////////////////////////////////////////////////////////////////////// TITLE: GCN/AMON NOTICE NOTICE_DATE: Sun 15 Oct 17 01:35:02 UT NOTICE_TYPE: AMON ICECUBE HESE RUN_NUM: 130126 EVENT_NUM: 56068624 SRC_RA: 162.5790d {+10h 50m 19s} (J2000), 162.7985d {+10h 51m 12s} (current), 161.9624d {+10h 47m 51s} (1950) SRC_DEC: -15.8611d {-15d 51' 39"} (J2000), -15.9556d {-15d 57' 19"} (current), -15.5959d {-15d 35' 44"} (1950) SRC_ERROR: 73.79 [arcmin radius, stat+sys, 90% containment] SRC_ERROR50: 25.19 [arcmin radius, stat+sys, 50% containment] DISCOVERY_DATE: 18041 TJD; 288 DOY; 17/10/15 (yy/mm/dd) DISCOVERY_TIME: 5670 SOD {01:34:30.06} UT REVISION: 0 N_EVENTS: 1 [number of neutrinos] STREAM: 1 DELTA_T: 0.0000 [sec] SIGMA_T: 0.0000 [sec] FALSE_POS: 0.0000e+00 [s^-1 sr^-1] PVALUE: 0.0000e+00 [dn] CHARGE: 13906.14 [pe] SIGNAL_TRACKNESS: 0.51 [dn] SUN_POSTN: 200.24d {+13h 20m 58s} -8.53d {-08d 31' 43"} SUN_DIST: 37.28 [deg] Sun_angle= 2.5 [hr] (West of Sun) MOON_POSTN: 146.89d {+09h 47m 34s} +13.52d {+13d 31' 20"} MOON_DIST: 33.41 [deg] GAL_COORDS: 264.99, 37.93 [deg] galactic lon,lat of the event ECL_COORDS: 170.38,-21.43 [deg] ecliptic lon,lat of the event COMMENTS: AMON_ICECUBE_HESE. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22016 SUBJECT: IceCube-171015A - IceCube observation of a high-energy neutrino candidate event DATE: 17/10/15 14:30:35 GMT FROM: Erik Blaufuss at U. Maryland/IceCube The IceCube Collaboration (http://icecube.wisc.edu/) reports: On 15 October, 2017 IceCube detected a track-like, very-high-energy event with a high probability of being of astrophysical origin. The event was identified by the High Energy Starting Event (HESE) selection. The IceCube detector was in a normal operating state. HESE events have a neutrino vertex inside of the detector (to reduce background) and have a high light level (a proxy for energy). After the initial automated alert (https://gcn.gsfc.nasa.gov/notices_amon/56068624_130126.amon), more sophisticated reconstruction algorithms have been applied offline, with the direction refined to: Date: 2017-10-15 Time: 01:34:30.06 UT RA: 162.86 deg (-1.70 deg / +2.60 deg 90% PSF containment) J2000 Dec: -15.44 deg (-2.00 deg / +1.60 deg 90% PSF containment) J2000 We encourage follow-up by ground and space-based instruments to help identify a possible astrophysical source for the candidate neutrino. The IceCube Neutrino Observatory is a cubic-kilometer neutrino detector operating at the geographic South Pole, Antarctica. The IceCube realtime alert point of contact can be reached at roc@icecube.wisc.edu //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22018 SUBJECT: INTEGRAL SPI-ACS observation of IceCube-171015A DATE: 17/10/15 20:34:06 GMT FROM: Volodymyr Savchenko at ISDC,U of Geneve V. Savchenko, C. Ferrigno (ISDC, University of Geneva, CH) P. Ubertini, A. Bazzano, L. Natalucci. J. Rodi (INAF IAPS-Roma, Italy) S. Mereghetti (INAF IASF-Milano, Italy) P. Laurent (CEA, Saclay, France) E. Kuulkers (ESAC/ESA, Madrid, Spain) Using INTEGRAL SPI-ACS we have performed a search for a prompt gamma-ray counterpart of the cosmic neutrino candidate IceCube-171015A (GCN 22016). At the time of the event (2017-10-15 01:34:30 UTC, hereafter T0), INTEGRAL was operating in nominal mode. The neutrino localization was at an angle of 85 deg with respect to the spacecraft pointing axis. This orientation implies near-optimal response of SPI-ACS, and this instrument provides best sensitivity to both short and long GRBs. The background within +/-300 seconds around the event was very stable. We do not detect any significant counterparts and estimate a 3-sigma upper limit on the 75-2000 keV fluence of 2.2x10^-7 erg/cm^2 for a burst lasting less than 1 s with a characteristic short GRB spectrum (an exponentially cut off power law with alpha=-0.5 and Ep=600 keV) occurring at any time in the interval within 300 s around T0. For a typical long GRB spectrum (Band function with alpha=-1, beta=-2.5, and Ep=300 keV), the derived peak flux upper limit is ~1.9x10^-7 (6.2x10^-7) erg/cm^2/s at 1 s (8 s) time scale in 75-2000 keV energy range. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22019 SUBJECT: Search for counterpart to IceCube-171015A with ANTARES DATE: 17/10/16 06:20:01 GMT FROM: Damien Dornic at CPPM,France Damien Dornic (CPPM / CNRS), Alexis Coleiro (APC / IFIC) report on behalf of the ANTARES Collaboration: Using online data from the ANTARES detector, we have performed a follow-up analysis of the recently reported high-energy starting event (HESE) neutrino IceCube-171015 (AMON IceCube HESE 56068624_130126). The reconstructed origin was 24.5 degrees below the horizon for ANTARES. No up-going muon neutrino candidate events were recorded within three degrees of the IceCube event coordinates during a +/- 1h time-window centered on the IceCube event time (100% visibility probability). A search on an extended time window of +/- 1 day (58% visibility probability) has also yielded no detection. This yields a preliminary 90% confidence level upper limit on the muon-neutrino fluence from a point source of 14 GeV.cm^-2 over the energy range 2.7 TeV - 2.8 PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and 27 GeV.cm^-2 (440 GeV - 240 TeV) for an E^-2.5 spectrum. ANTARES is the largest neutrino detector installed in the Mediterranean Sea, and is primarily sensitive to astrophysical neutrinos in the TeV-PeV energy range. At 10 TeV, the median angular resolution for muon neutrinos is below 0.5 degrees. In the range 1-100 TeV, ANTARES has the best sensitivity to this position in the sky. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22043 SUBJECT: Fermi GBM Observations of IceCube-171015A DATE: 17/10/23 01:11:41 GMT FROM: Rachel Hamburg at UAH R. Hamburg (UAH) and A. Goldstein (USRA) report on behalf of the Fermi GBM team: We have searched the Fermi Gamma-ray Burst Monitor data for a gamma-ray counterpart to the IceCube neutrino 171015A (GCN 22016). The location of the neutrino was observed by GBM with good geometry. There were no associated on-board triggers +/- 15 hours of the neutrino event time. The ground-based untargeted search of GBM data (Briggs et al., in prep) did not find any candidates +/- 1 hour of the event time. The targeted search of GBM data ([1],[2]) also searched +/- 30 s around the neutrino event time, processing timescales of 0.256 s to 8.192 s. No significant candidates were found. Using a hard Band function with (Epeak, alpha, beta) = (500 keV, -0.5,-2.5), we set 3 sigma flux-averaged upper limits for any transient within 30 s of the neutrino event time. Averaged over (0.1 s, 1 s, and 10 s) timescales, the corresponding upper limits in the 10-1000 keV band are (16.4, 4.82, 1.47) E-7 erg/s/cm^2. Using an exponentially cut-off power law parametrized with (Epeak, index) = (566 keV, -0.42), which represents the average GBM-triggered short GRB, the flux-averaged upper limits are (18.0, 5.26, 1.61) E-7 erg/s/cm^2. [1] L. Blackburn et al. 2015, ApJS 217, 8 [2] A. Goldstein et al. arXiv:1612.02395 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 22282 SUBJECT: IceCube-171015A: Konus-Wind upper limits DATE: 17/12/25 10:44:28 GMT FROM: Anna Kozlova at Ioffe Institute A. Kozlova, S. Golenetskii, R.Aptekar, D. Frederiks, P. Oleynik, M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline, on behalf of the Konus-Wind team, report: Using Konus-Wind (KW) data, we have performed a search for a gamma-ray transient around the time of the cosmic neutrino candidate IceCube-171015A (2017-10-15 01:34:30.06 UT, hereafter T0; Blaufuss, GCN 22016; https://gcn.gsfc.nasa.gov/notices_amon/56068624_130126.amon) No triggered KW event happened from ~3.3 days before and up to ~3.6 days after T0. The closest waiting-mode event was ~1.9 hours after T0. Using waiting-mode data within the interval T0 +/- 1000 s, we found no significant (> 5 sigma) excess over the background in both KW detectors on temporal scales from 2.944 s to 100 s in the 80-1000 keV band. We estimate an upper limit (90% conf.) on the 10 keV – 10 MeV fluence to 8.7x10^-7 erg/cm^2 for a burst lasting less than 2.944 s and having a typical KW short GRB spectrum (an exponentially cut off power law with alpha =-0.5 and Ep=500 keV). For a typical long GRB spectrum (the Band function with alpha=-1, beta=-2.5, and Ep=300 keV), the corresponding limiting peak flux is 3.1x10^-7 erg/cm^2/s (10 keV - 10 MeV, 2.944 s scale). All the quoted values are preliminary.