//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27014 SUBJECT: LIGO/Virgo S200208q: Identification of a GW compact binary merger candidate DATE: 20/02/08 13:35:30 GMT FROM: Leo Singer at GSFC The LIGO Scientific Collaboration and the Virgo Collaboration report: We identified the compact binary merger candidate S200208q during real-time processing of data from LIGO Hanford Observatory (H1), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) at 2020-02-08 13:01:17.991 UTC (GPS time: 1265202095.991). The candidate was found by the MBTAOnline [1], CWB [2], PyCBC Live [3], and SPIIR [4] analysis pipelines. S200208q is an event of interest because its false alarm rate, as estimated by the online analysis, is 2.5e-09 Hz, or about one in 12 years. The event's properties can be found at this URL: https://gracedb.ligo.org/superevents/S200208q The classification of the GW signal, in order of descending probability, is BBH (>99%), Terrestrial (<1%), BNS (<1%), NSBH (<1%), or MassGap (<1%). Assuming the candidate is astrophysical in origin, the probability that the lighter compact object has a mass < 3 solar masses (HasNS) is <1%. Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. Two sky maps are available at this time and can be retrieved from the GraceDB event page: * bayestar.fits.gz,0, an initial localization generated by BAYESTAR [5], distributed via GCN notice about 3 minutes after the candidate event time. * bayestar.fits.gz,1, an initial localization generated by BAYESTAR [5], distributed via GCN notice about 9 minutes after the candidate event time. The preferred sky map at this time is bayestar.fits.gz,1. For the bayestar.fits.gz,1 sky map, the 90% credible region is 1120 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 2900 +/- 960 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] Adams et al. CQG 33, 175012 (2016) [2] Klimenko et al. PRD 93, 042004 (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: 27015 SUBJECT: LIGO/Virgo S200208q: Upper limits from IceCube neutrino searches DATE: 20/02/08 13:36:29 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 S200208q in a time range of 1000 seconds [3] centered on the alert event time (2020-02-08 12:52:57.991 UTC to 2020-02-08 13:09:37.991 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 S200208q calculated from the map circulated in the 3-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 S200208q ranges from 0.032 to 0.701 GeV cm^-2 in a 1000 second time window. The IceCube Neutrino Observatory is a cubic-kilometer neutrino detector operating at the geographic South Pole, Antarctica. The IceCube realtime alert point of contact can be reached at roc@icecube.wisc.edu [1] Bartos et al. arXiv:1810.11467 (2018) and Countryman et al.arXiv:1901.05486 (2019) [2] PoS(ICRC2019)918 and Braun et al., Astroparticle Physics 29, 299 (2008) [3] Baret et al., Astroparticle Physics 35, 1 (2011) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27016 SUBJECT: LIGO/Virgo S200208q : no neutrino counterpart candidate in ANTARES search DATE: 20/02/08 14:42:27 GMT FROM: Thierry Pradier at ANTARES/IPHC/U of Strasbourg 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 S200208q event using the 90% contour of the Preliminary probability map provided by the GW interferometers (GCN#27014 ). 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/S200208q_Preliminary.png . Considering the location probability provided by the LIGO/Virgo collaborations, there is a 68.5% 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 2020-02-08 13:01:17 and in the 90% contour of the S200208q event. The expected number of atmospheric background events in the region visible by ANTARES is 3.29e-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 2.37e-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: 27017 SUBJECT: LIGO/Virgo S200208q: No counterpart candidates in HAWC observations DATE: 20/02/08 15:15:55 GMT FROM: Hugo Ayala at Pennsylvania State University The HAWC Collaboration (https://www.hawc-observatory.org) reports: The HAWC Collaboration performed a follow-up of the gravitational wave trigger S200208q. At the time of the trigger the HAWC local zenith was oriented towards (RA, Dec) = (235.9 deg, 19.1 deg). 29% of the GW candidate sky location probability fell within our observable field of view (0-45 deg zenith angle). We performed a search for a short timescale emission using 6 sliding time windows (dt = 0.3s, 1s, 3s, 10s, 30s and 100s), shifted forward in time by 20% of their width. We searched the 95% probability containment area in a timescale-dependent time period, from t0-5dt to t0+10dt, where t0 is the time of the GW trigger. No significant gamma-ray detection above the background was observed. The sensitivity of this analysis is greatly dependent on zenith angle, ranging from 28.4deg 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 5.2e-06 erg/cm^2 to 1.1e-04 erg/cm^2 (2.6e-05 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: 27018 SUBJECT: LIGO/Virgo S200208q: Global MASTER-Net observations report DATE: 20/02/08 15:54:10 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva, D.Kuvshinov, D. Cheryasov (Lomonosov Moscow State University, SAI, Physics Department), R. Podesta, C.Lopez, F. Podesta, C.Francile (Observatorio Astronomico Felix Aguilar OAFA), 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-Tunka robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the LIGO/Virgo S200208q errorbox 9684 sec after trigger time at 2020-02-08 15:42:41 UT, with upper limit up to 16.7 mag. The observations began at zenith distance = 48 deg. The sun altitude is -49.0 deg. The galactic latitude b = 10 deg., longitude l = 263 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/ligo_1.php?id=11306 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 9774 | 2020-02-08 15:42:41 | MASTER-Tunka | (18h 08m 02.18s , +80d 05m 28.4s) | C | 180 | 16.7 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27019 SUBJECT: LIGO/Virgo S200208q: No counterpart candidates in INTEGRAL SPI-ACS prompt observation DATE: 20/02/08 15:54:25 GMT FROM: Sergey Molkov at Space Research Inst., Moscow Sergey Molkov (IKI, Moscow), James Rodi (IAPS-Roma, Italy), V. Savchenko, C. Ferrigno (ISDC/UniGE, Switzerland) 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 S200208q (GCN 27014). At the time of the event (2020-02-08 13:01:17 UTC, hereafter T0), INTEGRAL was operating in nominal mode. The peak of the event localization probability was at an angle of 88 deg with respect to the spacecraft pointing axis. This orientation implies strongly suppressed (12% of optimal) response of ISGRI, strongly suppressed (28% of optimal) response of IBIS/Veto, and somewhat suppressed (66% of optimal) response of SPI-ACS. The background within +/-300 seconds around the event was very stable (excess variance 1.1). 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 2.3e-07 erg/cm^2 (within the 50% probability containment region of the source localization) for a burst lasting less than 1 s with a characteristic short GRB spectrum (an exponentially cut off power law with alpha=-0.5 and Ep=600 keV) occurring at any time in the interval within 300 s around T0. For a typical long GRB spectrum (Band function with alpha=-1, beta=-2.5, and Ep=300 keV), the derived peak flux upper limit is ~2e-07 (5.9e-08) erg/cm^2/s at 1 s (8 s) time scale in 75-2000 keV energy range. For the mean reported distance 2900.0 Mpc this corresponds to the limit on the total isotropic equivalent energy in 1 s of 2.3e+50 erg for the short GRB spectrum and for a long GRB spectrum isotropic equivalent luminosity in 1 s (8 s) of 1.7e+50 erg/s (5.9e+49 erg/s) We report for completeness and in order of FAP, all excesses identified in the search region. We find: 2 likely background excesses: T-T0 | scale | S/N | luminosity ( x 1e+50 erg/s) | FAP -77 | 3.1 | 4 | 18.1 +/- 4.84 +/- 6.97 | 0.0803 -35.1 | 0.65 | 3.7 | 3.75 +/- 1.06 +/- 1.44 | 0.255 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: 27020 SUBJECT: LIGO/Virgo S200208q: upper limits from AGILE/MCAL observations DATE: 20/02/08 17:02:13 GMT FROM: Francesco Longo at U of Trieste,INFN Trieste F. Longo (Univ. Trieste, and INFN Trieste), M. Cardillo (INAF/IAPS), 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 S200208q at T0 = 2020-02-08 13:01:17.991 (UT), a preliminary analysis of the AGILE minicalorimeter (MCAL) triggered data found no event candidates within a time interval covering -/+ 15 sec from the LIGO/Virgo T0. At the T0, 100% of the S200208q 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 S200208q localization region, from a minimum of 1.4E-06 erg cm^-2 to a maximum of 6.6E-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: 27021 SUBJECT: LIGO/Virgo S200208q : upper limits from AGILE/GRID observations DATE: 20/02/08 17:52:26 GMT FROM: Francesco Longo at U of Trieste,INFN Trieste 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 S200208q at T0 = 2020-02-08 13:01:17.991 (UTC) a preliminary analysis of the AGILE exposure at T0 shows that the Gamma-Ray Imaging Detector (GRID) exposure covered the 37% of the 90% c.l. localization region (LR). We performed an analysis of the GRID data in the energy range 50 MeV - 10 GeV on T0, where good exposure of the S200208q 90% c.l. LR was available. No candidate gamma-ray transient was detected. The following preliminary GRID values of 3-sigma upper limit (UL) are obtained: from 7.0e-08 to 7.4e-06 erg cm^-2 s^-1, with exposure of about 72% of the LR over the time interval ( T0s ; T0 + 100s ); These measurements were obtained with AGILE observing a large portion of the sky in spinning mode. Additional analysis of AGILE data is in progress. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27022 SUBJECT: LIGO/Virgo S200208q: Upper limits from Fermi-GBM Observations DATE: 20/02/08 22:20:42 GMT FROM: Suraj Poolakkil at UAH S. Poolakkil (UAH) reports on behalf of the Fermi-GBM Team and the GBM-LIGO/Virgo group. For S200208q and using the bayestar.fits.gz,1 skymap, Fermi-GBM was observing 95.4% 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 S200208q (GCN 27014). 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=306.6, Dec=17.6 with a radius of 67.3 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: 7.3 9.9 17. 