LIGO/Virgo S190930s

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva, D.Kuvshinov 
(Lomonosov Moscow State University, SAI, Physics Department),

R. Podesta, C.Lopez, F. Podesta, C.Francile 
(Observatorio Astronomico Felix Aguilar OAFA),

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

R. Rebolo, M. Serra 
(The Instituto de Astrofisica de Canarias),

D. Buckley 
(South African Astronomical Observatory),

O.A. Gres, N.M. Budnev, O.Ershova 
(Irkutsk State University, API),

A. Tlatov, D. Dormidontov 
(Kislovodsk Solar Station of the Pulkovo Observatory),

V. Yurkov, A. Gabovich, Yu. Sergienko 
(Blagoveschensk Educational State University)




MASTER-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 S190930s errorbox  54 sec after trigger time at 2019-09-30 13:36:35 UT, with upper limit up to  17.4 mag. The observations began at zenit distance = 50 deg. The sun  altitude  is -37.8 deg. 

The galactic latitude b = -60 deg., longitude l = 98 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/ligo_1.php?id=10851

We obtain a following upper limits.  

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

     145 | 2019-09-30 13:36:35 |         MASTER-Amur | (02h 37m 02.088s , +27d 44m 29.67s) |   C |   180 | 17.4 |        
     541 | 2019-09-30 13:44:12 |         MASTER-Amur | (21h 02m 58.574s , +08d 26m 09.77s) |   C |    60 | 17.4 |        
Filter C is a clear (unfiltred) band. 


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

The LIGO Scientific Collaboration and the Virgo Collaboration report:

We identified the compact binary merger candidate S190930s during real-time
processing of data from LIGO Hanford Observatory (H1) and LIGO Livingston
Observatory (L1) at 2019-09-30 13:35:41.247 UTC (GPS time: 1253885759.247).
The candidate was found by the GstLAL [1], MBTAOnline [2], PyCBC Live [3],
and SPIIR [4] analysis pipelines.

S190930s is an event of interest because its false alarm rate, as estimated
by the online analysis, is 3e-09 Hz, or about one in 10 years. The event's
properties can be found at this URL:

https://gracedb.ligo.org/superevents/S190930s

The classification of the GW signal, in order of descending probability, is
MassGap (95%), Terrestrial (5%), BNS (<1%), BBH (<1%), or NSBH (<1%).

Assuming the candidate is astrophysical in origin, there is strong evidence
against the lighter compact object having a mass < 3 solar masses (HasNS:
<1%). Using the masses and spins inferred from the signal, there is strong
evidence against matter outside the final compact object (HasRemnant: <1%).

One sky map is available at this time and can be retrieved from the GraceDB
event page:

 * bayestar.fits.gz,0, an updated localization generated by BAYESTAR [5],
distributed via GCN notice about 6 minutes after the candidate trigger
time. For the bayestar.fits.gz,0 sky map, the 90% credible region is 1998
deg2. Marginalized over the whole sky, the a posteriori luminosity distance
estimate is 752 +/- 224 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] Adams et al. CQG 33, 175012 (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)

Maeve Doyle (UCD, Ireland), Diego Gotz (CEA, Saclay)
V. Savchenko, C. Ferrigno (ISDC/UniGE, Switzerland)
J. Rodi (IAPS-Roma, Italy)
A. Coleiro (APC, France)
S. Mereghetti (INAF IASF-Milano, Italy)

on behalf of the INTEGRAL multi-messenger collaboration:
https://www.astro.unige.ch/cdci/integral-multimessenger-collaboration

Using INTEGRAL/SPI-ACS realtime data (following [1]) we have performed
a search for a prompt gamma-ray counterpart of S190930s (GCN 25871
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 ).

At the time of the event (2019-09-30 13:35:41 UTC, hereafter T0),
INTEGRAL was operating in nominal mode. The peak of the event
localization probability was at an angle of 60 deg with respect to the
spacecraft pointing axis. This orientation implies strongly suppressed
(27% of optimal) response of ISGRI, somewhat suppressed (40% of
optimal) response of IBIS/Veto, and near-optimal (70% of optimal)
r esponse of SPI-ACS.

The background within +/-300 seconds around the event was very stable
(excess variance 1.2).

