LIGO/Virgo S191105e
GCN Circular 26181
Subject
LIGO/Virgo S191105e: Upper limits from IceCube neutrino searches
Date
2019-11-06T18:24:03Z (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
S191105e
in a time range of 1000 seconds [3] centered on the alert event time
(2019-11-05 14:27:01.933 UTC to 2019-11-05 14:43:41.933 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
S191105e 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 S191105e ranges from 0.029 to 0.694 GeV cm^-2 in a 1000 second
time window.
The IceCube Neutrino Observatory is a cubic-kilometer neutrino detector
operating at the geographic South Pole, Antarctica. The IceCube realtime
alert point of contact can be reached at roc@icecube.wisc.edu
[1] Bartos et al. arXiv:1810.11467 (2018) and Countryman et
al.arXiv:1901.05486 (2019)
[2] Braun et al., Astroparticle Physics 29, 299 (2008)
[3] Baret et al., Astroparticle Physics 35, 1 (2011)
GCN Circular 26182
Subject
LIGO/Virgo S191105e: Identification of a GW compact binary merger candidate
Date
2019-11-06T18:24:36Z (6 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 S191105e during
real-time processing of data from LIGO Hanford Observatory (H1), LIGO
Livingston Observatory (L1), and Virgo Observatory (V1) at 2019-11-05
14:35:21.933 UTC (GPS time: 1256999739.933). The candidate was found
by the PyCBC Live [1], SPIIR [2], and GstLAL [3] analysis pipelines.
The preliminary alert was delayed by approximately one day due to a
GraceDB authentication issue.
S191105e is an event of interest because its false alarm rate, as
estimated by the online analysis, is 2.3e-08 Hz, or about one in 1
year, 4 months. The event's properties can be found at this URL:
https://gracedb.ligo.org/superevents/S191105e
The classification of the GW signal, in order of descending
probability, is BBH (95%), Terrestrial (5%), BNS (<1%), NSBH (<1%), or
MassGap (<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%).
Two sky maps are available at this time and can be retrieved from the
GraceDB event page:
* "bayestar.fits.gz,0", a preliminary localization generated by
BAYESTAR [4] for an earlier trigger, not the current preferred
event, and
* "bayestar.fits.gz,1", an initial localization generated by BAYESTAR [4].
For the bayestar.fits.gz,1 sky map, the 90% credible region is 1297
deg2. Marginalized over the whole sky, the a posteriori luminosity
distance estimate is 1168 +/- 330 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] Nitz et al. PRD 98, 024050 (2018)
[2] Qi Chu, PhD Thesis, The University of Western Australia (2017)
[3] Messick et al. PRD 95, 042001 (2017)
[4] Singer & Price PRD 93, 024013 (2016)
GCN Circular 26183
Subject
LIGO/Virgo S191105e: upper limits from AGILE/MCAL observations
Date
2019-11-06T18:47:33Z (6 years ago)
From
Alessandro Ursi at INAF/IAPS <alessandro.ursi@gmail.com>
A. Ursi, C. Casentini (INAF/IAPS), M. Tavani (INAF/IAPS, and Univ. Roma Tor
Vergata), M. Cardillo, G. Piano (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 S191105e at T0 = 2019-11-05 14:35:21
(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 50% of the S191105e 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 S191105e localization region, from a minimum of 1.55E-06 erg
cm^-2 to a maximum of 7.19E-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 26184
Subject
LIGO/Virgo S191105e: Global MASTER-Net observations report
Date
2019-11-06T18:50:55Z (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-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 S191105e errorbox 55 sec
after trigger time at 2019-11-05 14:36:16 UT, with upper limit up to 18.5
mag. The observations began at zenith distance = 49 deg. The sun altitude
is -54.8 deg.
MASTER-Kislovodsk robotic telescope located in Russia (Lomonosov MSU,
Kislovodsk Solar Station of Pulkovo observatory) started inspect of the
LIGO/Virgo S191105e errorbox 12600 sec after trigger time at 2019-11-05
18:05:21 UT, with upper limit up to 19.4 mag. The observations began at
zenith distance = 54 deg. The sun altitude is -44.8 deg.
MASTER-IAC robotic telescope located in Spain (IAC Teide Observatory)
started inspect of the LIGO/Virgo S191105e errorbox 41784 sec after
trigger time at 2019-11-06 02:11:45 UT, with upper limit up to 21.1 mag.
The observations began at zenith distance = 58 deg. The sun altitude is
-66.8 deg.
MASTER-SAAO robotic telescope located in South Africa (South African
Astronomical Observatory) started inspect of the LIGO/Virgo S191105e
errorbox 16 sec after notice time and 1 days 12494 sec after trigger time
at 2019-11-06 18:03:35 UT, with upper limit up to 17.1 mag. Observations
started at twilight. The observations began at zenith distance = 30 deg.
