//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26202 SUBJECT: LIGO/Virgo S191109d: Identification of a GW compact binary merger candidate DATE: 19/11/09 01:50:16 GMT FROM: Brandon Piotrzkowski at U of Wisconsin-Milwaukee The LIGO Scientific Collaboration and the Virgo Collaboration report: We identified the compact binary merger candidate S191109d during real-time processing of data from LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) at 2019-11-09 01:07:17.221 UTC (GPS time: 1257296855.221). The candidate was found by the SPIIR [1], CWB [2], GstLAL [3], MBTAOnline [4], and PyCBC Live [5] analysis pipelines. S191109d is an event of interest because its false alarm rate, as estimated by the online analysis, is 1.5e-13 Hz, or about one in 2e5 years. The event's properties can be found at this URL: https://gracedb.ligo.org/superevents/S191109d The classification of the GW signal, in order of descending probability, is BBH (>99%), Terrestrial (<1%), BNS (<1%), NSBH (<1%), or MassGap (<1%). Assuming the candidate is astrophysical in origin, the probability that the lighter compact object has a mass < 3 solar masses (HasNS) is <1%. Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. One sky map is available at this time and can be retrieved from the GraceDB event page: * “bayestar.fits.gz,0”, an initial localization generated by BAYESTAR [6], distributed via GCN notice about 9 minutes after the candidate event time. For the bayestar.fits.gz,0 sky map, the 90% credible region is 1487 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1810 +/- 604 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] Qi Chu, PhD Thesis, The University of Western Australia (2017) [2] Klimenko et al. PRD 93, 042004 (2016) [3] Messick et al. PRD 95, 042001 (2017) [4] Adams et al. CQG 33, 175012 (2016) [5] Nitz et al. PRD 98, 024050 (2018) [6] Singer & Price PRD 93, 024013 (2016) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26203 SUBJECT: LIGO/Virgo S191109d: Upper limits from IceCube neutrino searches DATE: 19/11/09 03:02:00 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 S191109d in a time range of 1000 seconds [3] centered on the alert event time (2019-11-09 00:58:57.221 UTC to 2019-11-09 01:15:37.221 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 S191109d 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 S191109d ranges from 0.029 to 0.659 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] PoS(ICRC2019)918 and Braun et al., Astroparticle Physics 29, 299 (2008) [3] Baret et al., Astroparticle Physics 35, 1 (2011) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26204 SUBJECT: LIGO/Virgo S191109d: Coverage and upper limits from MAXI/GSC observations DATE: 19/11/09 03:23:34 GMT FROM: Motoko Serino at RIKEN/MAXI N. Kawai (Tokyo Tech), H. Negoro (Nihon U.), 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 S191109d at 2019-11-09 01:07:17.220 UTC (GCN 26202). At the trigger time of S191109d, the high-voltage of MAXI/GSC was off, and it was turned on at T0+335 sec (+5.6 min). The first one-orbit (92 min) scan observation with GSC after the event covered 91% of the 90% credible region of the bayestar skymap from 01:20:47 to 02:33:17 UTC (T0+810 to T0+5160 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: 26205 SUBJECT: LIGO/Virgo S191109d: Upper limits from Fermi-GBM Observations DATE: 19/11/09 05:51:52 GMT FROM: Peter Veres at UAH P. Veres (UAH) reports on behalf of the Fermi-GBM Team and the GBM-LIGO/Virgo group: For S191109d and using the initial BAYESTAR skymap, Fermi-GBM was observing 87.2% of the localization probability at event time. There was no Fermi-GBM onboard trigger around the event time of S191109d (GCN 26202). 