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\begin{document}
\IBVShead{4487}{4 June 1997}

\title{THE FIRST PHOTOELECTRIC OBSERVATIONS}
\vspace{-0.35in}
\title{FOR THE DOUBLE-MODE CEPHEID BD $-$10\degr 4669}

\begintext

Antipin (1997) recently analyzed photographic archival plates at the
Sternberg Astronomical Institute in Moscow and found that the star
BD\,$-$10\degr 4669 is a double-mode Cepheid with the elements:

\vspace{0.15in}
\centerline{fundamental:  Max JD$_{hel}$ = 2447733.42 + 4.84125 $\times$ E,}
\vskip 2mm
\centerline{first overtone: Max JD$_{hel}$ = 2441177.37 + 3.3853 $\times$ E.}
\vspace{0.15in}

\noindent
We observed the Cepheid photoelectrically at the South African Astronomical
Observatory in April-May 1997 using the 50-cm reflector. A total of 35 
$V(RI)_c$ measurements were obtained (Table 1), the accuracy
of the individual data being near $\pm 0\fm 01$ in all filters.
The elements cited above are used in Figures 1a and 1b for plotting our
new observations.
\vskip 3mm
\centerline{Table 1}
\vskip 1mm
\begin{center}
\begin{tabular}{cccccccc}
\hline
$JD_{hel}$&$V$&$(V-R)_c$&$(V-I)_c$&$JD_{hel}$&$V$&$(V-R)_c$&$(V-I)_c$\\
2450500+ & & & &2450500+ & & & \\
\hline
41.6167& 9.630&  .706& 1.412&   77.6427& 9.837&  .735& 1.474\\
68.5836& 9.798&  .743& 1.460&   78.5217& 9.720&  .721& 1.440\\
70.6007& 9.709&  .701& 1.412&   78.5880& 9.717&  .725& 1.443\\
72.4674& 9.848&  .743& 1.510&   78.6386& 9.721&  .720& 1.440\\
72.5547& 9.874&  .765& 1.517&   78.6450& 9.717&  .727& 1.440\\
73.4990&10.024&  .766& 1.542&   79.5696& 9.920&  .765& 1.516\\
73.5937&10.046&  .783& 1.546&   80.4662& 9.776&  .720& 1.450\\
73.6662&10.038&  .772& 1.549&   80.5775& 9.739&  .715& 1.434\\
74.5287& 9.683&  .702& 1.397&   80.6273& 9.722&  .707& 1.427\\
74.5901& 9.659&  .689& 1.388&   82.5589& 9.842&  .745& 1.494\\
75.4888& 9.662&  .690& 1.401&   82.6064& 9.886&  .753& 1.492\\
75.5739& 9.692&  .716& 1.434&   82.6545& 9.884&  .761& 1.511\\
75.6374& 9.698&  .703& 1.423&   83.5498&10.074&  .783& 1.553\\
76.5343& 9.902&  .735& 1.512&   83.6062&10.052&  .766& 1.541\\
76.6163& 9.915&  .763& 1.524&   84.5415& 9.638&  .685& 1.381\\
76.6528& 9.917&  .762& 1.520&   84.5977& 9.620&  .686& 1.375\\
77.5437& 9.865&  .739& 1.489&   84.6454& 9.593&  .662& 1.365\\
77.6024& 9.849&  .742& 1.479&          &      &      &      \\
\hline
\end{tabular}
\end{center}

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\centerline{2}
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\centerline{Figure 1}
\vskip 5mm

The research described here was supported in part by the Russian Foundation
of Basic Research and the State Science and Technology Program ``Astronomy"
to LNB and through NSERC Canada to DGT. We would also like to express
our gratitude to the administration of the SAAO for their allocation of a large
block of observing time.
\vskip 1cm

\beginauthors
\authorsrightcol
 L.N.~BERDNIKOV
 Sternberg Astronomical Institute
 13, Universitetskij prosp.
 Moscow 119899, Russia
\vskip 2mm
 D.G.~TURNER
 Saint Mary's University
 Halifax, Nova Scotia, B3H 3C3
 Canada
\endauthors

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Reference:

Antipin, S.V., 1997, {\it I.B.V.S.}, No.\,4485


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