//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28968 SUBJECT: IceCube Alert 201130.85: Global MASTER-Net observations report DATE: 20/11/30 20:39:08 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), 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-IAC robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Spain (IAC Teide Observatory) was pointed to the IceCube Alert 201130.85 (trigger No 31476488,02h 01m 58.80s , -11d 36m 50.4s, R=0.71) errorbox 38 sec after notice time and 82 sec after trigger time at 2020-11-30 20:23:09 UT, with upper limit up to 17.2 mag. The observations began at zenith distance = 49 deg. The sun altitude is -29.5 deg. MASTER-SAAO robotic telescope located in South Africa (South African Astronomical Observatory) was pointed to the IceCube Alert 201130.85 errorbox 57 sec after notice time and 101 sec after trigger time at 2020-11-30 20:23:27 UT, with upper limit up to 17.8 mag. The observations began at zenith distance = 21 deg. The sun altitude is -28.6 deg. The galactic latitude b = -67 deg., longitude l = 174 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=1493295 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 93 | 2020-11-30 20:23:09 | MASTER-IAC | (02h 01m 03.53s , -11d 41m 42.3s) | C | 20 | 15.9 | 118 | 2020-11-30 20:23:09 | MASTER-IAC | (02h 01m 03.53s , -11d 41m 42.3s) | C | 70 | 16.7 | Coadd 111 | 2020-11-30 20:23:27 | MASTER-SAAO | (02h 00m 40.65s , -11d 40m 55.8s) | P/ | 20 | 16.1 | 111 | 2020-11-30 20:23:27 | MASTER-SAAO | (01h 59m 49.05s , -11d 41m 44.3s) | P\ | 20 | 17.2 | 132 | 2020-11-30 20:23:48 | MASTER-IAC | (02h 00m 56.87s , -11d 42m 43.8s) | C | 20 | 16.0 | 156 | 2020-11-30 20:24:07 | MASTER-SAAO | (02h 00m 34.15s , -11d 41m 30.6s) | P/ | 30 | 16.4 | 156 | 2020-11-30 20:24:07 | MASTER-SAAO | (01h 59m 42.53s , -11d 42m 19.3s) | P\ | 30 | 17.7 | 176 | 2020-11-30 20:24:27 | MASTER-IAC | (02h 01m 02.80s , -11d 42m 35.9s) | C | 30 | 16.4 | 211 | 2020-11-30 20:24:57 | MASTER-SAAO | (02h 00m 34.44s , -11d 40m 30.0s) | P/ | 40 | 16.6 | 211 | 2020-11-30 20:24:57 | MASTER-SAAO | (01h 59m 42.85s , -11d 41m 18.6s) | P\ | 40 | 17.8 | 231 | 2020-11-30 20:25:17 | MASTER-IAC | (02h 00m 59.89s , -11d 40m 47.7s) | C | 40 | 16.4 | 291 | 2020-11-30 20:25:17 | MASTER-IAC | (02h 00m 59.88s , -11d 40m 47.7s) | C | 160 | 17.2 | Coadd 275 | 2020-11-30 20:25:56 | MASTER-SAAO | (02h 00m 41.18s , -11d 41m 29.0s) | P/ | 50 | 16.7 | 275 | 2020-11-30 20:25:56 | MASTER-SAAO | (01h 59m 49.59s , -11d 42m 17.8s) | P\ | 50 | 17.7 | 295 | 2020-11-30 20:26:16 | MASTER-IAC | (02h 00m 59.92s , -11d 42m 37.5s) | C | 50 | 16.5 | 350 | 2020-11-30 20:27:06 | MASTER-SAAO | (02h 00m 35.36s , -11d 42m 28.8s) | P/ | 60 | 16.9 | 350 | 2020-11-30 20:27:06 | MASTER-SAAO | (01h 59m 43.80s , -11d 43m 17.5s) | P\ | 60 | 17.8 | 375 | 2020-11-30 20:27:26 | MASTER-IAC | (02h 01m 03.90s , -11d 40m 52.2s) | C | 70 | 16.7 | 469 | 2020-11-30 20:28:55 | MASTER-IAC | (02h 00m 57.69s , -11d 41m 51.7s) | C | 80 | 16.7 | 578 | 2020-11-30 20:30:34 | MASTER-IAC | (02h 00m 57.12s , -11d 40m 52.6s) | C | 100 | 16.8 | 713 | 2020-11-30 20:32:34 | MASTER-IAC | (02h 01m 02.57s , -11d 41m 53.8s) | C | 130 | 17.1 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28969 SUBJECT: IceCube-201130A: IceCube observation of a high-energy neutrino candidate event DATE: 20/11/30 22:54:49 GMT FROM: Cristina Lagunas Gualda at DESY The IceCube Collaboration (http://icecube.wisc.edu/) reports: On 20/11/30 at 20:21:46.48 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 1.322 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/134751_31476488.amon), more sophisticated reconstruction algorithms have been applied offline, with the direction refined to: Date: 20/11/30 Time: 20:21:46.48 UT RA: 30.54 (+ 1.13 - 1.31 deg 90% PSF containment) J2000 Dec: -12.10 (+ 1.15 - 1.13 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 is one Fermi-LAT 4FGL source inside the 90% localization region, 4FGL J0206.4-1151, located at RA 31.6 deg and Dec -11.86 deg (J2000), at a distance of 1.07 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: 28973 SUBJECT: Swift-XRT observations of IceCube 201130A DATE: 20/12/01 13:34:12 GMT FROM: Timothee Gregoire at Penn State J. DeLaunay (PSU), D. B. Fox (PSU), A. Keivani (Columbia U.), J.P. Osborne (U. Leicester), F. Krauss (PSU), T. Gregoire (PSU), P.A. Evans (U. Leicester), J.A. Kennea (PSU), H. A. Ayala Solares (PSU) and D.F. Cowen (PSU) report: Swift observed the field of IceCube 201130A (GCN Circ. 28969) between 20:52:42 2020 November 30 and 22:53:21 on 2020 November 30, collecting a total of 3.8 ks of cleaned photon counting (PC) mode data. The observations used a 4-point tiling pattern with a radius of ~0.3 degrees. We found 2 X-ray sources, as detailed below. All of these are known X-ray sources consistent with catalogued fluxes. We therefore do not claim any of them as the likely counterpart to IceCube 201130A. The 3-sigma upper limit in the field was in the range 4-7 x 10^-3 ct/sec. The detected sources were: Source no: 1 RA (J2000): 30.47644 [degrees] = 02h 01m 54.34s Dec (J2000): -11.8212 [degrees] = -11d 49' 16.3" Error: +4.4 [arcsec, 90% conf. radius] Count rate (0.3-10 keV): 7.7 (+3.8, -2.9) x 10-3 ct s-1 Flux (0.3-10 keV): 3.3 (+1.6, -1.2) x 10-13 erg cm-2 s-1 Note: This source may be affected by optical loading. Note: This source matches SIMBAD source HD12460. Source no: 2 RA (J2000): 30.48834 [degrees] = 02h 01m 57.20s Dec (J2000): -11.5423 [degrees] = -11d 32' 32.2" Error: +2.2 [arcsec, 90% conf. radius] Count rate (0.3-10 keV): 0.117 (+/-0.013) ct s-1 Flux (0.3-10 keV): 5.0 (+/-0.5) x 10-12 erg cm-2 s-1 Note: This source matches SIMBAD source ICRF J020157.1-113233 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28977 SUBJECT: IceCube-201130A: Not observable by Fermi-GBM DATE: 20/12/01 22:10:40 GMT FROM: Rachel Hamburg at UAH R. Hamburg (UAH) reports on behalf of the Fermi-GBM team: For the IceCube high-energy neutrino candidate event IceCube-201130A (GCN 28969), the reported neutrino location at: RA: 30.54 (+1.13 -1.31 deg 90% PSF containment) J2000 Dec: -12.10 (+1.15 -1.13 deg 90% PSF containment) J2000 was occulted by the Earth for Fermi-GBM from approximately 10.9 minutes prior until 24.7 minutes after event time. Therefore, the GBM observations are not constraining for prompt gamma-ray emission. