LIGO/Virgo S200129m

The LIGO Scientific Collaboration and the Virgo Collaboration report:

We identified the compact binary merger candidate S200129m during
real-time processing of data from LIGO Hanford Observatory (H1), LIGO
Livingston Observatory (L1), and Virgo Observatory (V1) at 2020-01-29
06:54:58.435 UTC (GPS time: 1264316116.435). The candidate was found
by the GstLAL [1], CWB [2], PyCBC Live [3], MBTAOnline [4], and SPIIR [5]
analysis pipelines.

Some scattering noise could be seen around the time of the event in
Virgo data; follow-up studies are on-going. We will update the localization if
warranted by offline analysis.

S200129m is an event of interest because its false alarm rate, as
estimated by the online analysis, is 6.7e-32 Hz, or about one in 1e23
years. The event's properties can be found at this URL:
https://gracedb.ligo.org/superevents/S200129m

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
[6], distributed via GCN notice about 4 minutes after the candidate
event time.
 * bayestar.fits.gz,1, an initial localization generated by BAYESTAR
[6], distributed via GCN notice about 13 minutes after the candidate
event time.

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 53 deg2.
Marginalized over the whole sky, the a posteriori luminosity distance
estimate is 908 +/- 202 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] Nitz et al. PRD 98, 024050 (2018)
 [4] Adams et al. CQG 33, 175012 (2016)
 [5] Qi Chu, PhD Thesis, The University of Western Australia (2017)
 [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 S200129m
 in a time range of 1000 seconds [3] centered on the alert event time
(2020-01-29 06:46:38.435 UTC to 2020-01-29 07:03:18.435 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
S200129m 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 S200129m ranges from 0.029 to 0.044 GeV cm^-2 in a 1000 second
time window.

The IceCube Neutrino Observatory is a cubic-kilometer neutrino detector
operating at the geographic South Pole, Antarctica. The IceCube realtime
alert point of contact can be reached at roc@icecube.wisc.edu<mailto:roc@icecube.wisc.edu>


[1] Bartos et al. arXiv:1810.11467
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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)

LIGO/Virgo S200129m: No counterpart candidates in INTEGRAL SPI-ACS
prompt observationFrancesca Onori (IAPS, Italy), Sergey Molkov (IKI, Moscow)
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-collaborationUsing
INTEGRAL/SPI-ACS realtime data (following [1]) we have performed
a search for a prompt gamma-ray counterpart of S200129m (GCN 26926
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 ).At the
time of the event (2020-01-29 06:54:58 UTC, hereafter T0),
INTEGRAL was operating in nominal mode. The peak of the event
localization probability was at an angle of 112 deg with respect to
the spacecraft pointing axis. This orientation implies strongly
suppressed (5% of optimal) response of ISGRI, somewhat
suppressed (44% of optimal) response of IBIS/Veto, and strongly
suppressed (37% 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 4.5e-07 erg/cm^2 (within the
50% probability containment region of the source localization) for a
burst lasting less than 1s 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 300s 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 ~4.1e-07 (1.3e-07)
erg/cm^2/s at 1s (8s) time scale in 75-2000 keV energy range.For the mean
reported distance 908.0 Mpc this corresponds to the limit
on the total isotropic equivalent energy in 1s of 4.5e+49 erg for
the short GRB spectrum and for a long GRB spectrum isotropic
equivalent luminosity in 1s (8s) of 3.7e+49 erg/s (1.3e+49 erg/s)We report
for completeness and in order of FAP, all excesses
identified in the search region. We find: 1 possibly associated
excess:T-T0 | scale | S/N | luminosity ( x 1e+49 erg/s) | FAP
-1.52 | 0.1 | 4.2 | 20.7 +/- 4.89 +/- 6.38 | 0.03944 likely background
excesses:T-T0 | scale | S/N | luminosity ( x 1e+49 erg/s) | FAP
-16.2 | 1.95 | 3.4 | 3.88 +/- 1.09 +/- 1.2 | 0.0685
-38.6 | 0.5 | 3.8 | 8.01 +/- 2.16 +/- 2.48 | 0.344
25.7 | 0.15 | 4.4 | 17.8 +/- 3.98 +/- 5.51 | 0.373
-121 | 0.4 | 4.2 | 10.3 +/- 2.42 +/- 3.18 | 0.775Note 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

