\documentclass[twoside]{article}
\usepackage{epsfig}

\input ibvs2.sty
\input ibvst.sty

\begin{document}

\IBVShead{5302}{2 August 2002}

\IBVStitle{V982 O\lowercase{ph} is a Dwarf Nova}

\IBVSauth{ANTIPIN, S.V.$^1$; SAMUS, N.N.$^{2,1}$}

\IBVSinst{Sternberg Astronomical Institute, 13, University Ave.,
Moscow 119992, Russia, \\
e-mail: antipin@sai.msu.ru}

\IBVSinst{Institute of Astronomy, Russian Academy of Sciences,
48, Pyatnitskaya Str., Moscow 119017, Russia, \\
e-mail: samus@sai.msu.ru}

\SIMBADobj{V982 Oph}
\IBVSkey{photometry}
\IBVStyp{ UG }
\IBVSabs{V982 Oph, an SR: star in the GCVS, is actually a dwarf nova.}

\begintext

\IBVSTnam{V982 Oph}

\IBVSTcoo{17\hr52\mm38\fsec49}{+07\deg33\arcm04\farcs4}{2000}

\IBVSTobs{Crimean Laboratory of the Sternberg Astronomical Institute, 40-cm
astrograph}

\IBVSTdet{Photoplate}

\IBVSTfil{None}

\IBVSTdateobs{1976--1990}

\IBVSTsys{$B_{pg}$}{The $B$-band photoelectric standard sequence
in NGC~6426 (S.Yu.~Shugarov, private communication)}.

\IBVSTdata{Upon request}

\IBVSTtyp{ UG }

\IBVSTrem{ The variable V982 Oph (S 4187) was discovered by
Hoffmeister (1949) who attributed it to Mira stars. A finding
chart was published by Hoffmeister (1957). G\"otz (1957) also
considers the star a long-period variable and reports one gradual
rise of its brightness, from 16.9 to 15.9 during
JD~2429785--2429845. The GCVS (4th edition) gives the type SR:
for the star. Kinnunen and Skiff (2000) suggest an identification
with the US Naval Observatory A2.0 catalog star at
17\hr52\mm36\fsec27, +7\deg32\arcm20\farcs9 (2000). This
identification was found wrong in the course of our systematic
check of identifications and positions for all GCVS stars in
Ophiuchus, according to the program announced in Samus {\it et
al.} (2002). Instead, we identify it with a blue star ($b-r=-0.6$
in the USNO A2.0 catalog). The coordinates given are from
the Guide Star Catalogue, Version 2.2.01. The finding chart,
based upon the POSS~I blue image from the USNOFS Image and
Catalogue Archive, is presented in Fig.~1. The star's brightness
estimates on the Moscow collection plates reveal beyond doubt
that it is a dwarf nova, changing its brightness between 15.3 and
(17.2$B$. The star is visible on 39 of the 223 plates. A total of
18 outbursts were observed between JD 2442812--2448092. Figure~2 shows
the light curve for two best-documented outbursts. A cycle value
of 31 to 36\day \ can be expected. The brightness rise observed by
G\"otz (1957) probably resulted from estimates belonging to 2 or
3 individual outbursts.}


