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Searching for gravitational wave optical counterparts with the Zwicky Transient Facility: summary of O4a

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arXiv 2024年

作者： Ahumada, Tomás Anand, Shreya Coughlin, Michael W. Gupta, Vaidehi Kasliwal, Mansi M. Karambelkar, Viraj R. Stein, Robert D. Waratkar, Gaurav Swain, Vishwajeet Jegou du Laz, Theophile Anumarlapudi, Akash Andreoni, Igor bulla, Mattia Srinivasaragavan, Gokul P. Toivonen, Andrew Wold, Avery bellm, eric C. Cenko, S. bradley Kaplan, David L. Sollerman, Jesper bhalerao, Varun Perley, Daniel Salgundi, Anirudh Suresh, Aswin Hinds, K.-Ryan Reusch, Simeon Necker, Jannis Cook, David O. Pletskova, Natalya Singer, Leo P. banerjee, Smaranika barna, Tyler Copperwheat, Christopher M. Healy, brian Kiendrebeogo, R. Weizmann Kumar, Harsh Kumar, Ravi Pezzella, Marianna Sagués-Carracedo, Ana Sravan, Niharika bloom, Joshua S. Chen, Tracy X. Graham, Matthew Helou, George Laher, Russ R. Mahabal, Ashish A. Purdum, Josiah Anupama, G.C. barway, Sudhanshu basu, Judhajeet Raman, Dhananjay Roychowdhury, Tamojeet Division of Physics Mathematics and Astronomy California Institute of Technology PasadenaCA91125 United States School of Physics and Astronomy University of Minnesota MinneapolisMN55455 United States Department of Physics Indian Institute of Technology West Bengal Kharagpur721302 India Department of Physics Indian Institute of Technology Bombay Powai 400 076 India Department of Physics University of Wisconsin-Milwaukee P.O. Box 413 MilwaukeeWI53201 United States Joint Space-Science Institute University of Maryland College ParkMD20742 United States Department of Astronomy University of Maryland College ParkMD20742 United States Astrophysics Science Division NASA Goddard Space Flight Center MC 661 GreenbeltMD20771 United States Department of Physics and Earth Science University of Ferrara via Saragat 1 FerraraI-44122 Italy INFN Sezione di Ferrara via Saragat 1 FerraraI-44122 Italy INAF Osservatorio Astronomico d’Abruzzo via Mentore Maggini snc Teramo64100 Italy IPAC California Institute of Technology 1200 E. California Blvd PasadenaCA91125 United States DIRAC Institute Department of Astronomy University of Washington 3910 15th Avenue NE SeattleWA98195 United States The Oskar Klein Centre Department of Astronomy Albanova Stockholm University StockholmSE-106 91 Sweden Astrophysics Research Institute Liverpool John Moores University IC2 Liverpool Science Park 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Deutsches Elektronen-Synchrotron DESY Platanenallee 6 Zeuthen15738 Germany Department of Physics Drexel University PhiladelphiaPA19104 United States Astrophysics Research Institute IC2 Liverpool Science Park 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Laboratoire de Physique et de Chimie de l’Environnement Université Joseph KI-ZERBO Ouagadougou Burkina Faso Artemis Observatoire de la Côte d’Azur Université Côte d’Azur Boulevard de l’Observatoire NiceF-06304 France Department of Physics Indian Institute o

During the first half of the fourth ob.erving run (O4a) of the International Gravitational Wave Network (IGWN), the Zwicky Transient Facility (ZTF) conducted a systematic search for kilonova (KN) counterparts to binary neutron star (bNS) and neutron star–black hole (NSbH) merger candidates. Here, we present a comprehensive study of the five high-significance (False Alarm Rate less than 1 per year) bNS and NSbH candidates in O4a. Our follow-up campaigns relied on both target-of-opportunity ob.ervations (ToO) and re-weighting of the nominal survey schedule to maximize coverage. We describe the toolkit we have b.en developing, Fritz, an instance of SkyPortal, instrumental in coordinating and managing our telescope scheduling, candidate vetting, and follow-up ob.ervations through a user-friendly interface. ZTF covered a total of 2841 deg2 within the skymaps of the high-significance GW events, reaching a median depth of g ≈ 20.2 mag. We circulated 15 candidates, but found no viab.e KN counterpart to any of the GW events. based on the ZTF non-detections of the high-significance events in O4a, we used a bayesian approach, nimbus, to quantify the posterior probability of KN model parameters that are consistent with our non-detections. Our analysis favors KNe with initial absolute magnitude fainter than -16 mag. The joint posterior probability of a GW170817-like KN associated with all our O4a follow-ups was 64%. Additionally, we use a survey simulation software, simsurvey, to determine that our combined filtered efficiency to detect a GW170817-like KN is 36%, when considering the 5 confirmed astrophysical events in O3 (1 bNS and 4 NSbH events), along with our O4a follow-ups. Following Kasliwal et al. (2020), we derived joint constraints on the underlying KN luminosity function based on our O3 and O4a follow-ups, determining that no more than 76% of KNe fading at 1 mag day-1 can peak at a magnitude brighter than -17.5 mag. Copyright © 2024, The Authors. All rights reserved.

