505 research outputs found
Study of B c + → J / ψ D s + and B c + → J / ψ D s ∗ + decays in pp collisions at √s = 13 TeV with the ATLAS detector
No full textA study of B+
c → J/ψD+
s and B+
c → J/ψD∗+
s decays using 139 fb−1 of integrated luminosity collected with the ATLAS detector from √
s = 13 TeV pp collisions
at the LHC is presented. The ratios of the branching fractions of the two decays to the
branching fraction of the B+
c → J/ψπ+ decay are measured: B(B+
c → J/ψD+
s
)/B(B+
c →
J/ψπ+) = 2.76 ± 0.47 and B(B+
c → J/ψD∗+
s
)/B(B+
c → J/ψπ+) = 5.33 ± 0.96. The ratio
of the branching fractions of the two decays is found to be B(B+
c → J/ψD∗+
s
)/B(B+
c →
J/ψD+
s
) = 1.93 ± 0.26. For the B+
c → J/ψD∗+
s decay, the transverse polarization fraction,
Γ±±/Γ, is measured to be 0.70 ± 0.11. The reported uncertainties include both the statistical and systematic components added in quadrature. The precision of the measurements
exceeds that in all previous studies of these decays. These results supersede those obtained
in the earlier ATLAS study of the same decays with √s = 7 and 8 TeV pp collision data. A
comparison with available theoretical predictions for the measured quantities is presented
Search for lepton-flavour violation in high-mass dilepton final states using 139 fb −1 of pp collisions at √s = 13 TeV with the ATLAS detector
No full textÁlvarez Piqueras, D.; Aikot, Arya; Amos, K.R. ; Aparisi, Pozo, J.A.; Bailey, A.J.; Barranco, Laura; Bouchhar, Naseem; Cabrera, Susana; Cantero, Josu; Cardillo, Fabio Castillo, F.L.; Castillo Mª Victoria; Chitishvili, Mariam Cerda Alberich, L.; Costa, María José; Didenko, Mariia , Escobar, Carlos; Estrada, Oscar; Ferrer, Antonio; Fiorini, L.; Fullana, Esteban; Fuster, Juan; García García, Carmen; García Navarro, José Enrique; Gomez Delegido, A.J.; González de la Hoz, Santiago; Gonzalvo Rodríguez, Galo Rafael; Guerrero Rojas, J.G.R.; Higón, Emilio; Jimenez Pena, Javier; Lacasta Llácer, Carlos; Lozano Bahilo, José J.; Madaffari, Daniele; Mamuzic, Judita; Martí García, Salvador; Martinez Agullo, Pablo;; Melini, Davide; Miñano Moya, M.; Mitsou, Vasiliki A.; Miralles López, Marcos; Monsonis Romero, Luis; Moreno Llácer, María; Muñoz Perez, David; Navarro Gonzalez, Josep; Poveda, Joaquín; Prades Ibañez, Alberto; Rodriguez Bosca, S.; Rodriguez Rodriguez, D.; Rubio Jiménez, Adrián ; Ruiz Martínez, Arantxa; Sabatini, Paolo , Salt, José; Sanchez Sebastian, Victoria Santra, A.; Sánchez Martínez, Javier; Sayago Galvan, Ivan; Senthilkumar, Varsha ; Soldevila, Urmila; Torró Pastor, Emma; Valero, Alberto; Valls Ferrer, Juan Antonio; Valiente Moreno, Enrique ; Villaplana Pérez, Miguel , Varriale, Lorenzo; Vos, Marcel; ATLAS CollaborationA search is performed for a heavy particle decaying into different-flavour, dilepton final states, using 139 fb of proton-proton collision data at s = 13 TeV collected in 2015–2018 by the ATLAS detector at the Large Hadron Collider. Final states with electrons, muons and hadronically decaying tau leptons are considered (eμ, eτ or μτ). No significant excess over the Standard Model predictions is observed. Upper limits on the production cross-section are set as a function of the mass of a Z′ boson, a supersymmetric τ-sneutrino, and a quantum black-hole. The observed 95% CL lower mass limits obtained on a typical benchmark model Z′ boson are 5.0 TeV (eμ), 4.0 TeV (eτ), and 3.9 TeV (μτ), respectively. [Figure not available: see fulltext.].U.; Sanchez, J.; Torro Pastor, E.; Valero, A.; Valiente Moreno, E.; Valls Ferrer, J.A.; Varriale, L.; Villaplana Perez, M.; Vos, M.Peer reviewe
A search for new resonances in multiple final states with a high transverse momentum Z boson in √s = 13 TeV pp collisions with the ATLAS detector
No full textÁlvarez Piqueras, D.; Aikot, Arya; Amos, K.R. ; Aparisi, Pozo, J.A.; Bailey, A.J.; Barranco, Laura; Bouchhar, Naseem; Cabrera, Susana; Cantero, Josu; Cardillo, Fabio Castillo, F.L.; Castillo Mª Victoria; Chitishvili, Mariam Cerda Alberich, L.; Costa, María José; Didenko, Mariia , Escobar, Carlos; Estrada, Oscar; Ferrer, Antonio; Fiorini, L.; Fullana, Esteban; Fuster, Juan; García García, Carmen; García Navarro, José Enrique; Gomez Delegido, A.J.; González de la Hoz, Santiago; Gonzalvo Rodríguez, Galo Rafael; Guerrero Rojas, J.G.R.; Higón, Emilio; Jimenez Pena, Javier; Lacasta Llácer, Carlos; Lozano Bahilo, José J.; Madaffari, Daniele; Mamuzic, Judita; Martí García, Salvador; Martinez Agullo, Pablo;; Melini, Davide; Miñano Moya, M.; Mitsou, Vasiliki A.; Miralles López, Marcos; Monsonis Romero, Luis; Moreno Llácer, María; Muñoz Perez, David; Navarro Gonzalez, Josep; Poveda, Joaquín; Prades Ibañez, Alberto; Rodriguez Bosca, S.; Rodriguez Rodriguez, D.; Rubio Jiménez, Adrián ; Ruiz Martínez, Arantxa; Sabatini, Paolo , Salt, José; Sanchez Sebastian, Victoria Santra, A.; Sánchez Martínez, Javier; Sayago Galvan, Ivan; Senthilkumar, Varsha ; Soldevila, Urmila; Torró Pastor, Emma; Valero, Alberto; Valls Ferrer, Juan Antonio; Valiente Moreno, Enrique ; Villaplana Pérez, Miguel , Varriale, Lorenzo; Vos, Marcel; ATLAS CollaborationA generic search for resonances is performed with events containing a Z boson with transverse momentum greater than 100 GeV, decaying into e e or μ μ . The analysed data collected with the ATLAS detector in proton-proton collisions at a centre-of-mass energy of 13 TeV at the Large Hadron Collider correspond to an integrated luminosity of 139 fb. Two invariant mass distributions are examined for a localised excess relative to the expected Standard Model background in six independent event categories (and their inclusive sum) to increase the sensitivity. No significant excess is observed. Exclusion limits at 95% confidence level are derived for two cases: a model-independent interpretation of Gaussian-shaped resonances with the mass width between 3% and 10% of the resonance mass, and a specific heavy vector triplet model with the decay mode W′ → ZW → ℓℓqq. [Figure not available: see fulltext.]; Senthilkumar, V.; Soldevila, U.; Sanchez, J.; Torro Pastor, E.; Valero, A.; Valls Ferrer, J.A.; Varriale, L.; Villaplana Perez, M.; Vos, M.Peer reviewe
