High-energy and ultra-high-energy neutrinos: A Snowmass white paper

Pablo Correa Camiroaga; Simon De Kockere; Krijn De Vries; Nicolaas Van Eijndhoven

doi:10.1016/j.jheap.2022.08.001

High-energy and ultra-high-energy neutrinos: A Snowmass white paper

Pablo Correa Camiroaga, Simon De Kockere, Krijn De Vries, Nicolaas Van Eijndhoven

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Abstract

Astrophysical neutrinos are excellent probes of astroparticle physics and high-energy physics. With energies far beyond solar, supernovae, atmospheric, and accelerator neutrinos, high-energy and ultra-high-energy neutrinos probe fundamental physics from the TeV scale to the EeV scale and beyond. They are sensitive to physics both within and beyond the Standard Model through their production mechanisms and in their propagation over cosmological distances. They carry unique information about their extreme non-thermal sources by giving insight into regions that are opaque to electromagnetic radiation. This white paper describes the opportunities astrophysical neutrino observations offer for astrophysics and high-energy physics, today and in coming years.

Original language	English
Article number	55-110
Pages (from-to)	55-110
Number of pages <span style="color:red"p> <font size="1.5"> ✽ </span> </font>	56
Journal	Journal of high energy astrophysics
Volume	36
Issue number	2022
DOIs	https://doi.org/10.1016/j.jheap.2022.08.001
Publication status	Published - Nov 2022

Bibliographical note

Funding Information:
MA is supported by the Initiative and Networking Fund of the Helmholtz Association , the Deutsches Elektronen-Synchrotron (DESY). MB is supported by the Villum Fonden under project no. 29388 . LL is supported by the US National Science Foundation (US NSF)-Office of Polar Programs, the US NSF Physics Division through Awards PHY-1913607 and the Wisconsin Alumni Research Foundation . NO is supported by the US NSF through Award 2112769 . MHR is supported in part by the U.S. Department of Energy (US DOE) grant DE-SC-0010113 . SAW is supported by the US NSF through Awards 2111232 and CAREER 2033500 and NASA through Awards 80NSSC20K1288 , 80NSSC20K0925 , and 80NSSC20K0775 . SKA and AN acknowledge the financial support from the Swarnajayanti Fellowship Research Grant (File no. S̃B/SJF/2020-21/21 ) provided by the Science and Engineering Research Board (SERB) and Department of Science and Technology (DST), Govt. of India. SKA would like to thank the United States-India Educational Foundation for providing the financial support through the Fulbright-Nehru Academic and Professional Excellence Fellowship (Award No. 2710/F-N APE/2021 ). JAM and EZ have received financial support from Xunta de Galicia (Centro singular de investigación de Galicia accreditation 2019-2022), by European Union ERDF , and by the “María de Maeztu” Units of Excellence program MDM-2016-0692 and the Spanish Research State Agency , and from Ministerio de Ciencia e Innovación PID2019-105544GB-I00 and RED2018-102661-T (RENATA). RAB is funded by the “la Caixa” Foundation (ID 100010434 ) and the European Union's Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No 847648 , fellowship code LCF/BQ/PI21/11830030 . BAC thanks the National Science Foundation for support through the Astronomy and Astrophysics Postdoctoral Fellowship under Award AST-1903885 . PBD acknowledges support from the US DOE under Grant Contract DE-SC0012704 . YF would like to acknowledge support from the ICTP through the Associates Programme and from the Simons Foundation through grant number 284558FY19 . YSJ is supported by the National Research Foundation of Korea (NRF) grant funded by the Korea government through Ministry of Science and ICT Grant 2021R1A2C1009296 . The work of SRK was supported in part by the US NSF under grant number PHY-1307472 and the US DOE under contract number DE-AC-76SF00098 . JFK acknowledges support by NASA grant 80NSSC19K0626 at the University of Maryland, Baltimore County and under proposal 17-APRA17-0066 at NASA/GSFC . ER is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) SFB 1258 , Cluster of Excellence 2094 ORIGINS , and the European Research Council (ERC) (Grant agreement No. 101053168 ). ZhD and OVS are supported by the Ministry of Education and Science of the Russian Federation within the financing program of large scientific projects of the “Science” National Project (grant no. 075-15-2020-778 ). The work of SY is supported by JSPS KAKENHI Grant No. 18H05206 . BZ is supported by the Simons Foundation .

Publisher Copyright:
© 2022 Elsevier B.V.

Copyright:
Copyright 2022 Elsevier B.V., All rights reserved.