关键词： Gravity waves

The ALMA RebeLS Survey: Discovery of a massive, highly star-forming and morphologically complex ULIRG at z = 7.31

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arXiv 2023年

作者： Hygate, A.P.S. Hodge, J.A. da Cunha, e. Rybak, M. Schouws, S. Inami, H. Stefanon, M. Graziani, L. Schneider, R. Dayal, P. bouwens, R.J. Smit, R. bowler, R.A.A. endsley, R. Gonzalez, V. Oesch, P.A. Stark, D.P. Algera, H.S.b. Aravena, M. barrufet, L. Ferrara, A. Fudamoto, Y. Hilhorst, J.H.A. De Looze, I. Nanayakkara, T. Pallottini, A. Riechers, D.A. Sommovigo, L. Topping, M.W. van der Werf, P. Leiden Observatory Leiden University P.O. Box 9513 Leiden2300 RA Netherlands International Centre for Radio Astronomy Research University of Western Australia 35 Stirling Hwy Crawley26WA 6009 Australia 2601 Australia Faculty of Electrical Engineering Mathematics and Computer Science Delft University of Technology Delft Netherlands Hiroshima Astrophysical Science Center Hiroshima University 1-3-1 Kagamiyama Higashi-Hiroshima Hiroshima739-8526 Japan Departament d’Astronomia i Astrofísica Universitat de València C. Dr. Moliner 50 Burjassot ValènciaE-46100 Spain Dipartimento di Fisica Sapienza Università di Roma Piazzale Aldo Moro 5 RomaI-00185 Italy INAF Osservatorio Astrofisico di Arcetri Largo E. Fermi 5 FirenzeI-50125 Italy Sapienza School for Advanced Studies Viale Regina Elena 291 RomaI-00161 Italy INAF/Osservatorio Astronomico di Roma via Frascati 33 Monte Porzio Catone RomaI-00078 Italy Istituto Nazionale di Fisica Nucleare Sezione di Roma1 Piazzale Aldo Moro 2 RomaI-00185 Italy Jodrell Bank Centre for Astrophysics Department of Physics and Astronomy School of Natural Sciences The University of Manchester ManchesterM13 9PL United Kingdom Steward Observatory University of Arizona 933 N Cherry Ave TucsonAZ85721 United States Departmento de Astronomia Universidad de Chile Casilla 36-D Santiago7591245 Chile Camino del Observatorio 1515 Las Condes Santiago7591245 Chile Observatoire de Genève VersoixCH-1290 Switzerland Niels Bohr Institute University of Copenhagen Jagtvej 128 København NDK-2200 Denmark National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo Japan Nucleo de Astronomia Facultad de Ingenieria y Ciencias Universidad Diego Portales Av. Ejercito 441 Santiago Chile Scuola Normale Superiore Piazza dei Cavalieri 7 PisaI- 50126 Italy Waseda Research Institute for Science and Engineering Faculty of Science and Engineering Waseda University 3-4-1 Okubo Shinjuku Tokyo169-8555 Japan Sterrenkun

We present Atacama Large Millimeter/Submillimeter Array (ALMA) [Cii] and ∼ 158μm continuum ob.ervations of RebeLS-25, a massive, morphologically complex ultra-luminous infrared galaxy (ULIRG;LIR = 1.5+−00.85 × 1012 L) at z = 7.31, spectroscopically confirmed by the Reionization era bright emission Line Survey (RebeLS) ALMA Large Programme. RebeLS-25 has a significant stellar mass of M∗ = 8+−42 × 109 M . From dust-continuum and ultraviolet ob.ervations, we determine a total obscured + unobscured star formation rate of SFR = 199+−10163 M yr−1. This is about four times the SFR estimated from an extrapolated main-sequence. We also infer a [Cii]-based molecular gas mass of MH2 = 5.1+−52.16 × 1010 M, implying a molecular gas depletion time of tdepl,H2 = 0.3+−00.32 Gyr. We ob.erve a [Cii] velocity gradient consistent with disc rotation, but given the current resolution we cannot rule out a more complex velocity structure such as a merger. The spectrum exhibits excess [Cii] emission at large positive velocities (∼ 500 km s−1), which we interpret as either a merging companion or an outflow. In the outflow scenario, we derive a lower limit of the mass outflow rate of 200 M yr−1, which is consistent with expectations for a star formation-driven outflow. Given its large stellar mass, SFR and molecular gas reservoir ∼ 700 Myr after the big bang, we explore the future evolution of RebeLS-25. Considering a simple, conservative model assuming an exponentially declining star formation history, constant star formation efficiency, and no additional gas inflow, we find that RebeLS-25 has the potential to evolve into a galaxy consistent with the properties of high-mass quiescent galaxies recently ob.erved at z ∼ 4. Copyright © 2023, The Authors. All rights reserved.

关键词： Galaxies

Comparison of the atmospheric muon flux measured by the KM3NeT detectors with the CORSIKA simulation using the Global Spline Fit model

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Comparison of the atmospheric muon flux measured by the KM3N...

