaxies. The data provided in this part will help shine light into the importance of AGN presence in LIRGs, in the context of galaxy evolution. Parts II and III focus on the interaction of AGN jets with stellar populations. When the jet of an AGN impacts a stellar wind, or a blob of material, a shock is formed in which particles can be accelerated up to relativistic energies. We estimate, for different scenarios, the dynamical evolution of the obstacles in the jet and gamma-ray emission generated by the accelerated particles. Part II focuses on the presence of whole populations of stars with high mass-loss rates interacting with the jet, whether because they are inside it, or because they expel layers of accumulated shocked material at the moment they penetrate it. Part III deals with single obstacles, in particular the remnant of a supernova explosion that takes place within the jet. In both parts II and III we include dynamical simulations that illustrate the process and how it affects the jet. Part IV focuses on the interaction of AGN jets with the environment at large scales, in this case considering them as possible sources of reionization at z=6. We estimate the number of jetted sources at the epoch of reionization using rest-UV detections of AGN. We then correct the observed density of sources for effects of obscuration using X-ray data. Jets at high redshift interact strongly with the CMB, upscattering its photons up to ionizing wavelengths through IC, and possibly ionizing the ambient medium significantly., [spa] Esta tesis tiene como objetivo el estudio de fenómenos altamente energéticos en las regiones centrales de las galaxias activas. La formación intensa de estrellas se produce tras una fusión de galaxias, y este mismo fenómeno puede resultar en la acreción de material sobre el agujero negro supermasivo central (AGN). Incluso cuando el episodio de formación de estrellas ha terminado, este ha dado lugar a un bulbo galáctico; por lo que las densidades estelares en las zonas centrales de las galaxias son típicamente elevadas. Por lo tanto, es de esperar que las interacciones entre estrellas y AGN sean un fenómeno frecuente, que puede dar lugar a una gran cantidad de fenómenos interesantes. En particular, la tesis tiene como objetivo estudiar la emisión producida por estos fenómenos, en el rango de rayos X a rayos gamma, ya sea para distinguir las contribuciones individuales de cada uno o para estudiar la emisión generada en su interacción. La tesis pretende proveer datos para continuar el estudio de la relación entre formación estelar y actividad AGN, y nuevos modelos para explicar la producción de rayos gamma en otras galaxias. La primera parte de la tesis es un estudio en rayos X de galaxias lumínicas en el infrarojo. Se analiza una muestra local, proporcionando imágenes, flujos, luminosidades y perfiles radiales en rayos X de 84 galaxias individuales. También se proporciona información sobre la presencia de AGN en ellas, usando datos en rayos X e infrarojo. La parte central de la tesis se centra en el estudio de la interacción entre jets de AGN y estrellas, ya sea porque estas se encuentran dentro de él, porque le inyectan material al penetrarlo, o porque explotan como supernovas en su interior. Se estudia la evolución dinámica de estos fenómenos, y los rayos gamma producidos. La última parte estima la contribución de los jets de AGN a la reionización del universo, puesto que su interacción con los fotones del fondo cósmico de microondas puede resultar en radiación ionizante a través del mecanismo de Compton inverso.
Published: 2019

35. Estudio de una galga de retrodispersión de radiación gamma

Author: Tello Guizado, Josué Eduardo, Blas del Hoyo, Alfredo de, Universitat Politècnica de Catalunya. Departament de Física, and De Blas Del Hoyo, Alfredo
Subjects: Raigs gamma, Gamma rays, Física::Electromagnetisme [Àrees temàtiques de la UPC]
Abstract: El presente informe es un estudio sobre la optimización de la configuración de una galga inclinada de retrodispersión que es un sistema formado por un detector de centelleo 3”x3” de NaI, una fuente de radiación gamma, 60Co o 137Cs en este caso, para poder medir el espesor de diferentes muestras. Las simulaciones con PENELOPE, que es un código de simulación de transporte de radiaciones ionizantes como los rayos gamma que está basado en métodos Monte Carlo, permite estudiar cual es la mejor configuración de las galgas, para llegar a esta se han hecho muchas simulaciones y con el análisis de las primeras simulaciones se decide nuevas configuraciones para conseguir el objetivo de optimizar la galga. Para verificar que los resultados obtenidos con PENELOPE se asemejan a la realidad, primero se realiza una simulación básica de una fuente de 60Co y un detector de centelleo 3”x3” de NaI y posteriormente un experimento con los mismos elementos y configuración para verificar que el número de cuentas por segundo detectadas son iguales para ambas. Además de encontrar la mejor configuración, se determina diferentes curvas de retrodispersión para distintos materiales (Al y Fe) y fuentes (60Co o 137Cs) para distintos tipos de galgas, y sus respectivos espesores de saturación. También se comprueban la relación entre número atómico y el número de cuentas netas de las partículas gamma. Este trabajo contiene información sobre diferentes tipos de galgas (inclinadas y sin barrera), la teoría sobre la determinación de espesores de distintas muestras y como utilizar el programa PENELOPE. Finalmente se realiza un presupuesto orientativo y un estudio de impacto ambiental de este proyecto.
Published: 2019

36. The search for high-energy neutrinos coincident with fast radio bursts with the ANTARES neutrino telescope

Author: Albert, A, André, M, Anghinolfi, M, Anton, G, Ardid, M, Aubert, J-J, Aublin, J, Avgitas, T, Baret, B, Barrios-Martí, J, Basa, S, Belhorma, B, Bertin, V, Biagi, S, Bormuth, R, Boumaaza, J, Bourret, S, Bouwhuis, M C, Brânzaş, H, Bruijn, R, Brunner, J, Busto, J, Capone, A, Caramete, L, Carr, J, Celli, S, Chabab, M, Cherkaoui&nbsp, El&nbsp, Moursli, R, Chiarusi, T, Circella, M, Coelho, J A B, Coleiro, A, Colomer, M, Coniglione, R, Costantini, H, Coyle, P, Creusot, A, Díaz, A F, Deschamps, A, Distefano, C, Palma, I Di, Domi, A, Donzaud, C, Dornic, D, Drouhin, D, Eberl, T, Bojaddaini, I El, Khayati, N El, Elsässer, D, Enzenhöfer, A, Ettahiri, A, Fassi, F, Felis, I, Fermani, P, Ferrara, G, Fusco, L, Gay, P, Glotin, H, Grégoire, T, Gracia-Ruiz, R, Graf, K, Hallmann, S, van&nbsp, Haren, H, Heijboer, A J, Hello, Y, Hernández-Rey, J J, Hößl, J, Hofestädt, J, Illuminati, G, James, C W, de&nbsp, Jong, M, Jongen, M, Kadler, M, Kalekin, O, Katz, U, Kouchner, A, Kreter, M, Kreykenbohm, I, Kulikovskiy, V, Lachaud, C, Lahmann, R, Lefèvre, D, Leonora, E, Levi, G, Lotze, M, Loucatos, S, Marcelin, M, Margiotta, A, Marinelli, A, Martínez-Mora, J A, Mele, R, Melis, K, Migliozzi, P, Moussa, A, Navas, S, Nezri, E, Nuñez, A, Organokov, M, Păvălaş, G E, Pellegrino, C, Piattelli, P, Popa, V, Pradier, T, Quinn, L, Racca, C, Randazzo, N, Riccobene, G, Sánchez-Losa, A, Saldaña, M, Salvadori, I, Samtleben, D F E, Sanguineti, M, Sapienza, P, Schüssler, F, Spurio, M, Stolarczyk, Th, Taiuti, M, Tayalati, Y, Trovato, A, Turpin, D, Vallage, B, Van&nbsp, Elewyck, V, Versari, F, Vivolo, D, Wilms, J, Zaborov, D, Zornoza, J D, Zúñiga, J, Albert, A., Andre, M., Anghinolfi, M., Anton, G., Ardid, M., Aubert, J. -J., Aublin, J., Avgitas, T., Baret, B., Barrios-Marti, J., Basa, S., Belhorma, B., Bertin, V., Biagi, S., Bormuth, R., Boumaaza, J., Bourret, S., Bouwhuis, M. C., Branzas, H., Bruijn, R., Brunner, J., Busto, J., Capone, A., Caramete, L., Carr, J., Celli, S., Chabab, M., Cherkaoui El Moursli, R., Chiarusi, T., Circella, M., Coelho, J., Coleiro, A., Colomer, M., Coniglione, R., Costantini, H., Coyle, P., Creusot, A., Diaz, A. F., Deschamps, A., Distefano, C., Di Palma, I., Domi, A., Donzaud, C., Dornic, D., Drouhin, D., Eberl, T., El Bojaddaini, I., El Khayati, N., Elsasser, D., Enzenhofer, A., Ettahiri, A., Fassi, F., Felis, I., Fermani, P., Ferrara, G., Fusco, L., Gay, P., Glotin, H., Gregoire, T., Gracia-Ruiz, R., Graf, K., Hallmann, S., van Haren, H., Heijboer, A. J., Hello, Y., Hernandez-Rey, J. J., Hossl, J., Hofestadt, J., Illuminati, G., James, C. W., de Jong, M., Jongen, M., Kadler, M., Kalekin, O., Katz, U., Kouchner, A., Kreter, M., Kreykenbohm, I., Kulikovskiy, V., Lachaud, C., Lahmann, R., Lefevre, D., Leonora, E., Levi, G., Lotze, M., Loucatos, S., Marcelin, M., Margiotta, A., Marinelli, A., Martinez-Mora, J. A., Mele, R., Melis, K., Migliozzi, P., Moussa, A., Navas, S., Nezri, E., Nunez, A., Organokov, M., Pavalas, G. E., Pellegrino, C., Piattelli, P., Popa, V., Pradier, T., Quinn, L., Racca, C., Randazzo, N., Riccobene, G., Sanchez-Losa, A., Saldana, M., Salvadori, I., Samtleben, D. F. E., Sanguineti, M., Sapienza, P., Schussler, F., Spurio, M., Stolarczyk, T., Taiuti, M., Tayalati, Y., Trovato, A., Turpin, D., Vallage, B., Van Elewyck, V., Versari, F., Vivolo, D., Wilms, J., Zaborov, D., Zornoza, J. D., Zuniga, J., André, M., Aubert, J.-J., Barrios-Martí, J., Bouwhuis, M.C., Brânzaş, H., Coelho, J.A.B., Díaz, A.F., Elsässer, D., Enzenhöfer, A., Grégoire, T., Heijboer, A.J., Hernández-Rey, J.J., Hößl, J., Hofestädt, J., James, C.W., Lefèvre, D., Martínez-Mora, J.A., Nuñez, A., Păvălaş, G.E., Sánchez-Losa, A., Saldaña, M., Samtleben, D.F.E., Schüssler, F., Stolarczyk, Th., Zornoza, J.D., Zúñiga, J., KM3NeT (IHEF, IoP, FNWI), IHEF (IoP, FNWI), Institut Pluridisciplinaire Hubert Curien (IPHC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), 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), Laboratoire de Physique Corpusculaire - Clermont-Ferrand (LPC), Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), 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), 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), Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Université Paris-Sud - Paris 11 (UP11), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Informatique et Systèmes (LIS), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Institut méditerranéen d'océanologie (MIO), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Aix Marseille Université (AMU)-Institut de Recherche pour le Développement (IRD), Département de Physique des Particules (ex SPP) (DPP), 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, Groupe de Recherche en Physique des Hautes Energies (GRPHE), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut Universitaire de Technologie de Colmar, ANTARES, Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-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)-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), 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), 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)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-IUT de Colmar, Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Institut Universitaire de Technologie de Colmar-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), Ministerio de Economía y Competitividad (España), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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 de Paris (UP), 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)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN), Albert, A, Andre, M, Anghinolfi, M, Anton, G, Ardid, M, Aubert, Jj, Aublin, J, Avgitas, T, Baret, B, Barrios-Marti, J, Basa, S, Belhorma, B, Bertin, V, Biagi, S, Bormuth, R, Boumaaza, J, Bourret, S, Bouwhuis, Mc, Branzas, H, Bruijn, R, Brunner, J, Busto, J, Capone, A, Caramete, L, Carr, J, Celli, S, Chabab, M, El Moursli, Rc, Chiarusi, T, Circella, M, Coelho, Jab, Coleiro, A, Colomer, M, Coniglione, R, Costantini, H, Coyle, P, Creusot, A, Diaz, Af, Deschamps, A, Distefano, C, Di Palma, I, Domi, A, Donzaud, C, Dornic, D, Drouhin, D, Eberl, T, El Bojaddaini, I, El Khayati, N, Elsasser, D, Enzenhofer, A, Ettahiri, A, Fassi, F, Felis, I, Fermani, P, Ferrara, G, Fusco, L, Gay, P, Glotin, H, Gregoire, T, Gracia-Ruiz, R, Graf, K, Hallmann, S, van Haren, H, Heijboer, Aj, Hello, Y, Hernandez-Rey, Jj, Hossl, J, Hofestadt, J, Illuminati, G, James, Cw, de Jong, M, Jongen, M, Kadler, M, Kalekin, O, Katz, U, Kouchner, A, Kreter, M, Kreykenbohm, I, Kulikovskiy, V, Lachaud, C, Lahmann, R, Lefevre, D, Leonora, E, Levi, G, Lotze, M, Loucatos, S, Marcelin, M, Margiotta, A, Marinelli, A, Martinez-Mora, Ja, Mele, R, Melis, K, Migliozzi, P, Moussa, A, Navas, S, Nezri, E, Nunez, A, Organokov, M, Pavalas, Ge, Pellegrino, C, Piattelli, P, Popa, V, Pradier, T, Quinn, L, Racca, C, Randazzo, N, Riccobene, G, Sanchez-Losa, A, Saldana, M, Salvadori, I, Samtleben, Dfe, Sanguineti, M, Sapienza, P, Schussler, F, Spurio, M, Stolarczyk, T, Taiuti, M, Tayalati, Y, Trovato, A, Turpin, D, Vallage, B, Van Elewyck, V, Versari, F, Vivolo, D, Wilms, J, Zaborov, D, Zornoza, Jd, Zuniga, J, Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-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), and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])
Subjects: Astrofísica, Acceleration of particles, acceleration of particles, neutrinos, astroparticle physics, radio continuum: transients, methods: data analysis, Hadron, transient [radio continuum], transients [Radio continuum], Astrophysics, power spectrum, 7. Clean energy, 01 natural sciences, neutrino: flux, particle: acceleration, neutrino, Raigs gamma, Gamma ray astronomy, Radiative transfer, data analysis [Methods], 010303 astronomy & astrophysics, acceleration of particle, Astroparticle physics, Methods: data analysis, Neutrinos, Radio continuum: transients, Physics, [PHYS]Physics [physics], High Energy Astrophysical Phenomena (astro-ph.HE), energy: high, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], astroparticle physic, Radio continuum: transient, Acceleration of particle, Particle acceleration, neutrino: detector, Neutrino detector, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, signature, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, cosmic radiation: energy, FOS: Physical sciences, Astroparticle physic, Astronomy and Astrophysics, Space and Planetary Science, neutrino: energy, 0103 physical sciences, Neutrins, data analysis. [methods], ANTARES, 010308 nuclear & particles physics, Spectral density, Astronomy and Astrophysic, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], FISICA APLICADA, neutrino: burst, High Energy Physics::Experiment, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Energy (signal processing), Methods: data analysi
Abstract: In the past decade, a new class of bright transient radio sources with millisecond duration has been discovered. The origin of these so-called Fast Radio Bursts (FRBs) is still a great mystery despite the growing observational efforts made by various multi-wavelength and multi-messenger facilities. So far, many models have been proposed to explain FRBs but neither the progenitors nor the radiative and the particle acceleration processes at work have been clearly identified. In this paper, the question whether some hadronic processes may occur in the vicinity of the FRB source is assessed. If so, FRBs may contribute to the high energy cosmic-ray and neutrino fluxes. A search for these hadronic signatures has been done using the ANTARES neutrino telescope. The analysis consists in looking for high-energy neutrinos, in the TeV-PeV regime, spatially and temporally coincident with the detected FRBs. Most of the FRBs discovered in the period 2013-2017 were in the field of view of the ANTARES detector, which is sensitive mostly to events originating from the Southern hemisphere. From this period, 12 FRBs have been selected and no coincident neutrino candidate was observed. Upper limits on the per burst neutrino fluence have been derived using a power law spectrum, $\rm{\frac{dN}{dE_\nu}\propto E_\nu^{-\gamma}}$, for the incoming neutrino flux, assuming spectral indexes $\gamma$ = 1.0, 2.0, 2.5. Finally, the neutrino energy has been constrained by computing the total energy radiated in neutrinos assuming different distances for the FRBs. Constraints on the neutrino fluence and on the energy released are derived from the associated null results., Comment: 16 pages, 5 figures, 2 tables
Published: 2019

