//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26181 SUBJECT: LIGO/Virgo S191105e: Upper limits from IceCube neutrino searches DATE: 19/11/06 18:24:03 GMT FROM: Raamis Hussain at IceCube IceCube Collaboration (http://icecube.wisc.edu/) reports: Searches [1,2] for track-like muon neutrino events detected by IceCube consistent with the sky localization of gravitational-wave candidate S191105e in a time range of 1000 seconds [3] centered on the alert event time (2019-11-05 14:27:01.933 UTC to 2019-11-05 14:43:41.933 UTC) have been performed. During this time period IceCube was collecting good quality data. No significant track-like events are found in spatial coincidence of S191105e calculated from the map circulated in the 2-Initial notice. IceCube's sensitivity assuming an E^-2 spectrum (E^2 dN/dE) to neutrino point sources within the locations spanned by the 90% spatial containment of S191105e ranges from 0.029 to 0.694 GeV cm^-2 in a 1000 second time window. 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 [1] Bartos et al. arXiv:1810.11467 (2018) and Countryman et al.arXiv:1901.05486 (2019) [2] Braun et al., Astroparticle Physics 29, 299 (2008) [3] Baret et al., Astroparticle Physics 35, 1 (2011) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26182 SUBJECT: LIGO/Virgo S191105e: Identification of a GW compact binary merger candidate DATE: 19/11/06 18:24:36 GMT FROM: Leo Singer at GSFC The LIGO Scientific Collaboration and the Virgo Collaboration report: We identified the compact binary merger candidate S191105e during real-time processing of data from LIGO Hanford Observatory (H1), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) at 2019-11-05 14:35:21.933 UTC (GPS time: 1256999739.933). The candidate was found by the PyCBC Live [1], SPIIR [2], and GstLAL [3] analysis pipelines. The preliminary alert was delayed by approximately one day due to a GraceDB authentication issue. S191105e is an event of interest because its false alarm rate, as estimated by the online analysis, is 2.3e-08 Hz, or about one in 1 year, 4 months. The event's properties can be found at this URL: https://gracedb.ligo.org/superevents/S191105e The classification of the GW signal, in order of descending probability, is BBH (95%), Terrestrial (5%), BNS (<1%), NSBH (<1%), or MassGap (<1%). Assuming the candidate is astrophysical in origin, there is strong evidence against the lighter compact object having a mass < 3 solar masses (HasNS: <1%). Using the masses and spins inferred from the signal, there is strong evidence against matter outside the final compact object (HasRemnant: <1%). Two sky maps are available at this time and can be retrieved from the GraceDB event page: * "bayestar.fits.gz,0", a preliminary localization generated by BAYESTAR [4] for an earlier trigger, not the current preferred event, and * "bayestar.fits.gz,1", an initial localization generated by BAYESTAR [4]. For the bayestar.fits.gz,1 sky map, the 90% credible region is 1297 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1168 +/- 330 Mpc (a posteriori mean +/- standard deviation). For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo Public Alerts User Guide . [1] Nitz et al. PRD 98, 024050 (2018) [2] Qi Chu, PhD Thesis, The University of Western Australia (2017) [3] Messick et al. PRD 95, 042001 (2017) [4] Singer & Price PRD 93, 024013 (2016) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26183 SUBJECT: LIGO/Virgo S191105e: upper limits from AGILE/MCAL observations DATE: 19/11/06 18:47:33 GMT FROM: Alessandro Ursi at INAF/IAPS A. Ursi, C. Casentini (INAF/IAPS), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, G. Piano (INAF/IAPS), F. Lucarelli, C. Pittori, F. Verrecchia (SSDC, and INAF/OAR), A. Bulgarelli, V. Fioretti, N. Parmiggiani (INAF/OAS-Bologna), M. Pilia (INAF/OA-Cagliari), F. Longo (Univ. Trieste, and INFN Trieste), report on behalf of the AGILE Team: In response to the LIGO/Virgo GW event S191105e at T0 = 2019-11-05 14:35:21 (UT), a preliminary analysis of the AGILE minicalorimeter (MCAL) triggered data found no event candidates within a time interval covering -/+ 15 sec from the LIGO/Virgo T0. At the T0, about 50% of the S191105e 90% c.l. localization region was accessible to the AGILE MCAL.Three-sigma upper limits (ULs) are obtained for a 1 s integration time at different celestial positions within the accessible S191105e localization region, from a minimum of 1.55E-06 erg cm^-2 to a maximum of 7.19E-06 erg cm^-2 (assuming as spectral model a single power law with photon index 1.5). The AGILE-MCAL detector is a CsI detector with a 4 pi FoV, sensitive in the energy range 0.4-100 MeV. Additional analysis of AGILE data is in progress. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26184 SUBJECT: LIGO/Virgo S191105e: Global MASTER-Net observations report DATE: 19/11/06 18:50:55 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 (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-Amur robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the LIGO/Virgo S191105e errorbox 55 sec after trigger time at 2019-11-05 14:36:16 UT, with upper limit up to 18.5 mag. The observations began at zenith distance = 49 deg. The sun altitude is -54.8 deg. MASTER-Kislovodsk robotic telescope located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the LIGO/Virgo S191105e errorbox 12600 sec after trigger time at 2019-11-05 18:05:21 UT, with upper limit up to 19.4 mag. The observations began at zenith distance = 54 deg. The sun altitude is -44.8 deg. MASTER-IAC robotic telescope located in Spain (IAC Teide Observatory) started inspect of the LIGO/Virgo S191105e errorbox 41784 sec after trigger time at 2019-11-06 02:11:45 UT, with upper limit up to 21.1 mag. The observations began at zenith distance = 58 deg. The sun altitude is -66.8 deg. MASTER-SAAO robotic telescope located in South Africa (South African Astronomical Observatory) started inspect of the LIGO/Virgo S191105e errorbox 16 sec after notice time and 1 days 12494 sec after trigger time at 2019-11-06 18:03:35 UT, with upper limit up to 17.1 mag. Observations started at twilight. The observations began at zenith distance = 30 deg. The sun altitude is -11.7 deg. MASTER-Tavrida robotic telescope located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the LIGO/Virgo S191105e errorbox 29 sec after notice time and 1 days 12507 sec after trigger time at 2019-11-06 18:03:48 UT, with upper limit up to 14.7 mag. The observations began at zenith distance = 83 deg. The sun altitude is -39.0 deg. The galactic latitude b = -77 deg., longitude l = 296 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/ligo_1.php?id=10882 The observation and reduction will continue. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26185 SUBJECT: LIGO/Virgo S191105e: Upper limits from Fermi-GBM Observations DATE: 19/11/06 18:57:48 GMT FROM: Adam Goldstein at Fermi-GBM, USRA A. Goldstein (USRA) reports on behalf of the Fermi-GBM Team and the GBM-LIGO/Virgo group For S191105e and using the initial BAYESTAR skymap, Fermi-GBM was observing 77.5% of the localization probability at event time. There was no Fermi-GBM onboard trigger around the event time of S191105e (GCN Circ. 26182). 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 merger time, and also identified no counterpart candidates. Part of the LVC localization region is behind the Earth for Fermi, located at RA=315.6, Dec=21.5 with a radius of 67.5 degrees. We therefore set upper limits on impulsive gamma-ray emission for the LVC localization region visible to GBM at merger time. 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, weighted by GW localization probability (in units of 10^-7 erg/s/cm^2): Timescale soft norm hard -------------------------------------- 0.128 s: 4.1 6.9 14. 1.024 s: 1.3 2.1 4.7 8.192 s: 0.3 0.6 1.6 Assuming the median luminosity distance of 1168 Mpc from the GW detection, we estimate the following intrinsic luminosity upper limits over the 1 keV-10 MeV energy range (in units of 10^49 erg/s): Timescale soft norm hard -------------------------------------- 0.128 s: 10. 16. 53. 1.024 s: 3.3 4.8 18. 8.192 s: 0.8 1.4 6.1 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26186 SUBJECT: LIGO/Virgo S191105e: upper limits from AGILE/GRID observations DATE: 19/11/06 19:04:08 GMT FROM: Claudio Casentini at INAF-IAPS C. Casentini, A. Ursi (INAF/IAPS), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, G. Piano (INAF/IAPS), F. Lucarelli, C. Pittori, F. Verrecchia (SSDC, and INAF/OAR), A. Bulgarelli, V. Fioretti, N. Parmiggiani (INAF/OAS-Bologna), M. Pilia (INAF/OA-Cagliari), F. Longo (Univ. Trieste, and INFN Trieste), report on behalf of the AGILE Team: In response to the LIGO-Virgo GW event S191105e at T0 = 2019-11-05 14:35:21.933 UTC a preliminary analysis of the AGILE exposure at T0 shows that the Gamma-Ray Imaging Detector (GRID) exposure covered less than 10% of the 90% c.l. localization region (LR) (30% of 90% c.l. LR is occulted by Earth). We performed an analysis of the GRID data in the energy range 50 MeV - 10 GeV on T0, where good exposure of the S191105e 90% c.l. LR was available. No candidate gamma-ray transient was detected. The following preliminary GRID values of 3-sigma upper limit (UL) are obtained: from 1.44e-06 to 9.71e-06 erg cm^-2 s^-1, with exposure of about 11% of the LR over the time interval ( T0s ; T0 + 5s ); from 6.45e-07 to 9.88e-06 erg cm^-2 s^-1, with exposure of about 16% of the LR over the time interval ( T0s ; T0 + 10s ); from 3.65e-08 to 2.73e-06 erg cm^-2 s^-1, with exposure of about 52% of the LR over the time interval ( T0s ; T0 + 100s ); These measurements were obtained with AGILE observing a large portion of the sky in spinning mode. Additional analysis of AGILE data is in progress. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26187 SUBJECT: LIGO/Virgo S191105e: No counterpart candidates in INTEGRAL SPI-ACS and,IBIS prompt observation DATE: 19/11/06 19:04:23 GMT FROM: Carlo Ferrigno at IAAT/ISDC C. Ferrigno, V. Savchenko (ISDC/UniGE, Switzerland) Sergey Molkov (IKI, Russia) 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 a combination of the INTEGRAL all-sky detectors: SPI/ACS, IBIS/Veto, and IBIS (following [1]) we have performed a search for a prompt gamma-ray counterpart of S191105e (GCN 26182). At the time of the event (2019-11-05 14:35:21 UTC, hereafter T0), INTEGRAL was operating in nominal mode. The peak of the event localization probability was at an angle of 93 deg with respect to the spacecraft pointing axis. This orientation implies strongly suppressed (9.1% of optimal) response of ISGRI, strongly suppressed (27% of optimal) response of IBIS/Veto, and near-optimal (79% 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 2.3e-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 ~2e-07 (5.2e-08) erg/cm^2/s at 1 s (8 s) time scale in 75-2000 keV energy range. For the mean reported distance 1168 Mpc this corresponds to the limit on the total isotropic equivalent energy in 1 s of 3.7e+49 erg for the short GRB spectrum and for a long GRB spectrum isotropic equivalent luminosity in 1 s (8 s) of 2.7e+49 erg/s (8.5e+48 erg/s) We find: 4 likely background excesses that we report for completeness and in order of FAP in the search region of SPI-ACS data. scale | T | S/N | luminosity ( x 1e+49 erg/s) | FAP 13.8 | 167 | 3.4 | 12.2 +/- 5 +/- 7.36 | 0.113 0.15 | -2.86 | 3.1 | 12.2 +/- 4.85 +/- 7.37 | 0.358 2.55 | -295 | 3.6 | 3.32 +/- 1.17 +/- 2 | 0.701 0.5 | -168 | 4.3 | 9.36 +/- 2.65 +/- 5.66 | 0.797 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: 26188 SUBJECT: LIGO/Virgo S191105e: No counterpart candidates in HAWC observations DATE: 19/11/06 19:25:34 GMT FROM: Israel Martinez-Castellanos at UMD/HAWC The HAWC Collaboration (https://www.hawc-observatory.org) reports: The HAWC Collaboration performed a follow-up of the gravitational wave trigger S191105e (GCN #26182). At the time of the trigger the HAWC local zenith was oriented towards (RA, Dec) = (165.8deg, 19.1 deg). 24% of the GW candidate sky location probability fell within our observable field of view (0-45 deg zenith angle). We performed a search for a short timescale emission using 6 sliding time windows (dt = 0.3s, 1s, 3s, 10s, 30s and 100s), shifted forward in time by 20% of their width. We searched the 95% probability containment area in a timescale-dependent time period, from t0-5dt to t0+10dt, where t0 is the time of the GW trigger. No significant gamma-ray detection above the background was observed. The sensitivity of this analysis is greatly dependent on zenith angle, ranging from 28 deg to 45 deg for the area searched in this analysis. The 5sigma detection sensitivity to a 1s (100s) burst in the 80-800GeV energy range goes from 4.1e-6 erg/cm^2 to 1.1e-4 erg/cm^2 (2.5e-5 erg/cm^2 to 5.5e-4 erg/cm^2), depending on the zenith angle. HAWC is a TeV gamma ray water Cherenkov array located in the state of Puebla, Mexico. It is sensitive to the energy range ~0.1-100TeV, and monitors 2/3 of the sky every day with an instantaneous field-of-view of ~2 sr. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26189 SUBJECT: LIGO/Virgo S191105e : no neutrino counterpart candidate in ANTARES search DATE: 19/11/06 20:26:21 GMT FROM: Antoine Kouchner at ANTARES Collaboration M. Ageron (CPPM/CNRS), B. Baret (APC/CNRS), A. Coleiro (APC/Universite de Paris), M. Colomer (APC/Universite de Paris), D. Dornic (CPPM/CNRS), A. Kouchner (APC/Universite de Paris), T. Pradier (IPHC/Universite de Strasbourg) report on behalf of the ANTARES Collaboration: Using on-line data from the ANTARES detector, we have performed a follow-up analysis of the recently reported LIGO/Virgo S191105e event using the 90% contour of the Initial bayestar probability map provided by the GW interferometers (GCN#26182 ). The ANTARES visibility at the time of the alert, together with the 50% and 90% contours of the probability map are shown at http://antares.in2p3.fr/GW/S191105e_Initial.png . Considering the location probability provided by the LIGO/Virgo collaborations, there is a 66.4% chance that the GW emitter was in the ANTARES **upgoing** field of view at the time of the alert. No up-going muon neutrino candidate events were recorded in the ANTARES sky during a +/-500s time-window centered on the time 2019-11-05 14:35:21 and in the 90% contour of the S191105e event. The expected number of atmospheric background events in the region visible by ANTARES is 5.16e-04 in the +/- 500s time window. An extended search during +/- 1 hour gives no up-going muon neutrino coincidence. The expected number of atmospheric background events in the region visible