Astronomy & Astrophysics

All Tables

Table 1: Observing parameters of the molecular line data: Cols. 1 and 2 indicate the line and transition frequency, followed by the number of points observed, the observing grid and Half Power Beam Width ( HPBW); $\eta _{\rm mb}$ is the main beam efficiency, $T_{\rm sys}$ the double sideband system temperature, $\Delta v_{\rm res}$ denotes the velocity resolution, and $\Delta T_{\rm rms}$ the average rms noise temperature per channel on a $T_{\rm mb}$ scale.
Table 2: ISO LWS flux densities, surface brightnesses, and beam sizes (from Table 4.9 in the ISO-LWS handbook v. 1.2) for the observed FIR lines in S 106 IR and S 106 West. ^*The [O I] 63 $\mu$ m, [O III] 88 $\mu$ m, and [O I] 145 $\mu$ m lines were each present in two detectors so that we calculated the error from the weighted mean for the flux and brightness. The errors given in the Table reflect the uncertainty from the line fitting process, not the 30% absolute photometry uncertainty for LWS.
Table 3: Intensities and ratios (from the intensities in erg s^-1 cm^-2 sr^-1) of the observed atomic and molecular lines (ISO, KAO, KOSMA). All intensities are reported for 55'' angular resolution, higher angular resolution data have been smoothed. Beam filling effects therefore to first order cancel out for the line ratios. ^*For these offsets, the [C I] 1 $\to$ 0 line intensities and [C I] 1 $\to$ 0/CO 4 $\to$ 3 ratios are lower limits, and the [C I] 2 $\to$ 1/1 $\to$ 0 ratios upper limits due to possible self-chopping effects in the 1 $\to$ 0 line.
Table 4: Excitation conditions (excitation temperature, opacity, column density) derived from the observed FIR- and (sub)mm lines listed in Table 3 along a cut through S 106 IR. The last line gives the relative amount of material in each of the main carbon phases. ^*These values are lower limits since the beam filling is not known. ⁺Upper limit for $T_{\rm ex}$ , adapted from high-J CO line ratio (Sect. 4.2).