//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25693 SUBJECT: LIGO/Virgo S190910d: Upper limits from IceCube neutrino searches DATE: 19/09/10 01:52:35 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 S190910d in a time range of 1000 seconds [3] centered on the alert event time (2019-09-10 01:17:59.243 UTC to 2019-09-10 01:34:39.243 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 S190910d calculated from the map circulated in the 1-Preliminary 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 S190910d ranges from 0.029 to 1.107 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 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25694 SUBJECT: LIGO/Virgo S190910d Global MASTER-Net observations report DATE: 19/09/10 01:57:31 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-SAAO robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South Africa (South African Astronomical Observatory) started inspect of the LIGO/Virgo S190910d errorbox 157 sec after trigger time at 2019-09-10 01:28:56 UT, with upper limit up to 19.0 mag. The observations began at zenit distance = 43 deg. The sun altitude is -41.6 deg. The galactic latitude b = -60 deg., longitude l = 98 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/ligo_1.php?id=10782 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 248 | 2019-09-10 01:28:56 | MASTER-SAAO | (04h 49m 50.020s , -67d 59m 39.61s) | C | 180 | 17.8 | 482 | 2019-09-10 01:32:50 | MASTER-SAAO | (02h 57m 56.175s , -08d 53m 48.13s) | C | 180 | 18.0 | 512 | 2019-09-10 01:34:05 | MASTER-SAAO | (04h 59m 49.012s , -45d 34m 00.88s) | C | 90 | 19.0 | 668 | 2019-09-10 01:36:27 | MASTER-SAAO | (04h 48m 33.843s , -45d 27m 12.28s) | C | 120 | 18.1 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25695 SUBJECT: LIGO/Virgo S190910d: Identification of a GW compact binary merger candidate DATE: 19/09/10 02:29:05 GMT FROM: Francesca Badaracco at GSSI, Ligo/VIRGO The LIGO Scientific Collaboration and the Virgo Collaboration report: We identified the compact binary merger candidate S190910d during real-time processing of data from LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) at 2019-09-10 01:26:19.243 UTC (GPS time: 1252113997.243). The candidate was found by the SPIIR [1] and MBTAOnline [2] analysis pipelines. S190910d is an event of interest because its false alarm rate, as estimated by the online analysis, is 3.7e-09 Hz, or about one in 8 years. The event's properties can be found at this URL: https://gracedb.ligo.org/superevents/S190910d The classification of the GW signal, in order of descending probability, is NSBH (98%), Terrestrial (2%), BNS (<1%), BBH (<1%), or MassGap (<1%). Assuming the candidate is astrophysical in origin, there is strong evidence for the lighter compact object having a mass < 3 solar masses (HasNS: >99%). Using the masses and spins inferred from the signal, there is strong evidence against matter outside the final compact object (HasRemnant: <1%). One sky map is available at this time and can be retrieved from the GraceDB event page: * bayestar.fits.gz, an updated localization generated by BAYESTAR [3], distributed via GCN notice about 6 minutes after the candidate For the bayestar.fits.gz sky map, the 90% credible region is 3829 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 606 +/- 197 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] Adams et al. CQG 33, 175012 (2016) [3] Singer & Price PRD 93, 024013 (2016) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25696 SUBJECT: LIGO/Virgo S190910d: No counterpart candidates in HAWC observations DATE: 19/09/10 02:30:24 GMT FROM: Antonio Galvan at Inst.de Astronomia,UNAM The HAWC Collaboration (https://www.hawc-observatory.org) reports: The HAWC Collaboration performed a follow-up of the gravitational wave trigger S190910d. At the time of the trigger the HAWC local zenith was oriented towards (RA, Dec) = (272.9deg, 19.0deg). 32% 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 0.0deg to 45.0deg for the area searched in this analysis. The 5sigma detection sensitivity to a 1s (100s) burst in the 80-800GeV energy range goes from 1.2e-06 erg/cm^2 to 1.1e-04 erg/cm^2 (6.4e-06 erg/cm^2 to 5.0e-04 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: 25698 SUBJECT: LIGO/Virgo S190910d: No counterpart candidates in INTEGRAL SPI-ACS prompt observation DATE: 19/09/10 06:14:09 GMT FROM: Volodymyr Savchenko at ISDC,U of Geneve A. Coleiro (APC, France), S. Schanne (CEA, France) V. Savchenko, C. Ferrigno (ISDC/UniGE, Switzerland) J. Rodi (IAPS-Roma, Italy) 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 S190910d (GCN 25695). At the time of the event (2019-09-10 01:26:19 UTC, hereafter T0), INTEGRAL was operating in nominal mode. The peak of the event localization probability was at an angle of 66 deg with respect to the spacecraft pointing axis. This orientation implies strongly suppressed (18% of optimal) response of ISGRI, somewhat suppressed (42% of optimal) response of IBIS/Veto, and near-optimal (91% of optimal) response of SPI-ACS. The background within ±300 seconds around the event was very stable (excess variance 1.2). 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 2.2e-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 ~1.8e-07 (5.4e-08) erg/cm^2/s at 1 s (8 s) time scale in 75-2000 keV energy range. For the mean reported distance 606.0 Mpc this corresponds to the limit on the total isotropic equivalent energy in 1 s of 9.5e+48 erg for the short GRB spectrum and for a long GRB spectrum isotropic equivalent luminosity in 1 s (8 s) of 7.1e+48 erg/s (2.4e+48 erg/s) We report for completeness and in order of FAP, all excesses identified in the search region. We find: 5 likely background excesses: scale | T | S/N | luminosity ( x 1e+49 erg/s) | FAP 0.05 | 270 | 12 | 30.7 +/- 3.24 +/- 23.6 | 0.355 0.35 | -30.3 | 3.4 | 2.96 +/- 1.14 +/- 2.28 | 0.72 0.6 | 136 | 3.9 | 25.7 +/- 8.66 +/- 19.8 | 0.819 1.7 | 234 | 3.6 | 13.6 +/- 5.13 +/- 10.5 | 0.87 1.25 | -269 | 3.8 | 17.7 +/- 5.99 +/- 13.6 | 0.934 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. We additionally note that the excess at T0+270s despite high S/N of 12 has FAP of only 0.355, due to the large offset from T0 and high rate of excesses at this timescale. 