//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25870 SUBJECT: LIGO/Virgo S190930s: Global MASTER-Net observations report DATE: 19/09/30 13:53:27 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva, D.Kuvshinov (Lomonosov Moscow State University, SAI, Physics Department), R. Podesta, C.Lopez, F. Podesta, C.Francile (Observatorio Astronomico Felix Aguilar OAFA), H.Levato (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE), R. Rebolo, M. Serra (The Instituto de Astrofisica de Canarias), D. Buckley (South African Astronomical Observatory), O.A. Gres, N.M. Budnev, O.Ershova (Irkutsk State University, API), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), V. Yurkov, A. Gabovich, Yu. Sergienko (Blagoveschensk Educational State University) MASTER-Amur robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the LIGO/Virgo S190930s errorbox 54 sec after trigger time at 2019-09-30 13:36:35 UT, with upper limit up to 17.4 mag. The observations began at zenit distance = 50 deg. The sun altitude is -37.8 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=10851 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 145 | 2019-09-30 13:36:35 | MASTER-Amur | (02h 37m 02.088s , +27d 44m 29.67s) | C | 180 | 17.4 | 541 | 2019-09-30 13:44:12 | MASTER-Amur | (21h 02m 58.574s , +08d 26m 09.77s) | C | 60 | 17.4 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25871 SUBJECT: LIGO/Virgo S190930s: Identification of a GW compact binary merger candidate DATE: 19/09/30 14:07:14 GMT FROM: Olivier Minazzoli at LIGO Virgo Collaboration The LIGO Scientific Collaboration and the Virgo Collaboration report: We identified the compact binary merger candidate S190930s during real-time processing of data from LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) at 2019-09-30 13:35:41.247 UTC (GPS time: 1253885759.247). The candidate was found by the GstLAL [1], MBTAOnline [2], PyCBC Live [3], and SPIIR [4] analysis pipelines. S190930s is an event of interest because its false alarm rate, as estimated by the online analysis, is 3e-09 Hz, or about one in 10 years. The event's properties can be found at this URL: https://gracedb.ligo.org/superevents/S190930s The classification of the GW signal, in order of descending probability, is MassGap (95%), Terrestrial (5%), BNS (<1%), BBH (<1%), or NSBH (<1%). Assuming the candidate is astrophysical in origin, there is strong evidence against the lighter compact object having a mass < 3 solar masses (HasNS: <1%). Using the masses and spins inferred from the signal, there is strong evidence against matter outside the final compact object (HasRemnant: <1%). One sky map is available at this time and can be retrieved from the GraceDB event page: * bayestar.fits.gz,0, an updated localization generated by BAYESTAR [5], distributed via GCN notice about 6 minutes after the candidate trigger time. For the bayestar.fits.gz,0 sky map, the 90% credible region is 1998 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 752 +/- 224 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 < https://emfollow.docs.ligo.org/userguide/>. [1] Messick et al. PRD 95, 042001 (2017) [2] Adams et al. CQG 33, 175012 (2016) [3] Nitz et al. PRD 98, 024050 (2018) [4] Qi Chu, PhD Thesis, The University of Western Australia (2017) [5] Singer & Price PRD 93, 024013 (2016) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25872 SUBJECT: LIGO/Virgo S190930s: No counterpart candidates in INTEGRAL SPI-ACS prompt observation DATE: 19/09/30 14:30:11 GMT FROM: Maeve Doyle at U College Dublin, Ireland Maeve Doyle (UCD, Ireland), Diego Gotz (CEA, Saclay) 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 S190930s (GCN 25871). At the time of the event (2019-09-30 13:35:41 UTC, hereafter T0), INTEGRAL was operating in nominal mode. The peak of the event localization probability was at an angle of 60 deg with respect to the spacecraft pointing axis. This orientation implies strongly suppressed (27% of optimal) response