LIGO/Virgo S190510g

N. P. M. Kuin (UCL-MSSL), A. A. Breeveld (MSSL-UCL),  C. Gronwall (PSU),
F. E. Marshall (NASA/GSFC), S. R. Oates (Uni. of Warwick), M.J. Page
(UCL-MSSL),
M. de Pasquale (Istambul U), M. H. Siegel (PSU), A. D'Ai (INAF-IASFPA),
P. D'Avanzo (INAF-OAB), S. D. Barthelmy (NASA/GSFC), A. P. Beardmore (U.
Leicester),
D. N. Burrows (PSU), S. Campana (INAF-OAB), S. B. Cenko (NASA/GSFC),
G. Cusumano (INAF-IASF PA), V. D'Elia(ASDC), P. A. Evans (U. Leicester),
P. Giommi (ASI), D. Hartmann (Clemson U.), J. A. Kennea (PSU),
H. A. Krimm (NSF), A. Y. Lien (GSFC/UMBC), D. B. Malesani (DTU Space),
A. Melandri (INAF-OAB), J. A.  Nousek (PSU), P. T. O'Brien (U. Leicester),
J. P. Osborne (U. Leicester), C. Pagani (U. Leicester), K. L. Page
(U.Leicester),
D.M. Palmer (LANL), M. Perri (ASDC), J. L. Racusin (NASA/GSFC), T. Sakamoto
(AGU),
B. Sbarufatti (INAF-OAB/PSU), G. Tagliaferri (INAF-OAB), A. Tohuvavohu
(PSU),
and E. Troja (NASA/GSFC/UMCP) report on behalf of the Swift team:

Swift UVOT instrument started follow up observations of LVC event S190510g
121 minutes after the event until just over 3 days later, observing 977
fields
in the highest probability region (Evans et al., GCN Circ. No. 24541).

The UVOT approach for searching for the ultraviolet-optical counterpart has
been described in Kuin et al. (GCN Circ. No. 24767). The limiting magnitude
can vary but typically is 18.6th magnitude (Vega). The automated UVOT
processing
found 2836 galaxies using the GLADE catalog and flagged 121 counterpart
candidates. Human inspection of these 121 candidates found no credible
optical-ultraviolet source for the event, but 105 out of the 121 candidates
were due to an unstable attitude or due to image artifacts from very bright
sources. Neither did further inspection of the images of the galaxies lead
to a candidate missed by the automated processing.

Z. Kostrzewa-Rutkowska (SRON/RU), S. Hodgkin, A. Delgado, D.L. Harrison, M.
van Leeuwen, G. Rixon, A. Yoldas (IoA Cambridge), D. Eappachen, P.G. Jonker
(SRON/RU) on behalf of Gaia Alerts team report the discovery of a transient
candidate within the probability skymap of S190510g (the LIGO Scientific
Collaboration and the Virgo Collaboration, GCN 24442
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 ):

---------------------------------------------------------------------------
Name      TNSid     Date [TCB]          RaDeg     DecDeg    AlertMag URL
---------------------------------------------------------------------------
Gaia19btm AT2019fhw
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  2019-05-11T18:20:30 92.78350 -18.11934  18.36
       http://gsaweb.ast.cam.ac.uk/alerts/alert/Gaia19btm/
---------------------------------------------------------------------------


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.

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

Swift has performed a series of 977 observations, covering 977 separate
locations within the LVC error region for the GW trigger S190510g
convolved with the 2MPZ catalogue (Bilicki et al. 2014, ApJS, 210, 9),
using 226 fields from the 'bayestar' GW localisation map and 751 fields
from the 'LALInference' GW localisation map. As these are 3D skymaps,
galaxy distances were taken into account in selecting which ones to
observe. The observations currently span from 7.2 ks to 270 ks after
the LVC trigger, and cover 76.9 sq degrees on the sky (corrected for
overlaps). This covers 58% of the probability in the 'LALInference'
skymap, and 67% after convolving with the 2MPZ galaxy catalogue, as
described by Evans et al., (2016, MNRAS,  462, 1591). Using the earlier
'bayestar' skymap our observations cover 10% of the probability (14%
when convolved).

We have detected 33 X-ray sources. Each source is assigned a rank of
1-4 which describes how likely it is to be related to the GW trigger,
with 1 being the most likely and 4 being the least likely. The ranks
are described at http://www.swift.ac.uk/ranks.php.

We have found:

   * 0 sources of rank 1
   * 0 sources of rank 2
   * 5 sources of rank 3
   * 28 sources of rank 4

Details of these sources can be viewed online via 
http://www.swift.ac.uk/LVC/

For all GW triggers from O3 onwards, XRT results will appear on this 
page, once human verification has taken place to remove spurious sources.

Additionally, our search serendipitously covered the locations of some 
of the other reported candidates. In particular the location of 
DG19fqqk/desgw-190510c (GCNs 24467
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 , 24480
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 ) was covered 4 times. No XRT 
source was found with a 3-sigma upper limit of 6.1 x 10^-2 ct/sec, 
corresponding to a 0.3-10 keV flux of 2.6 x 10^-12 erg cm^-2 s^-1. The 
location of DG19llhk (GCNs 24467
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 ) was covered 3 times with no detection 
found, down to a  3-sigma upper limit of 6.4 x 10^-2 ct/sec, 
corresponding to 2.8e-12 erg cm^-2 s^-1. Both flux conversions assume a 
power-law spectrum with photon index=1.7 and absorption column NH=3 x 
10^20 cm^-2.

This circular is an official product of the Swift-XRT team.

Erik Kool (OKC), Daniel A. Goldstein (Caltech), and Igor Andreoni (Caltech) on behalf of the Global Relay of Observatories Watching Transients Happen (GROWTH) collaborations:

As part of the follow up effort described in Andreoni et al. (2019, GCN #24467
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 ) of the high-probability region of the LALInference skymap of gravitational wave source S190510g (LIGO/VIRGO Collaboration, GCN #24448
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 ) with the Dark Energy Camera (DECam), we report the detection of an additional optical counterpart candidate, DS19qcso. The transient was detected ~2��� offset to the N of the nucleus of its host galaxy through difference imaging using an automated pipeline, and appeared in g and r-band, but not in z-band. Coordinates and observed magnitudes (at jday 2458614.5) are as follows:

DS19qcso
Coordinates: 88.208631 -30.381382 (05:52:50.07 -30:22:53.0)
g mag: 21.57 (0.13)
r mag: 22.69 (0.21)
z mag: > 21.9

The host galaxy is identified as 2MASXi J0552500-302254, but no host redshift is available. From Pan-STARRS imaging, we measure the host galaxy to be 15������ across. Postage stamp images of the candidate can be viewed at the following link:

https://portal.nersc.gov/project/ptf/cutouts/DG19qcso.png

We thank the CTIO staff, Steve Heathcote, Kathy Vivas, Tim Abbott, for facilitating these Target of Opportunity observations.

GROWTH is a worldwide collaboration comprising Caltech, USA; IPAC, USA, WIS, Israel; OKC, Sweden; JSI/UMd, USA; U Washington, USA; DESY, Germany; MOST, Taiwan; UW Milwaukee, USA; LANL USA; Tokyo Tech, Japan; IIT-B, India; IIA, India; LJMU, UK; TTU USA and USyd, Australia. GROWTH acknowledges generous support of the NSF under PIRE Grant No 1545949. An optimized schedule was generated using the ToO marshal system (Coughlin et al. 2019). Alert filtering and follow-up co-ordination is being undertaken by the GROWTH marshal system (Kasliwal et al. 2019).

This research draws upon DECam data as distributed by the Science Data Archive at NOAO. NOAO is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. This project used data obtained with the Dark Energy Camera (DECam), which was constructed by the Dark Energy Survey (DES) collaboration.

This message may be cited.

A. J. Castro-Tirado (IAA-CSIC), A. F. Valeev and V. V. Sokolov 
(SAO-RAS), Y.-D. Hu, X.-Y. Li, A. Ayala, and E.  Fernandez-Garcia 
(IAA-CSIC), R. Sanchez-Ramirez (INAF-IAPS), A. Castellon (UMA) and G. 
Gomez-Velarde (GRANTECAN, IAC, ULL), on behalf of a larger 
collaboration, report:

Following the detection of AT2019ezb
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  and AT2019far
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  (Srivastav et al., 
GCNC 24517) within the error area of the GW event S190510g (LVC, GCNC 
24442), we obtained optical spectra (900s) covering the range 3700-7500 
A with the 10.4m GTC telescope equipped with OSIRIS in La Palma (Spain) 
starting on May 13, 23:55 UT.

The AT2019ezb
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  spectrum is consistent with a SNIc at the host galaxy 
redshift (z=0.0712).

The AT2019far
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  spectrum is consistent with a SNIIp at the host galaxy 
redshift (z=0.0583).

Therefore both transients are unrelated to the GW event S190510g.

We acknowledge the excellent support from the GTC staff.

Myungshin Im (SNU), Joonho Kim (SNU), Chung-Uk Lee (KASI), Seung-Lee Kim
(KASI), Gregory S. H. Paek (SNU),  Gu Lim (SNU),  Changsu Choi (SNU),
 Sungyong Hwang (SNU), Bomi Park (SNU), Sophia Kim (SNU),  Hyung Mok Lee
(KASI), on behalf of a larger collaboration

We report the results from further KMTNet observation of the optical
counterpart candidates from DECam-GROWTH and DESGW (Andreoni et al. GCN
24467
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 ; Annis et al. GCN 24474
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 ; Sores-Santos et al. GCN 24480
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 ) of the BNS
merger candidate event, S190510g (LIGO/Virgo GCN 24448
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 ). This is a
follow-up report of the KMTNet result (Im et al. GCN 24493
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 ), adding data
points taken after our earlier report.  With the additional data, we now
have at least one day cadence of KMTNet data of all the objects enabling us
to determine their variability for 1 day or more using internally
consistent photometry. The list of the observed targets are given below,
 along with preliminary R-band magnitudes. None of the candidates below
show significant fading (> 0.5 mag) over ~1 day. All of the candidates show
very slow (<0.2 mag) or no fading, consistent with them being supernovae.

We thank the KMTNet staffs for performing the observation.

  ::::::::::::::
desgw-190510a
::::::::::::::
#Date_Obs   MJD   Mag   Magerr   Depth
2019-05-11T17:33:16    58614.73125     21.26     0.061     21.55
2019-05-11T23:30:03    58614.97917     21.27     0.034     22.10
::::::::::::::
DG19bexl
::::::::::::::
#Date_Obs   MJD   Mag   Magerr   Depth
2019-05-10T17:54:47    58613.74583     21.21     0.041     21.95
2019-05-11T16:57:13    58614.70625     21.50     0.094     21.21
2019-05-11T23:48:04    58614.99167     21.57     0.053     22.02
::::::::::::::
DG19etsk
::::::::::::::
#Date_Obs   MJD   Mag   Magerr   Depth
2019-05-10T16:57:54    58613.70625     20.87     0.048     21.57
2019-05-10T17:33:32    58613.73125     21.12     0.067     21.92
2019-05-10T17:33:32    58613.73125     20.92     0.046     21.92
2019-05-11T17:42:31    58614.73750     20.89     0.063     21.52
2019-05-11T23:54:11    58614.99583     20.88     0.066     21.97
::::::::::::::
DG19fqqk
::::::::::::::
#Date_Obs   MJD   Mag   Magerr   Depth
2019-05-10T18:08:23    58613.75556     20.58     0.042     21.53
2019-05-10T23:45:52    58613.98958     20.89     0.037     21.75
2019-05-11T17:36:25    58614.73333     20.72     0.043     21.85
2019-05-11T23:36:06    58614.98333     20.80     0.038     22.10
::::::::::::::
DG19lcnl
::::::::::::::
#Date_Obs   MJD   Mag   Magerr   Depth
2019-05-10T23:33:34    58613.98125     19.92     0.040     21.48
2019-05-11T17:23:49    58614.72431     19.82     0.026     21.17
2019-05-11T23:24:10    58614.97500     19.85     0.037     22.08
::::::::::::::
DG19llhk
::::::::::::::
#Date_Obs   MJD   Mag   Magerr   Depth
2019-05-10T17:08:10    58613.71389     21.24     0.042     21.61
2019-05-10T17:20:36    58613.72222     21.17     0.051     22.81
2019-05-11T08:33:29    58614.35625     99.00    99.000     20.95
2019-05-11T17:20:40    58614.72222     21.37     0.114     21.15
2019-05-11T23:18:08    58614.97083     21.25     0.049     22.04
::::::::::::::
DG19nanl
::::::::::::::
#Date_Obs   MJD   Mag   Magerr   Depth
2019-05-10T23:33:34    58613.98125     20.42     0.035     21.44
2019-05-11T22:59:57    58614.95764     20.52     0.032     21.53
::::::::::::::
DG19nouo
::::::::::::::
#Date_Obs   MJD   Mag   Magerr   Depth
2019-05-10T17:20:36    58613.72222     21.64     0.048     21.85
2019-05-10T23:21:17    58613.97292     21.51     0.052     22.04
2019-05-11T17:55:27    58614.74653     21.38     0.057     21.43
::::::::::::::
DG19oahn
::::::::::::::
#Date_Obs   MJD   Mag   Magerr   Depth
2019-05-11T16:50:54    58614.70139     19.48     0.030     20.74
2019-05-11T23:42:11    58614.98750     19.58     0.033     22.02
::::::::::::::
DG19ootl
::::::::::::::
#Date_Obs   MJD   Mag   Magerr   Depth
2019-05-10T23:33:34    58613.98125     21.51     0.068     21.49
2019-05-11T23:06:06    58614.96250     21.42     0.062     21.81
::::::::::::::
DG19ukvo
::::::::::::::
#Date_Obs   MJD   Mag   Magerr   Depth
2019-05-10T16:48:24    58613.70000     21.56     0.146     20.92
2019-05-11T17:49:08    58614.74236     21.71     0.082     21.58
::::::::::::::
DG19yhhm
::::::::::::::
#Date_Obs   MJD   Mag   Magerr   Depth
2019-05-10T17:20:36    58613.72222     20.43     0.042     21.67
2019-05-10T23:21:17    58613.97292     20.33     0.052     22.08
2019-05-11T23:12:03    58614.96667     20.35     0.041     21.87
::::::::::::::
DG19zaxn
::::::::::::::
#Date_Obs   MJD   Mag   Magerr   Depth
2019-05-10T17:27:13    58613.72708     21.16     0.040     22.02
2019-05-11T18:01:33    58614.75069     21.13     0.047     21.53

S. Srivastav, K. W. Smith, S. J. Smartt (QUB), K. Chambers, M. Huber,
T. de Boer, J. Bulger, J. Fairlamb, C.-C. Lin, T. Lowe, E. Magnier
A. Schultz, R. J. Wainscoat, M. Willman (IfA, Univ. Hawaii),
D. R. Young, O. McBrien, J. Gillanders.  D. O'Neil, P. Clark, S. Sim
(QUB), L. Denneau, H. Flewelling, A. Heinze, J. Tonry, H. Weiland
(IfA, Univ. Hawaii), A. Rest (STScI), B. Stalder (LSST), C. Stubbs
(Harvard)

We report observations of the BAYESTAR skymap of the BNS event S190510g
(The LIGO Scientific Collaboration and the Virgo Collaboration, GCN
24442
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 ) with the Pan-STARRS1 telescope (Chambers et al. 2016,
arXiv:1612.05560
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 C) and the ATLAS telescopes (Tonry et al. 2018, PASP
PASP, 13, 164505). 

We acknowledge that is now a marginal candidate (LSC & VC, GCN 24489
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 )
and note that we completed our scanning of the BAYESTAR skymap, before
the LALInference map was available (resulting in a final 4%
probability coverage).

For Pan-STARRS1 : images were taken in the PS1 w and i-bands (Tonry
et al. 2012, ApJ 750, 99) in the standard NEO search sequence. At each
pointing position a sequence of quads (4 x 45 sec) was taken. This
observing sequence ensures exactly the same pointing position for each
of the quads.

The PS1 images were processed with the IPP (Magnier et al. 2016,
arXiv:1612.05240
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 ) and difference images were produced using the
Pan-STARRS1 Science Consortium 3Pi images as reference
frames. Transient candidates were run through our standard filtering
procedures, combined with a machine learning algorithm (Wright et
al. 2015, MNRAS, 449, 451) and all candidates were
spatially cross-matched with known minor planets, and major star,
galaxy, AGN and multi-wavelength catalogues (as described in Smartt et
al. 2016, MNRAS, 462 4094).

For ATLAS, we observed with sequences of 4 x 30s, typically reaching
o ~ 19.5 in each pointing (e.g. Weiland et al. GCN 24107
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 ).

We covered the small probability region of the LalInference map (total
summed probability of 4%) at 13-14hrs (the 6hr region was not visible
from Hawaii).  We began taking Pan-STARRS data at 2019-05-10 07:09
(UTC), ~4.2 hrs after the GW trigger. ATLAS started at a similar time.

No new extragalactic transient candidates were discovered with ATLAS
within the 90% contour (brighter than about o ~ 19.5) 

In the PS1 data, the following 23 transients were found lying within
the 90% contour of the LALInference map. We give them 3 ranks : 

Rank 1 candidates are plausibly within the distance range reported by
the LIGO-Virgo analysis (~130 Mpc < d < ~220 Mpc). This comes from
host galaxy association and their spectroscopic or photometric
redshifts. 

Rank 2 candidates are not obviously associated with a catalogued
host galaxy. 

Rank 3 candidates are probably associated with a galaxy outside the
distance range.

