LIGO/Virgo S191129u
GCN Circular 26824
Subject
LIGO/Virgo S191129u: Upper limits from Konus-Wind observations
Date
2020-01-20T12:44:31Z (6 years ago)
From
Anna Ridnaia at Ioffe Institute <ridnaia@mail.ioffe.ru>
A. Ridnaia, S. Golenetskii, R.Aptekar, D. Frederiks,
M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline,
on behalf of the Konus-Wind team, report:
Konus-Wind (KW) was observing the whole sky at the time of the
LIGO/Virgo event S191129u (2019-11-29 13:40:29.197 UTC, hereafter T0;
LIGO/Virgo Collaboration GCN Circ. 26303).
No triggered KW GRBs happened between ~10 hours before and ~2 days
after T0. The closest waiting-mode GRB was observed ~16 hours after T0.
Using waiting-mode data within the interval T0 +/- 100 s,
we found no significant (> 5 sigma) excess over the background
in both KW detectors on temporal scales from 2.944 s to 100 s.
We estimate an upper limit (90% conf.) on the 20 - 1500 keV fluence
to 9.2x10^-7 erg/cm^2 for a burst lasting less than 2.944 s and having a
typical KW short GRB spectrum (an exponentially cut off power law with
alpha =-0.5 and Ep=500 keV). For a typical long GRB spectrum (the Band
function with alpha=-1, beta=-2.5, and Ep=300 keV), the corresponding
limiting peak flux is 2.5x10^-7 erg/cm^2/s (20 - 1500 keV, 2.944 s scale).
All the quoted values are preliminary.
GCN Circular 26383
Subject
LIGO/Virgo S191129u: Updated Sky Localization
Date
2019-12-08T21:30:47Z (6 years ago)
From
Leo Singer at GSFC <leo.p.singer@nasa.gov>
The LIGO Scientific Collaboration and the Virgo Collaboration report:
We have conducted further analysis of the LIGO Hanford Observatory
(H1), LIGO Livingston Observatory (L1), and Virgo Observatory (V1)
data around the time of the compact binary merger (CBC) candidate
S191129u (GCN Circular 26303).
Parameter estimation has been performed using LALInference [1] and a
new sky map, LALInference.fits.gz,0, distributed via GCN Notice, is
available for retrieval from the GraceDB event page:
https://gracedb.ligo.org/superevents/S191129u/
The preferred sky map at this time is LALInference.fits.gz,0. For the
LALInference.fits.gz,0 sky map, the 90% credible region is 852 deg2.
Marginalized over the whole sky, the a posteriori luminosity distance
estimate is 742 +/- 180 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 26362
Subject
LIGO/Virgo S191129u : No significant candidates in FRAM-TAROT-GRANDMA observations.
Date
2019-12-06T10:26:54Z (6 years ago)
From
Cyril Lachaud at APC/Univ. Paris Diderot <cyril.lachaud@in2p3.fr>
S. Beradze (Iliauni), T. Sadibekova (AIM-CEA), D. Coward (OzGrav-UWA), C.
Lachaud (APC), M. Boer (Artemis), N. Christensen (Artemis), L. Eymar
(Artemis), S. Karpov, M. Masek, M. Prouza (FZU), A. Klotz (IRAP), K.
Noysena (Artemis, IRAP), S. Antier (APC), A. Coleiro (APC), D. Corre
(LAL), M. Coughlin (Caltech), J.G. Ducoin (LAL), B. Gendre (OzGrav-UWA),
P. Hello (LAL), D. A. Kann (HETH/IAA-CSIC), N. Kochiashvili (Iliauni),
N. Leroy (LAL), C. Thoene (HETH/IAA-CSIC), D. Turpin (AIM-CEA, NAOC),
X. Wang (THU)
report on behalf of the FRAM-Auger, TAROT-Calern (TCA), TAROT-Chili
(TCH) and GRANDMA collaborations.
We performed tiled observations of the LIGO/Virgo S191129u event with the
FRAM-Auger, TAROT-Calern (TCA) and TAROT-Chili (TCH)
telescopes, operating in the R-band for FRAM and Clear for TAROT, located
respectively at Pierre Auger Observatory (Malargue, Argentina),
the Cote d'Azur Observatory and La Silla ESO (LaS/ESO).