The sun altitude is -11.7 deg.
MASTER-Tavrida robotic telescope located in Russia (Lomonosov MSU, SAI
Crimea astronomical station) started inspect of the LIGO/Virgo S191105e
errorbox 29 sec after notice time and 1 days 12507 sec after trigger time
at 2019-11-06 18:03:48 UT, with upper limit up to 14.7 mag. The
observations began at zenith distance = 83 deg. The sun altitude is
-39.0 deg.
The galactic latitude b = -77 deg., longitude l = 296 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/ligo_1.php?id=10882
The observation and reduction will continue.
The message may be cited.
GCN Circular 26185
Subject
LIGO/Virgo S191105e: Upper limits from Fermi-GBM Observations
Date
2019-11-06T18:57:48Z (6 years ago)
From
Adam Goldstein at Fermi-GBM, USRA <adam.michael.goldstein@gmail.com>
A. Goldstein (USRA) reports on behalf of the Fermi-GBM Team and the
GBM-LIGO/Virgo group
For S191105e and using the initial BAYESTAR skymap, Fermi-GBM was observing
77.5% of the localization probability at event time.
There was no Fermi-GBM onboard trigger around the event time of S191105e
(GCN Circ. 26182). 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=315.6, Dec=21.5 with a radius of 67.5 degrees. We therefore set upper
limits on impulsive gamma-ray emission for the LVC localization region
visible to GBM 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: 4.1 6.9 14.
1.024 s: 1.3 2.1 4.7
8.192 s: 0.3 0.6 1.6
Assuming the median luminosity distance of 1168 Mpc from the GW detection,
we estimate the following intrinsic luminosity upper limits over the 1
keV-10 MeV energy range (in units of 10^49 erg/s):
Timescale soft norm hard
--------------------------------------
0.128 s: 10. 16. 53.
1.024 s: 3.3 4.8 18.
8.192 s: 0.8 1.4 6.1
GCN Circular 26186
Subject
LIGO/Virgo S191105e: upper limits from AGILE/GRID observations
Date
2019-11-06T19:04:08Z (6 years ago)
From
Claudio Casentini at INAF-IAPS <claudio.casentini@inaf.it>
C. Casentini, A. Ursi (INAF/IAPS), M. Tavani (INAF/IAPS, and Univ. Roma Tor
Vergata), M. Cardillo, G. Piano (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 S191105e at T0 = 2019-11-05
14:35:21.933 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) (30% of 90% c.l. LR is occulted by
Earth).
We performed an analysis of the GRID data in the energy range 50 MeV - 10
GeV on T0, where good exposure of the S191105e 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 1.44e-06 to 9.71e-06 erg cm^-2 s^-1, with exposure of about 11% of the
LR over the time interval ( T0s ; T0 + 5s );
from 6.45e-07 to 9.88e-06 erg cm^-2 s^-1, with exposure of about 16% of the
LR over the time interval ( T0s ; T0 + 10s );
from 3.65e-08 to 2.73e-06 erg cm^-2 s^-1, with exposure of about 52% 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. Additional analysis of AGILE data is in
progress.
GCN Circular 26187
Subject
LIGO/Virgo S191105e: No counterpart candidates in INTEGRAL SPI-ACS and,IBIS prompt observation
Date
2019-11-06T19:04:23Z (6 years ago)
From
Carlo Ferrigno at IAAT/ISDC <carlo.Ferrigno@unige.ch>
C. Ferrigno, V. Savchenko (ISDC/UniGE, Switzerland)
Sergey Molkov (IKI, Russia)
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 a combination of the INTEGRAL all-sky detectors:
SPI/ACS, IBIS/Veto, and IBIS (following [1]) we have performed a search
for a prompt
gamma-ray counterpart of S191105e (GCN 26182).
At the time of the event (2019-11-05 14:35:21 UTC, hereafter T0),
INTEGRAL was operating in nominal mode. The peak of the event
localization probability was at an angle of 93 deg with respect to the
spacecraft pointing axis. This orientation implies strongly suppressed
(9.1% of optimal) response of ISGRI, strongly suppressed (27% of
optimal) response of IBIS/Veto, and near-optimal (79% of optimal)
response of SPI-ACS.
The background within +/-300 seconds around the event was rather
stable (excess variance 1.2).
We have performed a search for any impulsive events in INTEGRAL SPI-
ACS (as described in [2]), IBIS, and IBIS/Veto data.
We do not detect any significant counterparts and estimate a 3-sigma
upper limit on the 75-2000 keV fluence of 2.3e-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 ~2e-07 (5.2e-08)
erg/cm^2/s at 1 s (8 s) time scale in 75-2000 keV energy range.
