LIGO/Virgo S191204r

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-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the LIGO/Virgo S191204r errorbox  401 sec after notice time and 3049 sec after trigger time at 2019-12-04 18:06:15 UT, with upper limit up to  19.2 mag. The observations began at zenith distance = 50 deg. The sun  altitude  is -42.5 deg. 

The galactic latitude b = -19 deg., longitude l = 252 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/ligo_1.php?id=10960

We obtain a following upper limits.  

Tmid-T0  |      Date Time      |          Site       |             Coord (J2000)          |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________

    3139 | 2019-12-04 18:06:15 |      MASTER-Tavrida | (02h 54m 34.70s , -00d 56m 20.8s) |   C |   180 | 19.2 |        
Filter C is a clear (unfiltred) band. 


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

Diego Gotz (AIM/CEA Saclay, France), Enrico Bozzo, 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 <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 S191204r (GCN 26332
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 ).

At the time of the event (2019-12-04 17:15:26 UTC, hereafter T0),
INTEGRAL was operating in nominal mode. The peak of the event
localization probability was at an angle of 118 deg with respect to
the spacecraft pointing axis. This orientation implies strongly
suppressed (2.2% of optimal) response of ISGRI, somewhat suppressed
(41% of optimal) response of IBIS/Veto, and somewhat suppressed (5! 0%
of optimal) response of SPI-ACS.

The background within +/-300 seconds around the event was very stable
(excess variance 1.1).

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 3.4e-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 ~2.9e-07 (9.1e-08)
erg/cm^2/s at 1 s (8 s) time scale in 75-2000 keV energy range.

For the mean reported distance 678.0 Mpc this corresponds to the limit
on the total isotropic equivalent energy in 1 s of 1.9e+49 erg for
the short GRB spectrum and for a long GRB spectrum isotropic
equivalent luminosity in 1 s (8 s) of 1.4e+49 erg/s (5e+48 erg/s)

We report for completeness and in order of FAP, all excesses
identified in the search region. We find: 1 possibly associated
excess:

scale | T | S/N | luminosity ( x 1e+49 erg/s) | FAP  
1.7 | 19.1 | 3.8 | 17.9 +/- 4.56 +/- 5.02 | 0.0482 

5 likely background excesses:

scale | T | S/N | luminosity ( x 1e+49 erg/s) | FAP  
0.5 | -30.1 | 3.5 | 30.6 +/- 8.43 +/- 8.56 | 0.44  
1.25 | 253 | 4 | 21.6 +/- 5.32 +/- 6.05 | 0.661 
0.2 | -8.5 | 3.1 | 4.25 +/- 1.34 +/- 1.19 | 0.753 
1.4 | 144 | 3.4 | 18.3 +/- 5.02 +/- 5.12 | 0.814 
2 | -152 | 3.3 | 14.9 +/- 4.2 +/- 4.16 | 0.864 

Note that FAP estimates (especially at timescales above 2s) may be
possibly ! further a ffected 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 OPS NOTE(04dec19):  Per author's request, the Circular referenced
in the first paragraph was changed from "GCN 99999" to "GCN 26332".]

The LIGO Scientific Collaboration and the Virgo Collaboration report:

We identified the compact binary merger candidate S191204r during
real-time processing of data from LIGO Hanford Observatory (H1), LIGO
Livingston Observatory (L1), and Virgo Observatory (V1) at 2019-12-04
17:15:26.092 UTC (GPS time: 1259514944.092). The candidate was found
by the GstLAL [1], CWB [2], MBTAOnline [3], and SPIIR [4] analysis
pipelines.

S191204r is an event of interest because its false alarm rate, as
estimated by the online analysis, is 3.1e-25 Hz, or about one in 1e17
years. The event's properties can be found at this URL:
https://gracedb.ligo.org/superevents/S191204r

At the time of the event the Virgo detector was performing calibration
injections, and was in low noise mode but not observing. At the exact
time of the event Virgo was between calibration injections and the
data was undisturbed. After discussion we agreed that the data was
usable for sky localization.

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%.

