Abstract
Core-collapse supernovae are a promising potential high-energy neutrino source class. We test for correlation between seven years of IceCube neutrino data and a catalog containing more than 1000 core-collapse supernovae of types IIn and IIP and a sample of stripped-envelope supernovae. We search both for neutrino emission from individual supernovae as well as for combined emission from the whole supernova sample, through a stacking analysis. No significant spatial or temporal correlation of neutrinos with the cataloged supernovae was found. All scenarios were tested against the background expectation and together yield an overall p-value of 93%; therefore, they show consistency with the background only. The derived upper limits on the total energy emitted in neutrinos are 1.7 × 1048 erg for stripped-envelope supernovae, 2.8 × 1048 erg for type IIP, and 1.3 × 1049 erg for type IIn SNe, the latter disfavoring models with optimistic assumptions for neutrino production in interacting supernovae. We conclude that stripped-envelope supernovae and supernovae of type IIn do not contribute more than 14.6% and 33.9%, respectively, to the diffuse neutrino flux in the energy range of about [ 103-105] GeV, assuming that the neutrino energy spectrum follows a power-law with an index of −2.5. Under the same assumption, we can only constrain the contribution of type IIP SNe to no more than 59.9%. Thus, core-collapse supernovae of types IIn and stripped-envelope supernovae can both be ruled out as the dominant source of the diffuse neutrino flux under the given assumptions.
| Originalsprog | Engelsk |
|---|---|
| Artikelnummer | L12 |
| Tidsskrift | Astrophysical Journal Letters |
| Vol/bind | 949 |
| Udgave nummer | 1 |
| Antal sider | 14 |
| ISSN | 2041-8205 |
| DOI | |
| Status | Udgivet - 2023 |
Bibliografisk note
Publisher Copyright:© 2023. The Author(s). Published by the American Astronomical Society.
Citationsformater
- APA
- Standard
- Harvard
- Vancouver
- Author
- BIBTEX
- RIS
Constraining High-energy Neutrino Emission from Supernovae with IceCube. / Abbasi, R.; Ackermann, M.; Adams, J.; Agarwalla, S. K.; Aguilar, J. A.; Ahlers, M.; Alameddine, J. M.; Amin, N. M.; Andeen, K.; Anton, G.; Argüelles, C.; Ashida, Y.; Athanasiadou, S.; Axani, S. N.; Bai, X.; A. Balagopal, V.; Baricevic, M.; Barwick, S. W.; Basu, V.; Bay, R.; Beatty, J. J.; Becker, K. H.; Tjus, J. Becker; Beise, J.; Bellenghi, C.; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D. Z.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, S.; Bontempo, F.; Book, J. Y.; Meneguolo, C. Boscolo; Böser, S.; Botner, O.; Böttcher, J.; Bourbeau, E.; Braun, J.; Brinson, B.; Brostean-Kaiser, J.; Burley, R. T.; Busse, R. S.; Koskinen, D. J.; Kozynets, T.; Mead, J. V.; Søgaard, A.; Stuttard, T.; Icecube Collaboration.
I: Astrophysical Journal Letters, Bind 949, Nr. 1, L12, 2023.Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › peer review
}
TY - JOUR
T1 - Constraining High-energy Neutrino Emission from Supernovae with IceCube
AU - Abbasi, R.
AU - Ackermann, M.
AU - Adams, J.
AU - Agarwalla, S. K.
AU - Aguilar, J. A.
AU - Ahlers, M.
AU - Alameddine, J. M.
AU - Amin, N. M.
AU - Andeen, K.
AU - Anton, G.
AU - Argüelles, C.
AU - Ashida, Y.
AU - Athanasiadou, S.
AU - Axani, S. N.
AU - Bai, X.
AU - A. Balagopal, V.
AU - Baricevic, M.
AU - Barwick, S. W.
AU - Basu, V.
AU - Bay, R.
AU - Beatty, J. J.
AU - Becker, K. H.
AU - Tjus, J. Becker
AU - Beise, J.
AU - Bellenghi, C.
AU - BenZvi, S.
AU - Berley, D.
AU - Bernardini, E.
AU - Besson, D. Z.
