LIGO/Virgo S190910d
GCN Circular 25749
Subject
LIGO/Virgo S190910d : No significant candidates in TAROT-GRANDMA observations
Date
2019-09-14T13:51:57Z (6 years ago)
From
Kanthanakorn Noysena at U of Toulouse III/GAHEC <kanthanakorn.noysena@irap.omp.eu>
H. Crisp (OzGrav-UWA), K. Barynova (Kyiv Uni), K. Noysena (Artemis,
IRAP), C. Stachie (Artemis), M. Boer (Artemis), N. Christensen
(Artemis), L. Eymar (Artemis), A. Klotz (IRAP), S. Antier (APC), S.
Basa (LAM), D. Corre (LAL), M. Coughlin (Caltech), D. Coward (OzGrav-
UWA), J.G. Ducoin (LAL), B. Gendre (OzGrav-UWA), P. Hello (LAL), C.
Lachaud (APC), N. Leroy (LAL), D. Turpin (NAOC), X. Wang (THU)
Report on behalf of the TAROT network and GRANDMA collaborations.
We performed tiled observations of LIGO/Virgo S190910d event with the
TAROT-Chile (TCH), TAROT-Calern (TCA) and TAROT-Reunion (TRE)
telescopes operating in the visible located respectively at
La Silla ESO observatory (LaS/ESO), the Calern site at
the Cote d'Azur observatory and at La Reunion Island, France.
The observation started for TCA at 09/10/19 02:26:06 UTC which
corresponds approximately to 60 minutes after the GW trigger time,
for TCH at 09/10/19 04:54:23 UTC which corresponds approximately to
208 minutes after the GW trigger time, and for TRE at 09/10/19
19:42:20 UTC which corresponds approximately to 1096 minutes
after the GW trigger time.
We performed the following tiled observations :
+-------+------------+------------+---------+---------+---------+
| Tele | TStart | TEnd | RA | DEC | Proba |
| scope | [UTC] | [UTC] | [deg] | [deg] | [%] |
|-------|------------+------------+---------+---------+---------|
| TCA | 2019-09-10 | 2019-09-11 | 288.95 | 42.703 | 0.1 |
| | 02:26:06 | 00:23:41 | | | |
| TCA | 2019-09-10 | 2019-09-12 | 293.916 | 42.703 | 0.1 |
| | 02:38:12 | 03:53:25 | | | |
| TCA | 2019-09-10 | 2019-09-10 | 292.014 | 44.558 | 0.2 |
| | 03:10:43 | 03:12:43 | | | |
| TCA | 2019-09-10 | 2019-09-10 | 288.467 | 40.372 | 0.1 |
| | 19:03:55 | 19:10:25 | | | |
| TCA | 2019-09-10 | 2019-09-12 | 291.433 | 42.703 | 0.1 |
| | 19:10:44 | 00:25:43 | | | |
| TCA | 2019-09-10 | 2019-09-12 | 290.883 | 40.847 | 0.1 |
| | 19:43:07 | 00:18:54 | | | |
| TCA | 2019-09-10 | 2019-09-12 | 296.398 | 42.703 | 0.2 |
| | 20:21:59 | 01:17:51 | | | |
| TCA | 2019-09-10 | 2019-09-10 | 300.95 | 48.27 | 0.1 |
| | 20:28:49 | 23:05:01 | | | |
| TCA | 2019-09-10 | 2019-09-10 | 298.223 | 48.27 | 0.1 |
| | 20:40:45 | 20:47:15 | | | |
| TCA | 2019-09-10 | 2019-09-10 | 281.219 | 39.897 | 0.1 |
| | 20:47:35 | 23:23:44 | | | |
| TCA | 2019-09-10 | 2019-09-10 | 293.299 | 40.847 | 0.1 |
| | 20:54:25 | 23:30:34 | | | |
| TCA | 2019-09-10 | 2019-09-11 | 297.421 | 46.414 | 0.1 |
| | 22:19:34 | 00:55:47 | | | |
| TCA | 2019-09-10 | 2019-09-10 | 279.525 | 29.713 | 0.2 |
| | 22:26:24 | 22:32:55 | | | |
| TCA | 2019-09-10 | 2019-09-10 | 270.95 | 20.434 | 0.1 |
| | 23:30:54 | 23:37:26 | | | |
| TCA | 2019-09-11 | 2019-09-12 | 298.881 | 42.703 | 0.2 |
| | 00:59:25 | 03:01:04 | | | |
| TCA | 2019-09-11 | 2019-09-12 | 288.467 | 39.897 | 0.2 |
| | 01:31:13 | 01:24:36 | | | |
| TCA | 2019-09-11 | 2019-09-11 | 306.329 | 42.703 | 0.2 |
| | 01:38:03 | 19:01:53 | | | |
| TCA | 2019-09-11 | 2019-09-12 | 299.673 | 44.558 | 0.2 |
| | 01:44:53 | 03:46:39 | | | |
| TCA | 2019-09-11 | 2019-09-11 | 302.715 | 46.414 | 0.1 |
| | 02:23:09 | 21:56:23 | | | |
| TCA | 2019-09-11 | 2019-09-11 | 297.12 | 44.558 | 0.2 |
| | 02:30:02 | 22:03:09 | | | |
| TCA | 2019-09-11 | 2019-09-12 | 302.227 | 44.558 | 0.2 |
| | 03:15:20 | 03:07:52 | | | |
| TCA | 2019-09-11 | 2019-09-12 | 303.847 | 42.703 | 0.2 |
| | 03:22:11 | 03:14:37 | | | |
| TCA | 2019-09-11 | 2019-09-12 | 304.78 | 44.558 | 0.2 |
| | 03:29:01 | 01:11:08 | | | |
| TCA | 2019-09-11 | 2019-09-11 | 273.093 | 31.569 | 0.1 |
| | 19:14:29 | 23:40:37 | | | |
| TCA | 2019-09-11 | 2019-09-12 | 286.051 | 39.897 | 0.1 |
| | 19:21:15 | 01:56:16 | | | |
| TCA | 2019-09-11 | 2019-09-11 | 307.333 | 44.558 | 0.2 |
| | 19:27:59 | 21:43:59 | | | |
| TCA | 2019-09-11 | 2019-09-12 | 291.433 | 42.703 | 0.1 |
| | 19:59:49 | 00:25:43 | | | |
| TCA | 2019-09-12 | 2019-09-12 | 55.325 | -9.256 | 0.1 |
| | 00:26:15 | 00:32:35 | | | |
| TCA | 2019-09-12 | 2019-09-12 | 301.364 | 42.703 | 0.2 |
| | 02:41:47 | 02:48:05 | | | |
| TCA | 2019-09-13 | 2019-09-13 | 305.362 | 46.414 | 0.1 |
| | 21:16:13 | 21:22:32 | | | |
| TCA | 2019-09-13 | 2019-09-13 | 278.402 | 35.711 | 0.2 |
| | 22:01:36 | 22:07:56 | | | |
+-------+------------+------------+---------+---------+---------+
| TCH | 2019-09-10 | 2019-09-10 | 71.936 | -43.595 | 0.5 |
| | 04:54:23 | 09:43:01 | | | |
| TCH | 2019-09-10 | 2019-09-10 | 68.305 | -38.141 | 0.4 |
| | 05:01:28 | 07:19:33 | | | |
| TCH | 2019-09-10 | 2019-09-11 | 73.993 | -45.414 | 0.5 |
| | 05:14:37 | 08:32:07 | | | |
| TCH | 2019-09-10 | 2019-09-10 | 70.627 | -38.141 | 0.3 |
| | 05:26:48 | 05:33:18 | | | |
| TCH | 2019-09-10 | 2019-09-10 | 77.221 | -52.686 | 0.5 |
| | 05:33:37 | 07:46:47 | | | |
| TCH | 2019-09-10 | 2019-09-10 | 84.283 | -56.323 | 0.4 |
| | 05:47:04 | 05:53:34 | | | |
| TCH | 2019-09-10 | 2019-09-10 | 71.326 | -47.232 | 0.5 |
| | 05:59:14 | 06:05:44 | | | |
| TCH | 2019-09-10 | 2019-09-10 | 83.782 | -54.505 | 0.4 |
| | 06:06:03 | 06:12:33 | | | |
| TCH | 2019-09-10 | 2019-09-11 | 71.385 | -45.414 | 0.5 |
| | 06:12:52 | 06:55:42 | | | |
| TCH | 2019-09-10 | 2019-09-11 | 72.473 | -39.959 | 0.3 |
| | 06:19:40 | 07:07:00 | | | |
| TCH | 2019-09-10 | 2019-09-11 | 76.74 | -47.232 | 0.4 |
| | 06:47:14 | 07:53:38 | | | |
| TCH | 2019-09-10 | 2019-09-11 | 69.991 | -41.777 | 0.5 |
| | 06:59:27 | 08:20:28 | | | |
| TCH | 2019-09-10 | 2019-09-11 | 74.075 | -49.05 | 0.5 |
| | 07:32:26 | 08:34:25 | | | |
| TCH | 2019-09-10 | 2019-09-10 | 76.888 | -49.05 | 0.5 |
| | 08:57:02 | 09:03:32 | | | |
| TCH | 2019-09-10 | 2019-09-11 | 74.033 | -47.232 | 0.5 |
| | 09:03:50 | 07:40:02 | | | |
| TCH | 2019-09-10 | 2019-09-11 | 70.089 | -39.959 | 0.4 |
| | 09:10:38 | 07:46:50 | | | |
| TCH | 2019-09-10 | 2019-09-11 | 80.596 | -54.505 | 0.5 |
| | 09:23:14 | 06:36:14 | | | |
| TCH | 2019-09-10 | 2019-09-10 | 80.272 | -52.686 | 0.4 |
| | 09:48:54 | 09:55:24 | | | |
| TCH | 2019-09-11 | 2019-09-11 | 69.401 | -43.595 | 0.5 |
| | 07:08:34 | 07:15:04 | | | |
| TCH | 2019-09-11 | 2019-09-11 | 71.263 | -49.05 | 0.5 |
| | 07:53:56 | 08:00:26 | | | |
