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\IBVShead{4742}{6 August 1999}

\IBVStitle{IRAS 19035-0134: A NEW MIRA VARIABLE}

\IBVSauth{ B. Hassforther$^{1,2}$, U. Bastian$^{3}$  }

\IBVSinst{Ringstr.\ 27, 69115 Heidelberg, Germany, e-mail:  bela1996@aol.com}

\IBVSinst{Bundesdeutsche Arbeitsgemeinschaft f\"ur Ver\"anderliche Sterne e.V. (BAV), Munsterdamm 90, D-12169 Berlin, Germany}

\IBVSinst{Astronomisches Rechen-Institut, M\"onchhofstr.\ 14, 69120 Heidelberg, Germany,\\ e-mail: s01@ix.urz.uni-heidelberg.de}


\SIMBADobj{IRAS 19035-0134}
\IBVStyp{ M }
\IBVSkey{Mira variables}
\IBVSabs{IRAS 19035-0134 is found to be a Mira variable with}
\IBVSabs{a period of about 247 days from {\it Stardial} and TASS}
\IBVSabs{data.}

\begintext


The {\it Stardial} project of the University of Illinois at Urbana-Champaign provides a sky patrol of a declination band just south of the equator, using a drift-scan robotic CCD camera. All the images are immediately made available on the world-wide web under http://www.astro.uiuc.edu/stardial/\@. While ``blinking'' {\it Stardial} frames in a search for new variables, the star IRAS 19035-0134 = USNO--A2.0 0825-14421517, located at $19\hr06\mm05\fsec65~~-01\deg 29\arcm59\farcs0$ (J2000, from USNO--A2.0), was found to vary between about 10 and fainter than 12.5 in unfiltered CCD magnitudes.

The {\it Stardial} lightcurve from all 181 usable frames (collected
over 4 observing seasons) indicated Mira-type variability with
a period of about 250~days. Fig.~1 shows positive magnitude
measurements relative to GSC 5128-945 as solid diamonds, and
upper limits from non-detections as very small triangles.
There is a clear-cut maximum around JD~$2\,450\,620$, and an incomplete
one at about JD~$2\,451\,360$. In between, a minimum is indicated
by a decline around JD~$2\,450\,950$ and a rise around JD~$2\,451\,060$.
The minimum itself is indicated by the large number of non-detections
(small symbols) around JD~$2\,451\,000$. In addition, there is a
rise around JD~$2\,450\,330$, given by a group of non-detections
followed by a group of positive observations.

This interpretation of the {\it Stardial} data is corroborated by 14
frames from {\it The Amateur Sky Survey} (TASS, another public
CCD sky patrol project, see http://www.tass-survey.org/). $I$-band
magnitudes derived from the 14 frames
are displayed as crosses in Fig.~1. Due to the larger optics
compared to {\it Stardial}, the TASS data give positive observations
even close to the minimum.

From Fig.~1 the following rough ephemeris can be derived:
$$
{\rm JD~(Max)} =  2450620 + 247 \times E.
$$

\bigskip
{\it Acknowledgements:} This research made use of the SIMBAD data base, operated by the CDS at Strasbourg, France.

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\IBVSfig{8cm}{4742-f1.ps}{Lightcurve of IRAS 19035-0134. Symbols are explained in the text.}

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