LIGO/Virgo S190513bm
GCN Circular 24522
Subject
LIGO/Virgo S190513bm: Identification of a GW compact binary merger candidate
Date
2019-05-13T21:37:24Z (6 years ago)
From
Marco Drago at GSSI <marco.drago@gssi.it>
The LIGO Scientific Collaboration and the Virgo Collaboration report:
We identified the compact binary merger candidate S190513bm during
real-time processing of data from LIGO Hanford Observatory (H1), LIGO
Livingston Observatory (L1), and Virgo Observatory (V1) at 2019-05-13
20:54:28.747 UTC (GPS time: 1241816086.747). The candidate was found
by the GstLAL [1], CWB [2], MBTAOnline [3], and spiir [4] analysis
pipelines.
S190513bm is an event of interest because its false alarm rate, as
estimated by the online analysis, is 3.7e-13 Hz, or about one in 1e5
years. The event's properties can be found at this URL:
https://gracedb.ligo.org/superevents/S190513bm
The classification of the GW signal, in order of descending
probability, is BBH (94%), MassGap (5%), NSBH (<1%), Terrestrial
(<1%), or BNS (<1%).
Assuming the candidate is astrophysical in origin, there is strong
evidence against the lighter compact object having a mass < 3 solar
masses (HasNS: <1%). Using the masses and spins inferred from the
signal, there is strong evidence against matter outside the final
compact object (HasRemnant: <1%).
One skymap is available at this time and can be retrieved from the
GraceDB event page:
* bayestar.fits.gz, an updated localization generated by BAYESTAR
[5], distributed via GCN notice about 27 minutes after the candidate
For the bayestar.fits.gz skymap, the 90% credible region is 691 deg2.
Marginalized over the whole sky, the a posteriori luminosity distance
estimate is 1987 +/- 501 Mpc (a posteriori mean +/- standard
deviation).
For further information about analysis methodology and the contents of
this alert, refer to the LIGO/Virgo Public Alerts User Guide
<https://emfollow.docs.ligo.org/userguide/>.
[1] Messick et al. PRD 95, 042001 (2017)
[2] Klimenko et al. PRD 93, 042004 (2016)
[3] Adams et al. CQG 33, 175012 (2016)
[4] Qi Chu, PhD Thesis, The University of Western Australia (2017)
[5] Singer & Price PRD 93, 024013 (2016)
GCN Circular 24523
Subject
LIGO/Virgo S190513bm: HAWC follow-up
Date
2019-05-13T21:48:56Z (6 years ago)
From
Hugo Ayala at Pennsylvania State University <hgayala@psu.edu>
The HAWC Collaboration (https://www.hawc-observatory.org) reports:The
HAWC Collaboration performed a follow-up of the gravitational
wavetrigger S190513bm. At the time of the trigger the HAWClocal zenith
was oriented towards (RA, Dec) = (87.4deg, 19.0deg).46% of the GW
candidate sky location probability fell within ourobservable field of
view (0-45 deg zenith angle).We performed a search for a short
timescale emission using 6 slidingtime windows (dt = 0.3s, 1s, 3s,
10s, 30s and 100s), shifted forwardin time by 20% of their width. We
searched the 95% probabilitycontainment area in a timescale-dependent
time period, from t0-5dt tot0+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 33.3deg to 45.0deg for the area searched in
thisanalysis. The 5sigma detection sensitivity to a 1s (100s) burst in
the80-800GeV energy range goes from 1.1e-05 erg/cm^2 to 1.1e-04
erg/cm^2(5.4e-05 erg/cm^2 to 5.0e-04 erg/cm^2), depending on the
zenithangle.HAWC is a TeV gamma ray water Cherenkov array located in
the state ofPuebla, Mexico. It is sensitive to the energy range
~0.1-100TeV, andmonitors 2/3 of the sky every day with an
instantaneous field-of-viewof ~2 sr.
GCN Circular 24524
Subject
LIGO/Virgo S190513bm: IceCube Neutrino Search
Date
2019-05-13T22:18:49Z (6 years ago)
From
Raamis Hussain at IceCube <raamis.hussain@icecube.wisc.edu>
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 S190513bm-2-Initial in a time range
of 1000
seconds centered on the alert event time (2019-05-13 20:46:08.747 UTC to
2019-05-13 21:02:48.747 UTC)
during which IceCube was collecting good quality data.
No track-like events are found in spatial coincidence with the 90% spatial
containment of S190513bm 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 S190513bm ranges from
0.029 to 0.506 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
GCN Circular 24525
Subject
LIGO/Virgo S190513bm Global MASTER-Net observations report
Date
2019-05-13T22:48:29Z (6 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
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-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 S190513bm errorbox 1803 sec after trigger time at 2019-05-13 21:24:31 UT, with upper limit up to 19.2 mag. The observations began at zenit distance = 136 deg. The sun altitude is -69.1 deg.
MASTER-IAC robotic telescope located in Spain (IAC Teide Observatory) started inspect of the LIGO/Virgo S190513bm errorbox 2233 sec after trigger time at 2019-05-13 21:31:41 UT, with upper limit up to 19.2 mag. The observations began at zenit distance = 152 deg. The sun altitude is -21.6 deg.
MASTER-Kislovodsk robotic telescope located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the LIGO/Virgo S190513bm errorbox 2620 sec after trigger time at 2019-05-13 21:38:08 UT, with upper limit up to 17.7 mag. The observations began at zenit distance = 113 deg. The sun altitude is -28.2 deg.
MASTER-Tavrida robotic telescope located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the LIGO/Virgo S190513bm errorbox 2699 sec after trigger time at 2019-05-13 21:39:27 UT, with upper limit up to 17.9 mag. The observations began at zenit distance = 117 deg. The sun altitude is -27.6 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=10365
We obtain a following upper limits.
Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________
1893 | 2019-05-13 21:24:31 | MASTER-SAAO | ( 19h 10m 55.36s , -29d 49m 09.78s) | C | 180 | 18.7 |
2073 | 2019-05-13 21:24:31 | MASTER-SAAO | ( 19h 10m 55.36s , -29d 49m 09.78s) | C | 540 | 19.2 | Coadd
2103 | 2019-05-13 21:28:01 | MASTER-SAAO | ( 19h 11m 02.82s , -29d 49m 02.77s) | C | 180 | 18.6 |
2313 | 2019-05-13 21:31:30 | MASTER-SAAO | ( 19h 11m 02.98s , -29d 49m 01.27s) | C | 180 | 18.5 |
2323 | 2019-05-13 21:31:41 | MASTER-IAC | ( 3h 49m 51.07s , +59d 49m 36.05s) | C | 180 | 17.2 |
2324 | 2019-05-13 21:31:42 | MASTER-IAC | ( 3h 33m 28.49s , +59d 52m 09.70s) | C | 180 | 16.9 |
2522 | 2019-05-13 21:35:00 | MASTER-SAAO | ( 19h 11m 03.19s , -29d 48m 59.91s) | C | 180 | 18.5 |
2570 | 2019-05-13 21:35:48 | MASTER-IAC | ( 3h 33m 54.78s , +59d 56m 27.96s) | C | 180 | 16.8 |
2571 | 2019-05-13 21:35:48 | MASTER-IAC | ( 3h 50m 22.01s , +59d 53m 47.58s) | C | 180 | 17.7 |
2710 | 2019-05-13 21:38:08 | MASTER-Kislovodsk | ( 3h 23m 05.55s , +57d 56m 50.54s) | C | 180 | 17.5 |
2710 | 2019-05-13 21:38:08 | MASTER-Kislovodsk | ( 3h 38m 05.13s , +57d 29m 30.15s) | C | 180 | 17.7 |
2790 | 2019-05-13 21:39:27 | MASTER-Tavrida | ( 3h 53m 37.36s , +55d 40m 46.76s) | C | 180 | 16.1 |
2917 | 2019-05-13 21:41:34 | MASTER-Kislovodsk | ( 3h 23m 05.08s , +57d 56m 47.73s) | C | 180 | 15.8 |
2917 | 2019-05-13 21:41:35 | MASTER-Kislovodsk | ( 3h 38m 04.38s , +57d 29m 25.31s) | C | 180 | 15.8 |
2961 | 2019-05-13 21:42:18 | MASTER-SAAO | ( 19h 24m 44.34s , -31d 59m 41.26s) | C | 180 | 18.6 |
3026 | 2019-05-13 21:43:24 | MASTER-Tavrida | ( 4h 8m 10.44s , +59d 59m 42.95s) | C | 180 | 14.4 |
3026 | 2019-05-13 21:43:24 | MASTER-Tavrida | ( 4h 20m 50.42s , +59d 57m 10.66s) | C | 180 | 17.7 |
3049 | 2019-05-13 21:43:47 | MASTER-IAC | ( 3h 49m 52.42s , +59d 49m 12.05s) | C | 180 | 17.1 |
3049 | 2019-05-13 21:43:47 | MASTER-IAC | ( 3h 33m 29.32s , +59d 51m 40.38s) | C | 180 | 16.4 |
3132 | 2019-05-13 21:45:10 | MASTER-Kislovodsk | ( 3h 54m 17.16s , +58d 14m 20.21s) | C | 180 | 13.2 |
3178 | 2019-05-13 21:45:56 | MASTER-SAAO | ( 18h 47m 01.14s , -31d 58m 43.48s) | C | 180 | 18.1 |
3290 | 2019-05-13 21:47:47 | MASTER-IAC | ( 3h 33m 56.08s , +59d 56m 25.74s) | C | 180 | 15.9 |
3290 | 2019-05-13 21:47:47 | MASTER-IAC | ( 3h 50m 23.71s , +59d 53m 50.71s) | C | 180 | 17.4 |
3395 | 2019-05-13 21:49:32 | MASTER-SAAO | ( 19h 43m 35.98s , -32d 0m 16.46s) | C | 180 | 18.1 |
3529 | 2019-05-13 21:51:47 | MASTER-IAC | ( 16h 56m 10.01s , + 5d 59m 00.35s) | C | 180 | 16.0 |
3530 | 2019-05-13 21:51:48 | MASTER-IAC | ( 16h 47m 51.76s , + 6d 2m 23.47s) | C | 180 | 18.3 |
3609 | 2019-05-13 21:53:07 | MASTER-SAAO | ( 19h 24m 43.72s , -31d 59m 34.72s) | C | 180 | 18.1 |
3735 | 2019-05-13 21:55:12 | MASTER-Tavrida | ( 3h 53m 31.81s , +55d 40m 14.64s) | C | 180 | 14.4 |
3755 | 2019-05-13 21:55:32 | MASTER-IAC | ( 17h 3m 57.68s , + 6d 1m 28.60s) | C | 180 | 18.3 |
3823 | 2019-05-13 21:56:40 | MASTER-SAAO | ( 19h 34m 09.51s , -32d 0m 12.55s) | C | 180 | 18.2 |
3971 | 2019-05-13 21:59:09 | MASTER-Tavrida | ( 4h 8m 11.76s , +59d 59m 34.87s) | C | 180 | 14.8 |
3971 | 2019-05-13 21:59:09 | MASTER-Tavrida | ( 4h 20m 50.88s , +59d 57m 01.62s) | C | 180 | 17.9 |
3976 | 2019-05-13 21:59:14 | MASTER-IAC | ( 17h 8m 24.41s , + 8d 1m 15.82s) | C | 180 | 18.5 |
4039 | 2019-05-13 22:00:16 | MASTER-SAAO | ( 18h 47m 03.44s , -31d 58m 38.95s) | C | 180 | 18.3 |
4207 | 2019-05-13 22:03:04 | MASTER-Tavrida | ( 4h 21m 13.77s , +59d 40m 53.44s) | C | 180 | 17.7 |
4207 | 2019-05-13 22:03:04 | MASTER-Tavrida | ( 4h 8m 34.55s , +59d 46m 36.53s) | C | 180 | 14.8 |
4224 | 2019-05-13 22:03:22 | MASTER-IAC | ( 16h 48m 07.95s , + 6d 6m 39.52s) | C | 180 | 18.0 |
4224 | 2019-05-13 22:03:22 | MASTER-IAC | ( 16h 56m 24.49s , + 6d 3m 18.60s) | C | 180 | 17.1 |
4254 | 2019-05-13 22:03:51 | MASTER-SAAO | ( 18h 56m 29.05s , -31d 58m 37.53s) | C | 180 | 18.7 |
4442 | 2019-05-13 22:06:59 | MASTER-Tavrida | ( 3h 13m 08.91s , +56d 2m 53.04s) | C | 180 | 14.5 |
4442 | 2019-05-13 22:06:59 | MASTER-Tavrida | ( 3h 24m 27.42s , +56d 0m 12.60s) | C | 180 | 14.3 |
4446 | 2019-05-13 22:07:03 | MASTER-IAC | ( 16h 48m 06.87s , + 6d 6m 28.56s) | C | 180 | 18.7 |
4446 | 2019-05-13 22:07:03 | MASTER-IAC | ( 16h 56m 23.45s , + 6d 3m 08.76s) | C | 180 | 17.8 |
4470 | 2019-05-13 22:07:28 | MASTER-SAAO | ( 19h 43m 35.85s , -32d 0m 08.06s) | C | 180 | 19.1 |
