//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24392 SUBJECT: IceCube-190504A - IceCube observation of a high-energy neutrino candidate event DATE: 19/05/04 22:57:44 GMT FROM: Claudio Kopper at IceCube/U of Alberta The IceCube Collaboration (http://icecube.wisc.edu/) reports: On 19/05/04 18:25:18.39 UT 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/766165_132518.amon), the detailed angular uncertainty is still being evaluated and will be published later. At this time we propose to use the preliminary values reported in the GCN Notice: Date: 19/05/04 Time: 18:25:18.39 UT RA: 65.7866 (J2000) Dec: -37.4431 (J2000) Error radius: 73.79 arcmin (90% containment) 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: 24395 SUBJECT: IceCube-190504A: MASTER optical follow-up observations DATE: 19/05/05 08:23:03 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, E. Gorbovskoy, N.Tyurina, V.Kornilov, D.Vlasenko, V.Vladimirov, D.Zimnukhov, A.Kuznetsov, P.Balanutsa, A. Chasovnikov, V.Topolev, F.Balakin, K.Zhirkov, D.Kuvshinov (Lomonosov Moscow State University, SAI, Physics Department), R. Podesta, C. Lopez, C.Francile, F. Podesta (Observatorio Astronomico Felix Aguilar OAFA, San Juan National University), H.Levato (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE, SJNU) R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres (The Instituto de Astrofisica de Canarias), D. Buckley (South African Astronomical Observatory), O. Gress, N.M. Budnev, O.Ershova, S.Yazev (Applied Physics Institute, Irkutsk State University), V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev (Blagoveschensk Educational State University), A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), 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 Alert190504.77 39 sec after notice time and 133 sec after trigger time at 2019-05-04 18:27:31 UT. MASTER-OAFA robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Argentina ( Observatorio Astronomico Felix Aguilar ) was pointed to the IceCube Alert190504.77 at 2019-05-04 23:10:52.949 UT. The cover map and images limits are available at https://master.sai.msu.ru/site/master2/event.php??not=2019-05-04%2018:26:52&sat=IceCube&gcrd=(65.7833d,-37.4425d)&eb=1.23&trig=2019-05-04%2018:25:18&n=Alert190504.77 The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24400 SUBJECT: Search for counterpart to IceCube-190504A with ANTARES DATE: 19/05/05 20:35:44 GMT FROM: Damien Dornic at CPPM,France Alexis Coleiro (APC/Univ Paris Diderot) and Damien Dornic (CPPM/CNRS) on behalf of the ANTARES Collaboration Using data from the ANTARES detector, we have performed a follow-up analysis of the recently reported single high-energy starting event (HESE) neutrino IceCube-190504A (GCN 24392). The reconstructed origin was 18 degrees below the horizon for ANTARES. No up-going muon neutrino candidate events were recorded within 3 degrees of the IceCube event coordinates during a +/- 1h time-window centered on the IceCube event time, and over which the potential source remained visible all time. A search over an extended time window of +/- 1 day has also yielded no detection (74% visibility). This leads to a preliminary 90% confidence level upper limit on the muon-neutrino fluence from a point source of 16 GeV.cm^-2 over the energy range 3.1 TeV - 3.5 PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and 32 GeV.cm^-2 (630 GeV - 316 TeV) for an E^-2.5 spectrum. ANTARES is the largest undersea neutrino detector (Mediterranean Sea) and it is primarily sensitive to astrophysical neutrinos in the TeV-PeV energy range. At 10 TeV, the median angular resolution for muon neutrinos is about 0.5 degrees. In the range 1-100 TeV ANTARES has a competitive sensitivity to this position in the sky. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24401 SUBJECT: Fermi-LAT Gamma-ray Observations of IceCube-190504A DATE: 19/05/05 20:47:04 GMT FROM: Sara Buson at GSFC/Fermi S. Garrappa (DESY-Zeuthen, DE), S. Buson (Univ. of Wuerzburg, DE; UMBC, USA) and S. Ciprini (INFN Roma Tor Vergata, ASI, IT) on behalf of the Fermi-LAT collaboration: We report an analysis of observations of the vicinity of the high-energy IC190504A neutrino event (GCN 24392 and https://gcn.gsfc.nasa.gov/notices_amon/42419327_132508.amon ) 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 2019-05-04 18:26:49 UTC (T0) with J2000 position RA = 65.7866 deg, Decl. = -37.4431 deg (74 arcmin and 25 arcmin 90% and 50% PSF containment, respectively). Two cataloged >100 MeV gamma-ray source are located within the 90% IC190504A localization error. The closest one is the object 4FGL J0420.3-3745 (The Fermi-LAT Fourth Source Catalog, arXiv:1902.10045) also catalogued as 3FHL J0420.4-3744 (Ajello, M. et al. 2017, ApJS, 232, 18), at a distance of roughly 37 arcmin, and associated with the radio source NVSS J042025-374443. Based on a preliminary analysis of the LAT data over the timescale of one week before T0, this object is not significantly detected at gamma rays. The second one is 4FGL J0428.6-3756 (a.k.a. 3FHL J0428.6-3756), associated with the blazar PKS 0426-380, located at a distance of roughly 72 arcmin. This object is significantly detected at gamma rays over a timescale of one week before T0, at a flux level consistent with the 10 years average, and does not display recent remarkable activity at gamma rays. We searched for the existence of intermediate (months to years) timescale emission from a new gamma-ray transient source. Preliminary analysis indicates no significant (>5sigma) new excess emission (> 100 MeV) within the IC190504A 90% confidence localization. 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 < 1e-9 ph cm^-2 s^-1 for ~10.8-years (2008-08-04 / 2019-05-04 UTC) and < 1.1e-9ph cm^-2 s^-1 for a 8-month integration time before T0. Since Fermi normally operates in an all-sky scanning mode, regular monitoring of this source will continue. For this source the Fermi-LAT contact persons are Simone Garrappa (simone.garrappa at desy.de ) and Sara Buson (sara.buson at astro.uni-wuerzburg.edu ). 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: 24405 SUBJECT: IceCube-190504A: Swift-XRT Follow-up Observations DATE: 19/05/06 11:00:22 GMT FROM: Azadeh Keivani at Columbia U IceCube-190504A: Swift-XRT Follow-up Observations A. Keivani (Columbia U.), D. B. Fox (PSU), P. A. Evans (U. Leicester), J. A. Kennea (PSU), M. Santander (U. Alabama), & F. Krauss (GRAPPA/API, University of Amsterdam) report: The Neil Gehrels Swift Observatory observed the field of the IceCube HESE astrophysical neutrino candidate event IceCube-190504A (revision 1, https://gcn.gsfc.nasa.gov/gcn3/24392.gcn3) beginning May 4, 20:09:37 UT (1.74 hours after the neutrino arrival time). Swift utilized its onboard 19-point tiling pattern to cover a region centered on R.A., Dec. (J2000) = 65.7866d, -37.4431d, with a radius of approximately 0.8 deg; estimated 90%-containment radius for this event is 1.23 deg. Swift-XRT collected ~800 s per field of PC mode data per tile between 20:12:40 UT on 4 May and 09:08:01 UT on 5 May. Data have been reduced using the analysis approach and software routines of Evans et al. 2014 (ApJS, 210, 8). Several X-ray sources are detected in these observations, most of which are previously uncataloged and relatively low in flux, consistent with expectations for serendipitous (unrelated) sources over a region of this extent. The highest-significance X-ray source is located at R.A. 66.17568d, Dec. -37.93938d (J2000), 35 arcmin away from the neutrino direction, and matches the known (SIMBAD) X-ray source