37. MAGIC observations with bright Moon and their application to measuring the VHE gamma-ray spectral cut-off of the PeVatron candidate Cassiopeia A

Author: Moralejo Olaizola, Abelardo, Cortina Blanco, Juan, Fernandez, E., Guberman, Daniel Alberto, Universitat Autònoma de Barcelona. Departament de Física., Institut de Física d'Altes Energies., Moralejo Olaizola, Abelardo, Cortina Blanco, Juan, Fernandez, E., Guberman, Daniel Alberto, Universitat Autònoma de Barcelona. Departament de Física., and Institut de Física d'Altes Energies.
Published: 2018

38. Joint Constraints on Galactic Diffuse Neutrino Emission from the ANTARES and IceCube Neutrino Telescopes

Author: Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, Albert, A., André, Michel, Anghinolfi, Marco, Ardid Ramírez, Miguel, Aubert, J.-J., Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, Albert, A., André, Michel, Anghinolfi, Marco, Ardid Ramírez, Miguel, and Aubert, J.-J.
Abstract: The existence of diffuse Galactic neutrino production is expected from cosmic-ray interactions with Galactic gas and radiation fields. Thus, neutrinos are a unique messenger offering the opportunity to test the products of Galactic cosmic-ray interactions up to energies of hundreds of TeV. Here we present a search for this production using ten years of Astronomy with a Neutrino Telescope and Abyss environmental RESearch (ANTARES) track and shower data, as well as seven years of IceCube track data. The data are combined into a joint likelihood test for neutrino emission according to the KRAg model assuming a 5 PeV per nucleon Galactic cosmic-ray cutoff. No significant excess is found. As a consequence, the limits presented in this Letter start constraining the model parameter space for Galactic cosmic-ray production and transport, Postprint (published version)
Published: 2018

39. Indirect dark matter searches : MAGIC & CTA

Author: Rico Castro, Javier, Fernandez, E., Palacio Navarro, Joaquim, Universitat Autònoma de Barcelona. Departament de Física., Rico Castro, Javier, Fernandez, E., Palacio Navarro, Joaquim, and Universitat Autònoma de Barcelona. Departament de Física.
Abstract: Després de dècades d'observacions, és evident que les partíicules del model estàndard són insuficients per explicar el fort desequilibri gravitacional observat a diverses regions astronòmiques, de diferents escales cosmològiques, des de satèl·lits de la Via Làctia fins a cúmuls de galàxies. Si bé és veritat que algunes teories suggereixen a una modificació de les lleis gravitacionals actuals, l'existència d'una partícula (o un grup de partícules) nova, interaccionant de forma feble amb les partícules del model estàndard està considerada com l'opció més viable. Estimacions recents prediuen que aquest tipus de matèria fosca és 4 vegades més present que la matèria del model estàndard, modelant així la formació de les grans estructures de l'univers al llarg de la vida d'aquest. Un escenari general de la matèria fosca és el dels WIMPs, partícules genèriques massives, amb masses entre pocs GeVs i alguns TeV, interaccions de l'ordre de les interaccions dèbils del model estàndard, i o bé estables o amb temps de vida mitjana prou llargs. L'escenari WIMP ha estat llargament debatut, i té l'avantatja d'estar a l'abast dels instruments més potents construïts a la terra, proporcionant així possibles deteccions independents que podria validar el descobriment. En particular em centro en cerques indirectes de matèria fosca, on s'espera que WIMPs anihilats o decaient emetin rajos gamma amb energies detectables per telescopis IACT, com per exemple els telescopis MAGIC, actualment operant des de La Palma o la futura xarxa de telescopis CTA. El senyal esperat de rajos gamma d'aquesta matèria fosca pot ser moderadament extensa, comparada amb el camp de visió dels IACTs, cosa que afegeix certa complexitat a les cerques de matèria fosca realitzades per a aquests telescopis. En aquesta tesi, he contribuït a l'esforç realitzat per MAGIC en cerques indirectes de matèria fosca a diferents nivells d'analisis. He desenvolupat una eina per gestionar volums massius de dades que són típicament gen, Decades of observational evidences have been accumulated to show that Standard Model (SM) particles cannot totally explain the strong gravitational unbalance observed in several astronomical regions, at all cosmological scales, from that of Milky Way (MW) satellite galaxies, to that of Cluster of Galaxies (CGs). Although some theories argue for the modification of the gravitational laws, the existence of a new massive particle (or a set of them), interacting only weakly with SM particles, provides a preferred explanation. It is estimated that this form of Dark Matter (DM) roughly accounts for 4 times the amount of SM matter, therefore shaping the evolution of cosmic structures along the history of the Universe. A well-motivated general framework for DM is that of a Weakly Interacting Massive Particle (WIMP), generic massive particles with a mass range expected between few GeVs and few hundreds TeV, interaction strengths at the weak scale, and either stable or very long lived. The WIMP paradigm has been long debated, and has the advantage of being at reach by different of the top-class instruments of the current times, so that a putative discovery could be validated independently. We focus on the indirect search of DM, where annihilating or decaying WIMPs are expected to emit gamma rays at energies detectable by Imaginc Atmospheric Cherenkov Telescopes (IACTs), as the currently operating MAGIC telescopes or the future Cherenkov Telescope Array (CTA). The expected DM signal can be moderate extended when compared to IACTs Field of View (FoV), what challenges the performance of the \acrshort{dm} search of these instruments. In this thesis, I contribute to the MAGIC ongoing efforts on indirect DM searches at different analysis levels. A tool for handling the massive data products generated by current high energy experiments is developed. More over, a tailored Monte Carlo (MC) for moderate extended sources is proposed as an upgrade of the current general MC for extended s
Published: 2018

40. The 26.3-h orbit and multiwavelength properties of the 'redback' millisecond pulsar PSR J1306-40

Author: Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica, Linares Alegret, Manuel, Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica, and Linares Alegret, Manuel
Abstract: We present the discovery of the variable optical and X-ray counterparts to the radio millisecond pulsar (MSP) PSR J1306–40, recently discovered by Keane et al. We find that both the optical and X-ray fluxes are modulated with the same period, which allows us to measure for the first time the orbital period Porb = 1.097¿16[6] d. The optical properties are consistent with a main-sequence companion with spectral type G to mid K and, together with the X-ray luminosity (8.8¿×¿1031¿erg¿s-1 in the 0.5–10¿keV band, for a distance of 1.2¿kpc), confirm the redback classification of this pulsar. Our results establish the binary nature of PSR J1306–40, which has the longest Porb among all known compact binary MSPs in the Galactic disc. We briefly discuss these findings in the context of irradiation and intrabinary shock emission in compact binary MSPs., Postprint (published version)
Published: 2018