4666 | 2019-05-13 22:10:44 | MASTER-IAC | ( 17h 4m 12.93s , + 6d 5m 37.49s) | C | 180 | 18.4 |
4667 | 2019-05-13 22:10:44 | MASTER-IAC | ( 17h 12m 29.50s , + 6d 2m 16.30s) | C | 180 | 16.8 |
4676 | 2019-05-13 22:10:53 | MASTER-Tavrida | ( 4h 22m 05.81s , +55d 40m 58.01s) | C | 180 | 15.9 |
4685 | 2019-05-13 22:11:03 | MASTER-SAAO | ( 19h 53m 01.69s , -32d 0m 44.82s) | C | 180 | 18.9 |
4899 | 2019-05-13 22:14:37 | MASTER-SAAO | ( 19h 34m 12.34s , -32d 0m 05.95s) | C | 180 | 18.3 |
4906 | 2019-05-13 22:14:44 | MASTER-IAC | ( 17h 16m 44.15s , + 7d 58m 04.13s) | C | 180 | 16.7 |
4907 | 2019-05-13 22:14:44 | MASTER-IAC | ( 17h 8m 23.61s , + 8d 1m 29.87s) | C | 180 | 18.1 |
5115 | 2019-05-13 22:18:13 | MASTER-SAAO | ( 18h 56m 30.33s , -31d 58m 33.69s) | C | 180 | 18.5 |
5148 | 2019-05-13 22:18:45 | MASTER-IAC | ( 17h 8m 39.19s , + 8d 6m 00.52s) | C | 180 | 18.2 |
5148 | 2019-05-13 22:18:45 | MASTER-IAC | ( 17h 16m 57.85s , + 8d 2m 39.87s) | C | 180 | 17.4 |
5332 | 2019-05-13 22:21:49 | MASTER-SAAO | ( 19h 53m 02.59s , -32d 0m 20.78s) | C | 180 | 19.0 |
5355 | 2019-05-13 22:22:13 | MASTER-Tavrida | ( 4h 21m 32.61s , +56d 2m 13.57s) | C | 180 | 16.1 |
5372 | 2019-05-13 22:22:29 | MASTER-IAC | ( 16h 52m 28.10s , + 8d 6m 20.04s) | C | 180 | 18.6 |
5372 | 2019-05-13 22:22:30 | MASTER-IAC | ( 17h 0m 46.89s , + 8d 3m 00.48s) | C | 180 | 18.5 |
5547 | 2019-05-13 22:25:25 | MASTER-SAAO | ( 19h 32m 10.82s , -34d 0m 00.10s) | C | 180 | 19.0 |
5719 | 2019-05-13 22:28:16 | MASTER-IAC | ( 9h 28m 52.82s , +84d 3m 07.47s) | C | 180 | 18.8 |
5719 | 2019-05-13 22:28:16 | MASTER-IAC | ( 10h 48m 36.03s , +83d 59m 52.83s) | C | 180 | 18.8 |
5764 | 2019-05-13 22:29:02 | MASTER-SAAO | ( 19h 12m 53.05s , -33d 59m 03.54s) | C | 180 | 18.8 |
5937 | 2019-05-13 22:31:54 | MASTER-IAC | ( 9h 28m 51.57s , +84d 3m 12.89s) | C | 180 | 19.0 |
5937 | 2019-05-13 22:31:54 | MASTER-IAC | ( 10h 48m 35.30s , +84d 0m 00.56s) | C | 180 | 19.2 |
5980 | 2019-05-13 22:32:38 | MASTER-SAAO | ( 19h 19m 07.04s , -29d 59m 34.24s) | C | 180 | 18.7 |
6195 | 2019-05-13 22:36:12 | MASTER-SAAO | ( 19h 32m 11.84s , -33d 59m 38.71s) | C | 180 | 18.7 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
GCN Circular 24526
Subject
LIGO/Virgo S190513bm: AGILE MCAL observation
Date
2019-05-13T22:49:51Z (6 years ago)
From
Claudio Casentini at INAF-IAPS <claudio.casentini@inaf.it>
C.Casentini (INAF/IAPS), F.Lucarelli (SSDC, and INAF/OAR), M. Tavani
(INAF/IAPS, and Univ. Roma Tor Vergata), M.Cardillo, G.Piano, A.Ursi
(INAF/IAPS), C. Pittori, F. Verrecchia (SSDC, and INAF/OAR), A. Bulgarelli,
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 S190513bm at T0 = 2019-05-13
20:54:28 (UT), a preliminary analysis of the AGILE minicalorimeter (MCAL)
triggered data found no event candidates within a time interval covering
+/- 100 sec from the LIGO-Virgo T0.
Three-sigma upper limits (ULs) are obtained for a 1 s integration time at
different celestial positions within the accessible S190513bm 90% c.l.
localization region (almost 80% of the given GW contour), from a minimum of
8.54E-07 erg cm^-2 to a maximum of 1.73E-06 erg cm^-2 (assuming as
spectral model a single power law with photon index 1.5). The average
off-axis angle is almost 90 degrees.
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 24527
Subject
LIGO/Virgo S190513bm: INTEGRAL prompt observation
Date
2019-05-13T23:32:01Z (6 years ago)
From
Carlo Ferrigno at IAAT/ISDC <carlo.Ferrigno@unige.ch>
James Rodi, Bozzo Enrico
V. Savchenko, C. Ferrigno (ISDC/UniGE, Switzerland)
J. Rodi (IAPS-Roma, Italy)
A. Coleiro (APC, France)
S. Mereghetti (INAF IASF-Milano, Italy)
on behalf of the INTEGRAL multi-messenger collaboration:
https://www.astro.unige.ch/cdci/integral-multimessenger-collaboration
Using combination of INTEGRAL all-sky detectors (following Savchenko
et al. 2017, A&A 603, A46): SPI/ACS, IBIS/Veto, and IBIS we have
performed a search for a prompt gamma-ray counterpart of S190513bm
(GCN 24522).
At the time of the event (2019-05-13 20:54:28 UTC, hereafter T0),
INTEGRAL was operating in nominal mode. The peak of the event
localization probability was at an angle of 39 deg with respect to the
spacecraft pointing axis. This orientation implies strongly suppressed
(16% of optimal) response of ISGRI, strongly suppressed (25% of
optimal) response of IBIS/Veto, and somewhat suppressed (62% 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 Savchenko et al. 2012, A&A 541A, 122S), IBIS, and
IBIS/Veto data.
