THE DETECTION OF A SN IIn IN OPTICAL FOLLOW-UP OBSERVATIONS OF ICECUBE NEUTRINO EVENTS

Aartsen, M. G.; Abraham, K.; Ackermann, M.; Adams, J. H.; Aguilar, J. A.; Ahlers, M.; Ahrens, M.; Altmann, D.; Anderson, Tyler; Archinger, M.; Argüelles, C.; Arlen, T. C.; Auffenberg, J.; Bai, X.; Barwick, S. W.; Baum, V.; Bay, R.; Beatty, J. J.; Tjus, J. Becker; Becker, K. H.; Beiser, E.; BenZvi, S.; Berghaus, P.; Berley, D.; Bernardini, E.; Bernhard, A.; Besson, D.; Binder, G.; Bindig, D.; Bissok, M.; Blaufuss, E.; Blumenthal, J.; Boersma, D. J.; Böhm, C.; Börner, M.; Bos, F.; Bose, D.; Böser, S.; Botner, O.; Braun, J.; Brayeur, L.; Bretz, H.-P.; Brown, A. M.; Buzinsky, N.; Casey, J.; Casier, M.; Cheung, E.; Chirkin, D.; Christov, A.; Christy, B.; Clark, K.; Classen, L.; Coenders, S.; Cowen, D. F.; Silva, A. H. Cruz; Daughhetee, J.; Davis, J.; Day, M.; André, J. P. A. M. de; Clercq, C. De; Dembinski, H.-P.; Ridder, S. De; Desiati, P.; Vries, Krijn de; Wasseige, G. de; With, M. de; DeYoung, T.; Díaz–Vélez, Juan Carlos; Dumm, J. P.; Dunkman, M.; Eagan, R.; Eberhardt, B.; Ehrhardt, Thomas; Eichmann, B.; Euler, S.; Evenson, P. A.; Fadiran, O.; Fahey, S.; Fazely, A. R.; Fedynitch, Anatoli; Feintzeig, J.; Felde, J.; Filimonov, K.; Finley, C.; Fischer-Wasels, T.; Flis, S.; Fuchs, T.; Glagla, M.; Gaisser, T. K.; Gaïor, R.; Gallagher, J.; Gerhardt, L.; Ghorbani, K.; Gier, D.; Gladstone, L.; Glüsenkamp, T.; Goldschmidt, A.; Golup, G.; González, J. G.; Góra, D.; Grant, David; Gretskov, P.; Groh, J. C.; Groß, A.; Ha, C.; Haack, Christian; Ismail, A. Haj; Hallgren, A.; Halzen, F.; Hansmann, B.; Hanson, K.; Hebecker, D.; Heereman, D.; Helbing, K.; Hellauer, R.; Hellwig, D.; Hickford, S.; Hignight, J.; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Holzapfe, K.; Homeier, A.; Hoshina, K.; Huang, F.; Huber, Matthías; Huelsnitz, W.; Hulth, P. O.; Hultqvist, K.; In, S.; Ishihara, A.; Jacobi, E.; Japaridze, G. S.; Jero, K.; Jurković, M.; Kaminsky, B.; Kappes, A.; Karg, T.; Karle, A.; Kauer, M.; Keivani, A.; Kelley, J. L.; Kemp, J.; Kheirandish, Ali; Kiryluk, J.; Kläs, J.; Klein, S. R.; Kohnen, G.; Koirala, R.; Kolanoski, H.; Konietz, R.; Koob, A.; Köpke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Kowalski, M.; Krings, K.; Kroll, G.; Kroll, M.; Kunnen, J.; Kurahashi, N.; Kuwabara, T.; Labare, M.; Lanfranchi, J. L.; Larson, M. J.; Lesiak-Bzdak, M.; Leuermann, M.; Leuner, J.; Lünemann, J.; Madsen, J.; Maggi, G.; Mahn, Kendall; Maruyama, R.; Mase, K.; Matis, H. S.; Maunu, R.; McNally, F.; Meagher, K.; Medici, M.; Meli, A.; Menne, T.; Merino, G.; Meures, T.; Miarecki, S.; Middell, E.; Middlemas, E.; Miller, J.; Mohrmann, L.; Montaruli, T.; Morse, R.; Nahnhauer, R.; Naumann, Uwe; Niederhausen, H.; Nowicki, S. C.; Nygren, D. R.; Obertacke, A.; Olivas, A.; Omairat, A.; O’Murchadha, A.; Palczewski, T.; Pandya, Hershal; Paul, Larissa; Pepper, Joshua; Heros, C. Pérez de los; Pfendner, C.; Pieloth, D.; Pinat, E.; Posselt, J.; Price, P. B.; Przybylski, G. T.; Pütz, J.; Quinnan, M.; Rädel, L.; Rameez, M.; Rawlins, K.; Redl, P.; Reimann, R.; Relich, M.; Resconi, E.; Rhode, W.; Richman, M.; Richter, Stephan R.; Riedel, Benedikt; Robertson, Sally; Rongen, Martin; Rott, C.; Ruhe, T.; Ryckbosch, D.; Saba, S. M.; Sabbatini, L.; Sander, H. G.; Sandrock, A.; Sandroos, J.; Sarkar, S.; Schatto, K.; Scheriau, F.; Schimp, Michael; Schmidt, T.; Schmitz, M.; Schoenen, S.; Schöneberg, S.; Schönwald, A.; Schukraft, A.; Schulte, L.; Seckel, D.; Seunarine, S.; Shanidze, R.; Smith, M. W. E.; Soldin, D.; Spiczak, G. M.; Spiering, C.; Stahlberg, M.; Stamatikos, M.; Stanev, T.; Stanisha, N. A.; Stasik, A.; Stezelberger, T.; Stokstad, R. G.; Stößl, A.; Strahler, E. A.; Strom, Lars Rickard; Strotjohann, N. L.; Sullivan, G. W.; Sutherland, M.; Taavola, H.; Taboada, I.; Ter–Antonyan, S.; Terliuk, A.; Tešić, G.; Tilav, S.; Toale, P. A.; Tobin, M. N.; Tosi, D.; Tselengidou, M.; Turcati, A.; Unger, E.; Usner, M.; Vallecorsa, S.; Eijndhoven, N. van; Vandenbroucke, J.; Santen, J. V.; Vanheule, S.; Veenkamp, J.; Vehring, M.; Vöge, M.; Vraeghe, M.; Walck, C.; Wallraff, M.; Wandkowsky, N.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whelan, B. J.; Whitehorn, N.; Wichary, C.; Wiebe, K.; Wiebusch, C. H.; Wille, L.; Williams, D. R.; Wissing, H.; Wolf, M.; Wood, T. R.; Woschnagg, K.; Xu, D. L.; Xu, X. W.; Xu, Yi; Yañez, J. P.; Yodh, G.; Yoshida, Shigeru; Zarzhitsky, P.; Zoll, M.; Ofek, E. O.; Kasliwal, M. M.; Nugent, P.; Arcavi, I.; Bloom, J.; Kulkarni, S. R.; Perley, D. A.; Barlow, Tom A.; Horesh, A.; Gal‐Yam, A.; Howell, D. A.; Dilday, B.; Evans, P. A.; Kennea, J. A.; Burgett, W. S.; Chambers, K.; Kaiser, N.; Waters, C.; Flewelling, H.; Tonry, J.; Rest, A.; Smartt, S. J.