by ANTARES is 3.72e-03 in this larger time window. ANTARES is the largest undersea neutrino detector, installed in the Mediterranean Sea, and it is primarily sensitive to 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: 26192 SUBJECT: LIGO/Virgo S191105e: no counterpart candidates in the Swift/BAT observations DATE: 19/11/07 01:15:59 GMT FROM: Amy Lien at GSFC D. M. Palmer (LANL), S. D. Barthelmy (NASA/GSFC), A. Y. Lien (GSFC/UMBC), T. Sakamoto (AGU), A. P. Beardmore (U. Leicester), M. G. Bernardini (INAF-OAB), A. A. Breeveld (MSSL-UCL), D. N. Burrows (PSU), S. Campana (INAF-OAB), S. B. Cenko (NASA/GSFC), G. Cusumano (INAF-IASF PA), A. D'Ai (INAF-IASFPA), P. D'Avanzo (INAF-OAB), V. D'Elia (ASI-ASDC), S. Emery (UCL-MSSL), P. A. Evans (U. Leicester), P. Giommi (ASI), C. Gronwall (PSU), D. Hartmann (Clemson U.), J. A. Kennea (PSU), N. Klingler (PSU), H. A. Krimm (NSF), N. P. M. Kuin (UCL-MSSL), F. E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB), J. A. Nousek (PSU), S. R. Oates (Uni. of Warwick), P. T. O'Brien (U. Leicester), J. P. Osborne (U. Leicester), C. Pagani (U. Leicester), K. L. Page (U.Leicester), M. J. Page (UCL-MSSL), M. Perri (ASDC), J. L. Racusin (NASA/GSFC), B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU), G. Tagliaferri (INAF-OAB), A. Tohuvavohu (Toronto), E. Troja (NASA/GSFC/UMCP) report on behalf of the Swift team: We report the search results in the BAT data within T0 +/- 100 s of the LVC event S191105e (LIGO/VIRGO Collaboration GCN Circ. 26182), where T0 is the LVC trigger time (2019-11-05T14:35:21.933 UTC). The center of the BAT field of view (FOV) at T0 is RA = 317.289 deg, DEC = 48.187 deg, and the roll angle is 258.590 deg. The BAT FOV (>10% partial coding) covers 11.73% of the integrated LVC localization probability, and 12.37% of the galaxy convolved probability (Evans et al. 2016). Note that the sensitivity in the BAT FOV changes with the partial coding fraction. Please see the BAT FOV figure in the summary page (link below) for the specific location of the LVC region relative to the BAT FOV. Within T0 +/- 100 s, no significant detections (signal-to-noise ratio >~ 5 sigma) are found in the BAT raw light curves with time bins of 64 ms, 1 s, and 1.6 s. Assuming an on-axis (100% coded) short GRB with a typical spectrum in the BAT energy range (i.e., a simple power-law model with a power-law index of -1.32, Lien & Sakamoto et al. 2016), the 5-sigma upper limit in the 1-s binned light curve corresponds to a flux upper limit (15-350 keV) of ~ 8.37 x 10^-8 erg/s/cm^2. Assuming a luminosity of ~ 2 x 10^47 erg/s (similar to GW170817) and an average Epeak of ~ 400 keV for short GRBs (Bhat et al. 2016), this flux upper limit corresponds to a distance of ~ 78.55 Mpc. No event data are available within T0 +/- 100 s. BAT retains decreased, but significant, sensitivity to rate increases for gamma-ray events outside of its FOV. About 66.72% of the integrated LVC localization probability was outside of the BAT FOV but above the Earth's limb from Swift's location, and the corresponding flux upper limits for this region are within roughly an order of magnitude higher than those within the FOV. The results of the BAT analysis are available at https://swift.gsfc.nasa.gov/results/BATbursts/team_web/S191105e/web/source_public.html //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26193 SUBJECT: LIGO/Virgo S191105e: Coverage and upper limits from MAXI/GSC observations DATE: 19/11/07 04:31:53 GMT FROM: Hitoshi Negoro at Nihon U H. Negoro (Nihon U.), N. Kawai (Tokyo Tech), S. Sugita, M. Serino (AGU), M. Nakajima, W. Maruyama, M. Aoki, K. Kobayashi (Nihon U.), T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN), T. Sakamoto, H. Nishida, A. Yoshida (AGU), Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, T. Sato (Chuo U.), M. Shidatsu (Ehime U.), M. Oeda, K. Shiraishi (Tokyo Tech), S. Nakahira, Y. Sugawara, S. Ueno, H. Tomida, M. Ishikawa, N. Isobe, R. Shimomukai, M. Tominaga (JAXA), Y. Ueda, A. Tanimoto, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake (Kyoto U.), H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.), M. Yamauchi, S. Iwahori, Y. Kurihara, K. Kurogi, K. Miike (Miyazaki U.), T. Kawamuro (NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC) report on behalf of the MAXI team: We examined MAXI/GSC all-sky X-ray images (2-20 keV) after the LVC trigger S191105e at 2019-11-05 14:35:21.933 UTC (GCN 26182). At the trigger time of S191105e, the high-voltage of MAXI/GSC was off, and it was turned on at T0+1729 sec (+28.8 min). The first one-orbit (92 min) scan observation with GSC after the event covered 72% of the 90% credible region of the bayestar skymap from 15:04:11 to 15:20:01 UTC (T0+1730 to T0+2680 sec). No significant new source was found in the region in the one-orbit scan observation. A typical 1-sigma averaged upper limit obtained in one scan observation is 20 mCrab at 2-20 keV. If you require information about X-ray flux by MAXI/GSC at specific coordinates, please contact the submitter of this circular by email. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26194 SUBJECT: LIGO/Virgo S191105e: No counterpart candidates in Fermi-LAT observations DATE: 19/11/07 06:17:36 GMT FROM: Magnus Axelsson at Stockholm U. M. Axelsson (KTH and Stockholm Univ.), N. Omodei (Stanford Univ.), D. Kocevski (NASA/MSFC), F. Longo (Univ. and INFN Trieste), E. Bissaldi (Politecnico and INFN Bari) and M. Moss (GWU) report on behalf of the Fermi-LAT Collaboration: We have searched data collected by the Fermi Large Area Telescope (LAT) on Nov 05, 2019, for possible high-energy (E > 100 MeV) gamma-ray emission in spatial/temporal coincidence with the LIGO/Virgo trigger S191105e (GCN 26182). We define "instantaneous coverage" as the integral over the region of the LIGO probability map that is within the LAT field of view at a given time, and "cumulative coverage" as the integral of the instantaneous coverage over time. Fermi-LAT had an instantaneous coverage of ~20% of the LIGO probability region at the time of the trigger (T0 = 2019-11-05 14:35:21.933 UTC) and reached ~100% cumulative coverage at approximately T0 + 3 ks. We performed a search for a transient counterpart within the observed region of the 90% contour of the LIGO map in a fixed time window from T0 to T0 + 10 ks. One significant excess (with TS>25) was found at R.A., Dec. = 342.2, -12.9, but it is likely associated with the known source RBS 1899 (lies within the 90% uncertainty region). We also performed a search which adapted the time interval of the analysis to the exposure of each region of the sky, and no additional excesses were found. Energy flux upper bounds between 100 MeV and 1 GeV for the fixed time interval of this search vary between 1.4e-10 and 1.3e-9 [erg/cm^2/s]. The Fermi-LAT point of contact for this event is Michael Moss (michaelmoss@gwmail.gwu.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: 26195 SUBJECT: LIGO/Virgo S191105e: Not observable by CALET DATE: 19/11/07 06:27:32 GMT FROM: Yuta Kawakubo at Louisiana State U./CALET S. Nakahira (RIKEN), A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU), Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), Y. Asaoka, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), N. Cannady (GSFC/UMBC), M. L. Cherry (LSU), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena), and the CALET collaboration: At the trigger time of the compact binary merger candidate S191105e, T0 = 2019-11-05 14:35:21.933 UT (The LIGO Scientific Collaboration and Virgo Collaboration, GCN Circ. 26182), the CALET Gamma-ray Burst Monitor (CGBM) high voltages were off (from T0-6 min to T0+27 min). The CALET Calorimeter (CAL) was operating in the high energy trigger mode at the trigger time of S191105e. Using the CAL data, we have searched for gamma-ray events in the 10-100 GeV band from -60 sec to +60 sec from the GW trigger time and found no candidates. There is no significant overlap with the LVC high probability localization region. The CAL FOV was centered at RA=223.0 deg, Dec=-27.4 deg at T0. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26196 SUBJECT: LIGO/Virgo S191105e: AstroSat CZTI upper limits DATE: 19/11/07 07:34:18 GMT FROM: Varun Bhalerao at Indian Inst of Tech V. Shenoy (IITB), A. Anumarlapudi (IUCAA), R. Gaikwad (IUCAA), S. Gupta (IUCAA), Aarthy E. (PRL), V. Bhalerao (IITB), D. Bhattacharya (IUCAA), A. R. Rao (TIFR), S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration: We have carried a search for X-ray candidates in Astrosat CZTI data in a 100-second window around the trigger time of the BBH merger event S191105e (UTC 2019-11-05 14:35:21.000, GraceDB event). CZTI is a coded aperture mask instrument that has considerable effective area for about 29% of the entire sky, but is also sensitive to brighter transients from the entire sky. At the time of merger, Astrosat's nominal pointing is RA, DEC = 9:50:13.4, 31:28:40.3 (147.5558,31.4779), which is 142 deg away from the maximum probability location. At the time of merger event, the Earth-satellite-transient angle corresponding to maximum probability location is ~ 44.14 deg and hence is occulted by Earth in satellite's frame. In a time interval of 100 sec around the event, the region of the localisation map which is not occulted by Earth in the satellite's frame has a cumulative probability of 0.36 (36%). CZTI data were de-trended to remove orbit-wise background variation. We then searched data from the four independent, identical quadrants to look for coincident spikes in the count rates. Searches were undertaken by binning the data in 0.1s, 1s, and 10s respectively. Statistical fluctuations in background count rates were estimated by using data from 10 (+-5) neighbouring orbits. We selected