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28978 SUBJECT: Fermi-LAT Gamma-ray Observations of IceCube-201130A DATE: 20/12/02 08:34:52 GMT FROM: Simone Garrappa at DESY S. Garrappa (DESY-Zeuthen), S. Buson (Univ. of Wuerzburg) and M. Kadler (Univ. of Wuerzburg) on behalf of the Fermi-LAT collaboration: We report an analysis of observations of the vicinity of the high-energy IC201130A neutrino event (GCN 28969) 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 2020-11-30 at 20:21:46.48 UT (T0) with J2000 position RA = 30.54 (+1.13, -1.31) deg, Decl. = -12.10 (+1.15, -1.13) deg (90% PSF containment). One cataloged gamma-ray (>100 MeV) source is located within the 90% IC201130A localization region. This is the source 4FGL J0206.4-1151 (4FGL, The Fermi-LAT collaboration 2020, ApJS, 247, 33), associated with the flat-spectrum radio quasar PMN J0206-1150 (Griffith et al. 1994, ApJS, 90, 179) at redshift z = 1.663 (Healey et al. 2008, ApJS, 175, 97). Based on a preliminary analysis of the LAT data over the timescales of 1-day and 1-month prior to T0, this object is not significantly detected (> 5 sigma). 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 IC201130A best-fit position. Assuming a power-law spectrum (photon index = 2.0 fixed) for a point source at the IC201130A best-fit position, the >100 MeV flux upper limit (95% confidence) is < 6.3e-10 ph cm^-2 s^-1 for ~12-years (2008-08-04 to 2020-11-30 UTC), and < 1.4e-8 (< 1.5e-7) 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: 28979 SUBJECT: Swift observations of the Fermi-LAT source 4FGL J0206.4-1151 in the error region of IceCube-201130A DATE: 20/12/02 14:17:04 GMT FROM: Timothee Gregoire at Penn State T. Gregoire (PSU), F. D'Ammando (INAF-IRA Bologna), D. B. Fox (PSU), A. Keivani (Columbia U.), J.P. Osborne (U. Leicester), F. Krauss (PSU), P.A. Evans (U. Leicester), J.A. Kennea (PSU), H. A. Ayala Solares (PSU), D.F. Cowen (PSU) and J. DeLaunay (PSU) report: Swift observed the location of 4FGL J0206.4-1151, the Fermi-LAT source closest to the location of IceCube 201130A (IceCube Collaboration; GCN Circ. 28969) for 4.0 ks between 14:42 UT and 18:05 UT on 2020 December 1. The source is detected by XRT at RA, Dec = 31.6094, -11.8440 (degrees) which corresponds to: RA (J2000): 02h 06m 26.25s Dec (J2000): -11d 50' 38.1" With an uncertainty of 6.4 arcsec (radius, 90% confidence). This position is 2.8 arcmin from the position of the flat spectrum radio quasar PMN J0206-1150, that is associated to the gamma-ray source 4FGL J0206.4-1151 in the Forth Fermi LAT source catalog (Abdollahi et al. 2020, ApJS, 247, 33). The X-ray spectrum (0.3-10 keV) can be fit by an absorbed power law model with a HI column density consistent with the Galactic value in the direction of the source (n_H = 1.7 x 10^20 cm^-2, Ben Bekhti N. et al., 2016, A&A, 594, A116) and a photon index of 1.7+/-0.7. The corresponding 0.3-10 keV flux (unabsorbed) is 1.6 (+1.1, -0.4) x 10^-13 erg cm^-2 s^-1. Simultaneous UVOT observations were performed on 2020 December 1 and the source is detected above 3 sigma in all UVOT filters. The measured magnitudes (Vega system) are V = 19.48 +/- 0.42, B = 19.68 +/- 0.21, U = 18.99 +/- 0.17, W1 = 19.24 +/- 0.18, M2 = 19.30 +/- 0.11, and W2 = 19.21 +/- 0.11. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28982 SUBJECT: IceCube-201130A: No counterpart candidates in INTEGRAL SPI-ACS and IBIS prompt observation DATE: 20/12/02 16:08:35 GMT FROM: Volodymyr Savchenko at ISDC,U of Geneve 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 combination of INTEGRAL all-sky detectors (following [1]): SPI/ACS, IBIS/Veto, and IBIS we have performed a search for a prompt gamma-ray counterpart of IceCube-201130A (GCN 28969). At the time of the event (2020-11-30 20:21:46 UTC, hereafter T0), INTEGRAL was operating in nominal mode. The