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LIGO/Virgo S200208q

GCN Circular 27014

Subject
LIGO/Virgo S200208q: Identification of a GW compact binary merger candidate
Date
2020-02-08T13:35:30Z (5 years ago)
From
Leo Singer at GSFC <leo.p.singer@nasa.gov>
The LIGO Scientific Collaboration and the Virgo Collaboration report:

We identified the compact binary merger candidate S200208q during
real-time processing of data from LIGO Hanford Observatory (H1), LIGO
Livingston Observatory (L1), and Virgo Observatory (V1) at 2020-02-08
13:01:17.991 UTC (GPS time: 1265202095.991). The candidate was found
by the MBTAOnline [1], CWB [2], PyCBC Live [3], and SPIIR [4] analysis
pipelines.

S200208q is an event of interest because its false alarm rate, as
estimated by the online analysis, is 2.5e-09 Hz, or about one in 12
years. The event's properties can be found at this URL:
https://gracedb.ligo.org/superevents/S200208q

The classification of the GW signal, in order of descending
probability, is BBH (>99%), Terrestrial (<1%), BNS (<1%), NSBH (<1%),
or MassGap (<1%).

Assuming the candidate is astrophysical in origin, the probability
that the lighter compact object has a mass < 3 solar masses (HasNS) is
<1%. Using the masses and spins inferred from the signal, the
probability of matter outside the final compact object (HasRemnant) is
<1%.

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
[5], distributed via GCN notice about 3 minutes after the candidate
event time.
 * bayestar.fits.gz,1, an initial localization generated by BAYESTAR
[5], distributed via GCN notice about 9 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 1120 deg2.
Marginalized over the whole sky, the a posteriori luminosity distance
estimate is 2900 +/- 960 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] Adams et al. CQG 33, 175012 (2016)
 [2] Klimenko et al. PRD 93, 042004 (2016)
 [3] Nitz et al. PRD 98, 024050 (2018)
 [4] Qi Chu, PhD Thesis, The University of Western Australia (2017)
 [5] Singer & Price PRD 93, 024013 (2016)

GCN Circular 27015

Subject
LIGO/Virgo S200208q: Upper limits from IceCube neutrino searches
Date
2020-02-08T13:36:29Z (5 years ago)
From
Raamis Hussain at IceCube <raamis.hussain@icecube.wisc.edu>
IceCube Collaboration (http://icecube.wisc.edu/) reports:

Searches [1,2] for track-like muon neutrino events detected by IceCube
consistent with the sky localization of gravitational-wave candidate
S200208q
 in a time range of 1000 seconds [3] centered on the alert event time
(2020-02-08 12:52:57.991 UTC to 2020-02-08 13:09:37.991 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
S200208q 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 S200208q ranges from 0.032 to 0.701 GeV cm^-2 in a 1000 second
time window.

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


[1] Bartos et al. arXiv:1810.11467 (2018) and Countryman et
al.arXiv:1901.05486 (2019)
[2] PoS(ICRC2019)918 and Braun et al., Astroparticle Physics 29, 299 (2008)
[3] Baret et al., Astroparticle Physics 35, 1 (2011)

GCN Circular 27016

Subject
LIGO/Virgo S200208q : no neutrino counterpart candidate in ANTARES search
Date
2020-02-08T14:42:27Z (5 years ago)
From
Thierry Pradier at ANTARES/IPHC/U of Strasbourg <tpradier@km3net.de>
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 S200208q event using the 90% contour of the Preliminary probability
map provided by the GW interferometers (GCN#27014 <https://gcn.gsfc.nasa.gov/gcn3/27014.gcn3>). The ANTARES visibility at the time of the
alert, together with the 50% and 90% contours of the probability map are shown at http://antares.in2p3.fr/GW/S200208q_Preliminary.png <http://antares.in2p3.fr/GW/S200208q_Preliminary.png>.
Considering the location probability provided by the LIGO/Virgo collaborations, there is a
68.5% 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 2020-02-08 13:01:17 and in the 90% contour of the S200208q
event. The expected number of atmospheric background events in the region visible by ANTARES is
3.29e-04 in the +/- 500s time window. An extended search during +/- 1 hour gives no
up-going muon neutrino coincidence. The expected number of atmospheric background events in the
region visible by ANTARES is 2.37e-03 in this larger time window.

ANTARES is the largest undersea neutrino detector, installed in the Mediterranean Sea, and it is
primarily sensitive to neutrinos in the TeV-PeV  energy range. At 10 TeV, the median angular
resolution for muon neutrinos is about 0.5 degrees. In the range 1-100 TeV ANTARES has a
competitive sensitivity to this position in the sky.

GCN Circular 27017

Subject
LIGO/Virgo S200208q: No counterpart candidates in HAWC observations
Date
2020-02-08T15:15:55Z (5 years ago)
From
Hugo Ayala at Pennsylvania State University <hgayala@psu.edu>
The HAWC Collaboration (https://www.hawc-observatory.org) reports:

The HAWC Collaboration performed a follow-up of the gravitational wave
trigger S200208q. At the time of the trigger the HAWC
local zenith was oriented towards (RA, Dec) = (235.9 deg, 19.1 deg).
29% of the GW candidate sky location probability fell within our
observable field of view (0-45 deg zenith angle).

