\documentstyle[12pt,epsf,rotate,fancyheadings,supertabular]{report}


\begin{document}
\begin{center}
\footnotesize
\tablefirsthead{\multicolumn{4}{l}{ {\bf Table 2.} Radial velocities of 
standard stars}  \\ \\ \hline  HD  & HJD     & $V_r$ & $I$ \\
    & (+2449000)&km\,s$^{-1}$&km\,s$^{-1}$ \\ \hline}
\tablehead{\multicolumn{4}{l}{ {\bf Table 2.} (Continued)} \\ \\ \hline  
HD  & HJD     & $V_r$ & $I$ \\
    & (+2449000)&km\,s$^{-1}$&km\,s$^{-1}$ \\ \hline}
\tabletail{\hline}
\begin{supertabular}{r r l r}
693 & 663.367 & 15.12 &0.28\\
693 & 692.408 & 15.99 & 0.48\\
693 & 693.411 & 15.57 &0.28\\
    &    $\overline{V_{r}}=$     & 15.44$\pm$0.36&\\
\\
22484 & 663.507 & 27.59 &0.28\\
22484 & 663.528 & 27.97 & 0.48\\
22484 & 665.610 & 28.11 &0.28\\
22484 & 689.403 & 27.45 &0.28\\
22484 & 689.450 & 28.05 & 0.48\\
22484 & 692.473 & 27.73 &0.28\\
22484 & 692.544 & 27.07 & 0.48\\
22484 & 693.546 & 28.62 &0.28\\
    &   $\overline{V_{r}}=$      & 27.86$\pm$0.44&\\
\\
89449 & 470.375 & 6.07 &0.28\\
89449 & 471.311 & 6.13 &0.28\\
89449 & 472.383 & 5.04 & 0.48\\
89449 & 472.433 & 6.87 & 0.69\\
89449 & 473.347 & 5.39 &0.28\\
89449 & 474.319 & 6.19 &0.28\\
89449 & 505.366 & 6.49 &0.28\\
89449 & 506.346 & 5.83 &0.28\\
89449 & 507.345 & 4.69 &0.28\\
89449 & 509.356 & 6.03 &0.28\\
89449 & 663.674 &  5.62 & 0.48\\
89449 & 692.618 &  5.88 &0.28\\
89449 & 692.681 &  5.65 &0.28\\
89449 & 693.668 &  5.72 & 0.48\\
89449 & 693.722 &  6.13 &0.28\\
    &       $\overline{V_{r}}=$  & 5.84$\pm$0.52&\\
\\
114762 & 470.503 & 47.51 & 0.48\\
114762 & 471.411 & 47.38 &0.28\\
114762 & 472.526 & 47.75 & 0.48\\
114762 & 473.420 & 48.02 &0.28\\
114762 & 474.432 & 48.01 &0.28\\
    &      $\overline{V_{r}}=$   & 47.77$\pm$0.26&\\
\\
136202 & 470.593 & 54.33 & 0.48\\
136202 & 471.499 & 54.22 & 0.48\\
136202 & 472.597 & 54.16 & 0.48\\
136202 & 473.555 & 54.30 & 0.48\\
136202 & 474.504 & 54.37 &0.28\\
136202 & 505.503 & 54.89 & 0.48\\
136202 & 506.474 & 54.93 & 1.56\\
136202 & 508.381 & 54.48 & 0.48\\
    &    $\overline{V_{r}}=$     & 54.39$\pm$0.27\\
\\
187691 & 470.642 &  -0.58 &0.28\\
187691 & 471.638 &  -0.07 &0.28\\
187691 & 472.638 &  \ 0.21 &0.28\\
187691 & 473.640 &  -0.01 & 0.48\\
187691 & 474.639 & -0.86 &0.28\\
187691 & 505.598 & \ 0.23 &0.28\\
187691 & 506.558 & -0.08 & 0.48\\
187691 & 507.599 & -0.39 &0.28\\
187691 & 509.501 & -1.30 & 0.48\\
    &   $\overline{V_{r}}=$      &  -0.27$\pm$0.49&\\
\\
222368 & 663.287 &  4.76 &0.28\\
222368 & 663.395 &  5.67 &0.28\\
222368 & 689.321 &  4.98 & 0.48\\
222368 & 690.296 &  4.39 &0.28\\
222368 & 692.320 &  5.23 &0.28\\
222368 & 693.300 &  5.62 &0.28\\
    &   $\overline{V_{r}}=$      & 5.12$\pm$0.45&\\
\end{supertabular}
\end{center}

