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

\input ibvs2.sty
\input ibvst.sty


\begin{document}

\IBVShead{5328}{29 October 2002}

\IBVStitle{V928 and V929 Ophiuchi}

\IBVSauth{Pastukhova, E. N.$^{1}$; Samus, N. N.$^{1,2}$}

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

\IBVSinst{Sternberg Astronomical Institute, 13, University Ave.,
Moscow 119992, Russia}

\SIMBADobj{V928 Oph}
\SIMBADobj{V929 Oph}
\IBVSabs{From our new photographic study, we derive new types, different}
\IBVSabs{from those in the 4th edition of the GCVS, for V928 and V929 Oph.}


\begintext

\IBVSTnam{V928 Oph}

\IBVSTcoo{18\hr40\mm28\fsec93}{+12\deg04\arcm01\farcs4}{2000}

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

\IBVSTdet{Photoplate}

\IBVSTfil{None}

\IBVSTsys{$B_{\rm pg}$}{Calibrated using surrounding stars of the USNO A2.0
catalog}

\IBVSTdateobs{JD 2437023--2448414}

\IBVSTdata{Upon request}

\IBVSTtyp{ RRAB }

\IBVSTrem{V928~Oph (S 4338) was discovered by Hoffmeister
(1949) who attributed it to the long-period variable stars. His
finding was later confirmed by G\"otz (G\"otz and Wenzel, 1956)
who, on the base of about 150 photographic brightness estimates
(JD~2425688--2434253), attributed it to Miras, with a period
of 140\day\ and a photographic range from 13\fmm9 to fainter than
15\fmm5, and reported three times of maxima. The finding chart was
published by Hoffmeister (1957), it permits a reliable
identification with modern positional catalogs (Kinnunen and
Skiff, 2000), and the corresponding star is by no means red. 
Decades ago (Richter, 1965) it was noticed that the star's colour
was discrepant with its classification.
Our new estimates show that the star
is an RRAB variable varying between 14\fmm9 and 17\fmm0, with the
light elements Max~JD~Hel = 2445961.289 + 0\fday497511$\times E$.
The finding chart is shown in Fig.~1 (left panel), the light
curve is presented in Fig.~2.}


\IBVSTnam{V929 Oph}

\IBVSTcoo{18\hr40\mm56\fsec37}{+08\deg17\arcm50\farcs7}{2000}

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

\IBVSTdet{Photoplate}

\IBVSTfil{None}

\IBVSTsys{$B_{\rm pg}$}{Calibrated using surrounding stars of the
USNO A2.0 catalog}

\IBVSTdateobs{JD 2437023--2448414}

\IBVSTdata{Upon request}

\IBVSTtyp{ LB }

\IBVSTrem{V929~Oph (S 4339) was discovered by Hoffmeister
(1949). He could not determine a reliable variability type but
suspected that the star was an eclipsing binary. G\"otz and
Wenzel (1956) found the same type, with variations between
photographic magnitudes 15.0 and 15.6, and determined the light
elements; they considered the derived period value (2\fday3401)
uncertain because of too few observations. Four times of minima
were published. The finding chart was published by Hoffmeister
(1957), it permits a reliable identification with modern
positional catalogs (Kinnunen and Skiff, 2000). The star is red,
it is associated with the IRAS Point Source Catalog object
IRAS~18385+0814. Our first guess was that the two stars had been mixed
up by their Sonneberg investigators. However, neither V928 Oph
turned out to be eclipsing, nor V929 Oph is a Mira. Our study
reveals apparently irregular variations of V929 Oph between
14\fmm7 and 16\fmm2. The finding chart is presented in Fig.~1
(right panel) and a fragment of the light curve is shown in Fig.~3.
 The reason for the wrong classification of both
stars in Sonneberg publications remains unclear.}

\IBVSTack{The work of the GCVS team is supported, in part, by
grants from the Russian Foundation for Basic Research (grant 02-02-16069),
The Federal Scientific and Technological Program ``Astronomy'', and the
program of support for leading scientific schools of Russia
(00-15-96627). The Digitized Sky Survey images are provided by
the Hubble Space Telescope Science Institute under support from
grant NAG W-2166 of the USA Government. Thanks are due to
Dr.~S.V.~Antipin for his assistance during the preparation of the
manuscript.}

\vspace*{1cm}

\IBVSfig{8cm}{5328-f1.eps}{The finding charts for V928 Oph (left) and V929 Oph
(right). Both charts show $4\arcm\times4\arcm$ fields from the second Digitized
Sky Survey, in blue light for V928 Oph and in red light for V929 Oph.}
%\IBVSfigKey{5328-f1.eps}{V928 Oph ; V929 Oph}{finding chart}

\IBVSefigure{5328-f1a.eps}
\IBVSefigure{5328-f1b.eps}

\IBVSfig{8cm}{5328-f2.eps}{The light curve of V928 Oph, folded with the elements
presented above.}
%\IBVSfigKey{5328-f2.eps}{V928 Oph}{light curve}

\IBVSfig{8cm}{5328-f3.eps}{A fragment of the light curve of V929 Oph.}
%\IBVSfigKey{5328-f3.eps}{V929 Oph}{light curve}


\references

G\"otz, W., Wenzel, W., 1956, {\it Ver\"off. Sternw. Sonneberg}, {\bf 2}, 5

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

Hoffmeister, C., 1957, {\it Mitt. ver\"and. Sterne}, {\bf Nr. 303}

Kinnunen, T., Skiff, B.A., 2000, {\it IBVS}, No. 4905

Richter, G., 1965, {\it Astronomische Abhandlungen. Professor Dr. Cuno
Hoffmeister zum 70. Geburtstag gewidmet}, Leipzig: J.A.~Barth, {\bf S. 98}

\endreferences


\end{document}
