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\IBVShead{4195}{24 May 1995}                      % Use it with dummy or empty arguments

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\centerline{\ft A LIST OF VARIABLE STARS SIMILAR TO $\gamma$ Dor}
\vspace{8mm}

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In this note we compile data on stars that appear to constitute a new class of
variable stars. These stars typically have spectral types near F0 and luminosity
classes of V or IV-V.  They are variable up to 0.1 mag in $V$ on a time scale of
0.5 to 3 days -- an order of magnitude longer than the fundamental radial
pulsation period for stars of this density. Some exhibit two or more
frequencies. The evidence is that these stars are variable owing to non-radial
$g$-mode pulsations. Given that $\gamma$ Dor was the first one found to be
variable (Cousins \& Warren 1963), it has been suggested that they be known as
``$\gamma$ Doradus stars''. Our list is a consequence of the rapidly growing
scientific interest in these stars. For instance, multi-longitude campaigns are
planned for four of the stars during 1995; these are necessary to avoid aliasing
of the frequencies of variation for stars with $\approx$ 1 day periods.

In Tables 1, 2, and 3, respectively, we give various data on the bona fide 
members of the group, on other candidates, and on one star formerly regarded 
as being of the $\gamma$~Dor type. The coordinates are equinox 2000.
The photometric periods are given in days.  The projected rotational
velocities $v$ sin $i$ are in km s$^{-1}$. Table 1 is only for stars with a
considerable amount of available data. Table 2 contains all objects we found in
the literature which were reported to be related with the $\gamma$ Dor
phenomenon. In the tables we provide Str\"omgren photometry from Hauck \&
Mermilliod (1990) supplemented by new observations of Handler (1995). 
In the references
we include only published papers. 
We do note, however, that Zerbi (private communication) informs us there
is a paper in preparation on NGC 2516 which provides evidence for 
additional four $\gamma$ Dor candidates in that cluster.
\vskip 1mm
\centerline{Table 1. Bona Fide Members}
\vskip 1mm
\begin{center}
\begin{tabular}{llllllr}
\hline
Star & HD & $<V>$ & $(b-y)$ & $m_1$ & $c_1$ & $\beta$\\
RA & DEC & Sp & Period(s) & $v \sin i$ & Remarks & References\\
\hline
 & 224945 & 6.9 & 0.192 & 0.147 & 0.719 & 2.743\\
\vspace{1.5mm}
 00:02:02.4 & $-$02:45:59 & (F0) & 1.072, 1.495 & 55 & & 11, 12, 14\\
$\gamma$ Dor & 27290 & 4.25 & 0.201 & 0.173 & 0.658 & 2.742\\
\vspace{1.5mm}
 04:16:01.0 & $-$51:29:21 & F0\,V & 0.733, 0.757 & 62 & & 2, 3, 21\\
9 Aur & 32537 & 5.00 & 0.217 & 0.152 & 0.642 & 2.723\\
\vspace{1.5mm}
 05:06:40.7 & +51:36:01 & F0\,V & 1.258, 2.895 & 18 & 1 & 4, 13, 16\\
2 Pup B & 62683 & 6.89 & 0.201 & 0.165 & 0.634 & 2.727\\
\vspace{1.5mm}
 07:45:28.7 & $-$14:41:09 & A8\,V & 1.92 or 0.48 & & & 20\\
 & 164615 & 7.06 & 0.230 & 0.178 & 0.624 & 2.715\\
\vspace{1.5mm}
 18:01:32.9 & +11:17:08 & F2\,IV--V & 0.815 & 60 & & 9, 10\\
 & 224638 & 7.2 & 0.198 & 0.157 & 0.680 & 2.726\\
23:59:34.5 & $-$01:51:02 & (F0) & 1.233, 1.460 & 24 & & 11, 12, 14\\
\hline
\end{tabular}
\end{center}
\vfill \eject