\newpage
\begin{center}
\footnotesize
\tablefirsthead{\multicolumn{4}{l}{ {\bf Table 3.} Radial velocities of A and
 F giants}  \\ \\ \hline  HD  & HJD     & $V_r$ & $I$ \\
    & (+2449000)&km\,s$^{-1}$&km\,s$^{-1}$ \\ \hline}
\tablehead{\multicolumn{4}{l}{ {\bf Table 3.} (Continued)} \\ \\ \hline  HD  
& HJD     & $V_r$ & $I$ \\
    & (+2449000)&km\,s$^{-1}$&km\,s$^{-1}$ \\ \hline}
\tabletail{\hline}
\begin{supertabular}{r r r r}
1671 & 663.445 & 10.53 & 0.48\\
1671 & 689.354 & 10.55 & 0.28\\
1671 & 693.444 & 10.34 & 0.48\\
\\
2628 & 663.451 &  -10.86 &0.28\\
2628 & 689.366 &  -10.67 &1.12\\
2628 & 693.448 &  -10.40 &0.28\\
\\
4338 & 663.410 &  2.08 & 0.69\\
4338 & 689.381 & -0.47 & 1.34\\
4338 & 693.470 &  5.84 & 0.94\\
\\
6706 & 663.426 & 23.81 &0.28\\
6706 & 692.487 & 23.57 & 0.69\\
\\
10845 & 663.458 &  -13.97 & 0.48\\
10845 & 689.412 &  -13.67 & 0.90\\
\\
11522 & 663.436 &  1.16 & 0.69\\
11522 & 693.514 &  1.99 & 1.34\\
\\
12573 & 663.471 &  8.62 & 0.69\\
12573 & 692.522 &  7.38 & 0.90\\
\\
17584 & 689.423 & 18.41 & 0.94\\
17584 & 663.481 & 18.60 & 0.90\\
17584 & 692.387 & 19.42 & 0.69\\
\\
17918 & 663.491 & 17.21 & 0.48\\
17918 & 663.552 & 18.40 & 0.69\\
17918 & 689.434 & 17.11 & 0.90\\
17918 & 692.396 & 18.08 & 0.90\\
\\
21770 & 663.500 &  -46.18 &0.28\\
21770 & 689.444 &  -46.35 & 0.48\\
21770 & 692.469 &  -46.01 &0.28\\
\\
24832 & 663.538 & 20.61 & 1.56\\
24832 & 692.433 & 18.20 & 0.90\\
24832 & 693.569 & 22.67 & 0.69\\
\\
30020 & 663.570 & 34.31 & 0.69\\
30020 & 692.567 & 37.19 & 0.48\\
30020 & 693.609 & 37.87 & 0.90\\
\\
34045 & 663.591 & 29.89 & 0.48\\
34045 & 689.467 & 26.19 & 0.94\\
34045 & 692.587 & 29.18 & 0.48\\
\\
48737 & 663.606 & 26.12 & 0.90\\
48737 & 665.620 & 26.30 & 0.48\\
48737 & 689.459 & 25.77 & 0.48\\
48737 & 692.598 & 27.35 & 0.69\\
48737 & 693.630 & 27.56 & 0.48\\
\\
50019 & 663.611 & 31.17 & 0.69\\
50019 & 664.643 & 30.75 & 0.69\\
50019 & 665.626 & 30.30 & 0.69\\
50019 & 692.601 & 30.04 & 0.69\\
50019 & 693.633 & 32.39 & 0.90\\
\\
60489 & 663.617 & 52.67 & 0.69\\
60489 & 665.645 & 53.42 & 0.69\\
60489 & 692.608 & 30.81 & 0.48\\
60489 & 693.650 & 31.65 &0.28\\
\\
62437 & 663.627 & 11.13 & 0.48\\
62437 & 665.677 & 14.46 & 1.34\\
62437 & 692.628 & 15.99 &0.28\\
62437 & 693.639 & 14.12 & 0.69\\
\\
69997 & 663.642 & 31.67 &0.28\\
69997 & 692.641 & 32.79 &0.28\\
69997 & 692.703 & 33.18 &0.28\\
69997 & 693.661 & 32.59 &0.28\\
\\
82043 & 663.652 & 12.25 & 0.48\\
82043 & 692.649 &  1.73 & 0.69\\
82043 & 692.712 &  1.41 & 0.69\\
82043 & 693.679 &  0.14 & 0.48\\
\\
84607 & 663.660 & 13.65 & 0.48\\
84607 & 692.660 & 12.25 & 0.69\\
84607 & 692.723 & 13.50 & 0.69\\
84607 & 693.690 & 13.09 & 0.48\\
\\