of ISGRI, somewhat suppressed (40% of optimal) response of IBIS/Veto, and near-optimal (70% of optimal) r esponse 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 1.8e-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 ~1.6e-07 (5.5e-08) erg/cm^2/s at 1 s (8 s) time scale in 75-2000 keV energy range. For the mean reported distance 752.0 Mpc this corresponds to the limit on the total isotropic equivalen t energy in 1 s of 1.3e+49 erg for the short GRB spectrum and for a long GRB spectrum isotropic equivalent luminosity in 1 s (8 s) of 9.6e+48 erg/s (3.7e+48 erg/s) We report for completeness and in order of FAP, all excesses identified in the search region. We find 4 likely background excesses: scale | T | S/N | luminosity ( x 1e+49 erg/s) | FAP 4 | 175 | 3.6 | 9.8 +/- 2.96 +/- 4.96 | 0.238 0.55 | 121 | 4.2 | 29 +/- 8.03 +/- 14.7 | 0.559 0.35 | 43.7 | 3.6 | 3.13 +/- 1.01 +/- 1.58 | 0.751 0.65 | 52 | 3.4 | 21.4 +/- 7.37 +/- 10.8 | 0.786 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: 25873 SUBJECT: LIGO/Virgo S190930s: Upper limits from IceCube neutrino searches DATE: 19/09/30 14:37:28 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 S190930s in a time range of 1000 seconds [3] centered on the alert event time (2019-09-30 13:27:21.247 UTC to 2019-09-30 13:44:01.247 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 S190930s 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 S190930s ranges from 0.029 to 0.173 GeV cm^-2 in a 1000 second time window. The IceCube Neutrino Observatory is a cubic-kilometer neutrino detector operating at the geographic South Pole, Antarctica. The IceCube realtime alert point of contact can be reached at roc@icecube.wisc.edu [1] Bartos et al. arXiv:1810.11467 (2018) and Countryman et al.arXiv:1901.05486 (2019) [2] Braun et al., Astroparticle Physics 29, 299 (2008) [3] Baret et al., Astroparticle Physics 35, 1 (2011) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25877 SUBJECT: LIGO/Virgo S190930s: Coverage and upper limits from MAXI/GSC observations DATE: 19/09/30 15:32:49 GMT FROM: Satoshi Sugita at Aoyama Gakuin U. S. Sugita, M. Serino (AGU), N. Kawai (Tokyo Tech), H. Negoro (Nihon U.), 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 S190930s at 2019-09-30 13:35:41.246 UTC (GCN 25871). At the trigger time of S190930s, the high-voltage of MAXI/GSC was on, but the FOV was out of the 90% credible region of the bayestar skymap. 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 14:25:05 to 15:03:54 UTC (T0+2964 to T0+5293 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: 25878 SUBJECT: LIGO/Virgo S190930s: No counterpart candidates in AGILE-MCAL observations DATE: 19/09/30 15:36:47 GMT FROM: Martina Cardillo at INAF-IAPS M. Cardillo (INAF/IAPS), F. Longo (Univ. Trieste, and INFN Trieste), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), C. Casentini, G. Piano, 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),  report on behalf of the AGILE Team: In response to the LIGO/Virgo GW event S190930s at T0 = 2019-09-30 13:35:41 (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, the 100% of the S190930s 90 c.l. localization region (LR) 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 S190930s LR, from a minimum of 1.41E-06 erg cm^-2 to a maximum of 6.51E-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: 25881 SUBJECT: LIGO/Virgo S190930s : no neutrino counterpart candidate in ANTARES search DATE: 19/09/30 16:05:37 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 S190930s event using the 90% contour of the Initial bayestar probability map provided by the GW interferometers (GCN#25871). 