Constraining High-energy Neutrino Emission from Supernovae with IceCube

被引：15

作者：

Abbasi, R. ^{[1
]}

Ackermann, M. ^{[2
]}

Adams, J. ^{[3
]}

Agarwalla, S. K. ^{[4
,5
]}

Aguilar, J. A. ^{[6
]}

Ahlers, M. ^{[7
]}

Alameddine, J. M. ^{[8
]}

Amin, N. M. ^{[9
,10
]}

Andeen, K. ^{[11
,36
]}

Anton, G. ^{[12
]}

Argueelles, C. ^{[13
,14
]}

Ashida, Y. ^{[4
,5
]}

Athanasiadou, S. ^{[2
]}

Axani, S. N. ^{[9
,10
]}

Bai, X. ^{[15
]}

Balagopal, A., V ^{[4
,5
]}

Baricevic, M. ^{[4
,5
]}

Barwick, S. W. ^{[16
]}

Basu, V. ^{[4
,5
]}

Bay, R. ^{[17
]}

Beatty, J. J. ^{[18
,19
,20
]}

Becker, K. -H. ^{[21
]}

Tjus, J. Becker ^{[22
,72
]}

Beise, J. ^{[23
]}

Bellenghi, C. ^{[24
]}

BenZvi, S. ^{[25
]}

Berley, D. ^{[26
]}

Bernardini, E. ^{[27
]}

Besson, D. Z. ^{[28
]}

Binder, G. ^{[17
,29
]}

Bindig, D. ^{[21
]}

Blaufuss, E. ^{[26
]}

Blot, S. ^{[2
]}

Bontempo, F. ^{[30
]}

Book, J. Y. ^{[13
,14
]}

Meneguolo, C. Boscolo ^{[27
]}

Boeser, S. ^{[31
]}

Botner, O. ^{[23
]}

Boettcher, J. ^{[32
]}

Bourbeau, E. ^{[7
]}

Braun, J. ^{[4
,5
]}

Brinson, B. ^{[33
,34
]}

Brostean-Kaiser, J. ^{[2
]}

Burley, R. T. ^{[35
]}

Busse, R. S. ^{[36
]}

Butterfield, D. ^{[4
,5
]}

Campana, M. A. ^{[37
]}

Carloni, K. ^{[13
,14
]}

Carnie-Bronca, E. G. ^{[35
]}

Chattopadhyay, S. ^{[4
,5
]}

机构：

[1] Loyola Univ Chicago, Dept Phys, Chicago, IL 60660 USA

[2] Deutsch Elektronen Synchrotron DESY, Platanenallee 6, D-15738 Zeuthen, Germany

[3] Univ Canterbury, Dept Phys & Astron, Private Bag 4800, Christchurch, New Zealand

[4] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA

[5] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA

[6] Univ Libre Bruxelles, Fac Sci, CP230, B-1050 Brussels, Belgium

[7] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark

[8] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany

[9] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA

[10] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA

[11] Marquette Univ, Dept Phys, Milwaukee, WI 53201 USA

[12] Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany

[13] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA

[14] Harvard Univ, Lab Particle Phys & Cosmol, Cambridge, MA 02138 USA

[15] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA

[16] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA

[17] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[18] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA

[19] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA

[20] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA

[21] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany

[22] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany

[23] Uppsala Univ, Dept Phys & Astron, Box 516, SE-75120 Uppsala, Sweden

[24] Tech Univ Munich, Phys Dept, D-85748 Garching, Germany

[25] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA

[26] Univ Maryland, Dept Phys, College Pk, MD 20742 USA

[27] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35122 Padua, PD, Italy

[28] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA

[29] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA

[30] Karlsruhe Inst Technol, Inst Astroparticle Phys, D-76021 Karlsruhe, Germany

[31] Johannes Gutenberg Univ Mainz, Inst Phys, Staudinger Weg 7, D-55099 Mainz, Germany

[32] Rhein Westfal TH Aachen, Phys Inst 3, D-52056 Aachen, Germany

[33] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA

[34] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA

[35] Univ Adelaide, Dept Phys, Adelaide, SA 5005, Australia

[36] Westfalische Wilhelms Univ Munster, Inst Kernphys, D-48149 Munster, Germany

[37] Drexel Univ, Dept Phys, 3141 Chestnut St, Philadelphia, PA 19104 USA

[38] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA

[39] Sungkyunkwan Univ, Dept Phys, Suwon 16419, South Korea

[40] MIT, Dept Phys, Cambridge, MA 02139 USA

[41] VUB, Dienst ELEM, B-1050 Brussels, Belgium

[42] Columbia Univ, Columbia Astrophys & Nevis Labs, New York, NY 10027 USA

[43] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA

[44] Penn State Univ, Dept Phys, 104 Davey Lab, University Pk, PA 16802 USA

[45] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA

[46] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden

[47] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden

[48] Catholic Univ Louvain, Ctr Cosmol Particle Phys & Phenomenol CP3, Louvain La Neuve, Belgium

[49] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA

[50] Karlsruhe Inst Technol, Inst Expt Particle Phys, D-76021 Karlsruhe, Germany

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2023年 / 949卷 / 01期

基金：

加拿大自然科学与工程研究理事会; 新加坡国家研究基金会; 澳大利亚研究理事会; 美国国家科学基金会; 瑞典研究理事会; 瑞士国家科学基金会; 加拿大创新基金会;

关键词：

MASTER OT J120451.50+265946.6; CORE-COLLAPSE SUPERNOVAE; GAMMA-RAY BURSTS; IIP SUPERNOVA; SN; PROGENITOR; SEARCH; EVOLUTION; OUTBURST; BLAZARS;

D O I：

10.3847/2041-8213/acd2c9

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 x 10(48) erg for stripped-envelope supernovae, 2.8 x 10(48) erg for type IIP, and 1.3 x 10(49) 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 [ 10(3)-10(5)] 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.

引用

页数：14

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