peak of the event localization probability was at an angle of 113 deg with respect to the spacecraft pointing axis. This orientation implies strongly suppressed (3.8% of optimal) response of ISGRI, strongly suppressed (30% of optimal) response of IBIS/Veto, and somewhat suppressed (54% of optimal) response of SPI-ACS. The background within +/-300 seconds around the event was rather stable (excess variance 1.2). We have performed a search for any impulsive events in INTEGRAL SPI- ACS (as described in [2]), IBIS, and IBIS/Veto data. We do not detect any significant counterparts and estimate a 3-sigma upper limit on the 75-2000 keV fluence of 3.3e-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 ~2.8e-07 (1e-07) 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 7.64 | 0.3 | 3.3 | 0.698 +/- 0.213 +/- 0.223 | 0.263 34.1 | 0.75 | 3.3 | 0.436 +/- 0.134 +/- 0.139 | 0.508 9.37 | 0.15 | 3.3 | 0.989 +/- 0.302 +/- 0.316 | 0.624 -14.9 | 0.35 | 3.1 | 0.605 +/- 0.197 +/- 0.193 | 0.705 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: 28983 SUBJECT: IceCube-201130A: Upper limits from a search for additional neutrino events in IceCube DATE: 20/12/02 16:51:16 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-201130A (https://gcn.gsfc.nasa.gov/gcn3/28969.gcn3) in a time range of 2 days centered on the alert event time (2020-11-29 20:21:46.48 UTC to 2020-12-01 20:21:46.48 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% containment region of IceCube-201130A. We find that these data are consistent with atmospheric background expectations, with a p-value of 0.07. We accordingly derive a time-integrated muon-neutrino flux upper limit at the alert position of E^2 dN/dE = 1.4 x 10^-4 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 10 TeV and 10 PeV. A subsequent search was performed to include the month of data prior to the alert event (2020-10-31 20:21:46.48 UTC to 2020-12-01 20:21:46.48 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 1.5 x 10^-4 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: 28984 SUBJECT: IceCube-201130A: No significant detection in HAWC DATE: 20/12/03 01:44:04 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 2020/11/30 20:21:46 UTC, the IceCube collaboration reported a track-like very-high-energy event that has a high probability of being an astrophysical neutrino, IceCube-201130A. Location is at RA: 30.54 (+1.13/-1.31 deg 90% PSF containment) J2000 Dec: -12.10 (+1.15/-1.13 deg 90% PSF containment) J2000 (GCN circular 28969). 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 June 2019. We searched inside the reported IceCube error region. The most significant location, with p-value 5.23e-3 (1.38e-1 post-trials), is at RA 29.22 deg, Dec -12.71 deg (±0.21 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 = 5.46e-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 2020/11/29 05:47:42 UTC and ended 2020/12/01 06:08:38 UTC. The most significant location, with p-value S.SS (S.SS post-trials), is at RA 29.62 deg, Dec +10.92 deg (±0.92 deg 68% containment) J2000. We set a time-integrated 95% CL upper limit at the position of maximum significance of: E^2 dN/dE = 1.87e-11 (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: 28989 SUBJECT: IceCube-201130A: No Candidate Counterparts from the Zwicky Transient Facility DATE: 20/12/03 14:08:23 GMT FROM: Sven Weimann at Ruhr University Bochum Sven