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/S190930s_Initial.png . Considering the location probability provided by the LIGO/Virgo collaborations, there is a 25.9% 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 2019-09-30 13:35:41 and in the 90% contour of the S190930s event. The expected number of atmospheric background events in the region visible by ANTARES is 2.28e-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 1.64e-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: 25884 SUBJECT: LIGO/Virgo S190930s: no counterpart candidates in AGILE-GRID observations DATE: 19/09/30 17:06:48 GMT FROM: Martina Cardillo at INAF-IAPS LIGO/Virgo S190930s: no counterpart candidates in AGILE-GRID observations M. Cardillo (INAF/IAPS),  F. Verrecchia (SSDC, and INAF/OAR), F. Longo (Univ. Trieste, and INFN Trieste), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), C. Casentini, G. Piano, A. Ursi (INAF/IAPS), F. Lucarelli, C. Pittori (SSDC, and INAF/OAR), A. Bulgarelli, V. Fioretti, N. Parmiggiani (INAF/OAS-Bologna), M. Pilia (INAF/OA-Cagliari),  report on behalf of the AGILE Team: In response to the LIGO/Virgo GW event S190930s at T0 = 2019-09-30 13:35:41 (UT), a preliminary analysis of the AGILE exposure at T0 shows that the Gamma-Ray Imaging Detector (GRID) exposure covered about 27% of the 90% c.l. localization region (LR) (40% of 90% c.l. LR is occulted by Earth) at an off-axis angle of about 5 degrees. We performed an analysis of the GRID data in the energy range 50 MeV - 10 GeV on T0, where good exposure of the S190930s 90% c.l. LR was available. No candidate gamma-ray transient was detected. The following preliminary GRID values of 3-sigma upper limit (UL) are obtained: - from 1.0e-06 to 4.9e-06 erg cm^-2 s^-1, with exposure of about 27% of the LR over the time interval ( T0 -2s ; T0 + 2s ); - from 8.4e-07 to 2.5e-06 erg cm^-2 s^-1, with exposure of about 26% of the LR over the time interval ( T0s ; T0 + 10s ); - from 1.4e-07 to 1.6e-06 erg cm^-2 s^-1, with exposure of about 26% of the LR over the time interval ( T0 ; 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: 25886 SUBJECT: LIGO/Virgo S190930s: Upper limits from Fermi-GBM Observations DATE: 19/09/30 19:52:14 GMT FROM: Joshua Wood at MSFC/Fermi-GBM J. Wood (NASA/MSFC) reports on behalf of the Fermi-GBM Team and the GBM-LIGO/Virgo group For S190930s and using the initial bayestar.fits.gz skymap, Fermi-GBM was observing 62.2% 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 S190930s (GCN 25871). 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. We therefore set upper limits on impulsive gamma-ray emission. 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: 5.7 6.6 10. 1.024 s: 1.6 2.2 3.5 8.192 s: 0.6 0.7 1.0 Assuming the median luminosity distance of 752 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 ------------------------------------ 0.128 s: 5.94 6.29 15.8 1.024 s: 1.67 2.10 5.53 8.192 s: 0.62 0.65 1.58 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25889 SUBJECT: LIGO/Virgo S190930s: no counterpart candidates in the Swift/BAT observations DATE: 19/10/01 01:13:46 GMT FROM: Amy Lien at GSFC A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (NASA/GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), A. P. Beardmore (U. Leicester), M. G. Bernardini (INAF-OAB), A. A. Breeveld (MSSL-UCL), D. N. Burrows (PSU), S. Campana (INAF-OAB), S. B. Cenko (NASA/GSFC), G. Cusumano (INAF-IASF PA), A. D'Ai (INAF-IASFPA), P. D'Avanzo (INAF-OAB), V. D'Elia (ASI-SSDC), 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 S190930s (LIGO/VIRGO Collaboration GCN Circ. 25871), where T0 is the LVC trigger time (2019-09-30T13:35:41.246 UTC). The center of the BAT field of view (FOV) at T0 is RA = 20.932 deg, DEC = -58.811 deg, and the roll angle is 164.350 deg. The BAT FOV (>10% partial coding) covers 0.40% of the integrated LVC localization probability, and 0.45% 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) from astrophysical origins are found in the BAT raw light curves with time bins of 64 ms, 1 s, and 1.6 s. The short spike at ~T-95.9 s in the 15-25 keV light curve is due to a detector glitch (see more explanation in the "Investigation of the detector glitch" section in the link below). 