Three sky maps are 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.
 * bayestar.fits.gz,1, an initial localization generated by BAYESTAR
[5], distributed via GCN notice about 54 minutes after the candidate
event time.
 * bayestar.fits.gz,2, an initial localization generated by BAYESTAR
[5], distributed via GCN notice about an hour after the candidate
event time.

The preferred sky map at this time is bayestar.fits.gz,2. For the
bayestar.fits.gz,2 sky map, the 90% credible region is 103 deg2.
Marginalized over the whole sky, the a posteriori luminosity distance
estimate is 678 +/- 149 Mpc (a posteriori mean +/- standard
deviation).

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

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

[GCN OPS NOTE (04dec19):  The typo extra "SUBJECT:" was removed from the SUBJECT:-line.]

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
S191204r
 in a time range of 1000 seconds [3] centered on the alert event time
(2019-12-04 17:07:06.092 UTC to 2019-12-04 17:23:46.092 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
S191204r calculated from the map circulated in the 4-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 S191204r ranges from 0.032 to 0.558 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
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  (2018) and Countryman et
al.arXiv:1901.05486
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  (2019)
[2] PoS(ICRC2019)918 and Braun et al., Astroparticle Physics 29, 299 (2008)
[3] Baret et al., Astroparticle Physics 35, 1 (2011)

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 S191204r event using the 90% contour of the Initial bayestar probability
map provided by the GW interferometers (GCN#26334
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  <https://gcn.gsfc.nasa.gov/gcn3/26334.gcn3
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 >). 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/S191204r_Initial.png <http://antares.in2p3.fr/GW/S191204r_Initial.png>.
Considering the location probability provided by the LIGO/Virgo collaborations, there is a
92.9% chance that the GW emitter was in the ANTARES **upgoing** field of view at the time of
the alert.

No up-going muon neutrino candidate events were recorded in the ANTARES sky during a
+/-500s time-window centered on the time 2019-12-04 17:15:26 and in the 90% contour of the S191204r
event. The expected number of atmospheric background events in the region visible by ANTARES is
8.66e-05 in the +/- 500s time window. An extended search during +/- 1 hour gives no
up-going muon neutrino coincidence. The expected number of atmospheric background events in the
region visible by ANTARES is 6.24e-04 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.

F. Longo (Univ. Trieste, and INFN Trieste), G. Piano (INAF/IAPS), M. Tavani
(INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, C. Casentini, A. Ursi
(INAF/IAPS), F. Lucarelli, C. Pittori, F. Verrecchia (SSDC, and INAF/OAR),
A. Bulgarelli, V. Fioretti, N. Parmiggiani (INAF/OAS-Bologna), M. Pilia
(INAF/OA-Cagliari) report on behalf of the AGILE Team:

In response to the LIGO/Virgo GW event S191204r at T0 = 2019-12-04
17:15:26.092 (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 80% of the S191204r 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 S191204r localization region, from a minimum of 2.0E-06 erg
cm^-2 to a maximum of 3.0E-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.

G. Piano (INAF/IAPS), F. Longo (Univ. Trieste, and INFN Trieste), M. Tavani
(INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, C. Casentini, A. Ursi
(INAF/IAPS), F. Lucarelli, C. Pittori, F. Verrecchia (SSDC, and INAF/OAR),
A. Bulgarelli, V. Fioretti, N. Parmiggiani (INAF/OAS-Bologna), M. Pilia
(INAF/OA-Cagliari) report on behalf of the AGILE Team:

In response to the LIGO-Virgo GW event S191204r at T0 = 2019-12-04
17:15:26.092 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) (16% 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 S191204r 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 3.5e-08 to 9.0e-07 erg cm^-2 s^-1, with exposure of about 65% of the
LR over the time interval (T0; T0 + 100 s);

These measurements were obtained with AGILE observing a large portion of
the sky in spinning mode. Additional analysis of AGILE data is in progress.

