\documentstyle[twoside,epsf]{article}

\input ibvs2.sty
\input ibvst.sty

\begin{document}

\IBVShead{4732}{1 July 1999}

\IBVStitle{Photometric Observations of NSV 07180}

\IBVSauth{P. Merch\'an-Ben\'{\i}tez$^1$, M. Jurado-Vargas$^1$, F. S\'anchez-Bajo$^2$}

\IBVSinst{Departamento de F\'{\i}sica, Facultad de Ciencias, Universidad de Extremadura, Ctra de Elvas 06071, Badajoz (Spain), e-mail: pedromer@unex.es, mjv@unex.es}

\IBVSinst{Departamento de Electr\'onica e Ingenier\'{\i}a Electromec\'anica, Escuela de Ingenier\'{\i}as Industriales. Universidad de Extremadura, Ctra de Elvas 06071, Badajoz (Spain), e-mail: fsanbajo@unex.es}

\SIMBADobj{NSV 07180}

\begintext

\IBVSTnam{NSV 07180 = CSV 002403}

\IBVSTcoo{15\hr39\mm23\fsec3}{$-12\deg06\arcm47\arcs$}{2000.0}

\IBVSTobs{Observatorio del Departamento de F\'{\i}sica de la Universidad de Extremadura, Reflector Newton 0.4-m f/4.5}

\IBVSTdet{Starlight Xpress CCD Camera (based in the chip SONY ICX027BL $6.4 \times 4.35$ mm$^2$, $500 \times 256$ pixels)}

\IBVSTfil{$V$ (Kron-Cousins system)}

\IBVSTcomp{GSC 5604.231}

\IBVSTchk{GSC 5604.564}

\IBVSTsysn

\IBVSTdata{Upon request}

\IBVSTtyp{ RR Lyr }

\IBVSTrem{
The results of the observations carried out show that NSV 07180 seems to be an RR Lyrae star with a period close to 7 hours. Although the data display a high
dispersion, the star shows an almost symmetric light curve ($\varepsilon = 0.48$) and a 0.5 magnitude amplitude in the $V$ band. We have derived the following ephemeris for the maximum:
$$\begin{array}{r@{}r@{}l}
{\rm Max = HJD}~2451342.4375 & {} + 0\fday2850 & {} \times E. \\
 \pm 0.0036 & \pm 0.0001 \\
\end{array}$$}

\IBVSTack{This research was supported by the Consejer\'{\i}a de Educaci\'on y Juventud (Junta de Extremadura) and Fondo Social Europeo under project IPR98A047.}

\IBVSfig{6.5cm}{4732-f1.ps}{Identification chart of NSV 07180. C = comparison star, Ck = Check star, V = NSV 07180. North is on the top.}

\IBVSfig{7cm}{4732-f2.eps}{The $V$ light curve obtained for NSV 07180. Delta magnitudes (variable minus comparison) are plotted versus phase, where the phases are computed using the ephemeris calculated in this work.}


\reference 

Kukarkin et al.\ 1982, New Catalogue of Suspected Variable Stars, Moscow

\end{document}
