//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24435 SUBJECT: LIGO/Virgo S190510g: IceCube Neutrino Search DATE: 19/05/10 04:58:21 GMT FROM: Alex Pizzuto at ICECUBE/U of Wisconsin The IceCube Collaboration (http://icecube.wisc.edu/) reports: IceCube has performed a search for track-like muon neutrino events consistent with the sky localization of S190510g-1-Preliminary in a time range of 1000 seconds centered on the alert event time (2019-05-10 02:51:19.292 UTC to 2019-05-10 03:07:59.292 UTC) during which IceCube was collecting good quality data. No track-like events are found in spatial coincidence with the 90% spatial containment of S190510g calculated from the map circulated in the preliminary notice. IceCube's sensitivity to point sources within the location spanned by the 90% spatial containment of S190510g ranges from 0.029 to 0.806 GeV cm^-2 in a 1000 second time window. The IceCube Neutrino Observatory is a cubic-kilometer neutrino detector operating at the geographic South Pole, Antarctica. The IceCube realtime alert point of contact can be reached at roc@icecube.wisc.edu //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24436 SUBJECT: LIGO/Virgo S190510g Global MASTER-Net observations report DATE: 19/05/10 05:16:07 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, E. Gorbovskoy, V.Kornilov, D.Kuvshinov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.V.Chazov, D. Vlasenko (Lomonosov Moscow State University, Sternberg Astronomical Institute, Moscow State University) A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory) K. Ivanov, O. Gres, N.M. Budnev, S. Yazev, O. Chuvalaev, V. Poleshchuk (Irkutsk State University) V. Yurkov, A. Gabovich, Yu. Sergienko (Blagoveschensk Educational State University, Blagoveschensk) R. Podesta, Carlos Lopez and F. Podesta (Observatorio Astronomico Felix Aguilar (OAFA)) Hugo Levato and Carlos Saffe (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)) R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres (The Instituto de Astrofisica de Canarias) D. Buckley, S. Potter, A. Kniazev, M. Kotze (South African Astronomical Observatory) MASTER-IAC robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Spain (IAC Teide Observatory) started inspect of the LIGO/Virgo S190510g errorbox 5366 sec after trigger time at 2019-05-10 04:29:05 UT, with upper limit up to 19.4 mag. The observations began at zenit distance = 82 deg. The sun altitude is -21.9 deg. MASTER-OAFA robotic telescope located in Argentina (OAFA observatory of San Juan National University) started inspect of the LIGO/Virgo S190510g errorbox 5771 sec after trigger time at 2019-05-10 04:35:50 UT, with upper limit up to 19.5 mag. The observations began at zenit distance = 125 deg. The sun altitude is -76.4 deg. The galactic latitude b = -60 deg., longitude l = 98 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/ligo_1.php?id=10342 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 5456 | 2019-05-10 04:29:05 | MASTER-IAC | ( 13h 40m 40.55s , - 3d 55m 12.32s) | C | 180 | 18.0 | 5674 | 2019-05-10 04:32:42 | MASTER-IAC | ( 13h 55m 09.10s , - 1d 55m 34.40s) | C | 180 | 19.1 | 5861 | 2019-05-10 04:35:50 | MASTER-OAFA | ( 13h 31m 14.55s , - 1d 53m 24.34s) | C | 180 | 18.9 | 5904 | 2019-05-10 04:36:33 | MASTER-IAC | ( 13h 55m 08.87s , - 1d 56m 01.81s) | C | 180 | 19.4 | 6086 | 2019-05-10 04:39:34 | MASTER-OAFA | ( 13h 30m 45.90s , + 0d 6m 18.43s) | C | 180 | 19.2 | 6314 | 2019-05-10 04:43:22 | MASTER-OAFA | ( 13h 46m 43.91s , + 0d 6m 21.28s) | C | 180 | 19.5 | 6545 | 2019-05-10 04:47:13 | MASTER-OAFA | ( 13h 31m 12.81s , - 1d 53m 49.56s) | C | 180 | 19.3 | 6770 | 2019-05-10 04:50:58 | MASTER-OAFA | ( 13h 39m 14.80s , - 1d 53m 52.77s) | C | 180 | 19.4 | 7002 | 2019-05-10 04:54:50 | MASTER-OAFA | ( 13h 30m 44.89s , + 0d 6m 29.70s) | C | 180 | 19.3 | 7228 | 2019-05-10 04:58:36 | MASTER-OAFA | ( 13h 38m 43.67s , + 0d 6m 26.15s) | C | 180 | 19.5 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24437 SUBJECT: LIGO-Virgo S190510g: AGILE MCAL observations DATE: 19/05/10 05:26:58 GMT FROM: Alessandro Ursi at INAF/IAPS A. Ursi (INAF/IAPS), F. Verrecchia (SSDC, and INAF/OAR), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, C. Casentini, G. Piano (INAF/IAPS), F. Lucarelli, C. Pittori (SSDC, and INAF/OAR), A. Bulgarelli, V. Fioretti, N. Parmiggiani (INAF/OAS-Bologna), M. Pilia (INAF/OA-Cagliari), F. Longo (Univ. Trieste, and INFN Trieste), report on behalf of the AGILE Team: In response to the LIGO-Virgo GW event S190510g at T0 = 2019-05-10 02:59:39 (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 90% of the S190510g 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 S190510g localization region, from a minimum of 1.30E-06 erg cm^-2 to a maximum of 3.22E-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: 24438 SUBJECT: LIGO/Virgo S190510g: Fermi GBM Observations DATE: 19/05/10 05:27:10 GMT FROM: Peter Veres at UAH P. Veres (UAH) reports on behalf of the Fermi-GBM Team and the GBM+LIGO/Virgo Working Group: At the time of S190510g, Fermi was passing through the South Atlantic Anomaly therefore the GBM detectors were disabled. We note that the Fermi-GBM trigger (190510120 / 579149538) that occurred about 7 minutes prior to the LVC trigger is a long gamma-ray burst that is unassociated with S190510g based on the preliminary bayestar map. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24441 SUBJECT: LIGO/Virgo S190510g: HAWC follow-up DATE: 19/05/10 05:47:46 GMT FROM: Harm Schoorlemmer at MPIK, HAWC The HAWC Collaboration (https://www.hawc-observatory.org) reports: The HAWC Collaboration performed a follow-up of the gravitational wave trigger S190510g. At the time of the trigger the HAWC local zenith was oriented towards (RA, Dec) = (175.0 deg, 19.1 deg). 25% 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 15.3 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-06 erg/cm^2 to 1.1e-04 erg/cm^2 (6.4e-06 erg/cm^2 to 5.0e-04 erg/cm^2), depending on the zenith angle. HAWC is a TeV gamma ray water Cherenkov array located in the state of Puebla, Mexico. It is sensitive to the energy range ~0.1-100TeV, and monitors 2/3 of the sky every day with an instantaneous field-of-view of ~2 sr. //////////////////////////////////////////////////////////////////////// iTITLE: GCN CIRCULAR NUMBER: 24442 SUBJECT: LIGO/Virgo S190510g: Identification of a GW compact binary merger candidate DATE: 19/05/10 05:51:38 GMT FROM: Eric Howell at Aus.Intl.Grav.Res.Centre/UWA The LIGO Scientific Collaboration and the Virgo Collaboration report: We identified the compact binary merger candidate S190510g during real-time processing of data from LIGO Hanford Observatory (H1), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) at 2019-05-10 02:59:39.292 UTC (GPS time: 1241492397.292). The candidate was found by the GstLAL [1] analysis pipeline. S190510g is an event of interest because its false alarm rate, as determined by the online analysis, is 8.4e-10 Hz, or about one in 37 years. The event's properties can be found at this URL: https://gracedb.ligo.org/superevents/S190510g The classification of the GW signal, in order of descending probability, is BNS (98%), Terrestrial (2%), NSBH (<1%), BBH (<1%), or MassGap (<1%). Assuming the candidate is astrophysical in origin, there is strong evidence for the lighter compact object having a mass < 3 solar masses (HasNS: >99%). Using the masses and spins inferred from the signal, there is strong evidence for matter outside the final compact object (HasRemnant: >99%). One skymap is available at this time and can be retrieved from the GraceDB event page: * bayestar.fits.gz, an updated localization generated by BAYESTAR [2], distributed via GCN notice about an hour after the candidate For the bayestar.fits.gz skymap, the 90% credible region is 3462 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 269 +/- 108 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: 24443 SUBJECT: LIGO/Virgo S190510g: Public DECam Observations DATE: 19/05/10 06:15:13 GMT FROM: Igor Andreoni at Caltech Igor Andreoni (Caltech), Daniel A. Goldstein (Caltech), Michael Coughlin (Caltech), Mansi M. Kasliwal (Caltech), Peter E. Nugent (LBNL), Michael Medford (UC Berkeley), Shreya Anand (Caltech), Jennifer Barnes (Columbia), S. Bradley Cenko (NASA GSFC), Jeffrey Cooke (Swinburne), Jorge Martínez Palomera (UC Berkeley), Leo P. Singer (NASA GSFC), on behalf of the Global Relay of Observatories Watching Transients Happen (GROWTH) and ZTF collaborations: On 2019-05-10 06:00:00 UT we started the follow-up of the gravitational wave trigger S190510g (LIGO Scientific Collaboration and the Virgo Collaboration, GCN #24442) with the Victor M. Blanco 4m Telescope at Cerro Tololo Inter-American Observatory, equipped with the Dark Energy Camera (DECam). An observational tiling for the event was automatically and optimally determined and triggered using the GROWTH Target of Opportunity marshal (Coughlin et al. 2019a, Kasliwal et al. 2019b). The data from this program are immediately public and we invite anyone interested to search the images for optical counterparts. We are searching the images in real time for optical counterpart candidates using an image subtraction pipeline written for this program. The images are available under proposal ID 2019A-0205 from the NOAO archive (archive.noao.edu). For any questions on the data or the observations, please contact the PIs of this program, Danny Goldstein and Igor Andreoni (danny@caltech.edu, andreoni@caltech.edu). GROWTH and ZTF are worldwide collaborations comprising Caltech, USA; IPAC, USA, WIS, Israel; OKC, Sweden; JSI/UMd, USA; U Washington, USA; DESY, Germany; MOST, Taiwan; UW Milwaukee, USA; TTU, USA; LANL USA; Tokyo Tech, Japan; IIT-B, India; IIA, India; LJMU, UK and USyd, Australia. ZTF acknowledges the generous support of the NSF under AST MSIP Grant No 1440341. GROWTH acknowledges generous support of the NSF under PIRE Grant No 1545949. Alert distribution service provided by DIRAC@UW (Patterson et al. 2019). Alert filtering and follow-up co-ordination is being undertaken by the GROWTH marshal system (Kasliwal et al. 2019). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24444 SUBJECT: LIGO/Virgo S190510g: Potential host galaxies from the GLADE catalog DATE: 19/05/10 06:24:33 GMT FROM: Gergely Dalya at Eotvos U Gergely Dálya and Peter Raffai (Eotvos Univ.) reports on behalf of the GLADE team: We have found 69,543 galaxies in the GLADE catalog [1,2], within the 90% GW localization area (bayestar.fits.gz) reported by the LVC in GCN 24442, and within 269 +/- 108 Mpc distance limits. The galaxies found can be accessed on the GLADE website (19.5 MB txt file; please note that the order of galaxies in the list only follow the ordering as the appear in GLADE): http://glade.elte.hu/O3/S190510g_GLADE_90.txt There are 12,813 galaxies within the 50% GW localization area and within the same distance limits (3.6 kB txt file; please note that the order of galaxies in the list only follow the ordering as the appear in GLADE): http://glade.elte.hu/O3/S190510g_GLADE_50.txt [1] Dálya, G., Galgóczi G., Dobos, L. et al., 2018 MNRAS, 479, 2374 [2] http://glade.elte.hu //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24445 SUBJECT: S190510g: INTEGRAL inactive at the time of the event DATE: 19/05/10 07:07:00 GMT FROM: James Rodi at IAPS-INAF Enrico Bozzo, Volodymyr Savchenko, Carlo Ferrigno (ISDC/UniGE, Switzerland) James Rodi, (IAPS-Roma, Italy) Sandro Mereghetti (INAF IASF-Milano, Italy) on behalf of the INTEGRAL multi-messenger collaboration: https://www.astro.unige.ch/cdci/integral-multimessenger-collaboration The INTEGRAL spacecraft has a highly elliptical orbit and the instruments are switched off around the perigee passage, every 2.6 days, to prevent radiation-induced damages. Unfortunately, at the time of the LIGO/Virgo trigger S190510g (2019-05-10 02:59:39 UTC) the spacecraft was preparing to the start the observations after the perigee passage between the orbits number 2088 and 2089 and no scientific instrument data are available. INTEGRAL observations will restart in about 4.6 hours. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24446 SUBJECT: LIGO/Virgo S190510g: ANTARES neutrino search DATE: 19/05/10 08:48:42 GMT FROM: Damien Dornic at CPPM,France M. Ageron (CPPM/CNRS), B. Baret (APC/CNRS), A. Coleiro (APC/Universite Paris Diderot), M. Colomer (APC/Universite Paris Diderot)), D. Dornic (CPPM/CNRS), A. Kouchner (APC/Universite Paris Diderot), 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 S190510g event using the 90% contour of the initial bayestar probability map provided by the GW interferometers (GCN#24442). The ANTARES visibility at the time of the alert, together with the 50% and 90% contours of the probability map are shown in https://www.cppm.in2p3.fr/~dornic/events_runo3/S190510g.png . Considering the location probability provided by the LIGO/Virgo collaborations, there is a 58.7% chance that the GW emitter was in the ANTARES **upgoing** field of view at the time of the alert. No up-going muon neutrino candidate events were recorded in the ANTARES sky during a +/- 500s time-window centered on the time (2019-05-10 02:59:39 UT) and in the 90% contour of the S190510g event. The expected number of atmospheric background events in the region visible by ANTARES is 3.1e-4 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 2.2e-3 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: 24447 SUBJECT: LIGO/Virgo S190510g: MAXI/GSC Observations DATE: 19/05/10 09:53:26 GMT FROM: Satoshi Sugita at Aoyama Gakuin U. N. Kawai, M. Sugizaki (Tokyo Tech), H. Negoro (Nihon U.), S. Sugita, M. Serino (AGU), M. Nakajima, W. Maruyama, M. Aoki, K. Kobayashi (Nihon U.), S. Nakahira, T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN), T. Sakamoto, H. Nishida, A. Yoshida (AGU), Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, T. Sato (Chuo U.), M. Shidatsu (Ehime U.), M. Oeda, K. Shiraishi (Tokyo Tech), S. Ueno, H. Tomida, M. Ishikawa, Y. Sugawara, N. Isobe, R. Shimomukai, M. Tominaga (JAXA), Y. Ueda, A. Tanimoto, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake (Kyoto U.), H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.), M. Yamauchi, S. Iwahori, Y. Kurihara (Miyazaki U.), T. Kawamuro (NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU) report on behalf of the MAXI team: We examined MAXI/GSC all-sky X-ray images (2-20 keV) after the LVC trigger S190510g at 2019-05-10 02:59:39.292 UTC (GCN 24442). At the trigger time of S190510g, the high-voltage of MAXI/GSC was off, and it was turned on at T0+358 sec (=T0+6.0 min). The first one-orbit (92 min) scan observation with GSC after the event covered 91% of the 90% credible region of the bayestar skymap from 03:05:37 to 04:15:54 UTC (T0+358 to T0+4575 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: 24448 SUBJECT: LIGO/Virgo S190510g: Updated localization from LIGO and Virgo data DATE: 19/05/10 10:30:18 GMT FROM: Qi Chu at LSC The LIGO Scientific Collaboration and the Virgo Collaboration report: We have re-analyzed LIGO and Virgo data around the time of the compact binary coalescence (CBC) candidate S190510g (GCN 24442). Parameter estimation has been performed using LALInference [1] and a new sky map, LALInference.fits.gz, distributed via GCN Notice, is available for retrieval from the GraceDB event page: https://gracedb.ligo.org/superevents/S190510g For the LALInference.fits.gz skymap, the 90% credible region is 1166 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 227 +/- 92 Mpc (a posteriori mean +/- standard deviation). This is the preferred sky map at this time. 