A. Pozanenko (IKI), S. Belkin (IKI, HSE), A. Volnova (IKI), A. Moskvitin
(SAO RAS), O. Burhonov (UBAI), V. Kim (FAI), M. Krugov (FAI), V.
Rumyantsev (CrAO), E. Klunko (ISTP), R. Ya. Inasaridze (AbAO), I. Reva
(FAI), P. Minaev (IKI), N. Pankov (HSE), Sh. Ehgamberdiev (UBAI) report
on behalf of GRB IKI FuN:
We observed the GRB 201015A (D'Elia et al., GCN 28632) with ZTSh 2.6m
telescope of CrAO observatory, AZT-33IK of Mondy observatory, AZT-20 of
Assy observatory, AS-32 of Abastumani observatory, Zeiss-1000 of SAO
RAS, AZT-22 of Maidanak observatory, and Zeiss-1000(E) of TSHAO.
The optical transient of GRB 201015A (Lipunov et al., GCN 28633; Kennea
et al., GCN 28635; Malesani et al., GCN 28637; Ackley et al., GCN 28639;
Hu et al., GCN 28645; Zhu et al., GCN 28653; Belkin et al., 28656;
Marshall et al., GCN 28662; Jelinek et al., GCN 28664; Belkin et al.,
GCN 28673; Grossan et al., GCN 28674; Rastinejad et al., GCN 28676; Zhu
et al., GCN 28677; Kumar et al., GCN 28680; Kumar et al., GCN 28681;
Moskvitin et al., GCN 28721) at redshift z=0.426 (de Ugarte Postigo et
al., GCN 28649; Izzo et al., GCN 28661) is not spatially resolved in
most of our images besides a few imaging in Maidanak observatory between
Oct. 26 - Nov. 6 when observations were carried out under good weather
conditions (FWHM = 0.8 - 0.9 arcsec). The finding chart of stacked image
obtained in Maidanak observatory on Oct. 26, Nov. 4 and Nov. 6 is
presented in the left panel of the Figure 1.
(In all of the stacked images in the Figure 1 we subtracted nearby stars
which positions are designated by white and green circles. The white
circles denote the stars presented in PS DR1 catalogue, and the green
circle denote the star is not presented in PS DR1. Stacked images of
Zeiss-1000 of SAO RAS observations on 32 days (central panel) and 47
days (right panel) are also presented in the Figure 1.)
Using the stacked image of Maidanak observations (left panel of the
Figure 1, an upper limit of the image is R=24.6) we obtained photometry
of the nearby stars. The photometry of the stars is used for flux
subtraction to obtain R-magnitudes of unresolved optical transient in
all of observations, and a light curve of the optical transient is
presented in Figure 2
The light curve is preliminary and represent the joint photometry of the
optical transient and a possible host galaxy.
The source raised on in the left panel of the Figure 1 (red circle)
coincides with an afterglow coordinates of GRB 201015A reported by NOT
observation (Malesani et al., GCN 28637). We suggest the object clearly
visible on Oct.26 - Nov.6 at the place of the afterglow is a supernova
associated with GRB 201015A. The light curve in the Figure 2 suggests
the supernova maximum between 12 and 20 days after GRB trigger. The
supernova identification rules out the GRB 201015A as a questionable
short burst with extended emission (Markwardt et al., GCN 28658) and
corroborates the GRB 201015A as a long duration burst (Minaev et al.,
GCN 28668). The afterglow in the first two days after the trigger can be
approximated by a power law with the index of -0.91 �� 0.03.
We apologize for late report due to delay of Maidanak data which is
critical for supernova identification.