41. Joint Constraints on Galactic Diffuse Neutrino Emission from the ANTARES and IceCube Neutrino Telescopes

Author: Albert, A., André, M., Belhorma, B., Piattelli, P., Popa, V., Pradier, T., Quinn, L., Racca, C., Randazzo, N., Riccobene, G., Sánchez-Losa, A., Saldaña, M., Salvadori, I., Bertin, V., Samtleben, D. F. E., Sanguineti, M., Sapienza, P., Schüssler, F., Spurio, M., Stolarczyk, Th., Taiuti, M., Tayalati, Y., Trovato, A., Vallage, B., Biagi, S., Elewyck, V. Van, Versari, F., Vivolo, D., Wilms, J., Zaborov, D., Zornoza, J. D., Zúñiga, J., Aartsen, M. G., Ackermann, Markus, Adams, J., Bormuth, R., Aguilar, J. A., Ahlers, M., Ahrens, M., Samarai, I. Al, Altmann, D., Andeen, K., Anderson, T., Ansseau, I., Anton, G., Argüelles, C., Boumaaza, J., Auffenberg, J., Axani, S., Backes, P., Bagherpour, H., Bai, X., Barbano, A., Barron, J. P., Barwick, S. W., Baum, V., Bay, R., Bourret, S., Beatty, J. J., Tjus, J. Becker, Becker, K.-H., BenZvi, S., Berley, D., Bernardini, E., Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Bouwhuis, M. C., Blot, S., Bohm, C., Börner, M., Bos, F., Böser, S., Botner, O., Bourbeau, E., Bourbeau, J., Bradascio, F., Braun, J., Brânzaş, H., Brenzke, M., Bretz, H.-P., Bron, S., Brostean-Kaiser, J., Burgman, A., Busse, R. S., Carver, T., Cheung, E., Chirkin, D., Christov, A., Bruijn, R., Clark, K., Classen, L., Collin, G. H., Conrad, J. M., Coppin, P., Correa, P., Cowen, D. F., Cross, R., Dave, P., Day, M., Brunner, J., de André, J. P. A. M., Clercq, C. De, DeLaunay, J. J., Dembinski, H., Deoskar, K., Ridder, S. De, Desiati, P., Vries, K. D. de, Wasseige, G. de, With, M. de, Anghinolfi, M., Busto, J., DeYoung, T., Díaz-Vélez, J. C., di Lorenzo, V., Dujmovic, H., Dumm, J. P., Dunkman, M., Dvorak, E., Eberhardt, B., Ehrhardt, T., Eichmann, B., Capone, A., Eller, P., Evenson, P. A., Fahey, S., Fazely, A. R., Felde, J., Filimonov, K., Finley, C., Franckowiak, A., Friedman, E., Fritz, A., Caramete, L., Gaisser, T. K., Gallagher, J., Ganster, E., Gerhardt, L., Ghorbani, K., Giang, W., Glauch, T., Glüsenkamp, T., Goldschmidt, A., Gonzalez, J. G., Carr, J., Grant, D., Griffith, Z., Haack, C., Hallgren, A., Halve, L., Halzen, F., Hanson, K., Hebecker, D., Heereman, D., Helbing, K., Celli, S., Hellauer, R., Hickford, S., Hignight, J., Hill, G. C., Hoffman, K. D., Hoffmann, R., Hoinka, T., Hokanson-Fasig, B., Hoshina, K., Huang, F., Chabab, M., Huber, M., Hultqvist, K., Hünnefeld, M., Hussain, R., In, S., Iovine, N., Ishihara, A., Jacobi, Emanuel, Japaridze, G. S., Jeong, M., El Moursli, R. Cherkaoui, Jero, K., Jones, B. J. P., Kalaczynski, P., Kang, W., Kappes, A., Kappesser, D., Karg, T., Karle, A., Katz, U., Kauer, M., Chiarusi, T., Keivani, A., Kelley, J. L., Kheirandish, A., Kim, J., Kintscher, T., Kiryluk, J., Kittler, T., Klein, S. R., Koirala, R., Kolanoski, H., Circella, M., Köpke, L., Kopper, C., Kopper, S., Koschinsky, J. P., Koskinen, D. J., Kowalski, Marek, Krings, K., Kroll, M., Krückl, G., Kunwar, Samridha, Coelho, J. A. B., Kurahashi, N., Kyriacou, A., Labare, M., Lanfranchi, J. L., Larson, M. J., Lauber, F., Leonard, K., Leuermann, M., Liu, Q. R., Lohfink, E., Ardid, M., Coleiro, A., Mariscal, C. J. Lozano, Lu, L., Lünemann, J., Luszczak, W., Madsen, J., Maggi, G., Mahn, K. B. M., Makino, Y., Mancina, S., Maruyama, R., Colomer, M., Mase, K., Maunu, R., Meagher, K., Medici, M., Meier, M., Menne, T., Merino, G., Meures, T., Miarecki, S., Micallef, J., Coniglione, R., Momenté, G., Montaruli, T., Moore, R. W., Moulai, M., Nagai, R., Nahnhauer, R., Nakarmi, P., Naumann, U., Neer, G., Niederhausen, H., Costantini, H., Nowicki, S. C., Nygren, D. R., Pollmann, A. Obertacke, Olivas, A., O’Murchadha, A., O’Sullivan, E., Palczewski, T., Pandya, H., Pankova, D. V., Peiffer, P., Coyle, P., Pepper, J. A., de los Heros, C. Pérez, Pieloth, D., Pinat, E., Pizzuto, A., Plum, M., Price, P. B., Przybylski, G. T., Raab, C., Rameez, M., Creusot, A., Rauch, L., Rawlins, K., Rea, I. C., Reimann, R., Relethford, B., Resconi, E., Rhode, W., Richman, M., Robertson, S., Rongen, M., Díaz, A. F., Rott, C., Ruhe, T., Ryckbosch, D., Rysewyk, D., Safa, I., Herrera, S. E. Sanchez, Sandrock, A., Sandroos, J., Santander, M., Sarkar, S., Deschamps, A., Satalecka, K., Schaufel, M., Schlunder, P., Schmidt, T., Schneider, A., Schöneberg, S., Schumacher, L., Sclafani, S., Seckel, D., Distefano, C., Seunarine, S., Soedingrekso, J., Soldin, D., Song, M., Spiczak, G. M., Spiering, C., Stachurska, J., Stamatikos, M., Stanev, T., Stasik, Alexander, Palma, I. Di, Stein, Robert, Stettner, J., Steuer, A., Stezelberger, T., Stokstad, R. G., Stößl, A., Strotjohann, N. L., Stuttard, T., Sullivan, G. W., Sutherland, M., Aubert, J.-J., Domi, A., Taboada, I., Tenholt, F., Ter-Antonyan, S., Terliuk, A., Tilav, S., Toale, P. A., Tobin, M. N., Tönnis, C., Toscano, S., Tosi, D., Donzaud, C., Tselengidou, M., Tung, C. F., Turcati, A., Turley, C. F., Ty, B., Unger, E., Elorrieta, M. A. Unland, Usner, M., Vandenbroucke, J., Driessche, W. Van, Dornic, D., Eijk, D. van, Eijndhoven, N. van, Vanheule, S., Santen, J. van, Vraeghe, M., Walck, C., Wallace, A., Wallraff, M., Wandler, F. D., Wandkowsky, N., Drouhin, D., Watson, T. B., Waza, A., Weaver, C., Weiss, M. J., Wendt, C., Werthebach, J., Westerhoff, S., Whelan, B. J., Whitehorn, N., Wiebe, K., Eberl, T., Wiebusch, C. H., Wille, L., Williams, D. R., Wills, L., Wolf, M., Wood, J., Wood, T. R., Woolsey, E., Woschnagg, K., Wrede, G., Bojaddaini, I. El, Xu, D. L., Xu, X. W., Xu, Y., Yanez, J. P., Yodh, G., Yoshida, S., Yuan, T., Gaggero, D., Grasso, D., ANTARES Collaboration, Khayati, N. El, IceCube Collaboration, Elsässer, D., Enzenhöfer, A., Ettahiri, A., Aublin, J., Fassi, F., Felis, I., Fermani, P., Ferrara, G., Fusco, L., Gay, P., Glotin, H., Grégoire, T., Ruiz, R. Gracia, Graf, K., Avgitas, T., Hallmann, S., Haren, H. van, Heijboer, A. J., Hello, Y., Hernández-Rey, J. J., Hößl, J., Hofestädt, J., Illuminati, G., James, C. W., Jong, M. de, Baret, B., Jongen, M., Kadler, M., Kalekin, O., Khan-Chowdhury, N. R., Kouchner, A., Kreter, M., Kreykenbohm, I., Kulikovskiy, V., Lachaud, C., Barrios-Martí, J., Lahmann, R., Lefèvre, D., Leonora, E., Levi, G., Lotze, M., Loucatos, S., Marcelin, M., Margiotta, A., Marinelli, A., Martínez-Mora, J. A., Basa, S., Mele, R., Melis, K., Migliozzi, P., Moussa, A., Navas, S., Nezri, E., Nuñez, A., Organokov, M., Păvălaş, G. E., Pellegrino, C., Physics, Elementary Particle Physics, Vriendenkring VUB, Faculty of Sciences and Bioengineering Sciences, Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'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), Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA), Université Paris-Sud - Paris 11 (UP11), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Informatique et Systèmes (LIS), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Institut méditerranéen d'océanologie (MIO), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPP), 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, Groupe de Recherche en Physique des Hautes Energies (GRPHE), Institut Universitaire de Technologie de Colmar-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), ANTARES, IceCube, Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-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)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-IUT de Colmar, Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), Albert, A., Andre, M., Anghinolfi, M., Ardid, M., Aubert, J. -J., Aublin, J., Avgitas, T., Baret, B., Barrios-Marti, J., Basa, S., Belhorma, B., Bertin, V., Biagi, S., Bormuth, R., Boumaaza, J., Bourret, S., Bouwhuis, M. C., Branzas, H., Bruijn, R., Brunner, J., Busto, J., Capone, A., Caramete, L., Carr, J., Celli, S., Chabab, M., El Moursli, R. C., Chiarusi, T., Circella, M., Coelho, J. A. B., Coleiro, A., Colomer, M., Coniglione, R., Costantini, H., Coyle, P., Creusot, A., Diaz, A. F., Deschamps, A., Distefano, C., Palma, I. D., Domi, A., Donzaud, C., Dornic, D., Drouhin, D., Eberl, T., Bojaddaini, I. E., Khayati, N. E., Elsasser, D., Enzenhofer, A., Ettahiri, A., Fassi, F., Felis, I., Fermani, P., Ferrara, G., Fusco, L., Gay, P., Glotin, H., Gregoire, T., Ruiz, R. G., Graf, K., Hallmann, S., Haren, H. V., Heijboer, A. J., Hello, Y., Hernandez-Rey, J. J., Hossl, J., Hofestadt, J., Illuminati, G., James, C. W., Jong, M. D., Jongen, M., Kadler, M., Kalekin, O., Katz, U., Khan-Chowdhury, N. R., Kouchner, A., Kreter, M., Kreykenbohm, I., Kulikovskiy, V., Lachaud, C., Lahmann, R., Lefevre, D., Leonora, E., Levi, G., Lotze, M., Loucatos, S., Marcelin, M., Margiotta, A., Marinelli, A., Martinez-Mora, J. A., Mele, R., Melis, K., Migliozzi, P., Moussa, A., Navas, S., Nezri, E., Nunez, A., Organokov, M., Pavalas, G. E., Pellegrino, C., Piattelli, P., Popa, V., Pradier, T., Quinn, L., Racca, C., Randazzo, N., Riccobene, G., Sanchez-Losa, A., Saldana, M., Salvadori, I., Samtleben, D. F. E., Sanguineti, M., Sapienza, P., Schussler, F., Spurio, M., Stolarczyk, T., Taiuti, M., Tayalati, Y., Trovato, A., Vallage, B., Elewyck, V. V., Versari, F., Vivolo, D., Wilms, J., Zaborov, D., Zornoza, J. D., Zniga, J., Aartsen, M. G., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Samarai, I. A., Altmann, D., Andeen, K., Anderson, T., Ansseau, I., Anton, G., Arguelles, C., Auffenberg, J., Axani, S., Backes, P., Bagherpour, H., Bai, X., Barbano, A., Barron, J. P., Barwick, S. W., Baum, V., Bay, R., Beatty, J. J., Tjus, J. B., Becker, K. -H., Benzvi, S., Berley, D., Bernardini, E., Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Blot, S., Bohm, C., Borner, M., Bos, F., Boser, S., Botner, O., Bourbeau, E., Bourbeau, J., Bradascio, F., Braun, J., Brenzke, M., Bretz, H. -P., Bron, S., Brostean-Kaiser, J., Burgman, A., Busse, R. S., Carver, T., Cheung, E., Chirkin, D., Christov, A., Clark, K., Classen, L., Collin, G. H., Conrad, J. M., Coppin, P., Correa, P., Cowen, D. F., Cross, R., Dave, P., Day, M., De Andre, J. P. A. M., Clercq, C. D., Delaunay, J. J., Dembinski, H., Deoskar, K., Ridder, S. D., Desiati, P., Vries, K. D. D., Wasseige, G. D., With, M. D., Deyoung, T., Diaz-Velez, J. C., Di Lorenzo, V., Dujmovic, H., Dumm, J. P., Dunkman, M., Dvorak, E., Eberhardt, B., Ehrhardt, T., Eichmann, B., Eller, P., Evenson, P. A., Fahey, S., Fazely, A. R., Felde, J., Filimonov, K., Finley, C., Franckowiak, A., Friedman, E., Fritz, A., Gaisser, T. K., Gallagher, J., Ganster, E., Gerhardt, L., Ghorbani, K., Giang, W., Glauch, T., Glusenkamp, T., Goldschmidt, A., Gonzalez, J. G., Grant, D., Griffith, Z., Haack, C., Hallgren, A., Halve, L., Halzen, F., Hanson, K., Hebecker, D., Heereman, D., Helbing, K., Hellauer, R., Hickford, S., Hignight, J., Hill, G. C., Hoffman, K. D., Hoffmann, R., Hoinka, T., Hokanson-Fasig, B., Hoshina, K., Huang, F., Huber, M., Hultqvist, K., Hunnefeld, M., Hussain, R., In, S., Iovine, N., Ishihara, A., Jacobi, E., Japaridze, G. S., Jeong, M., Jero, K., Jones, B. J. P., Kalaczynski, P., Kang, W., Kappes, A., Kappesser, D., Karg, T., Karle, A., Kauer, M., Keivani, A., Kelley, J. L., Kheirandish, A., Kim, J., Kintscher, T., Kiryluk, J., Kittler, T., Klein, S. R., Koirala, R., Kolanoski, H., Kopke, L., Kopper, C., Kopper, S., Koschinsky, J. P., Koskinen, D. J., Kowalski, M., Krings, K., Kroll, M., Kruckl, G., Kunwar, S., Kurahashi, N., Kyriacou, A., Labare, M., Lanfranchi, J. L., Larson, M. J., Lauber, F., Leonard, K., Leuermann, M., Liu, Q. R., Lohfink, E., Mariscal, C. J. L., Lu, L., Lunemann, J., Luszczak, W., Madsen, J., Maggi, G., Mahn, K. B. M., Makino, Y., Mancina, S., Maruyama, R., Mase, K., Maunu, R., Meagher, K., Medici, M., Meier, M., Menne, T., Merino, G., Meures, T., Miarecki, S., Micallef, J., Momente, G., Montaruli, T., Moore, R. W., Moulai, M., Nagai, R., Nahnhauer, R., Nakarmi, P., Naumann, U., Neer, G., Niederhausen, H., Nowicki, S. C., Nygren, D. R., Pollmann, A. O., Olivas, A., O'Murchadha, A., O'Sullivan, E., Palczewski, T., Pandya, H., Pankova, D. V., Peiffer, P., Pepper, J. A., De Los