The following table shows for each telescope: the delay in minutes
from the trigger, which filter is used, the field of view of the
telescope in degrees and the typical magnitude in R (AB mag) for a
given exposure in seconds.
+-------------+---------+----------+-----------+------------+
| Telescope | Delay | Filter | f.o.v. | Limiting |
| | [min] | | [deg] | Mag. |
|-------------+---------+----------+-----------+------------|
| FRAM-Auger | 677 | R | 1.0 x 1.0 | 17.0 (60s) |
| TCA | 633 | Clear | 1.9 x 1.9 | 18.0 (60s) |
| TCH | 640 | Clear | 1.9 x 1.9 | 18.0 (60s) |
+-------------+---------+----------+-----------+------------+
We performed the following joint tiled observations [1]:
+-------------+------------+------------+---------+---------+---------+
| Telescope | TStart | TEnd | RA | DEC | Proba |
| | [UTC] | [UTC] | [deg] | [deg] | [%] |
|-------------+------------+------------+---------+---------+---------|
| FRAM-Auger | 2019-11-30 | 2019-11-30 | 337.391 | -55.946 | 0.3 |
| | 00:57:25 | 01:01:52 | | | |
| FRAM-Auger | 2019-11-30 | 2019-11-30 | 338.614 | -56.919 | 0.3 |
| | 01:20:02 | 01:22:02 | | | |
| FRAM-Auger | 2019-11-30 | 2019-11-30 | 334.170 | -53.027 | 0.3 |
| | 01:22:39 | 01:27:06 | | | |
| FRAM-Auger | 2019-11-30 | 2019-11-30 | 335.785 | -53.027 | 0.3 |
| | 01:27:42 | 01:32:09 | | | |
| FRAM-Auger | 2019-11-30 | 2019-11-30 | 336.832 | -56.919 | 0.3 |
| | 01:32:45 | 01:37:12 | | | |
| FRAM-Auger | 2019-11-30 | 2019-11-30 | 338.071 | -57.892 | 0.3 |
| | 01:37:47 | 01:42:14 | | | |
| FRAM-Auger | 2019-11-30 | 2019-11-30 | 339.899 | -57.892 | 0.3 |
| | 01:42:50 | 01:47:17 | | | |
| FRAM-Auger | 2019-11-30 | 2019-11-30 | 336.881 | -54.000 | 0.3 |
| | 01:48:50 | 01:53:17 | | | |
| FRAM-Auger | 2019-11-30 | 2019-11-30 | 342.099 | -60.811 | 0.3 |
| | 01:54:00 | 01:58:27 | | | |
| FRAM-Auger | 2019-11-30 | 2019-11-30 | 340.645 | -59.838 | 0.3 |
| | 01:59:56 | 02:04:23 | | | |
| FRAM-Auger | 2019-11-30 | 2019-11-30 | 339.267 | -58.865 | 0.2 |
| | 02:05:14 | 02:09:41 | | | |
| FRAM-Auger | 2019-11-30 | 2019-11-30 | 335.652 | -55.946 | 0.2 |
| | 02:10:36 | 02:15:03 | | | |
| FRAM-Auger | 2019-11-30 | 2019-11-30 | 335.279 | -51.081 | 0.2 |
| | 02:30:51 | 02:35:18 | | | |
| FRAM-Auger | 2019-11-30 | 2019-11-30 | 338.028 | -54.973 | 0.2 |
| | 02:35:54 | 02:40:21 | | | |
| FRAM-Auger | 2019-11-30 | 2019-11-30 | 341.152 | -58.865 | 0.2 |
| | 02:40:58 | 02:45:25 | | | |
| FRAM-Auger | 2019-11-30 | 2019-11-30 | 344.634 | -63.730 | 0.2 |
| | 02:46:01 | 02:50:28 | | | |
| FRAM-Auger | 2019-11-30 | 2019-11-30 | 340.111 | -60.811 | 0.2 |
| | 02:51:02 | 03:08:26 | | | |
| ----- | ----- | ----- | ----- | ----- | ----- |