QSO B0422-380 (1.4 arcsec away) as well as 1SXPS J042442.5-375618 (6 arcsec away). We recover it at a mean observed XRT count rate of 3.2 (+0.8, -0.7) e-2 ct s^-1, consistent with (1.5-sigma above) the cataloged flux from 1SXPS. Although the brightness of this object does not look significantly elevated over the previous Swift observations, it is catalogued as a blazar and would be interesting if there is other electromagnetic emission from this source. Fermi-LAT has reported (GCN Circular #24401) significant emission at gamma ray over a timescale of one week before the neutrino arrival time (at a flux level consistent with the 10 years average) but no recent remarkable activity at gamma rays. Excluding identified sources, the 3-sigma upper limit on the count rate of any point-like counterpart over the rest of the tiled region is 0.01 ct s^-1, which corresponds to a 0.3-10 keV flux of 4.0e-13 erg cm^-2 s^-1 for a typical AGN spectrum (nH=3e20 cm^-2, Gamma=1.7). Coordinates, count rates, and possible counterparts for the X-ray sources are provided below. Source, RA, Dec, Error_90 (arcsec), XRT count rate (ct s^-1), Possible counterparts ------------------------------------------------------------------------------------------------------------------ #1: 66.17568d, -37.93938d, 7.9, 3.2 (+0.8, -0.7) e-2, QSO B0422-380 (1.4 arcsec away) & 1SXPS J042442.5-375618 (6 arcsec away) ------------------------------------------------------------------------------------------------------------------ #2: 66.39382d, -37.70566d, 6.6, 1.3 (+0.7, -0.5) e-2, 1RXS J042532.5-374212 (25.4 arcsec away) ------------------------------------------------------------------------------------------------------------------ #3: 65.19589d, -37.26399d, 9.5, 1.0 (+0.6, -0.4) e-2, 1RXS J042449.3-365537 (13.2 arcsec away) ------------------------------------------------------------------------------------------------------------------ #4: 66.20972d, -36.92833d, 6.3, 1.4 (+0.6, -0.5) e-2, -- ------------------------------------------------------------------------------------------------------------------ #5: 65.70905d, -37.94807d, 7.5, 1.2 (+0.6, -0.5) e-2, -- ------------------------------------------------------------------------------------------------------------------ #6: 66.39458d, -37.70534d, 7.9, 1.3 (+0.7, -0.5) e-2, 1RXS J042532.5-374212 (27.1 arcsec away) ------------------------------------------------------------------------------------------------------------------ #7: 65.29548d, -38.09169d, 10.5, 1.3 (+0.6, -0.5) e-2, 1RXS J042110.9-380533 (2.9 arcsec away) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24407 SUBJECT: IceCube-190504A: Insight-HXMT/HE observation DATE: 19/05/06 13:40:07 GMT FROM: QiBin Yi at IHEP, HXMT Q. B. Yi, Q. Luo, C. Cai, S. Xiao, C. K. Li, X. B. Li, G. Li, J. Y. Liao, S. L. Xiong, C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, M. Wu, Y. P. Xu, S. N. Zhang (IHEP), report on behalf of the Insight-HXMT team: Insight-HXMT was taking data normally around the trigger time (T0=2019-05-04 18:25:18.39 UTC) of this high-energy neutrino event (GCN 24392), which was monitored without any occultation by the Earth. Within T0 ± 100 s, no significant excess events (SNR > 3 sigma) are found in a search of the Insight-HXMT/HE raw light curves. Assuming the counterpart GRB with three typical GRB Band spectral models, two typical duration timescales(1 s, 10 s) coming from the position of this neutrino event, the 5-sigma upper-limits fluence (0.2 - 5 MeV, incident energy) are reported below: Band model 1 (alpha=-1.9, beta=-3.7, Ep=70 keV): 1s: 4.9e-08 erg cm^-2 10s: 3.0e-07 erg cm^-2 Band model 2 (alpha=-1.0, beta=-2.3, Ep=230 keV): 1s: 6.9e-08 erg cm^-2 10s: 5.0e-07 erg cm^-2 Band model 3 (alpha=-0.0, beta=-1.5, Ep=1000 keV): 1s: 1.8e-07 