confidence levels such that the probability of a false trigger in a 1000 sec window is 10^-4. We do not find any evidence for any hard X-ray transient in this window, in the CZTI energy range of 20-200 keV. We use a detailed mass model of the satellite to calculate the direction-dependent instrument response for points in the visible sky. We then assume the source is modelled as a power law with photon index alpha = -1, and convert our count rate upper limits to direction-dependent flux limits. We obtain the following upper limits for source flux in the 20-200 keV band by taking a probability weighted mean over the visible sky: 0.1 s: flux limit= 6.34e-06 ergs/cm^2/s; fluence limit = 6.34e-07 ergs/cm^2 1.0 s: flux limit= 1.96e-06 ergs/cm^2/s; fluence limit = 1.96e-06 ergs/cm^2 10.0 s: flux limit= 2.36e-07 ergs/cm^2/s; fluence limit = 2.36e-06 ergs/cm^2 CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26213 SUBJECT: LIGO/Virgo S191105e: Upper limits from Insight-HXMT/HE observations DATE: 19/11/10 06:10:33 GMT FROM: Ce Cai at IHEP C. Cai, Y. G. Zheng, Q. Luo, S. Xiao, Q. B. Yi, Y. Huang, C. K. Li, G. Li, X. B. 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 reported LIGO/Virgo S191105e event (GCN #26182), trigger time 2019-11-05T14:35:21.933 UTC. At T0, about 78% of the LIGO localization region was covered by the Insight-HXMT without occultationby 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 GW counterpart GRB with three typical GRB Band spectral models, two typical duration timescales (1 s, 10 s) from the center of the LIGO-Virgo location probability map (RA=14 deg, DEC=-40 deg), 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): 1 s: 2.9e-07 erg cm^-2 10 s: 1.4e-06 erg cm^-2 Band model 2 (alpha=-1.0, beta=-2.3, Ep=230 keV): 1 s: 3.6e-07 erg cm^-2 10 s: 2.0e-06 erg cm^-2 Band model 3 (alpha=-0.0, beta=-1.5, Ep=1000 keV): 1 s: 4.3e-07 erg cm^-2 10 s: 3.1e-06 erg cm^-2 All measurements above are made with the CsI detectors operating in the regular mode with the energy range of about 80-800 keV (deposited 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 spacecraft. Insight-HXMT is the first Chinese space X-ray telescope, which was funded jointly by the China National Space Administration (CNSA) and the Chinese Academy of Sciences (CAS). More information could be found at: http://www.hxmt.org. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26215 SUBJECT: LIGO/Virgo S191105e: No significant candidates in FRAM-TAROT-GRANDMA observations DATE: 19/11/10 15:31:14 GMT FROM: Kateryna Barynova at Kiev Uni., GRANDMA K. Barynova (Kyiv Uni), P.A. Duverne (LAL), B. Gendre (OzGrav-UWA), N. Kochiashvili (Iliauni), S. Karpov, M. Masek, M. Prouza (FZU), M. Boer (Artemis), N. Christensen (Artemis), L. Eymar (Artemis), A. Klotz (IRAP), K. Noysena (Artemis, IRAP), S. Antier (APC), A. Coleiro (APC), D. Corre (LAL), M. Coughlin (Caltech), D. A. Kann (HETH/IAA-CSIC), D.Coward (OzGrav-UWA), J.G. Ducoin (LAL), P. Hello (LAL), C. Lachaud (APC), N. Leroy (LAL), C. C. Thoene (HETH/IAA-CSIC), D. Turpin (NAOC), X. Wang (THU) report on behalf of the FRAM network, TAROT network and GRANDMA collaborations: We performed tiled observations of the LIGO/Virgo S191105e event with the FRAM-Auger (FRAM-A), FRAM-CTA-N (FRAM-C), TAROT-Reunion (TRE), TAROT-Calern (TCA) and TAROT-Chili (TCH) telescopes operating in the r-band and visible located respectively at Pierre Auger observatory (Malargue, Argentina), Roque de los Muchachos observatory (La Palma, Spain), Les Makes astronomical observatory, the Cote d'Azur observatory and La Silla ESO observatory (LaS/ESO). The observation started on 11/08/19 00:10:14 UTC for FRAM-Auger which corresponds approximately to 3456 minutes after the GW trigger time. The observation started on 11/08/19 01:17:32 UTC for FRAM-CTA-N which corresponds approximately to 3523 minutes after the GW trigger time. The observation started on 11/07/19 15:32:23 UTC for TRE which corresponds approximately to 2938 minutes after the GW trigger time. For TCA it started on 11/07/19 22:37:51 UTC which corresponds approximately to 3363 minutes after the GW trigger time. For TCH it started on 11/07/19 23:55:24 UTC which corresponds approximately to 3441 minutes after the GW trigger time. We performed the following joint tiled observations [1]: +-------+------------+------------+---------+---------+---------+ | Tele | TStart | TEnd | RA | DEC | Proba | | scope | [UTC] | [UTC] | [deg] | [deg] | [%] | |-------+------------+------------+---------+---------+---------| |FRAM-A | 2019-11-08 | 2019-11-08 | 24.26 | -40.38 | 0.3 | | | 00:10:14 | 00:14:14 | | | | |FRAM-A | 2019-11-08 | 2019-11-08 | 24.61 | -41.35 | 0.3 | | | 00:15:17 | 00:19:17 | | | | |FRAM-A | 2019-11-08 | 2019-11-08 | 39.37 | -46.22 | 0.2 | | | 00:20:21 | 00:24:21 | | | | |FRAM-A | 2019-11-08 | 2019-11-08 | 38.56 | -47.19 | 0.2 | | | 00:25:23 | 00:29:23 | | | | |FRAM-A | 2019-11-08 | 2019-11-08 | 24.97 | -42.33 | 0.2 | | | 00:30:28 | 00:34:28 | | | | |FRAM-A | 2019-11-08 | 2019-11-08 | 25.54 | -40.38 | 0.2 | | | 00:35:30 | 00:39:30 | | | | |FRAM-A | 2019-11-08 | 2019-11-08 | 39.99 | -47.19 | 0.2 | | | 00:40:36 | 00:44:36 | | | | |FRAM-A | 2019-11-08 | 2019-11-08 | 37.97 | -46.22 | 0.2 | | | 00:45:37 | 00:49:37 | | | | |FRAM-A | 2019-11-08 | 2019-11-08 | 25.91 | -41.35 | 0.2 | | | 00:50:42 | 00:54:42 | | | | |FRAM-A | 2019-11-08 | 2019-11-08 | 40.00 | -45.24 | 0.2 | | | 00:55:46 | 00:59:46 | | | | |FRAM-A | 2019-11-08 | 2019-11-08 | 39.35 | -48.16 | 0.2 | | | 01:00:49 | 01:04:49 | | | | |FRAM-A | 2019-11-08 | 2019-11-08 | 38.62 | -45.24 | 0.1 | | | 01:05:51 | 01:09:51 | | | | |FRAM-A | 2019-11-08 | 2019-11-08 | 37.89 | -48.16 | 0.2 | | | 01:10:54 | 01:14:54 | | | | |FRAM-A | 2019-11-08 | 2019-11-08 | 37.14 | -47.19 | 0.1 | | | 01:15:55 | 01:18:55 | | | | |FRAM-A | 2019-11-08 | 2019-11-08 | 40.78 | -46.22 | 0.1 | | | 01:20:58 | 01:24:58 | | | | |FRAM-A | 2019-11-08 | 2019-11-08 | 26.82 | -40.38 | 0.1 | | | 01:26:03 | 01:30:03 | | | | |FRAM-A | 2019-11-08 | 2019-11-08 | 26.29 | -42.33 | 0.1 | | | 01:31:05 | 01:35:05 | | | | |FRAM-A | 2019-11-08 | 2019-11-08 | 27.20 | -41.35 | 0.1 | | | 01:36:06 | 01:40:06 | | | | |FRAM-A | 2019-11-08 | 2019-11-08 | 38.68 | -49.13 | 0.1 | | | 01:41:11 | 01:45:11 | | | | |FRAM-A | 2019-11-08 | 2019-11-08 | 37.24 | -45.24 | 0.1 | | | 01:46:14 | 01:50:14 | | | | |-------+------------+------------+---------+---------+---------| |FRAM-C | 2019-11-08 | 2019-11-08 | 193.18 | 77.00 | 0.06 | | | 01:17:32 | 01:21:32 | | | | |FRAM-C | 2019-11-08 | 2019-11-08 | 192.59 | 77.44 | 0.06 | | | 01:21:52 | 01:25:52 | | | | |FRAM-C | 2019-11-08 | 2019-11-08 | 190.95 | 76.57 | 0.06 | | | 01:26:11 | 01:30:11 | | | | |FRAM-C | 2019-11-08 | 2019-11-08 | 191.49 | 78.32 | 0.07 | | | 01:30:31 | 01:34:31 | | | | |FRAM-C | 2019-11-08 | 2019-11-08 | 193.62 | 78.32 | 0.07 | | | 01:34:52 | 01:38:52 | | | | |FRAM-C | 2019-11-08 | 2019-11-08 | 190.65 | 77.45 | 0.06 | | | 01:39:21 | 01:43:21 | | | | |FRAM-C | 2019-11-08 | 2019-11-08 | 196.54 | 76.57 | 0.06 | | | 01:43:43 | 01:47:43 | | | | |FRAM-C | 2019-11-08 | 2019-11-08 | 191.14 | 77.89 | 0.06 | | | 01:48:05 | 01:52:05 | | | | |FRAM-C | 2019-11-08 | 2019-11-08 | 195.25 | 77.89 | 0.06 | | | 01:52:28 | 01:56:28 | | | | |FRAM-C | 2019-11-08 | 2019-11-08 | 196.63 | 77.45 | 0.06 | | | 01:56:49 | 02:00:49 | | | | |FRAM-C | 2019-11-08 | 2019-11-08 | 196.65 | 77.01 | 0.06 | | | 02:01:08 | 02:05:08 | | | | |FRAM-C | 2019-11-08 | 2019-11-08 | 192.88 | 76.59 | 0.07 | | | 02:05:27 | 02:09:27 | | | | |FRAM-C | 2019-11-08 | 2019-11-08 | 194.80 | 77.46 | 0.06 | | | 02:09:49 | 02:13:49 | | | | |FRAM-C | 2019-11-08 | 2019-11-08 | 194.75 | 76.57 | 0.06 | | | 02:14:09 | 02:18:09 | | | | |FRAM-C | 2019-11-08 | 2019-11-08 | 193.15 | 77.90 | 0.06 | | | 02:18:28 | 02:22:28 | | | | |FRAM-C | 2019-11-08 | 2019-11-08 | 194.77 | 76.59 | 0.06 | | | 02:22:49 | 02:26:49 | | | | |FRAM-C | 2019-11-08 | 2019-11-08 | 196.14 | 76.15 | 0.05 | | | 02:27:09 | 02:31:09 | | | | |FRAM-C | 2019-11-08 | 2019-11-08 | 189.08 | 77.91 | 0.05 | | | 02:31:32 | 02:35:32 | | | | |FRAM-C | 2019-11-08 | 2019-11-08 | 197.41 | 77.90 | 0.05 | | | 02:35:54 | 02:39:54 | | | | |FRAM-C | 2019-11-08 | 2019-11-08 | 192.57 | 76.17 | 0.05 | | | 02:40:16 | 02:44:16 | | | | |-------+------------+------------+---------+---------+---------| | TRE | 2019-11-07 | 2019-11-08 | 16.364 | -40.909 | 4.7 | | | 15:32:23 | 00:09:41 | | | | | TRE | 2019-11-07 | 2019-11-07 | 10.909 | -40.909 | 4.6 | | | 15:45:35 | 15:51:58 | | | | | TRE | 2019-11-07 | 2019-11-08 | 15.429 | -36.818 | 2.2 | | | 16:04:21 | 15:35:02 | | | | | TRE | 2019-11-07 | 2019-11-08 | 40.645 | -45 | 1.6 | | | 16:17:31 | 15:48:13 | | | | | TRE | 2019-11-07 | 2019-11-07 | 37.895 | -49.091 | 1.4 | | | 16:29:49 | 22:59:13 | | | | | TRE | 2019-11-07 | 2019-11-08 | 20.571 | -36.818 | 1 | | | 16:42:55 | 16:13:20 | | | | | TRE | 2019-11-07 | 2019-11-07 | 0 | -32.727 | 0.9 | | | 17:01:43 | 17:08:04 | | | | | TRE | 2019-11-07 | 2019-11-07 | 23.226 | -45 | 0.7 | | | 17:36:11 | 21:55:55 | | | | | TRE | 2019-11-07 | 2019-11-07 | 10.286 | -36.818 | 4.6 | | | 17:47:07 | 22:08:03 | | | | | TRE | 2019-11-07 | 2019-11-07 | 5.143 | -36.818 | 4.6 | | | 17:59:14 | 22:21:23 | | | | | TRE | 2019-11-07 | 2019-11-07 | 5.455 | -40.909 | 0.9 | | | 19:16:01 | 23:37:25 | | | | | TRE | 2019-11-07 | 2019-11-07 | 126 | 24.545 | 0.7 | | | 21:36:12 | 23:50:51 | | | | | TRE | 2019-11-07 | 2019-11-07 | 127.317 | 20.455 | 0.9 | | | 23:18:23 | 23:24:40 | | | | | TRE | 2019-11-08 | 2019-11-08 | 21.818 | -40.909 | 4.4 | | | 00:28:34 | 00:34:51 | | | | |-------+------------+------------+---------+---------+---------| | TCA | 2019-11-07 | 2019-11-08 | 139.638 | 51.981 | 0.5 | | | 22:37:51 | 05:11:02 | | | | | TCA | 2019-11-07 | 2019-11-08 | 188.15 | 76.105 | 0.5 | | | 22:42:30 | 05:17:48 | | | | | TCA | 2019-11-08 | 2019-11-08 | 142.379 | 55.692 | 0.4 | | | 03:46:58 | 03:48:58 | | | | | TCA | 2019-11-08 | 2019-11-08 | 193.508 | 77.96 | 0.8 | | | 04:32:02 | 05:24:21 | | | | | TCA | 2019-11-08 | 2019-11-08 | 195.35 | 76.105 | 0.7 | | | 04:38:48 | 04:45:07 | | | | | TCA | 2019-11-08 | 2019-11-08 | 142.488 | 53.837 | 0.6 | | | 04:45:34 | 04:51:54 | | | | | TCA | 2019-11-08 | 2019-11-08 | 139.848 | 50.125 | 0.5 | | | 04:57:54 | 05:04:14 | | | | |-------+------------+------------+---------+---------+---------| | TCH | 2019-11-07 | 2019-11-08 | 5.287 | -32.686 | 0.8 | | | 23:55:24 | 06:29:05 | | | | | TCH | 2019-11-08 | 2019-11-08 | 7.456 | -32.686 | 0.7 | | | 00:02:10 | 00:06:19 | | | | | TCH | 2019-11-08 | 2019-11-08 | 9.625 | -33.636 | 0.3 | | | 00:06:45 | 06:41:37 | | | | | TCH | 2019-11-08 | 2019-11-08 | 15.255 | -39.959 | 1.5 | | | 00:25:59 | 07:01:42 | | | | | TCH | 2019-11-08 | 2019-11-08 | 15.308 | -40.041 | 1.5 | | | 00:32:40 | 07:08:13 | | | | | TCH | 2019-11-08 | 2019-11-08 | 12.563 | -38.141 | 1.4 | | | 00:45:07 | 07:20:39 | | | | | TCH | 2019-11-08 | 2019-11-08 | 10.24 | -38.141 | 1.4 | | | 00:51:51 | 07:27:11 | | | | | TCH | 2019-11-08 | 2019-11-08 | 10.371 | -38.223 | 1.4 | | | 00:58:35 | 07:34:07 | | | | | TCH | 2019-11-08 | 2019-11-08 | 5.394 | -34.505 | 1.4 | | | 01:05:19 | 01:11:37 | | | | | TCH | 2019-11-08 | 2019-11-08 | 10.486 | -39.959 | 1.2 | | | 01:17:46 | 07:53:05 | | | | | TCH | 2019-11-08 | 2019-11-08 | 7.742 | -36.323 | 1.1 | | | 01:24:17 | 07:59:48 | | | | | TCH | 2019-11-08 | 2019-11-08 | 7.617 | -34.505 | 1.1 | | | 01:31:15 | 08:06:32 | | | | | TCH | 2019-11-08 | 2019-11-08 | 22.276 | -40.041 | 1 | | | 01:50:14 | 08:25:31 | | | | | TCH | 2019-11-08 | 2019-11-08 | 22.407 | -39.959 | 1 | | | 01:56:56 | 08:32:13 | | | | | TCH | 2019-11-08 | 2019-11-08 | 12.87 | -39.959 | 1.7 | | | 02:22:21 | 06:48:08 | | | | | TCH | 2019-11-08 | 2019-11-08 | 12.986 | -40.041 | 1.7 | | | 02:29:20 | 06:54:58 | | | | | TCH | 2019-11-08 | 2019-11-08 | 7.939 | -36.405 | 1 | | | 03:53:06 | 08:18:42 | | | | | TCH | 2019-11-08 | 2019-11-08 | 12.635 | -38.223 | 1.5 | | | 04:57:55 | 05:04:14 | | | | | TCH | 2019-11-08 | 2019-11-08 | 5.478 | -36.323 | 1.3 | | | 05:30:19 | 07:46:24 | | | | +-------+------------+------------+---------+---------+---------+ TStart and TEnd refers respectively to the time of the first and last exposure for a given tile. Observations are not necessarily continuous in this interval. The Probability refers to the 2D spatial probability of the GW skymap enclosed in a given tile. Each FRAM-Auger tile is 1.0x1.0 degrees and 0.45x0.45 degrees for FRAM-CTA-N. Each TRE tile is 4.2x4.2 degrees and 1.9x1.9 degrees for TCA and TCH. These observations cover about 40% of the cumulative probability of the Bayestar skymap available on Nov 6, 2019 18:01:59 UTC. The typical limiting magnitude in R (AB mode) is 16.0 and 18.0 for a 120 s exposure for FRAM-CTA-N and FRAM-Auger, respectively. The typical limiting magnitude in AB mode is 17.0 and 18.0 for a 60.0 s exposure for TRE and TCA/TCH, respectively. The coverage map is available at: https://grandma-owncloud.lal.in2p3.fr/index.php/s/FnfqEwZtgcSxeLl No significant transient candidates were found during our low latency analysis [2,3]. GRANDMA (Global Rapid Advanced Network Devoted to the Multi-messenger Addicts) is a network of robotic telescopes connected all over the world with both photometry and spectrometry capabilities for Time- domain Astronomy [2]. Details on the FRAM and TAROT telescopes are available on the GRANDMA web pages https://grandma.lal.in2p3.fr/. [1] M. W Coughlin et al., MNRAS 2019, doi.org/10.1093/mnras/stz2485 [2] S. Antier et al., MNRAS 2019, arXiv:1910.11261, 2019 [3] K. Noysena et al., ApJ 2019, arXiv:1910.02770 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26245 SUBJECT: LIGO/Virgo S191105e: Updated Sky Localization DATE: 19/11/13 22:30:06 GMT FROM: Brandon Piotrzkowski at U of Wisconsin-Milwaukee The LIGO Scientific Collaboration and the Virgo Collaboration report: We have conducted further analysis of the LIGO Hanford Observatory (H1), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) data around the time of the compact binary merger (CBC) candidate S191105e (GCN Circular 26182). Parameter estimation has been performed using LALInference [1] and a new sky map, LALInference.fits.gz,0, distributed via GCN Notice, is available for retrieval from the GraceDB event page: https://gracedb.ligo.org/superevents/S191105e The preferred sky map at this time is LALInference.fits.gz,0. For the LALInference.fits.gz,0 sky map, the 90% credible region is 643 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1183 +/- 281 Mpc (a posteriori mean +/- standard deviation). For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo Public Alerts User Guide . [1] Veitch et al. PRD 91, 042003 (2015)