LIGO/Virgo S200112r

LIGO/Virgo S200112r: Identification of a GW compact binary merger candidate

The LIGO Scientific Collaboration and the Virgo Collaboration report:

We identified the compact binary merger candidate S200112r during
real-time processing of data from LIGO Livingston Observatory (L1) and
Virgo Observatory (V1) at 2020-01-12 15:58:38.094 UTC (GPS time:
1262879936.094). The candidate was found by the GstLAL [1] analysis
pipeline.

S200112r is an event of interest because its false alarm rate, as
estimated by the online analysis, is 1.3e-11 Hz, or about one in 1e3
years. The event's properties can be found at this URL:
https://gracedb.ligo.org/superevents/S200112r

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%.

Two 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
[2], distributed via GCN notice about 2 minutes after the candidate
event time.
 ��* bayestar.fits.gz,1�� -- identical to bayestar.fits.gz,0

The preferred sky map at this time is bayestar.fits.gz,1. For the
bayestar.fits.gz,1 sky map, the 90% credible region is 6199 deg2.
Marginalized over the whole sky, the a posteriori luminosity distance
estimate is 1136 +/- 320 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] 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
S200112r
 in a time range of 1000 seconds [3] centered on the alert event time
(2020-01-12 15:50:18.094 UTC to 2020-01-12 16:06:58.094 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
S200112r calculated from the map circulated in the 3-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 S200112r ranges from 0.029 to 0.930 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)

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,  D. Cheryasov
(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 S200112r errorbox  223 sec after trigger time at 2020-01-12 16:02:21 UT, with upper limit up to  17.6 mag. The observations began at zenith distance = 76 deg. The sun  altitude  is -61.3 deg. 

The galactic latitude b = -14 deg., longitude l = 35 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/ligo_1.php?id=11211

We obtain a following upper limits.  

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

     243 | 2020-01-12 16:02:21 |         MASTER-Amur | (15h 49m 38.40s , +39d 01m 12.7s) |   C |    40 | 16.0 |        
     308 | 2020-01-12 16:03:20 |         MASTER-Amur | (15h 49m 38.58s , +39d 01m 51.2s) |   C |    50 | 16.1 |        
     382 | 2020-01-12 16:04:30 |         MASTER-Amur | (15h 49m 38.51s , +39d 00m 17.2s) |   C |    60 | 16.2 |        
     462 | 2020-01-12 16:05:49 |         MASTER-Amur | (15h 49m 41.99s , +39d 01m 46.9s) |   C |    60 | 15.6 |        
    1818 | 2020-01-12 16:27:26 |         MASTER-Amur | (17h 13m 19.61s , +51d 59m 49.8s) |   C |   180 | 16.9 |        
    2031 | 2020-01-12 16:30:58 |         MASTER-Amur | (15h 51m 14.18s , +44d 01m 04.0s) |   C |   180 | 16.9 |        
    2245 | 2020-01-12 16:34:33 |         MASTER-Amur | (16h 13m 40.13s , +54d 00m 14.5s) |   C |   180 | 17.5 |        
    2460 | 2020-01-12 16:38:08 |         MASTER-Amur | (17h 13m 24.34s , +52d 00m 30.0s) |   C |   180 | 17.0 |        
    2673 | 2020-01-12 16:41:41 |         MASTER-Amur | (17h 26m 22.02s , +51d 58m 50.4s) |   C |   180 | 16.8 |        
    2889 | 2020-01-12 16:45:17 |         MASTER-Amur | (15h 51m 15.54s , +44d 02m 13.6s) |   C |   180 | 17.0 |        
    3101 | 2020-01-12 16:48:48 |         MASTER-Amur | (16h 02m 16.42s , +44d 01m 10.6s) |   C |   180 | 17.0 |        
    3313 | 2020-01-12 16:52:20 |         MASTER-Amur | (16h 13m 35.41s , +54d 02m 05.0s) |   C |   180 | 17.5 |        
    3525 | 2020-01-12 16:55:53 |         MASTER-Amur | (16h 27m 16.53s , +54d 00m 56.3s) |   C |   180 | 17.6 |        
Filter C is a clear (unfiltred) band. 


