//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27277 SUBJECT: LIGO/Virgo S200302c: Global MASTER-Net observations report DATE: 20/03/02 02:08:16 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-Kislovodsk robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the LIGO/Virgo S200302c errorbox 2 sec after notice time and 208 sec after trigger time at 2020-03-02 02:01:39 UT, with upper limit up to 17.5 mag. The observations began at zenith distance = 71 deg. The sun altitude is -19.7 deg. The galactic latitude b = -3 deg., longitude l = 317 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/ligo_1.php?id=11407 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 228 | 2020-03-02 02:01:39 | MASTER-Kislovodsk | (22h 50m 53.42s , +46d 08m 51.7s) | C | 40 | 17.5 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27278 SUBJECT: LIGO/Virgo S200302c: Identification of a GW compact binary merger candidate DATE: 20/03/02 02:20:13 GMT FROM: Peter Shawhan at U of Maryland/LSC The LIGO Scientific Collaboration and the Virgo Collaboration report: We identified the compact binary merger candidate S200302c during real-time processing of data from LIGO Hanford Observatory (H1) and Virgo Observatory (V1) at 2020-03-02 01:58:11.519 UTC (GPS time: 1267149509.519). The candidate was found by the GstLAL [1] analysis pipeline. S200302c is an event of interest because its false alarm rate, as estimated by the online analysis, is 9.3e-09 Hz, or about one in 3 years. The event's properties can be found at this URL: https://gracedb.ligo.org/superevents/S200302c The classification of the GW signal, in order of descending probability, is BBH (89%), Terrestrial (11%), BNS (<1%), MassGap (<1%), or NSBH (<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 [2], distributed via GCN notice about a minute after the candidate event time. * bayestar.fits.gz,1, distributed via GCN notice about 7 minutes after the candidate event time. (This is identical to bayestar.fits.gz,0 ) 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 6704 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1737 +/- 500 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] Messick et al. PRD 95, 042001 (2017) [2] Singer & Price PRD 93, 024013 (2016) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27279 SUBJECT: LIGO/Virgo S200302c: Upper limits from IceCube neutrino searches DATE: 20/03/02 02:23:37 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 S200302c in a time range of 1000 seconds [3] centered on the alert event time (2020-03-02 01:49:51.519 UTC to 2020-03-02 02:06:31.519 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 S200302c calculated from the map circulated in the 2-Preliminary notice. IceCube's sensitivity assuming an E^-2 spectrum (E^2 dN/dE) to neutrino point sources within the locations spanned by the 90% spatial containment of S200302c ranges from 0.029 to 0.954 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: 27280 SUBJECT: LIGO/Virgo S200302c: Coverage and upper limits from MAXI/GSC observations DATE: 20/03/02 04:01:12 GMT FROM: Satoshi Sugita at Aoyama Gakuin U. N. Kawai (Tokyo Tech), H. Negoro (Nihon U.), 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 S200302c at 2020-03-02 01:58:11.519 UTC (GCN 27278). At the trigger time of S200302c, the high-voltage of MAXI/GSC was off, and it was turned on at T0+557 sec (+9.3 min). The first one-orbit (92 min) scan observation with GSC after the event covered 57% of the 90% credible region of the bayestar skymap from 02:07:28 to 03:24:53 UTC (T0+557 to T0+5202 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: 27283 SUBJECT: LIGO/Virgo S200302c: upper limits from AGILE/MCAL observations DATE: 20/03/02 07:05:51 GMT FROM: Maura Pillia at INAF M. Pilia (INAF/OA-Cagliari), F. Longo (Univ. Trieste, and INFN Trieste), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, 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), report on behalf of the AGILE Team: In response to the LIGO/Virgo GW event S200302c at T0 = 2020-03-02 01:58:11.519 (UT), a preliminary analysis of the AGILE minicalorimeter (MCAL) triggered data found no event candidates within a time interval covering -/+ 15 sec from the LIGO/Virgo T0. At the T0, about 65% of the S200302c 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 S200302c localization region, from a minimum of 1.3E-06 erg cm^-2 to a maximum of 7.1E-06 erg cm^-2 (assuming as spectral model a single power-law with photon index 1.5). An independent procedure based on photon counting statistics provides UL fluences in the range 0.4-1 MeV, for a 300 us integration time, from a minimum of 1.0E-08 erg cm^-2 to a maximum of 4.4E-08 erg cm^-2. 