Establishing accretion flares from supermassive black holes as a source of high-energy neutrinos

被引：23

作者：

van Velzen, Sjoert ^{[1
]}

Stein, Robert ^{[2
,3
,4
]}

Gilfanov, Marat ^{[5
,6
]}

Kowalski, Marek ^{[2
,3
]}

Hayasaki, Kimitake ^{[7
,8
]}

Reusch, Simeon ^{[2
,3
]}

Yao, Yuhan ^{[9
]}

Garrappa, Simone ^{[2
,3
]}

Franckowiak, Anna ^{[2
,10
]}

Gezari, Suvi ^{[11
,12
]}

Nordin, Jakob ^{[3
]}

Fremling, Christoffer ^{[4
]}

Sharma, Yashvi ^{[9
]}

Yan, Lin ^{[13
]}

Kool, Erik C. ^{[14
]}

Stern, Daniel ^{[15
]}

Veres, Patrik M. ^{[10
]}

Sollerman, Jesper

Medvedev, Pavel ^{[6
]}

Sunyaev, Rashid ^{[5
,6
]}

Bellm, Eric C. ^{[16
]}

Dekany, Richard G. ^{[13
]}

Duev, Dimitri A. ^{[4
]}

Graham, Matthew J. ^{[4
]}

Kasliwal, Mansi M. ^{[4
]}

Kulkarni, Shrinivas R. ^{[4
]}

Laher, Russ R. ^{[17
]}

Riddle, Reed L.

Rusholme, Ben ^{[17
]}

机构：

[1] Leiden Univ, Leiden Observ, Postbus 9513, NL-2300 RA Leiden, Netherlands

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

[3] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany

[4] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA

[5] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, Garching 85741, Germany

[6] Russian Acad Sci, Space Res Inst, Profsoyuznaya Ul 84-32, Moscow 117997, Russia

[7] Chungbuk Natl Univ, Dept Astron & Space Sci, Cheongju 361763, South Korea

[8] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

[9] CALTECH, Cahill Ctr Astrophys, MC 249-17,1200 E East Calif Blvd, Pasadena, CA 91125 USA

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

[11] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

[12] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[13] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA

[14] Stockholm Univ, Oskar Klein Ctr, Dept Astron, AlbaNova, SE-10691 Stockholm, Sweden

[15] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA

[16] Univ Washington, DIRAC Inst, Dept Astron, 3910 15th Ave NE, Seattle, WA 98195 USA

[17] CALTECH, IPAC, 1200 E Calif Blvd, Pasadena, CA 91125 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2024年 / 529卷 / 03期

基金：

俄罗斯科学基金会; 美国国家科学基金会; 美国国家航空航天局; 瑞典研究理事会; 新加坡国家研究基金会; 加拿大创新基金会;

关键词：

neutrinos; galaxies: active; transients: tidal disruption events; TIDAL DISRUPTION EVENTS; ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; SEYFERT-GALAXIES; EDDINGTON RATIO; LOW-RESOLUTION; SKY SURVEY; EMISSION; REVERBERATION; DISK;

D O I：

10.1093/mnras/stae610

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The origin of cosmic high-energy neutrinos remains largely unexplained. For high-energy neutrino alerts from IceCube, a coincidence with time-variable emission has been seen for three different types of accreting black holes: (1) a gamma-ray flare from a blazar (TXS 0506+056), (2) an optical transient following a stellar tidal disruption event (TDE; AT2019dsg), and (3) an optical outburst from an active galactic nucleus (AGN; AT2019fdr). For the latter two sources, infrared follow-up observations revealed a powerful reverberation signal due to dust heated by the flare. This discovery motivates a systematic study of neutrino emission from all supermassive black hole with similar dust echoes. Because dust reprocessing is agnostic to the origin of the outburst, our work unifies TDEs and high-amplitude flares from AGN into a population that we dub accretion flares. Besides the two known events, we uncover a third flare that is coincident with a PeV-scale neutrino (AT2019aalc). Based solely on the optical and infrared properties, we estimate a significance of 3.6 sigma for this association of high-energy neutrinos with three accretion flares. Our results imply that at least similar to 10 per cent of the IceCube high-energy neutrino alerts could be due to accretion flares. This is surprising because the sum of the fluence of these flares is at least three orders of magnitude lower compared to the total fluence of normal AGN. It thus appears that the efficiency of high-energy neutrino production in accretion flares is increased compared to non-flaring AGN. We speculate that this can be explained by the high Eddington ratio of the flares.

引用

页码：2559 / 2576

页数：18

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