Abstract
Context. Transient neutrino sources such as gamma-ray bursts (GRBs) and supernovae (SNe) are hypothesized to emit bursts of high-energy neutrinos on a time-scale of ≲ 100 s. While GRB neutrinos would be produced in high relativistic jets, core-collapse SNe might host soft-relativistic jets, which become stalled in the outer layers of the progenitor star leading to an efficient production of high-energy neutrinos. Aims. To increase the sensitivity to these neutrinos and identify their sources, a low-threshold optical follow-up program for neutrino multiplets detected with the IceCube observatory has been implemented. Methods. If a neutrino multiplet, i.e. two or more neutrinos from the same direction within 100 s, is found by IceCube a trigger is sent to the Robotic Optical Transient Search Experiment, ROTSE. The 4 ROTSE telescopes immediately start an observation program of the corresponding region of the sky in order to detect an optical counterpart to the neutrino events. Results. No statistically significant excess in the rate of neutrino multiplets has been observed and furthermore no coincidence with an optical counterpart was found. Conclusions. The search allows, for the first time, to set stringent limits on current models predicting a high-energy neutrino flux from soft relativistic hadronic jets in core-collapse SNe. We conclude that a sub-population of SNe with typical Lorentz boost factor and jet energy of 10 and 3 × 1051 erg, respectively, does not exceed 4.2% at 90% confidence.
| Original language | English (US) |
|---|---|
| Article number | A60 |
| Journal | Astronomy and Astrophysics |
| Volume | 539 |
| DOIs | |
| State | Published - 2012 |
Keywords
- Gamma-ray burst: general
- Neutrinos
- Supernovae: general
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science
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In: Astronomy and Astrophysics, Vol. 539, A60, 2012.
Research output: Contribution to journal › Article › peer-review
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TY - JOUR
T1 - Searching for soft relativistic jets in core-collapse supernovae with the IceCube optical follow-up program
AU - Abbasi, R.
AU - Abdou, Y.
AU - Abu-Zayyad, T.
AU - Ackermann, M.
AU - Adams, J.
AU - Aguilar, J. A.
AU - Ahlers, M.
AU - Allen, M. M.
AU - Altmann, D.
AU - Andeen, K.
AU - Auffenberg, J.
AU - Bai, X.
AU - Baker, M.
AU - Barwick, S. W.
AU - Bay, R.
AU - Bazo Alba, J. L.
AU - Beattie, K.
AU - Beatty, J. J.
AU - Bechet, S.
AU - Becker, J. K.
AU - Becker, K. H.
AU - Benabderrahmane, M. L.
AU - Benzvi, S.
AU - Berdermann, J.
AU - Berghaus, P.
AU - Berley, D.
AU - Bernardini, E.
AU - Bertrand, D.
AU - Besson, D. Z.
AU - Bindig, D.
AU - Bissok, M.
AU - Blaufuss, E.
AU - Blumenthal, J.
AU - Boersma, D. J.
AU - Bohm, C.
AU - Bose, D.
AU - Böser, S.
AU - Botner, O.
AU - Brown, A. M.
AU - Buitink, S.
AU - Caballero-Mora, K. S.
AU - Carson, M.
AU - Chirkin, D.
AU - Christy, B.
AU - Clevermann, F.
AU - Cohen, S.
AU - Colnard, C.
AU - Cowen, D. F.
AU - Cruz Silva, A. H.
AU - D'Agostino, M. V.
AU - Danninger, M.
AU - Daughhetee, J.
AU - Davis, J. C.
AU - De Clercq, C.
AU - Degner, T.
AU - Demirörs, L.
AU - Descamps, F.
AU - Desiati, P.
AU - De Vries-Uiterweerd, G.
AU - Deyoung, T.
AU - Díaz-Vélez, J. C.
AU - Dierckxsens, M.
AU - Dreyer, J.
AU - Dumm, J. P.
AU - Dunkman, M.
AU - Eisch, J.
AU - Ellsworth, R. W.
AU - Engdegård, O.
AU - Euler, S.
AU - Evenson, P. A.
AU - Fadiran, O.
AU - Fazely, A. R.
AU - Fedynitch, A.
AU - Feintzeig, J.
AU - Feusels, T.
AU - Filimonov, K.
AU - Finley, C.
AU - Fischer-Wasels, T.
AU - Fox, B. D.
AU - Franckowiak, A.
AU - Franke, R.
AU - Gaisser, T. K.
AU - Gallagher, J.
AU - Gerhardt, L.
AU - Gladstone, L.
AU - Glüsenkamp, T.
AU - Goldschmidt, A.