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: 25699 SUBJECT: LIGO/Virgo S190910d: Upper limits from Fermi-GBM Observations DATE: 19/09/10 06:18:11 GMT FROM: Cori Fletcher at USRA C. Fletcher (USRA) reports on behalf of the Fermi-GBM Team and the GBM-LIGO/Virgo group For S190910d and using the initial bayestar skymap, Fermi-GBM was observing 91.6% of the localization probability at event time. There was no Fermi-GBM onboard trigger around the event time of the LIGO/Virgo detection of GW trigger S190910d (GCN 25695). 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=194.6, Dec=-9.9 with a radius of 67.2 degrees. We therefore set upper limits on impulsive gamma-ray emission for the LVC localization region visible to Fermi 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: 3.3 6.5 12 1.024 s: 1.0 1.8 4.6 8.192 s: 0.4 0.67 1.3 Assuming the median luminosity distance of 606 Mpc from the GW detection, we estimate the following intrinsic luminosity upper limits over the 1 keV-10 MeV energy range (in units of 10^48 erg/s): Timescale Soft Normal Hard ------------------------------------ 0.128 s: 22 40 122 1.024 s: 6.7 11 47 8.192 s: 2.7 4.1 13 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25700 SUBJECT: LIGO/Virgo S190910d : no neutrino counterpart candidate in ANTARES search DATE: 19/09/10 06:25:25 GMT FROM: Damien Dornic at CPPM,France 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 S190910d event using the 90% contour of the bayestar probability map provided by the GW interferometers (GCN#25695 ). 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/S190910d_Initial.png . Considering the location probability provided by the LIGO/Virgo collaborations, there is a 50.9% 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 2019-09-10 01:26:19 and in the 90% contour of the S190910d event. The expected number of atmospheric background events in the region visible by ANTARES is 9.24e-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 6.65e-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: 25701 SUBJECT: LIGO/Virgo S190910d: Coverage and upper limits from MAXI/GSC observations DATE: 19/09/10 07:03:55 GMT FROM: Motoko Serino at RIKEN/MAXI N. Kawai, M. Sugizaki (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) report on behalf of the MAXI team: We examined MAXI/GSC all-sky X-ray images (2-20 keV) after the LVC trigger S190910d at 2019-09-10 01:26:19.242 UTC (GCN 25695). At the trigger time of S190910d, the high-voltage of MAXI/GSC was on. The instantaneous field of view of GSC at the GW trigger time covered 2% of the 90% credible region of the bayestar sky map, in which we found no significant new X-ray source. The first one-orbit (92 min) scan observation with GSC after the event covered 100% of the 90% credible region of the bayestar skymap from 01:26:19 to 02:58:18 UTC (T0+0 to T0+5519 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: 25703 SUBJECT: LIGO/Virgo S190910d: No counterpart candidates in AGILE-MCAL observations DATE: 19/09/10 08:01:53 GMT FROM: Claudio Casentini at INAF-IAPS C. Casentini, G. Piano, M. Tavani, M. Cardillo, A. Ursi (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 S190910d at T0 = 2019-09-10 01:26:19 (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 60% of the S190910d 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 S190910d localization region, from a minimum of 1.18E-06 erg cm^-2 to a maximum of 2.89E-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: 25704 SUBJECT: LIGO/Virgo S190910d: no counterpart candidates in the Swift/BAT Observations DATE: 19/09/10 08:11:54 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-SSDC), S. Emery (UCL-MSSL), P. A. Evans (U. Leicester), P. Giommi (ASI), C. Gronwall (PSU), D. Hartmann (Clemson U.), J. A. Kennea (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 S190910d (LIGO/VIRGO Collaboration GCN Circ. 25695), where T0 is the LVC trigger time (2019-09-10T01:26:19.242 UTC). The center of the BAT field of view (FOV) at T0 is RA = 7.546 deg, DEC = -73.147 deg, and the roll angle is 164.159 deg. The BAT FOV (>10% partial coding) covers 44.85% of the integrated LVC localization probability, and 45.56% 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 ~ 8.39 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 ~ 55.49 Mpc. Event data is available from T0-21.827 to T0-18.767. No significant detections are found in the 15-350 keV images created using this event data interval. BAT retains decreased, but significant, sensitivity to rate increases for gamma-ray events outside of its FOV. About 21.26% 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/S190910d/web/source_public.html //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25705 SUBJECT: LIGO/Virgo S190910d: no counterpart candidates in AGILE-GRID observations DATE: 19/09/10 08:23:57 GMT FROM: Giovanni Piano at INAF-IAPS G. Piano, C. Casentini (INAF/IAPS), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, A. Ursi (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 S190910d at T0 = 2019-09-10 01:26:19.243 UTC a preliminary analysis of the AGILE exposure at T0 shows that the Gamma-Ray Imaging Detector (GRID) exposure covered the 11% of the 90% c.l. localization region (LR) (19% 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. No candidate gamma-ray transient was detected. The following preliminary GRID values of 3-sigma upper limit (UL) are obtained: - from 7.5e-07 to 4.0e-06 erg cm^-2 s^-1, with exposure of about 11% of the LR over the time interval (T0 - 2 s; T0 + 2 s); - from 6.1e-07 to 3.2e-06 erg cm^-2 s^-1, with exposure of about 11% of the LR over the time interval (T0; T0 + 5 s); - from 3.1e-07 to 2.3e-06 erg cm^-2 s^-1, with exposure of about 11% of the LR over the time interval (T0; T0 + 10 s); - from 1.1e-07 to 1.6e-06 erg cm^-2 s^-1, with exposure of about 21% of the LR over the time interval (T0; T0 + 100 s). 