For the mean reported distance 1168 Mpc this corresponds to the
limit on the total isotropic equivalent energy in 1 s of 3.7e+49 erg
for the short GRB spectrum and for a long GRB spectrum isotropic
equivalent luminosity in 1 s (8 s) of 2.7e+49 erg/s (8.5e+48 erg/s)
We find: 4 likely background
excesses that we report for completeness and in order of FAP
in the search region of SPI-ACS data.
scale | T | S/N | luminosity ( x 1e+49 erg/s) | FAP
13.8 | 167 | 3.4 | 12.2 +/- 5 +/- 7.36 | 0.113
0.15 | -2.86 | 3.1 | 12.2 +/- 4.85 +/- 7.37 | 0.358
2.55 | -295 | 3.6 | 3.32 +/- 1.17 +/- 2 | 0.701
0.5 | -168 | 4.3 | 9.36 +/- 2.65 +/- 5.66 | 0.797
Note that FAP estimates (especially at timescales above 2s) may be
possibly further affected by enhanced non-stationary local background
noise. This list excludes any excesses for which FAP is close to
unity.
All results quoted are preliminary.
This circular is an official product of the INTEGRAL Multi-Messenger
team.
[1] Savchenko et al. 2017, A&A 603, A46
[2] Savchenko et al. 2012, A&A 541A, 122S
GCN Circular 26188
Subject
LIGO/Virgo S191105e: No counterpart candidates in HAWC observations
Date
2019-11-06T19:25:34Z (6 years ago)
From
Israel Martinez-Castellanos at UMD/HAWC <imc@umd.edu>
The HAWC Collaboration (https://www.hawc-observatory.org) reports:
The HAWC Collaboration performed a follow-up of the gravitational wave
trigger S191105e (GCN #26182). At the time of the trigger the HAWC
local zenith was oriented towards (RA, Dec) = (165.8deg, 19.1 deg).
24% 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 28 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 4.1e-6 erg/cm^2 to 1.1e-4 erg/cm^2
(2.5e-5 erg/cm^2 to 5.5e-4 erg/cm^2), depending on the zenith
angle.
HAWC is a TeV gamma ray water Cherenkov array located in the state of
Puebla, Mexico. It is sensitive to the energy range ~0.1-100TeV, and
monitors 2/3 of the sky every day with an instantaneous field-of-view
of ~2 sr.
GCN Circular 26189
Subject
LIGO/Virgo S191105e : no neutrino counterpart candidate in ANTARES search
Date
2019-11-06T20:26:21Z (6 years ago)
From
Antoine Kouchner at ANTARES Collaboration <kouchner@apc.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 S191105e event using the 90% contour of the Initial bayestar probability
map provided by the GW interferometers (GCN#26182 <https://gcn.gsfc.nasa.gov/gcn3/26182.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/S191105e_Initial.png <http://antares.in2p3.fr/GW/S191105e_Initial.png>.
Considering the location probability provided by the LIGO/Virgo collaborations, there is a
66.4% 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 2019-11-05 14:35:21 and in the 90% contour of the S191105e
event. The expected number of atmospheric background events in the region visible by ANTARES is
5.16e-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 3.72e-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 26192
Subject
LIGO/Virgo S191105e: no counterpart candidates in the Swift/BAT observations
Date
2019-11-07T01:15:59Z (6 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
D. M. Palmer (LANL), S. D. Barthelmy (NASA/GSFC),
A. Y. Lien (GSFC/UMBC), 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 S191105e (LIGO/VIRGO Collaboration GCN Circ. 26182),
where T0 is the LVC trigger time (2019-11-05T14:35:21.933 UTC).
The center of the BAT field of view (FOV) at T0 is
RA = 317.289 deg,
DEC = 48.187 deg,
and the roll angle is 258.590 deg.
The BAT FOV (>10% partial coding) covers 11.73% of the integrated
LVC localization probability, and 12.37% 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 ~ 8.37 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 ~ 78.55 Mpc.
No event data are available within T0 +/- 100 s.
BAT retains decreased, but significant, sensitivity to rate increases for
gamma-ray events outside of its FOV. About 66.72% 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/S191105e/web/source_public.html
GCN Circular 26193
Subject
LIGO/Virgo S191105e: Coverage and upper limits from MAXI/GSC observations
Date
2019-11-07T04:31:53Z (6 years ago)
From
Hitoshi Negoro at Nihon U <negoro.hitoshi@nihon-u.ac.jp>
H. Negoro (Nihon U.), N. Kawai (Tokyo Tech), 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), 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 S191105e at 2019-11-05 14:35:21.933 UTC (GCN 26182).
At the trigger time of S191105e, the high-voltage of MAXI/GSC was off,
and it was turned on at T0+1729 sec (+28.8 min).