doi:10.1088/0004-637x/811/1/52

Cited by 47 publications

(42 citation statements)

References 80 publications

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“…In March 2012, the most significant alert during the first three years of operation of the optical and X-ray follow-up program was issued by IceCube. In the follow-up observations performed by the PTF, a Type IIn supernova PTF12csy was found 0.2 • away from the neutrino alert direction [35]. The supernova has a redshift of z = 0.0684, corresponding to a luminosity distance of about 300 Mpc, and the Pan-STARRS1 survey shows that its explosion time was at least 158 days (in the host-galaxy rest frame) before the neutrino alert, implying that a causal connection is unlikely [35].…”

Section: Results Of Ntoo Programmentioning

confidence: 94%

Very high-energy gamma-ray follow-up program using neutrino triggers from IceCube

2016

J. Inst.

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We describe and report the status of a neutrino-triggered program in IceCube that generates real-time alerts for gamma-ray follow-up observations by atmospheric-Cherenkov telescopes (MAGIC and VERITAS). While IceCube is capable of monitoring the whole sky continuously, high-energy gamma-ray telescopes have restricted fields of view and in general are unlikely to be observing a potential neutrino-flaring source at the time such neutrinos are recorded. The use of neutrino-triggered alerts thus aims at increasing the availability of simultaneous multi-messenger data during potential neutrino flaring activity, which can increase the discovery potential and constrain the phenomenological interpretation of the high-energy emission of selected source classes (e.g. blazars). The requirements of a fast and stable online analysis of potential neutrino signals and its operation are presented, along with first results of the program operating between