38th International Cosmic Ray Conference, ICRC 2023

作者： Romanov, Andrey Kalaczynski, Piotr Aiello, S. Albert, A. Alves Garre, S. Aly, Z. Ambrosone, A. Ameli, F. Andre, M. Androutsou, e. Anguita, M. Aphecetche, L. Ardid, M. Ardid, S. Atmani, H. Aublin, J. bailly-Salins, L. bardačová, Z. baret, b. bariego-Quintana, A. basegmez du Pree, S. becherini, Y. bendahman, M. benfenati, F. benhassi, M. benoit, D.M. berb.e, e. bertin, V. biagi, S. b.ettcher, M. bonanno, D. boumaaza, J. bouta, M. bouwhuis, M. bozza, C. bozza, R.M. brânzaş, H. b.etaudeau, F. bruijn, R. brunner, J. bruno, R. buis, e. buompane, R. busto, J. Caiffi, b. Calvo, D. Campion, S. Capone, A. Carenini, F. Carretero, V. Cartraud, T. Castaldi, P. Cecchini, V. Celli, S. Cerisy, L. Chabab, M. Chadolias, M. Chen, A. Cherubini, S. Chiarusi, T. Circella, M. Cocimano, R. Coelho, J.A.b. Coleiro, A. Coniglione, R. Coyle, P. Creusot, A. Cruz, A. Cuttone, G. Dallier, R. Darras, Y. De benedittis, A. De Martino, b. Decoene, V. Del burgo, R. Di Cerbo, U.M. Di Mauro, L.S. Di Palma, I. Díaz, A.F. Diaz, C. Diego-Tortosa, D. Distefano, C. Domi, A. Donzaud, C. Dornic, D. Dörr, M. Drakopoulou, e. Drouhin, D. Dvornický, R. eberl, T. eckerová, e. eddymaoui, A. van eeden, T. eff, M. van eijk, D. el bojaddaini, I. el Hedri, S. enzenhöfer, A. Ferrara, G. Filipović, M.D. Filippini, F. Franciotti, D. Fusco, L.A. Gabriel, J. Gagliardini, S. Gal, T. García Méndez, J. Garcia Soto, A. Gatius Oliver, C. Geißelb.echt, N. Ghaddari, H. Gialanella, L. Gibson, b.K. Giorgio, e. Goos, I. Goupilliere, D. Gozzini, S.R. Gracia, R. Graf, K. Guidi, C. Guillon, b. Gutiérrez, M. van Haren, H. Heijb.er, A. Hekalo, A. Hennig, L. Hernández-Rey, J.J. Huang, F. Idrissi Ibnsalih, W. Illuminati, G. James, C.W. de Jong, M. de Jong, P. Jung, b.J. Kalaczyński, P. Kalekin, O. Katz, U.F. Khan Chowdhury, N.R. Khatun, A. Kistauri, G. Kopper, C. Kouchner, A. Kulikovskiy, V. Kvatadze, R. Labalme, M. Lahmann, R. Larosa, G. Lastoria, C. Lazo, A. Le Stum, S. Lehaut, G. Dipartimento di Fisica dell’Università di Genova Via Dodecaneso 33 Genova16146 Italy INFN - Sezione di Genova Via Dodecaneso 33 Genova16146 Italy National Centre for Nuclear Research Warsaw02-093 Poland Nicolaus Copernicus Astronomical Center Polish Academy of Sciences Particle Astrophysics Science and Technology Centre Rektorska 4 Warsaw00-614 Poland INFN Sezione di Catania Via Santa Sofia 64 Catania95123 Italy Université de Strasbourg CNRS IPHC UMR 7178 StrasbourgF-67000 France IFIC - Instituto de Física Corpuscular CSIC Universitat de València c/Catedrático José Beltrán 2 Paterna Valencia46980 Spain Aix Marseille Univ CNRS IN2P3 CPPM Marseille France INFN Sezione di Napoli Complesso Universitario di Monte S. Angelo Via Cintia ed. G Napoli80126 Italy Università di Napoli "Federico II" Dip. Scienze Fisiche "E. Pancini" Complesso Universitario di Monte S. Angelo Via Cintia ed. G Napoli80126 Italy INFN Sezione di Roma Piazzale Aldo Moro 2 Roma00185 Italy Universitat Politècnica de Catalunya Laboratori d’Aplicacions Bioacústiques Centre Tecnològic de Vilanova i la Geltrú Avda. Rambla Exposició s/n Vilanova i la Geltrú08800 Spain NCSR Demokritos Institute of Nuclear and Particle Physics Ag. Paraskevi Attikis Athens15310 Greece University of Granada Dept. of Computer Architecture and Technology CITIC Granada18071 Spain Subatech IMT Atlantique IN2P3-CNRS Université de Nantes 4 rue Alfred Kastler - La Chantrerie BP 20722 Nantes44307 France Universitat Politècnica de València Instituto de Investigación para la Gestión Integrada de las Zonas Costeras C/ Paranimf 1 Gandia46730 Spain University Mohammed V in Rabat Faculty of Sciences 4 av. Ibn Battouta B.P. 1014 RabatR.P. 10000 Morocco Université Paris Cité CNRS Astroparticule et Cosmologie ParisF-75013 France LPC CAEN Normandie Univ ENSICAEN UNICAEN CNRS IN2P3 6 boulevard Maréchal Juin Caen14050 France Czech Technical University in Prague Institute of Experimental a

Atmospheric muons are the dominant component of the down-going events for the KM3NeT neutrino telescopes. Deep underwater measurements of muons provide important information about the cosmic ray properties. The KM3NeT research infrastructure includes two telescopes currently in operation while still being under construction in the Mediterranean Sea. The KM3NeT/ORCA detector is deployed at 2450 m depth near Toulon, France. The KM3NeT/ARCA telescope is located at 3500 m depth off-shore Capo Passero, Italy. In this work, the measured atmospheric muon flux is compared to the Monte Carlo simulation using the CORSIKA package with the Sibyll 2.3d model for high-energy hadronic interactions and the GSF model for mass composition. The data from both KM3NeT/ORCA and KM3NeT/ARCA telescopes are considered for this analysis. In the current configuration, KM3NeT/ORCA covers cosmic ray energy range from several TeV up to hundreds of TeV per nucleon, while for KM3NeT/ARCA the range is from several TeV up to PeV per nucleon. Systematic uncertainties considered for the analysis include that on the cosmic ray flux normalization and its composition, water properties, detector response, and high-energy hadronic interaction models. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Hadrons

energy-Dependent expectations for the Full KM3NeT/ARCA Detector: Application to Starburst Galaxies 38

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Energy-Dependent Expectations for the Full KM3NeT/ARCA Detec...