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 1.8e-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 ~1.6e-07 (5.5e-08)
erg/cm^2/s at 1 s (8 s) time scale in 75-2000 keV energy range.

For the mean reported distance 752.0 Mpc this corresponds to the limit
on the total isotropic equivalen t energy in 1 s of 1.3e+49 erg for
the short GRB spectrum and for a long GRB spectrum isotropic
equivalent luminosity in 1 s (8 s) of 9.6e+48 erg/s (3.7e+48 erg/s)

We report for completeness and in order of FAP, all excesses
identified in the search region. We find 4 likely background
excesses:

scale | T | S/N | luminosity ( x 1e+49 erg/s) | FAP  
4 | 175 | 3.6 | 9.8 +/- 2.96 +/- 4.96 | 0.238 
0.55 | 121 | 4.2 | 29 +/- 8.03 +/- 14.7 | 0.559 
0.35 | 43.7 | 3.6 | 3.13 +/- 1.01 +/- 1.58 | 0.751 
0.65 | 52 | 3.4 | 21.4 +/- 7.37 +/- 10.8 | 0.786 

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

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
S190930s
 in a time range of 1000 seconds [3] centered on the alert event time
(2019-09-30 13:27:21.247 UTC to 2019-09-30 13:44:01.247 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 S190930s calculated from the map
circulated in the 2-Initial notice.

IceCube's sensitivity assuming an E^-2 spectrum (E^2 dN/dE) to neutrino
point sources within the locations spanned by the 90% spatial  containment
of S190930s ranges from  0.029 to 0.173 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] Braun et al., Astroparticle Physics 29, 299 (2008)
[3] Baret et al., Astroparticle Physics 35, 1 (2011)

S. Sugita, M. Serino (AGU),
N. Kawai (Tokyo Tech), H. Negoro (Nihon U.),
M. Nakajima, W. Maruyama, M. Aoki, K. Kobayashi (Nihon U.),
T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN),
T. Sakamoto, H. Nishida, A. Yoshida (AGU),
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, T. Sato (Chuo U.),
M. Shidatsu (Ehime U.), M. Oeda, K. Shiraishi (Tokyo Tech),
S. Nakahira, Y. Sugawara, S. Ueno, H. Tomida, M. Ishikawa, N. Isobe,
R. Shimomukai, M. Tominaga (JAXA),
Y. Ueda, A. Tanimoto, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake
(Kyoto U.),
H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.),
M. Yamauchi, S. Iwahori, Y. Kurihara, K. Kurogi, K. Miike (Miyazaki U.),
T. Kawamuro (NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M.
Sugizaki (NAOC)
report on behalf of the MAXI team:

We examined MAXI/GSC all-sky X-ray images (2-20 keV)
after the LVC trigger S190930s at 2019-09-30 13:35:41.246 UTC (GCN 25871
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 ).

At the trigger time of S190930s, the high-voltage of MAXI/GSC was on,
but the FOV was out of the 90% credible region of the bayestar skymap.
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 14:25:05 to
15:03:54 UTC (T0+2964 to T0+5293 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.

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 S190930s at T0 = 2019-09-30 
13:35:41 (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, the 100% of the S190930s 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 S190930s LR, from a minimum of 1.41E-06 erg cm^-2 
to a maximum of 6.51E-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.

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 S190930s event using the 90% contour of the Initial bayestar probability
map provided by the GW interferometers (GCN#25871
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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/S190930s_Initial.png <http://antares.in2p3.fr/GW/S190930s_Initial.png>.
Considering the location probability provided by the LIGO/Virgo collaborations, there is a
25.9% chance that the GW emitter was in the ANTARES **upgoing** field of view at the time of
the alert.

No up-going muon neutrino candidate events were recorded in the ANTARES sky during a
+/-500s time-window centered on the time 2019-09-30 13:35:41 and in the 90% contour of the S190930s
event. The expected number of atmospheric background events in the region visible by ANTARES is
2.28e-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 1.64e-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.

LIGO/Virgo S190930s: no counterpart candidates in AGILE-GRID observations

M. Cardillo (INAF/IAPS),� F. Verrecchia (SSDC, and INAF/OAR), 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 (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 S190930s at T0 = 2019-09-30 
13:35:41 (UT), a preliminary analysis of the AGILE exposure at T0 shows 
that the Gamma-Ray Imaging Detector (GRID) exposure covered about 27% of 
the 90% c.l. localization region (LR) (40% of 90% c.l. LR is occulted by 
Earth) at an off-axis angle of about 5 degrees.