erg cm^-2 10s: 1.8e-06 erg cm^-2 Further analysis will be reported in the following circulars. All measurements above are made with the CsI detectors operating in the regular mode with the energy range of about 80-800 keV (record energy). Only gamma-rays with energy greater than about 200 keV can penetrate the spacecraft and leave signals in the CsI detectors installed inside of the telescope. Insight-HXMT is the first Chinese space X-ray telescope, which was fundedjointly by the China National Space Administration (CNSA) and the Chinese Academy of Sciences (CAS). More information could be found at: http://www.hxmt.org. _______________________________________________ Hxmt-ba mailing list Hxmt-ba@maillist.ihep.ac.cn http://maillist.ihep.ac.cn/mailman/listinfo/hxmt-ba //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24410 SUBJECT: Search for additional neutrino events from the direction of IceCube-190504A with IceCube DATE: 19/05/06 16:15:33 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-190504A (https://gcn.gsfc.nasa.gov/gcn3/24392.gcn3) in a time range of 2 days centered on the alert event time (2019-05-03 18:26:49 UTC to 2019-05-05 18:26:49 UTC) during which IceCube was collecting good quality data. Excluding the event that prompted the alert, two additional track-like events are found in spatial coincidence with the 90% PSF containment of IceCube-190504A. We find that these data are well described by atmospheric background expectations, with a p-value of 0.06. Accordingly, these data would represent a time-integrated muon-neutrino flux upper limit assuming an E^-2 spectrum (E^2 dN/dE) at the 90% CL of 8.4 x 10^-4 TeV cm^-2 for this observation period. 90% of events IceCube would detect from a source at this declination with an E^-2 spectrum are between approximately 100 TeV and 20 PeV. A subsequent search was performed to include the previous month of data (2019-04-04 18:26:49 UTC to 2019-05-05 18:26:49 UTC). In this case, we report a p-value of 1.0, consistent with no significant excess of track events, and a corresponding time-integrated muon-neutrino flux upper limit assuming an E^-2 spectrum (E^2 dN/dE) at the 90% CL of 1.0 x 10^-3 TeV cm^-2. 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: 24416 SUBJECT: IceCube-190504A: MASTER optical monitoring analysis DATE: 19/05/07 10:57:24 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, O. Gress, E. Gorbovskoy, N.Tyurina, V.Kornilov, P.Balanutsa, D.Vlasenko, F.Balakin, V.Vladimirov, D.Zimnukhov, A.Kuznetsov, A. Chasovnikov, V.Topolev(Lomonosov Moscow State University, SAI, Physics Department), R. Podesta, C. Lopez, C.Francile, F. Podesta (Observatorio Astronomico Felix Aguilar OAFA, San Juan National University), H.Levato (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE, SJNU) R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres (The Instituto de Astrofisica de Canarias), D. Buckley (South African Astronomical Observatory), N.M. Budnev, O.Ershova (Applied Physics Institute, Irkutsk State University), V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev (Blagoveschensk Educational State University), A. Tlatov, V.Senik, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), MASTER-SAAO robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South African Astronomical Observatory was pointed to the IceCube-190504A (Kopper et al. GCN 24392) alert 39 sec after notice time (133 sec after trigger time) at 2019-05-04 18:27:31 UT (Lipunov et al. GCN 24395). MASTER-OAFA robotic telescope started IceCube-190504A inspection at 2019-05-04 23:10:52.949 UT. MASTER auto-detection system didn't find new or variable sources, that can be connected with this alert. But. MASTER observed this error-box during the following GRB/LVC alerts observations: event_name | grbtime | GRBcenter_coord2000 |Er.B.deg|Exper.