38th International Cosmic Ray Conference, ICRC 2023

作者： Ibnsalih, W.I. Ambrosone, A. Marinelli, A. Miele, G. Migliozzi, P. Musone, M.R. Aiello, S. Albert, A. Alves Garre, S. Aly, Z. Ambrosone, A. Ameli, F. Andre, M. Androutsou, e. Anguita, M. Aphecetche, L. Ardid, M. Ardid, S. Atmani, H. Aublin, J. bailly-Salins, L. bardačová, Z. baret, b. bariego-Quintana, A. basegmez du Pree, S. becherini, Y. bendahman, M. benfenati, F. benhassi, M. benoit, D.M. berb.e, e. bertin, V. biagi, S. b.ettcher, M. bonanno, D. boumaaza, J. bouta, M. bouwhuis, M. bozza, C. bozza, R.M. brânzaş, H. b.etaudeau, F. bruijn, R. brunner, J. bruno, R. buis, e. buompane, R. busto, J. Caiffi, b. Calvo, D. Campion, S. Capone, A. Carenini, F. Carretero, V. Cartraud, T. Castaldi, P. Cecchini, V. Celli, S. Cerisy, L. Chabab, M. Chadolias, M. Chen, A. Cherubini, S. Chiarusi, T. Circella, M. Cocimano, R. Coelho, J.A.b. Coleiro, A. Coniglione, R. Coyle, P. Creusot, A. Cruz, A. Cuttone, G. Dallier, R. Darras, Y. De benedittis, A. De Martino, b. Decoene, V. Del burgo, R. Di Cerbo, U.M. Di Mauro, L.S. Di Palma, I. Díaz, A.F. Diaz, C. Diego-Tortosa, D. Distefano, C. Domi, A. Donzaud, C. Dornic, D. Dörr, M. Drakopoulou, e. Drouhin, D. Dvornický, R. eberl, T. eckerová, e. eddymaoui, A. van eeden, T. eff, M. van eijk, D. el bojaddaini, I. el Hedri, S. enzenhöfer, A. Ferrara, G. Filipović, M.D. Filippini, F. Franciotti, D. Fusco, L.A. Gabriel, J. Gagliardini, S. Gal, T. García Méndez, J. Garcia Soto, A. Gatius Oliver, C. Geißelb.echt, N. Ghaddari, H. Gialanella, L. Gibson, b.K. Giorgio, e. Goos, I. Goupilliere, D. Gozzini, S.R. Gracia, R. Graf, K. Guidi, C. Guillon, b. Gutiérrez, M. van Haren, H. Heijb.er, A. Hekalo, A. Hennig, L. Hernández-Rey, J.J. Huang, F. Idrissi Ibnsalih, W. Illuminati, G. James, C.W. de Jong, M. de Jong, P. Jung, b.J. Kalaczyński, P. Kalekin, O. Katz, U.F. Khan Chowdhury, N.R. Khatun, A. Kistauri, G. Kopper, C. Kouchner, A. Kulikovskiy, V. Kvatadze, R. Labalme, M. Lahmann, R. Dipartimento di Fisica "Ettore Pancini" Università degli studi di Napoli "Federico II" Complesso Univ. Monte S. Angelo NapoliI-80126 Italy INFN - Sezione di Napoli Complesso Univ. Monte S. Angelo NapoliI-80126 Italy Università degli studi della Campania Luigi Vanvitelli Italy Scuola Superiore Meridionale Università degli studi di Napoli "Federico II" Largo San Marcellino 10 Napoli80138 Italy INAF-Osservatorio Astronomico di Capodimonte Salita Moiariello 16 NaplesI-80131 Italy INFN Sezione di Catania Via Santa Sofia 64 Catania95123 Italy Université de Strasbourg CNRS IPHC UMR 7178 StrasbourgF-67000 France c/Catedrático José Beltrán 2 Paterna Valencia46980 Spain Aix Marseille Univ CNRS IN2P3 CPPM Marseille France INFN Sezione di Napoli Complesso Universitario di Monte S. Angelo Via Cintia ed. G Napoli80126 Italy Università di Napoli "Federico II" Dip. Scienze Fisiche "E. Pancini" Complesso Universitario di Monte S. Angelo Via Cintia ed. G Napoli80126 Italy INFN Sezione di Roma Piazzale Aldo Moro 2 Roma00185 Italy Universitat Politècnica de Catalunya Laboratori d’Aplicacions Bioacústiques Centre Tecnològic de Vilanova i la Geltrú Avda. Rambla Exposició s/n Vilanova i la Geltrú08800 Spain NCSR Demokritos Institute of Nuclear and Particle Physics Ag. Paraskevi Attikis Athens15310 Greece University of Granada Dept. of Computer Architecture and Technology/CITIC Granada18071 Spain Subatech IMT Atlantique IN2P3-CNRS Université de Nantes 4 rue Alfred Kastler - La Chantrerie BP 20722 Nantes44307 France Universitat Politècnica de València Instituto de Investigación para la Gestión Integrada de las Zonas Costeras C/ Paranimf 1 Gandia46730 Spain University Mohammed V in Rabat Faculty of Sciences 4 av. Ibn Battouta B.P. 1014 R.P. Rabat10000 Morocco Université Paris Cité CNRS Astroparticule et Cosmologie ParisF-75013 France LPC CAEN Normandie Univ ENSICAEN UNICAEN CNRS IN2P3 6 boulevard Maréchal Juin Caen14050 France Czec