| TCA | 2019-11-30 | 2019-11-30 | 191.012 | 35.280 | 0.6 |
| | 00:13:27 | 00:19:46 | | | |
| TCA | 2019-11-30 | 2019-11-30 | 185.236 | 31.569 | 0.5 |
| | 00:26:27 | 05:33:02 | | | |
| TCA | 2019-11-30 | 2019-11-30 | 193.561 | 37.136 | 0.5 |
| | 00:33:14 | 03:09:47 | | | |
| TCA | 2019-11-30 | 2019-11-30 | 187.535 | 33.424 | 0.5 |
| | 00:39:58 | 05:45:47 | | | |
| TCA | 2019-11-30 | 2019-11-30 | 187.379 | 31.569 | 0.7 |
| | 00:54:20 | 02:00:21 | | | |
| TCA | 2019-11-30 | 2019-11-30 | 201.487 | 40.847 | 0.4 |
| | 01:05:54 | 03:41:42 | | | |
| TCA | 2019-11-30 | 2019-11-30 | 189.521 | 31.569 | 0.4 |
| | 01:18:41 | 01:25:00 | | | |
| TCA | 2019-11-30 | 2019-11-30 | 198.147 | 37.136 | 0.4 |
| | 01:25:20 | 04:01:08 | | | |
| TCA | 2019-11-30 | 2019-11-30 | 204.536 | 42.703 | 0.3 |
| | 01:44:51 | 04:20:52 | | | |
| TCA | 2019-11-30 | 2019-11-30 | 185.738 | 29.713 | 0.7 |
| | 02:11:10 | 04:47:26 | | | |
| TCA | 2019-11-30 | 2019-11-30 | 189.731 | 33.424 | 0.7 |
| | 02:17:53 | 04:54:12 | | | |
| TCA | 2019-11-30 | 2019-11-30 | 193.248 | 35.280 | 0.6 |
| | 02:30:33 | 05:06:52 | | | |
| TCA | 2019-11-30 | 2019-11-30 | 195.855 | 37.136 | 0.6 |
| | 02:37:18 | 05:13:37 | | | |
| TCA | 2019-11-30 | 2019-11-30 | 198.597 | 38.991 | 0.5 |
| | 02:49:57 | 05:26:17 | | | |
| TCA | 2019-11-30 | 2019-11-30 | 200.950 | 38.991 | 0.4 |
| | 03:15:58 | 03:22:17 | | | |
| TCA | 2019-11-30 | 2019-11-30 | 191.926 | 33.424 | 0.4 |
| | 03:22:43 | 03:29:02 | | | |
| TCA | 2019-11-30 | 2019-11-30 | 196.244 | 38.991 | 0.4 |
| | 03:42:21 | 03:48:40 | | | |
| TCA | 2019-11-30 | 2019-11-30 | 207.019 | 42.703 | 0.4 |
| | 04:01:33 | 04:07:52 | | | |
| ----- | ----- | ----- | ----- | ----- | ----- |
| TCH | 2019-11-30 | 2019-12-01 | 334.643 | -52.686 | 1.0 |
| | 00:20:23 | 04:09:13 | | | |
| TCH | 2019-11-30 | 2019-11-30 | 335.463 | -54.505 | 1.0 |
| | 00:27:00 | 00:33:18 | | | |
| TCH | 2019-11-30 | 2019-12-01 | 326.623 | -39.959 | 1.0 |
| | 00:39:24 | 04:16:01 | | | |
| TCH | 2019-11-30 | 2019-12-01 | 339.298 | -58.141 | 0.9 |
| | 00:46:12 | 06:52:11 | | | |
| TCH | 2019-11-30 | 2019-11-30 | 326.111 | -38.141 | 0.9 |
| | 00:52:57 | 01:11:40 | | | |
| TCH | 2019-11-30 | 2019-12-02 | 341.443 | -59.959 | 0.9 |
| | 01:18:24 | 00:35:44 | | | |
| TCH | 2019-11-30 | 2019-12-02 | 344.009 | -63.595 | 0.7 |
| | 01:31:19 | 01:07:37 | | | |
| TCH | 2019-11-30 | 2019-12-02 | 337.732 | -60.434 | 0.4 |
| | 01:38:05 | 01:14:23 | | | |
| TCH | 2019-11-30 | 2019-12-02 | 342.950 | -65.414 | 0.4 |
| | 01:44:51 | 01:21:08 | | | |
| TCH | 2019-11-30 | 2019-12-01 | 332.350 | -49.050 | 1.1 |
| | 02:11:04 | 03:30:54 | | | |
| TCH | 2019-11-30 | 2019-12-01 | 329.646 | -45.414 | 1.1 |
| | 02:17:50 | 03:24:11 | | | |