Heros, C. P., Pieloth, D., Pinat, E., Pizzuto, A., Plum, M., Price, P. B., Przybylski, G. T., Raab, C., Rameez, M., Rauch, L., Rawlins, K., Rea, I. C., Reimann, R., Relethford, B., Resconi, E., Rhode, W., Richman, M., Robertson, S., Rongen, M., Rott, C., Ruhe, T., Ryckbosch, D., Rysewyk, D., Safa, I., Herrera, S. E. S., Sandrock, A., Sandroos, J., Santander, M., Sarkar, S., Satalecka, K., Schaufel, M., Schlunder, P., Schmidt, T., Schneider, A., Schoneberg, S., Schumacher, L., Sclafani, S., Seckel, D., Seunarine, S., Soedingrekso, J., Soldin, D., Song, M., Spiczak, G. M., Spiering, C., Stachurska, J., Stamatikos, M., Stanev, T., Stasik, A., Stein, R., Stettner, J., Steuer, A., Stezelberger, T., Stokstad, R. G., Stossl, A., Strotjohann, N. L., Stuttard, T., Sullivan, G. W., Sutherland, M., Taboada, I., Tenholt, F., Ter-Antonyan, S., Terliuk, A., Tilav, S., Toale, P. A., Tobin, M. N., Tonnis, C., Toscano, S., Tosi, D., Tselengidou, M., Tung, C. F., Turcati, A., Turley, C. F., Ty, B., Unger, E., Elorrieta, M. A. U., Usner, M., Vandenbroucke, J., Driessche, W. V., Eijk, D. V., Eijndhoven, N. V., Vanheule, S., Santen, J. V., Vraeghe, M., Walck, C., Wallace, A., Wallraff, M., Wandler, F. D., Wandkowsky, N., Watson, T. B., Waza, A., Weaver, C., Weiss, M. J., Wendt, C., Werthebach, J., Westerhoff, S., Whelan, B. J., Whitehorn, N., Wiebe, K., Wiebusch, C. H., Wille, L., Williams, D. R., Wills, L., Wolf, M., Wood, J., Wood, T. R., Woolsey, E., Woschnagg, K., Wrede, G., Xu, D. L., Xu, X. W., Xu, Y., Yanez, J. P., Yodh, G., Yoshida, S., Yuan, T., Gaggero, D., Grasso, D., Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Aix Marseille Université (AMU)-Institut de Recherche pour le Développement (IRD), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut Universitaire de Technologie de Colmar, Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, KM3NeT (IHEF, IoP, FNWI), GRAPPA (ITFA, IoP, FNWI), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-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 de Paris (UP), Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-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 de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN), Albert, A, Andre, M, Anghinolfi, M, Ardid, M, Aubert, Jj, Aublin, J, Avgitas, T, Baret, B, Barrios-Marti, J, Basa, S, Belhorma, B, Bertin, V, Biagi, S, Bormuth, R, Boumaaza, J, Bourret, S, Bouwhuis, Mc, Branzas, H, Bruijn, R, Brunner, J, Busto, J, Capone, A, Caramete, L, Carr, J, Celli, S, Chabab, M, El Moursli, Rc, Chiarusi, T, Circella, M, Coelho, Jab, Coleiro, A, Colomer, M, Coniglione, R, Costantini, H, Coyle, P, Creusot, A, Diaz, Af, Deschamps, A, Distefano, C, Di Palma, I, Domi, A, Donzaud, C, Dornic, D, Drouhin, D, Eberl, T, El Bojaddaini, I, El Khayati, N, Elsasser, D, Enzenhofer, A, Ettahiri, A, Fassi, F, Felis, I, Fermani, P, Ferrara, G, Fusco, L, Gay, P, Glotin, H, Gregoire, T, Ruiz, Rg, Graf, K, Hallmann, S, van Haren, H, Heijboer, Aj, Hello, Y, Hernandez-Rey, Jj, Hossl, J, Hofestadt, J, Illuminati, G, James, Cw, de Jong, M, Jongen, M, Kadler, M, Kalekin, O, Katz, U, Khan-Chowdhury, Nr, Kouchner, A, Kreter, M, Kreykenbohm, I, Kulikovskiy, V, Lachaud, C, Lahmann, R, Lefevre, D, Leonora, E, Levi, G, Lotze, M, Loucatos, S, Marcelin, M, Margiotta, A, Marinelli, A, Martinez-Mora, Ja, Mele, R, Melis, K, Migliozzi, P, Moussa, A, Navas, S, Nezri, E, Nunez, A, Organokov, M, Pavalas, Ge, Pellegrino, C, Piattelli, P, Popa, V, Pradier, T, Quinn, L, Racca, C, Randazzo, N, Riccobene, G, Sanchez-Losa, A, Saldana, M, Salvadori, I, Samtleben, Dfe, Sanguineti, M, Sapienza, P, Schussler, F, Spurio, M, Stolarczyk, T, Taiuti, M, Tayalati, Y, Trovato, A, Vallage, B, Van Elewyck, V, Versari, F, Vivolo, D, Wilms, J, Zaborov, D, Zornoza, Jd, Zuniga, J, Aartsen, Mg, Ackermann, M, Adams, J, Aguilar, Ja, Ahlers, M, Ahrens, M, Al Samarai, I, Altmann, D, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Arguelles, C, Auffenberg, J, Axani, S, Backes, P, Bagherpour, H, Bai, X, Barbano, A, Barron, Jp, Barwick, Sw, Baum, V, Bay, R, Beatty, Jj, Tjus, Jb, Becker, Kh, Benzvi, S, Berley, D, Bernardini, E, Besson, Dz, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bohm, C, Borner, M, Bos, F, Boser, S, Botner, O, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Brenzke, M, Bretz, Hp, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, R, Carver, T, Cheung, E, Chirkin, D, Christov, A, Clark, K, Classen, L, Collin, Gh, Conrad, Jm, Coppin, P, Correa, P, Cowen, Df, Cross, R, Dave, P, Day, M, de Andre, Jpam, De Clercq, C, Delaunay, Jj, Dembinski, H, Deoskar, K, De Ridder, S, Desiati, P, de Vries, Kd, de Wasseige, G, de With, M, Deyoung, T, Diaz-Velez, Jc, di Lorenzo, V, Dujmovic, H, Dumm, Jp, Dunkman, M, Dvorak, E, Eberhardt, B, Ehrhardt, T, Eichmann, B, Eller, P, Evenson, Pa, Fahey, S, Fazely, Ar, Felde, J, Filimonov, K, Finley, C, Franckowiak, A, Friedman, E, Fritz, A, Gaisser, Tk, Gallagher, J, Ganster, E, Gerhardt, L, Ghorbani, K, Giang, W, Glauch, T, Glusenkamp, T, Goldschmidt, A, Gonzalez, Jg, Grant, D, Griffith, Z, Haack, C, Hallgren, A, Halve, L, Halzen, F, Hanson, K, Hebecker, D, Heereman, D, Helbing, K, Hellauer, R, Hickford, S, Hignight, J, Hill, Gc, Hoffman, Kd, Hoffmann, R, Hoinka, T, Hokanson-Fasig, B, Hoshina, K, Huang, F, Huber, M, Hultqvist, K, Hunnefeld, M, Hussain, R, In, S, Iovine, N, Ishihara, A, Jacobi, E, Japaridze, G, Jeong, M, Jero, K, Jones, Bjp, Kalaczynski, P, Kang, W, Kappes, A, Kappesser, D, Karg, T, Karle, A, Kauer, M, Keivani, A, Kelley, Jl, Kheirandish, A, Kim, J, Kintscher, T, Kiryluk, J, Kittler, T, Klein, Sr, Koirala, R, Kolanoski, H, Kopke, L, Kopper, C, Kopper, S, Koschinsky, Jp, Koskinen, Dj, Kowalski, M, Krings, K, Kroll, M, Kruckl, G, Kunwar, S, Kurahashi, N, Kyriacou, A, Labare, M, Lanfranchi, Jl, Larson, Mj, Lauber, F, Leonard, K, Leuermann, M, Liu, Qr, Lohfink, E, Mariscal, Cjl, Lu, L, Lunemann, J, Luszczak, W, Madsen, J, Maggi, G, Mahn, Kbm, Makino, Y, Mancina, S, Maruyama, R, Mase, K, Maunu, R, Meagher, K, Medici, M, Meier, M, Menne, T, Merino, G, Meures, T, Miarecki, S, Micallef, J, Momente, G, Montaruli, T, Moore, Rw, Moulai, M, Nagai, R, Nahnhauer, R, Nakarmi, P, Naumann, U, Neer, G, Niederhausen, H, Nowicki, Sc, Nygren, Dr, Pollmann, Ao, Olivas, A, O'Murchadha, A, O'Sullivan, E, Palczewski, T, Pandya, H, Pankova, Dv, Peiffer, P, Pepper, Ja, de los Heros, Cp, Pieloth, D, Pinat, E, Pizzuto, A, Plum, M, Price, Pb, Przybylski, Gt, Raab, C, Rameez, M, Rauch, L, Rawlins, K, Rea, Ic, Reimann, R, Relethford, B, Resconi, E, Rhode, W, Richman, M, Robertson, S, Rongen, M, Rott, C, Ruhe, T, Ryckbosch, D, Rysewyk, D, Safa, I, Herrera, Se, Sandrock, A, Sandroos, J, Santander, M, Sarkar, S, Satalecka, K, Schaufel, M, Schlunder, P, Schmidt, T, Schneider, A, Schoneberg, S, Schumacher, L, Sclafani, S, Seckel, D, Seunarine, S, Soedingrekso, J, Soldin, D, Song, M, Spiczak, Gm, Spiering, C, Stachurska, J, Stamatikos, M, Stanev, T, Stasik, A, Stein, R, Stettner, J, Steuer, A, Stezelberger, T, Stokstad, Rg, Stossl, A, Strotjohann, Nl, Stuttard, T, Sullivan, Gw, Sutherland, M, Taboada, I, Tenholt, F, Ter-Antonyan, S, Terliuk, A, Tilav, S, Toale, Pa, Tobin, Mn, Tonnis, C, Toscano, S, Tosi, D, Tselengidou, M, Tung, Cf, Turcati, A, Turley, Cf, Ty, B, Unger, E, Elorrieta, Mau, Usner, M, Vandenbroucke, J, Van Driessche, W, van Eijk, D, van Eijndhoven, N, Vanheule, S, van Santen, J, Vraeghe, M, Walck, C, Wallace, A, Wallraff, M, Wandler, Fd, Wandkowsky, N, Watson, Tb, Waza, A, Weaver, C, Weiss, Mj, Wendt, C, Werthebach, J, Westerhoff, S, Whelan, Bj, Whitehorn, N, Wiebe, K, Wiebusch, Ch, Wille, L, Williams, Dr, Wills, L, Wolf, M, Wood, J, Wood, Tr, Woolsey, E, Woschnagg, K, Wrede, G, Xu, Dl, Xu, Xw, Xu, Y, Yanez, Jp, Yodh, G, Yoshida, S, Yuan, T, Gaggero, D, Grasso, D, André, M., Aubert, J.-J., Barrios-Martí, J., Bouwhuis, M.C., Brânzaş, H., El Moursli, R. Cherkaoui, Coelho, J.A.B., Díaz, A.F., Palma, I. Di, Bojaddaini, I. El, Khayati, N. El, Elsässer, D., Enzenhöfer, A., Grégoire, T., Ruiz, R. Gracia, Haren, H. Van, Heijboer, A.J., Hernández-Rey, J.J., Hößl, J., Hofestädt, J., James, C.W., Jong, M. De, Khan-Chowdhury, N.R., Lefèvre, D., Martínez-Mora, J.A., Nuñez, A., Pǎvǎlaş, G.E., Sánchez-Losa, A., Saldaña, M., Samtleben, D.F.E., Schüssler, F., Stolarczyk, Th., Elewyck, V. Van, Zornoza, J.D., Zñiga, J., Aartsen, M.G., Aguilar, J.A., Samarai, I. Al, Argüelles, C., Barron, J.P., Barwick, S.W., Beatty, J.J., Tjus, J. Becker, Becker, K.-H., Besson, D.Z., Börner, M., Böser, S., Bretz, H.-P., Busse, R.S., Collin, G.H., Conrad, J.M., Cowen, D.F., De André, J.P.A.M., Clercq, C. De, Delaunay, J.J., Ridder, S. De, Vries, K. D. De, Wasseige, G. De, With, M. De, Díaz-Vélez, J.C., Dumm, J.P., Evenson, P.A., Fazely, A.R., Gaisser, T.K., Glüsenkamp, T., Gonzalez, J.G., Hill, G.C., Hoffman, K.D., Hünnefeld, M., Japaridze, G.S., Jones, B.J.P., Kelley, J.L., Klein, S.R., Köpke, L., Koschinsky, J.P., Koskinen, D.J., Krückl, G., Lanfranchi, J.L., Larson, M.J., Liu, Q.R., Mariscal, C. J. Lozano, Lünemann, J., Mahn, K.B.M., Momenté, G., Moore, R.W., Nowicki, S.C., Nygren, D.R., Pollmann, A. Obertacke, Pankova, D.V., Pepper, J.A., De Los Heros, C. Pérez, Price, P.B., Przybylski, G.T., Rea, I.C., Herrera, S. E. Sanchez, Schöneberg, S., Spiczak, G.M., Stokstad, R.G., Stößl, A., Strotjohann, N.L., Sullivan, G.W., Toale, P.A., Tobin, M.N., Tönnis, C., Tung, C.F., Turley, C.F., Elorrieta, M. A. Unland, Driessche, W. Van, Eijk, D. Van, Eijndhoven, N. Van, Santen, J. Van, Wandler, F.D., Watson, T.B., Weiss, M.J., Whelan, B.J., Wiebusch, C.H., Williams, D.R., Wood, T.R., Xu, D.L., Xu, X.W., Yanez, J.P., and 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)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])
Subjects: Astrofísica, Astrophysics, cosmic radiation: interaction, 7. Clean energy, 01 natural sciences, neutrino: flux, IceCube, Diffusion, neutrino, KASCADE, Raigs gamma, cosmic rays, diffusion, Galaxy: disk, gamma rays: diffuse background, neutrinos, Astronomy and Astrophysics, Space and Planetary Science, gamma ray: flux, 010303 astronomy & astrophysics, cosmic ray, Physics, radio wave, density, photomultiplier, ELEMENTAL GROUPS, cosmic radiation: spectrum, nucleon, Astrophysics::Instrumentation and Methods for Astrophysics, Model parameter, Physique [physics]/Astrophysique [astro-ph], astroparticle physics, cosmic radiation: galaxy, neutrino: flavor, Diffuse background, Neutrino, Nucleon, numerical calculations: Monte Carlo, Disk [Galaxy], CREAM, Astrophysics::High Energy Astrophysical Phenomena, energy spectrum, elementary particles, Joint likelihood, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Radiation, GLAST, neutrino: production, diffuse background [gamma rays], gas, 0103 physical sciences, ENERGY-SPECTRA, Neutrins, Neutrinos, Cosmic rays, Astrophysics::Galaxy Astrophysics, cosmic radiation: production, ANTARES, 010308 nuclear & particles physics, Gamma rays, showers, Astronomy and Astrophysic, radiation mechanisms: non-thermal, radiation: Cherenkov, sensitivity, tracks, Neutrino astrophysics, messenger, Physics and Astronomy, 13. Climate action, Joint constraints, FISICA APLICADA, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], ddc:520, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: © 2018. The American Astronomical Society. All rights reserved. The existence of diffuse Galactic neutrino production is expected from cosmic-ray interactions with Galactic gas and radiation fields. Thus, neutrinos are a unique messenger offering the opportunity to test the products of Galactic cosmic-ray interactions up to energies of hundreds of TeV. Here we present a search for this production using ten years of Astronomy with a Neutrino Telescope and Abyss environmental RESearch (ANTARES) track and shower data, as well as seven years of IceCube track data. The data are combined into a joint likelihood test for neutrino emission according to the KRAg model assuming a 5 PeV per nucleon Galactic cosmic-ray cutoff. No significant excess is found. As a consequence, the limits presented in this Letter start constraining the model parameter space for Galactic cosmic-ray production and transport.
Published: 2018