The first one-orbit (92 min) scan observation with GSC after the event covered 72%
of the 90% credible region of the bayestar skymap from 15:04:11 to 15:20:01 UTC (T0+1730 to T0+2680 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 26194
Subject
LIGO/Virgo S191105e: No counterpart candidates in Fermi-LAT observations
Date
2019-11-07T06:17:36Z (6 years ago)
From
Magnus Axelsson at Stockholm U. <magaxe@kth.se>
M. Axelsson (KTH and Stockholm Univ.), N. Omodei (Stanford Univ.), D. Kocevski (NASA/MSFC), F. Longo (Univ. and INFN Trieste), E. Bissaldi (Politecnico and INFN Bari) and M. Moss (GWU) report on behalf of the Fermi-LAT Collaboration:
We have searched data collected by the Fermi Large Area Telescope (LAT) on Nov 05, 2019, for possible high-energy (E > 100 MeV) gamma-ray emission in spatial/temporal coincidence with the LIGO/Virgo trigger S191105e (GCN 26182).
We define "instantaneous coverage" as the integral over the region of the LIGO probability map that is within the LAT field of view at a given time, and "cumulative coverage" as the integral of the instantaneous coverage over time. Fermi-LAT had an instantaneous coverage of ~20% of the LIGO probability region at the time of the trigger (T0 = 2019-11-05 14:35:21.933 UTC) and reached ~100% cumulative coverage at approximately T0 + 3 ks.
We performed a search for a transient counterpart within the observed region of the 90% contour of the LIGO map in a fixed time window from T0 to T0 + 10 ks. One significant excess (with TS>25) was found at R.A., Dec. = 342.2, -12.9, but it is likely associated with the known source RBS 1899 (lies within the 90% uncertainty region).
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 between 100 MeV and 1 GeV for the fixed time interval of this search vary between 1.4e-10 and 1.3e-9 [erg/cm^2/s].
The Fermi-LAT point of contact for this event is Michael Moss (michaelmoss@gwmail.gwu.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 26195
Subject
LIGO/Virgo S191105e: Not observable by CALET
Date
2019-11-07T06:27:32Z (6 years ago)
From
Yuta Kawakubo at Louisiana State U./CALET <kawakubo1@lsu.edu>
S. Nakahira (RIKEN), A. Yoshida, T. Sakamoto, V. Pal'shin,
S. Sugita (AGU), Y. Kawakubo (LSU), K. Yamaoka (Nagoya U),
Y. Asaoka, S. Torii (Waseda U), Y. Shimizu,
T. Tamura (Kanagawa U), N. Cannady (GSFC/UMBC),
M. L. Cherry (LSU), S. Ricciarini (U of Florence),
P. S. Marrocchesi (U of Siena),
and the CALET collaboration:
At the trigger time of the compact binary merger candidate S191105e,
T0 = 2019-11-05 14:35:21.933 UT (The LIGO Scientific Collaboration
and Virgo Collaboration, GCN Circ. 26182), the CALET Gamma-ray
Burst Monitor (CGBM) high voltages were off (from T0-6 min to
T0+27 min).
The CALET Calorimeter (CAL) was operating in the high energy trigger
mode at the trigger time of S191105e. 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. The CAL FOV was centered at RA=223.0 deg, Dec=-27.4 deg
at T0.
GCN Circular 26196
Subject
LIGO/Virgo S191105e: AstroSat CZTI upper limits
Date
2019-11-07T07:34:18Z (6 years ago)
From
Varun Bhalerao at Indian Inst of Tech <varunb@iitb.ac.in>
V. Shenoy (IITB), A. Anumarlapudi (IUCAA), R. Gaikwad (IUCAA), S. Gupta (IUCAA), 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-second window around the trigger time of the BBH merger event S191105e (UTC 2019-11-05 14:35:21.000, 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, DEC = 9:50:13.4, 31:28:40.3 (147.5558,31.4779), which is 142 deg away from the maximum probability location. At the time of merger event, the Earth-satellite-transient angle corresponding to maximum probability location is ~ 44.14 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 0.36 (36%).
CZTI data were de-trended to remove orbit-wise background variation. We then searched data from the four independent, identical quadrants to look for coincident spikes in the count rates. Searches were undertaken by binning the data in 0.1s, 1s, and 10s respectively. Statistical fluctuations in background count rates were estimated by using data from 10 (+-5) neighbouring orbits. We selected confidence levels such that the probability of a false trigger in a 1000 sec window is 10^-4. We do not find any evidence for any hard X-ray transient in this window, in the CZTI energy range of 20-200 keV.