| MASTERobs_starttime | mlim. --------------+---------------------+-------------------------------+-------+---------+-------------------------+------- GRB190504.77 | 2019-05-04 18:25:18 | ( 4h 23m 09s , -37d 26m 35s) | 1.2 | ICECUBE | 2019-05-04 18:27:31 | 18.6 GRB190313.15 | 2019-03-13 03:36:00 | ( 4h 27m 52s , -37d 12m 00s) | 14.3 | FERMI | 2019-03-13 20:40:04 | 18.8 GW190425 | 2019-04-29 00:21:41 | LVC S190425z | | LVC | 2019-04-29 00:06:38 | 18.3 GRB180826.06 | 2018-08-26 01:19:15 | ( 4h 09m 50s , -22d 26m 59s | 6.9 | FERMI | 2018-08-29 02:38:42 | 19.6 GRB180508.64 | 2018-05-08 15:23:50 | ( 3h 50m 48s , -39d 12m 00s) | 9.1 | FERMI | 2018-05-09 16:55:07 | 19.0 GRB180423.34 | 2018-04-23 08:16:05 | ( 7h 13m 24s , -30d 30m 00s) | 37.9 | FERMI | 2018-04-24 18:17:15 | 18.5 GRB180311.07 | 2018-03-11 01:45:53 | ( 4h 28m 24s , -43d 18m 00s) | 11.1 | FERMI | 2018-03-11 20:37:31 | 19.4 GRB180309.14 | 2018-03-09 03:28:35 | ( 3h 55m 52s , -39d 25m 00s) | 12.7 | FERMI | 2018-03-10 02:37:03 | 18.6 GRB180114.45 | 2018-01-14 10:42:23 | ( 3h 40m 40s , -44d 9m 00s) | 10.4 | FERMI | 2018-01-14 21:11:40 | 18.1 GRB171121.83 | 2017-11-21 20:01:59 | ( 5h 7m 40s , -36d 58m 00s) | 8.7 | FERMI | 2017-11-22 01:37:28 | 19.3 GRB171004.78 | 2017-10-04 18:46:40 | ( 2h 56m 40s , -37d 10m 59s) | 26.6 | FERMI | 2017-10-06 21:05:18 | 18.7 GRB171004.67 | 2017-10-04 16:07:16 | ( 5h 22m 52s , -26d 15m 00s) | 17.0 | FERMI | 2017-10-06 21:05:18 | 18.7 GRB170422.37 | 2017-04-22 08:58:23 | ( 4h 17m 52s , -45d 52m 60s) | 18.4 | FERMI | 2017-04-24 23:04:59 | 18.3 GRB170307.22 | 2017-03-07 05:15:05 | ( 4h 18m 48s , -30d 58m 60s) | 6.4 | FERMI | 2017-03-07 19:49:33 | 18.9 GRB160430.35 | 2016-04-30 08:22:08 | ( 2h 58m 56s , -16d 34m 00s) | 36.6 | FERMI | 2016-04-30 16:54:00 | 18.9 GRB160319.34 | 2016-03-19 08:08:10 | ( 2h 57m 52s , -14d 24m 00s) | 35.5 | FERMI | 2016-03-19 19:29:48 | 18.5 GRB150824.55 | 2015-08-24 13:14:25 | ( 4h 2m 56s , -46d 43m 60s) | 13.4 | FERMI | 2015-08-26 02:14:38 | 20.3 GRB150806.63 | 2015-08-06 15:07:37 | ( 3h 55m 12s , -54d 54m 00s) | 34.8 | FERMI | 2015-08-09 03:34:30 | 19.7 GRB150801.09 | 2015-08-01 02:16:43 | ( 4h 19m 08s , -36d 6m 00s) | 10.9 | FERMI | 2015-08-01 02:17:04 | 15.3 GRB141222.41 | 2014-12-22 09:53:57 | ( 6h 26m 56s , -54d 27m 00s) | 34.7 | FERMI | 2014-12-24 22:12:28 | 19.8 and during own survey Dec2014-May2019. We checked Swift sources (Keivani et al. GCN 24405 )in MASTER database. The 7th source is in maximum in optic now 1) 66.17568d, -37.93938d m_OT=19.6 at 2014-12-24 22:12:28.681, m_OT=19.6 at 2018-11-15 00:47:43.986, m_OT Sasada, M., Nakaoka, T., Akitaya, H., Kawabata K., S. (Hiroshima U), Utsumi, Y. (Stanford/SLAC), Itoh, R. (Bisei Astronomical Observatory), Morokuma, T. (U. Tokyo), Ohta, K., Yamanaka, M. (Kyoto U) In response to the IceCube-190503A alert (GCN Circular No. 24378), HONIR -- the optical-NIR muti-band simultaneous multi-capable instrument -- on the 1.5m Kanata telescope observed possible Blazar candidates. The candidates were selected from our sample prepared for finding an IceCube counterpart. None of them were flared up within two days observations. We also checked our images with archival PanSTARRS images, and didn't find any transient. ra, dec, 5/4 R J Ks, 5/5 R J Ks 119.797654, 6.627546, 19.6 18.8 ----, 19.4 19.0 ---- 120.038609, 6.164517, 20.3 19.4 17.4, 19.3 19.3 17.0 120.222161, 6.857248, 16.0 ---- ----, 17.7 17.9 ---- 120.267315, 6.441576, 19.1 18.6 ----, 18.6 18.6 ---- 120.318049, 6.476643, 17.3 15.8 ----, 17.6 18.0 ---- 120.375726, 6.197231, 19.8 19.2 17.5, 19.8 19.3 13.0 All limiting magnitudes with 5 sigma in AB unit are calibrated with PanSTARRS and 2MASS point sources. This result is consistent with GCN Circular No. 24409. We acknowledge OISTER collaboration.