H. Negoro (Nihon U.), N. Kawai (Tokyo Tech), 
S. Sugita, M. Serino (AGU), 
M. Nakajima, W. Maruyama, M. Aoki, K. Kobayashi, R. Takagi (Nihon U.), 
T. Mihara, C. Guo, Y. Zhou, 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, 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 S191204r at 2019-12-04 17:15:26.092 UTC (GCN 26334
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 ). 

At the trigger time of S191204r, the high-voltage of MAXI/GSC was off, 
and it was turned on at T0+1159 sec (+19.3 min). 
The first one-orbit (92 min) scan observation with GSC after the event covered 100% 
of the 90% credible region of the bayestar skymap from 17:35:26 to 17:54:51 UTC (T0+1200 to T0+2365 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.

C. Malacaria (NASA-MSFC/USRA) reports on behalf of the Fermi-GBM Team
 and the GBM-LIGO/Virgo group

At the time of S191204r, Fermi was passing through the South Atlantic 
Anomaly from 3.0 minutes prior to 19.7 minutes after the trigger time; 
therefore the GBM detectors were disabled.

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 S191204r (LIGO/VIRGO Collaboration GCN Circ. 26334
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 ),
where T0 is the LVC trigger time (2019-12-04T17:15:26.091 UTC).

The center of the BAT field of view (FOV) at T0 is
RA = 46.016 deg,
DEC = -16.004 deg,
and the roll angle is 201.965 deg.
The BAT FOV (>10% partial coding) covers 96.35% of the integrated
LVC localization probability, and 96.35% of the galaxy convolved
probability (Evans et al. 2016). BAT starts slewing at ~T+13 s.
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 astrophysical detections
(signal-to-noise
ratio >~ 5 sigma) are found in the BAT raw light curves with time bins of
64 ms,
1 s, and 1.6 s. The dip in the 64-ms and 1.6-s light curve, and the pulse
in the 1-s around ~T+20 s to ~T+30 s are due to standard onboard calibration
process during spacecraft slews.

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 ~ 2.08 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 ~ 49.83 Mpc.

Event data analysis are available from T-46.18 s to T+43.86 s.
No significant detections (above our typical image threshold
of ~ 6.5 to 7 sigma) are found in the 15-350 keV images created
using intervals of T0-0.1 to T0+0.1 s, T0-2 s to T0+8 s, and the whole
event data range from T0-46.18 s to T0+13.62 s (excluding the spacecraft
slew period).

BAT retains decreased, but significant, sensitivity to rate increases for
gamma-ray events outside of its FOV. About 3.65% 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/S191204r/web/source_public.html

L. Scotton (CNRS/IN2P3/LUPM), M. Axelsson (KTH & Stockholm Univ.),
E. Bissaldi (Politecnico & INFN Bari), N. Omodei (Stanford U.), D. Kocevski (NASA/MSFC),
F. Longo (University and INFN, Trieste), M. Arimoto (Kanazawa Univ.) and P. Veres (UAH)
report on behalf of the Fermi-LAT Collaboration:

We have searched data collected by the Fermi Large Area Telescope (LAT) on
December 4th, 2019, for possible high-energy (E > 100 MeV) gamma-ray emission in
spatial/temporal coincidence with the LIGO/Virgo trigger S191204r (GCN 26334
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 ).

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 = 2019-12-04 17:15:26 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 + 1.3 ks. At that time no
part of the LIGO probability map was observable. The region entered the LAT field
of view around T0 + 2 ks, and 100% cumulative coverage was reached after ~7.3 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 + 1.3 ks 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
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 1e-10 and 5e-10 [erg/cm^2/s].

The Fermi-LAT point of contact for this event is
Lorenzo Scotton (lorenzo.scotton@lupm.in2p3.fr<mailto:lorenzo.scotton@lupm.in2p3.fr>).

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.

M. L. Cherry (LSU), A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU), 
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
Y. Asaoka, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U),
N. Cannady (GSFC/UMBC), 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 S191204r T0 = 2019-12-04 17:15:26.092  UT (The LIGO Scientific
Collaboration and Virgo Collaboration, GCN Circ. 26334
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 ).

