LIGO/Virgo S191109d

The LIGO Scientific Collaboration and the Virgo Collaboration report:

We identified the compact binary merger candidate S191109d during
real-time processing of data from LIGO Hanford Observatory (H1) and
LIGO Livingston Observatory (L1) at 2019-11-09 01:07:17.221 UTC (GPS
time: 1257296855.221). The candidate was found by the SPIIR [1], CWB
[2], GstLAL [3], MBTAOnline [4], and PyCBC Live [5] analysis
pipelines.

S191109d is an event of interest because its false alarm rate, as
estimated by the online analysis, is 1.5e-13 Hz, or about one in 2e5
years. The event's properties can be found at this URL:
https://gracedb.ligo.org/superevents/S191109d

The classification of the GW signal, in order of descending
probability, is BBH (>99%), Terrestrial (<1%), BNS (<1%), NSBH (<1%),
or MassGap (<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
[6], distributed via GCN notice about 9 minutes after the candidate
event time.

For the bayestar.fits.gz,0 sky map, the 90% credible region is 1487
deg2. Marginalized over the whole sky, the a posteriori luminosity
distance estimate is 1810 +/- 604 Mpc (a posteriori mean +/- standard
deviation).

For further information about analysis methodology and the contents of
this alert, refer to the LIGO/Virgo Public Alerts User Guide
<https://emfollow.docs.ligo.org/userguide/>.

 [1] Qi Chu, PhD Thesis, The University of Western Australia (2017)
 [2] Klimenko et al. PRD 93, 042004 (2016)
 [3] Messick et al. PRD 95, 042001 (2017)
 [4] Adams et al. CQG 33, 175012 (2016)
 [5] Nitz et al. PRD 98, 024050 (2018)
 [6] Singer & Price PRD 93, 024013 (2016)

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
S191109d
 in a time range of 1000 seconds [3] centered on the alert event time
(2019-11-09 00:58:57.221 UTC to 2019-11-09 01:15:37.221 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
S191109d 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 S191109d ranges from 0.029 to 0.659 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
Loading...
 
  (2018) and Countryman et
al.arXiv:1901.05486
Loading...
 
  (2019)
[2] PoS(ICRC2019)918 and Braun et al., Astroparticle Physics 29, 299 (2008)
[3] Baret et al., Astroparticle Physics 35, 1 (2011)

N. Kawai (Tokyo Tech), H. Negoro (Nihon U.),
S. Sugita, M. Serino (AGU),
M. Nakajima, W. Maruyama, M. Aoki, K. Kobayashi (Nihon U.),
T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN),
T. Sakamoto, H. Nishida, A. Yoshida (AGU),
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, T. Sato (Chuo U.),
M. Shidatsu (Ehime U.), M. Oeda, K. Shiraishi (Tokyo Tech),
S. Nakahira, Y. Sugawara, S. Ueno, H. Tomida, M. Ishikawa, N. Isobe, R. Shimomukai, M. Tominaga (JAXA),
Y. Ueda, A. Tanimoto, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake (Kyoto U.),
H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.),
M. Yamauchi, S. Iwahori, Y. Kurihara, K. Kurogi, K. Miike (Miyazaki U.),
T. Kawamuro (NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), 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 S191109d at 2019-11-09 01:07:17.220 UTC (GCN 26202
Loading...
 
 ).

At the trigger time of S191109d, the high-voltage of MAXI/GSC was off,
and it was turned on at T0+335 sec (+5.6 min).
The first one-orbit (92 min) scan observation with GSC after the event covered 91%
of the 90% credible region of the bayestar skymap from 01:20:47 to 02:33:17 UTC (T0+810 to T0+5160 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.

P. Veres (UAH) reports on behalf of the Fermi-GBM Team and the
GBM-LIGO/Virgo group:

For S191109d and using the initial BAYESTAR skymap, Fermi-GBM was observing
87.2% of the localization probability at event time.

There was no Fermi-GBM onboard trigger around the event time of S191109d
(GCN 26202
Loading...
 
 ). 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= 320.9, Dec= 12.1 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
Loading...
 