We do not detect any significant counterparts and estimate a 3-sigma
upper limit on the 75-2000 keV fluence of 2.6e-07 erg/cm^2 for a burst
lasting less than 1 s with a characteristic short GRB spectrum (an
exponentially cut off power law with alpha=-0.5 and Ep=600 keV)
occurring at any time in the interval within 300 s around T0. For a
typical long GRB spectrum (Band function with alpha=-1, beta=-2.5, and
Ep=300 keV), the derived peak flux upper limit is ~2.3e-07 (8.2e-08)
erg/cm^2/s at 1 s (8 s) time scale in 75-2000 keV energy range.
GCN Circular 24528
Subject
LIGO/Virgo S190513bm: AGILE GRID observations
Date
2019-05-14T00:13:57Z (6 years ago)
From
Fabrizio Lucarelli at SSDC/INAF-OAR <fabrizio.lucarelli@ssdc.asi.it>
F. Lucarelli (SSDC, and INAF-OAR), C. Casentini (INAF/IAPS), M. Tavani (INAF/IAPS,
and Univ. Roma Tor Vergata), C. Pittori, F. Verrecchia (SSDC, and INAF-OAR),
M. Cardillo, G. Piano, A. Ursi (INAF/IAPS), A. Bulgarelli, 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 S190513bm at T0 = 2019-05-13 20:54:28 (UT)
(GCN #24522), we performed an analysis of the AGILE Gamma-Ray Imaging Detector
(GRID) data.
An analysis of the data in the energy range 50 MeV - 10 GeV was performed over
the time interval (T0 - 100s; T0), where an exposure of about 40% of the S190513bm
90% c.l. localization region was available.
The following preliminary GRID values of 3-sigma upper limits (UL) are obtained:
from 5.0e-08 to 5.0e-07 erg cm^-2 s^-1.
These measurements were obtained with AGILE observing a large portion of the sky
in spinning mode. Additional AGILE GRID data analysis is in progress.
GCN Circular 24530
Subject
LIGO/Virgo S190513bm: MAXI/GSC Observations
Date
2019-05-14T03:04:41Z (6 years ago)
From
Motoko Serino at RIKEN/MAXI <motoko@crab.riken.jp>
M. Serino, S. Sugita (AGU), H. Negoro (Nihon U.), M. Sugizaki, N. Kawai (Tokyo Tech),
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.),
Y. Tachibana, K. Morita, 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, T. Morita, S. Yamada, S. Ogawa (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 the MAXI/GSC all-sky X-ray images (2-20 keV) obtained
in the orbit after the LVC trigger
S190513bm at 2019-05-13 20:54:28.747 UTC (GCN 24522).
At the trigger time of S190513bm, the high-voltage of MAXI/GSC was on,
and it was turned off at T0+864 sec (+14.4 min).
The instantaneous field of view of GSC at the GW trigger time covered 4% of the 90% credible region
of the bayestar sky map, in which we found no significant new X-ray source.
The one-orbit (92 min) scan of GSC covered 87% of the 90% credible region
of the bayestar skymap.
The scan was mainly performed by the degraded GSC_3 camera.
No significant new source was found in the error region with the one-orbit scan.
The 1-sigma averaged upper limit obtained
from the scan was 50 mCrab at 2-10 keV.
If you require information of X-ray flux by MAXI/GSC at specific coordinates,
please contact the submitter of this circular by email.
GCN Circular 24532
Subject
LIGO/Virgo S190513bm: Fermi-LAT search for a high-energy gamma-ray counterpart
Date
2019-05-14T06:52:45Z (6 years ago)
From
Magnus Axelsson at Stockholm U. <magaxe@kth.se>
M. Axelsson (KTH and Stockholm Univ.), D. Kocevski (NASA/MSFC), M. Arimoto (Kanazawa Univ.) and N. Omodei (Stanford Univ.) report on behalf of the Fermi-LAT Collaboration:
We have searched data collected by the Fermi Large Area Telescope (LAT) on May 13, 2019, for possible high-energy (E > 100 MeV) gamma-ray emission in spatial/temporal coincidence with the LIGO/Virgo trigger S190513bm (GCN 24522).
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. Fermi-LAT had instantaneous coverage of ~65% of the LIGO probability at the time of the trigger (T0 = 2019-05-13 20:54:28.747 UTC), and reached 100% cumulative coverage after ~4 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. = 278.3, -21.2, but it is associated with the known and currently flaring source PKS 1830-211.
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 2.6e-10 and 8.8e-9 [erg/cm^2/s].
The Fermi-LAT point of contact for this event is Magnus Axelsson (magaxe@kth.se<mailto:magaxe@kth.se>).
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 24537
Subject
LIGO/Virgo S190513bm: Fermi GBM Observations
Date
2019-05-14T12:36:11Z (6 years ago)
From
Suraj Poolakkil at UAH <sp0076@uah.edu>
S. Poolakkil (UAH) and A. Goldstein (USRA) report on behalf of the
Fermi-GBM Team and the GBM-LIGO/Virgo group:
For S190513bm, and using the updated BAYESTAR skymap, Fermi-GBM was
observing 61.6% 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 S190513bm (GCN 24522). 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 = 280.7 and Dec = -12.3 with a radius of 67.4 degrees.
We therefore set upper limits on impulsive gamma-ray emission. Using the
representative soft, normal, and hard GRB-like spectral templates described
in arXiv:1612.02395, we set the following 3 sigma flux upper limits over
10-1000 keV, weighted by the remaining visible GW localization probability
(in units of erg/s/cm^2):
Timescale soft norm hard
--------------------------------------
0.128 s: 3.5e-07 5.5e-07 1.0e-06
1.024 s: 1.2e-07 2.0e-07 3.5e-07
8.192 s: 3.5e-08 5.9e-08 1.2e-07
Assuming the median luminosity distance of ~1987 Mpc from the GW detection,
we estimate intrinsic luminosity upper limits of (2.6-26.2)E49 erg/s for the
soft template, (3.9-36.5)E49 erg/s for the normal template, and
(1.3-11.2)E50
erg/s for the hard template over the 1 keV-10 MeV energy range.
GCN Circular 24539
Subject
LIGO/Virgo S190513bm: ANTARES neutrino search
Date
2019-05-14T13:03:35Z (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 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 S190513bm event using the 90% contour of the bayestar probability map provided by the GW interferometers (GCN#24522). The ANTARES visibility at the time of the alert, together with the 50% and 90% contours of the probability map are shown at https://www.cppm.in2p3.fr/~dornic/events_runo3/S190513bm.png. Considering the location probability provided by the LIGO/Virgo collaborations, there is a 55% 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 (2019-05-13
20:54:28.747 UT) and in the 90% contour of the S190513 event. The expected number of atmospheric background events in the region visible by ANTARES is 1.7e-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 1.2e-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.
