\documentclass[twoside]{article}
\usepackage{epsfig}

\input ibvs2.sty
\input ibvst.sty

\begin{document}
\IBVShead{5573}{26 October 2004}

\IBVStitle{New Dwarf Novae on Moscow Plates III}

\IBVSauth{Antipin, S. V.}

\IBVSinsto{Sternberg Astronomical Institute, 13, University Ave.,
Moscow 119992, Russia; \\e-mail: antipin@sai.msu.ru}

\IBVSinsto{Institute of Astronomy, Russian Academy of Sciences,
48, Pyatnitskaya Str., Moscow 119017, Russia}

\IBVSobj{Antipin V79}

\IBVSobj{Antipin V80}


\IBVSabs{We report discovery and photographic investigation of}
\IBVSabs{two new Dwarf Nova, Var79 Peg (=1RXS J215434.4+355023)}
\IBVSabs{and Var80 Per, on Moscow archive plates.}

\begintext

\IBVSTnam{Antipin V79 (Var\,79 Peg) = 1RXS J215434.4+355023}

\IBVSTcoo{21\hr54\mm33\fsec66}{+35\deg50\arcm17\farcs4}{2000}

\IBVSTobs{40-cm astrograph in Crimea}

\IBVSTdet{Photoplate}

\IBVSTfil{None}

\IBVSTcomp{
 \begin{tabular}{ccc}
 \noalign{\smallskip} $\alpha$ (J2000) &
                      $\delta$ (J2000) & $B_{pg}$ \\
 \noalign{\smallskip}
 \hline
 \noalign{\smallskip}
21\hr54\mm18\fsec7 & +35\deg48\arcm04\arcs & 14\fmm01 \\
21\hr54\mm35\fsec6 & +35\deg49\arcm16\arcs & 14\fmm53 \\
21\hr54\mm18\fsec4 & +35\deg51\arcm07\arcs & 14\fmm86 \\
21\hr54\mm21\fsec1 & +35\deg52\arcm49\arcs & 15\fmm29 \\
21\hr54\mm30\fsec2 & +35\deg51\arcm46\arcs & 15\fmm61 \\
21\hr54\mm34\fsec2 & +35\deg51\arcm50\arcs & 15\fmm90 \\
21\hr54\mm38\fsec9 & +35\deg51\arcm22\arcs & 16\fmm70 \\
21\hr54\mm37\fsec4 & +35\deg50\arcm43\arcs & 17\fmm0  \\
21\hr54\mm37\fsec9 & +35\deg49\arcm32\arcs & 17\fmm1  \\
21\hr54\mm32\fsec5 & +35\deg50\arcm14\arcs & 17\fmm6  \\
21\hr54\mm34\fsec1 & +35\deg50\arcm35\arcs & 18\fmm1  \\
 \noalign{\smallskip}
 \end{tabular}
}

\IBVSTsys{$B_{\rm pg}$}{Calibrated using the photoelectric B-band
standard sequence near Cyg\,X-2 (Basko~{\it et al.}, 1976) and the
blue magnitudes of neighboring stars from the GSC\,2.2 catalogue.}

\IBVSTdateobs{1974--1996}

\IBVSTdata{Upon request}

\IBVSTtyp{  UG  }

\IBVSTrem{  We investigated Var\,79 Peg on 440 plates of Moscow
collection taken for the interval JD\,2442278--50279 (mostly in
JD2442278--47828). The finding chart is given in Fig.\,1. The
light curve (Fig.\,2) shows two important features. First, two
kinds of outbursts were found: the short-lasting ones and the
longer ones. The long-lasting outbursts with flat maxima,
resembling superoutbursts of SU UMa-type dwarf novae, are clearly
seen in Fig.\,3b and 3d. The outbursts are relatively frequent.
Second, the amplitude of variability strongly changed during the
interval of observation: the brightness of Var\,79 in minimum
smoothly increased in 1980--1982. The photographic magnitudes
changed within 14\fmm0--$<$18\fmm1 before 1980 and within
14\fmm35--17\fmm0 after 1982. The only exception is the year 1987
when the star was fainter than 17\fmm1 on Moscow plates and
appeared at $b$=18\fmm26, as measured in the GSC\,2.2 catalog, on
a POSS II blue plate (the asterisk in Fig.\,2). Furthermore, we
propose to identify the new variable with the X-ray source
1RXS~J215434.4+355023. The source is relatively hard, the ROSAT
hardness ratios are HR1\,$=1.00\pm0.13$ and HR2\,$=0.91\pm0.13$
(Voges et al., 2000). All foregoing characteristics make
Var\,79~Peg a very interesting and important object for
investigation. Further observations are encouraged.}

\IBVSfig{6.0cm}{5573-f1.eps}{The finding charts, size 5' x 5'.}
\IBVSfigKey{5573-f1.eps}{Antipin V79, Antipin V80}{finding chart}

\IBVSefigure{5573-f1a.eps}
\IBVSefigure{5573-f1b.eps}

\IBVSfig{7.0cm}{5573-f2.eps}{The photographic light curve of
Var\,79 Peg. Open circles: uncertain observations; open triangles:
brighter limits; the asterisk: the GSC\,2.2 estimate.}
\IBVSfigKey{5573-f2.eps}{Antipin V79}{light curve}