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 ~ 2.20 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 ~ 48.44 Mpc. Event data analysis is available from T0-100.968 s to T+99.102 s. No significant detections are found in the 15-350 keV images created using intervals of T0 to T0+0.1 s, T0-2 s to T0+8 s, and the whole event data range. BAT retains decreased, but significant, sensitivity to rate increases for gamma-ray events outside of its FOV. About 99.60% 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/S190930s/web/source_public.html //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25891 SUBJECT: LIGO/Virgo S190930s: Upper limits from CALET observations. DATE: 19/10/01 04:39:30 GMT FROM: Yuta Kawakubo at Louisiana State U./CALET S. Sugita, A. Yoshida, T. Sakamoto, V. Pal'shin (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), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena), and the CALET collaboration: The CALET Gamma-ray Burst Monitor (CGBM) was operating at the trigger time of S190930s T0 = 2019-09-30 13:35:41.247 UT (The LIGO Scientific Collaboration and Virgo Collaboration, GCN Circ.25871). 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 20 % and 100 %, respectively (and 100 % credible region of the initial sky map was above the horizon). The HXM and SGM fields of view were centered at RA = 28.1 deg, Dec = 3.4 deg and RA = 20.8 deg, Dec = -3.3 deg at T0, respectively. Based on the analysis of the light curve data with 0.125 sec time resolution from T0-60 sec to T0+60 sec, we found no significant excess around the trigger time in either the HXM or the SGM data. The CALET Calorimeter (CAL) was operating in the high energy trigger mode at the trigger time of S190930s. 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 in the overwrap region with the LIGO-Virgo high probability localization region. The 90% upper limit of CAL is 3.5x10^-5 erg/cm^2/s (10-100 GeV) when the summed LIGO-Virgo probability reaches 5%. The CAL FOV was centered at RA= 20.7 deg, DEC= -3.3 deg at T0. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25895 SUBJECT: LIGO/Virgo S190930s: No counterpart candidates in Fermi-LAT observations DATE: 19/10/01 09:59:05 GMT FROM: Magnus Axelsson at Stockholm U. M. Kovacevic (INFN Perugia), L. Scotton (Univ. and INFN, Torino), M. Axelsson (KTH and Stockholm Univ.), F. Longo (Univ. and INFN Trieste), E. Bissaldi (Politecnico and INFN Bari), N. Omodei (Stanford Univ.), M. Arimoto (Kanazawa Univ.) and D. Kocevski (NASA/MSFC) report on behalf of the Fermi-LAT Collaboration: We have searched data collected by the Fermi Large Area Telescope (LAT) on Sep 30, 2019, for possible high-energy (E > 100 MeV) gamma-ray emission in spatial/temporal coincidence with the LIGO/Virgo trigger S190930s (GCN 25871). 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 null instantaneous coverage of the LIGO probability region at the time of the trigger (T0 = 2019-09-30 13:35:41.247 UTC). Coverage started around 300 s after the trigger and reached 99% cumulative coverage at approximately T0 + 4 ks. The remaining area was not observed within 10 ks after the trigger. 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 1.4e-10 and 8.1e-08 [erg/cm^2/s]. The Fermi-LAT point of contact for this event is Nicola Omodei (nikomo@stanford.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: 25897 SUBJECT: LIGO/Virgo S190930t and S190930s: MASTER optical observation and optical transient DATE: 19/10/01 13:32:24 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tiurina, F.Balakin,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 S190930t (LVC GCN 25876) 146 sec after trigger time at 2019-09-30 14:36:33 UT (Lipunov et al. GCN 25875) and observed it at MASTER-Amur, -Tunka, -Kislovods, -Tavrida, -SAAO, -OAFA), see real-time coverage map at https://master.sai.msu.ru/site/master2/ligo_1.php?id=10861 During this inspect we found OT, but there are 2 PanSTARR sources in 1.6" and 1.8", and the blue one can