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: 25706 SUBJECT: LIGO/Virgo S190910d: Candidates from the Zwicky Transient Facility DATE: 19/09/10 09:16:46 GMT FROM: Igor Andreoni at Caltech Shreya Anand (Caltech), Igor Andreoni (Caltech), Maitreya Khandagale (IITB), Kunal Deshmukh (IITB), Varun Bhalerao (IITB), Pradip Gatkine (UMD), Viraj Karambelkar (Caltech), Yashvi Sharma (Caltech), Robert Stein (DESY), Mansi Kasliwal (Caltech), Tomas Ahumada (UMD), Michael Coughlin (Caltech), Jakob Nordin (HU Berlin), Leo P. Singer (NASA GSFC), Eric Bellm (UW) 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 gravitational wave trigger S190910d (LVC et al. GCN 25695) with the Palomar 48-inch telescope equipped with the 47 square degree ZTF camera (Bellm et al. 2019, Graham et al. 2019). The tiling was optimally determined and triggered using the GROWTH Target of Opportunity marshal (Coughlin et al. 2019a, Kasliwal et al. 2019b). We started obtaining target-of-opportunity observations in the g-band and r-band beginning at 2019-09-10 02:58:42.5 UT. We covered 34% of the enclosed probability based on the bayestar map in 2118 sq deg mapped over 90 minutes of observations. Each exposure was 30s with a typical depth of 20.8 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) and Kowalski (Duev et al. 2019) was used to search the alerts database for candidates. After rejecting stellar sources (Tachibana and Miller 2018) and moving objects and applying machine learning algorithms (Mahabal et al. 2019), and after removing candidates with history of variability prior to the merger time, the following high-significance transient candidates were identified by our pipeline in the 90% localization of the bayestar skymap (LVC et al. GCN 25695). +--------------------------------------------------------------------------------+ | ZTF Name | IAU Name | RA (deg) | DEC (deg) | JD | Filter | Mag | +--------------------------------------------------------------------------------+ | ZTF19abyfhov | AT2019pvu | 260.693429 | 11.424436 | 2458736.70 | r | 20.3 | | ZTF19abyfhaq | AT2019pvv | 303.148593 | 49.392607 | 2458736.70 | r | 20.5 | | ZTF19abyfbii | AT2019pvz | 255.441620 | 11.602254 | 2458736.70 | r | 20.2 | | ZTF19abyfazm | AT2019pwa | 290.535876 | 48.069162 | 2458736.70 | r | 18.2 | +--------------------------------------------------------------------------------+ Amongst our candidates, we note that ZTF19abyfazm is a blue transient (g-r~0.4) with the last non-detection one day before the merger. There is a faint object detected in Pan-STARRS images about 2.5 arcsec from the source. Also ZTF19abyfbii is a candidate of interest because of its proximity to a galaxy with SDSS photometric redshift z=0.124, corresponding to a luminosity distance of about 580 Mpc. 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 and follow-up coordination is being undertaken by the GROWTH marshal system (Kasliwal et al. 2019). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25717 SUBJECT: LIGO/Virgo S190910d: No counterpart candidates in Fermi-LAT observations DATE: 19/09/10 15:05:24 GMT FROM: Magnus Axelsson at Stockholm U. M. Axelsson (KTH and Stockholm Univ.), L. Scotton (University and INFN, Torino), D. Kocevski (NASA/MSFC), N. Omodei (Stanford Univ.), E. Bissaldi (Politecnico and INFN Bari), F. Longo (Univ. and INFN Trieste) and M. Arimoto (Kanazawa Univ.) report on behalf of the Fermi-LAT Collaboration: We have searched data collected by the Fermi Large Area Telescope (LAT) on Sep 10, 2019, for possible high-energy (E > 100 MeV) gamma-ray emission in spatial/temporal coincidence with the LIGO/Virgo trigger S190910d (GCN 25695). 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 instantaneous coverage of 50% of the LIGO probability region at the time of the trigger (T0 = 2019-09-10 01:26:19.243 UTC), and reached 100% cumulative coverage after ~9 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. = 57.5, -27.7 (the 90% containment radius is 0.4 deg, statistical uncertainty only), but it is associated with the known and flaring source PKS 0346-27 (0.29 deg from the best-fit position). 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 for the fixed time interval between 100 MeV and 1 GeV for this search vary between 1.9E-10 and 4.7E-09 [erg/cm^2/s]. The Fermi-LAT point of contact for this event is Makoto Arimoto (arimoto@se.kanazawa-u.ac.jp). 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: 25719 SUBJECT: LIGO/Virgo S190910d: AstroSat CZTI upper limits DATE: 19/09/10 16:36:44 GMT FROM: Varun Bhalerao at Indian Inst of Tech A. Anumarlapudi (IUCAA), V. Shenoy (IITB), 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 NSBH merger event S190910d (UTC 2019-09-10 01:26:19.000, 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=0:33:36.4 (8.401), DEC=28:41:36.7 (28.694)), which is 94.84 deg away from the maximum probability location. At the time of merger event, the Earth-satellite-transient angle corresponding to maximum probability location is ~ 61.63 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 0.64 (64%). CZTI data were de-trended to remove orbit-wise background variation. We then searched data from three of 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 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 convert our count rates into flux by assuming that the source spectrum is a power law with alpha = -1.0. We use a detailed mass model of the satellite to calculate the instrument response for every htm grid point that fall in LIGO localization region and calculate flux limit in that direction. We get the following upper limits for source flux in the 20-200 keV band by taking a probability weighted mean of flux limit and are reported here in terms of binning time: 0.1 s: flux limit= 9.84e-06 ergs/cm^2/s ; fluence limit= 9.84e-07 ergs/cm^2 1.0 s: flux limit= 2.97e-06 ergs/cm^2/s ; fluence limit= 2.97e-06 ergs/cm^2 10.0 s: flux limit= 3.88e-07 ergs/cm^2/s ; fluence limit= 3.88e-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: 25720 SUBJECT: LIGO/Virgo S190910d: Liverpool Telescope spectroscopy of ZTF19abyfazm DATE: 19/09/10 21:48:22 GMT FROM: Daniel Perley at Liverpool JMU D. A. Perley and C. M. Copperwheat (LJMU) report on behalf of the GROWTH collaboration: We acquired imaging and spectroscopy of ZTF19abyfazm/AT2019pwa (Anand et al., GCN 25706), an optical transient within the error region of gravitational wave trigger S190910d (LVC et al. GCN 25695), with the 2m Liverpool Telescope. A sequence of 60-second images was acquired in g, r, and i filters using IO:O, followed by 2x500s of spectroscopy with SPRAT, between 20:53 and 21:20 on 2019-09-10 (UT). The source remains bright and blue, although has faded slightly since the time of ZTF discovery (we measure AB magnitudes of g=17.95, r=18.30, i=18.65 at approximately MJD=58736.87). No significant absorption or emission features are visible in the spectrum. We conclude that this source is likely the eruption of an uncatalogued cataclysmic variable within our Galaxy, although further monitoring will be needed to confirm this. We thank the MOPTOP commissioning team for their patience while acquiring these observations. DisclaimerNone //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25721 SUBJECT: LIGO/Virgo S190910d: AT2019pvu, AT2019pvv, AT2019pvz and AT2019pwa 10.4m GTC spectroscopy DATE: 19/09/10 23:31:49 GMT FROM: Alberto J. Castro-Tirado at IAA-CSIC A. J. Castro-Tirado (IAA-CSIC), A. F. Valeev and V. V. Sokolov (SAO-RAS), Y.