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: 24450 SUBJECT: LIGO/Virgo S190510g: HSC Y-band follow-up observation DATE: 19/05/10 10:56:39 GMT FROM: Michitoshi Yoshida at NAOJ/Subaru Michitoshi Yoshida, Yuhei Takagi, Tsuyoshi Terai (NAOJ) Yousuke Utsumi (Stanford Univ.), Nozomu Tominaga (Konan Univ.), Mahito Sasada, Hiroshi Akitaya (Hiroshima Univ.) on behalf of J-GEM collaboration We report optical imaging follow-up observations for a part of the equator region (RA:13h, Dec:0d) of S190510g (LIGO Scientific Collaboration and the Virgo Collaboration, GCN #24442) with Hyper Suprime-Cam (HSC) attached to the 8.2-m Subaru Telescope. HSC has a circular field-of-view whose area is 1.7 deg^2. We performed Y-band imaging observations on 2019-05-10 UT. The exposure time per frame was 30 sec. We covered 140 deg^2 around the high probability area in the equator region of the Bayestar skymap of S190510g with 120 pointings of HSC. We revisited each pointing position two times. The 5-sigma limiting AB magnitude of Y-band was about 22.7 mag. The observed regions are as follows: JGEM28175 13:27:11.25 -08:23:07.9 JGEM28432 13:30:00.00 -08:59:21.5 JGEM27663 13:27:11.25 -07:10:50.7 JGEM27920 13:30:00.00 -07:46:57.8 JGEM28176 13:32:48.75 -08:23:07.9 JGEM28433 13:35:37.50 -08:59:21.5 JGEM26895 13:24:22.50 -05:22:45.8 JGEM27151 13:27:11.25 -05:58:45.0 JGEM27408 13:30:00.00 -06:34:46.5 JGEM27664 13:32:48.75 -07:10:50.7 JGEM27921 13:35:37.50 -07:46:57.8 JGEM28177 13:38:26.25 -08:23:07.9 JGEM26383 13:24:22.50 -04:10:53.5 JGEM26639 13:27:11.25 -04:46:48.7 JGEM26896 13:30:00.00 -05:22:45.8 JGEM27152 13:32:48.75 -05:58:45.0 JGEM27409 13:35:37.50 -06:34:46.5 JGEM27665 13:38:26.25 -07:10:50.7 JGEM27922 13:41:15.00 -07:46:57.8 JGEM25871 13:24:22.50 -02:59:07.8 JGEM26127 13:27:11.25 -03:34:60.0 JGEM26384 13:30:00.00 -04:10:53.5 JGEM26640 13:32:48.75 -04:46:48.7 JGEM26897 13:35:37.50 -05:22:45.8 JGEM27153 13:38:26.25 -05:58:45.0 JGEM27410 13:41:15.00 -06:34:46.5 JGEM27666 13:44:03.75 -07:10:50.7 JGEM25615 13:27:11.25 -02:23:16.9 JGEM25872 13:30:00.00 -02:59:07.8 JGEM26128 13:32:48.75 -03:34:60.0 JGEM26385 13:35:37.50 -04:10:53.5 JGEM26641 13:38:26.25 -04:46:48.7 JGEM26898 13:41:15.00 -05:22:45.8 JGEM27154 13:44:03.75 -05:58:45.0 JGEM25103 13:27:11.25 -01:11:37.5 JGEM25360 13:30:00.00 -01:47:26.8 JGEM25616 13:32:48.75 -02:23:16.9 JGEM25873 13:35:37.50 -02:59:07.8 JGEM26129 13:38:26.25 -03:34:60.0 JGEM26386 13:41:15.00 -04:10:53.5 JGEM26642 13:44:03.75 -04:46:48.7 JGEM24591 13:27:11.25 -00:00:00.0 JGEM26899 13:46:52.50 -05:22:45.8 JGEM24848 13:30:00.00 -00:35:48.6 JGEM25104 13:32:48.75 -01:11:37.5 JGEM25361 13:35:37.50 -01:47:26.8 JGEM25617 13:38:26.25 -02:23:16.9 JGEM25874 13:41:15.00 -02:59:07.8 JGEM26130 13:44:03.75 -03:34:60.0 JGEM26387 13:46:52.50 -04:10:53.5 JGEM24336 13:30:00.00 -00:35:48.6 JGEM24592 13:32:48.75 -00:00:00.0 JGEM24849 13:35:37.50 -00:35:48.6 JGEM25105 13:38:26.25 -01:11:37.5 JGEM25362 13:41:15.00 -01:47:26.8 JGEM23824 13:30:00.00 +01:47:26.8 JGEM25618 13:44:03.75 -02:23:16.9 JGEM25875 13:46:52.50 -02:59:07.8 JGEM24080 13:32:48.75 +01:11:37.5 JGEM24337 13:35:37.50 -00:35:48.6 JGEM24593 13:38:26.25 -00:00:00.0 JGEM23312 13:30:00.00 +02:59:07.8 JGEM24850 13:41:15.00 -00:35:48.6 JGEM25106 13:44:03.75 -01:11:37.5 JGEM23568 13:32:48.75 +02:23:16.9 JGEM25363 13:46:52.50 -01:47:26.8 JGEM25619 13:49:41.25 -02:23:16.9 JGEM23825 13:35:37.50 +01:47:26.8 JGEM24081 13:38:26.25 +01:11:37.5 JGEM24338 13:41:15.00 -00:35:48.6 JGEM23056 13:32:48.75 +03:34:60.0 JGEM24594 13:44:03.75 -00:00:00.0 JGEM24851 13:46:52.50 -00:35:48.6 JGEM23313 13:35:37.50 +02:59:07.8 JGEM25107 13:49:41.25 -01:11:37.5 JGEM23569 13:38:26.25 +02:23:16.9 JGEM22544 13:32:48.75 +04:46:48.7 JGEM23826 13:41:15.00 +01:47:26.8 JGEM24082 13:44:03.75 +01:11:37.5 JGEM22801 13:35:37.50 +04:10:53.5 JGEM24339 13:46:52.50 -00:35:48.6 JGEM24595 13:49:41.25 -00:00:00.0 JGEM23057 13:38:26.25 +03:34:60.0 JGEM22032 13:32:48.75 +05:58:45.0 JGEM23314 13:41:15.00 +02:59:07.8 JGEM22289 13:35:37.50 +05:22:45.8 JGEM23570 13:44:03.75 +02:23:16.9 JGEM23827 13:46:52.50 +01:47:26.8 JGEM22545 13:38:26.25 +04:46:48.7 JGEM22802 13:41:15.00 +04:10:53.5 JGEM21777 13:35:37.50 +06:34:46.5 JGEM23058 13:44:03.75 +03:34:60.0 JGEM22033 13:38:26.25 +05:58:45.0 JGEM23315 13:46:52.50 +02:59:07.8 JGEM22290 13:41:15.00 +05:22:45.8 JGEM22546 13:44:03.75 +04:46:48.7 JGEM23835 14:31:52.50 +01:47:26.8 JGEM23578 14:29:03.75 +02:23:16.9 JGEM23322 14:26:15.00 +02:59:07.8 JGEM23323 14:31:52.50 +02:59:07.8 JGEM23066 14:29:03.75 +03:34:60.0 JGEM22810 14:26:15.00 +04:10:53.5 JGEM23067 14:34:41.25 +03:34:60.0 JGEM22811 14:31:52.50 +04:10:53.5 JGEM22298 14:26:15.00 +05:22:45.8 JGEM22554 14:29:03.75 +04:46:48.7 JGEM22555 14:34:41.25 +04:46:48.7 JGEM22042 14:29:03.75 +05:58:45.0 JGEM22299 14:31:52.50 +05:22:45.8 JGEM22813 14:43:07.50 +04:10:53.5 JGEM22557 14:45:56.25 +04:46:48.7 JGEM22301 14:43:07.50 +05:22:45.8 JGEM22044 14:40:18.75 +05:58:45.0 JGEM22302 14:48:45.00 +05:22:45.8 JGEM22045 14:45:56.25 +05:58:45.0 JGEM21789 14:43:07.50 +06:34:46.5 JGEM22303 14:54:22.50 +05:22:45.8 JGEM22046 14:51:33.75 +05:58:45.0 JGEM21790 14:48:45.00 +06:34:46.5 JGEM21791 14:54:22.50 +06:34:46.5 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24451 SUBJECT: LIGO/Virgo S190510g: Insight-HXMT/HE observation DATE: 19/05/10 12:01:31 GMT FROM: Qi Luo at IHEP Q. Luo, C. Cai, Q. B. Yi, S. Xiao, C. K. Li, X. B. Li, G. Li, J. Y. Liao, S. L. Xiong, C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, M. Wu, Y. P. Xu, S. N. Zhang (IHEP), report on behalf of the Insight-HXMT team: Insight-HXMT was taking data normally around the GW trigger time (T0=2019-05-10 02:59:39 UTC). At T0, more than 70% of the LIGO localization region was covered by Insight-HXMT without occultation by the Earth. Within T0 +/- 100 s, no significant excess events (SNR > 3 sigma) are found in a search of the Insight-HXMT/HE raw light curves. Assuming the GW counterpart GRB with three typical GRB Band spectral models, two typical duration timescales (1 s, 10 s) from the peak position of the LIGO-Virgo location probability map, the 5-sigma upper-limits fluence (0.2 - 5 MeV, incident energy) are reported below: Band model 1 (alpha=-1.9, beta=-3.7, Ep=70 keV): 1 s: 2.4e-07 erg cm^-2 10 s: 9.1e-07 erg cm^-2 Band model 2 (alpha=-1.0, beta=-2.3, Ep=230 keV): 1 s: 3.0e-07 erg cm^-2 10 s: 1.2e-06 erg cm^-2 Band model 3 (alpha=-0.0, beta=-1.5, Ep=1000 keV): 1 s: 3.0e-07 erg cm^-2 10 s: 1.3e-06 erg cm^-2 All measurements above are made with the CsI detectors operating in the regular mode with the energy range of about 80-800 keV (deposited energy). Only gamma-rays with energy greater than about 200 keV can penetrate the spacecraft and leave signals in the CsI detectors installed inside of the spacecraft. Insight-HXMT is the first Chinese space X-ray telescope, which was funded jointly by the China National Space Administration (CNSA) and the Chinese Academy of Sciences (CAS). More information could be found at: http://www.hxmt.org. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24453 SUBJECT: LIGO/Virgo S190510g: CLU/NED Galaxies in the Localization Volume DATE: 19/05/10 13:46:34 GMT FROM: David Cook at IPAC/Caltech LIGO/Virgo S190510g: CLU/NED Galaxies in the Localization Volume David O. Cook (Caltech/IPAC), Angela Van Sistine (UW Milwaukee), Leo Singer (NASA/GSFC), Igor Andreoni (Caltech), Michael Coughlin (Caltech), Bob Aloisi (UW Milwaukee), Patrick R. Brady (UW Milwaukee), Rick Ebert (Caltech/IPAC), George Helou (Caltech/IPAC), David Kaplan (UW Milwaukee), Mansi M. Kasliwal (Caltech), Joseph M. Mazzarella (Caltech/IPAC), and Marion Schmitz (Caltech/IPAC) On behalf of the Global Relay of Observatories Watching Transients Happen (GROWTH) collaboration and the NASA/IPAC Extragalactic Database (NED) Team. We spatially cross-matched the LIGO/Virgo S190510g trigger sky localization (90% containment volume) with the Census of the Local Universe (CLU; Cook et al. 2017; arxiv:1710.05016) galaxy catalog and found 8044 galaxies within the volume. The CLU catalog is a compilation of galaxies with existing redshifts from many sources (e.g., NED, SDSS, etc) and new galaxies from a 3PI narrow-band survey to look for redshifted Halpha emission out to 200 Mpc with the Palomar Oschin 48-inch telescope (Cook et al. 2017; arxiv:1710.05016). We list here the top 20 galaxies sorted by stellar mass (Mstar) for galaxies whose location on the sky and distance falls in the 90% volume reported by the BAYESTAR probability sky map (Singer et al. 2016). We also list the dust-corrected star formation rates (SFRs) for galaxies with GALEX FUV detections and a 'nan' for those with no detection. For an extended list of galaxies in the 90% volume go to the NED Gravitational Wave Followup service at https://ned.ipac.caltech.edu/uri/NED::GWF/. This service provides downloadable galaxy lists and visualizations for candidate host galaxies. For each GW alert, these products are automatically generated and made available within minutes to expedite efficient electromagnetic followup observations. The NED top 20 list is sorted by 2MASS absolute K-band magnitude, but users can sort the entire list on a variety of other criteria (probability density, UV magnitudes, etc) after download. name ra dec distmpc logsfr_fuv logmstar dP_dV ------------------------ -------- ------- ------- ---------- -------- -------- 2MASX J05580206-3820043 89.5083 -38.3346 141.03 1.50 11.84 1.17e-06 ESO 307- G 011 89.9994 -38.1782 186.91 0.14 11.62 1.14e-06 ESO 413- G 024 25.4956 -31.0094 83.04 -1.09 11.26 1.33e-07 GALEXASC J132755.20+000653.7 201.9799 0.1149 198.20 -0.62 11.24 2.74e-08 NGC 0612 23.4906 -36.4933 123.96 0.71 11.16 4.56e-08 NGC 0526A 20.9766 -35.0655 79.52 0.74 11.12 5.77e-08 ESO 363- G 006 83.1713 -32.9618 193.70 nan 11.11 3.31e-08 2MASX J05453627-2555305 86.4012 -25.9252 188.60 -0.47 11.09 3.82e-07 ESO 365- G 005 94.6886 -35.3041 188.09 nan 11.09 5.73e-07 2MASX J05403062-3548505 85.1277 -35.8141 196.74 nan 11.09 3.94e-08 MCG -04-14-035 87.1797 -25.4773 181.00 -0.55 11.08 4.34e-07 TOLOLO 0611-379 93.3691 -37.9971 159.89 0.97 11.08 1.29e-06 MCG -07-13-001 89.9648 -39.1343 187.64 -0.54 11.08 2.83e-07 2MASX J06090797-2730329 92.2832 -27.5092 194.94 nan 11.06 3.59e-07 GIN 298 86.1235 -26.0589 200.00 -0.41 11.05 3.42e-07 ESO 307- G 013 90.1712 -40.0445 194.07 -0.42 11.04 9.21e-08 ESO 364- G 033 92.1921 -33.9163 157.00 nan 11.03 6.75e-06 MCG -04-14-014 85.5302 -26.1982 158.50 -0.73 11.03 3.15e-07 2MASX J06004280-3925378 90.1783 -39.4271 194.96 -0.65 11.03 2.19e-07 ESO 488- G 013 86.7310 -25.6356 194.51 -0.56 11.03 3.47e-07 Table: Top 20 galaxies in CLU that fall in the 90% probability volume for S190510g sorted by stellar mass. Column descriptions are as follows. name: galaxy name. ra: RA (J2000, decimal degrees). dec: Dec (J2000, decimal degrees). distmpc: galaxy distance (Mpc). logsfr_fuv: log10 of the star formation rate (SFR, Msun per year), derived from GALEX All Sky Kron FUV magnitudes via the prescription of Murphy et al. (2011), corrected for internal dust extinction using a combination of GALEX FUV and 22um ALLWISE fluxes (Hao et al. 2011). logmstar: log10 of the galaxy stellar mass (Msun), estimated from 3.4um ALLWISE fluxes and a mass-to-light ratio of 0.5 (McGaugh & Schombert et al. 2015). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24454 SUBJECT: LIGO/Virgo S190510g: Swift/BAT Counterpart Search DATE: 19/05/10 14:09:56 GMT FROM: Amy Lien at GSFC D. M. Palmer (LANL), S. D. Barthelmy (NASA/GSFC), A. Y. Lien (GSFC/UMBC), T. Sakamoto (AGU), A. A. Breeveld (MSSL-UCL), A. P. Beardmore (U. Leicester), 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(ASDC), S. Emery (UCL-MSSL), P. A. Evans (U. Leicester), P. Giommi (ASI), C. Gronwall (PSU), D. Hartmann (Clemson U.), J. A. Kennea (PSU), H. A. Krimm (NSF), N. P. M. Kuin (UCL-MSSL), F. E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB), B. Mingo (U. Leicester), J. A. Nousek (PSU), S. R. Oates (Uni. of Warwick), P. T. O'Brien (U. Leicester), J. P. Osborne (U. Leicester), C. Pagani (U. Leicester), K. L. Page (U.Leicester), M. Perri (ASDC), J. L. Racusin (NASA/GSFC), B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU), G. Tagliaferri (INAF-OAB), A. Tohuvavohu (PSU), 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 S190510g (LIGO/VIRGO Collaboration GCN Circ. 24442), where T0 is the LVC trigger time (2019-05-10T02:59:39.292 UTC). The center of the BAT FOV at T0 is RA = 288.846 deg, DEC = 10.936 deg, ROLL = 58.998 deg. The BAT Field of View (>10% partial coding) covers 0.95% of the integrated LVC localization probability, and 0.00% of the galaxy convolved probability (Evans et al. 2016). Within T0 +/- 100 s, no significant detections (signal-to-noise ratio >~ 5 sigma) are found in the BAT raw light curves with time bins of 64 ms, 1 s, and 1.6 s. Assuming an on-axis (100% coded) short GRB with a typical spectrum in the BAT energy range (i.e., a simple power-law model with a power-law index of -1.32, Lien & Sakamoto et al. 2016), the 5-sigma upper limit in the 1-s binned light curve corresponds to a flux upper limit (15-350 keV) of ~ 1.57 x 10^-7 erg/s/cm^2. No event data are available at this time. BAT retains decreased, but significant, sensitivity to rate increases for gamma-ray events outside of its FOV. About 24.12% 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/S190510g/web/source.html //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24455 SUBJECT: LIGO/Virgo S190510g: GRAWITA REM optical observations DATE: 19/05/10 14:42:46 GMT FROM: Maria Grazia Bernardini at INAF/Brera P. D'Avanzo (INAF-OAB), L. Izzo (IAA), S. Yang (INAF-OAPd), E. Palazzi (INAF-OAS), S Campana (INAF-OAB), S. Benetti (INAF-OAPd), M.G. Bernardini (INAF-OAB), M.T. Botticella (INAF-OAC), M. Branchesi (GSSI), A. Bulgarelli (INAF-OAS), S. Campana (INAF-OAB), E. Cappellaro (INAF-OAPd), R. Carini (INAF-OAR), R. Ciolfi (INAF-OAPd), S. Covino (INAF-OAB), V. D'Elia (ASI-SSDC), M. Della Valle (INAF-OAC), A. Grado (INAF-OAC), G. Greco (Univ. Urbino), A. Melandri (INAF-OAB), L. Nicastro (INAF-OAS), S. Piranomonte (INAF-OAR), A. Rossi (INAF-OAS), V. Testa (INAF-OAR), L. Tomasella (INAF-OAPd), E. Brocato (INAF-OAAb, INAF-OAR), on behalf of GRAWITA report: We carried out optical follow-up observations of the LIGO/Virgo GW trigger S190509g (LVC, GCN Circ. 24442) with the 60-cm robotic telescope REM located at the La Silla Observatory (Chile). The observations started at 2019-05-10 at 05:27:51 UT, simultaneously in the g, r, i, z bands (the REM NIR camera was not operational). We observed the following galaxies within the 90% probability of the initial bayestar skymap visible from La Silla: RA(J2000) Dec(J2000) Dist(Mpc) Abs_Mag(B) -------------------------------------------------------------- 14:40:29.9303:14:01.1 400.91 -20.19 13:40:22.5600:14:12.1 335.74 -19.36 13:39:26.41-04:38:43.7 331.50 -20.14 14:40:56.6403:09:10.7 376.70 -19.83 14:17:12.5701:59:31.5 261.43 -20.30 13:17:09.12-00:57:28.1 366.44 -19.74 13:40:11.16-04:36:24.0 351.69 -19.99 14:55:34.8008:39:43.5 376.70 -19.51 14:32:03.12-01:10:03.7 243.01 -19.33 14:31:11.16-02:37:20.2 315.22 -19.81 14:29:11.5209:38:11.6 385.48 -18.77 14:17:44.1601:58:52.6 259.42 -20.12 14:30:39.4007:16:30.0 21.40 -19.47 14:44:57.6000:50:40.1 317.69 -18.18 13:53:50.6400:50:43.3 279.25 -19.74 No clear counterpart for S190509g is found down to a typical 3sigma magnitude of r > 19 (AB). We report the presence of a possible transient (likely unrelated to S190509g) found in the analysis of the REM frames at the following coordinates (J2000): RA = 14:29:15.99 Dec = +09:41:12.3 (+/- 1"). The source has a magnitude of r = 17.3 +/- 0.1 (AB, calibrated against the SDSS). We note that this object is 3.5" from the SDSS galaxy SDSS J142916.22+094112.1, whose catalogue magnitude is r = 22.56 +/- 0.20 and photometric redshift is z = 0.182 +/- 0.073. Further analysis and observations are planned. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24456 SUBJECT: LIGO/Virgo S190510g: Potential host galaxies on the updated skymap from the GLADE catalog DATE: 19/05/10 16:01:06 GMT FROM: Gergely Dalya at Eotvos U Gergely Dálya and Peter Raffai (Eotvos Univ.) reports on behalf of the GLADE team: We have found 17,197 galaxies in the GLADE catalog [1,2], within the updated 90% GW localization area (LALInference.fits.gz) reported by the LVC in GCN 24448, and within 227 +/- 92 Mpc distance limits. The galaxies found can be accessed on the GLADE website (4.6 MB txt file; please note that the order of galaxies in the list only follow the ordering as the appear in GLADE): http://glade.elte.hu/O3/S190510g_GLADE_90_upd.txt There are 353 galaxies within the 50% GW localization area and within the same distance limits (97 kB txt file; please note that the order of galaxies in the list only follow the ordering as the appear in GLADE): http://glade.elte.hu/O3/S190510g_GLADE_50_upd.txt [1] Dálya, G., Galgóczi G., Dobos, L. et al., 2018 MNRAS, 479, 2374 [2] http://glade.elte.hu //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24457 SUBJECT: LIGO-Virgo S190510g: AGILE GRID observations DATE: 19/05/10 16:27:22 GMT FROM: Francesco Verrecchia at ASDC F. Verrecchia (SSDC, and INAF-OAR), A. Ursi (INAF/IAPS), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), F. Lucarelli, C. Pittori (SSDC, and INAF-OAR), M. Cardillo, C. Casentini, G. Piano (INAF/IAPS), A. Bulgarelli, V. Fioretti, N. Parmiggiani (INAF/OAS-Bologna), M. Pilia (INAF/OA-Cagliari), F. Longo (Univ. Trieste, and INFN Trieste), report on behalf of the AGILE Team: In response to the LIGO-Virgo GW event S190510g at T0 = 2019-05-10 02:59:39.292 UTC (GCN #24442 including an updated localization) a preliminary analysis of the AGILE exposure at T0 showed that about 60% of the S190510g 90% c.l. localization region (LR) was exposed at off-axis angles between 25 and 75 deg by the Gamma-Ray Imaging Detector (GRID). We performed an analysis of the GRID data in the energy range 50 MeV - 10 GeV over three time intervals before and after T0, where good exposure of the S190510g 90% c.l. LR was available. No candidate gamma-ray transient was detected. The following preliminary GRID 3-sigma upper limit (UL) values are obtained: (T0 - 2s; T0 + 2s): from 7.4e-07 to 1.7e-06 erg cm^-2 s^-1 (T0 - 10s; T0 + 10s): from 1.5e-07 to 3.5e-07 erg cm^-2 s^-1 (T0; T0 + 100s): from 4.2e-08 to 1.8e-07 erg cm^-2 s^-1 An image of the AGILE-GRID exposure near T0 is available at the site https://tools.ssdc.asi.it/ImgView/Agile/S190510g_d4s_FM_UL-E50bemod8 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: 24460 SUBJECT: LIGO/Virgo S190510g: Fermi-LAT search for a high-energy gamma-ray counterpart DATE: 19/05/10 19:24:26 GMT FROM: Magnus Axelsson at Stockholm U. M. Axelsson (KTH and Stockholm Univ.), M. Arimoto (Kanazawa Univ.), E. Moretti (IFAE, Barcelona), D. Kocevski (NASA/MSFC), N. Omodei (Stanford Univ.) and F. Dirirsa (Univ. of Johannesburg) report on behalf of the Fermi-LAT collaboration: We have searched data collected by the Fermi Large Area Telescope (LAT) on May 10, 2019, for possible high-energy (E > 100 MeV) gamma-ray emission in spatial/temporal coincidence with the LIGO/Virgo trigger S190510g (GCN 24442). 