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 S200112r event using the 90% contour of the Initial GW_SKYMAP probability
map provided by the GW interferometers (GCN#26715
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  <https://gcn.gsfc.nasa.gov/gcn3/26715.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/S200112r_Initial.png <http://antares.in2p3.fr/GW/S200112r_Initial.png>.
Considering the location probability provided by the LIGO/Virgo collaborations, there is a
38.4% 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 2020-01-12 15:58:38 and in the 90% contour of the S200112r
event. The expected number of atmospheric background events in the region visible by ANTARES is
2.34e-03 in the +/- 500s time window. An extended search during +/- 1 hour gives no
up-going muon neutrino coincidence. The expected number of atmospheric background events in the
region visible by ANTARES is 1.68e-02 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.

The HAWC Collaboration (https://www.hawc-observatory.org) reports:

The HAWC Collaboration performed a follow-up of the gravitational wave
trigger S200112r (GCN #26715
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 ). At the time of the trigger the HAWC
local zenith was oriented towards (RA, Dec) = (253.8 deg, 19.0 deg).
48% of the GW candidate sky location probability fell within our
observable field of view (0-45 deg zenith angle).

We performed a search for a short timescale emission using 6 sliding
time windows (dt = 0.3s, 1s, 3s, 10s, 30s and  100s), shifted forward
in time by 20% of their width. We searched the 95% probability
containment area in a timescale-dependent time period, from t0-5dt to
t0+10dt, where t0 is the time of the GW trigger.

No significant gamma-ray detection above the background was observed.

The sensitivity of this analysis is greatly dependent on zenith angle,
ranging from 0.0 deg to 45.0 deg for the area searched in this
analysis. The 5sigma detection sensitivity to a 1s (100s) burst in the
80-800GeV energy range goes from 1.2e-06 erg/cm^2 to 1.1e-04 erg/cm^2
(6.4e-06 erg/cm^2 to 5.0e-04 erg/cm^2), depending on the zenith
angle.

HAWC is a TeV gamma ray water Cherenkov array located in the state of
Puebla, Mexico. It is sensitive to the energy range ~0.1-100TeV, and
monitors 2/3 of the sky every day with an instantaneous field-of-view
of ~2 sr.

M. Serino, S. Sugita (AGU), 
N. Kawai (Tokyo Tech), H. Negoro (Nihon U.), 
M. Nakajima, W. Maruyama, M. Aoki, K. Kobayashi, R. Takagi (Nihon U.), 
T. Mihara, 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 S200112r at 2020-01-12 15:58:38.094 UTC (GCN 26715
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 ). 

At the trigger time of S200112r, the high-voltage of MAXI/GSC was on. 
The instantaneous field of view of GSC at the GW trigger time covered 3% of the 90% credible region 
of the bayestar sky map, in which we found no significant new X-ray source. 
The first one-orbit (92 min) scan observation with GSC after the event covered 96% 
of the 90% credible region of the bayestar skymap from 15:58:38 to 17:30:33 UTC (T0+0 to T0+5515 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.

Alexis Coleiro (APC, France), Carlo Ferrigno (ISDC/UniGE, Switzerland),
V. Savchenko (ISDC/UniGE, Switzerland),
S. Mereghetti (INAF IASF-Milano, Italy),
J. Rodi (IAPS-Roma, Italy)
on behalf of the INTEGRAL multi-messenger collaboration:
https://www.astro.unige.ch/cdci/integral-multimessenger-collaboration

The INTEGRAL spacecraft has a highly elliptical orbit and the
instruments are not acquiring science data during perigee passage,
every 2.6 days to prevent radiation-induced damages. Unfortunately, at
the time of the S200112r (2020-01-12 15:58:38) the spacecraft was
preparing to the start the observations after the perigee passage
between the orbits number 2182 and 2183 and no scientific instrument
data are available between 2020-01-12T08:15:40 and
2020-01-12T18:14:13.

C. Casentini (INAF/IAPS), F. Verrecchia (SSDC, and INAF/OAR), M. Tavani
(INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, G. Piano, A. Ursi
(INAF/IAPS), F. Lucarelli, C. Pittori (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 S200112r at T0 = 2020-01-12 15:58:38
(UT), a preliminary analysis of the AGILE minicalorimeter (MCAL) triggered
data found no event candidates within a time interval covering -/+ 15 s
from the LIGO/Virgo T0.