86611 & 663.688 & 26.47 & 0.90\\
86611 & 692.669 & 24.42 & 0.90\\
86611 & 692.732 & 25.79 & 0.69\\
86611 & 693.699 & 25.04 & 1.34\\
\\
89025 & 692.676 &  -21.20 & 0.69\\
89025 & 693.710 &  -22.07 &0.28\\
\\
92787 & 692.689 &  4.47 & 0.90\\
92787 & 692.692 &  4.47 & 0.90\\
92787 & 693.715 &  3.82 & 0.48\\
\\
100418 & 470.406 & 1.02 & 0.69\\
100418 & 471.327 & 0.76 & 0.58 \\
100418 & 471.390 & -0.57 & 0.69\\
100418 & 472.398 & 2.28 &0.28\\
100418 & 473.336 & 0.22 & 0.69\\
100418 & 474.359 & -1.81 & 0.48\\
100418 & 506.372 & -0.28 &0.28\\
\\
103313 & 470.461 & 16.10 & 0.69\\
103313 & 471.340 & 16.75 & 0.48\\
103313 & 471.463 & 14.71 &0.28\\
103313 & 472.413 & 19.14 & 0.90\\
103313 & 473.359 & 17.59 & 0.69\\
103313 & 473.440 & 17.88 & 0.90\\
103313 & 474.378 & 16.54 & 0.69\\
103313 & 474.414 & 16.72 & 0.48\\
103313 & 505.387 & 22.17 & 1.56\\
103313 & 507.364 & 18.64 & 0.48\\
103313 & 507.397 & 15.74 & 2.01\\
\\
104827 & 470.475 & 10.21 & 0.48\\
104827 & 471.352 & 8.07& 0.90\\
104827 & 471.399 & 7.33 & 0.48\\
104827 & 472.443 & 7.70 & 0.48\\
104827 & 473.373 & 7.60 & 0.48\\
104827 & 473.482 & 8.42 & 0.48\\
104827 & 474.332 & 7.37 & 0.69\\
104827 & 474.479 & 6.93 & 0.48\\
104827 & 506.394 & 8.89 & 0.48\\
\\
108382 & 470.486 & -2.33 & 0.48\\
108382 & 471.364 & -1.97 & 0.48\\
108382 & 471.471 & -1.82 & 0.48\\
108382 & 472.457 & -2.86 & 0.69\\
108382 & 473.383 & -1.97 & 0.90\\
108382 & 473.430 & -2.71 & 0.69\\
108382 & 474.345 & -1.55 & 0.90\\
108382 & 474.446 & -1.89 & 0.90\\
\\
118295 & 470.535 &   -20.00 & 0.69\\
118295 & 471.375 &   -19.63 & 0.69\\
118295 & 471.447 &   -17.52 & 1.56\\
118295 & 472.470 &   -20.59 & 0.69\\
118295 & 473.401 &   -18.46 & 0.94\\
118295 & 474.394 &   -17.76 & 0.69\\
118295 & 505.410 &  -24.23 & 0.94\\
118295 & 506.420 &   -19.84 & 1.34\\
\\
122703 & 470.522 &   -17.63 & 0.69\\
122703 & 471.430 &   -13.34 & 0.90\\
122703 & 471.485 &   -21.60 & 0.69\\
122703 & 472.509 &   -19.21 & 2.01\\
122703 & 473.455 &   -15.39 & 0.69\\
122703 & 474.464 &   -17.16 & 0.94\\
\\
150453 & 471.521 & 0.82 & 0.69\\
150453 & 471.620 & 0.47 & 0.69\\
150453 & 472.586 & 0.12 &0.28\\
150453 & 473.541 & 0.64 & 0.48\\
150453 & 474.568 & -0.10 &0.28\\
150453 & 506.486 & 1.54 &0.28\\
\\
150557 & 471.510 &   -49.75 & 0.48\\
150557 & 472.492 &   -49.42 & 0.69\\
150557 & 473.496 &   -48.36 & 0.90\\
150557 & 474.494 &   -49.64 & 0.69\\
150557 & 474.540 &   -50.22 & 0.48\\
150557 & 505.532 &   -48.20 & 0.48\\
150557 & 506.412 &   -48.49 & 0.94\\
150557 & 506.467 &   -50.15 &0.28\\
150557 & 509.393 &   -49.60 & 0.48\\
\\
155646 & 470.552 & 59.76 & 0.48\\
155646 & 471.535 & 61.08 & 0.48\\
155646 & 472.542 & 62.36 & 0.48\\
155646 & 473.518 & 59.78 &0.28\\