| TCH | 2019-11-30 | 2019-12-01 | 330.701 | -47.232 | 1.1 |
| | 02:24:34 | 01:00:55 | | | |
| TCH | 2019-11-30 | 2019-12-01 | 333.659 | -50.868 | 1.0 |
| | 02:37:02 | 03:43:18 | | | |
| TCH | 2019-11-30 | 2019-12-01 | 327.945 | -41.777 | 1.0 |
| | 02:43:45 | 01:20:06 | | | |
| TCH | 2019-11-30 | 2019-12-01 | 337.617 | -56.323 | 1.0 |
| | 03:02:59 | 01:39:22 | | | |
| TCH | 2019-11-30 | 2019-12-01 | 328.434 | -38.141 | 0.4 |
| | 04:08:05 | 02:44:21 | | | |
| TCH | 2019-11-30 | 2019-11-30 | 327.352 | -36.323 | 0.4 |
| | 04:14:50 | 04:21:09 | | | |
| TCH | 2019-12-01 | 2019-12-01 | 328.627 | -43.595 | 1.0 |
| | 03:43:46 | 03:50:04 | | | |
+-------------+------------+------------+---------+---------+---------+
TStart and TEnd refer respectively to the time of the first and last
exposure for a given tile. Observations are not necessarily continuous
in this interval.
The Probability refers to the 2D spatial probability of the GW skymap
enclosed in a given tile.
These observations cover about 24% of the cumulative probability of
the BAYESTAR skymap available on 2019-11-29 13:42:00 (UTC).
The coverage map is available at:
https://grandma-owncloud.lal.in2p3.fr/index.php/s/YMk334EKRjSfnGD
No significant transient candidates were found during our low latency
analysis [2,3].
GRANDMA (Global Rapid Advanced Network Devoted to the Multi-messenger
Addicts) is a network of robotic telescopes connected all over the
world with both photometry and spectrometry capabilities for Time-
domain Astronomy [2](https://grandma.lal.in2p3.fr/).
Details on the different telescopes are available on the GRANDMA web
pages.
[1] M. W Coughlin et al., MNRAS 2019, doi.org/10.1093/mnras/stz2485
[2] S. Antier et al., MNRAS 2019, arXiv:1910.11261
[3] K. Noysena et al., ApJ 2019, arXiv:1910.02770
GCN Circular 26321
Subject
LIGO/Virgo S191129u: No transient candidates in CALET observations
Date
2019-12-01T04:02:04Z (7 years ago)
From
Yuta Kawakubo at Louisiana State U./CALET <kawakubo1@lsu.edu>
N. Cannady (GSFC/UMBC), 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), 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 S191129u T0 = 2019-11-29 13:40:29.197 UT (The LIGO Scientific
Collaboration and Virgo Collaboration, GCN Circ. 26303).
No CGBM on-board trigger occurred around the event time. Based on the
LVC high probability localization region, the summed LIGO probabilities
inside the CGBM HXM (7 - 3000 keV) and SGM (40 keV - 28 MeV) fields
of view are 1 % and 27 %, respectively (and 68 % credible region of the
initial localization map was above the horizon). The HXM and SGM fields
of view were centered at RA = 356.9 deg, Dec = 60.7 deg and
RA = 356.7 deg, Dec = 50.7 deg at T0, respectively.