We use a detailed mass model of the satellite to calculate the direction-dependent instrument response for points in the visible sky. We then assume the source is modelled as a power law with photon index alpha = -1, and convert our count rate upper limits to direction-dependent flux limits. We obtain the following upper limits for source flux in the 20-200 keV band by taking a probability weighted mean over the visible sky:
0.1 s: flux limit= 6.34e-06 ergs/cm^2/s; fluence limit = 6.34e-07 ergs/cm^2
1.0 s: flux limit= 1.96e-06 ergs/cm^2/s; fluence limit = 1.96e-06 ergs/cm^2
10.0 s: flux limit= 2.36e-07 ergs/cm^2/s; fluence limit = 2.36e-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 26213
Subject
LIGO/Virgo S191105e: Upper limits from Insight-HXMT/HE observations
Date
2019-11-10T06:10:33Z (6 years ago)
From
Ce Cai at IHEP <caice@ihep.ac.cn>
C. Cai, Y. G. Zheng, Q. Luo, S. Xiao, Q. B. Yi,
Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang,
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin,
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song,
M. Wu, Y. P. Xu, S. N. Zhang (IHEP),
report on behalf of the Insight-HXMT team:
Insight-HXMT was taking data normally around the reported LIGO/Virgo
S191105e event (GCN #26182), trigger time 2019-11-05T14:35:21.933 UTC.
At T0, about 78% of the LIGO localization region was covered by the
Insight-HXMT without occultationby 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=14 deg, DEC=-40 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: 2.9e-07 erg cm^-2
10 s: 1.4e-06 erg cm^-2
Band model 2 (alpha=-1.0, beta=-2.3, Ep=230 keV):
1 s: 3.6e-07 erg cm^-2
10 s: 2.0e-06 erg cm^-2
Band model 3 (alpha=-0.0, beta=-1.5, Ep=1000 keV):
1 s: 4.3e-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 26215
Subject
LIGO/Virgo S191105e: No significant candidates in FRAM-TAROT-GRANDMA observations
Date
2019-11-10T15:31:14Z (6 years ago)
From
Kateryna Barynova at Kiev Uni., GRANDMA <katiaffoni@gmail.com>
K. Barynova (Kyiv Uni), P.A. Duverne (LAL), B. Gendre (OzGrav-UWA), N.
Kochiashvili (Iliauni), S. Karpov, M. Masek, M. Prouza (FZU),
M. Boer (Artemis), N. Christensen (Artemis), L. Eymar (Artemis),
A. Klotz (IRAP), K. Noysena (Artemis, IRAP), S. Antier (APC),
A. Coleiro (APC), D. Corre (LAL), M. Coughlin (Caltech),
D. A. Kann (HETH/IAA-CSIC), D.Coward (OzGrav-UWA), J.G. Ducoin (LAL),
P. Hello (LAL), C. Lachaud (APC), N. Leroy (LAL),
C. C. Thoene (HETH/IAA-CSIC), D. Turpin (NAOC), X. Wang (THU)
report on behalf of the FRAM network, TAROT network
and GRANDMA collaborations:
We performed tiled observations of the LIGO/Virgo S191105e event with
the FRAM-Auger (FRAM-A), FRAM-CTA-N (FRAM-C), TAROT-Reunion (TRE),
TAROT-Calern (TCA) and TAROT-Chili (TCH) telescopes operating
in the r-band and visible located respectively at
Pierre Auger observatory (Malargue, Argentina), Roque de los Muchachos
observatory (La Palma, Spain), Les Makes astronomical
observatory, the Cote d'Azur observatory and La Silla ESO
observatory (LaS/ESO).
The observation started on 11/08/19 00:10:14 UTC for FRAM-Auger which
corresponds approximately to 3456 minutes after the GW trigger time.
The observation started on 11/08/19 01:17:32 UTC for FRAM-CTA-N which
corresponds approximately to 3523 minutes after the GW trigger time.
The observation started on 11/07/19 15:32:23 UTC for TRE which
corresponds approximately to 2938 minutes after the GW trigger time.
For TCA it started on 11/07/19 22:37:51 UTC which corresponds
approximately to 3363 minutes after the GW trigger time.
For TCH it started on 11/07/19 23:55:24 UTC which corresponds
approximately to 3441 minutes after the GW trigger time.