Author Correction: A detailed map of Higgs boson interactions by the ATLAS experiment ten years after the discovery
No full textIn the version of this article initially published, the ATLAS Collaboration
author names, affiliations and acknowledgements were omitted and
have now been included in the HTML and PDF versions of the article
Prospects for a survey of the galactic plane with the Cherenkov Telescope Array
No full textAbe, S. et al.-- Full list of authors: Abe, S.; Abhir, J.; Abhishek, A.; Acero, F.; Acharyya, A.; Adam, R.; Aguasca-Cabot, A.; Agudo, I.; Aguirre-Santaella, A.; Alfaro, J.; Alvarez-Crespo, N.; Alves Batista, R.; Amans, J. -P.; Amato, E.; Ambrosi, G.; Ambrosino, F.; Angüner, E. O.; Aramo, C.; Arcaro, C.; Arrabito, L.; Asano, K.; Ascasíbar, Y.; Aschersleben, J.; Augusto Stuani, L.; Backes, M.; Balazs, C.; Balbo, M.; Ballet, J.; Baquero Larriva, A.; Barbosa Martins, V.; Barres de Almeida, U.; Barrio, J. A.; Batković, I.; Batzofin, R.; Baxter, J.; Becerra González, J.; Beck, G.; Beiske, L.; Belmont, R.; Benbow, W.; Bernardini, E.; Bernete, J.; Bernlöhr, K.; Berti, A.; Bertucci, B.; Beshley, V.; Bhattacharjee, P.; Bhattacharyya, S.; Bi, B.; Biederbeck, N.; Biland, A.; Bissaldi, E.; Biteau, J.; Blanch, O.; Blazek, J.; Bocchino, F.; Boisson, C.; Bolmont, J.; Bonneau Arbeletche, L.; Bonnoli, G.; Bonollo, A.; Bordas, P.; Bosnjak, Z.; Bottacini, E.; Braiding, C.; Bronzini, E.; Brose, R.; Brown, A. M.; Brun, F.; Brunelli, G.; Bucciantini, N.; Bulgarelli, A.; Burelli, I.; Burmistrov, L.; Burton, M.; Burtovoi, A.; Bylund, T.; Calisse, P. G.; Campoy-Ordaz, A.; Cantlay, B. K.; Caproni, A.; Capuzzo-Dolcetta, R.; Caraveo, P.; Caroff, S.; Carosi, A.; Carosi, R.; Carquin, E.; Carrasco, M. -S.; Cascone, E.; Cassol, F.; Castrejon, N.; Castro-Tirado, A. J.; Cerasole, D.; Cerruti, M.; Chadwick, P. M.; Chambery, P.; Chaty, S.; Chen, A. W.; Chernyakova, M.; Chiavassa, A.; Chytka, L.; Cifuentes, A.; Coimbra Araujo, C. H.; Conforti, V.; Conte, F.; Contreras, J. L.; Cortina, J.; Costa, A.; Costantini, H.; Cotter, G.; Crestan, S.; Cristofari, P.; Cuevas, O.; Curtis-Ginsberg, Z.; D'Aì, A.; D'Amico, G.; D'Ammando, F.; Dadina, M.; Dalchenko, M.; David, L.; Dazzi, F.; de Bony de Lavergne, M.; De Caprio, V.; De Frondat Laadim, F.; de Gouveia Dal Pino, E. M.; De Lotto, B.; De Lucia, M.; de Martino, D.; de Menezes, R.; de Naurois, M.; de Ona Wilhelmi, E.; de Souza, V.; del Peral, L.; Delgado Giler, A. G.; Delgado, C.; Dell'aiera, M.; Della Valle, M.; della Volpe, D.; Depaoli, D.; Di Girolamo, T.; Di Piano, A.; Di Pierro, F.; Di Tria, R.; Di Venere, L.; Díaz, C.; Diebold, S.; Dinesh, A.; Djannati-Ataï, A.; Djuvsland, J.; Domínguez, A.; Dominik, R. M.; Donini, A.; Dörner, J.; Doro, M.; dos Anjos, R. D. C.; Dournaux, J. -L.; Duangchan, C.; Dubos, C.; Dubus, G.; Duffy, S.; Dumora, D.; Dwarkadas, V. V.; Ebr, J.; Eckner, C.; Egberts, K.; Einecke, S.; Elsässer, D.; Emery, G.; Errando, M.; Escanuela, C.; Escarate, P.; Escobar Godoy, M.; Escudero, J.; Esposito, P.; Evoli, C.; Falceta-Goncalves, D.; Fattorini, A.; Fegan, S.; Feijen, K.; Feng, Q.; Ferrand, G.; Ferrarotto, F.; Fiandrini, E.; Fiasson, A.; Filipovic, M.; Fioretti, V.; Fiori, M.; Flores, H.; Foffano, L.; Font Guiteras, L.; Fontaine, G.; Fröse, S.; Fukazawa, Y.; Fukui, Y.; Funk, S.; Furniss, A.; Gaggero, D.; Galanti, G.; Galaz, G.; Gallant, Y. A.; Gallozzi, S.; Gammaldi, V.; Garczarczyk, M.; Gasbarra, C.; Gasparrini, D.; Gaug, M.; Ghalumyan, A.; Giarrusso, M.; Giesbrecht, J.; Giglietto, N.; Giordano, F.; Giuffrida, R.; Giuliani, A.; Glicenstein, J. -F.; Glombitza, J.; Godinovic, N.; Goldoni, P.; González, J. M.; Goulart Coelho, J.; Granot, J.; Grasso, D.; Grau, R.; Gréaux, L.; Green, D.; Green, J. G.; Greenshaw, T.; Grenier, I.; Grolleron, G.; Grondin, M. -H.; Gueta, O.; Gunji, S.; Hackfeld, J.; Hadasch, D.; Hanlon, W.; Hara, S.; Harvey, V. M.; Hassan, T.; Hayashi, K.; Heckmann, L.; Heller, M.; Hermann, G.; Hernández Cadena, S.; Hervet, O.; Hinton, J.; Hiroshima, N.; Hnatyk, B.; Hnatyk, R.; Hofmann, W.; Holder, J.; Holler, M.; Horan, D.; Horvath, P.; Hovatta, T.; Hrabovsky, M.; Iarlori, M.; Inada, T.; Incardona, F.; Inoue, S.; Iocco, F.; Iori, M.; Jamrozy, M.; Janecek, P.; Jankowsky, F.; Jarnot, C.; Jean, P.; Jiménez Martínez, I.; Jin, W.; Juramy-Gilles, C.; Jurysek, J.; Kagaya, M.; Kalekin, O.; Kantzas, D.; Karas, V.; Katagiri, H.; Kataoka, J.; Kaufmann, S.; Kazanas, D.; Kerszberg, D.; Khélifi, B.; Kieda, D. B.; Kissmann, R.; Kleiner, T.; Kluge, G.; Kluźniak, W.; Knödlseder, J.; Kobayashi, Y.; Kohri, K.; Komin, N.; Kornecki, P.; Kosack, K.; Kostunin, D.; Kowal, G.; Kubo, H.; Kushida, J.; La Barbera, A.; La