//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27950 SUBJECT: IceCube-200615A: IceCube observation of a high-energy neutrino candidate event DATE: 20/06/15 16:11:39 GMT FROM: Cristina Lagunas Gualda at DESY The IceCube Collaboration (http://icecube.wisc.edu/) reports: On 20/06/15 at 14:49:17.38 UT IceCube detected a track-like event with a high probability of being of astrophysical origin. The event was selected by the ICECUBE_Astrotrack_Gold alert stream. The average astrophysical neutrino purity for Gold alerts is 50%. This alert has an estimated false alarm rate of 0.29 events per year due to atmospheric backgrounds. The IceCube detector was in a normal operating state at the time of detection. After the initial automated alert (https://gcn.gsfc.nasa.gov/notices_amon_g_b/134191_17593623.amon), more sophisticated reconstruction algorithms have been applied offline, with the direction refined to: Date: 20/06/15 Time: 14:49:17.38 UT RA: 142.95 (+1.18 -1.45 deg 90% PSF containment) J2000 Dec: 3.66 (+1.19 -1.06 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. There are no Fermi-LAT 4FGL or 3FHL sources inside the 90% localization region. The closest source is 4FGL J0922.6+0434 located at RA 140.67 deg and Dec 4.58 deg (J2000), at a distance of 2.46 degrees from the best-fit location. 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: 27953 SUBJECT: IceCube Alert 200615.62: Global MASTER-Net observations report DATE: 20/06/15 17:13:10 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva, D.Kuvshinov, D. Cheryasov (Lomonosov Moscow State University, SAI, Physics Department), R. Podesta, C.Lopez, F. Podesta, C.Francile (Observatorio Astronomico Felix Aguilar OAFA), H.Levato (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE), R. Rebolo, M. Serra (The Instituto de Astrofisica de Canarias), D. Buckley (South African Astronomical Observatory), O.A. Gres, N.M. Budnev, O.Ershova (Irkutsk State University, API), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), V. Yurkov, A. Gabovich, Yu. Sergienko (Blagoveschensk Educational State University) MASTER-SAAO robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South Africa (South African Astronomical Observatory) was pointed to the IceCube Alert 200615.62 (trigger No 17593623,09h 33m 48.48s , +03d 47m 20.4s, R=0.92) errorbox 5739 sec after notice time and 5852 sec after trigger time at 2020-06-15 16:26:49 UT, with upper limit up to 18.7 mag. Observations started at twilight. The observations began at zenith distance = 45 deg. The sun altitude is -9.6 deg. The galactic latitude b = 38 deg., longitude l = 231 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=1382374 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 5942 | 2020-06-15 16:26:49 | MASTER-SAAO | (09h 30m 17.21s , +03d 46m 48.2s) | C | 180 | 15.8 | 5942 | 2020-06-15 16:26:49 | MASTER-SAAO | (09h 29m 23.02s , +03d 46m 13.0s) | C | 180 | 15.8 | 6370 | 2020-06-15 16:34:57 | MASTER-SAAO | (09h 35m 47.73s , +04d 08m 34.8s) | C | 60 | 17.7 | 6370 | 2020-06-15 16:34:57 | MASTER-SAAO | (09h 34m 53.19s , +04d 08m 01.2s) | C | 60 | 18.0 | 6510 | 2020-06-15 16:36:17 | MASTER-SAAO | (09h 30m 09.71s , +03d 46m 21.7s) | C | 180 | 17.7 | 6510 | 2020-06-15 16:36:17 | MASTER-SAAO | (09h 29m 15.24s , +03d 45m 47.4s) | C | 180 | 18.0 | 6730 | 2020-06-15 16:40:57 | MASTER-SAAO | (09h 35m 42.82s , +04d 07m 50.8s) | C | 60 | 18.7 | 6730 | 2020-06-15 16:40:57 | MASTER-SAAO | (09h 34m 48.55s , +04d 07m 17.1s) | C | 60 | 18.7 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27954 SUBJECT: IceCube-200615A: No counterpart candidates in INTEGRAL SPI-ACS prompt observation DATE: 20/06/15 17:51:12 GMT FROM: Maeve Doyle at U College Dublin, Ireland M. Doyle, A. Martin-Carrillo (UCD, Ireland) V. Savchenko, C. Ferrigno (ISDC/UniGE, Switzerland) J. Rodi (IAPS-Roma, Italy) A. Coleiro (APC, France) S. Mereghetti (INAF IASF-Milano, Italy) on behalf of the INTEGRAL multi-messenger collaboration: https://www.astro.unige.ch/cdci/integral-multimessenger-collaboration Using INTEGRAL/SPI-ACS realtime data (following [1]) we have performed a search for a prompt gamma-ray counterpart of IceCube-200615A (GCN 27950). At the time of the event (2020-06-15 14:49:17 UTC, hereafter T0), INTEGRAL was operating in nominal mode. The peak of the event localization probability was at an angle of 132 deg with respect to the spacecraft pointing axis. This orientation implies strongly suppressed (3.4% of optimal) response of ISGRI, somewhat suppressed (43% of optimal) response of IBIS/Veto, and somewhat suppressed (50% of optimal) response of SPI-ACS. The background within +/-300 seconds around the event was very stable (excess variance 1.1). We have performed a search for any impulsive events in INTEGRAL SPI- ACS (as described in [2]) data. We do not detect any significant counterparts and estimate a 3-sigma upper limit on the 75-2000 keV fluence of 3.5e-07 erg/cm^2 (within the 50% probability containment region of the source localization) 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 ~3.2e-07 (9.4e-08) erg/cm^2/s at 1 s (8 s) time scale in 75-2000 keV energy range. We report for completeness and in order of FAP, all excesses identified in the search region. We find 4 likely background excesses: T-T0 | scale | S/N | flux ( x 1e-06 erg/cm2/s) | FAP -4.06 | 0.3 | 3.3 | 0.709 +/- 0.223 +/- 0.271 | 0.143 -13.8 | 0.35 | 3.6 | 0.711 +/- 0.207 +/- 0.272 | 0.226 67.8 | 4.6 | 3.1 | 1.67 +/- 0.566 +/- 0.641 | 0.301 18.1 | 0.2 | 3.7 | 0.974 +/- 0.274 +/- 0.372 | 0.409 Note that FAP estimates (especially at timescales above 2s) may be possibly further affected by enhanced non-stationary local background noise. This list excludes any excesses for which FAP is close to unity. All results quoted are preliminary. This circular is an official product of the INTEGRAL Multi-Messenger team. [1] Savchenko et al. 2017, A&A 603, A46 [2] Savchenko et al. 2012, A&A 541A, 122S //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27957 SUBJECT: IceCube-200615A: Upper limits from Fermi-GBM Observations DATE: 20/06/15 20:31:57 GMT FROM: Joshua Wood at MSFC/Fermi-GBM J. Wood (NASA/MSFC) reports on behalf of the Fermi-GBM team: For the IceCube high-energy neutrino candidate event IceCube-200615A (GCN 27950), at the event time Fermi-GBM was observing the reported neutrino location at: RA: 142.95 (+1.18 -1.45 deg 90% PSF containment) J2000 Dec: 3.66 (+1.19 -1.06 deg 90% PSF containment) J2000 There was no Fermi-GBM onboard trigger around the event time of the neutrino candidate. An automated, blind search for short gamma-ray bursts below the onboard triggering threshold in Fermi-GBM also identified no counterpart candidates. The GBM targeted search, the most sensitive, coherent search for GRB-like signals, was run from +/-30 s around the neutrino candidate time. From this search, no significant signal was found related to IceCube-200615A. We set upper limits on impulsive gamma-ray emission. Using the representative soft, normal, and hard GRB-like templates described in arXiv:1612.02395, we set the following 3 sigma flux upper limits over 10-1000 keV (in units of 10^-7 erg/s/cm^2): Timescale Soft Normal Hard ------------------------------------------- 0.128 s: 7.5 11. 26. 1.024 s: 1.8 2.9 6.4 8.192 s: 0.4 0.9 2.2 These results are preliminary. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27968 SUBJECT: IceCube-200615A: Upper limits from a search for additional neutrino events in IceCube DATE: 20/06/16 16:08:39 GMT FROM: Alex Pizzuto at ICECUBE/U of Wisconsin The IceCube Collaboration (http://icecube.wisc.edu/) reports: IceCube has performed a search for additional track-like muon neutrino events arriving from the direction of IceCube-200615A (https://gcn.gsfc.nasa.gov/gcn3/27950.gcn3) in a time range of 2 days centered on the alert event time (2020-06-14 14:49:17.380 UTC to 2020-06-16 14:49:17.380 UTC) during which IceCube was collecting good quality data. Excluding the event that prompted the alert, zero additional track-like events are found in spatial coincidence with the 90% containment region of IceCube-200615A. We accordingly derive a time-integrated muon-neutrino flux upper limit at the alert position of E^2 dN/ dE = 3.3 x 10^-5 TeV cm^-2 at 90% CL, under the assumption of an E^-2 power law. 90% of events IceCube would detect from a source at this declination with an E^-2 spectrum are approximately between 1 TeV and 5 PeV. A subsequent search was performed to include the month of data prior to the alert event (2020-05-16 14:49:17.380 UTC to 2020-06-16 14:49:17.380 UTC). In this case, we report a p-value of 1.0, consistent with no significant excess of track-like events, and a corresponding time-integrated muon-neutrino flux upper limit assuming an E^-2 spectrum (E^2 dN/dE) of 5.9 x 10^-5 TeV cm^-2 at the 90% CL. 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: 27970 SUBJECT: Fermi-LAT Gamma-ray Observations of IceCube-200615A DATE: 20/06/16 21:20:18 GMT FROM: Simone Garrappa at DESY S. Garrappa (DESY-Zeuthen) and S. Buson (Univ. of Wuerzburg) on behalf of the Fermi-LAT collaboration: We report an analysis of observations of the vicinity of the high-energy IC200615A neutrino event (GCN 27950) with all-sky survey data from the Large Area Telescope (LAT), on board the Fermi Gamma-ray Space Telescope. The IceCube event was detected on 2020-06-15 at 14:49:17.38 UT (T0) with J2000 position RA =142.95 (+1.18 -1.45) deg, Decl. = 3.66 (+1.19 -1.06) deg 90% PSF containment. No cataloged >100 MeV gamma-ray sources (The Fermi-LAT Collaboration 2019, arXiv:1902.10045) are located within the 90% IC200615A localization error. We searched for intermediate (days to years) timescale emission from a new gamma-ray transient source. Preliminary analysis indicates no significant (> 5 sigma) new excess emission (> 100 MeV), at the IC200615A best-fit position. Assuming a power-law spectrum (photon index = 2.0 fixed) for a point source at the IceCube best-fit position, the >100 MeV flux upper limit (95% confidence) is < 3e-10 ph cm^-2 s^-1 for ~11-years (2008-08-04 / 2020-06-15 UTC), < 3e-9 (< 3e-8) ph cm^-2 s^-1 for a 1-month (1-day) integration time before T0. Since Fermi normally operates in an all-sky scanning mode, regular monitoring of this source will continue. For these observations the Fermi-LAT contact persons are S. Garrappa (simone.garrappa at desy.de ) and S. Buson (sara.buson at uni-wuerzburg.de ). The Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27972 SUBJECT: IceCube-200615A: No significant detection in HAWC DATE: 20/06/17 03:29:03 GMT FROM: Hugo Ayala at Pennsylvania State University Hugo Ayala (Penn State) reports on behalf of the HAWC collaboration (http://www.hawc-observatory.org/collaboration): On 2020/06/15 14:49:17 UTC, the IceCube collaboration reported a track-like very-high-energy event that has a high probability of being an astrophysical neutrino, IceCube-200615A. Location is at RA: 142.95 (+1.18/-1.45 deg 90% PSF containment) J2000 Dec: 3.66 (+1.19/-1.06 deg 90% PSF containment) J2000 (GCN circular 27950). We performed two types of analyses for the follow-up. The first is for a steady source in archival data and the second is a search for a transient source. We assume a power-law