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 3 % and 4 %, respectively (and 4 % credible region of the
initial localization map was above the horizon).  The HXM and SGM fields
of view were centered at RA = 259.9 deg, Dec = 41.0 deg and 
RA = 269.2 deg, Dec = 34.3 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 S191204r. 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=269.2 deg,
Dec=34.3 deg at T0.

T. Sadibekova (AIM-CEA), S. Beradze (Iliauni), 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 (NAOC), X. Wang (THU)

report on behalf of the FRAM network, TAROT network and GRANDMA 
collaboration:

We performed tiled observations of the LIGO/Virgo S191204r event with the 
FRAM-Auger, TAROT-Reunion (TRE), 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), Les Makes 
Astronomical Observatory, 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 (AB mag) for a given exposure in 
seconds:
+-------------+---------+----------+-----------+------------+
| Telescope   | Delay   | Filter   | f.o.v.    | Limiting   |
|             | [min]   |          | [deg]     | Mag.       |
|-------------+---------+----------+-----------+------------|
| FRAM-Auger  | 446     |    R     | 1.0 x 1.0 | 18.0 (60s) |
| TCA         | 53      |  Clear   | 1.9 x 1.9 | 18.0 (60s) |
| TCH         | 451     |  Clear   | 1.9 x 1.9 | 18.0 (60s) |
| TRE         | 60      |  Clear   | 4.2 x 4.2 | 17.0 (60s) |
+-------------+---------+----------+-----------+------------+

We performed the following joint tiled observations [1] :