Palombara, N.; Láinez, M.; Lamastra, A.; Lapington, J.; Laporte, P.; Lazarević, S.; Lazendic-Galloway, J.; Lemoine-Goumard, M.; Lenain, J. -P.; Leone, F.; Leto, G.; Leuschner, F.; Lindfors, E.; Linhoff, M.; Liodakis, I.; Lombardi, S.; Longo, F.; López-Coto, R.; López-Moya, M.; López-Oramas, A.; Loporchio, S.; Lozano Bahilo, J.; Lucarelli, F.; Luque-Escamilla, P. L.; Lyard, E.; Macias, O.; Mackey, J.; Maier, G.; Malyshev, D.; Mandat, D.; Manicò, G.; Marcowith, A.; Marinos, P.; Mariotti, M.; Markoff, S.; Marquez, P.; Marsella, G.; Martí, J.; Martin, P.; Martínez, G. A.; Martínez, M.; Martinez, O.; Marty, C.; Mas-Aguilar, A.; Mastropietro, M.; Maurin, G.; Mazin, D.; McKeague, S.; Mello, A. J. T. S.; Menchiari, S.; Mereghetti, S.; Mestre, E.; Meunier, J. -L.; Meyer, D. M. -A.; Miceli, D.; Miceli, M.; Michailidis, M.; Michałowski, J.; Miener, T.; Miranda, J. M.; Mitchell, A.; Mizuno, T.; Moderski, R.; Mohrmann, L.; Molero, M.; Molfese, C.; Molina, E.; Montaruli, T.; Moralejo, A.; Morcuende, D.; Morik, K.; Morlino, G.; Morselli, A.; Moulin, E.; Moya Zamanillo, V.; Mukherjee, R.; Munari, K.; Murach, T.; Muraczewski, A.; Muraishi, H.; Nagataki, S.; Nakamori, T.; Nemmen, R.; Nickel, L.; Niemiec, J.; Nieto, D.; Nievas Rosillo, M.; Nikołajuk, M.; Nikolić, L.; Noda, K.; Nosek, D.; Novosyadlyj, B.; Novotny, V.; Nozaki, S.; Ohishi, M.; Ohtani, Y.; Okumura, A.; Olive, J. -F.; Olmi, B.; Ong, R. A.; Orienti, M.; Orito, R.; Orlandini, M.; Orlando, E.; Orlando, S.; Ostrowski, M.; Oya, I.; Pagano, I.; Pagliaro, A.; Palatiello, M.; Panebianco, G.; Paneque, D.; Pantaleo, F. R.; Paoletti, R.; Paredes, J. M.; Parmiggiani, N.; Patel, S. R.; Patricelli, B.; Pavlović, D.; Pech, M.; Pecimotika, M.; Peresano, M.; Pérez-Romero, J.; Pérez-Torres, M. A.; Peron, G.; Persic, M.; Petrucci, P. -O.; Petruk, O.; Piano, G.; Pierre, E.; Pietropaolo, E.; Pihet, M.; Pintore, F.; Pittori, C.; Plard, C.; Podobnik, F.; Pohl, M.; Pons, E.; Ponti, G.; Prandini, E.; Principe, G.; Priyadarshi, C.; Produit, N.; Prokhorov, D.; Pueschel, E.; Pühlhofer, G.; Pumo, M. L.; Punch, M.; Queiroz, F.; Quirrenbach, A.; Rando, R.; Ravel, T.; Razzaque, S.; Regeard, M.; Reichherzer, P.; Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Reposeur, T.; Rhode, W.; Ribeiro, D.; Ribó, M.; Richtler, T.; Rico, J.; Rieger, F.; Rigoselli, M.; Rizi, V.; Roache, E.; Rodriguez Fernandez, G.; Rodríguez-Vázquez, J. J.; Romano, P.; Romeo, G.; Rosado, J.; Rosales de Leon, A.; Rowell, G.; Rudak, B.; Ruiter, A. J.; Rulten, C. B.; Russo, F.; Sadeh, I.; Saha, L.; Saito, T.; Salzmann, H.; Sánchez-Conde, M.; Sangiorgi, P.; Sano, H.; Santander, M.; Santangelo, A.; Santos-Lima, R.; Sapienza, V.; Šarić, T.; Sarkar, S.; Saturni, F. G.; Scherer, A.; Schiavone, F.; Schipani, P.; Schleicher, B.; Schovanek, P.; Schubert, J. L.; Schussler, F.; Schwanke, U.; Schwefer, G.; Seglar Arroyo, M.; Seitenzahl, I.; Sergijenko, O.; Servillat, M.; Sguera, V.; Sharma, P.; Siejkowski, H.; Siqueira, C.; Sizun, P.; Sliusar, V.; Slowikowska, A.; Sol, H.; Spencer, S. T.; Spiga, D.; Stamerra, A.; Stanič, S.; Starling, R.; Stawarz, Ł.; Steinmassl, S.; Steppa, C.; Stolarczyk, T.; Suda, Y.; Suomijärvi, T.; Tajima, H.; Takeishi, R.; Tanaka, S. J.; Tavecchio, F.; Tavernier, T.; Terada, Y.; Terrier, R.; Teshima, M.; Tian, W. W.; Tibaldo, L.; Tibolla, O.; Torradeflot, F.; Torres, D. F.; Tothill, N.; Toussenel, F.; Touzard, V.; Travnicek, P.; Tripodo, G.; Trois, A.; Tsiahina, A.; Tutone, A.; Umana, G.; Vaclavek, L.; Vacula, M.; Vallania, P.; van Eldik, C.; Vassiliev, V.; Vazquez Acosta, M. L.; Vecchi, M.; Ventura, S.; Vercellone, S.; Verna, G.; Viana, A.; Viaux, N.; Vigliano, A.; Vignatti, J.; Vigorito, C. F.; Villanueva, J.; Vink, J.; Vitale, V.; Vodeb, V.; Voisin, V.; Vorobiov, S.; Voutsinas, G.; Vovk, I.; Vuillaume, T.; Waegebaert, V.; Wagner, S. J.; Walter, R.; Wechakama, M.; White, R.; Wierzcholska, A.; Williams, D. A.; Wohlleben, F.; Yamazaki, R.; Yang, L.; Yoshida, T.; Yoshikoshi, T.; Zacharias, M.; Zaharijas, G.; Zampieri, L.; Zanin, R.; Zavrtanik, D.; Zavrtanik, M.; Zdziarski, A. A.; Zech, A.; Zhdanov, V. I.; Ziętara, K.; Živec, M.; Zuriaga-Puig, J.; De la Torre Luque, P.; Guillemot, L.; Smith, D. A.; CTA ConsortiumApproximately one hundred sources of very-high-energy (VHE) gamma rays are known in the Milky Way, detected with a combination of targeted observations and surveys. A survey of the entire Galactic Plane in the energy range from a few tens of GeV to a few hundred TeV has been proposed as a Key Science Project for the upcoming Cherenkov Telescope Array Observatory (CTAO). This article presents the status of the studies towards the Galactic Plane Survey (GPS). We build and make publicly available a sky model that combines data from recent observations of known gamma-ray emitters with state-of-the-art physically-driven models of synthetic populations of the three main classes of established Galactic VHE sources (pulsar wind nebulae, young and interacting supernova remnants, and compact binary systems), as well as of interstellar emission from cosmic-ray interactions in the Milky Way. We also perform an optimisation of the observation strategy (pointing pattern and scheduling) based on recent estimations of the instrument performance. We use the improved sky model and observation strategy to simulate GPS data corresponding to a total observation time of 1620 hours spread over ten years. Data are then analysed using the methods and software tools under development for real data. Under our model assumptions and for the realisation