Name      | PS Name | RA (J2000)  | Dec (J2000) | Disc. MJD  | Disc Mag | Notes
-------------------------------------------------------------------------------
Rank 1 
AT2019ezb
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  | PS19xv  | 13 43 59.78 | +01 50 32.7 |  58613.30  |  20.50 i |  (1)
AT2019far
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  | PS19aaf | 14 17 22.53 | +05 01 08.7 |  58613.48  |  20.29 i |  (2)

Rank 2 
AT2019ezc
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  | PS19yn  | 13 24 04.80 | -09 02 05.8 |  58613.34  |  20.16 i | 
AT2019eya
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  | PS19yi  | 13 27 23.56 | -07 01 41.2 |  58613.39  |  20.78 i | 
AT2019fam
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  | PS19yp  | 13 39 00.66 | -04 28 30.7 |  58613.39  |  20.25 i | 
AT2019eyg
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  | PS19yz  | 13 42 05.60 | -09 43 24.7 |  58613.35  |  20.60 i |  
AT2019fal
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  | PS19zf  | 13 46 08.91 | -03 22 40.1 |  58613.39  |  20.92 i |   
AT2019eyp
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  | PS19zh  | 14 05 46.51 | +03 25 21.4 |  58613.50  |  21.36 w |
AT2019eyu
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  | PS19aaj | 14 06 15.69 | +03 45 58.4 |  58613.48  |  20.57 i |  

Rank 3 
AT2019exz
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  | PS19yh  | 13 17 59.93 | -04 36 33.5 |  58613.39  |  19.93 i |  (3)
AT2019faa
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  | PS19xz  | 13 21 30.14 | +01 59 03.5 |  58613.30  |  21.02 i |  (4)
AT2019ezy
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  | PS19xx  | 13 27 22.91 | +01 28 19.0 |  58613.30  |  20.11 i |  (5)
AT2019fan
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  | PS19yo  | 13 28 01.32 | -03 47 08.3 |  58613.39  |  20.76 i |  (6)
AT2019eyi
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  | PS19xs  | 13 31 45.46 | -00 04 26.5 |  58613.30  |  20.23 i |  (7)
AT2019eza
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  | PS19xr  | 13 51 04.52 | +03 54 53.4 |  58613.30  |  20.42 i |  
AT2019fae
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  | PS19yd  | 13 51 53.52 | +00 45 54.8 |  58613.30  |  20.68 i |  (8)
AT2019fac
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  | PS19yb  | 13 53 05.69 | +08 16 45.3 |  58613.30  |  20.84 i |  (9)
AT2019eyf
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  | PS19yg  | 13 58 13.27 | +05 13 28.2 |  58613.30  |  19.87 i |   
AT2019eyv
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  | PS19aah | 14 03 35.78 | +08 11 25.3 |  58613.48  |  21.14 i |  
AT2019fbj
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  | PS19abe | 14 05 22.17 | +06 35 48.7 |  58613.48  |  21.14 i |  
AT2019eyn
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  | PS19zk  | 14 07 17.08 | +08 23 33.3 |  58613.48  |  20.49 i |  (10)
AT2019ezl
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  | PS19zx  | 14 13 00.93 | +07 50 02.5 |  58613.48  |  20.09 i |   
AT2019ezv
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  | PS19aau | 14 17 39.18 | +02 08 39.1 |  58613.50  |  19.80 w |  (11)


(1) Probable host is SDSS J134359.83+015034.4 at a spectroscopic z = 0.072 or D ~ 323 Mpc (NED), yielding an absolute i-band magnitude of ~-17.0 mag 
(2) Probable host is SDSS J141300.92+075002.6 at a spectroscopic z = 0.058 or D ~ 259 Mpc (NED), yielding an absolute i-band magnitude of ~ -16.8 
(3) Probable host is GALEXASC J131800.06-043633.9 at a spectroscopic z = 0.132 or D ~ 603 Mpc (NED) 
(4) Probable host is SDSS J132130.22+015903.0 at a photometric z = 0.291 +/- 0.141 or D ~ 1431 Mpc (SDSS) 
(5) Probable host is SDSS J132722.06+012818.6 at a photometric z = 0.068 +/- 0.012 or D ~ 308 Mpc (NED) 
(6) Probable host is LCRS B132526.4-033142 at a spectroscopic z = 0.087 or D ~ 388 Mpc (NED) 
(7) Probable host is SDSS J133145.14-000431.3 at a photometric z = 0.185 +/- 0.018 or D ~ 899 Mpc (SDSS) 
(8) Probable host is 2MASX J13515347+0045515 at a spectroscopic z = 0.088 or D ~ 389 Mpc (NED) 
(9) Probable host is SDSS J135153.50+004551.2 at a photometric z = 0.230 +/-0.151 or D ~ 1148 Mpc (SDSS) 
(10) Probable host is 2MASX J14071678+0823347 at a spectroscopic z = 0.115 or D ~ 532 Mpc (NED) 
(11) Probable host is SDSS J141738.94+020831.9 at a spectroscopic redshift of z = 0.129 or D ~ 584 Mpc (NED)

S. Gomez (Harvard), P. S. Cowperthwaite (Carnegie), G. Hosseinzadeh (Harvard), E. Berger (Harvard), P. K. Blanchard (Harvard), M. R. Drout (Carnegie/U. Toronto), T. Eftekhari (Harvard), M. Nicholl (Edinburgh), L. Patton (Harvard), A. L. Piro (Carnegie), V. A. Villar (Harvard), P.K.G. Williams (Harvard), P. Goudfrooij (STScI), and T. Puzia (PUC, Chile)


We report on spectroscopic observations conducted with the IMACS Spectrograph on the 6.5m Magellan-Baade telescope of a candidate optical counterpart to the gravitational wave event S190510g (The LIGO Scientific Collaboration and the Virgo Collaboration, GCN 24442
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 ). The counterpart was identified during difference image processing of public DECam observations (Andreoni et al. GCN 24443
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 , Andreoni et al. GCN 24467
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 , Soares-Santos et al. GCN 24480
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 ).

Lists of promising counterparts were identified on the basis of factors such as their brightness, colors, and possible host galaxy association. We were able to obtain deep spectroscopy of DG19fqqk/desgw-190510c, which is an interesting source as it was flagged by a light curve classifier trained to identify kilonovae (KN-Classify, GCN 24480
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 ).

Target                                   | Reference                         | Classification                     
----------------------------------------------------------------------------------------------------------------
DG19fqqk/desgw-190510c  | GCN 24467
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 , GCN 24480
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   | Type II (phase = +6 days)

DG19fqqk/desgw-190510c shows a broad feature consistent with H-alpha at a redshift of 0.06 and template matching using Superfit (Howell et al. 2005, ApJ, 634, 1190) suggests a good match to a Type II SNe approximately one week after peak brightness. This candidate was also observed by KMTNet (GCN #24493
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 ) and showed no significant fading over ~1 day.

We conclude that the transient is not associated with the gravitational wave event S190510g.

We thank Paul Goudfrooij and Thomas Puzia for taking these observations.

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

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres (The Instituto 
de Astrofisica de Canarias),


D. Buckley (South African Astronomical Observatory),


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


R. Podesta, C. Lopez, C.Francile, F. Podesta (Observatorio Astronomico  Felix 
Aguilar OAFA, San Juan National University),

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


O. Gress, N.M. Budnev, O.Ershova (Applied Physics Institute, Irkutsk Stat 
University),

V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev (Blagoveschensk EducationState 
University),

MASTER OT J135130.87-525534.4 (2019fcc) - OT inside PGC087378

MASTER-OAFA auto-detection system ( <A 
HREF="http://www.hindawi.com/journals/aa/2010/349171/">Lipunov et al., 
"MASTER Global Robotic Net",
Advances in Astronomy, 2010, 30L</A> ) discovered OT source at (RA, Dec) = 
13h 51m 30.87s -52d 55m 34.4s on 2019-05-12.29047 UT.
The OT unfiltered magnitude is ~ 17m (mlim=18.4m).

The OT is seen in 2 images. There is no minor planet at this place.

We have reference image without OT on 2016-07-06.02547 UT with magnitude 
limit in 'clear' filter 19.0m.

THe OT offset from center of the PGC087378 galaxy is 2.1E 11S.
The distance is about ~50Mpc.

The same transient we see 12 hours after trigger time in MASTER-SAAO 
database.

Folow up observations are required.

Gregory S.H. Paek, Myungshin Im (CEOU/SNU), Taewoo Kim, and Wonseok Kang
(DOAO) on behalf of a larger collaboration

We observed 12 host galaxy candidates with the 1.0-m telescope at the
Deokheung Optical Astronomy Observatorythe in the 90% updated localization
area of S190510g, detected by LIGO/Virgo (GCN #24442
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 ).
The observation started at 2019-05-10 14:35:16, and 9 images were taken in
R-band with 120 sec exposure time for each fields. No obvious transient has
been identified to a preliminary 3-sigma depth of R=21.5 AB mag. The list
of the inspected targets in the observed fields is given below.

FIELD     date-obs[UT]         UL[AB]  NOTE
G0028316  2019-05-10 15:03:14  20.359  PGC159415, PGC1050569
G0031507  2019-05-10 15:47:31  21.881  PGC48754, PGC48717
G0450408  2019-05-10 14:43:43  21.432  PGC95645, PGC1109881, NGC5192,
PGC1104597
G0550129  2019-05-10 15:57:40  21.791  PGC158865, PGC3105750, PGC1068483
G0595818  2019-05-10 15:22:47  21.829  PGC0595818

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. Ozawa, 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:

The CALET Gamma-ray Burst Monitor (CGBM) was operating at the 
trigger time of S190510g T0=2019/05/10 02:59:39.292 UT (The LIGO 
Scientific Collaboration and Virgo Collaboration, GCN Circ. 24442
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 , 
24448
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  and 24462
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 ).  

No CGBM on-board trigger occurred around the event time.  Based 
on the LIGO-Virgo localization sky map, most of the part of the high
probability area was outside of the field-of-view of CGBM.  The 
summed LIGO probabilities inside the HXM and the SGM field of
view are 2% and 7% (and 84% credible region of the updated
localization map were Earth-occulted).  The HXM and SGM field of
views were centered at RA=298.7 deg, Dec = 60.7 deg and
RA=295.7 deg, Dec=50.8 deg at T0.

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 (7-3000 keV) or the SGM (40 keV -28 MeV) data. 

The CALET Calorimeter (CAL) was operating in high energy trigger
mode at the trigger time of S190510g. Using 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 is no significant overlap with the LVC location 
probability map.  The CAL FOV was centered at RA=295.7 deg, 
Dec=50.8 deg at T0.

Myungshin Im (SNU), Joonho Kim (SNU), Chung-Uk Lee (KASI), Seung-Lee Kim
(KASI), Gregory S. H. Paek (SNU),  Gu Lim (SNU),  Changsu Choi (SNU),
 Sungyong Hwang (SNU), Bomi Park (SNU), Sophia Kim (SNU),  Hyung Mok Lee
(KASI), on behalf of a larger collaboration

With KMTNet, we observed the optical counterpart candidates from
DECam-GROWTH and DESGW (Andreoni et al. GCN 24467
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 ; Annis et al. GCN 24474
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 ;
Sores-Santos et al. GCN 24480
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 ) of the BNS merger candidate event, S190510g
(LIGO/Virgo GCN 24448
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 ). The observation took place at the KMTNet South
Africa (SAAO), Chile (CTIO), and Australia (SSO) stations. The list of the
observed targets are given below,  along with preliminary R-band
magnitudes. Note that the errors do not include systematic errors due to
image subtraction. The error associated with the image subtraction should
be considered to be 0.1-0.2 mag at this moment. None of the candidates
below show significant fading (> 0.5 mag) over ~1 day. All of the
candidates show very slow or no fading, consistent with them being
supernovae. Further observation is ongoing.
We thank the KMTNet staffs for performing the observation.


Object name       UT                                R(mag) Rerr
desgw-190510a   2019-05-11T17:33:16   21.26  0.07

DG19bexl            2019-05-10T17:54:47    21.21  0.04
                            2019-05-11T16:57:13    21.49  0.09

DG19etsk            2019-05-10T17:33:32    20.92  0.10


DG19fqqk            2019-05-10T18:08:23   20.57   0.04
(desgw-190510c) 2019-05-10T23:45:52   20.88   0.04
                              2019-05-11T17:36:25   20.71  0.04

DG19lcnl             2019-05-10T23:33:34   19.92   0.04

                            2019-05-11T17:23:49   19.82   0.03

DG19llhk             2019-05-10T17:08:10   21.23   0.04
                            2019-05-10T17:20:36   21.17   0.05
                            2019-05-11T17:20:40   21.37   0.11

DG19nanl           2019-05-10T23:33:34   20.43   0.04

DG19nouo          2019-05-10T17:20:36   21.64  0.05
                            2019-05-10T23:21:17   21.51  0.05


DG19oahn          2019-05-11T16:50:54   19.48  0.03

DG19ootl            2019-05-10T23:33:34   21.51  0.07

DG19ukvo          2019-05-10T16:48:24   21.56  0.14

DG19yhhm         2019-05-10T17:20:36   20.43   0.04
                            2019-05-10T23:21:17  20.33  0.05


DG19zaxn          2019-05-10T17:27:13  21.16   0.04

V. Lipunov,(Lomonosov Moscow State University, SAI, Physics Department),

I am sorry.
The OT MASTER142812.05-013615.2 is the known SN 2019dde and can not 
connected with  LIGO/Virgo S190510g .
https://wis-tns.weizmann.ac.il/object/2019dde

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

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres (The 
Instituto de Astrofisica de Canarias),


D. Buckley (South African Astronomical Observatory),


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


R. Podesta, C. Lopez, C.Francile, F. Podesta (Observatorio Astronomico  Felix 
Aguilar OAFA, San Juan National University),

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


O. Gress, N.M. Budnev, O.Ershova (Applied Physics Institute, Irkutsk Stat 
University),

V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev (Blagoveschensk EducationState 
University),

OT MASTER142812.05-013615.2 discovery.


MASTER-IAC auto-detection system discovered OT source at (RA, Dec) = 14h 
28m 12.05s -01d 36m 15.2s on 2019-05-11.03821 UT.
The OT unfiltered magnitude is 17.6m (limit 20.0m).

The OT is seen in 2 images. There is no minor planet at this place.

We have reference image without OT on 2016-03-09.04372 UT with unfiltered 
magnitude limit 20.3m.
There is low surface brightness galaxy (from HSC-SSP)  with 2.7 arcsec 
offset at 14 28 12.0144	-01 36 17.316
This OT  is good candidate for Gravitational Waves counterpart.

Spectral observations are required.

The discovery and reference images are available at:

http://master.sai.msu.ru/static/OT/142812.05-013615.2.png

Folow up observations are required.

The LIGO Scientific Collaboration and the Virgo Collaboration report:


We have conducted subsequent analysis of data around the time of S190510g

including LIGO and Virgo data collected in the 24 hour period after the

event.  The resulting re-estimate of the background model yields a

FAR (False Alarm Rate) of 1 in 3.6 years compared to 1 in 37 years initially

reported in GCN 24442
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 .


Using the updated background model, the classification of the event,

in order of descending probability, is estimated to be:

Terrestrial (58%), BNS (42%), NSBH (<1%), BBH (<1%), or MassGap (<1%).


Further analysis of the event is ongoing. Updates will be provided

as and when available.


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/>.

Iair Arcavi (Tel Aviv University), D. Andrew Howell (LCO/UCSB), Daichi Hiramatsu (LCO/UCSB), Jamison Burke (LCO/UCSB), Curtis McCully (LCO), Craig Pellegrino (LCO/UCSB), Paul Groot (Radboud University), on behalf of the Las Cumbres GW Follow-up Collaboration


We report 300s g- and i-band images of the following galaxies (obtained from the GLADE 2.3 catalog; Dalya et al. 2018, MNRAS, 479, 2374) in the LIGO/Virgo S190510g localization region (Chu et al, GCN 24448
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 ) with the Las Cumbres Observatory 1m telescopes at the SAAO, South Africa and the CTIO, Chile. We find no significant counterpart candidates from visual inspection of the images.


Name                    GLADE-ID RA Dec      UT FILTER Approx Lim-mag

2MASS 05482759-3258380  4768 87.11500 -32.9772  2019-05-1017:25:56 g 22.66

2MASS 05482759-3258380  4768 87.11500 -32.9772  2019-05-1017:31:38 i 22.09

2MASS 05490223-3129287  30042 87.25932 -31.4913  2019-05-1016:47:07 g 21.83

2MASS 05490223-3129287  30042 87.25932 -31.4913  2019-05-1016:52:48 i 21.56

2MASS 05500408-3034504  110676 87.51703 -30.5807  2019-05-1016:59:54 g 22.49

2MASS 05500408-3034504  110676 87.51703 -30.5807  2019-05-1017:05:36 i 23.00

2MASS 05502872-3344293  26624 87.61970 -33.7415  2019-05-1023:22:16 g 22.38

2MASS 05502872-3344293  26624 87.61970 -33.7415  2019-05-1023:27:57 i 21.69

2MASS 05504985-3144266  19812 87.70773 -31.7407  2019-05-1017:12:54 g 22.69

2MASS 05504985-3144266  19812 87.70773 -31.7407  2019-05-1017:18:36 i 21.87

2MASS 05505599-3447027  7534 87.73330 -34.7841  2019-05-1017:12:54 g 22.87

2MASS 05505599-3447027  7534 87.73330 -34.7841  2019-05-1017:18:36 i 21.83

2MASS 05511621-3106167  9683 87.81755 -31.1046  2019-05-1016:47:01 g 21.69

2MASS 05511621-3106167  9683 87.81755 -31.1046  2019-05-1016:52:42 i 21.31

2MASS 05514992-3144460  13462 87.95801 -31.7461  2019-05-1023:35:19 g 22.38

2MASS 05514992-3144460  13462 87.95801 -31.7461  2019-05-1023:41:00 i 21.63

2MASS 05574070-3456018  22967 89.41962 -34.9338  2019-05-1023:48:21 g 22.45

2MASS 05574070-3456018  22967 89.41962 -34.9338  2019-05-1023:54:02 i 21.72

2MASS 06011509-3132255  21382 90.31288 -31.5404  2019-05-1017:38:57 g 23.60

2MASS 06011509-3132255  21382 90.31288 -31.5404  2019-05-1017:44:46 i 21.85

2MASS 06024073-3420093  130705 90.66974 -34.3359  2019-05-1017:38:58 g 22.64

2MASS 06024073-3420093  130705 90.66974 -34.3359  2019-05-1017:44:40 i 22.21

2MASS 06033989-3208521  5089 90.91624 -32.1478  2019-05-1017:25:56 g 22.41

2MASS 06033989-3208521  5089 90.91624 -32.1478  2019-05-1017:31:38 i 21.70

2MASS 06055976-3250371  9684 91.49903 -32.8437  2019-05-1023:10:04 g 22.31

2MASS 06055976-3250371  9684 91.49903 -32.8437  2019-05-1023:15:45 i 21.35

2MASS 06064749-3348522  13891 91.69790 -33.8145  2019-05-1017:52:00 g 21.81

2MASS 06064749-3348522  13891 91.69790 -33.8145  2019-05-1017:53:58 g 22.59

2MASS 06064749-3348522  13891 91.69790 -33.8145  2019-05-1017:59:40 i 22.06

2MASS 06084611-3354584  14569 92.19215 -33.9162  2019-05-1022:55:30 g 21.58

2MASS 06084611-3354584  14569 92.19215 -33.9162  2019-05-1023:01:11 i 21.23

2MASS 06100073-3338309  136310 92.50307 -33.6419  2019-05-1016:59:54 g 22.59

2MASS 06100073-3338309  136310 92.50307 -33.6419  2019-05-1017:05:36 i 21.93

2MASS 06105136-3352566  5855 92.71404 -33.8824  2019-05-1017:52:39 g 22.49

2MASS 06105136-3352566  5855 92.71404 -33.8824  2019-05-1017:58:20 i 21.95

Po-Chieh Yu (NCU), Han-Jie Tan (NCU), Albert Kong (NTHU), Atharva Sunil
Patil (NCU), Chow-Choong Ngeow (NCU), Wing-Huen Ip (NCU), on behalf of the
Global Relay of Observatories Watching Transients Happen (GROWTH)
collaboration

We observed the possible OT in PGC 094244 (GCN #24470
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 , Lipunov et al.) at
2019-05-11 12:50:12 UT using the Lulin One-meter Telescope (LOT) in Taiwan.
We obtained g-, r-, i-band images with 300s exposure time, and the
transient is not detected in all images. The r-band limiting magnitude is
about 21 by comparing with Pan-STARRS images. This is consistent with the
results of Tucker et al. (GCN #24477
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 ).

We thank the staff in Lulin Observatory for helping the observations.

P. D'Avanzo (INAF-OAB), E. Palazzi (INAF-OAS), G. Greco (Univ. Urbino), S.
Yang (INAF-OAPd), S. Campana (INAF-OAB), G. Stratta (INAF-OAS), A. Rossi
(INAF-OAS), Nicola Masetti (inaf-oas) and E. Brocato on behalf of GRAWITA
report:


We carried out further optical follow-up observations of the LIGO/Virgo GW
trigger S190509g (LVC, GCN Circ. 24442
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 ) with the 60-cm robotic telescope
REM located at the La Silla Observatory (Chile). The observations started
at 2019-05-11 at 00:49:48 UT, simultaneously in the g, r, i, z bands (the
REM NIR camera was not operational).
We observed the following galaxies within the 50% probability of the
updated skymap visible from La Silla:


RA(J2000) Dec(J2000) Dist(Mpc)
----------------------------------------------------
J055219-342051   05:52:19.00   -34:20:51.4   138.68
J055149-314446   05:51:49.92   -31:44:46.0   210.86
J054827-325838   05:48:27.60   -32:58:38.1   160.69
J060115-313225   06:01:15.09   -31:32:25.5   191.43
J055425-350235   05:54:25.29   -35:02:35.1   143.88
J055028-334429   05:50:28.73   -33:44:29.3   165.20
J055740-345601   05:57:40.71   -34:56:01.8   146.97
J055949-353200   05:59:49.81   -35:32:00.5   138.04

No clear counterpart for S190509g is found down to a typical 3sigma
magnitude of r > 19 (AB).