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

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

The sensitivity of this analysis is greatly dependent on zenith angle,
ranging from 28.4deg to 45.0deg for the area searched in this
analysis. The 5sigma detection sensitivity to a 1s (100s) burst in the
80-800GeV energy range goes from 5.2e-06 erg/cm^2 to 1.1e-04 erg/cm^2
(2.6e-05 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.

GCN Circular 27018

Subject
LIGO/Virgo S200208q: Global MASTER-Net observations report
Date
2020-02-08T15:54:10Z (5 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  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 S200208q errorbox  9684 sec after trigger time at 2020-02-08 15:42:41 UT, with upper limit up to  16.7 mag. The observations began at zenith distance = 48 deg. The sun  altitude  is -49.0 deg. 

The galactic latitude b = 10 deg., longitude l = 263 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/ligo_1.php?id=11306

We obtain a following upper limits.  

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

    9774 | 2020-02-08 15:42:41 |        MASTER-Tunka | (18h 08m 02.18s , +80d 05m 28.4s) |   C |   180 | 16.7 |        
Filter C is a clear (unfiltred) band. 


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

GCN Circular 27019

Subject
LIGO/Virgo S200208q: No counterpart candidates in INTEGRAL SPI-ACS prompt observation
Date
2020-02-08T15:54:25Z (5 years ago)
From
Sergey Molkov at Space Research Inst., Moscow <molkov@iki.rssi.ru>
Sergey Molkov (IKI, Moscow), James Rodi (IAPS-Roma, Italy),
V. Savchenko, C. Ferrigno (ISDC/UniGE, Switzerland)
A. Coleiro (APC, France)
S. Mereghetti (INAF IASF-Milano, Italy)
on behalf of the INTEGRAL multi-messenger collaboration:
https://www.astro.unige.ch/cdci/integral-multimessenger-collaboration

Using INTEGRAL/SPI-ACS realtime data (following [1]) we have performed
a search for a prompt gamma-ray counterpart of S200208q (GCN 27014).

At the time of the event (2020-02-08 13:01:17 UTC, hereafter T0),
INTEGRAL was operating in nominal mode. The peak of the event
localization probability was at an angle of 88 deg with respect to the
spacecraft pointing axis. This orientation implies strongly suppressed
(12% of optimal) response of ISGRI, strongly suppressed (28% of
optimal) response of IBIS/Veto, and somewhat suppressed (66% 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 2.3e-07 erg/cm^2 (within the
50% probability containment region of the source localization) for a
burst lasting less than 1 s with a characteristic short GRB spectrum
(an exponentially cut off power law with alpha=-0.5 and Ep=600 keV)
occurring at any time in the interval within 300 s around T0. For a
typical long GRB spectrum (Band function with alpha=-1, beta=-2.5, and
Ep=300 keV), the derived peak flux upper limit is ~2e-07 (5.9e-08)
erg/cm^2/s at 1 s (8 s) time scale in 75-2000 keV energy range.

For the mean reported distance 2900.0 Mpc this corresponds to the
limit on the total isotropic equivalent energy in 1 s of 2.3e+50 erg
for the short GRB spectrum and for a long GRB spectrum isotropic
equivalent luminosity in 1 s (8 s) of 1.7e+50 erg/s (5.9e+49 erg/s)

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

T-T0 | scale | S/N | luminosity ( x 1e+50 erg/s) | FAP
-77 | 3.1 | 4 | 18.1 +/- 4.84 +/- 6.97 | 0.0803
-35.1 | 0.65 | 3.7 | 3.75 +/- 1.06 +/- 1.44 | 0.255

Note that FAP estimates (especially at timescales above 2s) may be
possibly further affected by enhanced non-stationary local background
noise. This list excludes any excesses for which FAP is close to
unity.

All results quoted are preliminary.

This circular is an official product of the INTEGRAL Multi-Messenger
team.

[1] Savchenko et al. 2017, A&A 603, A46

[2] Savchenko et al. 2012, A&A 541A, 122S

GCN Circular 27020

Subject
LIGO/Virgo S200208q: upper limits from AGILE/MCAL observations
Date
2020-02-08T17:02:13Z (5 years ago)
From
Francesco Longo at U of Trieste,INFN Trieste <franzlongo1969@gmail.com>
F. Longo (Univ. Trieste, and INFN Trieste), M. Cardillo (INAF/IAPS),
M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), C. Casentini,
G. Piano, 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 S200208q at T0 = 2020-02-08
13:01:17.991 (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 S200208q 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 S200208q localization
region, from a minimum of 1.4E-06 erg cm^-2 to a maximum of 6.6E-06
erg cm^-2 (assuming as spectral model a single power law with
photon index 1.5).