AU - Goodman, J. A.
AU - Góra, D.
AU - Grant, D.
AU - Griesel, T.
AU - Groß, A.
AU - Grullon, S.
AU - Gurtner, M.
AU - Ha, C.
AU - Haj Ismail, A.
AU - Hallgren, A.
AU - Halzen, F.
AU - Han, K.
AU - Hanson, K.
AU - Heinen, D.
AU - Helbing, K.
AU - Hellauer, R.
AU - Herquet, P.
AU - Hickford, S.
AU - Hill, G. C.
AU - Hoffman, K. D.
AU - Hoffmann, B.
AU - Homeier, A.
AU - Hoshina, K.
AU - Huelsnitz, W.
AU - Hülß, J. P.
AU - Hulth, P. O.
AU - Hultqvist, K.
AU - Hussain, S.
AU - Ishihara, A.
AU - Jacobi, E.
AU - Jacobsen, J.
AU - Japaridze, G. S.
AU - Johansson, H.
AU - Kampert, K. H.
AU - Kappes, A.
AU - Karg, T.
AU - Karle, A.
AU - Kenny, P.
AU - Kiryluk, J.
AU - Kislat, F.
AU - Klein, S. R.
AU - Köhne, J. H.
AU - Kohnen, G.
AU - Kolanoski, H.
AU - Köpke, L.
AU - Kopper, S.
AU - Koskinen, D. J.
AU - Kowalski, M.
AU - Kowarik, T.
AU - Krasberg, M.
AU - Kroll, G.
AU - Kurahashi, N.
AU - Kuwabara, T.
AU - Labare, M.
AU - Laihem, K.
AU - Landsman, H.
AU - Larson, M. J.
AU - Lauer, R.
AU - Lünemann, J.
AU - Madsen, J.
AU - Marotta, A.
AU - Maruyama, R.
AU - Mase, K.
AU - Matis, H. S.
AU - Meagher, K.
AU - Merck, M.
AU - Mészáros, P.
AU - Meures, T.
AU - Miarecki, S.
AU - Middell, E.
AU - Milke, N.
AU - Miller, J.
AU - Montaruli, T.
AU - Morse, R.
AU - Movit, S. M.
AU - Nahnhauer, R.
AU - Nam, J. W.
AU - Naumann, U.
AU - Nygren, D. R.
AU - Odrowski, S.
AU - Olivas, A.
AU - Olivo, M.
AU - O'Murchadha, A.
AU - Panknin, S.
AU - Paul, L.
AU - Pérez De Los Heros, C.
AU - Petrovic, J.
AU - Piegsa, A.
AU - Pieloth, D.
AU - Porrata, R.
AU - Posselt, J.
AU - Price, P. B.
AU - Przybylski, G. T.
AU - Rawlins, K.
AU - Redl, P.
AU - Resconi, E.
AU - Rhode, W.
AU - Ribordy, M.
AU - Richman, M.
AU - Rodrigues, J. P.
AU - Rothmaier, F.
AU - Rott, C.
AU - Ruhe, T.
AU - Rutledge, D.
AU - Ruzybayev, B.
AU - Ryckbosch, D.
AU - Sander, H. G.
AU - Santander, M.
AU - Sarkar, S.
AU - Schatto, K.
AU - Schmidt, T.
AU - Schönwald, A.
AU - Schukraft, A.
AU - Schultes, A.
AU - Schulz, O.
AU - Schunck, M.
AU - Seckel, D.
AU - Semburg, B.
AU - Seo, S. H.
AU - Sestayo, Y.
AU - Seunarine, S.
AU - Silvestri, A.
AU - Spiczak, G. M.
AU - Spiering, C.
AU - Stamatikos, M.
AU - Stanev, T.
AU - Stezelberger, T.
AU - Stokstad, R. G.
AU - Stössl, A.
AU - Strahler, E. A.
AU - Ström, R.
AU - Stüer, M.
AU - Sullivan, G. W.
AU - Swillens, Q.
AU - Taavola, H.
AU - Taboada, I.
AU - Tamburro, A.
AU - Ter-Antonyan, S.
AU - Tilav, S.
AU - Toale, P. A.
AU - Toscano, S.
AU - Tosi, D.
AU - Van Eijndhoven, N.
AU - Vandenbroucke, J.
AU - Van Overloop, A.
AU - Van Santen, J.
AU - Vehring, M.
AU - Voge, M.
AU - Walck, C.
AU - Waldenmaier, T.
AU - Wallraff, M.
AU - Walter, M.
AU - Weaver, Ch
AU - Wendt, C.