-D. Hu and E. Fernandez-Garcia (IAA-CSIC), I. Carrasco and A. Castellon (UMA) and J. Font Serra (GRANTECAN, IAC, ULL), on behalf of a larger collaboration, report: Following the detection of ZTF19abyfhov/AT2019pvu, ZTF19abyfhaq/AT2019pvv, ZTF19abyfbii/AT2019pvz and ZTF19abyfazm/AT2019pwa (Anand et al., GCN 25706) within the error area of the GW event S190910d (LVC, GCNC 25695), we obtained imaging and optical spectra covering the range 3700-10000 A with the 10.4m GTC telescope equipped with OSIRIS in La Palma (Spain) starting on Sep 10, 20:25 UT. For AT2019pvu, a magnitude r = 20.33 +/- 0.05 on Sep 10, 20:58 UT is derived. Cross-correlating the transient spectrum (broad lines) with supernova template spectra in SNID (Blondin & Tonry, 2007), we find a good match to the spectra of SNIa at redshift z = 0.133 +/- 0.001. For AT2019pvv, a magnitude r = 21.08 +/- 0.05 on Sep 10, 22:14 UT is derived. The spectrum shows a faint H-alpha line in emission at z = 0 but the low S/N ratio prevents a more precise classification at this stage. For AT2019pvz, a magnitude r = 20.26 +/- 0.05 on Sep 10, 20:27 UT is derived. The spectrum is consistent with that of a SN Ia at the nearby host galaxy redshift z = 0.1286 +/- 0.0005 (based on H-alpha, H-beta, [O III] and others narrow emission lines). For AT2019pwa, a magnitude r = 18.38 +- 0.03 on Sep 10, 21:31 UT is derived. The spectrum displays a blue continuum with the Ca II H&K 3934 A and 3969 A doublet in absorption at z = 0 being the only clear features, which supports the object being a cataclysmic variable in our Galaxy, in agreement with Perley and Copperwheat (GCNC 25720). Therefore we consider ZTF19abyfhov/AT2019pvu, ZTF19abyfhaq/AT2019pvv, ZTF19abyfbii/AT2019pvz and ZTF19abyfazm/AT2019pwa to be unrelated to the GW event S190910d. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25723 SUBJECT: LIGO/Virgo S190910d: Updated Sky Localization DATE: 19/09/11 01:15:04 GMT FROM: Shreya Anand at GROWTH Caltech The LIGO Scientific Collaboration and the Virgo Collaboration report: We have conducted further analysis of the data from LIGO Hanford Observatory (H1), LIGO Livingston Observatory (L1) and Virgo Observatory (V1) around the time of the compact binary merger (CBC) candidate S190910d (GCN Circular 25695). Parameter estimation has been performed using LALInference [1] and a new sky map, LALInference.fits.gz, distributed via GCN Notice, is available for retrieval from the GraceDB event page: https://gracedb.ligo.org/superevents/S190910d The preferred sky map at this time is LALInference.fits.gz. The 90% credible region is 2482 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 632 +/- 186 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) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25725 SUBJECT: LIGO/Virgo S190910d: WHT spectroscopy of ZTF19abyfhov, ZTF19abyfhaq, ZTF19abyfbii DATE: 19/09/11 06:24:35 GMT FROM: Giacomo Cannizzaro at SRON G. Cannizzaro (SRON/Radboud Univ), I. Pastor-Marazuela (API/ASTRON), P. Jonker (SRON/Radboud Univ), K. Maguire (TCD), M. Fraser (UCD), report on behalf of the GW@WHT collaboration: We obtained optical spectroscopy of ZTF19abyfhov/AT2019pvu, ZTF19abyfhaq/AT2019pvv and ZTF19abyfbii/AT2019pvz (GCN 25706), three optical transients within the LIGO/Virgo S190910d sky localisation (GCN 25695) with the ACAM instrument mounted on the William Herschel Telescope located at the Roque de Los Muchachos Observatory, La Palma, Spain. We cross-correlate the transient spectra with a library of supernova template spectra using the code SNID (Blondin and Tonry, 2007). ZTF19abyfhov/AT2019pvu is classified as a SNIa, 3 days before peak, at redshift z=0.132. The spectrum of ZTF19abyfhaq/AT2019pvv has a low SNR, preventing a precise classification. ZTF19abyfbii/AT2019pvz is classified as a SNIa 91T-like, 5 days before peak, at redshift z=0.118. This redshift is consistent with the photometric redshift reported in GCN 25706. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25728 SUBJECT: LIGO/Virgo S190910d: No neutrino candidates at Pierre Auger Observatory DATE: 19/09/11 16:15:41 GMT FROM: Jaime Alvarez-Muniz at Pierre Auger Observatory J. Alvarez-Muniz, F. Pedreira, E. Zas (Univ. Santiago de Compostela, Spain), K. H. Kampert & M. Schimp (Bergische Universitat, Wuppertal, Germany) on behalf of the Pierre Auger Collaboration. In response to: LIGO/Virgo GW trigger S190910d T0=2019-09-10 01:26:19 UTC We searched for Ultra-High-Energy (UHE) neutrinos with energies above ~ 1e17 eV in data collected with the Surface Detector (SD) of the Pierre Auger Observatory in a [-500,500] second interval about the LIGO-Virgo trigger S190910d as well as in a 24 hr time interval following the event. NO events survived the cuts applied to reject the background due to UHE Cosmic Rays i.e. NO neutrino candidates were detected. The field of view (fov) where the SD of Auger is sensitive to UHE neutrinos (corresponding to inclined directions with respect to the vertical relative to the ground) was PARTIALLY COINCIDENT (74.9%) with the LIGO/Virgo 90% localization region (LALInference.fits.gz,0) at the time T0 of the merger alert, achieving TOTAL OVERLAP at approximately T0+1.4 hours ------- The Pierre Auger Observatory is an UHE Cosmic Ray detector located in the Mendoza Province in Argentina. It consists of an array of Water Cherenkov detectors spread over a total surface of 3000 km^2 arranged in a triangular grid of 1.5 km side as well as Fluorescence telescopes and other systems (see 10.1016/j.nima.2015.06.058 for more information). For neutrino searches from GW events with Auger, please refer to: https://journals.aps.org/prd/pdf/10.1103/PhysRevD.94.122007 https://arxiv.org/abs/1906.07422 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25729 SUBJECT: LIGO/Virgo S190910d and S190910h: No counterpart candidates in KAIT observations DATE: 19/09/11 22:57:48 GMT FROM: Weikang Zheng at UC Berkeley James Sunseri, Shaunak Modak, Benjamin E. Stahl, Thomas de Jaeger, Yukei Murakami, WeiKang Zheng, Sergiy Vasylyev, Andrew