All Tables

Table 1: IRAS 18151-1208 sources characteristics, showing offsets from IRAS position, J2000 coordinates, and velocity in the local standard of rest (Beuther et al. 2002b).
Table 2: List of observational parameters for IRAM 30 m and 22 m Mopra telescopes.
Table 3: Sources extension at 3 $\sigma _{\rm noise}$ , minor-to-major axis ratio b/a, and position angle (PA; counterclockwise angle relative to the north) for each molecular transition observed. When the emission is almost spherical ( $b/a \geq 0.85$ ) PA is uncertain and set to 0 $^\circ$ .
Table 4: Momentum flux of CO (2-1) calculated as in Bontemps et al. (1996).
Table 5: Continuum flux densities of the three cores within IRAS 18151-1208 region.
Table 6: Summary of results from dust continuum emission modeling (above mid-line) and from molecular line emission modeling (below mid-line). The relative uncertainties are at the 3 $\sigma$ level, and theycorrespond to the rms noise propagated through the modeling process.