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: 27284 SUBJECT: LIGO/Virgo S200302c : no neutrino counterpart candidate in ANTARES search DATE: 20/03/02 07:45:26 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 S200302c event using the 90% contour of the Initial GW_SKYMAP probability map provided by the GW interferometers (GCN#27278). 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/S200302c_Initial.png . Considering the location probability provided by the LIGO/Virgo collaborations, there is a 49.5% 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 2020-03-02 01:58:11 and in the 90% contour of the S200302c event. The expected number of atmospheric background events in the region visible by ANTARES is 2.84e-03 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 2.05e-02 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: 27285 SUBJECT: LIGO/Virgo S200302c: No counterpart candidates in INTEGRAL SPI-ACS and IBIS prompt observation DATE: 20/03/02 09:28:09 GMT FROM: Alexis Coleiro at APC/U. Paris Diderot Alexis Coleiro (APC, France), Maeve Doyle (UCD, Ireland), V. Savchenko, C. Ferrigno (ISDC/UniGE, Switzerland), J. Rodi (IAPS-Roma, Italy) S. Mereghetti (INAF IASF-Milano, Italy) on behalf of the INTEGRAL multi-messenger collaboration: https://www.astro.unige.ch/cdci/integral-multimessenger-collaboration Using combination of INTEGRAL all-sky detectors (following [1]): SPI/ACS, IBIS/Veto, and IBIS we have performed a search for a prompt gamma-ray counterpart of S200302c (GCN 27278). At the time of the event (2020-03-02 01:58:11 UTC, hereafter T0), INTEGRAL was operating in nominal mode. The peak of the event localization probability was at an angle of 42 deg with respect to the spacecraft pointing axis. This orientation implies strongly suppressed (19% of optimal) response of ISGRI, strongly suppressed (39% of optimal) response of IBIS/Veto, and near-optimal (78% of optimal) response of SPI-ACS. 6.6% of the gravitational-wave localization was within the IBIS field-of-view at the trigger time. 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]), IBIS, and IBIS/Veto data. We do not detect any significant counterparts and estimate a 3-sigma upper limit on the 75-2000 keV fluence of 3.2e-07 erg/cm^2 (within the 50% probability containment region of the source localization) for a burst lasting less than 1 s with a characteristic short GRB spectrum (an exponentially cut off power law with alpha=-0.5 and Ep=600 keV) occurring at any time in the interval within 300 s around T0. For a typical long GRB spectrum (Band function with alpha=-1, beta=-2.5, and Ep=300 keV), the derived peak flux upper limit is ~2.8e-07 (1.8e-08) erg/cm^2/s at 1 s (8 s) time scale in 75-2000 keV energy range. For the mean reported distance of 1737.0 Mpc, this corresponds to a limit on the total isotropic equivalent energy in 1 s of 1.2e+50 erg for the short GRB spectrum and for a long GRB spectrum isotropic equivalent luminosity in 1 s (8 s) of 2e+49 erg/s (6.7e+48 erg/s) We report for completeness and in order of FAP, all excesses identified in the search region. We find: 1 possibly associated excess: T-T0 | scale | S/N | luminosity ( x 1e+50 erg/s) | FAP -31.9 | 8.75 | 3.5 | 5.86 +/- 2.59 +/- 5.07 | 0.0264 5 likely background excesses: T-T0 | scale | S/N | luminosity ( x 1e+50 erg/s) | FAP 9.25 | 0.8 | 3.4 | 20.7 +/- 8.6 +/- 17.9 | 0.0935 -170 | 1.4 | 4.8 | 22 +/- 6.5 +/- 19 | 0.21 220 | 0.9 | 4.1 | 23.5 +/- 8.11 +/- 20.3 | 0.707 120 | 0.55 | 3.9 | 2.84 +/- 1.04 +/- 2.46 | 0.833 -73 | 0.55 | 3.5 | 2.61 +/- 1.04 +/- 2.26 | 0.86 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: 27286 SUBJECT: LIGO/Virgo S200302c: Upper limits from Fermi-GBM Observations DATE: 20/03/02 15:25:48 GMT FROM: Colleen A. Wilson at NASA/MSFC/NSSTC For S200302c and using the initial bayestar.fits.gz skymap, Fermi-GBM was observing 71.1% 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 S200302c (GCN 27278). 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=288.0, Dec=1.6 with a radius of 67.2 degrees. We therefore set upper limits on impulsive gamma-ray emission for the LVC localization region visible to Fermi at merger time. Using the representative soft, normal, and hard GRB-like templates described in arXiv:1612.02395, we set the following 3 sigma flux upper limits over 10-1000 keV, weighted by GW localization probability (in units of 10^-7 erg/s/cm^2): Timescale Soft Normal Hard ------------------------------------ 0.128 s: 3.9 6.1 12 1.024 s: 1.4 2.0 3.7 8.192 s: 0.40 0.73 1.8 Assuming the median luminosity distance of 1737.4 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 ------------------------------------ 0.128 s: 2.2 3.1 10 1.024 s: 0.79 1.0 3.1 8.192 s: 0.23 0.37 1.5 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27287 SUBJECT: LIGO/Virgo S200302c: No counterpart candidates in HAWC observations DATE: 20/03/02 15:39:53 GMT FROM: Israel Martinez-Castellanos at UMD/HAWC The HAWC Collaboration (https://www.hawc-observatory.org) reports: The HAWC Collaboration performed a follow-up of the gravitational wave trigger S200302c (GCN #27278). At the time of the trigger the HAWC local zenith was oriented towards (RA, Dec) = (92.3 deg, 19.0 deg). 