GCN Circular 24543
Subject
LIGO/Virgo S190513bm: Swift/BAT Counterpart Search
Date
2019-05-14T17:44:05Z (6 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
S. D. Barthelmy (NASA/GSFC), A. Y. Lien (GSFC/UMBC),
D. M. Palmer (LANL), 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), 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 S190513bm (LIGO/VIRGO Collaboration GCN Circ. 24522),
where T0 is the LVC trigger time (2019-05-13T20:54:28.747 UTC).
The center of the BAT FOV at T0 is
RA = 126.463 deg,
DEC = -20.241 deg,
ROLL = 292.213 deg.
The BAT Field of View (>10% partial coding) covers 0.00% 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. The short spike around ~T0+278 s is due to noisy detectors.
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 ~ 8.71 x 10^-8 erg/s/cm^2.
Event data are not available within T0 +/- 100 s.
BAT retains decreased, but significant, sensitivity to rate increases for
gamma-ray events outside of its FOV. About 61.63% 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/S190513bm/web/source.html
GCN Circular 24546
Subject
LIGO/Virgo S190513bm: Lick/KAIT Follow-Up Observations
Date
2019-05-14T22:41:13Z (6 years ago)
From
Weikang Zheng at UC Berkeley <weikang@berkeley.edu>
Keto Zhang, Benjamin Stahl, Thomas de Jaeger, Yukei Murakami,
Sergiy Vasylyev, WeiKang Zheng, and Alexei V. Filippenko
(UC Berkeley) report on behalf of the Lick/KAIT GW follow-up team:
The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, observed the 90% region of the gravitational-wavei
event S190513bm (GCN 24522) 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 271 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 05:59:25, May. 14 UT,
about 9.1 hours after the trigger, and the last image at 12:21:06 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)
-----------------------------------------------
G1181335 05:59:25 16:35:37.830 +17:24:26.60
G1152863 06:00:34 16:36:03.880 +20:25:23.50
G0679845 06:01:43 16:36:30.560 +17:34:00.20
G0714754 06:02:53 16:37:29.640 +16:10:01.80
G0688824 06:04:02 16:37:40.650 +17:02:46.20
G0408645 06:05:12 16:38:32.770 +19:13:11.70
G1282809 06:06:21 16:39:04.670 +16:02:25.00
G0730489 06:07:30 16:39:10.060 +15:56:46.10
G0848031 06:08:39 16:39:41.170 +15:51:05.60
G1352160 06:09:49 16:39:53.970 +19:32:39.90
G1129213 06:10:56 16:40:45.040 +18:20:55.30
G1157222 06:12:06 16:41:14.590 +15:38:46.90
G1141615 06:13:15 16:41:13.960 +18:12:58.60
G0149363 06:14:24 16:41:31.360 +19:16:16.30
G1068227 06:15:33 16:41:34.720 +19:00:57.80
G1232588 06:16:43 16:42:25.320 +17:59:37.00
G0349023 06:17:52 16:42:26.090 +17:33:34.20
G1227301 06:19:01 16:42:29.840 +16:18:29.90
G0775288 06:20:15 16:42:32.550 +13:39:23.30
G0027469 06:21:24 16:43:34.110 +14:24:05.30
G0980349 06:22:33 16:43:44.090 +11:59:26.20
G0859605 06:23:45 16:43:41.520 +17:50:26.00
G0200181 06:24:54 16:43:45.080 +16:57:17.10
G0986785 06:26:03 16:43:58.450 +19:47:12.90
G1325288 06:27:15 16:44:10.970 +11:35:37.80
G0974745 06:28:26 16:44:11.130 +19:39:00.50
G0551637 06:29:37 16:44:19.110 +13:20:30.20
G0173494 06:30:51 16:44:23.160 +09:24:11.70
G0417778 06:32:00 16:44:22.420 +12:44:09.90
G0358155 06:33:09 16:44:21.590 +14:05:54.90
G1383019 06:53:32 16:44:22.390 +12:43:53.30
G0854058 06:54:44 16:44:35.370 +19:25:43.80
G1339289 06:55:53 16:44:39.100 +17:43:44.70
G1340645 06:57:06 16:44:59.180 +11:19:20.70
G0999584 06:58:16 16:45:15.820 +09:45:10.40
G0350396 06:59:25 16:45:28.670 +11:21:29.40
G1270621 07:00:34 16:45:36.590 +08:58:58.00
G1278670 07:01:46 16:45:34.020 +16:44:47.50
G0053116 07:02:55 16:45:37.160 +18:14:16.30
G1470678 07:04:04 16:45:42.150 +15:12:31.40
G1187220 07:05:13 16:45:52.000 +12:08:41.40
G0240845 07:06:23 16:45:55.140 +16:32:41.20
G1124450 07:07:32 16:45:55.860 +16:37:52.70
G0689333 07:08:41 16:45:59.490 +19:39:28.00
G0220002 07:09:53 16:46:05.290 +08:44:15.10
G1194480 07:11:04 16:46:01.240 +19:39:40.30
G0835941 07:12:13 16:46:13.990 +13:06:24.30
G0636473 07:13:25 16:46:17.670 +18:10:26.10
G0148430 07:14:36 16:46:20.830 +13:23:08.20
G0043388 07:15:47 16:46:27.530 +18:41:41.00
G0416934 07:16:59 16:47:00.830 +11:53:52.20
G0814773 07:18:08 16:47:18.250 +11:42:25.10
G1167489 07:19:21 16:47:27.540 +08:05:57.70
G1199890 07:20:31 16:47:31.540 +11:38:27.80
G0216837 07:21:40 16:47:30.530 +14:45:09.70
G1317457 07:22:49 16:47:31.010 +15:43:17.20
G1012876 07:23:59 16:47:34.280 +14:08:03.30
G0322910 07:25:08 16:47:33.370 +15:55:40.50
G1225799 07:26:19 16:47:45.570 +10:49:36.60
G0136772 07:27:30 16:47:59.220 +18:06:28.70
G1373123 07:37:51 16:48:06.810 +12:49:25.10
G0906724 07:39:01 16:48:16.280 +12:32:07.20
G0940514 07:40:10 16:48:39.380 +08:53:09.10
G0042623 07:41:19 16:48:45.670 +12:06:01.90
G1414190 07:42:28 16:49:12.490 +14:51:10.40
G1048270 07:43:38 16:49:27.570 +17:33:30.40
G0295022 07:44:47 16:49:34.960 +18:12:26.80
G0364218 07:45:57 16:49:51.860 +14:44:02.00
G1382997 07:47:06 16:49:57.220 +13:09:28.60
G0333648 07:48:15 16:50:13.680 +14:00:50.10
G1183789 07:49:24 16:50:24.930 +14:53:42.00
G0980425 07:50:34 16:50:53.690 +11:50:47.90
G0424901 07:51:45 16:50:53.650 +16:43:43.40
G0972547 07:52:56 16:51:27.160 +11:21:51.60
G0614395 07:54:06 16:51:33.530 +11:58:31.00
G1403122 07:55:15 16:52:04.830 +14:21:43.70
G1193848 07:56:24 16:52:05.760 +14:42:07.80
G1081487 07:57:38 16:52:25.650 +07:13:38.50