| TCH | 2019-09-11 | 2019-09-11 | 74.17 | -52.686 | 0.5 |
| | 08:07:10 | 08:13:40 | | | |
| TCH | 2019-09-11 | 2019-09-14 | 67.705 | -39.959 | 0.4 |
| | 08:52:49 | 03:58:36 | | | |
| TCH | 2019-09-11 | 2019-09-13 | 77.41 | -54.505 | 0.5 |
| | 09:50:26 | 09:30:15 | | | |
| TCH | 2019-09-12 | 2019-09-14 | 74.121 | -50.868 | 0.5 |
| | 06:35:37 | 06:10:08 | | | |
| TCH | 2019-09-12 | 2019-09-13 | 77.048 | -50.868 | 0.5 |
| | 06:42:25 | 08:44:52 | | | |
| TCH | 2019-09-13 | 2019-09-13 | 80.95 | -56.323 | 0.5 |
| | 05:56:17 | 06:02:47 | | | |
+-------+------------+------------+---------+---------+---------+
| TRE | 2019-09-10 | 2019-09-12 | 76.154 | -53.182 | 2.3 |
| | 19:42:20 | 21:40:33 | | | |
| TRE | 2019-09-10 | 2019-09-10 | 68.108 | -32.727 | 1.2 |
| | 19:55:17 | 20:01:51 | | | |
| TRE | 2019-09-10 | 2019-09-13 | 65.455 | -40.909 | 1.9 |
| | 20:26:43 | 00:13:13 | | | |
| TRE | 2019-09-10 | 2019-09-12 | 60.779 | -28.636 | 1.4 |
| | 20:40:01 | 22:57:13 | | | |
| TRE | 2019-09-10 | 2019-09-10 | 63 | -24.545 | 1.1 |
| | 20:52:16 | 20:58:44 | | | |
| TRE | 2019-09-10 | 2019-09-13 | 84.255 | -57.273 | 1.9 |
| | 21:53:12 | 00:26:27 | | | |
| TRE | 2019-09-10 | 2019-09-12 | 69.677 | -45 | 2.3 |
| | 22:06:21 | 00:29:45 | | | |
| TRE | 2019-09-10 | 2019-09-12 | 65.455 | -28.636 | 1.1 |
| | 22:31:13 | 21:27:20 | | | |
| TRE | 2019-09-10 | 2019-09-10 | 72 | -36.818 | 1.1 |
| | 22:44:27 | 22:51:01 | | | |
| TRE | 2019-09-10 | 2019-09-10 | 82.105 | -49.091 | 1.1 |
| | 23:03:28 | 23:09:56 | | | |
| TRE | 2019-09-10 | 2019-09-12 | 100 | -65.455 | 1.2 |
| | 23:16:21 | 23:28:34 | | | |
| TRE | 2019-09-11 | 2019-09-13 | 61.714 | -36.818 | 1.3 |
| | 19:17:10 | 01:10:44 | | | |
| TRE | 2019-09-11 | 2019-09-13 | 58.5 | -24.545 | 1.2 |
| | 19:29:41 | 01:23:57 | | | |
| TRE | 2019-09-12 | 2019-09-12 | 75.79 | -49.091 | 2.3 |
| | 00:11:02 | 23:41:55 | | | |
| TRE | 2019-09-12 | 2019-09-12 | 66.857 | -36.818 | 1.9 |
| | 00:36:30 | 00:43:04 | | | |
| TRE | 2019-09-12 | 2019-09-13 | 76.596 | -57.273 | 1.6 |
| | 01:20:51 | 00:52:08 | | | |
| TRE | 2019-09-12 | 2019-09-12 | 69.474 | -49.091 | 1.7 |
| | 20:10:59 | 20:17:33 | | | |
| TRE | 2019-09-12 | 2019-09-12 | 70.909 | -40.909 | 2.1 |
| | 21:46:19 | 21:52:47 | | | |
| TRE | 2019-09-13 | 2019-09-13 | 83.077 | -53.182 | 1.7 |
| | 00:32:21 | 00:38:49 | | | |
| TRE | 2019-09-13 | 2019-09-13 | 63.243 | -32.727 | 1.6 |
| | 19:47:45 | 19:54:13 | | | |
| TRE | 2019-09-13 | 2019-09-13 | 85.714 | -61.364 | 1.5 |
| | 20:00:58 | 20:07:32 | | | |
+-------+------------+------------+---------+---------+---------+
TStart and TEnd refers respectively to the time of the first and last
exposure for a given tile. Observations are not necessarily continuous
in this interval. The Probability refers to the 2D spatial
probability of the GW skymap enclosed in a given tile. Each tile is
1.9x1.9 degrees for both TCA and TCH and 4.2x4.2 degrees for TRE.
These observations cover about 37% of the cumulative probability
of the LALInference skymap available on Sep 10, 2019 22:33:43 UTC.
The typical limiting magnitude in AB mode is 18.0
for a 60.0 s exposure for TCH and TCA and 17.0 for
a 60.0 s exposure for TRE.
The coverage map is available at:
https://grandma-owncloud.lal.in2p3.fr/index.php/s/D0YLFF9t7LBekQM
No significant transient candidates were found during our
low latency analysis.
GRANDMA (Global Rapid Advanced Network Devoted to the Multi-messenger
Addicts) is a network of robotic telescopes connected all over the
world with both photometry and spectrometry capabilities for
Time-domain Astronomy (https://grandma.lal.in2p3.fr/). Details on
the TAROT telescopes are available on the GRANDMA web pages.
GCN Circular 25741
Subject
LIGO/Virgo S190910d: MASTER previous detection of Gaia19eba/AT2019qam
Date
2019-09-13T12:18:57Z (6 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, F.Balakin, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa,A.Kuznetsov, V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov,
V.Senik, T.Pogrosheva, K.Pozdnyakov, A.Chasovnikov, V.Topolev, D.Kuvshinov(Lomonosov Moscow State University, SAI, Physics Department),
R. Podesta, C.Lopez, F. Podesta, C.Francile(Observatorio Astronomico Felix Aguilar OAFA),
H.Levato(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),
R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias),
D. Buckley(South African Astronomical Observatory),
O.A. Gres, N.M. Budnev, O.Ershova(Irkutsk State University, API),
A. Tlatov, D. Dormidontov(Kislovodsk Solar Station of the Pulkovo Observatory),
V. Yurkov, A. Gabovich, Yu. Sergienko(Blagoveschensk Educational State University)
MASTER Global Robotic Net (http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol.2010, 30L)
started inspect of LIGO/Virgo S190910d (GCN 25695) 157 sec after trigger time
at 2019-09-10 01:28:56 UT (Lipunov et al. GCN 25694)
We analyzed Gaia OT candidates from compact binary merger candidate LIGO/Virgo S190910d
Gaia19eba/AT2019qam ( Kostrzewa-Rutkowska et al. GCN25739 )
at RA,Dec(2000)=52.99630 -26.07598
at MASTER archieve images.
There is OT with unfiltered m_OT~18.5 on 2 images at
2019-09-02 23:00:27, 22:48:02UT, it means no connection with GW S190910d
GCN Circular 25739
Subject
LIGO/Virgo S190910d: Gaia Photometric Alerts transient candidate
Date
2019-09-13T11:33:37Z (6 years ago)
From
Zuzanna Kostrzewa-Rutkowska at SRON <z.p.kostrzewa@sron.nl>
Z. Kostrzewa-Rutkowska (Leiden Observatory), S. Hodgkin, A. Delgado, D.L. Harrison, M. van Leeuwen, G. Rixon, A. Yoldas (IoA Cambridge), D. Eappachen, P.G. Jonker (SRON/RU) on behalf of Gaia Alerts team report the discovery of a transient candidate within the probability skymap of S190910d (the LIGO Scientific Collaboration and the Virgo Collaboration, GCN 25695):
---------------------------------------------------------------------------
Name TNSid Date [TCB] RaDeg DecDeg AlertMag URL
---------------------------------------------------------------------------
Gaia19eba AT2019qam 2019-09-11T07:02:41 52.99630 -26.07598 18.14 http://gsaweb.ast.cam.ac.uk/alerts/alert/Gaia19eba/
Acknowledgements: This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. ZKR acknowledges funding from the Netherlands Research School for Astronomy (NOVA). DE and PGJ acknowledge support from the European Research Council under ERC Consolidator Grant agreement no 647208.