spectrum with an index of -2.3 for both analyses. Search for a steady source in archival data: The archival data spans from November 2014 to May 2018. We searched inside the reported IceCube error region. The most significant location, with p-value 7.89e-4 (2.35e-2 post-trials), is at RA 141.46 deg, Dec 2.91 deg (±0.15 deg 68% containment) J2000. We set a time-integrated 95% CL upper limit on gamma rays at the maximum position of: E^2 dN/dE = 3.08e-13 (E/TeV)^-0.3 TeV.cm^-2.s^-1 Search for a transient source. Since the event was not in our field of view at the time reported, we report the combined result for the transits before and after the IceCube event. Data acquisition started on 2020/06/14 01:10:07 UTC and ended 2020/06/16 01:16:55 UTC. The most significant location, with p-value 1.19e-2 (3.03e-1 post-trials), is at RA 141.68 deg, Dec 3.10 deg (±0.22 deg 68% containment) J2000. We set a time-integrated 95% CL upper limit at the position of maximum significance of: E^2 dN/dE = 7.04e-12 (E/TeV)^-0.3 TeV.cm^-2.s^-1 HAWC is a very-high-energy gamma-ray observatory operating in Central Mexico at latitude 19 deg. north. Operating day and night with over 95% duty cycle, HAWC has an instantaneous field of view of 2 sr and surveys 2/3 of the sky every day. It is sensitive to gamma rays from 300 GeV to 100 TeV. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27973 SUBJECT: Swift-XRT observations of IceCube 200615A DATE: 20/06/17 07:53:24 GMT FROM: Phil Evans at U of Leicester P.A. Evans (U. Leicester), T. Gregoire (PSU), J.A. Kennea (PSU), H. A. Ayala Solares (PSU), D.F. Cowen (PSU), J. DeLaunay (PSU) , D. B. Fox (PSU), A. Keivani (Columbia U.), F. Krauss (PSU), F.E. Marshell (GSFC) J.P. Osborne (U. Leicester) report: Swift observed the field of IceCube 200615A (GCN Circ. 27950) between 08:58:51 UT 2020 June 15 and 11:12:28 UT on 2020 June 16, collecting a total of 12.8 ks of cleaned photon counting (PC) mode data. The observations used a 7-point tiling pattern with a radius of ~0.5 degrees. We found 9 X-ray sources, as detailed below. All of these are either known X-ray sources consistent with catalogued fluxes, or are unknown but with count rates consistent with the previous non-detections. We therefore do not claim any of them as the likely counterpart to IceCube 200615A The 3-sigma upper limit in the field was in the range 3.6-6.4 x 10^-3 ct/sec. The detected sources were: Source 1: RA (J2000): `09h 31m 17.80s` = 142.82418 deg Dec (J2000): `+03d 31' 18.4"` = 3.52179 deg Err(radius): 2.5" Count rate (0.3-10 keV): 0.040 ( +/- 0.004) Flux (0.3-10 keV): 1.72 (+/- 0.19) x 10^-12 Notes: This source corresponds to 1RXS J093117.6+033146. Source 2: RA (J2000): `09h 31m 00.25s` = 142.75103 deg Dec (J2000): `+03d 30' 02.6"` = 3.50071 deg Err(radius): 6.9" Count rate (0.3-10 keV): 2.3 (+1.7, -1.1) x 10^-3 Flux (0.3-10 keV): 10 (+7, -5) x 10^-14 Notes: This does not match a catalogued X-ray source, but the RASS 3-sigma upper limit at this position corresponds to 0.028 ct/sec in XRT. WARNING: This was a low significance detection which may well be spurious. Source 3: RA (J2000): `09h 30m 32.99s` = 142.63746 deg Dec (J2000): `+03d 44' 43.2"` = 3.74534 deg Err(radius): 4.0" Count rate (0.3-10 keV): 0.020 ( +/- 0.004) Flux (0.3-10 keV): 8.5 (+1.8, -1.6) x 10^-13 Notes: This does not match a catalogued X-ray source, but the RASS 3-sigma upper limit at this position corresponds to 0.031 ct/sec in XRT. The position is consistent with 2MASX J09303302+0344432 Source 4: RA (J2000): `09h 33m 04.66s` = 143.26942 deg Dec (J2000): `+03d 56' 42.4"` = 3.94512 deg Err(radius): 5.6" Count rate (0.3-10 keV): 8.7 (+3.1, -2.5) x 10^-3 Flux (0.3-10 keV): 3.8 (+1.3, -1.1) x 10^-13 Notes: This source corresponds to 1RXS