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 a time, and "cumulative coverage" as the integral of the instantaneous coverage over time. The Fermi Gamma-ray Space Telescope was passing through the South Atlantic Anomaly (SAA) at the time of the trigger (T0 = 2019-05-10 02:59:39.292 UTC). During SAA passages both the LAT and Gamma-ray Burst Monitor (GBM) do not collect data due to the high charged particle background in this region. The LAT resumed taking data upon exiting the SAA at roughly T0 + 1340 s. At that time the instantaneous coverage was ~30% of the LIGO probability map, and reached 100% cumulative coverage after ~8.3 ks. We performed a search for a transient counterpart within the observed region of the 90% contour of the LIGO map in a fixed time window from T0 + 1340 s to T0 + 10 ks. No significant new sources are found. We also performed a search which adapted the time interval of the analysis to the exposure of each region of the sky, and no additional excesses were found. Energy flux upper bounds for the fixed time interval between 100 MeV and 100 GeV for this search vary between 1.1e-10 and 1.0e-9 [erg/cm^2/s]. The Fermi-LAT point of contact for this event is Feraol Dirirsa (fdirirsa@uj.ac.za). 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: 24461 SUBJECT: LIGO/Virgo S190510g: Lulin Optical Follow-up Observations DATE: 19/05/10 20:13:15 GMT FROM: Albert Kong at NTHU Po-Chieh Yu (NCU), Han-Jie Tan (NCU), Albert Kong (NTHU), Atharva Sunil Patil (NCU), Chow-Choong Ngeow (NCU), Wing-Huen Ip (NCU), on behalf of the Global Relay of Observatories Watching Transients Happen (GROWTH) collaboration We report observations of 81 galaxies in the 90% localization of the BNS merger candidate, S190510g, detected by LIGO/Virgo (GCN #24442; GCN #24448) using the Lulin One-meter Telescope (LOT) in Taiwan. The observation started at 2019-05-10 12:54:43 UT, ~10 hours after the trigger. The observations were conducted using the r-band filter with 180 second exposure time. By comparing with Pan-STARRS images, we do not detect transient candidates brighter than r~21 mag (AB). We thank the staff in Lulin Observatory for helping the observations. The galaxy coordinates are listed below. RA (hh mm ss.ss) Dec (dd mm ss.s) 13 00 30.12 -09 09 05.1 13 00 37.49 -07 48 41.1 13 00 52.36 -07 45 26.1 13 01 23.02 -08 59 37.6 13 02 12.79 -04 44 29.1 13 02 52.28 -04 48 03.1 13 03 38.53 -06 51 24.2 13 04 02.72 -08 43 33.5 13 04 09.43 -07 28 24.5 13 04 09.49 -07 19 24.5 13 04 42.00 -12 37 29.0 13 04 48.48 -04 22 26.8 13 05 00.24 -11 15 24.4 13 05 03.06 -11 12 48.8 13 05 08.16 -04 16 23.1 13 05 10.38 -10 40 25.7 13 05 12.72 -04 03 07.6 13 05 13.06 -11 21 30.7 13 05 20.26 -10 36 31.1 13 05 26.54 -06 20 25.1 13 05 28.69 -11 16 04.1 13 05 28.80 -11 16 04.1 13 05 30.07 -09 37 48.1 13 05 30.29 -10 26 18.1 13 05 35.04 -04 14 35.2 13 05 35.43 -07 13 59.1 13 05 41.00 -10 26 43.1 13 05 47.28 -03 59 07.1 13 05 51.84 -05 30 16.2 13 05 52.40 -05 22 12.4 13 05 56.88 -03 03 17.8 13 06 03.36 -12 22 28.2 13 06 04.57 -11 33 44.0 13 06 04.58 -05 22 30.4 13 06 04.80 -02 40 08.4 13 06 08.27 -05 22 40.3 13 06 11.37 -11 33 13.0 13 06 17.41 -07 45 42.3 13 06 21.36 -12 31 25.1 13 06 28.55 -06 51 11.3 13 06 32.34 -05 13 49.6 13 06 33.14 -07 23 50.3 13 06 37.68 -05 04 19.2 13 06 45.57 -08 08 03.9 13 06 45.84 -03 57 35.3 13 06 52.10 -06 31 05.9 13 06 58.32 -11 47 28.0 13 07 02.40 -04 37 05.9 13 07 04.80 -03 15 50.0 13 07 05.28 -11 55 48.0 13 07 17.06 -10 56 51.2 13 07 17.52 -04 54 11.7 13 07 19.64 -10 54 11.2 13 07 20.64 -05 17 03.1 13 07 26.00 -04 16 23.7 13 07 26.39 -06 42 24.2 13 07 30.55 -07 19 28.2 13 07 36.74 -02 44 25.7 13 07 37.30 -08 33 09.2 13 07 37.44 -01 11 35.3 13 07 41.28 -02 48 07.3 13 07 41.78 -07 36 13.2 13 07 42.00 -05 42 58.0 13 07 42.24 -06 24 53.8 13 07 42.62 -06 22 14.2 13 07 55.44 -06 25 41.2 13 07 57.12 -12 51 04.7 13 07 58.64 -12 11 21.7 13 07 59.28 -03 53 33.8 13 08 03.31 -05 23 27.8 13 08 10.87 -12 58 48.7 13 08 11.86 -04 31 09.8 13 08 16.21 -03 44 46.8 13 08 17.68 -07 02 37.2 13 08 20.91 -11 49 03.2 13 08 22.56 -11 24 51.2 13 08 24.72 -06 23 46.2 13 08 28.60 -06 22 11.2 13 08 29.04 -06 22 40.3 13 08 29.67 -12 26 32.9 13 08 32.40 -05 31 52.7 13 08 34.16 -10 06 39.2 13 08 35.20 -12 09 01.9 13 08 37.44 -12 05 26.2 13 08 38.15 -11 01 16.2 13 08 40.17 -06 47 17.2 13 08 42.67 -10 04 54.3 13 08 59.52 -05 16 45.8 13 08 59.52 -09 54 34.3 13 09 04.25 -07 13 52.3 13 09 04.33 -10 02 04.3 13 09 06.96 -05 18 37.4 13 09 18.31 -06 52 26.1 13 09 19.68 -05 21 43.2 13 09 21.47 -07 26 25.1 13 09 22.41 -13 35 58.6 13 09 30.48 -04 38 13.2 13 09 36.00 -04 17 35.5 13 09 36.97 -10 29 45.0 13 09 39.53 -06 57 44.0 13 09 39.84 -12 20 19.5 13 09 39.96 -12 20 19.6 13 09 42.20 -07 53 07.2 13 09 43.09 -03 04 51.9 13 09 45.36 -05 12 35.7 13 09 47.04 -03 05 26.6 13 09 51.12 -03 25 13.4 13 09 56.40 -03 31 02.6 13 10 02.15 -06 07 41.2 13 10 04.56 -03 05 11.2 13 10 06.42 -07 35 59.2 13 10 06.47 -12 15 38.8 13 10 12.81 -07 02 43.4 13 10 13.20 -05 52 47.9 13 10 14.28 -07 31 10.4 13 10 17.28 -03 47 12.5 13 10 21.75 -07 38 56.4 13 10 24.72 -11 41 13.2 13 10 27.39 -07 04 30.4 13 10 34.08 -05 52 13.8 13 10 37.44 -03 41 48.2 13 10 41.47 -04 39 34.6 13 10 44.16 -01 48 07.7 13 10 45.47 -12 34 54.5 13 10 46.08 -01 49 19.2 13 10 46.28 -06 02 11.1 13 10 48.93 -09 15 34.1 13 10 49.92 -10 52 29.4 13 10 50.53 -12 27 24.6 13 10 51.01 -12 18 23.6 13 10 51.37 -06 53 53.1 13 10 54.76 -13 05 46.6 13 10 55.92 -03 26 06.4 13 10 58.65 -11 55 37.6 13 11 00.70 -12 09 10.6 13 11 02.88 -04 57 06.8 13 11 06.00 -12 22 38.6 13 11 07.44 -12 13 14.9 13 11 08.13 -12 07 27.5 13 11 16.65 -07 16 19.5 13 11 20.84 -12 29 34.1 13 11 23.04 -05 53 16.5 13 11 28.32 -01 34 01.6 13 11 29.28 -02 28 24.3 13 11 29.92 -01 35 53.1 13 11 30.24 -05 22 58.8 13 11 30.48 -11 48 56.4 13 11 31.20 -03 23 46.0 13 11 34.19 -04 18 17.1 13 11 34.26 -09 06 03.5 13 11 41.36 -05 26 23.9 13 11 42.21 -10 38 57.0 13 11 42.43 -10 07 01.0 13 11 50.14 -08 52 26.0 13 11 54.62 -12 41 20.2 13 11 55.92 -12 05 52.4 13 12 00.07 -09 18 18.0 13 12 04.40 -12 52 35.2 13 12 06.72 -02 40 56.0 13 12 12.48 -01 05 42.5 13 12 20.89 -13 16 46.6 13 12 22.54 -12 34 28.6 13 12 26.16 -06 20 25.3 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24462 SUBJECT: LIGO/Virgo S190510g: Updated classification and data quality report DATE: 19/05/10 20:56:46 GMT FROM: Shasvath J. Kapadia at U. of Wisconsin, Milwaukee The LIGO Scientific Collaboration and the Virgo Collaboration report: We continue analyzing the LIGO and Virgo data around the time of the Compact Binary Coalescence (CBC) candidate S190510g (GCN 24442 and GCN 24448): https://gracedb.ligo.org/superevents/S190510g/ A new version of the classification estimation code, which better accounts for the significance of the event using detection-pipeline-specific foreground and background models, was applied to the data. This yields the following updated classification of the GW signal, in order of descending probability: BNS (85%), Terrestrial (15%), NSBH (<1%), BBH (<1%), or MassGap (<1%). This new version of the classification estimation code will be deployed in the front-end of the low latency pipelines on the next detector maintenance intervention on Tuesday, May 14th 2019 15:00UTC. Continued examination of this event also revealed there are data quality issues and non-stationary noise behavior around the time of the event. Its significance may decrease as our estimate of the background improves. If the event is astrophysical, the currently preferred skymap still represents our best estimate of source location. However, the noise characteristics around the time of the event could bias such localizations. Further analysis of the event is ongoing. For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo Public Alerts User Guide . //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24463 SUBJECT: LIGO/Virgo S190510g: Lick/KAIT Follow-Up Observations DATE: 19/05/10 21:18:40 GMT FROM: Weikang Zheng at UC Berkeley Keto Zhang, Thomas de Jaeger, Benjamin Stahl, WeiKang Zheng, James Sunseri, Yukei Murakami, Andrew Hoffman, Emily Ma, Julia Hestenes, Sergiy Vasylyev, and Alexei V. Filippenko (UC Berkeley) report on behalf of the Lick/KAIT GW follow-up team: The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at Lick Observatory, observed the field of the gravitational-wave event S190510g (GCN 24442) 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 303 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 04:26:32, May. 10 UT, about 1.4 hours after the trigger, and the last image at 12:17:12 UT. Our typical limiting mag is 19.0. No viable counterparts were identified and the analysis is ongoing. A full list of galaxies observed by KAIT is given below. GladeID UT(May 10) RA (J2000) Dec (J2000) ----------------------------------------------- G0650384 04:26:32 13:46:10.220 +00:01:22.60 G0711430 04:32:02 14:25:32.320 +01:05:25.10 G0600743 04:39:14 14:55:52.310 +00:33:46.50 G0125934 04:41:06 13:37:14.310 -01:08:19.50 G0612428 04:42:23 12:58:51.500 -17:14:23.30 G0808644 04:43:40 13:43:51.330 -12:13:41.70 G0576307 04:44:56 13:11:34.840 -17:31:40.50 G0629956 04:46:07 12:58:50.810 -17:22:39.00 G0599598 04:47:32 15:18:20.550 +07:49:18.80 G0598294 04:48:48 15:34:23.420 -08:45:52.10 G0573739 04:50:08 14:02:08.470 -09:20:51.30 G0806622 04:51:29 15:18:54.400 +10:49:33.20 G0597451 04:52:48 14:46:05.640 -14:01:38.40 G0790561 04:54:08 15:47:04.880 +08:44:01.70 G0756031 04:55:23 15:12:30.640 +01:41:30.40 G0122092 05:06:58 14:34:50.360 +05:22:26.10 G0800181 05:08:15 13:33:56.620 -03:07:35.10 G0761596 05:09:33 14:36:06.820 +05:16:29.80 G1849600 05:10:44 14:51:48.610 +05:02:20.60 G0720328 05:12:04 13:41:42.330 -04:52:32.60 G0626893 05:13:13 13:43:56.930 -05:09:38.60 G0553544 05:14:22 13:38:20.950 -03:40:52.80 G0568021 05:15:40 14:41:41.460 +03:23:02.20 G0004973 05:18:08 13:40:56.980 +00:44:00.00 G0572321 05:19:24 14:31:41.450 +01:47:47.00 G0750998 05:20:41 13:37:01.000 +00:09:52.10 G0724509 05:21:57 14:34:08.230 +03:51:43.50 G0660276 05:23:15 13:28:57.590 -02:01:28.30 G0044657 05:24:24 13:30:22.630 -04:35:43.10 G0660959 05:25:46 14:58:32.700 +08:12:30.00 G0680774 05:27:02 14:18:34.450 +01:57:53.30 G0788945 05:28:19 13:36:38.510 -01:01:07.40 G0581157 05:29:30 13:45:24.920 +02:00:46.10 G0602455 05:30:39 13:31:31.550 -00:42:09.60 G0774899 05:31:57 14:28:30.690 +04:44:06.50 G0631517 05:33:10 15:02:20.190 +01:33:41.90 G0703829 05:34:22 14:51:11.830 +06:25:43.20 G0750493 05:45:47 13:40:41.320 -06:04:22.40 G0669926 05:46:56 13:46:40.490 -05:36:21.00 G0710006 05:48:13 14:28:16.580 +04:43:00.20 G0653845 05:49:28 13:42:58.330 +00:30:16.10 G0275674 05:50:38 13:37:13.790 -01:08:10.50 G0158239 05:51:47 13:37:44.500 -03:35:45.20 G0610030 05:53:08 14:53:09.090 +04:36:10.90 G1486915 05:54:27 13:40:52.080 +00:44:33.40 G0800724 05:55:36 13:37:51.700 +01:05:24.00 G0273501 05:56:46 13:38:06.080 +00:16:13.20 G0814094 05:57:55 13:37:47.130 +01:03:19.70 G0686579 06:13:02 14:29:31.820 +03:10:35.80 G0494561 06:14:13 14:51:49.580 +05:02:06.40 G0708336 06:15:33 13:41:19.990 -04:53:32.80 G0634594 06:16:42 13:26:45.250 -03:57:53.10 G0665502 06:18:00 14:31:59.060 +05:53:37.60 G0810237 06:37:52 14:53:38.650 +07:51:14.60 G0001044 06:39:09 13:50:12.390 -07:19:11.60 G0817994 06:40:21 13:37:09.180 -08:35:45.90 G0624135 06:41:32 13:41:11.690 +02:22:56.30 G0562882 06:42:43 13:41:43.280 -07:50:52.30 G0650788 06:43:55 13:46:07.980 -02:53:34.80 G0687855 06:45:38 13:22:48.960 -16:31:14.90 G0505015 06:46:47 13:10:23.760 -13:42:09.40 G0652463 06:47:59 13:37:41.070 -08:30:00.80 G0698538 06:49:10 13:21:01.060 -10:34:58.00 G0730033 06:50:21 13:38:15.220 -05:02:22.50 G0616171 06:51:33 13:50:39.050 -06:12:04.80 G0555307 06:53:14 13:38:09.000 +02:33:13.70 G0590897 06:58:47 14:18:36.630 +00:14:25.10 G0035007 07:00:24 14:57:37.080 +06:23:00.20 G0793412 07:01:40 14:48:27.660 +00:56:45.00 G0720022 07:02:51 14:24:07.910 +06:04:03.00 G0609958 07:04:02 14:51:19.760 +10:14:55.30 G0601108 07:05:12 14:56:38.250 +09:30:35.10 G0799448 07:06:31 13:44:44.870 +00:22:11.50 G0792678 07:07:51 14:54:34.470 -00:04:03.10 G0574038 07:09:02 14:36:24.670 +00:15:01.50 G0668231 07:10:13 14:59:38.390 +07:54:32.00 G0596305 07:29:38 14:18:48.990 +00:25:20.20 G0759911 07:31:00 12:51:58.080 -14:26:17.80 G0651733 07:32:09 12:55:07.060 -16:11:17.50 G1851320 07:33:19 12:57:56.340 -18:03:06.00 G0608829 07:34:28 12:58:13.050 -17:30:50.70 G1851307 07:36:07 12:52:16.000 -15:18:22.50 G0860662 07:37:16 12:52:16.080 -15:18:20.30 G0665649 07:38:26 12:54:19.670 -15:38:20.10 G1856321 07:39:35 12:59:33.680 -20:05:18.90 G0762568 07:40:44 12:59:33.230 -18:25:01.30 G0825435 07:41:54 13:06:17.940 -17:32:55.90 G0820468 07:43:05 13:06:29.600 -11:22:15.60 G1175244 07:44:14 13:12:51.000 -08:58:34.70 G0623406 07:45:23 13:14:33.990 -10:51:50.20 G0655184 07:46:33 13:16:02.430 -13:22:22.30 G0801615 07:47:42 13:18:47.250 -15:37:38.10 G0552025 07:48:55 13:18:58.230 -00:24:48.40 G0814012 07:50:09 13:19:02.980 -15:24:46.00 G1433257 07:51:20 13:19:19.340 -04:24:42.70 G0700184 07:52:29 13:19:40.480 -10:43:57.70 G0566980 07:53:41 13:19:56.820 -00:17:59.40 G0827880 07:54:50 13:24:40.070 +01:15:41.30 G0649473 07:56:01 13:24:57.500 -04:29:43.10 G0787749 07:57:11 13:25:11.080 -03:56:04.90 G0772246 07:58:20 13:27:17.110 +00:07:19.00 G0806831 07:59:29 13:28:21.780 -01:06:29.90 G0660292 08:00:41 13:28:25.440 +08:36:46.50 G0283060 08:01:57 13:29:20.790 -14:22:48.60 G0788918 08:03:08 13:31:57.190 -01:50:28.40 G1851429 08:04:18 13:32:10.480 -01:49:46.50 G0487238 08:05:27 13:32:10.690 -01:49:35.50 G0827441 08:06:36 13:32:54.380 -01:32:43.20 G0749829 08:07:45 13:32:59.000 +01:48:07.10 G0765550 08:08:55 13:33:44.280 +00:14:29.10 G0414403 08:10:06 13:34:51.850 -09:13:51.30 G0668924 08:11:15 13:35:02.760 -02:51:59.10 G0811073 08:12:27 13:35:04.210 +02:39:19.20 G0812204 08:13:36 13:35:07.720 +02:13:57.80 G0650083 08:14:45 13:35:43.380 -00:59:48.70 G0676469 08:15:57 13:35:47.290 -12:02:06.30 G0762641 08:17:10 13:35:55.380 -00:16:22.40 G0578072 08:18:19 13:36:04.120 -00:24:16.50 G0582392 08:19:33 13:36:07.410 -15:57:58.10 G0784848 08:20:44 13:36:26.760 -10:14:39.80 G0645795 08:21:55 13:38:01.220 +00:15:43.60 G0695555 08:23:09 13:38:04.760 +03:39:44.80 G0792948 08:24:18 13:38:08.190 +02:34:32.90 G1126565 08:31:41 13:38:14.450 -06:09:20.30 G1346597 08:32:54 13:38:22.350 +06:05:05.40 G0788796 08:34:04 13:38:51.030 +03:50:02.40 G0477760 08:35:17 13:39:34.350 -13:39:44.30 G0636354 08:36:29 13:39:39.430 -04:38:37.90 G0788111 08:37:40 13:39:52.820 +03:16:23.10 G0698851 08:40:01 13:41:32.800 -05:10:10.70 G0711105 08:41:12 13:42:04.490 +01:41:35.20 G0573061 08:42:25 13:42:15.220 -14:44:30.30 G0791457 08:43:35 13:42:40.420 -12:11:58.60 G0815563 08:44:46 13:42:46.260 -04:58:48.60 G0684407 08:45:55 13:42:54.650 +02:24:56.60 G0479347 08:47:05 13:42:54.770 +02:20:26.00 G0563322 08:48:16 13:43:00.270 -04:28:08.20 G0730683 08:49:29 13:43:00.760 +03:31:31.50 G1127151 08:50:39 13:43:14.120 +01:42:13.90 G0617196 08:51:48 13:45:36.880 +00:27:53.40 G0697080 08:52:57 13:45:39.540 +02:45:54.50 G0802136 08:54:06 13:45:56.300 -01:14:24.80 G1473253 08:55:18 13:46:13.940 -06:37:02.90 G0574578 08:56:27 13:46:20.650 -02:03:56.30 G0719849 08:57:38 13:46:23.520 -10:33:10.10 G0826962 08:58:48 13:47:11.210 -11:07:21.90 G0596597 08:59:57 13:49:34.150 -06:40:22.60 G0768556 09:01:06 13:51:21.980 -08:33:04.80 G0593502 09:02:20 13:51:30.770 +03:05:55.00 G0822015 09:03:33 13:52:38.330 -08:55:51.50 G0687515 09:04:44 13:57:24.270 -00:20:30.30 G0555591 09:05:54 14:03:10.260 -00:19:43.20 G0271717 09:07:05 14:05:44.990 -09:48:19.90 G0648520 09:08:14 14:09:08.710 -09:09:47.20 G0783648 09:09:28 14:13:09.900 -10:10:07.00 G0207460 09:10:39 14:15:04.570 +00:52:18.30 G0608535 09:11:48 14:15:26.620 -00:17:04.10 G0717771 09:12:58 14:15:48.260 +03:40:01.00 G0232102 09:14:07 14:15:50.150 +03:02:29.70 G0796975 09:15:16 14:16:07.850 +04:50:13.10 G0602117 09:16:26 14:18:01.310 +00:23:17.70 G0695699 09:17:35 14:18:21.570 -00:03:54.20 G0607064 09:18:44 14:18:27.510 +00:23:37.60 G0614442 09:19:53 14:18:30.010 +00:15:43.20 G0631845 09:23:59 14:27:06.440 +05:09:06.10 G0645566 09:25:10 14:25:10.680 -00:45:56.70 G0583981 09:26:26 14:59:04.230 +03:13:10.00 G0715490 09:27:37 14:39:16.110 -00:25:56.60 G0775953 09:28:57 13:33:19.680 +01:28:04.00 G0792877 09:30:14 14:30:52.930 +07:10:07.90 G1258137 09:31:31 13:44:11.940 +03:44:15.80 G0552562 09:32:50 14:52:20.270 +09:30:48.40 G0159954 09:33:59 14:43:37.110 +05:16:10.50 G0770215 09:35:11 14:30:40.580 +07:10:04.80 G0782845 09:36:29 13:38:17.990 +06:23:15.20 G1851589 09:37:49 14:51:59.380 -00:06:59.10 G0585556 09:39:00 15:02:47.110 +04:51:24.10 G0784007 09:40:41 14:31:08.220 -06:30:50.10 G0855361 09:41:52 14:38:33.720 +07:44:48.50 G0775171 09:43:13 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15:04:25.320 +04:36:30.70 G0738987 11:12:37 15:05:58.560 +05:43:23.20 G0558058 11:13:46 15:12:35.210 +05:19:32.50 G0583283 11:14:55 15:17:41.890 +06:57:04.10 G0798657 11:16:05 15:19:59.630 +04:27:05.10 G0630232 11:17:14 15:22:49.080 +07:38:25.10 G0777754 11:18:23 15:30:26.610 +07:30:28.80 G1856457 11:19:37 15:50:27.600 +00:10:32.10 G0596305 11:21:26 14:18:49.140 +00:25:18.90 G0549862 11:22:35 14:18:57.720 +04:58:52.40 G0594358 11:23:49 14:19:36.290 +07:17:19.70 G0573840 11:24:58 14:19:45.250 +10:45:20.70 G0606388 11:26:09 14:19:49.520 -00:10:55.30 G1123685 11:27:21 14:20:05.680 +07:49:31.40 G0567452 11:28:34 14:20:17.170 -03:51:46.50 G0671077 11:29:44 14:22:54.960 -00:38:40.20 G0643002 11:30:53 14:26:50.110 -02:25:12.10 G0813325 11:32:02 14:29:02.340 -01:56:14.80 G0721949 11:33:18 14:30:34.980 +10:29:56.90 G0690948 11:34:33 14:31:18.930 -01:52:22.50 G0814206 11:35:42 14:36:19.600 -05:31:40.20 G0600204 11:36:52 14:37:16.810 -01:28:14.50 G1850386 11:38:07 14:37:26.640 +11:18:42.00 G0559943 11:39:16 14:39:10.730 +11:28:46.80 G0692513 11:40:32 14:39:45.680 -01:59:58.00 G0675092 11:41:47 14:42:14.510 +10:33:03.10 G0009688 11:42:57 14:42:59.340 +11:59:18.30 G0658340 11:44:12 14:44:04.670 -03:43:40.70 G0031927 11:45:28 