GCN Circular 25737
Subject
LIGO/Virgo S190910d: No Counterparts in DDOTI/OAN Optical Observations
Date
2019-09-13T06:02:44Z (6 years ago)
From
Emma Margarita Pereyra Talamantes at IA-UNAM Ensenada <mpereyra@astro.unam.mx>
Margarita Pereyra <mpereyra@astro.unam.mx> (UNAM), Alan M. Watson (UNAM),
Nat Butler (ASU), Simone Dichiara (GSFC/UMD), Rosa L. Becerra (UNAM), Diego
Gonzalez (UNAM), Alexander Kutyrev (GSFC/UMD), William H. Lee (UNAM),
Eleonora Troja (GSFC/UMD), Gabriele Minervini (INAF/IAPS-Rome) and Tanner
Wolfram (ASU) report:
We observed LIGO/Virgo S190910d event (Badaracco F; LVC et al.; GCN #25695)
with the DDOTI/OAN wide-field imager at the Observatorio Astronomico
Nacional on Sierra San Pedro Martir (http://ddoti.astroscu.unam.mx) from
2019-09-10 04:25 to 2019-09-10 08:15 UTC ( ~ 3.0 to 7.8 hours after the
event).
We observed approximately 289 square degrees of the sky, with 5 pointings
centered on 17:30:00.089 +19:08:01.30, 17:49:53.330 +17:34:38.58,
17:49:53.330 +24:35:33.03, 18:09:04.387 +22:40:56.15 and 18:09:46.574
+30:03:26.65. We obtained about 18, 36, 18, 30 and 18 minutes total
exposure on each pointing, respectively. These regions include about 6% of
the 2D probability in the current BAYESTAR map and 5% of the 2D probability
in the LALInference map.
We calibrated our images against the APASS catalog. Our 10-sigma limiting
magnitude are typically between w = 18.04 and w = 18.96.
Comparing our 10-sigma detections against the USNO-B1 catalog, we detect no
uncataloged sources with significant fading.
We thank the staff of the Observatorio Astronomico Nacional in San Pedro
Martir.
GCN Circular 25734
Subject
LIGO/Virgo S190910d: No transient candidates in CALET observations.
Date
2019-09-13T03:22:51Z (6 years ago)
From
Yuta Kawakubo at Louisiana State U./CALET <kawakubo1@lsu.edu>
S. Ricciarini (U of Florence), A. Yoshida, T. Sakamoto,
V. Pal'shin, S. Sugita (AGU), Y. Kawakubo (LSU),
K. Yamaoka (Nagoya U), S. Nakahira (RIKEN), Y. Asaoka,
S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U),
N. Cannady (GSFC/UMBC), M. L. Cherry (LSU),
P. S. Marrocchesi (U of Siena),
and the CALET collaboration:
The CALET Gamma-ray Burst Monitor (CGBM) was operating at the trigger
time of S190910d T0 = 2019-09-10 01:26:19.243 UT (The LIGO Scientific
Collaboration and Virgo Collaboration, GCN Circ. 25695 and 25723).
No CGBM on-board trigger occurred around the event time. Based
on the LIGO-Virgo localization sky map, the summed LIGO probabilities
inside the CGBM HXM (7 - 3000 keV) and SGM (40 keV - 28 MeV) fields
of view are 1 % and 64 %, respectively (and 77 % credible region of the
updated localization map was above the horizon). The HXM and SGM
fields of view were centered at RA = 108.8 deg, Dec = 29.9 deg and
RA = 100.8 deg, Dec = 22.9 deg at T0, respectively.
The CALET Calorimeter (CAL) was operating in the low energy
trigger mode at the trigger time of S190910d. Using the CAL data,
we have searched for gamma-ray events in the 1-10 GeV band
from -60 sec to +60 sec from the GW trigger time and found no
candidates. There is no significant overlap with the LIGO-Virgo
high probability localization region. The CAL FOV was centered at
RA=100.8 deg, Dec=22.9 deg at T0.
GCN Circular 25729
Subject
LIGO/Virgo S190910d and S190910h: No counterpart candidates in KAIT observations
Date
2019-09-11T22:57:48Z (6 years ago)
From
Weikang Zheng at UC Berkeley <weikang@berkeley.edu>
James Sunseri, Shaunak Modak, Benjamin E. Stahl, Thomas de Jaeger,
Yukei Murakami, WeiKang Zheng, Sergiy Vasylyev, Andrew Hoffman,
Nachiket Girish, Keto D. Zhang, and Alexei V. Filippenko (UC Berkeley)
report on behalf of the Lick/KAIT GW follow-up team:
The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, observed the 90% region of the gravitational-wave
event S190910h (GCN 25606; GCN 25614) and S190910d detected by LIGO/Virgo.
More than one thousand galaxies were selected from the Glade catalog V1.0
(Dalya et al., 2018, MNRAS, 479, 2374; http://aquarius.elte.hu/glade/)
according to their priority score. On Sep. 11 UT, KAIT observed 224 of
them for event S190910d (started at 1.08 days after trigger), and 154 of
them for event S190910h (started at 0.98 days after trigger), according
to their priority scores and elevation visibility, with each clear-filter
exposure time being 60 s. Our typical limiting mag is 19.0. No viable
counterparts were identified and the analysis is ongoing. A full list
of galaxies observed by KAIT is given below.
GladeID UT(Sep11) RA_J2000 Dec_J2000
For S190910d
-----------------------------------------------
G1313601 03:23:13 17:01:09.972 +01:38:37.9248
G1315118 03:24:24 17:02:20.0501 -05:10:43.1436
G0824618 03:28:23 17:41:18.2885 +17:22:04.8144
G0793601 03:29:32 17:43:57.81 +19:35:09.1896
G1048996 03:30:45 17:53:50.7787 +14:02:53.718
G1217685 03:31:56 17:55:20.6544 +23:15:12.3948
G0636803 03:33:05 17:56:20.2442 +26:21:59.58
G0862839 03:34:15 17:56:56.6748 +22:14:02.9544
G1437178 03:35:24 17:59:21.8261 +20:44:31.7184
G0782167 03:36:33 17:59:33.7939 +23:52:52.7628
G0149658 03:37:45 18:02:22.5367 +28:54:05.0868
G0130482 03:38:54 18:04:57.0703 +30:26:47.0724
G1346624 03:40:05 18:06:43.2348 +22:25:07.194
G0929719 03:41:15 18:07:28.0517 +23:06:47.9304
G1317538 03:42:26 18:09:42.1802 +28:15:52.7976
G1400962 03:43:35 18:15:13.4326 +30:51:10.6776
G0484840 03:44:45 18:16:17.3803 +27:31:51.2508
G0634483 03:45:56 18:17:21.4894 +19:42:55.1412
G0066266 03:47:07 18:17:55.2247 +31:51:53.424
G0755437 03:48:18 18:17:56.1036 +33:48:59.4324
G0948596 03:49:29 18:17:59.8462 +28:36:08.3988
G1188319 03:50:36 18:18:49.043 +29:01:33.9276
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For S190910h
-----------------------------------------------
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G0756115 11:14:31 02:57:53.0868 +13:01:50.8656
G0641223 11:15:40 02:58:57.8184 +13:34:58.332
G0595607 11:17:03 03:00:30.444 +49:21:13.3848
G0032459 11:18:14 03:00:55.9003 +44:21:01.4508
G0664397 11:19:34 03:02:01.4923 +35:45:35.3628
G0624050 11:21:36 03:02:41.2565 +64:20:54.6936
G0755906 11:23:40 03:03:25.3682 +35:46:21.5328
G0687315 11:24:51 03:03:31.2542 +27:41:12.012
G0777619 11:26:12 03:03:40.4251 +51:34:31.8144
G0672859 11:27:24 03:05:05.8877 +50:19:24.096
G0819835 11:29:23 03:06:04.0193 +65:16:38.7408
G0738775 11:31:20 03:06:24.3511 +52:34:54.9264
G0773786 11:32:46 03:07:32.3208 -00:57:51.7176
G0560446 11:33:58 03:08:26.249 +04:06:38.8368
G0618299 11:36:10 03:08:55.199 +70:33:47.7756
G0653455 11:38:17 03:09:12.4054 +48:43:41.034
G0668711 11:39:36 03:09:36.9415 +18:30:02.34
G0583767 11:40:54 03:09:42.3797 +46:25:08.958
G0599454 11:42:06 03:10:38.0302 +48:52:10.7328
G0689860 11:43:19 03:11:04.26 +52:13:21.1764
G0699846 11:44:30 03:11:28.7182 +51:50:01.8636
G0714449 11:45:52 03:13:06.6686 +28:38:05.6796
G0709552 11:47:11 03:13:33.0982 +51:41:22.8408
G0478585 11:48:24 03:15:41.7965 +47:42:30.7512
