\documentstyle[twoside,epsf]{article}

\input ibvs2.sty
\input ibvst.sty

\begin{document}

\IBVShead{4974}{27 October 2000}

\IBVStitle{NSV 11766 is a New Short Period Pulsating Variable}

\IBVSauth{Garcia-Melendo, Enrique$^1$; Nomen-Torres, Jaime$^2$}

\IBVSinst{Esteve Duran Observatory Foundation, Montseny 46 -- Urb.\ El
Montanya, 08553 Seva, Barcelona, Spain\\ \indent e-mail: duranobs@astrogea.org}

\IBVSinst{Grup d'Estudis Astronomics, Apartado 9481, 08080 Barcelona,
Spain}

\SIMBADobj{NSV 11766}

\begintext

\IBVSTnam{NSV 11766 = GSC 4431\_546 = BV 0062 = CSV 008121}

\IBVSTcoo{19\hr 06\mm 26\fsec3}{+68\deg 29\arcm 2\arcs}{2000.0}

\IBVSTobs{Esteve Duran Observatory, 0.6-m Cassegrain telescope\\
l'Estelot Observatory, 0.3-m Newtonian telescope}

\IBVSTdet{CCD in all cases}

\IBVSTfil{$B,V,R$}

\IBVSTcomp{GSC 4431\_386}

\IBVSTchk{None}

\IBVSTsysn

\IBVSTdata{Upon request}

\IBVSTtyp{ SX Phe: }

\IBVSfig{10cm}{4974-f1.eps}

\IBVSTrem{
The variability of NSV 11766 was first announced by Geyer et al.\ (1955), and
finally listed in the NSV catalogue (Kholopov, 1982) as an unstudied variable 
with rapid light changes between the photographic magnitudes 11.6 and 12.0. 
In a program for searching new variables, the star was observed in the $B$, $V$, 
and $R$ bands between May 1997 and June 2000, and also some observations 
where obtained in $I$. Photometric data show that NSV 11766 is actually a 
periodic rapid variable with a period close to 0.12 days and an amplitude 
of 0\fmm30 in the $V$ band (Figure 1), 0\fmm39 in $B$, 0\fmm25 in $R$, 
and 0\fmm25 in $I$. Its short period and 
relatively large amplitude suggest that this object might be an SX Phe variable, 
although additional data should definitively determine its type. Photometry 
also indicates that the period of this object has remained stable within 
the given uncertainty. The following ephemeris was computed for light maxima:
\belowdisplayskip-12pt
$$ \begin{array}{r@{}r@{}l}
{\rm Max. = HJD}~2451697.6040 & {} + 0\fday1181533 & {} \times E. \\
{} \pm 0.0015 & {} \pm 0.0000002 \\
\end{array} $$
}

\references

Geyer, E., Kippenhahn, R., Strohmeier,  W., 1955, {\it Kleine Ver\"offentlichungen der 
  Universit\"ats-Sternwarte zu Berlin-Babelsberg}, No.\ 9

Kholopov, P.N., editor, 1982, New Catalogue of Suspected Variable Stars, Moscow

\end{document} 
