=Paper=
{{Paper
|id=Vol-2523/paper22
|storemode=property
|title=
Search and Observations of Optical Counterparts for Events Registered by LIGO/Virgo Gravitational Wave
Detectors
|pdfUrl=https://ceur-ws.org/Vol-2523/paper22.pdf
|volume=Vol-2523
|authors=Elena Mazaeva,Alexei Pozanenko,Alina Volnova,Pavel Minaev,Sergey Belkin,Raguli Inasaridze,Evgeny Klunko,Anatoly Kusakin,Inna Reva,Vasily Rumyantsev,Artem Novichonok,Alexander Moskvitin,Gurgen Paronyan,Sergey Schmalz,Namkhai Tungalag
|dblpUrl=https://dblp.org/rec/conf/rcdl/MazaevaPVMBIKKR19
}}
==
Search and Observations of Optical Counterparts for Events Registered by LIGO/Virgo Gravitational Wave
Detectors
==
https://ceur-ws.org/Vol-2523/paper22.pdf
Search and Observations of Optical Counterparts
for Events Registered by LIGO/Virgo Gravitational
Wave Detectors
Elena Mazaeva1, Alexei Pozanenko1, Alina Volnova1, Pavel Minaev1, Sergey
Belkin1, Raguli Inasaridze2, Evgeny Klunko3, Anatoly Kusakin4, Inna Reva4, Vasilij
Rumyantsev5, Artem Novichonok6,7, Alexander Moskvitin7, Gurgen Paronyan8,
Sergey Schmalz6, and Namkhai Tungalag10
1Space Research Institute (IKI), 84/32 Profsoyuznaya Str, Moscow, Russia, 117997
2KharadzeAbastumani Astrophysical Observatory, Ilia State University, Tbilisi, 0162,
Georgia
3Institute of Solar Terrestrial Physics, Irkutsk, Russia, 664033
4Fesenkov Astrophysical Institute,
Almaty, 050020, Kazakhstan
5 Crimean Astrophysical Observatory, Nauchny, Crimea, Russia 298409
6Keldysh
Institute of Applied Mathematics, Russian Academy of Sciences, Miusskaya 4,
Moscow, Russia, 125047
7Petrozavodsk State University, Leninast., 33, Petrozavodsk, Russia, 185910
8 Special Astrophysical Observatory of Russian Academy of Sciences, Nizhniy Arkhyz, Russia,
369167
9Byurakan Astrophysical Observatory, 0213, Byurakan, Aragatzotn Province, Republic
of Armenia
10Institute of Astronomy and Geophysics, Mongolian Academy of Sciences, 13343,
Ulaanbaatar, Mongolia
elena.mazaeva@phystech.edu
Abstract. The problem of search for optical counterpart of LIGO/Virgo events
are discussing. Multi-messenger astronomy boosts the use a huge amount of as-
tronomical data obtained by virtually all observatories around the world. We are
discussing different methods used for observations, problem of search for transi-
ents in the extremely large localization error-box of LIGO/Virgo events, and les-
sons obtained during second observational run of LIGO/Virgo in 2017. In partic-
ular we present our experience and results of follow up observations of
LIGO/Virgo optical counterpart candidates.
Keywords: Multi-messenger astronomy, gravitational waves, LIGO/Virgo,
gamma-ray bursts, afterglow, kilonova, photometry.
1 Introduction
The problem of search and observations of new transient objects is one of the main
problems in modern astrophysics. It requires wide-field observations with some initial
all-sky catalogue of stationary sources for comparison. Dedicated surveys and experi-
Copyright © 2019 for this paper by its authors. Use permitted under Creative
Commons License Attribution 4.0 International (CC BY 4.0).
229
ments produce huge amounts of data daily in every domain of electromagnetic spec-
trum: in high energy range [1], optics [2, 3], and radio [4], as well as in cosmic particles
window [5] and gravitational waves [6]. The surveys of new generation, like Large
Synoptic Survey Telescope [7], will produce data of unprecedented volume and com-
plexity. Reduction and analysis of these enormous data sets is already out of human’s
capacity and is similar to a search of a needle in a haystack. This problem is also con-
nected to the search of transients related to the gravitational waves detections in very
large localization areas, provided by LIGO and Virgo observations during theirs third
scientific observational run in 2019.