G0716337 11:49:46 03:16:16.1443 +12:55:54.1632
G0566054 11:51:02 03:17:31.6068 +37:02:46.5108
G0576329 11:52:19 03:18:50.6928 +08:47:33.8208
G0618362 11:53:43 03:20:16.1976 +47:33:03.7584
G0571206 11:55:51 03:20:36.935 +67:50:43.6812
G0600454 12:19:27 03:20:38.1098 +43:04:44.778
G0616471 12:20:43 03:22:34.3661 +14:54:48.9204
G0710733 12:21:53 03:24:00.2059 +16:10:57.882
G0732746 12:23:09 03:25:11.5723 -06:10:51.006
G0562026 12:24:29 03:27:03.3938 +31:44:52.062
G0819943 12:26:42 03:27:45.0631 +69:44:57.0048
G0713851 12:28:54 03:27:46.0903 +31:15:27.2124
G0557004 12:30:05 03:30:07.3673 +35:55:17.8428
G0658066 12:31:20 03:31:21.2311 +14:23:05.4744
G0779270 12:32:42 03:33:30.8496 +48:28:40.224
G0756702 12:34:04 03:34:37.5595 +12:03:53.1936
G1361052 12:35:21 03:34:49.5794 -09:50:33.2196
G1085027 12:36:43 03:35:04.9274 +33:03:14.526
G0695101 12:38:00 03:37:07.4249 +49:03:08.7444
G0705569 12:39:24 03:37:50.9911 +09:36:30.0528
G1206515 12:40:31 03:38:14.0918 +10:05:03.8832
G0783345 12:42:42 03:38:21.4646 +64:19:22.9044
G0659256 12:44:51 03:38:40.5679 +09:58:11.9388
G0695313 12:47:02 03:38:53.2718 +64:14:58.9272
G0844381 12:49:08 03:38:57.2554 +32:39:11.0736
G0793910 12:50:22 03:39:15.0166 +14:27:37.7352
G0496810 12:51:32 03:39:28.3063 +13:23:41.7444
G0795493 12:52:52 03:39:39.0948 +45:43:47.9856
G0734420 12:54:08 03:40:45.1327 +17:44:28.2084
G0039699 12:55:18 03:41:01.3459 +13:34:19.1136
G0739254 12:56:34 03:41:05.8008 +39:34:57.7416
G0620810 12:57:51 03:41:17.3868 +10:44:32.676
G0746601 12:59:09 03:42:24.0298 +39:14:40.362
G0743139 13:00:25 03:44:42.691 +15:44:11.7312
G0734211 13:01:44 03:47:39.7678 +39:20:48.8724
G1296306 13:07:06 03:50:23.4166 +06:58:23.1672
G0784665 13:09:14 03:51:58.2413 +64:13:51.7764
G0737259 13:11:18 03:52:16.3944 +13:24:19.3608
G0815176 13:12:34 03:52:17.9206 +41:06:54.9396
G0233228 13:13:43 03:53:38.6417 +40:53:20.7168
GCN Circular 25728
Subject
LIGO/Virgo S190910d: No neutrino candidates at Pierre Auger Observatory
Date
2019-09-11T16:15:41Z (6 years ago)
From
Jaime Alvarez-Muniz at Pierre Auger Observatory <jaime.alvarezmuniz@gmail.com>
J. Alvarez-Muniz, F. Pedreira, E. Zas (Univ. Santiago de Compostela, Spain),
K. H. Kampert & M. Schimp (Bergische Universitat, Wuppertal, Germany)
on behalf of the Pierre Auger Collaboration.
In response to:
LIGO/Virgo GW trigger S190910d
T0=2019-09-10 01:26:19 UTC
We searched for Ultra-High-Energy (UHE) neutrinos with energies
above ~ 1e17 eV in data collected with the Surface Detector (SD)
of the Pierre Auger Observatory in a [-500,500] second interval
about the LIGO-Virgo trigger S190910d as well as in a 24 hr time
interval following the event.
NO events survived the cuts applied to reject the background due
to UHE Cosmic Rays i.e. NO neutrino candidates were detected.
The field of view (fov) where the SD of Auger is sensitive to UHE
neutrinos (corresponding to inclined directions with respect to the
vertical relative to the ground) was PARTIALLY COINCIDENT (74.9%) with
the LIGO/Virgo 90% localization region (LALInference.fits.gz,0)
at the time T0 of the merger alert, achieving TOTAL OVERLAP
at approximately T0+1.4 hours
-------
The Pierre Auger Observatory is an UHE Cosmic Ray detector
located in the Mendoza Province in Argentina. It consists of
an array of Water Cherenkov detectors spread over a total surface
of 3000 km^2 arranged in a triangular grid of 1.5 km side as well
as Fluorescence telescopes and other systems
(see 10.1016/j.nima.2015.06.058 for more information).
For neutrino searches from GW events with Auger, please refer to:
https://journals.aps.org/prd/pdf/10.1103/PhysRevD.94.122007
https://arxiv.org/abs/1906.07422
GCN Circular 25725
Subject
LIGO/Virgo S190910d: WHT spectroscopy of ZTF19abyfhov, ZTF19abyfhaq, ZTF19abyfbii
Date
2019-09-11T06:24:35Z (6 years ago)
From
Giacomo Cannizzaro at SRON <g.cannizzaro@sron.nl>
G. Cannizzaro (SRON/Radboud Univ), I. Pastor-Marazuela (API/ASTRON), P. Jonker (SRON/Radboud Univ), K. Maguire (TCD), M. Fraser (UCD), report on behalf of the GW@WHT collaboration:
We obtained optical spectroscopy of ZTF19abyfhov/AT2019pvu, ZTF19abyfhaq/AT2019pvv and ZTF19abyfbii/AT2019pvz (GCN 25706), three optical transients within the LIGO/Virgo S190910d sky localisation (GCN 25695) with the ACAM instrument mounted on the William Herschel Telescope located at the Roque de Los Muchachos Observatory, La Palma, Spain. We cross-correlate the transient spectra with a library of supernova template spectra using the code SNID (Blondin and Tonry, 2007).
ZTF19abyfhov/AT2019pvu is classified as a SNIa, 3 days before peak, at redshift z=0.132.
The spectrum of ZTF19abyfhaq/AT2019pvv has a low SNR, preventing a precise classification.
ZTF19abyfbii/AT2019pvz is classified as a SNIa 91T-like, 5 days before peak, at redshift z=0.118. This redshift is consistent with the photometric redshift reported in GCN 25706.
GCN Circular 25723
Subject
LIGO/Virgo S190910d: Updated Sky Localization
Date
2019-09-11T01:15:04Z (6 years ago)
From
Shreya Anand at GROWTH Caltech <sanand@caltech.edu>
The LIGO Scientific Collaboration and the Virgo Collaboration report:
We have conducted further analysis of the data from LIGO Hanford
Observatory (H1), LIGO Livingston Observatory (L1) and Virgo
Observatory (V1) around the time of the compact binary merger (CBC)
candidate S190910d (GCN Circular 25695). Parameter estimation has
been performed using LALInference [1] and a new sky map,
LALInference.fits.gz, distributed via GCN Notice, is available for retrieval
from the GraceDB event page:
https://gracedb.ligo.org/superevents/S190910d
The preferred sky map at this time is LALInference.fits.gz. The 90%
credible region is 2482 deg2. Marginalized over the whole sky, the a
posteriori luminosity distance estimate is 632 +/- 186 Mpc (a posteriori
mean +/- standard deviation).
For further information about analysis methodology and the contents of
this alert, refer to the LIGO/Virgo Public Alerts User Guide
<https://emfollow.docs.ligo.org/userguide/>.
[1] Veitch et al. PRD 91, 042003 (2015)
GCN Circular 25721
Subject
LIGO/Virgo S190910d: AT2019pvu, AT2019pvv, AT2019pvz and AT2019pwa 10.4m GTC spectroscopy
Date
2019-09-10T23:31:49Z (6 years ago)
From
Alberto J. Castro-Tirado at IAA-CSIC <ajct@iaa.es>
A. J. Castro-Tirado (IAA-CSIC), A. F. Valeev and V. V. Sokolov
(SAO-RAS), Y.-D. Hu and E. Fernandez-Garcia (IAA-CSIC), I. Carrasco and
A. Castellon (UMA) and J. Font Serra (GRANTECAN, IAC, ULL), on behalf of
a larger collaboration, report:
Following the detection of ZTF19abyfhov/AT2019pvu,
ZTF19abyfhaq/AT2019pvv, ZTF19abyfbii/AT2019pvz and
ZTF19abyfazm/AT2019pwa (Anand et al., GCN 25706) within the error area
of the GW event S190910d (LVC, GCNC 25695), we obtained imaging and
optical spectra covering the range 3700-10000 A with the 10.4m GTC
telescope equipped with OSIRIS in La Palma (Spain) starting on Sep 10,
20:25 UT.
