LIGO/Virgo S190630ag

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 S190630ag in a time range of
1000 seconds [3] centered
on the alert event time (2019-06-30 18:43:45.180 UTC to 2019-06-30
19:00:25.180 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 S190630ag calculated from the map circulated in
the 1-Preliminary 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 S190630ag ranges
from  0.029 to
0.977 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
Loading...
 
  (2018) and Countryman et
al.arXiv:1901.05486
Loading...
 
  (2019)
[2] Braun et al., Astroparticle Physics 29, 299 (2008)
[3] Baret et al., Astroparticle Physics 35, 1 (2011)

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the LIGO/Virgo S190630ag errorbox  387 sec after trigger time at 2019-06-30 18:58:32 UT, with upper limit up to  18.6 mag. Observations started at twilight.  The observations began at zenit distance = 113 deg. The sun  altitude  is -12.6 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=10447

We obtain a following upper limits.  

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

     477 | 2019-06-30 18:58:32 |      MASTER-Tavrida | ( 18h 46m 19.53s , + 0d 58m 53.19s) |   C |   180 | 18.3 |        
     478 | 2019-06-30 18:58:32 |      MASTER-Tavrida | ( 18h 45m 05.49s , + 0d 56m 03.34s) |   C |   180 | 18.4 |        
     717 | 2019-06-30 19:02:32 |      MASTER-Tavrida | ( 10h 51m 18.45s , +16d  5m 22.47s) |   C |   180 | 17.9 |        
     938 | 2019-06-30 19:06:12 |      MASTER-Tavrida | ( 10h 57m 51.75s , +22d  5m 24.42s) |   C |   180 | 18.6 |        
     938 | 2019-06-30 19:06:12 |      MASTER-Tavrida | ( 10h 59m 12.44s , +22d  9m 14.84s) |   C |   180 | 17.2 |        
    1158 | 2019-06-30 19:09:52 |      MASTER-Tavrida | ( 10h 49m 08.87s , +20d  5m 32.01s) |   C |   180 | 13.6 |        
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 S190630ag during

real-time processing of data from LIGO Livingston Observatory (L1) and

Virgo Observatory (V1) at 2019-06-30 18:52:05.180 UTC (GPS time:

1245955943.180). The candidate was found by the GstLAL [1] analysis

pipeline.


S190630ag is an event of interest because its false alarm rate, as

estimated by the online analysis, is 1.4e-13 Hz, or about one in 1e5

years. The event's properties can be found at this URL:


https://gracedb.ligo.org/superevents/S190630ag


The classification of the GW signal, in order of descending

probability, is BBH (94%), MassGap (5%), NSBH (<1%), Terrestrial

(<1%), or BNS (<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, an updated localization generated by BAYESTAR

[2], distributed via GCN notice about 3 minutes after the candidate


The preferred sky map at this time is bayestar.fits.gz, with 90% credible

region of 8493 deg2. Marginalized over the whole sky, the a posteriori

luminosity distance estimate is 1059 +/- 307 Mpc (a posteriori mean +/-

standard deviation).


For further information about analysis methodology and the contents of

this alert, refer to the LIGO/Virgo Public Alerts User Guide

<https://emfollow.docs.ligo.org/userguide/>.


 [1] Messick et al. PRD 95, 042001 (2017)

 [2] Singer & Price PRD 93, 024013 (2016)

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

The HAWC Collaboration performed a follow-up of the gravitational wave
trigger S190630ag (GCN #24922
Loading...
 
 ). At the time of the trigger the HAWC
local zenith was oriented towards (RA, Dec) = (104.0deg, 19deg).
26% 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 0deg to 45deg for the area searched in this
analysis. The 5sigma detection sensitivity to a 1s (100s) burst in the
80-800GeV energy range goes from 1.2e-06 erg/cm^2 to 1.1e-04 erg/cm^2
(6.4e-06 erg/cm^2 to 5.0e-04 erg/cm^2), depending on the zenith
angle.

