Abstract
Abstract The Super-Kamiokande detector can be used to search for neutrinos in time coincidence with gravitational waves detected by the LIGO–Virgo Collaboration (LVC). Both low-energy (7–100 MeV) and high-energy (0.1–105 GeV) samples were analyzed in order to cover a very wide neutrino spectrum. Follow-ups of 36 (out of 39) gravitational waves reported in the GWTC-2 catalog were examined; no significant excess above the background was observed, with 10 (24) observed neutrinos compared with 4.8 (25.0) expected events in the high-energy (low-energy) samples. A statistical approach was used to compute the significance of potential coincidences. For each observation, p-values were estimated using neutrino direction and LVC sky map; the most significant event (GW190602_175927) is associated with a post-trial p-value of 7.8% (1.4σ). Additionally, flux limits were computed independently for each sample and by combining the samples. The energy emitted as neutrinos by the identified gravitational wave sources was constrained, both for given flavors and for all flavors assuming equipartition between the different flavors, independently for each trigger and by combining sources of the same nature.
Highlights
We have entered a new phase of astronomical observations, the so-called multimessenger astronomy era
The detected gravitational waves (GW) emitters are categorized by LIGO/Virgo collaboration (LVC) into several types, for which high-energy neutrino (HE-ν) emission is expected from relativistic outflows and hadronic interactions within these sources: binary neutron star mergers (BNS, Kimura et al (2018)), neutron star-black hole mergers (NSBH, Kimura et al (2017)) or binary black hole mergers (BBH, Kotera & Silk (2016))
It is optically separated into an inner detector (ID) and an outer detector (OD) by a structure at ∼ 2 m from the wall
Summary
We have entered a new phase of astronomical observations, the so-called multimessenger astronomy era. The detected GW emitters are categorized by LVC into several types, for which high-energy neutrino (HE-ν) emission is expected from relativistic outflows and hadronic interactions within these sources: binary neutron star mergers (BNS, Kimura et al (2018)), neutron star-black hole mergers (NSBH, Kimura et al (2017)) or binary black hole mergers (BBH, Kotera & Silk (2016)). Such astrophysical objects may emit MeV neutrinos (LE-ν) (for BNS, see Foucart et al (2016)). The data release accompanying this article (Abe et al 2021a) includes all the figures, the tables of observations and calculated flux limits, and the SK effective area
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