considered, we show that the GPS has the potential to increase the number of known Galactic VHE emitters by almost a factor of five. This corresponds to the detection of more than two hundred pulsar wind nebulae and a few tens of supernova remnants at average integral fluxes one order of magnitude lower than in the existing sample above 1 TeV, therefore opening the possibility to perform unprecedented population studies. The GPS also has the potential to provide new VHE detections of binary systems and pulsars, to confirm the existence of a hypothetical population of gamma-ray pulsars with an additional TeV emission component, and to detect bright sources capable of accelerating particles to PeV energies (PeVatrons). Furthermore, the GPS will constitute a pathfinder for deeper follow-up observations of these source classes. Finally, we show that we can extract from GPS data an estimate of the contribution to diffuse emission from unresolved sources, and that there are good prospects of detecting interstellar emission and statistically distinguishing different scenarios. Thus, a survey of the entire Galactic plane carried out from both hemispheres with CTAO will ensure a transformational advance in our knowledge of Galactic VHE source populations and interstellar emission. © 2024 The Author(s).We gratefully acknowledge financial support from the following agencies and organisations:
State Committee of Science of Armenia, Armenia; The Australian Research Council, Astronomy Australia Ltd, The University of Adelaide, Australian National University, Monash
University, The University of New South Wales, The University of Sydney, Western Sydney
University, Australia; Federal Ministry of Education, Science and Research, and Innsbruck
University, Austria; Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq),
Fundação de Amparo à Pesquisa do Estado do Rio de Janeiro (FAPERJ), Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP), Fundação de Apoio à Ciência, Tecnologia
e Inovação do Paraná — Fundação Araucária, Ministry of Science, Technology, Innovations
and Communications (MCTIC), Brasil; Ministry of Education and Science, National RI
Roadmap Project DO1-153/28.08.2018, Bulgaria; The Natural Sciences and Engineering
Research Council of Canada and the Canadian Space Agency, Canada; CONICYT-Chile grants CATA AFB 170002, ANID PIA/APOYO AFB 180002, ACT 1406, FONDECYT-Chile
grants, 1161463, 1170171, 1190886, 1171421, 1170345, 1201582, Gemini-ANID 32180007,
Chile, W.M. gratefully acknowledges support by the ANID BASAL projects ACE210002
and FB210003, and FONDECYT 11190853; Croatian Science Foundation, Rudjer Boskovic
Institute, University of Osijek, University of Rijeka, University of Split, Faculty of Electrical
Engineering, Mechanical Engineering and Naval Architecture, University of Zagreb, Faculty
of Electrical Engineering and Computing, Croatia; Ministry of Education, Youth and Sports,
MEYS LM2015046, LM2018105, LTT17006, EU/MEYS CZ.02.1.01/0.0/0.0/16_013/0001403,
CZ.02.1.01/0.0/0.0/18_046/0016007 and CZ.02.1.01/0.0/0.0/16_019/0000754, Czech Republic; Academy of Finland (grant nr.317636 and 320045), Finland; Ministry of Higher
Education and Research, CNRS-INSU and CNRS-IN2P3, CEA-Irfu, ANR, Regional Council
Ile de France, Labex ENIGMASS, OCEVU, OSUG2020 and P2IO, France; The German
Ministry for Education and Research (BMBF), the Max Planck Society, the German Research
Foundation (DFG, with Collaborative Research Centres 876 & 1491), and the Helmholtz
Association, Germany; Department of Atomic Energy, Department of Science and Technology, India; Istituto Nazionale di Astrofisica (INAF), Istituto Nazionale di Fisica Nucleare
(INFN), MIUR, Istituto Nazionale di Astrofisica (INAF-OABRERA) Grant Fondazione
Cariplo/Regione Lombardia ID 2014-1980/RST_ERC, Italy; ICRR, University of Tokyo,
JSPS, MEXT, Japan; Netherlands Research School for Astronomy (NOVA), Netherlands
Organization for Scientific Research (NWO), Netherlands; University of Oslo, Norway; Ministry of Science and Higher Education, DIR/WK/2017/12, the National Centre for Research
and Development and the National Science Centre, UMO-2016/22/M/ST9/00583, Poland;
Slovenian Research Agency, grants P1-0031, P1-0385, I0-0033, J1-9146, J1-1700, N1-0111,
and the Young Researcher program, Slovenia; South African Department of Science and
Technology and National Research Foundation through the South African Gamma-Ray
Astronomy Programme, South Africa; The Spanish groups acknowledge the Spanish Ministry of Science and Innovation and the Spanish Research State Agency (AEI) through
the government budget lines PGE2021/28.06.000X.411.01, PGE2022/28.06.000X.411.01
and PGE2022/28.06.000X.711.04, and grants PID2022-139117NB-C44, PID2019-104114RBC31, PID2019-107847RB-C44, PID2019-104114RB-C32, PID2019-105510GB-C31, PID2019-
104114RB-C33, PID2019-107847RB-C41, PID2019-107847RB-C43, PID2019-107847RB-C42,
PID2019-107988GB-C22, PID2021-124581OB-I00, PID2021-125331NB-I00; the “Centro de
Excelencia Severo Ochoa” program through grants no. CEX2019-000920-S, CEX2020-001007-
S, CEX2021-001131-S; the “Unidad de Excelencia María de Maeztu” program through grants
no. CEX2019-000918-M, CEX2020-001058-M; the “Ramón y Cajal” program through grants
RYC2021-032552-I, RYC2021-032991-I, RYC2020-028639-I and RYC-2017-22665; the “Juan
de la Cierva-Incorporación” program through grants no. IJC2018-037195-I, IJC2019-040315-I.