31% of the GW candidate sky location probability fell within our observable field of view (0-45 deg zenith angle). We performed a search for a short timescale emission using 6 sliding time windows (dt = 0.3s, 1s, 3s, 10s, 30s and 100s), shifted forward in time by 20% of their width. We searched the 95% probability containment area in a timescale-dependent time period, from t0-5dt to t0+10dt, where t0 is the time of the GW trigger. No significant gamma-ray detection above the background was observed. The sensitivity of this analysis is greatly dependent on zenith angle, ranging from 0 deg to 45 deg for the area searched in this analysis. The 5sigma detection sensitivity to a 1s (100s) burst in the 80-800GeV energy range goes from 1.2e-6 erg/cm^2 to 1.1e-4 erg/cm^2 (6.4e-6 erg/cm^2 to 5.0e-4 erg/cm^2), depending on the zenith angle. HAWC is a TeV gamma ray water Cherenkov array located in the state of Puebla, Mexico. It is sensitive to the energy range ~0.1-100TeV, and monitors 2/3 of the sky every day with an instantaneous field-of-view of ~2 sr. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27289 SUBJECT: LIGO/Virgo S200302c: no counterpart candidates in the Swift/BAT observations DATE: 20/03/02 22:53:03 GMT FROM: Amy Lien at GSFC T. Sakamoto (AGU), S. D. Barthelmy (NASA/GSFC), A. Y. Lien (GSFC/UMBC), D. M. Palmer (LANL) A. P. Beardmore (U. Leicester), M. G. Bernardini (INAF-OAB), A. A. Breeveld (MSSL-UCL), D. N. Burrows (PSU), S. Campana (INAF-OAB), S. B. Cenko (NASA/GSFC), G. Cusumano (INAF-IASF PA), A. D'Ai (INAF-IASFPA), P. D'Avanzo (INAF-OAB), V. D'Elia (ASI-ASDC), S. Emery (UCL-MSSL), P. A. Evans (U. Leicester), P. Giommi (ASI), C. Gronwall (PSU), D. Hartmann (Clemson U.), J. A. Kennea (PSU), N. Klingler (PSU), H. A. Krimm (NSF), N. P. M. Kuin (UCL-MSSL), F. E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB), J. A. Nousek (PSU), S. R. Oates (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 S200302c (LIGO/VIRGO Collaboration GCN Circ. 27278), where T0 is the LVC trigger time (2020-03-02T01:58:11.519 UTC). The center of the BAT field of view (FOV) at T0 is RA = 10.655 deg, DEC = 41.334 deg, and the roll angle is 223.231 deg. The BAT FOV (>10% partial coding) covers 24.48% of the integrated LVC localization probability, and 24.02% 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 astrophysical 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. The ~5.9 sigma detection seen at ~T-17.8 s in the 64 ms light curve is likely due to cosmic ray shower. Assuming a 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 ~ 6.99 x 10^-8 erg/s/cm^2 for the 100% coded region (i.e., for a burst with 0 deg from BAT boresight) and ~ 1.47 x 10^-6 erg/s/cm2 for the 10% coded region (~56 deg from BAT boresight). 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), these flux upper limits corresponds to a distance of ~ 85.94 Mpc (100% coded)and ~ 18.73 Mpc (10% coded). Event data are available from T0-45.142 s to T0+44.9692 s via the GUANO system (Tohuvavohu et al. 2020, in prep). 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 the whole event data range. BAT retains decreased, but significant, sensitivity to rate increases for gamma-ray events outside of its FOV. About 52.88% 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/S200302c/web/source_public.html //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27290 SUBJECT: LIGO/Virgo S200302c: No counterpart candidates in KAIT observations DATE: 20/03/02 23:15:05 GMT FROM: Weikang Zheng at UC Berkeley Keto D. Zhang, Shaunak Modak, Sergiy Vasylyev, Benjamin E. Stahl, 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 S200302c (GCN 27278) 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 101 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 03:39:07, Mar. 02nd UT, about 1.7 hours after the trigger, and the last image at 06:25:13 UT. Our typical limiting mag is 18.5. No viable counterparts were identified and the analysis is ongoing. A full list of galaxies observed by KAIT