1.024 s: 2.3 2.9 6.0 8.192 s: 0.6 0.9 2.2 Assuming the median luminosity distance of 2900 Mpc from the GW detection, we estimate the following intrinsic luminosity upper limits over the 1 keV-10 MeV energy range (in units of 10^50 erg/s): Timescale Soft Normal Hard ------------------------------------ 0.128s: 11.6 13.7 39.8 1.024s: 3.6 4.0 14.0 8.192s: 1.0 1.4 5.1 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27023 SUBJECT: LIGO/Virgo S200208q: no counterpart candidates in the Swift/BAT observations DATE: 20/02/08 22:47:19 GMT FROM: Amy Lien at GSFC D. M. Palmer (LANL), S. D. Barthelmy (NASA/GSFC), A. Y. Lien (GSFC/UMBC), T. Sakamoto (AGU), A. P. Beardmore (U. Leicester), M. G. Bernardini (INAF-OAB), A. A. Breeveld (MSSL-UCL), D. N. Burrows (PSU), S. Campana (INAF-OAB), S. B. Cenko (NASA/GSFC), G. Cusumano (INAF-IASF PA), A. D'Ai (INAF-IASFPA), P. D'Avanzo (INAF-OAB), V. D'Elia (ASI-ASDC), S. Emery (UCL-MSSL), P. A. Evans (U. Leicester), P. Giommi (ASI), C. Gronwall (PSU), D. Hartmann (Clemson U.), J. A. Kennea (PSU), N. Klingler (PSU), H. A. Krimm (NSF), N. P. M. Kuin (UCL-MSSL), F. E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB), J. A. Nousek (PSU), S. R. Oates (U. of Birmingham), 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 (U. 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 S200208q (LIGO/VIRGO Collaboration GCN Circ. 27014), where T0 is the LVC trigger time (2020-02-08T13:01:17.991 UTC). The center of the BAT field of view (FOV) at T0 is RA = 256.575 deg, DEC = -40.369 deg, and the roll angle is 92.479 deg. The BAT FOV (>10% partial coding) covers 0.00% of the integrated LVC localization probability. Note that the sensitivity in the BAT FOV changes with the partial coding fraction. Please see the BAT FOV figure in the summary page (link below) for the specific location of the LVC region relative to the BAT FOV. Within T0 +/- 100 s, no significant detections (signal-to-noise ratio >~ 5 sigma) are found in the BAT raw light curves with time bins of 64 ms, 1 s, and 1.6 s. Assuming an on-axis (100% coded) short GRB with a typical spectrum in the BAT energy range (i.e., a simple power-law model with a power-law index of -1.32, Lien & Sakamoto et al. 2016), the 5-sigma upper limit in the 1-s binned light curve corresponds to a flux upper limit (15-350 keV) of ~ 7.70 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 ~ 81.88 Mpc. Event data are available from T0-45.46 s to T0+44.61 s and from T0+98.54 to T0+101.56. No significant detections (above our typical image threshold of ~ 6.5 to 7 sigma) are found in the 15-350 keV images created using intervals of T0-0.1 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 81.00% 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/S200208q/web/source_public.html //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27024 SUBJECT: LIGO/Virgo S200208q: Coverage and upper limits from MAXI/GSC observations DATE: 20/02/08 23:55:38 GMT FROM: Hitoshi Negoro at Nihon U H. Negoro (Nihon U.), N. Kawai (Tokyo Tech), S. Sugita, M. Serino (AGU), M. Nakajima, W. Maruyama, M. Aoki, K. Kobayashi, R. Takagi (Nihon U.), T. Mihara, C. Guo, Y. Zhou, 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, 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 S200208q at 2020-02-08 13:01:17.991 UTC (GCN 27014). At the trigger time of S200208q, the high-voltage of MAXI/GSC was on. The instantaneous field of view of GSC at the GW trigger time covered 1% 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 63% of the 90% credible region of the bayestar skymap from 13:01:17 to 14:11:25 UTC (T0+0 to T0+4208 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: 27028 SUBJECT: LIGO/Virgo S200208q: No counterpart candidates in Fermi-LAT observations DATE: 20/02/09 22:25:19 GMT FROM: Lorenzo Scotton at CNRS/IN2P3/LUPM L. Scotton (CNRS/IN2P3/LUPM), D. Tak (Univ. of Maryland & NASA/GSFC), M. Axelsson (KTH & Stockholm Univ), E. Bissaldi (Politecnico & INFN Bari), D. Kocevski (NASA/MSFC), N. Omodei (Stanford Univ.) and F. Longo (University and INFN, Trieste) report on behalf of the Fermi-LAT Collaboration: We have searched data collected by the Fermi Large Area Telescope (LAT) on February 8, 2020, for possible high-energy (E > 100 MeV) gamma-ray emission in spatial/temporal coincidence with the LIGO/Virgo trigger S200208q (GCN 27014). We define "instantaneous coverage" as the integral over the region of the LIGO probability map that is within the LAT field of view at a given time, and "cumulative coverage" as the integral of the instantaneous coverage over time. Fermi-LAT had an instantaneous coverage of ~47% of the LIGO probability at the time of the trigger (T0 = 2020-02-08 13:01:17.991 UTC), and reached 100% cumulative coverage after ~3.8 ks. We performed a search for a transient counterpart within the observed region of the 90% contour of LIGO map in a fixed time window from T0 to T0 + 10 ks. No significant new sources are found. Energy flux upper bounds for the fixed time interval between 100 MeV and 1 GeV for this search vary between 1.3e-10 and 2.5e-09 [erg/cm^2/s]. The Fermi-LAT point of contact for this event is Lorenzo Scotton (lorenzo.scotton@lupm.in2p3.fr). 