We also carried out optical follow-up of the possible transient we reported
in D'Avanzo et al. (GCN Circ. #24455
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 ) found in REM images at RA(J2000),
Dec(J2000) = 14:29:15.99, +09:41:12.3 with magnitude r = 17.3 (AB) on
2019-05-10 at 08:07:18 UT. Optical imaging follow-up observations of this
possible transient were carried out with the 1.5m Loiano telescope (Italy)
in the R band on 2019-05-10 at 20:44:08 UT (i.e. about 12.6 hours after the
REM detection reported in GCN Circ. #24455
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 ). In the Loiano images the
object is not detected down to a 3-sigma limiting magnitude of R > 20.3
(AB, calibrated against the SDSS). This non-detection is in agreement with
the findings reported by Zhu et al. (GCN Circ. #24479
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 ) and favor a fast
transient (like a stellar flare) interpretation for the nature of this
object, although the hypothesis of an image artifact cannot be completely
excluded.

*S. Yang (INAF-OAPd), E. Cappellaro (INAF-OAPd), F. Getman (INAF-OAC), A.
Grado (INAF-OAC), G. Greco (Univ. Urbino), S. Covino (INAF-OAB), L. Izzo
(IAA), E. Palazzi (INAF-OAS), L. Nicastro (INAF-OAS), M.T. Botticella
(INAF-OAC), P. D'Avanzo (INAF-OAB), M. Branchesi (GSSI), E. Brocato
(INAF-OAAb, INAF-OAR) on behalf of GRAWITA report:We observed part of the
50% probability of the updated skymap of the LIGO/Virgo GW trigger S190509g
(LVC, GCN Circ. 24442
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 ), with the VLT Survey Telescope (VST) at ESO-Paranal
equipped with OMEGACAM (FOV=1 square degree). The observations were taken
in the r-sloan band and started on 2019-05 11 at 00:03:23 UT.The covered
area is of about 15 square degrees divided in of 80 sec of exposure time
each.The pointings are centered on the following coordinates RA, Dec
(J2000):05:57:42.54, -33:00:00.005:57:02.43, -34:00:00.005:52:56.37,
-33:00:00.005:53:45.21, -32:00:00.006:01:51.92, -34:00:00.005:52:12.94,
-34:00:00.005:58:28.21, -32:00:00.006:02:28.71, -33:00:00.006:01:20.96,
-35:00:00.005:56:27.97, -35:00:00.006:03:59.38, -31:00:00.006:11:06.93,
-35:00:00.006:06:13.94, -35:00:00.006:10:49.22, -36:00:00.006:11:30.91,
-34:00:00.0The image analysis is ongoing.*

LIGO/Virgo S190510g: DESGW counterpart candidates over 80% of the GW localization area

Marcelle Soares-Santos for the DESGW collaboration


We report candidate counterparts to the binary neutron star merger S190510g reported by the LIGO/VIRGO Collaboration (GCN Circular No. 24442, updated GCN Circular No. 24448). The region was imaged by DECam on the night of 2019 May 10 (GCN Circular No. 24467) in g,r,z bands.


These candidates were identified by our difference imaging pipeline. All newly obtained images were subtracted from deep pre-existing Dark Energy Survey images. The total coverage difference imaged is 28 fields of 3 square degrees each, i.e., a total of 84 square degrees which overlap ~80% of the total localization probability of S190510g.


After processing the entire area, we select high-confidence detections (machine learning score>0.7, rejecting dipoles) and perform post-processing vetting of the candidates (rejection of variable objects, matching to host galaxies, and visual inspection).


The resulting list of candidates is provided. We encourage followup:

NAME           RA DEC       MAG MAGERR BAND MJD     HOST_Z COMMENT

desgw-190510a  91.526744 -35.541616  21.05 0.03 r 58613.958  0.08 Also reported in GCN No. 24474

desgw-190510b  93.704382 -36.980727  21.13 0.01 r 58613.989  -1.0 Hostless candidate

desgw-190510c  92.851468 -36.517324  20.41 0.01 r 58613.989  0.30 Also reported in GCN No. 24467

desgw-190510d  87.311398 -35.955853  19.85 0.02 r 58613.991  0.31 Also reported in GCN No. 24467

desgw-190510e  89.100926 -30.473987  20.64 0.02 r 58613.986  0.13 Second possible host at z=0.3

desgw-190510f  92.294458 -34.884684  21.30 0.02 r 58613.983  -1.0 Hostless candidate

desgw-190510g  92.468923 -34.08657   21.89 0.01 r 58613.987  -1.0 Hostless candidate

desgw-190510h  87.762354 -27.956502  20.31 0.03 r 58613.988  -1.0 Host found via visual inspection, no redshift

desgw-190510i  91.936973 -30.824747  20.14 0.01 r 58613.996  0.61 Probably not associated with S190510g

desgw-190510j  92.307977 -35.149829  20.75 0.02 r 58613.983  0.17 Redshift suggests possible association with S190510g

desgw-190510k  87.146843 -35.994357  19.75 0.02 z 58613.966  -1.0 Host redshift not available


As an alternative means of selecting high interest candidates, we used KN-Classify, a random forest classifier trained on transient light curves from PLAsTiCC models to determine the probability of a transient being a kilonova. The only such candidate found that survived the vetting process was also found by the normal method and is listed in the table above (desgw-190510c).


Transients matched to a galaxy at a redshift beyond distances plausible for the S190510g event are interpreted as supernova unassociated with S190510g.



DESGW collaboration:

Sahar Allam (Fermilab),  James Annis (Fermilab), Iair Arcavi (Tel Aviv University),  Paulo Barchi (INPE/Brazil), Keith Bechtol (LSST), Federico Berlfein (Brandeis U),  Antonio Bernardo (IAG-USP/Brazil), Dillon Brout (University of Pennsylvania), Robert Butler (Indiana University),  Melissa Butner, (Fermilab), Annalisa Calamida (STScI), Hsin-Yu Chen (Harvard U), Chris Conselice (University of Nottingham),  Carlos Contreras (STScI), Jeff Cooke (Swinburne University), Chris D���Andrea (University of Pennsylvania), Tamara Davis (UQ/Australia),  Reinaldo de Carvalho (NAT - Universidade Cruzeiro do Sul/Universidade Cidade de Sao Paulo), H. Thomas Diehl (Fermilab), Zoheyr Doctor (U Chicago),  Alex Drlica-Wagner (Fermilab), Maria Drout (U Toronto), Maya Fishbach (U Chicago), Francisco Forster (U de Chile/Chile), Ryan Foley (UCSC), Joshua Frieman (Fermilab & University of Chicago),  Chris Frohmaier (University of Portsmouth), Ori Fox (STScI), Alyssa Garcia (Brandeis U), Juan Garcia-Bellido (Universidad Autonoma de Madrid), Mandeep Gill (SLAC/Stanford U), Robert Gruendl (NCSA),  Will Hartley (University College London), Kenneth Herner (Fermilab), Daniel Holz (U Chicago), Jorge Horvath (IAG-USP/Brazil), D. Andrew Howell (Las Cumbres Observatory), Richard Kessler (University of Chicago),  Charles Kilpatrick (UCSC), Nikolay Kuropatkin (Fermilab), Ofer Lahav (University College London), Huan Lin (Fermilab), Andrew Lundgren (Portsmouth), Martin Makler (CBPF/Brazil), Curtis McCully (Las Cumbres Observatory),  Robert Morgan (University of Wisconsin-Madison), Gautham Narayan (STScI), Eric Neilsen (Fermilab), Robert Nichol (University of Portsmouth), Antonella Palmese (Fermilab), Francisco Paz-Chinchon (NCSA & UIUC), Maria Pereira (Brandeis University),  Sandro Rembold (UFSM/Brazil), Armin Rest (STScI & JHU), Livia Rocha (IAG-USP/Brazil), Russell Ryan (STScI), Masao Sako (University of Pennsylvania), Samir Salim (Indiana University), David Sand (U of Arizona), Daniel Scolnic (Duke University), J. Allyn Smith (Austin Peay State University),  Mathew Smith (University of Southampton), Marcelle Soares-Santos (Brandeis U), Lou Strolger (STScI), Riccardo Sturani (UFRN/Brazil), Mark Sullivan (University of Southampton), Masaomi Tanaka (NAOJ/Japan), Nozomu Tominaga (Konan U/Japan), Douglas Tucker (Fermilab), Yousuke Utsumi (Stanford U), Stefano Valenti (UC Davis),  Kathy Vivas (NOAO/CTIO), Alistair Walker (NOAO/CTIO), Sara Webb (Swinburne University), Matt Wiesner (Benedictine University), Brian Yanny (Fermilab), Michitoshi Yoshida (NAOJ/Japan), Alfredo Zenteno (NOAO/CTIO), Luidhy Santana-Silva (Valongo Observatory)


This project used data obtained with the Dark Energy Camera (DECam), which was constructed by the Dark Energy Survey collaboration, and draws on upon data as distributed by the Science Data Archive at NOAO. NOAO is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation.

Z.P. Zhu, D. Xu, B.Y. Yu, J.J. Ren, T.M. Zhang, X. Zhou, H.J. Wang, C.Z. 
Cui, D.W. Fan, Y.F. Xu (NAOC), X. Gao (Urumqi No.1 Senior High School), 
S. Yang (INAF-OAPd), H.B. Zhao, B. Li (PMO), J.Z. Liu, H.B. Niu (XAO), 
J.R. Mao, J.M. Bai (YNAO), report on behalf of the GWFUNC collaboration:

We observed the optical transient (OT), r = 17.3 +/- 0.1 (AB, calibrated 
against
the SDSS), in P. D'Avanzo et al. (GCN 24455
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 ) of the gravitational-wave 
event S190510g (GCN 24442
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 ) using the Xinglong-60cm telescope located at 
Xinglong, Hebei, China.

The OT is ~20" away from the SDSS galaxy, SDSS J142914.95+094059.4, 
which has a photoZ=0.041 +/- 0.0149, corresponding to a luminosity 
distance of 182.2 Mpc, thus being consistent with the LIGO's luminosity 
distance estimate of 227 +/- 92 Mpc (GCN 24448
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 ). At the above redshift, 
SDSS J142914.95+094059.4 has an absolute magnitude of M(r) = 17.92-36.30 
= -18.38, at the border of dwarf/normal galaxies. The OT is ~16.3 kpc 
away from the nucleus of the SDSS galaxy, much larger than usual radii 
of such galaxies. If double neutron stars are considered having been 
kicked out of their host galaxy earlier before, such a scenario might be 
possible.

Under the above assumption, we obtained 15x360 s frames in R band, 
started at 16:12:27 on 2019-05-10, i.e., about 10 hr after the OT 
detected. The OT has decayed and is not detected in our stacked image of 
5400 s, down to a limiting magnitude of r ~ 20.6, calibrated with the 
SDSS field.

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

D. Buckley (South African Astronomical Observatory),


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

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres (The Instituto 
de Astrofisica de Canarias),

R. Podesta, C. Lopez, C.Francile, F. Podesta (Observatorio Astronomico  Felix 
Aguilar OAFA, San Juan National University),

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


O. Gress, N.M. Budnev, O.Ershova (Applied Physics Institute, Irkutsk Stat 
University),

V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev (Blagoveschensk EducationState 
University),


After publication OT desgw-190510a detection (Jim Annis et al., GCN 24474
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 ) 
After the publication OT desgw-190510a detection (Jim Annis et al., GCN 
24474
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 ), the we  checked the candidates of the 
MASTER-SAAO robots and found MASTER  transient in this place.

MASTER OT J060606.43-353229.8 at desgw-190510a position.

MASTER-SAAO auto-detection system ( Lipunov et al., "MASTER Global Robotic 
Net", Advances in Astronomy, 2010, 30L )
  discovered OT source at (RA, Dec) = 06h 06m 06.43s -35d 32m 29.8s on 
~ 2019-05-10 UT.

The OT unfiltered magnitude is ~20 m in our red CCD.

The OT is seen in 2 images. There is no minor planet at this place.

We have reference image on 2019-02-04.86162 UT with  unfiltered mlim= 
20.2 m.

Folow up observations are required.

M. A. Tucker, A. Do, A. V. Payne, M. E. Huber, B. J. Shappee (UH Manoa,
Institute for Astronomy):

Following the discovery of an optical transient in PGC 094244 (GCN 24470
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 ,
Lipunov et al.), we obtained follow up V-band imaging with the SuperNova
Integral Field Spectrograph (SNIFS) on the University of Hawai'i 88-inch
(UH88) telescope. The transient is undetected in 2 images to a limiting
magnitude of V ~ 22, calibrated to PanSTARRS sources using the photometric
transformations of Tonry et al. (2012, ApJ).

Date Obs (UT)             | Expt. (s) | mlim
-------------------------------------------------------------
2019-05-11T07:09:45 |  180        | ~21.5
2019-05-11T07:14:23 |  300        | ~22
-------------------------------------------------------------

Z.P. Zhu, D. Xu, B.Y. Yu, T.M. Zhang, X. Zhou, H.J. Wang, C.Z. Cui, D.W. 
Fan, Y.F. Xu (NAOC), X. Gao (Urumqi No.1 Senior High School), S. Yang 
(INAF-OAPd), H.B. Zhao, B. Li (PMO), J.Z. Liu, H.B. Niu (XAO), J.R. Mao, 
J.M. Bai (YNAO), report on behalf of the GWFUNC collaboration:

We performed the search for the optical counterpart of LIGO/Virgo 
S190510g (LVC, GCN 24442
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 ) using the Half-Meter Telescope (HMT) located 
at Dabancheng, Xinjiang, China. Observations started at 16:00:00 UT on 
2019-05-10 and ended at 22:32:00 UT on 2019-05-10, and the 60x40 
arcmin^2 unfiltered imager scanned relatively high probability regions 
of the LVC localization that are accessible to HMT.

The total area is about 97 deg^2, and listed below are the field centers 
observed.

  RA		  DEC
13:31:59	+00:39:25
13:31:59	+00:40:37
13:31:59	+00:40:37
13:32:00	+00:00:36
13:32:29	-01:19:26
13:32:30	+01:20:38
13:32:29	-01:59:27
13:32:30	+02:00:39
13:32:29	-02:39:28
13:32:29	+02:40:40
13:33:58	-03:19:30
13:33:59	+03:20:42
13:33:58	-03:59:31
13:33:59	+04:00:43
13:33:58	-04:39:32
13:33:59	+04:40:44
13:36:00	+00:39:25
13:36:00	+00:00:36
13:36:00	+00:40:37
13:36:00	+00:00:36
13:36:00	+00:40:37
13:36:29	-01:19:26
13:36:30	+01:20:38
13:36:29	-01:59:27
13:36:30	+02:00:39
13:36:29	-02:39:28
13:36:30	+02:40:40
13:36:28	-05:19:33
13:36:27	-05:59:34
13:36:27	-06:39:36
13:37:59	-03:19:30
13:37:59	-03:59:31
13:37:59	-04:39:32
13:38:00	+03:20:42
13:38:00	+04:00:43
13:38:00	+04:40:44
13:40:00	+00:39:25
13:40:00	+00:00:36
13:40:00	+00:40:37
13:40:00	+00:00:36
13:40:00	+00:40:37
13:40:29	-01:19:26
13:40:30	+01:20:38
13:40:29	-01:59:27
13:40:30	+02:00:39
13:40:29	-02:39:28
13:40:30	+02:40:40
13:40:29	-05:19:33
13:40:29	-05:59:34
13:40:29	-06:39:36
13:41:59	-03:19:30
13:41:59	-03:59:31
13:41:59	-04:39:32
13:42:00	+03:20:42
13:42:00	+04:00:43
13:42:01	+04:40:44
13:43:59	+00:39:25
13:43:59	+00:40:37
13:43:59	+00:40:37
13:44:00	+00:00:36
13:44:29	-01:19:26
13:44:30	+01:20:38
13:44:29	-01:59:27
13:44:30	+02:00:39
13:44:29	-02:39:28
13:44:30	+02:40:40
13:44:30	-05:19:33
13:44:30	-05:59:34
13:44:30	-06:39:36
13:48:00	+00:39:25
13:48:00	+00:00:36
13:48:00	+00:40:37
13:48:00	+00:00:36
13:48:00	+00:40:37
13:48:30	-01:19:26
13:48:30	+01:20:38
13:48:30	-01:59:27
13:48:30	+02:00:39
13:48:30	-02:39:28
13:48:30	+02:40:40
13:52:00	+00:39:25
13:52:00	+00:00:36
13:52:00	+00:40:37
13:52:00	+00:00:36
13:52:00	+00:40:37
13:52:30	-01:19:26
13:52:30	+01:20:38
13:52:30	-01:59:27
13:52:30	+02:00:39
13:52:30	-02:39:28
13:52:30	+02:40:40
14:22:06	+03:20:42
14:22:06	+04:00:43
14:22:06	+04:40:44
14:24:45	+05:20:45
14:24:45	+06:00:46
14:24:45	+06:40:48
14:26:07	+03:20:42
14:26:07	+04:00:43
14:26:07	+04:40:44
14:28:46	+05:20:45
14:28:46	+06:00:46
14:28:46	+06:40:48
14:30:07	+03:20:42
14:30:07	+04:00:43
14:30:08	+04:40:44
14:32:32	+01:20:38
14:32:32	+02:00:39
14:32:32	+02:40:40
14:32:47	+05:20:45
14:32:48	+06:00:46
14:32:48	+06:40:48
14:32:31	+08:40:51
14:34:08	+03:20:42
14:34:08	+04:00:43
14:34:08	+04:40:44
14:36:32	+01:20:38
14:36:32	+02:00:39
14:36:32	+02:40:40
14:36:33	+07:20:49
14:36:33	+08:00:50
14:36:34	+08:40:51
14:38:09	+03:20:42
14:38:09	+04:00:43
14:38:09	+04:40:44
14:40:32	+01:20:38
14:40:32	+02:00:39
14:40:32	+02:40:40
14:40:36	+07:20:49
14:40:35	+08:00:50
14:40:35	+08:40:51
14:42:09	+03:20:42
14:42:09	+04:00:43
14:42:09	+04:40:44
14:44:52	+06:40:48
14:44:38	+07:20:49
14:44:38	+08:00:50
14:44:38	+08:40:51
14:46:10	+03:20:42
14:46:10	+04:00:43
14:46:10	+04:40:44
14:48:53	+05:20:45
14:48:53	+06:00:46
14:48:53	+06:40:48
14:48:40	+07:20:49
14:48:40	+08:00:50
14:48:41	+08:40:51
14:49:33	+10:40:55
14:50:10	+03:20:42
14:50:10	+04:00:43
14:50:10	+04:40:44
14:52:54	+05:20:45
14:52:54	+06:00:46
14:52:54	+06:40:48
14:52:43	+07:20:49
14:52:43	+08:00:50
14:52:42	+08:40:51
14:53:36	+09:20:52
14:53:37	+10:00:54
14:53:37	+10:40:55
14:54:11	+03:20:42
14:54:11	+04:00:43
14:54:11	+04:40:44
14:56:55	+05:20:45
14:56:56	+06:00:46
14:56:56	+06:40:48
14:56:45	+07:20:49
14:56:45	+08:00:50
14:56:45	+08:40:51
15:00:47	+07:20:49
15:00:47	+08:00:50
15:00:48	+08:40:51

Data analysis is ongoing. Optical transients from the above fields, if 
interesting, will be reported later.

Z.P. Zhu, D. Xu, B.Y. Yu, T.M. Zhang, X. Zhou, X.M. Teng, P.F. Liu, X. 
N. Guan, H.J. Wang, C.Z. Cui, D.W. Fan, Y.F. Xu (NAOC), S. Yang 
(INAF-OAPd), H.B. Zhao, B. Li (PMO), J.Z. Liu, H.B. Niu (XAO), J.R. Mao, 
J.M. Bai (YNAO), X. Gao (Urumqi No.1 Senior High School), report on 
behalf of the GWFUNC collaboration:

We performed the search for the optical counterpart of LIGO/Virgo 
S190510g (LVC, GCN 24442
Loading...
 