They also acknowledge the “Atracción de Talento” program of Comunidad de Madrid through
grant no. 2019-T2/TIC-12900; the project “Tecnologiás avanzadas para la exploracioń del
universo y sus componentes” (PR47/21 TAU), funded by Comunidad de Madrid, by the
Recovery, Transformation and Resilience Plan from the Spanish State, and by NextGenerationEU from the European Union through the Recovery and Resilience Facility; the La Caixa
Banking Foundation, grant no. LCF/BQ/PI21/11830030; the “Programa Operativo” FEDER 2014-2020, Consejería de Economía y Conocimiento de la Junta de Andalucía (ref. 1257737),
PAIDI 2020 (ref. P18-FR-1580) and Universidad de Jaén; “Programa Operativo de Crecimiento Inteligente” FEDER 2014-2020 (ref. ESFRI-2017-IAC-12), Ministerio de Ciencia e
Innovación, 15% co-financed by Consejería de Economía, Industria, Comercio y Conocimiento
del Gobierno de Canarias; the “CERCA” program and the grant 2021SGR00426, both funded
by the Generalitat de Catalunya; and the European Union’s Horizon 2020 GA:824064 and
NextGenerationEU (PRTR-C17.I1); Swedish Research Council, Royal Physiographic Society
of Lund, Royal Swedish Academy of Sciences, The Swedish National Infrastructure for Computing (SNIC) at Lunarc (Lund), Sweden; State Secretariat for Education, Research and
Innovation (SERI) and Swiss National Science Foundation (SNSF), Switzerland; Durham
University, Leverhulme Trust, Liverpool University, University of Leicester, University of
Oxford, Royal Society, Science and Technology Facilities Council, U.K.; U.S. National Science
Foundation, U.S. Department of Energy, Argonne National Laboratory, Barnard College,
University of California, University of Chicago, Columbia University, Georgia Institute of
Technology, Institute for Nuclear and Particle Astrophysics (INPAC-MRPI program), Iowa
State University, the Smithsonian Institution, V.V.D. is funded by NSF grant AST-1911061,
Washington University McDonnell Center for the Space Sciences, The University of Wisconsin
and the Wisconsin Alumni Research Foundation, U.S.A..
The research leading to these results has received funding from the European Union’s
Seventh Framework Programme (FP7/2007-2013) under grant agreements No 262053 and
No 317446. This project is receiving funding from the European Union’s Horizon 2020
research and innovation programs under agreement No 676134.
This research made use of ctools, a community-developed gamma-ray astronomy science
analysis software. ctools is based on GammaLib, a community-developed toolbox for the
scientific analysis of astronomical gamma-ray data. This research made use of gammapy,12
a community-developed core Python package for TeV gamma-ray astronomy.Peer reviewe
A search for heavy Higgs bosons decaying into vector bosons in same-sign two-lepton final states in pp collisions at √s = 13 TeV with the ATLAS detector
No full textÁlvarez Piqueras, D.; Aikot, Arya; Amos, K.R. ; Aparisi, Pozo, J.A.; Bailey, A.J.; Barranco, Laura; Bouchhar, Naseem; Cabrera, Susana; Cantero, Josu; Cardillo, Fabio Castillo, F.L.; Castillo Mª Victoria; Chitishvili, Mariam Cerda Alberich, L.; Costa, María José; Didenko, Mariia , Escobar, Carlos; Estrada, Oscar; Ferrer, Antonio; Fiorini, L.; Fullana, Esteban; Fuster, Juan; García García, Carmen; García Navarro, José Enrique; Gomez Delegido, A.J.; González de la Hoz, Santiago; Gonzalvo Rodríguez, Galo Rafael; Guerrero Rojas, J.G.R.; Higón, Emilio; Jimenez Pena, Javier; Lacasta Llácer, Carlos; Lozano Bahilo, José J.; Madaffari, Daniele; Mamuzic, Judita; Martí García, Salvador; Martinez Agullo, Pablo;; Melini, Davide; Miñano Moya, M.; Mitsou, Vasiliki A.; Miralles López, Marcos; Monsonis Romero, Luis; Moreno Llácer, María; Muñoz Perez, David; Navarro Gonzalez, Josep; Poveda, Joaquín; Prades Ibañez, Alberto; Rodriguez Bosca, S.; Rodriguez Rodriguez, D.; Rubio Jiménez, Adrián ; Ruiz Martínez, Arantxa; Sabatini, Paolo , Salt, José; Sanchez Sebastian, Victoria Santra, A.; Sánchez Martínez, Javier; Sayago Galvan, Ivan; Senthilkumar, Varsha ; Soldevila, Urmila; Torró Pastor, Emma; Valero, Alberto; Valls Ferrer, Juan Antonio; Valiente Moreno, Enrique ; Villaplana Pérez, Miguel , Varriale, Lorenzo; Vos, Marcel; ATLAS CollaborationA search for heavy Higgs bosons produced in association with a vector boson and decaying into a pair of vector bosons is performed in final states with two leptons (electrons or muons) of the same electric charge, missing transverse momentum and jets. A data sample of proton–proton collisions at a centre-of-mass energy of 13 TeV recorded with the ATLAS detector at the Large Hadron Collider between 2015 and 2018 is used. The data correspond to a total integrated luminosity of 139 fb. The observed data are in agreement with Standard Model background expectations. The results are interpreted using higher-dimensional operators in an effective field theory. Upper limits on the production cross-section are calculated at 95% confidence level as a function of the heavy Higgs boson’s mass and coupling strengths to vector bosons. Limits are set in the Higgs boson mass range from 300 to 1500 GeV, and depend on the assumed couplings. The highest excluded mass for a heavy Higgs boson with the coupling combinations explored is 900 GeV. Limits on coupling strengths are also provided. [Figure not available: see fulltext.]Article funded by SCOAP3.Peer reviewe