Based on the analysis of the light curve data with 0.125 sec time
resolution from T0-60 sec to T0+60 sec, we found no significant excess
(signal-to-noise ratio >= 7) around the trigger time in either the HXM or
the SGM data.
The CALET Calorimeter (CAL) was operating in the high energy trigger
mode at the trigger time of S191129u. Using the CAL data, we have
searched for gamma-ray events in the 10-100 GeV band from -60 sec
to +60 sec from the GW trigger time and found no candidates. There is
no significant overlap with the LVC high probability localization
region at T0+-60 sec. The CAL FOV was centered at RA=356.9 deg,
Dec=50.7 deg at T0.
GCN Circular 26317
Subject
LIGO/Virgo S191129u: Upper limits from Insight-HXMT/HE observations
Date
2019-11-30T13:45:12Z (7 years ago)
From
QiBin Yi at IHEP, HXMT <yiqb@ihep.ac.cn>
Q. B. Yi, S. Xiao, C. Cai, Q. Luo, C. K. Li,
X. B. Li, G. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang,
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin,
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song,
M. Wu, Y. P. Xu, S. N. Zhang (IHEP),
report on behalf of the Insight-HXMT team:
Insight-HXMT was taking data normally around the reported LIGO/Virgo
S191129u event (GCN #26303), trigger time 2019-11-29T13:40:29 UTC.
At T0, more than 59% of the LIGO localization region was covered by
Insight-HXMT without occultation by the Earth.
Within T0 +/- 100 s, no significant excess events (SNR > 3 sigma) are
found in a search of the Insight-HXMT/HE raw light curves.
Assuming the GW counterpart GRB with three typical GRB Band spectral
models, two typical duration timescales (1 s, 10 s) from the center
of the LIGO-Virgo location probability map (RA=315 deg, DEC=-60 deg),
the 5-sigma upper-limits fluence (0.2 - 5 MeV, incident energy) are
reported below:
Band model 1 (alpha=-1.9, beta=-3.7, Ep=70 keV):
1 s: 6.6e-08 erg cm^-2
10 s: 6.4e-07 erg cm^-2
Band model 2 (alpha=-1.0, beta=-2.3, Ep=230 keV):
1 s: 9.4e-08 erg cm^-2
10 s: 1.1e-06 erg cm^-2
Band model 3 (alpha=-0.0, beta=-1.5, Ep=1000 keV):
1 s: 2.0e-07 erg cm^-2
10 s: 3.1e-06 erg cm^-2
All measurements above are made with the CsI detectors operating in the
regular mode with the energy range of about 80-800 keV (deposited energy).
Only gamma-rays with energy greater than about 200 keV can penetrate
the spacecraft and leave signals in the CsI detectors installed inside
of the spacecraft.
Insight-HXMT is the first Chinese space X-ray telescope, which was
funded jointly by the China National Space Administration (CNSA) and
the Chinese Academy of Sciences (CAS).
More information could be found at: http://www.hxmt.org.
GCN Circular 26315
Subject
LIGO/Virgo S191129u: No counterpart candidates in Fermi-LAT observations
Date
2019-11-30T08:56:10Z (7 years ago)
From
Magnus Axelsson at Stockholm U. <magaxe@kth.se>
M. Crnogorcevic (Univ. of Maryland & NASA/GSFC), E. Bissaldi (Politecnico & INFN Bari), M. Axelsson (KTH & Stockholm Univ.), and F. Longo (University and INFN, Trieste), report on behalf of the Fermi-LAT Collaboration:
We have searched data collected by the Fermi Large Area Telescope (LAT) on Nov 29, 2019, for possible high-energy (E > 100 MeV) gamma-ray emission in spatial/temporal coincidence with the LIGO/Virgo trigger S191129u (GCN 26303).
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.
The Fermi Gamma-ray Space Telescope was passing through the South Atlantic Anomaly (SAA) at the time of the trigger (T0 = 2019-11-29 13:40:29.197 UTC). During SAA passages both the LAT and the Gamma-ray Burst Monitor (GBM) do not collect data due to the high charged particle background in this region. The LAT resumed taking data upon exiting the SAA at roughly T0 + 150 s. At that time the instantaneous coverage was ~25% of the LIGO probability map, and reached 100% cumulative coverage after ~6.2 ks.