The AGILE-MCAL detector is a CsI detector with a 4 pi FoV,
sensitive in the energy range 0.4-100 MeV.
Additional analysis of AGILE data is in progress.

GCN Circular 27021

Subject
LIGO/Virgo S200208q : upper limits from AGILE/GRID observations
Date
2020-02-08T17:52:26Z (5 years ago)
From
Francesco Longo at U of Trieste,INFN Trieste <franzlongo1969@gmail.com>
M. Cardillo (INAF/IAPS), F. Longo (Univ. Trieste, and INFN Trieste),
M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), C. Casentini,
G. Piano, 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 S200208q at T0 = 2020-02-08
13:01:17.991 (UTC) a preliminary analysis of the AGILE exposure at T0
shows that the Gamma-Ray Imaging Detector (GRID) exposure covered
the 37% of the 90% c.l. localization region (LR).

We performed an analysis of the GRID data in the energy range 50 MeV -
10 GeV on T0, where good exposure of the S200208q 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 7.0e-08 to 7.4e-06 erg cm^-2 s^-1, with exposure of about 72% of
the LR over the time interval ( T0s ; T0 + 100s );

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

GCN Circular 27022

Subject
LIGO/Virgo S200208q: Upper limits from Fermi-GBM Observations
Date
2020-02-08T22:20:42Z (5 years ago)
From
Suraj Poolakkil at UAH <sp0076@uah.edu>
S. Poolakkil (UAH) reports on behalf of the Fermi-GBM Team and the
GBM-LIGO/Virgo group.

For S200208q and using the bayestar.fits.gz,1 skymap, Fermi-GBM was
observing
95.4% of the localization probability at event time.

There was no Fermi-GBM onboard trigger around the event time of the
LIGO/Virgo detection of GW trigger S200208q (GCN 27014). An
automated, blind search for short gamma-ray bursts below the onboard
triggering threshold in Fermi-GBM also identified no counterpart
candidates. The GBM targeted search, the most sensitive, coherent search
for GRB-like signals, was run from +/-30 s around merger time, and also
identified no counterpart candidates.

Part of the LVC localization region is behind the Earth for Fermi, located
at RA=306.6, Dec=17.6 with a radius of 67.3 degrees. We therefore set upper
limits on impulsive gamma-ray emission for the LVC localization region
visible to Fermi at merger time. Using the representative soft, normal, and
hard GRB-like templates described in arXiv:1612.02395, we set the following
3 sigma flux upper limits over 10-1000 keV, weighted by GW localization
probability (in units of 10^-7 erg/s/cm^2):

Timescale  soft norm hard
--------------------------
0.128 s:   7.3  9.9  17.
1.024 s:   2.3  2.9  6.0
8.192 s:   0.6  0.9  2.2

Assuming the median luminosity distance of 2900 Mpc from the GW detection,
we estimate the following intrinsic luminosity upper limits over the 1
keV-10 MeV energy range (in units of 10^50 erg/s):

Timescale  Soft     Normal   Hard
------------------------------------
0.128s:    11.6     13.7    39.8
1.024s:    3.6      4.0     14.0
8.192s:    1.0      1.4     5.1

GCN Circular 27023

Subject
LIGO/Virgo S200208q: no counterpart candidates in the Swift/BAT observations
Date
2020-02-08T22:47:19Z (5 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
D. M. Palmer (LANL), S. D. Barthelmy (NASA/GSFC),
A. Y. Lien (GSFC/UMBC), T. Sakamoto (AGU),
A. P. Beardmore (U. Leicester), M. G. Bernardini (INAF-OAB),
A. A. Breeveld (MSSL-UCL), D. N. Burrows (PSU),
S. Campana (INAF-OAB), S. B. Cenko (NASA/GSFC),
G. Cusumano (INAF-IASF PA), A. D'Ai (INAF-IASFPA),
P. D'Avanzo (INAF-OAB), V. D'Elia (ASI-ASDC), S. Emery (UCL-MSSL),
P. A. Evans (U. Leicester), P. Giommi (ASI), C. Gronwall (PSU),
D. Hartmann (Clemson U.), J. A. Kennea (PSU),
N. Klingler (PSU), H. A. Krimm (NSF),
N. P. M. Kuin (UCL-MSSL), F. E. Marshall (NASA/GSFC),
A. Melandri (INAF-OAB), J. A. Nousek (PSU),
S. R. Oates (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 S200208q (LIGO/VIRGO Collaboration GCN Circ. 27014),
where T0 is the LVC trigger time (2020-02-08T13:01:17.991 UTC).

The center of the BAT field of view (FOV) at T0 is
RA = 256.575 deg,
DEC = -40.369 deg,
and the roll angle is 92.479 deg.
The BAT FOV (>10% partial coding) covers 0.00% of the integrated
LVC localization probability. Note that the sensitivity in the BAT FOV
changes with the partial coding fraction. Please see the BAT FOV figure
in the summary page (link below) for the specific location of the LVC
region relative to the BAT FOV.