For AT2019pvu, a magnitude r = 20.33 +/- 0.05 on Sep 10, 20:58 UT is
derived. Cross-correlating the transient spectrum (broad lines) with
supernova template spectra in SNID (Blondin & Tonry, 2007), we find
a good match to the spectra of SNIa at redshift z = 0.133 +/- 0.001.
For AT2019pvv, a magnitude r = 21.08 +/- 0.05 on Sep 10, 22:14 UT is
derived. The spectrum shows a faint H-alpha line in emission at z = 0
but the low S/N ratio prevents a more precise classification at this
stage.
For AT2019pvz, a magnitude r = 20.26 +/- 0.05 on Sep 10, 20:27 UT is
derived. The spectrum is consistent with that of a SN Ia at the nearby
host galaxy redshift z = 0.1286 +/- 0.0005 (based on H-alpha, H-beta, [O
III] and others narrow emission lines).
For AT2019pwa, a magnitude r = 18.38 +- 0.03 on Sep 10, 21:31 UT is
derived. The spectrum displays a blue continuum with the Ca II H&K 3934
A and 3969 A doublet in absorption at z = 0 being the only clear
features, which supports the object being a cataclysmic variable in our
Galaxy, in agreement with Perley and Copperwheat (GCNC 25720).
Therefore we consider ZTF19abyfhov/AT2019pvu, ZTF19abyfhaq/AT2019pvv,
ZTF19abyfbii/AT2019pvz and ZTF19abyfazm/AT2019pwa to be unrelated to the
GW event S190910d.
GCN Circular 25720
Subject
LIGO/Virgo S190910d: Liverpool Telescope spectroscopy of ZTF19abyfazm
Date
2019-09-10T21:48:22Z (6 years ago)
From
Daniel Perley at Liverpool JMU <d.a.perley@ljmu.ac.uk>
D. A. Perley and C. M. Copperwheat (LJMU) report on behalf of the GROWTH
collaboration:
We acquired imaging and spectroscopy of ZTF19abyfazm/AT2019pwa (Anand et
al., GCN 25706), an optical transient within the error region of
gravitational wave trigger S190910d (LVC et al. GCN 25695), with the 2m
Liverpool Telescope. A sequence of 60-second images was acquired in g,
r, and i filters using IO:O, followed by 2x500s of spectroscopy with
SPRAT, between 20:53 and 21:20 on 2019-09-10 (UT).
The source remains bright and blue, although has faded slightly since
the time of ZTF discovery (we measure AB magnitudes of g=17.95, r=18.30,
i=18.65 at approximately MJD=58736.87). No significant absorption or
emission features are visible in the spectrum. We conclude that this
source is likely the eruption of an uncatalogued cataclysmic variable
within our Galaxy, although further monitoring will be needed to confirm
this.
We thank the MOPTOP commissioning team for their patience while
acquiring these observations.
DisclaimerNone
GCN Circular 25719
Subject
LIGO/Virgo S190910d: AstroSat CZTI upper limits
Date
2019-09-10T16:36:44Z (6 years ago)
From
Varun Bhalerao at Indian Inst of Tech <varunb@iitb.ac.in>
A. Anumarlapudi (IUCAA), V. Shenoy (IITB), Aarthy E. (PRL), V. Bhalerao (IITB), D. Bhattacharya (IUCAA), A. R. Rao (TIFR), S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:
We have carried a search for X-ray candidates in Astrosat CZTI data in a 100 sec window around the trigger time of the NSBH merger event S190910d (UTC 2019-09-10 01:26:19.000, GraceDB event). CZTI is a coded aperture mask instrument that has considerable effective area for about 29% of the entire sky, but is also sensitive to brighter transients from the entire sky. At the time of merger, Astrosat's nominal pointing is (RA=0:33:36.4 (8.401), DEC=28:41:36.7 (28.694)), which is 94.84 deg away from the maximum probability location. At the time of merger event, the Earth-satellite-transient angle corresponding to maximum probability location is ~ 61.63 deg and hence is occulted by Earth in satellite's frame. In a time interval of 100 sec around the event, the region of the localisation map which is not occulted by Earth in the satellite's frame has a cumulative probability of 0.64 (64%).
CZTI data were de-trended to remove orbit-wise background variation. We then searched data from three of the four independent, identical quadrants to look for coincident spikes in the count rates. Searches were undertaken by binning the data in 0.1s, 1s, and 10s respectively. Statistical fluctuations in count rates were estimated by using data from 10 (+-5) neighbouring orbits. We selected confidence levels such that the probability of a false trigger in a 1000 sec window is 10^-4. We do not find any evidence for any hard X-ray transient in this window, in the CZTI energy range of 20-200 keV.
We convert our count rates into flux by assuming that the source spectrum is a power law with alpha = -1.0. We use a detailed mass model of the satellite to calculate the instrument response for every htm grid point that fall in LIGO localization region and calculate flux limit in that direction. We get the following upper limits for source flux in the 20-200 keV band by taking a probability weighted mean of flux limit and are reported here in terms of binning time:
0.1 s: flux limit= 9.84e-06 ergs/cm^2/s ; fluence limit= 9.84e-07 ergs/cm^2
1.0 s: flux limit= 2.97e-06 ergs/cm^2/s ; fluence limit= 2.97e-06 ergs/cm^2
10.0 s: flux limit= 3.88e-07 ergs/cm^2/s ; fluence limit= 3.88e-06 ergs/cm^2
CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.
GCN Circular 25717
Subject
LIGO/Virgo S190910d: No counterpart candidates in Fermi-LAT observations
Date
2019-09-10T15:05:24Z (6 years ago)
From
Magnus Axelsson at Stockholm U. <magaxe@kth.se>
M. Axelsson (KTH and Stockholm Univ.), L. Scotton (University and INFN, Torino), D. Kocevski (NASA/MSFC), N. Omodei (Stanford Univ.), E. Bissaldi (Politecnico and INFN Bari), F. Longo (Univ. and INFN Trieste) and M. Arimoto (Kanazawa Univ.) report on behalf of the Fermi-LAT Collaboration:
We have searched data collected by the Fermi Large Area Telescope (LAT) on Sep 10, 2019, for possible high-energy (E > 100 MeV) gamma-ray emission in spatial/temporal coincidence with the LIGO/Virgo trigger S190910d (GCN 25695).
We define "instantaneous coverage" as the integral over the region of the LIGO probability map that is within the LAT field of view at a given time, and "cumulative coverage" as the integral of the instantaneous coverage over time. Fermi-LAT had instantaneous coverage of 50% of the LIGO probability region at the time of the trigger (T0 = 2019-09-10 01:26:19.243 UTC), and reached 100% cumulative coverage after ~9 ks.
We performed a search for a transient counterpart within the observed region of the 90% contour of the LIGO map in a fixed time window from T0 to T0 + 10 ks. One significant excess (with TS>25) was found at R.A., Dec. = 57.5, -27.7 (the 90% containment radius is 0.4 deg, statistical uncertainty only), but it is associated with the known and flaring source PKS 0346-27 (0.29 deg from the best-fit position).
We also performed a search which adapted the time interval of the analysis to the exposure of each region of the sky, and no additional excesses were found.
Energy flux upper bounds for the fixed time interval between 100 MeV and 1 GeV for this search vary between 1.9E-10 and 4.7E-09 [erg/cm^2/s].
The Fermi-LAT point of contact for this event is Makoto Arimoto (arimoto@se.kanazawa-u.ac.jp<mailto:arimoto@se.kanazawa-u.ac.jp>).
The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
GCN Circular 25706
Subject
LIGO/Virgo S190910d: Candidates from the Zwicky Transient Facility
Date
2019-09-10T09:16:46Z (6 years ago)
From
Igor Andreoni at Caltech <igor.andreoni@gmail.com>
Shreya Anand (Caltech), Igor Andreoni (Caltech), Maitreya Khandagale (IITB), Kunal Deshmukh (IITB), Varun Bhalerao (IITB), Pradip Gatkine (UMD), Viraj Karambelkar (Caltech), Yashvi Sharma (Caltech), Robert Stein (DESY), Mansi Kasliwal (Caltech), Tomas Ahumada (UMD), Michael Coughlin (Caltech), Jakob Nordin (HU Berlin), Leo P. Singer (NASA GSFC), Eric Bellm (UW)
On behalf of the Zwicky Transient Facility (ZTF) and Global Relay of Observatories Watching Transients Happen (GROWTH) collaborations
We observed the localization region of the gravitational wave trigger S190910d (LVC et al. GCN 25695) with the Palomar 48-inch telescope equipped with the 47 square degree ZTF camera (Bellm et al. 2019, Graham et al. 2019). The tiling was optimally determined and triggered using the GROWTH Target of Opportunity marshal (Coughlin et al. 2019a, Kasliwal et al. 2019b). We started obtaining target-of-opportunity observations in the g-band and r-band beginning at 2019-09-10 02:58:42.5 UT. We covered 34% of the enclosed probability based on the bayestar map in 2118 sq deg mapped over 90 minutes of observations. Each exposure was 30s with a typical depth of 20.8 mag.