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

M. Ageron (CPPM/CNRS), B. Baret (APC/CNRS), A. Coleiro (APC/Universite Paris Diderot), M. Colomer (APC/Universite Paris Diderot)), D. Dornic (CPPM/CNRS), A. Kouchner (APC/Universite Paris Diderot), 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 S190630ag event using the 90% contour of the bayestar probability map provided by the GW interferometers (GCN#24922
Loading...
 
 ). 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/S190630ag.png <http://antares.in2p3.fr/GW/S190630ag.png>. Considering the location probability provided by the LIGO/Virgo collaborations, there is a 68.6% 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 2019-06-30 18:52:05 and in the 90% contour of the S190630ag event. The expected number of atmospheric background events in the region visible by ANTARES is 1.25e-03 in the +/- 500s time window. An extended search during +/- 1 hour gives no up-going muon neutrino coincidence. The expected number of atmospheric background events in the region visible by ANTARES is 9.04e-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.

Alexis Coleiro (APC, France), F. Onori (IAPS-Roma, Italy)
V. Savchenko, C. Ferrigno (ISDC/UniGE, Switzerland)
J. Rodi (IAPS-Roma, Italy)
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 S190630ag (GCN 24922
Loading...
 
 ).

At the time of the event (2019-06-30 18:52:05 UTC, hereafter T0), INTEGRAL was operating in nominal mode. The peak of the event localization probability was at an angle of 150 deg with respect to the spacecraft pointing axis. This orientation implies strongly suppressed (4% of optimal) response of ISGRI, near-optimal (94% of optimal) response of IBIS/Veto, and strongly suppressed (24% of optimal) response of SPI-ACS.

The background within +/-300 seconds around the event was rather stable (excess variance 1.3).

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 1.9e-07 erg/cm^2 (within the 50% probability containement 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 (6.9e-08) erg/cm^2/s at 1 s (8 s) time scale in 75-2000 keV energy range.

For the mean reported distance of 1059.0 Mpc, this corresponds to the limit on the total isotropic equivalent energy in 1 s of 2.5e+49 erg for the short GRB spectrum and for a long GRB spectrum isotropic equivalent luminosity in 1 s (8 s) of 2.1e+49 erg/s (9.3e+48 erg/s).

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

N. Kawai, M. Sugizaki (Tokyo Tech), H. Negoro (Nihon U.),
S. Sugita, M. Serino (AGU),
M. Nakajima, W. Maruyama, M. Aoki, K. Kobayashi (Nihon U.),
S. Nakahira, 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. Ueno, H. Tomida, M. Ishikawa, Y. Sugawara, 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)
report on behalf of the MAXI team:

We examined MAXI/GSC all-sky X-ray images (2-20 keV)
after the LVC trigger S190630ag at 2019-06-30 18:52:05.179 UTC (GCN 24922
Loading...
 
 ).

At the trigger time of S190630ag, the high-voltage of MAXI/GSC was off,
and it was turned on at T0+176 sec (+2.9 min).
The first one-orbit (92 min) scan observation with GSC after the event
covered 60%
of the 90% credible region of the bayestar skymap from 18:58:20 to
20:05:46 UTC (T0+375 to T0+4421 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.A. Wilson-Hodge (NASA/MSFC) & R. Hamburg (UAH) on behalf of the Fermi-GBM Team and the GBM-LIGO/Virgo group

For S190630ag and using the initial bayestar.fits skymap, Fermi-GBM was observing 87.7% 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 S190630ag (GCN 24922
Loading...
 
 ). 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 = 169.7 and Dec = -3.8 with a radius of 67.5 degrees. 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
Loading...
 