We performed a search for a transient counterpart within the observed region of the 90% contour of LIGO map in a fixed time window from T0 to T0 + 10 ks. No significant new sources are found.
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 5.4e-11 and 2.0e-07 [erg/cm^2/s].
The Fermi-LAT point of contact for this event is Milena Crnogorcevic (mcrnogor@astro.umd.edu<mailto:mcrnogor@astro.umd.edu>).
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 26314
Subject
LIGO/Virgo S191129u: not observable by Fermi-GBM
Date
2019-11-29T20:24:15Z (7 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
At the time of S191129u, Fermi was passing through the South Atlantic Anomaly from 22.7 minutes prior to 1.2 minutes after the trigger time; therefore the GBM detectors were disabled.
GCN Circular 26313
Subject
LIGO/Virgo S191129u: Swift/BAT in SAA
Date
2019-11-29T18:43:01Z (7 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (NASA/GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
A. P. Beardmore (U. Leicester), M. G. Bernardini (INAF-OAB),
A. A. Breeveld (MSSL-UCL), D. N. Burrows (PSU),
S. Campana (INAF-OAB), S. B. Cenko (NASA/GSFC),
G. Cusumano (INAF-IASF PA), A. D'Ai (INAF-IASFPA),
P. D'Avanzo (INAF-OAB), V. D'Elia (ASI-ASDC), S. Emery (UCL-MSSL),
P. A. Evans (U. Leicester), P. Giommi (ASI), C. Gronwall (PSU),
D. Hartmann (Clemson U.), J. A. Kennea (PSU),
N. Klingler (PSU), H. A. Krimm (NSF),
N. P. M. Kuin (UCL-MSSL), F. E. Marshall (NASA/GSFC),
A. Melandri (INAF-OAB), J. A. Nousek (PSU),
S. R. Oates (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 S191129u (LIGO/VIRGO Collaboration GCN Circ. 26303),
where T0 is the LVC trigger time (2019-11-29T13:40:29.197 UTC).
The center of the BAT field of view (FOV) at T0 is
RA = 270.454 deg,
DEC = 18.713 deg,
and the roll angle is 210.645 deg.
The BAT FOV (>10% partial coding) covers 10.00% of the integrated
LVC localization probability, and 10.12% of the galaxy convolved
probability (Evans et al. 2016).
BAT was in SAA from T0-786 s to T0+352 s. Therefore, BAT data
analyses are unavailable around T0.
The results of the BAT analysis are available at
https://swift.gsfc.nasa.gov/results/BATbursts/team_web/S191129u/web/source_public.html
GCN Circular 26311
Subject
LIGO/Virgo S191129u: no INTEGRAL data available
Date
2019-11-29T18:04:55Z (7 years ago)
From
Enrico Bozzo at ISDC <Enrico.Bozzo@unige.ch>
Celia Sanchez-Fernandez, (ESAC-ESA, Spain), Enrico Bozzo (ISDC/UniGE,
Switzerland)
V. Savchenko, C. Ferrigno (ISDC/UniGE, Switzerland)
S. Mereghetti (INAF IASF-Milano, Italy)
A. Coleiro (APC, France)
on behalf of the INTEGRAL multi-messenger collaboration:
https://www.astro.unige.ch/cdci/integral-multimessenger-collaboration
Due to data reception issues at the ground stations, INTEGRAL data
around the time of LIGO/Virgo S191129u were lost (-300 s to 700 s) and
will not be recovered. No INTEGRAL coverage is thus available for
LIGO/Virgo S191129u.
GCN Circular 26310
Subject
LIGO/Virgo S191129u: No counterpart candidates in HAWC observations
Date
2019-11-29T16:06:54Z (7 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 S191129u (GCN #26303). At the time of the trigger the HAWC
local zenith was oriented towards (RA, Dec) = (175.7 deg, 19.1 deg).
37% of the GW candidate sky location probability fell within our
observable field of view (0-45 deg zenith angle).