\centerline{2}
\vskip 1mm
\centerline{Table 2. Other Candidates}
\vskip 1mm
\begin{center}
\begin{tabular}{llllllr}
\hline
Star & HD & $<V>$ & $(b-y)$ & $m_1$ & $c_1$ & $\beta$\\
 RA & DEC & Sp & Period(s) & $v \sin i$ & Remarks & References\\
\hline
 & 23375 & 8.58 & 0.228 & 0.172 & 0.719 & 2.765\\
\vspace{1.5mm}
03:45:34.4 & +24:27:50 & A9\,V & $> 0.2$ & 75 & & 1\\
NGC\,2516 C52 & & 10.29 & 0.278 & 0.176 & 0.673 & 2.761\\
\vspace{1.5mm}
 7:55:52 & $-$60:24:37 & & 0.2-0.4 & & 2 & 5 \\
NGC\,2516 C69 & & 11.21 & 0.282 & 0.117 & 0.739 & 2.761\\
\vspace{1.5mm}
 7:56:19 & $-$60:36:59 & & 0.2-0.4 & & & 5 \\
NGC\,2516 C93 & & 11.13 & 0.263 & 0.144 & 0.797 & 2.776\\
\vspace{1.5mm}
 7:54:25 & $-$60:30:40 & & 0.2-0.4 & & & 5 \\
NGC\,2516 C96 & & 11.23 & 0.257 & 0.151 & 0.720 & 2.766\\
\vspace{1.5mm}
 7:54:13 & $-$60:35:09 & & 0.2-0.4 & & & 5 \\
$\tau^1$ Hya & 81997A & 4.60 & 0.296 & 0.164 & 0.448 & 2.661\\
\vspace{1.5mm}
 9:29:08.4 & $-$02:46:07 & F6\,V & (days) & 25 & & 18 \\
 & 106103 & 8.12 & 0.264 & 0.160 & 0.449 & 2.675\\
\vspace{1.5mm}
 12:12:24.9 & +27:22:49 & F4\,V & (0.83) & 6 & 3 & 19 \\
$\gamma$ Vir & 110379/80 & 3.48 & 0.242 & 0.152 & 0.522 & 2.708\\
\vspace{1.5mm}
 12:41:41.4 & $-$01:26:58 & F0\,V & ? & 28 & 4 & 23 \\
 & 111829 & 9.46 & 0.228 & 0.100 & 1.000 & 2.806\\
\vspace{1.5mm}
12:53:41.3 & $-$74:53:46 & A1\,IV-V & 1.8 ? & & 5 & 8 \\
 & 117777 & 9.25 & & & &\\
\vspace{1.5mm}
13:32:03.3 & +28:35:05 & F2\,V & (1) & & & 22 \\
BS 8799 & 218396 & 5.99 & 0.181 & 0.142 & 0.678 & 2.745\\
23:07:28.3 & +21:08:05 & A5\,V & 0.510 & 45 & & 17 \\
\hline
\end{tabular}
\end{center}
\vskip 5mm
\centerline{Table 3. Star formerly on the list}
\begin{center}
\begin{tabular}{llllllr}
\hline
Star & HD & $<V>$ & $(b-y)$ & $m_1$ & $c_1$ & $\beta$\\
RA & DEC & Sp & Period(s) & $v \sin i$ & Remarks & References\\
\hline
& 96008 & 6.74 & 0.209 & 0.165 & 0.703 & 2.727\\
 11:03:43.7 & $-$51:21:11 & F0\,V & 0.309873 & 85 & 6 & 6, 7, 15 \\
\hline
\end{tabular}
\end{center}
\vskip 3mm
\noindent References to Tables 1--3:\\
 1. Breger M., 1972, ApJ, 176, 367\\
 2. Cousins A. W. J., 1992, The Observatory, 112, 53\\
 3. Balona L. A., et al., 1994, MNRAS 267, 103\\
 4. Krisciunas K., et al., 1993, MNRAS, 263, 781\\
 5. Antonello E., Mantegazza, L., 1986, A\&A, 164, 40\\
 6. Lampens P., 1987, A\&A, 172, 173\\
 7. Matthews J. M., 1990, A\&A, 229, 452\\
 8. Mantegazza L., Poretti E., Antonello E., 1991, IBVS, No. 3612\\
 9. Abt H. A., Bollinger G., Burke E. W., Jr., 1983, ApJ, 272, 196\\
 10. Rucinski S. M., 1985, PASP, 97, 657\\ 


\vfill \eject

\centerline{3}
\vskip 1mm
\noindent
11. Mantegazza L., Poretti E., 1991, IBVS, No. 3690\\
12. Mantegazza L., et al., 1993, ASP Conf. Ser. 40, 651\\
13. Kazovarets E. V., Samus N. N., 1995, IBVS, No. 4140\\
14. Mantegazza L., Poretti E., Zerbi, F. M., 1994, MNRAS, 270, 439\\
15.~Mantegazza L., Poretti E., 1995, A\&A, 294, 190. See also Delta Scuti Star
Newsletter 

