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\IBVShead{4349}{3 June 1996}                      % Use it with dummy or empty a

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\centerline{\ft PHOTOMETRIC VARIABILITY OF THE\ $\lambda$ BOOTIS
STAR HD\,30422}

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HD\,30422 was classified by Gray \& Corbally (1993) as a $\lambda$ Bootis
star with peculiar hydrogen line profiles.
With an age of
$3.8\times10^{8} yr$ (Iliev \& Barzova, 1995) it is one of the
youngest $\lambda$ Bootis stars.
The peculiar nature of this group leads to a severe
uncertainty to establish their location in the Hertzsprung--Russell diagram.
The importance of discovering
pulsation among $\lambda$ Bootis stars was discussed by Weiss et al. (1994).
As part of our global survey for pulsating $\lambda$ Bootis stars, we observed
HD\,30422 for two nights in January 1994 with the Lowell 0.6m telescope at
CTIO (observer: M. Gelbmann). Table 1 lists the observing log. The light curves
of the first night are plotted in Figure 1. The variation of HD\,30422
compared to the measurements of the comparison star is clearly visible. The
amplitude spectrum of the differential data in Str\"omgren $b$ and
the spectral window
derived by a standard Fourier technique is shown in Figure 2. The highest
peak appears at 47 c/d, which corresponds to a period of 30 minutes, and with
an amplitude of about 10 mmag. This is the second star we found to be variable
with such a high frequency (Kuschnig et al., 1994).

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Figure 1. Light curve for HD\,30422 and the comparison star HD\,30182 in
Str\"omgren $b$ for the second night
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Figure 2. Amplitude spectrum and spectral window for the differential data of HD\,30422 and HD\,30182 in Str\"omgren $b$ for both nights
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\centerline{Table 1. Observing log for the program and comparison star}
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\begin{tabular}{|llccccc|}
\hline
Star & Durchm. & JD & hours & $m_{V}$ & Spec. &\\
\hline
HD 30422 & CD $-28\degr$ 1735 & 2449690 & 2 & 6.2 & $\lambda$ Boo &\\
& & 2449697 & 3.5 & & &\\
HD 30182 & CD $-27\degr$ 629 & & & 6.8 & K4III &\\
\hline
\end{tabular}
\end{center}
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{\it Acknowledgement:} This research was done within the working group
{\it Asteroseismology-AMS}. Computing resources and financial support for
this international collaboration were provided by the Fonds zur F\"orderung
der wissenschaftlichen Forschung (project {\it S 8303-AST}) and the
Hochschuljubil\"aumsstiftung der Stadt Wien ($\lambda$ Bootis Sterne). This
research has made use of the Simbad database, operated at CDS, Strasbourg,
France.

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\beginauthors
\authorsrightcol
R. KUSCHNIG
M. GELBMANN
E. PAUNZEN
W.W. WEISS
Institut f\"ur Astronomie,
T\"urkenschanzstra\ss e 17,
A-1180 Wien, Austria
e-mail: paunzen@astro.ast.univie.ac.at
\endauthors

\references

Gray, R.O., Corbally, C.J., 1993, {\it AJ}, {\bf 106}, 632

Iliev, I.K., Barzova, I.S., 1995, {\it A\&A}, {\bf 302}, 735

Kuschnig R., Paunzen, E., Weiss, W.W., 1994, {\it IBVS}, No.\,4070

Weiss, W.W., Paunzen, E., Kuschnig, R., Schneider, H., 1994, {\it A\&A}, {\bf 281}, 797

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\centerline{3}
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\centerline{\bf ERRATUM}
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In Table 1 of the IBVS No.\,4302 several cross-identifications have been
erroneously given. The correct version of the Table is given below.
\vskip 1cm

\begin{center}
\centerline{Table 1. Program and comparison stars, $\star$ this comparison
star is used for the figure}
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\begin{tabular}{|llcccccc|}
\hline
Star & Durchm. & JD & hours & $m_{V}$ & Spec. &   & Upper level [$b$]\\
\hline
HD\,319 & CD $-23^{\circ}$ 13 & 2449166 & 2 & 5.93 & $\lambda$ Boo & & 0.004 \\
HD\,203 & CD $-23^{\circ}$ 4 & & & 6.18 & F2IV & $\star$ & \\
\hline
HD\,141851 & BD $-02^{\circ}$ 4058 & 2449168 & 4 & 5.10 & $\lambda$ Boo  & & 0.004 \\
& & 2449175 & 5 & & & & \\
HD\,141378 & BD $-03^{\circ}$ 3829 & & & 5.52 & A5IV & $\star$ & \\
HD\,140873 & BD $-01^{\circ}$ 3092 & & & 5.39 & B8III & & \\
\hline
HD\,143148 & CD $-31^{\circ}$ 12442 & 2449560 & 4 & 7.39 & $\lambda$ Boo(?) & & 0.004 \\
HD\,142542 & CD $-31^{\circ}$ 12407 & & & 6.29 & F5V & $\star$ & \\
HD\,142851 & CD $-31^{\circ}$ 12426 & & & 7.13 & A0V & & \\
\hline
HD\,145782 & CP $-57^{\circ}$ 7716 & 2449166 & 4 & 5.71 & $\lambda$ Boo(?) & & 0.006 \\
HD\,144480 & CP $-57^{\circ}$ 7613 & & & 5.57 & B9.5V & $\star$ &\\
\hline
HD\,154153 & CD $-43^{\circ}$ 11396 & 2449175 & 3 & 6.18 & $\lambda$ Boo(?) & & 0.004 \\
HD 153234 & CD $-44^{\circ}$ 11339 & & & 6.51 & F3V & & \\
HD\,154025 & CD $-45^{\circ}$ 11188 & & & 6.28 & A2V & $\star$ & \\
\hline
HD 179791 & BD $+05^{\circ}$ 4081 & 2449166 & 3 & 6.51 & $\lambda$ Boo(?) & & 0.006 \\
HD\,178596 & BD $+05^{\circ}$ 4040 & & & 5.22 & F0III & $\star$ & \\
HD\,180482 & BD $+04^{\circ}$ 4045 & & & 5.59 & A3IV & & \\
\hline
HD\,188164 & CP $-69^{\circ}$ 3073 & 2449173 & 3 & 6.35 & $\lambda$ Boo(?) & & 0.004 \\
& & 2449174 & 6 & & & & \\
HD 188097 & CP $-69^{\circ}$ 3072 & & & 5.75 & Am & $\star$ & \\
\hline
HD\,193256 & CD $-29^{\circ}$ 16980 & 2449560 & 5 & 7.70 & $\lambda$ Boo & & 0.002 \\
& & 2449563 & 3 & & & & \\
& & 2449564 & 5 & & & & \\
HD\,193281 & CD $-29^{\circ}$ 16981 & 2449563 & 3 & 6.61 & $\lambda$ Boo & & 0.004 \\
& & 2449564 & 5 & & & & \\
HD\,194170 & CD $-29^{\circ}$ 17046 & & & 8.27 & A4V & $\star$ & \\
\hline
HD\,204041 & BD $-00^{\circ}$ 4215 & 2449568 & 3 & 6.45 & $\lambda$ Boo & & 0.002 \\
HD\,203405 & BD $+00^{\circ}$ 4714 & & & 6.78 & F2 & & \\
HD\,204121 & BD $+00^{\circ}$ 4726 & & & 6.13 & F5V & $\star$ & \\
\hline
\end{tabular}
\end{center}

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