We performed an analysis of the GRID data in the energy range 50 MeV - 
10 GeV on T0, where good exposure of the S190930s 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 1.0e-06 to 4.9e-06 erg cm^-2 s^-1, with exposure of about 27% of 
the LR over the time interval ( T0 -2s ; T0 + 2s );
- from 8.4e-07 to 2.5e-06 erg cm^-2 s^-1, with exposure of about 26% of 
the LR over the time interval ( T0s ; T0 + 10s );
- from 1.4e-07 to 1.6e-06 erg cm^-2 s^-1, with exposure of about 26% of 
the LR over the time interval ( T0 ; 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.

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

For S190930s and using the initial bayestar.fits.gz skymap, Fermi-GBM was observing 62.2% 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 S190930s (GCN 25871
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 ). 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.

We therefore set upper limits on impulsive gamma-ray emission. Using the representative soft, normal, and hard GRB-like templates described in arXiv:1612.02395
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 , we set the following 3 sigma flux upper limits over 10-1000 keV, weighted by GW localization probability (in units of 10^-7 erg/s/cm^2):

Timescale  Soft     Normal   Hard
------------------------------------
0.128 s:   5.7      6.6      10.
1.024 s:   1.6      2.2      3.5
8.192 s:   0.6      0.7      1.0

Assuming the median luminosity distance of 752 Mpc from the GW detection, we estimate the following intrinsic luminosity upper limits over the 1 keV-10 MeV energy range (in units of 10^49 erg/s):

Timescale  Soft     Normal   Hard
------------------------------------
0.128 s:   5.94     6.29     15.8
1.024 s:   1.67     2.10     5.53
8.192 s:   0.62     0.65     1.58

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-SSDC), S. Emery (UCL-MSSL),
P. A. Evans (U. Leicester), P. Giommi (ASI), C. Gronwall (PSU),
D. Hartmann (Clemson U.), J. A. Kennea (PSU),
N. Klingler (PSU), H. A. Krimm (NSF),
N. P. M. Kuin (UCL-MSSL), F. E. Marshall (NASA/GSFC),
A. Melandri (INAF-OAB), J. A. Nousek (PSU),
S. R. Oates (Uni. of Warwick), P. T. O'Brien (U. Leicester),
J. P. Osborne (U. Leicester), C. Pagani (U. Leicester),
K. L. Page (U.Leicester), M. J. Page (UCL-MSSL), M. Perri (ASDC),
J. L. Racusin (NASA/GSFC), B. Sbarufatti (INAF-OAB/PSU),
M. H. Siegel (PSU), G. Tagliaferri (INAF-OAB), A. Tohuvavohu (Toronto),
E. Troja (NASA/GSFC/UMCP) report on behalf of the Swift team:

We report the search results in the BAT data within T0 +/- 100 s of the
LVC event S190930s (LIGO/VIRGO Collaboration GCN Circ. 25871
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 ),
where T0 is the LVC trigger time (2019-09-30T13:35:41.246 UTC).

The center of the BAT field of view (FOV) at T0 is
RA = 20.932 deg,
DEC = -58.811 deg,
and the roll angle is 164.350 deg.
The BAT FOV (>10% partial coding) covers 0.40% of the integrated
LVC localization probability, and 0.45% 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 detections (signal-to-noise ratio
>~ 5 sigma) from astrophysical origins are found in the BAT raw light
curves with time bins of 64 ms, 1 s, and 1.6 s. The short spike at
~T-95.9 s in the 15-25 keV light curve is due to a detector glitch
(see more explanation in the "Investigation of the detector glitch"
section in the link below).

Assuming an on-axis (100% coded) short GRB with a typical
spectrum in the BAT energy range (i.e., a simple power-law model with a
power-law index of -1.32, Lien & Sakamoto et al. 2016), the 5-sigma upper
limit in the 1-s binned light curve corresponds to a flux upper
limit (15-350 keV) of ~ 2.20 x 10^-7 erg/s/cm^2.
Assuming a luminosity of ~ 2 x 10^47 erg/s (similar to GW170817)
and an average Epeak of ~ 400 keV for short GRBs (Bhat et al. 2016),
this flux upper limit corresponds to a distance of ~ 48.44 Mpc.

