All Figures

$\begin{figure} \par\includegraphics[angle=270,width=18cm,clip]{ms3001f1.eps} \end{figure}$ Figure 1: Channel maps of the BP Tau $^{12}{\rm CO}$ $J=2\!\!\rightarrow\!\! 1$ emission, at 0.8 km s^-1 resolution, with the LSR velocity (in $~{\rm km~s}^{-1}$ ) indicated in the upper left corner of each panel. The continuum emission has been subtracted. Contour levels are in steps of 25 mJy/beam, or 0.61 K (approximately 2 $\sigma$ ), with the zero level omitted. The cross indicates the orientation of the disk.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{ms3001f2.eps} \end{figure}$ Figure 2: Integrated $^{12}{\rm CO}$ $J=2\!\!\rightarrow\!\! 1$ emission and 1.3 mm continuum emission towards BP Tau. Left: Integrated $^{12}{\rm CO}$ $J=2\!\!\rightarrow\!\! 1$ emission; contour step is 60 mJy km s^-1/beam. Right: 1.3 mm continuum emission; contour step is 3 mJy/beam.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3001f3.eps} \end{figure}$ Figure 3: Spectra of $^{12}{\rm CO}$ and $^{13}{\rm CO}$ $J=2\!\!\rightarrow\!\! 1$ towards BP Tau. From top to bottom: a) $^{12}{\rm CO}$ $J=2\!\!\rightarrow\!\! 1$ observed in frequency switch (thin spectrum) and wobbler switch (shaded spectrum); b) $^{13}{\rm CO}$ $J=2\!\!\rightarrow\!\! 1$ spectra in frequency switch (thin spectrum) and wobbler switch (shaded spectrum); c) superposition of the $^{12}{\rm CO}$ $J=2\!\!\rightarrow\!\! 1$ integrated spectrum from the PdB observations (grey shaded histogram with errorbars) and the wobbler switch $^{12}{\rm CO}$ $\;$ $J=2\!\!\rightarrow\!\! 1$ spectrum obtainedwith the 30-m (dark grey shaded histogram); d) superposition of the $^{12}{\rm CO}$ $J=2\!\!\rightarrow\!\! 1$ integrated spectrum from the PdB observations (grey shaded histogram with error bars) and the wobbler switch $^{13}{\rm CO}$ $J=2\!\!\rightarrow\!\! 1$ spectrum obtained with the 30-m (dark grey shaded histogram). Comparison between PdBI and 30-m data shows that emission from the disk is free of confusion outside the velocity range $[5.9{-}8.9]~{\rm km~s}^{-1}$ (which is given by the thin vertical lines).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{ms3001f4.eps} \end{figure}$ Figure 4: $\chi ^2$ surfaces for pairs of parameters. Contours are spaced by 1 $\sigma$ , with the $3~\sigma$ and $6 \sigma$ contours in thick lines. The 3 curves on panel b) correspond to stellar masses of 0.96, 1.32 and 1.92 $~{M}_{\odot}$ , corresponding to $\pm$ $3\sigma$ on the stellar mass determination.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{ms3001f5.eps} \end{figure}$ Figure 5: The location of BP Tau in the (L/M² vs. $T_{\rm eff}$ ) diagram using the two extreme dynamical mass determinations in this work (for q=-0.1 (filled circle) and q=0.3 (open circle)). The theoretical evolutionary tracks are presented in the same way as in Fig. 3 of SDG. Upper left-hand panel: Tracks calculated by d'Antona & Mazzitelli (1997) for stars of mass 0.1, 0.2, 0.3, 0.4, 0.5, 0.6, 0.7, 0.8, 0.9, 1.0, and 1.2 $~{M}_{\odot}$ ; the dots indicate ages 1, 2, 3, 5, 7, and 10 Myr. Upper right-hand panel: Same but for tracks calculated by Baraffe et al. (1998); the dots indicate ages 2, 3, 5, 7, and 10 Myr. Lower left: Same but for calculations by Palla & Stahler (1999) for stars of mass 0.1, 0.2, 0.4, 0.6, 0.8, 1.0, and 1.2 $~{M}_{\odot}$ at indicated ages 1, 2, 3, 5, and 10 Myr. Lower right: Same for calculations by Siess et al. (2000) for the same masses and ages as in the upper left.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{ms3001f2.eps} \end{figure}$	Figure 2: Integrated $^{12}{\rm CO}$ $J=2\!\!\rightarrow\!\! 1$ emission and 1.3 mm continuum emission towards BP Tau. Left: Integrated $^{12}{\rm CO}$ $J=2\!\!\rightarrow\!\! 1$ emission; contour step is 60 mJy km s^-1/beam. Right: 1.3 mm continuum emission; contour step is 3 mJy/beam.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=18cm,clip]{ms3001f4.eps} \end{figure}$	Figure 4: $\chi ^2$ surfaces for pairs of parameters. Contours are spaced by 1 $\sigma$ , with the $3~\sigma$ and $6 \sigma$ contours in thick lines. The 3 curves on panel b) correspond to stellar masses of 0.96, 1.32 and 1.92 $~{M}_{\odot}$ , corresponding to $\pm$ $3\sigma$ on the stellar mass determination.
Open with DEXTER