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\IBVShead{4337}{7 May 1996}

\title{\ft GT AQUARII: NEW ELEMENTS}

\begintext

   GT Aquarii = SVS\,2659 = GSC\,5226.00945 $(\alpha_{1950.0}: 22\fh 25\fmm 44\fss;
\delta_{1950.0}:-01\degr\,14\farcm 8)$ was reported by Kurochkin (1986) as a variable star with a range of variation from 13\fm 1\ to
14\fm 1. He found a possible pulsational variation with an uncertain period of
1\fd 1901204. In view of this finding, this star warrants some further
investigation as it might be a new member of the AHB1 class of pulsating
variables (see Sandage, Diethelm and Tammann, 1994). No other source of
data is known to the author.

   During the 1995 season, GT Aquarii was observed with the 35cm RC
telescope at R. Szafraniec Observatory in Metzerlen, Switzerland, by the
author. An unfiltered ST-6 CCD camera was employed. A total of 101
observations in 22 nights could be secured. As comparison star
GSC\,5226.01225 (13\fm 97), lying very close to the variable, was used. The
comparison star showed no variation exceeding the accuracy of the
photometry. Due to the proximity of the comparison star to GT Aqr as
well as to the limited accuracy of the photometry (see below), no
correction for differential extinction was allowed for.

   With the period given by Kurochkin (1986) our data do not yield a satisfactory light
curve. A coarse period finding algorithm leads to a most likely value
of P = 0\fd 3516. In Figure 1, the observations are presented, folded
with the elements:
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   Max$_{JD,hel}$ = 2449898.505 + 0.3516 $\times$ E .  \hfill(1)
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Figure 1. Unfiltered CCD light curve  of GT Aqr, folded with the elements given above
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   The rather large scatter seen in Figure 1 is primarily due to two
circumstances. The star is about one magnitude fainter than
given by Kurochkin (14\fm 1 - 15\fm 2). In addition, due to the
negative declination of the variable, the air mass was relatively large
for an observer at the latitude of Switzerland. Therefore, the signal to
noise ratio of our CCD frames was smaller than hoped for. Nevertheless
we dare to state that some of the scatter might be caused by some intrinsic
variability in the light curve.
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\beginauthors
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R. DIETHELM
Rennweg 1
CH-4118 Rodersdorf
Switzerland
\endauthors
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\references

Kurochkin, N.E., 1986, {\it Perem. Zv.}, {\bf 22}, 327

Sandage, A., Diethelm, R., Tammann, G.A., 1994, {\it Astron. Astrophys.},
{\bf  283}, 111

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