All Tables

Table 1: Overview of the velocity-integrated intensities ( $\int T_{\rm mb}~{\rm d}v$ in K km s^-1) for the observed line transitions. The frequency is listed in GHz and the lower energy level in cm^-1. The integrated intensity of detected lines with a low S/N-ratio is given between brackets. In case of a non-detection, an upper limit on the integrated intensity is computed as $3\sigma \times$ expected linewidth, with $\sigma$ the noise on the data. A ``-'' indicates lines that were not observed. APEX-data are reported in plain front, JCMT-data are given in italics.
Table 2: Velocity-integrated intensities (in K km s^-1), upper state column densities in cm^-2 calculated using Eq. (2) and critical densites in cm^-3 for the detected multiple-transitions ``parent'' molecules used in the excitation analysis. In a few cases, extra integrated-intensity values (listed in italics) as found in literature are added to perform the excitation analysis. Literature references are given in the footnote.
Table 3: For each target, the first row lists the minimum number density for $n_{{\rm H_2}}$ in cm^-3 as derived using Eq. (4) at $T_{{\rm kin}}$ = 300 K and the second row gives the corresponding maximum radius for the emission regions obtained using the GASTRoNOoM-code. The third row gives the maximum radius for the emitting region calculated using Eq. (6).
Table 4: Stellar parameters used as input for the GASTRoNOoM-code. The terminal velocity, $v_{\infty }$ , is derived from the CO lines; the stellar radius from the stellar luminosity and temperature. The envelope density decreases as $\sim$ r^-2. Literature references are given in the footnote.