The Laser Interferometer Gravitational-Wave Observatory (LIGO) is designed to
open the field of gravitational-wave astrophysics through the direct detection of gravi-
tational waves predicted by Einstein’s General Theory of Relativity [8]. LIGO’s multi-
kilometer-scale gravitational wave detectors use laser interferometry to measure the
minute ripples in space-time caused by passing gravitational waves from cataclysmic
cosmic events such as merging neutron stars (NSs) or black holes (BHs), or by super-
novae. LIGO consists of two widely separated interferometers within the United States
– one in Hanford, Washington and the other in Livingston, Louisiana – operated in
unison to detect gravitational waves.
The first success of LIGO observations came in 2015 with the first direct observa-
tions of gravitational waves from the binary black hole merging GW150914 [9]. In
2017, when the sensitivity of LIGO detectors increased, and Virgo detector in Italy
started its first observational cycle [10], the merging of binary neutron star was detected
for the first time [11].
In the context of gravitational waves detection, the most important problem for as-
trophysics is the search, identification, and observations of the possible electromagnetic
(EM) counterpart of the event. The General Relativity predicts no EM radiation from
the binary BH coalescence since, in theory, there is no enough matter outer the source
that can produce it. In practice, there may be some radiation caused by accretion of a
circumstellar matter on the resulting black hole, but its predicted flux is extremely low
(e.g. [12]). Quite different situation is the binary NS merging (BNS). In this case, the
merging objects consist of an ordinary matter that may produce high-energy EM radi-
ation process (short gamma-ray burst) after the merging BNS an afterglow of wide en-
ergy range, and most interesting BSN counterpart which is called ‘kilonova’.
The association between BNS merging, short gamma-ray bursts and kilonovae was
first predicted theoretically [13], and then was confirmed observationally with the de-
tection of GW170817/ GRB 170817A / AT2017gfo [14]. Besides the fact that
GW170817 was the first case of the registration of gravitational waves from a BNS
merging, it was also the first detection of gravitational waves and EM radiation from
the same source [15].
A signal from the binary system merging is modeled numerically based on the Ein-
stein’s General Theory of Relativity and represents a package of oscillations increasing
in amplitude with a decreasing period. The processing algorithm of LIGO and Virgo
detectors searches for modeled templates in the received data using wavelet analysis.
Localization on the sky is performed by triangulation method, measuring the time lag
between the detection time for spatially distributed detectors, which determines the sky
230
area of the most probable localization of the source. The time of the signal registration
is measured with a high accuracy; however, the localization area may be very large,
tens to hundreds of square degrees (see Table 1). GW170817 [16] has a localization
region of ~30 square degrees, and there were reported ~190 galaxies in the volume
limited by the sky area and distance estimates [17]. The kilonova AT2017gfo was dis-
covered independently by 6 survey projects and was observed during several dozens of
days in wide energy range from X-rays to radio [18]. The co-authors of the paper were
used the mosaic method to search for optical counterpart, observed of kilonova and
proposed the model of prompt emission of GW170817/GRB 170817A [19].
In this paper, we discuss the problem of the search of a new transient optical source
in large areas provided by detections of gravitational wave sources. We describe two
basic methods of the search: mosaic observations of localization area and pre-deter-
mined goals observations, i.e. search for transients in galaxies inside the detection vol-
ume. We also provide several examples of such semi-manual searches using available
ground-based optical telescopes performed during the LIGO/Virgo observational run
O2. Multi-messenger Astronomy is becoming a commonplace [20].
Table 1. Selected source parameters of the eleven confident GW detections [21]
Event Type a d L /Mpcb ΔΩ=deg2c
GW150914 BBH 430 (+150/-170) 180
GW151012 BBH 1060 (+540/-480) 1555
GW151226 BBH 440 (+180/-190) 1033
GW170104 BBH 960 (+430/-410) 924
GW170608 BBH 320 (+120/-110) 396
GW170729 BBH 2750 (+1350/-1320) 1033
GW170809 BBH 990 (+320/-380) 340
GW170814 BBH 580 (+160/-210) 87
GW170817 BNS 40 (+10/-10) 16
GW170818 BBH 1020 (+430/-360) 39
GW170823 BBH 1850 (+840/-840) 1651
a BBH – binary black holes. BNS – binary neutron stars.
b Luminosity distance.
c Error box of sky localization.
2 The Optical Transient Search Procedure
After receiving the alert signal from LIGO/Virgo, our observations are carried out on
ground-based optical telescopes to search for counterpart.
