Astronomy & Astrophysics

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$\begin{figure} \par\includegraphics[width = 8.8cm,clip]{h4174F1.epsi} \end{figure}$ Figure 1: H band (pixel to pixel) detection limits during the observations of HIP 1113 (G6V; V = 8.8) in classical mode during 30 $\times$ 2 s (solid line) and in coronagraphic mode during 15 $\times$ 20 s (dashed line). Filled circles are HIP 1910 B and the CC to HIP 108422 detected in classical mode. The open circle is the CC to GSC 80047-0232 detected in coronagraphy.
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In the text

$\begin{figure} \par\includegraphics[width = 8.8cm,angle=-90,clip]{h4174F2.ps}\end{figure}$ Figure 2: ADONIS/SHARPII AO classical imaging of HIP 108422 and HIP 1910 AB obtained in H-band (linear stretch) and coronagraphic imaging of GSC 8047-0232 and HIP 6856, respectively in K band (linear stretch).
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In the text

$\begin{figure} \par\includegraphics[width=8cm, height=7.5cm,clip]{h4174F3.epsi}\... ...1.2cm} \includegraphics[width=8cm, height=7.5cm,clip]{h4174F4.epsi} \end{figure}$ Figure 3: Left: We show the 1 $\sigma$ error ellipses of the positions of the companion candidate to HIP 6856 relative to HIP 6856 on 12 November 2000 and 29 October 2001. We took into account the proper motion of HIP 6856, starting at ( $\alpha ,\delta )=(0,0)$ and then moving south-east to ( $\alpha ,\delta )=(0.100,-0.042)$ . Regarding the ellipse errors, it is not possible to discriminate between bound or background objects for the HIP 6856 CC. Right: We show the 1 $\sigma$ error ellipses of the position of the companion HIP 1910 B relative to HIP 1910 A on 12 November and 28 October 2001. We took into account proper motions of HIP 1910 A, starting at ( $\alpha ,\delta )=(0,0)$ which then moves south-east to ( $\alpha ,\delta )=(0.081, -0.053)$ . The proper motions of HIP 1910 A and HIP 1910 B are significantly similar. The observed separations and PA are in total similar to $0.12~\sigma$ in the case of a co-moving pair and $1.5~\sigma$ discrepant from being a background object.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{h4174F5.eps}\hspace*{0.8cm} \includegraphics[width=7.8cm,clip]{h4174F6.eps} \end{figure}$ Figure 4: Left: CMD for the near-IR color (J-K) from the BCAH98 model and the CBAH00 DUSTY and COND models. The data of HIP 108422 and its CC, GSC 8047-0232 and its CC and the CC to HIP 6856 are overplotted with their uncertainties and also the sub-stellar companion HR 7329 B detected by Lowrance et al. (2000). In the case of GSC 8047-0232 and its CC, two distances are considered, 60 pc (lower) and 85 pc (upper). Right: CMD for the near-IR color (H-K) from the BCAH98 model. The data of HIP 108422 and its CC, and HIP 1910 A and B are overplotted.
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In the text

$\begin{figure} \par\includegraphics[width = 8.8cm,clip]{h4174F1.epsi} \end{figure}$	Figure 1: H band (pixel to pixel) detection limits during the observations of HIP 1113 (G6V; V = 8.8) in classical mode during 30 $\times$ 2 s (solid line) and in coronagraphic mode during 15 $\times$ 20 s (dashed line). Filled circles are HIP 1910 B and the CC to HIP 108422 detected in classical mode. The open circle is the CC to GSC 80047-0232 detected in coronagraphy.
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$\begin{figure} \par\includegraphics[width = 8.8cm,angle=-90,clip]{h4174F2.ps}\end{figure}$	Figure 2: ADONIS/SHARPII AO classical imaging of HIP 108422 and HIP 1910 AB obtained in H-band (linear stretch) and coronagraphic imaging of GSC 8047-0232 and HIP 6856, respectively in K band (linear stretch).
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