Modelling and computational improvements to the simulation of single vector-boson plus jet processes for the ATLAS experiment
No full textÁlvarez Piqueras, D.; Aikot, Arya; Amos, K.R. ; Aparisi, Pozo, J.A.; Bailey, A.J.; Barranco, Laura; Bouchhar, Naseem; Cabrera, Susana; Cantero, Josu; Cardillo, Fabio Castillo, F.L.; Castillo Mª Victoria; Chitishvili, Mariam Cerda Alberich, L.; Costa, María José; Didenko, Mariia , Escobar, Carlos; Estrada, Oscar; Ferrer, Antonio; Fiorini, L.; Fullana, Esteban; Fuster, Juan; García García, Carmen; García Navarro, José Enrique; Gomez Delegido, A.J.; González de la Hoz, Santiago; Gonzalvo Rodríguez, Galo Rafael; Guerrero Rojas, J.G.R.; Higón, Emilio; Jimenez Pena, Javier; Lacasta Llácer, Carlos; Lozano Bahilo, José J.; Madaffari, Daniele; Mamuzic, Judita; Martí García, Salvador; Martinez Agullo, Pablo;; Melini, Davide; Miñano Moya, M.; Mitsou, Vasiliki A.; Miralles López, Marcos; Monsonis Romero, Luis; Moreno Llácer, María; Muñoz Perez, David; Navarro Gonzalez, Josep; Poveda, Joaquín; Prades Ibañez, Alberto; Rodriguez Bosca, S.; Rodriguez Rodriguez, D.; Rubio Jiménez, Adrián ; Ruiz Martínez, Arantxa; Sabatini, Paolo , Salt, José; Sanchez Sebastian, Victoria Santra, A.; Sánchez Martínez, Javier; Sayago Galvan, Ivan; Senthilkumar, Varsha ; Soldevila, Urmila; Torró Pastor, Emma; Valero, Alberto; Valls Ferrer, Juan Antonio; Valiente Moreno, Enrique ; Villaplana Pérez, Miguel , Varriale, Lorenzo; Vos, Marcel; ATLAS CollaborationThis paper presents updated Monte Carlo configurations used to model the production of single electroweak vector bosons (W, Z/γ) in association with jets in proton-proton collisions for the ATLAS experiment at the Large Hadron Collider. Improvements pertaining to the electroweak input scheme, parton-shower splitting kernels and scale-setting scheme are shown for multi-jet merged configurations accurate to next-to-leading order in the strong and electroweak couplings. The computational resources required for these set-ups are assessed, and approximations are introduced resulting in a factor three reduction of the per-event CPU time without affecting the physics modelling performance. Continuous statistical enhancement techniques are introduced by ATLAS in order to populate low cross-section regions of phase space and are shown to match or exceed the generated effective luminosity. This, together with the lower per-event CPU time, results in a 50% reduction in the required computing resources compared to a legacy set-up previously used by the ATLAS collaboration. The set-ups described in this paper will be used for future ATLAS analyses and lay the foundation for the next generation of Monte Carlo predictions for single vector-boson plus jets production. [Figure not available: see fulltext.]
Description of atmospheric conditions at the Pierre Auger Observatory using the Global Data Assimilation System (GDAS)
No full textAtmospheric conditions at the site of a cosmic ray observatory must be known for reconstructing observed extensive air showers. The Global Data Assimilation System (GDAS) is a global atmospheric model predicated on meteorological measurements and numerical weather predictions. GDAS provides altitude-dependent profiles of the main state variables of the atmosphere like temperature, pressure, and humidity. The original data and their application to the air shower reconstruction of the Pierre Auger Observatory are described. By comparisons with radiosonde and weather station measurements obtained on-site in Malargüe and averaged monthly models, the utility of the GDAS data is shown. © 2012 Elsevier B.V. All rights reserved.The Pierre Auger Collaboration... K. B. Barber... J. A. Bellido... R. W. Clay... M. J. Cooper... B. R. Dawson... T. A. Harrison... A. E. Herve... V. C. Holmes... J. Sorokin... P. Wahrlich... B. J. Whelan... et al
Performance of the joint LST-1 and MAGIC observations evaluated with Crab Nebula data
No full textFull list of the authors: Abe, H.; Abe, K.; Abe, S.; Acciari, V. A.; Aguasca-Cabot, A.; Agudo, I.; Alvarez Crespo, N.; Aniello, T.; Ansoldi, S.; Antonelli, L. A.; Aramo, C.; Arbet-Engels, A.; Arcaro, C.; Artero, M.; Asano, K.; Aubert, P.; Baack, D.; Babić, A.; Baktash, A.; Bamba, A.; Baquero Larriva, A.; Baroncelli, L.; Barres de Almeida, U.; Barrio, J. A.; Batković, I.; Baxter, J.; Becerra González, J.; Bednarek, W.; Bernardini, E.; Bernardos, M. I.; Bernete Medrano, J.; Berti, A.; Besenrieder, J.; Bhattacharjee, P.; Biederbeck, N.; Bigongiari, C.; Biland, A.; Bissaldi, E.; Blanch, O.; Bonnoli, G.; Bordas, P.; Bošnjak, Ž.; Bulgarelli, A.; Burelli, I.; Burmistrov, L.; Buscemi, M.; Busetto, G.; Campoy