We performed the following joint tiled observations [1]:
+-------+------------+------------+---------+---------+---------+
| Tele | TStart | TEnd | RA | DEC | Proba |
| scope | [UTC] | [UTC] | [deg] | [deg] | [%] |
|-------+------------+------------+---------+---------+---------|
|FRAM-A | 2019-11-08 | 2019-11-08 | 24.26 | -40.38 | 0.3 |
| | 00:10:14 | 00:14:14 | | | |
|FRAM-A | 2019-11-08 | 2019-11-08 | 24.61 | -41.35 | 0.3 |
| | 00:15:17 | 00:19:17 | | | |
|FRAM-A | 2019-11-08 | 2019-11-08 | 39.37 | -46.22 | 0.2 |
| | 00:20:21 | 00:24:21 | | | |
|FRAM-A | 2019-11-08 | 2019-11-08 | 38.56 | -47.19 | 0.2 |
| | 00:25:23 | 00:29:23 | | | |
|FRAM-A | 2019-11-08 | 2019-11-08 | 24.97 | -42.33 | 0.2 |
| | 00:30:28 | 00:34:28 | | | |
|FRAM-A | 2019-11-08 | 2019-11-08 | 25.54 | -40.38 | 0.2 |
| | 00:35:30 | 00:39:30 | | | |
|FRAM-A | 2019-11-08 | 2019-11-08 | 39.99 | -47.19 | 0.2 |
| | 00:40:36 | 00:44:36 | | | |
|FRAM-A | 2019-11-08 | 2019-11-08 | 37.97 | -46.22 | 0.2 |
| | 00:45:37 | 00:49:37 | | | |
|FRAM-A | 2019-11-08 | 2019-11-08 | 25.91 | -41.35 | 0.2 |
| | 00:50:42 | 00:54:42 | | | |
|FRAM-A | 2019-11-08 | 2019-11-08 | 40.00 | -45.24 | 0.2 |
| | 00:55:46 | 00:59:46 | | | |
|FRAM-A | 2019-11-08 | 2019-11-08 | 39.35 | -48.16 | 0.2 |
| | 01:00:49 | 01:04:49 | | | |
|FRAM-A | 2019-11-08 | 2019-11-08 | 38.62 | -45.24 | 0.1 |
| | 01:05:51 | 01:09:51 | | | |
|FRAM-A | 2019-11-08 | 2019-11-08 | 37.89 | -48.16 | 0.2 |
| | 01:10:54 | 01:14:54 | | | |
|FRAM-A | 2019-11-08 | 2019-11-08 | 37.14 | -47.19 | 0.1 |
| | 01:15:55 | 01:18:55 | | | |
|FRAM-A | 2019-11-08 | 2019-11-08 | 40.78 | -46.22 | 0.1 |
| | 01:20:58 | 01:24:58 | | | |
|FRAM-A | 2019-11-08 | 2019-11-08 | 26.82 | -40.38 | 0.1 |
| | 01:26:03 | 01:30:03 | | | |
|FRAM-A | 2019-11-08 | 2019-11-08 | 26.29 | -42.33 | 0.1 |
| | 01:31:05 | 01:35:05 | | | |
|FRAM-A | 2019-11-08 | 2019-11-08 | 27.20 | -41.35 | 0.1 |
| | 01:36:06 | 01:40:06 | | | |
|FRAM-A | 2019-11-08 | 2019-11-08 | 38.68 | -49.13 | 0.1 |
| | 01:41:11 | 01:45:11 | | | |
|FRAM-A | 2019-11-08 | 2019-11-08 | 37.24 | -45.24 | 0.1 |
| | 01:46:14 | 01:50:14 | | | |
|-------+------------+------------+---------+---------+---------|
|FRAM-C | 2019-11-08 | 2019-11-08 | 193.18 | 77.00 | 0.06 |
| | 01:17:32 | 01:21:32 | | | |
|FRAM-C | 2019-11-08 | 2019-11-08 | 192.59 | 77.44 | 0.06 |
| | 01:21:52 | 01:25:52 | | | |
|FRAM-C | 2019-11-08 | 2019-11-08 | 190.95 | 76.57 | 0.06 |
| | 01:26:11 | 01:30:11 | | | |
|FRAM-C | 2019-11-08 | 2019-11-08 | 191.49 | 78.32 | 0.07 |
| | 01:30:31 | 01:34:31 | | | |
|FRAM-C | 2019-11-08 | 2019-11-08 | 193.62 | 78.32 | 0.07 |
| | 01:34:52 | 01:38:52 | | | |
|FRAM-C | 2019-11-08 | 2019-11-08 | 190.65 | 77.45 | 0.06 |
| | 01:39:21 | 01:43:21 | | | |
|FRAM-C | 2019-11-08 | 2019-11-08 | 196.54 | 76.57 | 0.06 |
| | 01:43:43 | 01:47:43 | | | |
|FRAM-C | 2019-11-08 | 2019-11-08 | 191.14 | 77.89 | 0.06 |
| | 01:48:05 | 01:52:05 | | | |
|FRAM-C | 2019-11-08 | 2019-11-08 | 195.25 | 77.89 | 0.06 |
| | 01:52:28 | 01:56:28 | | | |
|FRAM-C | 2019-11-08 | 2019-11-08 | 196.63 | 77.45 | 0.06 |
| | 01:56:49 | 02:00:49 | | | |
|FRAM-C | 2019-11-08 | 2019-11-08 | 196.65 | 77.01 | 0.06 |