+-------------+------------+------------+---------+---------+---------+
| Telescope   | TStart     | TEnd       | RA      | DEC     | Proba   |
|             | [UTC]      | [UTC]      | [deg]   | [deg]   | [%]     |
|-------------+------------+------------+---------+---------+---------|
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 101.168 | -42.324 | <0.1    |
|             | 00:40:35   | 00:45:02   |         |         |         |
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 102.482 | -42.324 | <0.1    |
|             | 00:45:37   | 00:50:04   |         |         |         |
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 94.532  | -41.351 | <0.1    |
|             | 00:50:42   | 00:55:09   |         |         |         |
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 95.827  | -41.351 | <0.1    |
|             | 00:55:44   | 01:00:11   |         |         |         |
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 99.854  | -42.324 | <0.1    |
|             | 01:00:47   | 01:05:14   |         |         |         |
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 103.796 | -42.324 | <0.1    |
|             | 01:05:50   | 01:10:17   |         |         |         |
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 91.915  | -40.378 | <0.1    |
|             | 01:10:54   | 01:15:21   |         |         |         |
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 98.540  | -42.324 | <0.1    |
|             | 01:15:57   | 01:20:24   |         |         |         |
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 90.638  | -40.378 | <0.1    |
|             | 01:21:00   | 01:25:27   |         |         |         |
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 97.122  | -41.351 | <0.1    |
|             | 01:26:04   | 01:30:31   |         |         |         |
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 108.000 | -43.297 | <0.1    |
|             | 01:31:09   | 01:35:36   |         |         |         |
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 109.333 | -43.297 | <0.1    |
|             | 01:36:11   | 01:40:37   |         |         |         |
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 93.237  | -41.351 | <0.1    |
|             | 01:41:15   | 01:45:42   |         |         |         |
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 106.667 | -43.297 | <0.1    |
|             | 01:46:20   | 01:50:47   |         |         |         |
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 110.667 | -43.297 | <0.1    |
|             | 01:51:23   | 01:55:50   |         |         |         |
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 46.703  | -2.432  | <0.1    |
|             | 01:56:32   | 02:00:59   |         |         |         |
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 112.000 | -43.297 | <0.1    |
|             | 02:01:42   | 02:06:08   |         |         |         |
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 89.362  | -40.378 | <0.1    |
|             | 02:06:47   | 02:11:14   |         |         |         |
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 88.112  | -39.405 | <0.1    |
|             | 02:11:50   | 02:16:16   |         |         |         |
| FRAM-Auger  | 2019-12-05 | 2019-12-05 | 98.417  | -41.351 | <0.1    |
|             | 02:16:53   | 02:21:20   |         |         |         |
| -----       | -----      | -----      | -----   | -----   | -----   |
| TCA         | 2019-12-04 | 2019-12-04 | 52.500  | -9.256  | <0.1    |
|             | 18:07:48   | 22:29:08   |         |         |         |
| TCA         | 2019-12-04 | 2019-12-05 | 37.174  | 19.485  | <0.1    |
|             | 18:14:34   | 00:35:54   |         |         |         |
| TCA         | 2019-12-04 | 2019-12-04 | 40.531  | 13.012  | <0.1    |
|             | 18:21:19   | 18:27:38   |         |         |         |
| TCA         | 2019-12-04 | 2019-12-05 | 46.867  | -7.445  | <0.1    |
|             | 18:33:44   | 01:25:19   |         |         |         |
| TCA         | 2019-12-04 | 2019-12-05 | 35.627  | 16.248  | <0.1    |
|             | 18:40:29   | 03:01:14   |         |         |         |
| TCA         | 2019-12-04 | 2019-12-04 | 36.751  | 21.340  | <0.1    |
|             | 18:47:14   | 18:53:33   |         |         |         |
| TCA         | 2019-12-04 | 2019-12-05 | 31.777  | 26.002  | <0.1    |
|             | 18:59:40   | 01:50:44   |         |         |         |
| TCA         | 2019-12-04 | 2019-12-05 | 32.153  | 27.857  | <0.1    |
|             | 19:13:09   | 02:48:18   |         |         |         |
| TCA         | 2019-12-04 | 2019-12-05 | 53.833  | -19.009 | <0.1    |
|             | 19:54:21   | 00:08:39   |         |         |         |
| TCA         | 2019-12-04 | 2019-12-05 | 48.000  | -0.928  | <0.1    |
|             | 20:56:24   | 01:44:10   |         |         |         |
| TCA         | 2019-12-04 | 2019-12-04 | 31.579  | 29.713  | <0.1    |
|             | 21:22:19   | 21:28:38   |         |         |         |
| TCA         | 2019-12-04 | 2019-12-05 | 32.862  | 22.290  | <0.1    |
|             | 21:36:08   | 02:23:03   |         |         |         |
| TCA         | 2019-12-04 | 2019-12-05 | 41.986  | 0.928   | <0.1    |
|             | 21:48:14   | 02:36:38   |         |         |         |
| TCA         | 2019-12-04 | 2019-12-05 | 35.248  | 25.527  | <0.1    |