Within T0 +/- 100 s, no significant detections (signal-to-noise ratio
>~ 5 sigma) are found in the BAT raw light curves with time bins of 64 ms,
1 s, and 1.6 s. Assuming an on-axis (100% coded) short GRB with a typical
spectrum in the BAT energy range (i.e., a simple power-law model with a
power-law index of -1.32, Lien & Sakamoto et al. 2016), the 5-sigma upper
limit in the 1-s binned light curve corresponds to a flux upper
limit (15-350 keV) of ~ 7.70 x 10^-8 erg/s/cm^2.
Assuming a luminosity of ~ 2 x 10^47 erg/s (similar to GW170817)
and an average Epeak of ~ 400 keV for short GRBs (Bhat et al. 2016),
this flux upper limit corresponds to a distance of ~ 81.88 Mpc.

Event data are available from T0-45.46 s to T0+44.61 s and
from T0+98.54 to T0+101.56. 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 81.00% 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/S200208q/web/source_public.html

GCN Circular 27024

Subject
LIGO/Virgo S200208q: Coverage and upper limits from MAXI/GSC observations
Date
2020-02-08T23:55:38Z (5 years ago)
From
Hitoshi Negoro at Nihon U <negoro.hitoshi@nihon-u.ac.jp>
H. Negoro (Nihon U.), N. Kawai (Tokyo Tech), 
S. Sugita, M. Serino (AGU),
M. Nakajima, W. Maruyama, M. Aoki, K. Kobayashi, 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 S200208q at 2020-02-08 13:01:17.991 UTC (GCN 27014).

At the trigger time of S200208q, the high-voltage of MAXI/GSC was on.
The instantaneous field of view of GSC at the GW trigger time covered 1% 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 63%
of the 90% credible region of the bayestar skymap from 13:01:17 to 14:11:25 UTC (T0+0 to T0+4208 sec).

No significant new source was found in the region in the one-orbit scan observation.
A typical 1-sigma averaged upper limit obtained in one scan observation
is 20 mCrab at 2-20 keV.

If you require information about X-ray flux by MAXI/GSC at specific coordinates,
please contact the submitter of this circular by email.

GCN Circular 27028

Subject
LIGO/Virgo S200208q: No counterpart candidates in Fermi-LAT observations
Date
2020-02-09T22:25:19Z (5 years ago)
From
Lorenzo Scotton at CNRS/IN2P3/LUPM <lorenzoscotton@live.it>
L. Scotton (CNRS/IN2P3/LUPM), D. Tak (Univ. of Maryland & NASA/GSFC),
M. Axelsson (KTH & Stockholm Univ), E. Bissaldi (Politecnico & INFN Bari),
D. Kocevski (NASA/MSFC), N. Omodei (Stanford Univ.) and F. Longo (University and INFN, Trieste)

report on behalf of the Fermi-LAT Collaboration:

We have searched data collected by the Fermi Large Area Telescope (LAT) on
February 8, 2020, for possible high-energy (E > 100 MeV) gamma-ray emission in
spatial/temporal coincidence with the LIGO/Virgo trigger S200208q (GCN 27014).

We define "instantaneous coverage" as the integral over the region of the LIGO
probability map that is within the LAT field of view at a given time, and "cumulative
coverage" as the integral of the instantaneous coverage over time. Fermi-LAT had
an instantaneous coverage of ~47% of the LIGO probability at the time of the trigger
(T0 = 2020-02-08 13:01:17.991 UTC), and reached 100% cumulative coverage
after ~3.8 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 to T0 + 10 ks.
No significant new sources are found.

Energy flux upper bounds for the fixed time interval between 100 MeV and 1 GeV
for this search vary between 1.3e-10 and 2.5e-09 [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.

GCN Circular 27030

Subject
LIGO/Virgo S200208q: Not observable by CALET
Date
2020-02-11T05:53:50Z (5 years ago)
From
Yuta Kawakubo at Louisiana State U./CALET <kawakubo1@lsu.edu>
P. S. Marrocchesi (U of Siena),
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), 
M. L. Cherry (LSU), S. Ricciarini (U of Florence),
and the CALET collaboration:

At the trigger time of the compact binary merger candidate S200208q,
T0 = 2020-02-08 13:01:17.991 UT (The LIGO Scientific Collaboration 
and Virgo Collaboration, GCN Circ. 27014), the CALET Gamma-ray 
Burst Monitor (CGBM) high voltages were off (from T0-19 min to 
T0+13 min).

The CALET Calorimeter (CAL) was operating in the high energy trigger
mode at the trigger time of S200208q. 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
was no significant overlap with the LVC high probability localization 
region at T0+-60 sec.  The CAL FOV was centered at RA = 224.1 deg, 
Dec= -41.8 deg at T0.