 ) using the 0.9-m Schmidt telescope located at 
Xinglong, Hebei, China. Observations started at 12:50:37 UT on 
2019-05-10 and ended at 18:39:16 UT on 2019-05-10, and the 1.5 x 1.5 
deg^2 imager scanned relatively high probability regions of the LVC 
localization that are accessible to the Xinglong/Schmidt telescope. The 
unfiltered images were taken with 60 sec exposure time and typical 
limiting depth is around 18.5 mag.

Below listed are the field centers observed.

RA(J2000)      DEC(J2000)
13:27:04.200 +02:54:36.00
13:33:04.800 +02:53:57.00
13:38:46.100 +02:54:04.00
13:27:42.000 +04:23:47.00
13:33:29.900 +04:24:04.00
13:39:29.300 +04:24:08.00
13:27:58.390 +05:53:48.00
13:32:47.200 +05:54:02.00
13:38:41.700 +05:54:05.00
13:25:40.400 -01:36:36.00
13:30:58.590 -01:36:02.00
13:36:36.600 -01:35:57.00
13:25:00.000 -00:06:21.00
13:30:59.990 -00:06:01.00
13:37:00.600 -00:05:57.00
13:24:58.500 +01:23:38.00
13:30:56.700 +01:23:59.00
13:36:58.300 +01:24:03.00
13:42:59.190 -01:35:59.00
13:48:57.790 -01:35:49.00
13:54:59.590 -01:35:44.00
13:42:59.700 -00:05:46.00
13:49:00.000 -00:05:53.00
13:54:59.690 -00:05:40.00
13:42:58.290 +01:23:52.00
13:48:32.500 +01:24:12.00
13:54:48.900 +01:24:15.00
13:27:37.600 -06:06:12.00
13:33:29.800 -06:06:00.00
13:39:30.800 -06:05:56.00
13:27:31.400 -04:36:25.00
13:33:32.200 -04:35:56.00
13:39:30.900 -04:35:55.00
13:27:29.000 -03:05:51.00
13:33:30.100 -03:06:02.00
13:39:31.290 -03:05:56.00
14:21:26.200 +02:54:44.00
14:27:12.790 +02:54:45.00
14:33:19.100 +02:54:50.00
14:21:38.600 +04:24:25.00
14:27:12.590 +04:24:46.00
14:33:13.090 +04:24:50.00
14:21:57.890 +05:54:37.00
14:27:13.200 +05:54:46.00
14:33:41.100 +05:54:51.00
14:39:44.300 +02:54:57.00
14:45:25.600 +02:55:02.00
14:51:22.800 +02:55:09.00
14:39:40.400 +04:25:05.00
14:45:28.800 +04:25:00.00
14:50:45.490 +04:25:09.00
14:39:58.600 +05:54:56.00
14:45:15.190 +05:55:04.00
14:51:43.090 +05:55:16.00
13:45:31.900 -06:05:48.00
13:51:19.200 -06:05:48.00
13:57:02.000 -06:05:43.00
13:45:37.800 -04:35:48.00
13:51:35.000 -04:35:47.00
13:57:32.200 -04:35:41.00
13:45:39.100 -03:05:44.00
13:51:31.700 -03:05:50.00
13:57:31.900 -03:05:42.00
14:47:43.790 +07:24:57.00
14:53:54.800 +07:25:13.00
14:59:56.500 +07:25:18.00
14:47:52.300 +08:54:32.00
14:54:00.100 +08:55:17.00
15:00:00.990 +08:55:18.00
14:48:00.100 +10:24:57.00
14:54:03.790 +10:25:12.00
15:00:03.800 +10:25:26.00
14:29:40.400 +07:24:50.00
14:29:50.890 +07:24:50.00
14:29:50.890 +07:24:50.00
14:29:38.400 +08:54:58.00
14:35:43.000 +08:54:50.00
14:41:45.600 +08:54:59.00
14:30:07.600 +10:24:40.00
14:35:33.300 +10:24:58.00
14:41:31.500 +10:24:59.00
14:37:00.800 -01:35:07.00
14:42:51.890 -01:35:02.00
14:48:30.600 -01:34:54.00
14:37:11.290 -00:05:13.00
14:42:32.200 -00:05:00.00
14:48:27.600 -00:04:53.00
14:37:04.800 +01:24:42.00
14:42:54.700 +01:25:00.00
14:48:41.390 +01:25:08.00
14:18:44.800 -01:35:26.00
14:24:52.200 -01:35:19.00
14:30:47.900 -01:35:12.00
14:19:08.790 -00:05:36.00
14:25:00.800 -00:05:12.00
14:30:33.800 -00:05:12.00
14:19:07.000 +01:24:23.00
14:25:00.100 +01:24:47.00
14:30:30.890 +01:24:48.00
13:45:48.100 +02:54:01.00
13:51:23.200 +02:54:13.00
13:57:09.200 +02:54:17.00
13:45:38.890 +04:23:56.00
13:50:57.600 +04:24:13.00
13:57:32.500 +04:24:22.00
13:45:37.500 +05:54:01.00
13:51:14.300 +05:54:14.00
13:57:13.490 +05:54:18.00
14:57:54.700 +02:55:13.00
15:03:41.600 +02:55:24.00
15:09:44.690 +02:55:31.00
14:57:52.300 +04:25:23.00
15:03:43.790 +04:25:25.00
15:09:18.300 +04:25:31.00
14:57:54.490 +05:54:43.00
15:03:45.290 +05:55:25.00
15:09:43.290 +05:55:31.00
13:34:58.900 +07:24:03.00
13:40:47.400 +07:24:02.00
13:47:06.400 +07:24:09.00
13:35:04.590 +08:53:46.00
13:40:09.500 +08:54:05.00
13:47:08.800 +08:54:10.00
13:35:03.600 +10:24:05.00
13:40:29.690 +10:24:05.00
13:46:49.590 +10:24:10.00
14:55:11.900 -01:34:45.00
15:00:58.800 -01:34:41.00
15:07:16.700 -01:34:33.00
14:55:11.300 -00:04:41.00
15:00:26.000 -00:04:42.00
15:06:07.400 -00:04:32.00
14:55:02.700 +01:25:20.00
15:00:58.200 +01:25:22.00
15:06:59.000 +01:25:27.00
14:11:25.300 +07:24:21.00
14:16:38.690 +07:24:36.00
14:22:40.490 +07:24:41.00
14:11:24.900 +08:54:34.00
14:17:55.400 +08:54:36.00
14:23:07.990 +08:54:41.00
14:11:40.700 +10:24:18.00
14:16:32.190 +10:24:36.00
14:23:03.390 +10:24:41.00
14:03:48.200 +02:54:12.00
14:08:13.700 +02:54:27.00
14:15:21.300 +02:54:32.00
14:03:44.100 +04:24:27.00
14:09:21.890 +04:24:32.00
14:15:26.000 +04:24:32.00
14:03:31.790 +05:54:16.00
14:09:37.790 +05:54:29.00
14:15:35.100 +05:54:32.00
14:43:29.400 +11:55:14.00
14:49:28.000 +11:55:04.00
14:55:21.690 +11:55:14.00
14:43:17.290 +13:25:06.00
14:49:14.900 +13:25:07.00
14:55:41.100 +13:25:15.00
14:43:15.300 +14:54:59.00
14:49:29.000 +14:55:07.00
14:55:14.100 +14:55:15.00

Data analysis is ongoing. Optical transients from the above fields, if 
interesting, will be reported later.

LIGO/Virgo S190510g: DESGW counterpart candidate (desgw-190510a)

Jim Annis for the DESGW collaboration

We report a candidate counterpart to the binary neutron star merger S190510g reported by LIGO/VIRGO Collaboration (GCN Circular No. 24442, updated GCN Circular No. 24448). The region was imaged by DECam on the night of 2019 May 10 (GCN Circular No. 24467).  The candidate was identified by visual inspection of 566 galaxies nearby galaxies within the 50% localization probability region of the merger. The visual inspection compared the new images with deep pre-existing imaging data obtained by the Dark Energy Survey. The transient appears in our g,r,z images.

Transient:  desgw-190510a
Coordinates:  91.52679,  -35.54160  ( 6:06:06.429,-35:32:29.77 )
g mag: 22.5 +/- 0.2
r mag: 20.9 +/- 0.05
z mag: 20.7 +/- 0.1
These magnitudes are as observed, uncorrected for reddening.

Host galaxy:  2MASS06060625-3532351
Coordinates:  91.52605,   -35.54311  ( 6:06:06.252,-35:32:35.20 )
Radius of galaxy:  6.6���
J mag: 14.64
Redshift: 0.089 (2MPZ photo-z)

DESGW collaboration:
Sahar Allam (Fermilab),  James Annis (Fermilab),  Iair Arcavi (Tel Aviv University),  Paulo Barchi (INPE/Brazil),  Keith Bechtol (LSST),  Federico Berlfein (Brandeis U),  Antonio Bernardo (IAG-USP/Brazil),  Dillon Brout (University of Pennsylvania),  Robert Butler (Indiana University),  Melissa Butner,  (Fermilab),  Annalisa Calamida (STScI), Hsin-Yu Chen (Harvard U),  Chris Conselice (University of Nottingham),  Carlos Contreras (STScI),  Jeff Cooke (Swinburne University),  Chris D���Andrea (University of Pennsylvania),  Tamara Davis (UQ/Australia),  Reinaldo de Carvalho (NAT - Universidade Cruzeiro do Sul/Universidade Cidade de Sao Paulo),  H. Thomas Diehl (Fermilab),  Zoheyr Doctor (U Chicago),  Alex Drlica-Wagner (Fermilab),  Maria Drout (U Toronto),  Maya Fishbach (U Chicago),  Francisco Forster (U de Chile/Chile),  Ryan Foley (UCSC),  Joshua Frieman (Fermilab & University of Chicago),  Chris Frohmaier (University of Portsmouth),  Ori Fox (STScI), Alyssa Garcia (Brandeis U),  Juan Garcia-Bellido (Universidad Autonoma de Madrid),  Mandeep Gill (SLAC/Stanford U),  Robert Gruendl (NCSA),  Will Hartley (University College London),  Kenneth Herner (Fermilab),  Daniel Holz (U Chicago),  Jorge Horvath (IAG-USP/Brazil),  D. Andrew Howell (Las Cumbres Observatory),  Richard Kessler (University of Chicago),  Charles Kilpatrick (UCSC),  Nikolay Kuropatkin (Fermilab),  Ofer Lahav (University College London),  Huan Lin (Fermilab),  Andrew Lundgren (Portsmouth),  Martin Makler (CBPF/Brazil),  Curtis McCully (Las Cumbres Observatory),  Robert Morgan (University of Wisconsin-Madison),  Gautham Narayan (STScI),  Eric Neilsen (Fermilab),  Robert Nichol (University of Portsmouth), Antonella Palmese (Fermilab),  Francisco Paz-Chinchon (NCSA & UIUC),  Maria Pereira (Brandeis University),  Sandro Rembold (UFSM/Brazil),  Armin Rest (STScI & JHU),  Livia Rocha (IAG-USP/Brazil),  Russell Ryan (STScI), Masao Sako (University of Pennsylvania),  Samir Salim (Indiana University),  David Sand (U of Arizona),  Daniel Scolnic (Duke University),  J. Allyn Smith (Austin Peay State University),  Mathew Smith (University of Southampton), Marcelle Soares-Santos (Brandeis U), Lou Strolger (STScI), Riccardo Sturani (UFRN/Brazil),  Mark Sullivan (University of Southampton),  Masaomi Tanaka (NAOJ/Japan),  Nozomu Tominaga (Konan U/Japan),  Douglas Tucker (Fermilab),  Yousuke Utsumi (Stanford U),  Stefano Valenti (UC Davis),  Kathy Vivas (NOAO/CTIO),  Alistair Walker (NOAO/CTIO),  Sara Webb (Swinburne University), Matt Wiesner (Benedictine University),  Brian Yanny (Fermilab),  Michitoshi Yoshida (NAOJ/Japan),  Alfredo Zenteno (NOAO/CTIO), Luidhy Santana-Silva (Valongo Observatory)

This project used data obtained with the Dark Energy Camera (DECam), which was constructed by the Dark Energy Survey collaboration, and draws on upon data as distributed by the Science Data Archive at NOAO. NOAO is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation.

J. Alvarez-Muniz, F. Pedreira, E. Zas (Univ. Santiago de Compostela, Spain),
K. H. Kampert & M. Schimp (Bergische Universitat, Wuppertal, Germany)
on behalf of the Pierre Auger Collaboration.

In response to:
LIGO/Virgo GW trigger S190510g
T0=2019-05-10 02:59:39 UTC

We searched for Ultra-High-Energy (UHE) neutrinos with energies
above ~ 1e17 eV in data collected with the Surface Detector (SD)
of the Pierre Auger Observatory in a [-500,500] second interval
about the LIGO-Virgo trigger S190510g as well as 1 day after it.

The field of view (fov) where the SD of Auger is sensitive to UHE
neutrinos (corresponding to inclined directions with respect to the
vertical relative to the ground) was PARTIALLY COINCIDENT (18.1%) with
the LIGO 90% localization region at the time T0 of the merger alert,
achieving MAXIMUM OVERLAP (78.8%) at approximately T0+5.9 hours.

NO events survived the cuts applied to reject the background due to UHE
Cosmic Rays i.e.
NO NEUTRINO CANDIDATES WERE DETECTED.

-------
The Pierre Auger Observatory is an UHE Cosmic Ray detector
located in the Mendoza Province in Argentina. It consists of
an array of Water Cherenkov detectors spread over a total surface
of 3000 km^2 arranged in a triangular grid of 1.5 km side as well
as Fluorescence telescopes and other systems
(see 10.1016/j.nima.2015.06.058 for more information).
For neutrino searches from GW events with Auger, please refer to:
https://journals.aps.org/prd/pdf/10.1103/PhysRevD.94.122007

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

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

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres (The Instituto 
de Astrofisica de Canarias),

R. Podesta, C. Lopez, C.Francile, F. Podesta (Observatorio Astronomico  Felix 
Aguilar OAFA, San Juan National University),

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

D. Buckley (South African Astronomical Observatory),

O. Gress, N.M. Budnev, O.Ershova (Applied Physics Institute, Irkutsk Stat 
University),

V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev (Blagoveschensk EducationState 
University),


OT MASTER140133.93-110805.8 in PGC094244 galaxy.


MASTER-Kislovodsk auto-detection system discovered OT source at (RA, Dec) 
= 14h 01m 33.93s -11d 08m 05.8s on 2019-05-10.82038 UT.
The OT unfiltered magnitude is ~19.0m (limit 19.2m).

The OT is seen in 2 unfiltered images. There is no minor planet at this 
place.

We have reference image without OT on 2014-05-26.82247 UT with unfiltered 
magnitude limit 19.8m.

There is PGC094244 galaxy near OT. OT offset is 36W 
22.6S . The galaxy distance is ~300 Mpc .

Follow up observations are required.


The message may be cited.

C. D. Kilpatrick, M. R. Siebert, J. S. Brown, D. A. Coulter, G. Dimitriadis, R. J. Foley, C. Rojas-Bravo,  K. Siellez, T. Hung, D. O. Jones, A. Murguia-Berthier, J. X. Prochaska, E. Ramirez-Ruiz (UCSC), J. A. Smith (Austin Peay State University), M. Wiesner (Benedictine University), F. Berlfein, A. Garcia, M. Pereira, M. Soares-Santos (Brandeis University), I. Souza (CBPF), M. Makler, I. Souza (CBPF/Brazil), B. Madore, A. L. Piro (Carnegie), H.-Y. Chen (Harvard), R. Kirshner (CfA), B. Metzger (Columbia University), D. Scolnic (Duke University), S. Allam, J. Annis, M. Butner, H. T. Diehl, A. Drlica-Wagner, J. Frieman, K. Herner, N. Kuropatkin, H. Lin, E. Neilsen, A. Palmese, D. Tucker, B. Yanny (Fermilab), J. Horvath, L. Rocha (IAG-USP/Brazil), A. Bernardo (IAS-USP/Brazil), P. Barchi, R. de Carvalho (INPE/Brazil), R. Butler, S. Salim (Indiana University), A. Riess (JHU), N. Tominaga (Konan U/Japan), J. Vinko (Konkoly Observatory), K. Bechtol (LSST), J. Burke, D. Hiramatsu, C. McCully (Las Cumbres Observatory), D. Haggard (McGill University), Y. Pan, M. Tanaka, M. Yoshida, M. Yoshida (NAOJ), R. Gruendl, F. Paz-Chinchon (NCSA), K. Vivas, A. Walker, A. Zenteno (NOAO), F. Bauer, A. Clocchiatti (Pontificia Universidad Catolica de Chile), K. Spekkens (Royal Military College of Canada), S. Jha (Rutgers University), A. Calamida, C. Contreras, G. Narayan, A. Rest (STScI), M. Gill, Y. Utsumi (Stanford), J. Cooke (Swinburne University of Technology), I. Arcavi (Tel Aviv University), K. Krisciunas, N. Suntzeff, L. Wang (Texas A&M), A. Corsi (Texas Tech University), A. Horesh (The Hebrew University), X. Wang (Tsinghua University), J. S. Bloom, T. Brink, A. V. Filippenko, D. Kasen, E. Quataert, W. Zheng (UC Berkeley), A. Bostroem, S. Valenti (UC Davis), A. Howell (UC Santa Barbara), R. Sturani (UFRN/Brazil), S. Rembold (UFSM/Brazil), T. Davis (UQ/Australia), O. Rodri (Universidad Andres Bello), F. Forster-Buron (Universidad de Chile), W. Hartley, O. Lahav (University College London), J. Andrews, M. Lundquist, D. Sand (University of Arizona), Z. Doctor, M. Fishbach, W. Freedman, D. Holz, R. Kessler (University of Chicago), P. M. Garnavich (University of Notre Dame), C. Conselice (University of Nottingham), D. Brout, C. D'Andrea, M. Sako (University of Pennsylvania), C. Frohmaier, A. Lundgren, R. Nichol, L. Nuttall (University of Portsmouth), M. Smith, M. Sullivan (University of Southampton), J. C. Wheeler (University of Texas/Austin), M. Drout (University of Toronto), R. Morgan (University of Wisconsin-Madison), K. Lukosiute (Wellesley College)

report on behalf of the 1M2H and DESGW collaborations:

In the process of searching the localization region of LIGO/Virgo S190510g (LIGO/VIRGO Collaboration, GCN #24448
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 ), we obtained 3-minute r-band exposures of the following regions with the Goodman High Throughput Spectrograph on the SOAR 4-m telescope.  The field of view is a 7.2-arcmin diameter circle.  The approximate center of each image is noted in the table below.  We also note the approximate 3-sigma limiting magnitude of each image.

Comparing our images to DES DR1 r-band images of the same fields, we did not detect any transient sources.