14:45:16.500 +12:03:02.80 G0001035 11:46:41 14:45:54.870 +01:52:27.00 G1058466 11:47:55 14:47:49.470 +11:17:57.80 G0765998 11:49:04 14:48:14.600 +09:38:04.70 G0634986 11:50:13 14:49:32.530 +11:14:44.40 G1436476 11:51:23 14:49:54.190 +12:24:39.70 G0566792 11:52:32 14:51:24.220 +11:02:06.20 G0812708 11:53:47 14:59:31.160 -06:53:44.10 G0558644 11:54:59 15:06:18.340 +04:24:21.90 G0787664 11:56:12 15:07:19.610 +06:18:23.00 G0725617 11:57:23 15:09:08.930 +01:10:35.10 G0593641 11:58:35 15:11:15.280 +07:37:58.60 G0616339 11:59:44 15:12:03.180 +04:13:20.10 G0730896 12:00:53 15:12:28.440 +07:10:46.80 G0563214 12:02:03 15:13:44.610 +07:21:46.40 G0635905 12:03:12 15:14:11.940 +04:12:58.40 G0235323 12:04:21 15:17:28.690 +07:40:23.10 G0563336 12:05:31 15:18:47.560 +04:05:34.70 G0564919 12:06:40 15:19:05.970 +05:14:25.80 G0648544 12:07:49 15:21:16.620 +03:26:58.90 G0768102 12:09:01 15:22:51.830 +08:21:19.50 G0768809 12:10:10 15:24:01.970 +08:32:29.20 G0702070 12:11:19 15:26:09.290 +07:05:16.10 G0559285 12:12:28 15:29:40.980 +07:19:18.40 G0759705 12:13:38 15:33:42.080 +04:41:04.10 G0806928 12:14:49 15:41:49.270 +09:41:18.90 G0232365 12:15:58 15:45:24.370 +11:29:25.50 G0781399 12:17:12 15:50:18.870 +00:07:30.20 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24464 SUBJECT: LIGO/Virgo S190510g: J-GEM optical/NIR follow-up observations DATE: 19/05/10 22:34:06 GMT FROM: Koji S. Kawabata at JGEM Kawabata, K. S., Sasada, M., Nakaoka, T., Akitaya, H., Imazato, F., Nishinaka, Y. (Hiroshima U.), Yanagisawa, K., Yoshida, M. (NAOJ), Morokuma, T. (U. of Tokyo), Tominaga N. (Konan U.), Utsumi, Y. (Stanford/SLAC), Yatsu, Y., Murata, K. L. (Tokyo Tech.), Kamei, Y. (Nagoya U.), Tristram, P. (Mt. John U. Observatory), Suematsu, H., Yamawaki, T. (Osaka U.), Matsubayashi, K. (Kyoto U.), Saito, T., Onozato, H. (Nishi-Harima Astronomical Observatory), Itoh, R. (Bisei Astronomical Observatory), Sekiguchi, Y. (Toho U.), Oasa, Y., Takarada, T., Kanai, K., Takeuchi, H., Shigeyoshi, T. (Saitama U.) on behalf of J-GEM collaboration We report our optical and near-infrared imaging observations for the gravitational wave event S190510g. We started our observations about 7.5 hours after the alert. We performed galaxy-targeted observations for 28 galaxies (see the table below) selected from the GLADE catalog (Dalya et al. 2016) in the probability skymap of S190510g using the following telescopes and instruments. - 50 cm MITSuME telescope at Akeno Observatory and a 3 color imager (g, Rc, Ic) - 50 cm MITSuME telescope at Okayama Astrophysical Observatory and a 3 color imager (g, Rc, Ic) - 55 cm SaCRA telescope at Saitama University and MuSaSHI (r, i, z) - 61 cm Boller & Chivens telescope at Mt. John Observatory in New Zealand (B&C) and a three color imager Tripole5 (g, r, i) - 91 cm Okayama Astrophysical Observatory NIR Wide$B!>(BField Camera, OAOWFC (J) (Yanagisawa, K., et al. 2016, Proc. SPIE, 9908, 99085D) - 150 cm Kanata telescope at Higashi-Hiroshima Observatory and HONIR -- a 2 channel imager (Rc and H or J) (Akitaya et al. 2014, 9147, 91474O) - 200 cm Nayuta telescope at Nishi-Harima Astronomical Observatory and Nishiharima Infrared Camera, NIC (J, H, Ks) - 380 cm Seimei telescope at Okayama Observatory and optical-fiber integral field spectrograph, KOOLS-IFU We found no apparent transient object in these galaxies to 5 sigma limiting magnitudes listed below, except for a few marginal cases that are being carefully investigated by spectroscopy. We will post it if it is likely an actual transient. galid ra dec G g r R i I z J H K obsid GL055116-310617 87.8176 -31.1046 -- 19.51 20.06 -- 19.47 -- -- -- -- -- BandC-Tripol GL055150-314446 87.958 -31.7461 -- 19.82 19.81 -- 19.32 -- -- -- -- -- BandC-Tripol GL054828-325838 87.115 -32.9772 -- 18.61 19.01 -- 18.31 -- -- -- -- -- BandC-Tripol GL055050-314427 87.7077 -31.7407 -- 17.25 17.05 -- 16.56 -- -- -- -- -- BandC-Tripol GL055504-313735 88.7683 -31.6263 -- 16.75 16.91 -- 16.25 -- -- -- -- -- BandC-Tripol GL055140-313123 87.9168 -31.5231 -- 18.70 18.97 -- 18.29 -- -- -- -- -- BandC-Tripol GL055352-324437 88.4666 -32.7436 -- 17.75 -- -- 17.18 -- -- -- -- -- BandC-Tripol GL054902-312929 87.2593 -31.4913 -- 14.98 14.89 -- 17.76 -- -- -- -- -- BandC-Tripol GL055123-310146 87.8458 -31.0294 -- 17.40 17.77 -- 17.25 -- -- -- -- -- BandC-Tripol GL055552-320353 88.9671 -32.0647 -- 13.71 13.00 -- 13.38 -- -- -- -- -- BandC-Tripol GL055050-314426 87.7074 -31.7404 -- 17.25 17.05 -- 16.56 -- -- -- -- -- BandC-Tripol GL055349-324625 88.4551 -32.7736 -- 17.75 -- -- 17.18 -- -- -- -- -- BandC-Tripol GL055054-314721 87.726 -31.7891 -- 17.25 17.05 -- 16.56 -- -- -- -- -- BandC-Tripol GL055137-313213 87.9051 -31.537 -- 18.70 18.97 -- 18.29 -- -- -- -- -- BandC-Tripol GL054835-330005 87.147 -33.0013 -- 18.61 19.01 -- 18.31 -- -- -- -- -- BandC-Tripol GL145211+044054 223.0459 4.6818 -- -- -- 21.88 -- -- -- 16.08 19.77 -- OAOWFC,Kanata-HONIR GL055045-314528 87.6857 -31.7579 -- 17.25 17.05 -- 16.56 -- -- -- -- -- BandC-Tripol GL134200+003605 205.4958 0.6015 -- -- 17.40 18.07 18.78 -- 18.78 16.89 15.72 -- OAOWFC,Kanata-HONIR,SaCRA-MuSaSHI GL142718+044810 216.8261 4.8029 18.74 -- -- 21.84 -- 18.04 -- 18.49 19.94 -- OAOWFC,Kanata-HONIR,MITSuME-Akeno GL133953+005024 204.97 0.8399 -- -- 16.64 20.94 18.37 -- 16.64 18.98 18.56 -- Kanata-HONIR,SaCRA-MuSaSHI GL144043+032756 220.1787 3.4654 18.18 -- -- 21.41 -- 17.63 -- 19.01 19.44 99.99 MITSuME-Akeno,Kanata-HONIR,OAOWFC,Nayuta GL134511+000710 206.2954 0.1194 -- -- -- 20.62 -- -- -- 17.57 19.18 -- Kanata-HONIR,OAOWFC GL133648+010914 204.1999 1.1538 -- -- -- 20.34 -- -- -- -- 18.84 -- Kanata-HONIR GL145412+044501 223.5521 4.7502 19.10 -- -- 19.08 -- 18.36 -- -- -- -- MITSuME-Akeno GL133644-032952 204.1844 -3.4978 17.95 -- -- 18.36 -- 17.94 -- -- -- -- MITSuME-Akeno GL133614-010217 204.0588 -1.0381 16.19 -- -- 19.15 -- 16.83 -- -- 17.82 -- MITSuME-Akeno,Kanata-HONIR GL134042-044642 205.175 -4.7784 13.92 -- 15.82 13.34 18.78 13.41 18.78 -- -- -- MITSuME-Okayama,SaCRA-MuSaSHI GL133715-045629 204.3112 -4.9413 14.85 -- -- 20.78 -- 14.39 -- -- 19.27 -- MITSuME-Akeno,Kanata-HONIR //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24465 SUBJECT: LIGO/Virgo S190510g: CNEOST Follow-Up Observations DATE: 19/05/11 00:03:02 GMT FROM: Bin Li at PMO Bin Li, Hai-bin Zhao (PMO),Dong Xu, Zi-pei Zhu, Bang-Yao Yu,Tian-meng Zhang, Xu Zhou,Chen-zhou Cui, Hui-juan Wang(NAOC), Xue-feng Wu, Zhi-ping Jin, Tian-rui Sun, Hao Lu, Ge-tu Zhaori, Ren-quan Hong, Long-fei Hu (PMO), Xiao-feng Wang, Wen-xiong Li (THU),Li-fan Wang (PMO/TAMU), Tian-meng Zhang, Xu Zhou (NAOC), Jin-zhong Liu (XAO), Ji-rong Mao, Jin-ming Bai (YNAO), report on behalf of the CNEOST collaboration. We conducted optical imaging observations in the 50% localization of the BNS merger candidate, S190510g, detected by LIGO/Virgo (GCN #24442; GCN #24448) with Chinese Near Earth Object Survey Telescope (CNEOST) at Xuyi astronomical station in Jiangsu Province, China (32.75N, 118.47E). The information of observations and preliminary results are listed below. The new resulte will available at http://www.cneost.org/opem/list.php?gdate=2019-05-10 Alert: LIGO/Virgo S190510g (GCN #24442; GCN #24448) StartTime (UT): 2019-05-10T12:50:28.882 EndTime (UT): 2019-05-10T16:08:20.544 Skycover (Square Degree): 468.0 Telescope FoV (Square Degree):9.0 #id CentRA(D) CentDEC(D) LimiteMag3_sig 5_sig 10_sig Filter 1 194.681900 -6.772099 20.146 19.182 18.347 VR 2 193.277298 1.611395 20.388 19.429 18.607 VR 3 201.675400 1.593076 20.333 19.376 18.588 VR 4 201.708038 -1.210821 20.342 19.391 18.584 VR 5 196.550156 -3.985157 20.324 19.372 18.544 VR 6 204.972916 -4.021634 20.392 19.430 18.639 VR 7 200.313248 -6.826698 20.042 19.117 18.268 VR 8 201.741806 -9.605056 20.066 19.137 18.270 VR 9 200.856903 -12.393054 20.072 19.115 18.220 VR 10 196.088699 -9.623263 20.140 19.181 18.356 VR 11 193.260544 -1.180493 20.322 19.363 18.535 VR 12 198.905228 1.592129 20.188 19.226 18.423 VR 13 204.490967 -1.201643 20.353 19.383 18.603 VR 14 196.080017 -1.200560 20.328 19.367 18.539 VR 15 202.159622 -4.002045 20.335 19.389 18.566 VR 16 203.151154 -6.804635 20.197 19.245 18.344 VR 17 198.895706 -9.611844 19.975 19.040 18.193 VR 18 203.697418 -12.420897 20.083 19.142 18.267 VR 19 195.085129 -12.402555 20.104 19.149 18.278 VR 20 193.729477 -3.975807 20.104 19.159 18.360 VR 21 196.057327 1.575039 20.284 19.326 18.509 VR 22 204.475555 1.618571 20.388 19.451 18.648 VR 23 198.890839 -1.214557 20.269 19.288 18.486 VR 24 199.370056 -3.989921 20.349 19.399 18.578 VR 25 205.977844 -6.794784 20.267 19.332 18.478 VR 26 197.471542 -6.809984 20.133 19.183 18.371 VR 27 204.595169 -9.631298 20.081 19.156 18.277 VR 28 197.989578 -12.395603 20.063 19.098 18.233 VR 29 207.799149 -4.024509 20.537 19.600 18.804 VR 30 207.752518 4.390663 20.787 19.850 19.091 VR 31 216.195114 4.405424 20.795 19.866 19.054 VR 32 210.057693 1.565380 20.756 19.814 19.042 VR 33 215.674347 -1.192254 20.882 19.907 19.076 VR 34 210.591507 -4.026485 20.662 19.709 18.878 VR 35 217.247604 -6.805941 20.539 19.622 18.803 VR 36 210.298050 -9.601982 20.422 19.480 18.642 VR 37 207.799149 -4.024509 20.537 19.600 18.804 VR 38 207.752518 4.390663 20.787 19.850 19.091 VR 39 216.195114 4.405424 20.795 19.866 19.054 VR 40 210.057693 1.565380 20.756 19.814 19.042 VR 41 215.674347 -1.192254 20.882 19.907 19.076 VR 42 210.591507 -4.026485 20.662 19.709 18.878 VR 43 217.247604 -6.805941 20.539 19.622 18.803 VR 44 210.298050 -9.601982 20.422 19.480 18.642 VR 45 207.799149 -4.024509 20.537 19.600 18.804 VR 46 207.752518 4.390663 20.787 19.850 19.091 VR 47 216.195114 4.405424 20.795 19.866 19.054 VR 48 210.057693 1.565380 20.756 19.814 19.042 VR 49 215.674347 -1.192254 20.882 19.907 19.076 VR 50 210.591507 -4.026485 20.662 19.709 18.878 VR 51 217.247604 -6.805941 20.539 19.622 18.803 VR 52 210.298050 -9.601982 20.422 19.480 18.642 VR Detailed data analysis is still in progress and any interesting transients will be reported later. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24466 SUBJECT: LIGO/Virgo S190510g: KMTNet observation DATE: 19/05/11 01:35:31 GMT FROM: Myungshin Im at Seoul Nat U Myungshin Im (SNU), Joonho Kim (SNU), Chung-Uk Lee (KASI), Seung-Lee Kim (KASI), Gregory S. H. Paek (SNU), Gu Lim (SNU), Changsu Choi (SNU), Sungyong Hwang (SNU), Bomi Park (SNU), Sophia Kim (SNU), Hyung Mok Lee (KASI), on behalf of a larger collaboration With KMTNet, we observed the whole 60\% credible region of the updated localization map of the BNS merger candidate, S190510g (LIGO/Virgo GCN 24448). The observation took place at the KMTNet South Africa (SAAO) and Chile (CTIO) stations, starting at 2019-5-10 16:38 UT. The images were taken in R-band with 240 sec exposure time to the depth of R ~ 21.7 (5-sigma detection). The search for transients is ongoing, although no obvious transient has been identified so far. We thank the KMTNet staffs for performing the observation. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24467 SUBJECT: LIGO/Virgo S190510g: Optical Counterpart Candidates from DECam-GROWTH DATE: 19/05/11 02:18:53 GMT FROM: Igor Andreoni at Caltech Igor Andreoni (Caltech), Daniel A. Goldstein (Caltech), Shreya Anand (Caltech), Mansi M. Kasliwal (Caltech), Michael S. Medford (UC Berkeley), Christoffer Fremling (Caltech), Michael Coughlin (Caltech), Tomas Ahumada (UMD), Pradip Gatkine (UMD), Peter E. Nugent (LBNL), Joshua S. Bloom (UC Berkeley), Keming Zhang (UC Berkeley), Jeff Cooke (Swinburne/OzGrav), Jorge Martínez Palomera (UC Berkeley), Ashish Mahabal (Caltech), Leo P. Singer (NASA GSFC), Sara Webb (Swinburne/OzGrav), Ariel Goobar (OKC), Harsh Kumar (IITB), Varun Bhalerao (IITB), Samaya Nissanke (UvA) on behalf of the Global Relay of Observatories Watching Transients Happen (GROWTH) collaborations: Starting on 2019 May 10 22:56 UTC, we observed the high-probability region of the LALInference skymap of gravitational wave source S190510g (LIGO/VIRGO Collaboration, GCN #24448) using the Dark Energy Camera (DECam) on the Victor M. Blanco 4m Telescope at Cerro Tololo Inter-American Observatory, Chile, continuing the observations described in Andreoni et al. (2019; GCN #24443). We covered 78.9 deg^2 of the localization region and 66% of the probability in the r and z filters to average limiting magnitudes of 23.1 (r-band) and 21.9 (z-band), obtaining 1 epoch in z and 1 in r. We obtained g-band for roughly 85% of the fields to a limiting magnitude of 22.9. We performed difference imaging in real-time using an automated pipeline we developed for gravitational wave counterpart searches, taking reference images from the Dark Energy Survey and the Dark Energy Camera Legacy Survey, covering 100% of the observed area. Below is a preliminary list of interesting candidates based on our real-time pipeline. Each candidate has at least two detections in two different filters and a prominent host galaxy. ---------------------------------------------------------------------------------- Name | RA | Dec |filter| mag | err |filter| mag | err ---------------------------------------------------------------------------------- DG19lcnl | 87.14690 | -35.99441 | r | 19.45 | 0.02 | g | 20.27 | 0.04 DG19ukvo | 89.21146 | -33.44248 | r | 21.57 | 0.07 | g | 21.54 | 0.12 DG19nanl | 87.31139 | -35.95584 | r | 20.01 | 0.03 | g | 20.33 | 0.05 DG19zaxn | 92.30795 | -35.14981 | r | 20.81 | 0.06 | g | 20.88 | 0.06 DG19etsk | 89.10091 | -30.47397 | r | 20.83 | 0.06 | g | 20.61 | 0.06 DG19yhhm | 91.93699 | -30.82476 | r | 20.13 | 0.03 | g | 20.06 | 0.04 DG19llhk | 90.86311 | -32.38554 | r | 21.14 | 0.07 | z | 21.12 | 0.12 DG19fqqk | 92.85149 | -36.51731 | r | 20.43 | 0.03 | z | 20.59 | 0.09 DG19yhhm | 91.93699 | -30.82476 | r | 20.13 | 0.03 | z | 20.35 | 0.10 DG19bexl | 90.45378 | -28.66039 | r | 21.10 | 0.08 | z | 21.03 | 0.16 DG19ootl | 87.03556 | -36.07611 | r | 21.74 | 0.10 | z | 21.51 | 0.14 DG19nouo | 92.00130 | -31.66915 | r | 21.19 | 0.08 | g | 21.43 | 0.11 DG19oahn | 86.33527 | -26.84768 | r | 19.30 | 0.02 | z | 18.97 | 0.03 We note that the host of DG19llhk is at z=0.07, consistent with the current LVC distance estimate. At this distance, the absolute magnitude would be -16.4, consistent with GW170817 at +1 day. We also note that the colors of DG19lcnl appear consistent with GW170817, but we do not have a host redshift. However, we caution that we do not have any constraints on the light curve history and hence, the phase of this event. We strongly encourage spectroscopic follow-up to classify these transients. We thank the CTIO staff, Steve Heathcote, Kathy Vivas, Tim Abbott, for facilitating these Target of Opportunity observations. GROWTH is a worldwide collaboration comprising Caltech, USA; IPAC, USA, WIS, Israel; OKC, Sweden; JSI/UMd, USA; U Washington, USA; DESY, Germany; MOST, Taiwan; UW Milwaukee, USA; LANL USA; Tokyo Tech, Japan; IIT-B, India; IIA, India; LJMU, UK; TTU USA and USyd, Australia. GROWTH acknowledges generous support of the NSF under PIRE Grant No 1545949. An optimized schedule was generated using the ToO marshal system (Coughlin et al. 2019). Alert filtering and follow-up co-ordination is being undertaken by the GROWTH marshal system (Kasliwal et al. 2019). This research draws upon DECam data as distributed by the Science Data Archive at NOAO. NOAO is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. This project used data obtained with the Dark Energy Camera (DECam), which was constructed by the Dark Energy Survey (DES) collaboration. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24468 SUBJECT: LIGO/Virgo S190510g: SOAR/Goodman follow-up observations DATE: 19/05/11 03:44:04 GMT FROM: Charles Kilpatrick at UC Santa Cruz C. D. Kilpatrick, M. R. Siebert, J. S. Brown, D. A. Coulter, G. Dimitriadis, R. J. Foley, C. Rojas-Bravo, K. Siellez, T. Hung, D. O. Jones, A. Murguia-Berthier, J. X. Prochaska, E. Ramirez-Ruiz (UCSC), J. A. Smith (Austin Peay State University), M. Wiesner (Benedictine University), F. Berlfein, A. Garcia, M. Pereira, M. Soares-Santos (Brandeis University), I. Souza (CBPF), M. Makler, I. Souza (CBPF/Brazil), B. Madore, A. L. Piro (Carnegie), H.