155646 & 474.524 & 58.64 & 0.48\\
155646 & 505.545 & 60.05 & 0.48\\
155646 & 506.445 & 59.95 &0.28\\
155646 & 506.547 & 60.70 &0.28\\
\\
159561 & 470.565 & 10.69 & 0.69\\
159561 & 472.550 & 12.23 & 0.69\\
159561 & 472.631 & 10.25 & 0.94\\
159561 & 473.527 & 12.03 & 0.90\\
159561 & 474.510 & 10.82 & 0.69\\
159561 & 505.431 & 11.46 & 0.90\\
159561 & 506.457 & 10.65 & 0.48\\
159561 & 507.608 & 9.68 & 0.69\\
159561 & 509.446 & 8.29 & 0.48\\
\\
171856 & 470.639 & -5.56 & 2.01\\
171856 & 473.620 & -5.96 & 1.34\\
171856 & 506.584 &   -21.70 & 0.48\\
171856 & 508.544 &   -19.14 & 0.69\\
\\
174866 & 470.625 &   -39.39 & 0.94\\
174866 & 472.615 &   -38.50 & 0.69\\
174866 & 473.606 &   -40.45 & 0.48\\
174866 & 505.585 &   -40.89 & 0.90\\
174866 & 506.571 &   -43.56 & 1.34\\
174866 & 509.521 &   -42.08 & 0.69\\
\\
176971 & 470.575 &   -34.62 & 0.90\\
176971 & 471.553 &   -34.28 & 0.48\\
176971 & 472.559 &   -31.63 & 0.69\\
176971 & 473.560 &   -35.13 & 0.48\\
176971 & 474.579 &   -33.63 & 0.69\\
176971 & 474.625 &   -34.88 & 1.34\\
176971 & 505.461 &   -34.60 & 0.94\\
176971 & 506.517 &   -32.51 & 0.69\\
176971 & 509.414 &   -29.47 & 1.78\\
\\
177392 & 470.608 & 10.13 & 0.48\\
177392 & 471.577 &  9.51 & 1.56\\
177392 & 472.603 & 12.38 & 0.69\\
177392 & 473.580 & 10.12 & 0.90\\
177392 & 474.593 & 6.75 & 0.90\\
177392 & 505.481 & 11.21 & 0.90\\
177392 & 506.502 & 10.31 & 2.01\\
177392 & 508.525 & 6.75 & 0.90\\
177392 & 509.459 & 8.69 &0.28\\
177392 & 509.539 & 7.37 & 0.90\\
\\
178187 & 470.600 &   -24.85 & 0.69\\
178187 & 471.563 &   -24.43 & 0.69\\
178187 & 472.568 &   -24.82 & 0.48\\
178187 & 473.570 &   -25.11 & 0.94\\
178187 & 474.602 &   -24.69 & 0.90\\
178187 & 505.440 &   -24.69 & 0.69\\
178187 & 505.518 &   -25.04 & 0.90\\
178187 & 506.531 &  -25.03 & 0.90\\
178187 & 507.585 &  -22.70 & 0.48\\
178187 & 508.506 &   -23.06 & 0.69\\
\\
186005 & 472.623 &   -40.39 & 1.34\\
186005 & 474.634 &   -39.98 & 0.90\\
186005 & 506.593 &   -39.50 & 0.90\\
186005 & 509.593 &   -42.63 & 0.48\\
\\
187764 & 471.598 & -8.02 & 0.69\\
187764 & 473.589 & -5.96 & 0.48\\
187764 & 474.551 & -8.39 & 0.90\\
187764 & 474.612 & -4.71 & 0.90\\
187764 & 505.560 & -6.14 & 0.69\\
187764 & 506.554 & -3.10 & 0.69\\
187764 & 509.477 & -4.64 & 0.69\\
\\
190172 & 471.628 & 2.82 & 0.48\\
190172 & 473.628 & 6.00 &0.28\\
190172 & 506.602 & 3.11 & 0.48\\
\\
203842 & 663.228 &  -25.94 & 0.69\\
203842 & 665.246 &  -27.74 & 0.48\\
203842 & 690.313 &  -26.43 & 0.69\\
203842 & 692.296 &  -24.73 & 0.90\\
203842 & 693.243 &  -23.22 & 0.48\\
\\
204577 & 663.245 &  -10.45 & 0.48\\
204577 & 693.273 & -8.69 & 0.69\\
\\
205852 & 663.262 &  -31.90 & 0.90\\
205852 & 692.307 &  -31.83 & 0.69\\
205852 & 693.308 &  -32.48 & 0.69\\
\\
209166 & 663.275 &  5.22 &0.28\\
209166 & 692.314 &  6.36 &0.28\\
209166 & 693.322 &  6.82 & 0.48\\
\\
210516 & 663.295 & 10.46 & 0.69\\
210516 & 692.332 & 11.38 & 0.94\\
210516 & 693.339 & 12.16 & 0.94\\
\\
216701 & 663.314 & 12.70 & 0.48\\
216701 & 692.352 & 15.26 & 0.69\\
216701 & 693.355 & 11.36 & 0.48\\
\\
217131 & 663.334 &  -12.12 &0.28\\
217131 & 693.374 &  -11.35 & 0.48\\
\\
219891 & 663.352 & -3.04 & 0.90\\
219891 & 689.338 & -3.01 & 2.01\\
219891 & 693.396 & -0.48 & 0.94\\
\\
224995 & 663.383 &  8.13 & 0.48\\
224995 & 689.302 &  7.14 & 0.90\\
224995 & 693.431 &  7.48 & 0.69\\
\end{supertabular}
\end{center}

