A Search for Neutrino Emission from Fast Radio Bursts with Six Years of IceCube Data

Aartsen, M. G.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Ahrens, M.; Samarai, I. Al; Altmann, D.; Andeen, K.; Anderson, W. G.; Ansseau, I.; Anton, Gisela; Argüelles, C.; Auffenberg, J.; Axani, Spencer; Bagherpour, H.; Bai, X.; Barron, J. P.; Barwick, S. W.; Baum, V.; Bay, R.; Beatty, J. J.; Tjus, J. Becker; Becker, Karl‐Heinz; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, Summer; Böhm, C.; Börner, M.; Bos, F.; Böser, S.; Botner, O.; Bourbeau, Etienne; Bourbeau, J.; Bradascio, Federica; Braun, J.; Brenzke, M.; Bretz, H.-P.; Bron, S.; Brostean-Kaiser, Jannes; Burgman, A.; Busse, Raffaela; Carver, T.; Cheung, E.; Chirkin, D.; Christov, A.; Clark, K.; Classen, L.; Collin, Gabriel; Conrad, J. M.; Coppin, Paul; Correa, Pablo; Cowen, D. F.; Cross, R.; Dave, Pranav; Day, M.; André, J. P. A. M. de; Clercq, C. De; DeLaunay, James; Dembinski, H.-P.; Ridder, S. De; Desiati, P.; Vries, Krijn de; Wasseige, G. de; With, M. de; DeYoung, T.; Díaz-Vélez, J. C.; Lorenzo, V. di; Dujmović, Hrvoje; Dumm, J. P.; Dunkman, M.; Dvorak, Emily; Eberhardt, B.; Ehrhardt, Thomas; Eichmann, B.; Eller, P.; Evenson, P. A.; Fahey, S.; Fazely, A. R.; Felde, J.; Filimonov, K.; Finley, C.; Flis, S.; Franckowiak, A.; Friedman, E.; Fritz, A.; Gaisser, T. K.; Gallagher, J.; Gerhardt, L.; Ghorbani, K.; Giang, W.; Glauch, Theo; Glüsenkamp, T.; Goldschmidt, A.; González, J. G.; Grant, D.; Griffith, Z.; Haack, Christian; Hallgren, A.; Halzen, F.; Hanson, K.; Hebecker, D.; Heereman, D.; Helbing, K.; Hellauer, R.; Hickford, S.; Hignight, J.; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Hoinka, Tobias; Hokanson-Fasig, B.; Hoshina, K.; Huang, F.; Huber, M. E.; Hultqvist, K.; Hünnefeld, Mirco; Hussain, Raamis; In, S.; Iovine, N.; Ishihara, A.; Jacobi, E.; Japaridze, G. S.; Jeong, Minjin; Jero, K.; Jones, B. J. P.; Kalaczyński, P.; Kang, Woosik; Kappes, A.; Kappesser, David; Karg, T.; Karle, A.; Katz, U.; Kauer, M.; Keivani, A.; Kelley, J. L.; Kheirandish, Ali; Kim, J.; Kim, M.; Kintscher, T.; Kiryluk, J.; Kittler, T.; Klein, S. R.; Koirala, R.; Kolanoski, H.; Köpke, L.; Kopper, C.; Kopper, S.; Koschinsky, J. P.; Koskinen, D. J.; Kowalski, M.; Krings, K.; Kroll, M.; Krückl, G.; Kunwar, S.; Kurahashi, N.; Kuwabara, T.; Kyriacou, A.; Labare, M.; Lanfranchi, J. L.; Larson, M. J.; Lauber, Frederik Hermann; Leonard, K.; Lesiak-Bzdak, M.; Leuermann, M.; Liu, Q. R.; Mariscal, Cristian Jesús Lozano; Lu, Lu; Lünemann, J.; Luszczak, William; Madsen, J.; Maggi, G.; Mahn, Kendall; Mancina, Sarah; Maruyama, R.; Mase, K.; Maunu, R.; Meagher, K.; Medici, M.; Meier, Maximilian; Menne, T.; Merino, G.; Meures, T.; Miarecki, S.; Micallef, Jessie; Momenté, G.; Montaruli, T.; Moore, R. W.; Moulai, Marjon; Nahnhauer, R.; Nakarmi, P.; Naumann, Uwe; Neer, G.; Niederhausen, H.; Nowicki, S. C.; Nygren, D. R.; Pollmann, A. Obertacke; Olivas, A.; O’Murchadha, A.; O’Sullivan, Erin; Palczewski, T.; Pandya, Hershal; Pankova, D. V.; Peiffer, P.; Pepper, J. A.; Heros, C. Pérez de los; Pieloth, D.; Pinat, E.; Plum, M.; Price, P. B.; Przybylski, G. T.; Raab, Christoph; Rädel, L.; Rameez, M.; Rauch, L.; Rawlins, K.; Rea, Immacolata Carmen; Reimann, R.; Relethford, B.; Relich, M.; Resconi, E.; Rhode, W.; Richman, M.; Robertson, S.; Rongen, Martin; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk, D.; Safa, Ibrahim; Sälzer, T.; Herrera, S. E. Sanchez; Sandrock, A.; Sandroos, J.; Santander, M.; Sarkar, S.; Satalecka, K.; Schlunder, P.; Schmidt, T.; Schneider, A.; Schoenen, S.; Schöneberg, S.; Schumacher, Lisa Johanna; Sclafani, S.; Seckel, D.; Seunarine, S.; Soedingrekso, Jan; Soldin, D.; Song, M.; Spiczak, G. M.; Spiering, C.; Stachurska, J.; Stamatikos, M.; Stanev, T.; Stasik, A.; Stein, R.; Stettner, J.; Steuer, A.; Stezelberger, T.; Stokstad, R. G.; Stößl, A.; Strotjohann, N. L.; Stuttard, T.; Sullivan, G. W.; Sutherland, M.; Taboada, I.; Tatar, J.; Tenholt, F.; Ter–Antonyan, S.; Terliuk, A.; Tilav, S.; Toale, P. A.; Tobin, M. N.; Tönnis, Christoph; Toscano, S.; Tosi, D.; Tselengidou, M.; Tung, Chun Fai; Turcati, A.; Turley, C. F.; Ty, Bunheng; Unger, E.; Usner, M.; Vandenbroucke, J.; Driessche, W. Van; Eijk, D. van; Eijndhoven, N. van; Vanheule, S.; Santen, J. V.; Vogel, E.; Vraeghe, M.; Walck, C.; Wallace, A.; Wallraff, M.; Wandler, F. D.; Wandkowsky, N.; Waza, A.; Weaver, Ch.; Weiss, Matthew J.; Wendt, C.; Werthebach, Johannes; Westerhoff, S.; Whelan, B. J.; Wiebe, K.; Wiebusch, C. H.; Wille, L.; Williams, D. R.; Wills, L.; Wolf, M.; Wood, J.; Wood, T. R.; Woolsey, E.; Woschnagg, K.; Xu, D. L.; Xu, X. W.; Xu, Y.; Yañez, J. P.; Yodh, G.; Yoshida, Shigeru; Yuan, Tony

