Search for neutrino counterparts to the gravitational wave sources from LIGO/Virgo O3 run with the ANTARES detector
Albert, A.; Alves, S.; André, M.; Ardid, M.; Ardid, S.; Aubert, J.-J.; Aublin, J.; Baret, B.; Basa, S.; Becherini, Y.; Belhorma, B.; Bendahman, M.; Benfenati, F.; Bertin, V.; Biagi, S.; Bissinger, M.; Boumaaza, J.; Bouta, M.; Bouwhuis, M.C.; Brânzaş, H.; Bruijn, R.; Brunner, J.; Busto, J.; Caiffi, B.; Calvo, D.; Campion, S.; Capone, A.; Caramete, L.; Carenini, F.; Carr, J.; Carretero, V.; Celli, S.; Cerisy, L.; Chabab, M.; Chau, T.N.; Cherkaoui El Moursli, R.; Chiarusi, T.; Circella, M.; Coelho, J.A.B.; Coleiro, A.; Coniglione, R.; Coyle, P.; Creusot, A.; Cruz, A.S.M.; Díaz, A.F.; De Martino, B.; Distefano, C.; Di Palma, I.; Domi, A.; Donzaud, C.; Dornic, D.; Drouhin, D.; Eberl, T.; van Eeden, T.; van Eijk, D.; El Hedri, S.; El Khayati, N.; Enzenhöfer, A.; Fermani, P.; Ferrara, G.; Filippini, F.; Fusco, L.; Gagliardini, S.; García, J.; Gatius Oliver, C.; Gay, P.; Geißelbrecht, N.; Glotin, H.; Gozzini, R.; Gracia Ruiz, R.; Graf, K.; Guidi, C.; Haegel, L.; Hallmann, S.; van Haren, H.; Heijboer, A.J.; Hello, Y.; Hernández-Rey, J.J.; Hößl, J.; Hofestädt, J.; Huang, F.; Illuminati, G.; James, C.W.; Jisse-Jung, B.; de Jong, M.; de Jong, P.; Kadler, M.; Kalekin, O.; Katz, U.; Kouchner, A.; Kreykenbohm, I.; Kulikovskiy, V.; Lahmann, R.; Lamoureux, M.; Lazo, A.; Lefèvre, D.; Leonora, E.; Levi, G.; Le Stum, S.; Lopez-Coto, D.; Loucatos, S.; Maderer, L.; Manczak, J.; Marcelin, M.; Margiotta, A.; Marinelli, A.; Martínez-Mora, J.A.; Migliozzi, P.; Moussa, A.; Muller, R.; Nauta, L.; Navas, S.; Nezri, E.; Ó Fearraigh, B.; Păun, A.; Păvălaş, G.E.; Perrin-Terrin, M.; Pestel, V.; Piattelli, P.; Poirè, C.; Popa, V.; Pradier, T.; Randazzo, N.; Real, D.; Reck, S.; Riccobene, G.; Romanov, A.; Sánchez-Losa, A.; Saina, A.; Salesa Greus, F.; Samtleben, D.F.E.; Sanguineti, M.; Sapienza, P.; Schnabel, J.; Schumann, J.; Schüssler, F.; Seneca, J.; Spurio, M.; Stolarczyk, Th.; Taiuti, M.; Tayalati, Y.; Tingay, S.J.; Vallage, B.; Vannoye, G.; Van Elewyck, V.; Viola, S.; Vivolo, D.; Wilms, J.; Zavatarelli, S.; Zegarelli, A.; Zornoza, J.D.; Zúñiga, J. (2023). Search for neutrino counterparts to the gravitational wave sources from LIGO/Virgo O3 run with the ANTARES detector. Journal of Cosmology and Astroparticle Physics 2023(04): 004. https://dx.doi.org/10.1088/1475-7516/2023/04/004
In: Journal of Cosmology and Astroparticle Physics. IOP Publishing: Bristol. ISSN 1475-7516; e-ISSN 1475-7516, meer
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| Author keywords |
gravitational waves / sources; neutrino astronomy; neutron stars |
| Abstract |
Since 2015 the LIGO and Virgo interferometers have detected gravitational waves from almost one hundred coalescences of compact objects (black holes and neutron stars). This article presents the results of a search performed with data from the ANTARES telescope to identify neutrino counterparts to the gravitational wave sources detected during the third LIGO/Virgo observing run and reported in the catalogues GWTC-2, GWTC-2.1, and GWTC-3. This search is sensitive to all-sky neutrinos of all flavours and of energies > 100 GeV, thanks to the inclusion of both track-like events (mainly induced by νμ charged-current interactions) and shower-like events (induced by other interaction types). Neutrinos are selected if they are detected within ± 500 s from the GW merger and with a reconstructed direction compatible with its sky localisation. No significant excess is found for any of the 80 analysed GW events, and upper limits on the neutrino emission are derived. Using the information from the GW catalogues and assuming isotropic emission, upper limits on the total energy Etot, ν emitted as neutrinos of all flavours and on the ratio fν = Etot,ν/E GW between neutrino and GW emissions are also computed. Finally, a stacked analysis of all the 72 binary black hole mergers (respectively the 7 neutron star-black hole merger candidates) has been performed to constrain the typical neutrino emission within this population, leading to the limits: Etot, ν < 4.0 × 10 53 erg and fν < 0.15 (respectively, Etot,ν < 3.2 × 10^53 erg and fν < 0.88) for E -2 spectrum and isotropic emission. Other assumptions including softer spectra and non-isotropic scenarios have also been tested. |
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