We performed a search for a short timescale emission using 6 sliding
time windows (dt = 0.3s, 1s, 3s, 10s, 30s and 100s), shifted forward
in time by 20% of their width. We searched the 95% probability
containment area in a timescale-dependent time period, from t0-5dt to
t0+10dt, where t0 is the time of the GW trigger.
No significant gamma-ray detection above the background was observed.
The sensitivity of this analysis is greatly dependent on zenith angle,
ranging from 0 deg to 45 deg for the area searched in this
analysis. The 5sigma detection sensitivity to a 1s (100s) burst in the
80-800GeV energy range goes from 1.2e-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 26309
Subject
LIGO/Virgo S191129u: Coverage and upper limits from MAXI/GSC observations
Date
2019-11-29T15:54:49Z (7 years ago)
From
Motoko Serino at RIKEN/MAXI <motoko@crab.riken.jp>
M. Serino, S. Sugita (AGU),
N. Kawai (Tokyo Tech), H. Negoro (Nihon U.),
M. Nakajima, W. Maruyama, M. Aoki, K. Kobayashi, R. Takagi (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), M. Sugizaki (NAOC)
report on behalf of the MAXI team:
We examined MAXI/GSC all-sky X-ray images (2-20 keV)
after the LVC trigger S191129u at 2019-11-29 13:40:29.197 UTC (GCN 26303).
At the trigger time of S191129u, the high-voltage of MAXI/GSC was off,
and it was turned on at T0+446 sec (+7.4 min).
The first one-orbit (92 min) scan observation with GSC after the event covered 77%
of the 90% credible region of the bayestar skymap from 13:59:21 to 14:59:00 UTC (T0+1132 to T0+4711 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 26308
Subject
LIGO/Virgo S191129u: upper limits from AGILE/GRID observations
Date
2019-11-29T15:48:40Z (7 years ago)
From
Martina Cardillo at INAF-IAPS <martina.cardillo@inaf.it>
M. Cardillo (INAF/IAPS), C.Pittori (SSDC, and INAF/OAR), M. Tavani
(INAF/IAPS, and Univ. Roma Tor Vergata), C. Casentini, G. Piano, A.
Ursi (INAF/IAPS), F. Lucarelli, 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 S191129u at T0 = 2019-11-29 13:40:29
UTC a preliminary analysis of the AGILE exposure at T0 shows that the
Gamma-Ray
Imaging Detector (GRID) exposure covered less than 10% of the 90% c.l.
localization
region (LR) (36% 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 between T0 and T0+100s, where good exposure of the S191129u 90%
c.l. LR was available.
No candidate gamma-ray transient was detected.
The following preliminary GRID values of 3-sigma upper limit (UL) are
obtained:
from 3.4e-08 to 2.9e-06 erg cm^-2 s^-1, with exposure of about 46% of
the LR over
the time interval ( T0s ; T0 + 100s );
These measurements were obtained with AGILE observing a large portion of
the sky in spinning mode.
GCN Circular 26307
Subject
LIGO/Virgo S191129u : no neutrino counterpart candidate in ANTARES search
Date
2019-11-29T15:28:30Z (7 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 S191129u event using the 90% contour of the Initial bayestar probability
map provided by the GW interferometers (GCN#26303 <https://gcn.gsfc.nasa.gov/gcn3/26303.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/S191129u_Initial.png <http://antares.in2p3.fr/GW/S191129u_Initial.png>.
Considering the location probability provided by the LIGO/Virgo collaborations, there is a
51.6% 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 2019-11-29 13:40:29 and in the 90% contour of the S191129u
event. The expected number of atmospheric background events in the region visible by ANTARES is
4.78e-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 3.44e-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 26306
Subject
LIGO/Virgo S191129u: upper limits from AGILE/MCAL observations
Date
2019-11-29T15:14:45Z (7 years ago)
From
Martina Cardillo at INAF-IAPS <martina.cardillo@inaf.it>
M. Cardillo (INAF/IAPS), C.Pittori (SSDC, and INAF/OAR), M. Tavani
(INAF/IAPS, and Univ. Roma Tor Vergata), C. Casentini, G. Piano, A.