The energy-dependent expectations for the full KM3NeT/ARCA detector, both for diffuse and point-like signals are presented. For the diffuse analysis, the 90% C.L. quasi-differential sensitivity for 10 years of the full detector operations is computed, and compared with the IceCube measured diffuse spectrum. The whole energy range ob.ervab.e by ARCA ∼ (1 TeV − 100 PeV) is taken into account, selecting upgoing track-like as well as all-sky cascade-like events. For the point-like analysis, the differential sensitivity for several declinations is computed, selecting upgoing tracks νμ and ν¯μ charge-current interactions. Some particular starburst galaxies (SbGs) are considered such as NGC 1068, the Small Magellanic Cloud (SMC) and Circinus Galaxy. The resulting sensitvities demonstrate the importance of KM3NeT/ARCA to link star-forming processes with high-energy neutrino production within a few years of operation. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Galaxies

Selecting stopping muons with KM3NeT/ORCA 38

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Selecting stopping muons with KM3NeT/ORCA

38th International Cosmic Ray Conference, ICRC 2023

作者： bailly-Salins, Louis Aiello, S. Albert, A. Alves Garre, S. Aly, Z. Ambrosone, A. Ameli, F. Andre, M. Androutsou, e. Anguita, M. Aphecetche, L. Ardid, M. Ardid, S. Atmani, H. Aublin, J. bailly-Salins, L. bardačová, Z. baret, b. bariego-Quintana, A. basegmez du Pree, S. becherini, Y. bendahman, M. benfenati, F. benhassi, M. benoit, D.M. berb.e, e. bertin, V. biagi, S. b.ettcher, M. bonanno, D. boumaaza, J. bouta, M. bouwhuis, M. bozza, C. bozza, R.M. brânzaş, H. b.etaudeau, F. bruijn, R. brunner, J. bruno, R. buis, e. buompane, R. busto, J. Caiffi, b. Calvo, D. Campion, S. Capone, A. Carenini, F. Carretero, V. Cartraud, T. Castaldi, P. Cecchini, V. Celli, S. Cerisy, L. Chabab, M. Chadolias, M. Chen, A. Cherubini, S. Chiarusi, T. Circella, M. Cocimano, R. Coelho, J.A.b. Coleiro, A. Coniglione, R. Coyle, P. Creusot, A. Cruz, A. Cuttone, G. Dallier, R. Darras, Y. De benedittis, A. De Martino, b. Decoene, V. Del burgo, R. Di Cerbo, U.M. Di Mauro, L.S. Di Palma, I. Díaz, A.F. Diaz, C. Diego-Tortosa, D. Distefano, C. Domi, A. Donzaud, C. Dornic, D. Dörr, M. Drakopoulou, e. Drouhin, D. Dvornický, R. eberl, T. eckerová, e. eddymaoui, A. van eeden, T. eff, M. van eijk, D. el bojaddaini, I. el Hedri, S. enzenhöfer, A. Ferrara, G. Filipović, M.D. Filippini, F. Franciotti, D. Fusco, L.A. Gabriel, J. Gagliardini, S. Gal, T. García Méndez, J. Garcia Soto, A. Gatius Oliver, C. Geißelb.echt, N. Ghaddari, H. Gialanella, L. Gibson, b.K. Giorgio, e. Goos, I. Goupilliere, D. Gozzini, S.R. Gracia, R. Graf, K. Guidi, C. Guillon, b. Gutiérrez, M. van Haren, H. Heijb.er, A. Hekalo, A. Hennig, L. Hernández-Rey, J.J. Huang, F. Idrissi Ibnsalih, W. Illuminati, G. James, C.W. de Jong, M. de Jong, P. Jung, b.J. Kalaczyński, P. Kalekin, O. Katz, U.F. Khan Chowdhury, N.R. Khatun, A. Kistauri, G. Kopper, C. Kouchner, A. Kulikovskiy, V. Kvatadze, R. Labalme, M. Lahmann, R. Larosa, G. Lastoria, C. Lazo, A. Le Stum, S. Lehaut, G. Leonora, e. Université de Caen Normandie ENSICAEN CNRS IN2P3 LPC Caen UMR 6534 CaenF-14000 France INFN Sezione di Catania Via Santa Sofia 64 Catania95123 Italy Université de Strasbourg CNRS IPHC UMR 7178 StrasbourgF-67000 France IFIC - Instituto de Física Corpuscular CSIC - Universitat de València c/Catedrático José Beltrán 2 Paterna Valencia46980 Spain Aix Marseille Univ CNRS IN2P3 CPPM Marseille France INFN Sezione di Napoli Complesso Universitario di Monte S. Angelo Via Cintia ed. G Napoli80126 Italy Università di Napoli "Federico II" Dip. Scienze Fisiche "E. Pancini" Complesso Universitario di Monte S. Angelo Via Cintia ed. G Napoli80126 Italy INFN Sezione di Roma Piazzale Aldo Moro 2 Roma00185 Italy Universitat Politècnica de Catalunya Laboratori d’Aplicacions Bioacústiques Centre Tecnològic de Vilanova i la Geltrú Avda. Rambla Exposició s/n Vilanova i la Geltrú08800 Spain NCSR Demokritos Institute of Nuclear and Particle Physics Ag. Paraskevi Attikis Athens15310 Greece University of Granada Dept. of Computer Architecture and Technology CITIC Granada18071 Spain Subatech IMT Atlantique IN2P3-CNRS Université de Nantes 4 rue Alfred Kastler - La Chantrerie BP Nantes20722 44307 France Universitat Politècnica de València Instituto de Investigación para la Gestión Integrada de las Zonas Costeras C/ Paranimf 1 Gandia46730 Spain University Mohammed V in Rabat Faculty of Sciences 4 av. Ibn Battouta B.P. 1014 RabatR.P. 10000 Morocco Université Paris Cité CNRS Astroparticule et Cosmologie ParisF-75013 France LPC CAEN Normandie Univ ENSICAEN UNICAEN CNRS IN2P3 6 boulevard Maréchal Juin Caen14050 France Czech Technical University in Prague Institute of Experimental and Applied Physics Husova 240/5 Prague110 00 Czech Republic Comenius University in Bratislava Department of Nuclear Physics and Biophysics Mlynska dolina F1 Bratislava842 48 Slovakia Nikhef National Institute for Subatomic Physics PO Box 41882 Amsterdam1009 DB N