-- 
Dr. Francesca Onori
Postdoctoral Researcher
IAPS, via Fosso del Cavaliere, 100, 00133 - Rome, Italy
e-mail: francesca.onori@inaf.it
Tel: +39 06 45488128

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 S200129m at 2020-01-29 06:54:58.435 UTC (GCN 26926
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 ). 

At the trigger time of S200129m, the high-voltage of MAXI/GSC was off, 
and it was turned on at T0+195 sec (+3.3 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 07:06:13 to 07:11:43 UTC (T0+675 to T0+1005 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. Pittori, F. Verrecchia (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 (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 S200129m at T0 = 2020-01-29 06:54:58.435
(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 S200129m 90% c.l. localization region was accessible to the
AGILE MCAL. 3-sigma upper limits (ULs) are obtained for a 1 s integration time at
different celestial positions within the accessible S200129m localization region,
from a minimum of 1.3E-06 erg cm^-2 to a maximum of 2.7E-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.

C. Pittori, F. Verrecchia (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 (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 S200129m at T0 = 2020-01-29
06:54:58.435 (UT) 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) (due to solar panel constraints).

We performed an analysis of the GRID data in the energy range 50 MeV -
10 GeV over time intervals before and after T0, where good exposure of the
S200129m 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 8.3e-07 to 9.1e-06 erg cm^-2 s^-1, with exposure of about 51% of the LR over
the time interval ( T0 + 100s ; T0 + 200s );

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,  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-Tunka robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the LIGO/Virgo S200129m errorbox  15067 sec after trigger time at 2020-01-29 11:06:05 UT, with upper limit up to  16.4 mag. Observations started at twilight.  The observations began at zenith distance = 74 deg. The sun  altitude  is -11.8 deg. 

The galactic latitude b = -29 deg., longitude l = 56 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/ligo_1.php?id=11295

We obtain a following upper limits.  

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

   15157 | 2020-01-29 11:06:05 |        MASTER-Tunka | (21h 12m 26.71s , +12d 10m 03.5s) |   C |   180 | 14.1 |        
   15402 | 2020-01-29 11:10:09 |        MASTER-Tunka | (21h 12m 30.70s , +12d 11m 17.9s) |   C |   180 | 15.2 |        
   15903 | 2020-01-29 11:18:31 |        MASTER-Tunka | (21h 14m 27.13s , +14d 09m 07.8s) |   C |   180 | 16.4 |        
   16115 | 2020-01-29 11:22:03 |        MASTER-Tunka | (20h 38m 50.12s , +22d 10m 14.8s) |   C |   180 | 15.9 |        
Filter C is a clear (unfiltred) band. 


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

A. Goldstein (USRA) reports on behalf of the Fermi-GBM Team and the
GBM-LIGO/Virgo group:

For S200129m and using the bayestar.fits.gz,1 skymap, Fermi-GBM did not
observe any of the localization probability at event time due to Earth
occultation. Therefore, the GBM observations are not constraining for
prompt gamma-ray emission.

M. Axelsson (KTH & Stockholm Univ.), F. Longo (University and INFN,  
Trieste), M. Kovacevic (INFN Perugia), E. Bissaldi (Politecnico & INFN  
Bari), D. Kocevski (NASA/MSFC), N. Omodei (Stanford Univ.) and M.  
Arimoto (Kanazawa University) report on behalf of the Fermi-LAT  
Collaboration:

We have searched data collected by the Fermi Large Area Telescope  
(LAT) on January 29, 2020, for possible high-energy (E > 100 MeV)  
gamma-ray emission in spatial/temporal coincidence with the LIGO/Virgo  
trigger S200129m (GCN 26926
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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. At the time of the trigger (T0 =  
2020-01-29 06:54:58.435 UTC), no part of the LIGO probability map was  
observable by Fermi-LAT. The region entered the LAT field of view  
around T0 + 3 ks, and 100% cumulative coverage was reached after ~8.8  
ks.