At the T0, about 70% of the S200112r 90 % c.l. localization region (LR) 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 S200112r LR, from a minimum of 1.42E-06 erg cm^-2 to a maximum
of 7.90E-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.

A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (NASA/GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
A. P. Beardmore (U. Leicester), M. G. Bernardini (INAF-OAB),
A. A. Breeveld (MSSL-UCL), D. N. Burrows (PSU),
S. Campana (INAF-OAB), S. B. Cenko (NASA/GSFC),
G. Cusumano (INAF-IASF PA), A. D'Ai (INAF-IASFPA),
P. D'Avanzo (INAF-OAB), V. D'Elia (ASI-ASDC), S. Emery (UCL-MSSL),
P. A. Evans (U. Leicester), P. Giommi (ASI), C. Gronwall (PSU),
D. Hartmann (Clemson U.), J. A. Kennea (PSU),
N. Klingler (PSU), H. A. Krimm (NSF),
N. P. M. Kuin (UCL-MSSL), F. E. Marshall (NASA/GSFC),
A. Melandri (INAF-OAB), J. A. Nousek (PSU),
S. R. Oates (U. of Birmingham), 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 (U. Toronto),
E. Troja (NASA/GSFC/UMCP) report on behalf of the Swift team:

Around the trigger time (T0) of LIGO/Virgo S200112r
(LIGO/VIRGO Collaboration GCN Circ. 26715
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 ),
Swift/BAT was in the South Atlantic Anomaly (SAA)
from T0-246 s to T0+858 s. Therefore, no science data
were collected during this time.

The BAT summary page is at
https://swift.gsfc.nasa.gov/results/BATbursts/team_web/S200112r/web/source_public.html

F. Verrecchia (SSDC, and INAF/OAR), C. Casentini (INAF/IAPS), M. Tavani
(INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, G. Piano, A. Ursi
(INAF/IAPS), F. Lucarelli, C. Pittori (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 S200112r at T0 = 2020-01-12
15:58:38.094 UTC a preliminary analysis of the AGILE exposure at T0 shows
that the Gamma-Ray Imaging Detector (GRID) exposure covered the 28% of the
90% c.l. localization region (LR) (11% of the 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 S200112r 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 7.4e-07 to 6e-06 erg cm^-2 s^-1, with exposure of about 28% of the LR
over the time interval ( T0 -2s ; T0 + 2s );
from 3.0e-07 to 9.1e-06 erg cm^-2 s^-1, with exposure of about 27% of the LR
over the time interval ( T0s ; T0 + 10s );
from 7.7e-08 to 1e-05 erg cm^-2 s^-1, with exposure of about 36% 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.

D. Kocevski (NASA/MSFC) and J. Wood (NASA/MSFC) report on behalf of the Fermi-GBM Team and the GBM-LIGO/Virgo group


At the time of S200112r, Fermi was passing through the South Atlantic Anomaly from 5 minutes prior to 23 minutes after the trigger time; therefore the GBM detectors were disabled.

D. Kocevski (NASA/MSFC) and J. Wood (NASA/MSFC) report on behalf of the Fermi-GBM Team and the GBM-LIGO/Virgo group

At the time of S200112r, Fermi was passing through the South Atlantic Anomaly from 5.1 minutes prior to 23.5 minutes after the trigger time; therefore the GBM detectors were disabled.

C. Cai, W. C. Xue, 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 
S200112r event (GCN #26715
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 ), trigger time 2020-01-12T15:58:38.094 UTC. 
At T0, about 41% 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=45 deg, DEC=-45 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:   2.2e-07 erg cm^-2
10 s:  6.5e-07 erg cm^-2

Band model 2 (alpha=-1.0, beta=-2.3, Ep=230 keV):
1 s:   3.0e-07 erg cm^-2
10 s:  8.4e-07 erg cm^-2

Band model 3 (alpha=-0.0, beta=-1.5, Ep=1000 keV):
1 s:   4.0e-07 erg cm^-2
10 s:  1.1e-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.

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:

The CALET Gamma-ray Burst Monitor (CGBM) was operating at the trigger
time of S200112r T0 = 2020-01-12 15:58:38.094 UT (The LIGO Scientific
Collaboration and Virgo Collaboration, GCN Circ.26715
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 ).