One can observe the whole range of localization with wide-field telescopes. This
observation tactic is suitable if the localization area is not very large (up to about one
hundred square degrees), or it is possible to observe on a large number of telescopes.
231
Since we know not only the localization region in the celestial sphere of the gravita-
tional-wave event, but also the distance to the source, we can only observe galaxies
from the localization region that are located at a given distance. For this purpose, there
is a value-added full-sky catalogue of galaxies, named as Galaxy List for the Advanced
Detector Era, or GLADE [22]. GLADE was constructed by cross-matching and com-
bining data from five separate (but not independent) astronomical catalogues: GWGC,
2MPZ, 2MASS XSC, HyperLEDA, and SDSS-DR12Q. But GLADE is complete up
only to d L =37(+3/-4) Mpc in terms of the cumulative B-band luminosity of galaxies
within luminosity distance d L , and contains all of the brightest galaxies giving half of
the total B-band luminosity up to d L =91 Mpc. While the distance to the registered
source can be several thousand Mpc (see Table 1).
But whatever method we use, we need to find a transient on the obtained optical
images.
We use the method of comparison with all-sky catalogs using the generated catalog
of sources selected from the image. A block diagram of the method is presented in
Fig. 2.
Fig. 1. A block diagram of the match algorithm
Block 1 – detection, measure and classification of sources from astronomical images,
the formation of an object catalog. In this case, we used SExtractor – software for source
extraction [23]. Comparison of object catalogs is best done using equatorial coordinates
of objects; first of all, astrometry is necessary (for example, using Apex [24] or other
software). To avoid incorrect comparison, it is useful to reject objects at the border of
232
a frame that do not fully fit into the frame (either at a distance of < 4 FWHM from the
border or to use the value of the SExtractor flags).
Block 2 – formation of the catalog of the comparison stars. For comparison of objects
it is better to use photometric catalogs (e.g. SDSS, Pan-STARRS, APASS, 2MASS, it
depends on the filter of the original image, the image upper limit and the region of the
celestial sphere).
Block 3 – search for transient sources.Comparison of objects is performed simulta-
neously by equatorial coordinates and magnitude within the measurement error.
3 Results Obtained for our Procedures of Search
and Identification
Our collaboration is based at the Space Research Institute and provided follow-up grav-
itational wave observations in the optical range during Second Observing Run of
LIGO/Virgo.
The optical data were obtained by IKI GRB Follow-up Network which is collabo-
rating with Crimean Astrophysical Observatory (CrAO), Sayan Solar Observatory
(Mondy), Tian Shan Astrophysical Observatory (TShAO), Abastumani Astrophysical
Observatory (AbAO), Special Astrophysical Observatory (SAO), ISON-Khureltogoot,
Koshka observatory of INASAN and Byurakan Astrophysical Observatory (BAO).
3.1 LIGO/Virgo G299232: Compact Binary Coalescence Candidate
GW170825 G299232is a low-significance compact binary coalescence candidate iden-
tified from LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1)
at 2017-08-25 13:13:31 UTC. If the candidate is astrophysical in origin, it appears con-
sistent with the merger of a black hole and a neutron star [25]. Subsequently, the event
was not confirmed.
Localization generated by the BAYESTAR pipeline [26] including information from
H1, L1, and V1 is presented in Fig. 1. The 90% credible region spans about 2040 deg2.
The a posteriori luminosity distance estimate is 339 +/-110 Mpc [25].
The IceCube Neutrino Observatory (a cubic-kilometer neutrino detector operating at
the geographic South Pole, Antarctica) searched IceCube online track-like neutrino
candidates (GFU) detected in a [-500,500] second interval about the LIGO/Virgo trig-
ger G299232 [27]. Comparison of the candidate source directions of 7 temporally-co-
incident neutrinos to the BAYESTAR skymap is presented in Fig. 2.
One of the neutrino candidate (marked as X1) was within the LIGO/Virgo localiza-
tion area and detected 233.82 seconds before LIGO/Virgo trigger G299232.X1 sky lo-
cation is R.A.=28.2, Dec.=44.8 with 3.8 degrees uncertainty of direction reconstruction
[28].