We performed a search for a transient counterpart within the observed  
region of the 90% contour of LIGO map in a fixed time window from T0 +  
3 ks to T0 + 10 ks. No significant new 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 for the fixed time interval between 100 MeV  
and 1 GeV for this search vary between 2.9e-10 and 7.1e-10 [erg/cm^2/s].

The Fermi-LAT point of contact for this event is Makoto Arimoto  
(arimoto@se.kanazawa-u.ac.jp)

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.

David O. Cook (Caltech/IPAC), Angela Van Sistine (UW Milwaukee), Leo Singer (NASA/GSFC), Igor Andreoni (Caltech), Michael Coughlin (Caltech), Bob Aloisi (UW Milwaukee), Patrick R. Brady (UW Milwaukee), Rick Ebert (Caltech/IPAC), George Helou (Caltech/IPAC), David Kaplan (UW Milwaukee), Mansi M. Kasliwal (Caltech), Joseph M. Mazzarella (Caltech/IPAC), and Marion Schmitz (Caltech/IPAC)

On behalf of the Global Relay of Observatories Watching Transients Happen (GROWTH) collaboration and the NASA/IPAC Extragalactic Database (NED) Team.

We spatially cross-matched the LIGO/Virgo S200129m trigger sky localization with the galaxies in NED and found 909 galaxies within the 90% containment. Due to the large number of candidates in this volume, we provide here the top 20 (out of 252) galaxies located in the 50% volume sorted by 2MASS absolute K-band magnitude. 

For an extended list of galaxies in the 90% volume go to the NED Gravitational Wave Followup service at https://ned.ipac.caltech.edu/uri/NED::GWF/. This service provides downloadable galaxy lists and visualizations for candidate host galaxies. For each GW alert, these products are automatically generated and made available within minutes to expedite efficient electromagnetic followup observations. 


         objname               ra      dec    DistMpc k_m_k20fe    M_Ks     dP_dV  
---------------------------- -------- -------- ------- --------- ---------- --------
2MASX J21112414+0730549 317.8505  7.5152  885.09    13.093 -26.641947 3.91e-07
2MASX J21153810+0154415 318.9088  1.9116  948.02    13.333 -26.551079 3.40e-07
2MASX J21075194+0554019 316.9664  5.9004  757.87    12.925 -26.472973 1.69e-07
2MASX J21185415+0124556 319.7257  1.4155  976.72    13.498  -26.45084 2.08e-07
2MASX J21103552+0750027 317.6480  7.8342  833.18    13.163 -26.440691 3.93e-07
2MASX J21155885+0200085 318.9952  2.0024  938.12    13.421 -26.440298 3.70e-07
2MASX J21143195+0414596 318.6333  4.2500  919.87    13.418 -26.400635 6.34e-07
2MASX J21094540+0607107 317.4393  6.1197  714.28    12.901 -26.368343 3.20e-07
2MASX J21162901+0410260 319.1210  4.1739  949.09    13.546  -26.34054 3.98e-07
2MASX J21164905+0117390 319.2043  1.2943  996.72    13.672 -26.320866 2.38e-07
2MASX J21145876+0432013 318.7448  4.5338  872.70    13.384 -26.320324 5.53e-07
2MASX J21135815+0637355 318.4923  6.6264  832.72     13.32 -26.282505 2.63e-07
2MASX J21145735+0527483 318.7390  5.4633  846.10    13.389 -26.248108 3.80e-07
2MASX J21082698+0811032 317.1124  8.1842  629.96    12.818  -26.17855 2.09e-07
2MASX J21104382+0450527 317.6825  4.8479  811.92    13.412  -26.13556 4.01e-07
2MASX J21141482+0644183 318.5617  6.7384  884.61    13.632 -26.101768 2.27e-07
2MASX J21103115+0658277 317.6298  6.9744  774.34    13.354 -26.090672 4.70e-07
2MASX J21114509+0726560 317.9379  7.4488  779.98    13.413 -26.047419 3.54e-07
2MASX J21080192+0652462 317.0081  6.8794  749.31    13.341  -26.03231 2.62e-07
2MASX J21172667+0309342 319.3611  3.1595  947.08    13.862 -26.019924 3.69e-07