\begin{table}
\centerline{{\bf Table 1.} The 18 detected outbursts of V982 Oph}
\begin{center}
\begin{tabular}{ccrccrccr}
No.& JD24...  & $B_{pg}$   & No. & JD24...  & $B_{pg}$   & No. & JD24...  & $B_{pg}$\\
\hline
\#1& 42870.546& $<17.2$&  \#6& 43332.356& 15.28  & \#12& 44428.350& 15.28  \\
   & 42871.574& $<16.4$&     &          &        &     &          &        \\
   & 42872.494& 15.63  &  \#7& 43391.277& $<16.4$& \#13& 44782.327& 15.49  \\
   & 42872.523& 15.58  &     & 43394.288& 15.54  &     & 44789.394& $<17.2$\\
   & 42872.553& 15.54  &     & 43395.262& 15.49  &     &          &        \\
   & 42873.568& 15.72  &     & 43399.256& 16.50  & \#14& 45137.428& 16.50  \\
   & 42874.531& 15.58  &     & 43400.250& 16.40  &     &          &        \\
   & 42874.564& 15.58  &     &          &        & \#15& 45915.327& 16.32  \\
   & 42875.531& 15.63  &  \#8& 43424.216& $<17.2$&     &          &        \\
   & 42876.499& 15.63  &     & 43425.241& 17.00  & \#16& 45941.312& 16.07  \\
   & 42876.531& 15.80  &     & 43426.226& 15.67  &     &          &        \\
   & 42876.562& 15.89  &     & 43428.211& 16.80  & \#17& 46591.462& 16.12  \\
   &          &        &     & 43429.214& $<16.4$&     & 46596.478& $<17.2$\\
\#2& 42982.309& 16.32  &     &          &        &     &          &        \\
   & 42983.341& $<16.4$&  \#9& 43717.297& 15.41  & \#18& 48090.305& 16.40  \\
   &          &        &     & 43718.347& 15.9:  &     & 48091.305& 16.80  \\
\#3& 43016.345& 15.54  &     &          &        &     & 48092.427& $<17.2$\\
   &          &        & \#10& 44043.431& $<17.2$ \\
\#4& 43243.437& 15.76  &     & 44050.409& 15.30   \\
   & 43249.546& 16.03  &     &          &         \\
   & 43253.517& $<16.4$& \#11& 44105.283& 16.16   \\
   &          &        &     & 44106.318& 16.07   \\
\#5& 43272.375& $<17.2$&     & 44107.290& 17.20   \\
   & 43277.523& 16.16  &     & 44110.301& $<16.4$ \\
   & 43279.448& $<17.2$&     & 44111.300& $<17.2$ \\
\end{tabular}
\end{center}
\end{table}
\bigskip


\IBVSTack{We are grateful for the financial support to the
Russian Foundation for Basic Research (grants 02-02-06569,
02-02-16069), to the Council of the program of support for
leading scientific schools of Russia (project 00-15-96627), and
to the Federal Scientific and Technological Program
``Astronomy''. This research has made use of the USNOFS Image and
Catalogue Archive operated by the United States Naval
Observatory, Flagstaff Station
({\tt http://www.nofs.navy.mil/data/fchpix/}).}

\IBVSfig{7cm}{5302-f1.eps}{The finding chart for V982 Oph (from
the blue POSS~I image retrieved from the UNSOFS Image and
Catalogue Archive).}
%IBVSfigKey{5302-f1.eps}{V982 Oph}{finding chart}

\IBVSfig{6.5cm}{5302-f2.eps}{The light curves for two outbursts of V982
Oph.}
%IBVSfigKey{5302-f2.eps}{V982 Oph}{light curve}

\newpage

\references

G\"otz, W., et al., 1957, {\it Ver\"off. Sternwarte Sonneberg}, {\bf 4}, 123, - G\"otz, W., p. 135.
%Original: G\"otz, W., 1957, {\it Ver\"off. Sternwarte Sonneberg}, {\bf 4}, 35
%Corrected: Tue May 31 16:59:12 MEST 2005

Hoffmeister, C., 1949, {\it Erg\"anzungshefte Astron. Nachr.}, {\bf 12}, Nr. 1

Hoffmeister, C., 1957, {\it Mitt. ver\"anderl. Sterne}, Nr. 2999

Kinnunen, T., Skiff, B.A., 2000, {\it IBVS}, No. 4897

Samus, N.N., Goranskii, V.P., Durlevich, O.V., Zharova, A.V.,
Kazarovets, E.V., Pastukhova, E.N., Hazen, M.L., Tsvetkova, T.M., 2002,
{\it Astronomy Letters}, {\bf 28}, 174

\endreferences


\end{document}