Weimann (Ruhr University Bochum), Robert Stein (DESY), Simeon Reusch (DESY) and Anna Franckowiak (DESY/Ruhr University Bochum) report: On behalf of the Zwicky Transient Facility (ZTF) and Global Relay of Observatories Watching Transients Happen (GROWTH) collaborations: We observed the localization region of the neutrino event IceCube-201130A (Lagunas Gualda et al., GCN 28969) with the Palomar 48-inch telescope, equipped with the 47 square degree ZTF camera (Bellm et al. 2019, Graham et al. 2019). We started observations in the g- and r-band beginning at 2020-12-01 03:30 UTC, approximately 7.1 hours after event time and observed in two consecutive nights. We covered 4.5 sq deg, corresponding to 98.3% of the reported localization region. This estimate accounts for chip gaps. Each exposure was 300s with a typical depth of 21.0 mag. The images were processed in real-time through the ZTF reduction and image subtraction pipelines at IPAC to search for potential counterparts (Masci et al. 2019). AMPEL (Nordin et al. 2019, Stein et al. 2020) was used to search the alerts database for candidates. We reject stellar sources (Tachibana and Miller 2018) and moving objects, and apply machine learning algorithms (Mahabal et al. 2019). No counterpart candidates were detected. ZTF and GROWTH are worldwide collaborations comprising Caltech, USA; IPAC, USA, WIS, Israel; OKC, Sweden; JSI/UMd, USA; U Washington, USA; DESY, Germany; MOST, Taiwan; UW Milwaukee, USA; LANL USA; Tokyo Tech, Japan; IITB, India; IIA, India; LJMU, UK; TTU, USA; SDSU, USA and USyd, Australia. ZTF acknowledges the generous support of the NSF under AST MSIP Grant No 1440341. GROWTH acknowledges generous support of the NSF under PIRE Grant No 1545949. Alert distribution service provided by DIRAC@UW (Patterson et al. 2019). Alert database searches are done by AMPEL (Nordin et al. 2019). Alert filtering is performed with the AMPEL Follow-up Pipeline (Stein et al. 2020). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 28994 SUBJECT: Swift follow-up observations of the flat spectrum radio quasar PMN J0206-1150 in the error region of IceCube-201130A DATE: 20/12/04 19:32:33 GMT FROM: Timothee Gregoire at Penn State T. Gregoire (PSU), F. D'Ammando (INAF-IRA Bologna), D. B. Fox (PSU), A. Keivani (Columbia U.), J. P. Osborne (U. Leicester), F. Krauss (PSU), P. A. Evans (U. Leicester), J. A. Kennea (PSU), H. A. Ayala Solares (PSU), D. F. Cowen (PSU) and J. DeLaunay (PSU) We report on continuing Swift observations of the flat spectrum radio quasar PMN J0206-1150, associated with the gamma-ray source 4FGL J0206.4-1151 (Abdollahi et al. 2020, ApJS, 247, 33), the Fermi-LAT source closest to the location of IceCube 201130A (IceCube Collaboration; GCN Circ. 28969). After the first Swift observation performed on 2020 December 1 (ATel #14240, GCN Circ. 28979), the source has been observed again by Swift between 20:39 UT on 2020 December 2 and 11:24 UT on 2020 December 3 for a total of 3.9 ks. The source has been detected by XRT with a net count rate of (2.2 +/- 0.9)e-3 cps. As a comparison, the net count rate of the source on December 1 was (3.1 +/- 0.9)e-3 cps, showing a mild decrease of the source activity in X-rays. Assuming a photon index of 1.7, as observed on December 1, and fitting the X-ray spectrum with an absorbed power law model with a HI column density consistent with the Galactic value in the