AU - Westerhoff, S.
AU - Whitehorn, N.
AU - Wiebe, K.
AU - Wiebusch, C. H.
AU - Williams, D. R.
AU - Wischnewski, R.
AU - Wissing, H.
AU - Wolf, M.
AU - Wood, T. R.
AU - Woschnagg, K.
AU - Xu, C.
AU - Xu, D. L.
AU - Xu, X. W.
AU - Yanez, J. P.
AU - Yodh, G.
AU - Yoshida, S.
AU - Zarzhitsky, P.
AU - Zoll, M.
AU - Akerlof, C. W.
AU - Pandey, S. B.
AU - Yuan, F.
AU - Zheng, W.
N1 - Funding Information: We acknowledge the support from the following agencies: US National Science Foundation-Office of Polar Programs, US National Science Foundation-Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin – Madison, the Open Science Grid (OSG) grid infrastructure; US Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; National Science and Engineering Research Council of Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; A. Groß acknowledges support by the EU Marie Curie OIF Program; J. P. Rodrigues acknowledges support by the Capes Foundation, Ministry of Education of Brazil. The research of M. Voge was supported in part by a GIF grant. The ROTSE project is supported by NSF grant PHY-0801007 and NASA grant NNX08AV63G. We are grateful to Andre Phillips at Siding Spring Observatory, David Doss at the McDonald Observatory, Toni Hanke at the HESS Observatory and Tuncay Özişik at TUBITAK National Observatory for their invaluable efforts in maintaining the ROTSE telescopes.
PY - 2012
Y1 - 2012
N2 - Context. Transient neutrino sources such as gamma-ray bursts (GRBs) and supernovae (SNe) are hypothesized to emit bursts of high-energy neutrinos on a time-scale of ≲ 100 s. While GRB neutrinos would be produced in high relativistic jets, core-collapse SNe might host soft-relativistic jets, which become stalled in the outer layers of the progenitor star leading to an efficient production of high-energy neutrinos. Aims. To increase the sensitivity to these neutrinos and identify their sources, a low-threshold optical follow-up program for neutrino multiplets detected with the IceCube observatory has been implemented. Methods. If a neutrino multiplet, i.e. two or more neutrinos from the same direction within 100 s, is found by IceCube a trigger is sent to the Robotic Optical Transient Search Experiment, ROTSE. The 4 ROTSE telescopes immediately start an observation program of the corresponding region of the sky in order to detect an optical counterpart to the neutrino events. Results. No statistically significant excess in the rate of neutrino multiplets has been observed and furthermore no coincidence with an optical counterpart was found. Conclusions. The search allows, for the first time, to set stringent limits on current models predicting a high-energy neutrino flux from soft relativistic hadronic jets in core-collapse SNe. We conclude that a sub-population of SNe with typical Lorentz boost factor and jet energy of 10 and 3 × 1051 erg, respectively, does not exceed 4.2% at 90% confidence.
AB - Context. Transient neutrino sources such as gamma-ray bursts (GRBs) and supernovae (SNe) are hypothesized to emit bursts of high-energy neutrinos on a time-scale of ≲ 100 s. While GRB neutrinos would be produced in high relativistic jets, core-collapse SNe might host soft-relativistic jets, which become stalled in the outer layers of the progenitor star leading to an efficient production of high-energy neutrinos. Aims. To increase the sensitivity to these neutrinos and identify their sources, a low-threshold optical follow-up program for neutrino multiplets detected with the IceCube observatory has been implemented. Methods. If a neutrino multiplet, i.e. two or more neutrinos from the same direction within 100 s, is found by IceCube a trigger is sent to the Robotic Optical Transient Search Experiment, ROTSE. The 4 ROTSE telescopes immediately start an observation program of the corresponding region of the sky in order to detect an optical counterpart to the neutrino events. Results. No statistically significant excess in the rate of neutrino multiplets has been observed and furthermore no coincidence with an optical counterpart was found. Conclusions. The search allows, for the first time, to set stringent limits on current models predicting a high-energy neutrino flux from soft relativistic hadronic jets in core-collapse SNe. We conclude that a sub-population of SNe with typical Lorentz boost factor and jet energy of 10 and 3 × 1051 erg, respectively, does not exceed 4.2% at 90% confidence.
KW - Gamma-ray burst: general
KW - Neutrinos
KW - Supernovae: general
UR - http://www.scopus.com/inward/record.url?scp=84863295832&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84863295832&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/201118071
DO - 10.1051/0004-6361/201118071
M3 - Article
AN - SCOPUS:84863295832
SN - 0004-6361
VL - 539
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A60
ER -