 , we set the following 3 sigma flux upper limits over 10-1000 keV (in units of 10^-7 erg/s/cm^2):

Timescale  Soft     Normal   Hard
------------------------------------
0.1 s:     4.4        5.8     17.0
1.0 s:     1.1      1.9      4.4
10  s:     0.47     0.56     1.0

Assuming the median luminosity distance of 1059 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
------------------------------------
0.1 s:     9.2      10.       53.
1.0 s:     2.3      3.6       14.
10  s:     1.0      1.1       3.1

M. Axelsson (KTH and Stockholm Univ.), D. Kocevski (NASA/MSFC), F. Piron (CNRS/IN2P3/LUPM) and E. Bissaldi (Politecnico and INFN Bari) report on behalf of the Fermi-LAT Collaboration:

We have searched data collected by the Fermi Large Area Telescope (LAT) on June 30, 2019, for possible high-energy (E > 100 MeV) gamma-ray emission in spatial/temporal coincidence with the LIGO/Virgo trigger S190630ag (GCN 24922
Loading...
 
 ).

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 a time, and "cumulative coverage" as the integral of the instantaneous coverage over time. Fermi-LAT had instantaneous coverage of ~20% of the LIGO probability at the time of the trigger (T0 = 2019-06-30 18:52:05.180 UTC), and reached 98% cumulative coverage after ~7.2 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 for the fixed time interval between 100 MeV and 1 GeV for this search vary between 2.3e-10 and 1.8e-08 [erg/cm^2/s].

The Fermi-LAT point of contact for this event is Magnus Axelsson (magaxe@kth.se<mailto:magaxe@kth.se>).

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.

C. Pittori (SSDC, and INAF/OAR), A. Ursi (INAF/IAPS), M. Tavani
(INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, C. Casentini, G.
Piano (INAF/IAPS), F. Lucarelli, F. Verrecchia (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 S190630ag at T0 = 2019-06-30
18:52:05 (UT), a preliminary analysis of the AGILE minicalorimeter
(MCAL) triggered data found no event candidates within a time interval
covering -/+ 15 sec from the LIGO/Virgo T0.

At the T0, about 60% of the S190630ag 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 S190630ag localization region, from a minimum of
1.6E-06 erg cm^-2 to a maximum of 7.4E-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.

D. M. Palmer (LANL), S. D. Barthelmy (NASA/GSFC),
A. Y. Lien (GSFC/UMBC), T. Sakamoto (AGU),
A. A. Breeveld (MSSL-UCL), A. P. Beardmore (U. Leicester),
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(ASDC), S. Emery (UCL-MSSL),
P. A. Evans (U. Leicester), P. Giommi (ASI), C. Gronwall (PSU),
D. Hartmann (Clemson U.), J. A. Kennea (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. Perri (ASDC),
J. L. Racusin (NASA/GSFC), B. Sbarufatti (INAF-OAB/PSU),
M. H. Siegel (PSU), G. Tagliaferri (INAF-OAB), A. Tohuvavohu (PSU),
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 S190630ag (LIGO/VIRGO Collaboration GCN Circ. 24922
Loading...
 
 ),
where T0 is the LVC trigger time (2019-06-30T18:52:05.179 UTC).

The center of the BAT FOV at T0 is
RA = 223.634 deg,
DEC = 41.517 deg,
ROLL = 310.061 deg.
The BAT Field of View (>10% partial coding) covers 4.77% of the integrated
LVC localization probability, and 2.54% of the galaxy convolved
probability (Evans et al. 2016).

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 ~ 1.98 x 10^-7 erg/s/cm^2. Please note that
because Swift slewed at T+5.8 s, the background around T0 changes
significantly, and thus results in a higher standard deviation calculated
using data from T0 +/- 100 s and consequently a higher flux upper limit..

No event data are available around T0.

BAT retains decreased, but significant, sensitivity to rate increases for
gamma-ray events outside of its FOV. About 20.35% 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/S190630ag/web/source.html

C. Pittori (SSDC, and INAF/OAR), A. Ursi (INAF/IAPS), M. Tavani
(INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, C. Casentini, G.
Piano (INAF/IAPS), F. Lucarelli, F. Verrecchia (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 S190630ag at T0 = 2019-06-30 18:52:05.180
UTC a preliminary analysis of the AGILE exposure at T0 shows that
the Gamma-Ray Imaging Detector (GRID) exposure covered less than 20%
of the 90% c.l. localization region (LR)  (due to Earth occultation
and 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 S190630ag 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 5.9e-08 to 5.5e-06 erg cm^-2 s^-1, with exposure of about 42% of the LR
over the time interval ( T0 -200s ; 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.