 RA (J2000) | DEC (J2000)  | MJD             | Limiting Magnitude
06:06:00.86 | -32:47:28.55 | 58613.9634598   |  21.3
05:51:48.47 | -31:28:21.43 | 58613.9697709   |  21.6
05:55:10.63 | -32:04:19.33 | 58613.9807059   |  21.7
05:59:44.38 | -32:54:47.42 | 58613.9842936   |  21.7
06:07:49.70 | -33:30:45.58 | 58613.9875954   |  21.7
05:51:48.38 | -31:21:10.17 | 58613.9908477   |  21.6
05:59:08.22 | -32:04:26.44 | 58613.9943430   |  21.7
05:50:37.29 | -32:18:50.38 | 58613.9979812   |  21.6
05:52:16.38 | -33:38:02.52 | 58614.0014418   |  21.6
05:58:02.52 | -34:06:49.28 | 58614.0052499   |  21.6
05:50:31.75 | -33:45:17.44 | 58614.0084120   |  21.5
05:53:24.15 | -34:21:14.39 | 58614.0116271   |  21.6
05:47:57.74 | -30:23:38.45 | 58614.0149357   |  21.5
05:51:38.62 | -34:28:28.46 | 58614.0181796   |  21.5
05:52:18.83 | -32:47:42.32 | 58614.0222639   |  21.5
05:55:44.58 | -32:04:30.50 | 58614.0257728   |  21.4
05:52:47.96 | -34:42:54.55 | 58614.0289522   |  21.5
05:59:41.23 | -31:42:57.35 | 58614.0323124   |  21.4
06:00:24.86 | -35:11:38.23 | 58614.0357864   |  21.4
06:09:01.75 | -33:52:31.40 | 58614.0391655   |  21.4
06:11:07.09 | -32:33:16.39 | 58614.0432460   |  21.4

We did not cover the location of any candidate identified in Andreoni et al. (GCN #24467
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 ).

We would like to thank Jay Elias for facilitating these Target of Opportunity observations.

Please direct all communication related to this circular to Charlie Kilpatrick (cdkilpat@ucsc.edu).

Igor Andreoni (Caltech), Daniel A. Goldstein (Caltech), Shreya Anand (Caltech), Mansi M. Kasliwal (Caltech), Michael S. Medford (UC Berkeley), Christoffer Fremling (Caltech), Michael Coughlin (Caltech), Tomas Ahumada (UMD), Pradip Gatkine (UMD), Peter E. Nugent (LBNL), Joshua S. Bloom (UC Berkeley), Keming Zhang (UC Berkeley), Jeff Cooke (Swinburne/OzGrav), Jorge Mart��nez Palomera (UC Berkeley), Ashish Mahabal (Caltech), Leo P. Singer (NASA GSFC), Sara Webb (Swinburne/OzGrav), Ariel Goobar (OKC), Harsh Kumar (IITB), Varun Bhalerao (IITB), Samaya Nissanke (UvA) on behalf of the Global Relay of Observatories Watching Transients Happen (GROWTH) collaborations:

Starting on 2019 May 10 22:56 UTC, we observed the high-probability region of the LALInference skymap of gravitational wave source S190510g (LIGO/VIRGO Collaboration, GCN #24448
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 ) using the Dark Energy Camera (DECam) on the Victor M. Blanco 4m Telescope at Cerro Tololo Inter-American Observatory, Chile, continuing the observations described in Andreoni et al. (2019; GCN #24443
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 ). We covered 78.9 deg^2 of the localization region and 66% of the probability in the r and z filters to average limiting magnitudes of 23.1 (r-band) and 21.9 (z-band), obtaining 1 epoch in z and 1 in r. We obtained g-band for roughly 85% of the fields to a limiting magnitude of 22.9. We performed difference imaging in real-time using an automated  pipeline we developed for gravitational wave counterpart searches, taking reference images from the Dark Energy Survey and the Dark Energy Camera Legacy Survey, covering 100% of the observed area.

Below is a preliminary list of interesting candidates based on our real-time pipeline. Each candidate has at least two detections in two different filters and a prominent host galaxy.
----------------------------------------------------------------------------------
Name     |    RA    |    Dec   |filter| mag | err |filter| mag | err
----------------------------------------------------------------------------------
DG19lcnl | 87.14690 | -35.99441 | r | 19.45 | 0.02 | g | 20.27 | 0.04
DG19ukvo | 89.21146 | -33.44248 | r | 21.57 | 0.07 | g | 21.54 | 0.12 
DG19nanl | 87.31139 | -35.95584 | r | 20.01 | 0.03 | g | 20.33 | 0.05
DG19zaxn | 92.30795 | -35.14981 | r | 20.81 | 0.06 | g | 20.88 | 0.06
DG19etsk | 89.10091 | -30.47397 | r | 20.83 | 0.06 | g | 20.61 | 0.06
DG19yhhm | 91.93699 | -30.82476 | r | 20.13 | 0.03 | g | 20.06 | 0.04
DG19llhk | 90.86311 | -32.38554 | r | 21.14 | 0.07 | z | 21.12 | 0.12 
DG19fqqk | 92.85149 | -36.51731 | r | 20.43 | 0.03 | z | 20.59 | 0.09
DG19yhhm | 91.93699 | -30.82476 | r | 20.13 | 0.03 | z | 20.35 | 0.10 
DG19bexl | 90.45378 | -28.66039 | r | 21.10 | 0.08 | z | 21.03 | 0.16
DG19ootl | 87.03556 | -36.07611 | r | 21.74 | 0.10 | z | 21.51 | 0.14
DG19nouo | 92.00130 | -31.66915 | r | 21.19 | 0.08 | g | 21.43 | 0.11
DG19oahn | 86.33527 | -26.84768 | r | 19.30 | 0.02 | z | 18.97 | 0.03 

We note that the host of DG19llhk is at z=0.07, consistent with the current LVC distance estimate. At this distance, the absolute magnitude would be -16.4, consistent with GW170817 at +1 day. We also note that the colors of DG19lcnl appear consistent with GW170817, but we do not have a host redshift. However, we caution that we do not have any constraints on the light curve history and hence, the phase of this event. We strongly encourage spectroscopic follow-up to classify these transients. 

We thank the CTIO staff, Steve Heathcote, Kathy Vivas, Tim Abbott, for facilitating these Target of Opportunity observations.

GROWTH is a worldwide collaboration comprising Caltech, USA; IPAC, USA, WIS, Israel; OKC, Sweden; JSI/UMd, USA; U Washington, USA; DESY, Germany; MOST, Taiwan; UW Milwaukee, USA; LANL USA; Tokyo Tech, Japan; IIT-B, India; IIA, India; LJMU, UK; TTU USA and USyd, Australia. GROWTH acknowledges generous support of the NSF under PIRE Grant No 1545949. An optimized schedule was generated using the ToO marshal system (Coughlin et al. 2019). Alert filtering and follow-up co-ordination is being undertaken by the GROWTH marshal system (Kasliwal et al. 2019).

This research draws upon DECam data as distributed by the Science Data Archive at NOAO. NOAO is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. This project used data obtained with the Dark Energy Camera (DECam), which was constructed by the Dark Energy Survey (DES) collaboration.

This message may be cited.

Myungshin Im (SNU), Joonho Kim (SNU), Chung-Uk Lee (KASI), Seung-Lee Kim
(KASI), Gregory S. H. Paek (SNU), Gu Lim (SNU), Changsu Choi (SNU),
Sungyong Hwang (SNU), Bomi Park (SNU), Sophia Kim (SNU), Hyung Mok Lee
(KASI), on behalf of a larger collaboration


With KMTNet, we observed the whole 60\% credible region of the updated
localization map of the BNS merger candidate, S190510g (LIGO/Virgo GCN
24448
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 ). The observation took place at the KMTNet South Africa (SAAO) and
Chile (CTIO) stations, starting at 2019-5-10 16:38 UT. The images were
taken in R-band with 240 sec exposure time to the depth of R ~ 21.7
(5-sigma detection). The search for transients is ongoing, although no
obvious transient has been identified so far.


We thank the KMTNet staffs for performing the observation.

Bin Li, Hai-bin Zhao (PMO),Dong Xu, Zi-pei Zhu, Bang-Yao Yu,Tian-meng Zhang, Xu Zhou,Chen-zhou Cui, Hui-juan Wang(NAOC), Xue-feng Wu, Zhi-ping Jin, Tian-rui Sun, Hao Lu, Ge-tu Zhaori, Ren-quan Hong, Long-fei Hu (PMO), Xiao-feng Wang, Wen-xiong Li (THU),Li-fan Wang (PMO/TAMU), Tian-meng Zhang, Xu Zhou (NAOC), Jin-zhong Liu (XAO), Ji-rong Mao, Jin-ming Bai (YNAO),  report on behalf of the CNEOST collaboration.

 We conducted optical imaging observations  in the 50% localization of the BNS merger candidate, S190510g, detected by LIGO/Virgo (GCN #24442
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 ; GCN #24448
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 ) with Chinese Near Earth Object Survey Telescope (CNEOST) at Xuyi astronomical station in Jiangsu Province, China (32.75N, 118.47E). The information of observations and preliminary results are listed below.

The new resulte will available at http://www.cneost.org/opem/list.php?gdate=2019-05-10

Alert: LIGO/Virgo S190510g (GCN #24442
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 ; GCN #24448
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 )
StartTime (UT):               2019-05-10T12:50:28.882       
EndTime (UT):                 2019-05-10T16:08:20.544       
Skycover (Square Degree):     468.0   
Telescope FoV (Square Degree):9.0     
#id CentRA(D) CentDEC(D) LimiteMag3_sig 5_sig 10_sig Filter 
  1 194.681900  -6.772099   20.146   19.182   18.347   VR
  2 193.277298   1.611395   20.388   19.429   18.607   VR
  3 201.675400   1.593076   20.333   19.376   18.588   VR
  4 201.708038  -1.210821   20.342   19.391   18.584   VR
  5 196.550156  -3.985157   20.324   19.372   18.544   VR
  6 204.972916  -4.021634   20.392   19.430   18.639   VR
  7 200.313248  -6.826698   20.042   19.117   18.268   VR
  8 201.741806  -9.605056   20.066   19.137   18.270   VR
  9 200.856903 -12.393054   20.072   19.115   18.220   VR
 10 196.088699  -9.623263   20.140   19.181   18.356   VR
 11 193.260544  -1.180493   20.322   19.363   18.535   VR
 12 198.905228   1.592129   20.188   19.226   18.423   VR
 13 204.490967  -1.201643   20.353   19.383   18.603   VR
 14 196.080017  -1.200560   20.328   19.367   18.539   VR
 15 202.159622  -4.002045   20.335   19.389   18.566   VR
 16 203.151154  -6.804635   20.197   19.245   18.344   VR
 17 198.895706  -9.611844   19.975   19.040   18.193   VR
 18 203.697418 -12.420897   20.083   19.142   18.267   VR
 19 195.085129 -12.402555   20.104   19.149   18.278   VR
 20 193.729477  -3.975807   20.104   19.159   18.360   VR
 21 196.057327   1.575039   20.284   19.326   18.509   VR
 22 204.475555   1.618571   20.388   19.451   18.648   VR
 23 198.890839  -1.214557   20.269   19.288   18.486   VR
 24 199.370056  -3.989921   20.349   19.399   18.578   VR
 25 205.977844  -6.794784   20.267   19.332   18.478   VR
 26 197.471542  -6.809984   20.133   19.183   18.371   VR
 27 204.595169  -9.631298   20.081   19.156   18.277   VR
 28 197.989578 -12.395603   20.063   19.098   18.233   VR
 29 207.799149  -4.024509   20.537   19.600   18.804   VR
 30 207.752518   4.390663   20.787   19.850   19.091   VR
 31 216.195114   4.405424   20.795   19.866   19.054   VR
 32 210.057693   1.565380   20.756   19.814   19.042   VR
 33 215.674347  -1.192254   20.882   19.907   19.076   VR
 34 210.591507  -4.026485   20.662   19.709   18.878   VR
 35 217.247604  -6.805941   20.539   19.622   18.803   VR
 36 210.298050  -9.601982   20.422   19.480   18.642   VR
 37 207.799149  -4.024509   20.537   19.600   18.804   VR
 38 207.752518   4.390663   20.787   19.850   19.091   VR
 39 216.195114   4.405424   20.795   19.866   19.054   VR
 40 210.057693   1.565380   20.756   19.814   19.042   VR
 41 215.674347  -1.192254   20.882   19.907   19.076   VR
 42 210.591507  -4.026485   20.662   19.709   18.878   VR
 43 217.247604  -6.805941   20.539   19.622   18.803   VR
 44 210.298050  -9.601982   20.422   19.480   18.642   VR
 45 207.799149  -4.024509   20.537   19.600   18.804   VR
 46 207.752518   4.390663   20.787   19.850   19.091   VR
 47 216.195114   4.405424   20.795   19.866   19.054   VR
 48 210.057693   1.565380   20.756   19.814   19.042   VR
 49 215.674347  -1.192254   20.882   19.907   19.076   VR
 50 210.591507  -4.026485   20.662   19.709   18.878   VR
 51 217.247604  -6.805941   20.539   19.622   18.803   VR
 52 210.298050  -9.601982   20.422   19.480   18.642   VR

Detailed data analysis is still in progress and any interesting transients will be reported later.

Kawabata, K. S., Sasada, M., Nakaoka, T., Akitaya, H., Imazato, F.,
Nishinaka, Y. (Hiroshima U.), Yanagisawa, K., Yoshida, M. (NAOJ),
Morokuma, T. (U. of Tokyo), Tominaga N. (Konan U.), Utsumi, Y.
(Stanford/SLAC), Yatsu, Y., Murata, K. L. (Tokyo Tech.), Kamei, Y.
(Nagoya U.), Tristram, P. (Mt. John U. Observatory), Suematsu, H.,
Yamawaki, T. (Osaka U.), Matsubayashi, K. (Kyoto U.),  Saito, T.,
Onozato, H. (Nishi-Harima Astronomical Observatory),
Itoh, R. (Bisei Astronomical Observatory), Sekiguchi, Y. (Toho U.),
Oasa, Y., Takarada, T., Kanai, K., Takeuchi, H., Shigeyoshi, T.
(Saitama U.) on behalf of J-GEM collaboration

We report our optical and near-infrared imaging observations for
the gravitational wave event S190510g. We started our observations
about 7.5 hours after the alert.

We performed galaxy-targeted observations for 28 galaxies (see the
table below) selected from the GLADE catalog (Dalya et al. 2016)
in the probability skymap of S190510g using the following
telescopes and instruments.

 - 50 cm MITSuME telescope at Akeno Observatory and a 3 color imager (g, Rc, Ic)
 - 50 cm MITSuME telescope at Okayama Astrophysical Observatory and a 3 color imager (g, Rc, Ic)
 - 55 cm SaCRA telescope at Saitama University and MuSaSHI (r, i, z)
 - 61 cm Boller & Chivens telescope at Mt. John Observatory in New Zealand (B&C) and a three color imager Tripole5 (g, r, i)
 - 91 cm Okayama Astrophysical Observatory NIR Wide$B!>(BField Camera, OAOWFC (J) (Yanagisawa, K., et al. 2016, Proc. SPIE, 9908, 99085D)
 - 150 cm Kanata telescope at Higashi-Hiroshima Observatory and HONIR -- a 2 channel imager (Rc and H or J) (Akitaya et al. 2014, 9147, 91474O)
 - 200 cm Nayuta telescope at Nishi-Harima Astronomical Observatory and Nishiharima Infrared Camera, NIC (J, H, Ks)
 - 380 cm Seimei telescope at Okayama Observatory and optical-fiber integral field spectrograph, KOOLS-IFU

We found no apparent transient object in these galaxies to 5 sigma
limiting magnitudes listed below, except for a few marginal cases
that are being carefully investigated by spectroscopy. We will post
it if it is likely an actual transient.
 
galid            ra        dec       G      g      r      R      i      I      z      J      H      K                                     obsid
GL055116-310617   87.8176  -31.1046     --  19.51  20.06     --  19.47     --     --     --     --     --                              BandC-Tripol
GL055150-314446    87.958  -31.7461     --  19.82  19.81     --  19.32     --     --     --     --     --                              BandC-Tripol
GL054828-325838    87.115  -32.9772     --  18.61  19.01     --  18.31     --     --     --     --     --                              BandC-Tripol
GL055050-314427   87.7077  -31.7407     --  17.25  17.05     --  16.56     --     --     --     --     --                              BandC-Tripol
GL055504-313735   88.7683  -31.6263     --  16.75  16.91     --  16.25     --     --     --     --     --                              BandC-Tripol
GL055140-313123   87.9168  -31.5231     --  18.70  18.97     --  18.29     --     --     --     --     --                              BandC-Tripol
GL055352-324437   88.4666  -32.7436     --  17.75     --     --  17.18     --     --     --     --     --                              BandC-Tripol
GL054902-312929   87.2593  -31.4913     --  14.98  14.89     --  17.76     --     --     --     --     --                              BandC-Tripol
GL055123-310146   87.8458  -31.0294     --  17.40  17.77     --  17.25     --     --     --     --     --                              BandC-Tripol
GL055552-320353   88.9671  -32.0647     --  13.71  13.00     --  13.38     --     --     --     --     --                              BandC-Tripol
GL055050-314426   87.7074  -31.7404     --  17.25  17.05     --  16.56     --     --     --     --     --                              BandC-Tripol
GL055349-324625   88.4551  -32.7736     --  17.75     --     --  17.18     --     --     --     --     --                              BandC-Tripol
GL055054-314721    87.726  -31.7891     --  17.25  17.05     --  16.56     --     --     --     --     --                              BandC-Tripol
GL055137-313213   87.9051   -31.537     --  18.70  18.97     --  18.29     --     --     --     --     --                              BandC-Tripol
GL054835-330005    87.147  -33.0013     --  18.61  19.01     --  18.31     --     --     --     --     --                              BandC-Tripol
GL145211+044054  223.0459    4.6818     --     --     --  21.88     --     --     --  16.08  19.77     --                       OAOWFC,Kanata-HONIR
GL055045-314528   87.6857  -31.7579     --  17.25  17.05     --  16.56     --     --     --     --     --                              BandC-Tripol
GL134200+003605  205.4958    0.6015     --     --  17.40  18.07  18.78     --  18.78  16.89  15.72     --         OAOWFC,Kanata-HONIR,SaCRA-MuSaSHI
GL142718+044810  216.8261    4.8029  18.74     --     --  21.84     --  18.04     --  18.49  19.94     --         OAOWFC,Kanata-HONIR,MITSuME-Akeno
GL133953+005024    204.97    0.8399     --     --  16.64  20.94  18.37     --  16.64  18.98  18.56     --                Kanata-HONIR,SaCRA-MuSaSHI
GL144043+032756  220.1787    3.4654  18.18     --     --  21.41     --  17.63     --  19.01  19.44  99.99  MITSuME-Akeno,Kanata-HONIR,OAOWFC,Nayuta
GL134511+000710  206.2954    0.1194     --     --     --  20.62     --     --     --  17.57  19.18     --                       Kanata-HONIR,OAOWFC
GL133648+010914  204.1999    1.1538     --     --     --  20.34     --     --     --     --  18.84     --                              Kanata-HONIR
GL145412+044501  223.5521    4.7502  19.10     --     --  19.08     --  18.36     --     --     --     --                             MITSuME-Akeno
GL133644-032952  204.1844   -3.4978  17.95     --     --  18.36     --  17.94     --     --     --     --                             MITSuME-Akeno
GL133614-010217  204.0588   -1.0381  16.19     --     --  19.15     --  16.83     --     --  17.82     --                MITSuME-Akeno,Kanata-HONIR
GL134042-044642   205.175   -4.7784  13.92     --  15.82  13.34  18.78  13.41  18.78     --     --     --             MITSuME-Okayama,SaCRA-MuSaSHI
GL133715-045629  204.3112   -4.9413  14.85     --     --  20.78     --  14.39     --     --  19.27     --                MITSuME-Akeno,Kanata-HONIR