\newpage
\footnotesize
\noindent
{\bf Table 6.} Discussion about the duplicity of all photometric 
metallic F giant stars of Hauck  (1986)
 
  
\vspace{5mm}
\begin{minipage}[t]{2cm}HD 1324
\end{minipage}
\begin{minipage}[t]{6.8cm}Single star (Evans et al.,  1964).
\end{minipage}
   
\vspace{3mm}
\begin{minipage}[t]{2cm}HD 2724
\end{minipage}
\begin{minipage}[t]{6.8cm}$\delta$ Scuti (Rodriguez et al., 1994). 
   The $V_{r}$ measurements of Nordstroem \& Andersen (1985) show no variation.
\end{minipage}
    
     
\vspace{3mm}
\begin{minipage}[t]{2cm}HD 4849
\end{minipage}
\begin{minipage}[t]{6.8cm}$\delta$ Scuti (Rodriguez et al., 1994). 
The $V_{r}$ measurements of Nordstroem \& Andersen (1985) show no variation.
\end{minipage}
 
  
\vspace{3mm}
\begin{minipage}[t]{2cm}HD 4919
\end{minipage}
\begin{minipage}[t]{6.8cm} $\delta$ Scuti (Rodriguez et al., 1994).
   As we only have an old $V_{r}$ from the catalogue of Campbell (1913).
    We cannot conclude about the duplicity.
\end{minipage}
     
      
       
\vspace{3mm}
\begin{minipage}[t]{2cm}HD 10845
\end{minipage}
\begin{minipage}[t]{6.8cm} $\delta$ Scuti (Rodriguez et al., 1994).
	Our measurements show no variation.
	\end{minipage}

\vspace{3mm}
\begin{minipage}[t]{2cm}HD 12311
\end{minipage}
\begin{minipage}[t]{6.8cm} From his 15 exposures, Campbell 
(1928) indicated that this star is probably variable. At the 
time, he had only a few broad lines. Catchpole et al. (1982) observed 
no variation from 4 measurements. They obtained a mean radial 
velocity of 15.2 $\pm$3.1 km\,s$^{-1}$. 
\end{minipage}
 
\vspace{3mm}
\begin{minipage}[t]{2cm}HD 13174
\end{minipage}
\begin{minipage}[t]{6.8cm} Campbell (1928) obtained values 
 covering a large interval  [-10,+20 km\,s$^{-1}$]. This 
 dispersion is probably due essentially to a fast rotation 
 ($v\sin i$ =154), nevertheless we cannot exclude a close companion.
  Adams et al. (1929) and Abt (1969) gave coherent velocities of
   about -6 km\,s$^{-1}$. 
\end{minipage}

\newpage
 
\noindent
 {\bf Table 6.} (Continued)
  
   
\vspace{3mm}
\begin{minipage}[t]{2cm}HD 15233
\end{minipage}
\begin{minipage}[t]{6.8cm} The comparison between values obtained 
   by Campbell (1913,1928) and by Buscombe\& Morris (1958) shows 
   that this star must be a binary with a long period. Indeed, these
    authors gave very different radial velocities: one found positive 
    velocities, the others negative velocities, with a very good internal 
    coherence if we consider the high rotation ($v\sin i$ = 106 km\,s$^{-1}$).
     We find a value of $P(\chi^2)$ of 0.08 for the measurements of Buscombe
\& Morris (1958) showing, according to this criterion, that no variation
       is detected on a scale of 700 days. 
	