No CGBM on-board trigger occurred around the event time. Based on the
LIGO-Virgo localization sky map, the summed LIGO probabilities inside
the CGBM HXM (7 - 3000 keV) and SGM (40 keV - 28 MeV) fields of view
are 10 % and 41 %, respectively (and 70 % credible region of the
initial sky map was above the horizon).  The HXM and SGM fields of
view were centered at RA = 75.2 deg, Dec = +47.3 deg and RA = 84.6 
deg, Dec =  +40.0 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 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 S200112r. 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 in the
overwrap region with the LIGO-Virgo high probability localization
region. 

The 90% upper limit of CAL is 1.1 x 10^-6 erg/cm^2/s (10-100 GeV) 
when the summed LIGO-Virgo probability reaches 5%.
The CAL FOV was centered at RA= 84.7 deg, DEC= +40.0 deg at T0.

P. Hello (IJCLab), S. Antier (APC), M. Blazek (HETH/IAA-CSIC), E. Howell,
(OzGrav-UWA), S. Karpov (FZU), M. Masek (FZU), M. Prouza (FZU), M. Boer
(Artemis), N. Christensen (Artemis), L. Eymar (Artemis), A. Klotz (IRAP),
K. Noysena (Artemis, IRAP), A. Coleiro (APC), D. Corre (IJCLab), M. 
Coughlin
(UMinn), D. Coward (OzGrav-UWA), J.G. Ducoin (IJCLab), B. Gendre
(OzGrav-UWA), D. A. Kann (HETH/IAA-CSIC), N. Kochiashvili (Iliauni),
C. Lachaud (APC), N. Leroy (IJCLab), C. Thoene (HETH/IAA-CSIC), D. Turpin
(AIM-CEA), X. Wang (THU)

report on behalf of the FRAM, TAROT and GRANDMA collaborations.

We performed tiled observations of LIGO/Virgo S200112r event (#GCN26715) 
with the
FRAM-Auger, FRAM-CTA-N, TAROT-Calern (TCA), TAROT-Chili (TCH), TAROT-
Reunion (TRE) telescopes.

FRAM-Auger is located at Pierre Auger Observatory. FRAM-CTA-N is
located at Observatorio del Roque de los Muchachos. TCA is located at
Calern site at the Cote d'Azur observatory. TCH is located at La Silla
ESO observatory (LaS/ESO). TRE is located at Les Makes astronomical
observatory.

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 limiting magnitude (AB mag) for a
given exposure in seconds (s).

