All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{6162_f01.eps}\end{figure}$ Figure 1: Final combined spectrum of SE 70, taken with ISIS/WHT (F $_\lambda$ , 3-pixel smoothing). Top window: whole spectral range. Bottom windows: portions of 20 Å width centred in H $\alpha$ ( left) and Li I ( right). Line identifications are marked with dotted vertical lines. The spectrum has not been corrected for heliocentric or intrinsic radial velocities.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,angle=0]{6162_f02.eps}\end{figure}$ Figure 2: I vs. I-J colour-magnitude diagram showing the $\sigma$ Orionis members fainter than I = 12 mag with spectroscopic features of youth compiled by Caballero (2005), in small open circles, and SE 70 and S Ori 68, in large filled stars. Rough hydrogen (top) and deuterium (bottom) burning mass limits are shown with dotted lines.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,angle=0]{6162_f03.eps}\end{figure}$ Figure 3: Spectral energy distributions of SE 70 from the optical R band to 8.0 $\mu$ m (filled circles, " $\bullet$ '') The spectral energy distributions of two very low-mass cluster members with lithium in absorption and other cluster membership indices are also given for comparison. They are S Ori J053911.4-023333, M $5.0\pm 0.5$ (open circles " $\circ$ ''), and S Ori 45, M $8.5\pm 0.5$ (solar symbol, " $\odot$ '').
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,angle=0,clip]{6162_f04.eps}\end{figure}$ Figure 4: Angular separation to the nearest neighbour vs. separation to the centre of the $\sigma$ Orionis cluster. Small dots represent the star and massive brown-dwarf photometric member candidates in the study by Caballero (in prep.), while the large filled stars represent the SE 70 + S Ori 68 system. Low-mass brown-dwarf and IPMO cluster member candidates are not included. Horizontal lines denote the 90 (dotted) and 95% (solid) confidence limits below which the probabilities for a pair at 5 to 10 arcmin to $\sigma$ Ori A to be a visual alineation are less than 10 and 5%, respectively. There are only two systems below the 95% confidence limit: [W96] 4771-899 AB + C and SE 70 + S Ori 68. The results from 0 to 30 arcmin to the cluster centre and the description of the spatial distribution study will be given in Caballero (in prep.).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{6162_f01.eps}\end{figure}$	Figure 1: Final combined spectrum of SE 70, taken with ISIS/WHT (F $_\lambda$ , 3-pixel smoothing). Top window: whole spectral range. Bottom windows: portions of 20 Å width centred in H $\alpha$ ( left) and Li I ( right). Line identifications are marked with dotted vertical lines. The spectrum has not been corrected for heliocentric or intrinsic radial velocities.
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$\begin{figure} \par\includegraphics[width=8.8cm,angle=0]{6162_f02.eps}\end{figure}$	Figure 2: I vs. I-J colour-magnitude diagram showing the $\sigma$ Orionis members fainter than I = 12 mag with spectroscopic features of youth compiled by Caballero (2005), in small open circles, and SE 70 and S Ori 68, in large filled stars. Rough hydrogen (top) and deuterium (bottom) burning mass limits are shown with dotted lines.
Open with DEXTER