\hspace*{6mm}(Vienna), No. 8, 13\\
16. Krisciunas K., et al., 1995, MNRAS, 273, 662\\
17. Rodriguez E., Zerbi, F. M., 1995, IBVS, No. 4170\\
18. Lockwood G. W., Skiff B. A., Thompson D. T., 1993, IAU Colloq. 136, Stellar

\hspace*{6mm}Photometry - Current Techniques and Future Developments, C. J. Butler \& 

\hspace*{5mm} I. Elliott (eds.), p.~99\\
19. Handler G., 1994, Delta Scuti Star Newsletter (Vienna), No. 7, 11\\
20. Vaz L. P. R., Andersen J., 1984, A\&A, 132, 219\\
21. Balona L. A., Krisciunas K., Cousins, A. W. J., 1994, MNRAS, 270, 905\\
22.~Hall D. S., 1995, Robotic Telescopes: Current Capabilities, Present
Developments, 

\hspace*{6mm}and Future Prospects for Automated Astronomy, G. W. Henry \&
J. A. Eaton (eds.), 

\hspace*{6mm}ASP Conf. Series, No.\,79, p.\,65\\
23. Hoffleit D., 1992, JAAVSO, 21, 55\\
\vskip 1mm
\small
\noindent Remarks to Tables 1--3:\\
 1. 9 Aur was designated V398 Aur in the latest name-list of variable stars
(Ref.~13 above).\\
 2. Cluster membership doubtful (Ref.~5 above); Str\"omgren indices suggest high metallicity, thus the absolute 
\hspace*{6mm} magnitude of the star in Figure~1 could be too low\\
 3. Period uncertain due to aliasing\\
 4. The magnitudes and colors given are for the slightly brighter of the two
nearly identical components.\\
 5. Note correct HD number\\
 6. Shown to be an ellipsoidal binary (Ref.~15 above)
\large

\epsfysize=8cm
\centerline{\epsffile{4195-f1.ps}}
\begin{center}
Figure 1. Color-magnitude diagram of the stars similar to $\gamma$ Dor. Circles:
stars from Table~1. Triangles: NGC 2516 stars. Dots: other candidates from 
Table~2. The Zero Age Main Sequence is adopted from Crawford (1975, 1979), while
the borders of the instability strip are taken from Breger (1979).
\end{center}
\vfill \eject 

\centerline{4}
\vskip 2mm

In Figure 1 we give a color-magnitude diagram of the bona fide members and the
other candidates. For field stars and doubtful members of clusters, we
calculated the unreddened colors and absolute magnitudes from the Str\"omgren
photometry by applying the calibrations of Crawford (1975, 1979).


The authors would appreciate receiving from other observers further data and 
news of new candidates, since this list will be continuously updated.

Some information in the table was obtained from the {\sc simbad}
data retrieval system, a data base of the Astronomical Data Centre, 
Strasbourg, France.
\medskip

{\it{Acknowledgements:}} L.~Mantegazza kindly supplied a program for calculating
dereddened colors and absolute magnitudes from uvby$\beta$ photometry.


\vskip 1cm
\beginauthors
\authorsrightcol
K. KRISCIUNAS$^{\star}$
G. HANDLER$^{\star\star}$
\endauthors

\vspace{8mm}

$^{\star}$\ Joint Astronomy Centre,~660 N.~A'oh\={o}k\={u} Place,
University Park, Hilo, Hawaii 96720, \\
\hspace*{8mm}USA, 
e-mail: kevin@jach.hawaii.edu\\

$^{\star\star}$\ Institut f\"ur Astronomie, T\"urkenschanzstra\ss e 17,
A-1180 Wien, Austria\\
\hspace*{10mm}
e-mail: handler@astro.ast.univie.ac.at


\references

Breger, M., 1979, {\it PASP}, {\bf 91}, 5

Cousins, A. W. J., Warren, P. R., 1963, {\it MNASSA}, {\bf 22}, 65

Crawford, D. L., 1975, {\it AJ}, {\bf 80}, 955

Crawford, D. L., 1979, {\it AJ}, {\bf 84}, 1858

Handler, G., 1995, The Observatory, submitted

Hauck, B., Mermilliod, M., 1990, {\it A\&AS}, {\bf 86}, 107


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