J093305.7+035648. Source 5: RA (J2000): `09h 30m 36.31s` = 142.65130 deg Dec (J2000): `+03d 31' 25.3"` = 3.52369 deg Err(radius): 5.0" Count rate (0.3-10 keV): 3.4 (+1.6, -1.2) x 10^-3 Flux (0.3-10 keV): 1.5 (+0.7, -0.5) x 10^-13 Notes: This does not match a catalogued X-ray source, but the RASS 3-sigma upper limit at this position corresponds to 0.021 ct/sec in XRT. WARNING: This was a low significance detection which may well be spurious. Source 6: RA (J2000): `09h 32m 01.68s` = 143.00700 deg Dec (J2000): `+03d 18' 57.7"` = 3.31602 deg Err(radius): 5.8" Count rate (0.3-10 keV): 7.8 (+2.8, -2.3) x 10^-3 Flux (0.3-10 keV): 3.34 (+1.22, -0.98) x 10^-13 Notes: This does not match a catalogued X-ray source, but the RASS 3-sigma upper limit at this position corresponds to 0.12 ct/sec in XRT. The position is consistent with QSO J0932+0318 Source 7: RA (J2000): `09h 30m 57.98s` = 142.74159 deg Dec (J2000): `+03d 31' 51.0"` = 3.53083 deg Err(radius): 4.4" Count rate (0.3-10 keV): 1.95 (+1.20, -0.86) x 10^-3 Flux (0.3-10 keV): 8 (+5, -4) x 10^-14 Notes: This does not match a catalogued X-ray source, but the RASS 3-sigma upper limit at this position corresponds to 0.027 ct/sec in XRT. WARNING: This was a low significance detection which may well be spurious. Source 8: RA (J2000): `09h 32m 53.51s` = 143.22296 deg Dec (J2000): `+04d 05' 00.4"` = 4.08343 deg Err(radius): 5.2" Count rate (0.3-10 keV): 5.4 (+2.6, -1.9) x 10^-3 Flux (0.3-10 keV): 2.31 (+1.10, -0.84) x 10^-13 Notes: This does not match a catalogued X-ray source, but the RASS 3-sigma upper limit at this position corresponds to 0.035 ct/sec in XRT. Source 9: RA (J2000): `09h 30m 58.40s` = 142.74333 deg Dec (J2000): `+03d 48' 33.3"` = 3.80925 deg Err(radius): 4.9" Count rate (0.3-10 keV): 2.3 (+2.1, -1.3) x 10^-3 Flux (0.3-10 keV): 10 (+9, -6) x 10^-14 Notes: This does not match a catalogued X-ray source, but the RASS 3-sigma upper limit at this position corresponds to 0.017 ct/sec in XRT. The position is consistent with SDSS-C4-DR3 1119 WARNING: This was a low significance detection which may well be spurious. All errors are at the 90% confidence level, fluxes are observed flux in erg cm^-2 s^-1 and are calculated assuming an absorbed power-law with NH=3e20 and Gamma=1.7 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27979 SUBJECT: Swift/UVOT Observations of IceCube 200615A DATE: 20/06/18 12:15:15 GMT FROM: Frank Marshall at Swift/UVOT F.E. Marshall (GSFC), P.A. Evans (U. Leicester), T. Gregoire (PSU), J.A. Kennea (PSU), H. A. Ayala Solares (PSU), D.F. Cowen (PSU), J. DeLaunay (PSU) , D. B. Fox (PSU), A. Keivani (Columbia U.), F. Krauss (PSU), and J.P. Osborne (U. Leicester) report: Swift observed the field of IceCube 200615A (GCN Circ. 27950) between 08:58:51 UT 2020 June 15 and 11:12:28 UT on 2020 June 16. The observations used 7 pointing directions to tile the inner part of the 90% confidence region for the neutrino event. The results of the XRT observations were reported by Evans et al. (GCN Circ. 27973). UVOT observed the 7 tiling directions using the U filter covering a total of ~0.57 deg**2. The UVOT field-of-view is co-aligned with the XRT's but is smaller than the XRT's. We analyzed the longest exposure for each direction, which ranged from 337 s to 363 s. The averge exposure was 348 s. No uncatalogued point sources were found with a typical sensitivity limit of 19.0 mag. We also searched for counterparts to the XRT sources reported by Evans et al. (GCN Circ. 27973). Sources 1, 3, 4, and 6 were detected with UVOT and are also in the Digital Sky Survey. Source 2 was not detected with UVOT. Source 9 is near a bright galaxy, which was detected with UVOT. Sources 5, 7, and 8 are outside the field-of-view of UVOT for all the observations.