\documentstyle[twoside,epsfig]{article}

\input ibvs2.sty
\input ibvst.sty

\begin{document}

\IBVShead{5270}{1 May 2002}

\IBVStitle{GSC\,1609.00690, a New Classical Cepheid}

\IBVSauth{Sorokin, P.$^1$; Antipin, S.$^2$; Samus, N.$^{2,3}$}

\IBVSinst{Moscow Astronomy Club, c/o Sternberg Astronomical
Institute, 13 Universitetskij Ave., Moscow 119992, Russia}

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

\IBVSinst{Institute of Astronomy, Russian Academy of Sciences, 48
Pyatnitskaya Str., Moscow 119017, Russia}

\IBVSabs{We report discovery and investigation of a new classical Cepheid}
\IBVSabs{on Moscow archive plates.}

\SIMBADobj{GSC 1609-00690}
\IBVStyp{ DCEP }
\IBVSkey{photometry}


\begintext

\IBVSTnam{GSC 1609.00690}

\IBVSTcoo{19\hr31\mm12\fsec0}{+19\deg01\arcm19\arcs}{J2000.0}

\IBVSTobs{40-cm astrograph in Crimea}

\IBVSTdet{Photoplate}

\IBVSTfil{None}

\IBVSTdateobs{1960-1993}

\IBVSTcomp{
 \begin{tabular}{lccc}
 \noalign{\smallskip} GSC or USNO-A2.0 & $\alpha$ (J2000) &
                      $\delta$ (J2000) & $B_{pg}$ \\
 \noalign{\smallskip}
 \hline
 \noalign{\smallskip}
1609.00518 & 19\hr31\mm14\fsec3 & +19\deg03\arcm35\arcs & 14\fmm78 \\
1609.00944 & 19\hr31\mm23\fsec0 & +18\deg59\arcm50\arcs & 15\fmm18 \\
1050.13998661 & 19\hr31\mm15\fsec0 & +18\deg59\arcm40\arcs & 16\fmm09 \\
1050.14001553 & 19\hr31\mm20\fsec0 & +18\deg59\arcm37\arcs & 16\fmm54 \\
 \noalign{\smallskip}
 \end{tabular}
}

\IBVSTchk{None}

\IBVSTsys{$B_{pg}$}{$B$-band standard sequence in NGC~6802 (Hoag
et al., 1961)}

\IBVSTdata{Upon request}

\IBVSTtyp{  DCEP  }

\IBVSTrem{ The new Cepheid was independently discovered by one of
us (S.A.); the log of the Sternberg Institute blink comparator
shows that, in the early 1980s, the star had been noticed by
E.~Kolevatykh (unpublished). We estimated the star by eye on 288
plates from Moscow archive, JD\,2437136--49104. It turned out to
be a classical Cepheid. Its light elements are:
$${\rm JD_{max}} = 2442599.47 + 6\fday 3236\times E.$$
The variability range is 15\fmm 1--16\fmm 4. ${\rm
Max-min}=0\fper3$. The phased light curve is presented in Figure~1.
The new variable is close to a known Cepheid, V354 Sge (Metzger
and Schechter, 1998), at $\alpha=19$\hr31\mm15\fsec5, $\delta=
+19$\deg00\arcm42\arcs (J2000). The latter Cepheid is, however,
much fainter and has a different period, $P=4\fday1643$. The two
Cepheids are not the same object beyond doubt.}

\IBVSTack{ This study was supported in part by the Russian
Foundation for Basic Research through grant No.~02-02-06569. We
acknowledge support from the Russian Federal Program ``Studies in
High-Priority Fields of Science''.}

\IBVSfig{6.5cm}{5270-f1.eps}{The phased light curve of the new
Cepheid. Uncertain estimates are shown as open circles.}


\references

Hoag, A.A., Johnson, H.L., Iriarte, B., Mitchell, R.I., Hallam, K.L.,
Sharpless, S., 1961, {\it Publ.\ of the US Naval Obs.}, {\bf Vol.\ XVII},
Part VII, Washington

Metzger, M.R., Schechter, P.L., 1998, {\it Astron. J.}, {\bf
116}, 469

\endreferences


\end{document}