AU - Binder, G.
AU - Bindig, D.
AU - Blaufuss, E.
AU - Blot, S.
AU - Bontempo, F.
AU - Book, J. Y.
AU - Meneguolo, C. Boscolo
AU - Böser, S.
AU - Botner, O.
AU - Böttcher, J.
AU - Bourbeau, E.
AU - Braun, J.
AU - Brinson, B.
AU - Brostean-Kaiser, J.
AU - Burley, R. T.
AU - Busse, R. S.
AU - Koskinen, D. J.
AU - Kozynets, T.
AU - Mead, J. V.
AU - Søgaard, A.
AU - Stuttard, T.
AU - Icecube Collaboration
N1 - Funding Information: The IceCube collaboration acknowledges the significant contributions to this manuscript from Jannis Necker, Alexander Stasik, and Robert Stein. We also gratefully acknowledge support from: USA—the U.S. National Science Foundation–Office of Polar Programs, the U.S. National Science Foundation–Physics Division, the U.S. National Science Foundation–EPSCoR, the Wisconsin Alumni Research Foundation, the Center for High Throughput Computing (CHTC) at the University of Wisconsin–Madison, the Open Science Grid (OSG), Advanced Cyberinfrastructure Coordination Ecosystem: Services & Support (ACCESS), the Frontera computing project at the Texas Advanced Computing Center, the U.S. Department of Energy–National Energy Research Scientific Computing Center, the Particle Astrophysics Research Computing Center at the University of Maryland, the Institute for Cyber-Enabled Research at Michigan State University, and the Astroparticle Physics Computational Facility at Marquette University; Belgium—Funds for Scientific Research (FRS-FNRS and FWO), the FWO Odysseus and Big Science programmes, and the Belgian Federal Science Policy Office (Belspo); Germany—Bundesministerium für Bildung und Forschung (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), the Initiative and Networking Fund of the Helmholtz Association, Deutsches Elektronen Synchrotron (DESY), and the High Performance Computing Cluster of the RWTH Aachen; Sweden—the Swedish Research Council, the Swedish Polar Research Secretariat, the Swedish National Infrastructure for Computing (SNIC), and the Knut and Alice Wallenberg Foundation; European Union—EGI Advanced Computing for Research; Australia—the Australian Research Council; Canada—the Natural Sciences and Engineering Research Council of Canada, Calcul Québec, Compute Ontario, the Canada Foundation for Innovation, WestGrid, and Compute Canada; Denmark—Villum Fonden, the Carlsberg Foundation, and the European Commission; New Zealand—the Marsden Fund; Japan—the Japan Society for Promotion of Science (JSPS) and the Institute for Global Prominent Research (IGPR) of Chiba University; Korea—the National Research Foundation of Korea (NRF); Switzerland—the Swiss National Science Foundation (SNSF); United Kingdom—Oxford University, Department of Physics. Funding Information: The IceCube collaboration acknowledges the significant contributions to this manuscript from Jannis Necker, Alexander Stasik, and Robert Stein. We also gratefully acknowledge support from: USA—the U.S. National Science Foundation-Office of Polar Programs, the U.S. National Science Foundation-Physics Division, the U.S. National Science Foundation-EPSCoR, the Wisconsin Alumni Research Foundation, the Center for High Throughput Computing (CHTC) at the University of Wisconsin-Madison, the Open Science Grid (OSG), Advanced Cyberinfrastructure Coordination Ecosystem: Services & Support (ACCESS), the Frontera computing project at the Texas Advanced Computing Center, the U.S. Department of Energy-National Energy Research Scientific Computing Center, the Particle Astrophysics Research Computing Center at the University of Maryland, the Institute for Cyber-Enabled Research at Michigan State University, and the Astroparticle Physics Computational Facility at Marquette University; Belgium—Funds for Scientific Research (FRS-FNRS and FWO), the FWO Odysseus and Big Science programmes, and the Belgian Federal Science Policy Office (Belspo); Germany—Bundesministerium für Bildung und Forschung (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), the Initiative and Networking Fund of the Helmholtz Association, Deutsches Elektronen Synchrotron (DESY), and the High Performance Computing Cluster of the RWTH Aachen; Sweden—the Swedish Research Council, the Swedish Polar Research Secretariat, the Swedish National Infrastructure for Computing (SNIC), and the Knut and Alice Wallenberg Foundation; European Union—EGI Advanced Computing for Research; Australia—the Australian Research Council; Canada—the Natural Sciences and Engineering Research Council of Canada, Calcul Québec, Compute Ontario, the Canada Foundation for Innovation, WestGrid, and Compute Canada; Denmark—Villum Fonden, the Carlsberg Foundation, and the European Commission; New Zealand—the Marsden Fund; Japan—the Japan Society for Promotion of Science (JSPS) and the Institute for Global Prominent Research (IGPR) of Chiba University; Korea—the National Research Foundation of Korea (NRF); Switzerland—the Swiss National Science Foundation (SNSF); United Kingdom—Oxford University, Department of Physics. Publisher Copyright: © 2023. The Author(s). Published by the American Astronomical Society.
