Astronomy & Astrophysics

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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{5411fig1a.eps}\hspace*{3mm... ...eps}\hspace*{3mm} \includegraphics[width=7.4cm,clip]{5411fig1d.eps} \end{figure}$ Figure 1: CO( $3\rightarrow 2$ ) spectra of the star-forming regions Hubble I, Hubble X, and Holmberg 18 and the stellar emission-line object S28 in NGC 6822, overplotted with the best fitting Gaussian. The black curve indicates the H I emission as derived by de Blok & Walter (2006). Evidently, the molecular gas associated with Hubble I and Holmberg 18 has the same velocity as the neutral gas. The velocity of the molecular gas associated with the stellar object S28 differs from that of the H I. Hubble X was not detected.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5411fig2.eps} \end{figure}$ Figure 2: $^{12}{\rm CO}(3\rightarrow 2)$ map of Hubble V. Each panel shows the brightness temperature $T_{\rm mb}$ as a function of velocity with respect to the Local Standard of Rest (LSR). Some spectra still show some residual variations even after subtracting off a double sinusoidal baseline. Nearest neighbor panels overlap by 8'', i.e. about half of the APEX beam width at this frequency, so that next nearest neighbor panels are roughly independent. The CO source associated with Hubble V is clearly resolved in this map and is extended towards the north-east.
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In the text

$\begin{figure} \par\includegraphics[width=6.3cm,angle=0]{5411fig3.eps} \end{figure}$ Figure 3: Spatial distribution of the CO(3 $\rightarrow$ 2) emission of Hubble V at 18'' resolution (contours) plotted over an H $\alpha$ image (greyscale). The square indicates the region mapped by our APEX observations. The contour values are 1 (which corresponds to 3 $\sigma$ ), 1.5, 2, 2.5, 3.0, and 3.5 K km s^-1. The CO emission is not centered on the H $\alpha$ emission. The positions of the CO clouds MC1 and MC2, identified by Wilson (1994), are indicated in the figure.
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In the text