Keywords

hep-ph
astro-ph.HE
hep-ex

Access to Document

10.1016/j.jheap.2022.08.001Licence: Unspecified

1-s2.0-S2214404822000416-mainFinal published version, 9.69 MBLicence: Unspecified

Cite this

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title = "High-energy and ultra-high-energy neutrinos: A Snowmass white paper",

abstract = " Astrophysical neutrinos are excellent probes of astroparticle physics and high-energy physics. With energies far beyond solar, supernovae, atmospheric, and accelerator neutrinos, high-energy and ultra-high-energy neutrinos probe fundamental physics from the TeV scale to the EeV scale and beyond. They are sensitive to physics both within and beyond the Standard Model through their production mechanisms and in their propagation over cosmological distances. They carry unique information about their extreme non-thermal sources by giving insight into regions that are opaque to electromagnetic radiation. This white paper describes the opportunities astrophysical neutrino observations offer for astrophysics and high-energy physics, today and in coming years. ",

keywords = "hep-ph, astro-ph.HE, hep-ex",

author = "{Correa Camiroaga}, Pablo and {De Kockere}, Simon and {De Vries}, Krijn and {Van Eijndhoven}, Nicolaas",

note = "Funding Information: MA is supported by the Initiative and Networking Fund of the Helmholtz Association , the Deutsches Elektronen-Synchrotron (DESY). MB is supported by the Villum Fonden under project no. 29388 . LL is supported by the US National Science Foundation (US NSF)-Office of Polar Programs, the US NSF Physics Division through Awards PHY-1913607 and the Wisconsin Alumni Research Foundation . NO is supported by the US NSF through Award 2112769 . MHR is supported in part by the U.S. Department of Energy (US DOE) grant DE-SC-0010113 . SAW is supported by the US NSF through Awards 2111232 and CAREER 2033500 and NASA through Awards 80NSSC20K1288 , 80NSSC20K0925 , and 80NSSC20K0775 . SKA and AN acknowledge the financial support from the Swarnajayanti Fellowship Research Grant (File no. {\~S}B/SJF/2020-21/21 ) provided by the Science and Engineering Research Board (SERB) and Department of Science and Technology (DST), Govt. of India. SKA would like to thank the United States-India Educational Foundation for providing the financial support through the Fulbright-Nehru Academic and Professional Excellence Fellowship (Award No. 2710/F-N APE/2021 ). JAM and EZ have received financial support from Xunta de Galicia (Centro singular de investigaci{\'o}n de Galicia accreditation 2019-2022), by European Union ERDF , and by the “Mar{\'i}a de Maeztu” Units of Excellence program MDM-2016-0692 and the Spanish Research State Agency , and from Ministerio de Ciencia e Innovaci{\'o}n PID2019-105544GB-I00 and RED2018-102661-T (RENATA). RAB is funded by the “la Caixa” Foundation (ID 100010434 ) and the European Union's Horizon 2020 research and innovation program under the Marie Sk{\l}odowska-Curie grant agreement No 847648 , fellowship code LCF/BQ/PI21/11830030 . BAC thanks the National Science Foundation for support through the Astronomy and Astrophysics Postdoctoral Fellowship under Award AST-1903885 . PBD acknowledges support from the US DOE under Grant Contract DE-SC0012704 . YF would like to acknowledge support from the ICTP through the Associates Programme and from the Simons Foundation through grant number 284558FY19 . YSJ is supported by the National Research Foundation of Korea (NRF) grant funded by the Korea government through Ministry of Science and ICT Grant 2021R1A2C1009296 . The work of SRK was supported in part by the US NSF under grant number PHY-1307472 and the US DOE under contract number DE-AC-76SF00098 . JFK acknowledges support by NASA grant 80NSSC19K0626 at the University of Maryland, Baltimore County and under proposal 17-APRA17-0066 at NASA/GSFC . ER is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) SFB 1258 , Cluster of Excellence 2094 ORIGINS , and the European Research Council (ERC) (Grant agreement No. 101053168 ). ZhD and OVS are supported by the Ministry of Education and Science of the Russian Federation within the financing program of large scientific projects of the “Science” National Project (grant no. 075-15-2020-778 ). The work of SY is supported by JSPS KAKENHI Grant No. 18H05206 . BZ is supported by the Simons Foundation . Publisher Copyright: {\textcopyright} 2022 Elsevier B.V. Copyright: Copyright 2022 Elsevier B.V., All rights reserved.",

