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\IBVShead{5550}{3 August 2004}

\IBVStitle{CCD Photometry of Five Faint Cataclysmic Variables}

\IBVSauth{Haefner, R.}

\IBVSinsto{Universit\"ats-Sternwarte M\"unchen, Scheinerstr. 1, D-81679
  M\"unchen, Germany; e-mail: haefner@usm.uni-muenchen.de}

\SIMBADobj{FV Ara}
\SIMBADobj{NSV 13783}
\SIMBADobj{NSV 14292}
\SIMBADobj{V604 Aql}
\SIMBADobj{V1141 Aql}
\GCVSobj{FV Ara}
\GCVSobj{NSV 13783}
\GCVSobj{NSV 14292}
\GCVSobj{V604 Aql}
\GCVSobj{V1141 Aql}

\IBVSabs{Results of CCD photometry of the faint cataclysmic variables}  
\IBVSabs{FV Ara, NSV 13783, NSV 14292, V604 Aql, and V1141 Aql are reported.}

\begintext

Photometric observations of several faint cataclysmic variables were
obtained in Aug.~1994 using the CCD camera on the 0.9m Dutch telescope 
at the European Southern Observatory (La Silla) to search for
orbital variability and eclipses. Differential instrumental magnitudes 
were then derived relative to nearby comparison stars on the same CCD
image. This note presents results for some of the targets for which no 
photometric time series exist to date and gives additional information
for a recently established SU UMa variable. Table 1 lists the
observing log. 

\begin{table}[h]
\caption{Journal of observations. The measurements were performed in
  integral light. Classifications and magnitudes are from  the on-line 
  data catalog by Downes et al. (2001) and literature cited
  therein. Start is the time for the midpoint of the first exposure.}
\vskip5mm
\begin{tabular}{lccccccc} 
\hline
Object & Type & Date & Start & Duration & Int. Time & Frames & Mag \\
       &    &  & (UT)  & (h)      & (m)       & (No.)  &     \\
\hline
FV Ara & UG & 1994 Aug. 14 & 23:31 & 1.92 & 4 & 25 & 18p \\
NSV 13783 & NL? & 1994 Aug. 16 & 01:28 & 2.58 & 4 & 33 & 19p \\
NSV 14292 & NL? & 1994 Aug. 15 & 03:42 & 2.65 & 4 & 35 & 19.2p\\
V604 Aql & NA & 1994 Aug. 13 & 00:35 & 3:30 & 4 & 42 & 19.6v\\
V1141 Aql & UGSU & 1994 Aug. 11 & 00:29 & 3.07 & 5/7 & 30 & 19.5v\\
\hline
\end{tabular}
\end{table}

{\bf FV Ara}\\

\smallskip

Based on its outburst behaviour this object has recently been
suggested to be a candidate for a WZ Sge-type dwarf nova (Kato et al. 2001). 
Bateson (1998) reported that FV~Ara may have intervals of inactivity
where in active phases the outburst cycle is on the order of 15 days. 
During the present observations the object was  quiescent. It
showed no obvious variability exceeding the 0.03 mag level,
i.e. the behaviour of constant nearby stars of the same brightness.\\[1em] 

\pagebreak

{\bf NSV 13783, NSV 14292}\\

Both objects were tentatively classified as nova-like variables by 
Vogt (1989). Whereas NSV 13783 showed nearly constant behaviour with
the scatter of measurements being of the same order as those of nearby stars 
of the same brightness, the measurements of NSV 14292 indicate some kind of 
flickering activity (scatter enhanced by a factor of 3 as compared to 
constant stars). \\[1em]  

{\bf V604 Aql}\\

The outburst light curve of the fast nova V604 Aql (Nova Aquilae 1905)
was recorded by Walker (1923). Features of the outburst spectra 
were described by Moore (1906) and Cannon (1916). The object was
revisited by  Szkody (1994) who reports BVRJK magnitudes for the postnova.
The present light curve exhibits variations 
with up to about 0.45 mag which might be caused by flaring
events or partly by the appearance of an orbital hump (Fig. 1).\\[1em]
    

{\bf V1141 Aql}\\

Based on the appearance of humps during a superoutburst this object 
has recently been classified  by Olech (2003) as a member of the SU UMa 
class of dwarf novae. A spectrum obtained by Mason \& Howell (2003)
during minimum light shows large double peaked emission lines 
indicating a high orbital inclination. The photometric observations
presented here were also performed during minimum light. They reveal 
the existence of pronounced orbital humps with an amplitude of about 
0.4 mag and indicate an intermediate hump structure (Fig. 2). Eclipses
are obviously not present. The data can be best fitted with a period 
of 89.31 min. Given the superhump period of 85.39 min (Olech 2003) one
would expect an orbital period of the order of 84 min. But the present
data set is too sparse to draw any definitive conclusion (Fig. 3). 
Further, it is worthwhile to note that the image of V1141 Aql is
contaminated by a faint background star (Fig. 4).    

\IBVSfig{8cm}{5550-f1.eps}{Differential photometry of V604 Aql obtained in integral
  light on 1994 Aug. 13. Flaring events as well as a possible hump
  structure are recognizable.}
\IBVSfigKey{5550-f1.eps}{V604 Aql}{light curve}

\IBVSfig{8cm}{5550-f2.eps}{Differential photometry of V1141 Aql obtained in integral
  light on 1994 Aug. 11. The system is at minimum light and shows
  pronounced orbital humps. At 2:21 UT the integration time of 5 min
  was changed to 7 min.}
\IBVSfigKey{5550-f2.eps}{V1141 Aql}{light curve}

\IBVSfig{8cm}{5550-f3.eps}{The photometric measurements of V1141 Aql folded with
  different periods: (1) 89.31 min as suggested by a periodogram analysis
  (top), (2) 85.39 min as given by Olech (2003) for the superhump
  period (middle), (3) 84.0 min as suggested by Olech (2003) for the
  orbital period (bottom). Phase zero is arbitrary.}
\IBVSfigKey{5550-f3.eps}{V1141 Aql}{light curve}

\IBVSfig{8cm}{5550-f4.eps}{The field around V1141 Aql (N is at top, E to the left) during 
  the 1994 observations. The variable (marked by a circle) is estimated to 
  be at about 19 mag, i.e. at minimum brightness. During Olech's measurements
  its brightness was comparable to that of the 15 mag star to the SSE
  of V1141~Aql. Note that the image of V1141 Aql is contaminated by a
  faint background star which was previously not known.}
\IBVSfigKey{5550-f4.eps}{V1141 Aql}{finding chart}


\references


Bateson, F.M., 1998, {\it PVSS}, {\bf 23}, 46

Cannon, A.J., 1916, {\it Harvard Annals}, {\bf 76}, No. 3

Downes, R.A., Webbink, R.F., Shara, M.M., Ritter, H., Kolb, U.,
Duerbeck, H.W., 2001, {\it PASP}, {\bf 113}, 764

Kato, T., Sekine, Y., Hirata, R., 2001, {\it PASJ}, {\bf 53}, 1191

Mason, E., Howell, S.B., 2003, {\it A\&A}, {\bf 403}, 699

Moore, J.H., 1906, {\it ApJ}, {\bf 23}, 261

Olech, A., 2003, {\it Acta Astron.}, {\bf 53}, 85

Szkody, P., 1994, {\it AJ}, {\bf 108}, 639

Vogt, N., 1989, in: Classical Novae, ed. M.F. Bode and A. Evans, p. 225

Walker, A.D., 1923, {\it Harvard Annals}, {\bf 84}, No. 7

\endreferences

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