Ordaz, A.; Cardillo, M.; Caroff, S.; Carosi, A.; Carosi, R.; Carrasco, M. S.; Carretero-Castrillo, M.; Cassol, F.; Castro-Tirado, A. J.; Cauz, D.; Cerasole, D.; Ceribella, G.; Chai, Y.; Cheng, K.; Chiavassa, A.; Chikawa, M.; Chytka, L.; Cifuentes, A.; Cikota, S.; Colombo, E.; Contreras, J. L.; Cornelia, A.; Cortina, J.; Costantini, H.; Covino, S.; D'Amico, G.; D'Elia, V.; Da Vela, P.; Dalchenko, M.; Dazzi, F.; De Angelis, A.; de Bony de Lavergne, M.; De Lotto, B.; De Lucia, M.; de Menezes, R.; Del Peral, L.; Del Popolo, A.; Deleglise, G.; Delfino, M.; Delgado Mendez, C.; Delgado Mengual, J.; della Volpe, D.; Dellaiera, M.; Depaoli, D.; De Angelis, A.; Di Piano, A.; Di Pierro, F.; Di Pilato, A.; Di Tria, R.; Di Venere, L.; Dominik, R. M.; Dominis Prester, D.; Donini, A.; Dorner, D.; Doro, M.; Díaz, C.; Eisenberger, L.; Elsässer, D.; Emery, G.; Escudero, J.; Fallah Ramazani, V.; Fariña, L.; Fattorini, A.; Ferrara, G.; Ferrarotto, F.; Fiasson, A.; Foffano, L.; Font, L.; Freixas Coromina, L.; Fröse, S.; Fukami, S.; Fukazawa, Y.; Garcia López, R. J.; Garcia, E.; Garczarczyk, M.; García López, R. J.; Gasbarra, C.; Gasparrini, D.; Gasparyan, S.; Gaug, M.; Geyer, D.; Giesbrecht Paiva, J. G.; Giglietto, N.; Giordano, F.; Gliwny, P.; Godinović, N.; Grau, R.; Green, D.; Green, J. G.; Gunji, S.; Günther, P.; Hackfeld, J.; Hadasch, D.; Hahn, A.; Hashiyama, K.; Hassan, T.; Hayashi, K.; Heckmann, L.; Heller, M.; Herrera Llorente, J.; Hirotani, K.; Hoffmann, D.; Horns, D.; Houles, J.; Hrabovsky, M.; Hrupec, D.; Hui, D.; Hütten, M.; Iarlori, M.; Imazawa, R.; Inada, T.; Inome, Y.; Ioka, K.; Iori, M.; Iotov, R.; Ishio, K.; Jacquemont, M.; Jiménez Martínez, I.; Jobst, E.; Jormanainen, J.; Jurysek, J.; Kagaya, M.; Karas, V.; Katagiri, H.; Kataoka, J.; Kerszberg, D.; Kluge, G. W.; Kobayashi, Y.; Kohri, K.; Kong, A.; Kouch, P. M.; Kubo, H.; Kushida, J.; Lainez, M.; Lamanna, G.; Lamastra, A.; Le Flour, T.; Leone, F.; Lindfors, E.; Linhoff, L.; Linhoff, M.; Lombardi, S.; Longo, F.; Loporchio, S.; Lorini, A.; Lozano Bahilo, J.; Luque-Escamilla, P. L.; Lyard, E.; Láinez Lezáun, M.; López-Coto, R.; López-Moya, M.; López-Oramas, A.; Machado de Oliveira Fraga, B.; Majumdar, P.; Makariev, M.; Mandat, D.; Maneva, G.; Manganaro, M.; Mangano, S.; Mang, N.; Manicò, G.; Mannheim, K.; Mariotti, M.; Marquez, P.; Marsella, G.; Martinez, O.; Martínez, G.; Martínez, M.; Martí, J.; Mas-Aguilar, A.; Maurin, G.; Mazin, D.; Menchiari, S.; Mender, S.; Mestre Guillen, E.; Micanovic, S.; Miceli, D.; Miener, T.; Miranda, J. M.; Mirzoyan, R.; Mizuno, T.; Mićanović, S.; Molero González, M.; Molina, E.; Mondal, H. A.; Montaruli, T.; Monteiro, I.; Moralejo, A.; Morcuende, D.; Morselli, A.; Moya, V.; Muraishi, H.; Murase, K.; Nagataki, S.; Nakamori, T.; Nanci, C.; Neronov, A.; Neustroev, V.; Nickel, L.; Nievas Rosillo, M.; Nigro, C.; Nikolić, L.; Nilsson, K.; Nishijima, K.; Njoh Ekoume, T.; Noda, K.; Nosek, D.; Nozaki, S.; Ohishi, M.; Ohtani, Y.; Oka, T.; Okumura, A.; Orito, R.; Otero-Santos, J.; Paiano, S.; Palatiello, M.; Paneque, D.; Pantaleo, F. R.; Paoletti, R.; Paredes, J. M.; Pavletić, L.; Pech, M.; Pecimotika, M.; Peresano, M.; Persic, M.; Pfeiffle, F.; Pietropaolo, E.; Pihet, M.; Pirola, G.; Plard, C.; Podobnik, F.; Poireau, V.; Polo, M.; Pons, E.; Prada Moroni, P. G.; Prandini, E.; Prast, J.; Principe, G.; Priyadarshi, C.; Prouza, M.; Rando, R.; Rhode, W.; Ribó, M.; Rico, J.; Righi, C.; Rizi, V.; Rodriguez Fernandez, G.; Rodríguez Frías, M. D.; Sahakyan, N.; Saito, T.; Sakurai, S.; Sanchez, D. A.; Satalecka, K.; Sato, M.; Sato, Y.; Saturni, F. G.; Savchenko, V.; Schleicher, B.; Schmidt, K.; Schmuckermaier, F.; Schubert, J. L.; Schussler, F.; Schweizer, T.; Sciaccaluga, A.; Siegert, T.; Silvia, R.; Sitarek, J.; Sliusar, V.; Sobczynska, D.; Spolon, A.; Stamerra, A.; Strišković, J.; Strom, D.; Strzys, M.; Suda, Y.; Suutarinen, S.; Šarić, T.; Tajima, H.; Takahashi, H.; Takahashi, M.; Takata, J.; Takeishi, R.; Tam, P. H. T.; Tanaka, S. J.; Tateishi, D.; Tavecchio, F.; Temnikov, P.; Terada, Y.; Terauchi, K.; Terzić, T.; Teshima, M.; Tluczykont, M.; Tokanai, F.; Torres, D. F.; Tosti, L.; Travnicek, P.; Truzzi, S.; Tutone, A.; Ubach, S.; Vacula, M.; Vallania, P.; van Scherpenberg, J.; Vazquez Acosta, M.; Ventura, S.; Verguilov, V.; Viale, I.; Vigliano, A.; Vigorito, C. F.; Visentin, E.; Vitale, V.; Voutsinas, G.; Vovk, I.; Vuillaume, T.; Vázquez Acosta, M.; Walter, R.; Wei, Z.; Will, M.; Yamamoto, T.; Yamazaki, R.; Yoshida, T.; Yoshikoshi, T.; Zywucka, N.Aims. Large-Sized Telescope 1 (LST-1), the prototype for the Large-Sized Telescope at the upcoming Cherenkov Telescope Array Observatory, is concluding its commissioning phase at the Observatorio del Roque de los Muchachos on the island of La Palma. The proximity of LST-1 to the two MAGIC (Major Atmospheric Gamma Imaging Cherenkov) telescopes makes it possible to carry out observations of the same gamma-ray events with both systems.
Methods. We describe the joint LST-1+MAGIC analysis pipeline and used simultaneous Crab Nebula observations and Monte Carlo simulations to assess the performance of the three-telescope system. The addition of the LST-1 telescope allows for the recovery of events in which one of the MAGIC images is too dim to survive analysis quality cuts.