Yukei Murakami, Shaunak Modak, Sergiy Vasylyev, Benjamin Stahl,
WeiKang Zheng, Andrew Hoffman, Nachiket Girish, and Alexei 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-wavei
event S190630ag (GCN 24922
Loading...
 
 ) 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 148 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 10:39:35, July 1st
UT,
about 16.0 hours after the trigger, and the last image at 11:18:34 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   RA_deg(J2000)   Dec_deg(J2000)
-----------------------------------------------
G0061445  341.9249572753906   1.907817006111145
G0092394  319.9082946777344   23.86920928955078
G0110246  316.32904052734375  12.999917984008789
G0113330  343.4059143066406   1.6700730323791504
G0128008  343.24871826171875  3.5833311080932617
G0138166  318.15472412109375  12.344159126281738
G0146771  330.15570068359375  36.799217224121094
G0176149  342.5879211425781   5.086748123168945
G0188614  317.3526306152344   12.957232475280762
G0191566  316.4395751953125   7.965785026550293
G0197115  343.0567932128906   2.2420759201049805
G0203366  317.57708740234375  17.720905303955078
G0217228  319.831787109375    13.57975959777832
G0228798  343.8270568847656   9.654282569885254
G0253695  342.6175231933594   4.694252967834473
G0259099  306.0604553222656   21.34751319885254
G0288824  318.0233459472656   21.468807220458984
G0317142  314.04083251953125  15.730732917785645
G0331434  317.4542541503906   19.71814727783203
G0343435  319.633056640625    22.522260665893555
G0353352  318.4770202636719   19.369688034057617
G0364054  309.0512390136719   14.561393737792969
G0372182  318.5006103515625   17.060741424560547
G0381768  319.09576416015625  16.906875610351562
G0401046  316.5504455566406   13.690340995788574
G0522663  319.3000183105469   18.278528213500977
G0523053  343.2687683105469   4.272221088409424
G0527283  316.3482666015625   15.099641799926758
G0534476  318.4536437988281   14.539608001708984
G0539495  318.87933349609375  20.40052032470703
G0545746  316.9638366699219   14.697251319885254
G0547445  341.9770202636719   5.525643825531006
G0554727  306.6247863769531   11.826129913330078
G0556840  341.6595153808594   -5.284846782684326
G0573762  317.7817077636719   -2.038830041885376
G0598776  341.6076354980469   -0.02823299914598465
G0602666  342.7663879394531   7.761270999908447
G0605573  342.9013671875      11.007864952087402
G0607582  342.7892150878906   14.765083312988281
G0614708  341.5901184082031   -0.0615679994225502
G0620749  327.75787353515625  36.54386901855469
G0631040  341.7713623046875   1.530542016029358
G0635624  341.1427307128906   -4.696380138397217
G0642167  341.23883056640625  -4.472480773925781
G0653922  341.8634338378906   -4.3395609855651855
G0660376  319.55120849609375  65.61320495605469
G0662217  342.4907531738281   10.862078666687012
G0689029  311.7810363769531   0.3004690110683441
G0744560  342.2490539550781   -0.039427999407052994
G0747850  341.4222717285156   -1.4947960376739502
G0751988  342.1326599121094   12.047146797180176
G0751994  342.0005187988281   12.067659378051758
G0770966  341.9466247558594   12.857375144958496
G0771349  341.1048278808594   -5.725611209869385
G0809046  315.7451477050781   10.550166130065918
G0823379  342.5821228027344   10.903489112854004
G0829519  342.0823059082031   -5.330543041229248
G0830281  305.8343811035156   20.03953742980957
G0851960  318.37353515625     16.89679718017578
G0866592  319.7909851074219   19.712661743164062
G0867336  341.8969421386719   3.8530919551849365
G0870427  343.1185607910156   7.70672082901001
G0886808  343.18524169921875  6.3733930587768555
G0888699  341.6392517089844   -2.4654040336608887
G0888752  317.9061584472656   20.872385025024414
G0898451  319.516357421875    23.73065948486328
G0915065  308.6819763183594   17.92630386352539
G0915839  305.86822509765625  23.06815528869629