42. MAGIC observations with bright Moon and their application to measuring the VHE gamma-ray spectral cut-off of the PeVatron candidate Cassiopeia A

Author: Guberman, Daniel Alberto, Moralejo Olaizola, Abelardo, Cortina Blanco, Juan, Fernandez, E. (Fernández Sánchez, Enrique), and Universitat Autònoma de Barcelona. Departament de Física
Subjects: Raigs gamma, Ciències Experimentals, Radiació Cherenkov, Gamma rays, Cherenkov radiation, Rayos cósmicos, Radiación Cherenkov, Rayos gamma, Cosmic rays, Raigs cosmics
Abstract: Los rayos cósmicos son núcleos atómicos que constantemente bombardean la Tierra. Está largamente aceptado que estos núcleos con energías de hasta ~3 PeV son de origen Galáctico. Pero aún no se sabe dónde en la Galaxia ni cómo son acelerados. Durante muchos años la hipótesis más popular ha sido que son acelerados en remanentes de supernova. En esta tesis presento los detalles de una serie de observaciones de la joven remanente de supernova Cassiopeia A, uno de los candidatos más prometedores a ser un Pevatrón, un sistema capaz de acelerar rayos cósmicos hasta energías de PeV. Las observaciones fueron realizadas con los telescopios MAGIC, que observan rayos gamma de muy alta energía (VHE, E > 50 GeV), entre Diciembre de 2014 y Octubre de 2016, adquiriendo 191 horas de datos buena calidad. Acumular una gran cantidad de horas de observación era indispensable para obtener una medida precisa del espectro y fue posible gracias a la posibilidad de extender el tiempo activo de MAGIC operando los telescopios bajo una luminosidad lunar intensa. Trabajé en la optimización de las observaciones con Luna en MAGIC, tanto en el momento de operar los telescopios como en la etapa del análisis de los datos. Abordo los detalles de este desarrollo y evaluó su rendimiento. Con más del 70 % de las horas obtenidas con la Luna presente en el cielo, he podido obtener el espectro más preciso hasta ahora de Cassiopeia A en VHE. Por primera vez se encuentra evidencia de un corte a E = 3,5 (+1,6\—1,0) stat (+0,8\−0,9) sys TeV en el espectro. El modelado de dicho espectro sugiere que la mayoría de los rayos gamma emitidos pueden ser atribuidos a una población de protones de muy alta energía con un índice espectral de ~2.2 y un corte a ~10 TeV. Esto implica que, asumiendo que no hay una difusión significativa d elos rayos cósmicos en el entorno de la supernova, Cassiopeia A no puede ser un PeVatrón en este momento. Cosmic rays are atomic nuclei that are constantly bombarding the Earth. It is widely accepted that these nuclei with energies up to ~3 PeV are of Galactic origin. But the question about where in the Galaxy and how they are accelerated still remains unanswered. For several years the most popular hypothesis has been that they are accelerated in supernova remnants. In this thesis I present the details of a deep observation campaign on the young supernova remnant Cassiopeia A, one of the most promising candidates to be a PeVatron, a system capable of accelerating cosmic rays up to PeV energies. The observations were performed with the MAGIC telescopes, that observe very high energy (VHE, E > 50 GeV) gamma rays, between December 2014 and October 2016, acquiring 191 hours of good-quality data. Accumulating a large amount of observation hours was indispensable to obtain a precise measurement of the spectrum and it was possible thanks to the possibility of extending the MAGIC duty cycle by operating the telescopes under bright moonlight. I worked in the optimization of moonlight observations with MAGIC, both during the operation of the telescopes and at the data analysis stage. I discuss the details of these developments and the resulting performance. With more than 70% of the data obtained under moonlight, I was able to obtain the most precise spectrum of Cassiopeia A to date at VHE. The obtained spectrum shows for the rst time 4:9 evidence of a cut-o at E = 3,5 (+1,6\—1,0) stat (+0,8\−0,9) sys TeV. The modelling of the spectrum suggests that the bulk of the gamma-rays emitted can be attributed to a population of high-energy protons with spectral index ~2.2 and energy cuto at ~10 TeV. This implies that, assuming there is no signicant cosmic-ray diusion, Cassiopeia A cannot be a PeVatron at its present age.
Published: 2018

43. Detection of persistent VHE gamma-ray emission from PKS 1510–089 by the MAGIC telescopes during low states between 2012 and 2017

