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ASAS-SN follow-up of IceCube high-energy neutrino alerts

Necker, Jannis and de Jaeger, Thomas and Stein, Robert and Franckowiak, Anna and Shappee, Benjamin J. and Kowalski, Marek and Kochanek, Christopher S. and Stanek, Krzysztof Z. and Beacom, John F. and Desai, Dhvanil D. and Neumann, Kyle and Jayasinghe, Tharindu and Holoien, T. W-S and Thompson, Todd A. and Holmbo, Simon (2022) ASAS-SN follow-up of IceCube high-energy neutrino alerts. Monthly Notices of the Royal Astronomical Society, 516 (2). pp. 2455-2469. ISSN 0035-8711. doi:10.1093/mnras/stac2261. https://resolver.caltech.edu/CaltechAUTHORS:20220926-576716400.17

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Abstract

We report on the search for optical counterparts to IceCube neutrino alerts released between 2016 April and 2021 August with the All-Sky Automated Survey for SuperNovae (ASAS-SN). Despite the discovery of a diffuse astrophysical high-energy neutrino flux in 2013, the source of those neutrinos remains largely unknown. Since 2016, IceCube has published likely astrophysical neutrinos as public real-time alerts. Through a combination of normal survey and triggered target-of-opportunity observations, ASAS-SN obtained images within 1 h of the neutrino detection for 20 per cent (11) of all observable IceCube alerts and within one day for another 57 per cent (32). For all observable alerts, we obtained images within at least two weeks from the neutrino alert. ASAS-SN provides the only optical follow-up for about 17 per cent of IceCube’s neutrino alerts. We recover the two previously claimed counterparts to neutrino alerts, the flaring-blazar TXS 0506 + 056 and the tidal disruption event AT2019dsg. We investigate the light curves of previously detected transients in the alert footprints, but do not identify any further candidate neutrino sources. We also analysed the optical light curves of Fermi 4FGL sources coincident with high-energy neutrino alerts, but do not identify any contemporaneous flaring activity. Finally, we derive constraints on the luminosity functions of neutrino sources for a range of assumed evolution models.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stac2261DOIArticle
ORCID:
AuthorORCID
Necker, Jannis0000-0003-0280-7484
de Jaeger, Thomas0000-0001-6069-1139
Stein, Robert0000-0003-2434-0387
Franckowiak, Anna0000-0002-5605-2219
Shappee, Benjamin J.0000-0003-4631-1149
Kowalski, Marek0000-0001-8594-8666
Kochanek, Christopher S.0000-0001-6017-2961
Jayasinghe, Tharindu0000-0002-6244-477X
Holoien, T. W-S0000-0001-9206-3460
Thompson, Todd A.0000-0003-2377-9574
Additional Information:J.N. was supported by the Helmholtz Weizmann Research School on Multimessenger Astronomy, funded through the Initiative and Networking Fund of the Helmholtz Association, DESY, the Weizmann Institute, the Humboldt University of Berlin, and the University of Potsdam. Support for TdJ has been provided by NSF grants AST-1908952 and AST-1911074. RS and AF were supported by the Initiative and Networking Fund of the Helmholtz Association, Deutsches Elektronen-Synchrotron (DESY). BJS is supported by NSF grants AST-1907570, AST-1908952, AST-1920392, and AST-1911074. CSK and KZS are supported by NSF grants AST-1814440 and AST-1908570. JFB is supported by National Science Foundation grant no. PHY-2012955. Support for TW-SH was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51458.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-265. ASAS-SN is funded in part by the Gordon and Betty Moore Foundation through grants GBMF5490 and GBMF10501 to the Ohio State University, NSF grant AST-1908570, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics (CCAPP) at OSU, the Chinese Academy of Sciences South America Center for Astronomy (CAS-SACA), and the Villum Fonden (Denmark). Development of ASAS-SN has been supported by NSF grant AST-0908816, the Center for Cosmology and AstroParticle Physics at the Ohio State University, the Mt. Cuba Astronomical Foundation, and by George Skestos. Some of the results in this paper have been derived using the HEALPY and HEALPIX packages. The ZTF forced-photometry service was funded under the Heising-Simons Foundation grant no. 12540303 (PI: Graham). AF acknowledges funding from the German Science Foundation DFG, via the Collaborative Reasearch Center SFB1491 "Cosmic Interacting Matters - From Source to Signal".
Funders:
Funding AgencyGrant Number
Helmholtz AssociationUNSPECIFIED
Deutsches Elektronen-SynchrotronUNSPECIFIED
Weizmann InstituteUNSPECIFIED
Humboldt University (Berlin)UNSPECIFIED
University of PotsdamUNSPECIFIED
NSFAST-1908952
NSFAST-1911074
NSFAST-1907570
NSFAST-1908952
NSFAST-1920392
NSFAST-1911074
NSFAST-1814440
NSFAST-1908570
NSFPHY-2012955
NASA Hubble FellowshipHST-HF2-51458.001-A
NASANAS5-26555
Gordon and Betty Moore FoundationGBMF5490
Gordon and Betty Moore FoundationGBMF10501
NSFAST-1908570
Mt. Cuba Astronomical FoundationUNSPECIFIED
Center for Cosmology and AstroParticle Physics (CCAPP)UNSPECIFIED
Chinese Academy of Sciences South America Center for Astronomy (CASSACA)UNSPECIFIED
Villum FondenUNSPECIFIED
NSFAST-0908816
George SkestosUNSPECIFIED
Heising-Simons Foundation12540303
Deutsche Forschungsgemeinschaft (DFG)SFB1491
Issue or Number:2
DOI:10.1093/mnras/stac2261
Record Number:CaltechAUTHORS:20220926-576716400.17
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20220926-576716400.17
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:117150
Collection:CaltechAUTHORS
Deposited By: Melissa Ray
Deposited On:04 Oct 2022 14:22
Last Modified:04 Oct 2022 14:22

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