 , 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     normal   hard
--------------------------------------
0.128 s:   6.3      9.5      23
1.024 s:   1.5      2.3      5.5
8.192 s:   0.50     0.76     1.4

Assuming the median luminosity distance of 1810 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     Normal   Hard
------------------------------------
0.128s:    38       52       210
1.024s:    9.2      13       50
8.192s:    3.1      4.1      13

C. Pittori (SSDC, and INAF/OAR), V. Fioretti (INAF/OAS-Bologna), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, C. Casentini, G. Piano, A. Ursi (INAF/IAPS), F. Lucarelli, 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 S191109d at T0 = 2019-11-09 01:07:17 (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, 100% of the S191109d 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 S191109d localization region, from a minimum of 1.47E-06 erg cm^-2 to a maximum of 6.95E-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.

Sergey Molkov (IKI, Russia), Maeve Doyle (UCD, Ireland)
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 INTEGRAL/SPI-ACS realtime data (following [1]) we have performed
a search for a prompt gamma-ray counterpart of S191109d (GCN 26202
Loading...
 
 ).

At the time of the event (2019-11-09 01:07:17 UTC, hereafter T0),
INTEGRAL was operating in nominal mode. The peak of the event
localization probability was at an angle of 120 deg with respect to
the spacecraft pointing axis. This orientation implies strongly
suppressed (4.8% of optimal) response of ISGRI, somewhat suppressed
(54% of optimal) response of IBIS/Veto, and strongly suppressed (20%
of optimal) response of SPI-ACS.

The background within +/-300 seconds around the event was rather
stable (excess variance 1.3).

We have performed a search for any impulsive events in INTEGRAL SPI-
ACS (as described in [2]) data.

We do not detect any significant counterparts and estimate a 3-sigma
upper limit on the 75-2000 keV fluence of 5.3e-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 ~4.8e-07 (6.2e-08)
erg/cm^2/s at 1 s (8 s) time scale in 75-2000 keV energy range.

For the mean reported distance 1810.0 Mpc this corresponds to the
limit on the total isotropic equivalent energy in 1 s of 2.1e+50 erg
for the short GRB spectrum and for a long GRB spectrum isotropic
equivalent luminosity in 1 s (8 s) of 6.2e+49 erg/s (2.4e+49 erg/s)

We report for completeness and in order of FAP, all excesses
identified in the search region. We find: 2 likely background
excesses:

scale | T | S/N | luminosity ( x 1e+50 erg/s) | FAP
4.5 | -31.8 | 3.2 | 11.6 +/- 5.18 +/- 11.8 | 0.0977
0.5 | 178 | 4.4 | 4.52 +/- 1.56 +/- 4.6 | 0.815

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

V. Fioretti (INAF/OAS-Bologna), C. Pittori (SSDC, and INAF/OAR), M.
Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, C.
Casentini, G. Piano, A. Ursi (INAF/IAPS), F. Lucarelli, 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 S191109d at T0 = 2019-11-09
01:07:17.221 UTC a preliminary analysis of the AGILE exposure at T0 shows
that the Gamma-Ray Imaging Detector (GRID) exposure covered about 25% of
the 90% c.l. localization region (LR) (0% of 90% c.l. localization region
(LR) is occulted by Earth).

We performed an analysis of the GRID data in the energy range 50 MeV -
10 GeV on T0, where good exposure of the S191109d 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 7.77e-07 to 8.79e-06 erg cm^-2 s^-1, with exposure of about 26% of
the LR over the time interval ( T0 -2s ; T0 + 2s );
from 6.16e-07 to 8.61e-06 erg cm^-2 s^-1, with exposure of about 25% of
the LR over the time interval ( T0s ; T0 + 5s );
from 3.06e-07 to 7.69e-06 erg cm^-2 s^-1, with exposure of about 25% of
the LR over the time interval ( T0s ; T0 + 10s );
from 3.78e-08 to 7.69e-06 erg cm^-2 s^-1, with exposure of about 25% 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.

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-IAC robotic telescope  (Global MASTER-Net: 
http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, 
vol. 2010, 30L)  located in Spain (IAC Teide Observatory) started inspect 
of the LIGO/Virgo S191109d errorbox  863 sec after notice time and 1475 
sec after trigger time at 2019-11-09 01:31:52 UT, with upper limit up to 
19.8 mag. The observations began at zenith distance = 71 deg. The sun 
altitude  is -74.6 deg.

MASTER-Kislovodsk robotic telescope  located in Russia (Lomonosov MSU, 
Kislovodsk Solar Station of Pulkovo observatory) started inspect of the 
LIGO/Virgo S191109d errorbox  1389 sec after notice time and 2002 sec 
after trigger time at 2019-11-09 01:40:39 UT, with upper limit up to  19.6 
mag. The observations began at zenith distance = 40 deg. The sun  altitude 
is -24.7 deg.