is given below. GladeID UT(Mar02) RA_J2000 Dec_J2000 ----------------------------------------------- G0977981 03:39:07 08:46:23.2178 -15:45:38.7936 G0628480 03:40:16 08:46:48.5376 -14:47:52.8288 G0756544 03:41:28 08:47:08.1554 -12:29:37.7124 G1109681 03:42:39 08:52:48.8414 -23:15:28.962 G0729469 03:43:48 08:54:05.9693 -19:17:53.2536 G0758017 03:44:58 08:54:20.951 -16:14:14.406 G0610914 03:46:09 09:01:41.6309 -23:55:46.3476 G0648481 03:47:20 09:02:49.2847 -15:38:00.6468 G0769731 03:48:32 09:03:42.583 -21:53:39.8328 G0756540 03:49:43 09:04:48.4387 -17:00:48.402 G1264339 03:50:53 09:07:44.6374 -22:32:42.2412 G0490601 04:15:53 07:41:32.1624 +51:41:17.952 G1052741 04:17:27 07:45:28.4546 -21:59:55.4136 G1161155 04:18:36 07:49:28.493 -16:55:01.974 G1210259 04:19:46 07:51:22.1887 -19:17:28.266 G0574475 04:20:59 07:53:14.4965 -03:35:56.958 G0790912 04:22:08 07:54:16.573 -03:54:54.2916 G1202125 04:23:22 07:54:22.6044 -21:33:18 G0799865 04:24:35 07:54:48.415 -04:27:08.0424 G1344201 04:25:46 07:56:44.4067 -10:46:32.502 G1114070 04:27:00 07:56:44.7912 -16:23:08.3616 G1023494 04:28:10 07:57:02.1624 -11:59:53.4228 G0829552 04:29:20 07:57:13.0114 -11:09:51.7428 G1441820 04:30:31 07:57:13.4179 -05:20:47.0904 G1390582 04:31:40 07:57:13.927 -08:55:08.7456 G1313908 04:32:52 07:58:00.6317 -14:14:11.2452 G1378903 04:33:59 07:58:02.9059 -14:47:50.244 G0592514 04:35:11 07:58:41.801 -06:03:36.1764 G1299638 04:36:20 07:59:07.4158 -10:21:53.3088 G1379691 04:37:29 07:59:15.3698 -12:04:31.5768 G1293714 04:38:38 07:59:20.6287 -10:26:41.352 G0727439 04:39:48 08:00:07.5055 -07:39:54.2052 G1399423 04:40:59 08:00:13.9068 -12:22:42.5064 G0985954 04:42:09 08:00:25.4407 -13:56:12.5556 G0953501 04:43:20 08:00:34.2662 -08:56:27.924 G1309230 04:44:29 08:01:02.4922 -12:47:27.5028 G0648186 04:45:41 08:01:20.1746 -02:21:50.13 G0636265 04:46:52 08:01:22.2821 -09:11:00.7476 G1296421 04:48:00 08:01:34.8816 -10:10:59.3436 G1147199 04:49:09 08:01:35.9875 -12:57:11.7792 G1231402 04:50:19 08:01:41.1199 -09:56:08.3652 G1403493 05:02:24 08:02:33.6254 -09:16:24.4776 G0606950 05:03:34 08:02:34.3615 -07:04:36.48 G1069958 05:04:45 08:02:37.6831 -16:13:17.022 G1181634 05:05:56 08:02:39.4958 -09:41:58.488 G0619911 05:07:06 08:02:39.6276 -09:51:31.4892 G1293495 05:08:15 08:02:49.7167 -13:31:23.1168 G1189118 05:09:24 08:02:50.7953 -09:57:18.486 G0681918 05:10:37 08:02:53.9758 -01:23:28.2192 G0264755 05:11:48 08:03:04.1218 -09:55:16.7376 G1217193 05:12:57 08:03:09.4812 -03:49:38.46 G1412002 05:14:09 08:03:13.2641 -09:36:00.7596 G0572915 05:15:18 08:03:17.4902 -05:34:07.464 G0682527 05:16:28 08:03:29.3078 -09:14:44.0772 G0236099 05:17:37 08:03:36.059 -09:21:49.0932 G1090217 05:18:46 08:03:42.4183 -14:58:53.9436 G0815853 05:19:57 08:03:42.8578 -03:52:35.9256 G0621743 05:21:07 08:03:51.7366 -01:14:46.9392 G1159686 05:22:18 08:04:19.7736 -04:10:13.6848 G1191210 05:23:29 08:04:25.7702 -10:48:49.4928 G0809742 05:24:41 08:04:52.9999 -01:08:47.6268 G1047594 05:25:52 08:04:59.707 -07:43:02.7084 G1010785 05:27:02 08:05:10.7189 -09:39:00.7236 G1197882 05:28:13 08:05:44.729 -03:31:11.4672 G1326803 05:29:24 08:06:39.9281 -13:12:56.7072 G1304457 05:30:38 08:06:46.3954 +00:48:57.9888 G1455092 05:31:50 08:06:49.3358 -04:28:10.9164 G1001544 05:33:04 08:06:51.4874 -15:29:22.7652 G1387447 05:34:13 08:06:52.2089 -12:49:44.7708 G0874860 05:35:22 08:07:51.385 -10:46:50.826 G1474742 05:36:32 08:08:32.3146 -13:46:23.8044 G0835746 05:51:17 08:08:49.5391 -15:42:41.2272 G0595489 05:52:30 08:08:52.5091 +01:37:45.2064 G0692051 05:53:41 08:08:53.6004 -10:27:39.708 G1401743 05:54:51 08:09:02.5507 -15:02:50.244 G1409823 05:56:02 08:09:05.7751 -09:44:55.7664 G0966575 05:57:12 08:09:07.8132 -09:35:56.7708 G1346118 05:58:21 08:09:26.5997 -09:37:51.2328 G0619099 05:59:30 08:10:54.3218 -06:35:52.3428 G0997722 06:00:40 08:10:55.2778 -07:49:32.3436 G0236534 06:01:51 08:13:44.8553 -15:52:59.2392 G1312536 06:03:00 08:16:29.1888 -11:12:04.554 G1219145 06:04:12 08:17:04.0538 -21:12:53.604 G1432830 06:05:23 08:17:07.2473 -16:00:48.654 G0246154 06:06:32 08:22:42.8832 -19:28:28.4556 G0801490 06:07:42 08:22:57.8906 -17:55:04.5012 G0828812 06:08:51 08:25:11.6254 -18:39:18.2556 G1462815 06:10:00 08:25:39.6442 -20:53:06.9432 G1143512 06:11:09 08:28:54.6074 -17:13:33.312 G1145838 06:12:19 08:29:50.7403 -20:50:18.9888 G1127333 06:13:28 08:31:12.1858 -16:45:44.0208 G1073158 06:14:38 08:31:56.6914 -16:55:54.0624 G1301619 06:15:49 08:34:53.7672 -24:23:56.3604 G0578988 06:17:02 08:36:04.4458 -19:26:35.0556 G0887576 06:18:12 08:36:10.1734 -19:23:19.0608 G1323437 06:19:21 08:36:16.2487 -23:46:56.064 G0058197 06:20:33 08:37:15.2784 -19:11:02.7168 G0546315 06:21:42 08:37:32.3657 -14:59:04.7616 