PY - 2023
Y1 - 2023
N2 - Core-collapse supernovae are a promising potential high-energy neutrino source class. We test for correlation between seven years of IceCube neutrino data and a catalog containing more than 1000 core-collapse supernovae of types IIn and IIP and a sample of stripped-envelope supernovae. We search both for neutrino emission from individual supernovae as well as for combined emission from the whole supernova sample, through a stacking analysis. No significant spatial or temporal correlation of neutrinos with the cataloged supernovae was found. All scenarios were tested against the background expectation and together yield an overall p-value of 93%; therefore, they show consistency with the background only. The derived upper limits on the total energy emitted in neutrinos are 1.7 × 1048 erg for stripped-envelope supernovae, 2.8 × 1048 erg for type IIP, and 1.3 × 1049 erg for type IIn SNe, the latter disfavoring models with optimistic assumptions for neutrino production in interacting supernovae. We conclude that stripped-envelope supernovae and supernovae of type IIn do not contribute more than 14.6% and 33.9%, respectively, to the diffuse neutrino flux in the energy range of about [ 103-105] GeV, assuming that the neutrino energy spectrum follows a power-law with an index of −2.5. Under the same assumption, we can only constrain the contribution of type IIP SNe to no more than 59.9%. Thus, core-collapse supernovae of types IIn and stripped-envelope supernovae can both be ruled out as the dominant source of the diffuse neutrino flux under the given assumptions.
AB - Core-collapse supernovae are a promising potential high-energy neutrino source class. We test for correlation between seven years of IceCube neutrino data and a catalog containing more than 1000 core-collapse supernovae of types IIn and IIP and a sample of stripped-envelope supernovae. We search both for neutrino emission from individual supernovae as well as for combined emission from the whole supernova sample, through a stacking analysis. No significant spatial or temporal correlation of neutrinos with the cataloged supernovae was found. All scenarios were tested against the background expectation and together yield an overall p-value of 93%; therefore, they show consistency with the background only. The derived upper limits on the total energy emitted in neutrinos are 1.7 × 1048 erg for stripped-envelope supernovae, 2.8 × 1048 erg for type IIP, and 1.3 × 1049 erg for type IIn SNe, the latter disfavoring models with optimistic assumptions for neutrino production in interacting supernovae. We conclude that stripped-envelope supernovae and supernovae of type IIn do not contribute more than 14.6% and 33.9%, respectively, to the diffuse neutrino flux in the energy range of about [ 103-105] GeV, assuming that the neutrino energy spectrum follows a power-law with an index of −2.5. Under the same assumption, we can only constrain the contribution of type IIP SNe to no more than 59.9%. Thus, core-collapse supernovae of types IIn and stripped-envelope supernovae can both be ruled out as the dominant source of the diffuse neutrino flux under the given assumptions.
U2 - 10.3847/2041-8213/acd2c9
DO - 10.3847/2041-8213/acd2c9
M3 - Journal article
AN - SCOPUS:85160286860
VL - 949
JO - The Astrophysical Journal Letters
JF - The Astrophysical Journal Letters
SN - 2041-8205
IS - 1
M1 - L12
ER -