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\IBVShead{5973}{7 February 2011}

\IBVStitletl{New Radial Velocities of}{ Some Semi-Regular Variable Stars}

\IBVSauth{Aslan, Z.}
\IBVSinsto{\.{I}stanbul K\"{u}lt\"{u}r University, Department of Physics, 34156 Bakirk\"{o}y, \.{I}stanbul, Turkey\\
  e-mail: z.aslan@iku.edu.tr }



\begintext

\vspace*{-0.6cm}

New radial velocities of 11 Semi-Regular variable stars measured in conjunction with the  radial velocity program of the Vilnius University Observatory (Sperauskas et al. 2002)  are reported here. The radial velocities were measured with the CORrelation RAdial VELocities (CORAVEL) spectrometer of the Vilnius University Observatory (Upgren, Sperauskas, and Boyle, 2002) attached to the 1.5 m Russian Turkish Telescope (RTT150)  at the T\"{U}B\.{I}TAK National Observatory (TUG), Turkey.  Observations are described in Sperauskas et al. (2002). These stars were observed on two or more nights to check for possible variability. The results are tabulated in Table 1. 

\begin{table}[hb]
\centerline{{\bf Table 1.} Observed Radial Velocities}
\vskip 3mm
\begin {center}
\begin{tabular}{rcrc}
\hline
Variable & HJD 24\dots & Vr (km/s) & $\pm$ 
\\
\hline     

V0347 And	&	51887.297	&	$-$47.4	&	0.8\\
         	&	51888.218	&	$-$47.1	&	0.9\\
           &	51892.312	&	$-$45.8	&	0.9\\
        &	51893.271	&	$-$44.9	&	0.8\\ \hline								
AH Ari	&	51887.368	&	    $-$3.5	&	0.7\\
	&	51888.200	&	    $-$3.1	&	0.8\\
	&	51890.419	&	    $-$5.0	&	0.7\\
	&	51892.349	&	    $-$2.9	&	0.7\\
   &	51893.310	&	    $-$2.5	&	0.8\\
	&	51894.380	&	    $-$4.0	&	0.7\\ \hline						
AU Ari	&	51887.356	&	      44.9	&	0.7\\
	&	51888.208	&	      45.0	&	0.8\\
	&	51892.337	&	      45.9	&	0.8\\
	&	51893.301	&	      45.8	&	0.8\\
	&	51894.370	&	      44.6	&	0.7\\  \hline								
V0453 Aur	&	51887.569	&	    0.4	&	0.9\\
	&	51888.411	&	    1.0	&	0.8\\
	&	51889.374	&	    0.7	&	0.7\\
	&	51890.483	&	    1.4	&	0.8\\
	&	51894.521	&   $-$0.2	&	0.8\\	\hline						
\end{tabular}
\end{center}
\end{table}



