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

\input ibvs2.sty

\begin{document}

\IBVShead{5450}{18 September 2003}

\IBVStitle{V597 Scorpii and its Neighbour: A Double Mira Star?}

\IBVSauth{Samus, N. N.$^1$; Hazen, M. L.$^2$}

\IBVSinst{Institute of Astronomy, Russian Academy of Sciences, 48,
Pyatnitskaya Str., Moscow 119017, Russia and Sternberg
Astronomical Institute, University of Moscow, 13, University
Ave., Moscow 119992, Russia\\
\indent [samus@sai.msu.ru]} %email

\IBVSinst{Harvard College Observatory, 60, Garden Str., 
Cambridge, MA, 02138 USA\\
\indent [mhazen@cfa.harvard.edu]} %email


\SIMBADobj{V597 Sco}
\GCVSobj{V0597 Sco}

\IBVStyp{ M }

\IBVSabs{We identify V597 Sco using Harvard archives. Two}
\IBVSabs{large-amplitude red variables are found in the star's}
\IBVSabs{position, forming a double star with a 10'' separation.}

\begintext

The variable star V597~Sco (HV~10835) was discovered by Swope
(1943) who had classified it as a Mira variable, with the light
elements ${\rm Max} = 2429460+216\day\times E$ and the photographic
range from 14\fmm5 to fainter than 17\fmm0, and published a
low-quality photographic chart. During our work on the new
version of the GCVS with improved coordinates (cf. Samus {\it et
al.}, 2002, 2003), we found two variable objects near the
published position of V597~Sco on images of the US Naval
Observatory Image and Catalogue Archive. The existing finding
chart did not permit us to decide which of the stars was the
original Harvard variable, so we had to identify HV~10835 using
the discoverer's notebooks and plates of the Harvard stacks.

The Figure shows the field of V597~Sco on two sky survey images
in red light, retrieved from the USNO Image and Catalogue
Archive. The variability of two stars is quite evident. Star~1
($R=10.7$, $V=15.66$ in the GSC2.2 catalog) is the original
V597~Sco = HV~10835. Star~2 ($R=16.85$, $V=17.06$) is the new
variable. Their coordinates, based upon the GSC2.2 catalog, are
the following.

\begin{center}
\begin{tabular}{ll}
V597 Sco = HV 10835 & 17\hr02\mm28\fsec44 \ --35\deg14\arcm47\farcs8 (2000.0)\\
New variable        & 17\hr02\mm28\fsec84 \ --35\deg14\arcm57\farcs1 (2000.0)\\
\end{tabular}
\end{center}

\medskip

Thus, the two variables are only about 10\arcs\ apart.

\IBVSfig{5cm}{5450-f1.eps}{The field of V597 Sco on two sky survey
images in red light from the USNO Image and Catalog Archive. Left
panel: epoch 1986.2847; right panel: epoch 1993.2991. North is on
top, east is to the left. The size of both images is $1'$ from
north to south.}

%%\IBVSfigKey{5450-f1.eps}{V597 Sco}{finding chart}

Note that, for the four red-light images (JD~2438559--2449097)
available in the USNO Image and Catalog Archive, the phases
computed with the light elements for V597~Sco from Swope (1943)
are in a narrow range (0.912--0.125), whereas both stars exhibit
strong variations of brightness (within 10.8--12.7~$R$ for
V597~Sco and 14.6--16.1~$R$ for the new variable, roughly
estimated using magnitudes of field stars from the GSC2.2
catalog). Thus, apparently the light elements are not quite valid
for either of the stars.

Both stars are bright in the near-infrared range: in the 2MASS
catalog, $K=5.943$ for V597~Sco and $K=5.348$ for the new
variable. The new variable is also present in the IRAS Point
Source Catalog (IRAS~16591--3510). Its colors make it a possible
carbon star candidate.

In our opinion, both stars are probable Miras. The star
associated with \\\mbox{IRAS~16591--3510} seems to be too faint for
Harvard plates, but it is not excluded that, near epochs of its
maximum, it could contaminate Swope's estimates for V597 Sco,
thus causing insufficient accuracy of the light elements in Swope
(1943) (or even leading to spurious elements).

\bigskip

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'',
the program ``Unstable Processes in Astronomy'' of the Presidium
of Russian Academy of Sciences, and the program of support for
leading scientific schools of Russia (grant NSh-389-2003-2). 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/}). Thanks are due to
Dr.~S.V.~Antipin for his assistance during the preparation of the
manuscript.



\references

Samus, N.N., Goranskii, V.P., Durlevich, O.V. {\it et al.}, 2002,
{\it Astronomy Letters}, {\bf 28}, 174

Samus, N.N., Goranskii, V.P., Durlevich, O.V. {\it et al.}, 2003,
{\it Astronomy Letters}, {\bf 29}, 468

Swope, H.H., 1943, {\it Harvard Obs. Ann.}, {\bf 109}, No.~9

\endreferences

\bigskip


\IBVSerratum{5422}

\begin{center}

Kazarovets, E.V., Kireeva, N.N., Samus, N.N., Durlevich. O.V.

The 77th Name-List of Variable Stars

\end{center}


The following corrections are needed to the list of identifications
(Table 2).

\begin{verbatim}
V1657 Aql: the USNO identification should be USNO-A2.0 900-17903132
LY Dra: the SAO identification should be SAO 018231
DU Lyn: the AFGL identification should be AFGL 1187
OX Vir: the SAO identification should be SAO 138579
\end{verbatim}

Thanks are due to Dr. F. Ochsenbein (Strasbourg) for turning our
attention to the mistakes.


\end{document}