|             | 22:01:44   | 00:19:39   |         |         |         |
| TCA         | 2019-12-04 | 2019-12-04 | 52.929  | -15.298 | 0.4     |
|             | 22:16:06   | 22:22:26   |         |         |         |
| TCA         | 2019-12-04 | 2019-12-04 | 62.133  | -21.340 | <0.1    |
|             | 23:21:24   | 23:27:43   |         |         |         |
| TCA         | 2019-12-04 | 2019-12-04 | 57.849  | -23.671 | 0.1     |
|             | 23:44:59   | 23:46:59   |         |         |         |
| TCA         | 2019-12-05 | 2019-12-05 | 38.221  | 9.300   | <0.1    |
|             | 02:23:34   | 02:29:53   |         |         |         |
| -----       | -----      | -----      | -----   | -----   | -----   |
| TCH         | 2019-12-05 | 2019-12-05 | 86.410  | -38.616 | <0.1    |
|             | 00:46:01   | 08:22:19   |         |         |         |
| TCH         | 2019-12-05 | 2019-12-05 | 69.116  | -30.868 | 5.9     |
|             | 00:52:47   | 05:59:04   |         |         |         |
| TCH         | 2019-12-05 | 2019-12-05 | 60.177  | -21.777 | 0.3     |
|             | 00:59:33   | 08:31:31   |         |         |         |
| TCH         | 2019-12-05 | 2019-12-05 | 100.458 | -43.595 | <0.1    |
|             | 01:11:59   | 06:16:10   |         |         |         |
| TCH         | 2019-12-05 | 2019-12-05 | 68.671  | -29.050 | 1.1     |
|             | 01:18:46   | 06:25:17   |         |         |         |
| TCH         | 2019-12-05 | 2019-12-05 | 59.669  | -23.595 | 0.3     |
|             | 01:25:31   | 04:01:49   |         |         |         |
| TCH         | 2019-12-05 | 2019-12-05 | 36.000  | 18.223  | <0.1    |
|             | 01:37:59   | 06:44:29   |         |         |         |
| TCH         | 2019-12-05 | 2019-12-05 | 88.733  | -38.141 | <0.1    |
|             | 01:44:41   | 06:51:15   |         |         |         |
| TCH         | 2019-12-05 | 2019-12-05 | 35.236  | 20.041  | <0.1    |
|             | 01:51:26   | 04:27:57   |         |         |         |
| TCH         | 2019-12-05 | 2019-12-05 | 69.398  | -32.686 | 4.7     |
|             | 02:03:49   | 07:10:08   |         |         |         |
| TCH         | 2019-12-05 | 2019-12-05 | 60.000  | -19.959 | <0.1    |
|             | 02:10:36   | 07:12:38   |         |         |         |
| TCH         | 2019-12-05 | 2019-12-05 | 71.226  | -30.000 | 1.6     |
|             | 02:29:44   | 07:36:04   |         |         |         |
| TCH         | 2019-12-05 | 2019-12-05 | 120.105 | -44.070 | <0.1    |
|             | 02:36:31   | 07:42:49   |         |         |         |
| TCH         | 2019-12-05 | 2019-12-05 | 33.337  | 25.495  | <0.1    |
|             | 02:43:21   | 05:19:38   |         |         |         |
| TCH         | 2019-12-05 | 2019-12-05 | 134.460 | -39.959 | <0.1    |
|             | 04:47:22   | 07:21:31   |         |         |         |
| TCH         | 2019-12-05 | 2019-12-05 | 40.883  | 10.950  | <0.1    |
|             | 06:31:25   | 06:35:34   |         |         |         |
| TCH         | 2019-12-05 | 2019-12-05 | 137.982 | -38.616 | <0.1    |
|             | 07:49:22   | 07:55:40   |         |         |         |
| -----       | -----      | -----      | -----   | -----   | -----   |
| TRE         | 2019-12-04 | 2019-12-04 | 49.655  | -8.182  | 1.2     |
|             | 18:14:49   | 22:36:01   |         |         |         |
| TRE         | 2019-12-04 | 2019-12-04 | 77.143  | -36.818 | 39.8    |
|             | 19:18:16   | 19:24:38   |         |         |         |
| TRE         | 2019-12-04 | 2019-12-04 | 65.455  | -28.636 | 1.0     |
|             | 19:33:42   | 19:37:50   |         |         |         |
| TRE         | 2019-12-04 | 2019-12-04 | 109.091 | -40.909 | <0.1    |
|             | 19:43:46   | 19:50:07   |         |         |         |
| TRE         | 2019-12-04 | 2019-12-05 | 50.233  | -12.273 | 1.1     |
|             | 19:57:02   | 00:17:35   |         |         |         |
| TRE         | 2019-12-04 | 2019-12-04 | 120.000 | -40.909 | <0.1    |
|             | 20:09:17   | 20:15:33   |         |         |         |
| TRE         | 2019-12-04 | 2019-12-04 | 125.455 | -40.909 | <0.1    |
|             | 20:22:32   | 20:28:54   |         |         |         |
| TRE         | 2019-12-04 | 2019-12-04 | 38.571  | 16.364  | <0.1    |
|             | 20:34:53   | 20:41:14   |         |         |         |
| TRE         | 2019-12-04 | 2019-12-04 | 45.000  | -4.091  | 0.4     |
|             | 20:54:02   | 21:00:18   |         |         |         |
| TRE         | 2019-12-04 | 2019-12-04 | 130.909 | -40.909 | <0.1    |
|             | 21:06:59   | 21:13:20   |         |         |         |
| TRE         | 2019-12-04 | 2019-12-04 | 92.727  | -40.909 | <0.1    |
|             | 22:16:26   | 22:22:42   |         |         |         |
| TRE         | 2019-12-04 | 2019-12-04 | 82.286  | -36.818 | 12.4    |
|             | 22:41:57   | 22:48:13   |         |         |         |
| TRE         | 2019-12-04 | 2019-12-04 | 72.973  | -32.727 | 14.4    |
|             | 23:07:43   | 23:14:04   |         |         |         |
| TRE         | 2019-12-04 | 2019-12-04 | 63.000  | -24.545 | 0.6     |
|             | 23:26:41   | 23:32:57   |         |         |         |
| TRE         | 2019-12-04 | 2019-12-04 | 54.419  | -12.273 | 0.4     |
|             | 23:52:11   | 23:58:33   |         |         |         |
+-------------+------------+------------+---------+---------+---------+

