SNEWS 2.0: a next-generation supernova early warning system for multi-messenger astronomy

被引：59

作者：

Al Kharusi, S. ^{[1
]}

BenZvi, S. Y. ^{[2
]}

Bobowski, J. S. ^{[3
]}

Bonivento, W. ^{[4
]}

Brdar, V ^{[5
,6
,7
]}

Brunner, T. ^{[1
,8
]}

Caden, E. ^{[9
]}

Clark, M. ^{[10
]}

Coleiro, A. ^{[11
]}

Colomer-Molla, M. ^{[11
,12
]}

Crespo-Anadon, J., I ^{[13
]}

Depoian, A. ^{[10
]}

Dornic, D. ^{[14
]}

Fischer, V ^{[15
]}

Franco, D. ^{[11
]}

Fulgione, W. ^{[16
,17
]}

Gallo Rosso, A. ^{[18
]}

Geske, M. ^{[19
]}

Griswold, S. ^{[2
]}

Gromov, M. ^{[20
,21
]}

Haggard, D. ^{[1
]}

Habig, A. ^{[22
]}

Halim, O. ^{[23
]}

Higuera, A. ^{[24
,25
,26
]}

Hill, R. ^{[18
]}

Horiuchi, S. ^{[27
]}

Ishidoshiro, K. ^{[28
]}

Kato, C. ^{[29
]}

Katsavounidis, E. ^{[30
]}

Khaitan, D. ^{[2
]}

Kneller, J. P. ^{[31
]}

Kopec, A. ^{[10
]}

Kulikovskiy, V ^{[32
]}

Lai, M. ^{[33
,34
]}

Lamoureux, M. ^{[35
,36
]}

Lang, R. F. ^{[10
]}

Li, H. L. ^{[37
]}

Lincetto, M. ^{[14
]}

Lunardini, C. ^{[38
]}

Migenda, J. ^{[39
]}

Milisavljevic, D. ^{[10
]}

McCarthy, M. E. ^{[2
]}

Connor, E. ^{[40
,41
]}

Sullivan, E. ^{[42
]}

Pagliaroli, G. ^{[43
,44
]}

Patel, D. ^{[45
]}

Peres, R. ^{[46
]}

Pointon, B. W. ^{[8
,10
,47
]}

Qin, J. ^{[10
]}

Raj, N. ^{[8
]}

机构：

[1] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada

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

[3] Univ British Columbia, Phys, Kelowna, BC V1V 1V7, Canada

[4] Complesso Univ Monserrato, Cagliari Ist Nazl, INFN Sez, SP 8 Km 0-700, I-09042 Cagliari, Italy

[5] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA

[6] Northwestern Univ, Dept Phys & Astron, 2145 Sheridan Rd, Evanston, IL 60208 USA

[7] Max Planck Inst Kernphys, Postfach 103980, D-69029 Heidelberg, Germany

[8] TRIUMF, Vancouver, BC V6T 2A3, Canada

[9] SNOLAB, Creighton Mine 9,1039 Reg Rd 24, Sudbury, ON P3Y 1N2, Canada

[10] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA

[11] Univ Paris, CNRS, AstroParticule & Cosmol, F-75013 Paris, France

[12] Univ Valencia, CSIC, Inst Fis Corpuscular, Catedrat Jose Beltran 2, E-46980 Valencia, Spain

[13] Columbia Univ, Dept Phys, New York, NY 10027 USA

[14] Aix Marseille Univ, CPPM, CNRS, IN2P3, Marseille, France

[15] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA

[16] OATo Torino, Assergi, Italy

[17] Lab Nazl Gran Sasso LNGS, INFN Sez, Assergi, Italy

[18] Laurentian Univ, Dept Phys, Sudbury, ON P3E 2C6, Canada

[19] Gonzaga Univ, Dept Phys, Spokane, WA 99258 USA

[20] Lomonosov Moscow State Univ, Skobeltsyn Inst Nucl Phys, Moscow 119234, Russia

