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

\begin{document}

\IBVShead{5340}{18 November 2002}

\IBVStitle{A New Eclipsing Binary Near BL C\lowercase{am}}

\IBVSauth{YOUNG-BEOM, JEON$^{1}$; CHULHEE, KIM$^2$; HO, LEE$^3$}

\IBVSinst{Korea Astronomy Observatory, Daejon, 305-348, Korea; e-mail: ybjeon@boao.re.kr}
\IBVSinst{Dept of Earth Science Education, Chonbuk National University, Chonju, 561-706, Korea; \\e-mail: chkim@astro.chonbuk.ac.kr}
\IBVSinst{Dep. of Earth Science Education, Korea National University of Education, Choongbuk, 363-791, Korea}


\IBVStyp{ EB }
\IBVSkey{eclipsing binary, photometry}

\IBVSabs{We present observational results of a newly discovered}
\IBVSabs{eclipsing binary in the field of BL Cam.}


\begintext

\IBVSTnam{W1}

\IBVSTcoo{03$\hr$ 47$\mm$ 45$\fsec$03}{63$\deg$ 28$\arcm$ 25$\farcs$8}{2000.0}

\IBVSTobs{BOAO (Bohyunsan Optical Astronomy Observatory), 1.8m reflector \\(f/8, Cassegrain focus)}

\IBVSTdet{Thinned back illuminated SITe 2048$\times$2048 chip \ \ \ \ \ \ \ ($11\farcm6\times11\farcm6$)}

\IBVSTfil{$B$, $V$} 

\IBVSTdateobs{JD 2451871, 2451872, 2451874, 2452269$-$2452272 }

\IBVSTsys{Landolt 1992}

\IBVSTdata{From the IBVS website, as 5340-t1.txt}

\IBVSedata{5340-t1.txt}

\IBVSTtyp{ EB }

\IBVSEmin{
  W1 & 51871.186 & 0.001 & I & $V$ & 0.0000 & \\
     & 51872.163 & 0.001 & I & $V$ & $-$0.0015 & \\
     & 51874.122 & 0.001 & I & $V$ & +0.0005 & \\
     & 52272.375 & 0.005 & I & $V$ & $-$0.0013 & \\
}

\IBVSTrem{
Time-series BV CCD photometry was performed over five nights for W1 
from November 4, 2000 to December 28, 2001.
Using {\tt IRAF/CCDRED} package, we processed CCD images to correct 
overscan regions, trim
unreliable subsections, subtract bias frames and correct flat field images.
Instrumental magnitudes were obtained using the {\tt Point Spread Function}
fitting photometry routine in {\tt IRAF/DAOPHOT} package 
(Massey \& Davis, 1992).
We applied the ensemble normalisation technique (Gilliland \& Brown, 1988)
to standardise the instrumental magnitudes of all stars in the time-series CCD frames.
A new faint field eclipsing binary star ($\langle V\rangle =19.92$ mag, $\langle B\rangle -\langle V\rangle =0.84 $ mag) was discovered.\\
$O-C$ values were calculated according to the following ephemeris:
$${\rm Min\ I}\ =\ {\rm HJD}\ 2451871.186\ +\ 0.326171\times E.$$
The period is preliminary, similar solution as shown in Fig.~2 can be obtained with other periods in the 0.325-0.329 d period range. 
}


\references

Gilliland, R. L., Brown, T. M., 1988, {\it PASP}, {\bf 100}, 754

Landolt, A. U., 1992, {\it AJ}, {\bf 104}, 340

Massey, P., Davis, L. E. 1992, A User's Guide to Stellar CCD photometry with IRAF

\endreferences

\newpage

\IBVSfig{7.50cm}{5340-f1.eps}{Finding chart of the new variable star, W1 in the field of BL Cam.}

\IBVSfig{7.00cm}{5340-f2.eps}{Light curves of the new variable star, W1.}


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