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= 320.9, Dec= 12.1 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 normal hard -------------------------------------- 0.128 s: 6.3 9.5 23 1.024 s: 1.5 2.3 5.5 8.192 s: 0.50 0.76 1.4 Assuming the median luminosity distance of 1810 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 Normal Hard ------------------------------------ 0.128s: 38 52 210 1.024s: 9.2 13 50 8.192s: 3.1 4.1 13 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26206 SUBJECT: LIGO/Virgo S191109d: upper limits from AGILE/MCAL observations DATE: 19/11/09 05:57:52 GMT FROM: Carlotta Pittori at ASI SSDC, INAF-OAR C. Pittori (SSDC, and INAF/OAR), V. Fioretti (INAF/OAS-Bologna), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, C. Casentini, G. Piano, A. Ursi (INAF/IAPS), F. Lucarelli, F. Verrecchia (SSDC, and INAF/OAR), A. Bulgarelli, 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 S191109d at T0 = 2019-11-09 01:07:17 (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, 100% of the S191109d 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 S191109d localization region, from a minimum of 1.47E-06 erg cm^-2 to a maximum of 6.95E-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: 26207 SUBJECT: LIGO/Virgo S191109d: No counterpart candidates in INTEGRAL SPI-ACS,prompt observation DATE: 19/11/09 06:48:58 GMT FROM: Sergey Molkov at Space Research Inst., Moscow Sergey Molkov (IKI, Russia), Maeve Doyle (UCD, Ireland) V. Savchenko, C. Ferrigno (ISDC/UniGE, Switzerland) J. Rodi (IAPS-Roma, Italy) A. Coleiro (APC, France) S. Mereghetti (INAF IASF-Milano, Italy) on behalf of the INTEGRAL multi-messenger collaboration: https://www.astro.unige.ch/cdci/integral-multimessenger-collaboration Using INTEGRAL/SPI-ACS realtime data (following [1]) we have performed a search for a prompt gamma-ray counterpart of S191109d (GCN 26202). At the time of the event (2019-11-09 01:07:17 UTC, hereafter T0), INTEGRAL was operating in nominal mode. The peak of the event localization probability was at an angle of 120 deg with respect to the spacecraft pointing axis. This orientation implies strongly suppressed (4.8% of optimal) response of ISGRI, somewhat suppressed (54% of optimal) response of IBIS/Veto, and strongly suppressed (20% of optimal) response of SPI-ACS. The background within +/-300 seconds around the event was rather stable (excess variance 1.3). We have performed a search for any impulsive events in INTEGRAL SPI- ACS (as described in [2]) data. We do not detect any significant counterparts and estimate a 3-sigma upper limit on the 75-2000 keV fluence of 5.3e-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 ~4.8e-07 (6.2e-08) erg/cm^2/s at 1 s (8 s) time scale in 75-2000 keV energy range. For the mean reported distance 1810.0 Mpc this corresponds to the limit on the total isotropic equivalent energy in 1 s of 2.1e+50 erg for the short GRB spectrum and for a long GRB spectrum isotropic equivalent luminosity in 1 s (8 s) of 6.2e+49 erg/s (2.4e+49 erg/s) We report for completeness and in order of FAP, all excesses identified in the search region. We find: 2 likely background excesses: scale | T | S/N | luminosity ( x 1e+50 erg/s) | FAP 4.5 | -31.8 | 3.2 | 11.6 +/- 5.18 +/- 11.8 | 0.0977 0.5 | 178 | 4.4 | 4.52 +/- 1.56 +/- 4.6 | 0.815 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: 26208 SUBJECT: LIGO/Virgo S191109d: upper limits from AGILE-GRID observations mailed-by: DATE: 19/11/09 06:57:35 GMT FROM: Carlotta Pittori at ASI SSDC, INAF-OAR V. Fioretti (INAF/OAS-Bologna), C. Pittori (SSDC, and INAF/OAR), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, C. Casentini, G. Piano, A. Ursi (INAF/IAPS), F. Lucarelli, F. Verrecchia (SSDC, and INAF/OAR), A. Bulgarelli, 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 S191109d at T0 = 2019-11-09 01:07:17.221 UTC a preliminary analysis of the AGILE exposure at T0 shows that the Gamma-Ray Imaging Detector (GRID) exposure covered about 25% of the 90% c.l. localization region (LR) (0% of 90% c.l. localization region (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 S191109d 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 7.77e-07 to 8.79e-06 erg cm^-2 s^-1, with exposure of about 26% of the LR over the time interval ( T0 -2s ; T0 + 2s ); from 6.16e-07 to 8.61e-06 erg cm^-2 s^-1, with exposure of about 25% of the LR over the time interval ( T0s ; T0 + 5s ); from 3.06e-07 to 7.69e-06 erg cm^-2 s^-1, with exposure of about 25% of the LR over the time interval ( T0s ; T0 + 10s ); from 3.78e-08 to 7.69e-06 erg cm^-2 s^-1, with exposure of about 25% 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: 26209 SUBJECT: LIGO/Virgo S191109d: Global MASTER-Net observations report DATE: 19/11/09 06:59:44 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-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) started inspect of the LIGO/Virgo S191109d errorbox 863 sec after notice time and 1475 sec after trigger time at 2019-11-09 01:31:52 UT, with upper limit up to 19.8 mag. The observations began at zenith distance = 71 deg. The sun altitude is -74.6 deg. MASTER-Kislovodsk robotic telescope located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the LIGO/Virgo S191109d errorbox 1389 sec after notice time and 2002 sec after trigger time at 2019-11-09 01:40:39 UT, with upper limit up to 19.6 mag. The observations began at zenith distance = 40 deg. The sun altitude is -24.7 deg. The galactic latitude b = 16 deg., longitude l = 326 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/ligo_1.php?id=10893 The observation and reduction will continue. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26210 SUBJECT: LIGO/Virgo S191109d : no neutrino counterpart candidate in ANTARES search DATE: 19/11/09 09:00:38 GMT FROM: Alexis Coleiro at APC/U. Paris Diderot 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 S191109d event using the 90% contour of the Initial bayestar probability map provided by the GW interferometers (GCN#26202). 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/S191109d_Initial.png. Considering the location probability provided by the LIGO/Virgo collaborations, there is a 79.1% 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 2019-11-09 01:07:17 and in the 90% contour of the S191109d event. The expected number of atmospheric background events in the region visible by ANTARES is 9.75e-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 7.02e-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: 26211 SUBJECT: LIGO/Virgo S191109d: no counterpart candidates in the Swift/BAT observations DATE: 19/11/09 09:09:37 GMT FROM: Amy Lien at GSFC T. Sakamoto (AGU), S. D. Barthelmy (NASA/GSFC), A. Y. Lien (GSFC/UMBC), D. M. Palmer (LANL) 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 S191109d (LIGO/VIRGO Collaboration GCN Circ. 26202), where T0 is the LVC trigger time (2019-11-09T01:07:17.220 UTC). The center of the BAT field of view (FOV) at T0 is RA = 183.545 deg, DEC = 14.085 deg, and the roll angle is 132.514 deg. The BAT FOV (>10% partial coding) covers 17.59% of the integrated LVC localization probability. 