Author: M. I. Martínez, P. Bangale, Sabrina Einecke, Jae-Young Kim, M. Makariev, Aaron Dominguez, Alicia Fattorini, G. Pedaletti, Ivica Puljak, Stefano Covino, B. De Lotto, Pierre Colin, J. Kushida, Jose Luis Contreras, Walter Max-Moerbeck, J. Becerra González, A. Arbet Engels, A. De Angelis, Vitaly Neustroev, M. Peresano, Chiara Righi, Juan Abel Barrio, D. Elsaesser, J. Palacio, Satoshi Masuda, J. E. Ward, Juan Cortina, Takashi Saito, Wrijupan Bhattacharyya, P. Temnikov, Sidika Merve Colak, Wolfgang Rhode, Giovanni Ceribella, I. Agudo, José L. Gómez, V. A. Acciari, Antonio Stamerra, D. Hadasch, D. Fidalgo, Camilla Maggio, Abelardo Moralejo, A. López-Oramas, P. Munar-Adrover, E. Moretti, Daniela Dorner, Pablo Peñil, Alexander Hahn, Dominik Baack, Gaia Vanzo, G. Maneva, E. Do Souto Espiñera, Joni Tammi, Adrian Biland, Elina Lindfors, Jürgen Besenrieder, C. M. Raiteri, Louis Antonelli, Sol N. Molina, Daniel Mazin, Ievgen Vovk, A. Berti, Francesco Dazzi, A. Fernández-Barral, K. Nishijima, Manuel Delfino, M. Gaug, R. J. García López, Nikola Godinovic, D. Dominis Prester, J. Rico, V. Ramakrishnan, Francesco Longo, Pratik Majumdar, D. Zarić, M. V. Fonseca, J. Herrera, T. Schweizer, Antonio Fuentes, Sebastian Kiehlmann, Marc Ribó, Ana Babić, A. Somero, Koji Noda, L. Maraschi, E. Prandini, Elisa Bernardini, P. Giammaria, V. Fallah Ramazani, John Hoang, Massimo Persic, Stefano Ansoldi, S. Paiano, Efthalia Traianou, Riccardo Paoletti, Tomislav Terzić, Ciro Bigongiari, Clemens Thum, B. Banerjee, P. G. Prada Moroni, Hidetoshi Kubo, C. Arcaro, J. van Scherpenberg, Karl Mannheim, I. Snidaric, Oscar Blanch, D. Kuveždić, Razmik Mirzoyan, U. Barres de Almeida, F. Leone, Carolina Casadio, Kari Nilsson, Damir Lelas, Anne Lähteenmäki, Masahiro Teshima, Stefan Cikota, M. Strzys, M. Will, Markus Garczarczyk, Dorota Sobczyńska, D. Ninci, M. Vazquez Acosta, Angela Sandrinelli, Cosimo Nigro, M. Nievas Rosillo, G. Ferrara, M. Minev, Victoria Moreno, G. Bonnoli, Kazuma Ishio, Yuki Iwamura, Susumu Inoue, Tarek M. Hassan, W. Bednarek, Fabrizio Tavecchio, Dario Hrupec, Luca Foffano, Ll. Font, L. Nogués, M. A. Lopez, Rodolfo Carosi, Mosè Mariotti, J. M. Paredes, J. R. Garcia, V. D'Elia, Saverio Lombardi, A. Rugliancich, Marina Manganaro, Ioannis Myserlis, D. Galindo, Merja Tornikoski, E. Molina, E. Colombo, Konstancja Satalecka, Michele Doro, Lab Saha, A. Niedzwiecki, David Paneque, D. Guberman, Jordi Delgado, F. Di Pierro, Talvikki Hovatta, P. Da Vela, Julian Sitarek, C. Fruck, N. Torres-Albà, Stefano Gallozzi, Jose Miguel Miranda, Alessandra Lamastra, T. Surić, Shimpei Tsujimoto, Acciari, V. A., Ansoldi, S., Antonelli, L. A., Arbet Engels, A., Arcaro, C., Baack, D., Babić, A., Banerjee, B., Bangale, P., Barres De Almeida, U., Barrio, J. A., Bednarek, W., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Carosi, R., Ceribella, G., Cikota, S., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., DI Pierro, F., Do Souto Espiñera, E., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Fallah Ramazani, V., Fattorini, A., Fernández-Barral, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., Gallozzi, S., García López, R. J., Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Herrera, J., Hoang, J., Hrupec, D., Inoue, S., Ishio, K., Iwamura, Y., Kubo, H., Kushida, J., Kuveždić, D., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López, M., López-Oramas, A., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Masuda, S., Mazin, D., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Moreno, V., Moretti, E., Munar-Adrover, P., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peñil, P., Peresano, M., Persic, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Garcia, J. R., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Somero, A., Stamerra, A., Strzys, M., Surić, T., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Tsujimoto, S., Van Scherpenberg, J., Vanzo, G., Vazquez Acosta, M., Vovk, I., Ward, J. E., Will, M., Zarić, D., Becerra González, J., Raiteri, C. M., Sandrinelli, A., Hovatta, T., Kiehlmann, S., Max-Moerbeck, W., Tornikoski, M., Lähteenmäki, A., Tammi, J., Ramakrishnan, V., Thum, C., Agudo, I., Molina, S. N., Gómez, J. L., Fuentes, A., Casadio, C., Traianou, E., Myserlis, I., Kim, J. -Y., Metsähovi Radio Observatory, Department of Electronics and Nanoengineering, Aalto-yliopisto, Aalto University, Universitat de Barcelona, Federal Ministry of Education and Research (Germany), Max Planck Society, Ministerio de Economía y Competitividad (España), Swiss National Science Foundation, and Junta de Andalucía
Subjects: galaxies [Gamma rays], Astrophysics, 01 natural sciences, 7. Clean energy, jet [Galaxies], law.invention, Raigs gamma, law, Jets (Astrofísica), Broadband, 010303 astronomy & astrophysics, Physics, galaxies: active, galaxies: jets, gamma rays: galaxies, quasars: individual: PKS 1510-089, galaxie [Gamma rays], Gamma ray, Galaxies: active, 3. Good health, Magnetic field, Gamma rays: galaxies, Spectral energy distribution, Física nuclear, Galaxies: jets, Quasars: individual: PKS 1510-089, Astronomy and Astrophysics, Space and Planetary Science, Flare, Spectral shape analysis, active [Galaxies], astro-ph.GA, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 0103 physical sciences, individual: PKS 1510-089 [Quasars], Quasars, Quàsars, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Gamma rays, Quasar, Plasma, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Astrophysical jets, Astrophysics of Galaxies (astro-ph.GA), Galàxies actives, Active galaxies, ddc:520, jets [Galaxies]
Abstract: PKS 1510-089 is a flat spectrum radio quasar strongly variable in the optical and GeV range. To date, very high-energy (VHE, > 100 GeV) emission has been observed from this source either during long high states of optical and GeV activity or during short flares. Aims. We search for low-state VHE gamma-ray emission from PKS 1510-089. We characterize and model the source in a broadband context, which would provide a baseline over which high states and flares could be better understood. Methods. PKS 1510-089 has been monitored by the MAGIC telescopes since 2012. We use daily binned Fermi-LAT flux measurements of PKS 1510-089 to characterize the GeV emission and select the observation periods of MAGIC during low state of activity. For the selected times we compute the average radio, IR, optical, UV, X-ray, and gamma-ray emission to construct a low-state spectral energy distribution of the source. The broadband emission is modeled within an external Compton scenario with a stationary emission region through which plasma and magnetic fields are flowing. We also perform the emission-model-independent calculations of the maximum absorption in the broad line region (BLR) using two different models. Results. The MAGIC telescopes collected 75 hr of data during times when the Fermi-LAT flux measured above 1 GeV was below 3? × 10 -8 ? cm -2 ? s -1 , which is the threshold adopted for the definition of a low gamma-ray activity state. The data show a strongly significant (9.5¿) VHE gamma-ray emission at the level of (4.27 ± 0.61 stat ) × 10 -12 ? cm -2 ? s -1 above 150 GeV, a factor of 80 lower than the highest flare observed so far from this object. Despite the lower flux, the spectral shape is consistent with earlier detections in the VHE band. The broadband emission is compatible with the external Compton scenario assuming a large emission region located beyond the BLR. For the first time the gamma-ray data allow us to place a limit on the location of the emission region during a low gamma-ray state of a FSRQ. For the used model of the BLR, the 95% confidence level on the location of the emission region allows us to place it at a distance > 74% of the outer radius of the BLR. © ESO 2018., The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, CSD2009-00064), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Spanish Centro de Exce-lencia “Severo Ochoa” SEV-2012-0234 and SEV-2015-0548, and Unidad de Excelencia “María de Maeztu” MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382, and by the Brazilian MCTIC, CNPq and FAPERJ. IA acknowledges support from a Ramón y Cajal grant of the Ministerio de Economía, Industria, y Competitividad (MINECO) of Spain. Acquisition and reduction of the POLAMI and MAPCAT data was supported in part by MINECO through grants AYA2010-14844, AYA2013-40825-P, and AYA2016-80889-P, and by the Regional Government of Andalucía through grant P09-FQM-4784.
Published: 2018

44. Study of the extreme gamma-ray emission from Supernova Remnants and the Crab Pulsar

Author: Galindo Fernández, Daniel, Paredes i Poy, Josep Maria, Zanin, Roberta, Manrique Oliva, Alberto, and Universitat de Barcelona. Departament de Física Quàntica i Astrofísica
Subjects: Astrofísica, Supernovas, Pulsares, Supernoves, Astrophysics::High Energy Astrophysical Phenomena, Raigs còsmics, Gamma rays, Astrophysics::Cosmology and Extragalactic Astrophysics, Rayos gamma, Astrophysics, Ciències Experimentals i Matemàtiques, Púlsars, Raigs gamma, Supernovae, Rayos cósmicos, Cosmic rays, Astrophysics::Galaxy Astrophysics, Pulsars
Abstract: [eng] In our Galaxy, supernova remnants and pulsars are the two most numerous populations of non-thermal objects. The goal of this thesis is to study the extreme gamma-ray emission from these two astrophysical objects with Fermi -LAT and MAGIC. In particular, supernova remnants Cassiopeia A and SNR G24.7+0.6 and the Crab pulsar. Cassiopeia A, one of the historical supernova remnants and the prime candidate of its class to be a PeVatron accelerator, has been discarded as so since we provided the first measurement of a turn-off in the gamma-ray spectrum at 3 TeV, implying the emission observed is produced by the decay of neutral pions, produced in proton- proton interactions of a parent population of accelerated protons with an energy cut-off at about 10TeV. Such a maximum energy of accelerated cosmic rays in Cassiopeia A falls short to explain the high energy end ( PeV) of the Galactic cosmic ray spectrum. Considering that Cassiopeia A was the main PeVatron candidate, the results obtained in this work challenge the existence of supernova remnants as galactic Pevatrons and therefore the popular conviction that supernova remnants are the main source of Galactic cosmic ray up to the knee. In the case of SNR G24.7+0.6, the remnant is evolving in a dense medium and might be interacting with the CO-rich surrounding. The observations performed allowed us to detect for the first time the counterpart of the radio emission, MAGIC J1835–069, from 60MeV up to 5TeV. This very high energy emission results from proton-proton interactions between the runaway protons from the supernova remnant and a nearby molecular cloud. These observations of the field of view of SNR G24.7+0.6, also resulted in the detection of another new source, MAGIC J1837–073, that is likely to be associated with a stellar cluster as suggested by its localization in a region rich in molecular content and crowded of sources. The total energy obtained in accelerated protons can be explained assuming a quasi-continuous injection of cosmic rays during the cluster lifetime. The second part of this thesis is focused on the study and understanding of the Crab pulsar, the young and most energetic pulsar in our galaxy. Observations carried out with MAGIC resulted in the first ever detection of very energetic pulsed emission from a pulsar, reaching up to about 1.5 TeV. Moreover, the light curve of the Crab above 400 GeV shows two peaks synchronized with those measured at lower energies. Such extremely energetic pulsed emission has to be produced by electrons with very high Lorentz factor scattering low energy photons in the vicinity of the light cylinder, either inside or outside of it. Currently, none of the postulated models is yet capable of reproducing at the same time the light curve and the spectral shape for both peaks above 400 GeV., [spa] Esta tesis tiene como objetivo el estudio de la emisión extrema de rayos gamma proveniente de remanentes de supernova y el pulsar del Cangrejo. Dos remanentes de supernova han sido observados tanto con Fermi, como con MAGIC; Cassiopeia A y SNR G24.7+0.6. Cassiopeia A, el principal candidato de su clase a revelarse como PeVatrón, ha sido descartado como tal, al haberse detectado un corte en el espectro de rayos gamma en torno a 3 TeV, lo cual implica que, la emisión observada es producida por el de- caimiento de piones neutros, originados en colisiones protón-protón por una población de protones que presenta un corte exponencial en su espectro en torno a una energía de 10 TeV. Esta energía máxima a la que son acelerados estos rayos cósmicos pone en serias dudas la existencia de remanentes de supernova que se comporten como PeVa- trones, y por tanto, la teoría de que éstos son la fuente principal de rayos cósmicos galácticos. En el caso de SNR G24.7+0.6, con las observaciones llevadas a cabo, hemos conseguido detectar por primera vez la contrapartida de la emisión radio a energías desde 60 MeV hasta 5 TeV, MAGIC J1835–069, producida por protones que escapan del remanente de supernova y que interaccionan con una nube molecular cercana. En estas mismas observaciones, hemos podido detectar otra fuente nueva, MAGIC J1837–073, la cual está asociada, muy probablemente, con un cumulo estelar tal y como sugiere su lo- calización. Su emisión puede ser explicada asumiendo una inyección casi continua de rayos cósmicos durante la totalidad de la vida estimada del cumulo estelar. Por otra parte, el estudio del púlsar del Cangrejo, llevado a cabo con MAGIC ha re- sultado en el descubrimiento de emisión pulsada hasta 1.5 TeV, refutando cualquiera de los modelos presentados hasta el momento. Además, la curva de luz que carac- teriza la emisión proveniente del púlsar por encima de 400 GeV, presenta dos picos sincronizados en fase con los picos hallados a energías más bajas. Esta emisión, ex- tremadamente energética, únicamente puede ser producida por electrones acelerados hasta factores de Lorentz muy altos en regiones cercanas al cilindro de luz, ya sea en su interior o en su exterior, y que posteriormente colisionan y transfieren su energía a fotones térmicos
Published: 2018