doi:10.3847/1538-4357/aab4f8

Cited by 32 publications

(23 citation statements)

References 43 publications

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“…Analogous results were obtained at very high energies, above 100 GeV (H.E.S.S. Collaboration et al 2017;MAGIC Collaboration et al 2018) as well as for TeV-PeV neutrinos coincident with FRBs (Aartsen et al 2018;Albert et al 2019).…”

Section: Introductionsupporting

confidence: 68%

A Search for Gamma-Ray Prompt Emission Associated with the Lorimer Burst FRB 010724

Guidorzi

Marongiu

Martone

et al. 2019

ApJ

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No transient electromagnetic emission has yet been found in association to fast radio bursts (FRBs), the only possible exception (3σ confidence) being the putative γ-ray signal detected in Swift/BAT data in the energy band 15-150 keV at the time and position of FRB 131104. Systematic searches for hard X/γ-ray counterparts to other FRBs ended up with just lower limits on the radio/γ-ray fluence ratios. In 2001, at the time of the earliest discovered FRBs, the BeppoSAX Gamma-Ray Burst Monitor (GRBM) was one of the most sensitive open sky γ-ray monitors in the 40-700 keV energy band. During its lifetime, one of the FRBs with the highest radio fluence ever recorded, FRB 010724 (800 ± 400 Jy ms), also known as the "Lorimer burst", was promptly visible to the GRBM. Upon an accurate modeling of the GRBM background, eased by its equatorial orbit, we searched for a possible γ-ray signal in the first 400 s following the FRB, similar to that claimed for FRB 131104 and found no significant emission down to a 5σ limit in the range (0.24-4.7) × 10 −6 erg cm −2 (corresponding to 1 and 400 s integration time, respectively), in the energy band 40-700 keV. This corresponds to η = F radio /F γ > 10 8−9 Jy ms erg −1 cm 2 , i.e. the deepest limit on the ratio between radio and γ-ray fluence, which rules out a γ-ray counterpart similar to that of FRB 131104. We discuss the implications on the possible mechanisms and progenitors that have been proposed in the literature, also taking into account its relatively low dispersion measure (375 ± 3 pc cm −3 ) and an inferred redshift limit of z < 0.4.