The KM3NeT collaboration operates two water Cherenkov neutrino telescopes in the Mediterranean sea, ORCA and ARCA. The flux of atmospheric muons produced in cosmic ray air showers forms a background to the main ob.ectives of KM3NeT/ORCA and KM3NeT/ARCA, respectively measuring atmospheric neutrino oscillations and detecting neutrinos from astrophysical sources. A small portion of the atmospheric muons stops inside the detector’s instrumented volume. The stopping muons are 5% of the muons reconstructed using the 6 first strings deployed for ORCA. This still amounts to 1000 events per hour. We present two methods for selecting them, applied on both simulations and data. The first method uses simple cuts on a set of reconstructed variab.es. The second method uses a machine learning model to classify muons as "stopping" or "crossing". both methods allow to reach a high selection purity, close to 95%. Detecting stopping muons can serve many purposes like studying muon decay via the detection of Michel electrons or estimating the flux of atmospheric muons at sea level. This work highlights the accurate reconstruction capabilities of ORCA. The median error on the reconstructed stopping point of selected muons is less than 5 meters, and the median angular deviation is 1°. This is to be compared with the 20 meters horizontal distance between strings and the 9 meters vertical distance between optical modules. Another important result is the excellent agreement between distribution of stopping muons selected in data and in simulations. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Cosmic rays

Deep learning-based automated image segmentation for concrete petrographic analysis

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arXiv 2020年

作者： Song, Yu Huang, Zilong Shen, Chuanyue Shi, Humphrey Lange, David A. Dept. of Civil and Environmental Engineering University of Illinois Urbana-Champaign 2145 Newmark Civil Engineering Bldg 205 N. Mathews UrbanaIL61801 United States IFP Group Beckman Institute University of Illinois Urbana-Champaign 405 N Mathews Ave UrbanaIL61801 United States Dept. of Computer and Information Science University of Oregon 258 Deschutes Hall 1477 E. 13th Ave EugeneOR97403 United States Dept. of Civil and Environmental Engineering University of Illinois Urbana-Champaign 2129b Newmark Civil Engineering Bldg 205 N Mathews UrbanaIL61801 United States

The standard petrography test method for measuring air voids in concrete (ASTM C457) requires a meticulous and long examination of sample phase composition under a stereomicroscope. The high expertise and specialized equipment discourage this test for routine concrete quality control. Though the task can be alleviated with the aid of color-based image segmentation, additional surface color treatment is required. Recently, deep learning algorithms using convolutional neural networks (CNN) have achieved unprecedented segmentation performance on image testing benchmarks. In this study, we investigated the feasibility of using CNN to conduct concrete segmentation without the use of color treatment. The CNN demonstrated a strong potential to process a wide range of concretes, including those not involved in model training. The experimental results showed that CNN outperforms the color-based segmentation by a considerab.e margin, and has comparab.e accuracy to human experts. Furthermore, the segmentation time is reduced to mere seconds. Copyright © 2020, The Authors. All rights reserved.