+-------------+---------+----------+-------------+------------+
| Telescope | Delay | Filter | f.o.v. | Limiting |
| | [min] | | [deg] | Mag. |
|-------------+---------+----------+-------------+------------|
| FRAM-Auger | 568 | R | 1.0 x 1.0 | 18.0 (60s) |
| FRAM-CTA-N | 812 | R | 0.45 x 0.45 | 17.0 (90s) |
| TCA | 88 | Clear | 1.9 x 1.9 | 18.0 (60s) |
| TCH | 516 | Clear | 1.9 x 1.9 | 18.0 (60s) |
| TRE | 17 | 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 | 2020-01-13 | 2020-01-13 | 37.969 | -46.216 | <0.1 |
| | 01:26:25 | 01:28:25 | | | |
| FRAM-Auger | 2020-01-13 | 2020-01-13 | 35.156 | -46.216 | <0.1 |
| | 01:36:33 | 01:38:33 | | | |
| FRAM-Auger | 2020-01-13 | 2020-01-13 | 34.483 | -45.243 | <0.1 |
| | 01:44:04 | 01:46:04 | | | |
| FRAM-Auger | 2020-01-13 | 2020-01-13 | 42.152 | -31.622 | <0.1 |
| | 01:51:49 | 01:56:18 | | | |
| FRAM-Auger | 2020-01-13 | 2020-01-13 | 33.103 | -45.243 | <0.1 |
| | 01:56:56 | 02:01:26 | | | |
| FRAM-Auger | 2020-01-13 | 2020-01-13 | 48.987 | -31.622 | <0.1 |
| | 02:02:06 | 02:06:34 | | | |
| FRAM-Auger | 2020-01-13 | 2020-01-13 | 44.430 | -31.622 | <0.1 |
| | 02:07:13 | 02:11:45 | | | |
| FRAM-Auger | 2020-01-13 | 2020-01-13 | 46.709 | -31.622 | <0.1 |
| | 02:14:48 | 02:16:48 | | | |
| FRAM-Auger | 2020-01-13 | 2020-01-13 | 35.862 | -45.243 | <0.1 |
| | 02:17:27 | 02:21:55 | | | |
| FRAM-Auger | 2020-01-13 | 2020-01-13 | 39.375 | -46.216 | <0.1 |
| | 02:22:32 | 02:27:00 | | | |
| FRAM-Auger | 2020-01-13 | 2020-01-13 | 36.562 | -46.216 | <0.1 |
| | 02:32:41 | 02:37:10 | | | |
| FRAM-Auger | 2020-01-13 | 2020-01-13 | 38.571 | -47.189 | <0.1 |
| | 06:12:04 | 06:16:32 | | | |
| FRAM-Auger | 2020-01-13 | 2020-01-13 | 40.000 | -45.243 | <0.1 |
| | 06:17:09 | 06:21:37 | | | |
| FRAM-Auger | 2020-01-13 | 2020-01-13 | 37.241 | -45.243 | <0.1 |
| | 06:27:19 | 06:29:19 | | | |
| FRAM-Auger | 2020-01-13 | 2020-01-13 | 42.188 | -46.216 | <0.1 |
| | 06:32:25 | 06:36:53 | | | |
| ----- | ----- | ----- | ----- | ----- | ----- |
| FRAM-CTA-N | 2020-01-13 | 2020-01-13 | 254.426 | 52.215 | <0.1 |
| | 05:30:11 | 05:34:17 | | | |
| FRAM-CTA-N | 2020-01-13 | 2020-01-13 | 255.396 | 52.215 | <0.1 |
| | 05:34:32 | 05:38:37 | | | |
| FRAM-CTA-N | 2020-01-13 | 2020-01-13 | 264.621 | 48.720 | <0.1 |
| | 06:09:16 | 06:13:22 | | | |
| FRAM-CTA-N | 2020-01-13 | 2020-01-13 | 265.287 | 46.973 | <0.1 |
| | 06:13:37 | 06:17:43 | | | |
| FRAM-CTA-N | 2020-01-13 | 2020-01-13 | 261.758 | 48.720 | <0.1 |
| | 06:17:59 | 06:22:04 | | | |
| FRAM-CTA-N | 2020-01-13 | 2020-01-13 | 267.199 | 46.973 | <0.1 |
| | 06:22:21 | 06:26:27 | | | |
| FRAM-CTA-N | 2020-01-13 | 2020-01-13 | 264.000 | 47.734 | <0.1 |
| | 06:26:47 | 06:30:53 | | | |
| FRAM-CTA-N | 2020-01-13 | 2020-01-13 | 265.522 | 47.734 | <0.1 |
| | 06:31:08 | 06:35:14 | | | |
| FRAM-CTA-N | 2020-01-13 | 2020-01-13 | 266.449 | 46.973 | <0.1 |
| | 06:35:29 | 06:39:35 | | | |
| FRAM-CTA-N | 2020-01-13 | 2020-01-13 | 263.849 | 48.720 | <0.1 |
| | 06:39:55 | 06:44:01 | | | |
| FRAM-CTA-N | 2020-01-13 | 2020-01-13 | 264.761 | 47.734 | <0.1 |
| | 06:44:16 | 06:48:21 | | | |
| FRAM-CTA-N | 2020-01-13 | 2020-01-13 | 263.077 | 48.720 | <0.1 |
| | 06:48:42 | 06:52:48 | | | |