G0953131 06:22:52 08:39:04.8377 -14:54:29.4696 G0981974 06:24:03 08:40:09.287 -17:08:07.0044 G1250613 06:25:13 08:40:15.3734 -18:21:33.0984 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27291 SUBJECT: LIGO/Virgo S200302c: No significant counterpart candidates in Fermi-LAT observations DATE: 20/03/03 01:38:51 GMT FROM: Makoto Arimoto at Tokyo Inst of Tech N. Di Lalla (Stanford Univ.), F. Longo (University and INFN, Trieste), D. Kocevski (NASA/MSFC), N. Omodei (Stanford Univ.), M. Arimoto (Kanazawa Univ.), A. Berretta (University & INFN Perugia), M. Crnogorcevic (Univ. of Maryland & NASA/GSFC), M. Axelsson (KTH & Stockholm Univ) and E. Bissaldi (Politecnico & INFN Bari) report on behalf of the Fermi-LAT Collaboration: We have searched data collected by the Fermi Large Area Telescope (LAT) on March 2, 2020, for possible high-energy (E > 100 MeV) gamma-ray emission in spatial/temporal coincidence with the LIGO/Virgo trigger S200302c (GCN 27278). 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 ~23% of the LIGO probability at the time of the trigger (T0 = 2020-03-02 01:58:11.519 UTC), and reached 100% cumulative coverage after ~5 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. A marginally significant excess (with a soft spectrum) was found at the location RA, Dec 63.3, Dec = 18.8 (degrees, J2000) with an error radius of 1.0 deg (90% containment, statistical error only). We also performed a search which adapted the time interval of the analysis to the exposure of each region of the sky, and no additional excesses were found. Energy flux upper bounds for the fixed time interval between 100 MeV and 1 GeV for this search vary between 1.1e-10 and 1.1e-09 [erg/cm^2/s]. The Fermi-LAT point of contact for this event is Makoto Arimoto (arimoto@se.kanazawa-u.ac.jp). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27292 SUBJECT: LIGO/Virgo S200302c: Updated Sky Localization DATE: 20/03/03 01:52:46 GMT FROM: Peter Shawhan at U of Maryland/LSC The LIGO Scientific Collaboration and the Virgo Collaboration report: We have conducted further analysis of the LIGO Hanford Observatory (H1) and Virgo Observatory (V1) data around the time of the compact binary merger (CBC) candidate S200302c (GCN Circular 27278). 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/S200302c 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 5656 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1820 +/- 536 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: 27299 SUBJECT: LIGO/Virgo S200302c: No transient candidates in CALET observations DATE: 20/03/03 06:34:52 GMT FROM: Yuta Kawakubo at Louisiana State U./CALET S. Nakahira (RIKEN), A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU), Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), Y. Asaoka, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), N. Cannady (GSFC/UMBC), M. L. Cherry (LSU), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena), and the CALET collaboration: The CALET Gamma-ray Burst Monitor (CGBM) was operating at the trigger time of S200302c T0 = 2020-03-02 01:58:11.519 UT (The LIGO Scientific Collaboration and Virgo Collaboration, GCN Circ. 27278). No CGBM on-board trigger occurred around the event time. Based on the LVC high probability localization region, the summed LIGO probabilities inside the CGBM HXM (7 - 3000 keV) and SGM (40 keV - 28 MeV) fields of view are 23 % and 54 %, respectively (and 81 % credible region of the updated localization map was above the horizon). The HXM and SGM fields of view were centered at RA = 243.2 deg, Dec = +61.5 deg and RA = 245.4 deg, Dec = +51.6 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 (signal-to-noise ratio >= 7) 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 S200302c. 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 = 245.4 deg, Dec = +51.6 deg at T0. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27310 SUBJECT: LIGO/Virgo S200302c: Upper limits from Insight-HXMT/HE observations DATE: 20/03/03 16:44:50 GMT FROM: Qi Luo at IHEP Q. Luo, Y. G. Zheng, C. Cai, S. Xiao, Q. B. Yi, Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong, C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, M. Wu, Y. P. Xu, S. N. Zhang (IHEP), report on behalf of the Insight-HXMT team: Insight-HXMT was taking data normally around the reported LIGO/Virgo S200302c event (GCN #27278). At the GW trigger time 2020-03-02T01:58:21.38 UTC (denoted as T0), about 55.0% of the GW localization region was covered by the 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=40.1 deg, DEC=70.0 deg) without occultation by the Earth, 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: 3.2e-07 erg cm^-2 10 s: 1.4e-06 erg cm^-2 Band model 2 (alpha=-1.0, beta=-2.3, Ep=230 keV): 1 s: 4.5e-07 erg cm^-2 10 s: 1.6e-06 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: 1.7e-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. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27315 SUBJECT: LIGO/Virgo S200302c: AstroSat CZTI upper limits DATE: 20/03/04 17:13:39 GMT FROM: Varun Bhalerao at Indian Inst of Tech V. Shenoy (IITB), Aarthy E. (PRL), V. Bhalerao (IITB), D. Bhattacharya (IUCAA), A. R. Rao (TIFR), S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration: We have carried a search for X-ray candidates in Astrosat CZTI data in a 100 sec window around the trigger time of the BBH Merger event S200302c (UTC 2020-03-02 01:58:11, GraceDB event). We use the LALInference.fits.gz,0 map (https://gracedb.ligo.org/api/superevents/S200302c/files/LALInference.fits.gz,0) for our analysis. CZTI is a coded aperture mask instrument that has considerable effective area for about 29% of the entire sky, but is also sensitive to brighter transients from the entire sky. At the time of the merger, Astrosat's nominal pointing is RA,DEC = 17:29:19.1, -36:43:40.5 (262.3296,-36.7279), which is ~29 deg away from the maximum probability location. At the time of the merger event, the Earth-satellite-transient angle corresponding to maximum probability location is ~74 deg and hence is not occulted by Earth in satellite's frame. In a time interval of 100 sec around the event, the region of the localisation map which is not occulted by Earth in the satellite's frame has a cumulative probability of 0.79 (79%). CZTI data were de-trended to remove orbit-wise background variation. We then searched data from the four independent, identical quadrants to look for coincident spikes in the count rates. Searches were undertaken by binning the data in 0.1s, 1s, and 10s respectively. Statistical fluctuations in background count rates were estimated by using data from 10 (+-5) neighbouring orbits. We selected confidence levels such that the probability of a false trigger in a 1000 sec window is 10^-4. We do not find any evidence for any hard X-ray transient in this window, in the CZTI energy range of 20-200 keV. We use a detailed mass model of the satellite to calculate the direction-dependent instrument response for points in the visible sky. We then assume the source is modelled as a power law with photon index alpha = -1, and convert our count rate upper limits to direction-dependent flux limits. We obtain the following upper limits for source flux in the 20-200 keV band by taking a probability weighted mean over the visible sky: 0.1 s: flux limit= 2.19e-05 ergs/cm^2/s; fluence limit = 2.19e-06 ergs/cm^2 1.0 s: flux limit= 6.45e-06 ergs/cm^2/s; fluence limit = 6.45e-06 ergs/cm^2 10.0 s: flux limit= 1.16e-06 ergs/cm^2/s; fluence limit = 1.16e-05 ergs/cm^2 CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27322 SUBJECT: LIGO/Virgo S200302c : No significant candidates in FRAM - TAROT - GRANDMA observations. DATE: 20/03/06 13:21:22 GMT FROM: Jean-Gregoire Ducoin at LAL J.-G. Ducoin (IJCLab), S. Beradze (Iliauni), N. Christensen (Artemis), X. Zhang (THU), M. Prouza (FZU), M. Boer (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), B. Gendre (OzGrav-UWA), P. Hello (IJCLab), D. A. Kann (HETH/IAA-CSIC), N. Kochiashvili (Iliauni), C. Lachaud (APC), N. Leroy (IJCLab), 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 S200302c event with the FRAM-Auger, TAROT-Calern (TCA), TAROT-Reunion (TRE) telescopes. FRAM-Auger is located at Pierre Auger Observatory. TCA is located at Calern site at the Cote d'Azur observatory. 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 | 60 | R | 1.0 x 1.0 | 18.0 (60s) | | TCA | 1051 | Clear | 1.9 x 1.9 | 18.0 (60s) | | TRE | 1016 | 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 | 2020-03-02 | 2020-03-02 | 225.799 | -62.757 | <0.1 | | | 02:57:54 | 03:02:21 | | | | | FRAM-Auger | 2020-03-02 | 2020-03-02 | 226.286 | -61.784 | <0.1 | | | 03:02:55 | 03:07:22 | | | | | FRAM-Auger | 2020-03-02 | 2020-03-02 | 244.873 | -57.892 | <0.1 | | | 03:08:01 | 03:12:28 | | | | | FRAM-Auger | 2020-03-02 | 2020-03-02 | 236.685 | -60.811 | <0.1 | | | 03:13:04 | 03:17:31 | | | | | FRAM-Auger | 2020-03-02 | 2020-03-02 | 230.718 | -60.811 | <0.1 | | | 03:18:07 | 03:22:34 | | | | | FRAM-Auger | 2020-03-02 | 2020-03-02 | 232.707 | -60.811 | <0.1 | | | 03:23:09 | 03:27:36 | | | | | FRAM-Auger | 2020-03-02 | 2020-03-02 | 230.400 | -61.784 | <0.1 | | | 03:28:10 | 03:32:37 | | | | | FRAM-Auger | 2020-03-02 | 2020-03-02 | 227.929 | -62.757 | <0.1 | | | 03:33:11 | 03:37:38 | | | | | FRAM-Auger | 2020-03-02 | 2020-03-02 | 218.057 | -61.784 | <0.1 | | | 03:38:15 | 03:42:42 | | | | | FRAM-Auger | 2020-03-02 | 2020-03-02 | 222.171 | -61.784 | <0.1 | | | 03:43:17 | 03:47:44 | | | | | FRAM-Auger | 2020-03-02 | 2020-03-02 | 223.669 | -62.757 | <0.1 | | | 03:48:18 | 03:52:45 | | | | | FRAM-Auger | 2020-03-02 | 2020-03-02 | 232.457 | -61.784 | <0.1 | | | 03:53:21 | 03:57:48 | | | | | FRAM-Auger | 2020-03-02 | 2020-03-02 | 216.000 | -61.784 | <0.1 | | | 03:58:25 | 04:02:52 | | | | | FRAM-Auger | 2020-03-02 | 2020-03-02 | 228.343 | -61.784 | <0.1 | | | 04:03:30 | 04:07:57 | | | | | FRAM-Auger | 2020-03-02 | 2020-03-02 | 220.114 | -61.784 | <0.1 | | | 04:08:33 | 04:13:00 | | | | | FRAM-Auger | 2020-03-02 | 2020-03-02 | 221.538 | -62.757 | <0.1 | | | 04:13:35 | 04:18:02 | | | | | FRAM-Auger | 2020-03-02 | 2020-03-02 | 224.229 | -61.784 | <0.1 | | | 04:18:38 | 04:23:05 | | | | | FRAM-Auger | 2020-03-02 | 2020-03-02 | 210.829 | -60.811 | <0.1 | | | 04:23:41 | 04:28:08 | | | | | FRAM-Auger | 2020-03-02 | 2020-03-02 | 214.807 | -60.811 | <0.1 | | | 04:42:19 | 04:46:46 | | | | | FRAM-Auger | 2020-03-02 | 2020-03-02 | 226.740 | -60.811 | <0.1 | | | 04:47:23 | 04:51:50 | | | | | ----- | ----- | ----- | ----- | ----- | ----- | | TCA | 2020-03-02 | 2020-03-03 | 53.891 | 70.538 | 0.2 | | | 19:28:46 | 01:40:32 | | | | | TCA | 2020-03-02 | 2020-03-05 | 39.869 | 68.682 | 0.3 | | | 19:35:33 | 01:33:59 | | | | | TCA | 2020-03-02 | 2020-03-02 | 64.193 | 68.682 | 0.2 | | | 19:42:18 | 23:22:54 | | | | | TCA | 2020-03-02 | 2020-03-05 | 25.274 | 68.682 | 0.3 | | | 19:54:40 | 02:19:03 | | | | | TCA | 2020-03-02 | 2020-03-03 | 59.185 | 70.538 | 0.2 | | | 20:01:28 | 01:07:47 | | | | | TCA | 2020-03-02 | 2020-03-03 | 59.328 | 68.682 | 0.2 | | | 20:08:12 | 01:14:32 | | | | | TCA | 2020-03-02 | 2020-03-03 | 72.950 | 64.971 | 0.2 | | | 20:20:40 | 01:26:58 | | | | | TCA | 2020-03-02 | 2020-03-05 | 35.004 | 68.682 | 0.3 | | | 20:27:28 | 01:46:16 | | | | | TCA | 2020-03-02 | 2020-03-02 | 64.748 | 66.826 | 0.2 | | | 20:53:25 | 23:29:41 | | | | | TCA | 2020-03-02 | 2020-03-02 | 69.304 | 66.826 | 0.2 | | | 21:00:07 | 23:36:25 | | | | | TCA | 2020-03-02 | 2020-03-05 | 69.058 | 68.682 | 0.3 | | | 21:12:31 | 00:42:01 | | | | | TCA | 2020-03-02 | 2020-03-05 | 19.178 | 66.826 | 0.2 | | | 21:19:19 | 01:08:00 | | | | | TCA | 2020-03-02 | 2020-03-05 | 30.139 | 68.682 | 0.3 | | | 21:58:44 | 01:59:53 | | | | | TCA | 2020-03-02 | 2020-03-04 | 48.597 | 70.538 | 0.3 | | | 22:05:33 | 19:36:42 | | | | | TCA | 2020-03-02 | 2020-03-05 | 54.464 | 68.682 | 0.3 | | | 22:12:17 | 02:12:11 | | | | | TCA | 2020-03-02 | 2020-03-04 | 44.734 | 68.682 | 0.3 | | | 22:31:28 | 18:18:55 | | | | | TCA | 2020-03-03 | 2020-03-05 | 38.009 | 70.538 | 0.3 | | | 02:01:10 | 02:25:45 | | | | | TCA | 2020-03-03 | 2020-03-04 | 43.303 | 70.538 | 0.3 | | | 02:27:02 | 18:44:56 | | | | | TCA | 2020-03-03 | 2020-03-04 | 73.923 | 68.682 | 0.3 | | | 02:53:00 | 20:02:39 | | | | | TCA | 2020-03-03 | 2020-03-04 | 82.975 | 66.826 | 0.3 | | | 02:59:43 | 22:18:50 | | | | | TCA | 2020-03-03 | 2020-03-05 | 78.418 | 66.826 | 0.3 | | | 03:25:45 | 00:54:22 | | | | | TCA | 2020-03-03 | 2020-03-04 | 91.939 | 63.115 | 0.2 | | | 03:44:54 | 03:37:08 | | | | | TCA | 2020-03-03 | 2020-03-05 | 23.735 | 66.826 | 0.2 | | | 03:57:27 | 01:27:10 | | | | | TCA | 2020-03-03 | 2020-03-05 | 85.656 | 64.971 | 0.3 | | | 05:15:18 | 00:35:18 | | | | | TCA | 2020-03-03 | 2020-03-05 | 49.599 | 68.682 | 0.3 | | | 18:39:13 | 01:53:08 | | | | | TCA | 2020-03-03 | 2020-03-05 | 14.621 | 66.826 | 0.2 | | | 20:22:59 | 01:20:18 | | | | | TCA | 2020-03-03 | 2020-03-05 | 32.715 | 70.538 | 0.3 | | | 20:48:51 | 01:01:11 | | | | | ----- | ----- | ----- | ----- | ----- | ----- | | TRE | 2020-03-02 | 2020-03-02 | 226.452 | -45.000 | 0.3 | | | 18:54:05 | 19:00:22 | | | | | TRE | 2020-03-02 | 2020-03-03 | 230.000 | -65.455 | 0.4 | | | 19:13:14 | 00:19:30 | | | | | TRE | 2020-03-02 | 2020-03-03 | 226.286 | -36.818 | 0.5 | | | 19:51:28 | 20:44:29 | | | | | TRE | 2020-03-02 | 2020-03-03 | 220.645 | -45.000 | 0.3 | | | 20:04:43 | 01:10:37 | | | | | TRE | 2020-03-02 | 2020-03-03 | 231.429 | -61.364 | 1.4 | | | 21:59:10 | 18:05:12 | | | | | TRE | 2020-03-02 | 2020-03-02 | 214.286 | -61.364 | 1.2 | | | 22:12:21 | 22:18:44 | | | | | TRE | 2020-03-02 | 2020-03-02 | 205.714 | -61.364 | 0.7 | | | 22:31:04 | 22:37:21 | | | | | TRE | 2020-03-02 | 2020-03-02 | 256.154 | -53.182 | 0.7 | | | 22:44:19 | 22:50:42 | | | | | TRE | 2020-03-02 | 2020-03-02 | 237.447 | -57.273 | 1.0 | | | 22:56:37 | 23:02:55 | | | | | TRE | 2020-03-02 | 2020-03-02 | 249.231 | -53.182 | 0.8 | | | 23:09:53 | 23:16:10 | | | | | TRE | 2020-03-02 | 2020-03-02 | 223.636 | -40.909 | 0.4 | | | 23:22:10 | 23:28:27 | | | | | TRE | 2020-03-02 | 2020-03-02 | 234.545 | -40.909 | 0.4 | | | 23:35:23 | 23:41:46 | | | | | TRE | 2020-03-02 | 2020-03-02 | 238.065 | -45.000 | 0.3 | | | 23:47:39 | 23:53:57 | | | | | TRE | 2020-03-03 | 2020-03-03 | 218.182 | -40.909 | 0.3 | | | 00:00:52 | 00:07:15 | | | | | TRE | 2020-03-03 | 2020-03-03 | 231.429 | -36.818 | 0.4 | | | 00:26:27 | 00:32:50 | | | | | TRE | 2020-03-03 | 2020-03-03 | 245.455 | -40.909 | 0.3 | | | 00:38:43 | 00:45:00 | | | | | TRE | 2020-03-03 | 2020-03-03 | 257.143 | -61.364 | 0.4 | | | 20:51:24 | 20:53:24 | | | | | TRE | 2020-03-03 | 2020-03-03 | 267.273 | -40.909 | 0.5 | | | 22:58:53 | 23:05:16 | | | | | TRE | 2020-03-03 | 2020-03-03 | 214.468 | -57.273 | 0.5 | | | 23:22:03 | 23:24:03 | | | | | TRE | 2020-03-03 | 2020-03-03 | 233.766 | -28.636 | 0.5 | | | 23:30:59 | 23:37:22 | | | | +-------------+------------+------------+---------+---------+---------+ 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 18.1% of the cumulative probability of the LALinference skymap created on 2020-03-02 19:23:46 (UTC). The coverage map is available at: https://grandma- owncloud.lal.in2p3.fr/index.php/s/XgtMhPRxcyL09gR/download?path=%2F&files=GRANDMA_S200302c_1583492088.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: 27330 SUBJECT: LIGO/Virgo S200302c: No notable candidates in GOTO imaging DATE: 20/03/07 00:13:26 GMT FROM: Kendall Ackley at Monash University Y.-L. Mong (1); K. Ackley (1); D. K. Galloway (1); D. Steeghs (2); V. Dhillon (3); P. O'Brien (4); G. Ramsay (5); D. Pollacco (2); E. Thrane (1); S. Poshyachinda (6); R. Kotak (7); L. Nuttall (8); E. Pall\'e (9); K. Ulaczyk (2); J. Lyman (2); R. Cutter (2); A. Levan (2); T. Marsh (2); R. West (2); E. Stanway (2); B. Gompertz (2); K. Wiersema (2); T. Killestein (2); A. Casey (1); M. Brown (1); B. Muller (1); M. Dyer (3); J. Mullaney (3); E. Daw (3); S. Littlefair (3); J. Maund (3); L. Makrygianni (3); U. Burhanudin (3); R. Starling (4); R. Eyles (4); S. Tooke (4); S. Aukkaravittayapun (6); U. Sawangwit (6); S. Awiphan (6); D. Mkrtichian (6); P. Irawati (6); S. Mattila (7); T. Heikkil\"a (7); E. Rol (1) We report on optical observations with the Gravitational-wave Optical Transient Observer prototype in response to S200302c (GCN #27278). Targeted observations started shortly after the preliminary event notification was received. These spanned 102 unique tile pointings containing 30.8% of the source location probability (based on the initial BAYESTAR skymap) and were acquired between 20:15 UT Mar 02 2020 and 20:35 UT Mar 04 2020 (starting 18.3 hours after the event trigger time 01:58 UT Mar 02 2020). No new transients that could be credibly associated with S200302c were detected. Each pointing spans 4.9x3.7 square degrees and consisted of 3x60s exposures in our L-band filter (400-700nm passband similar to g+r) with a median 5-sigma photometric depth equivalent to g=19.1 for an individual pointing. Limits are based on a photometric calibration against PS1 sources. Most pointings were observed multiple times, typically 2-3 times. Images are processed immediately after acquisition using the GOTOphoto pipeline. Difference imaging was performed on the median of each triplet of exposures using recent survey observations of the same pointings. Source candidates were initially filtered using a classifier and cross-matched against a variety of catalogs, including the MPC and PS1. Human candidate vetting was performed following data acquisition and automated classifier cuts. GOTO is operated at the La Palma observing facilities of the University of Warwick on behalf of a consortium including the University of Warwick, Monash University, Armagh Observatory, the University of Leicester, the University of Sheffield, the National Astronomical Research Institute of Thailand (NARIT), The University of Portsmouth, the University of Turku and the Instituto de Astrofisica de Canarias (IAC) (https://goto-observatory.org/) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 27486 SUBJECT: LIGO/Virgo S200302c: Upper limits from Konus-Wind observations DATE: 20/04/03 22:17:21 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 S200302c (2020-03-02 01:58:11.519 UTC, hereafter T0; LIGO/Virgo Collaboration GCN Circ. 27278). No triggered KW GRBs happened between ~18 hours before and ~1 day 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 8.5x10^-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 2.5x10^-7 erg/cm^2/s (20 - 1500 keV, 2.944 s scale). All the quoted values are preliminary.