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 84% of the cumulative probability of the 
BAYESTAR skymap created on 2019-12-04 18:02:07 (UTC).


The coverage map is available at: 
https://grandma-owncloud.lal.in2p3.fr/index.php/s/PqlwSoGEclSr2VJ

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
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[3] K. Noysena et al., ApJ 2019, arXiv:1910.02770
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Y. G. Zheng, C. Cai, 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 
S191204r event (GCN #26334
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 ), trigger time 2019-12-04T17:15:26.092 UTC. 
At T0, about 4% 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=218.29 deg, DEC=65.30 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:   1.4e-07 erg cm^-2
10 s:  8.9e-07 erg cm^-2

Band model 2 (alpha=-1.0, beta=-2.3, Ep=230 keV):
1 s:   1.7e-07 erg cm^-2
10 s:  1.3e-06 erg cm^-2

Band model 3 (alpha=-0.0, beta=-1.5, Ep=1000 keV):
1 s:   3.6e-07 erg cm^-2
10 s:  2.3e-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.

AUTHORS: A. Grado (INAF-Napoli), E. Cappellaro (INAF-Padova), F. Getman
(INAF-Napoli), E. Brocato (INAF-Abruzzo), S. Covino (INAF-Brera),
L. Nicastro (INAF-OAS),  F. Onori (IAPS), S. Piranomonte (INAF-OARm)
on behalf of GRAWITA.

We observed the field of the gravitational wave event S191204r (GCN
circular #26334
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 ) in r' band with the VLT Survey Telescope (VST) equipped
with Omegacam (1 square degree FOV) (Proposal ID ESO 0104.D-0049).
We secured three epochs distributed in time as reported in the following
table where the last column contains the average FWHM in arcsec.

epoch 1 2019-12-05 from 01:18:13.867 to 02:52:28.862 1.05
epoch 2 2019-12-05 from 07:28:59.733 to 09:03:39.067 1.29
epoch 3 2019-12-06 from 01:46:07.055 to 03:28:14.961 0.7

all time are in UTC.

Individual epoch covers 20 square degrees enclosing ~ 60% of the
localization probability region.
Each one square degree pointing is the coaddition of three dithered
exposures for a total exposure time of 135 seconds.
Weather conditions were good in particular in the last epoch where the
FWHM reached a lower value < 0.5".

Automatic VST data processing was done with the VSTTube pipeline
(Grado et al. 2012 Mem.SAIt 19, 362).
Transient search is in progress.
We acknowledge excellent support from the ESO User Support Department
and from ESO observing staff in Paranal.

AUTHORS: E. Cappellaro, N. Elias-Rosa (INAF-Padova), A. Grado, F. Getman
(INAF-Napoli), P. D'Avanzo, A. Melandri (INAF-OABr) L. Nicastro (INAF-OAS),
E. Brocato (INAF-Abruzzo), on behalf of GRAWITA.

We report the results of the observation of the field of the gravitational
wave event S191204r (GCN circular #26334
Loading...
 
 ) obtained with the VLT Survey
Telescope (VST) equipped with Omegacam (described in GCN 26334
Loading...
 
 , Proposal
ID ESO 0104.D-0049).