Keto Zhang, Thomas de Jaeger, Benjamin Stahl, WeiKang Zheng,
James Sunseri, Yukei Murakami, Andrew Hoffman, Emily Ma,
Julia Hestenes, 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 field of the gravitational-wave event
S190510g (GCN 24442
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 303 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 04:26:32, May. 10 UT,
about 1.4 hours after the trigger, and the last image at 12:17:12 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(May 10)  RA (J2000)   Dec (J2000)
-----------------------------------------------
G0650384 04:26:32 13:46:10.220 +00:01:22.60
G0711430 04:32:02 14:25:32.320 +01:05:25.10
G0600743 04:39:14 14:55:52.310 +00:33:46.50
G0125934 04:41:06 13:37:14.310 -01:08:19.50
G0612428 04:42:23 12:58:51.500 -17:14:23.30
G0808644 04:43:40 13:43:51.330 -12:13:41.70
G0576307 04:44:56 13:11:34.840 -17:31:40.50
G0629956 04:46:07 12:58:50.810 -17:22:39.00
G0599598 04:47:32 15:18:20.550 +07:49:18.80
G0598294 04:48:48 15:34:23.420 -08:45:52.10
G0573739 04:50:08 14:02:08.470 -09:20:51.30
G0806622 04:51:29 15:18:54.400 +10:49:33.20
G0597451 04:52:48 14:46:05.640 -14:01:38.40
G0790561 04:54:08 15:47:04.880 +08:44:01.70
G0756031 04:55:23 15:12:30.640 +01:41:30.40
G0122092 05:06:58 14:34:50.360 +05:22:26.10
G0800181 05:08:15 13:33:56.620 -03:07:35.10
G0761596 05:09:33 14:36:06.820 +05:16:29.80
G1849600 05:10:44 14:51:48.610 +05:02:20.60
G0720328 05:12:04 13:41:42.330 -04:52:32.60
G0626893 05:13:13 13:43:56.930 -05:09:38.60
G0553544 05:14:22 13:38:20.950 -03:40:52.80
G0568021 05:15:40 14:41:41.460 +03:23:02.20
G0004973 05:18:08 13:40:56.980 +00:44:00.00
G0572321 05:19:24 14:31:41.450 +01:47:47.00
G0750998 05:20:41 13:37:01.000 +00:09:52.10
G0724509 05:21:57 14:34:08.230 +03:51:43.50
G0660276 05:23:15 13:28:57.590 -02:01:28.30
G0044657 05:24:24 13:30:22.630 -04:35:43.10
G0660959 05:25:46 14:58:32.700 +08:12:30.00
G0680774 05:27:02 14:18:34.450 +01:57:53.30
G0788945 05:28:19 13:36:38.510 -01:01:07.40
G0581157 05:29:30 13:45:24.920 +02:00:46.10
G0602455 05:30:39 13:31:31.550 -00:42:09.60
G0774899 05:31:57 14:28:30.690 +04:44:06.50
G0631517 05:33:10 15:02:20.190 +01:33:41.90
G0703829 05:34:22 14:51:11.830 +06:25:43.20
G0750493 05:45:47 13:40:41.320 -06:04:22.40
G0669926 05:46:56 13:46:40.490 -05:36:21.00
G0710006 05:48:13 14:28:16.580 +04:43:00.20
G0653845 05:49:28 13:42:58.330 +00:30:16.10
G0275674 05:50:38 13:37:13.790 -01:08:10.50
G0158239 05:51:47 13:37:44.500 -03:35:45.20
G0610030 05:53:08 14:53:09.090 +04:36:10.90
G1486915 05:54:27 13:40:52.080 +00:44:33.40
G0800724 05:55:36 13:37:51.700 +01:05:24.00
G0273501 05:56:46 13:38:06.080 +00:16:13.20
G0814094 05:57:55 13:37:47.130 +01:03:19.70
G0686579 06:13:02 14:29:31.820 +03:10:35.80
G0494561 06:14:13 14:51:49.580 +05:02:06.40
G0708336 06:15:33 13:41:19.990 -04:53:32.80
G0634594 06:16:42 13:26:45.250 -03:57:53.10
G0665502 06:18:00 14:31:59.060 +05:53:37.60
G0810237 06:37:52 14:53:38.650 +07:51:14.60
G0001044 06:39:09 13:50:12.390 -07:19:11.60
G0817994 06:40:21 13:37:09.180 -08:35:45.90
G0624135 06:41:32 13:41:11.690 +02:22:56.30
G0562882 06:42:43 13:41:43.280 -07:50:52.30
G0650788 06:43:55 13:46:07.980 -02:53:34.80
G0687855 06:45:38 13:22:48.960 -16:31:14.90
G0505015 06:46:47 13:10:23.760 -13:42:09.40
G0652463 06:47:59 13:37:41.070 -08:30:00.80
G0698538 06:49:10 13:21:01.060 -10:34:58.00
G0730033 06:50:21 13:38:15.220 -05:02:22.50
G0616171 06:51:33 13:50:39.050 -06:12:04.80
G0555307 06:53:14 13:38:09.000 +02:33:13.70
G0590897 06:58:47 14:18:36.630 +00:14:25.10
G0035007 07:00:24 14:57:37.080 +06:23:00.20
G0793412 07:01:40 14:48:27.660 +00:56:45.00
G0720022 07:02:51 14:24:07.910 +06:04:03.00
G0609958 07:04:02 14:51:19.760 +10:14:55.30
G0601108 07:05:12 14:56:38.250 +09:30:35.10
G0799448 07:06:31 13:44:44.870 +00:22:11.50
G0792678 07:07:51 14:54:34.470 -00:04:03.10
G0574038 07:09:02 14:36:24.670 +00:15:01.50
G0668231 07:10:13 14:59:38.390 +07:54:32.00
G0596305 07:29:38 14:18:48.990 +00:25:20.20
G0759911 07:31:00 12:51:58.080 -14:26:17.80
G0651733 07:32:09 12:55:07.060 -16:11:17.50
G1851320 07:33:19 12:57:56.340 -18:03:06.00
G0608829 07:34:28 12:58:13.050 -17:30:50.70
G1851307 07:36:07 12:52:16.000 -15:18:22.50
G0860662 07:37:16 12:52:16.080 -15:18:20.30
G0665649 07:38:26 12:54:19.670 -15:38:20.10
G1856321 07:39:35 12:59:33.680 -20:05:18.90
G0762568 07:40:44 12:59:33.230 -18:25:01.30
G0825435 07:41:54 13:06:17.940 -17:32:55.90
G0820468 07:43:05 13:06:29.600 -11:22:15.60
G1175244 07:44:14 13:12:51.000 -08:58:34.70
G0623406 07:45:23 13:14:33.990 -10:51:50.20
G0655184 07:46:33 13:16:02.430 -13:22:22.30
G0801615 07:47:42 13:18:47.250 -15:37:38.10
G0552025 07:48:55 13:18:58.230 -00:24:48.40
G0814012 07:50:09 13:19:02.980 -15:24:46.00
G1433257 07:51:20 13:19:19.340 -04:24:42.70
G0700184 07:52:29 13:19:40.480 -10:43:57.70
G0566980 07:53:41 13:19:56.820 -00:17:59.40
G0827880 07:54:50 13:24:40.070 +01:15:41.30
G0649473 07:56:01 13:24:57.500 -04:29:43.10
G0787749 07:57:11 13:25:11.080 -03:56:04.90
G0772246 07:58:20 13:27:17.110 +00:07:19.00
G0806831 07:59:29 13:28:21.780 -01:06:29.90
G0660292 08:00:41 13:28:25.440 +08:36:46.50
G0283060 08:01:57 13:29:20.790 -14:22:48.60
G0788918 08:03:08 13:31:57.190 -01:50:28.40
G1851429 08:04:18 13:32:10.480 -01:49:46.50
G0487238 08:05:27 13:32:10.690 -01:49:35.50
G0827441 08:06:36 13:32:54.380 -01:32:43.20
G0749829 08:07:45 13:32:59.000 +01:48:07.10
G0765550 08:08:55 13:33:44.280 +00:14:29.10
G0414403 08:10:06 13:34:51.850 -09:13:51.30
G0668924 08:11:15 13:35:02.760 -02:51:59.10
G0811073 08:12:27 13:35:04.210 +02:39:19.20
G0812204 08:13:36 13:35:07.720 +02:13:57.80
G0650083 08:14:45 13:35:43.380 -00:59:48.70
G0676469 08:15:57 13:35:47.290 -12:02:06.30
G0762641 08:17:10 13:35:55.380 -00:16:22.40
G0578072 08:18:19 13:36:04.120 -00:24:16.50
G0582392 08:19:33 13:36:07.410 -15:57:58.10
G0784848 08:20:44 13:36:26.760 -10:14:39.80
G0645795 08:21:55 13:38:01.220 +00:15:43.60
G0695555 08:23:09 13:38:04.760 +03:39:44.80
G0792948 08:24:18 13:38:08.190 +02:34:32.90
G1126565 08:31:41 13:38:14.450 -06:09:20.30
G1346597 08:32:54 13:38:22.350 +06:05:05.40
G0788796 08:34:04 13:38:51.030 +03:50:02.40
G0477760 08:35:17 13:39:34.350 -13:39:44.30
G0636354 08:36:29 13:39:39.430 -04:38:37.90
G0788111 08:37:40 13:39:52.820 +03:16:23.10
G0698851 08:40:01 13:41:32.800 -05:10:10.70
G0711105 08:41:12 13:42:04.490 +01:41:35.20
G0573061 08:42:25 13:42:15.220 -14:44:30.30
G0791457 08:43:35 13:42:40.420 -12:11:58.60
G0815563 08:44:46 13:42:46.260 -04:58:48.60
G0684407 08:45:55 13:42:54.650 +02:24:56.60
G0479347 08:47:05 13:42:54.770 +02:20:26.00
G0563322 08:48:16 13:43:00.270 -04:28:08.20
G0730683 08:49:29 13:43:00.760 +03:31:31.50
G1127151 08:50:39 13:43:14.120 +01:42:13.90
G0617196 08:51:48 13:45:36.880 +00:27:53.40
G0697080 08:52:57 13:45:39.540 +02:45:54.50
G0802136 08:54:06 13:45:56.300 -01:14:24.80
G1473253 08:55:18 13:46:13.940 -06:37:02.90
G0574578 08:56:27 13:46:20.650 -02:03:56.30
G0719849 08:57:38 13:46:23.520 -10:33:10.10
G0826962 08:58:48 13:47:11.210 -11:07:21.90
G0596597 08:59:57 13:49:34.150 -06:40:22.60
G0768556 09:01:06 13:51:21.980 -08:33:04.80
G0593502 09:02:20 13:51:30.770 +03:05:55.00
G0822015 09:03:33 13:52:38.330 -08:55:51.50
G0687515 09:04:44 13:57:24.270 -00:20:30.30
G0555591 09:05:54 14:03:10.260 -00:19:43.20
G0271717 09:07:05 14:05:44.990 -09:48:19.90
G0648520 09:08:14 14:09:08.710 -09:09:47.20
G0783648 09:09:28 14:13:09.900 -10:10:07.00
G0207460 09:10:39 14:15:04.570 +00:52:18.30
G0608535 09:11:48 14:15:26.620 -00:17:04.10
G0717771 09:12:58 14:15:48.260 +03:40:01.00
G0232102 09:14:07 14:15:50.150 +03:02:29.70
G0796975 09:15:16 14:16:07.850 +04:50:13.10
G0602117 09:16:26 14:18:01.310 +00:23:17.70
G0695699 09:17:35 14:18:21.570 -00:03:54.20
G0607064 09:18:44 14:18:27.510 +00:23:37.60
G0614442 09:19:53 14:18:30.010 +00:15:43.20
G0631845 09:23:59 14:27:06.440 +05:09:06.10
G0645566 09:25:10 14:25:10.680 -00:45:56.70
G0583981 09:26:26 14:59:04.230 +03:13:10.00
G0715490 09:27:37 14:39:16.110 -00:25:56.60
G0775953 09:28:57 13:33:19.680 +01:28:04.00
G0792877 09:30:14 14:30:52.930 +07:10:07.90
G1258137 09:31:31 13:44:11.940 +03:44:15.80
G0552562 09:32:50 14:52:20.270 +09:30:48.40
G0159954 09:33:59 14:43:37.110 +05:16:10.50
G0770215 09:35:11 14:30:40.580 +07:10:04.80
G0782845 09:36:29 13:38:17.990 +06:23:15.20
G1851589 09:37:49 14:51:59.380 -00:06:59.10
G0585556 09:39:00 15:02:47.110 +04:51:24.10
G0784007 09:40:41 14:31:08.220 -06:30:50.10
G0855361 09:41:52 14:38:33.720 +07:44:48.50
G0775171 09:43:13 13:22:27.490 -08:17:30.90
G0398790 09:44:24 13:04:52.250 -16:39:23.10
G0706070 09:45:35 13:25:08.090 -12:45:51.80
G1851418 09:46:45 13:30:29.740 -11:14:27.70
G0707702 09:48:02 14:30:40.070 +00:16:52.60
G0762973 09:49:13 14:16:18.060 -02:32:01.70
G0678760 09:50:27 14:45:33.850 -03:18:27.60
G0560281 09:51:44 13:39:07.070 -01:59:28.70
G0776622 09:53:04 14:53:10.620 -00:20:03.30
G0728663 09:54:17 14:25:46.130 +02:34:39.90
G0498545 09:55:27 14:29:44.640 +00:37:33.60
G0699635 09:56:36 14:31:45.650 +00:09:46.10
G0610131 09:57:47 14:44:35.640 +11:03:28.50
G0003364 09:59:01 14:28:11.850 -02:20:53.90
G0591552 10:00:20 13:22:13.470 -08:54:55.00
G0562491 10:01:40 14:36:22.760 +01:46:46.90
G0823067 10:02:51 14:32:33.050 -03:22:38.20
G0678990 10:04:02 14:59:23.450 +08:07:54.00
G0558309 10:05:14 14:37:38.690 +09:50:46.10
G1851565 10:06:23 14:32:26.600 +06:46:13.60
G0618864 10:07:34 14:42:16.780 +10:42:54.00
G0758997 10:08:48 14:25:01.430 +07:40:27.90
G0729352 10:11:23 13:24:49.290 -06:32:25.20
G0774152 10:12:43 14:58:27.850 +08:18:49.80
G0720700 10:13:59 14:25:06.920 +06:06:15.50
G0600447 10:15:10 14:51:37.560 +09:25:43.60
G0551463 10:16:22 14:37:40.920 +08:02:28.90
G0736858 10:17:33 14:29:10.190 -00:46:13.90
G0777105 10:18:42 14:29:38.810 -03:25:01.30
G0678446 10:19:57 14:59:21.540 +08:27:27.90
G0617350 10:21:12 14:15:13.020 -00:59:01.90
G0549236 10:22:23 14:42:18.050 +09:06:40.40
G0811027 10:23:35 14:24:48.460 +06:29:21.20
G0618435 10:24:48 14:57:32.700 +09:17:32.60
G0651141 10:31:05 14:24:46.250 -00:45:04.40
G0586815 10:32:14 14:25:59.510 -03:09:14.10
G0789714 10:33:23 14:26:33.180 -01:12:03.50
G0811835 10:34:33 14:29:15.860 -02:04:05.20
G0712741 10:35:42 14:32:43.630 -02:04:35.20
G0702786 10:36:53 14:35:04.250 +09:00:09.70
G0611833 10:38:07 14:35:27.630 +09:41:29.30
G0691187 10:39:16 14:35:38.770 +09:44:25.90
G0785942 10:40:32 14:35:57.700 -04:11:43.40
G0629470 10:41:47 14:36:40.010 +08:13:00.50
G0558147 10:42:56 14:37:26.080 +09:51:17.60
G1171775 10:44:06 14:37:32.230 +05:25:04.70
G0589229 10:45:15 14:39:44.100 +10:02:18.10
G0799707 10:46:24 14:40:36.840 +09:25:40.80
G0552775 10:47:34 14:42:11.300 +09:58:28.90
G0627386 10:48:47 14:45:41.900 -04:25:09.30
G1851580 10:49:59 14:47:20.160 +06:27:31.10
G0670265 10:51:10 14:47:48.630 -02:02:19.00
G0032799 10:52:23 14:47:56.010 +11:30:42.70
G0675423 10:53:35 14:48:03.250 +00:23:55.90
G0811089 10:54:46 14:48:02.420 +11:30:47.80
G0826283 10:56:00 14:48:28.340 -01:42:50.50
G0650014 10:57:13 14:49:37.560 -04:48:56.90
G0630052 10:58:29 14:50:07.080 +11:02:08.30
G0619206 10:59:38 14:50:30.710 +11:10:08.20
G0716381 11:00:47 14:50:57.620 +05:38:40.60
G0706975 11:02:01 14:51:24.940 -01:15:11.60
G0686544 11:03:12 14:52:39.400 +08:29:12.90
G1437018 11:04:22 14:52:50.030 +05:10:02.10
G0788095 11:05:33 14:58:53.250 -02:20:26.90
G0619732 11:06:42 14:59:01.400 -06:47:59.70
G0618812 11:07:52 14:59:08.270 -06:32:00.60
G0649036 11:09:05 15:00:00.110 +08:36:44.80
G0800605 11:10:16 15:04:02.280 -02:39:25.00
G1851610 11:11:27 15:04:25.320 +04:36:30.70
G0738987 11:12:37 15:05:58.560 +05:43:23.20
G0558058 11:13:46 15:12:35.210 +05:19:32.50
G0583283 11:14:55 15:17:41.890 +06:57:04.10
G0798657 11:16:05 15:19:59.630 +04:27:05.10
G0630232 11:17:14 15:22:49.080 +07:38:25.10
G0777754 11:18:23 15:30:26.610 +07:30:28.80
G1856457 11:19:37 15:50:27.600 +00:10:32.10
G0596305 11:21:26 14:18:49.140 +00:25:18.90
G0549862 11:22:35 14:18:57.720 +04:58:52.40
G0594358 11:23:49 14:19:36.290 +07:17:19.70
G0573840 11:24:58 14:19:45.250 +10:45:20.70
G0606388 11:26:09 14:19:49.520 -00:10:55.30
G1123685 11:27:21 14:20:05.680 +07:49:31.40
G0567452 11:28:34 14:20:17.170 -03:51:46.50
G0671077 11:29:44 14:22:54.960 -00:38:40.20
G0643002 11:30:53 14:26:50.110 -02:25:12.10
G0813325 11:32:02 14:29:02.340 -01:56:14.80
G0721949 11:33:18 14:30:34.980 +10:29:56.90
G0690948 11:34:33 14:31:18.930 -01:52:22.50
G0814206 11:35:42 14:36:19.600 -05:31:40.20
G0600204 11:36:52 14:37:16.810 -01:28:14.50
G1850386 11:38:07 14:37:26.640 +11:18:42.00
G0559943 11:39:16 14:39:10.730 +11:28:46.80
G0692513 11:40:32 14:39:45.680 -01:59:58.00
G0675092 11:41:47 14:42:14.510 +10:33:03.10
G0009688 11:42:57 14:42:59.340 +11:59:18.30
G0658340 11:44:12 14:44:04.670 -03:43:40.70
G0031927 11:45:28 14:45:16.500 +12:03:02.80
G0001035 11:46:41 14:45:54.870 +01:52:27.00
G1058466 11:47:55 14:47:49.470 +11:17:57.80
G0765998 11:49:04 14:48:14.600 +09:38:04.70
G0634986 11:50:13 14:49:32.530 +11:14:44.40
G1436476 11:51:23 14:49:54.190 +12:24:39.70
G0566792 11:52:32 14:51:24.220 +11:02:06.20
G0812708 11:53:47 14:59:31.160 -06:53:44.10
G0558644 11:54:59 15:06:18.340 +04:24:21.90
G0787664 11:56:12 15:07:19.610 +06:18:23.00
G0725617 11:57:23 15:09:08.930 +01:10:35.10
G0593641 11:58:35 15:11:15.280 +07:37:58.60
G0616339 11:59:44 15:12:03.180 +04:13:20.10
G0730896 12:00:53 15:12:28.440 +07:10:46.80
G0563214 12:02:03 15:13:44.610 +07:21:46.40
G0635905 12:03:12 15:14:11.940 +04:12:58.40
G0235323 12:04:21 15:17:28.690 +07:40:23.10
G0563336 12:05:31 15:18:47.560 +04:05:34.70
G0564919 12:06:40 15:19:05.970 +05:14:25.80
G0648544 12:07:49 15:21:16.620 +03:26:58.90
G0768102 12:09:01 15:22:51.830 +08:21:19.50
G0768809 12:10:10 15:24:01.970 +08:32:29.20
G0702070 12:11:19 15:26:09.290 +07:05:16.10
G0559285 12:12:28 15:29:40.980 +07:19:18.40
G0759705 12:13:38 15:33:42.080 +04:41:04.10
G0806928 12:14:49 15:41:49.270 +09:41:18.90
G0232365 12:15:58 15:45:24.370 +11:29:25.50
G0781399 12:17:12 15:50:18.870 +00:07:30.20

The LIGO Scientific Collaboration and the Virgo Collaboration report:


We continue analyzing the LIGO and Virgo data around the time of

the Compact Binary Coalescence (CBC) candidate S190510g

(GCN 24442
Loading...
 
  and GCN 24448
Loading...
 