关键词： Semantic Segmentation

VaTeST III: Validation of 8 Potential Super-earths from TeSS Data

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arXiv 2023年

作者： Mistry, Priyashkumar Prasad, Aniket Maity, Mousam Pathak, Kamlesh Gharat, Sarvesh Lekkas, Georgios bhattarai, Surendra Kumar, Dhruv Lissauer, Jack J. Twicken, Joseph D. Soubkiou, Ab.erahmane Pozuelos, Francisco J. Jenkins, Jon Horne, Keith Giacalone, Steven barkaoui, Khalid Timmermans, Mathilde Watkins, Cristilyn N. Sefako, Ramotholo Collins, Karen A. Ciardi, David R. Clark, Catherine A. Safonov, boris S. Shporer, Avi Schlieder, Joshua e. benkhaldoun, Zouhair Stockdale, Chris Ziegler, Carl Gilbert, emily A. Jehin, emmanuël Murgas, Felipe Crossfield, Ian J.M. Paegert, Martin Lund, Michael b. Narita, Norio Schwarz, Richard P. Goeke, Robert F. Fajardo-Acosta, Sergio b. Howell, Steve b. Tan, Thiam-Guan barclay, Thomas Kawai, Yugo Department of Physics Sardar Vallabhbhai National Institute of Technology Gujarat Surat395007 India School of Physics Faculty of Science University of New South Wales Kensington SydneyNSW2052 Australia Department of Earth and Space Science Indian Institute of Space Science and Technology Thiruvananthapuram India Department of Physics Presidency University West Bengal Kolkata700073 India Centre for Machine Intelligence and Data Science Indian Institute of Technology Bombay India Department of Computer Science International Hellenic University Kavala65404 Greece Department of Physics Indian Institute of Science Education and Research Kolkata West Bengal Mohanpur741246 India Department of Physics National Institute of Technology Tripura Agartala799046 India NASA Ames Research Center Moffett FieldCA94035 United States SETI Institute Mountain ViewCA94043 United States Oukaimeden Observatory High Energy Physics and Astrophysics Laboratory Cadi Ayyad University Marrakech Morocco Astrobiology Research Unit Université de Liège 19C Allée du 6 Août Liège4000 Belgium Glorieta de la Astronomía s/n Granada18008 Spain SUPA Physics and Astronomy University of St. Andrews FifeKY16 9SS United Kingdom Department of Astronomy University of California Berkeley BerkeleyCA94720 United States Department of Earth Atmospheric and Planetary Science Massachusetts Institute of Technology 77 Massachusetts Avenue CambridgeMA02139 United States Calle Vía Láctea s/n Tenerife La Laguna38200 Spain Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States South African Astronomical Observatory P.O. Box 9 Observatory Cape Town7935 South Africa NASA Exoplanet Science Institute IPAC California Institute of Technology PasadenaCA91125 United States Jet Propulsion Laboratory California Institute of Technology PasadenaCA91109 United States Sternberg Astronomical Institute Lomonosov Moscow State University Russia Depart

NASA’s all-sky survey mission, the Transiting exoplanet Survey Satellite (TeSS), is specifically engineered to detect exoplanets that transit bright stars. Thus far, TeSS has successfully identified approximately 400 transiting exoplanets, in addition to roughly 6000 candidate exoplanets pending confirmation. In this study, we present the results of our ongoing project, the Validation of Transiting exoplanets using Statistical Tools (VaTeST). Our dedicated effort is focused on the confirmation and characterization of new exoplanets through the application of statistical validation tools. Through a combination of ground-based telescope data, high-resolution imaging, and the utilization of the statistical validation tool known as TRICeRATOPS, we have successfully discovered eight potential super-earths. These planets bear the designations: TOI-238b (1.61+0.09–0.10 R⊗), TOI-771b (1.42+0.11–0.09 R⊗), TOI-871b (1.66+0.11–0.11 R⊗), TOI-1467b (1.83+0.16–0.15 R⊗), TOI-1739b (1.69+0.10–0.08 R⊗), TOI-2068b (1.82+0.16–0.15 R⊗), TOI-4559b (1.42+0.13–0.11 R⊗), and TOI-5799b (1.62+0.19–0.13 R⊗). Among all these planets, six of them fall within the region known as’keystone planets,’ which makes them particularly interesting for study. based on the location of TOI-771b and TOI-4559b below the radius valley we characterized them as likely super-earths, though radial velocity mass measurements for these planets will provide more details about their characterization. It is noteworthy that planets within the size range investigated herein are ab.ent from our own solar system, making their study crucial for gaining insights into the evolutionary stages between earth and Neptune. © 2023, CC bY.

关键词： Satellites

Particle identification in KM3NeT/ORCA 38

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Particle identification in KM3NeT/ORCA