Hoffman, Nachiket Girish, Keto D. Zhang, and Alexei V. Filippenko (UC Berkeley) report on behalf of the Lick/KAIT GW follow-up team: The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at Lick Observatory, observed the 90% region of the gravitational-wave event S190910h (GCN 25606; GCN 25614) and S190910d detected by LIGO/Virgo. More than one thousand galaxies were selected from the Glade catalog V1.0 (Dalya et al., 2018, MNRAS, 479, 2374; http://aquarius.elte.hu/glade/) according to their priority score. On Sep. 11 UT, KAIT observed 224 of them for event S190910d (started at 1.08 days after trigger), and 154 of them for event S190910h (started at 0.98 days after trigger), according to their priority scores and elevation visibility, with each clear-filter exposure time being 60 s. Our typical limiting mag is 19.0. No viable counterparts were identified and the analysis is ongoing. A full list of galaxies observed by KAIT is given below. GladeID UT(Sep11) RA_J2000 Dec_J2000 For S190910d ----------------------------------------------- G1313601 03:23:13 17:01:09.972 +01:38:37.9248 G1315118 03:24:24 17:02:20.0501 -05:10:43.1436 G0824618 03:28:23 17:41:18.2885 +17:22:04.8144 G0793601 03:29:32 17:43:57.81 +19:35:09.1896 G1048996 03:30:45 17:53:50.7787 +14:02:53.718 G1217685 03:31:56 17:55:20.6544 +23:15:12.3948 G0636803 03:33:05 17:56:20.2442 +26:21:59.58 G0862839 03:34:15 17:56:56.6748 +22:14:02.9544 G1437178 03:35:24 17:59:21.8261 +20:44:31.7184 G0782167 03:36:33 17:59:33.7939 +23:52:52.7628 G0149658 03:37:45 18:02:22.5367 +28:54:05.0868 G0130482 03:38:54 18:04:57.0703 +30:26:47.0724 G1346624 03:40:05 18:06:43.2348 +22:25:07.194 G0929719 03:41:15 18:07:28.0517 +23:06:47.9304 G1317538 03:42:26 18:09:42.1802 +28:15:52.7976 G1400962 03:43:35 18:15:13.4326 +30:51:10.6776 G0484840 03:44:45 18:16:17.3803 +27:31:51.2508 G0634483 03:45:56 18:17:21.4894 +19:42:55.1412 G0066266 03:47:07 18:17:55.2247 +31:51:53.424 G0755437 03:48:18 18:17:56.1036 +33:48:59.4324 G0948596 03:49:29 18:17:59.8462 +28:36:08.3988 G1188319 03:50:36 18:18:49.043 +29:01:33.9276 G0261957 03:51:50 18:19:52.0678 +35:36:30.9888 G1164511 03:53:01 18:20:07.1558 +27:43:10.0128 G0904555 03:54:10 18:20:40.1294 +28:29:59.9028 G1344935 03:55:19 18:20:42.3048 +32:28:03.1044 G1107716 03:56:31 18:21:02.2778 +27:42:55.908 G0898259 03:57:40 18:21:20.7202 +28:31:34.0032 G1027552 03:58:49 18:21:26.7187 +29:26:49.0092 G1324458 03:59:59 18:21:26.9386 +26:39:35.01 G0410221 04:01:08 18:21:30.901 +28:45:01.008 G1399597 04:02:19 18:21:39.9096 +33:27:15.6168 G1177048 04:07:25 18:22:41.6016 +27:30:52.74 G1142911 04:08:34 18:22:44.8536 +30:51:12.4776 G0429648 04:09:45 18:23:00.6593 +25:27:22.0572 G1330516 04:10:55 18:23:08.7305 +29:28:17.0724 G0677536 04:12:10 18:23:21.5698 +34:21:47.7972 G0611374 04:13:23 18:24:06.87 +30:29:31.7292 G1381720 04:14:32 18:24:07.8809 +30:23:10.7304 G1060061 04:15:41 18:24:27.8174 +33:09:47.8224 G0960970 04:16:52 18:24:28.5058 +29:31:18.2028 G0600469 04:18:02 18:24:36.4159 +30:14:08.8872 G1429122 04:19:11 18:24:45.5126 +27:25:06.24 G1409508 04:20:22 18:24:50.537 +30:18:51.93 G1452657 04:21:32 18:25:04.5264 +30:16:10.1208 G0930859 04:22:41 18:25:19.3433 +30:26:16.1808 G0586504 04:23:52 18:25:31.5382 +30:26:46.7916 G0704832 04:25:02 18:25:48.911 +30:44:10.932 G1125000 04:26:13 18:26:06.504 +25:02:09.798 G1293873 04:27:24 18:26:46.062 +32:01:30.9684 G1244792 04:28:34 18:27:07.5732 +27:59:14.4672 G1208813 04:29:43 18:27:12.7589 +29:57:21.5028 G0823717 04:30:52 18:28:11.1254 +29:46:31.0836 G0561966 04:32:02 18:28:12.4366 +33:11:23.6256 G0696616 04:33:11 18:28:54.5508 +29:32:34.6524 G0818963 04:34:18 18:28:56.7701 +29:50:34.656 G0666785 04:35:28 18:28:56.9386 +32:20:04.7184 G0650501 04:36:37 18:29:02.9957 +32:25:57.7776 G1432590 04:37:46 18:30:31.8384 +28:00:48.7944 G1394305 04:38:57 18:30:38.7598 +31:34:56.4312 G0791069 04:40:07 18:31:19.1676 +31:36:52.4412 G0803491 04:41:16 18:31:22.0824 +31:22:44.454 G1417764 04:43:03 17:48:11.3671 +21:43:42.0996 G0713284 04:44:15 17:49:08.7305 +14:21:56.0412 G0543762 04:45:26 17:50:07.1851 +25:25:17.8968 G0087917 04:46:35 17:52:10.0488 +24:24:35.064 G1048996 04:47:47 17:53:50.7787 +14:02:53.718 G1261189 04:48:58 17:54:50.2368 +19:54:16.7112 G1217685 04:50:07 17:55:20.6544 +23:15:12.3948 G1241494 04:51:17 17:55:59.5459 +24:18:18.9612 G0636803 04:52:26 17:56:20.2442 +26:21:59.58 G1028180 04:53:35 17:56:41.4991 +22:37:17.5512 G0944250 04:54:45 17:56:48.8818 +24:13:59.178 G0862839 04:55:54 17:56:56.6748 +22:14:02.9544 G1437178 04:57:03 17:59:21.8261 +20:44:31.7184 G0782167 04:58:12 17:59:33.7939 +23:52:52.7628 G0149658 04:59:24 18:02:22.5367 +28:54:05.0868 G0130482 05:00:33 18:04:57.0703 +30:26:47.0724 G1346624 05:01:44 18:06:43.2348 +22:25:07.194 G0929719 05:02:54 18:07:28.0517 +23:06:47.9304 G1128906 05:04:08 18:08:34.1234 +26:50:48.7896 G1317538 05:05:17 18:09:42.1802 +28:15:52.7976 G1400962 05:06:27 18:15:13.4326 +30:51:10.6776 G0484840 05:07:38 18:16:17.3803 +27:31:51.2508 G0066266 05:08:48 18:17:55.2247 +31:51:53.424 G0776931 05:10:19 18:31:44.9779 +32:05:27.3804 G0797182 05:11:29 18:31:56.814 +31:44:28.4676 G1391705 05:12:38 18:32:05.8301 +31:23:32.4924 G1258716 05:13:47 18:32:52.2509 +31:45:53.5932 G0119107 05:14:57 18:32:59.773 +32:24:15.6456 G0839682 05:16:08 18:33:04.6363 +31:49:22.6776 G1014305 05:17:17 18:33:04.6363 +31:49:38.676 G0971043 05:18:27 18:33:23.723 +27:28:24.1572 G1167368 05:19:38 18:33:45.857 +33:50:39.7248 G0756312 05:20:47 18:33:53.2032 +35:35:43.692 G1196337 05:21:57 18:34:02.5123 +33:51:59.4576 G0655695 05:23:06 18:34:18.7426 +35:00:30.582 G0584460 05:24:15 18:35:03.4205 +32:41:47.1624 G0553596 05:25:27 18:35:06.504 +27:46:15.2364 G0668492 05:26:36 18:35:07.0606 +32:17:26.1852 G1222724 05:27:45 18:35:17.9882 +31:22:35.2452 G0802458 05:28:54 18:35:46.0399 +29:29:00.2544 G1243008 05:30:04 18:35:56.6162 +28:54:53.226 G1187149 05:31:13 18:37:01.2818 +29:32:12.102 G1026457 05:32:22 18:37:06.3574 +32:54:51.12 G1333421 05:33:32 18:37:11.7554 +29:48:28.782 G0850210 05:34:43 18:37:21.5112 +29:55:54.8112 G0621560 05:35:52 18:38:32.6074 +32:57:58.7232 G0813679 05:37:08 18:38:35.4346 +35:52:19.7544 G0619413 05:38:17 18:38:46.831 +32:51:15.7752 G0979195 05:39:26 18:38:58.9159 +32:56:40.7616 G0922107 05:40:36 18:39:10.8545 +30:56:50.8488 G1055527 05:41:48 18:39:19.248 +31:34:36.8688 G0941280 05:42:57 18:39:29.7583 +33:48:50.8356 G0619588 05:44:07 18:39:47.8418 +32:51:43.5564 G1465549 05:47:17 18:40:34.3066 +34:02:20.4612 G1418785 