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: 27030 SUBJECT: LIGO/Virgo S200208q: Not observable by CALET DATE: 20/02/11 05:53:50 GMT FROM: Yuta Kawakubo at Louisiana State U./CALET P. S. Marrocchesi (U of Siena), 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), S. Ricciarini (U of Florence), and the CALET collaboration: At the trigger time of the compact binary merger candidate S200208q, T0 = 2020-02-08 13:01:17.991 UT (The LIGO Scientific Collaboration and Virgo Collaboration, GCN Circ. 27014), the CALET Gamma-ray Burst Monitor (CGBM) high voltages were off (from T0-19 min to T0+13 min). The CALET Calorimeter (CAL) was operating in the high energy trigger mode at the trigger time of S200208q. Using the CAL data, we have searched for gamma-ray events in the 10-100 GeV band from -60 sec to +60 sec from the GW trigger time and found no candidates. There was no significant overlap with the LVC high probability localization region at T0+-60 sec. The CAL FOV was centered at RA = 224.1 deg, Dec= -41.8 deg at T0. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27033 SUBJECT: LIGO/Virgo S200208q: No counterpart candidates in KAIT observations DATE: 20/02/11 08:24:51 GMT FROM: Weikang Zheng at UC Berkeley James Sunseri, Yukei Murakami, WeiKang Zheng, 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 S200208q (GCN 27014) 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 115 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 09:03:56, Feb. 09th UT, about 20 hours after the trigger, and the last image at 12:34:44 UT. Our typical limiting mag is 18.0. No viable counterparts were identified and the analysis is ongoing. A full list of galaxies observed by KAIT is given below. GladeID UT(Feb09) RA_J2000 Dec_J2000 ----------------------------------------------- G0611504 09:03:56 12:39:33.1495 +10:58:03.7164 G0704258 09:06:17 12:52:19.5336 +13:21:29.6604 G0284556 09:07:33 13:01:32.7722 +18:48:30.978 G0618945 09:08:42 13:03:24.4262 +20:11:49.0776 G0675119 09:09:52 13:03:46.5857 +19:16:17.0616 G0727874 09:13:34 13:29:21.4123 +37:24:50.1444 G0195216 09:14:43 13:34:32.4792 +37:35:15.2376 G0801463 09:15:52 13:35:35.1854 +40:06:40.122 G0603678 09:17:02 13:41:42.1949 +40:52:28.0344 G0697332 09:18:11 13:43:40.5689 +41:41:44.6892 G0595963 09:19:20 13:44:41.521 +40:28:02.7624 G0637326 09:20:46 13:50:14.7583 +56:02:32.9712 G0721271 09:22:03 13:52:38.5913 +46:20:59.1036 G0663946 09:23:23 13:53:54.1442 +57:10:05.6892 G0739375 09:24:33 13:55:00.564 +53:59:42.1044 G0747150 09:25:53 13:55:01.355 +45:50:06.684 G1817667 09:27:02 13:55:53.76 +43:29:52.44 G0568505 09:28:21 13:56:14.425 +55:43:23.0448 G1123852 09:29:36 13:56:37.0934 +49:14:49.0416 G1326493 09:30:46 13:56:37.9394 +53:14:13.0344 G0821694 09:31:55 13:56:56.7151 +53:51:59.1156 G0755125 09:33:04 13:58:02.0544 +53:01:01.7148 G0766898 09:34:14 13:58:31.6478 +49:32:23.7156 G0617024 09:35:23 13:58:41.0998 +54:05:07.314 G0272146 09:36:32 14:02:25.3968 +51:12:31.8492 G0348702 10:23:42 14:02:28.2166 +54:16:25.6368 G1812485 10:24:51 14:02:52.8 +54:26:11.868 G0676140 10:26:11 14:03:32.7722 +49:58:07.1004 G0732463 10:27:20 14:04:05.2186 +49:58:47.0784 G0627353 10:28:29 14:04:55.7081 +54:24:10.4976 G0765189 10:29:39 14:05:01.3037 +52:46:21.3384 G0703757 10:31:02 14:05:10.47 +60:12:19.5732 G1796893 10:32:22 14:05:17.28 +53:19:10.668 G0575685 10:33:33 14:05:24.6569 +58:24:48.33 G0642817 10:34:42 14:05:29.5495 +55:05:38.3784 G0622798 10:35:52 14:06:09.0528 +55:22:03.414 G0647407 10:37:01 14:06:49.9183 +57:53:49.308 G0638901 10:38:10 14:07:08.573 +56:32:24.4572 G0592101 10:39:20 14:07:29.5459 +52:08:29.1048 G0704739 10:40:29 14:07:47.6698 +53:22:13.2456 G0642359 10:41:38 14:08:08.3789 +55:43:13.7496 G0791124 10:42:47 14:08:10.5029 +52:40:48.1656 G1087595 10:44:08 14:08:12.9456 +60:14:32.8092 G0594415 10:45:26 14:08:21.5333 +55:18:05.7924 G0661360 10:46:35 14:08:35.5481 +55:32:24.774 G0647066 10:47:42 14:08:54.0674 +55:26:26.5344 G1042806 10:48:52 14:09:02.2486 +54:33:22.5864 G0581800 10:50:03 14:09:36.9763 +58:25:53.6448 G0577065 10:51:12 14:09:38.0822 +58:30:33.66 G0664391 10:52:22 14:09:42.1032 +55:27:38.6892 G0672191 10:53:33 14:09:46.681 +55:29:14.7084 G0603349 10:54:42 14:09:50.7679 +58:59:25.7244 G0785568 10:55:54 14:09:55.6788 +52:33:10.8612 G0823819 10:57:05 14:09:59.5898 +59:11:33.7308 G0671853 10:58:15 14:10:01.289 +55:38:12.7356 G0813080 11:07:30 14:10:01.5454 +54:52:54.7464 G0977197 11:08:39 14:10:13.169 +59:01:00.6708 G0717223 11:09:50 14:10:15.0989 +53:20:06.8352 G0748846 11:11:10 14:10:34.7021 +51:27:52.8336 G0580346 11:12:32 14:10:43.4362 +58:31:03.5436 G0671301 11:13:55 14:11:03.7574 +48:57:55.8288 G0729374 11:15:17 14:11:15.8753 +57:36:08.892 G0676919 11:16:26 14:11:17.2193 +55:18:23.9076 G0822872 11:17:33 14:11:18.4462 +55:10:52.9176 G0827466 11:18:43 14:11:24.5801 +57:14:55.9752 G0559334 11:19:52 14:11:29.0844 +55:07:18.9984 G0723066 11:21:12 14:11:40.5432 +52:38:07.5732 G0566578 11:22:21 14:11:47.8087 +54:57:46.9836 G0735801 11:23:30 14:11:49.5043 +52:49:00.5196 G0688629 11:24:40 14:11:49.5521 +54:57:32.9616 