 ):


https://gracedb.ligo.org/superevents/S190510g/


A new version of the classification estimation code, which better accounts

for the significance of the event using detection-pipeline-specific foreground

and background models, was applied to the data. This yields the following

updated classification of the GW signal, in order of descending probability:

BNS (85%), Terrestrial (15%), NSBH (<1%), BBH (<1%), or MassGap (<1%).

This new version of the classification estimation code will be deployed in

the front-end of the low latency pipelines on the next detector maintenance

intervention on Tuesday, May 14th 2019 15:00UTC.


Continued examination of this event also revealed there are data

quality issues and non-stationary noise behavior around the time of the

event. Its significance may decrease as our estimate of the background

improves. If the event is astrophysical, the currently preferred

skymap still represents our best estimate of source location. However,

the noise characteristics around the time of the event could bias such

localizations.


Further analysis of the event is ongoing.


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/>.

Po-Chieh Yu (NCU), Han-Jie Tan (NCU), Albert Kong (NTHU), Atharva Sunil
Patil (NCU), Chow-Choong Ngeow (NCU), Wing-Huen Ip (NCU), on behalf of the
Global Relay of Observatories Watching Transients Happen (GROWTH)
collaboration

We report observations of 81 galaxies in the 90% localization of the BNS
merger candidate, S190510g, detected by LIGO/Virgo (GCN #24442
Loading...
 
 ; GCN #24448
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 )
using the Lulin One-meter Telescope (LOT) in Taiwan. The observation
started at 2019-05-10 12:54:43 UT, ~10 hours after the trigger. The
observations were conducted using the r-band filter with 180 second
exposure time. By comparing with Pan-STARRS images, we do not detect
transient candidates brighter than r~21 mag (AB). We thank the staff in
Lulin Observatory for helping the observations. The galaxy coordinates are
listed below.

RA (hh mm ss.ss)      Dec (dd mm ss.s)
    13 00 30.12    -09 09 05.1
    13 00 37.49    -07 48 41.1
    13 00 52.36    -07 45 26.1
    13 01 23.02    -08 59 37.6
    13 02 12.79    -04 44 29.1
    13 02 52.28    -04 48 03.1
    13 03 38.53    -06 51 24.2
    13 04 02.72    -08 43 33.5
    13 04 09.43    -07 28 24.5
    13 04 09.49    -07 19 24.5
    13 04 42.00    -12 37 29.0
    13 04 48.48    -04 22 26.8
    13 05 00.24    -11 15 24.4
    13 05 03.06    -11 12 48.8
    13 05 08.16    -04 16 23.1
    13 05 10.38    -10 40 25.7
    13 05 12.72    -04 03 07.6
    13 05 13.06    -11 21 30.7
    13 05 20.26    -10 36 31.1
    13 05 26.54    -06 20 25.1
    13 05 28.69    -11 16 04.1
    13 05 28.80    -11 16 04.1
    13 05 30.07    -09 37 48.1
    13 05 30.29    -10 26 18.1
    13 05 35.04    -04 14 35.2
    13 05 35.43    -07 13 59.1
    13 05 41.00    -10 26 43.1
    13 05 47.28    -03 59 07.1
    13 05 51.84    -05 30 16.2
    13 05 52.40    -05 22 12.4
    13 05 56.88    -03 03 17.8
    13 06 03.36    -12 22 28.2
    13 06 04.57    -11 33 44.0
    13 06 04.58    -05 22 30.4
    13 06 04.80    -02 40 08.4
    13 06 08.27    -05 22 40.3
    13 06 11.37    -11 33 13.0
    13 06 17.41    -07 45 42.3
    13 06 21.36    -12 31 25.1
    13 06 28.55    -06 51 11.3
    13 06 32.34    -05 13 49.6
    13 06 33.14    -07 23 50.3
    13 06 37.68    -05 04 19.2
    13 06 45.57    -08 08 03.9
    13 06 45.84    -03 57 35.3
    13 06 52.10    -06 31 05.9
    13 06 58.32    -11 47 28.0
    13 07 02.40    -04 37 05.9
    13 07 04.80    -03 15 50.0
    13 07 05.28    -11 55 48.0
    13 07 17.06    -10 56 51.2
    13 07 17.52    -04 54 11.7
    13 07 19.64    -10 54 11.2
    13 07 20.64    -05 17 03.1
    13 07 26.00    -04 16 23.7
    13 07 26.39    -06 42 24.2
    13 07 30.55    -07 19 28.2
    13 07 36.74    -02 44 25.7
    13 07 37.30    -08 33 09.2
    13 07 37.44    -01 11 35.3
    13 07 41.28    -02 48 07.3
    13 07 41.78    -07 36 13.2
    13 07 42.00    -05 42 58.0
    13 07 42.24    -06 24 53.8
    13 07 42.62    -06 22 14.2
    13 07 55.44    -06 25 41.2
    13 07 57.12    -12 51 04.7
    13 07 58.64    -12 11 21.7
    13 07 59.28    -03 53 33.8
    13 08 03.31    -05 23 27.8
    13 08 10.87    -12 58 48.7
    13 08 11.86    -04 31 09.8
    13 08 16.21    -03 44 46.8
    13 08 17.68    -07 02 37.2
    13 08 20.91    -11 49 03.2
    13 08 22.56    -11 24 51.2
    13 08 24.72    -06 23 46.2
    13 08 28.60    -06 22 11.2
    13 08 29.04    -06 22 40.3
    13 08 29.67    -12 26 32.9
    13 08 32.40    -05 31 52.7
    13 08 34.16    -10 06 39.2
    13 08 35.20    -12 09 01.9
    13 08 37.44    -12 05 26.2
    13 08 38.15    -11 01 16.2
    13 08 40.17    -06 47 17.2
    13 08 42.67    -10 04 54.3
    13 08 59.52    -05 16 45.8
    13 08 59.52    -09 54 34.3
    13 09 04.25    -07 13 52.3
    13 09 04.33    -10 02 04.3
    13 09 06.96    -05 18 37.4
    13 09 18.31    -06 52 26.1
    13 09 19.68    -05 21 43.2
    13 09 21.47    -07 26 25.1
    13 09 22.41    -13 35 58.6
    13 09 30.48    -04 38 13.2
    13 09 36.00    -04 17 35.5
    13 09 36.97    -10 29 45.0
    13 09 39.53    -06 57 44.0
    13 09 39.84    -12 20 19.5
    13 09 39.96    -12 20 19.6
    13 09 42.20    -07 53 07.2
    13 09 43.09    -03 04 51.9
    13 09 45.36    -05 12 35.7
    13 09 47.04    -03 05 26.6
    13 09 51.12    -03 25 13.4
    13 09 56.40    -03 31 02.6
    13 10 02.15    -06 07 41.2
    13 10 04.56    -03 05 11.2
    13 10 06.42    -07 35 59.2
    13 10 06.47    -12 15 38.8
    13 10 12.81    -07 02 43.4
    13 10 13.20    -05 52 47.9
    13 10 14.28    -07 31 10.4
    13 10 17.28    -03 47 12.5
    13 10 21.75    -07 38 56.4
    13 10 24.72    -11 41 13.2
    13 10 27.39    -07 04 30.4
    13 10 34.08    -05 52 13.8
    13 10 37.44    -03 41 48.2
    13 10 41.47    -04 39 34.6
    13 10 44.16    -01 48 07.7
    13 10 45.47    -12 34 54.5
    13 10 46.08    -01 49 19.2
    13 10 46.28    -06 02 11.1
    13 10 48.93    -09 15 34.1
    13 10 49.92    -10 52 29.4
    13 10 50.53    -12 27 24.6
    13 10 51.01    -12 18 23.6
    13 10 51.37    -06 53 53.1
    13 10 54.76    -13 05 46.6
    13 10 55.92    -03 26 06.4
    13 10 58.65    -11 55 37.6
    13 11 00.70    -12 09 10.6
    13 11 02.88    -04 57 06.8
    13 11 06.00    -12 22 38.6
    13 11 07.44    -12 13 14.9
    13 11 08.13    -12 07 27.5
    13 11 16.65    -07 16 19.5
    13 11 20.84    -12 29 34.1
    13 11 23.04    -05 53 16.5
    13 11 28.32    -01 34 01.6
    13 11 29.28    -02 28 24.3
    13 11 29.92    -01 35 53.1
    13 11 30.24    -05 22 58.8
    13 11 30.48    -11 48 56.4
    13 11 31.20    -03 23 46.0
    13 11 34.19    -04 18 17.1
    13 11 34.26    -09 06 03.5
    13 11 41.36    -05 26 23.9
    13 11 42.21    -10 38 57.0
    13 11 42.43    -10 07 01.0
    13 11 50.14    -08 52 26.0
    13 11 54.62    -12 41 20.2
    13 11 55.92    -12 05 52.4
    13 12 00.07    -09 18 18.0
    13 12 04.40    -12 52 35.2
    13 12 06.72    -02 40 56.0
    13 12 12.48    -01 05 42.5
    13 12 20.89    -13 16 46.6
    13 12 22.54    -12 34 28.6
    13 12 26.16    -06 20 25.3

M. Axelsson (KTH and Stockholm Univ.), M. Arimoto (Kanazawa Univ.), E. Moretti (IFAE, Barcelona), D. Kocevski (NASA/MSFC), N. Omodei (Stanford Univ.) and F. Dirirsa (Univ. of Johannesburg) report on behalf of the Fermi-LAT collaboration:

We have searched data collected by the Fermi Large Area Telescope (LAT) on May 10, 2019, for possible high-energy (E > 100 MeV) gamma-ray emission in spatial/temporal coincidence with the LIGO/Virgo trigger S190510g (GCN 24442
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.

The Fermi Gamma-ray Space Telescope was passing through the South Atlantic Anomaly (SAA) at the time of the trigger (T0 = 2019-05-10 02:59:39.292 UTC). During SAA passages both the LAT and Gamma-ray Burst Monitor (GBM) do not collect data due to the high charged particle background in this region. The LAT resumed taking data upon exiting the SAA at roughly T0 + 1340 s. At that time the instantaneous coverage was ~30% of the LIGO probability map, and reached 100% cumulative coverage after ~8.3 ks.

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 + 1340 s to T0 + 10 ks. No significant new sources are 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 100 GeV for this search vary between 1.1e-10 and 1.0e-9 [erg/cm^2/s].

The Fermi-LAT point of contact for this event is Feraol Dirirsa (fdirirsa@uj.ac.za<mailto:fdirirsa@uj.ac.za>).

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.

Gergely D��lya and Peter Raffai (Eotvos Univ.) reports on behalf of the GLADE
team:

We have found 17,197 galaxies in the GLADE catalog [1,2], within the
updated 90% GW
localization area (LALInference.fits.gz) reported by the LVC in GCN 24448
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 ,
and within 227 +/- 92 Mpc distance limits.

The galaxies found can be accessed on the GLADE website (4.6 MB txt file;
please note that the order of galaxies in the list only follow the ordering
as the appear in GLADE):
http://glade.elte.hu/O3/S190510g_GLADE_90_upd.txt

There are 353 galaxies within the 50% GW localization area and within
the same distance limits (97 kB txt file; please note that the order of
galaxies in the list only follow the ordering as the appear in GLADE):
http://glade.elte.hu/O3/S190510g_GLADE_50_upd.txt

[1] D��lya, G., Galg��czi G., Dobos, L. et al., 2018 MNRAS, 479, 2374
[2] http://glade.elte.hu

P. D'Avanzo (INAF-OAB), L. Izzo (IAA), S. Yang (INAF-OAPd), E. Palazzi 
(INAF-OAS), S Campana (INAF-OAB),

S. Benetti (INAF-OAPd), M.G. Bernardini (INAF-OAB), M.T. Botticella 
(INAF-OAC), M. Branchesi (GSSI),

A. Bulgarelli (INAF-OAS), S. Campana (INAF-OAB), E. Cappellaro 
(INAF-OAPd), R. Carini (INAF-OAR), R. Ciolfi (INAF-OAPd),

S. Covino (INAF-OAB), V. D'Elia (ASI-SSDC), M. Della Valle (INAF-OAC), 
 �A. Grado (INAF-OAC), G. Greco (Univ. Urbino),

A. Melandri (INAF-OAB), L. Nicastro (INAF-OAS), S. Piranomonte 
(INAF-OAR), A. Rossi (INAF-OAS), V. Testa (INAF-OAR),

L. Tomasella (INAF-OAPd), E. Brocato (INAF-OAAb, INAF-OAR), on behalf of 
GRAWITA report:


We carried out optical follow-up observations of the LIGO/Virgo GW 
trigger S190509g (LVC, GCN Circ. 24442
Loading...
 
 ) with the 60-cm

robotic telescope REM located at the La Silla Observatory (Chile). The 
observations started at 2019-05-10 at 05:27:51 UT,

simultaneously in the g, r, i, z bands (the REM NIR camera was not 
operational).


We observed the following galaxies within the 90% probability of the 
initial bayestar skymap visible from La Silla:


RA(J2000) Dec(J2000) Dist(Mpc) Abs_Mag(B)

--------------------------------------------------------------

 �14:40:29.9303:14:01.1 ��400.91 -20.19

 �13:40:22.5600:14:12.1 ��335.74 -19.36

 �13:39:26.41-04:38:43.7 ��331.50 -20.14

 �14:40:56.6403:09:10.7 ��376.70 -19.83

 �14:17:12.5701:59:31.5 ��261.43 -20.30

 �13:17:09.12-00:57:28.1 ��366.44 -19.74

 �13:40:11.16-04:36:24.0 ��351.69 -19.99

 �14:55:34.8008:39:43.5 ��376.70 -19.51

 �14:32:03.12-01:10:03.7 ��243.01 -19.33

 �14:31:11.16-02:37:20.2 ��315.22 -19.81

 �14:29:11.5209:38:11.6 ��385.48 -18.77

 �14:17:44.1601:58:52.6 ��259.42 -20.12

 �14:30:39.4007:16:30.0 ���21.40 -19.47

 �14:44:57.6000:50:40.1 ��317.69 -18.18

 �13:53:50.6400:50:43.3 ��279.25 -19.74


No clear counterpart for S190509g is found down to a typical 3sigma 
magnitude of r > 19 (AB).


We report the presence of a possible transient (likely unrelated to 
S190509g) found in the analysis of the REM

frames at the following coordinates (J2000):

RA = 14:29:15.99

Dec = +09:41:12.3

(+/- 1").


The source has a magnitude of r = 17.3 +/- 0.1 (AB, calibrated against 
the SDSS). We note that this object is

3.5" from the SDSS galaxy SDSS J142916.22+094112.1, whose catalogue 
magnitude is r = 22.56 +/- 0.20 and

photometric redshift is z = 0.182 +/- 0.073.


Further analysis and observations are planned.

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), B. Mingo (U. Leicester), 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 S190510g (LIGO/VIRGO Collaboration GCN Circ. 24442
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 ),
where T0 is the LVC trigger time (2019-05-10T02:59:39.292 UTC).

The center of the BAT FOV at T0 is
RA = 288.846 deg,
DEC = 10.936 deg,
ROLL = 58.998 deg.
The BAT Field of View (>10% partial coding) covers 0.95% of the integrated
LVC localization probability, and 0.00% 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 ~ 1.57 x 10^-7 erg/s/cm^2.

No event data are available at this time.

BAT retains decreased, but significant, sensitivity to rate increases for
gamma-ray events outside of its FOV. About 24.12% 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/S190510g/web/source.html

LIGO/Virgo S190510g: CLU/NED Galaxies in the Localization Volume

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

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

We spatially cross-matched the LIGO/Virgo S190510g trigger sky localization (90% containment volume) with the Census of the Local Universe (CLU; Cook et al. 2017; arxiv:1710.05016) galaxy catalog and found 8044 galaxies within the volume. The CLU catalog is a compilation of galaxies with existing redshifts from many sources (e.g., NED, SDSS, etc) and new galaxies from a 3PI narrow-band survey to look for redshifted Halpha emission out to 200 Mpc with the Palomar Oschin 48-inch telescope (Cook et al. 2017; arxiv:1710.05016). We list here the top 20 galaxies sorted by stellar mass (Mstar) for galaxies whose location on the sky and distance falls in the 90% volume reported by the BAYESTAR probability sky map (Singer et al. 2016). We also list the dust-corrected star formation rates (SFRs) for galaxies with GALEX FUV detections and a 'nan' for those with no detection.

For an extended list of galaxies in the 90% volume go to the NED Gravitational Wave Followup service at https://ned.ipac.caltech.edu/uri/NED::GWF/. This service provides downloadable galaxy lists and visualizations for candidate host galaxies. For each GW alert, these products are automatically generated and made available within minutes to expedite efficient electromagnetic followup observations. The NED top 20 list is sorted by 2MASS absolute K-band magnitude, but users can sort the entire list on a variety of other criteria (probability density, UV magnitudes, etc) after download.


          name                ra       dec   distmpc logsfr_fuv logmstar  dP_dV
------------------------     --------  ------- ------- ---------- -------- --------
     2MASX J05580206-3820043  89.5083 -38.3346  141.03       1.50    11.84 1.17e-06
              ESO 307- G 011  89.9994 -38.1782  186.91       0.14    11.62 1.14e-06
              ESO 413- G 024  25.4956 -31.0094   83.04      -1.09    11.26 1.33e-07
GALEXASC J132755.20+000653.7 201.9799   0.1149  198.20      -0.62    11.24 2.74e-08
                    NGC 0612  23.4906 -36.4933  123.96       0.71    11.16 4.56e-08
                   NGC 0526A  20.9766 -35.0655   79.52       0.74    11.12 5.77e-08
              ESO 363- G 006  83.1713 -32.9618  193.70        nan    11.11 3.31e-08
     2MASX J05453627-2555305  86.4012 -25.9252  188.60      -0.47    11.09 3.82e-07
              ESO 365- G 005  94.6886 -35.3041  188.09        nan    11.09 5.73e-07
     2MASX J05403062-3548505  85.1277 -35.8141  196.74        nan    11.09 3.94e-08
              MCG -04-14-035  87.1797 -25.4773  181.00      -0.55    11.08 4.34e-07
             TOLOLO 0611-379  93.3691 -37.9971  159.89       0.97    11.08 1.29e-06
              MCG -07-13-001  89.9648 -39.1343  187.64      -0.54    11.08 2.83e-07
     2MASX J06090797-2730329  92.2832 -27.5092  194.94        nan    11.06 3.59e-07
                     GIN 298  86.1235 -26.0589  200.00      -0.41    11.05 3.42e-07
              ESO 307- G 013  90.1712 -40.0445  194.07      -0.42    11.04 9.21e-08
              ESO 364- G 033  92.1921 -33.9163  157.00        nan    11.03 6.75e-06
              MCG -04-14-014  85.5302 -26.1982  158.50      -0.73    11.03 3.15e-07
     2MASX J06004280-3925378  90.1783 -39.4271  194.96      -0.65    11.03 2.19e-07
              ESO 488- G 013  86.7310 -25.6356  194.51      -0.56    11.03 3.47e-07


Table: Top 20 galaxies in CLU that fall in the 90% probability volume for S190510g sorted by stellar mass. Column descriptions are as follows. name: galaxy name. ra: RA (J2000, decimal degrees). dec: Dec (J2000, decimal degrees). distmpc: galaxy distance (Mpc). logsfr_fuv: log10 of the star formation rate (SFR, Msun per year), derived from GALEX All Sky Kron FUV magnitudes via the prescription of Murphy et al. (2011), corrected for internal dust extinction using a combination of GALEX FUV and 22um ALLWISE fluxes (Hao et al. 2011). logmstar: log10 of the galaxy stellar mass (Msun), estimated from 3.4um ALLWISE fluxes and a mass-to-light ratio of 0.5 (McGaugh & Schombert et al. 2015).