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 ~ 1.26 x 10^-7 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 ~ 63.91 Mpc. No event data are available at this time. BAT retains decreased, but significant, sensitivity to rate increases for gamma-ray events outside of its FOV. About 82.41% 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/S191109d/web/source_public.html //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26212 SUBJECT: LIGO/Virgo S191109d: AstroSat CZTI upper limits DATE: 19/11/10 06:03:38 GMT FROM: Varun Bhalerao at Indian Inst of Tech V. Shenoy (IITB), A. Anumarlapudi (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 sec window around the trigger time of the BBH merger event S191109d (UTC 2019-11-09 01:07:17.000, 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 = 6:36:08.2,-42:50:44.7 (99.0342,-42.8458), which is 81 deg away from the maximum probability location. At the time of merger event, the Earth-satellite-transient angle corresponding to maximum probability location is ~ 73.52 deg and hence is not 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 0.66 (66%). 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= 1.78e-05 ergs/cm^2/s; fluence limit = 1.78e-06 ergs/cm^2 1.0 s: flux limit= 5.98e-06 ergs/cm^2/s; fluence limit = 5.98e-06 ergs/cm^2 10.0 s: flux limit= 7.45e-07 ergs/cm^2/s; fluence limit = 7.45e-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: 26216 SUBJECT: LIGO/Virgo S191109d: No counterpart candidates in Fermi-LAT observations DATE: 19/11/10 17:21:09 GMT FROM: Sara Cutini at INFN S. Cutini (INFN Perugia), 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 09, 2019, for possible high-energy (E > 100 MeV) gamma-ray emission in spatial/temporal coincidence with the LIGO/Virgo trigger S191109d (GCN 26202). 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 ~50% of the LIGO probability region at the time of the trigger (T0 = 2019-11-09 01:07:17.221 UTC) and reached 100% cumulative coverage at approximately T0 + 5.3 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. No significant sources were found. 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 1.8e-10 and 1.7e-7 [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: 26219 SUBJECT: LIGO/Virgo S191109d: No significant candidates in FRAM-TAROT-GRANDMA observations DATE: 19/11/10 22:12:12 GMT FROM: Nelson Christensen at Obs.de la Cote dAzur,Nice N. Christensen (Artemis), M. Coughlin (Caltech), W. Lin (THU), C. Stachie (Artemis), S. Karpov, M. Masek, M. Prouza (FZU), M. Boer (Artemis), L. Eymar (Artemis), A. Klotz (IRAP), K. Noysena (Artemis, IRAP), S. Antier (APC), A. Coleiro (APC), D. Corre (LAL), D. A. Kann (HETH/IAA-CSIC), D.Coward (OzGrav-UWA), J.G. Ducoin (LAL), B. Gendre (OzGrav-UWA), N.Kochiashvili (Iliauni), 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 S191109d 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 11/09/19 01:32:55 UTC for FRAM-CTA-N which corresponds approximately to 26 minutes after the GW trigger time. The observation started on 11/09/19 06:45:28 UTC for FRAM-Auger which corresponds approximately to 339 minutes after the GW trigger time. The observation started on 11/09/19 21:21:00 UTC for TRE which corresponds approximately to 1214 minutes after the GW trigger time. The observation started on 11/09/19 02:09:58 UTC for TCA which corresponds approximately to 63 minutes after the GW trigger time. The observation started on 11/10/19 06:34:37 UTC for TCH which corresponds approximately to 1768 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 | 2019-11-09 | 2019-11-09 | 192.906 | -44.27 | 0.1 | | | 06:45:28 | 06:49:55 | | | | |FRAM-A | 2019-11-09 | 2019-11-09 | 193.103 | -45.243 | 0.1 | | | 06:50:30 | 06:54:57 | | | | |FRAM-A | 2019-11-09 | 2019-11-09 | 188.83 | -44.27 | 0.1 | | | 06:55:33 | 07:00:00 | | | | |FRAM-A | 2019-11-09 | 2019-11-09 | 200 | -45.243 | 0.1 | | | 07:07:59 | 07:12:26 | | | | |FRAM-A | 2019-11-09 | 2019-11-09 | 198.621 | -45.243 | 0.1 | | | 07:13:01 | 07:17:28 | | | | |FRAM-A | 2019-11-09 | 2019-11-09 | 194.483 | -45.243 | 0.1 | | | 07:18:04 | 07:22:31 | | | | |FRAM-A | 2019-11-09 | 2019-11-09 | 196.981 | -44.27 | 0.1 | | | 07:23:07 | 07:27:34 | | | | |FRAM-A | 2019-11-09 | 2019-11-09 | 197.241 | -45.243 | 0.1 | | | 07:28:09 | 07:32:36 | | | | |FRAM-A | 2019-11-09 | 2019-11-09 | 198.34 | -44.27 | 0.1 | | | 07:33:11 | 07:37:38 | | | | |FRAM-A | 2019-11-09 | 2019-11-09 | 195.623 | -44.27 | 0.2 | | | 07:38:13 | 07:42:40 | | | | |FRAM-A | 2019-11-09 | 2019-11-09 | 195.862 | -45.243 | 0.1 | | | 07:43:14 | 07:47:41 | | | | |FRAM-A | 2019-11-09 | 2019-11-09 | 205.517 | -45.243 | 0.2 | | | 07:48:20 | 07:52:47 | | | | |FRAM-A | 2019-11-09 | 2019-11-09 | 202.415 | -44.27 | 0.1 | | | 07:53:21 | 07:57:48 | | | | |FRAM-A | 2019-11-09 | 2019-11-09 | 203.774 | -44.27 | 0.2 | | | 07:58:24 | 08:02:51 | | | | |FRAM-A | 2019-11-09 | 2019-11-09 | 202.759 | -45.243 | 0.2 | | | 08:03:26 | 08:07:53 | | | | |FRAM-A | 2019-11-09 | 2019-11-09 | 201.379 | -45.243 | 0.2 | | | 08:08:27 | 08:12:54 | | | | |FRAM-A | 2019-11-09 | 2019-11-09 | 204.138 | -45.243 | 0.2 | | | 08:13:30 | 08:17:57 | | | | |FRAM-A | 2019-11-09 | 2019-11-09 | 201.057 | -44.27 | 0.1 | | | 08:18:32 | 08:22:59 | | | | |FRAM-A | 2019-11-09 | 2019-11-09 | 205.132 | -44.27 | 0.1 | | | 08:23:34 | 08:28:01 | | | | |FRAM-A | 2019-11-09 | 2019-11-09 | 199.698 | -44.27 | 0.1 | | | 08:28:37 | 08:33:04 | | | | |-------+------------+------------+---------+---------+---------| |FRAM-C | 2019-11-09 | 2019-11-09 | 132.926 | 4.045 | 0.03 | | | 01:32:55 | 02:36:07 | | | | |FRAM-C | 2019-11-09 | 2019-11-09 | 137.472 | -5.243 | 0.03 | | | 01:37:17 | 04:08:52 | | | | |FRAM-C | 2019-11-09 | 2019-11-09 | 135.714 | -2.833 | 0.03 | | | 01:56:58 | 02:01:04 | | | | |FRAM-C | 2019-11-09 | 2019-11-09 | 134.788 | -0.649 | 0.03 | | | 02:01:20 | 02:05:26 | | | | |FRAM-C | 2019-11-09 | 2019-11-09 | 135.874 | -2.409 | 0.03 | | | 02:05:53 | 02:09:59 | | | | |FRAM-C | 2019-11-09 | 2019-11-09 | 135.324 | -1.086 | 0.03 | | | 02:10:14 | 02:14:20 | | | | |FRAM-C | 2019-11-09 | 2019-11-09 | 135.662 | -1.96 | 0.03 | | | 02:14:34 | 02:18:40 | | | | |FRAM-C | 2019-11-09 | 2019-11-09 | 135.549 | -1.523 | 0.02 | | | 02:18:54 | 02:23:00 | | | | |FRAM-C | 2019-11-09 | 2019-11-09 | 135.324 | -0.212 | 0.03 | | | 02:23:15 | 02:27:21 | | | | |FRAM-C | 2019-11-09 | 2019-11-09 | 134.788 | 0.874 | 0.03 | | | 02:27:36 | 02:31:42 | | | | |FRAM-C | 2019-11-09 | 2019-11-09 | 133.202 | 3.383 | 0.03 | | | 02:36:33 | 02:40:39 | | | | |FRAM-C | 2019-11-09 | 2019-11-09 | 133.202 | 2.846 | 0.03 | | | 02:40:54 | 02:45:00 | | | | |FRAM-C | 2019-11-09 | 2019-11-09 | 133.914 | 0.986 | 0.03 | | | 02:45:21 | 02:49:27 | | | | |FRAM-C | 2019-11-09 | 2019-11-09 | 133.914 | 1.973 | 0.03 | | | 02:49:43 | 02:53:49 | | | | |FRAM-C | 2019-11-09 | 2019-11-09 | 135.549 | -0.649 | 0.03 | | | 02:54:05 | 02:58:11 | | | | |FRAM-C | 2019-11-09 | 2019-11-09 | 134.451 | 0.225 | 0.03 | | | 02:58:27 | 03:02:33 | | | | |FRAM-C | 2019-11-09 | 2019-11-09 | 137.976 | -6.878 | 0.03 | | | 03:51:16 | 03:55:22 | | | | |FRAM-C | 2019-11-09 | 2019-11-09 | 137.415 | -5.891 | 0.03 | | | 03:55:38 | 03:59:44 | | | | |FRAM-C | 2019-11-09 | 2019-11-09 | 136.429 | -3.707 | 0.03 | | | 04:00:19 | 04:04:25 | | | | |FRAM-C | 2019-11-09 | 2019-11-09 | 136.264 | -3.27 | 0.03 | | | 04:09:18 | 04:13:23 | | | | |-------+------------+------------+---------+---------+---------| | TRE | 2019-11-09 | 2019-11-09 | 135 | 0 | 1.4 | | | 21:21:00 | 21:27:23 | | | | | TRE | 2019-11-09 | 2019-11-10 | 129.767 | 12.273 | 1.1 | | | 21:40:11 | 00:16:41 | | | | | TRE | 2019-11-09 | 2019-11-09 | 142.326 | -12.273 | 1.1 | | | 21:53:22 | 21:59:39 | | | | | TRE | 2019-11-09 | 2019-11-09 | 148.5 | -24.545 | 1.1 | | | 22:05:48 | 22:12:05 | | | | | TRE | 2019-11-09 | 2019-11-09 | 132.414 | 8.182 | 1.1 | | | 22:18:57 | 22:25:21 | | | | | TRE | 2019-11-09 | 2019-11-09 | 155.676 | -32.727 | 1 | | | 22:31:13 | 22:37:31 | | | | | TRE | 2019-11-09 | 2019-11-09 | 140.69 | -8.182 | 1 | | | 22:44:28 | 22:50:51 | | | | | TRE | 2019-11-09 | 2019-11-09 | 141.429 | -16.364 | 1 | | | 22:57:03 | 23:03:20 | | | | | TRE | 2019-11-09 | 2019-11-09 | 135 | 4.091 | 0.9 | | | 23:10:02 | 23:16:19 | | | | | TRE | 2019-11-09 | 2019-11-09 | 185.806 | -45 | 1.6 | | | 23:44:52 | 23:51:15 | | | | |-------+------------+------------+---------+---------+---------| | TCA | 2019-11-09 | 2019-11-10 | 126.664 | 14.867 | 0.2 | | | 02:09:58 | 02:46:56 | | | | | TCA | 2019-11-09 | 2019-11-10 | 129.459 | 15.298 | 0.2 | | | 02:16:42 | 05:23:09 | | | | | TCA | 2019-11-09 | 2019-11-10 | 126.758 | 13.012 | 0.1 | | | 03:40:47 | 01:47:23 | | | | | TCA | 2019-11-09 | 2019-11-10 | 128.009 | 16.723 | 0.2 | | | 04:33:53 | 05:10:44 | | | | | TCA | 2019-11-09 | 2019-11-10 | 126.084 | 16.723 | 0.2 | | | 22:38:39 | 03:45:32 | | | | | TCA | 2019-11-09 | 2019-11-10 | 126.167 | 20.434 | 0.2 | | | 22:58:04 | 04:04:42 | | | | | TCA | 2019-11-10 | 2019-11-10 | 137.565 | -0.928 | 0.2 | | | 01:02:28 | 03:38:47 | | | | | TCA | 2019-11-10 | 2019-11-10 | 132.027 | 0.022 | 0.2 | | | 01:21:38 | 03:57:57 | | | | | TCA | 2019-11-10 | 2019-11-10 | 144.385 | -15.298 | 0.2 | | | 02:20:50 | 04:57:14 | | | | | TCA | 2019-11-10 | 2019-11-10 | 126.756 | 18.579 | 0.2 | | | 03:06:18 | 03:12:38 | | | | | TCA | 2019-11-10 | 2019-11-10 | 128.991 | 7.445 | 0.2 | | | 03:25:40 | 03:31:59 | | | | | TCA | 2019-11-10 | 2019-11-10 | 145.227 | -24.102 | 0.1 | | | 04:05:08 | 04:07:08 | | | | |-------+------------+------------+---------+---------+---------| | TCH | 2019-11-10 | 2019-11-10 | 144.95 | -17.273 | 0.3 | | | 06:34:37 | 06:40:55 | | | | | TCH | 2019-11-10 | 2019-11-10 | 196.161 | -43.595 | 0.4 | | | 08:12:47 | 08:19:06 | | | | | TCH | 2019-11-10 | 2019-11-10 | 184.931 | -42.252 | 0.3 | | | 08:38:39 | 08:44:58 | | | | +-------+------------+------------+---------+---------+---------+ 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 17% of the cumulative probability of the Bayestar skymap available on Nov 9, 2019 01:15:21 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/utGS2Zigv2qGp8S 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: 26236 SUBJECT: LIGO/Virgo S191109d: Not observable by CALET DATE: 19/11/12 06:39:08 GMT FROM: Yuta Kawakubo at Louisiana State U./CALET Y. Asaoka (Waseda U), A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU), Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN), 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 S191109d, T0 = 2019-11-09 01:07:17.221 UT (The LIGO Scientific Collaboration and Virgo Collaboration, GCN Circ. 26202), the CALET Gamma-ray Burst Monitor (CGBM) high voltages were off (from T0-29 min to T0+3 min). The CALET Calorimeter (CAL) was operating in the high energy trigger mode at the trigger time of S191109d. 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 at T0+-60 sec. The CAL FOV was centered at RA=349.9 deg, Dec=-16.6 deg at T0.