Ursi (INAF/IAPS), F. Lucarelli, 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 S191129u at T0 = 2019-11-29
13:40:29 (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 70% of the S191129u 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 S191129u localization region, from a minimum of
1.64E-06 erg cm^-2 to a maximum of 7.59E-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 26305
Subject
LIGO/Virgo S191129u: Upper limits from IceCube neutrino searches
Date
2019-11-29T14:43:21Z (7 years ago)
From
Alex Pizzuto at ICECUBE/U of Wisconsin <pizzuto@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 S191129u
in a time range of 1000 seconds [3] centered on the alert event time
(2019-11-29 13:32:09.197 UTC to 2019-11-29 13:48:49.197 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
S191129u calculated from the map circulated in the 2-Initial notice.
IceCube's sensitivity assuming an E^-2 spectrum (E^2 dN/dE) to neutrino
point sources within the locations spanned by the 90% spatial containment
of S191129u ranges from 0.029 to 1.080 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<mailto:roc@icecube.wisc.edu>
[1] Bartos et al. arXiv:1810.11467 (2018) and Countryman et al.arXiv:1901.05486 (2019)
[2] PoS(ICRC2019)918 and Braun et al., Astroparticle Physics 29, 299 (2008)
[3] Baret et al., Astroparticle Physics 35, 1 (2011)
GCN Circular 26304
Subject
LIGO/Virgo S191129u: Global MASTER-Net observations report
Date
2019-11-29T14:40:40Z (7 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-Amur robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the LIGO/Virgo S191129u errorbox 365 sec after notice time and 2972 sec after trigger time at 2019-11-29 14:30:01 UT, with upper limit up to 16.2 mag. The observations began at zenith distance = 77 deg. The sun altitude is -59.9 deg.
The galactic latitude b = -52 deg., longitude l = 349 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/ligo_1.php?id=10946
We obtain a following upper limits.
Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________
3063 | 2019-11-29 14:30:01 | MASTER-Amur | (14h 36m 58.69s , +52d 00m 33.5s) | C | 180 | 16.2 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
GCN Circular 26303
Subject
LIGO/Virgo S191129u: Identification of a GW compact binary merger candidate
Date
2019-11-29T14:38:28Z (7 years ago)
From
Leo Singer at GSFC <leo.p.singer@nasa.gov>
The LIGO Scientific Collaboration and the Virgo Collaboration report:
We identified the compact binary merger candidate S191129u during
real-time processing of data from LIGO Hanford Observatory (H1) and
LIGO Livingston Observatory (L1) at 2019-11-29 13:40:29.197 UTC (GPS
time: 1259070047.197). The candidate was found by the GstLAL [1],
MBTAOnline [2], SPIIR [3], and PyCBC Live [4] analysis pipelines.
S191129u is an event of interest because its false alarm rate, as
estimated by the online analysis, is 2.7e-35 Hz, or about one in 1e27
years. The event's properties can be found at this URL:
https://gracedb.ligo.org/superevents/S191129u
The classification of the GW signal, in order of descending
probability, is BBH (99%), Terrestrial (1%), BNS (<1%), MassGap (<1%),
or NSBH (<1%).
Assuming the candidate is astrophysical in origin, the probability
that the lighter compact object has a mass < 3 solar masses (HasNS) is
<1%. Using the masses and spins inferred from the signal, the
probability of matter outside the final compact object (HasRemnant) is
<1%.
One sky map is available at this time and can be retrieved from the
GraceDB event page:
* bayestar.fits.gz,0, an initial localization generated by BAYESTAR
[5], distributed via GCN notice about 42 minutes after the candidate
event time.
For the bayestar.fits.gz,0 sky map, the 90% credible region is 1011
deg2. Marginalized over the whole sky, the a posteriori luminosity
distance estimate is 763 +/- 200 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] Adams et al. CQG 33, 175012 (2016)
[3] Qi Chu, PhD Thesis, The University of Western Australia (2017)
[4] Nitz et al. PRD 98, 024050 (2018)
[5] Singer & Price PRD 93, 024013 (2016)