GCN Circular 27033

Subject
LIGO/Virgo S200208q: No counterpart candidates in KAIT observations
Date
2020-02-11T08:24:51Z (5 years ago)
From
Weikang Zheng at UC Berkeley <weikang@berkeley.edu>
James Sunseri, Yukei Murakami, WeiKang Zheng, and Alexei V. Filippenko
(UC Berkeley) report on behalf of the Lick/KAIT GW follow-up team:

The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, observed the 90% region of the gravitational-wave
event S200208q (GCN 27014) detected by LIGO/Virgo. More than
one thousand galaxies were selected from the Glade catalog V1.0
(Dalya et al., 2018, MNRAS, 479, 2374; http://aquarius.elte.hu/glade/)
according to their priority score. KAIT observed 115 of them based on
their priority scores and elevation visibility, with each clear-filter
exposure time being 60 s. The first image was taken at 09:03:56, Feb.
09th UT, about 20 hours after the trigger, and the last image at
12:34:44 UT. Our typical limiting mag is 18.0. No viable counterparts
were identified and the analysis is ongoing. A full list of galaxies
observed by KAIT is given below.

GladeID   UT(Feb09)  RA_J2000   Dec_J2000
-----------------------------------------------
G0611504  09:03:56  12:39:33.1495  +10:58:03.7164
G0704258  09:06:17  12:52:19.5336  +13:21:29.6604
G0284556  09:07:33  13:01:32.7722  +18:48:30.978
G0618945  09:08:42  13:03:24.4262  +20:11:49.0776
G0675119  09:09:52  13:03:46.5857  +19:16:17.0616
G0727874  09:13:34  13:29:21.4123  +37:24:50.1444
G0195216  09:14:43  13:34:32.4792  +37:35:15.2376
G0801463  09:15:52  13:35:35.1854  +40:06:40.122
G0603678  09:17:02  13:41:42.1949  +40:52:28.0344
G0697332  09:18:11  13:43:40.5689  +41:41:44.6892
G0595963  09:19:20  13:44:41.521   +40:28:02.7624
G0637326  09:20:46  13:50:14.7583  +56:02:32.9712
G0721271  09:22:03  13:52:38.5913  +46:20:59.1036
G0663946  09:23:23  13:53:54.1442  +57:10:05.6892
G0739375  09:24:33  13:55:00.564   +53:59:42.1044
G0747150  09:25:53  13:55:01.355   +45:50:06.684
G1817667  09:27:02  13:55:53.76    +43:29:52.44
G0568505  09:28:21  13:56:14.425   +55:43:23.0448
G1123852  09:29:36  13:56:37.0934  +49:14:49.0416
G1326493  09:30:46  13:56:37.9394  +53:14:13.0344
G0821694  09:31:55  13:56:56.7151  +53:51:59.1156
G0755125  09:33:04  13:58:02.0544  +53:01:01.7148
G0766898  09:34:14  13:58:31.6478  +49:32:23.7156
G0617024  09:35:23  13:58:41.0998  +54:05:07.314
G0272146  09:36:32  14:02:25.3968  +51:12:31.8492
G0348702  10:23:42  14:02:28.2166  +54:16:25.6368
G1812485  10:24:51  14:02:52.8     +54:26:11.868
G0676140  10:26:11  14:03:32.7722  +49:58:07.1004
G0732463  10:27:20  14:04:05.2186  +49:58:47.0784
G0627353  10:28:29  14:04:55.7081  +54:24:10.4976
G0765189  10:29:39  14:05:01.3037  +52:46:21.3384
G0703757  10:31:02  14:05:10.47    +60:12:19.5732
G1796893  10:32:22  14:05:17.28    +53:19:10.668
G0575685  10:33:33  14:05:24.6569  +58:24:48.33
G0642817  10:34:42  14:05:29.5495  +55:05:38.3784
G0622798  10:35:52  14:06:09.0528  +55:22:03.414
G0647407  10:37:01  14:06:49.9183  +57:53:49.308
G0638901  10:38:10  14:07:08.573   +56:32:24.4572
G0592101  10:39:20  14:07:29.5459  +52:08:29.1048
G0704739  10:40:29  14:07:47.6698  +53:22:13.2456
G0642359  10:41:38  14:08:08.3789  +55:43:13.7496
G0791124  10:42:47  14:08:10.5029  +52:40:48.1656
G1087595  10:44:08  14:08:12.9456  +60:14:32.8092
G0594415  10:45:26  14:08:21.5333  +55:18:05.7924
G0661360  10:46:35  14:08:35.5481  +55:32:24.774
G0647066  10:47:42  14:08:54.0674  +55:26:26.5344
G1042806  10:48:52  14:09:02.2486  +54:33:22.5864
G0581800  10:50:03  14:09:36.9763  +58:25:53.6448