G1466453 07:58:47 16:52:57.500 +08:36:15.30
G1071784 07:59:58 16:53:02.420 +17:36:25.60
G1107093 08:01:12 16:53:14.990 +05:37:26.70
G1025069 08:02:23 16:53:44.880 +11:27:49.10
G1058185 08:03:32 16:53:43.850 +14:31:26.30
G1379126 08:04:42 16:53:45.180 +15:52:57.50
G0254728 08:05:55 16:54:01.840 +04:07:47.60
G1257069 08:07:04 16:54:02.360 +06:08:45.70
G0289582 08:08:14 16:54:09.070 +08:59:14.80
G0077399 08:09:25 16:54:05.790 +16:25:26.00
G0213121 08:10:34 16:54:08.380 +15:21:29.10
G1023514 08:11:46 16:54:15.870 +06:28:37.80
G0529235 08:13:51 18:49:23.670 -25:27:30.90
G0678640 08:15:02 18:49:36.670 -28:42:48.90
G0523832 08:16:14 18:50:38.310 -26:14:14.80
G0216976 08:17:25 18:50:43.230 -24:54:39.60
G0581909 08:18:39 18:52:44.630 -29:33:36.70
G1332029 08:19:50 18:53:05.440 -24:30:54.00
G0000596 08:21:02 18:53:12.370 -27:15:02.20
G0410804 08:22:13 18:53:15.300 -27:00:29.30
G0063058 08:23:24 18:53:23.630 -27:30:55.50
G0154905 08:24:34 18:53:24.610 -23:14:51.20
G0353400 08:25:43 18:53:37.300 -25:11:06.20
G0770089 08:26:50 18:53:39.030 -24:44:20.50
G1856468 08:28:02 18:54:37.350 -27:27:56.60
G0956297 08:29:13 18:55:24.450 -27:20:26.90
G0644902 08:30:25 18:55:47.230 -28:12:47.80
G0064241 08:31:36 18:56:12.420 -27:15:06.00
G0418646 08:32:47 18:56:42.130 -28:36:49.10
G0156862 08:33:59 18:56:49.390 -23:22:46.10
G1259929 08:35:10 18:57:43.570 -28:53:24.80
G0919815 08:36:22 18:58:42.530 -28:40:24.50
G0468115 08:37:33 18:59:17.820 -29:52:01.80
G0085787 08:38:45 19:00:27.860 -27:07:20.50
G1094397 08:39:56 19:02:39.540 -29:48:30.60
G0798864 08:41:08 19:03:20.700 -28:41:14.50
G0020291 08:42:19 19:05:29.590 -30:29:35.30
G1179259 08:43:30 19:06:13.980 -28:55:35.20
G1275107 08:44:42 19:07:11.290 -29:25:41.10
G0988333 08:45:53 19:07:22.950 -28:11:42.80
G1395264 08:47:05 19:08:28.450 -28:35:47.50
G0372384 08:48:16 19:08:31.960 -28:39:31.50
G0355859 08:50:08 19:08:40.190 -28:55:13.40
G1344287 08:51:19 19:08:40.470 -28:42:49.00
G1418553 08:52:31 19:09:04.160 -28:19:46.00
G0269208 08:53:38 19:09:16.990 -27:18:55.50
G1149313 08:54:50 19:09:20.610 -29:45:50.00
G0882612 08:56:01 19:09:36.420 -30:17:15.80
G0939469 08:57:10 19:09:48.390 -27:11:13.40
G0022513 08:58:20 19:10:19.580 -27:17:49.60
G1154465 08:59:31 19:10:34.430 -29:44:31.60
G1108515 09:00:43 19:10:34.100 -28:17:34.50
G1126435 09:01:52 19:10:42.800 -28:16:44.60
G0667059 09:03:04 19:11:21.990 -28:22:32.40
G1234439 09:04:15 19:11:53.840 -29:36:32.60
G1250678 09:05:24 19:12:26.500 -27:39:43.20
G0535632 09:06:36 19:12:51.640 -29:56:58.70
G0975066 09:07:45 19:12:58.700 -27:35:05.70
G1196911 09:08:57 19:13:24.310 -29:37:54.60
G1305631 09:10:08 19:13:30.780 -30:58:50.60
G0724116 09:11:17 19:13:40.810 -29:02:42.80
G1018941 09:12:29 19:14:08.560 -30:05:25.60
G0649026 09:13:41 19:14:50.750 -30:08:23.70
G0113459 09:14:52 19:14:55.330 -29:59:55.90
G0334535 09:16:03 19:15:02.750 -30:53:27.50
G1041184 09:17:15 19:15:20.230 -30:20:22.00
G0703260 09:18:26 19:15:36.840 -29:45:01.70
G0704081 09:19:38 19:15:55.930 -30:15:42.30
G0632806 09:20:47 19:15:56.760 -28:39:12.40
G1134092 09:21:56 19:17:07.010 -29:54:23.70
G1162544 09:23:06 19:17:25.130 -29:59:53.10
G0997093 09:24:15 19:18:15.670 -30:04:46.40
G0361538 09:26:15 16:54:12.420 +16:17:34.80
G1379119 09:27:24 16:54:16.890 +11:10:15.80
G0081827 09:28:34 16:54:21.730 +12:25:56.90
G0535610 09:29:43 16:54:21.710 +13:35:17.50
G1157961 09:30:56 16:54:29.040 +09:33:30.90
G0947829 09:32:06 16:54:45.060 +10:00:51.30
G1198883 09:33:15 16:54:48.490 +05:25:12.80
G1004711 09:34:24 16:54:54.350 +06:28:16.50
G0174046 09:35:33 16:55:08.000 +07:33:56.50
G0898653 09:36:44 16:55:15.290 +06:45:13.60
G1241265 09:37:53 16:55:17.280 +05:52:38.30
G0403804 09:39:02 16:55:21.350 +03:45:03.10
G0997900 09:40:14 16:55:20.210 +08:31:24.50
G1345115 09:41:25 16:55:27.190 +03:46:16.60
G1403843 09:42:38 16:55:35.640 +17:19:32.40
G1217709 09:43:49 16:56:32.870 +06:56:28.30
G0897516 09:44:59 16:56:35.780 +05:43:12.50
G0930990 09:46:08 16:56:35.540 +08:31:56.30
G1473608 09:47:17 16:56:40.880 +10:42:53.70
G0313920 09:48:27 16:57:16.920 +08:03:44.30
G0414300 09:49:36 16:57:16.740 +11:12:50.60
G1392880 09:50:45 16:57:22.480 +15:12:35.40
G1330110 09:51:57 16:57:37.540 +08:01:17.40
G0262809 09:53:06 16:57:38.160 +10:13:32.80
G0254740 09:54:15 16:57:49.570 +09:53:43.30
G0093646 09:55:27 16:57:54.950 +03:09:36.80
G1317922 09:56:36 16:58:04.160 +04:14:40.20
G0211187 09:57:49 16:58:02.850 +06:34:34.80
G1470346 09:58:59 16:58:19.050 +10:54:06.50
G0308247 10:00:08 16:58:24.780 +08:23:40.80
G0171164 10:02:13 19:18:22.810 -27:37:33.50
G1411264 10:03:22 19:18:31.890 -29:33:03.20
G1179003 10:04:32 19:18:33.610 -30:40:08.20
G1091770 10:05:41 19:19:38.530 -30:28:35.50
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G1219013 12:21:06 17:07:27.530 +02:15:34.10
GCN Circular 24548
Subject
LIGO/Virgo S190513bm: CALET Observations
Date
2019-05-15T03:51:49Z (6 years ago)
From
Yuta Kawakubo at Louisiana State U./CALET <kawakubo1@lsu.edu>
T. Sakamoto, A. Yoshida, 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), P. S. Marrocchesi (U of Siena),
and the CALET collaboration:
The CALET Gamma-ray Burst Monitor (CGBM) was operating at the
trigger time of S190513bm T0 = 2019-05-13 20:54:28.747 UT (The LIGO
Scientific Collaboration and Virgo Collaboration, GCN Circ. 24522).