45. A hydrodynamics-informed, radiation model for HESS J0632 + 057 from radio to gamma-rays

Author: Valentí Bosch-Ramon and Maxim V. Barkov
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Binary number, FOS: Physical sciences, Astrophysics, 01 natural sciences, Raigs gamma, Pulsar, 0103 physical sciences, X-rays, Binary system, 010303 astronomy & astrophysics, Estels binaris de raigs X, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Radiation model, Advection, Gamma rays, Gamma ray, Astronomy and Astrophysics, Wavelength, X-ray binaries, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Raigs X, Astrophysics - High Energy Astrophysical Phenomena, Phenomenology (particle physics)
Abstract: Relativistic hydrodynamical simulations of the eccentric gamma-ray binary HESS J0632$+$057, show that the energy of a putative pulsar wind should accumulate in the binary surroundings between periastron and apastron, being released by fast advection close to apastron. To assess whether this could lead to a maximum of the non-thermal emission before apastron, we derive simple prescriptions for the non-thermal energy content, the radiation efficiency, and the impact of energy losses on non-thermal particles, in the simulated hydrodynamical flow. These prescriptions are used to estimate the non-thermal emission in radio, X-rays, GeV, and TeV, from the shocked pulsar wind in a binary system simulated using a simplified 3-dimensional scheme for several orbital cycles. Lightcurves at different wavelengths are derived, together with synthetic radio images for different orbital phases. The dominant peak in the computed lightcurves is broad and appears close to, but before, apastron. This peak is followed by a quasi-plateau shape, and a minor peak only in gamma rays right after periastron. The radio maps show ejection of radio blobs before apastron in the periastron-apastron direction. The results show that a scenario with a highly eccentric high-mass binary hosting a young pulsar can explain the general phenomenology of HESS J0632$+$057: despite its simplicity, the adopted approach yields predictions that are robust at a semi-quantitative level and consistent with multiwavelength observations., 7 pages, 5 figures, submitted to MNRAS
Published: 2018

46. Periastron Observations of TeV Gamma-Ray Emission from a Binary System with a 50-year Period

Author: The VERITAS Collaboration, Abeysekara, A. U., Benbow, W., Bird, R., Brill, A., Brose, R., Buckley, J. H., Chromey, A. J., Daniel, M. K., Falcone, A., Finley, J. P., Fortson, L., Furniss, A., Gent, A., Gillanders, G. H., Hanna, D., Hassan, T., Hervet, O., Holder, J., Hughes, G., Humensky, T. B., Kaaret, P., Kar, P., Kertzman, M., Kieda, D., Krause, M., Krennrich, F., Kumar, S., Lang, M. J., Lin, T. T. Y., Maier, G., Moriarty, P., Mukherjee, R., O'Brien, S., Ong, R. A., Otte, A. N., Park, N., Petrashyk, A., Pohl, M., Pueschel, E., Quinn, J., Ragan, K., Richards, G. T., Roache, E., Sadeh, I., Santander, M., Schlenstedt, S., Sembroski, G. H., Sushch, I., Tyler, J., Vassiliev, V. V., Wakely, S. P., Weinstein, A., Wells, R. M., Wilcox, P., Wilhelm, A., Williams, D. A., Williamson, T. J, Zitzer, B., Collaboration, MAGIC, Acciari, V. A., Ansoldi, S., Antonelli, L. A., Engels, A. Arbet, Baack, D., Babi��, A., Banerjee, B., de Almeida, U. Barres, Barrio, J. A., Gonz��lez, J. Becerra, Bednarek, W., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Busetto, G., Carosi, R., Ceribella, G., Cikota, S., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Di Pierro, F., Espi��era, E. Do Souto, Dom��nguez, A., Prester, D. Dominis, Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Ramazani, V. Fallah, Fattorini, A., Fern��ndez-Barral, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., Gallozzi, S., L��pez, R. J. Garc��a, Garczarczyk, M., Gasparyan, S., Gaug, M., Giammaria, P., Godinovi��, N., Guberman, D., Hadasch, D., Hahn, A., Herrera, J., Hoang, J., Hrupec, D., Inoue, S., Ishio, K., Iwamura, Y., Kubo, H., Kushida, J., Kuve��di��, D., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., L��pez, M., L��pez-Oramas, A., Fraga, B. Machado de Oliveira, Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Mart��nez, M., Masuda, S., Mazin, D., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Moreno, V., Moretti, E., Munar-Adrover, P., Neustroev, V., Niedzwiecki, A., Rosillo, M. Nievas, Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogu��s, L., N��the, M., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Pe��il, P., Peresano, M., Persic, M., Moroni, P. G. Prada, Prandini, E., Puljak, I., Garcia, J. R., Rhode, W., Rib��, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., ��nidari��, I., Sobczynska, D., Somero, A., Stamerra, A., Strzys, M., Suri��, T., Tavecchio, F., Temnikov, P., Terzi��, T., Teshima, M., Torres-Alb��, N., Tsujimoto, S., van Scherpenberg, J., Vanzo, G., Acosta, M. Vazquez, Vovk, I., Will, M., Zari��, D., Abeysekara, A. U., Benbow, W., Bird, R., Brill, A., Brose, R., Buckley, J. H., Chromey, A. J., Daniel, M. K., Falcone, A., Finley, J. P., Fortson, L., Furniss, A., Gent, A., Gillanders, G. H., Hanna, D., Hassan, T., Hervet, O., Holder, J., Hughes, G., Humensky, T. B., Kaaret, P., Kar, P., Kertzman, M., Kieda, D., Krause, M., Krennrich, F., Kumar, S., Lang, M. J., Lin, T. T. Y., Maier, G., Moriarty, P., Mukherjee, R., O'Brien, S., Ong, R. A., Otte, A. N., Park, N., Petrashyk, A., Pohl, M., Pueschel, E., Quinn, J., Ragan, K., Richards, G. T., Roache, E., Sadeh, I., Santander, M., Schlenstedt, S., Sembroski, G. H., Sushch, I., Tyler, J., Vassiliev, V. V., Wakely, S. P., Weinstein, A., Wells, R. M., Wilcox, P., Wilhelm, A., Williams, D. A., Williamson, T. J., Zitzer, B., Acciari, V. A., Ansoldi, S., Antonelli, L. A., Engels, A. Arbet, Baack, D., Babić, A., Banerjee, B., De Almeida, U. Barre, Barrio, J. A., González, J. Becerra, Bednarek, W., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Busetto, G., Carosi, R., Ceribella, G., Cikota, S., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D'Elia, V., Vela, P. Da, Dazzi, F., Angelis, A. De, Lotto, B. De, Delfino, M., Delgado, J., Pierro, F. Di, Souto Espinera, E. Do, Dominguez, A., Prester, D. Domini, Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Ramazani, V. Fallah, Fattorini, A., Fernández-Barral, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., Gallozzi, S., López, R. J. Garcia, Garczarczyk, M., Gasparyan, S., Gaug, M., Giammaria, P., Godinović, N., Guberman, D., Hadasch, D., Hahn, A., Herrera, J., Hoang, J., Hrupec, D., Inoue, S., Ishio, K., Iwamura, Y., Kubo, H., Kushida, J., Kuveždić, D., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López, M., López-Oramas, A., De Oliveira Fraga, B. Machado, Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martinez, M., Masuda, S., Mazin, D., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Moreno, V., Moretti, E., Munar-Adrover, P., Neustroev, V., Niedzwiecki, A., Rosillo, M. Nieva, Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Nöthe, M., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Penil, P., Peresano, M., Persic, M., Moroni, P. G. Prada, Prandini, E., Puljak, I., Garcia, J. R., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Somero, A., Stamerra, A., Strzys, M., Surić, T., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Alba, N., Tsujimoto, S., Scherpenberg, J. Van, Vanzo, G., Acosta, M. Vazquez, Vovk, I., Will, M., Zarić, D., and Universitat de Barcelona
Subjects: gamma rays: general, pulsars: individual (PSR J2032+4127, VER J2032+414, MAGIC J2032 +4127), stars: individual (MT91 213), X-rays: binaries, Astronomy and Astrophysics, Space and Planetary Science, MAGIC J2032 +4127), Astrophysics, 01 natural sciences, law.invention, Raigs gamma, Observatory, law, Astrophysics::Solar and Stellar Astrophysics, MAGIC (telescope), 010303 astronomy & astrophysics, astro-ph.HE, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, binarie [X-rays], Púlsars, Física nuclear, Astrophysics - High Energy Astrophysical Phenomena, individual (MT91 213) [stars], Astrophysics and Astronomy, Be star, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Compact star, Telescope, Pulsar, 0103 physical sciences, pulsars: individual (PSR J2032+4127, individual (PSR J2032+4127, VER J2032+414, MAGIC J2032 +4127) [pulsars], 010306 general physics, education, MAGIC J2032+4127), Pulsars, pulsars: individual (PSR J2032+4127, VER J2032+414, MAGIC J2032+4127), Gamma rays, Institut für Physik und Astronomie, Astronomy and Astrophysic, Light curve, Stars, Estels, VER J2032+414, 13. Climate action, ddc:520, general [gamma rays]
Abstract: We report on observations of the pulsar / Be star binary system PSR J2032+4127 / MT91 213 in the energy range between 100 GeV and 20 TeV with the VERITAS and MAGIC imaging atmospheric Cherenkov telescope arrays. The binary orbit has a period of approximately 50 years, with the most recent periastron occurring on 2017 November 13. Our observations span from 18 months prior to periastron to one month after. A new, point-like, gamma-ray source is detected, coincident with the location of PSR J2032+4127 / MT91 213. The gamma-ray light curve and spectrum are well-characterized over the periastron passage. The flux is variable over at least an order of magnitude, peaking at periastron, thus providing a firm association of the TeV source with the pulsar / Be star system. Observations prior to periastron show a cutoff in the spectrum at an energy around 0.5 TeV. This result adds a new member to the small population of known TeV binaries, and it identifies only the second source of this class in which the nature and properties of the compact object are firmly established. We compare the gamma-ray results with the light curve measured with the X-ray Telescope (XRT) on board the Neil Gehrels \textit{Swift} Observatory and with the predictions of recent theoretical models of the system. We conclude that significant revision of the models is required to explain the details of the emission we have observed, and we discuss the relationship between the binary system and the overlapping steady extended source, TeV J2032+4130., Comment: 12 pages, 3 figures, 1 table. Accepted for publication in ApJL
Published: 2018
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47. The 26.3-h orbit and multiwavelength properties of the 'redback' millisecond pulsar PSR J1306-40