[21] Joint Inst Nucl Res, Dubna 141980, Russia

[22] Univ Minnesota, Dept Phys & Astron, Duluth, MN 55812 USA

[23] Univ Trieste, Dipartimento Fis, INFN Sez Trieste, I-34127 Trieste, Italy

[24] Rice Univ, Dept Phys, 6100 Main St, Houston, TX 77005 USA

[25] Rice Univ, Dept Astron, 6100 Main St, Houston, TX 77005 USA

[26] Rice Univ, Dept Comp Sci, 6100 Main St, Houston, TX 77005 USA

[27] Virginia Tech, Dept Phys, Ctr Neutrino Phys, Blacksburg, VA 24061 USA

[28] Tohoku Univ, Res Ctr Neutrino Sci, Sendai, Miyagi 9808578, Japan

[29] Tohoku Univ, Dept Aerosp Engn, Sendai, Miyagi 9808579, Japan

[30] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA

[31] NC State Univ, Dept Phys, Raleigh, NC 27695 USA

[32] INFN, Sez Genova, Via Dodecaneso 33, I-16146 Genoa, Italy

[33] Univ Cagliari, Dept Phys, I-09127 Cagliari, CA, Italy

[34] Ist Nazl Fis Nucl INFN, Frascati, Italy

[35] INFN, Sez Padova, Padua, Italy

[36] Univ Padua, Dipartimento Fis, Padua, Italy

[37] Chinese Acad Sci, Inst High Energy Phys, Beijing 100049, Peoples R China

[38] Arizona State Univ, Dept Phys, Tempe, AZ 85287 USA

[39] Kings Coll London, Dept Phys, London WC2R 2LS, England

[40] Stockholm Univ, AlbaNova, Dept Astron, S-10961 Stockholm, Sweden

[41] Stockholm Univ, AlbaNova, Oskar Klein Ctr, S-10961 Stockholm, Sweden

[42] Uppsala Univ, Deptartment Phys & Astron, Box 516, S-75120 Uppsala, Sweden

[43] Gran Sasso Sci Inst GSSI, Assergi, Italy

[44] INFN Sez, Lab Nazl Gran Sasso LNGS, Assergi, Italy

[45] Univ Regina, Dept Phys, Regina, SK S4S 0A2, Canada

[46] Univ Zurich, Phys Inst, Zurich, Switzerland

[47] British Columbia Inst Technol, Dept Phys, Burnaby, BC V5G 3H2, Canada

[48] Univ Houston, Dept Phys, Houston, TX 77204 USA

[49] Duke Univ, Dept Phys, Durham, NC 27708 USA

[50] Univ Minnesota Twin Cities, Sch Phys & Astron, Minneapolis, MN 55455 USA

来源：

NEW JOURNAL OF PHYSICS | 2021年 / 23卷 / 03期

基金：

欧盟地平线“2020”; 美国国家科学基金会;

关键词：

supernova neutrinos; multi-messenger astronomy; particle astrophysics; CORE-COLLAPSE SUPERNOVA; GRAVITATIONAL-WAVE SIGNAL; MASSIVE STARS; REAL-TIME; NEUTRINO EMISSIONS; SHOCK BREAKOUT; IA SUPERNOVAE; SENSITIVITY; EXPLOSION; PROGENITORS;

D O I：

10.1088/1367-2630/abde33

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

The next core-collapse supernova in the Milky Way or its satellites will represent a once-in-a-generation opportunity to obtain detailed information about the explosion of a star and provide significant scientific insight for a variety of fields because of the extreme conditions found within. Supernovae in our galaxy are not only rare on a human timescale but also happen at unscheduled times, so it is crucial to be ready and use all available instruments to capture all possible information from the event. The first indication of a potential stellar explosion will be the arrival of a bright burst of neutrinos. Its observation by multiple detectors worldwide can provide an early warning for the subsequent electromagnetic fireworks, as well as signal to other detectors with significant backgrounds so they can store their recent data. The supernova early warning system (SNEWS) has been operating as a simple coincidence between neutrino experiments in automated mode since 2005. In the current era of multi-messenger astronomy there are new opportunities for SNEWS to optimize sensitivity to science from the next galactic supernova beyond the simple early alert. This document is the product of a workshop in June 2019 towards design of SNEWS 2.0, an upgraded SNEWS with enhanced capabilities exploiting the unique advantages of prompt neutrino detection to maximize the science gained from such a valuable event.

引用

页数：34

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