All Figures

$\begin{figure}{\resizebox{6cm}{!}{\includegraphics[angle=270]{5306f1a.eps}}\hspa... ...m}\resizebox{2.8cm}{!}{\includegraphics[angle=270]{5306f1b.eps}} } \end{figure}$ Figure 1: a) CO(3-2) integrated intensity observed with APEX toward Cha-MMS1 (cross). The emission integrated over [3.6, 5.8] km s^-1 is shown in greyscale. The blueshifted, less blueshifted and redshifted emissions integrated over [-0.2, 1.0], [1.2, 2.4] and [6.6, 9.8] km s^-1 are plotted as long-dashed, short-dashed and thick contours, respectively. The steps are 3 $\sigma$ , 6 $\sigma$ and 3 $\sigma$ with rms $\sigma$ = 0.13, 0.13 and 0.24 K km s^-1, respectively. The HPBW is shown on the right. The star and square symbols mark the position of near-infrared (Persi et al. 2001) and 3.5 cm sources (Lehtinen et al. 2003). b) CO(3-2) position-velocity diagram along the axis going through IRS 4 and Cha-MMS1. The dotted line indicates the systemic velocity of Cha-MMS1. The other lines show the limits of the velocity ranges used for the contour maps. The logarithmic temperature scale varies from 0.3 to 6 K.
Open with DEXTER

In the text

$\begin{figure}{\resizebox{8.8cm}{!}{\includegraphics[angle=270]{5306f2.eps}} } \end{figure}$ Figure 2: Spectra observed with APEX toward Cha-MMS1 (histogram). Synthetic spectra corresponding to the model of Sect. 3.3 are superimposed (thick line). The hyperfine structure of the N₂H⁺ and N₂D⁺ lines is shown under each spectrum with statistical weighting. The dotted line indicates the systemic velocity assumed for the modeling.
Open with DEXTER

In the text

$\begin{figure}{\resizebox{8.8cm}{!}{\includegraphics[angle=270]{5306f2.eps}} } \end{figure}$	Figure 2: Spectra observed with APEX toward Cha-MMS1 (histogram). Synthetic spectra corresponding to the model of Sect. 3.3 are superimposed (thick line). The hyperfine structure of the N₂H⁺ and N₂D⁺ lines is shown under each spectrum with statistical weighting. The dotted line indicates the systemic velocity assumed for the modeling.
Open with DEXTER