All Figures

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4706fig1.ps}\end{figure}$ Figure 1: Equivalent width of the Pa $\beta$ emission line for all objects with known $L_\star$ . Circles are Class II sources, filled circles are detections, empty circles with arrows upper limits. Squares are Class III sources. Two objects with $L_\star$ < 0.01 $L_\odot$ and Pa $\beta$ undetected are not plotted.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4706fig2.ps}\end{figure}$ Figure 2: Accretion luminosity from the IR lines as function of $L_\star$ for Class II objects. Dots show $L_{\rm acc}$ measurements from Pa $\beta$ (filled: detections, empty: upper limits); diamonds measurements from Br $\gamma$ (filled: detections, empty: upper limits); The dotted lines show the locus of $L_{\rm acc}$ / $L_\star$ = 0.01, 0.1 and 1, as labelled. Crosses are objects in Taurus (see text for references).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4706fig3.ps}\end{figure}$ Figure 3: Mass accretion rate derived from the IR lines as function of $M_\star$ . Symbols as in Fig. 2. The dashed line shows the relation $\dot M_{\rm acc}$ $\propto$ $M_\star$ ^1.8, derived from a statistical analysis using ASURV; the dotted line plots, for comparison, the relation $\dot M_{\rm acc}$ $\propto$ $M_\star$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4706fig4.ps}\end{figure}$ Figure A.1: Same as Fig. 3 for different ages and evolutionary tracks. The top-left panel is for DM98 0.5 My (as in Fig. 3), the bottom-left for DM98, 1 My, the top right is for Siess (2000) evolutionary tracks at 0.5 My, the bottom right at 1 My. In each panel, the two dotted lines ( $\dot M_{\rm acc}$ $\propto$ $M_\star ^2$ ) have been drawn to guide the eye in the comparison.

In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{4706fig5.ps}\end{figure}$ Figure B.1: Top panel: $\dot M_{\rm acc}$ vs. $M_\star$ for objects in Taurus for which $\dot M_{\rm acc}$ has been obtained from veiling and/or by fitting the H $\alpha$ profiles with magnetospheric accretion models (crosses and squares). Data from Gullbring et al. (1998), Muzerolle et al. (1998b, 2003, 2005), White & Ghez (2001), White & Basri (2003), Calvet et al. (2004). Squares identify objects for which we could find in the literature Pa $\beta$ observations. Diamonds are very low mass objects in Ophiuchus and Chamaeleon with $\dot M_{\rm acc}$ estimates from H $\alpha$ profile fitting (from Natta et al. 2004). Bottom panel: both $M_\star$ and $\dot M_{\rm acc}$ have been derived following the method we use for the Ophiuchus objects in this paper (see text). As in Fig. 3, the two dotted lines show the run of the $\dot M_{\rm acc}$ $\propto$ $M_\star$ ^1.8 and $\dot M_{\rm acc}$ $\propto$ $M_\star$ relationships.

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4706fig1.ps}\end{figure}$	Figure 1: Equivalent width of the Pa $\beta$ emission line for all objects with known $L_\star$ . Circles are Class II sources, filled circles are detections, empty circles with arrows upper limits. Squares are Class III sources. Two objects with $L_\star$ < 0.01 $L_\odot$ and Pa $\beta$ undetected are not plotted.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4706fig3.ps}\end{figure}$	Figure 3: Mass accretion rate derived from the IR lines as function of $M_\star$ . Symbols as in Fig. 2. The dashed line shows the relation $\dot M_{\rm acc}$ $\propto$ $M_\star$ ^1.8, derived from a statistical analysis using ASURV; the dotted line plots, for comparison, the relation $\dot M_{\rm acc}$ $\propto$ $M_\star$ .
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