The galactic latitude b = 16 deg., longitude l = 326 deg.


Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/ligo_1.php?id=10893


The observation and reduction will continue.
The message may be cited.

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 S191109d event using the 90% contour of the Initial bayestar probability
map provided by the GW interferometers (GCN#26202
Loading...
 
 ). 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/S191109d_Initial.png.
Considering the location probability provided by the LIGO/Virgo collaborations, there is a
79.1% 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 2019-11-09 01:07:17 and in the 90% contour of the S191109d
event. The expected number of atmospheric background events in the region visible by ANTARES is
9.75e-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 7.02e-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.

T. Sakamoto (AGU), S. D. Barthelmy (NASA/GSFC),
A. Y. Lien (GSFC/UMBC), D. M. Palmer (LANL)
A. P. Beardmore (U. Leicester), M. G. Bernardini (INAF-OAB),
A. A. Breeveld (MSSL-UCL), D. N. Burrows (PSU),
S. Campana (INAF-OAB), S. B. Cenko (NASA/GSFC),
G. Cusumano (INAF-IASF PA), A. D'Ai (INAF-IASFPA),
P. D'Avanzo (INAF-OAB), V. D'Elia (ASI-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 S191109d (LIGO/VIRGO Collaboration GCN Circ. 26202
Loading...
 
 ),
where T0 is the LVC trigger time (2019-11-09T01:07:17.220 UTC).

The center of the BAT field of view (FOV) at T0 is
RA = 183.545 deg,
DEC = 14.085 deg,
and the roll angle is 132.514 deg.
The BAT FOV (>10% partial coding) covers 17.59% of the integrated
LVC localization probability. 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 ~ 1.26 x 10^-7 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 ~ 63.91 Mpc.

No event data are available at this time.

BAT retains decreased, but significant, sensitivity to rate increases for
gamma-ray events outside of its FOV. About 82.41% 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/S191109d/web/source_public.html

V. Shenoy (IITB), A. Anumarlapudi (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 sec window around the trigger time of the BBH merger event S191109d (UTC 2019-11-09 01:07:17.000, 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 = 6:36:08.2,-42:50:44.7 (99.0342,-42.8458), which is  81 deg away from the maximum probability location. At the time of merger event, the Earth-satellite-transient angle corresponding to maximum probability location is ~ 73.52 deg and hence is not 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 0.66 (66%).

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= 1.78e-05 ergs/cm^2/s; fluence limit = 1.78e-06 ergs/cm^2
1.0 s: flux limit= 5.98e-06 ergs/cm^2/s; fluence limit = 5.98e-06 ergs/cm^2
10.0 s: flux limit= 7.45e-07 ergs/cm^2/s; fluence limit = 7.45e-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.

S. Cutini (INFN Perugia), 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 09, 2019, for possible high-energy (E > 100 MeV) gamma-ray emission in spatial/temporal coincidence with the LIGO/Virgo trigger S191109d (GCN 26202
Loading...
 
 ).

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 ~50% of the LIGO probability region at the time of the trigger (T0 = 2019-11-09 01:07:17.221 UTC) and reached 100% cumulative coverage at approximately T0 + 5.3 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. No significant sources were 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 between 100 MeV and 1 GeV for the fixed time interval of this search vary between 1.8e-10 and 1.7e-7 [erg/cm^2/s].

The Fermi-LAT point of contact for this event is Michael Moss (michaelmoss@gwmail.gwu.edu <mailto: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.

N. Christensen (Artemis), M. Coughlin (Caltech), W. Lin (THU), C.
Stachie (Artemis), S. Karpov, M. Masek, M. Prouza (FZU), M. Boer
(Artemis), L. Eymar (Artemis), A. Klotz (IRAP), K. Noysena (Artemis,
IRAP), S. Antier (APC), A. Coleiro (APC), D. Corre (LAL), D. A. Kann
(HETH/IAA-CSIC), D.Coward (OzGrav-UWA), J.G. Ducoin (LAL), B. Gendre
(OzGrav-UWA), N.Kochiashvili (Iliauni), 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 S191109d 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 11/09/19 01:32:55 UTC for FRAM-CTA-N which
corresponds approximately to 26 minutes after the  GW trigger time.

The observation started on 11/09/19 06:45:28 UTC for FRAM-Auger which
corresponds approximately to 339 minutes after the GW trigger time.