-Y. Chen (Harvard), R. Kirshner (CfA), B. Metzger (Columbia University), D. Scolnic (Duke University), S. Allam, J. Annis, M. Butner, H. T. Diehl, A. Drlica-Wagner, J. Frieman, K. Herner, N. Kuropatkin, H. Lin, E. Neilsen, A. Palmese, D. Tucker, B. Yanny (Fermilab), J. Horvath, L. Rocha (IAG-USP/Brazil), A. Bernardo (IAS-USP/Brazil), P. Barchi, R. de Carvalho (INPE/Brazil), R. Butler, S. Salim (Indiana University), A. Riess (JHU), N. Tominaga (Konan U/Japan), J. Vinko (Konkoly Observatory), K. Bechtol (LSST), J. Burke, D. Hiramatsu, C. McCully (Las Cumbres Observatory), D. Haggard (McGill University), Y. Pan, M. Tanaka, M. Yoshida, M. Yoshida (NAOJ), R. Gruendl, F. Paz-Chinchon (NCSA), K. Vivas, A. Walker, A. Zenteno (NOAO), F. Bauer, A. Clocchiatti (Pontificia Universidad Catolica de Chile), K. Spekkens (Royal Military College of Canada), S. Jha (Rutgers University), A. Calamida, C. Contreras, G. Narayan, A. Rest (STScI), M. Gill, Y. Utsumi (Stanford), J. Cooke (Swinburne University of Technology), I. Arcavi (Tel Aviv University), K. Krisciunas, N. Suntzeff, L. Wang (Texas A&M), A. Corsi (Texas Tech University), A. Horesh (The Hebrew University), X. Wang (Tsinghua University), J. S. Bloom, T. Brink, A. V. Filippenko, D. Kasen, E. Quataert, W. Zheng (UC Berkeley), A. Bostroem, S. Valenti (UC Davis), A. Howell (UC Santa Barbara), R. Sturani (UFRN/Brazil), S. Rembold (UFSM/Brazil), T. Davis (UQ/Australia), O. Rodri (Universidad Andres Bello), F. Forster-Buron (Universidad de Chile), W. Hartley, O. Lahav (University College London), J. Andrews, M. Lundquist, D. Sand (University of Arizona), Z. Doctor, M. Fishbach, W. Freedman, D. Holz, R. Kessler (University of Chicago), P. M. Garnavich (University of Notre Dame), C. Conselice (University of Nottingham), D. Brout, C. D'Andrea, M. Sako (University of Pennsylvania), C. Frohmaier, A. Lundgren, R. Nichol, L. Nuttall (University of Portsmouth), M. Smith, M. Sullivan (University of Southampton), J. C. Wheeler (University of Texas/Austin), M. Drout (University of Toronto), R. Morgan (University of Wisconsin-Madison), K. Lukosiute (Wellesley College) report on behalf of the 1M2H and DESGW collaborations: In the process of searching the localization region of LIGO/Virgo S190510g (LIGO/VIRGO Collaboration, GCN #24448), we obtained 3-minute r-band exposures of the following regions with the Goodman High Throughput Spectrograph on the SOAR 4-m telescope. The field of view is a 7.2-arcmin diameter circle. The approximate center of each image is noted in the table below. We also note the approximate 3-sigma limiting magnitude of each image. Comparing our images to DES DR1 r-band images of the same fields, we did not detect any transient sources. RA (J2000) | DEC (J2000) | MJD | Limiting Magnitude 06:06:00.86 | -32:47:28.55 | 58613.9634598 | 21.3 05:51:48.47 | -31:28:21.43 | 58613.9697709 | 21.6 05:55:10.63 | -32:04:19.33 | 58613.9807059 | 21.7 05:59:44.38 | -32:54:47.42 | 58613.9842936 | 21.7 06:07:49.70 | -33:30:45.58 | 58613.9875954 | 21.7 05:51:48.38 | -31:21:10.17 | 58613.9908477 | 21.6 05:59:08.22 | -32:04:26.44 | 58613.9943430 | 21.7 05:50:37.29 | -32:18:50.38 | 58613.9979812 | 21.6 05:52:16.38 | -33:38:02.52 | 58614.0014418 | 21.6 05:58:02.52 | -34:06:49.28 | 58614.0052499 | 21.6 05:50:31.75 | -33:45:17.44 | 58614.0084120 | 21.5 05:53:24.15 | -34:21:14.39 | 58614.0116271 | 21.6 05:47:57.74 | -30:23:38.45 | 58614.0149357 | 21.5 05:51:38.62 | -34:28:28.46 | 58614.0181796 | 21.5 05:52:18.83 | -32:47:42.32 | 58614.0222639 | 21.5 05:55:44.58 | -32:04:30.50 | 58614.0257728 | 21.4 05:52:47.96 | -34:42:54.55 | 58614.0289522 | 21.5 05:59:41.23 | -31:42:57.35 | 58614.0323124 | 21.4 06:00:24.86 | -35:11:38.23 | 58614.0357864 | 21.4 06:09:01.75 | -33:52:31.40 | 58614.0391655 | 21.4 06:11:07.09 | -32:33:16.39 | 58614.0432460 | 21.4 We did not cover the location of any candidate identified in Andreoni et al. (GCN #24467). We would like to thank Jay Elias for facilitating these Target of Opportunity observations. Please direct all communication related to this circular to Charlie Kilpatrick (cdkilpat@ucsc.edu). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24469 SUBJECT: LIGO/Virgo S190510g: Insight-HXMT/HE updated observation DATE: 19/05/11 04:45:33 GMT FROM: Qi Luo at IHEP Q. Luo, C. Cai, Q. B. Yi, S. Xiao, C. K. Li, X. B. Li, G. Li, J. Y. Liao, S. L. Xiong, C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, M. Wu, Y. P. Xu, S. N. Zhang (IHEP), report on behalf of the Insight-HXMT team: Following up on the updated localization (GCN #24448), we have re-analyzed Insight-HXMT/HE data of S190510g (GCN #24451). The previous estimated location we used (GCN #24451) is RA = 190.0, Dec = 0.0 (J2000, degrees). And the updated estimated location we used is RA = 90.0, Dec = -34.0 (J2000, degrees). Insight-HXMT was taking data normally around the GW trigger time (T0=2019-05-10 02:59:39 UTC). For the preferred sky map (GCN #24448), at T0, all of the LIGO localization region was covered by Insight-HXMT without occultation by the Earth. Within T0 +/- 100 s, no significant excess events (SNR > 3 sigma) are found in a search of the Insight-HXMT/HE raw light curves. Assuming the GW counterpart GRB with three typical GRB Band spectral models, two typical duration timescales (1 s, 10 s) from the peak position of the LIGO-Virgo location probability map, 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: 5.5e-08 erg cm^-2 10 s: 1.5e-07 erg cm^-2 Band model 2 (alpha=-1.0, beta=-2.3, Ep=230 keV): 1 s: 9.2e-08 erg cm^-2 10 s: 2.6e-07 erg cm^-2 Band model 3 (alpha=-0.0, beta=-1.5, Ep=1000 keV): 1 s: 2.4e-07 erg cm^-2 10 s: 8.3e-07 erg cm^-2 All measurements above are made with the CsI detectors operating in the regular mode with the energy range of about 80-800 keV (deposited energy). Only gamma-rays with energy greater than about 200 keV can penetrate the spacecraft and leave signals in the CsI detectors installed inside of the spacecraft. Insight-HXMT is the first Chinese space X-ray telescope, which was funded jointly by the China National Space Administration (CNSA) and the Chinese Academy of Sciences (CAS). More information could be found at: http://www.hxmt.org. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24470 SUBJECT: LIGO/Virgo S190510g: MASTER possible OT in PGC094244 galaxy DATE: 19/05/11 05:22:00 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, F.Balakin, N.Tyurina, E. Gorbovskoy, V.Kornilov, D.Vlasenko, V.Vladimirov, D.Zimnukhov, A.Kuznetsov, P.Balanutsa, I.Gorbunov, A. Chasovnikov, V.Grinshpun, T.Pogrosheva (Lomonosov Moscow State University, SAI, Physics Department), A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres (The Instituto de Astrofisica de Canarias), R. Podesta, C. Lopez, C.Francile, F. Podesta (Observatorio Astronomico Felix Aguilar OAFA, San Juan National University), H.Levato (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE,SJNU) D. Buckley (South African Astronomical Observatory), O. Gress, N.M. Budnev, O.Ershova (Applied Physics Institute, Irkutsk Stat University), V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev (Blagoveschensk EducationState University), OT MASTER140133.93-110805.8 in PGC094244 galaxy. MASTER-Kislovodsk auto-detection system discovered OT source at (RA, Dec) = 14h 01m 33.93s -11d 08m 05.8s on 2019-05-10.82038 UT. The OT unfiltered magnitude is ~19.0m (limit 19.2m). The OT is seen in 2 unfiltered images. There is no minor planet at this place. We have reference image without OT on 2014-05-26.82247 UT with unfiltered magnitude limit 19.8m. There is PGC094244 galaxy near OT. OT offset is 36W 22.6S . The galaxy distance is ~300 Mpc . Follow up observations are required. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24473 SUBJECT: LIGO/Virgo S190510g: Pierre Auger Observatory follow-up DATE: 19/05/11 08:14:07 GMT FROM: Jaime Alvarez-Muniz at Pierre Auger Observatory J. Alvarez-Muniz, F. Pedreira, E. Zas (Univ. Santiago de Compostela, Spain), K. H. Kampert & M. Schimp (Bergische Universitat, Wuppertal, Germany) on behalf of the Pierre Auger Collaboration. In response to: LIGO/Virgo GW trigger S190510g T0=2019-05-10 02:59:39 UTC We searched for Ultra-High-Energy (UHE) neutrinos with energies above ~ 1e17 eV in data collected with the Surface Detector (SD) of the Pierre Auger Observatory in a [-500,500] second interval about the LIGO-Virgo trigger S190510g as well as 1 day after it. The field of view (fov) where the SD of Auger is sensitive to UHE neutrinos (corresponding to inclined directions with respect to the vertical relative to the ground) was PARTIALLY COINCIDENT (18.1%) with the LIGO 90% localization region at the time T0 of the merger alert, achieving MAXIMUM OVERLAP (78.8%) at approximately T0+5.9 hours. NO events survived the cuts applied to reject the background due to UHE Cosmic Rays i.e. NO NEUTRINO CANDIDATES WERE DETECTED. ------- The Pierre Auger Observatory is an UHE Cosmic Ray detector located in the Mendoza Province in Argentina. It consists of an array of Water Cherenkov detectors spread over a total surface of 3000 km^2 arranged in a triangular grid of 1.5 km side as well as Fluorescence telescopes and other systems (see 10.1016/j.nima.2015.06.058 for more information). For neutrino searches from GW events with Auger, please refer to: https://journals.aps.org/prd/pdf/10.1103/PhysRevD.94.122007 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24474 SUBJECT: LIGO/Virgo S190510g: DESGW counterpart candidate (desgw-190510a) DATE: 19/05/11 08:42:33 GMT FROM: James Annis at Fermilab LIGO/Virgo S190510g: DESGW counterpart candidate (desgw-190510a) Jim Annis for the DESGW collaboration We report a candidate counterpart to the binary neutron star merger S190510g reported by LIGO/VIRGO Collaboration (GCN Circular No. 24442, updated GCN Circular No. 24448). The region was imaged by DECam on the night of 2019 May 10 (GCN Circular No. 24467). The candidate was identified by visual inspection of 566 galaxies nearby galaxies within the 50% localization probability region of the merger. The visual inspection compared the new images with deep pre-existing imaging data obtained by the Dark Energy Survey. The transient appears in our g,r,z images. Transient: desgw-190510a Coordinates: 91.52679, -35.54160 ( 6:06:06.429,-35:32:29.77 ) g mag: 22.5 +/- 0.2 r mag: 20.9 +/- 0.05 z mag: 20.7 +/- 0.1 These magnitudes are as observed, uncorrected for reddening. Host galaxy: 2MASS06060625-3532351 Coordinates: 91.52605, -35.54311 ( 6:06:06.252,-35:32:35.20 ) Radius of galaxy: 6.6’ J mag: 14.64 Redshift: 0.089 (2MPZ photo-z) DESGW collaboration: Sahar Allam (Fermilab), James Annis (Fermilab), Iair Arcavi (Tel Aviv University), Paulo Barchi (INPE/Brazil), Keith Bechtol (LSST), Federico Berlfein (Brandeis U), Antonio Bernardo (IAG-USP/Brazil), Dillon Brout (University of Pennsylvania), Robert Butler (Indiana University), Melissa Butner, (Fermilab), Annalisa Calamida (STScI), Hsin-Yu Chen (Harvard U), Chris Conselice (University of Nottingham), Carlos Contreras (STScI), Jeff Cooke (Swinburne University), Chris D’Andrea (University of Pennsylvania), Tamara Davis (UQ/Australia), Reinaldo de Carvalho (NAT - Universidade Cruzeiro do Sul/Universidade Cidade de Sao Paulo), H. Thomas Diehl (Fermilab), Zoheyr Doctor (U Chicago), Alex Drlica-Wagner (Fermilab), Maria Drout (U Toronto), Maya Fishbach (U Chicago), Francisco Forster (U de Chile/Chile), Ryan Foley (UCSC), Joshua Frieman (Fermilab & University of Chicago), Chris Frohmaier (University of Portsmouth), Ori Fox (STScI), Alyssa Garcia (Brandeis U), Juan Garcia-Bellido (Universidad Autonoma de Madrid), Mandeep Gill (SLAC/Stanford U), Robert Gruendl (NCSA), Will Hartley (University College London), Kenneth Herner (Fermilab), Daniel Holz (U Chicago), Jorge Horvath (IAG-USP/Brazil), D. Andrew Howell (Las Cumbres Observatory), Richard Kessler (University of Chicago), Charles Kilpatrick (UCSC), Nikolay Kuropatkin (Fermilab), Ofer Lahav (University College London), Huan Lin (Fermilab), Andrew Lundgren (Portsmouth), Martin Makler (CBPF/Brazil), Curtis McCully (Las Cumbres Observatory), Robert Morgan (University of Wisconsin-Madison), Gautham Narayan (STScI), Eric Neilsen (Fermilab), Robert Nichol (University of Portsmouth), Antonella Palmese (Fermilab), Francisco Paz-Chinchon (NCSA & UIUC), Maria Pereira (Brandeis University), Sandro Rembold (UFSM/Brazil), Armin Rest (STScI & JHU), Livia Rocha (IAG-USP/Brazil), Russell Ryan (STScI), Masao Sako (University of Pennsylvania), Samir Salim (Indiana University), David Sand (U of Arizona), Daniel Scolnic (Duke University), J. Allyn Smith (Austin Peay State University), Mathew Smith (University of Southampton), Marcelle Soares-Santos (Brandeis U), Lou Strolger (STScI), Riccardo Sturani (UFRN/Brazil), Mark Sullivan (University of Southampton), Masaomi Tanaka (NAOJ/Japan), Nozomu Tominaga (Konan U/Japan), Douglas Tucker (Fermilab), Yousuke Utsumi (Stanford U), Stefano Valenti (UC Davis), Kathy Vivas (NOAO/CTIO), Alistair Walker (NOAO/CTIO), Sara Webb (Swinburne University), Matt Wiesner (Benedictine University), Brian Yanny (Fermilab), Michitoshi Yoshida (NAOJ/Japan), Alfredo Zenteno (NOAO/CTIO), Luidhy Santana-Silva (Valongo Observatory) This project used data obtained with the Dark Energy Camera (DECam), which was constructed by the Dark Energy Survey collaboration, and draws on upon data as distributed by the Science Data Archive at NOAO. NOAO is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24475 SUBJECT: LIGO/Virgo S190510g: Xinglong/Schmidt Follow-Up Observations DATE: 19/05/11 09:38:48 GMT FROM: Dong Xu at NAOC/CAS Z.P. Zhu, D. Xu, B.Y. Yu, T.M. Zhang, X. Zhou, X.M. Teng, P.F. Liu, X. N. Guan, H.J. Wang, C.Z. Cui, D.W. Fan, Y.F. Xu (NAOC), S. Yang (INAF-OAPd), H.B. Zhao, B. Li (PMO), J.Z. Liu, H.B. Niu (XAO), J.R. Mao, J.M. Bai (YNAO), X. Gao (Urumqi No.1 Senior High School), report on behalf of the GWFUNC collaboration: We performed the search for the optical counterpart of LIGO/Virgo S190510g (LVC, GCN 24442) using the 0.9-m Schmidt telescope located at Xinglong, Hebei, China. Observations started at 12:50:37 UT on 2019-05-10 and ended at 18:39:16 UT on 2019-05-10, and the 1.5 x 1.5 deg^2 imager scanned relatively high probability regions of the LVC localization that are accessible to the Xinglong/Schmidt telescope. The unfiltered images were taken with 60 sec exposure time and typical limiting depth is around 18.5 mag. Below listed are the field centers observed. RA(J2000) DEC(J2000) 13:27:04.200 +02:54:36.00 13:33:04.800 +02:53:57.00 13:38:46.100 +02:54:04.00 13:27:42.000 +04:23:47.00 13:33:29.900 +04:24:04.00 13:39:29.300 +04:24:08.00 13:27:58.390 +05:53:48.00 13:32:47.200 +05:54:02.00 13:38:41.700 +05:54:05.00 13:25:40.400 -01:36:36.00 13:30:58.590 -01:36:02.00 13:36:36.600 -01:35:57.00 13:25:00.000 -00:06:21.00 13:30:59.990 -00:06:01.00 13:37:00.600 -00:05:57.00 13:24:58.500 +01:23:38.00 13:30:56.700 +01:23:59.00 13:36:58.300 +01:24:03.00 13:42:59.190 -01:35:59.00 13:48:57.790 -01:35:49.00 13:54:59.590 -01:35:44.00 13:42:59.700 -00:05:46.00 13:49:00.000 -00:05:53.00 13:54:59.690 -00:05:40.00 13:42:58.290 +01:23:52.00 13:48:32.500 +01:24:12.00 13:54:48.900 +01:24:15.00 13:27:37.600 -06:06:12.00 13:33:29.800 -06:06:00.00 13:39:30.800 -06:05:56.00 13:27:31.400 -04:36:25.00 13:33:32.200 -04:35:56.00 13:39:30.900 -04:35:55.00 13:27:29.000 -03:05:51.00 13:33:30.100 -03:06:02.00 13:39:31.290 -03:05:56.00 14:21:26.200 +02:54:44.00 14:27:12.790 +02:54:45.00 14:33:19.100 +02:54:50.00 14:21:38.600 +04:24:25.00 14:27:12.590 +04:24:46.00 14:33:13.090 +04:24:50.00 14:21:57.890 +05:54:37.00 14:27:13.200 +05:54:46.00 14:33:41.100 +05:54:51.00 14:39:44.300 +02:54:57.00 14:45:25.600 +02:55:02.00 14:51:22.800 +02:55:09.00 14:39:40.400 +04:25:05.00 14:45:28.800 +04:25:00.00 14:50:45.490 +04:25:09.00 14:39:58.600 +05:54:56.00 14:45:15.190 +05:55:04.00 14:51:43.090 +05:55:16.00 13:45:31.900 -06:05:48.00 13:51:19.200 -06:05:48.00 13:57:02.000 -06:05:43.00 13:45:37.800 -04:35:48.00 13:51:35.000 -04:35:47.00 13:57:32.200 -04:35:41.00 13:45:39.100 -03:05:44.00 13:51:31.700 -03:05:50.00 13:57:31.900 -03:05:42.00 14:47:43.790 +07:24:57.00 14:53:54.800 +07:25:13.00 14:59:56.500 +07:25:18.00 14:47:52.300 +08:54:32.00 14:54:00.100 +08:55:17.00 15:00:00.990 +08:55:18.00 14:48:00.100 +10:24:57.00 14:54:03.790 +10:25:12.00 15:00:03.800 +10:25:26.00 14:29:40.400 +07:24:50.00 14:29:50.890 +07:24:50.00 14:29:50.890 +07:24:50.00 14:29:38.400 +08:54:58.00 14:35:43.000 +08:54:50.00 14:41:45.600 +08:54:59.00 14:30:07.600 +10:24:40.00 14:35:33.300 +10:24:58.00 14:41:31.500 +10:24:59.00 14:37:00.800 -01:35:07.00 14:42:51.890 -01:35:02.00 14:48:30.600 -01:34:54.00 14:37:11.290 -00:05:13.00 14:42:32.200 -00:05:00.00 14:48:27.600 -00:04:53.00 14:37:04.800 +01:24:42.00 14:42:54.700 +01:25:00.00 14:48:41.390 +01:25:08.00 14:18:44.800 -01:35:26.00 14:24:52.200 -01:35:19.00 14:30:47.900 -01:35:12.00 14:19:08.790 -00:05:36.00 14:25:00.800 -00:05:12.00 14:30:33.800 -00:05:12.00 14:19:07.000 +01:24:23.00 14:25:00.100 +01:24:47.00 14:30:30.890 +01:24:48.00 13:45:48.100 +02:54:01.00 13:51:23.200 +02:54:13.00 13:57:09.200 +02:54:17.00 13:45:38.890 +04:23:56.00 13:50:57.600 +04:24:13.00 13:57:32.500 +04:24:22.00 13:45:37.500 +05:54:01.00 13:51:14.300 +05:54:14.00 13:57:13.490 +05:54:18.00 14:57:54.700 +02:55:13.00 15:03:41.600 +02:55:24.00 15:09:44.690 +02:55:31.00 14:57:52.300 +04:25:23.00 15:03:43.790 +04:25:25.00 15:09:18.300 +04:25:31.00 14:57:54.490 +05:54:43.00 15:03:45.290 +05:55:25.00 15:09:43.290 +05:55:31.00 13:34:58.900 +07:24:03.00 13:40:47.400 +07:24:02.00 13:47:06.400 +07:24:09.00 13:35:04.590 +08:53:46.00 13:40:09.500 +08:54:05.00 13:47:08.800 +08:54:10.00 13:35:03.600 +10:24:05.00 13:40:29.690 +10:24:05.00 13:46:49.590 +10:24:10.00 14:55:11.900 -01:34:45.00 15:00:58.800 -01:34:41.00 15:07:16.700 -01:34:33.00 14:55:11.300 -00:04:41.00 15:00:26.000 -00:04:42.00 15:06:07.400 -00:04:32.00 14:55:02.700 +01:25:20.00 15:00:58.200 +01:25:22.00 15:06:59.000 +01:25:27.00 14:11:25.300 +07:24:21.00 14:16:38.690 +07:24:36.00 14:22:40.490 +07:24:41.00 14:11:24.900 +08:54:34.00 14:17:55.400 +08:54:36.00 14:23:07.990 +08:54:41.00 14:11:40.700 +10:24:18.00 14:16:32.190 +10:24:36.00 14:23:03.390 +10:24:41.00 14:03:48.200 +02:54:12.00 14:08:13.700 +02:54:27.00 14:15:21.300 +02:54:32.00 14:03:44.100 +04:24:27.00 14:09:21.890 +04:24:32.00 14:15:26.000 +04:24:32.00 14:03:31.790 +05:54:16.00 14:09:37.790 +05:54:29.00 14:15:35.100 +05:54:32.00 14:43:29.400 +11:55:14.00 14:49:28.000 +11:55:04.00 14:55:21.690 +11:55:14.00 14:43:17.290 +13:25:06.00 14:49:14.900 +13:25:07.00 14:55:41.100 +13:25:15.00 14:43:15.300 +14:54:59.00 14:49:29.000 +14:55:07.00 14:55:14.100 +14:55:15.00 Data analysis is ongoing. Optical transients from the above fields, if interesting, will be reported later. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24476 SUBJECT: LIGO/Virgo S190510g: Dabancheng/HMT Follow-Up Observations DATE: 19/05/11 09:53:20 GMT FROM: Dong Xu at NAOC/CAS Z.P. Zhu, D. Xu, B.Y. Yu, T.M. Zhang, X. Zhou, H.J. Wang, C.Z. Cui, D.W. Fan, Y.F. Xu (NAOC), X. Gao (Urumqi No.1 Senior High School), S. Yang (INAF-OAPd), H.B. Zhao, B. Li (PMO), J.Z. Liu, H.B. Niu (XAO), J.R. Mao, J.M. Bai (YNAO), report on behalf of the GWFUNC collaboration: We performed the search for the optical counterpart of LIGO/Virgo S190510g (LVC, GCN 24442) using the Half-Meter Telescope (HMT) located at Dabancheng, Xinjiang, China. Observations started at 16:00:00 UT on 2019-05-10 and ended at 22:32:00 UT on 2019-05-10, and the 60x40 arcmin^2 unfiltered imager scanned relatively high probability regions of the LVC localization that are accessible to HMT. The total area is about 97 deg^2, and listed below are the field centers observed. RA DEC 13:31:59 +00:39:25 13:31:59 +00:40:37 13:31:59 +00:40:37 13:32:00 +00:00:36 13:32:29 -01:19:26 13:32:30 +01:20:38 13:32:29 -01:59:27 13:32:30 +02:00:39 13:32:29 -02:39:28 13:32:29 +02:40:40 13:33:58 -03:19:30 13:33:59 +03:20:42 13:33:58 -03:59:31 13:33:59 +04:00:43 13:33:58 -04:39:32 13:33:59 +04:40:44 13:36:00 +00:39:25 13:36:00 +00:00:36 13:36:00 +00:40:37 13:36:00 +00:00:36 13:36:00 +00:40:37 13:36:29 -01:19:26 13:36:30 +01:20:38 13:36:29 -01:59:27 13:36:30 +02:00:39 13:36:29 -02:39:28 13:36:30 +02:40:40 13:36:28 -05:19:33 13:36:27 -05:59:34 13:36:27 -06:39:36 13:37:59 -03:19:30 13:37:59 -03:59:31 13:37:59 -04:39:32 13:38:00 +03:20:42 13:38:00 +04:00:43 13:38:00 +04:40:44 13:40:00 +00:39:25 13:40:00 +00:00:36 13:40:00 +00:40:37 13:40:00 +00:00:36 13:40:00 +00:40:37 13:40:29 -01:19:26 13:40:30 +01:20:38 13:40:29 -01:59:27 13:40:30 +02:00:39 13:40:29 -02:39:28 13:40:30 +02:40:40 13:40:29 -05:19:33 13:40:29 -05:59:34 13:40:29 -06:39:36 13:41:59 -03:19:30 13:41:59 -03:59:31 13:41:59 -04:39:32 13:42:00 +03:20:42 13:42:00 +04:00:43 13:42:01 +04:40:44 13:43:59 +00:39:25 13:43:59 +00:40:37 13:43:59 +00:40:37 13:44:00 +00:00:36 13:44:29 -01:19:26 13:44:30 +01:20:38 13:44:29 -01:59:27 13:44:30 +02:00:39 13:44:29 -02:39:28 13:44:30 +02:40:40 13:44:30 -05:19:33 13:44:30 -05:59:34 13:44:30 -06:39:36 13:48:00 +00:39:25 13:48:00 +00:00:36 13:48:00 +00:40:37 13:48:00 +00:00:36 13:48:00 +00:40:37 13:48:30 -01:19:26 13:48:30 +01:20:38 13:48:30 -01:59:27 13:48:30 +02:00:39 13:48:30 -02:39:28 13:48:30 +02:40:40 13:52:00 +00:39:25 13:52:00 +00:00:36 13:52:00 +00:40:37 13:52:00 +00:00:36 13:52:00 +00:40:37 13:52:30 -01:19:26 13:52:30 +01:20:38 13:52:30 -01:59:27 13:52:30 +02:00:39 13:52:30 -02:39:28 13:52:30 +02:40:40 14:22:06 +03:20:42 14:22:06 +04:00:43 14:22:06 +04:40:44 14:24:45 +05:20:45 14:24:45 +06:00:46 14:24:45 +06:40:48 14:26:07 +03:20:42 14:26:07 +04:00:43 14:26:07 +04:40:44 14:28:46 +05:20:45 14:28:46 +06:00:46 14:28:46 +06:40:48 14:30:07 +03:20:42 14:30:07 +04:00:43 14:30:08 +04:40:44 14:32:32 +01:20:38 14:32:32 +02:00:39 14:32:32 +02:40:40 14:32:47 +05:20:45 14:32:48 +06:00:46 14:32:48 +06:40:48 14:32:31 +08:40:51 14:34:08 +03:20:42 14:34:08 +04:00:43 14:34:08 +04:40:44 14:36:32 +01:20:38 14:36:32 +02:00:39 14:36:32 +02:40:40 14:36:33 +07:20:49 14:36:33 +08:00:50 14:36:34 +08:40:51 14:38:09 +03:20:42 14:38:09 +04:00:43 14:38:09 +04:40:44 14:40:32 +01:20:38 14:40:32 +02:00:39 14:40:32 +02:40:40 14:40:36 +07:20:49 14:40:35 +08:00:50 14:40:35 +08:40:51 14:42:09 +03:20:42 14:42:09 +04:00:43 14:42:09 +04:40:44 14:44:52 +06:40:48 14:44:38 +07:20:49 14:44:38 +08:00:50 14:44:38 +08:40:51 14:46:10 +03:20:42 14:46:10 +04:00:43 14:46:10 +04:40:44 14:48:53 +05:20:45 14:48:53 +06:00:46 14:48:53 +06:40:48 14:48:40 +07:20:49 14:48:40 +08:00:50 14:48:41 +08:40:51 14:49:33 +10:40:55 14:50:10 +03:20:42 14:50:10 +04:00:43 14:50:10 +04:40:44 14:52:54 +05:20:45 14:52:54 +06:00:46 14:52:54 +06:40:48 14:52:43 +07:20:49 14:52:43 +08:00:50 14:52:42 +08:40:51 14:53:36 +09:20:52 14:53:37 +10:00:54 14:53:37 +10:40:55 14:54:11 +03:20:42 14:54:11 +04:00:43 14:54:11 +04:40:44 14:56:55 +05:20:45 14:56:56 +06:00:46 14:56:56 +06:40:48 14:56:45 +07:20:49 14:56:45 +08:00:50 14:56:45 +08:40:51 15:00:47 +07:20:49 15:00:47 +08:00:50 15:00:48 +08:40:51 Data analysis is ongoing. Optical transients from the above fields, if interesting, will be reported later. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24477 SUBJECT: LIGO/Virgo S190510g: Unconfirmed OT in PGC 094244 DATE: 19/05/11 10:08:27 GMT FROM: Michael A Tucker at Inst. for Astronomy, UH Manoa M. A. Tucker, A. Do, A. V. Payne, M. E. Huber, B. J. Shappee (UH Manoa, Institute for Astronomy): Following the discovery of an optical transient in PGC 094244 (GCN 24470, Lipunov et al.), we obtained follow up V-band imaging with the SuperNova Integral Field Spectrograph (SNIFS) on the University of Hawai'i 88-inch (UH88) telescope. The transient is undetected in 2 images to a limiting magnitude of V ~ 22, calibrated to PanSTARRS sources using the photometric transformations of Tonry et al. (2012, ApJ). Date Obs (UT) | Expt. (s) | mlim ------------------------------------------------------------- 2019-05-11T07:09:45 | 180 | ~21.5 2019-05-11T07:14:23 | 300 | ~22 ------------------------------------------------------------- //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24478 SUBJECT: LIGO/Virgo S190510g: MASTER OT independ detection in WISE J060606.26-353233.9 galaxy at desgw-190510a position. DATE: 19/05/11 10:31:51 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, N.Tyurina, E. Gorbovskoy, V.Kornilov, D.Vlasenko, P.Balanutsa,D.Vlasenko, V.Vladimirov, D.Zimnukhov, A.Kuznetsov, P.Balanutsa, I.Gorbunov, A. Chasovnikov, F.Balakin, V.Grinshpun, T.Pogrosheva (Lomonosov Moscow State University, SAI, Physics Department), D. Buckley (South African Astronomical Observatory), A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres (The Instituto de Astrofisica de Canarias), R. Podesta, C. Lopez, C.Francile, F. Podesta (Observatorio Astronomico Felix Aguilar OAFA, San Juan National University), H.Levato (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE,SJNU) O. Gress, N.M. Budnev, O.Ershova (Applied Physics Institute, Irkutsk Stat University), V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev (Blagoveschensk EducationState University), After publication OT desgw-190510a detection (Jim Annis et al., GCN 24474) After the publication OT desgw-190510a detection (Jim Annis et al., GCN 24474), the we checked the candidates of the MASTER-SAAO robots and found MASTER transient in this place. MASTER OT J060606.43-353229.8 at desgw-190510a position. MASTER-SAAO auto-detection system ( Lipunov et al., "MASTER Global Robotic Net", Advances in Astronomy, 2010, 30L ) discovered OT source at (RA, Dec) = 06h 06m 06.43s -35d 32m 29.8s on ~ 2019-05-10 UT. The OT unfiltered magnitude is ~20 m in our red CCD. The OT is seen in 2 images. There is no minor planet at this place. We have reference image on 2019-02-04.86162 UT with unfiltered mlim= 20.2 m. Folow up observations are required. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24479 SUBJECT: LIGO/Virgo S190510g : Xinglong-60cm upper limit of the GRAWITA REM's OT DATE: 19/05/11 10:40:06 GMT FROM: Dong Xu at NAOC/CAS Z.P. Zhu, D. Xu, B.Y. Yu, J.J. Ren, T.M. Zhang, X. Zhou, H.J. Wang, C.Z. Cui, D.W. Fan, Y.F. Xu (NAOC), X. Gao (Urumqi No.1 Senior High School), S. Yang (INAF-OAPd), H.B. Zhao, B. Li (PMO), J.Z. Liu, H.B. Niu (XAO), J.R. Mao, J.M. Bai (YNAO), report on behalf of the GWFUNC collaboration: We observed the optical transient (OT), r = 17.3 +/- 0.1 (AB, calibrated against the SDSS), in P. D'Avanzo et al. (GCN 24455) of the gravitational-wave event S190510g (GCN 24442) using the Xinglong-60cm telescope located at Xinglong, Hebei, China. The OT is ~20" away from the SDSS galaxy, SDSS J142914.95+094059.4, which has a photoZ=0.041 +/- 0.0149, corresponding to a luminosity distance of 182.2 Mpc, thus being consistent with the LIGO's luminosity distance estimate of 227 +/- 92 Mpc (GCN 24448). At the above redshift, SDSS J142914.95+094059.4 has an absolute magnitude of M(r) = 17.92-36.30 = -18.38, at the border of dwarf/normal galaxies. The OT is ~16.3 kpc away from the nucleus of the SDSS galaxy, much larger than usual radii of such galaxies. If double neutron stars are considered having been kicked out of their host galaxy earlier before, such a scenario might be possible. Under the above assumption, we obtained 15x360 s frames in R band, started at 16:12:27 on 2019-05-10, i.e., about 10 hr after the OT detected. The OT has decayed and is not detected in our stacked image of 5400 s, down to a limiting magnitude of r ~ 20.6, calibrated with the SDSS field. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24480 SUBJECT: LIGO/Virgo S190510g: DESGW counterpart candidates over 80% of the GW localization area DATE: 19/05/11 11:06:55 GMT FROM: M. Soares-Santos at Fermi Lab LIGO/Virgo S190510g: DESGW counterpart candidates over 80% of the GW localization area Marcelle Soares-Santos for the DESGW collaboration We report candidate counterparts to the binary neutron star merger S190510g reported by the LIGO/VIRGO Collaboration (GCN Circular No. 24442, updated GCN Circular No. 24448). The region was imaged by DECam on the night of 2019 May 10 (GCN Circular No. 24467) in g,r,z bands. These candidates were identified by our difference imaging pipeline. All newly obtained images were subtracted from deep pre-existing Dark Energy Survey images. The total coverage difference imaged is 28 fields of 3 square degrees each, i.e., a total of 84 square degrees which overlap ~80% of the total localization probability of S190510g. After processing the entire area, we select high-confidence detections (machine learning score>0.7, rejecting dipoles) and perform post-processing vetting of the candidates (rejection of variable objects, matching to host galaxies, and visual inspection). The resulting list of candidates is provided. We encourage followup: NAME RA DEC MAG MAGERR BAND MJD HOST_Z COMMENT desgw-190510a 91.526744 -35.541616 21.05 0.03 r 58613.958 0.08 Also reported in GCN No. 24474 desgw-190510b 93.704382 -36.980727 21.13 0.01 r 58613.989 -1.0 Hostless candidate desgw-190510c 92.851468 -36.517324 20.41 0.01 r 58613.989 0.30 Also reported in GCN No. 24467 desgw-190510d 87.311398 -35.955853 19.85 0.02 r 58613.991 0.31 Also reported in GCN No. 24467 desgw-190510e 89.100926 -30.473987 20.64 0.02 r 58613.986 0.13 Second possible host at z=0.3 desgw-190510f 92.294458 -34.884684 21.30 0.02 r 58613.983 -1.0 Hostless candidate desgw-190510g 92.468923 -34.08657 21.89 0.01 r 58613.987 -1.0 Hostless candidate desgw-190510h 87.762354 -27.956502 20.31 0.03 r 58613.988 -1.0 Host found via visual inspection, no redshift desgw-190510i 91.936973 -30.824747 20.14 0.01 r 58613.996 0.61 Probably not associated with S190510g desgw-190510j 92.307977 -35.149829 20.75 0.02 r 58613.983 0.17 Redshift suggests possible association with S190510g desgw-190510k 87.146843 -35.994357 19.75 0.02 z 58613.966 -1.0 Host redshift not available As an alternative means of selecting high interest candidates, we used KN-Classify, a random forest classifier trained on transient light curves from PLAsTiCC models to determine the probability of a transient being a kilonova. The only such candidate found that survived the vetting process was also found by the normal method and is listed in the table above (desgw-190510c). Transients matched to a galaxy at a redshift beyond distances plausible for the S190510g event are interpreted as supernova unassociated with S190510g. DESGW collaboration: Sahar Allam (Fermilab), James Annis (Fermilab), Iair Arcavi (Tel Aviv University), Paulo Barchi (INPE/Brazil), Keith Bechtol (LSST), Federico Berlfein (Brandeis U), Antonio Bernardo (IAG-USP/Brazil), Dillon Brout (University of Pennsylvania), Robert Butler (Indiana University), Melissa Butner, (Fermilab), Annalisa Calamida (STScI), Hsin-Yu Chen (Harvard U), Chris Conselice (University of Nottingham), Carlos Contreras (STScI), Jeff Cooke (Swinburne University), Chris D’Andrea (University of Pennsylvania), Tamara Davis (UQ/Australia), Reinaldo de Carvalho (NAT - Universidade Cruzeiro do Sul/Universidade Cidade de Sao Paulo), H. Thomas Diehl (Fermilab), Zoheyr Doctor (U Chicago), Alex Drlica-Wagner (Fermilab), Maria Drout (U Toronto), Maya Fishbach (U Chicago), Francisco Forster (U de Chile/Chile), Ryan Foley (UCSC), Joshua Frieman (Fermilab & University of Chicago), Chris Frohmaier (University of Portsmouth), Ori Fox (STScI), Alyssa Garcia (Brandeis U), Juan Garcia-Bellido (Universidad Autonoma de Madrid), Mandeep Gill (SLAC/Stanford U), Robert Gruendl (NCSA), Will Hartley (University College London), Kenneth Herner (Fermilab), Daniel Holz (U Chicago), Jorge Horvath (IAG-USP/Brazil), D. Andrew Howell (Las Cumbres Observatory), Richard Kessler (University of Chicago), Charles Kilpatrick (UCSC), Nikolay Kuropatkin (Fermilab), Ofer Lahav (University College London), Huan Lin (Fermilab), Andrew Lundgren (Portsmouth), Martin Makler (CBPF/Brazil), Curtis McCully (Las Cumbres Observatory), Robert Morgan (University of Wisconsin-Madison), Gautham Narayan (STScI), Eric Neilsen (Fermilab), Robert Nichol (University of Portsmouth), Antonella Palmese (Fermilab), Francisco Paz-Chinchon (NCSA & UIUC), Maria Pereira (Brandeis University), Sandro Rembold (UFSM/Brazil), Armin Rest (STScI & JHU), Livia Rocha (IAG-USP/Brazil), Russell Ryan (STScI), Masao Sako (University of Pennsylvania), Samir Salim (Indiana University), David Sand (U of Arizona), Daniel Scolnic (Duke University), J. Allyn Smith (Austin Peay State University), Mathew Smith (University of Southampton), Marcelle Soares-Santos (Brandeis U), Lou Strolger (STScI), Riccardo Sturani (UFRN/Brazil), Mark Sullivan (University of Southampton), Masaomi Tanaka (NAOJ/Japan), Nozomu Tominaga (Konan U/Japan), Douglas Tucker (Fermilab), Yousuke Utsumi (Stanford U), Stefano Valenti (UC Davis), Kathy Vivas (NOAO/CTIO), Alistair Walker (NOAO/CTIO), Sara Webb (Swinburne University), Matt Wiesner (Benedictine University), Brian Yanny (Fermilab), Michitoshi Yoshida (NAOJ/Japan), Alfredo Zenteno (NOAO/CTIO), Luidhy Santana-Silva (Valongo Observatory) This project used data obtained with the Dark Energy Camera (DECam), which was constructed by the Dark Energy Survey collaboration, and draws on upon data as distributed by the Science Data Archive at NOAO. NOAO is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24484 SUBJECT: LIGO/Virgo S190510g: GRAWITA VST-ESO PARANAL optical observations DATE: 19/05/11 15:33:28 GMT FROM: Aniello Grado at INAF-OAC *S. Yang (INAF-OAPd), E. Cappellaro (INAF-OAPd), F. Getman (INAF-OAC), A. Grado (INAF-OAC), G. Greco (Univ. Urbino), S. Covino (INAF-OAB), L. Izzo (IAA), E. Palazzi (INAF-OAS), L. Nicastro (INAF-OAS), M.T. Botticella (INAF-OAC), P. D'Avanzo (INAF-OAB), M. Branchesi (GSSI), E. Brocato (INAF-OAAb, INAF-OAR) on behalf of GRAWITA report:We observed part of the 50% probability of the updated skymap of the LIGO/Virgo GW trigger S190509g (LVC, GCN Circ. 24442), with the VLT Survey Telescope (VST) at ESO-Paranal equipped with OMEGACAM (FOV=1 square degree). The observations were taken in the r-sloan band and started on 2019-05 11 at 00:03:23 UT.The covered area is of about 15 square degrees divided in of 80 sec of exposure time each.The pointings are centered on the following coordinates RA, Dec (J2000):05:57:42.54, -33:00:00.005:57:02.43, -34:00:00.005:52:56.37, -33:00:00.005:53:45.21, -32:00:00.006:01:51.92, -34:00:00.005:52:12.94, -34:00:00.005:58:28.21, -32:00:00.006:02:28.71, -33:00:00.006:01:20.96, -35:00:00.005:56:27.97, -35:00:00.006:03:59.38, -31:00:00.006:11:06.93, -35:00:00.006:06:13.94, -35:00:00.006:10:49.22, -36:00:00.006:11:30.91, -34:00:00.0The image analysis is ongoing.* //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24485 SUBJECT: LIGO/Virgo S190510g: GRAWITA REM and Loiano optical observations DATE: 19/05/11 15:55:17 GMT FROM: Aniello Grado at INAF-OAC P. D'Avanzo (INAF-OAB), E. Palazzi (INAF-OAS), G. Greco (Univ. Urbino), S. Yang (INAF-OAPd), S. Campana (INAF-OAB), G. Stratta (INAF-OAS), A. Rossi (INAF-OAS), Nicola Masetti (inaf-oas) and E. Brocato on behalf of GRAWITA report: We carried out further optical follow-up observations of the LIGO/Virgo GW trigger S190509g (LVC, GCN Circ. 24442) with the 60-cm robotic telescope REM located at the La Silla Observatory (Chile). The observations started at 2019-05-11 at 00:49:48 UT, simultaneously in the g, r, i, z bands (the REM NIR camera was not operational). We observed the following galaxies within the 50% probability of the updated skymap visible from La Silla: RA(J2000) Dec(J2000) Dist(Mpc) ---------------------------------------------------- J055219-342051 05:52:19.00 -34:20:51.4 138.68 J055149-314446 05:51:49.92 -31:44:46.0 210.86 J054827-325838 05:48:27.60 -32:58:38.1 160.69 J060115-313225 06:01:15.09 -31:32:25.5 191.43 J055425-350235 05:54:25.29 -35:02:35.1 143.88 J055028-334429 05:50:28.73 -33:44:29.3 165.20 J055740-345601 05:57:40.71 -34:56:01.8 146.97 J055949-353200 05:59:49.81 -35:32:00.5 138.04 No clear counterpart for S190509g is found down to a typical 3sigma magnitude of r > 19 (AB). We also carried out optical follow-up of the possible transient we reported in D'Avanzo et al. (GCN Circ. #24455) found in REM images at RA(J2000), Dec(J2000) = 14:29:15.99, +09:41:12.3 with magnitude r = 17.3 (AB) on 2019-05-10 at 08:07:18 UT. Optical imaging follow-up observations of this possible transient were carried out with the 1.5m Loiano telescope (Italy) in the R band on 2019-05-10 at 20:44:08 UT (i.e. about 12.6 hours after the REM detection reported in GCN Circ. #24455). In the Loiano images the object is not detected down to a 3-sigma limiting magnitude of R > 20.3 (AB, calibrated against the SDSS). This non-detection is in agreement with the findings reported by Zhu et al. (GCN Circ. #24479) and favor a fast transient (like a stellar flare) interpretation for the nature of this object, although the hypothesis of an image artifact cannot be completely excluded. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24487 SUBJECT: LIGO/Virgo S190510g: Non-detection of the OT in PGC 094244 DATE: 19/05/11 17:20:02 GMT FROM: Albert Kong at NTHU Po-Chieh Yu (NCU), Han-Jie Tan (NCU), Albert Kong (NTHU), Atharva Sunil Patil (NCU), Chow-Choong Ngeow (NCU), Wing-Huen Ip (NCU), on behalf of the Global Relay of Observatories Watching Transients Happen (GROWTH) collaboration We observed the possible OT in PGC 094244 (GCN #24470, Lipunov et al.) at 2019-05-11 12:50:12 UT using the Lulin One-meter Telescope (LOT) in Taiwan. We obtained g-, r-, i-band images with 300s exposure time, and the transient is not detected in all images. The r-band limiting magnitude is about 21 by comparing with Pan-STARRS images. This is consistent with the results of Tucker et al. (GCN #24477). We thank the staff in Lulin Observatory for helping the observations. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24488 SUBJECT: LIGO/Virgo S190510g: Las Cumbres Observatory Galaxy Targeted Counterpart Search DATE: 19/05/11 17:50:24 GMT FROM: Iair Arcavi at Tel Aviv University Iair Arcavi (Tel Aviv University), D. Andrew Howell (LCO/UCSB), Daichi Hiramatsu (LCO/UCSB), Jamison Burke (LCO/UCSB), Curtis McCully (LCO), Craig Pellegrino (LCO/UCSB), Paul Groot (Radboud University), on behalf of the Las Cumbres GW Follow-up Collaboration We report 300s g- and i-band images of the following galaxies (obtained from the GLADE 2.3 catalog; Dalya et al. 2018, MNRAS, 479, 2374) in the LIGO/Virgo S190510g localization region (Chu et al, GCN 24448) with the Las Cumbres Observatory 1m telescopes at the SAAO, South Africa and the CTIO, Chile. We find no significant counterpart candidates from visual inspection of the images. Name GLADE-ID RA Dec UT FILTER Approx Lim-mag 2MASS 05482759-3258380 4768 87.11500 -32.9772 2019-05-1017:25:56 g 22.66 2MASS 05482759-3258380 4768 87.11500 -32.9772 2019-05-1017:31:38 i 22.09 2MASS 05490223-3129287 30042 87.25932 -31.4913 2019-05-1016:47:07 g 21.83 2MASS 05490223-3129287 30042 87.25932 -31.4913 2019-05-1016:52:48 i 21.56 2MASS 05500408-3034504 110676 87.51703 -30.5807 2019-05-1016:59:54 g 22.49 2MASS 05500408-3034504 110676 87.51703 -30.5807 2019-05-1017:05:36 i 23.00 2MASS 05502872-3344293 26624 87.61970 -33.7415 2019-05-1023:22:16 g 22.38 2MASS 05502872-3344293 26624 87.61970 -33.7415 2019-05-1023:27:57 i 21.69 2MASS 05504985-3144266 19812 87.70773 -31.7407 2019-05-1017:12:54 g 22.69 2MASS 05504985-3144266 19812 87.70773 -31.7407 2019-05-1017:18:36 i 21.87 2MASS 05505599-3447027 7534 87.73330 -34.7841 2019-05-1017:12:54 g 22.87 2MASS 05505599-3447027 7534 87.73330 -34.7841 2019-05-1017:18:36 i 21.83 2MASS 05511621-3106167 9683 87.81755 -31.1046 2019-05-1016:47:01 g 21.69 2MASS 05511621-3106167 9683 87.81755 -31.1046 2019-05-1016:52:42 i 21.31 2MASS 05514992-3144460 13462 87.95801 -31.7461 2019-05-1023:35:19 g 22.38 2MASS 05514992-3144460 13462 87.95801 -31.7461 2019-05-1023:41:00 i 21.63 2MASS 05574070-3456018 22967 89.41962 -34.9338 2019-05-1023:48:21 g 22.45 2MASS 05574070-3456018 22967 89.41962 -34.9338 2019-05-1023:54:02 i 21.72 2MASS 06011509-3132255 21382 90.31288 -31.5404 2019-05-1017:38:57 g 23.60 2MASS 06011509-3132255 21382 90.31288 -31.5404 2019-05-1017:44:46 i 21.85 2MASS 06024073-3420093 130705 90.66974 -34.3359 2019-05-1017:38:58 g 22.64 2MASS 06024073-3420093 130705 90.66974 -34.3359 2019-05-1017:44:40 i 22.21 2MASS 06033989-3208521 5089 90.91624 -32.1478 2019-05-1017:25:56 g 22.41 2MASS 06033989-3208521 5089 90.91624 -32.1478 2019-05-1017:31:38 i 21.70 2MASS 06055976-3250371 9684 91.49903 -32.8437 2019-05-1023:10:04 g 22.31 2MASS 06055976-3250371 9684 91.49903 -32.8437 2019-05-1023:15:45 i 21.35 2MASS 06064749-3348522 13891 91.69790 -33.8145 2019-05-1017:52:00 g 21.81 2MASS 06064749-3348522 13891 91.69790 -33.8145 2019-05-1017:53:58 g 22.59 2MASS 06064749-3348522 13891 91.69790 -33.8145 2019-05-1017:59:40 i 22.06 2MASS 06084611-3354584 14569 92.19215 -33.9162 2019-05-1022:55:30 g 21.58 2MASS 06084611-3354584 14569 92.19215 -33.9162 2019-05-1023:01:11 i 21.23 2MASS 06100073-3338309 136310 92.50307 -33.6419 2019-05-1016:59:54 g 22.59 2MASS 06100073-3338309 136310 92.50307 -33.6419 2019-05-1017:05:36 i 21.93 2MASS 06105136-3352566 5855 92.71404 -33.8824 2019-05-1017:52:39 g 22.49 2MASS 06105136-3352566 5855 92.71404 -33.8824 2019-05-1017:58:20 i 21.95 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24489 SUBJECT: LIGO/Virgo S190510g: Update on candidate significance DATE: 19/05/11 20:19:22 GMT FROM: Shasvath J. Kapadia at U. of Wisconsin, Milwaukee The LIGO Scientific Collaboration and the Virgo Collaboration report: We have conducted subsequent analysis of data around the time of S190510g including LIGO and Virgo data collected in the 24 hour period after the event. The resulting re-estimate of the background model yields a FAR (False Alarm Rate) of 1 in 3.6 years compared to 1 in 37 years initially reported in GCN 24442. Using the updated background model, the classification of the event, in order of descending probability, is estimated to be: Terrestrial (58%), BNS (42%), NSBH (<1%), BBH (<1%), or MassGap (<1%). Further analysis of the event is ongoing. Updates will be provided as and when available. For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo Public Alerts User Guide . //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24490 SUBJECT: LIGO/Virgo S190510g: MASTER OT detection inside low surface brightness galaxy DATE: 19/05/11 20:28:33 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, N.Tyurina, E. Gorbovskoy, V.Kornilov, D.Vlasenko, P.Balanutsa,D.Vlasenko, V.Vladimirov, D.Zimnukhov, A.Kuznetsov, P.Balanutsa, I.Gorbunov, A. Chasovnikov, F.Balakin, V.Grinshpun, T.Pogrosheva (Lomonosov Moscow State University, SAI, Physics Department), R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres (The Instituto de Astrofisica de Canarias), D. Buckley (South African Astronomical Observatory), A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), R. Podesta, C. Lopez, C.Francile, F. Podesta (Observatorio Astronomico Felix Aguilar OAFA, San Juan National University), H.Levato (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE,SJNU) O. Gress, N.M. Budnev, O.Ershova (Applied Physics Institute, Irkutsk Stat University), V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev (Blagoveschensk EducationState University), OT MASTER142812.05-013615.2 discovery. MASTER-IAC auto-detection system discovered OT source at (RA, Dec) = 14h 28m 12.05s -01d 36m 15.2s on 2019-05-11.03821 UT. The OT unfiltered magnitude is 17.6m (limit 20.0m). The OT is seen in 2 images. There is no minor planet at this place. We have reference image without OT on 2016-03-09.04372 UT with unfiltered magnitude limit 20.3m. There is low surface brightness galaxy (from HSC-SSP) with 2.7 arcsec offset at 14 28 12.0144 -01 36 17.316 This OT is good candidate for Gravitational Waves counterpart. Spectral observations are required. The discovery and reference images are available at: http://master.sai.msu.ru/static/OT/142812.05-013615.2.png Folow up observations are required. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24491 SUBJECT: LIGO/Virgo S190510g: OT MASTER142812.05-013615.2 retraction as the kilonova candidate in GCN 24490 DATE: 19/05/11 20:46:28 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov,(Lomonosov Moscow State University, SAI, Physics Department), I am sorry. The OT MASTER142812.05-013615.2 is the known SN 2019dde and can not connected with LIGO/Virgo S190510g . https://wis-tns.weizmann.ac.il/object/2019dde //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24493 SUBJECT: LIGO/Virgo S190510g: KMTNet observation of DECam-GROWTH and DESGW candidates DATE: 19/05/11 23:37:09 GMT FROM: Myungshin Im at Seoul Nat U Myungshin Im (SNU), Joonho Kim (SNU), Chung-Uk Lee (KASI), Seung-Lee Kim (KASI), Gregory S. H. Paek (SNU), Gu Lim (SNU), Changsu Choi (SNU), Sungyong Hwang (SNU), Bomi Park (SNU), Sophia Kim (SNU), Hyung Mok Lee (KASI), on behalf of a larger collaboration With KMTNet, we observed the optical counterpart candidates from DECam-GROWTH and DESGW (Andreoni et al. GCN 24467; Annis et al. GCN 24474; Sores-Santos et al. GCN 24480) of the BNS merger candidate event, S190510g (LIGO/Virgo GCN 24448). The observation took place at the KMTNet South Africa (SAAO), Chile (CTIO), and Australia (SSO) stations. The list of the observed targets are given below, along with preliminary R-band magnitudes. Note that the errors do not include systematic errors due to image subtraction. The error associated with the image subtraction should be considered to be 0.1-0.2 mag at this moment. None of the candidates below show significant fading (> 0.5 mag) over ~1 day. All of the candidates show very slow or no fading, consistent with them being supernovae. Further observation is ongoing. We thank the KMTNet staffs for performing the observation. Object name UT R(mag) Rerr desgw-190510a 2019-05-11T17:33:16 21.26 0.07 DG19bexl 2019-05-10T17:54:47 21.21 0.04 2019-05-11T16:57:13 21.49 0.09 DG19etsk 2019-05-10T17:33:32 20.92 0.10 DG19fqqk 2019-05-10T18:08:23 20.57 0.04 (desgw-190510c) 2019-05-10T23:45:52 20.88 0.04 2019-05-11T17:36:25 20.71 0.04 DG19lcnl 2019-05-10T23:33:34 19.92 0.04 2019-05-11T17:23:49 19.82 0.03 DG19llhk 2019-05-10T17:08:10 21.23 0.04 2019-05-10T17:20:36 21.17 0.05 2019-05-11T17:20:40 21.37 0.11 DG19nanl 2019-05-10T23:33:34 20.43 0.04 DG19nouo 2019-05-10T17:20:36 21.64 0.05 2019-05-10T23:21:17 21.51 0.05 DG19oahn 2019-05-11T16:50:54 19.48 0.03 DG19ootl 2019-05-10T23:33:34 21.51 0.07 DG19ukvo 2019-05-10T16:48:24 21.56 0.14 DG19yhhm 2019-05-10T17:20:36 20.43 0.04 2019-05-10T23:21:17 20.33 0.05 DG19zaxn 2019-05-10T17:27:13 21.16 0.04 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24495 SUBJECT: LIGO/Virgo S190510g: CALET Observations DATE: 19/05/12 03:01:00 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. Ozawa, 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: The CALET Gamma-ray Burst Monitor (CGBM) was operating at the trigger time of S190510g T0=2019/05/10 02:59:39.292 UT (The LIGO Scientific Collaboration and Virgo Collaboration, GCN Circ. 24442, 24448 and 24462). No CGBM on-board trigger occurred around the event time. Based on the LIGO-Virgo localization sky map, most of the part of the high probability area was outside of the field-of-view of CGBM. The summed LIGO probabilities inside the HXM and the SGM field of view are 2% and 7% (and 84% credible region of the updated localization map were Earth-occulted). The HXM and SGM field of views were centered at RA=298.7 deg, Dec = 60.7 deg and RA=295.7 deg, Dec=50.8 deg at T0. Based on the analysis of the light curve data with 0.125 sec time resolution from T0-60 sec to T0+60 sec, we found no significant excess around the trigger time in either the HXM (7-3000 keV) or the SGM (40 keV -28 MeV) data. The CALET Calorimeter (CAL) was operating in high energy trigger mode at the trigger time of S190510g. Using CAL data, we have searched for gamma-ray events in the 10-100 GeV band from -60 sec to +60 sec from the GW trigger time and found no candidates. There is no significant overlap with the LVC location probability map. The CAL FOV was centered at RA=295.7 deg, Dec=50.8 deg at T0. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24496 SUBJECT: LIGO/Virgo S190510g: DOAO Observation DATE: 19/05/12 04:52:23 GMT FROM: Gregory SungHak Paek at SNU Gregory S.H. Paek, Myungshin Im (CEOU/SNU), Taewoo Kim, and Wonseok Kang (DOAO) on behalf of a larger collaboration We observed 12 host galaxy candidates with the 1.0-m telescope at the Deokheung Optical Astronomy Observatorythe in the 90% updated localization area of S190510g, detected by LIGO/Virgo (GCN #24442). The observation started at 2019-05-10 14:35:16, and 9 images were taken in R-band with 120 sec exposure time for each fields. No obvious transient has been identified to a preliminary 3-sigma depth of R=21.5 AB mag. The list of the inspected targets in the observed fields is given below. FIELD date-obs[UT] UL[AB] NOTE G0028316 2019-05-10 15:03:14 20.359 PGC159415, PGC1050569 G0031507 2019-05-10 15:47:31 21.881 PGC48754, PGC48717 G0450408 2019-05-10 14:43:43 21.432 PGC95645, PGC1109881, NGC5192, PGC1104597 G0550129 2019-05-10 15:57:40 21.791 PGC158865, PGC3105750, PGC1068483 G0595818 2019-05-10 15:22:47 21.829 PGC0595818 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24509 SUBJECT: LIGO/Virgo S190510g: MASTER OT detection inside PGC087378 galaxy DATE: 19/05/12 20:26:08 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, N.Tyurina, E. Gorbovskoy, V.Kornilov, D.Vlasenko, P.Balanutsa,D.Vlasenko, V.Vladimirov, D.Zimnukhov, A.Kuznetsov, P.Balanutsa, I.Gorbunov, A. Chasovnikov, F.Balakin, V.Grinshpun, T.Pogrosheva (Lomonosov Moscow State University, SAI, Physics Department), R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres (The Instituto de Astrofisica de Canarias), D. Buckley (South African Astronomical Observatory), A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), R. Podesta, C. Lopez, C.Francile, F. Podesta (Observatorio Astronomico Felix Aguilar OAFA, San Juan National University), H.Levato (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE,SJNU) O. Gress, N.M. Budnev, O.Ershova (Applied Physics Institute, Irkutsk Stat University), V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev (Blagoveschensk EducationState University), MASTER OT J135130.87-525534.4 (2019fcc) - OT inside PGC087378 MASTER-OAFA auto-detection system ( Lipunov et al., "MASTER Global Robotic Net", Advances in Astronomy, 2010, 30L ) discovered OT source at (RA, Dec) = 13h 51m 30.87s -52d 55m 34.4s on 2019-05-12.29047 UT. The OT unfiltered magnitude is ~ 17m (mlim=18.4m). The OT is seen in 2 images. There is no minor planet at this place. We have reference image without OT on 2016-07-06.02547 UT with magnitude limit in 'clear' filter 19.0m. THe OT offset from center of the PGC087378 galaxy is 2.1E 11S. The distance is about ~50Mpc. The same transient we see 12 hours after trigger time in MASTER-SAAO database. Folow up observations are required. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24511 SUBJECT: LIGO/Virgo S190510g: Spectroscopic Classification of DECam-GROWTH and DES-GW Candidate DG19fqqk/desgw-190510c with Magellan DATE: 19/05/12 21:49:07 GMT FROM: Sebastian Gomez at Harvard U S. Gomez (Harvard), P. S. Cowperthwaite (Carnegie), G. Hosseinzadeh (Harvard), E. Berger (Harvard), P. K. Blanchard (Harvard), M. R. Drout (Carnegie/U. Toronto), T. Eftekhari (Harvard), M. Nicholl (Edinburgh), L. Patton (Harvard), A. L. Piro (Carnegie), V. A. Villar (Harvard), P.K.G. Williams (Harvard), P. Goudfrooij (STScI), and T. Puzia (PUC, Chile) We report on spectroscopic observations conducted with the IMACS Spectrograph on the 6.5m Magellan-Baade telescope of a candidate optical counterpart to the gravitational wave event S190510g (The LIGO Scientific Collaboration and the Virgo Collaboration, GCN 24442). The counterpart was identified during difference image processing of public DECam observations (Andreoni et al. GCN 24443, Andreoni et al. GCN 24467, Soares-Santos et al. GCN 24480). Lists of promising counterparts were identified on the basis of factors such as their brightness, colors, and possible host galaxy association. We were able to obtain deep spectroscopy of DG19fqqk/desgw-190510c, which is an interesting source as it was flagged by a light curve classifier trained to identify kilonovae (KN-Classify, GCN 24480). Target | Reference | Classification ---------------------------------------------------------------------------------------------------------------- DG19fqqk/desgw-190510c | GCN 24467, GCN 24480 | Type II (phase = +6 days) DG19fqqk/desgw-190510c shows a broad feature consistent with H-alpha at a redshift of 0.06 and template matching using Superfit (Howell et al. 2005, ApJ, 634, 1190) suggests a good match to a Type II SNe approximately one week after peak brightness. This candidate was also observed by KMTNet (GCN #24493) and showed no significant fading over ~1 day. We conclude that the transient is not associated with the gravitational wave event S190510g. We thank Paul Goudfrooij and Thomas Puzia for taking these observations. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24517 SUBJECT: LIGO/Virgo S190510g: Pan-STARRS and ATLAS observations and candidates DATE: 19/05/13 11:31:11 GMT FROM: Stephen Smartt at Queen's U/Belfast S. Srivastav, K. W. Smith, S. J. Smartt (QUB), K. Chambers, M. Huber, T. de Boer, J. Bulger, J. Fairlamb, C.