\IBVSfig{20.0cm}{5573-f3.eps}{The sample light curves of
Var\,79~Peg. Open triangles: brighter limits.}
\IBVSfigKey{5573-f3.eps}{Antipin V79}{light curve}

\IBVSfig{7.0cm}{5573-f4.eps}{The photographic light curve of
Var\,80 Per. Open triangles: brighter limits.}
\IBVSfigKey{5573-f4.eps}{Antipin V80}{light curve}


\IBVSTnam{Antipin V80 (Var\,80 Per)}

\IBVSTcoo{2\hr46\mm02\fsec33}{+34\deg55\arcm08\farcs4}{2000}

\IBVSTobs{40-cm astrograph in Crimea}

\IBVSTdet{Photoplate}

\IBVSTfil{None}

\IBVSTcomp{
 \begin{tabular}{ccc}
 \noalign{\smallskip} $\alpha$ (J2000) &
                      $\delta$ (J2000) & $B_{pg}$ \\
 \noalign{\smallskip}
 \hline
 \noalign{\smallskip}
2\hr45\mm36\fsec0 & +34\deg56\arcm13\arcs & 13\fmm88 \\
2\hr45\mm54\fsec0 & +35\deg00\arcm05\arcs & 14\fmm51 \\
2\hr45\mm45\fsec2 & +34\deg56\arcm35\arcs & 15\fmm00 \\
2\hr46\mm03\fsec4 & +34\deg56\arcm10\arcs & 15\fmm20 \\
2\hr45\mm47\fsec6 & +34\deg55\arcm02\arcs & 15\fmm53 \\
2\hr45\mm57\fsec1 & +34\deg52\arcm44\arcs & 15\fmm90 \\
2\hr46\mm08\fsec6 & +34\deg58\arcm03\arcs & 16\fmm46 \\
2\hr46\mm03\fsec9 & +34\deg57\arcm10\arcs & 16\fmm74 \\
2\hr46\mm14\fsec3 & +34\deg53\arcm42\arcs & 17\fmm2  \\
2\hr46\mm04\fsec8 & +34\deg55\arcm26\arcs & 17\fmm4  \\
2\hr46\mm10\fsec2 & +34\deg52\arcm44\arcs & 17\fmm6  \\
 \noalign{\smallskip}
 \end{tabular}
}

\IBVSTsys{$B_{\rm pg}$}{Calibrated using the blue magnitudes of
neighboring stars from the GSC\,2.2 catalogue.}

\IBVSTdateobs{1963--1994}

\IBVSTdata{Upon request}

\IBVSTtyp{  UG  }

\IBVSTrem{ The new variable star was estimated on 205 plates
(JD\,2438101--49634). Eight outbursts have been revealed. The
range of variability on Moscow plates is 14\fmm1--$<$17\fmm6. All
observed outbursts are relatively short-lasting. The finding
chart and the light curve are shown in Fig.\,1 and Fig.\,4
respectively. Outbursts (JD24...): \vskip 0.2cm
 \begin{center}
 \begin{tabular}{ccccccccc}
 \noalign{\smallskip}
\#1& 38317.504&  15.25  & \#4& 43394.484& $<$17.6 & \#6& 45642.438& 14.45 \\
   & 38319.426&  17.40  &    & 43400.477&  14.56  &    & 45645.374& 16.83 \\
   & 38322.332& $<$17.6 &    & 43401.544&  15.25  &    &          &       \\
   &          &         &    & 43401.573&  15.27  & \#7& 45944.558& 14.07 \\
\#2& 41948.446& $<$17.6 &    & 43408.505& $<$17.6 &    &          &       \\
   & 41951.467&  14.66  &    &          &         & \#8& 47064.575& 14.29 \\
   & 41954.489&  17.46  & \#5& 45584.494& $<$17.6 &    & 47066.537& 14.35 \\
   & 41957.476& $<$17.6 &    & 45589.460& 15.53   &    &          &       \\
   &          &         &    & 45593.547& 14.83   &    &          &       \\
\#3& 42661.484&  14.63  &    & 45595.550& 16.01   &    &          &       \\
   & 42661.518&  14.63  &    & 45597.546& 17.60   &    &          &       \\
   & 42662.535&  14.93  &    & 45597.578& 17.50   &    &          &       \\
   & 42665.494& $<$15.9 &    &          &         &    &          &       \\
   & 42668.557& $<$17.6 &    &          &         &    &          &       \\
 \noalign{\smallskip}
 \end{tabular}
 \end{center}
 }

\IBVSTack{The author would like to thank Dr. N. N. Samus for his
help. The author is grateful to the Russian Foundation for Basic
Research (grants No.~02-02-16069 and No.~02-02-16462 ), the
Program for the Support of Leading Scientific Schools (grant
NSh-389-2003-2) and the Federal Program ``Astronomy'' for partial
support of this research.}

\newpage

\references

Basko, M.M., Goranskij, V.P., Lyuty, V.M., Ruzan, L.L., Sunyaev,
R.A., Shugarov, S.Yu., 1976, {\it Perem. Zvezdy}, {\bf 20}, 219

Voges, W., Aschenbach, B., Boller, Th., et al., 2000, {\it IAU
Circ.}, No.\,7432, ROSAT All-Sky Survey Faint Source Catalogue
(RASS-FSC)

\endreferences


\end{document}