Event data analysis is available from T0-100.968 s to T+99.102 s.
No significant detections are found in the 15-350 keV images created
using intervals of T0 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 99.60% 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/S190930s/web/source_public.html

S. Sugita, A. Yoshida, T. Sakamoto, V. Pal'shin (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), P. S. Marrocchesi (U of Siena),
and the CALET collaboration:

The CALET Gamma-ray Burst Monitor (CGBM) was operating at the trigger
time of S190930s T0 = 2019-09-30 13:35:41.247 UT (The LIGO Scientific
Collaboration and Virgo Collaboration, GCN Circ.25871
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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 20 % and 100 %, respectively (and 100 % credible region of the
initial sky map was above the horizon).  The HXM and SGM fields of
view were centered at RA = 28.1 deg, Dec = 3.4 deg and RA = 20.8 deg,
Dec = -3.3 deg at T0, respectively.

Based on the analysis of the light curve data with 0.125 sec time 
resolution from T0-60 sec to T0+60 sec, we found no significant 
excess 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 S190930s. 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 3.5x10^-5 erg/cm^2/s (10-100 GeV) when
the summed LIGO-Virgo probability reaches 5%.  The CAL FOV was 
centered at RA= 20.7 deg, DEC= -3.3 deg at T0.

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

We have searched data collected by the Fermi Large Area Telescope (LAT) on Sep 30, 2019, for possible high-energy (E > 100 MeV) gamma-ray emission in spatial/temporal coincidence with the LIGO/Virgo trigger S190930s (GCN 25871
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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. Fermi-LAT had null instantaneous coverage of the LIGO probability region at the time of the trigger (T0 = 2019-09-30 13:35:41.247 UTC). Coverage started around 300 s after the trigger and reached 99% cumulative coverage at approximately T0 + 4 ks. The remaining area was not observed within 10 ks after the trigger.

We performed a search for a transient counterpart within the observed region of the 90% contour of the LIGO map in a fixed time window from T0 to T0 + 10 ks. No significant sources were found.

We also performed a search which adapted the time interval of the analysis to the exposure of each region of the sky, and no additional excesses were found.

Energy flux upper bounds between 100 MeV and 1 GeV for the fixed time interval of this search vary between 1.4e-10 and 8.1e-08 [erg/cm^2/s].

The Fermi-LAT point of contact for this event is Nicola Omodei (nikomo@stanford.edu<mailto:nikomo@stanford.edu>).

The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.

Keto D. Zhang, Thomas de Jaeger, James Sunseri, Benjamin E. Stahl,
WeiKang Zheng, Andrew Hoffman, Yukei Murakami, Sergiy Vasylyev,
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 S190930s (GCN 25871
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 ) 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 367 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 03:42:23, Oct.
01th UT, about 14.1 minutes after the trigger, and the last image at
13:22:24 UT. Our typical limiting mag is 19.0. No viable counterparts
were identified and the analysis is ongoing. A full list of galaxies
observed by KAIT is given below.

GladeID   UT(Oct01)  RA_J2000   Dec_J2000
-----------------------------------------------
G0418118  03:42:23  20:24:50.8008  +43:02:35.0304
G0826512  03:43:38  20:28:08.2178  +28:29:57.0948
G0365855  03:44:56  20:29:59.9414  +49:52:17.1876
G0645883  03:46:14  20:30:29.5531  +27:40:42.906
G0547751  03:47:33  20:30:50.5663  +49:31:27.5628
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Kerry Paterson (Northwestern), Michael J. Lundquist, David J. Sand (UA), Wen-fai Fong, Jillian Rastinejad (Northwestern), Jennifer Andrews (UA), Sam Wyatt (UA), Eric Christensen, Alex Gibbs, Frank Shelly (UA/LPL), report on behalf of the SAGUARO collaboration:

We initiated observations of 12 fields (each 5 deg^2, totalling 60 deg^2) within the LVC localization region for the GW trigger S190930s (LVC Circ 25871) starting on 2019-10-01 02:09:22 UT (0.52 days after the GW trigger) with the 1.5m Catalina Sky Survey telescope on Mt. Lemmon, AZ. 

Below are the field centers observed.