Images were analised using our image difference pipelines (Brocato et al.
2018 MNRAS, 474,1).
As reference images we used DECAM archive images retrieved from
https://datalab.noao.edu/sia/des_dr1.
The final vetting was done via visual inspection.
We detected the following three interesting candidates:

Name   |  RA                | Dec            |      MJD     | Mag

VSTJ044435.43-332755.7 | 04:44:35.432 | -33:27:55.69 | 58222.081 | 21.5 +/-
0.1
VSTJ051111.58-373132.0 | 05:11:11.576 | -37:31:32.04 | 58822.079 | 20.6 +/-
0.1
VSTJ051052.17-335413.9 | 05:10:52.168 | -33:54:13.95 | 58823.140 | 22.2 +/-
0.2

The transients were detected at multiple epochs. Here we report epoch and
magnitude for the brightest detection.

All the transients appear projected near a galaxy. In particular
GWd_S191205r_12093 is located 7.4 arcsec from the nucleus of GLADE131392
which distance is 178Mpc (GLADE catalog).
The small distance appears to exclude that this transient is related to
the GW event.

-- 
Too short? See why http://www.emailcharter.org/
<<<<<<<<<<<<<<<<<<<<>>>>>>>>>>>>>>>>>>>>>

Aniello Grado, PhD

Ricercatore Astronomo
INAF- Osservatorio Astronomico di Capodimonte
Via Moiariello 16 80131 Napoli
ITALIA
Tel: 0039 0815575547
Fax: 0039 0815575433

<<<<<<<<<<<<<<<<<<<<>>>>>>>>>>>>>>>>>>>>>

E. Cappellaro, N. Elias-Rosa (INAF-Padova), A. Grado, F. Getman (INAF-Napoli), P. D'Avanzo, A. Melandri (INAF-OABr), L. Nicastro (INAF-OAS), G. Greco (Univ. Urbino), E. Brocato (INAF-Abruzzo), on behalf of GRAWITA.

We realised that the text of GCN 26390
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  was submitted while still incomplete. The correct text is the following:

We report the results of the observation of the field of the gravitational wave event S191204r (GCN 26334
Loading...
 
 ) obtained with the VLT Survey Telescope (VST) equipped with Omegacam (described in GCN 26334
Loading...
 
 , Proposal ID ESO 0104.D-0049). Images were analised using our image difference pipelines (Brocato et al. 2018 MNRAS, 474,1). As reference images we used DECAM archive images retrieced from https://datalab.noao.edu/sia/des_dr1 <https://datalab.noao.edu/sia/des_dr1>. The final vetting was done via visual inspection. We detected the following three interesting candidates:

Name    |  RA   |  Dec   |   MJD   |   Mag 
VSTJ044435.43-332755.7 | 04:44:35.432 | -33:27:55.69 | 58222.081 | 21.5 +/- 0.1
VSTJ051111.58-373132.0  | 05:11:11.576 | -37:31:32.04 | 58822.079 | 20.6 +/- 0.1
VSTJ051052.17-335413.9 | 05:10:52.168 | -33:54:13.95 | 58823.140 | 22.2 +/- 0.2

The transients were detected at multiple epochs. Here we report epoch and magnitude for the brightest detection. All the transients appear projected near a galaxy. In particular VSTJ051111.58-373132.0 is located 7.4 arcsec from the nucleus of GLADE131392 which distance is 178Mpc (GLADE catalog). The small distance appears to exclude that this transient is related to the GW event.

For the other two galaxies the distance is unknown. In the next days, a fourth observation epoch with the VST is scheduled to check for the transient luminosity evolution.

We apologise for any confusion.

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 S191204r (2019-12-04 17:15:26.092 UTC, hereafter T0;
LIGO/Virgo Collaboration GCN Circ. 26334
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 ).

No triggered KW GRBs happened between ~2 days before and ~14 days
after T0. The closest waiting-mode GRB was observed ~11 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 7.7x10^-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 1.9x10^-7 erg/cm^2/s (20 - 1500 keV, 2.944 s scale).

All the quoted values are preliminary.