The observation started on 11/09/19 21:21:00 UTC for TRE which
corresponds approximately to 1214 minutes after the GW trigger time.

The observation started on 11/09/19 02:09:58 UTC for TCA which
corresponds approximately to 63 minutes  after the GW trigger time.

The observation started on 11/10/19  06:34:37 UTC for TCH which
corresponds approximately to 1768 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 | 2019-11-09 | 2019-11-09 | 192.906 | -44.27  |	  0.1   |
|       | 06:45:28   | 06:49:55   |	    | 	      |	        |
|FRAM-A | 2019-11-09 | 2019-11-09 | 193.103 | -45.243 |	  0.1   |
|       | 06:50:30   | 06:54:57   |	    | 	      |	        |
|FRAM-A | 2019-11-09 | 2019-11-09 | 188.83  | -44.27  |	  0.1   |
|       | 06:55:33   | 07:00:00   |	    | 	      |	        |
|FRAM-A | 2019-11-09 | 2019-11-09 | 200     | -45.243 |	  0.1   |
|       | 07:07:59   | 07:12:26   |         | 	      |	        |
|FRAM-A | 2019-11-09 | 2019-11-09 | 198.621 | -45.243 |	  0.1   |
|       | 07:13:01   | 07:17:28   |	    | 	      |	        |
|FRAM-A | 2019-11-09 | 2019-11-09 | 194.483 | -45.243 |	  0.1   |
|       | 07:18:04   | 07:22:31   |         | 	      |	        |
|FRAM-A | 2019-11-09 | 2019-11-09 | 196.981 | -44.27  |	  0.1   |
|       | 07:23:07   | 07:27:34   |         | 	      |	        |
|FRAM-A | 2019-11-09 | 2019-11-09 | 197.241 | -45.243 |	  0.1   |
|       | 07:28:09   | 07:32:36   |         | 	      |	        |
|FRAM-A | 2019-11-09 | 2019-11-09 | 198.34  | -44.27  |	  0.1   |
|       | 07:33:11   | 07:37:38   |	    | 	      |	        |
|FRAM-A | 2019-11-09 | 2019-11-09 | 195.623 | -44.27  |	  0.2   |
|       | 07:38:13   | 07:42:40   |         | 	      |	        |
|FRAM-A | 2019-11-09 | 2019-11-09 | 195.862 | -45.243 |	  0.1   |
|       | 07:43:14   | 07:47:41   |         | 	      |	        |
|FRAM-A | 2019-11-09 | 2019-11-09 | 205.517 | -45.243 |	  0.2   |
|       | 07:48:20   | 07:52:47   |         | 	      |	        |
|FRAM-A | 2019-11-09 | 2019-11-09 | 202.415 | -44.27  |	  0.1   |
|       | 07:53:21   | 07:57:48   |         | 	      |	        |
|FRAM-A | 2019-11-09 | 2019-11-09 | 203.774 | -44.27  |	  0.2   |
|       | 07:58:24   | 08:02:51   |         | 	      |	        |
|FRAM-A | 2019-11-09 | 2019-11-09 | 202.759 | -45.243 |	  0.2   |
|       | 08:03:26   | 08:07:53   |         | 	      |	        |
|FRAM-A | 2019-11-09 | 2019-11-09 | 201.379 | -45.243 |	  0.2   |
|       | 08:08:27   | 08:12:54   |         | 	      |	        |
|FRAM-A | 2019-11-09 | 2019-11-09 | 204.138 | -45.243 |	  0.2   |
|       | 08:13:30   | 08:17:57   |         | 	      |	        |
|FRAM-A | 2019-11-09 | 2019-11-09 | 201.057 | -44.27  |	  0.1   |
|       | 08:18:32   | 08:22:59   |	    | 	      |	        |
|FRAM-A | 2019-11-09 | 2019-11-09 | 205.132 | -44.27  |	  0.1   |
|       | 08:23:34   | 08:28:01   |         | 	      |	        |
|FRAM-A | 2019-11-09 | 2019-11-09 | 199.698 | -44.27  |	  0.1   |
|       | 08:28:37   | 08:33:04   |         | 	      |	        |
|-------+------------+------------+---------+---------+---------|
|FRAM-C | 2019-11-09 | 2019-11-09 | 132.926 | 4.045   |   0.03  |
|       | 01:32:55   | 02:36:07   |         |         |         |
|FRAM-C | 2019-11-09 | 2019-11-09 | 137.472 | -5.243  |   0.03  |
|       | 01:37:17   | 04:08:52   |         |         |         |
|FRAM-C | 2019-11-09 | 2019-11-09 | 135.714 | -2.833  |   0.03  |