Author: Manuel Linares, Universitat Politècnica de Catalunya. Departament de Física, and Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Pulsar planet, FOS: Physical sciences, Context (language use), Type (model theory), 01 natural sciences, individual: PSR J1306-40 [stars], general [pulsars], Luminosity, general [binaries], neutron [stars], Raigs gamma, Pulsar, Millisecond pulsar, 0103 physical sciences, Disc, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Estels de neutrons, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Gamma rays, Astronomy, Astronomy and Astrophysics, Orbital period, stars [gamma rays], Space and Planetary Science, variables: general [stars], Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the discovery of the variable optical and X-ray counterparts to the radio millisecond pulsar (MSP) PSR J1306-40, recently discovered by Keane et al. We find that both the optical and X-ray fluxes are modulated with the same period, which allows us to measure for the first time the orbital period P$_{\rm orb}$=1.09716[6] d. The optical properties are consistent with a main sequence companion with spectral type G to mid K and, together with the X-ray luminosity (8.8$\times$10$^{31}$ erg s$^{-1}$ in the 0.5-10 keV band, for a distance of 1.2 kpc), confirm the redback classification of this pulsar. Our results establish the binary nature of PSR J1306-40, which has the longest P$_{\rm orb}$ among all known compact binary MSPs in the Galactic disk. We briefly discuss these findings in the context of irradiation and intrabinary shock emission in compact binary MSPs., 5 pages, 3 figures, MNRAS, accepted (minor changes after referee report). In memory of our esteemed colleague Enrique Garc\'ia-Berro
Published: 2018

48. Gamma-ray emission from interactions between jets and BLR clouds

Author: Del Palacio, S., Bosch i Ramon, Valentí, and Romero, Gustavo E.
Subjects: Raigs gamma, Astrophysics::High Energy Astrophysical Phenomena, Galàxies actives, Gamma rays, Active galaxies, Astrophysics::Galaxy Astrophysics
Abstract: Blazars -active galactic nuclei with a jet pointing towards the observer- are the most numerous γ-ray sources detected until date. In this work we show preliminary results of a model in which broad-line region (BLR) clouds penetrate in the jet, producing shocks capable of accelerating relativistic electrons; these electrons emit γ-rays when they interact with the photons coming from the BLR clouds. We calculate semi-analytically the dynamical evolution of a typical cloud inside the jet, the energy distribution of the locally accelerated electrons, and the high-energy emission the latter produce, taking into account relativistic effects. We estimate the dutycycle of these interactions in order to find whether they occur as discrete events or almost continuous. We compare the observed γ-ray fluxes with the ones predicted by our model and discuss the implications in terms of particle acceleration efficiency and mass-loading in the blazar jets.
Published: 2018

49. Constraining very-high-energy and optical emission from FRB 121102 with the MAGIC telescopes

Author: D. Elsaesser, Satoshi Masuda, Alessandra Lamastra, A. Hahn, Stefano Covino, K. Nishijima, Francesco Longo, Kazumi Kashiyama, Arka Chatterjee, Marc Ribó, Pierre Colin, D. Hadasch, J. Becerra González, Oscar Blanch, Julian Sitarek, P. Bangale, Abelardo Moralejo, Hidetoshi Kubo, W. Bhattacharyya, W. Rhode, J. Kushida, Jose Luis Contreras, J. Rico, P. Giammaria, Laura Spitler, F. Leone, M. Minev, L. Maraschi, E. Colombo, Juan Cortina, I. Puljak, Masahiro Teshima, G. Ferrara, Jordi Delgado, M. Vazquez Acosta, M. López, G. Bonnoli, J. Palacio, T. Schweizer, E. Molina, Victoria Moreno, Chiara Righi, J. M. Paredes, Antonio Stamerra, M. Delfino, Francesco Dazzi, A. Fernández-Barral, Jason W. T. Hessels, N. Torres-Albà, B. Banerjee, C. Arcaro, J. R. Garcia, Darko Zarić, P. Da Vela, Iva Šnidarić, D. Baack, D. Ninci, Jürgen Besenrieder, Alicia Fattorini, D. Dominis Prester, F. Di Pierro, M. Peresano, M. Makariev, A. Arbet Engels, Vitaly Neustroev, Lab Saha, Luca Foffano, Pablo Peñil, R. J. García López, Stefano Gallozzi, Jose Miguel Miranda, A. Somero, V. D'Elia, Aaron Dominguez, A. Niedzwiecki, J. E. Ward, C. Fruck, Ciro Bigongiari, Kari Nilsson, P. Majumdar, C. Nigro, G. Ceribella, Elina Lindfors, Juan Abel Barrio, L. Nogués, D. Dorner, M. Nievas Rosillo, M. Mariotti, S. M. Colak, M. Garczarczyk, D. Guberman, Kohta Murase, A. Rugliancich, Marina Manganaro, V. Fallah Ramazani, C. Maggio, G. Maneva, Daniel Mazin, Tomislav Terzić, Dario Hrupec, R. Paoletti, A. Berti, M. Will, A. López-Oramas, D. Paneque, N. Godinović, B. De Lotto, K. Mannheim, Tarek M. Hassan, W. Bednarek, Andrew Seymour, G. Pedaletti, Shimpei Tsujimoto, P. Cumani, Konstancja Satalecka, Michele Doro, Fabrizio Tavecchio, M. I. Martínez, Massimo Persic, V. A. Acciari, Ll. Font, Razmik Mirzoyan, P G Prada Moroni, Adrian Biland, Louis Antonelli, D. Lelas, G. Vanzo, E. Moretti, Ana Babić, Sabrina Einecke, A. De Angelis, Tihomir Surić, S. Paiano, K. Ishio, Dorota Sobczyńska, Benito Marcote, Stefano Ansoldi, D. Fidalgo, Markus Gaug, M. V. Fonseca, Saverio Lombardi, John Hoang, Takashi Saito, U. Barres de Almeida, Elisa Prandini, Rodolfo Carosi, Susumu Inoue, Daniele Michilli, Y. Iwamura, M. Strzys, D. Kuveždić, I. Vovk, Valentí Bosch-Ramon, Jose Carlos Herrera, Petar Temnikov, Koji Noda, Elisa Bernardini, Acciari, V. A., Ansoldi, S., Antonelli, L. A., Arbet Engels, A., Arcaro, C., Baack, D., Babić, A., Banerjee, B., Bangale, P., de Almeida, U. Barre, Barrio, J. A., González, J. Becerra, Bednarek, W., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Carosi, R., Ceribella, G., Chatterjee, A., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Di Pierro, F., Domínguez, A., Prester, D. Domini, Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Ramazani, V. Fallah, Fattorini, A., Fernández-Barral, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Gallozzi, S., López, R. J. García, Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Herrera, J., Hoang, J., Hrupec, D., Inoue, S., Ishio, K., Iwamura, Y., Kubo, H., Kushida, J., Kuveždić, D., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López, M., López-Oramas, A., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Masuda, S., Mazin, D., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Moreno, V., Moretti, E., Neustroev, V., Niedzwiecki, A., Rosillo, M. Nieva, Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peñil, P., Peresano, M., Persic, M., Moroni, P. G. Prada, Prandini, E., Puljak, I., Garcia, J. R., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Somero, A., Stamerra, A., Strzys, M., Surić, T., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Tsujimoto, S., Vanzo, G., Acosta, M. Vazquez, Vovk, I., Ward, J. E., Will, M., Zarić, D., Marcote, B., Spitler, L. G., Hessels, J. W. T., Kashiyama, K., Murase, K., Bosch-Ramon, V., Michilli, D., Seymour, A., Universitat de Barcelona, and ITA
Subjects: High energy, Photon, Radiation mechanisms: non-thermal, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Radiació, Raigs gamma, radiation mechanisms: non-thermal, methods: data analysis, methods: observational, gamma-rays: general, Methods: observational, Methods: data analysis, 0103 physical sciences, Gamma ray astronomy, Astronomia de raigs gamma, observational [Methods], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Millisecond, general [Gamma-rays], ta115, Radiation, non-thermal [Radiation mechanisms], 010308 nuclear & particles physics, Gamma rays, Gamma ray, Astronomy and Astrophysics, Astronomy and Astrophysic, Galaxy, Redshift, data analysi [Methods], Wavelength, 13. Climate action, Space and Planetary Science, Gamma-rays: general, ddc:520, Física nuclear, Optical emission spectroscopy, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Fast radio bursts (FRBs) are bright flashes observed typically at GHz frequencies with millisecond duration, whose origin is likely extragalactic. Their nature remains mysterious, motivating searches for counterparts at other wavelengths. FRB 121102 is so far the only source known to repeatedly emit FRBs and is associated with a host galaxy at redshift $z \simeq 0.193$. We conducted simultaneous observations of FRB 121102 with the Arecibo and MAGIC telescopes during several epochs in 2016--2017. This allowed searches for millisecond-timescale burst emission in very-high-energy (VHE) gamma rays as well as the optical band. While a total of five FRBs were detected during these observations, no VHE emission was detected, neither of a persistent nature nor burst-like associated with the FRBs. The average integral flux upper limits above 100 GeV at 95% confidence level are $6.6 \times 10^{-12}~\mathrm{photons\ cm^{-2}\ s^{-1}}$ (corresponding to luminosity $L_{\rm VHE} \lesssim 10^{45}~\mathrm{erg\ s^{-1}}$) over the entire observation period, and $1.2 \times 10^{-7}~ \mathrm{photons\ cm^{-2}\ s^{-1}}$ ($L_{\rm VHE} \lesssim 10^{49}~\mathrm{erg\ s^{-1}}$) over the total duration of the five FRBs. We constrain the optical U-band flux to be below 8.6 mJy at 5-$\sigma$ level for 1-ms intervals around the FRB arrival times. A bright burst with U-band flux $29~\mathrm{mJy}$ and duration $\sim 12$ ms was detected 4.3 s before the arrival of one FRB. However, the probability of spuriously detecting such a signal within the sampled time space is 1.5% (2.2 $\sigma$, post-trial), i.e. consistent with the expected background. We discuss the implications of the obtained upper limits for constraining FRB models., Comment: 9 pages, 3 figures. Accepted for publication in MNRAS the 2nd September 2018
Published: 2018

50. Adsorption of odorous sulfur compounds onto activated carbons modified by gamma irradiation

Author: Manuel Sánchez-Polo, Maria J. Martin, Esther Vega, Rafael Gonzalez-Olmos, and Ministerio de Ciencia e Innovación (Espanya)
Subjects: Thermal desorption spectroscopy, Inorganic chemistry, Carbó activat, chemistry.chemical_element, Gamma irradiation, Oxygen, Biomaterials, chemistry.chemical_compound, Raigs gamma, Colloid and Surface Chemistry, Adsorption, Sofre -- Compostos, Sulphur compounds, medicine, Adsorció, Dimethyl disulfide, Sulfur, Carbon, Activated, Surfaces, Coatings and Films, Electronic, Optical and Magnetic Materials, chemistry, Ultrapure water, Dimethyl sulfide, Activated carbon, medicine.drug
Abstract: A commercial activated carbon (AC) was modified by gamma irradiation and was tested as adsorbent for the removal of ethyl mercaptan, dimethyl disulfide and dimethyl disulfide in wet conditions. Modifications were carried out under five different conditions: irradiation in absence of water, in presence of ultrapure water, in ultrapure water at pH = 1.0 and 1000 mg L-1 Cl-, in ultrapure water at pH = 7.5 and 1000 mg L-1 Br-, and in ultrapure water at pH = 12.5 and 1000 mg L-1 NO3-. The chemical properties of each AC were characterized by elemental analysis, temperature programmed desorption and X-ray photoelectron spectroscopy. Outcomes show that a large number of oxygen functional groups were incorporated in the AC surface by gamma irradiation, especially in the AC irradiated in the presence of ultrapure water. The dynamic adsorption test results reveal that the incorporation of oxygen functional groups did not enhance the adsorption capacities for dimethyl sulfide and dimethyl disulfide. A significant improvement in the ethyl mercaptan adsorption capacity was correlated with the incorporation of phenolic groups in the AC surface. Moreover, diethyl disulfide was detected as by-product of ethyl mercaptan oxidation process under wet conditions and its formation depended on the chemical properties of ACs R. Gonzalez-Olmos thanks MICINN (Ministerio de Ciencia e Innovacion) for the Juan de la Cierva fellowship (JCI-2010-07104). The authors also greatly appreciate financial support from the Spanish MICINN (projects PET2008_0261, CTQ2011-24114). LEQUIA has been recognized as consolidated research group by the Catalan Government with code 2014-SGR-1168
Published: 2015

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