\documentstyle[epsf,twoside]{article}

\input ibvs2.sty
\input ibvst.sty

\begin{document}

\IBVShead{4804}{17 November 1999}

\IBVStitle{New CCD-Lightcurve and Improved Elements of TY A\lowercase{ri}}

\IBVSauth{Martignoni, M.}

\IBVSinsto{Via Don Minzoni 26, I-20020 Magnago (Milano), Italy}

\SIMBADobj{TY Ari}

\begintext

\IBVSTnam{TY Ari = GSC 1761.1085}

\IBVSTcoo{02\hr 08\mm 40\fsec28}{+25\deg13\arcm07\farcs1}{2000.0}

\IBVSTobs{Private Station in Busto Arsizio, 0.21-m Newton (F/5.0)}

\IBVSTdet{DTA Seti 245C CCD Camera}

\IBVSTfil{None}

\IBVSTcomp{GSC 1761.0989}

\IBVSTchk{GSC 1761.0901}

\IBVSTsysn

\IBVSTdata{Through IBVS Web-site as 4804-t1.txt}
\IBVSedata{4804-t1.txt}

\IBVSTtyp{ RRC }

\IBVSTrem{
The variability of TY Ari (= S 3543 = 218.1943 = CSV 193) was discovered 
by Hoffmeister (1944) and first observed by Meinunger (1966) who found a possible RR Lyrae nature and gave an approximate period of variation. 
First elements and type determination of variability were given by Schmidt 
and Seth (1996). We observed TY Ari during 1998 and obtained 307 measures on 6 nights from  JD 2451134 to JD 2451200. Using the period search algorithm Lancelot (Gaspani, 1995), in agreement 
with the period found by Schmidt and Seth, we derived the following new 
elements of variation:
$$
{\rm Max = HJD~} 2451166.333(3) + 0\fday329715(3) \times E.
$$
Figure 1 shows data folded with these elements.}

\IBVSfig{8.5cm}{4804-f1.eps}{CCD-lightcurve of TY Ari folded with elements given in the text}

\references

Gaspani, A., 1995, GEOS FT 78

Hoffmeister, C., 1944, MVS 52

Meinunger, L., 1966, MVS 3, 220

Schmidt, E.G., Seth, A., 1996, AJ 112, 2769

\end{document}

