\documentstyle[twoside, epsf]{article} 
 
\input ibvs2.sty 
\input ibvst.sty 
 
\begin{document} 
 
\IBVShead{4736}{21 July 1999} 
 
\IBVStitle{Photometry of the 1999 outburst of U Scorpii} 
 
\IBVSauth{Seiichiro Kiyota} 
 
\IBVSinsto{Variable Star Observers League in Japan, 1-401-810 Azuma,
Tsukuba, 305-0031 Japan,\\ e-mail: skiyota@abr.affrc.go.jp}

\SIMBADobj{U Sco}
 
\begintext 
 
\IBVSTnam{U Sco} 
 
\IBVSTcoo{16\hr22\mm31\fsec2}{$-17\deg52\arcm41\arcs$}{2000.0} 
 
\IBVSTobs{25-cm Schmidt Cassegrain (F/6.3)} 
 
\IBVSTdet{Apogee AP-7 CCD camera (SITe SIA502AB, $512\times 512$)} 
 
\IBVSTfil{Johnson-Cousins $BVR_c$} 
 
\IBVSTcomp{GSC~6206\_320 = BD~$-17\deg4559$ = PPM~23163, $V = 10.68$,
$B-V=0.496$ (based on Tycho catalog), $V-R=0.25$ (calculated from $B-V$
value)}
 
\IBVSTsysn 
 
\IBVSTdata{Through IBVS Web-site as 4736-t1.txt} 
 
\IBVSTtyp{ NR } 
 
\IBVSTrem{ 
Patrick Schmeer (1999) reported the 6th recurrent outburst of U Sco 
(9.5 m$_V$ on Feb.\ 25.1940, 1999) (Vsnet-alert 2688, IAUC 7113). L. 
Shaw reported that U Sco reached the maximum of 7.6 m$_V$ at Feb.\ 
25.562 (IAUC 7113). I began to observe this outburst immediately after 
maximum. The lightcurve consists of 3 parts; the 1st fast fading 
phase, plateau around Mar.\ 12--22, the 2nd fast fading. $B-V$ was 
steeply decreasing after maximum but almost constant in the plateau 
phase. The plateau around 15 days after the maximum was also reported 
at the outburst during 1987 (Sekiguchi et al., 1988).} 
 
\IBVSTack{I thank Dr.\ Taichi Kato, Kyoto University for useful
discussion and advice.} 
 
 
\IBVSfig{10cm}{4736-f1.eps}{} 
 
\references 
 
Schmeer et al., 1999, IAUC 7113 
 
Sekiguchi, K., Feast, M.W., Whitelock, P.A., Overbeek, M.D., 
Wargau, W., Jones, J.S., 1988, MNRAS, 234, 281 
 

\IBVSedata{4736-t1.txt}

\end{document} 

