\documentstyle[twoside, ibvs2, ibvst, epsf]{article} 

\begin{document}

\IBVShead{5168}{12 September 2001}

\IBVStitle{GSC 0752.2349 is an Eclipsing Binary of W UM\lowercase{a} Type}

\IBVSauth{Bernhard, K.$^{1,5}$; Kiyota, S.$^{2}$; Lloyd, C.$^{3}$; Frank, P.$^{4,5}$}

\IBVSinst{A--4030 Linz, Austria, e-mail: kl.bernhard@aon.at}

\IBVSinst{Tsukuba, 305-0031 Japan, skiyota@nias.affrc.go.jp} %email


\IBVSinst{Space Science \& Technology Department, Rutherford Appleton Laboratory, 
Chilton, Didcot, \\ \indent Oxon.\ OX11 0QX, UK, e-mail: cl@astro1.bnsc.rl.ac.uk}

\IBVSinst{D--84149 Velden, Germany, e-mail: frank.velden@t-online.de}

\IBVSinst{Bundesdeutsche Arbeitsge\-mein\-schaft f\"{u}r Ver\"{a}nderliche
Sterne e.V. (BAV), Munsterdamm 90,\\ \indent D--12169~Berlin, Germany}

\SIMBADobj{GSC 0752-2349}

\begintext

\IBVSTnam{GSC 0752.2349}

\IBVSTcoo{06\hr58\mm10\fsec8}{$+10\deg13\arcm58\arcs$}{2000}

\IBVSTobs{S. Kiyota: Private observatory, 25-cm Schmidt--Cassegrain telescope;\\
K. Bernhard: Private observatory, 20-cm Schmidt--Cassegrain telescope;\\
P. Frank: Private observatory, 30-cm flat-field camera}

\IBVSTdet{S. Kiyota: Apogee AP-7 CCD camera;\\ 
& K. Bernhard: Starlight Xpress SX camera;\\ 
& P. Frank: OES-LcCCD11 camera}

\IBVSTfil{S. Kiyota: Johnson-Cousins $V$;\\ 
& K. Bernhard: none;\\ 
& P. Frank: none}

\IBVSTcomp{K. Bernhard: GSC 0752.2661, $V\approx12\fmm6$}

\IBVSTchk{K. Bernhard: GSC 0752.2295}

\IBVSTsysn

\IBVSTdata{Upon request}

\IBVSTtyp{  W UMa  }

\IBVSTrem{
The variability of GSC 0752.2349 has been found as part of a programme
to discover and classify new variables using CCD observations of
selected fields on the edge of the northern Milky Way, during a survey
phase in January-February 2000, for the programme see Bernhard \& Lloyd
2000.  Further observations were performed on 4 nights in March 2000
(S. Kiyota), on one night in April 2000 (P. Frank) and on 3 nights in
March-April 2000 (K. Bernhard).  This star has previously been referred
to as Brh V37 (Bernhard 2000).\\ The ephemeris was calculated using the
``Phase Dispersion Minimization'' method. The light curve, reduced with
the period given below, shows variations of a W UMa-type eclipsing
binary.
\belowdisplayskip-12pt
\begin{equation}
\begin{array}{r@{}r@{}l}
{\rm Min\,I = HJD~}2451621.072 & {} + 0\fday5263 & {} \times E. \\ 
 \pm 5 & \pm 3 \\ 
\end{array}
\end{equation}}

\IBVSTack{This research made use of the SIMBAD data base, operated by
the CDS at Strasbourg, France. }

\IBVSfig{10cm}{5168-f1.ps}{Differential light curve of GSC 0752.2349; filled triangles: K. Bernhard, filled circles: P. Frank, open circles: S. Kiyota}

\references

Bernhard, K., 2000, {\it vsnet-newvar}, No.\ 276,\\ 
http://www.kusastro.kyoto-u.ac.jp/vsnet/Mail/vsnet-newvar/msg00276.html 

Bernhard, K., Lloyd. C., 2000, {\it IBVS}, No.\ 4920

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