be CV, but it is also inside LIGO/Virgo S190930s (LVC GCN 25871, Lipunov et al. GCN25870) and we need a Spectrum MASTER 205329.99+224421.2 discovery MASTER-IAC auto-detection system discovered OT source at (RA, Dec) = 20h 53m 29.99s +22d 44m 21.2s on 2019-09-30.90192 UT. The OT unfiltered magnitude is 18.1m (limit 19.3m). The OT is seen in 3 images. There is no minor planet at this place. We have reference image without OT on 2016-09-23.93716 UT with unfiltered magnitude limit 20.1m. Spectral observations are required. The discovery and reference images are available at: http://master.sai.msu.ru/static/OT/205329.99224421.2.png //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25912 SUBJECT: LIGO/Virgo S190930s: No counterpart candidates in KAIT observations DATE: 19/10/01 22:55:10 GMT FROM: Weikang Zheng at UC Berkeley Keto D. Zhang, Thomas de Jaeger, James Sunseri, Benjamin E. Stahl, WeiKang Zheng, Andrew Hoffman, Yukei Murakami, Sergiy Vasylyev, 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 S190930s (GCN 25871) 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. KAIT observed 367 of them based on their priority scores and elevation visibility, with each clear-filter exposure time being 60 s. The first image was taken at 03:42:23, Oct. 01th UT, about 14.1 minutes after the trigger, and the last image at 13:22:24 UT. 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(Oct01) RA_J2000 Dec_J2000 ----------------------------------------------- G0418118 03:42:23 20:24:50.8008 +43:02:35.0304 G0826512 03:43:38 20:28:08.2178 +28:29:57.0948 G0365855 03:44:56 20:29:59.9414 +49:52:17.1876 G0645883 03:46:14 20:30:29.5531 +27:40:42.906 G0547751 03:47:33 20:30:50.5663 +49:31:27.5628 G0412609 03:48:42 20:34:36.101 +44:24:56.6964 G0415068 03:49:52 20:34:42.1582 +44:22:01.668 G0611594 03:51:07 20:35:23.5474 +52:19:38.9172 G1462170 03:52:21 20:35:43.3668 +49:53:16.5552 G0222607 03:53:35 20:37:17.8565 +49:52:57.0144 G0217993 03:54:46 20:37:51.3941 +38:57:08.3808 G0434278 03:55:56 20:38:07.7417 +35:56:09.4776 G0216524 03:57:07 20:38:24.851 +43:10:45.516 G0688454 03:58:23 20:38:31.6699 +25:56:59.6256 G0447386 03:59:42 20:39:04.8706 +48:57:11.7432 G0213597 04:00:53 20:39:25.2686 +49:19:44.8608 G0461444 04:02:09 20:40:12.3852 +28:46:50.8728 G0217063 04:03:20 20:40:35.5738 +37:40:18.282 G0215614 04:04:30 20:40:49.8413 +37:53:28.2408 G0100676 04:05:45 20:41:14.7509 +53:10:44.4576 G0148818 04:06:56 20:41:16.2598 +40:45:10.3824 G1152068 04:08:16 20:41:16.5382 +21:50:10.7628 G0210865 04:09:31 20:41:21.5258 +41:33:30.3732 G0434947 04:10:44 20:41:29.8901 +29:56:40.4268 G0092724 04:12:02 20:42:13.9234 +51:13:31.3824 G0171171 04:13:13 20:42:15.6372 +37:40:31.4544 G1154608 04:14:27 20:42:57.8174 +21:11:45.582 G0413858 04:15:50 20:43:19.3946 +54:44:51.0864 G0105281 04:17:09 20:43:34.3579 +31:03:26.3232 G1175217 04:18:20 20:43:34.7899 +25:11:12.3756 G1226816 04:19:52 20:43:35.6177 +27:22:22.3788 G0839474 04:21:13 20:43:59.4946 +53:14:32.3016 G0628332 04:22:29 20:44:09.7999 +33:59:41.5968 G1211794 04:23:46 20:45:14.1065 +25:28:07.7268 G0106756 04:24:58 20:45:37.0678 +36:00:06.5088 G0991722 04:26:08 20:45:46.8749 +35:49:38.5032 G0776012 04:27:19 20:45:56.9458 +28:31:56.0208 G0057545 04:28:30 20:46:38.9942 +36:31:22.7424 G0974643 04:29:45 20:46:47.9518 +29:48:33.93 G1078443 04:30:54 20:47:04.7314 +28:41:03.0264 G1383881 04:32:05 20:47:07.7856 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G1003347 04:59:50 20:52:28.601 +22:17:38.148 G0205969 05:01:22 20:53:41.7041 +54:30:18.9252 G1224359 05:02:52 20:54:01.3697 +36:56:36.9744 G0417897 05:04:01 20:54:18.3106 +34:15:11.7288 G0466980 05:05:21 20:56:29.2382 +49:51:12.024 G0959750 05:06:43 20:56:48.4205 +28:17:15.2844 G0433910 05:08:11 20:57:04.1162 +52:43:51.5964 G0418628 05:09:25 20:57:09.8657 +52:49:06.0816 G0547945 05:10:38 20:57:12.2681 +51:47:13.1136 G1326683 05:12:08 20:57:13.1544 +26:19:38.4132 G0056855 05:13:19 20:57:13.4179 +36:45:03.8736 G0601857 05:14:36 