| | 02:01:08 | 02:05:08 | | | |
|FRAM-C | 2019-11-08 | 2019-11-08 | 192.88 | 76.59 | 0.07 |
| | 02:05:27 | 02:09:27 | | | |
|FRAM-C | 2019-11-08 | 2019-11-08 | 194.80 | 77.46 | 0.06 |
| | 02:09:49 | 02:13:49 | | | |
|FRAM-C | 2019-11-08 | 2019-11-08 | 194.75 | 76.57 | 0.06 |
| | 02:14:09 | 02:18:09 | | | |
|FRAM-C | 2019-11-08 | 2019-11-08 | 193.15 | 77.90 | 0.06 |
| | 02:18:28 | 02:22:28 | | | |
|FRAM-C | 2019-11-08 | 2019-11-08 | 194.77 | 76.59 | 0.06 |
| | 02:22:49 | 02:26:49 | | | |
|FRAM-C | 2019-11-08 | 2019-11-08 | 196.14 | 76.15 | 0.05 |
| | 02:27:09 | 02:31:09 | | | |
|FRAM-C | 2019-11-08 | 2019-11-08 | 189.08 | 77.91 | 0.05 |
| | 02:31:32 | 02:35:32 | | | |
|FRAM-C | 2019-11-08 | 2019-11-08 | 197.41 | 77.90 | 0.05 |
| | 02:35:54 | 02:39:54 | | | |
|FRAM-C | 2019-11-08 | 2019-11-08 | 192.57 | 76.17 | 0.05 |
| | 02:40:16 | 02:44:16 | | | |
|-------+------------+------------+---------+---------+---------|
| TRE | 2019-11-07 | 2019-11-08 | 16.364 | -40.909 | 4.7 |
| | 15:32:23 | 00:09:41 | | | |
| TRE | 2019-11-07 | 2019-11-07 | 10.909 | -40.909 | 4.6 |
| | 15:45:35 | 15:51:58 | | | |
| TRE | 2019-11-07 | 2019-11-08 | 15.429 | -36.818 | 2.2 |
| | 16:04:21 | 15:35:02 | | | |
| TRE | 2019-11-07 | 2019-11-08 | 40.645 | -45 | 1.6 |
| | 16:17:31 | 15:48:13 | | | |
| TRE | 2019-11-07 | 2019-11-07 | 37.895 | -49.091 | 1.4 |
| | 16:29:49 | 22:59:13 | | | |
| TRE | 2019-11-07 | 2019-11-08 | 20.571 | -36.818 | 1 |
| | 16:42:55 | 16:13:20 | | | |
| TRE | 2019-11-07 | 2019-11-07 | 0 | -32.727 | 0.9 |
| | 17:01:43 | 17:08:04 | | | |
| TRE | 2019-11-07 | 2019-11-07 | 23.226 | -45 | 0.7 |
| | 17:36:11 | 21:55:55 | | | |
| TRE | 2019-11-07 | 2019-11-07 | 10.286 | -36.818 | 4.6 |
| | 17:47:07 | 22:08:03 | | | |
| TRE | 2019-11-07 | 2019-11-07 | 5.143 | -36.818 | 4.6 |
| | 17:59:14 | 22:21:23 | | | |
| TRE | 2019-11-07 | 2019-11-07 | 5.455 | -40.909 | 0.9 |
| | 19:16:01 | 23:37:25 | | | |
| TRE | 2019-11-07 | 2019-11-07 | 126 | 24.545 | 0.7 |
| | 21:36:12 | 23:50:51 | | | |
| TRE | 2019-11-07 | 2019-11-07 | 127.317 | 20.455 | 0.9 |
| | 23:18:23 | 23:24:40 | | | |
| TRE | 2019-11-08 | 2019-11-08 | 21.818 | -40.909 | 4.4 |
| | 00:28:34 | 00:34:51 | | | |
|-------+------------+------------+---------+---------+---------|
| TCA | 2019-11-07 | 2019-11-08 | 139.638 | 51.981 | 0.5 |
| | 22:37:51 | 05:11:02 | | | |
| TCA | 2019-11-07 | 2019-11-08 | 188.15 | 76.105 | 0.5 |
| | 22:42:30 | 05:17:48 | | | |
| TCA | 2019-11-08 | 2019-11-08 | 142.379 | 55.692 | 0.4 |
| | 03:46:58 | 03:48:58 | | | |
| TCA | 2019-11-08 | 2019-11-08 | 193.508 | 77.96 | 0.8 |
| | 04:32:02 | 05:24:21 | | | |
| TCA | 2019-11-08 | 2019-11-08 | 195.35 | 76.105 | 0.7 |
| | 04:38:48 | 04:45:07 | | | |
| TCA | 2019-11-08 | 2019-11-08 | 142.488 | 53.837 | 0.6 |
| | 04:45:34 | 04:51:54 | | | |
| TCA | 2019-11-08 | 2019-11-08 | 139.848 | 50.125 | 0.5 |
| | 04:57:54 | 05:04:14 | | | |
|-------+------------+------------+---------+---------+---------|
| TCH | 2019-11-07 | 2019-11-08 | 5.287 | -32.686 | 0.8 |
| | 23:55:24 | 06:29:05 | | | |
| TCH | 2019-11-08 | 2019-11-08 | 7.456 | -32.686 | 0.7 |
| | 00:02:10 | 00:06:19 | | | |