The images were processed in real-time through the ZTF reduction and image subtraction pipelines at IPAC to search for potential counterparts (Masci et al. 2019). AMPEL (Nordin et al. 2019) and Kowalski (Duev et al. 2019) was used to search the alerts database for candidates. After rejecting stellar sources (Tachibana and Miller 2018) and moving objects and applying machine learning algorithms (Mahabal et al. 2019), and after removing candidates with history of variability prior to the merger time, the following high-significance transient candidates were identified by our pipeline in the 90% localization of the bayestar skymap (LVC et al. GCN 25695).
+--------------------------------------------------------------------------------+
| ZTF Name | IAU Name | RA (deg) | DEC (deg) | JD | Filter | Mag |
+--------------------------------------------------------------------------------+
| ZTF19abyfhov | AT2019pvu | 260.693429 | 11.424436 | 2458736.70 | r | 20.3 |
| ZTF19abyfhaq | AT2019pvv | 303.148593 | 49.392607 | 2458736.70 | r | 20.5 |
| ZTF19abyfbii | AT2019pvz | 255.441620 | 11.602254 | 2458736.70 | r | 20.2 |
| ZTF19abyfazm | AT2019pwa | 290.535876 | 48.069162 | 2458736.70 | r | 18.2 |
+--------------------------------------------------------------------------------+
Amongst our candidates, we note that ZTF19abyfazm is a blue transient (g-r~0.4) with the last non-detection one day before the merger. There is a faint object detected in Pan-STARRS images about 2.5 arcsec from the source.
Also ZTF19abyfbii is a candidate of interest because of its proximity to a galaxy with SDSS photometric redshift z=0.124, corresponding to a luminosity distance of about 580 Mpc.
ZTF and GROWTH are worldwide collaborations comprising Caltech, USA; IPAC, USA, WIS, Israel; OKC, Sweden; JSI/UMd, USA; U Washington, USA; DESY, Germany; MOST, Taiwan; UW Milwaukee, USA; LANL USA; Tokyo Tech, Japan; IITB, India; IIA, India; LJMU, UK; TTU, USA; SDSU, USA and USyd, Australia. ZTF acknowledges the generous support of the NSF under AST MSIP Grant No 1440341. GROWTH acknowledges generous support of the NSF under PIRE Grant No 1545949. Alert distribution service provided by DIRAC@UW (Patterson et al. 2019). Alert database searches are done by AMPEL (Nordin et al. 2019). Alert filtering and follow-up coordination is being undertaken by the GROWTH marshal system (Kasliwal et al. 2019).
GCN Circular 25705
Subject
LIGO/Virgo S190910d: no counterpart candidates in AGILE-GRID observations
Date
2019-09-10T08:23:57Z (6 years ago)
From
Giovanni Piano at INAF-IAPS <giovanni.piano@inaf.it>
G. Piano, C. Casentini (INAF/IAPS), M. Tavani (INAF/IAPS, and Univ. Roma
Tor Vergata), M. Cardillo, A. Ursi (INAF/IAPS), F. Lucarelli, C. Pittori,
F. Verrecchia (SSDC, and INAF/OAR), A. Bulgarelli, V. Fioretti, N.
Parmiggiani (INAF/OAS-Bologna), M. Pilia (INAF/OA-Cagliari), F. Longo
(Univ. Trieste, and INFN Trieste),
report on behalf of the AGILE Team:
In response to the LIGO-Virgo GW event S190910d at T0 = 2019-09-10
01:26:19.243 UTC a preliminary analysis of the AGILE exposure at T0 shows
that the Gamma-Ray Imaging Detector (GRID) exposure covered the 11% of the
90% c.l. localization region (LR) (19% of 90% c.l. localization region (LR)
is occulted by Earth).
We performed an analysis of the GRID data in the energy range 50 MeV - 10
GeV on T0.
No candidate gamma-ray transient was detected.
The following preliminary GRID values of 3-sigma upper limit (UL) are
obtained:
- from 7.5e-07 to 4.0e-06 erg cm^-2 s^-1, with exposure of about 11% of the
LR over the time interval (T0 - 2 s; T0 + 2 s);
- from 6.1e-07 to 3.2e-06 erg cm^-2 s^-1, with exposure of about 11% of the
LR over the time interval (T0; T0 + 5 s);
- from 3.1e-07 to 2.3e-06 erg cm^-2 s^-1, with exposure of about 11% of the
LR over the time interval (T0; T0 + 10 s);
- from 1.1e-07 to 1.6e-06 erg cm^-2 s^-1, with exposure of about 21% of the
LR over the time interval (T0; T0 + 100 s).
These measurements were obtained with AGILE observing a large portion of
the sky in spinning mode. Additional analysis of AGILE data is in progress.
GCN Circular 25704
Subject
LIGO/Virgo S190910d: no counterpart candidates in the Swift/BAT Observations
Date
2019-09-10T08:11:54Z (6 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
T. Sakamoto (AGU), S. D. Barthelmy (NASA/GSFC),
A. Y. Lien (GSFC/UMBC), D. M. Palmer (LANL)
A. P. Beardmore (U. Leicester), M. G. Bernardini (INAF-OAB),
A. A. Breeveld (MSSL-UCL), D. N. Burrows (PSU),
S. Campana (INAF-OAB), S. B. Cenko (NASA/GSFC),
G. Cusumano (INAF-IASF PA), A. D'Ai (INAF-IASFPA),
P. D'Avanzo (INAF-OAB), V. D'Elia (ASI-SSDC), S. Emery (UCL-MSSL),
P. A. Evans (U. Leicester), P. Giommi (ASI), C. Gronwall (PSU),
D. Hartmann (Clemson U.), J. A. Kennea (PSU), H. A. Krimm (NSF),
N. P. M. Kuin (UCL-MSSL), F. E. Marshall (NASA/GSFC),
A. Melandri (INAF-OAB), J. A. Nousek (PSU),
S. R. Oates (Uni. of Warwick), P. T. O'Brien (U. Leicester),
J. P. Osborne (U. Leicester), C. Pagani (U. Leicester),
K. L. Page (U.Leicester), M. J. Page (UCL-MSSL), M. Perri (ASDC),
J. L. Racusin (NASA/GSFC), B. Sbarufatti (INAF-OAB/PSU),
M. H. Siegel (PSU), G. Tagliaferri (INAF-OAB), A. Tohuvavohu (Toronto),
E. Troja (NASA/GSFC/UMCP) report on behalf of the Swift team:
We report the search results in the BAT data within T0 +/- 100 s of the
LVC event S190910d (LIGO/VIRGO Collaboration GCN Circ. 25695),
where T0 is the LVC trigger time (2019-09-10T01:26:19.242 UTC).
The center of the BAT field of view (FOV) at T0 is
RA = 7.546 deg,
DEC = -73.147 deg,
and the roll angle is 164.159 deg.
The BAT FOV (>10% partial coding) covers 44.85% of the integrated
LVC localization probability, and 45.56% of the galaxy convolved
probability (Evans et al. 2016). Note that the sensitivity in the BAT FOV
changes with the partial coding fraction. Please see the BAT FOV figure
in the summary page (link below) for the specific location of the LVC
region relative to the BAT FOV.
Within T0 +/- 100 s, no significant detections (signal-to-noise ratio
>~ 5 sigma) are found in the BAT raw light curves with time bins of 64 ms,
1 s, and 1.6 s. Assuming an on-axis (100% coded) short GRB with a typical
spectrum in the BAT energy range (i.e., a simple power-law model with a
power-law index of -1.32, Lien & Sakamoto et al. 2016), the 5-sigma upper
limit in the 1-s binned light curve corresponds to a flux upper
limit (15-350 keV) of ~ 8.39 x 10^-8 erg/s/cm^2.
Assuming a luminosity of ~ 2 x 10^47 erg/s (similar to GW170817)
and an average Epeak of ~ 400 keV for short GRBs (Bhat et al. 2016),
this flux upper limit corresponds to a distance of ~ 55.49 Mpc.
Event data is available from T0-21.827 to T0-18.767. No significant
detections are found in the 15-350 keV images created using this
event data interval.
BAT retains decreased, but significant, sensitivity to rate increases for
gamma-ray events outside of its FOV. About 21.26% of the integrated LVC
localization probability was outside of the BAT FOV but above the
Earth's limb from Swift's location, and the corresponding flux upper limits
for this region are within roughly an order of magnitude higher than those
within the FOV.