| FRAM-CTA-N | 2020-01-13 | 2020-01-13 | 257.154 | 52.215 | <0.1 |
| | 06:53:04 | 06:57:10 | | | |
| FRAM-CTA-N | 2020-01-13 | 2020-01-13 | 256.219 | 52.215 | <0.1 |
| | 06:57:30 | 07:01:36 | | | |
| FRAM-CTA-N | 2020-01-13 | 2020-01-13 | 259.808 | 50.468 | <0.1 |
| | 07:01:52 | 07:05:58 | | | |
| FRAM-CTA-N | 2020-01-13 | 2020-01-13 | 274.497 | 40.419 | <0.1 |
| | 07:15:59 | 07:20:05 | | | |
| FRAM-CTA-N | 2020-01-13 | 2020-01-13 | 270.348 | 44.788 | <0.1 |
| | 07:20:21 | 07:24:27 | | | |
| FRAM-CTA-N | 2020-01-13 | 2020-01-13 | 269.622 | 44.788 | <0.1 |
| | 07:24:41 | 07:28:47 | | | |
| FRAM-CTA-N | 2020-01-14 | 2020-01-14 | 272.034 | 42.604 | <0.1 |
| | 07:04:31 | 07:08:37 | | | |
| ----- | ----- | ----- | ----- | ----- | ----- |
| TCA | 2020-01-12 | 2020-01-14 | 242.021 | 55.692 | 0.3 |
| | 17:26:11 | 01:53:38 | | | |
| TCA | 2020-01-12 | 2020-01-14 | 238.807 | 55.692 | 0.3 |
| | 17:33:00 | 02:00:23 | | | |
| TCA | 2020-01-12 | 2020-01-12 | 271.571 | 42.703 | 0.5 |
| | 17:58:44 | 18:05:03 | | | |
| TCA | 2020-01-12 | 2020-01-13 | 269.035 | 44.558 | 0.5 |
| | 18:05:25 | 04:02:13 | | | |
| TCA | 2020-01-12 | 2020-01-14 | 250.181 | 53.837 | 0.4 |
| | 18:29:11 | 18:05:32 | | | |
| TCA | 2020-01-12 | 2020-01-14 | 261.737 | 50.125 | 0.5 |
| | 18:36:00 | 18:12:20 | | | |
| TCA | 2020-01-12 | 2020-01-14 | 258.903 | 50.125 | 0.4 |
| | 18:42:45 | 18:19:04 | | | |
| TCA | 2020-01-12 | 2020-01-13 | 254.720 | 51.981 | 0.4 |
| | 23:48:36 | 17:25:18 | | | |
| TCA | 2020-01-12 | 2020-01-14 | 231.847 | 42.703 | 0.2 |
| | 23:55:26 | 01:01:30 | | | |
| TCA | 2020-01-13 | 2020-01-14 | 236.812 | 42.703 | 0.2 |
| | 00:02:10 | 01:08:17 | | | |
| TCA | 2020-01-13 | 2020-01-13 | 240.145 | 40.847 | 0.2 |
| | 00:34:07 | 05:40:39 | | | |
| TCA | 2020-01-13 | 2020-01-13 | 237.728 | 40.847 | 0.2 |
| | 01:00:17 | 01:06:36 | | | |
| TCA | 2020-01-13 | 2020-01-14 | 239.295 | 42.703 | 0.2 |
| | 01:12:55 | 02:19:33 | | | |
| TCA | 2020-01-13 | 2020-01-13 | 243.303 | 38.991 | 0.1 |
| | 01:32:24 | 04:09:00 | | | |
| TCA | 2020-01-13 | 2020-01-13 | 234.329 | 42.703 | 0.2 |
| | 02:38:39 | 05:14:31 | | | |
| TCA | 2020-01-13 | 2020-01-14 | 247.104 | 53.837 | 0.3 |
| | 02:51:05 | 01:27:42 | | | |
| TCA | 2020-01-13 | 2020-01-14 | 229.364 | 42.703 | 0.2 |
| | 02:57:51 | 01:34:30 | | | |
| TCA | 2020-01-13 | 2020-01-14 | 268.303 | 46.414 | 0.6 |
| | 03:36:29 | 02:12:53 | | | |
| TCA | 2020-01-13 | 2020-01-14 | 262.768 | 48.270 | 0.4 |
| | 05:14:54 | 01:20:53 | | | |
| TCA | 2020-01-13 | 2020-01-14 | 226.881 | 42.703 | 0.1 |
| | 23:10:37 | 01:46:50 | | | |
| ----- | ----- | ----- | ----- | ----- | ----- |
| TCH | 2020-01-13 | 2020-01-14 | 55.054 | -29.525 | 0.2 |
| | 00:34:04 | 06:40:38 | | | |
| TCH | 2020-01-13 | 2020-01-14 | 50.892 | -30.000 | 0.2 |
| | 00:40:47 | 06:47:21 | | | |
| TCH | 2020-01-13 | 2020-01-15 | 38.407 | -29.525 | 0.2 |
| | 00:47:32 | 02:53:21 | | | |
| TCH | 2020-01-13 | 2020-01-15 | 64.509 | -29.050 | 0.2 |
| | 01:19:27 | 03:26:00 | | | |
| TCH | 2020-01-13 | 2020-01-15 | 52.925 | -39.959 | <0.1 |
| | 01:26:12 | 03:32:46 | | | |
| TCH | 2020-01-13 | 2020-01-15 | 44.649 | -29.525 | 0.2 |
| | 01:32:57 | 01:09:01 | | | |
| TCH | 2020-01-13 | 2020-01-15 | 38.845 | -47.232 | <0.1 |