Michitoshi Yoshida, Yuhei Takagi, Tsuyoshi Terai (NAOJ) Yousuke
Utsumi (Stanford Univ.), Nozomu Tominaga (Konan Univ.), Mahito
Sasada, Hiroshi Akitaya (Hiroshima Univ.) on behalf of J-GEM
collaboration

We report optical imaging follow-up observations for a part of
the equator region (RA:13h, Dec:0d) of S190510g (LIGO Scientific
Collaboration and the Virgo Collaboration, GCN #24442
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 ) with Hyper
Suprime-Cam (HSC) attached to the 8.2-m Subaru Telescope. HSC
has a circular field-of-view whose area is 1.7 deg^2.

We performed Y-band imaging observations on 2019-05-10 UT. The
exposure time per frame was 30 sec. We covered 140 deg^2 around
the high probability area in the equator region of the Bayestar skymap
of S190510g with 120 pointings of HSC. We revisited each pointing
position two times. The 5-sigma limiting AB magnitude of Y-band was
about 22.7 mag.

The observed regions are as follows:

JGEM28175 13:27:11.25 -08:23:07.9
JGEM28432 13:30:00.00 -08:59:21.5
JGEM27663 13:27:11.25 -07:10:50.7
JGEM27920 13:30:00.00 -07:46:57.8
JGEM28176 13:32:48.75 -08:23:07.9
JGEM28433 13:35:37.50 -08:59:21.5
JGEM26895 13:24:22.50 -05:22:45.8
JGEM27151 13:27:11.25 -05:58:45.0
JGEM27408 13:30:00.00 -06:34:46.5
JGEM27664 13:32:48.75 -07:10:50.7
JGEM27921 13:35:37.50 -07:46:57.8
JGEM28177 13:38:26.25 -08:23:07.9
JGEM26383 13:24:22.50 -04:10:53.5
JGEM26639 13:27:11.25 -04:46:48.7
JGEM26896 13:30:00.00 -05:22:45.8
JGEM27152 13:32:48.75 -05:58:45.0
JGEM27409 13:35:37.50 -06:34:46.5
JGEM27665 13:38:26.25 -07:10:50.7
JGEM27922 13:41:15.00 -07:46:57.8
JGEM25871 13:24:22.50 -02:59:07.8
JGEM26127 13:27:11.25 -03:34:60.0
JGEM26384 13:30:00.00 -04:10:53.5
JGEM26640 13:32:48.75 -04:46:48.7
JGEM26897 13:35:37.50 -05:22:45.8
JGEM27153 13:38:26.25 -05:58:45.0
JGEM27410 13:41:15.00 -06:34:46.5
JGEM27666 13:44:03.75 -07:10:50.7
JGEM25615 13:27:11.25 -02:23:16.9
JGEM25872 13:30:00.00 -02:59:07.8
JGEM26128 13:32:48.75 -03:34:60.0
JGEM26385 13:35:37.50 -04:10:53.5
JGEM26641 13:38:26.25 -04:46:48.7
JGEM26898 13:41:15.00 -05:22:45.8
JGEM27154 13:44:03.75 -05:58:45.0
JGEM25103 13:27:11.25 -01:11:37.5
JGEM25360 13:30:00.00 -01:47:26.8
JGEM25616 13:32:48.75 -02:23:16.9
JGEM25873 13:35:37.50 -02:59:07.8
JGEM26129 13:38:26.25 -03:34:60.0
JGEM26386 13:41:15.00 -04:10:53.5
JGEM26642 13:44:03.75 -04:46:48.7
JGEM24591 13:27:11.25 -00:00:00.0
JGEM26899 13:46:52.50 -05:22:45.8
JGEM24848 13:30:00.00 -00:35:48.6
JGEM25104 13:32:48.75 -01:11:37.5
JGEM25361 13:35:37.50 -01:47:26.8
JGEM25617 13:38:26.25 -02:23:16.9
JGEM25874 13:41:15.00 -02:59:07.8
JGEM26130 13:44:03.75 -03:34:60.0
JGEM26387 13:46:52.50 -04:10:53.5
JGEM24336 13:30:00.00 -00:35:48.6
JGEM24592 13:32:48.75 -00:00:00.0
JGEM24849 13:35:37.50 -00:35:48.6
JGEM25105 13:38:26.25 -01:11:37.5
JGEM25362 13:41:15.00 -01:47:26.8
JGEM23824 13:30:00.00 +01:47:26.8
JGEM25618 13:44:03.75 -02:23:16.9
JGEM25875 13:46:52.50 -02:59:07.8
JGEM24080 13:32:48.75 +01:11:37.5
JGEM24337 13:35:37.50 -00:35:48.6
JGEM24593 13:38:26.25 -00:00:00.0
JGEM23312 13:30:00.00 +02:59:07.8
JGEM24850 13:41:15.00 -00:35:48.6
JGEM25106 13:44:03.75 -01:11:37.5
JGEM23568 13:32:48.75 +02:23:16.9
JGEM25363 13:46:52.50 -01:47:26.8
JGEM25619 13:49:41.25 -02:23:16.9
JGEM23825 13:35:37.50 +01:47:26.8
JGEM24081 13:38:26.25 +01:11:37.5
JGEM24338 13:41:15.00 -00:35:48.6
JGEM23056 13:32:48.75 +03:34:60.0
JGEM24594 13:44:03.75 -00:00:00.0
JGEM24851 13:46:52.50 -00:35:48.6
JGEM23313 13:35:37.50 +02:59:07.8
JGEM25107 13:49:41.25 -01:11:37.5
JGEM23569 13:38:26.25 +02:23:16.9
JGEM22544 13:32:48.75 +04:46:48.7
JGEM23826 13:41:15.00 +01:47:26.8
JGEM24082 13:44:03.75 +01:11:37.5
JGEM22801 13:35:37.50 +04:10:53.5
JGEM24339 13:46:52.50 -00:35:48.6
JGEM24595 13:49:41.25 -00:00:00.0
JGEM23057 13:38:26.25 +03:34:60.0
JGEM22032 13:32:48.75 +05:58:45.0
JGEM23314 13:41:15.00 +02:59:07.8
JGEM22289 13:35:37.50 +05:22:45.8
JGEM23570 13:44:03.75 +02:23:16.9
JGEM23827 13:46:52.50 +01:47:26.8
JGEM22545 13:38:26.25 +04:46:48.7
JGEM22802 13:41:15.00 +04:10:53.5
JGEM21777 13:35:37.50 +06:34:46.5
JGEM23058 13:44:03.75 +03:34:60.0
JGEM22033 13:38:26.25 +05:58:45.0
JGEM23315 13:46:52.50 +02:59:07.8
JGEM22290 13:41:15.00 +05:22:45.8
JGEM22546 13:44:03.75 +04:46:48.7
JGEM23835 14:31:52.50 +01:47:26.8
JGEM23578 14:29:03.75 +02:23:16.9
JGEM23322 14:26:15.00 +02:59:07.8
JGEM23323 14:31:52.50 +02:59:07.8
JGEM23066 14:29:03.75 +03:34:60.0
JGEM22810 14:26:15.00 +04:10:53.5
JGEM23067 14:34:41.25 +03:34:60.0
JGEM22811 14:31:52.50 +04:10:53.5
JGEM22298 14:26:15.00 +05:22:45.8
JGEM22554 14:29:03.75 +04:46:48.7
JGEM22555 14:34:41.25 +04:46:48.7
JGEM22042 14:29:03.75 +05:58:45.0
JGEM22299 14:31:52.50 +05:22:45.8
JGEM22813 14:43:07.50 +04:10:53.5
JGEM22557 14:45:56.25 +04:46:48.7
JGEM22301 14:43:07.50 +05:22:45.8
JGEM22044 14:40:18.75 +05:58:45.0
JGEM22302 14:48:45.00 +05:22:45.8
JGEM22045 14:45:56.25 +05:58:45.0
JGEM21789 14:43:07.50 +06:34:46.5
JGEM22303 14:54:22.50 +05:22:45.8
JGEM22046 14:51:33.75 +05:58:45.0
JGEM21790 14:48:45.00 +06:34:46.5
JGEM21791 14:54:22.50 +06:34:46.5

The LIGO Scientific Collaboration and the Virgo Collaboration report:

We have re-analyzed LIGO and Virgo data around the time of the compact
binary coalescence (CBC) candidate S190510g (GCN 24442
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 ). Parameter
estimation has been performed using LALInference [1] and a new sky map,
LALInference.fits.gz, distributed via GCN Notice, is available for
retrieval from the GraceDB event page:

https://gracedb.ligo.org/superevents/S190510g

For the LALInference.fits.gz skymap, the 90% credible region is 1166 deg2.
Marginalized over the whole sky, the a posteriori luminosity distance
estimate is 227 +/- 92 Mpc (a posteriori mean +/- standard deviation).
This is the preferred sky map at this time.

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)

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 (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 S190510g at 2019-05-10 02:59:39.292 UTC (GCN 24442
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 ).

At the trigger time of S190510g, the high-voltage of MAXI/GSC was off,
and it was turned on at T0+358 sec (=T0+6.0 min).
The first one-orbit (92 min) scan observation with GSC after the event
covered 91%
of the 90% credible region of the bayestar skymap from 03:05:37 to
04:15:54 UTC (T0+358 to T0+4575 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. 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 S190510g event using the 90% contour of the initial bayestar probability map provided by the GW interferometers (GCN#24442
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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 in https://www.cppm.in2p3.fr/~dornic/events_runo3/S190510g.png <https://www.cppm.in2p3.fr/~dornic/events_runo3/S190510g.png>. Considering the location probability provided by the LIGO/Virgo collaborations, there is a 58.7% 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 (2019-05-10 02:59:39 UT) and in the 90% contour of the S190510g event. The expected number of atmospheric background events in the region visible by ANTARES is 3.1e-4 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 2.2e-3 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.

Gergely D��lya and Peter Raffai (Eotvos Univ.) reports on behalf of the GLADE
team:

We have found 69,543 galaxies in the GLADE catalog [1,2], within the 90% GW
localization area (bayestar.fits.gz) reported by the LVC in GCN 24442
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 , and
within 269 +/- 108 Mpc distance limits.

The galaxies found can be accessed on the GLADE website (19.5 MB txt file;
please note that the order of galaxies in the list only follow the ordering
as the appear in GLADE):
http://glade.elte.hu/O3/S190510g_GLADE_90.txt

There are 12,813 galaxies within the 50% GW localization area and within
the same distance limits (3.6 kB txt file; please note that the order of
galaxies in the list only follow the ordering as the appear in GLADE):
http://glade.elte.hu/O3/S190510g_GLADE_50.txt

[1] D��lya, G., Galg��czi G., Dobos, L. et al., 2018 MNRAS, 479, 2374
[2] http://glade.elte.hu

Igor Andreoni (Caltech), Daniel A. Goldstein (Caltech), Michael Coughlin (Caltech), Mansi M. Kasliwal (Caltech), Peter E. Nugent (LBNL), Michael Medford (UC Berkeley), Shreya Anand (Caltech), Jennifer Barnes (Columbia), S. Bradley Cenko (NASA GSFC), Jeffrey Cooke (Swinburne), Jorge Mart��nez Palomera (UC Berkeley), Leo P. Singer (NASA GSFC), on behalf of the Global Relay of Observatories Watching Transients Happen (GROWTH) and ZTF collaborations:

On 2019-05-10 06:00:00 UT we started the follow-up of the gravitational wave trigger S190510g (LIGO Scientific Collaboration and the Virgo Collaboration, GCN #24442
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 ) with the Victor M. Blanco 4m Telescope at Cerro Tololo Inter-American Observatory, equipped with the Dark Energy Camera (DECam). An observational tiling for the event was automatically and optimally determined and triggered using the GROWTH Target of Opportunity marshal (Coughlin et al. 2019a, Kasliwal et al. 2019b). 

The data from this program are immediately public and we invite anyone interested to search the images for optical counterparts. We are searching the images in real time for optical counterpart candidates using an image subtraction pipeline written for this program.  

The images are available under proposal ID 2019A-0205 from the NOAO archive (archive.noao.edu). For any questions on the data or the observations, please contact the PIs of this program, Danny Goldstein and Igor Andreoni (danny@caltech.edu, andreoni@caltech.edu).

GROWTH and ZTF are worldwide collaborations comprising Caltech, USA; IPAC, USA, WIS, Israel; OKC, Sweden; JSI/UMd, USA; U Washington, USA; DESY, Germany; MOST, Taiwan; UW Milwaukee, USA; TTU, USA; LANL USA; Tokyo Tech, Japan; IIT-B, India; IIA, India; LJMU, UK and USyd, Australia. ZTF acknowledges the generous support of the NSF under AST MSIP Grant No 1440341. GROWTH acknowledges generous support of the NSF under PIRE Grant No 1545949. Alert distribution service provided by DIRAC@UW (Patterson et al. 2019). Alert filtering and follow-up co-ordination is being undertaken by the GROWTH marshal system (Kasliwal et al. 2019).

The LIGO Scientific Collaboration and the Virgo Collaboration report:


We identified the compact binary merger candidate S190510g during

real-time processing of data from LIGO Hanford Observatory (H1), LIGO

Livingston Observatory (L1), and Virgo Observatory (V1) at 2019-05-10

02:59:39.292 UTC (GPS time: 1241492397.292). The candidate was found

by the GstLAL [1] analysis pipeline.


S190510g is an event of interest because its false alarm rate, as

determined by the online analysis, is 8.4e-10 Hz, or about one in 37

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


https://gracedb.ligo.org/superevents/S190510g


The classification of the GW signal, in order of descending

probability, is BNS (98%), Terrestrial (2%), NSBH (<1%), BBH (<1%), or

MassGap (<1%).


Assuming the candidate is astrophysical in origin, there is strong

evidence for the lighter compact object having a mass < 3 solar masses

(HasNS: >99%). Using the masses and spins inferred from the signal,

there is strong evidence for matter outside the final compact object

(HasRemnant: >99%).


One skymap 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 an hour after the candidate


For the bayestar.fits.gz skymap, the 90% credible region is 3462 deg2.

Marginalized over the whole sky, the a posteriori luminosity distance

estimate is 269 +/- 108 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 S190510g. At the time of the trigger the HAWC
local zenith was oriented towards (RA, Dec) = (175.0 deg, 19.1 deg).
25% 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 15.3 deg to 45 deg for the area searched in this
analysis. The 5sigma detection sensitivity to a 1s (100s) burst in the
80-800GeV energy range goes from 1.2e-06 erg/cm^2 to 1.1e-04 erg/cm^2
(6.4e-06 erg/cm^2 to 5.0e-04 erg/cm^2), depending on the zenith
angle.

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

P. Veres (UAH)
reports on behalf of the Fermi-GBM Team and the GBM+LIGO/Virgo Working
Group:


At the time of S190510g, Fermi was passing through the South Atlantic
Anomaly therefore the GBM detectors were disabled.

We note that the Fermi-GBM trigger (190510120 / 579149538) that occurred
about 7 minutes prior to the LVC trigger is a long gamma-ray burst that is
unassociated with S190510g based on the preliminary bayestar map.

V. Lipunov, E. Gorbovskoy, V.Kornilov, D.Kuvshinov, N.Tyurina, P.Balanutsa,
A.Kuznetsov, V.V.Chazov, D. Vlasenko
(Lomonosov Moscow State University,
Sternberg Astronomical Institute, Moscow State University)

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

K. Ivanov, O. Gres, N.M. Budnev, S. Yazev, O. Chuvalaev, V. Poleshchuk
(Irkutsk State University)

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

R. Podesta, Carlos Lopez and F. Podesta
(Observatorio Astronomico Felix Aguilar (OAFA))

Hugo Levato and Carlos Saffe
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE))

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
(The Instituto de Astrofisica de Canarias)

D. Buckley, S. Potter, A. Kniazev, M. Kotze
(South African Astronomical Observatory)



MASTER-IAC robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Spain (IAC Teide Observatory) started inspect of the LIGO/Virgo S190510g errorbox  5366 sec after trigger time at 2019-05-10 04:29:05 UT, with upper limit up to  19.4 mag. The observations began at zenit distance = 82 deg. The sun  altitude  is -21.9 deg. 

MASTER-OAFA robotic telescope  located in Argentina (OAFA observatory of San Juan National University) started inspect of the LIGO/Virgo S190510g errorbox  5771 sec after trigger time at 2019-05-10 04:35:50 UT, with upper limit up to  19.5 mag. The observations began at zenit distance = 125 deg. The sun  altitude  is -76.4 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=10342

We obtain a following upper limits.  

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

    5456 | 2019-05-10 04:29:05 |          MASTER-IAC | ( 13h 40m 40.55s , - 3d 55m 12.32s) |   C |   180 | 18.0 |        
    5674 | 2019-05-10 04:32:42 |          MASTER-IAC | ( 13h 55m 09.10s , - 1d 55m 34.40s) |   C |   180 | 19.1 |        
    5861 | 2019-05-10 04:35:50 |         MASTER-OAFA | ( 13h 31m 14.55s , - 1d 53m 24.34s) |   C |   180 | 18.9 |        
    5904 | 2019-05-10 04:36:33 |          MASTER-IAC | ( 13h 55m 08.87s , - 1d 56m 01.81s) |   C |   180 | 19.4 |        
    6086 | 2019-05-10 04:39:34 |         MASTER-OAFA | ( 13h 30m 45.90s , + 0d  6m 18.43s) |   C |   180 | 19.2 |        
    6314 | 2019-05-10 04:43:22 |         MASTER-OAFA | ( 13h 46m 43.91s , + 0d  6m 21.28s) |   C |   180 | 19.5 |        
    6545 | 2019-05-10 04:47:13 |         MASTER-OAFA | ( 13h 31m 12.81s , - 1d 53m 49.56s) |   C |   180 | 19.3 |        
    6770 | 2019-05-10 04:50:58 |         MASTER-OAFA | ( 13h 39m 14.80s , - 1d 53m 52.77s) |   C |   180 | 19.4 |        
    7002 | 2019-05-10 04:54:50 |         MASTER-OAFA | ( 13h 30m 44.89s , + 0d  6m 29.70s) |   C |   180 | 19.3 |        
    7228 | 2019-05-10 04:58:36 |         MASTER-OAFA | ( 13h 38m 43.67s , + 0d  6m 26.15s) |   C |   180 | 19.5 |        
Filter C is a clear (unfiltred) band. 


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

The IceCube Collaboration (http://icecube.wisc.edu/) reports:

IceCube has performed a search for track-like muon neutrino events
consistent with the sky localization of S190510g-1-Preliminary in a time range of 1000
seconds centered on the alert event time (2019-05-10 02:51:19.292 UTC to 2019-05-10 03:07:59.292 UTC)
during which IceCube was collecting good quality data.
No track-like events are found in spatial coincidence with the 90% spatial containment of S190510g calculated from the map
circulated in the preliminary notice. 

IceCube's sensitivity to point sources within the location spanned by the 90% spatial containment of S190510g ranges from
0.029 to 0.806 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