	\end{minipage}
	 
	\vspace{3mm}
	\begin{minipage}[t]{2cm}HD 17584

\end{minipage}
\begin{minipage}[t]{6.8cm} Our measurements show no variation. 
We obtain a velocity of 18 km\,s$^{-1}$ and Campbell (1913) 14 
km\,s$^{-1}$.
\end{minipage}
 
\vspace{3mm}
\begin{minipage}[t]{2cm}HD 17918
\end{minipage}
\begin{minipage}[t]{6.8cm} Our measurements show no variation 
 as is the case of the measurements of Shajn\& Albitzky (1932). 
\end{minipage}
  
\vspace{3mm}
\begin{minipage}[t]{2cm}HD 30020
\end{minipage}
\begin{minipage}[t]{6.8cm} The measurements made at OHP are 
  compatible with the preceding ones of Adams et al. (1929) and
   Abt (1969). The available values are distributed between 
   34.40 km\,s$^{-1}$ and 41.50 km\,s$^{-1}$ with a characteristic 
   time  variation of about 0.7 km\,s$^{-1}$/day taking into account 
   our measurements of December 1994. The variability is certainly
    due to an orbit because the photometric variations are less 
than 1 mmag in the filter B and V of Johnson (Nelson\& Kreidl 1993).
\end{minipage}
 
\vspace{3mm}
\begin{minipage}[t]{2cm}HD 33276
\end{minipage}
\begin{minipage}[t]{6.8cm}The measurements of Campbell (1928)
  and Abt (1965) show no variation. 
\end{minipage}
   
    
     
\newpage
      
\noindent
      {\bf Table 6.} (Continued)
       
	
	 
	  
	\vspace{3mm}
	\begin{minipage}[t]{2cm}HD 34045
	\end{minipage}
\begin{minipage}[t]{6.8cm}If we put together our measurements 
and those of  Nordstroem et al. (1985), the velocity varies between
 26.32 and 34.70 km\,s$^{-1}$. The characteristic time of variation 
 is 0.95 km\,s$^{-1}$/day for our measurements (3 days between
  two measurments) and 0.91 km\,s$^{-1}$/day for Nordstroem et al. (1985)
   (5 days between two measurements). As this star is not known as a 
   $\delta$ Scuti, we think it is a tight binary. 
    
\end{minipage}
     
      
\vspace{3mm}
\begin{minipage}[t]{2cm}HD 40455
\end{minipage}
\begin{minipage}[t]{6.8cm}For this star, we have only 3 
      measurements of Nordstroem et al. (1985) on a scale of 300 
      days. The $P(\chi^2)$ is 0.74 and so this star is probably 
      not a tight binary.
       
\end{minipage}
	
	 
	\vspace{3mm}

\begin{minipage}[t]{2cm}HD 43905
\end{minipage}
\begin{minipage}[t]{6.8cm}SB1 with a period of 6.5 days
 (Mayor\& Mazeh 1987).
\end{minipage}
  
\vspace{3mm}
\begin{minipage}[t]{2cm}
  HD 59881
\end{minipage}
\begin{minipage}[t]{6.8cm}
  The $P(\chi^2)$ is 0.06 and 0.13 for the measurements of 
   Frost et al. (1929) et Penfold (1971) respectively. So 
   this star is probably not a binary with a small period.
\end{minipage}
    
\vspace{3mm}
\begin{minipage}[t]{2cm}
    HD 61064
\end{minipage}
\begin{minipage}[t]{6.8cm}
    If we put together the measurements of Campbell (1913,1928) and those of Shajn 
\& Albitzky (1932), the mean value of the radial velocity is 45.72 km\,s$^{-1}$ 
with a dispersion of 1.72 km\,s$^{-1}$, so we observe no tangible variation.
\end{minipage}
 
\vspace{3mm}
\begin{minipage}[t]{2cm}
 HD 61110
\end{minipage}
\begin{minipage}[t]{6.8cm}
 The measurements taken from Campbell (1913,1928), Harper (1937), Buscombes\&
  Morris (1958), Abt (1969) give a mean radial velocity of 6.5 km\,s$^{-1}$ and a
  dispersion of 3.5 km\,s$^{-1}$ for 13 data. The dispersion is not so large if 
  we consider the quiet large rotational velocity (90 km\,s$^{-1}$). So this star
  is probably not a tight binary.
\end{minipage}
   
    
\newpage
     
\noindent
     {\bf Table 6.} (Continued)

\vspace{3mm}
\begin{minipage}[t]{2cm}
HD 69997
\end{minipage}
\begin{minipage}[t]{6.8cm}
$\delta$ Scuti (Rodriguez et al., 1994). Our measurements allow to detect
 intrinsic variations but no orbital motion.
\end{minipage}
  