233
Fig. 2. The localization with distance information generated by the BAYESTAR pipeline [26]
including information from H1, L1, and V1.X1 - X7 are neutrino candidates (GFU) detected in
a [–500,500] second interval about the LIGO-Virgo trigger G299232
We observed the field of LIGO/Virgo trigger G299232 [25] and error circle of
IceCube candidate X1 [27, 28] with wide field of view VT-78a telescope of ISON-
Khureltogoot observatory. We obtained several unfiltered images with the two time
series starting on 2017-08-25 (UT) 15:24:13 and 16:32:52 (time since LVC trigger are
0.11289 and 0.16054 days), each centered to the position of localization reported in
[27] and [28], respectively. Total coverage of the error region of IceCube candidate X1
[28] is 85.7 %. The map of the coverage can be found in Fig. 3.
Using the algorithm described in Chapter 3 we have distinguished 94.7 thousand
objects from the images (field of view is 7 x 7 degrees). After comparing these 94.7
thousand objects with the USNO-B.1 catalog we have 834 candidates left, of which 818
are processing artifacts. Finally, we found one cataloged asteroid (895) Helio and 24
objects, the magnitude of which was brighter than R2 of USNO-B1.0, but weaker than
R1 (see Table 1). There is no presented R-magnitude for the object 1352-0033439 in
USNO-B1.0 catalog, but magnitudes B1=18.27, B2=15.32 and I=13.87 for the object
1352-0033439 are presented in catalog and correspond to our photometric magnitude
(column name is “Mag SExtractor” in Table 2).
We found no significant variability of the sources between the two epochs. We found
no significant brighter sources, which could be galaxies, than their R-magnitudes pre-
sented in the USNO-B.1 catalog. Upper limit on the stellar magnitude of possible opti-
cal candidate is 19.2.
234
Fig. 3. The map of the coverage IceCube candidate X1 localization by VT-78a telescope of
Khureltogoot observatory. Red circle is preliminary IceCube X1 error box [27], blue circle is
final error box [28]
Fig. 4. Sky localization of LIGO/Virgo events. a – GW170104_G268556,
b – GW170120_G270580, c – GW170217_G274296, d – GW170227_G275697,
e – GW170313_G277583, f – GW170608_G288732, g – GW170817_G298048,
h – GW170823_G298936, i – GW170825_G299232
235
Table 2. List of object which magnitudes are brighter than R2 of USNO-B1.0
USNO-B1.0 id R1 R2 Mag SExtractor
1377-0046508 13.51 16.26 14.22
1377-0046571 15.49 18.48 16.41
1377-0046983 14.23 20.16 14.80
1378-0048129 11.44 14.42 12.40
1378-0048633 15.51 18.38 16.20
1378-0048730 13.89 16.87 14.49
1377-0048562 15.79 19.76 16.48
1377-0048684 13.69 16.37 14.34
1376-0047873 14.53 18.27 15.06
1372-0048226 15.56 19.83 16.30
1355-0039997 14.13 17.78 14.92
1352-0033439 - - 16.46
1327-0048518 13.94 18.19 14.11
1328-0048333 14.47 17.22 14.87
1327-0048405 15.19 20.70 15.79
1328-0048274 13.14 15.59 13.31
1324-0046318 19.27 - 15.76
1327-0038107 12.93 19.03 13.68
1327-0038122 15.42 20.47 16.24
1328-0038377 11.94 15.03 12.66
1328-0038222 12.87 18.22 13.66
1328-0038148 12.68 19.20 13.61
1328-0038142 14.50 20.47 15.29
1328-0038084 14.11 18.98 14.92
3.2 Observations of LIGO/Virgo Optical Candidates
In addition to searching the object in the localization area, we also observed objects in
the localization area of GW events that were found by other research groups.
The objects that we have observed are listed in the Table 3, the areas of localization
of each gravitational-wave event can be seen in the Fig. 4. Some gravitational-wave
events, the areas of which we observed, later were not officially confirmed and continue
remained candidates.