20:57:18.7939 +12:11:13.6032 G1057527 05:15:52 20:57:28.6817 +37:43:56.8956 G0418630 05:18:11 20:58:13.3886 +40:43:21.288 G0514048 05:19:40 20:58:28.535 +53:33:14.706 G1399446 05:21:10 20:58:37.7491 +22:33:08.766 G1399068 05:22:21 20:58:59.436 +31:19:40.386 G1111349 05:23:33 20:58:59.8022 +37:49:56.3016 G1459263 05:24:44 20:59:00 +31:24:40.3812 G0994371 05:25:53 20:59:47.0875 +38:24:56.916 G1028931 05:27:02 20:59:53.4667 +38:29:37.9176 G0449096 05:28:28 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+64:40:42.9204 G0894711 12:14:55 01:06:52.3582 +61:11:29.9148 G1247893 12:16:04 01:07:48.247 +62:15:23.7024 G0330397 12:17:13 01:09:11.5154 +62:07:10.8984 G0186355 12:53:41 01:09:51.0401 +62:31:08.2812 G0263288 12:54:51 01:10:14.88 +61:05:47.4 G0138582 12:56:08 01:11:56.5022 +65:13:52.518 G0207623 12:57:17 01:13:42.8297 +65:37:18.822 G0297094 12:58:28 01:14:20.381 +63:43:33.4128 G0544341 12:59:37 01:15:33.0602 +63:37:00.0624 G0651624 13:00:53 01:16:11.4902 +58:18:28.1376 G0138506 13:02:03 01:16:58.6692 +61:14:39.786 G0214396 13:03:18 01:17:16.003 +65:12:00.702 G0043239 13:04:28 01:18:36.6046 +63:48:39.78 G1194690 13:05:46 01:18:39.8539 +55:02:37.4352 G1016592 13:06:55 01:19:39.1022 +56:43:10.1784 G0241298 13:08:16 01:19:45.0454 +63:09:19.9188 G0387631 13:09:25 01:20:03.251 +62:31:07.896 G0320015 13:10:38 01:21:04.7736 +65:04:38.532 G0322665 13:11:49 01:23:11.1919 +59:21:35.4528 G0117741 13:12:58 01:23:59.7559 +62:12:16.632 G1033211 13:15:17 01:24:58.927 +60:29:25.4076 G0311124 13:16:26 01:26:41.1878 +60:33:29.646 G0364906 13:17:35 01:28:31.9313 +63:05:58.938 G1248819 13:18:51 01:29:54.0883 +56:56:25.026 G0212502 13:20:02 01:30:02.9846 +62:12:46.5696 G0850257 13:21:13 01:30:22.4086 +59:57:20.2032 G0041605 13:22:24 01:31:03.6425 +54:14:37.6296 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25915 SUBJECT: LIGO/Virgo S190930s: no counterpart candidates in SAGUARO/CSS observations DATE: 19/10/01 23:37:17 GMT FROM: Kerry Paterson at Northwestern Kerry Paterson (Northwestern), Michael J. Lundquist, David J. Sand (UA), Wen-fai Fong, Jillian Rastinejad (Northwestern), Jennifer Andrews (UA), Sam Wyatt (UA), Eric Christensen, Alex Gibbs, Frank Shelly (UA/LPL), report on behalf of the SAGUARO collaboration: We initiated observations of 12 fields (each 5 deg^2, totalling 60 deg^2) within the LVC localization region for the GW trigger S190930s (LVC Circ 25871) starting on 2019-10-01 02:09:22 UT (0.52 days after the GW trigger) with the 1.5m Catalina Sky Survey telescope on Mt. Lemmon, AZ. Below are the field centers observed. RA DEC 318.8895 7.7292 318.8895 9.9375 316.6665 9.9375 316.3965 12.1458 315.8490 14.3541 313.5840 14.3541 314.1615 12.1458 319.1415 5.5208 321.3495 3.3125 321.3495 5.5208 318.6330 12.1458 313.2915 16.5625 We have posted our pointings to the Treasure Map, and encourage others to do the same: http://treasuremap.space/alerts?graceids=S190930s&pointing_status=all&alert_type=Initial Performing image subtraction, we find no new transients within the 60 deg^2 searched down to a 3-sigma limit of G~21.3 AB mag (calibrated to Gaia DR2) relative to deep CSS reference images. A more detailed description of SAGUARO can be found in Lundquist et al. 2019, ApJL, 881, 2. SAGUARO is supported by the National Science Foundation under Award Nos. AST-1909358 and AST-1908972. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25933 SUBJECT: LIGO/Virgo S190930s: Upper limits from Insight-HXMT/HE observations DATE: 19/10/03 09:26:07 GMT FROM: Qi Luo at IHEP Q. Luo, Q. B. Yi, S. Xiao, C. Cai, Y. G. Zheng, Y. Huang, C. K. Li, X. B. Li, G. Li, J. Y. Liao, S. L. Xiong, C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, M. Wu, Y. P. Xu, S. N. Zhang (IHEP), report on behalf of the Insight-HXMT team: Insight-HXMT was taking data normally around the reported LIGO/Virgo S190930s event (GCN #25871), trigger time 2019-09-30T13:35:41 UTC. At T0, about 57% of the LIGO localization region was covered by Insight-HXMT without