\begin{table}[!ht]
\centerline{{\bf Table 1.} Observed Radial Velocities (continued)}
\vskip 3mm
\begin {center}
\begin{tabular}{rcrc}
\hline
Variable & HJD 24\dots & Vr (km/s) & $\pm$ 
\\
\hline     
RY Cam	&	51887.336	&     $-$19.6	&	0.9\\
	&	51888.395	&     $-$19.8	&	0.8\\
	&	51890.476	&	   $-$20.3	&	0.9\\
	&	51890.477	&	   $-$20.5	&	0.9\\
	&	51892.432	&	   $-$19.8	&	0.8\\
	&	51892.434	&	   $-$20.2	&	0.7\\
	&	51893.367	&	   $-$17.6	&	0.8\\
	&	51893.369	&	   $-$16.7	&	0.9\\
	&	51969.249	&	   $-$26.3	&	0.7\\
	&	51893.367	&	   $-$17.6	&	0.8\\
	&	51893.369	&	   $-$16.7	&	0.9\\
	&	51969.249	&	   $-$26.3	&	0.7\\
	&	51974.266	&	   $-$26.1	&	0.7\\
	&	51976.296	&	   $-$26.5	&	0.7\\
	&	52142.432	&	   $-$25.2	&	0.8\\
	&	52199.623	&	   $-$18.0	&	0.7\\
	&	52205.634	&	   $-$17.3	&	0.7\\
	&	52350.275	&	   $-$23.1	&	0.6\\
	&	52356.278	&	   $-$23.6	&	0.7\\ \hline
V0401 Cep	&	51887.312	&	 $-$2.6	&	0.8\\
	&	51887.319	&	 $-$1.4	&	0.8\\
  &	51888.228	&	 $-$1.1	&	0.8\\
	&	51892.325	&	 $-$1.9	&	0.8\\
	&	51893.288	&   $-$1.8	&	0.8\\	\hline
BX Lyn	&	51887.583	&	   $-$40.3	&	0.8\\
	&	51888.515	&	   $-$39.5	&	0.8\\
	&	51889.400	&	   $-$40.3	&	0.7\\
	&	51894.528	&	   $-$40.3	&	0.7\\ \hline 
X Mon	      &	51887.483	&	  167.6	&	1.5\\
	      &	51888.493	&	  166.6	&	1.2\\ \hline
V0719 Mon	&	51894.459	&	   13.0	&	0.8\\
	&	51894.467	&	   13.2	&	0.7\\ \hline
V1151 Tau	&	51887.457	&	   32.9	&	0.8\\
	&	51888.371	&	   33.1	&	0.8\\
	&	51888.455	&	   33.3	&	0.8\\
	&	51890.469	&	   32.0	&	0.7\\
	&	51893.423	&	   33.5	&	0.8\\  \hline
AG Tri	&	51887.378	&	       6.3	&	0.9\\
	&	51888.480	&	       6.8	&	0.9\\
	&	51890.427	&	       5.6	&	0.8\\
	&	51892.372	&	       8.3	&	1.0\\
	&	51893.325	&	       6.6	&	0.8\\
	&	51894.385	&	       6.0	&	0.9\\\hline
\end{tabular}
\end{center}
\end{table}

\clearpage

{\bf RY Cam} is a SRb type (M3IIIvar) variable with a photometric period of about 135~days. It is seen from Table 1 that its radial velocity is variable, but it is not possible to determine if the variation is periodic as the number of observations is too few. A search in {\it SIMBAD} gave us five more observations (between $-$14 to $-$23 km/s  with much less weight) more than 60 years earlier (Joy,  1942).  It suffices here to note that the radial velocity variation is not compatible with the photometric period of 135~days. 

{\it Hipparcos} discovered an astrometric companion to RY Cam at an angular distance of 0\farcs16 with a position angle of 87 degrees.  Prieur et al. (2002) give these as 0\farcs062$\pm$0\farcs008 and 325 degrees, respectively. However, a preliminary calculation indicated that the radial velocity variation is not likely to be due to an orbital motion but is compatible with radial pulsation with a variation of about 8\% in the radius (Aslan \& Ye\c{s}ilyaprak, 2002).  More observations are needed to determine the real cause. The star is on an observing program at TUG. 


{\bf Acknowledgements:}
I am grateful to Dr. Julius Sperauskas for his kind help with the observations with the CORAVEL spectrometer attached to the RTT150. I wish to thank TUG for observing time on RTT150.

\references

Aslan, Z. \& Ye\c{s}ilyaprak, C.,  2002, {\it Proceedings of the  XIIIth National   Astronomy Meeting}, September 2-6, Antalya, pp. 219-223 (in Turkish)

Joy, A. H., 1942,  {\it ApJ}, {\bf 96}, 344

Prieur, J. L., Aristidi, E.  et al., 2002, {\it ApJ Suppl}, {\bf 139}, 249
 
Sperauskas, J., Aslan, Z.,  Bartasiute, S., Boyle. R. P., 2002, {\it Baltic Astronomy}, {\bf 11}, 465

Upgren, A., Sperauskas, J., Boyle, R. P., 2002, {\it Baltic Astronomy}, {\bf 11}, 91

\endreferences

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