236
Table 3. Observations of optical candidates of LIGO/Virgo events
Event Type a Optical candidates Typeb
GW170104_G268556 CBC (+) [29] PS17fn n/c
PS17fl n/c
PS17dp n/c
PS17gl n/c
GW170120_G270580 n/c (-) [30] PS17yt SN Ia
MASTER OT
J090737.22+611200.5 n/c
PS17lk n/c
PS17nv n/c
PS17pv n/c
PS17qk n/c
PS17rc n/c
GW170217_G274296 n/c (-) [31] PS17bek SLSN
GW170227_G275697 CBC (-) [32] iPTF17bue SN Ia
XRT23 n/c
GW170313_G277583 n/c (-) [33] ATLAS17cgg SN IIn
GW170608_G288732 BBH (+) [21] GW170608X2 n/c
GW170817_G298048 BNS (+) [21] GW 170817 GRB, KN
GW170823_G298936 BBH (+)[21] GWFUNC-17ure SN Ia
GW170825_G299232 NS+BH (-) [34] SwiftJ014008.5+343403.6 n/c
MASTER OT SN IIb
a BBH – binary black holes merging, BNS – binary neutron stars merging, NS+BH – neutron star
and black hole merging, CBC – compact binary coalescence, n/c – this event candidate does
*not* have a chirp signature, and thus does not suggest a compact binary merger or the morphol-
ogy of the event candidate is unclear. (+) – event, (-) – candidate.
b SN – supernova, KN – kilonova, SLSN – super-luminous supernova, GRB – gamma-ray burst,
n/c – non classified.
237
GW170120_G270580. The Pan-STARRS covered northern area of the
GW170120_G270580 localization and detected 124 transients including rapidly rising
transient – PS17yt (R.A. 10:03:57.96 Dec. +49:02:28.3) [35,36]. Our collaboration ob-
served PS17yt source in BVR filters and a light curve of PS17yt were constructed (see
Fig. 5a). It was subsequently shown that PS17yt is Ia type supernova at a redshift z ~
0.026 [37].
Furthermore, we observed orphan sources PS17lk (R.A. 09:29:58.27 Dec.
+15:11:58.5), PS17nv (R.A. 09:57:41.01 Dec. +17:49:33.4), PS17qk (R.A. 09:29:12.15
Dec. +25:49:06.4), PS17pv (R.A. 09:25:07.35 Dec. +50:12:28.9), PS17rc (R.A.
09:32:19.16 Dec. +47:03:38.3) and MASTER J090737.22+611200.5 (R.A.
09:07:37.22 Dec. +61:12:00.5) in the field of the LIGO G270580 localizations. Results
of observations see in Table 4.
GW170217_G274296. Pan-STARRS covered 501 square degrees on the first night
following the release of the G274296 alert. They have located and vetted 10 transients
with host spectroscopic redshifts and 60 unknown transients with no host spectroscopic
redshifts. [38] We observed one of the transients with no host spectroscopic redshifts
(PS17bek) and the light curves in BR-filters are presented in Fig. 5b.
Afterwards a good correlation betweenPS17bek spectrum and the spectra of super-
luminous supernovae (SLSNe type I) was found. In particular, a good match with the
spectra of SN 2010gx at -5 days before peak if PS17bek is at a redshift of z~0.31 was
found. The weak emission line at 6559.4 is consistent with [O III] 5007 at z=0.31, and
we also detect [O III] 4959 at a consistent redshift but lower significance [39].
GW170825_G299232. Global MASTER robotic net discovered optical transient
source – MASTER OT J033744.97+723159.0(R.A. 03:37:44.97 Dec. +72:31:59.0).
[40]. Analysis of the MASTER spectrum suggests that it is a supernova Type IIb [41]
MASTER OT observation with the RoboPolpolarimeter shown that the R-band frac-
tional polarization of the source is 1.8+/–0.47% [42].
Our observations of the MASTER OT are shown in the Fig. 5c.
4 Summary
In 2017, coordinated hardworking of thousands of astronomers and other scientists
around the world allowed to find and successfully observe the electromagnetic coun-
terpart of the gravitational wave event GW170817 of binary neutron star merging. The
associated GRB 170817A and kilonova AT2017gfo were observed by hundreds of
space and ground-based experiments in all ranges of electromagnetic spectrum. The
unprecedented collaboration allowed to obtain detailed properties of kilonova and to
verify existing physical models of this phenomenon, which is not fully studied yet. At
the same time, there was no any reliable EM counterpart candidate detected for 10 bi-
nary black holes coalescences discovered during O1/O2 scientific runs of LIGO and
Virgo detectors. However, a huge amount of observational data, which covered vast
localization area of the events, led to the discovery of many other new transient sources
unrelated to the GW. The problem of search of a new optical transient with specific
properties in large localization areas arose here with the great actuality.