The results of the BAT analysis are available at
https://swift.gsfc.nasa.gov/results/BATbursts/team_web/S190910d/web/source_public.html
<https://swift.gsfc.nasa.gov/results/BATbursts/team_web/S190910d/web/source.html>
GCN Circular 25703
Subject
LIGO/Virgo S190910d: No counterpart candidates in AGILE-MCAL observations
Date
2019-09-10T08:01:53Z (6 years ago)
From
Claudio Casentini at INAF-IAPS <claudio.casentini@inaf.it>
C. Casentini, G. Piano, M. Tavani, M. Cardillo, A. Ursi (INAF/IAPS), F.
Lucarelli, C. Pittori, F. Verrecchia (SSDC, and INAF/OAR), A. Bulgarelli,
V. Fioretti, N. Parmiggiani (INAF/OAS-Bologna), M. Pilia
(INAF/OA-Cagliari), F. Longo (Univ. Trieste, and INFN Trieste), report on
behalf of the AGILE Team:
In response to the LIGO/Virgo GW event S190910d at T0 = 2019-09-10 01:26:19
(UT), a preliminary analysis of the AGILE minicalorimeter (MCAL) triggered
data found no event candidates within a time interval covering -/+ 15 sec
from the LIGO/Virgo T0.
At the T0, about 60% of the S190910d 90 c.l. localization region was
accessible to the AGILE MCAL. Three-sigma upper limits (ULs) are obtained
for a 1 s integration time at different celestial positions within the
accessible S190910d localization region, from a minimum of 1.18E-06 erg
cm^-2 to a maximum of 2.89E-06 erg cm^-2 (assuming as spectral model a
single power law with photon index 1.5).
The AGILE-MCAL detector is a CsI detector with a 4 pi FoV, sensitive in the
energy range 0.4-100 MeV. Additional analysis of AGILE data is in progress.
GCN Circular 25701
Subject
LIGO/Virgo S190910d: Coverage and upper limits from MAXI/GSC observations
Date
2019-09-10T07:03:55Z (6 years ago)
From
Motoko Serino at RIKEN/MAXI <motoko@crab.riken.jp>
N. Kawai, M. Sugizaki (Tokyo Tech), H. Negoro (Nihon U.),
S. Sugita, M. Serino (AGU),
M. Nakajima, W. Maruyama, M. Aoki, K. Kobayashi (Nihon U.),
T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN),
T. Sakamoto, H. Nishida, A. Yoshida (AGU),
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, T. Sato (Chuo U.),
M. Shidatsu (Ehime U.), M. Oeda, K. Shiraishi (Tokyo Tech),
S. Nakahira, Y. Sugawara, S. Ueno, H. Tomida, M. Ishikawa, N. Isobe, R. Shimomukai, M. Tominaga (JAXA),
Y. Ueda, A. Tanimoto, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake (Kyoto U.),
H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.),
M. Yamauchi, S. Iwahori, Y. Kurihara, K. Kurogi, K. Miike (Miyazaki U.),
T. Kawamuro (NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU)
report on behalf of the MAXI team:
We examined MAXI/GSC all-sky X-ray images (2-20 keV)
after the LVC trigger S190910d at 2019-09-10 01:26:19.242 UTC (GCN 25695).
At the trigger time of S190910d, the high-voltage of MAXI/GSC was on.
The instantaneous field of view of GSC at the GW trigger time covered 2% of the 90% credible region
of the bayestar sky map, in which we found no significant new X-ray source.
The first one-orbit (92 min) scan observation with GSC after the event covered 100%
of the 90% credible region of the bayestar skymap from 01:26:19 to 02:58:18 UTC (T0+0 to T0+5519 sec).
No significant new source was found in the region in the one-orbit scan observation.
A typical 1-sigma averaged upper limit obtained in one scan observation
is 20 mCrab at 2-20 keV.
If you require information about X-ray flux by MAXI/GSC at specific coordinates,
please contact the submitter of this circular by email.
GCN Circular 25700
Subject
LIGO/Virgo S190910d : no neutrino counterpart candidate in ANTARES search
Date
2019-09-10T06:25:25Z (6 years ago)
From
Damien Dornic at CPPM,France <dornic@cppm.in2p3.fr>
M. Ageron (CPPM/CNRS), B. Baret (APC/CNRS), A. Coleiro (APC/Universite de Paris), M. Colomer (APC/Universite de Paris), D. Dornic (CPPM/CNRS), A. Kouchner (APC/Universite de Paris), T. Pradier (IPHC/Universite de Strasbourg) report on behalf of the ANTARES Collaboration:
Using on-line data from the ANTARES detector, we have performed a follow-up analysis of the
recently reported LIGO/Virgo S190910d event using the 90% contour of the bayestar probability
map provided by the GW interferometers (GCN#25695 <https://gcn.gsfc.nasa.gov/gcn3/25695.gcn3>). The ANTARES visibility at the time of the
alert, together with the 50% and 90% contours of the probability map are shown at http://antares.in2p3.fr/GW/S190910d_Initial.png <http://antares.in2p3.fr/GW/S190910d_Initial.png>.
Considering the location probability provided by the LIGO/Virgo collaborations, there is a
50.9% chance that the GW emitter was in the ANTARES **upgoing** field of view at the time of
the alert.
No up-going muon neutrino candidate events were recorded in the ANTARES sky during a
+/-500s time-window centered on the time 2019-09-10 01:26:19 and in the 90% contour of the S190910d
event. The expected number of atmospheric background events in the region visible by ANTARES is
9.24e-04 in the +/- 500s time window. An extended search during +/- 1 hour gives no
up-going muon neutrino coincidence. The expected number of atmospheric background events in the
region visible by ANTARES is 6.65e-03 in this larger time window.
ANTARES is the largest undersea neutrino detector, installed in the Mediterranean Sea, and it is
primarily sensitive to neutrinos in the TeV-PeV energy range. At 10 TeV, the median angular
resolution for muon neutrinos is about 0.5 degrees. In the range 1-100 TeV ANTARES has a
competitive sensitivity to this position in the sky.
GCN Circular 25699
Subject
LIGO/Virgo S190910d: Upper limits from Fermi-GBM Observations
Date
2019-09-10T06:18:11Z (6 years ago)
From
Cori Fletcher at USRA <cfletcher@usra.edu>
C. Fletcher (USRA) reports on behalf of the Fermi-GBM Team and the GBM-LIGO/Virgo group
For S190910d and using the initial bayestar skymap, Fermi-GBM was observing 91.6% of the localization probability at event time.
There was no Fermi-GBM onboard trigger around the event time of the LIGO/Virgo detection of GW trigger S190910d (GCN 25695). An automated, blind search for short gamma-ray bursts below the onboard triggering threshold in Fermi-GBM also identified no counterpart candidates. The GBM targeted search, the most sensitive, coherent search for GRB-like signals, was run from +/-30 s around merger time, and also identified no counterpart candidates.
Part of the LVC localization region is behind the Earth for Fermi, located at RA=194.6, Dec=-9.9 with a radius of 67.2 degrees. We therefore set upper limits on impulsive gamma-ray emission for the LVC localization region visible to Fermi at merger time. Using the representative soft, normal, and hard GRB-like templates described in arXiv:1612.02395, we set the following 3 sigma flux upper limits over 10-1000 keV, weighted by GW localization probability (in units of 10^-7 erg/s/cm^2):
Timescale soft norm hard
--------------------------------------
0.128 s: 3.3 6.5 12
1.024 s: 1.0 1.8 4.6
8.192 s: 0.4 0.67 1.3
Assuming the median luminosity distance of 606 Mpc from the GW detection, we estimate the following intrinsic luminosity upper limits over the 1 keV-10 MeV energy range (in units of 10^48 erg/s):
Timescale Soft Normal Hard
------------------------------------
0.128 s: 22 40 122
1.024 s: 6.7 11 47
8.192 s: 2.7 4.1 13
GCN Circular 25698
Subject
LIGO/Virgo S190910d: No counterpart candidates in INTEGRAL SPI-ACS prompt observation
Date
2019-09-10T06:14:09Z (6 years ago)
From
Volodymyr Savchenko at ISDC,U of Geneve <savchenk@in2p3.fr>
A. Coleiro (APC, France), S. Schanne (CEA, France)
V. Savchenko, C. Ferrigno (ISDC/UniGE, Switzerland)
J. Rodi (IAPS-Roma, Italy)
S. Mereghetti (INAF IASF-Milano, Italy)
on behalf of the INTEGRAL multi-messenger collaboration:
https://www.astro.unige.ch/cdci/integral-multimessenger-collaboration
Using INTEGRAL/SPI-ACS realtime data (following [1]) we have performed
a search for a prompt gamma-ray counterpart of S190910d (GCN 25695).
At the time of the event (2019-09-10 01:26:19 UTC, hereafter T0),
INTEGRAL was operating in nominal mode. The peak of the event
localization probability was at an angle of 66 deg with respect to the
spacecraft pointing axis. This orientation implies strongly suppressed
(18% of optimal) response of ISGRI, somewhat suppressed (42% of
optimal) response of IBIS/Veto, and near-optimal (91% of optimal)
response of SPI-ACS.
The background within ��300 seconds around the event was very stable
(excess variance 1.2).
We have performed a search for any impulsive events in INTEGRAL SPI-
ACS (as described in [2]) data.
