Search for neutrino counterparts to the gravitational wave sources from O3 catalogues with the ANTARES detector. (arXiv:2302.07723v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_ANTARES/0/1/0/all/0/1">ANTARES Collaboration</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Albert_A/0/1/0/all/0/1">A. Albert</a> (1 and 2), <a href="http://arxiv.org/find/astro-ph/1/au:+Alves_S/0/1/0/all/0/1">S. Alves</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Andre_M/0/1/0/all/0/1">M. André</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Ardid_M/0/1/0/all/0/1">M. Ardid</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Ardid_S/0/1/0/all/0/1">S. Ardid</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Aubert_J/0/1/0/all/0/1">J.-J. Aubert</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Aublin_J/0/1/0/all/0/1">J. Aublin</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Baret_B/0/1/0/all/0/1">B. Baret</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Basa_S/0/1/0/all/0/1">S. Basa</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Becherini_Y/0/1/0/all/0/1">Y. Becherini</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Belhorma_B/0/1/0/all/0/1">B. Belhorma</a> (9), <a href="http://arxiv.org/find/astro-ph/1/au:+Bendahman_M/0/1/0/all/0/1">M. Bendahman</a> (7 and 10), <a href="http://arxiv.org/find/astro-ph/1/au:+Benfenati_F/0/1/0/all/0/1">F. Benfenati</a> (11 and 12), <a href="http://arxiv.org/find/astro-ph/1/au:+Bertin_V/0/1/0/all/0/1">V. Bertin</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Biagi_S/0/1/0/all/0/1">S. Biagi</a> (13), <a href="http://arxiv.org/find/astro-ph/1/au:+Bissinger_M/0/1/0/all/0/1">M. Bissinger</a> (14), <a href="http://arxiv.org/find/astro-ph/1/au:+Boumaaza_J/0/1/0/all/0/1">J. Boumaaza</a> (10), <a href="http://arxiv.org/find/astro-ph/1/au:+Bouta_M/0/1/0/all/0/1">M. Bouta</a> (15), <a href="http://arxiv.org/find/astro-ph/1/au:+Bouwhuis_M/0/1/0/all/0/1">M.C. Bouwhuis</a> (16), <a href="http://arxiv.org/find/astro-ph/1/au:+Branzas_H/0/1/0/all/0/1">H. Brânzaş</a> (17), <a href="http://arxiv.org/find/astro-ph/1/au:+Bruijn_R/0/1/0/all/0/1">R. Bruijn</a> (16 and 18), <a href="http://arxiv.org/find/astro-ph/1/au:+Brunner_J/0/1/0/all/0/1">J. Brunner</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Busto_J/0/1/0/all/0/1">J. Busto</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Caiffi_B/0/1/0/all/0/1">B. Caiffi</a> (19), <a href="http://arxiv.org/find/astro-ph/1/au:+Calvo_D/0/1/0/all/0/1">D. Calvo</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Campion_S/0/1/0/all/0/1">S. Campion</a> (20 and 21), <a href="http://arxiv.org/find/astro-ph/1/au:+Capone_A/0/1/0/all/0/1">A. Capone</a> (20 and 21), <a href="http://arxiv.org/find/astro-ph/1/au:+Caramete_L/0/1/0/all/0/1">L. Caramete</a> (17), <a href="http://arxiv.org/find/astro-ph/1/au:+Carenini_F/0/1/0/all/0/1">F. Carenini</a> (11 and 12), <a href="http://arxiv.org/find/astro-ph/1/au:+Carr_J/0/1/0/all/0/1">J. Carr</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Carretero_V/0/1/0/all/0/1">V. Carretero</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Celli_S/0/1/0/all/0/1">S. Celli</a> (20 and 21), <a href="http://arxiv.org/find/astro-ph/1/au:+Cerisy_L/0/1/0/all/0/1">L. Cerisy</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Chabab_M/0/1/0/all/0/1">M. Chabab</a> (22), <a href="http://arxiv.org/find/astro-ph/1/au:+Chau_T/0/1/0/all/0/1">T. N. Chau</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Moursli_R/0/1/0/all/0/1">R. Cherkaoui El Moursli</a> (10), <a href="http://arxiv.org/find/astro-ph/1/au:+Chiarusi_T/0/1/0/all/0/1">T. Chiarusi</a> (11), <a href="http://arxiv.org/find/astro-ph/1/au:+Circella_M/0/1/0/all/0/1">M. Circella</a> (23), <a href="http://arxiv.org/find/astro-ph/1/au:+Coelho_J/0/1/0/all/0/1">J.A.B. Coelho</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Coleiro_A/0/1/0/all/0/1">A. Coleiro</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Coniglione_R/0/1/0/all/0/1">R. Coniglione</a> (13), <a href="http://arxiv.org/find/astro-ph/1/au:+Coyle_P/0/1/0/all/0/1">P. Coyle</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Creusot_A/0/1/0/all/0/1">A. Creusot</a> (7), et al. (109 additional authors not shown)
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 $nu_mu$
charged-current interactions) and shower-like events (induced by other
interaction types). Neutrinos are selected if they are detected within $pm
500,$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 $E_{rm tot, nu}$ and on the fraction of the total
energy budget $f_nu = E_{rm tot, nu}/E_{rm rad}$ emitted as neutrinos of
all flavours 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: $E_{rm tot, nu} < 4.0 times
10^{53},$erg and $f_nu < 0.15$ (respectively, $E_{rm tot, nu} < 3.2 times
10^{53},$erg and $f_nu < 0.88$) for $E^{-2}$ spectrum and isotropic emission.
Other assumptions including softer spectra and non-isotropic scenarios have
also been tested.
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 $nu_mu$
charged-current interactions) and shower-like events (induced by other
interaction types). Neutrinos are selected if they are detected within $pm
500,$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 $E_{rm tot, nu}$ and on the fraction of the total
energy budget $f_nu = E_{rm tot, nu}/E_{rm rad}$ emitted as neutrinos of
all flavours 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: $E_{rm tot, nu} < 4.0 times
10^{53},$erg and $f_nu < 0.15$ (respectively, $E_{rm tot, nu} < 3.2 times
10^{53},$erg and $f_nu < 0.88$) for $E^{-2}$ spectrum and isotropic emission.
Other assumptions including softer spectra and non-isotropic scenarios have
also been tested.
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