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 inside of the field-of-view of SGM. The summed
LIGO probabilities inside the HXM and the SGM field of view are 33%
and 95% (and 0% credible region of the initial localization map were
Earth-occulted). The HXM and SGM field of views were centered at
RA = 355.5 deg, Dec=11.0 deg and RA = 348.0 deg, Dec = 4.3 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
(signal-to-noise ratio >= 7) 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 low energy trigger mode
at the trigger time of S190513bm. Using 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.
The 90% upper limit of CAL is 6.0x10^-5 erg/cm2/s (1-10 GeV) when
the summed LIGO-Virgo probability reaches 5%. The CAL FOV was
centered at RA = 348.0 deg, Dec = 4.4 deg at T0.
GCN Circular 24549
Subject
LIGO/Virgo S190513bm : TAROT-Calern and TAROT-Chile (TCA/TCH)/GRANDMA observation report.
Date
2019-05-15T04:10:45Z (6 years ago)
From
Hayden Crisp at OzGrav <20934203@student.uwa.edu.au>
H. Crisp (OzGrav-UWA), S. Alishov (SHAO), S. Beradze (Iliauni), P.
Lognone (LAL), M. Boer (Artemis), N. Christensen (Artemis), L. Eymar
(Artemis), A. Klotz (IRAP), K. Noysena (Artemis, 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)
Report on behalf of the TAROT network and GRANDMA collaborations.
We performed tiled observations of LIGO/Virgo S190513bm event (GCN
#24522) with the TAROT-Chili (TCH) telescope operating with a clear
filter located at La Silla ESO observatory (LaS/ESO), and with the
TAROT-Calern (TCA) telescope operating with a clear filter located at
Calern site at the Cote d'Azur observatory.
The TCA observation started on 05/13/19 21:34:47 UTC which corresponds
approximately to 41 minutes after the GW trigger time.
We performed the following tiled observations :
+------------+------------+---------+---------+---------+
| TStart | TEnd | RA | DEC | Proba |
| [UTC] | [UTC] | [deg] | [deg] | [%] |
|------------+------------+---------+---------+---------|
| 2019-05-13 | 2019-05-14 | 56.471 | 59.091 | 1.4 |
| 21:34:47 | 03:04:02 | | | |
| 2019-05-13 | 2019-05-14 | 53.333 | 57.273 | 1 |
| 21:41:36 | 03:10:51 | | | |
| 2019-05-13 | 2019-05-14 | 56.667 | 57.273 | 1.5 |
| 22:13:26 | 02:59:27 | | | |
| 2019-05-13 | 2019-05-14 | 60 | 57.273 | 1 |
| 23:19:10 | 02:21:45 | | | |
| 2019-05-14 | 2019-05-14 | 60 | 59.091 | 1 |
| 00:21:32 | 02:28:35 | | | |
| 2019-05-14 | 2019-05-14 | 55.67 | 60.909 | 0.7 |
| 00:34:43 | 02:40:30 | | | |
| 2019-05-14 | 2019-05-14 | 52.941 | 59.091 | 0.8 |
| 01:28:38 | 01:35:09 | | | |
+------------+------------+---------+---------+---------+
The TCH observation started on 05/14/19 02:55:11 UTC which corresponds
approximately to 361 minutes after the GW trigger time.
We performed the following tiled observations :
+------------+------------+---------+---------+---------+
| TStart | TEnd | RA | DEC | Proba |
| [UTC] | [UTC] | [deg] | [deg] | [%] |
|------------+------------+---------+---------+---------|
| 2019-05-14 | 2019-05-14 | 287.168 | -30 | 5.1 |
| 02:55:11 | 10:01:41 | | | |
| 2019-05-14 | 2019-05-14 | 286.364 | -28.182 | 3.6 |
| 03:02:00 | 10:08:29 | | | |
| 2019-05-14 | 2019-05-14 | 285.087 | -30 | 3 |
| 03:08:48 | 10:15:17 | | | |
| 2019-05-14 | 2019-05-14 | 288.409 | -28.182 | 2.3 |
| 03:21:12 | 10:27:36 | | | |
| 2019-05-14 | 2019-05-14 | 285.444 | -31.818 | 2.1 |
| 03:28:01 | 09:34:24 | | | |
| 2019-05-14 | 2019-05-14 | 289.249 | -30 | 1.6 |
| 03:34:49 | 09:41:13 | | | |
+------------+------------+---------+---------+---------+
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. The TCA and TCH telescope observations cover
7% and 17% of the cumulative probability of the skymap respectively,
for a total of 24% coverage. The typical limiting magnitude is 18.0
for a 60.0 s exposure.
The coverage map is available at:
https://grandma-owncloud.lal.in2p3.fr/index.php/s/Doq7WNvbtg47blh
Potential optical transient candidates list will be sent
through another GCN circular depending on our data 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
or on http://tarot.obs-hp.fr/.
This circular is citable.