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Section: Results Of Ntoo Programmentioning

confidence: 94%

Very high-energy gamma-ray follow-up program using neutrino triggers from IceCube

2016

J. Inst.

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“…The neutrino alert described in this paper was found by the optical follow-up program (see also Abbasi et al 2012b;Evans et al 2015;Aartsen et al 2015b) which searches for short transient neutrino sources and triggers optical telescopes as well as the Swift X-ray telescope.…”

Section: Real-time Event Selectionmentioning

confidence: 97%

“…For example a supernova of Type IIn was detected in follow-up observations of a neutrino doublet (Aartsen et al 2015b). It is however likely unrelated given the large implied neutrino luminosity.…”

Section: Introductionmentioning

confidence: 99%

“…When two or more muon neutrino candidates are detected within 100 s of each other optical and X-ray observations can be triggered automatically Aartsen et al 2015b). Real-time follow-up observations are also triggered by the ANTARES neutrino telescope, but have not lead to the discovery of an electromagnetic counterpart (Ageron et al 2012;Adrián-Martínez et al 2016).…”

Section: Introductionmentioning

confidence: 99%

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Multiwavelength follow-up of a rare IceCube neutrino multiplet

Aartsen¹,

Ackermann²,

Adams³

et al. 2017

A&A

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On February 17 2016, the IceCube real-time neutrino search identified, for the first time, three muon neutrino candidates arriving within 100 s of one another, consistent with coming from the same point in the sky. Such a triplet is expected once every 13.7 years as a random coincidence of background events. However, considering the lifetime of the follow-up program the probability of detecting at least one triplet from atmospheric background is 32%. Follow-up observatories were notified in order to search for an electromagnetic counterpart. Observations were obtained by Swift's X-ray telescope, by ASAS-SN, LCO and MASTER at optical wavelengths, and by VERITAS in the very-high-energy gamma-ray regime. Moreover, the Swift BAT serendipitously observed the location 100 s after the first neutrino was detected, and data from the Fermi LAT and HAWC observatory were analyzed. We present details of the neutrino triplet and the follow-up observations. No likely electromagnetic counterpart was detected, and we discuss the implications of these constraints on candidate neutrino sources such as gamma-ray bursts, core-collapse supernovae and active galactic nucleus flares. This study illustrates the potential of and challenges for future follow-up campaigns.

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“…For several years, alerts have been sent out to optical, gamma-ray, and X-ray telescopes [13], which has led to a number of interesting results [14,15,16,17,18] as well as fostering a rich collaboration between electromagnetic and neutrino observatories. These long-running follow-up programs are supplemented by new neutrino selections that target single events deemed likely to be of astrophys-ical origin in the IceCube realtime alert system.…”

Section: Introductionmentioning

confidence: 99%

IceCube real-time alert system

Satalecka¹

2017

AIP Conference Proceedings

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Although high-energy astrophysical neutrinos were discovered in 2013, their origin is still unknown. Aiming for the identification of an electromagnetic counterpart of a rapidly fading source, we have implemented a realtime analysis framework for the IceCube neutrino observatory. Several analyses selecting neutrinos of astrophysical origin are now operating in realtime at the detector site in Antarctica and are producing alerts for the community to enable rapid follow-up observations. The goal of these observations is to locate the astrophysical objects responsible for these neutrino signals. This paper highlights the infrastructure in place both at the South Pole site and at IceCube facilities in the north that have enabled this fast follow-up program to be implemented. Additionally, this paper presents the first realtime analyses to be activated within this framework, highlights their sensitivities to astrophysical neutrinos and background event rates, and presents an outlook for future discoveries.

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THE DETECTION OF A SN IIn IN OPTICAL FOLLOW-UP OBSERVATIONS OF ICECUBE NEUTRINO EVENTS

Cited by 47 publications

References 80 publications

Very high-energy gamma-ray follow-up program using neutrino triggers from IceCube

Very high-energy gamma-ray follow-up program using neutrino triggers from IceCube

Multiwavelength follow-up of a rare IceCube neutrino multiplet

IceCube real-time alert system

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