238
Table 4. The photometric observation results of orphan sources
Orphan Date Filter MJD Magnitude
PS17lk 2017-01-25 R 57778.72969 20.92 +/– 0.16
2017-01-29 R 57782.74483 > 22.5
2017-01-30 R 57783.70939 21.10 +/– 0.11
2017-01-31 R 57784.69874 21.22 +/– 0.12
2017-02-07 R 57791.93095 21.60 +/– 0.40
2017-02-18 R 57802.73167 21.89 +/– 0.24
PS17pv 2017-01-25 R 57778.82847 >20.5
2017-01-28 R 57781.86958 >22.4
2017-01-30 R 57783.80134 20.74 +/- 0.11
PS17nv 2017-01-25 R 57778.74557 >22.2
2017-01-27 R 57780.82339 >22.2
2017-01-31 R 57784.03700 >23.4
PS17qk 2017-01-25 R 57778.77275 21.01 +/– 0.12
2017-01-29 R 57782.78859 20.61 +/– 0.11
2017-01-30 R 57783.74301 20.46 +/– 0.06
2017-01-31 R 57784.73083 20.36 +/– 0.05
2017-01-31 R 57784.84479 20.50 +/– 0.03
2017-01-31 B 57784.85668 20.87 +/– 0.04
2017-02-01 R 57785.77138 20.17 +/– 0.05
2017-02-18 R 57802.75716 20.55 +/– 0.07
2017-03-06 CR 57818.86623 20.53 +/– 0.09
PS17rc 2017-01-25 R 57778.81470 20.96 +/– 0.15
2017-01-30 R 57783.77229 21.04 +/– 0.10
2017-01-31 R 57784.76358 21.13 +/– 0.11
2017-01-31 R 57784.88885 21.28 +/– 0.05
2017-01-31 R 57784.87345 23.57 +/– 0.24
2017-02-01 R 57785.80742 21.28 +/– 0.09
MASTER OT 2017-01-21 R 57774.62327 19.07 +/– 0.01
J090737.22+611200.5 2017-01-22 R 57775.64491 19.10 +/– 0.02
2017-01-23 R 57776.63227 19.18 +/– 0.03
239
Fig. 5. a – light curves of PS17yt (GW170120_G270580 optical candidate), b – light curves
of PS17bek (GW170217_G274296 optical candidate), c – light curves of MASTER-OT
(GW170825_G299232 optical candidate). Red points are R-band, blue points are B-band and
green points are V-band. Observations were obtained by TShAO (Zeiss-1000), CrAO (ZTSh –
2.6m), Mondy (AZT-33IK), AAO (AS-32), BAO (ZTA 2.6-m), Simeiz/Koshka (Zeiss-1000).
Host galaxy is not subtracted
240
We discussed the two main methods of the search for optical transients in the areas
of tens and hundreds of square degrees: mosaic surveys and observations of pre-defined
targets (potential host galaxies). The case of mosaic surveys is suitable for small-aper-
ture telescopes with wide fields of view, with rather low optical upper limit, though.
The search of the transient inside pre-defined target galaxies requires deeper limits and
thus require observations with large-aperture telescopes with >1 meter diameter. The
second case involves compiled catalogues of galaxies with known distance like Galaxy
List for the Advanced Detector Era (GLADE) [22]. This fact increases the actuality of
deep surveys of galaxies with measured distances. These methods are suitable not only
for the search of the EM counterpart of gravitational waves events detected by
LIGO/Virgo, but also for the search of optical counterparts of ordinary GRBs with large
localization region (e.g., from GBM/Fermi experiment).
We also provided results of the observations of localization regions of candidates for
real GW events detected with LIGO/Virgo during their second scientific run O2. We
did not find any optical transients with our facilities; however, we conducted a follow-
up of transients discovered by other teams worldwide. This valuable experience is now
being adapted for the third scientific run O3 of LIGO/Virgo, which started on April 1,
2019 and would continue for 1 year. Nevertheless, the problem of automatization of the
data processing algorithms remains unsolved for all cases and requires the development
of new conceptual approach, and generalized pipelines for data reduction are required.
Almost all space and ground-based astronomical facilities are now involved in the
follow-up of GW events. This makes multi-messenger astronomy a commonplace now-
adays. Quick availability of new obtained data and vast collaboration of observatories
and observers may guarantee further success.
Acknowledgments
Authors are grateful for a partial financial support to the grants RFBR 17-51-44018,
17-02-01388 and 19-42-910014 provided jointly by RFBF and the Republic of
Crimea.
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