G0928322  330.2781066894531   36.06706237792969
G0929178  316.63287353515625  23.183130264282227
G0932932  315.3785400390625   11.500997543334961
G0935605  307.2861328125      14.036181449890137
G0941438  316.7498474121094   16.186092376708984
G0945181  342.4139404296875   1.4307090044021606
G0952296  342.9849853515625   6.389228820800781
G0994698  316.0340881347656   14.70421314239502
G0999336  341.67108154296875  1.467797040939331
G1005682  319.7104797363281   23.598472595214844
G1008274  341.0709228515625   11.441901206970215
G1009351  317.86376953125     18.007173538208008
G1016681  306.0959777832031   20.025863647460938
G1021078  304.6157531738281   24.826311111450195
G1026057  332.6576232910156   27.30628776550293
G1034138  343.5093078613281   1.7944929599761963
G1037493  342.1183776855469   3.353332996368408
G1046084  341.8002624511719   1.3708219528198242
G1051237  319.9819030761719   19.465940475463867
G1054477  316.6243896484375   9.170035362243652
G1055764  319.5661926269531   19.174840927124023
G1067663  318.821044921875    21.971057891845703
G1077484  318.376220703125    14.921242713928223
G1079830  317.7655029296875   15.193946838378906
G1080012  315.2541809082031   12.184548377990723
G1080147  317.9605407714844   20.99880027770996
G1086075  304.7977600097656   22.706878662109375
G1090502  330.4983215332031   33.39694595336914
G1090610  331.0491027832031   38.59846115112305
G1104348  318.2252197265625   13.14095401763916
G1106349  318.9924011230469   21.520658493041992
G1107026  315.6747131347656   22.257457733154297
G1108527  319.6886901855469   19.316713333129883
G1110425  318.8880310058594   23.226354598999023
G1121342  317.30206298828125  15.693902015686035
G1125633  342.62713623046875  3.7509210109710693
G1139958  341.84130859375     -1.8711689710617065
G1140068  314.84710693359375  12.177216529846191
G1140350  317.4183654785156   15.956110954284668
G1156117  343.60394287109375  5.693478107452393
G1178742  318.2795104980469   21.693946838378906
G1185561  306.64056396484375  21.61431884765625
G1192099  342.04345703125     -4.658606052398682
G1195858  318.24822998046875  21.24338722229004
G1196493  304.9854736328125   18.736492156982422
G1198664  342.1663513183594   1.5813930034637451
G1199228  342.7058410644531   1.948989987373352
G1205282  317.37872314453125  19.153308868408203
G1212826  303.58270263671875  19.835834503173828
G1244768  342.6612854003906   4.645647048950195
G1249024  343.2779541015625   3.833332061767578
G1275042  315.7004699707031   24.66737937927246
G1275459  344.1455383300781   7.17429780960083
G1283274  341.17327880859375  0.6272280216217041
G1284258  316.2783508300781   13.577127456665039
G1301461  318.7709655761719   17.448251724243164
G1308708  318.75531005859375  12.57158374786377
G1314325  342.0331115722656   8.019875526428223
G1319236  319.9844055175781   23.858163833618164
G1334362  318.15118408203125  22.59657859802246
G1342808  341.9000549316406   -3.1834468841552734
G1361431  342.41815185546875  7.987196922302246
G1366506  318.9411926269531   22.696460723876953
G1367112  341.81072998046875  7.746367931365967
G1367500  341.3768615722656   2.083343982696533
G1369863  343.3456115722656   5.787590980529785
G1371060  305.9384460449219   19.860227584838867
G1389431  310.9674377441406   15.59082317352295
G1391634  317.9789733886719   18.553525924682617
G1398951  317.0672302246094   18.098711013793945
G1405412  317.8551940917969   18.500783920288086
G1410444  306.4672546386719   22.671737670898438
G1410599  313.4918518066406   10.406656265258789
G1417508  315.5130615234375   16.657384872436523
G1426221  319.7685852050781   13.95448112487793
G1445948  340.8894958496094   -5.12808895111084
G1449047  342.3941650390625   1.8826509714126587
G1451963  316.8103332519531   19.12601661682129
G1462570  318.6368408203125   18.65683364868164
G1738900  342.4949951171875   0.918330013751983