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doi = "10.1016/j.jheap.2022.08.001",

language = "English",

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N1 - Funding Information: MA is supported by the Initiative and Networking Fund of the Helmholtz Association , the Deutsches Elektronen-Synchrotron (DESY). MB is supported by the Villum Fonden under project no. 29388 . LL is supported by the US National Science Foundation (US NSF)-Office of Polar Programs, the US NSF Physics Division through Awards PHY-1913607 and the Wisconsin Alumni Research Foundation . NO is supported by the US NSF through Award 2112769 . MHR is supported in part by the U.S. Department of Energy (US DOE) grant DE-SC-0010113 . SAW is supported by the US NSF through Awards 2111232 and CAREER 2033500 and NASA through Awards 80NSSC20K1288 , 80NSSC20K0925 , and 80NSSC20K0775 . SKA and AN acknowledge the financial support from the Swarnajayanti Fellowship Research Grant (File no. S̃B/SJF/2020-21/21 ) provided by the Science and Engineering Research Board (SERB) and Department of Science and Technology (DST), Govt. of India. SKA would like to thank the United States-India Educational Foundation for providing the financial support through the Fulbright-Nehru Academic and Professional Excellence Fellowship (Award No. 2710/F-N APE/2021 ). JAM and EZ have received financial support from Xunta de Galicia (Centro singular de investigación de Galicia accreditation 2019-2022), by European Union ERDF , and by the “María de Maeztu” Units of Excellence program MDM-2016-0692 and the Spanish Research State Agency , and from Ministerio de Ciencia e Innovación PID2019-105544GB-I00 and RED2018-102661-T (RENATA). RAB is funded by the “la Caixa” Foundation (ID 100010434 ) and the European Union's Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No 847648 , fellowship code LCF/BQ/PI21/11830030 . BAC thanks the National Science Foundation for support through the Astronomy and Astrophysics Postdoctoral Fellowship under Award AST-1903885 . PBD acknowledges support from the US DOE under Grant Contract DE-SC0012704 . YF would like to acknowledge support from the ICTP through the Associates Programme and from the Simons Foundation through grant number 284558FY19 . YSJ is supported by the National Research Foundation of Korea (NRF) grant funded by the Korea government through Ministry of Science and ICT Grant 2021R1A2C1009296 . The work of SRK was supported in part by the US NSF under grant number PHY-1307472 and the US DOE under contract number DE-AC-76SF00098 . JFK acknowledges support by NASA grant 80NSSC19K0626 at the University of Maryland, Baltimore County and under proposal 17-APRA17-0066 at NASA/GSFC . ER is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) SFB 1258 , Cluster of Excellence 2094 ORIGINS , and the European Research Council (ERC) (Grant agreement No. 101053168 ). ZhD and OVS are supported by the Ministry of Education and Science of the Russian Federation within the financing program of large scientific projects of the “Science” National Project (grant no. 075-15-2020-778 ). The work of SY is supported by JSPS KAKENHI Grant No. 18H05206 . BZ is supported by the Simons Foundation . Publisher Copyright: © 2022 Elsevier B.V. Copyright: Copyright 2022 Elsevier B.V., All rights reserved.

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AB - Astrophysical neutrinos are excellent probes of astroparticle physics and high-energy physics. With energies far beyond solar, supernovae, atmospheric, and accelerator neutrinos, high-energy and ultra-high-energy neutrinos probe fundamental physics from the TeV scale to the EeV scale and beyond. They are sensitive to physics both within and beyond the Standard Model through their production mechanisms and in their propagation over cosmological distances. They carry unique information about their extreme non-thermal sources by giving insight into regions that are opaque to electromagnetic radiation. This white paper describes the opportunities astrophysical neutrino observations offer for astrophysics and high-energy physics, today and in coming years.

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High-energy and ultra-high-energy neutrinos: A Snowmass white paper

Abstract

Bibliographical note

Keywords

Access to Document

Other files and links

Fingerprint

FWOIRI11: Exploring the Extreme Universe with the (Extended) IceCube Neutrino and Cosmic Ray Observatory at the South Pole

SRP72: SRP-Onderzoekszwaartepunt: High-energy physics (HEP@VUB).

CONI734: Icecube collaboration meeting

Cite this

High-energy and ultra-high-energy neutrinos: A Snowmass white paper

Abstract

Bibliographical note

Keywords

Access to Document

Other files and links

Fingerprint

Projects

FWOIRI11: Exploring the Extreme Universe with the (Extended) IceCube Neutrino and Cosmic Ray Observatory at the South Pole

SRP72: SRP-Onderzoekszwaartepunt: High-energy physics (HEP@VUB).

CONI734: Icecube collaboration meeting

Cite this