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

\begin{document}
\IBVShead{5189}{19 October 2001}

\IBVStitletl{New W UM\lowercase{a} Type Eclipsing Binaries}{ in the Globular Cluster M15}

\IBVSauth{Jeon, Young-Beom$^{1,3}$; Lee, Ho$^2$; Kim, Seung-Lee$^1$; Lee, Myung Gyoon$^3$}

\IBVSinst{Korea Astronomy Observatory, Taejon, 305-348, Korea}
\IBVSinst{Dept.\ of Earth Science Education, Korea National University of Education, Choongbuk, 363-791, Korea}
\IBVSinst{Astronomy Program, SEES, Seoul National University, Seoul, 151-742, Korea}

\SIMBADobj{M 15}
\IBVStyp{ W UMa }
\IBVSkey{W UMa type star, photometry}
\IBVSabs{We present observational results of two newly discovered W UMa type stars}
\IBVSabs{in the globular cluster M15.}

\begintext

{\bf VAR 1}
\hrule

\IBVSTnam{W1}

\IBVSTcoo{21\hr30\mm21\fsec06}{+12\deg9\arcm9\farcs3}{2000}

{\bf VAR 2}
\hrule

\IBVSTnam{W2}

\IBVSTcoo{21\hr29\mm52\fsec25}{+12\deg 6\arcm 11\farcs2}{2000}

\hrule

\IBVSTobs{BOAO (Bohyunsan Optical Astronomy Observatory), 1.8-m reflector ($f/8$, Casse\-grain focus)}

\IBVSTdet{Thinned back illuminated SITe $2048\times2048$ chip ($11\farcm6\times11\farcm6$)}

\IBVSTfil{$B$, $V$} 

\IBVSTdata{Through IBVS Web-site as files 5189-t1.txt, 5189-t2.txt, 5189-t3.txt, and 5189-t4.txt}
\IBVSedata{5189-t1.txt}
\IBVSedata{5189-t2.txt}
\IBVSedata{5189-t3.txt}
\IBVSedata{5189-t4.txt}

\IBVSTsys{Landolt (1992)}

\IBVSTtyp{ W UMa }

\IBVSTrem{
Time-series $BV$ CCD photometry was performed over  three nights for W1
and nine nights for W2 from 1997 to 2000.  Using 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 Point Spread Function
fitting photometry routine in IRAF/DAOPHOT package (Massey \& Davis
1992).  We applied the ensemble normalization technique (Gilliland \&
Brown 1988, Jeon {\it et al.}\ 2001) to standardize the instrumental
magnitudes of all stars in the time-series CCD frames.  Two new faint
($\langle V\rangle=20\fmm246$, $\langle B\rangle-\langle
V\rangle=1\fmm014$ \& $P=0\fday23306$ for W1; $\langle
V\rangle=19\fmm791$, $\langle B\rangle-\langle V\rangle=0\fmm560$ \&
$P=0\fday23576$ for W2) W UMa type stars in globular cluster M15 were
discovered.}

\IBVSfig{8.5cm}{5189-f1.ps}{Finding chart of the two W UMa type
variable stars, W1 and W2, in globular cluster M15}

\clearpage

\IBVSfig{10cm}{5189-f2.ps}{Light curves of the two W UMa type stars}

\references

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

Jeon, Y-.B., Kim, S-.L., Lee, H., Lee, M.G., 2001, {\it AJ}, {\bf 121}, 2769

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

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