show abstract

Section: Introductionsupporting

confidence: 68%

A Search for Gamma-Ray Prompt Emission Associated with the Lorimer Burst FRB 010724

Guidorzi

Marongiu

Martone

et al. 2019

ApJ

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“…where t is the duration, A eff ðEÞ is the effective area of IceCube [30] and τðEÞ ≃ L=ð E dE=dx Þ. Then, we find the constraint on δ νe is only slightly weaker than that given by Eq.…”

Section: Constraints By Ic-170922amentioning

confidence: 66%

Limiting superluminal neutrino velocity and Lorentz invariance violation by neutrino emission from the blazar TXS 0506+056

Wang

Shao

et al. 2020

Phys. Rev. D

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The detection of high-energy neutrino coincident with the blazar TXS 0506 þ 056 provides a unique opportunity to test Lorentz invariance violation (LIV) in the neutrino sector. Thanks to the precisely measured redshift, i.e., z ¼ 0.3365, the comoving distance of the neutrino source is determined. In this work, we obtain and discuss the constraints on the superluminal neutrino velocity δ ν and the LIV by considering the energy loss of superluminal neutrino during propagation. Given superluminal electron velocity (δ e ≥ 0), a very stringent constraint on superluminal neutrino velocity can be reached, i.e., δ ν ≲ 1.3 × 10 −18 , corresponding to the quantum gravity (QG) scale M QG;1 ≳ 5.7 × 10 3 M Pl and M QG;2 ≳ 9.3 × 10 −6 M Pl for linear (quadratic) LIV, which are ∼12 orders of magnitude tighter for linear LIV and ∼9 orders tighter for quadratic LIV compared to the time-of-flight constraint from MeV neutrinos of SN 1987A. While given the subluminal electron velocity, a weaker constraint on the superluminal neutrino velocity is obtained, i.e., δ ν ≲ 8 × 10 −17 , which is consistent with the conclusions of previous works. We also study the neutrino detection probability due to the distortion of neutrino spectral shape during propagation, which gives slightly weaker constraints than above by a factor of ∼2.

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“…So far, there is no confirmed multiwavelength or multimessenger transient being associated with any FRB 4 (e.g., Petroff et al 2015;Callister et al 2016;Zhang & Zhang 2017;Aartsen et al 2018;Eftekhari et al 2018;MAGIC Collaboration et al 2018). In general, the following two physical mechanisms can give rise to an FRB-associated high-frequency counterpart during the FRB phase: (1) the inverse Compton (IC) scattering processes associated with an FRB, either for the one-zone case for which the IC and FRB emission processes are from the same emission region (the electrons responsible for the FRB emission and the IC emission could be the same or different) or for the two-zone case for which the IC process is located at a different region from the FRB emission; (2) the extension of the same mechanism of FRB emission to higher frequencies.…”

Section: Introductionmentioning

confidence: 99%

How Bright Are Fast Optical Bursts Associated With Fast Radio Bursts?

Yang

Zhang

Wei

2019

ApJ

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The origin of fast radio bursts (FRBs) is still unknown. Multiwavelength observations during or shortly after the FRB phase would be essential to identify the counterpart of an FRB and to constrain its progenitor and environment. In this work, we investigate the brightness of the "fast optical bursts" (FOBs) associated with FRBs and the prospects of detecting them. We investigate several inverse Compton (IC) scattering processes that might produce an FOB, including both the one-zone and two-zone models. We also investigate the extension of the same mechanism of FRB emission to the optical band. We find that a detectable FOB with the current and forthcoming telescopes is possible under the IC scenarios with very special conditions. In particular, the FRB environment would need to invoke a neutron star with an extremely strong magnetic field and an extremely fast spin, or an extremely young supernova remnant surrounding the FRB source. Furthermore, most electrons in the source are also required to have a fine-tuned energy distribution such that most of the IC energy is channeled in the optical band. We conclude that the prospect of detecting FOBs associated with FRBs is low. On the other hand, if FOBs are detected from a small fraction of FRBs, these FOBs would reveal extreme physical conditions in the FRB environments.

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A Search for Neutrino Emission from Fast Radio Bursts with Six Years of IceCube Data

Cited by 32 publications

References 43 publications

A Search for Gamma-Ray Prompt Emission Associated with the Lorimer Burst FRB 010724

A Search for Gamma-Ray Prompt Emission Associated with the Lorimer Burst FRB 010724

Limiting superluminal neutrino velocity and Lorentz invariance violation by neutrino emission from the blazar TXS 0506+056

How Bright Are Fast Optical Bursts Associated With Fast Radio Bursts?

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