G0577065  10:51:12  14:09:38.0822  +58:30:33.66
G0664391  10:52:22  14:09:42.1032  +55:27:38.6892
G0672191  10:53:33  14:09:46.681   +55:29:14.7084
G0603349  10:54:42  14:09:50.7679  +58:59:25.7244
G0785568  10:55:54  14:09:55.6788  +52:33:10.8612
G0823819  10:57:05  14:09:59.5898  +59:11:33.7308
G0671853  10:58:15  14:10:01.289   +55:38:12.7356
G0813080  11:07:30  14:10:01.5454  +54:52:54.7464
G0977197  11:08:39  14:10:13.169   +59:01:00.6708
G0717223  11:09:50  14:10:15.0989  +53:20:06.8352
G0748846  11:11:10  14:10:34.7021  +51:27:52.8336
G0580346  11:12:32  14:10:43.4362  +58:31:03.5436
G0671301  11:13:55  14:11:03.7574  +48:57:55.8288
G0729374  11:15:17  14:11:15.8753  +57:36:08.892
G0676919  11:16:26  14:11:17.2193  +55:18:23.9076
G0822872  11:17:33  14:11:18.4462  +55:10:52.9176
G0827466  11:18:43  14:11:24.5801  +57:14:55.9752
G0559334  11:19:52  14:11:29.0844  +55:07:18.9984
G0723066  11:21:12  14:11:40.5432  +52:38:07.5732
G0566578  11:22:21  14:11:47.8087  +54:57:46.9836
G0735801  11:23:30  14:11:49.5043  +52:49:00.5196
G0688629  11:24:40  14:11:49.5521  +54:57:32.9616
G0799824  11:25:51  14:12:43.8209  +49:52:06.6936
G0599287  11:27:02  14:12:56.4038  +55:21:13.2732
G0773650  11:28:12  14:13:12.3523  +53:59:34.332
G0678111  11:29:21  14:13:27.3595  +54:43:46.2684
G0772607  11:30:30  14:13:49.8523  +57:46:10.7112
G0740612  11:31:42  14:13:57.096   +52:45:52.4736
G0505067  11:32:54  14:14:25.1477  +57:37:50.6388
G0755393  11:34:18  14:14:54.4116  +60:00:40.1292
G0740964  11:35:27  14:15:08.4156  +56:57:01.0584
G0472742  11:36:52  14:15:20.3174  +52:20:44.6532
G0756243  11:38:14  14:15:27.4183  +57:36:33.0372
G0553864  11:39:36  14:15:30.1757  +51:29:54.906
G0031234  11:40:45  14:15:33.3142  +51:23:15.936
G0643903  11:41:52  14:15:39.7596  +52:32:37.968
G0816816  11:43:02  14:15:51.493   +53:35:07.9728
G0714551  11:56:47  14:15:52.8295  +50:19:25.9788
G0656839  11:58:08  14:16:00.6226  +55:47:13.0992
G0009685  11:59:29  14:16:17.1168  +51:16:46.0308
G0569557  12:00:49  14:16:17.8126  +55:22:44.3244
G0597629  12:02:02  14:16:38.5694  +54:07:20.3052
G1248064  12:03:26  14:17:45.3881  +59:04:08.9364
G0653802  12:04:45  14:17:47.2668  +55:30:58.914
G0766815  12:05:57  14:17:52.1009  +56:33:18.0432
G0014532  12:07:09  14:18:40.1587  +56:28:10.7148
G0790756  12:08:27  14:18:40.8766  +54:23:12.7248
G0579069  12:09:43  14:18:45.2306  +55:52:27.7608
G0749743  12:11:02  14:19:04.8413  +53:02:50.6868
G0761100  12:12:22  14:19:15.3077  +56:14:00.7692
G0777965  12:13:35  14:19:20.5224  +56:06:09.7308
G0723580  12:14:55  14:19:21.0828  +58:56:20.7132
G0748887  12:16:07  14:19:28.4582  +58:57:25.4232
G0716716  12:17:27  14:19:45.5712  +56:25:08.5332
G0752682  12:18:44  14:19:55.7592  +58:20:53.5272
G0600310  12:20:04  14:20:26.9604  +55:48:08.2908
G0553042  12:21:18  14:20:58.6193  +56:49:01.1928
G0722677  12:22:29  14:20:58.9637  +56:22:12.1872
G0603174  12:23:40  14:21:08.789   +56:46:36.5556
G1097052  12:25:08  14:21:15.6629  +61:35:16.6128
G0598447  12:26:34  14:21:27.6562  +57:00:20.628
G0902837  12:28:05  14:21:35.8226  +49:33:04.6404
G0724743  12:29:35  14:21:41.7919  +56:51:07.5744
G0652437  12:30:57  14:22:31.6774  +53:57:08.1036
G0819895  12:32:19  14:22:55.8581  +56:06:34.3548
G0713155  12:33:32  14:23:14.2018  +56:39:36.3276
G1190114  12:34:44  14:23:21.3684  +56:40:52.2732

GCN Circular 27036

Subject
LIGO/Virgo S200208q: Updated Sky Localization
Date
2020-02-12T06:57:42Z (5 years ago)
From
Leo Singer at GSFC <leo.p.singer@nasa.gov>
The LIGO Scientific Collaboration and the Virgo Collaboration report:

We have conducted further analysis of the LIGO Hanford Observatory (H1),
LIGO Livingston Observatory (L1), and Virgo Observatory (V1) data
around the time of the compact binary merger (CBC) candidate S200208q
(GCN 27014). Parameter estimation has been performed using LALInference
[1] and a new sky map, LALInference.fits.gz,0, distributed via GCN
Notice, is available for retrieval from the GraceDB event page:

https://gracedb.ligo.org/superevents/S200208q

The preferred sky map at this time is LALInference.fits.gz,0. For the
LALInference.fits.gz,0 sky map, the 90% credible region is well fit by
an ellipse with an area of 27 deg2 described by the following DS9
region (right ascension, declination, semi-major axis, semi-minor
axis, position angle of the semi-minor axis):
   icrs; ellipse(09h17m19s, -33d42m23s, 4d, 2d, 76d)
Marginalized over the whole sky, the a posteriori luminosity distance
estimate is 2142 +/- 459 Mpc (a posteriori mean +/- standard deviation).

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

 [1] Veitch et al. PRD 91, 042003 (2015)

GCN Circular 27053

Subject
LIGO/Virgo S200208q: no counterpart candidate in SVOM/C-GFT observations
Date
2020-02-13T08:36:33Z (5 years ago)
From
Xuhui Han at NAOC/SVOM <hxh@nao.cas.cn>
Z. Kang (CHO), B. W. Li (CHO), Z. W. Li (CHO), C. Wu (NAOC), 
X. H. Han (NAOC)���S. Antier (CNRS/APC), N. Leroy (CNRS/LAL), 
D. Turpin (CEA/AIM), C. Z. Liu (CHO), B. L. Niu (CHO), L. C. Han (CHO)

report on behalf of the SVOM Multi Messenger Astronomy and GWAC teams
(http://www.svom.fr/en/svom-mma-and-gwac-team):

We observed the LIGO/Virgo trigger S200208q (GCN #27014) with C-GFT 
(Chinese Ground Follow-up Telescope in SVOM mission). C-GFT is located 
at Jilin, Changchun Observatory, National Astronomical Observatories, CAS. 
It has FOV of 1.35 X 1.35 deg**2 with a 4k*4k CMOS detector mounted  
on the primary focus of 1.2-meter-aperure telescope. 

The first unfiltered image was taken ~23.4 hours after the event 
trigger time. No credible new source was detected in our pipeline. 
A total number of 16 fields was observed. The coordinates (J2000) 
of the fields, the observation time, limit mag (5sigma), are listed below.

No.   RA           Dec           obs_time (UTC)      limit_mag(5sigma)
=========================================================
1    18:01:49.3   +80:46:07.0  2020-02-09 12:23:38.5   17.7
2    18:01:41.3   +79:46:09.1  2020-02-09 12:25:28.5   17.9 
3    18:01:28.7   +77:46:31.4  2020-02-09 12:28:51.5   17.8 
4    18:01:23.0   +76:46:35.6  2020-02-09 12:30:07.5   17.8
5    18:01:31.8   +77:46:32.9  2020-02-09 12:31:50.5   17.8
6    19:00:29.1   +76:46:03.2  2020-02-09 12:33:21.5   17.7
7    18:01:34.6   +77:46:35.3  2020-02-09 12:34:40.5   17.9 
8    18:01:37.4   +79:58:12.7  2020-02-09 12:37:59.5   17.8 
9    17:01:32.2   +77:59:02.1  2020-02-09 12:39:42.5   17.8 
10   19:01:30.3   +80:57:33.9  2020-02-09 12:41:15.5   17.8
11   19:01:03.4   +76:57:35.9  2020-02-09 12:42:22.5   17.8
12   17:01:32.8   +77:59:06.5  2020-02-09 12:43:41.5   17.7 
13   18:01:49.9   +80:58:19.1  2020-02-09 12:44:42.5   17.9 
14   19:01:09.3   +77:57:37.1  2020-02-09 12:45:41.5   17.9
15   17:01:25.4   +76:59:08.0  2020-02-09 12:46:36.5   17.8
16   17:01:14.5   +74:59:06.7  2020-02-09 12:47:31.5   17.7