| TCH | 2019-11-08 | 2019-11-08 | 9.625 | -33.636 | 0.3 |
| | 00:06:45 | 06:41:37 | | | |
| TCH | 2019-11-08 | 2019-11-08 | 15.255 | -39.959 | 1.5 |
| | 00:25:59 | 07:01:42 | | | |
| TCH | 2019-11-08 | 2019-11-08 | 15.308 | -40.041 | 1.5 |
| | 00:32:40 | 07:08:13 | | | |
| TCH | 2019-11-08 | 2019-11-08 | 12.563 | -38.141 | 1.4 |
| | 00:45:07 | 07:20:39 | | | |
| TCH | 2019-11-08 | 2019-11-08 | 10.24 | -38.141 | 1.4 |
| | 00:51:51 | 07:27:11 | | | |
| TCH | 2019-11-08 | 2019-11-08 | 10.371 | -38.223 | 1.4 |
| | 00:58:35 | 07:34:07 | | | |
| TCH | 2019-11-08 | 2019-11-08 | 5.394 | -34.505 | 1.4 |
| | 01:05:19 | 01:11:37 | | | |
| TCH | 2019-11-08 | 2019-11-08 | 10.486 | -39.959 | 1.2 |
| | 01:17:46 | 07:53:05 | | | |
| TCH | 2019-11-08 | 2019-11-08 | 7.742 | -36.323 | 1.1 |
| | 01:24:17 | 07:59:48 | | | |
| TCH | 2019-11-08 | 2019-11-08 | 7.617 | -34.505 | 1.1 |
| | 01:31:15 | 08:06:32 | | | |
| TCH | 2019-11-08 | 2019-11-08 | 22.276 | -40.041 | 1 |
| | 01:50:14 | 08:25:31 | | | |
| TCH | 2019-11-08 | 2019-11-08 | 22.407 | -39.959 | 1 |
| | 01:56:56 | 08:32:13 | | | |
| TCH | 2019-11-08 | 2019-11-08 | 12.87 | -39.959 | 1.7 |
| | 02:22:21 | 06:48:08 | | | |
| TCH | 2019-11-08 | 2019-11-08 | 12.986 | -40.041 | 1.7 |
| | 02:29:20 | 06:54:58 | | | |
| TCH | 2019-11-08 | 2019-11-08 | 7.939 | -36.405 | 1 |
| | 03:53:06 | 08:18:42 | | | |
| TCH | 2019-11-08 | 2019-11-08 | 12.635 | -38.223 | 1.5 |
| | 04:57:55 | 05:04:14 | | | |
| TCH | 2019-11-08 | 2019-11-08 | 5.478 | -36.323 | 1.3 |
| | 05:30:19 | 07:46:24 | | | |
+-------+------------+------------+---------+---------+---------+
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 FRAM-Auger tile is 1.0x1.0 degrees and 0.45x0.45 degrees for
FRAM-CTA-N.
Each TRE tile is 4.2x4.2 degrees and 1.9x1.9 degrees for TCA and TCH.
These observations cover about 40% of the cumulative probability of the
Bayestar skymap available on Nov 6, 2019 18:01:59 UTC.
The typical limiting magnitude in R (AB mode) is 16.0 and 18.0 for a
120 s exposure for FRAM-CTA-N and FRAM-Auger, respectively.
The typical limiting magnitude in AB mode is 17.0 and 18.0
for a 60.0 s exposure for TRE and TCA/TCH, respectively.
The coverage map is available at:
https://grandma-owncloud.lal.in2p3.fr/index.php/s/FnfqEwZtgcSxeLl
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].
Details on the FRAM and TAROT telescopes are available on the GRANDMA
web pages https://grandma.lal.in2p3.fr/.
[1] M. W Coughlin et al., MNRAS 2019, doi.org/10.1093/mnras/stz2485
[2] S. Antier et al., MNRAS 2019, arXiv:1910.11261, 2019
[3] K. Noysena et al., ApJ 2019, arXiv:1910.02770
GCN Circular 26245
Subject
LIGO/Virgo S191105e: Updated Sky Localization
Date
2019-11-13T22:30:06Z (6 years ago)
From
Brandon Piotrzkowski at U of Wisconsin-Milwaukee <piotrzk3@uwm.edu>
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
S191105e (GCN Circular 26182).
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/S191105e
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 643 deg2.
Marginalized over the whole sky, the a posteriori luminosity distance
estimate is 1183 +/- 281 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)