occultation by the Earth. Within T0 +/- 100 s, no significant excess events (SNR > 3 sigma) are found in a search of the Insight-HXMT/HE raw light curves. Assuming the GW counterpart GRB with three typical GRB Band spectral models, two typical duration timescales (1 s, 10 s) from the center of the LIGO-Virgo location probability map (RA=313 deg, DEC=19 deg), the 5-sigma upper-limits fluence (0.2 - 5 MeV, incident energy) are reported below: Band model 1 (alpha=-1.9, beta=-3.7, Ep=70 keV): 1 s: 2.1e-07 erg cm^-2 10 s: 5.0e-07 erg cm^-2 Band model 2 (alpha=-1.0, beta=-2.3, Ep=230 keV): 1 s: 3.0e-07 erg cm^-2 10 s: 7.6e-07 erg cm^-2 Band model 3 (alpha=-0.0, beta=-1.5, Ep=1000 keV): 1 s: 4.6e-07 erg cm^-2 10 s: 1.3e-06 erg cm^-2 All measurements above are made with the CsI detectors operating in the regular mode with the energy range of about 80-800 keV (deposited energy). Only gamma-rays with energy greater than about 200 keV can penetrate the spacecraft and leave signals in the CsI detectors installed inside of the spacecraft. Insight-HXMT is the first Chinese space X-ray telescope, which was funded jointly by the China National Space Administration (CNSA) and the Chinese Academy of Sciences (CAS). More information could be found at: http://www.hxmt.org. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25968 SUBJECT: LIGO/Virgo S190930s: Updated Sky Localization DATE: 19/10/07 13:23:42 GMT FROM: Olivier Minazzoli at LIGO Virgo Collaboration The LIGO Scientific Collaboration and the Virgo Collaboration report: We have conducted further analysis of the data from LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) around the time of the compact binary merger (CBC) candidate S190930s (GCN Circular 25871). Parameter estimation has been performed using LALInference [1] and a new sky map, LALInference.fits.gz,0, distributed via GCN Notice, is available for retrieval from the GraceDB event page: https://gracedb.ligo.org/superevents/S190930s The preferred sky map at this time is LALInference.fits.gz,0. The 90% credible region is 1748 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 709 +/- 191 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 < https://emfollow.docs.ligo.org/userguide/>. [1] Veitch et al. PRD 91, 042003 (2015) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25969 SUBJECT: LIGO/Virgo S190930s: Updated Sky Localization DATE: 19/10/07 13:23:53 GMT FROM: Olivier Minazzoli at LIGO Virgo Collaboration The LIGO Scientific Collaboration and the Virgo Collaboration report: We have conducted further analysis of the data from LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) around the time of the compact binary merger (CBC) candidate S190930s (GCN Circular 25871). Parameter estimation has been performed using LALInference [1] and a new sky map, LALInference.fits.gz,0, distributed via GCN Notice, is available for retrieval from the GraceDB event page: https://gracedb.ligo.org/superevents/S190930s The preferred sky map at this time is LALInference.fits.gz,0. The 90% credible region is 1748 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 709 +/- 191 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 < https://emfollow.docs.ligo.org/userguide/>. [1] Veitch et al. PRD 91, 042003 (2015) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 25970 SUBJECT: LIGO/Virgo S190930s: no counterpart candidate in the SVOM/GWAC observations DATE: 19/10/07 13:51:36 GMT FROM: Cyril Lachaud at APC/Univ. Paris Diderot C.Lachaud (APC), X. G. Wang (GXU), A. Coleiro (APC), J.R. Mao (YNAO), G. W. Li (NAOC) on behalf of the SVOM Multi Messenger Astronomy and GWAC teams: http://www.svom.fr/en/svom-mma-and-gwac-team We observed 27 sky regions (total: 4050 square degrees with overlaps) to cover the skymap of the advanced LIGO/Virgo trigger S190930s, with SVOM/GWAC, at Xinglong Observatory equipped with a set of two types of wide angle cameras: FFOV cameras (FOV~900 square degrees/camera, aperture = 3.5 