| | 01:59:10 | 01:35:31 | | | |
| TCH | 2020-01-13 | 2020-01-15 | 34.863 | -45.414 | <0.1 |
| | 02:05:57 | 01:42:16 | | | |
| TCH | 2020-01-13 | 2020-01-15 | 37.472 | -45.414 | <0.1 |
| | 02:12:42 | 01:49:00 | | | |
| TCH | 2020-01-13 | 2020-01-15 | 32.254 | -45.414 | <0.1 |
| | 02:25:12 | 02:01:31 | | | |
| TCH | 2020-01-13 | 2020-01-15 | 40.080 | -45.414 | <0.1 |
| | 02:31:57 | 02:08:15 | | | |
| TCH | 2020-01-13 | 2020-01-15 | 33.431 | -47.232 | <0.1 |
| | 02:38:41 | 02:15:00 | | | |
| TCH | 2020-01-13 | 2020-01-15 | 40.488 | -30.000 | 0.2 |
| | 02:51:08 | 02:27:38 | | | |
| TCH | 2020-01-13 | 2020-01-14 | 57.135 | -29.050 | 0.2 |
| | 02:57:52 | 06:33:53 | | | |
| TCH | 2020-01-13 | 2020-01-15 | 42.569 | -29.525 | 0.2 |
| | 03:36:28 | 00:43:06 | | | |
| TCH | 2020-01-13 | 2020-01-15 | 34.245 | -29.525 | 0.1 |
| | 03:43:00 | 03:19:14 | | | |
| TCH | 2020-01-14 | 2020-01-15 | 52.973 | -29.525 | 0.2 |
| | 04:23:50 | 03:00:05 | | | |
| TCH | 2020-01-14 | 2020-01-15 | 36.326 | -29.525 | 0.1 |
| | 04:30:35 | 03:06:50 | | | |
| ----- | ----- | ----- | ----- | ----- | ----- |
| TRE | 2020-01-12 | 2020-01-12 | 40.645 | -45.000 | 0.4 |
| | 16:15:26 | 16:21:48 | | | |
| TRE | 2020-01-12 | 2020-01-13 | 29.032 | -45.000 | 0.3 |
| | 16:34:18 | 17:31:27 | | | |
| TRE | 2020-01-12 | 2020-01-13 | 38.182 | -40.909 | 0.3 |
| | 16:47:31 | 17:44:45 | | | |
| TRE | 2020-01-12 | 2020-01-13 | 38.919 | -32.727 | 0.6 |
| | 16:59:53 | 17:57:02 | | | |
| TRE | 2020-01-12 | 2020-01-13 | 43.636 | -40.909 | 0.3 |
| | 17:13:05 | 18:10:09 | | | |
| TRE | 2020-01-12 | 2020-01-13 | 46.452 | -45.000 | 0.4 |
| | 17:25:23 | 18:22:33 | | | |
| TRE | 2020-01-12 | 2020-01-13 | 46.286 | -36.818 | 0.4 |
| | 17:38:35 | 18:35:50 | | | |
| TRE | 2020-01-12 | 2020-01-13 | 51.429 | -36.818 | 0.4 |
| | 17:50:56 | 18:48:08 | | | |
| TRE | 2020-01-12 | 2020-01-13 | 58.378 | -32.727 | 0.8 |
| | 18:04:05 | 19:01:20 | | | |
| TRE | 2020-01-12 | 2020-01-12 | 34.054 | -32.727 | 0.4 |
| | 18:23:06 | 18:29:27 | | | |
| TRE | 2020-01-12 | 2020-01-13 | 56.571 | -36.818 | 0.4 |
| | 18:54:59 | 19:52:13 | | | |
| TRE | 2020-01-12 | 2020-01-13 | 107.586 | 8.182 | 0.1 |
| | 19:07:57 | 20:05:10 | | | |
| TRE | 2020-01-12 | 2020-01-13 | 34.839 | -45.000 | 0.4 |
| | 20:59:38 | 17:05:58 | | | |
| TRE | 2020-01-12 | 2020-01-13 | 43.784 | -32.727 | 0.7 |
| | 21:12:49 | 17:19:10 | | | |
| TRE | 2020-01-12 | 2020-01-12 | 44.211 | -49.091 | 0.2 |
| | 21:31:32 | 21:37:53 | | | |
| TRE | 2020-01-12 | 2020-01-12 | 53.514 | -32.727 | 1.0 |
| | 21:44:45 | 21:51:07 | | | |
| TRE | 2020-01-12 | 2020-01-12 | 56.842 | -49.091 | <0.1 |
| | 22:48:03 | 22:54:24 | | | |
| TRE | 2020-01-12 | 2020-01-14 | 108.837 | 12.273 | 0.2 |
| | 23:26:26 | 00:32:46 | | | |
| TRE | 2020-01-13 | 2020-01-13 | 36.000 | -36.818 | 0.2 |
| | 19:07:14 | 19:13:36 | | | |
| TRE | 2020-01-13 | 2020-01-13 | 60.779 | -28.636 | 0.9 |
| | 19:20:29 | 19:26:44 | | | |
| TRE | 2020-01-13 | 2020-01-13 | 27.273 | -40.909 | 0.2 |
| | 19:32:51 | 19:39:12 | | | |
| TRE | 2020-01-14 | 2020-01-14 | 63.158 | -49.091 | <0.1 |
| | 16:04:44 | 16:08:52 | | | |
+-------------+------------+------------+---------+---------+---------+