-C. Lin, T. Lowe, E. Magnier A. Schultz, R. J. Wainscoat, M. Willman (IfA, Univ. Hawaii), D. R. Young, O. McBrien, J. Gillanders. D. O'Neil, P. Clark, S. Sim (QUB), L. Denneau, H. Flewelling, A. Heinze, J. Tonry, H. Weiland (IfA, Univ. Hawaii), A. Rest (STScI), B. Stalder (LSST), C. Stubbs (Harvard) We report observations of the BAYESTAR skymap of the BNS event S190510g (The LIGO Scientific Collaboration and the Virgo Collaboration, GCN 24442) with the Pan-STARRS1 telescope (Chambers et al. 2016, arXiv:1612.05560C) and the ATLAS telescopes (Tonry et al. 2018, PASP PASP, 13, 164505). We acknowledge that is now a marginal candidate (LSC & VC, GCN 24489) and note that we completed our scanning of the BAYESTAR skymap, before the LALInference map was available (resulting in a final 4% probability coverage). For Pan-STARRS1 : images were taken in the PS1 w and i-bands (Tonry et al. 2012, ApJ 750, 99) in the standard NEO search sequence. At each pointing position a sequence of quads (4 x 45 sec) was taken. This observing sequence ensures exactly the same pointing position for each of the quads. The PS1 images were processed with the IPP (Magnier et al. 2016, arXiv:1612.05240) and difference images were produced using the Pan-STARRS1 Science Consortium 3Pi images as reference frames. Transient candidates were run through our standard filtering procedures, combined with a machine learning algorithm (Wright et al. 2015, MNRAS, 449, 451) and all candidates were spatially cross-matched with known minor planets, and major star, galaxy, AGN and multi-wavelength catalogues (as described in Smartt et al. 2016, MNRAS, 462 4094). For ATLAS, we observed with sequences of 4 x 30s, typically reaching o ~ 19.5 in each pointing (e.g. Weiland et al. GCN 24107). We covered the small probability region of the LalInference map (total summed probability of 4%) at 13-14hrs (the 6hr region was not visible from Hawaii). We began taking Pan-STARRS data at 2019-05-10 07:09 (UTC), ~4.2 hrs after the GW trigger. ATLAS started at a similar time. No new extragalactic transient candidates were discovered with ATLAS within the 90% contour (brighter than about o ~ 19.5) In the PS1 data, the following 23 transients were found lying within the 90% contour of the LALInference map. We give them 3 ranks : Rank 1 candidates are plausibly within the distance range reported by the LIGO-Virgo analysis (~130 Mpc < d < ~220 Mpc). This comes from host galaxy association and their spectroscopic or photometric redshifts. Rank 2 candidates are not obviously associated with a catalogued host galaxy. Rank 3 candidates are probably associated with a galaxy outside the distance range. Name | PS Name | RA (J2000) | Dec (J2000) | Disc. MJD | Disc Mag | Notes ------------------------------------------------------------------------------- Rank 1 AT2019ezb | PS19xv | 13 43 59.78 | +01 50 32.7 | 58613.30 | 20.50 i | (1) AT2019far | PS19aaf | 14 17 22.53 | +05 01 08.7 | 58613.48 | 20.29 i | (2) Rank 2 AT2019ezc | PS19yn | 13 24 04.80 | -09 02 05.8 | 58613.34 | 20.16 i | AT2019eya | PS19yi | 13 27 23.56 | -07 01 41.2 | 58613.39 | 20.78 i | AT2019fam | PS19yp | 13 39 00.66 | -04 28 30.7 | 58613.39 | 20.25 i | AT2019eyg | PS19yz | 13 42 05.60 | -09 43 24.7 | 58613.35 | 20.60 i | AT2019fal | PS19zf | 13 46 08.91 | -03 22 40.1 | 58613.39 | 20.92 i | AT2019eyp | PS19zh | 14 05 46.51 | +03 25 21.4 | 58613.50 | 21.36 w | AT2019eyu | PS19aaj | 14 06 15.69 | +03 45 58.4 | 58613.48 | 20.57 i | Rank 3 AT2019exz | PS19yh | 13 17 59.93 | -04 36 33.5 | 58613.39 | 19.93 i | (3) AT2019faa | PS19xz | 13 21 30.14 | +01 59 03.5 | 58613.30 | 21.02 i | (4) AT2019ezy | PS19xx | 13 27 22.91 | +01 28 19.0 | 58613.30 | 20.11 i | (5) AT2019fan | PS19yo | 13 28 01.32 | -03 47 08.3 | 58613.39 | 20.76 i | (6) AT2019eyi | PS19xs | 13 31 45.46 | -00 04 26.5 | 58613.30 | 20.23 i | (7) AT2019eza | PS19xr | 13 51 04.52 | +03 54 53.4 | 58613.30 | 20.42 i | AT2019fae | PS19yd | 13 51 53.52 | +00 45 54.8 | 58613.30 | 20.68 i | (8) AT2019fac | PS19yb | 13 53 05.69 | +08 16 45.3 | 58613.30 | 20.84 i | (9) AT2019eyf | PS19yg | 13 58 13.27 | +05 13 28.2 | 58613.30 | 19.87 i | AT2019eyv | PS19aah | 14 03 35.78 | +08 11 25.3 | 58613.48 | 21.14 i | AT2019fbj | PS19abe | 14 05 22.17 | +06 35 48.7 | 58613.48 | 21.14 i | AT2019eyn | PS19zk | 14 07 17.08 | +08 23 33.3 | 58613.48 | 20.49 i | (10) AT2019ezl | PS19zx | 14 13 00.93 | +07 50 02.5 | 58613.48 | 20.09 i | AT2019ezv | PS19aau | 14 17 39.18 | +02 08 39.1 | 58613.50 | 19.80 w | (11) (1) Probable host is SDSS J134359.83+015034.4 at a spectroscopic z = 0.072 or D ~ 323 Mpc (NED), yielding an absolute i-band magnitude of ~-17.0 mag (2) Probable host is SDSS J141300.92+075002.6 at a spectroscopic z = 0.058 or D ~ 259 Mpc (NED), yielding an absolute i-band magnitude of ~ -16.8 (3) Probable host is GALEXASC J131800.06-043633.9 at a spectroscopic z = 0.132 or D ~ 603 Mpc (NED) (4) Probable host is SDSS J132130.22+015903.0 at a photometric z = 0.291 +/- 0.141 or D ~ 1431 Mpc (SDSS) (5) Probable host is SDSS J132722.06+012818.6 at a photometric z = 0.068 +/- 0.012 or D ~ 308 Mpc (NED) (6) Probable host is LCRS B132526.4-033142 at a spectroscopic z = 0.087 or D ~ 388 Mpc (NED) (7) Probable host is SDSS J133145.14-000431.3 at a photometric z = 0.185 +/- 0.018 or D ~ 899 Mpc (SDSS) (8) Probable host is 2MASX J13515347+0045515 at a spectroscopic z = 0.088 or D ~ 389 Mpc (NED) (9) Probable host is SDSS J135153.50+004551.2 at a photometric z = 0.230 +/-0.151 or D ~ 1148 Mpc (SDSS) (10) Probable host is 2MASX J14071678+0823347 at a spectroscopic z = 0.115 or D ~ 532 Mpc (NED) (11) Probable host is SDSS J141738.94+020831.9 at a spectroscopic redshift of z = 0.129 or D ~ 584 Mpc (NED) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24529 SUBJECT: LIGO/Virgo S190510g: Further KMTNet observation of DECam-GROWTH and DESGW candidates DATE: 19/05/14 02:54:34 GMT FROM: Myungshin Im at Seoul Nat U Myungshin Im (SNU), Joonho Kim (SNU), Chung-Uk Lee (KASI), Seung-Lee Kim (KASI), Gregory S. H. Paek (SNU), Gu Lim (SNU), Changsu Choi (SNU), Sungyong Hwang (SNU), Bomi Park (SNU), Sophia Kim (SNU), Hyung Mok Lee (KASI), on behalf of a larger collaboration We report the results from further KMTNet observation of the optical counterpart candidates from DECam-GROWTH and DESGW (Andreoni et al. GCN 24467; Annis et al. GCN 24474; Sores-Santos et al. GCN 24480) of the BNS merger candidate event, S190510g (LIGO/Virgo GCN 24448). This is a follow-up report of the KMTNet result (Im et al. GCN 24493), adding data points taken after our earlier report. With the additional data, we now have at least one day cadence of KMTNet data of all the objects enabling us to determine their variability for 1 day or more using internally consistent photometry. The list of the observed targets are given below, along with preliminary R-band magnitudes. None of the candidates below show significant fading (> 0.5 mag) over ~1 day. All of the candidates show very slow (<0.2 mag) or no fading, consistent with them being supernovae. We thank the KMTNet staffs for performing the observation. :::::::::::::: desgw-190510a :::::::::::::: #Date_Obs MJD Mag Magerr Depth 2019-05-11T17:33:16 58614.73125 21.26 0.061 21.55 2019-05-11T23:30:03 58614.97917 21.27 0.034 22.10 :::::::::::::: DG19bexl :::::::::::::: #Date_Obs MJD Mag Magerr Depth 2019-05-10T17:54:47 58613.74583 21.21 0.041 21.95 2019-05-11T16:57:13 58614.70625 21.50 0.094 21.21 2019-05-11T23:48:04 58614.99167 21.57 0.053 22.02 :::::::::::::: DG19etsk :::::::::::::: #Date_Obs MJD Mag Magerr Depth 2019-05-10T16:57:54 58613.70625 20.87 0.048 21.57 2019-05-10T17:33:32 58613.73125 21.12 0.067 21.92 2019-05-10T17:33:32 58613.73125 20.92 0.046 21.92 2019-05-11T17:42:31 58614.73750 20.89 0.063 21.52 2019-05-11T23:54:11 58614.99583 20.88 0.066 21.97 :::::::::::::: DG19fqqk :::::::::::::: #Date_Obs MJD Mag Magerr Depth 2019-05-10T18:08:23 58613.75556 20.58 0.042 21.53 2019-05-10T23:45:52 58613.98958 20.89 0.037 21.75 2019-05-11T17:36:25 58614.73333 20.72 0.043 21.85 2019-05-11T23:36:06 58614.98333 20.80 0.038 22.10 :::::::::::::: DG19lcnl :::::::::::::: #Date_Obs MJD Mag Magerr Depth 2019-05-10T23:33:34 58613.98125 19.92 0.040 21.48 2019-05-11T17:23:49 58614.72431 19.82 0.026 21.17 2019-05-11T23:24:10 58614.97500 19.85 0.037 22.08 :::::::::::::: DG19llhk :::::::::::::: #Date_Obs MJD Mag Magerr Depth 2019-05-10T17:08:10 58613.71389 21.24 0.042 21.61 2019-05-10T17:20:36 58613.72222 21.17 0.051 22.81 2019-05-11T08:33:29 58614.35625 99.00 99.000 20.95 2019-05-11T17:20:40 58614.72222 21.37 0.114 21.15 2019-05-11T23:18:08 58614.97083 21.25 0.049 22.04 :::::::::::::: DG19nanl :::::::::::::: #Date_Obs MJD Mag Magerr Depth 2019-05-10T23:33:34 58613.98125 20.42 0.035 21.44 2019-05-11T22:59:57 58614.95764 20.52 0.032 21.53 :::::::::::::: DG19nouo :::::::::::::: #Date_Obs MJD Mag Magerr Depth 2019-05-10T17:20:36 58613.72222 21.64 0.048 21.85 2019-05-10T23:21:17 58613.97292 21.51 0.052 22.04 2019-05-11T17:55:27 58614.74653 21.38 0.057 21.43 :::::::::::::: DG19oahn :::::::::::::: #Date_Obs MJD Mag Magerr Depth 2019-05-11T16:50:54 58614.70139 19.48 0.030 20.74 2019-05-11T23:42:11 58614.98750 19.58 0.033 22.02 :::::::::::::: DG19ootl :::::::::::::: #Date_Obs MJD Mag Magerr Depth 2019-05-10T23:33:34 58613.98125 21.51 0.068 21.49 2019-05-11T23:06:06 58614.96250 21.42 0.062 21.81 :::::::::::::: DG19ukvo :::::::::::::: #Date_Obs MJD Mag Magerr Depth 2019-05-10T16:48:24 58613.70000 21.56 0.146 20.92 2019-05-11T17:49:08 58614.74236 21.71 0.082 21.58 :::::::::::::: DG19yhhm :::::::::::::: #Date_Obs MJD Mag Magerr Depth 2019-05-10T17:20:36 58613.72222 20.43 0.042 21.67 2019-05-10T23:21:17 58613.97292 20.33 0.052 22.08 2019-05-11T23:12:03 58614.96667 20.35 0.041 21.87 :::::::::::::: DG19zaxn :::::::::::::: #Date_Obs MJD Mag Magerr Depth 2019-05-10T17:27:13 58613.72708 21.16 0.040 22.02 2019-05-11T18:01:33 58614.75069 21.13 0.047 21.53 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24535 SUBJECT: LIGO/Virgo S190510g: AT2019ezb and AT2019far 10.4m GTC spectroscopy DATE: 19/05/14 10:33:23 GMT FROM: Alberto J. Castro-Tirado at IAA-CSIC A. J. Castro-Tirado (IAA-CSIC), A. F. Valeev and V. V. Sokolov (SAO-RAS), Y.-D. Hu, X.-Y. Li, A. Ayala, and E. Fernandez-Garcia (IAA-CSIC), R. Sanchez-Ramirez (INAF-IAPS), A. Castellon (UMA) and G. Gomez-Velarde (GRANTECAN, IAC, ULL), on behalf of a larger collaboration, report: Following the detection of AT2019ezb and AT2019far (Srivastav et al., GCNC 24517) within the error area of the GW event S190510g (LVC, GCNC 24442), we obtained optical spectra (900s) covering the range 3700-7500 A with the 10.4m GTC telescope equipped with OSIRIS in La Palma (Spain) starting on May 13, 23:55 UT. The AT2019ezb spectrum is consistent with a SNIc at the host galaxy redshift (z=0.0712). The AT2019far spectrum is consistent with a SNIIp at the host galaxy redshift (z=0.0583). Therefore both transients are unrelated to the GW event S190510g. We acknowledge the excellent support from the GTC staff. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24540 SUBJECT: LIGO/Virgo S190510g: DECam-GROWTH optical counterpart candidate DG19qcso DATE: 19/05/14 14:27:18 GMT FROM: Daniel Goldstein at Caltech Erik Kool (OKC), Daniel A. Goldstein (Caltech), and Igor Andreoni (Caltech) on behalf of the Global Relay of Observatories Watching Transients Happen (GROWTH) collaborations: As part of the follow up effort described in Andreoni et al. (2019, GCN #24467) of the high-probability region of the LALInference skymap of gravitational wave source S190510g (LIGO/VIRGO Collaboration, GCN #24448) with the Dark Energy Camera (DECam), we report the detection of an additional optical counterpart candidate, DS19qcso. The transient was detected ~2” offset to the N of the nucleus of its host galaxy through difference imaging using an automated pipeline, and appeared in g and r-band, but not in z-band. Coordinates and observed magnitudes (at jday 2458614.5) are as follows: DS19qcso Coordinates: 88.208631 -30.381382 (05:52:50.07 -30:22:53.0) g mag: 21.57 (0.13) r mag: 22.69 (0.21) z mag: > 21.9 The host galaxy is identified as 2MASXi J0552500-302254, but no host redshift is available. From Pan-STARRS imaging, we measure the host galaxy to be 15’’ across. Postage stamp images of the candidate can be viewed at the following link: https://portal.nersc.gov/project/ptf/cutouts/DG19qcso.png We thank the CTIO staff, Steve Heathcote, Kathy Vivas, Tim Abbott, for facilitating these Target of Opportunity observations. GROWTH is a worldwide collaboration comprising Caltech, USA; IPAC, USA, WIS, Israel; OKC, Sweden; JSI/UMd, USA; U Washington, USA; DESY, Germany; MOST, Taiwan; UW Milwaukee, USA; LANL USA; Tokyo Tech, Japan; IIT-B, India; IIA, India; LJMU, UK; TTU USA and USyd, Australia. GROWTH acknowledges generous support of the NSF under PIRE Grant No 1545949. An optimized schedule was generated using the ToO marshal system (Coughlin et al. 2019). Alert filtering and follow-up co-ordination is being undertaken by the GROWTH marshal system (Kasliwal et al. 2019). This research draws upon DECam data as distributed by the Science Data Archive at NOAO. NOAO is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. This project used data obtained with the Dark Energy Camera (DECam), which was constructed by the Dark Energy Survey (DES) collaboration. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24541 SUBJECT: LIGO/Virgo S190510g: Swift-XRT observations and results DATE: 19/05/14 14:56:23 GMT FROM: Phil Evans at U of Leicester P.A. Evans (U. Leicester), J.A. Kennea (PSU), A. Tohuvavohu (PSU), S.D. Barthelmy (NASA/GSFC), A.P. Beardmore (U. Leicester), A.A. Breeveld (UCL-MSSL), 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(ASDC), S.W.K. Emery (UCL-MSSL), P. Giommi (ASI), C. Gronwall (PSU), D. Hartmann (U. Clemson), H.A. Krimm (CRESST/GSFC/USRA), N.P.M. Kuin (UCL-MSSL), A.Y. Lien (GSFC/UMBC), F.E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB), J.A. Nousek (PSU), S.R. Oates (U. Warwick), P.T. O'Brien (U. Leicester), J.P. Osborne (U. Leicester), C. Pagani (U. Leicester), K.L. Page (U.Leicester), D.M. Palmer (LANL), M. Perri (ASDC), J.L. Racusin (NASA/GSFC), B. Sbarufatti (INAF-OAB/PSU), M.H. Siegel (PSU), G. Tagliaferri (INAF-OAB), E. Troja (NASA/GSFC/UMCP) report on behalf of the Swift team: Swift has performed a series of 977 observations, covering 977 separate locations within the LVC error region for the GW trigger S190510g convolved with the 2MPZ catalogue (Bilicki et al. 2014, ApJS, 210, 9), using 226 fields from the 'bayestar' GW localisation map and 751 fields from the 'LALInference' GW localisation map. As these are 3D skymaps, galaxy distances were taken into account in selecting which ones to observe. The observations currently span from 7.2 ks to 270 ks after the LVC trigger, and cover 76.9 sq degrees on the sky (corrected for overlaps). This covers 58% of the probability in the 'LALInference' skymap, and 67% after convolving with the 2MPZ galaxy catalogue, as described by Evans et al., (2016, MNRAS, 462, 1591). Using the earlier 'bayestar' skymap our observations cover 10% of the probability (14% when convolved). We have detected 33 X-ray sources. Each source is assigned a rank of 1-4 which describes how likely it is to be related to the GW trigger, with 1 being the most likely and 4 being the least likely. The ranks are described at http://www.swift.ac.uk/ranks.php. We have found: * 0 sources of rank 1 * 0 sources of rank 2 * 5 sources of rank 3 * 28 sources of rank 4 Details of these sources can be viewed online via http://www.swift.ac.uk/LVC/ For all GW triggers from O3 onwards, XRT results will appear on this page, once human verification has taken place to remove spurious sources. Additionally, our search serendipitously covered the locations of some of the other reported candidates. In particular the location of DG19fqqk/desgw-190510c (GCNs 24467, 24480) was covered 4 times. No XRT source was found with a 3-sigma upper limit of 6.1 x 10^-2 ct/sec, corresponding to a 0.3-10 keV flux of 2.6 x 10^-12 erg cm^-2 s^-1. The location of DG19llhk (GCNs 24467) was covered 3 times with no detection found, down to a 3-sigma upper limit of 6.4 x 10^-2 ct/sec, corresponding to 2.8e-12 erg cm^-2 s^-1. Both flux conversions assume a power-law spectrum with photon index=1.7 and absorption column NH=3 x 10^20 cm^-2. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 24862 SUBJECT: LIGO/Virgo S190510g: Swift UVOT - no new counterpart candidates identified DATE: 19/06/20 13:54:26 GMT FROM: Paul Kuin at MSSL N. P. M. Kuin (UCL-MSSL), A. A. Breeveld (MSSL-UCL), C. Gronwall (PSU), F. E. Marshall (NASA/GSFC), S. R. Oates (Uni. of Warwick), M.J. Page (UCL-MSSL), M. de Pasquale (Istambul U), M. H. Siegel (PSU), A. D'Ai (INAF-IASFPA), P. D'Avanzo (INAF-OAB), S. D. Barthelmy (NASA/GSFC), A. P. Beardmore (U. Leicester), D. N. Burrows (PSU), S. Campana (INAF-OAB), S. B. Cenko (NASA/GSFC), G. Cusumano (INAF-IASF PA), V. D'Elia(ASDC), P. A. Evans (U. Leicester), P. Giommi (ASI), D. Hartmann (Clemson U.), J. A. Kennea (PSU), H. A. Krimm (NSF), A. Y. Lien (GSFC/UMBC), D. B. Malesani (DTU Space), A. Melandri (INAF-OAB), J. A. Nousek (PSU), P. T. O'Brien (U. Leicester), J. P. Osborne (U. Leicester), C. Pagani (U. Leicester), K. L. Page (U.Leicester), D.M. Palmer (LANL), M. Perri (ASDC), J. L. Racusin (NASA/GSFC), T. Sakamoto (AGU), B. Sbarufatti (INAF-OAB/PSU), G. Tagliaferri (INAF-OAB), A. Tohuvavohu (PSU), and E. Troja (NASA/GSFC/UMCP) report on behalf of the Swift team: Swift UVOT instrument started follow up observations of LVC event S190510g 121 minutes after the event until just over 3 days later, observing 977 fields in the highest probability region (Evans et al., GCN Circ. No. 24541). The UVOT approach for searching for the ultraviolet-optical counterpart has been described in Kuin et al. (GCN Circ. No. 24767). The limiting magnitude can vary but typically is 18.6th magnitude (Vega). The automated UVOT processing found 2836 galaxies using the GLADE catalog and flagged 121 counterpart candidates. Human inspection of these 121 candidates found no credible optical-ultraviolet source for the event, but 105 out of the 121 candidates were due to an unstable attitude or due to image artifacts from very bright sources. Neither did further inspection of the images of the galaxies lead to a candidate missed by the automated processing.