38th International Cosmic Ray Conference, ICRC 2023

作者： Cerisy, L. Lazo, A. Lastoria, C. Perrin-Terrin, M. brunner, J. Dabhi, V. Aiello, S. Albert, A. Alves Garre, S. Aly, Z. Ambrosone, A. Ameli, F. Andre, M. Androutsou, e. Anguita, M. Aphecetche, L. Ardid, M. Ardid, S. Atmani, H. Aublin, J. bailly-Salins, L. bardačová, Z. baret, b. bariego-Quintana, A. basegmez du Pree, S. becherini, Y. bendahman, M. benfenati, F. benhassi, M. benoit, D.M. berb.e, e. bertin, V. biagi, S. b.ettcher, M. bonanno, D. boumaaza, J. bouta, M. bouwhuis, M. bozza, C. bozza, R.M. brânzaş, H. b.etaudeau, F. bruijn, R. bruno, R. buis, e. buompane, R. busto, J. Caiffi, b. Calvo, D. Campion, S. Capone, A. Carenini, F. Carretero, V. Cartraud, T. Castaldi, P. Cecchini, V. Celli, S. Chabab, M. Chadolias, M. Chen, A. Cherubini, S. Chiarusi, T. Circella, M. Cocimano, R. Coelho, J.A.b. Coleiro, A. Coniglione, R. Coyle, P. Creusot, A. Cruz, A. Cuttone, G. Dallier, R. Darras, Y. De benedittis, A. De Martino, b. Decoene, V. Del burgo, R. Di Cerbo, U.M. Di Mauro, L.S. Di Palma, I. Díaz, A.F. Diaz, C. Diego-Tortosa, D. Distefano, C. Domi, A. Donzaud, C. Dornic, D. Dörr, M. Drakopoulou, e. Drouhin, D. Dvornický, R. eberl, T. eckerová, e. eddymaoui, A. van eeden, T. eff, M. van eijk, D. el bojaddaini, I. el Hedri, S. enzenhöfer, A. Ferrara, G. Filipović, M.D. Filippini, F. Franciotti, D. Fusco, L.A. Gabriel, J. Gagliardini, S. Gal, T. García Méndez, J. Garcia Soto, A. Gatius Oliver, C. Geißelb.echt, N. Ghaddari, H. Gialanella, L. Gibson, b.K. Giorgio, e. Goos, I. Goupilliere, D. Gozzini, S.R. Gracia, R. Graf, K. Guidi, C. Guillon, b. Gutiérrez, M. van Haren, H. Heijb.er, A. Hekalo, A. Hennig, L. Hernández-Rey, J.J. Huang, F. Idrissi Ibnsalih, W. Illuminati, G. James, C.W. de Jong, M. de Jong, P. Jung, b.J. Kalaczyński, P. Kalekin, O. Katz, U.F. Khan Chowdhury, N.R. Khatun, A. Kistauri, G. Kopper, C. Kouchner, A. Kulikovskiy, V. Kvatadze, R. Labalme, M. Lahmann, R. Larosa, G. Le Stum, S. Lehaut, G. Leonora, e. Aix Marseille Univ CNRS IN2P3 CPPM Marseille France IFIC - Instituto de Física Corpuscular CSIC Universitat de València c/Catedrático José Beltrán 2 Paterna Valencia46980 Spain INFN Sezione di Catania Via Santa Sofia 64 Catania95123 Italy Université de Strasbourg CNRS IPHC UMR 7178 StrasbourgF-67000 France INFN Sezione di Napoli Complesso Universitario di Monte S. Angelo Via Cintia ed. G Napoli80126 Italy Università di Napoli "Federico II" Dip. Scienze Fisiche "E. Pancini" Complesso Universitario di Monte S. Angelo Via Cintia ed. G Napoli80126 Italy INFN Sezione di Roma Piazzale Aldo Moro 2 Roma00185 Italy Universitat Politècnica de Catalunya Laboratori d’Aplicacions Bioacústiques Centre Tecnològic de Vilanova i la Geltrú Avda. Rambla Exposició s/n Vilanova i la Geltrú08800 Spain NCSR Demokritos Institute of Nuclear and Particle Physics Ag. Paraskevi Attikis Athens15310 Greece University of Granada Dept. of Computer Architecture and Technology CITIC Granada18071 Spain Subatech IMT Atlantique IN2P3-CNRS Université de Nantes 4 rue Alfred Kastler - La Chantrerie BP 20722 Nantes44307 France Universitat Politècnica de València Instituto de Investigación para la Gestión Integrada de las Zonas Costeras C/ Paranimf 1 Gandia46730 Spain University Mohammed V in Rabat Faculty of Sciences 4 av. Ibn Battouta B.P. 1014 RabatR.P. 10000 Morocco Université Paris Cité CNRS Astroparticule et Cosmologie ParisF-75013 France LPC CAEN Normandie Univ ENSICAEN UNICAEN CNRS IN2P3 6 boulevard Maréchal Juin Caen14050 France Czech Technical University in Prague Institute of Experimental and Applied Physics Husova 240/5 Prague110 00 Czech Republic Comenius University in Bratislava Department of Nuclear Physics and Biophysics Mlynska dolina F1 Bratislava842 48 Slovakia Nikhef National Institute for Subatomic Physics PO Box 41882 Amsterdam1009 DB Netherlands INFN Sezione di Bologna v.le C. Berti-Pichat 6/2 Bologna40127 Italy Universit

One of the main goals of KM3NeT/ORCA is to measure atmospheric neutrino oscillation parameters with competitive precision. To achieve this goal, good discrimination between track-like and shower-like events is necessary, with particular focus on the measurement of the tau neutrino normalisation. The track-like signal is mainly carried by muon neutrinos from charged current interactions, while the shower-like signal comes from charged current interactions of electron and tau neutrinos, and neutral current interactions of all flavours. A Random Grid Search algorithm is optimised to separate these channels and its performance is compared with machine learning methods using boosted decision trees. This contribution will report on the technical aspects of the algorithm and the performance of the particle identification with data recorded in 2020 and 2021 using an early six-lines configuration of the ORCA detector (ORCA6). © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Neutrons

Real Time emotion Analysis Usingbrainwavesin Comparison to Facial expression

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IOP Conference Series: Materials science and engineering 2020年第1期994卷

作者： S. Devi Dr. M. Rajalakshmi S. Saranya b. Jeevanandan A. Ramya Assistant Professor Department of Information Technology Associate Professor Department of Information Technology Assistant Professor Department of Computer Science and Engineering B. E Student Department of Information Technology Coimbatore Institute of Technology

emotions play a vital role in human living and are correlated with every single word which is being spoken, without them life will be saturated and irrelevant. Understanding of the real apparent facial expressions might be difficult because part of the emotion might not be revealed outside by everyone. In the proposed method, the emotions of the human are analyzed in two different ways so that the real hidden emotion of the sub.ect can be detected. every human has unique brain waves, which gives better accuracy than other techniques. It ensures that the facial expression exhibited outside is real or not. The emotion analyzed will be useful in treating the person with high mental stress and also infinding the emotion of differently ab.ed person who requires medical treatment.

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