\vspace{3mm}
\begin{minipage}[t]{2cm}
  HD 79940
\end{minipage}
\begin{minipage}[t]{6.8cm}
  Single star (Evans et al., 1961). This star is noted SB in the BSC. This probably
   comes from Abt\& Biggs (1972). Indeed, in addition to the authors mentioned above  
   who find a radial velocity of $2.2\pm 1.5$ km\,s$^{-1}$, they list Campbell (1928, p. 143) 
   who found a radial velocity of 12 km\,s$^{-1}$ based on 3 measurements. The large rotational 
   velocity probably explains the discrepancy.
\end{minipage}
   
    
\vspace{3mm}
\begin{minipage}[t]{2cm}
    HD 84607
\end{minipage}
\begin{minipage}[t]{6.8cm}
    We detect no variation of this star at OHP. We obtain a mean radial velocity
     of 13 km\,s$^{-1}$ which is compatible with the value of 16.3 $\pm$ 2 given
      by Shajn\& Albitzky (1932). Wilson \& Joy (1950) and Abt (1969) both found
	important fluctuations of velocity, which are spurious, probably due to the
	 rotation. In both cases, the mean value is 13.4 km\,s$^{-1}$. The SB
	  notation in the BSC seems to be a premature decision.
	\end{minipage}

\vspace{3mm}
\begin{minipage}[t]{2cm}
HD 85040
\end{minipage}
\begin{minipage}[t]{6.8cm}
$\delta$ Scuti (Rodriguez et al., 1994). SB2 with a period of 4.14 
days (Rosvick\& Scarfe 1991)
\end{minipage}

\newpage
 
\noindent
 {\bf Table 6.} (Continued)

\vspace{3mm}
\begin{minipage}[t]{2cm}
HD 89025
\end{minipage}
\begin{minipage}[t]{6.8cm}
The data since the beginning of the century show a radial velocity 
variation about 50 km\,s$^{-1}$, but no short-term variation is detected,
 so it is probably not a tight binary as is suggested in the BSC.
  Indeed, apart from the values of Henroteau (1923) who obtained a
   mean velocity of about -54 km\,s$^{-1}$, the others have radial 
   velocities between -30 and 0 km\,s$^{-1}$ with a mean of -17 km\,s$^{-1}$.
    This scatter is probably due both to the quite large $v\sin i$  
    (81 km\,s$^{-1}$) and the low dispersion of the spectra ( $\approx$ 30\AA/mm).
     The computation of the $P(\chi^2)$ gives 0.88 and 0.53 for the measurements
      of Jones\& Haslam (1969) and Wooley et al. (1971) respectively, and 0 for
       the old measurements of Abt (1969). Our radial velocities are compatible 
       with those of Adams et al. (1929) who obtained -19.3 $\pm$ 2.9.
\end{minipage}
	
	\vspace{3mm}
	\begin{minipage}[t]{2cm}
	HD 89254
	\end{minipage}
\begin{minipage}[t]{6.8cm}
The measurements given by Adams et al. (1929), Buscombes\& Morris 
(1958), Abt (1969) and Evans et al. (1961) suggest a constant radial 
velocity ($\overline{V_{r}}=15.8\pm 4.4$). This dispersion is 
compatible with a rotational velocity of 76 km\,s$^{-1}$.
\end{minipage}
 
\vspace{3mm}
\begin{minipage}[t]{2cm}
 HD 90277
\end{minipage}
\begin{minipage}[t]{6.8cm}
 This star shows no variation. The mean velocity is 13.6 km\,s$^{-1}$
  with a dispersion of 2.7 km\,s$^{-1}$ from the 36 measurements 
  taken from 9 different authors.
\end{minipage}
   
    
\vspace{3mm}
\begin{minipage}[t]{2cm}
    HD 90454
\end{minipage}
\begin{minipage}[t]{6.8cm}

From the measurements of Cannon (1920) and those of Nordstroem 
\& Andersen (1985), the $P(\chi^2)$ is 0.31 and 0.03 respectively
 and so it is probably not a binary. 
\end{minipage}
  
\vspace{3mm}
\begin{minipage}[t]{2cm}
  HD 105841
\end{minipage}
\begin{minipage}[t]{6.8cm}
  Single star (Evans 1966).
\end{minipage}

\newpage
 
\noindent
 {\bf Table 6.} (Continued)

\vspace{3mm}
\begin{minipage}[t]{2cm}
HD 108722
\end{minipage}
\begin{minipage}[t]{6.8cm}
SB1 with a period of 17.954 days (Abt\& Levy 1976)
\end{minipage}
 
\vspace{3mm}
\begin{minipage}[t]{2cm}
 HD 110318
\end{minipage}
\begin{minipage}[t]{6.8cm}
 SB2 with a period of 44.4 days (Sanford\& Karr 1942)
\end{minipage}
  