05:48:29 18:40:50.808 +27:59:11.6664 G0653843 05:49:39 18:41:27.942 +32:21:10.7748 G0834734 05:50:54 18:42:28.0078 +35:29:45.9528 G0898839 05:52:03 18:42:46.399 +32:04:34.9464 G1105747 05:53:13 18:43:10.3344 +32:14:43.0404 G1087829 05:54:22 18:43:12.4366 +32:46:13.044 G1217228 05:55:31 18:43:31.5821 +34:30:57.87 G1122311 05:56:41 18:43:51.8554 +31:48:39.9672 G0365393 05:57:50 18:45:07.1923 +35:28:52.7088 G1160311 05:59:00 18:45:30.835 +33:33:10.8036 G1126916 06:00:09 18:45:49.9951 +33:37:47.5104 G0954738 06:01:18 18:45:51.7236 +34:23:22.5132 G0669492 06:02:27 18:45:55.8766 +31:38:21.5412 G1061412 06:03:37 18:46:29.6338 +31:46:13.5948 G0590088 06:04:46 18:47:39.5801 +33:19:11.8488 G1120103 06:05:55 18:47:51.599 +29:58:25.9176 G1361557 06:07:07 18:47:51.775 +35:54:52.0128 G0880875 06:08:16 18:48:00.769 +35:47:16.9044 G0343548 06:09:25 18:48:27.2974 +36:17:48.5844 G0733393 06:10:36 18:48:44.5238 +31:04:28.7472 G1248232 06:11:46 18:48:54.7265 +34:38:38.76 G0895352 06:12:57 18:49:03.7793 +29:19:32.6388 G0211654 06:14:08 18:49:46.787 +35:55:23.214 G0183791 06:15:18 18:49:55.6421 +34:19:45.246 G1101534 06:16:27 18:50:06.9434 +36:07:54.7608 G0416763 06:17:36 18:52:10.1002 +35:31:00.2892 G0462408 06:18:46 18:52:17.7905 +31:27:07.2864 G1416090 06:19:55 18:52:27.81 +35:45:32.6844 G0410846 06:21:04 18:52:48.5743 +37:07:36.2748 G0682884 06:26:48 18:53:03.8964 +27:50:27.5424 G1098771 06:28:00 18:54:14.1797 +33:20:23.604 G0789822 06:29:15 18:54:22.4633 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09:36:38 01:53:25.8696 +71:15:06.7032 G0555854 09:38:29 01:55:36.5268 +47:33:36.5544 G0640951 09:39:54 01:55:57.132 +01:17:06.6444 G0766909 09:41:03 02:00:23.9933 -01:33:10.0656 G0772566 09:43:04 02:02:17.3112 +68:21:46.0836 G0798822 09:45:04 02:02:18.8549 +19:04:01.7004 G0589569 09:46:18 02:04:53.3885 +35:08:56.9148 G0772833 09:47:39 02:05:40.2737 -00:41:41.8452 G0703131 10:06:48 02:07:51.0718 -06:32:14.6364 G0579190 10:08:56 02:09:21.5323 +75:31:35.2524 G0662822 10:11:05 02:09:28.3769 +19:46:35.6016 G0551460 10:12:18 02:09:38.5646 +35:47:49.9452 G0594465 10:14:26 02:09:55.9231 +75:20:14.2368 G0650416 10:16:38 02:14:17.255 +07:35:18.3192 G0500598 10:17:47 02:14:23.5766 +07:51:41.3244 G0761689 10:19:14 02:14:41.9009 +51:14:09.0096 G0690002 10:21:07 02:14:49.3726 +68:23:38.94 G0793052 10:22:57 02:18:53.0594 +52:00:03.5712 G0481478 10:24:46 02:21:30.9065 +70:38:11.886 G0698609 10:26:52 02:22:47.8373 +11:38:18.2868 G0801620 10:28:06 02:24:02.6266 -04:41:35.9016 G0631104 10:29:27 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11:51:02 03:17:31.6068 +37:02:46.5108 G0576329 11:52:19 03:18:50.6928 +08:47:33.8208 G0618362 11:53:43 03:20:16.1976 +47:33:03.7584 G0571206 11:55:51 03:20:36.935 +67:50:43.6812 G0600454 12:19:27 03:20:38.1098 +43:04:44.778 G0616471 12:20:43 03:22:34.3661 +14:54:48.9204 G0710733 12:21:53 03:24:00.2059 +16:10:57.882 G0732746 12:23:09 03:25:11.5723 -06:10:51.006 G0562026 12:24:29 03:27:03.3938 +31:44:52.062 G0819943 12:26:42 03:27:45.0631 +69:44:57.0048 G0713851 12:28:54 03:27:46.0903 +31:15:27.2124 G0557004 12:30:05 03:30:07.3673 +35:55:17.8428 G0658066 12:31:20 03:31:21.2311 +14:23:05.4744 G0779270 12:32:42 03:33:30.8496 +48:28:40.224 G0756702 12:34:04 03:34:37.5595 +12:03:53.1936 G1361052 12:35:21 03:34:49.5794 -09:50:33.2196 G1085027 12:36:43 03:35:04.9274 +33:03:14.526 G0695101 12:38:00 03:37:07.4249 +49:03:08.7444 G0705569 12:39:24 03:37:50.9911 +09:36:30.0528 G1206515 12:40:31 03:38:14.0918 +10:05:03.8832 G0783345 12:42:42 03:38:21.4646 +64:19:22.9044 G0659256 12:44:51 03:38:40.5679 +09:58:11.9388 G0695313 12:47:02 03:38:53.2718 +64:14:58.9272 G0844381 12:49:08 03:38:57.2554 +32:39:11.0736 G0793910 12:50:22 03:39:15.0166 +14:27:37.7352 G0496810 12:51:32 03:39:28.3063 +13:23:41.7444 G0795493 12:52:52 03:39:39.0948 +45:43:47.9856 G0734420 12:54:08 03:40:45.1327 +17:44:28.2084 G0039699 12:55:18 03:41:01.3459 +13:34:19.1136 G0739254 12:56:34 03:41:05.8008 +39:34:57.7416 G0620810 12:57:51 03:41:17.3868 +10:44:32.676 G0746601 12:59:09 03:42:24.0298 +39:14:40.362 G0743139 13:00:25 03:44:42.691 +15:44:11.7312 G0734211 13:01:44 03:47:39.7678 +39:20:48.8724 G1296306 13:07:06 03:50:23.4166 +06:58:23.1672 G0784665 13:09:14 03:51:58.2413 +64:13:51.7764 G0737259 13:11:18 03:52:16.3944 +13:24:19.3608 G0815176 13:12:34 03:52:17.9206 +41:06:54.9396 G0233228 13:13:43 03:53:38.6417 +40:53:20.7168 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25734 SUBJECT: LIGO/Virgo S190910d: No transient candidates in CALET observations. DATE: 19/09/13 03:22:51 GMT FROM: Yuta Kawakubo at Louisiana State U./CALET S. Ricciarini (U of Florence), A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU), Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN), Y. Asaoka, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), N. Cannady (GSFC/UMBC), M. L. Cherry (LSU), P. S. Marrocchesi (U of Siena), and the CALET collaboration: The CALET Gamma-ray Burst Monitor (CGBM) was operating at the trigger time of S190910d T0 = 2019-09-10 01:26:19.243 UT (The LIGO Scientific Collaboration and Virgo Collaboration, GCN Circ. 25695 and 25723). No CGBM on-board trigger occurred around the event time. Based on the LIGO-Virgo localization sky map, the summed LIGO probabilities inside the CGBM HXM (7 - 3000 keV) and SGM (40 keV - 28 MeV) fields of view are 1 % and 64 %, respectively (and 77 % credible region of the updated localization map was above the horizon). The HXM and SGM fields of view were centered at RA = 108.8 deg, Dec = 29.9 deg and RA = 100.8 deg, Dec = 22.9 deg at T0, respectively. The CALET Calorimeter (CAL) was operating in the low energy trigger mode at the trigger time of S190910d. Using the CAL data, we have searched for gamma-ray events in the 1-10 GeV band from -60 sec to +60 sec from the GW trigger time and found no candidates. There is no significant overlap with the LIGO-Virgo high probability localization region. The CAL FOV was centered at RA=100.8 deg, Dec=22.9 deg at T0. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25737 SUBJECT: LIGO/Virgo S190910d: No Counterparts in DDOTI/OAN Optical Observations DATE: 19/09/13 06:02:44 GMT FROM: Emma Margarita Pereyra Talamantes at IA-UNAM Ensenada Margarita Pereyra (UNAM), Alan M. Watson (UNAM), Nat Butler (ASU), Simone Dichiara (GSFC/UMD), Rosa L. Becerra (UNAM), Diego Gonzalez (UNAM), Alexander Kutyrev (GSFC/UMD), William H. Lee (UNAM), Eleonora Troja (GSFC/UMD), Gabriele Minervini (INAF/IAPS-Rome) and Tanner Wolfram (ASU) report: We observed LIGO/Virgo S190910d event (Badaracco F; LVC et al.; GCN #25695) with the DDOTI/OAN wide-field imager at the Observatorio Astronomico Nacional on Sierra San Pedro Martir (http://ddoti.astroscu.unam.mx) from 2019-09-10 04:25 to 2019-09-10 08:15 UTC ( ~ 3.0 to 7.8 hours after the event). We observed approximately 289 square degrees of the sky, with 5 pointings centered on 17:30:00.089 +19:08:01.30, 17:49:53.330 +17:34:38.58, 17:49:53.330 +24:35:33.03, 18:09:04.387 +22:40:56.15 and 18:09:46.574 +30:03:26.65. We obtained about 18, 36, 18, 30 and 18 minutes total exposure on each pointing, respectively. These regions include about 6% of the 2D probability in the current BAYESTAR map and 5% of the 2D probability in the LALInference map. We calibrated our images against the APASS catalog. Our 10-sigma limiting magnitude are typically between w = 18.04 and w = 18.96. Comparing our 10-sigma detections against the USNO-B1 catalog, we detect no uncataloged sources with significant fading. We thank the staff of the Observatorio Astronomico Nacional in San Pedro Martir. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25739 SUBJECT: LIGO/Virgo S190910d: Gaia Photometric Alerts transient candidate DATE: 19/09/13 11:33:37 GMT FROM: Zuzanna Kostrzewa-Rutkowska at SRON Z. Kostrzewa-Rutkowska (Leiden Observatory), S. Hodgkin, A. Delgado, D.L. Harrison, M. van Leeuwen, G. Rixon, A. Yoldas (IoA Cambridge), D. Eappachen, P.G. Jonker (SRON/RU) on behalf of Gaia Alerts team report the discovery of a transient candidate within the probability skymap of S190910d (the LIGO Scientific Collaboration and the Virgo Collaboration, GCN 25695): --------------------------------------------------------------------------- Name TNSid Date [TCB] RaDeg DecDeg AlertMag URL --------------------------------------------------------------------------- Gaia19eba AT2019qam 2019-09-11T07:02:41 52.99630 -26.07598 18.14 http://gsaweb.ast.cam.ac.uk/alerts/alert/Gaia19eba/ Acknowledgements: This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. ZKR acknowledges funding from the Netherlands Research School for Astronomy (NOVA). DE and PGJ acknowledge support from the European Research Council under ERC Consolidator Grant agreement no 647208. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25741 SUBJECT: LIGO/Virgo S190910d: MASTER previous detection of Gaia19eba/AT2019qam DATE: 19/09/13 12:18:57 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, F.Balakin, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa,A.Kuznetsov, V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva, K.Pozdnyakov, A.Chasovnikov, V.Topolev, 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 Global Robotic Net (http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol.2010, 30L) started inspect of LIGO/Virgo S190910d (GCN 25695) 157 sec after trigger time at 2019-09-10 01:28:56 UT (Lipunov et al. GCN 25694) We analyzed Gaia OT candidates from compact binary merger candidate LIGO/Virgo S190910d Gaia19eba/AT2019qam ( Kostrzewa-Rutkowska et al. GCN25739 ) at RA,Dec(2000)=52.99630 -26.07598 at MASTER archieve images. There is OT with unfiltered m_OT~18.5 on 2 images at 2019-09-02 23:00:27, 22:48:02UT, it means no connection with GW S190910d //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25749 SUBJECT: LIGO/Virgo S190910d : No significant candidates in TAROT-GRANDMA observations DATE: 19/09/14 13:51:57 GMT FROM: Kanthanakorn Noysena at U of Toulouse III/GAHEC H. Crisp (OzGrav-UWA), K. Barynova (Kyiv Uni), K. Noysena (Artemis, IRAP), C. Stachie (Artemis), M. Boer (Artemis), N. Christensen (Artemis), L. Eymar (Artemis), A. Klotz (IRAP), S. Antier (APC), S. Basa (LAM), D. Corre (LAL), M. Coughlin (Caltech), D. Coward (OzGrav- UWA), J.G. Ducoin (LAL), B. Gendre (OzGrav-UWA), P. Hello (LAL), C. Lachaud (APC), N. Leroy (LAL), D. Turpin (NAOC), X. Wang (THU) Report on behalf of the TAROT network and GRANDMA collaborations. We performed tiled observations of LIGO/Virgo S190910d event with the TAROT-Chile (TCH), TAROT-Calern (TCA) and TAROT-Reunion (TRE) telescopes operating in the visible located respectively at La Silla ESO observatory (LaS/ESO), the Calern site at the Cote d'Azur observatory and at La Reunion Island, France. The observation started for TCA at 09/10/19 02:26:06 UTC which corresponds approximately to 60 minutes after the GW trigger time, for TCH at 09/10/19 04:54:23 UTC which corresponds approximately to 208 minutes after the GW trigger time, and for TRE at 09/10/19 19:42:20 UTC which corresponds approximately to 1096 minutes after the GW trigger time. We performed the following tiled observations : +-------+------------+------------+---------+---------+---------+ | Tele | TStart | TEnd | RA | DEC | Proba | | scope | [UTC] | [UTC] | [deg] | [deg] | [%] | |-------|------------+------------+---------+---------+---------| | TCA | 2019-09-10 | 2019-09-11 | 288.95 | 42.703 | 0.1 | | | 02:26:06 | 00:23:41 | | | | | TCA | 2019-09-10 | 2019-09-12 | 293.916 | 42.703 | 0.1 | | | 02:38:12 | 03:53:25 | | | | | TCA | 2019-09-10 | 2019-09-10 | 292.014 | 44.558 | 0.2 | | | 03:10:43 | 03:12:43 | | | | | TCA | 2019-09-10 | 2019-09-10 | 288.467 | 40.372 | 0.1 | | | 19:03:55 | 19:10:25 | | | | | TCA | 2019-09-10 | 2019-09-12 | 291.433 | 42.703 | 0.1 | | | 19:10:44 | 00:25:43 | | | | | TCA | 2019-09-10 | 2019-09-12 | 290.883 | 40.847 | 0.1 | | | 19:43:07 | 00:18:54 | | | | | TCA | 2019-09-10 | 2019-09-12 | 296.398 | 42.703 | 0.2 | | | 20:21:59 | 01:17:51 | | | | | TCA | 2019-09-10 | 2019-09-10 | 300.95 | 48.27 | 0.1 | | | 20:28:49 | 23:05:01 | | | | | TCA | 2019-09-10 | 2019-09-10 | 298.223 | 48.27 | 0.1 | | | 20:40:45 | 20:47:15 | | | | | TCA | 2019-09-10 | 2019-09-10 | 281.219 | 39.897 | 0.1 | | | 20:47:35 | 23:23:44 | | | | | TCA | 2019-09-10 | 2019-09-10 | 293.299 | 40.847 | 0.1 | | | 20:54:25 | 23:30:34 | | | | | TCA | 2019-09-10 | 2019-09-11 | 297.421 | 46.414 | 0.1 | | | 22:19:34 | 00:55:47 | | | | | TCA | 2019-09-10 | 2019-09-10 | 279.525 | 29.713 | 0.2 | | | 22:26:24 | 22:32:55 | | | | | TCA | 2019-09-10 | 2019-09-10 | 270.95 | 20.434 | 0.1 | | | 23:30:54 | 23:37:26 | | | | | TCA | 2019-09-11 | 2019-09-12 | 298.881 | 42.703 | 0.2 | | | 00:59:25 | 03:01:04 | | | | | TCA | 2019-09-11 | 2019-09-12 | 288.467 | 39.897 | 0.2 | | | 01:31:13 | 01:24:36 | | | | | TCA | 2019-09-11 | 2019-09-11 | 306.329 | 42.703 | 0.2 | | | 01:38:03 | 19:01:53 | | | | | TCA | 2019-09-11 | 2019-09-12 | 299.673 | 44.558 | 0.2 | | | 01:44:53 | 03:46:39 | | | | | TCA | 2019-09-11 | 2019-09-11 | 302.715 | 46.414 | 0.1 | | | 02:23:09 | 21:56:23 | | | | | TCA | 2019-09-11 | 2019-09-11 | 297.12 | 44.558 | 0.2 | | | 02:30:02 | 22:03:09 | | | | | TCA | 2019-09-11 | 2019-09-12 | 302.227 | 44.558 | 0.2 | | | 03:15:20 | 03:07:52 | | | | | TCA | 2019-09-11 | 2019-09-12 | 303.847 | 42.703 | 0.2 | | | 03:22:11 | 03:14:37 | | | | | TCA | 2019-09-11 | 2019-09-12 | 304.78 | 44.558 | 0.2 | | | 03:29:01 | 01:11:08 | | | | | TCA | 2019-09-11 | 2019-09-11 | 273.093 | 31.569 | 0.1 | | | 19:14:29 | 23:40:37 | | | | | TCA | 2019-09-11 | 2019-09-12 | 286.051 | 39.897 | 0.1 | | | 19:21:15 | 01:56:16 | | | | | TCA | 2019-09-11 | 2019-09-11 | 307.333 | 44.558 | 0.2 | | | 19:27:59 | 21:43:59 | | | | | TCA | 2019-09-11 | 2019-09-12 | 291.433 | 42.703 | 0.1 | | | 19:59:49 | 00:25:43 | | | | | TCA | 2019-09-12 | 2019-09-12 | 55.325 | -9.256 | 0.1 | | | 00:26:15 | 00:32:35 | | | | | TCA | 2019-09-12 | 2019-09-12 | 301.364 | 42.703 | 0.2 | | | 02:41:47 | 02:48:05 | | | | | TCA | 2019-09-13 | 2019-09-13 | 305.362 | 46.414 | 0.1 | | | 21:16:13 | 21:22:32 | | | | | TCA | 2019-09-13 | 2019-09-13 | 278.402 | 35.711 | 0.2 | | | 22:01:36 | 22:07:56 | | | | +-------+------------+------------+---------+---------+---------+ | TCH | 2019-09-10 | 2019-09-10 | 71.936 | -43.595 | 0.5 | | | 04:54:23 | 09:43:01 | | | | | TCH | 2019-09-10 | 2019-09-10 | 68.305 | -38.141 | 0.4 | | | 05:01:28 | 07:19:33 | | | | | TCH | 2019-09-10 | 2019-09-11 | 73.993 | -45.414 | 0.5 | | | 05:14:37 | 08:32:07 | | | | | TCH | 2019-09-10 | 2019-09-10 | 70.627 | -38.141 | 0.3 | | | 05:26:48 | 05:33:18 | | | | | TCH | 2019-09-10 | 2019-09-10 | 77.221 | -52.686 | 0.5 | | | 05:33:37 | 07:46:47 | | | | | TCH | 2019-09-10 | 2019-09-10 | 84.283 | -56.323 | 0.4 | | | 05:47:04 | 05:53:34 | | | | | TCH | 2019-09-10 | 2019-09-10 | 71.326 | -47.232 | 0.5 | | | 05:59:14 | 06:05:44 | | | | | TCH | 2019-09-10 | 2019-09-10 | 83.782 | -54.505 | 0.4 | | | 06:06:03 | 06:12:33 | | | | | TCH | 2019-09-10 | 2019-09-11 | 71.385 | -45.414 | 0.5 | | | 06:12:52 | 06:55:42 | | | | | TCH | 2019-09-10 | 2019-09-11 | 72.473 | -39.959 | 0.3 | | | 06:19:40 | 07:07:00 | | | | | TCH | 2019-09-10 | 2019-09-11 | 76.74 | -47.232 | 0.4 | | | 06:47:14 | 07:53:38 | | | | | TCH | 2019-09-10 | 2019-09-11 | 69.991 | -41.777 | 0.5 | | | 06:59:27 | 08:20:28 | | | | | TCH | 2019-09-10 | 2019-09-11 | 74.075 | -49.05 | 0.5 | | | 07:32:26 | 08:34:25 | | | | | TCH | 2019-09-10 | 2019-09-10 | 76.888 | -49.05 | 0.5 | | | 08:57:02 | 09:03:32 | | | | | TCH | 2019-09-10 | 2019-09-11 | 74.033 | -47.232 | 0.5 | | | 09:03:50 | 07:40:02 | | | | | TCH | 2019-09-10 | 2019-09-11 | 70.089 | -39.959 | 0.4 | | | 09:10:38 | 07:46:50 | | | | | TCH | 2019-09-10 | 2019-09-11 | 80.596 | -54.505 | 0.5 | | | 09:23:14 | 06:36:14 | | | | | TCH | 2019-09-10 | 2019-09-10 | 80.272 | -52.686 | 0.4 | | | 09:48:54 | 09:55:24 | | | | | TCH | 2019-09-11 | 2019-09-11 | 69.401 | -43.595 | 0.5 | | | 07:08:34 | 07:15:04 | | | | | TCH | 2019-09-11 | 2019-09-11 | 71.263 | -49.05 | 0.5 | | | 07:53:56 | 08:00:26 | | | | | TCH | 2019-09-11 | 2019-09-11 | 74.17 | -52.686 | 0.5 | | | 08:07:10 | 08:13:40 | | | | | TCH | 2019-09-11 | 2019-09-14 | 67.705 | -39.959 | 0.4 | | | 08:52:49 | 03:58:36 | | | | | TCH | 2019-09-11 | 2019-09-13 | 77.41 | -54.505 | 0.5 | | | 09:50:26 | 09:30:15 | | | | | TCH | 2019-09-12 | 2019-09-14 | 74.121 | -50.868 | 0.5 | | | 06:35:37 | 06:10:08 | | | | | TCH | 2019-09-12 | 2019-09-13 | 77.048 | -50.868 | 0.5 | | | 06:42:25 | 08:44:52 | | | | | TCH | 2019-09-13 | 2019-09-13 | 80.95 | -56.323 | 0.5 | | | 05:56:17 | 06:02:47 | | | | +-------+------------+------------+---------+---------+---------+ | TRE | 2019-09-10 | 2019-09-12 | 76.154 | -53.182 | 2.3 | | | 19:42:20 | 21:40:33 | | | | | TRE | 2019-09-10 | 2019-09-10 | 68.108 | -32.727 | 1.2 | | | 19:55:17 | 20:01:51 | | | | | TRE | 2019-09-10 | 2019-09-13 | 65.455 | -40.909 | 1.9 | | | 20:26:43 | 00:13:13 | | | | | TRE | 2019-09-10 | 2019-09-12 | 60.779 | -28.636 | 1.4 | | | 20:40:01 | 22:57:13 | | | | | TRE | 2019-09-10 | 2019-09-10 | 63 | -24.545 | 1.1 | | | 20:52:16 | 20:58:44 | | | | | TRE | 2019-09-10 | 2019-09-13 | 84.255 | -57.273 | 1.9 | | | 21:53:12 | 00:26:27 | | | | | TRE | 2019-09-10 | 2019-09-12 | 69.677 | -45 | 2.3 | | | 22:06:21 | 00:29:45 | | | | | TRE | 2019-09-10 | 2019-09-12 | 65.455 | -28.636 | 1.1 | | | 22:31:13 | 21:27:20 | | | | | TRE | 2019-09-10 | 2019-09-10 | 72 | -36.818 | 1.1 | | | 22:44:27 | 22:51:01 | | | | | TRE | 2019-09-10 | 2019-09-10 | 82.105 | -49.091 | 1.1 | | | 23:03:28 | 23:09:56 | | | | | TRE | 2019-09-10 | 2019-09-12 | 100 | -65.455 | 1.2 | | | 23:16:21 | 23:28:34 | | | | | TRE | 2019-09-11 | 2019-09-13 | 61.714 | -36.818 | 1.3 | | | 19:17:10 | 01:10:44 | | | | | TRE | 2019-09-11 | 2019-09-13 | 58.5 | -24.545 | 1.2 | | | 19:29:41 | 01:23:57 | | | | | TRE | 2019-09-12 | 2019-09-12 | 75.79 | -49.091 | 2.3 | | | 00:11:02 | 23:41:55 | | | | | TRE | 2019-09-12 | 2019-09-12 | 66.857 | -36.818 | 1.9 | | | 00:36:30 | 00:43:04 | | | | | TRE | 2019-09-12 | 2019-09-13 | 76.596 | -57.273 | 1.6 | | | 01:20:51 | 00:52:08 | | | | | TRE | 2019-09-12 | 2019-09-12 | 69.474 | -49.091 | 1.7 | | | 20:10:59 | 20:17:33 | | | | | TRE | 2019-09-12 | 2019-09-12 | 70.909 | -40.909 | 2.1 | | | 21:46:19 | 21:52:47 | | | | | TRE | 2019-09-13 | 2019-09-13 | 83.077 | -53.182 | 1.7 | | | 00:32:21 | 00:38:49 | | | | | TRE | 2019-09-13 | 2019-09-13 | 63.243 | -32.727 | 1.6 | | | 19:47:45 | 19:54:13 | | | | | TRE | 2019-09-13 | 2019-09-13 | 85.714 | -61.364 | 1.5 | | | 20:00:58 | 20:07:32 | | | | +-------+------------+------------+---------+---------+---------+ 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 tile is 1.9x1.9 degrees for both TCA and TCH and 4.2x4.2 degrees for TRE. These observations cover about 37% of the cumulative probability of the LALInference skymap available on Sep 10, 2019 22:33:43 UTC. The typical limiting magnitude in AB mode is 18.0 for a 60.0 s exposure for TCH and TCA and 17.0 for a 60.0 s exposure for TRE. The coverage map is available at: https://grandma-owncloud.lal.in2p3.fr/index.php/s/D0YLFF9t7LBekQM No significant transient candidates were found during our low latency analysis. 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 (https://grandma.lal.in2p3.fr/). Details on the TAROT telescopes are available on the GRANDMA web pages.