RA DEC
318.8895 7.7292
318.8895 9.9375
316.6665 9.9375
316.3965 12.1458
315.8490 14.3541
313.5840 14.3541
314.1615 12.1458
319.1415 5.5208
321.3495 3.3125
321.3495 5.5208
318.6330 12.1458
313.2915 16.5625
We have posted our pointings to the Treasure Map, and encourage others to do the same:
http://treasuremap.space/alerts?graceids=S190930s&pointing_status=all&alert_type=Initial

Performing image subtraction, we find no new transients within the 60 deg^2 searched down to a 3-sigma limit of G~21.3 AB mag (calibrated to Gaia DR2) relative to deep CSS reference images.

A more detailed description of SAGUARO can be found in Lundquist et al. 2019, ApJL, 881, 2. SAGUARO is supported by the National Science Foundation under Award Nos. AST-1909358 and AST-1908972.

Q. Luo, Q. B. Yi, S. Xiao, C. Cai, Y. G. Zheng, Y. Huang,
C. K. Li, X. B. Li, G. 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 
S190930s event (GCN #25871
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 ), trigger time 2019-09-30T13:35:41 UTC. 
At T0, about 57% of the LIGO localization region was covered by 
Insight-HXMT without occultation by 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=313 deg, DEC=19 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:   2.1e-07 erg cm^-2
10 s:  5.0e-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:  7.6e-07 erg cm^-2

Band model 3 (alpha=-0.0, beta=-1.5, Ep=1000 keV):
1 s:   4.6e-07 erg cm^-2
10 s:  1.3e-06 erg cm^-2

All measurements above are made with the CsI detectors operating in the
regular mode with the energy range of about 80-800 keV (deposited energy).
Only gamma-rays with energy greater than about 200 keV can penetrate
the spacecraft and leave signals in the CsI detectors installed inside
of the spacecraft.

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.

The LIGO Scientific Collaboration and the Virgo Collaboration report:

We have conducted further analysis of the data from LIGO Hanford
Observatory (H1) and LIGO Livingston Observatory (L1) around the time of
the compact binary merger (CBC) candidate S190930s (GCN Circular 25871
Loading...
 
 ).
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/S190930s

The preferred sky map at this time is LALInference.fits.gz,0. The 90%
credible region is 1748 deg2. Marginalized over the whole sky, the a
posteriori luminosity distance estimate is 709 +/- 191 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)

C.Lachaud (APC), X. G. Wang (GXU), A. Coleiro (APC),
J.R. Mao (YNAO), G. W. Li (NAOC)

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

We observed 27 sky regions (total: 4050 square degrees with overlaps)
to cover the skymap of the advanced LIGO/Virgo trigger S190930s,
with SVOM/GWAC, at Xinglong Observatory equipped with a set of two
types of wide angle cameras: FFOV cameras (FOV~900 square degrees/camera,
aperture = 3.5 cm) and JFOV cameras (FOV~150 square degrees/camera,
aperture = 18 cm). SVOM/GWAC currently comprises 4 FFOV cameras and
16 JFOV cameras, working with unfiltered band. The observations are
operated in time-series mode, taking one exposure every 25 seconds
(20s exposure + 5s readout). We estimate a 77.2% prior
probability that the observed and processed regions contain
the true location of the source. The images were taken between
~15 minutes before and ~5 hours after the event trigger time.

The coordinates of the 27 sky regions observed after the trigger
and their observation times are listed below:

No. Ra  Dec start-obs(UTC)  end-obs(UTC)    Camera_TYPE
1  01:45:10.30 57:37:14.52 2019-09-30 17:15:39 2019-09-30 17:28:37 JFOV
2  02:13:24.41 68:57:30.24 2019-09-30 17:17:17 2019-09-30 17:23:45 JFOV
3  21:18:19.68 68:54:10.44 2019-09-30 15:10:18 2019-09-30 15:31:18 JFOV
4  20:49:49.20 57:34:23.88 2019-09-30 15:14:18 2019-09-30 15:31:18 JFOV
5  20:08:15.60 30:22:52.32 2019-09-30 14:28:46 2019-09-30 14:58:59 JFOV
6  21:05:10.80 30:36:19.08 2019-09-30 14:38:29 2019-09-30 14:55:29 JFOV
7  21:12:28.32 23:45:53.64 2019-09-30 15:56:29 2019-09-30 16:23:11 JFOV
8  20:23:50.64 24:02:03.12 2019-09-30 16:09:50 2019-09-30 16:24:24 JFOV
9  21:18:24.48 35:26:04.92 2019-09-30 16:24:23 2019-09-30 16:24:23 JFOV
10 21:45:58.80 52:18:05.04 2019-09-30 16:28:13 2019-09-30 16:45:12 JFOV
11 21:34:48.24 40:42:21.24 2019-09-30 16:28:37 2019-09-30 16:56:08 JFOV
12 20:35:59.04 40:59:54.60 2019-09-30 16:48:26 2019-09-30 16:56:08 JFOV
13 21:19:55.20 01:30:02.95 2019-09-30 13:54:35 2019-09-30 16:26:11 JFOV
14 20:29:44.16 13:30:14.04 2019-09-30 13:54:35 2019-09-30 16:24:15 JFOV
15 21:20:11.76 13:41:14.64 2019-09-30 13:54:35 2019-09-30 16:20:36 JFOV
16 02:35:50.35 35:29:03.84 2019-09-30 17:40:06 2019-09-30 18:01:35 JFOV
17 21:20:36.48 57:56:40.56 2019-09-30 13:54:12 2019-09-30 14:24:03 JFOV
18 23:12:45.60 68:55:31.80 2019-09-30 13:54:12 2019-09-30 14:24:03 JFOV
19 22:45:54.48 64:26:27.96 2019-09-30 16:30:13 2019-09-30 16:43:11 JFOV
20 20:52:14.16 64:01:55.92 2019-09-30 16:32:14 2019-09-30 16:32:14 JFOV
21 22:27:42.00 23:44:02.04 2019-09-30 18:01:32 2019-09-30 18:24:10 JFOV
22 21:39:04.08 24:00:06.12 2019-09-30 13:26:16 2019-09-30 18:24:10 JFOV
23 22:33:36.00 35:24:57.24 2019-09-30 13:40:48 2019-09-30 18:24:10 JFOV
24 22:42:58.56 13:51:07.56 2019-09-30 17:40:48 2019-09-30 18:00:13 JFOV
25 21:44:38.40 47:20:02.04 2019-09-30 18:07:20 2019-09-30 18:35:18 JFOV
26 22:52:12.24 35:28:24.60 2019-09-30 18:07:21 2019-09-30 18:35:18 JFOV
27 03:40:37.78 64:29:39.84 2019-09-30 17:29:25 2019-09-30 17:29:25 JFOV

The sky region #22 was observed at the time of the trigger (it has
3.5% probability to contain the true location of the source).

Some sky regions have been observed before the GW event
for a total of 1200 square degrees with overlap
(from ~2 hours to ~ 12 minutes before the event) :

No. Ra  Dec start-obs(UTC)  end-obs(UTC)    Camera_TYPE
1 21:23:18.96 35:17:43.08 2019-09-30 12:53:59 2019-09-30 13:22:59 JFOV
2 20:17:48.24 47:21:36.72 2019-09-30 12:52:55 2019-09-30 13:22:59 JFOV
3 22:32:05.04 13:41:29.40 2019-09-30 11:42:57 2019-09-30 12:14:29 JFOV
4 22:31:43.92 01:29:58.74 2019-09-30 11:43:44 2019-09-30 12:11:29 JFOV
5 21:41:35.52 13:30:04.68 2019-09-30 11:43:44 2019-09-30 12:12:59 JFOV
6 23:13:06.96 52:21:46.08 2019-09-30 11:43:42 2019-09-30 12:08:27 JFOV
7 22:02:56.88 41:04:53.76 2019-09-30 12:06:12 2019-09-30 12:12:27 JFOV
8 23:01:46.32 40:46:03.72 2019-09-30 12:08:57 2019-09-30 12:12:27 JFOV

The sky coverage map is available at:
http://cmm.svom.cn/gwpub/O3/S190930s/S190930s_post.png
(user:svomo3 pwd:gwo3)

The weather condition was clear during the observations. A 3 sigma
limiting magnitude of about 16.3 mag in R band was obtained in the single
frames. No credible new source is detected by our online pipeline during
follow-up observations. A more detailed image analysis including
co-addition is ongoing with our offline pipeline to search for transient
candidates.