\vspace{3mm}
\begin{minipage}[t]{2cm}
  HD 115604
\end{minipage}
\begin{minipage}[t]{6.8cm}
  $\delta$ Scuti (Rodriguez et al., 1994). On a time span of about
   130 days, M.A. Smith (1982) observes a variation of radial
 velocity of 6.2 km\,s$^{-1}$.
 Such a variation is probably due to pulsation only.
\end{minipage}
  
\vspace{3mm}
\begin{minipage}[t]{2cm}
  HD 125150
\end{minipage}
\begin{minipage}[t]{6.8cm}
  Single star (Evans et al. 1964).
\end{minipage}

\vspace{3mm}
\begin{minipage}[t]{2cm}
HD 126251
\end{minipage}
\begin{minipage}[t]{6.8cm}
Single star (Wilson\& Joy 1950).
\end{minipage}
 
\vspace{3mm}
\begin{minipage}[t]{2cm}
 HD 147547
\end{minipage}
\begin{minipage}[t]{6.8cm}
 Radial velocities are distributed between -60 and -30 km\,s$^{-1}$
  with a mean of about -44 km\,s$^{-1}$. The large dispersion is
   probably due to the fast rotation of 145 km\,s$^{-1}$, nevertheless 
   we cannot exclude a contribution of a companion.
\end{minipage}
    
\vspace{3mm}
\begin{minipage}[t]{2cm}
    HD 157919
\end{minipage}
\begin{minipage}[t]{6.8cm}
    It shows no variation. The mean radial velocity is 37.2$\pm$2.4 km\,s$^{-1}$ 
    for 14 measurements taken from Campbell (1913), Campbell (1928),
     Shajn\& Albitzky (1932), Evans et al. (1957)
\end{minipage}
      
       
	
	\vspace{3mm}
	\begin{minipage}[t]{2cm}
	HD 177392
	\end{minipage}
	\begin{minipage}[t]{6.8cm}
	$\delta$ Scuti (Rodriguez et al., 1994). Our measurements allow
	 to detect intrinsic variations but no orbital motion.
	\end{minipage}
	  
	\newpage
	   
	\noindent
	   {\bf Table 6.} (Continued)

\vspace{3mm}
\begin{minipage}[t]{2cm}HD 177482
\end{minipage}
\begin{minipage}[t]{6.8cm}
$\delta$ Scuti (Rodriguez et al., 1994). Campbell (1928) obtains
 values covering a large interval [+3,+26 km\,s$^{-1}$] with the
  remark ``poor lines'' and Neubauer (1930) gives a value of 6.5 
  km\,s$^{-1}$. With these old values, it is difficult to say
   anything about the duplicity.
\end{minipage}
    
\vspace{3mm}
\begin{minipage}[t]{2cm}
    HD 181333
\end{minipage}
\begin{minipage}[t]{6.8cm}
    $\delta$ Scuti (Rodriguez et al., 1994). On a time span of about
     38 days, M.A. Smith (1982) observes a variation of radial 
     velocity of 4.7 km\,s$^{-1}$.
     Such a variation is probably due to pulsation only.
\end{minipage}
      
\vspace{3mm}
\begin{minipage}[t]{2cm}
HD 196524
\end{minipage}
\begin{minipage}[t]{6.8cm}
Binary star with a probable period of 26.65 years (Abt\& Levy 1976).
 So it will not be integrated in the sample of close binaries. 
\end{minipage}
  
\vspace{3mm}
\begin{minipage}[t]{2cm}
  HD 205852
\end{minipage}
\begin{minipage}[t]{6.8cm}
  From the $P(\chi^2)$ value, the measurements of Frost et al. (1929),
   Jones\& Haslam (1969) and this paper show no variations.
\end{minipage}
    
\vspace{3mm}
\begin{minipage}[t]{2cm}
    HD 208741
\end{minipage}
\begin{minipage}[t]{6.8cm}
    Single star (Buscombe\& Morris 1958 and Evans et al. 1964).

\end{minipage}
     
\vspace{3mm}
\begin{minipage}[t]{2cm}
     HD 214441
\end{minipage}
\begin{minipage}[t]{6.8cm}
     $\delta$ Scuti with a variation of 0.05 mag in visual magnitude
      (Rodriguez et al., 1994). Nordstroem \& Andersen (1985) find a 
      $\Delta V_r$ of about 10 $kms^{-1}$ and  we then obtain a ratio
       of 200 $kms^{-1}mag^{-1}$ which is large in comparison with 
       the value of 92 $kms^{-1}mag^{-1}$ given by Breger (1979). 
       We cannot therefore exclude a companion for this star.
\end{minipage}


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\end{document}