G0799824 11:25:51 14:12:43.8209 +49:52:06.6936 G0599287 11:27:02 14:12:56.4038 +55:21:13.2732 G0773650 11:28:12 14:13:12.3523 +53:59:34.332 G0678111 11:29:21 14:13:27.3595 +54:43:46.2684 G0772607 11:30:30 14:13:49.8523 +57:46:10.7112 G0740612 11:31:42 14:13:57.096 +52:45:52.4736 G0505067 11:32:54 14:14:25.1477 +57:37:50.6388 G0755393 11:34:18 14:14:54.4116 +60:00:40.1292 G0740964 11:35:27 14:15:08.4156 +56:57:01.0584 G0472742 11:36:52 14:15:20.3174 +52:20:44.6532 G0756243 11:38:14 14:15:27.4183 +57:36:33.0372 G0553864 11:39:36 14:15:30.1757 +51:29:54.906 G0031234 11:40:45 14:15:33.3142 +51:23:15.936 G0643903 11:41:52 14:15:39.7596 +52:32:37.968 G0816816 11:43:02 14:15:51.493 +53:35:07.9728 G0714551 11:56:47 14:15:52.8295 +50:19:25.9788 G0656839 11:58:08 14:16:00.6226 +55:47:13.0992 G0009685 11:59:29 14:16:17.1168 +51:16:46.0308 G0569557 12:00:49 14:16:17.8126 +55:22:44.3244 G0597629 12:02:02 14:16:38.5694 +54:07:20.3052 G1248064 12:03:26 14:17:45.3881 +59:04:08.9364 G0653802 12:04:45 14:17:47.2668 +55:30:58.914 G0766815 12:05:57 14:17:52.1009 +56:33:18.0432 G0014532 12:07:09 14:18:40.1587 +56:28:10.7148 G0790756 12:08:27 14:18:40.8766 +54:23:12.7248 G0579069 12:09:43 14:18:45.2306 +55:52:27.7608 G0749743 12:11:02 14:19:04.8413 +53:02:50.6868 G0761100 12:12:22 14:19:15.3077 +56:14:00.7692 G0777965 12:13:35 14:19:20.5224 +56:06:09.7308 G0723580 12:14:55 14:19:21.0828 +58:56:20.7132 G0748887 12:16:07 14:19:28.4582 +58:57:25.4232 G0716716 12:17:27 14:19:45.5712 +56:25:08.5332 G0752682 12:18:44 14:19:55.7592 +58:20:53.5272 G0600310 12:20:04 14:20:26.9604 +55:48:08.2908 G0553042 12:21:18 14:20:58.6193 +56:49:01.1928 G0722677 12:22:29 14:20:58.9637 +56:22:12.1872 G0603174 12:23:40 14:21:08.789 +56:46:36.5556 G1097052 12:25:08 14:21:15.6629 +61:35:16.6128 G0598447 12:26:34 14:21:27.6562 +57:00:20.628 G0902837 12:28:05 14:21:35.8226 +49:33:04.6404 G0724743 12:29:35 14:21:41.7919 +56:51:07.5744 G0652437 12:30:57 14:22:31.6774 +53:57:08.1036 G0819895 12:32:19 14:22:55.8581 +56:06:34.3548 G0713155 12:33:32 14:23:14.2018 +56:39:36.3276 G1190114 12:34:44 14:23:21.3684 +56:40:52.2732 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27036 SUBJECT: LIGO/Virgo S200208q: Updated Sky Localization DATE: 20/02/12 06:57:42 GMT FROM: Leo Singer at GSFC The LIGO Scientific Collaboration and the Virgo Collaboration report: We have conducted further analysis of the LIGO Hanford Observatory (H1), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) data around the time of the compact binary merger (CBC) candidate S200208q (GCN 27014). 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/S200208q The preferred sky map at this time is LALInference.fits.gz,0. For the LALInference.fits.gz,0 sky map, the 90% credible region is well fit by an ellipse with an area of 27 deg2 described by the following DS9 region (right ascension, declination, semi-major axis, semi-minor axis, position angle of the semi-minor axis): icrs; ellipse(09h17m19s, -33d42m23s, 4d, 2d, 76d) Marginalized over the whole sky, the a posteriori luminosity distance estimate is 2142 +/- 459 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: 27053 SUBJECT: LIGO/Virgo S200208q: no counterpart candidate in SVOM/C-GFT observations DATE: 20/02/13 08:36:33 GMT FROM: Xuhui Han at NAOC/SVOM Z. Kang (CHO), B. W. Li (CHO), Z. W. Li (CHO), C. Wu (NAOC), X. H. Han (NAOC)，S. Antier (CNRS/APC), N. Leroy (CNRS/LAL), D. Turpin (CEA/AIM), C. Z. Liu (CHO), B. L. Niu (CHO), L. C. Han (CHO) report on behalf of the SVOM Multi Messenger Astronomy and GWAC teams (http://www.svom.fr/en/svom-mma-and-gwac-team): We observed the LIGO/Virgo trigger S200208q (GCN #27014) with C-GFT (Chinese Ground Follow-up Telescope in SVOM mission). C-GFT is located at Jilin, Changchun Observatory, National Astronomical Observatories, CAS. It has FOV of 1.35 X 1.35 deg**2 with a 4k*4k CMOS detector mounted on the primary focus of 1.2-meter-aperure telescope. The first unfiltered image was taken ~23.4 hours after the event trigger time. No credible new source was detected in our pipeline. A total number of 16 fields was observed. The coordinates (J2000) of the fields, the observation time, limit mag (5sigma), are listed below. No. RA Dec obs_time (UTC) limit_mag(5sigma) ========================================================= 1 18:01:49.3 +80:46:07.0 2020-02-09 12:23:38.5 17.7 2 18:01:41.3 +79:46:09.1 2020-02-09 12:25:28.5 17.9 3 18:01:28.7 +77:46:31.4 2020-02-09 12:28:51.5 17.8 4 18:01:23.0 +76:46:35.6 2020-02-09 12:30:07.5 17.8 5 18:01:31.8 +77:46:32.9 2020-02-09 12:31:50.5 17.8 6 19:00:29.1 +76:46:03.2 2020-02-09 12:33:21.5 17.7 7 18:01:34.6 +77:46:35.3 2020-02-09 12:34:40.5 17.9 8 18:01:37.4 +79:58:12.7 2020-02-09 12:37:59.5 17.8 9 17:01:32.2 +77:59:02.1 2020-02-09 12:39:42.5 17.8 10 19:01:30.3 +80:57:33.9 2020-02-09 12:41:15.5 17.8 11 19:01:03.4 +76:57:35.9 2020-02-09 12:42:22.5 17.8 12 17:01:32.8 +77:59:06.5 2020-02-09 12:43:41.5 17.7 13 18:01:49.9 +80:58:19.1 2020-02-09 12:44:42.5 17.9 14 19:01:09.3 +77:57:37.1 2020-02-09 12:45:41.5 17.9 15 17:01:25.4 +76:59:08.0 2020-02-09 12:46:36.5 17.8 16 17:01:14.5 +74:59:06.7 2020-02-09 12:47:31.5 17.7 The observation and reduction will continue. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27054 SUBJECT: LIGO/Virgo S200208q : No significant candidates in TAROT - FRAM - GRANDMA observations DATE: 20/02/13 09:14:19 GMT FROM: Sarah Antier at APC E. Howell (OzGrav-UWA), S. Agayeva (SHAO), A. Baransky (Kyiv Uni), P. Hello (IJCLab), M. Boer (Artemis), N. Christensen (Artemis), L. Eymar (Artemis), S. Karpov (FZU), A. Klotz (IRAP), M. Masek (FZU), K. Noysena (Artemis, IRAP), S. Antier (APC), A. Coleiro (APC), D. Corre (IJCLab), M. Coughlin (UMN), D. Coward (OzGrav-UWA), J.G. Ducoin  (IJCLab), B. Gendre (OzGrav-UWA), D. A. Kann (HETH/IAA-CSIC), N. Kochiashvili (Iliauni), C. Lachaud (APC), N. Leroy (IJCLab), M. Prouza (FZU)C. Thoene (HETH/IAA-CSIC), D. Turpin (AIM-CEA), X. Wang (THU) report on behalf of the FRAM, TAROT and GRANDMA collaborations. We performed tiled observations of LIGO/Virgo S200208q event with the FRAM-Auger, FRAM-CTA-N, TAROT-Calern (TCA), TAROT-Chili (TCH), TAROT- Reunion (TRE) telescopes. FRAM-Auger is located at Pierre Auger Observatory. FRAM-CTA-N is located at Observatorio del Roque de los Muchachos. TCA is located at Calern site at the Cote d'Azur observatory. TCH is located at La Silla  ESO observatory (LaS/ESO). TRE is located at Les Makes astronomical observatory. The following table shows for each telescope: the delay in minutes from the trigger, which filter is used, the field of view of the telescope in degrees and the typical limiting magnitude (AB mag) for a  given exposure in seconds (s). +-------------+---------+----------+-------------+------------+ | Telescope   | Delay   | Filter   | f.o.v.      | Limiting   | |             | [min]   |          | [deg]       | Mag.       | |-------------+---------+----------+-------------+------------| | FRAM-Auger  | 1102    | R        | 1.0 x 1.0   | 18.0 (60s) | | FRAM-CTA-N  | 563     | R        | 0.45 x 0.45 | 17.0 (90s) | | TCA         | 453     | Clear    | 1.9 x 1.9   | 18.0 (60s) | | TCH         | 686     | Clear    | 1.9 x 1.9   | 18.0 (60s) | | TRE         | 1619    | Clear    | 4.2 x 4.2   | 17.0 (60s) | +-------------+---------+----------+-------------+------------+ We performed the following joint tiled observations [1] : +-------------+------------+------------+---------+---------+---------+ | Telescope   | TStart     | TEnd       | RA      | DEC     | Proba   | |             | [UTC]      | [UTC]      | [deg]   | [deg]   | [%]     | |-------------+------------+------------+---------+---------+---------| | FRAM-Auger  | 2020-02-09 | 2020-02-09 | 140.134 | -36.486 | 3.2     | |             | 07:22:34   | 07:24:34   |         | |         | | FRAM-Auger  | 2020-02-09 | 2020-02-09 | 139.470 | -35.514 | 5.5     | |             | 07:27:35   | 07:29:35   |         | |         | | -----       | -----      | -----      | -----   | -----   | -----   | | FRAM-CTA-N  | 2020-02-08 | 2020-02-08 | 139.894 | -36.037 | 0.9     | |             | 22:24:17   | 22:26:17   |         | |         | | FRAM-CTA-N  | 2020-02-08 | 2020-02-08 | 140.195 | -36.474 | 0.6     | |             | 22:28:36   | 22:30:36   |         | |         | | FRAM-CTA-N  | 2020-02-08 | 2020-02-08 | 139.353 | -36.037 | 0.8     | |             | 22:30:52   | 22:34:58   |         | |         | | FRAM-CTA-N  | 2020-02-08 | 2020-02-08 | 139.267 | -35.600 | 1.0     | |             | 22:35:11   | 22:39:17   |         | |         | | FRAM-CTA-N  | 2020-02-08 | 2020-02-08 | 139.806 | -35.600 | 1.1     | |             | 22:39:30   | 22:43:36   |         | |         | | FRAM-CTA-N  | 2020-02-08 | 2020-02-08 | 139.650 | -36.474 | 0.6     | |             | 22:43:50   | 22:47:56   |         | |         | | FRAM-CTA-N  | 2020-02-08 | 2020-02-08 | 140.046 | -35.163 | 1.4     | |             | 22:48:09   | 22:52:15   |         | |         | | FRAM-CTA-N  | 2020-02-08 | 2020-02-08 | 140.345 | -35.600 | 1.1     | |             | 22:52:34   | 22:56:40   |         | |         | | FRAM-CTA-N  | 2020-02-08 | 2020-02-08 | 139.511 | -35.163 | 1.4     | |             | 22:56:53   | 23:00:59   |         | |         | | FRAM-CTA-N  | 2020-02-08 | 2020-02-08 | 140.256 | -37.348 | 0.3     | |             | 23:01:13   | 23:05:19   |         | |         | | FRAM-CTA-N  | 2020-02-08 | 2020-02-08 | 139.403 | -36.911 | 0.3     | |             | 23:05:32   | 23:09:38   |         | |         | | FRAM-CTA-N  | 2020-02-08 | 2020-02-08 | 141.047 | -36.911 | 0.3     | |             | 23:09:53   | 23:13:58   |         | |         | | FRAM-CTA-N  | 2020-02-08 | 2020-02-08 | 140.739 | -36.474 | 0.5     | |             | 23:14:12   | 23:18:18   |         | |         | | FRAM-CTA-N  | 2020-02-08 | 2020-02-08 | 139.704 | -37.348 | 0.2     | |             | 23:18:31   | 23:22:37   |         | |         | | -----       | -----      | -----      | -----   | -----   | -----   | | TCA         | 2020-02-08 | 2020-02-13 | 209.879 | 55.692  | <0.1    | |             | 20:34:17   | 00:02:22   |         | |         | | TCA         | 2020-02-08 | 2020-02-13 | 213.093 | 55.692  | <0.1    | |             | 21:08:40   | 03:56:03   |         | |         | | TCA         | 2020-02-08 | 2020-02-13 | 210.181 | 53.837  | <0.1    | |             | 22:15:24   | 04:02:46   |         | |         | | TCA         | 2020-02-09 | 2020-02-13 | 216.307 | 55.692  | <0.1    | |             | 01:22:06   | 01:59:07   |         | |         | | TCA         | 2020-02-09 | 2020-02-13 | 213.409 | 51.981  | <0.1    | |             | 02:41:11   | 02:18:17   |         | |         | | TCA         | 2020-02-09 | 2020-02-13 | 213.258 | 53.837  | <0.1    | |             | 03:01:52   | 01:39:54   |         | |         | | TCA         | 2020-02-09 | 2020-02-13 | 274.550 | 76.105  | <0.1    | |             | 18:22:46   | 02:44:09   |         | |         | | TCA         | 2020-02-09 | 2020-02-12 | 212.913 | 57.548  | <0.1    | |             | 20:39:13   | 05:01:02   |         | |         | | TCA         | 2020-02-10 | 2020-02-13 | 207.104 | 53.837  | <0.1    | |             | 00:22:06   | 03:30:33   |         | |         | | TCA         | 2020-02-10 | 2020-02-13 | 216.335 | 53.837  | <0.1    | |             | 01:04:44   | 04:14:58   |         | |         | | TCA         | 2020-02-10 | 2020-02-13 | 268.857 | 77.960  | <0.1    | |             | 02:37:59   | 01:26:20   |         | |         | | TCA         | 2020-02-11 | 2020-02-13 | 216.277 | 57.548  | <0.1    | |             | 20:29:49   | 05:00:20   |         | |         | | TCA         | 2020-02-11 | 2020-02-13 | 207.507 | 51.981  | <0.1    | |             | 20:48:45   | 01:00:42   |         | |         | | TCA         | 2020-02-11 | 2020-02-13 | 207.879 | 50.125  | <0.1    | |             | 20:55:28   | 03:16:52   |         | |         | | TCA         | 2020-02-11 | 2020-02-13 | 277.229 | 77.960  | <0.1    | |             | 22:45:47   | 02:57:45   |         | |         | | TCA         | 2020-02-12 | 2020-02-13 | 210.458 | 51.981  | <0.1    | |             | 00:22:23   | 04:35:10   |         | |         | | TCA         | 2020-02-12 | 2020-02-13 | 210.714 | 50.125  | <0.1    | |             | 00:29:10   | 02:31:47   |         | |         | | TCA         | 2020-02-12 | 2020-02-13 | 216.360 | 51.981  | <0.1    | |             | 01:01:37   | 00:53:58   |         | |         | | TCA         | 2020-02-12 | 2020-02-13 | 208.223 | 48.270  | <0.1    | |             | 01:20:43   | 03:23:37   |         | |         | | TCA         | 2020-02-12 | 2020-02-13 | 210.950 | 48.270  | <0.1    | |             | 03:49:52   | 03:42:32   |         | |         | | -----       | -----      | -----      | -----   | -----   | -----   | | TCH         | 2020-02-09 | 2020-02-11 | 61.953  | -29.050 | <0.1    | |             | 00:26:26   | 03:46:32   |         | |         | | TCH         | 2020-02-09 | 2020-02-11 | 52.108  | -16.323 | <0.1    | |             | 00:33:13   | 03:53:19   |         | |         | | TCH         | 2020-02-09 | 2020-02-11 | 79.626  | -39.959 | <0.1    | |             | 02:23:45   | 07:33:16   |         | |         | | TCH         | 2020-02-09 | 2020-02-11 | 64.380  | -31.818 | <0.1    | |             | 02:30:31   | 05:30:11   |         | |         | | TCH         | 2020-02-09 | 2020-02-11 | 53.339  | -13.161 | <0.1    | |             | 02:37:16   | 03:27:16   |         | |         | | TCH         | 2020-02-09 | 2020-02-11 | 135.000 | -49.050 | <0.1    | |             | 02:49:40   | 05:49:42   |         | |         | | TCH         | 2020-02-09 | 2020-02-11 | 139.902 | -36.323 | 11.2    | |             | 04:02:01   | 08:51:13   |         | |         | | TCH         | 2020-02-09 | 2020-02-11 | 139.525 | -34.505 | 25.6    | |             | 04:08:40   | 08:57:58   |         | |         | | TCH         | 2020-02-09 | 2020-02-11 | 140.305 | -38.141 | 2.1     | |             | 04:15:24   | 04:45:05   |         | |         | | TCH         | 2020-02-09 | 2020-02-11 | 108.615 | -45.889 | <0.1    | |             | 04:27:49   | 09:17:07   |         | |         | | TCH         | 2020-02-09 | 2020-02-11 | 103.112 | -49.050 | <0.1    | |             | 04:34:35   | 09:23:51   |         | |         | | TCH         | 2020-02-09 | 2020-02-11 | 140.372 | -30.000 | 2.1     | |             | 04:41:20   | 05:11:01   |         | |         | | TCH         | 2020-02-09 | 2020-02-11 | 82.010  | -39.959 | <0.1    | |             | 05:13:14   | 05:42:55   |         | |         | | TCH         | 2020-02-09 | 2020-02-09 | 194.213 | 18.223  | <0.1    | |             | 08:20:13   | 08:22:13   |         | |         | | TCH         | 2020-02-09 | 2020-02-09 | 197.314 | 29.132  | <0.1    | |             | 08:35:17   | 08:41:36   |         | |         | | TCH         | 2020-02-09 | 2020-02-11 | 81.191  | -33.636 | <0.1    | |             | 08:45:08   | 00:57:58   |         | |         | | TCH         | 2020-02-10 | 2020-02-11 | 138.291 | -30.000 | 3.6     | |             | 02:49:30   | 09:10:20   |         | |         | | TCH         | 2020-02-10 | 2020-02-10 | 195.950 | 16.405  | <0.1    | |             | 08:25:51   | 08:32:09   |         | |         | | TCH         | 2020-02-10 | 2020-02-10 | 201.359 | 25.495  | <0.1    | |             | 08:46:04   | 08:52:23   |         | |         | | -----       | -----      | -----      | -----   | -----   | -----   | | TRE         | 2020-02-09 | 2020-02-09 | 136.216 | -32.727 | 21.6    | |             | 16:00:09   | 22:29:52   |         | |         | | TRE         | 2020-02-09 | 2020-02-09 | 107.368 | -49.091 | <0.1    | |             | 16:13:27   | 22:42:24   |         | |         | | TRE         | 2020-02-09 | 2020-02-09 | 82.286  | -36.818 | <0.1    | |             | 16:25:46   | 16:32:09   |         | |         | | TRE         | 2020-02-09 | 2020-02-09 | 63.000  | -24.545 | <0.1    | |             | 16:38:59   | 16:45:22   |         | |         | | TRE         | 2020-02-09 | 2020-02-09 | 68.108  | -32.727 | <0.1    | |             | 16:57:40   | 20:15:31   |         | |         | | TRE         | 2020-02-09 | 2020-02-09 | 136.364 | -40.909 | 0.1     | |             | 17:23:24   | 23:53:02   |         | |         | | TRE         | 2020-02-09 | 2020-02-09 | 67.500  | -24.545 | <0.1    | |             | 17:42:21   | 17:48:38   |         | |         | | TRE         | 2020-02-09 | 2020-02-09 | 77.838  | -32.727 | <0.1    | |             | 17:55:32   | 18:01:55   |         | |         | | TRE         | 2020-02-09 | 2020-02-10 | 133.548 | -45.000 | <0.1    | |             | 18:27:28   | 00:56:21   |         | |         | | TRE         | 2020-02-09 | 2020-02-09 | 72.000  | -36.818 | <0.1    | |             | 18:39:51   | 18:46:14   |         | |         | | TRE         | 2020-02-09 | 2020-02-09 | 141.081 | -32.727 | 47.9    | |             | 18:53:07   | 22:11:00   |         | |         | | TRE         | 2020-02-09 | 2020-02-09 | 141.818 | -40.909 | 0.4     | |             | 19:05:20   | 19:11:37   |         | |         | | TRE         | 2020-02-09 | 2020-02-09 | 65.455  | -28.636 | <0.1    | |             | 19:22:57   | 19:24:57   |         | |         | | TRE         | 2020-02-09 | 2020-02-09 | 77.143  | -36.818 | <0.1    | |             | 19:33:06   | 19:37:15   |         | |         | | TRE         | 2020-02-09 | 2020-02-09 | 104.516 | -45.000 | <0.1    | |             | 19:44:04   | 23:01:34   |         | |         | | TRE         | 2020-02-09 | 2020-02-09 | 70.130  | -28.636 | <0.1    | |             | 19:56:26   | 20:02:43   |         | |         | | TRE         | 2020-02-09 | 2020-02-09 | 198.000 | 24.545  | <0.1    | |             | 20:22:25   | 23:39:48   |         | |         | | TRE         | 2020-02-09 | 2020-02-10 | 201.039 | 28.636  | <0.1    | |             | 21:13:01   | 00:30:48   |         | |         | | TRE         | 2020-02-09 | 2020-02-09 | 205.714 | 36.818  | <0.1    | |             | 23:14:19   | 23:20:37   |         | |         | | TRE         | 2020-02-09 | 2020-02-10 | 197.561 | 20.455  | <0.1    | |             | 23:58:59   | 00:05:17   |         | |         | | TRE         | 2020-02-10 | 2020-02-10 | 138.857 | -36.818 | 26.0    | |             | 01:09:08   | 01:15:25   |         | |         | +-------------+------------+------------+---------+---------+---------+ 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. These observations cover about 95.1% of the cumulative probability of the LALInference skymap created on 2020-02-10 21:14:05 (UTC). The coverage map is available at: https://grandma- owncloud.lal.in2p3.fr/index.php/s/XgtMhPRxcyL09gR/download?path=%2F&files=GRANDMA_S200208q_1581583078.svg No significant transient candidates were found during our low latency analysis [2,3]. GRANDMA (Global Rapid Advanced Network Devoted to the Multi-messenger Addicts) is a network of robotic telescopes connected all over the world with both photometry and spectrometry capabilities for Time- domain Astronomy [2](https://grandma.lal.in2p3.fr/). Details on the different telescopes are available on the GRANDMA web pages. [1] M. W Coughlin et al., MNRAS 2019, https://doi.org/10.1093/mnras/stz2485 [2] S. Antier et al., MNRAS 2019, https://doi.org/10.1093/mnras/stz3142 [3] K. Noysena et al., ApJ 2019, arXiv:1910.02770 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27223 SUBJECT: LIGO/Virgo S200208q: Upper limits from Konus-Wind observations DATE: 20/02/26 14:58:08 GMT FROM: Anna Ridnaia at Ioffe Institute A. Ridnaia, S. Golenetskii, R.Aptekar, D. Frederiks, M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline, on behalf of the Konus-Wind team, report: Konus-Wind (KW) was observing the whole sky at the time of the LIGO/Virgo event S200208q (2020-02-08 13:01:17.991 UTC, hereafter T0; LIGO/Virgo Collaboration GCN Circ. 27014). No triggered KW GRBs happened between ~1.5 days before and ~2 days after T0. Using waiting-mode data within the interval T0 +/- 100 s, we found no significant (> 5 sigma) excess over the background in both KW detectors on temporal scales from 2.944 s to 100 s. We estimate an upper limit (90% conf.) on the 20 - 1500 keV fluence to 8.9x10^-7 erg/cm^2 for a burst lasting less than 2.944 s and having a typical KW short GRB spectrum (an exponentially cut off power law with alpha =-0.5 and Ep=500 keV). For a typical long GRB spectrum (the Band function with alpha=-1, beta=-2.5, and Ep=300 keV), the corresponding limiting peak flux is 2.3x10^-7 erg/cm^2/s (20 - 1500 keV, 2.944 s scale). All the quoted values are preliminary.