Table: Top 20 galaxies in NED that fall in the 90% probability volume for S200129m sorted by 2MASS absolute K-band magnitude. Column descriptions are as follows. name: galaxy name. ra: RA (J2000, decimal degrees). dec: Dec (J2000, decimal degrees). distmpc: galaxy distance (Mpc). k_m_k20fe: the 2MASS apparent magnitude. M_Ks: the absolute K-band magnitude derived using the 'DistMpc' column. dP_dV: the 3D probability density per cubic megaparsec at the position of each galaxy.

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:

We report the search results in the BAT data within T0 +/- 100 s of the
LVC event S200129m (LIGO/VIRGO Collaboration GCN Circ. 26926
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 ),
where T0 is the LVC trigger time (2020-01-29T06:54:58.435 UTC).

The center of the BAT field of view (FOV) at T0 is
RA = 73.019 deg,
DEC = 49.562 deg,
and the roll angle is 287.138 deg.
The BAT FOV (>10% partial coding) covers 0.00% of the integrated
LVC localization probability, and 0.00% of the galaxy convolved
probability (Evans et al. 2016). Note that the sensitivity in the BAT FOV
changes with the partial coding fraction. Please see the BAT FOV figure
in the summary page (link below) for the specific location of the LVC
region relative to the BAT FOV.

Within T0 +/- 100 s, no significant 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 large structure
seen ~T-250 s to ~T-50 is due to noisy detectors.

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 ~ 1.75e-07 x 10^-7 erg/s/cm^2.
The flux limit calculation for this event only uses light curves from
T0 +/- 50 s to exclude the interval with the large noise structure.
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 ~ 54.32 Mpc.

Event data are available from T0-44.83 s to T0+45.21 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.

BAT retains decreased, but significant, sensitivity to rate increases for
gamma-ray events outside of its FOV. About 100.00% 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/S200129m/web/source_public.html

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:

At the trigger time of the compact binary merger candidate 
S200129m T0 = 2020-01-29 06:54:58.435 UT (The LIGO 
Scientific Collaboration and Virgo Collaboration, GCN 
Circ. 26926
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 ), the CALET Gamma-ray Burst Monitor (CGBM)
high voltages were off (from T0-31 min to T0+1 min).

The CALET Calorimeter (CAL) was operating in the high 
energy trigger mode at the trigger time of S200129m. 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 5.7 x 10^-5 erg/cm^2/s (10-100 GeV) 
when the summed LIGO-Virgo probability reaches 5%. The CAL 
FOV was centered at RA = 288.7 deg, DEC = -34.3 deg at T0.

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 S200129m (2020-01-29 06:54:58.435 UTC, hereafter T0;
LIGO/Virgo Collaboration GCN Circ. 26926
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 ).

No triggered KW GRBs happened between ~3 days before and ~1 day
after T0. The closest waiting-mode GRB was observed ~23 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 7.9x10^-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 2.0x10^-7 erg/cm^2/s (20 - 1500 keV, 2.944 s scale).

All the quoted values are preliminary.

Y. G. Zheng, C. Cai, Y. F. Du, W. C. Xue, 
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 
S200129m event (GCN #26926
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 ), trigger time 2020-01-29T06:54:58.435 UTC. 
At T0, about 97% 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=318.34 deg, DEC=4.57 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:   8.1e-08 erg cm^-2
10 s:  3.5e-07 erg cm^-2

Band model 2 (alpha=-1.0, beta=-2.3, Ep=230 keV):
1 s:   1.4e-07 erg cm^-2
10 s:  6.1e-07 erg cm^-2

Band model 3 (alpha=-0.0, beta=-1.5, Ep=1000 keV):
1 s:   5.4e-07 erg cm^-2
10 s:  1.9e-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.