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

GCN Circular 27054

Subject
LIGO/Virgo S200208q : No significant candidates in TAROT - FRAM - GRANDMA observations
Date
2020-02-13T09:14:19Z (5 years ago)
From
Sarah Antier at APC <antier@apc.in2p3.fr>
E. Howell (OzGrav-UWA), S. Agayeva (SHAO), A. Baransky (Kyiv Uni), P.
Hello (IJCLab), M. Boer (Artemis), N. Christensen (Artemis),
L. Eymar (Artemis), S. Karpov (FZU), A. Klotz (IRAP), M. Masek (FZU),
K. Noysena (Artemis, IRAP), S. Antier (APC), A. Coleiro (APC), D.
Corre (IJCLab), M. Coughlin (UMN), 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), M. Prouza
(FZU)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 S200208q event 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�� | 1102������ | R�������������� | 1.0 x 1.0���� | 18.0 (60s) |
| FRAM-CTA-N�� | 563�������� | R�������������� | 0.45 x 0.45 | 17.0 (90s) |
| TCA���������������� | 453�������� | Clear������ | 1.9 x 1.9���� | 18.0 (60s) |
| TCH���������������� | 686�������� | Clear������ | 1.9 x 1.9���� | 18.0 (60s) |
| TRE���������������� | 1619������ | 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�� | 2020-02-09 | 2020-02-09 | 140.134 | -36.486 | 3.2�������� |
|������������������������ | 07:22:34���� | 07:24:34���� |���������������� | |���������������� |
| FRAM-Auger�� | 2020-02-09 | 2020-02-09 | 139.470 | -35.514 | 5.5�������� |
|������������������������ | 07:27:35���� | 07:29:35���� |���������������� | |���������������� |
| -----������������ | -----���������� | -----���������� | -----���� | -----���� | -----���� |
| FRAM-CTA-N�� | 2020-02-08 | 2020-02-08 | 139.894 | -36.037 | 0.9�������� |
|������������������������ | 22:24:17���� | 22:26:17���� |���������������� | |���������������� |
| FRAM-CTA-N�� | 2020-02-08 | 2020-02-08 | 140.195 | -36.474 | 0.6�������� |
|������������������������ | 22:28:36���� | 22:30:36���� |���������������� | |���������������� |
| FRAM-CTA-N�� | 2020-02-08 | 2020-02-08 | 139.353 | -36.037 | 0.8�������� |
|������������������������ | 22:30:52���� | 22:34:58���� |���������������� | |���������������� |
| FRAM-CTA-N�� | 2020-02-08 | 2020-02-08 | 139.267 | -35.600 | 1.0�������� |
|������������������������ | 22:35:11���� | 22:39:17���� |���������������� | |���������������� |
| FRAM-CTA-N�� | 2020-02-08 | 2020-02-08 | 139.806 | -35.600 | 1.1�������� |
|������������������������ | 22:39:30���� | 22:43:36���� |���������������� | |���������������� |
| FRAM-CTA-N�� | 2020-02-08 | 2020-02-08 | 139.650 | -36.474 | 0.6�������� |
|������������������������ | 22:43:50���� | 22:47:56���� |���������������� | |���������������� |
| FRAM-CTA-N�� | 2020-02-08 | 2020-02-08 | 140.046 | -35.163 | 1.4�������� |
|������������������������ | 22:48:09���� | 22:52:15���� |���������������� | |���������������� |
| FRAM-CTA-N�� | 2020-02-08 | 2020-02-08 | 140.345 | -35.600 | 1.1�������� |
|������������������������ | 22:52:34���� | 22:56:40���� |���������������� | |���������������� |
| FRAM-CTA-N�� | 2020-02-08 | 2020-02-08 | 139.511 | -35.163 | 1.4�������� |
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| FRAM-CTA-N�� | 2020-02-08 | 2020-02-08 | 140.256 | -37.348 | 0.3�������� |
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| FRAM-CTA-N�� | 2020-02-08 | 2020-02-08 | 140.739 | -36.474 | 0.5�������� |
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| TCA���������������� | 2020-02-08 | 2020-02-13 | 209.879 | 55.692�� | <0.1������ |
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| TCA���������������� | 2020-02-08 | 2020-02-13 | 213.093 | 55.692�� | <0.1������ |
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| TRE���������������� | 2020-02-09 | 2020-02-09 | 198.000 | 24.545�� | <0.1������ |
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| TRE���������������� | 2020-02-10 | 2020-02-10 | 138.857 | -36.818 | 26.0������ |
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+-------------+------------+------------+---------+---------+---------+

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 95.1% of the cumulative probability of
the LALInference skymap created on 2020-02-10 21:14:05
(UTC).


The coverage map is available at:
https://grandma-
owncloud.lal.in2p3.fr/index.php/s/XgtMhPRxcyL09gR/download?path=%2F&files=GRANDMA_S200208q_1581583078.svg

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
[2] S. Antier et al., MNRAS 2019, https://doi.org/10.1093/mnras/stz3142
[3] K. Noysena et al., ApJ 2019, arXiv:1910.02770

GCN Circular 27223

Subject
LIGO/Virgo S200208q: Upper limits from Konus-Wind observations
Date
2020-02-26T14:58:08Z (5 years ago)
From
Anna Ridnaia at Ioffe Institute <ridnaia@mail.ioffe.ru>
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 S200208q (2020-02-08 13:01:17.991 UTC, hereafter T0;
LIGO/Virgo Collaboration GCN Circ. 27014).

No triggered KW GRBs happened between ~1.5 days before and ~2 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 8.9x10^-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 2.3x10^-7 erg/cm^2/s (20 - 1500 keV, 2.944 s 
scale).

All the quoted values are preliminary.

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