GCN Circular 24566
Subject
LIGO/Virgo S190513bm: Swope follow-up observations
Date
2019-05-16T23:00:08Z (6 years ago)
From
Charles Kilpatrick at UC Santa Cruz <cdkilpat@ucsc.edu>
C. D. Kilpatrick, D. A. Coulter, J. S. Brown, G. Dimitriadis, R. J. Foley, T. Hung, D. O. Jones, A. Murguia-Berthier, J. X. Prochaska, E. Ramirez-Ruiz, C. Rojas-Bravo, M. R. Siebert, K. Siellez (UCSC), A. L. Piro (Carnegie), A. Rest (STScI), Abdo Campillay (Universidad de La Serena), M. Drout (University of Toronto)
report on behalf of the 1M2H collaboration:
in the process of following up the localization region of LIGO/Virgo S190513bm on 2019 May 14 UT, we observed the following fields with the 1.0-m Swope telescope at Las Campanas Observatory. We covered approximately 15% of the probability region from the LALinference map provided by the LVC (GCN 24522).
The Swope Direct 4kx4k imager covers 29.8 arcmin x 29.7 arcmin. All images were 5-minute r-band exposures. We performed difference imaging using the photpipe image reduction and subtraction pipeline (Rest et al. 2005, ApJ, 634, 1103) with PS1 (Flewelling et al. 2016, arXiv:161205243) and SkyMapper (Wolf et al. 2018, PASA, 35, 10) r-band templates for reference. For each image, the approximate pointing center and 3-sigma limiting magnitude are indicated. We did not detect any new transients in these images.
RA (J2000) | DEC (J2000) | MJD | Limiting Magnitude
19:06:59.76 | -29:19:22.0 | 58617.33552 | 21.7
19:07:00.91 | -30:18:56.1 | 58617.33123 | 21.8
19:06:59.64 | -29:49:14.8 | 58617.34000 | 21.7
19:09:16.77 | -29:19:18.8 | 58617.34481 | 21.8
19:04:40.94 | -30:18:57.9 | 58617.32678 | 21.7
19:09:17.25 | -30:18:50.0 | 58617.34907 | 21.8
19:07:00.24 | -28:49:34.3 | 58617.32241 | 21.7
19:04:43.36 | -29:19:17.0 | 58617.31808 | 21.7
19:09:16.56 | -29:49:01.9 | 58617.35336 | 21.7
19:04:41.85 | -29:49:00.4 | 58617.31377 | 21.7
19:09:15.16 | -28:49:35.0 | 58617.35756 | 21.7
19:07:00.19 | -30:48:42.4 | 58617.30949 | 21.7
19:04:43.80 | -28:49:31.8 | 58617.36199 | 21.8
19:04:40.39 | -30:48:41.7 | 58617.30524 | 21.8
19:11:33.04 | -29:19:25.3 | 58617.36634 | 21.8
19:09:17.49 | -30:48:56.1 | 58617.37087 | 21.8
19:06:59.54 | -31:18:26.2 | 58617.30101 | 21.8
19:06:59.85 | -28:19:35.0 | 58617.29666 | 21.7
19:02:24.12 | -30:18:56.1 | 58617.29206 | 21.6
19:11:35.64 | -30:19:00.8 | 58617.37517 | 21.8
19:02:26.37 | -29:19:22.4 | 58617.28774 | 21.7
19:04:39.74 | -31:18:44.6 | 58617.38035 | 21.8
19:11:31.53 | -28:49:29.2 | 58617.38497 | 21.7
19:11:33.55 | -29:49:19.2 | 58617.38929 | 21.7
19:09:15.14 | -28:19:33.2 | 58617.28332 | 21.8
19:02:24.88 | -29:49:10.2 | 58617.27860 | 21.6
19:09:17.97 | -31:18:39.6 | 58617.39361 | 21.7
19:04:44.88 | -28:19:39.7 | 58617.27406 | 21.6
19:06:58.53 | -27:49:53.7 | 58617.39814 | 21.7
19:02:28.03 | -28:49:19.2 | 58617.26932 | 21.5
19:09:14.06 | -27:49:58.4 | 58617.40274 | 21.7
19:02:21.88 | -30:48:47.8 | 58617.26479 | 21.5
19:11:36.72 | -30:49:03.7 | 58617.40721 | 21.7
19:04:45.50 | -27:49:44.0 | 58617.26001 | 21.4
19:02:22.99 | -31:18:27.3 | 58617.25547 | 21.4
19:11:28.87 | -28:19:32.5 | 58617.24663 | 21.3
19:13:49.20 | -29:19:09.8 | 58617.24203 | 21.2
19:07:00.50 | -31:48:17.6 | 58617.23755 | 21.3
19:04:40.80 | -31:48:19.4 | 58617.23247 | 21.3
19:13:53.28 | -30:18:57.9 | 58617.22780 | 21.2
19:07:00.69 | -27:19:58.8 | 58617.22306 | 21.2
19:00:07.24 | -30:18:52.2 | 58617.21831 | 21.2
19:13:50.85 | -29:49:01.2 | 58617.21369 | 21.2
19:09:12.40 | -27:20:08.1 | 58617.20906 | 21.0
19:11:29.13 | -27:49:48.7 | 58617.20457 | 21.0
19:00:11.97 | -29:19:12.7 | 58617.19986 | 21.0
19:09:20.23 | -31:48:22.6 | 58617.19528 | 21.0
19:02:30.19 | -28:19:35.7 | 58617.19060 | 20.9
19:00:09.14 | -29:49:06.6 | 58617.18583 | 20.8
19:13:47.32 | -28:49:36.1 | 58617.18101 | 20.9
19:04:46.27 | -27:20:04.2 | 58617.17635 | 20.8
19:02:20.78 | -31:48:27.7 | 58617.17166 | 20.9
19:13:45.43 | -28:19:44.7 | 58617.16690 | 20.7
19:00:05.11 | -30:48:48.9 | 58617.15785 | 20.6
19:00:13.80 | -28:49:36.1 | 58617.15314 | 20.7
18:57:47.52 | -30:48:56.1 | 58617.14788 | 20.6
17:05:49.48 | +04:57:24.4 | 58617.14270 | 21.0
17:03:44.08 | +05:27:24.4 | 58617.13778 | 20.9
17:03:49.44 | +04:57:33.1 | 58617.13264 | 20.9
17:03:53.64 | +04:27:38.8 | 58617.12769 | 20.9
17:10:04.29 | +02:58:11.2 | 58617.12213 | 20.9
17:08:08.88 | +02:28:18.8 | 58617.11722 | 20.8
17:02:12.67 | +01:58:19.2 | 58617.11199 | 20.9
Please direct all communication related to this circular to Charlie Kilpatrick (cdkilpat@ucsc.edu).