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. Ozawa, 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 S190630ag,
T0 = 2019-06-30 18:52:05.180 UT (The LIGO Scientific Collaboration 
and Virgo Collaboration, GCN Circ. 24922
Loading...
 
 ), the CALET Gamma-ray 
Burst Monitor (CGBM) high voltages were off (from T0-15 min to 
T0+0.5 min).

The CALET Calorimeter (CAL) was operating in the high energy
trigger mode at the trigger time of S190630ag. 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.
The 90% upper limit of CAL is 1.2x10^-5 erg/cm^2/s (10-100 GeV) when
the summed LIGO-Virgo probability reaches 25%.
The CAL FOV was centered at RA= 84.0 deg, DEC= 31.5 deg at T0.

Q. B. Yi, S. Xiao, C. Cai, Q. Luo, 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 
S190630ag event (GCN #24922
Loading...
 
 ), trigger time 2019-06-30T18:52:05.18 UTC. 
At T0, more than 78% 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=220 deg, DEC=-60 deg), 
the 5-sigma upper-limits fluence (0.2 - 5 MeV, incident energy) are 
reported below:

Band model 1 (alpha=-1.9, beta=-3.7, Ep=70 keV):
1 s:   1.4e-07 erg cm^-2
10 s:  9.6e-07 erg cm^-2

Band model 2 (alpha=-1.0, beta=-2.3, Ep=230 keV):
1 s:   2.3e-07 erg cm^-2
10 s:  1.6e-06 erg cm^-2

Band model 3 (alpha=-0.0, beta=-1.5, Ep=1000 keV):
1 s:   5.3e-07 erg cm^-2
10 s:  4.5e-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.

D. Gotz (CEA/AIM), X.H. Han (NAOC), D. Dornic (CPPM), L.P. Xin (NAOC), 
D. Turpin (NAOC), Y.T. Zheng (GXU), C. Wu (NAOC)  on behalf of the SVOM consortium

We observed 52 sky regions (total: 7800 square degrees with overlaps)
to cover the skymap of the advanced LIGO/Virgo trigger S190630ag,
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 15 seconds
(10s exposure + 5s readout). 

The observations were made during two nights (2019.06.30-2019.07.01).
During the night of 2019.06.30, GWAC worked in survey mode. The survey
area covered over 5000 square degrees, including 15.2 % of the 90% c.l. GW error box. 
The images were taken between ~5 hours and ~1 hour before the event trigger
time, and no electromagnetic precursor has been found down to a 15.5
mag 3 sigma limit in the R band.

During the night of 2019.07.01, the GWAC worked on follow-up mode.
Over 5500 square degrees were observed. We estimate a 7.2% prior 
probability that the 19 observed and processed regions contain 
the true location of the source.

The coordinates of the 19 sky regions and observation times are listed below:

No. Ra  Dec start-obs(UTC)  end-obs(UTC)    Camera_ID

1 15:39:28.56 -15:20:36.24 2019-07-01 13:42:36 2019-07-01 14:10:58 034
2 17:06:36.00 -06:00:32.08 2019-07-01 13:37:08 2019-07-01 14:05:27 021
3 17:53:38.64 -06:34:09.05 2019-07-01 13:48:27 2019-07-01 14:08:40 022
4 18:03:11.52 +12:48:53.64 2019-07-01 14:32:56 2019-07-01 14:34:09 031
5 18:45:49.44 +01:11:14.78 2019-07-01 14:47:55 2019-07-01 15:09:24 033
6 18:53:52.32 +18:03:08.64 2019-07-01 13:21:25 2019-07-01 13:55:51 044
7 18:52:12.48 +30:09:05.40 2019-07-01 13:51:48 2019-07-01 13:55:51 041
8 19:16:11.76 +01:05:37.93 2019-07-01 14:09:31 2019-07-01 14:48:26 044
9 20:06:25.68 +01:07:06.78 2019-07-01 14:09:31 2019-07-01 14:57:44 043
10 20:07:04.56 +13:22:56.64 2019-07-01 14:09:32 2019-07-01 14:56:31 042
11 19:16:34.56 +13:12:15.48 2019-07-01 14:23:42 2019-07-01 14:57:44 041
12 21:10:37.92 +15:33:32.76 2019-07-01 14:32:34 2019-07-01 15:06:58 023
13 20:24:27.60 +15:51:24.48 2019-07-01 14:39:51 2019-07-01 15:02:54 024
14 20:22:31.20 +27:54:07.20 2019-07-01 14:41:28 2019-07-01 14:52:24 021
15 21:15:18.72 +27:15:52.92 2019-07-01 14:51:59 2019-07-01 15:08:09 022
16 21:19:04.56 +13:22:06.60 2019-07-01 15:03:19 2019-07-01 15:25:12 042
17 22:25:53.28 +15:31:49.44 2019-07-01 15:13:30 2019-07-01 15:27:40 023
18 21:39:43.20 +15:49:36.84 2019-07-01 15:13:30 2019-07-01 15:26:27 024
19 22:30:33.12 +27:14:10.32 2019-07-01 15:13:30 2019-07-01 15:28:52 022

The sky coverage map of the night 07.01 is available at: 
http://cmm.svom.cn/gwpub/O3/S190630ag/S190630ag_GWAC.png 
(user:svomo3 pwd:gwo3)

The weather conditions were good during the observations. A 3 sigma 
limiting magnitude of about 15.5 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.

Z. Kostrzewa-Rutkowska, D. Eappachen (SRON/RU), S. Hodgkin, A. Delgado, 
D.L. Harrison, M.van Leeuwen, G. Rixon, A. Yoldas (IoA Cambridge), P.G. Jonker
(SRON/RU) on behalf of Gaia Alerts team report the discovery of a transient
candidate within the probability skymap of S190630ag (LIGO/VIRGO
Collaboration GCN 24922
Loading...
 
 ):

---------------------------------------------------------------------------
Name      	TNSid    	 Date [TCB]       		RaDeg     DecDeg    AlertMag URL
----------------------------------------------------------------------------

Gaia19cua  AT2019kih
Loading...
 
   2019-07-02T10:26:22	219.41432   -54.98491  18.86
http://gsaweb.ast.cam.ac.uk/alerts/alert/Gaia19cua/
---------------------------------------------------------------------------

Note: Hostless galactic plane transient

Acknowledgements: This work has made use of data from the European Space
Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by
the Gaia Data Processing and Analysis Consortium (DPAC,
https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC
has been provided by national institutions, in particular the institutions
participating in the Gaia Multilateral Agreement. ZKR, DE, and PGJ
acknowledge support from the European Research Council under ERC
Consolidator Grant agreement no 647208.

The LIGO Scientific Collaboration and the Virgo Collaboration report:

We have conducted further analysis of the LIGO and Virgo data around
the time of the compact binary coalescence (CBC) candidate S190630ag
(GCN 24922
Loading...
 
 ). Parameter estimation has been performed using
LALInference [1] and a new sky map, LALInference.offline.fits.gz,
distributed via GCN Notice, is available for retrieval from the
GraceDB event page:

https://gracedb.ligo.org/superevents/S190630ag

LALInference.offline.fits.gz is the preferred sky map at this time.
The 90% credible region is 1483 deg2. Marginalized over the whole sky,
the a posteriori luminosity distance estimate is 926 � 259 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)