|       | 01:56:58   | 02:01:04   |         |         |         |
|FRAM-C | 2019-11-09 | 2019-11-09 | 134.788 | -0.649  |   0.03  |
|       | 02:01:20   | 02:05:26   |         |         |         |
|FRAM-C | 2019-11-09 | 2019-11-09 | 135.874 | -2.409  |   0.03  |
|       | 02:05:53   | 02:09:59   |         |         |         |
|FRAM-C | 2019-11-09 | 2019-11-09 | 135.324 | -1.086  |   0.03  |
|       | 02:10:14   | 02:14:20   |         |         |         |
|FRAM-C | 2019-11-09 | 2019-11-09 | 135.662 | -1.96   |   0.03  |
|       | 02:14:34   | 02:18:40   |         |         |         |
|FRAM-C | 2019-11-09 | 2019-11-09 | 135.549 | -1.523  |   0.02  |
|       | 02:18:54   | 02:23:00   |         |         |         |
|FRAM-C | 2019-11-09 | 2019-11-09 | 135.324 | -0.212  |   0.03  |
|       | 02:23:15   | 02:27:21   |         |         |         |
|FRAM-C | 2019-11-09 | 2019-11-09 | 134.788 | 0.874   |   0.03  |
|       | 02:27:36   | 02:31:42   |         |         |         |
|FRAM-C | 2019-11-09 | 2019-11-09 | 133.202 | 3.383   |   0.03  |
|       | 02:36:33   | 02:40:39   |         |         |         |
|FRAM-C | 2019-11-09 | 2019-11-09 | 133.202 | 2.846   |   0.03  |
|       | 02:40:54   | 02:45:00   |         |         |         |
|FRAM-C | 2019-11-09 | 2019-11-09 | 133.914 | 0.986   |   0.03  |
|       | 02:45:21   | 02:49:27   |         |         |         |
|FRAM-C | 2019-11-09 | 2019-11-09 | 133.914 | 1.973   |   0.03  |
|       | 02:49:43   | 02:53:49   |         |         |         |
|FRAM-C | 2019-11-09 | 2019-11-09 | 135.549 | -0.649  |   0.03  |
|       | 02:54:05   | 02:58:11   |         |         |         |
|FRAM-C | 2019-11-09 | 2019-11-09 | 134.451 | 0.225   |   0.03  |
|       | 02:58:27   | 03:02:33   |         |         |         |
|FRAM-C | 2019-11-09 | 2019-11-09 | 137.976 | -6.878  |   0.03  |
|       | 03:51:16   | 03:55:22   |         |         |         |
|FRAM-C | 2019-11-09 | 2019-11-09 | 137.415 | -5.891  |   0.03  |
|       | 03:55:38   | 03:59:44   |         |         |         |
|FRAM-C | 2019-11-09 | 2019-11-09 | 136.429 | -3.707  |   0.03  |
|       | 04:00:19   | 04:04:25   |         |         |         |
|FRAM-C | 2019-11-09 | 2019-11-09 | 136.264 | -3.27   |   0.03  |
|       | 04:09:18   | 04:13:23   |         |         |         |
|-------+------------+------------+---------+---------+---------|
|  TRE  | 2019-11-09 | 2019-11-09 | 135     | 0       |     1.4 |
|       | 21:21:00   | 21:27:23   |         |         |         |
|  TRE  | 2019-11-09 | 2019-11-10 | 129.767 | 12.273  |     1.1 |
|       | 21:40:11   | 00:16:41   |         |         |         |
|  TRE  | 2019-11-09 | 2019-11-09 | 142.326 | -12.273 |     1.1 |
|       | 21:53:22   | 21:59:39   |         |         |         |
|  TRE  | 2019-11-09 | 2019-11-09 | 148.5   | -24.545 |     1.1 |
|       | 22:05:48   | 22:12:05   |         |         |         |
|  TRE  | 2019-11-09 | 2019-11-09 | 132.414 | 8.182   |     1.1 |
|       | 22:18:57   | 22:25:21   |         |         |         |
|  TRE  | 2019-11-09 | 2019-11-09 | 155.676 | -32.727 |     1   |
|       | 22:31:13   | 22:37:31   |         |         |         |
|  TRE  | 2019-11-09 | 2019-11-09 | 140.69  | -8.182  |     1   |
|       | 22:44:28   | 22:50:51   |         |         |         |
|  TRE  | 2019-11-09 | 2019-11-09 | 141.429 | -16.364 |     1   |
|       | 22:57:03   | 23:03:20   |         |         |         |