Results. Thanks to the resulting increase in the collection area and stronger background rejection, we found a significant improvement in sensitivity, allowing for the detection of 30% weaker fluxes in the energy range between 200 GeV and 3 TeV. The spectrum of the Crab Nebula, reconstructed in the energy range between similar to 60 GeV and similar to 10 TeV, is in agreement with previous measurements. © The Authors 2023.We gratefully acknowledge financial support from the following agencies and organisations: Ministry of Education, Youth and Sports, MEYS LM2015046, LM2018105, LTT17006, EU/MEYS CZ.02.1.01/0.0/0.0/16_013/0001403, CZ.02.1.01/0.0/0.0/18_046/0016007 and CZ.02.1.01/0.0/0.0/16_019/0000754, Czech Republic; Max Planck Society, German Bundesministerium fur Bildung und Forschung (Verbundforschung/ErUM), Deutsche Forschungsgemeinschaft (SFBs 876 and 1491), Germany; Istituto Nazionale di Astrofisica (INAF), Istituto Nazionale di Fisica Nucleare (INFN), Italian Ministry for University and Research (MUR); ICRR, University of Tokyo, JSPS, MEXT, Japan; JST SPRING -JPMJSP2108; Narodowe Centrum Nauki, grant number 2019/34/E/ST9/00224, Poland; The Spanish groups acknowledge the Spanish Ministry of Science and Innovation and the Spanish Research State Agency (AEI) through the government budget lines PGE2021/28.06.000X.411.01, PGE2022/28.06.000X.411.01 and PGE2022/28.06.000X.711.04, and grants PGC2018-095512-B-I00, PID2019-104114RB-C31, PID2019-107847RB-C44, PID2019-104114RB-C32, PID2019-105510GB-C31, PID2019-104114RB-C33, PID2019-107847RB-C41, PID2019-107847RB-C43, PID2019-107988GB-C22; the "Centro de Excelencia Severo Ochoa" program through grants no. CEX2021-001131-S, CEX2019-000920S; the "Unidad de Excelencia Maria de Maeztu" program through grants no. CEX2019-000918-M, CEX2020-001058-M; the "Juan de la CiervaIncorporacion" program through grant no. IJC2019-040315-I. They also acknowledge the "Programa Operativo" FEDER 2014-2020, Consejeria de Economia y Conocimiento de la Junta de Andalucia (Ref. 1257737), PAIDI 2020 (Ref. P18-FR-1580) and Universidad de Jaen; "Programa Operativo de Crecimiento Inteligente" FEDER 2014-2020 (Ref. ESFRI-2017-IAC-12), Ministerio de Ciencia e Innovacion, 15% co-financed by Consejeria de Economia, Industria, Comercio y Conocimiento del Gobierno de Canarias; the "CERCA" program of the Generalitat de Catalunya; and the European Union's "Horizon 2020" GA:824064 and NextGenerationEU; We acknowledge the Ramon y Cajal program through grant RYC-2020-028639-I and RYC-2017-22665; State Secretariat for Education, Research and Innovation (SERI) and Swiss National Science Foundation (SNSF), Switzerland; The research leading to these results has received funding from the European Union's Seventh Framework Programme (FP7/2007-2013) under grant agreements No 262053 and No 317446. This project is receiving funding from the European Union's Horizon 2020 research and innovation programs under agreement No 676134. ESCAPE -The European Science Cluster of Astronomy & Particle Physics ESFRI Research Infrastructures has received funding from the European Union's Horizon 2020 research and innovation programme under Grant Agreement no. 824064. We would like to thank the Instituto de Astrofisica 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 the Spanish 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 "Maria de Maeztu" program of the Spanish MCIN/AEI/10.13039/501100011033 (SEV-2016-0588, CEX2019-000920-S, CEX2019-000918-M, CEX2021-001131-S, 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 Deutsche Forschungsgemeinschaft (SFB1491 and SFB876); the Polish Ministry Of Education and Science grant No. 2021/WK/08; and by the Brazilian MCTIC, CNPq and FAPERJ. This work was conducted in the context of the CTA LST Project. A. Berti: development and maintenance of the module ctapipe_io_magic, implementation of processing of MAGIC calibrated data within magic-cta-pipe, general maintenance of the magic-cta-pipe package; F. Di Pierro: development of the simultaneous observations' database and of the first versions of ctapipe_io_magic, cross-checks with the MARS analysis, coordination of the analysis cross-checks; E. Jobst: implementation of tests for low-level comparison of shower images and parameters for MAGIC-only analysis, upgrade of ctapipe_io_magic to new releases of ctapipe, test of magic-cta-pipe for MAGIC-only analysis; Y. Ohtani: responsible for most of magic-cta-pipe analysis code, many tests and optimization of the pipeline, calculation of performance parameters; J. Sitarek: reoptimization and processing of Monte Carlo simulations, calculation of performance parameters, paper drafting; Y. Suda: contribution to the first iteration of implementation of MAGIC to sim_telarray and coordinating the group from the MAGIC side together with F. Di Pierro; E. Visentin: performance parameters cross-check analysis. The rest of the authors have contributed in one or several of the following ways: design, construction, maintenance and operation of the instrument(s); preparation and/or evaluation of the observation proposals; data acquisition, processing, calibration and/or reduction; production of analysis tools and/or related Monte Carlo simulations; discussion and approval of the contents of the draft. J.S. would like to thank ICRR for excellent working conditions during final stages of preparation of this manuscript. Y.S.' work was supported by JSPS KAKENHI Grant Number JP21K20368 and JP23K13127. The authors would like to thank anonymous journal referee for the feedback which helped to improve the paper.Peer reviewe
Large-scale distribution of arrival directions of cosmic rays detected above 10(18) ev at the Pierre Auger observatory
No full textA thorough search for large-scale anisotropies in the distribution of arrival directions of cosmic rays detected above 10¹⁸ eV at the Pierre Auger Observatory is presented. This search is performed as a function of both declination and right ascension in several energy ranges above 10¹⁸ eV, and reported in terms of dipolar and quadrupolar coefficients. Within the systematic uncertainties, no significant deviation from isotropy is revealed. Assuming that any cosmic-ray anisotropy is dominated by dipole and quadrupole moments in this energy range, upper limits on their amplitudes are derived. These upper limits allow us to test the origin of cosmic rays above 10¹⁸ eV from stationary Galactic sources densely distributed in the Galactic disk and predominantly emitting light particles in all directions.The Pierre Auger Collaboration, P. Abreu ... K. B. Barber ... J. A. Bellido ... R. W. Clay ... M. J. Cooper ... B. R. Dawson ... T. A. Harrison ... A. E. Herve, G. C. Hill ... V. C. Holmes ... J. Sorokin ... P. Wahrlich ... B. J. Whelan ... et al
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