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.

These observations cover about 16.8% of the cumulative probability of
the LALInference skymap created on 2020-01-14 16:10:00
(UTC).


The coverage map is available at:
https://grandma-
owncloud.lal.in2p3.fr/index.php/s/XgtMhPRxcyL09gR/download?path=%2F&files=GRANDMA_S200112r_1579179387.png

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, https://doi.org/10.1093/mnras/stz2485
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[2] S. Antier et al., MNRAS 2019, https://doi.org/10.1093/mnras/stz3142
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[3] K. Noysena et al., ApJ 2019, arXiv:1910.02770
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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 S200112r (2020-01-12 15:58:38.094 UTC, hereafter T0;
LIGO/Virgo Collaboration GCN Circ. 26715
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 ).

No triggered KW GRBs happened ~3 hours before and ~1.5 days
after T0. Using waiting-mode data within the interval T0 +/- 100 s,
we found no significant (> 5 sigma) excess over the background
in both KW detectors on temporal scales from 2.944 s to 100 s.

We estimate an upper limit (90% conf.) on the 20 - 1500 keV fluence
to 9.3x10^-7 erg/cm^2 for a burst lasting less than 2.944 s and having a
typical KW short GRB spectrum (an exponentially cut off power law with
alpha =-0.5 and Ep=500 keV). For a typical long GRB spectrum (the Band
function with alpha=-1, beta=-2.5, and Ep=300 keV), the corresponding
limiting peak flux is 2.8x10^-7 erg/cm^2/s (20 - 1500 keV, 2.944 s scale).

All the quoted values are preliminary.

V. Shenoy (IITB), 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 S200112r (UTC 2020-01-12 15:58:38, GraceDB event). We use the LALInference.fits.gz,0 map (https://gracedb.ligo.org/api/superevents/S200112r/files/LALInference.fits.gz,0) for our analysis. 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 the BBH merger, Astrosat's nominal pointing is RA,DEC = 14:22:34.1, 32:20:01.5 (215.6421,32.3338), which is ~83 deg away from the maximum probability location, which severely reduces the effective area of CZTI. At the time of the BBH merger event, the Earth-satellite-transient angle corresponding to maximum probability location is ~72 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 0.78 (78%).

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= 1.86e-05 ergs/cm^2/s; fluence limit = 1.86e-06 ergs/cm^2
1.0 s: flux limit= 5.60e-06 ergs/cm^2/s; fluence limit = 5.60e-06 ergs/cm^2
10.0 s: flux limit= 7.00e-07 ergs/cm^2/s; fluence limit = 7.00e-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.