|  TRE  | 2019-11-09 | 2019-11-09 | 135     | 4.091   |     0.9 |
|       | 23:10:02   | 23:16:19   |         |         |         |
|  TRE  | 2019-11-09 | 2019-11-09 | 185.806 | -45     |     1.6 |
|       | 23:44:52   | 23:51:15   |         |         |         |
|-------+------------+------------+---------+---------+---------|
|  TCA  | 2019-11-09 | 2019-11-10 | 126.664 | 14.867  |     0.2 |
|       | 02:09:58   | 02:46:56   |         |         |         |
|  TCA  | 2019-11-09 | 2019-11-10 | 129.459 | 15.298  |     0.2 |
|       | 02:16:42   | 05:23:09   |         |         |         |
|  TCA  | 2019-11-09 | 2019-11-10 | 126.758 | 13.012  |     0.1 |
|       | 03:40:47   | 01:47:23   |         |         |         |
|  TCA  | 2019-11-09 | 2019-11-10 | 128.009 | 16.723  |     0.2 |
|       | 04:33:53   | 05:10:44   |         |         |         |
|  TCA  | 2019-11-09 | 2019-11-10 | 126.084 | 16.723  |     0.2 |
|       | 22:38:39   | 03:45:32   |         |         |         |
|  TCA  | 2019-11-09 | 2019-11-10 | 126.167 | 20.434  |     0.2 |
|       | 22:58:04   | 04:04:42   |         |         |         |
|  TCA  | 2019-11-10 | 2019-11-10 | 137.565 | -0.928  |     0.2 |
|       | 01:02:28   | 03:38:47   |         |         |         |
|  TCA	| 2019-11-10 | 2019-11-10 | 132.027 | 0.022   |     0.2 |
|       | 01:21:38   | 03:57:57   |         |         |         |
|  TCA	| 2019-11-10 | 2019-11-10 | 144.385 | -15.298 |     0.2 |
|       | 02:20:50   | 04:57:14   |         |         |         |
|  TCA	| 2019-11-10 | 2019-11-10 | 126.756 | 18.579  |     0.2 |
|       | 03:06:18   | 03:12:38   |         |         |         |
|  TCA	| 2019-11-10 | 2019-11-10 | 128.991 | 7.445   |     0.2 |
|       | 03:25:40   | 03:31:59   |         |         |         |
|  TCA	| 2019-11-10 | 2019-11-10 | 145.227 | -24.102 |     0.1 |
|       | 04:05:08   | 04:07:08   |         |         |         |
|-------+------------+------------+---------+---------+---------|
|  TCH  | 2019-11-10 | 2019-11-10 | 144.95  | -17.273 |     0.3 |
|       | 06:34:37   | 06:40:55   |         |         |         |
|  TCH  | 2019-11-10 | 2019-11-10 | 196.161 | -43.595 |     0.4 |
|       | 08:12:47   | 08:19:06   |         |         |         |
|  TCH  | 2019-11-10 | 2019-11-10 | 184.931 | -42.252 |     0.3 |
|       | 08:38:39   | 08:44:58   |         |         |         |
+-------+------------+------------+---------+---------+---------+
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 17% of the cumulative probability of the
Bayestar skymap available on Nov 9, 2019 01:15:21 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/utGS2Zigv2qGp8S

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
Loading...
 
 , 2019
[3] K. Noysena et al., ApJ 2019, arXiv:1910.02770
Loading...
 
 

Y. Asaoka (Waseda U), A. Yoshida, T. Sakamoto, 
V. Pal'shin, S. Sugita (AGU), Y. Kawakubo (LSU),
K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
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 
S191109d, T0 = 2019-11-09 01:07:17.221 UT (The LIGO 
Scientific Collaboration and Virgo Collaboration, GCN 
Circ. 26202
Loading...
 
 ), the CALET Gamma-ray Burst Monitor (CGBM)
high voltages were off (from T0-29 min to T0+3 min).

The CALET Calorimeter (CAL) was operating in the high energy 
trigger mode at the trigger time of S191109d. 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=349.9 deg, Dec=-16.6 deg at T0.