We do not detect any significant counterparts and estimate a 3-sigma
upper limit on the 75-2000 keV fluence of 2.2e-07 erg/cm^2 (within the
50% probability containment region of the source localization) for a
burst lasting less than 1 s with a characteristic short GRB spectrum
(an exponentially cut off power law with alpha=-0.5 and Ep=600 keV)
occurring at any time in the interval within 300 s around T0. For a
typical long GRB spectrum (Band function with alpha=-1, beta=-2.5, and
Ep=300 keV), the derived peak flux upper limit is ~1.8e-07 (5.4e-08)
erg/cm^2/s at 1 s (8 s) time scale in 75-2000 keV energy range.
For the mean reported distance 606.0 Mpc this corresponds to the limit
on the total isotropic equivalent energy in 1 s of 9.5e+48 erg for
the short GRB spectrum and for a long GRB spectrum isotropic
equivalent luminosity in 1 s (8 s) of 7.1e+48 erg/s (2.4e+48 erg/s)
We report for completeness and in order of FAP, all excesses
identified in the search region. We find: 5 likely background
excesses:
scale | T | S/N | luminosity ( x 1e+49 erg/s) | FAP
0.05 | 270 | 12 | 30.7 +/- 3.24 +/- 23.6 | 0.355
0.35 | -30.3 | 3.4 | 2.96 +/- 1.14 +/- 2.28 | 0.72
0.6 | 136 | 3.9 | 25.7 +/- 8.66 +/- 19.8 | 0.819
1.7 | 234 | 3.6 | 13.6 +/- 5.13 +/- 10.5 | 0.87
1.25 | -269 | 3.8 | 17.7 +/- 5.99 +/- 13.6 | 0.934
Note that FAP estimates (especially at timescales above 2s) may be
possibly further affected by enhanced non-stationary local background
noise. This list excludes any excesses for which FAP is close to
unity.
We additionally note that the excess at T0+270s despite high S/N of 12
has FAP of only 0.355, due to the large offset from T0 and high rate
of excesses at this timescale.
All results quoted are preliminary.
This circular is an official product of the INTEGRAL Multi-Messenger
team.
[1] Savchenko et al. 2017, A&A 603, A46
[2] Savchenko et al. 2012, A&A 541A, 122S
GCN Circular 25696
Subject
LIGO/Virgo S190910d: No counterpart candidates in HAWC observations
Date
2019-09-10T02:30:24Z (6 years ago)
From
Antonio Galvan at Inst.de Astronomia,UNAM <agalvan@astro.unam.mx>
The HAWC Collaboration (https://www.hawc-observatory.org) reports:
The HAWC Collaboration performed a follow-up of the gravitational wave
trigger S190910d. At the time of the trigger the HAWC
local zenith was oriented towards (RA, Dec) = (272.9deg, 19.0deg).
32% of the GW candidate sky location probability fell within our
observable field of view (0-45 deg zenith angle).
We performed a search for a short timescale emission using 6 sliding
time windows (dt = 0.3s, 1s, 3s, 10s, 30s and 100s), shifted forward
in time by 20% of their width. We searched the 95% probability
containment area in a timescale-dependent time period, from t0-5dt to
t0+10dt, where t0 is the time of the GW trigger.
No significant gamma-ray detection above the background was observed.
The sensitivity of this analysis is greatly dependent on zenith angle,
ranging from 0.0deg to 45.0deg for the area searched in this
analysis. The 5sigma detection sensitivity to a 1s (100s) burst in the
80-800GeV energy range goes from 1.2e-06 erg/cm^2 to 1.1e-04 erg/cm^2
(6.4e-06 erg/cm^2 to 5.0e-04 erg/cm^2), depending on the zenith
angle.
HAWC is a TeV gamma ray water Cherenkov array located in the state of
Puebla, Mexico. It is sensitive to the energy range ~0.1-100TeV, and
monitors 2/3 of the sky every day with an instantaneous field-of-view
of ~2 sr.
GCN Circular 25695
Subject
LIGO/Virgo S190910d: Identification of a GW compact binary merger candidate
Date
2019-09-10T02:29:05Z (6 years ago)
From
Francesca Badaracco at GSSI, Ligo/VIRGO <francesca.badaracco@gssi.it>
The LIGO Scientific Collaboration and the Virgo Collaboration report:
We identified the compact binary merger candidate S190910d during
real-time processing of data from LIGO Hanford Observatory (H1) and
LIGO Livingston Observatory (L1) at 2019-09-10 01:26:19.243 UTC (GPS
time: 1252113997.243). The candidate was found by the SPIIR [1] and
MBTAOnline [2] analysis pipelines.
S190910d is an event of interest because its false alarm rate, as
estimated by the online analysis, is 3.7e-09 Hz, or about one in 8
years. The event's properties can be found at this URL:
https://gracedb.ligo.org/superevents/S190910d
The classification of the GW signal, in order of descending
probability, is NSBH (98%), Terrestrial (2%), BNS (<1%), BBH (<1%), or
MassGap (<1%).
Assuming the candidate is astrophysical in origin, there is strong
evidence for the lighter compact object having a mass < 3 solar masses
(HasNS: >99%). Using the masses and spins inferred from the signal,
there is strong evidence against matter outside the final compact
object (HasRemnant: <1%).
One sky map is available at this time and can be retrieved from the
GraceDB event page:
* bayestar.fits.gz, an updated localization generated by BAYESTAR
[3], distributed via GCN notice about 6 minutes after the candidate
For the bayestar.fits.gz sky map, the 90% credible region is 3829
deg2. Marginalized over the whole sky, the a posteriori luminosity
distance estimate is 606 +/- 197 Mpc (a posteriori mean +/- standard
deviation).
For further information about analysis methodology and the contents of
this alert, refer to the LIGO/Virgo Public Alerts User Guide
<https://emfollow.docs.ligo.org/userguide/>.
[1] Qi Chu, PhD Thesis, The University of Western Australia (2017)
[2] Adams et al. CQG 33, 175012 (2016)
[3] Singer & Price PRD 93, 024013 (2016)
GCN Circular 25694
Subject
LIGO/Virgo S190910d Global MASTER-Net observations report
Date
2019-09-10T01:57:31Z (6 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin,
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva, D.Kuvshinov
(Lomonosov Moscow State University, SAI, Physics Department),
R. Podesta, C.Lopez, F. Podesta, C.Francile
(Observatorio Astronomico Felix Aguilar OAFA),
H.Levato
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),
R. Rebolo, M. Serra
(The Instituto de Astrofisica de Canarias),
D. Buckley
(South African Astronomical Observatory),
O.A. Gres, N.M. Budnev, O.Ershova
(Irkutsk State University, API),
A. Tlatov, D. Dormidontov
(Kislovodsk Solar Station of the Pulkovo Observatory),
V. Yurkov, A. Gabovich, Yu. Sergienko
(Blagoveschensk Educational State University)
MASTER-SAAO robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South Africa (South African Astronomical Observatory) started inspect of the LIGO/Virgo S190910d errorbox 157 sec after trigger time at 2019-09-10 01:28:56 UT, with upper limit up to 19.0 mag. The observations began at zenit distance = 43 deg. The sun altitude is -41.6 deg.
The galactic latitude b = -60 deg., longitude l = 98 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/ligo_1.php?id=10782
We obtain a following upper limits.
Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________
248 | 2019-09-10 01:28:56 | MASTER-SAAO | (04h 49m 50.020s , -67d 59m 39.61s) | C | 180 | 17.8 |
482 | 2019-09-10 01:32:50 | MASTER-SAAO | (02h 57m 56.175s , -08d 53m 48.13s) | C | 180 | 18.0 |
512 | 2019-09-10 01:34:05 | MASTER-SAAO | (04h 59m 49.012s , -45d 34m 00.88s) | C | 90 | 19.0 |
668 | 2019-09-10 01:36:27 | MASTER-SAAO | (04h 48m 33.843s , -45d 27m 12.28s) | C | 120 | 18.1 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
GCN Circular 25693
Subject
LIGO/Virgo S190910d: Upper limits from IceCube neutrino searches
Date
2019-09-10T01:52:35Z (6 years ago)
From
Raamis Hussain at IceCube <raamis.hussain@icecube.wisc.edu>
IceCube Collaboration (http://icecube.wisc.edu/) reports:
Searches [1,2] for track-like muon neutrino events detected by IceCube
consistent with the sky localization of gravitational-wave candidate
S190910d
in a time range of 1000 seconds [3] centered on the alert event time
(2019-09-10 01:17:59.243 UTC to 2019-09-10 01:34:39.243 UTC) have been
performed. During this time
period IceCube was collecting good quality data. No significant track-like
events are found in spatial coincidence of S190910d calculated from the map
circulated in the 1-Preliminary notice.
IceCube's sensitivity assuming an E^-2 spectrum (E^2 dN/dE) to neutrino
point sources within the locations spanned by the 90% spatial containment
of S190910d ranges from 0.029 to 1.107 GeV cm^-2 in a 1000 second
time window.
The IceCube Neutrino Observatory is a cubic-kilometer neutrino detector
operating at the geographic South Pole, Antarctica. The IceCube realtime
alert point of contact can be reached at roc@icecube.wisc.edu