direction of the source (n_H = 1.7 x 10^20 cm^-2, Ben Bekhti N. et al., 2016, A&A, 594, A116), we obtain a 0.3-10 keV flux (unabsorbed) of 4.1 (+2.4, -2.0) x 10^-14 erg cm^-2 s^-1. Simultaneous UVOT observations were performed on 2020 December 2-3 and the source is detected above 3 sigma in all UVOT filters, except for the V filter. The measured magnitudes (Vega system) are V > 19.46, B = 19.60 +/- 0.18, U = 18.72 +/- 0.16, W1 = 18.93 +/- 0.15, M2 = 19.17 +/- 0.10, and W2 = 19.21 +/- 0.12. Differently from the X-ray band, a moderate brightening has been observed from U to M2 filters on December 2-3 with respect to December 1. In GCN Circ. 28979 [and ATel #14240] we wrongly reported that the X-ray source detected by XRT was 2.8 arcmin from the position of PMN J0206-1150, while it should be 2.8 arcsec. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 29008 SUBJECT: IceCube-201130A: Optical and NIR Imaging Follow-up by Kanata Telescope DATE: 20/12/09 07:42:41 GMT FROM: Mahito Sasada at Hiroshima University Sasada, M., Nakaoka, T., Akitaya, H. (Hiroshima U.), Utsumi, Y. (Stanford U./SLAC) We report our optical and near-infrared imaging observations for the IceCube high-energy neutrino candidate event, IceCube-201130A (GCN Circ. 28969). We selected 11 radio sources from our BROS catalog (Itoh et al. 2020, ApJ 901, 3) including radio sources 3C 57, and 4FGL J0206.4-1151 (ATel #14235) and imaged each of them in R and J bands with the Kanata telescope using the HONIR imaging and spectropolarimeter (Akitaya et al. 2014, Proc. SPIE 9147, 91474O). We present magnitudes in the AB system. The upper limits are the 5-sigma detection limits. Each magnitude is calibrated by nearby stars listed in PanSTARRS for R, and in 2MASS catalogs for J. BROS_J0206.4-1150 was also observed by Swift (GCN Circ. 28994). They reported mild decrease of source activity in X-rays and a moderate brightening from U to M2 filter on December 2-3 with respect to December 1. Our observations on 2020-12-01 10:14UT and 2020-12-02 09:40UT in the R band shown below were not able to confirm this brightness trend by large photometric error. BROS_J0201.9-1132 (3C 57) RA:30.488288, Dec:-11.542607 MJD R J 59184.41560, 15.89+/-0.04, 16.04+/-0.04 59185.39238, 15.91+/-0.03, 16.09+/-0.04 59186.41061, 15.93+/-0.04, 16.12+/-0.05 59187.54670, 15.98+/-0.09, 16.19+/-0.06 59191.44694, 15.92+/-0.04, 16.08+/-0.03 BROS_J0206.4-1150 (4FGL J0206.4-1151) RA:31.608821, Dec:-11.844354 59184.42646, 19.5+/-0.3, >18.7 59185.40333, 19.8+/-0.3, >18.4 59191.46875, 19.6+/-0.3, >19.2 BROS_J0204.3-1157 RA:31.084787, Dec:-11.960983 59184.43740, 18.4+/-0.2, 17.2+/-0.1 59185.42506, 18.6+/-0.1, 17.3+/-0.1 59186.42147, 18.46+/-0.08, 17.32+/-0.08 59191.45787, 18.41+/-0.08, 17.37+/-0.09 BROS_J0203.7-1250 RA:30.942665, Dec:-12.846279 59184.45914, >19.8, >18.9 BROS_J0200.7-1258 RA:30.193870, Dec:-12.967430 59184.44823, >20.0, >19.0 BROS_J0158.8-0932 RA:29.721666, Dec:-9.539370 59184.48092, >19.7, >18.8 BROS_J0150.5-1212 RA:27.637326, Dec:-12.214537 59184.51353, >18.3, >18.3 BROS_J0155.9-0945 RA:28.988929, Dec:-9.759423 59184.47004, >20.3, >19.4 59185.44682, >20.4, >19.0 BROS_J0200.8-0936 RA:30.215875, Dec:-9.606755 59184.49623, >18.5, >17.5 BROS_J0202.0-1451 RA:30.523600, Dec:-14.863539 59184.52442, 17.9+/-0.2, 17.0+/-0.1 59191.47962, 17.8+/-0.1, 16.91+/-0.07 BROS_J0202.8-0930 RA:30.713050, Dec:-9.514563 59184.50265, >19.9, >19.0