cm) and JFOV cameras (FOV~150 square degrees/camera, aperture = 18 cm). SVOM/GWAC currently comprises 4 FFOV cameras and 16 JFOV cameras, working with unfiltered band. The observations are operated in time-series mode, taking one exposure every 25 seconds (20s exposure + 5s readout). We estimate a 77.2% prior probability that the observed and processed regions contain the true location of the source. The images were taken between ~15 minutes before and ~5 hours after the event trigger time. The coordinates of the 27 sky regions observed after the trigger and their observation times are listed below: No. Ra Dec start-obs(UTC) end-obs(UTC) Camera_TYPE 1 01:45:10.30 57:37:14.52 2019-09-30 17:15:39 2019-09-30 17:28:37 JFOV 2 02:13:24.41 68:57:30.24 2019-09-30 17:17:17 2019-09-30 17:23:45 JFOV 3 21:18:19.68 68:54:10.44 2019-09-30 15:10:18 2019-09-30 15:31:18 JFOV 4 20:49:49.20 57:34:23.88 2019-09-30 15:14:18 2019-09-30 15:31:18 JFOV 5 20:08:15.60 30:22:52.32 2019-09-30 14:28:46 2019-09-30 14:58:59 JFOV 6 21:05:10.80 30:36:19.08 2019-09-30 14:38:29 2019-09-30 14:55:29 JFOV 7 21:12:28.32 23:45:53.64 2019-09-30 15:56:29 2019-09-30 16:23:11 JFOV 8 20:23:50.64 24:02:03.12 2019-09-30 16:09:50 2019-09-30 16:24:24 JFOV 9 21:18:24.48 35:26:04.92 2019-09-30 16:24:23 2019-09-30 16:24:23 JFOV 10 21:45:58.80 52:18:05.04 2019-09-30 16:28:13 2019-09-30 16:45:12 JFOV 11 21:34:48.24 40:42:21.24 2019-09-30 16:28:37 2019-09-30 16:56:08 JFOV 12 20:35:59.04 40:59:54.60 2019-09-30 16:48:26 2019-09-30 16:56:08 JFOV 13 21:19:55.20 01:30:02.95 2019-09-30 13:54:35 2019-09-30 16:26:11 JFOV 14 20:29:44.16 13:30:14.04 2019-09-30 13:54:35 2019-09-30 16:24:15 JFOV 15 21:20:11.76 13:41:14.64 2019-09-30 13:54:35 2019-09-30 16:20:36 JFOV 16 02:35:50.35 35:29:03.84 2019-09-30 17:40:06 2019-09-30 18:01:35 JFOV 17 21:20:36.48 57:56:40.56 2019-09-30 13:54:12 2019-09-30 14:24:03 JFOV 18 23:12:45.60 68:55:31.80 2019-09-30 13:54:12 2019-09-30 14:24:03 JFOV 19 22:45:54.48 64:26:27.96 2019-09-30 16:30:13 2019-09-30 16:43:11 JFOV 20 20:52:14.16 64:01:55.92 2019-09-30 16:32:14 2019-09-30 16:32:14 JFOV 21 22:27:42.00 23:44:02.04 2019-09-30 18:01:32 2019-09-30 18:24:10 JFOV 22 21:39:04.08 24:00:06.12 2019-09-30 13:26:16 2019-09-30 18:24:10 JFOV 23 22:33:36.00 35:24:57.24 2019-09-30 13:40:48 2019-09-30 18:24:10 JFOV 24 22:42:58.56 13:51:07.56 2019-09-30 17:40:48 2019-09-30 18:00:13 JFOV 25 21:44:38.40 47:20:02.04 2019-09-30 18:07:20 2019-09-30 18:35:18 JFOV 26 22:52:12.24 35:28:24.60 2019-09-30 18:07:21 2019-09-30 18:35:18 JFOV 27 03:40:37.78 64:29:39.84 2019-09-30 17:29:25 2019-09-30 17:29:25 JFOV The sky region #22 was observed at the time of the trigger (it has 3.5% probability to contain the true location of the source). Some sky regions have been observed before the GW event for a total of 1200 square degrees with overlap (from ~2 hours to ~ 12 minutes before the event) : No. Ra Dec start-obs(UTC) end-obs(UTC) Camera_TYPE 1 21:23:18.96 35:17:43.08 2019-09-30 12:53:59 2019-09-30 13:22:59 JFOV 2 20:17:48.24 47:21:36.72 2019-09-30 12:52:55 2019-09-30 13:22:59 JFOV 3 22:32:05.04 13:41:29.40 2019-09-30 11:42:57 2019-09-30 12:14:29 JFOV 4 22:31:43.92 01:29:58.74 2019-09-30 11:43:44 2019-09-30 12:11:29 JFOV 5 21:41:35.52 13:30:04.68 2019-09-30 11:43:44 2019-09-30 12:12:59 JFOV 6 23:13:06.96 52:21:46.08 2019-09-30 11:43:42 2019-09-30 12:08:27 JFOV 7 22:02:56.88 41:04:53.76 2019-09-30 12:06:12 2019-09-30 12:12:27 JFOV 8 23:01:46.32 40:46:03.72 2019-09-30 12:08:57 2019-09-30 12:12:27 JFOV The sky coverage map is available at: http://cmm.svom.cn/gwpub/O3/S190930s/S190930s_post.png (user:svomo3 pwd:gwo3) The weather condition was clear during the observations. A 3 sigma limiting magnitude of about 16.3 mag in R band was obtained in the single frames. No credible new source is detected by our online pipeline during follow-up observations. A more detailed image analysis including co-addition is ongoing with our offline pipeline to search for transient candidates.