All Tables

Table 1: Observed molecules together with the observing parameters. The critical densities ( $n_{\rm cr}$ ) are computed for temperatures between 50 and 100 K using the collisional coefficients quoted in Sect. 4. The area mapped ( $\Delta \alpha \times \Delta \delta$ ) in each transition and the sampling of the map are reported in the last two lines. $B_{\rm eff}$ is the beam efficiency of the telescope. The symbol "-'' implies that only observations towards the "key'' positions have been obtained.
Table 2: Line parameters ( $T_{\rm MB}$ (K), $\Delta$ v (km s^-1), $v_{\rm LSR}$ (km s^-1), $\int T_{\rm MB} \delta v$ (K km s^-1)) for the various transitions observed at the "key'' positions: the two protostars IRAS 16293 and 16293E, the shocked regions E1, E2, W1, W2 and HE2, and the reference position in the cloud. The SiO observations were previously published in CCLCL01. When no signal is detected, we give an upper limit for the intensity equal to 3 RMS of the relevant spectrum. The parameters are taken from the spectra not smoothed. The symbol "-'' implies that the relevant transition has not been observed or detected.
Table 3: Gas temperature and density, and column densities of SO, SO₂, H₂S, SiO and $\rm H_{2}CO$ in six "key'' positions. The column densities are beam-averaged in the shocked regions (on 27'' for SiO, 26'' for H₂CO, 24'' for SO, 18'' for SO₂ and 25'' for H₂S), whereas they are corrected from the beam dilution in IRAS 16293. Errors on the estimates are around 15% if considering only the statistical uncertainties. However, a factor two of uncertainty has to be considered, when the uncertainty on the density and temperature of the emitting gas is considered.
Table 4: Abundances in molecular clouds. References: L1689N: SO, SO₂ and H₂S from this work, SiO from Ceccarelli et al. (2000b) and H₂CO from Ceccarelli et al. (2001); L134N: SO and SO₂ abundances from Swade (1989), H₂S from Minh et al. (1989), SiO from Ziurys et al. (1989), $\rm H_{2}CO$ from Ohishi et al. (1992); TCM-1: SO abundances from Hirahara et al. (1995) and Pratap et al. (1997), SO₂from Irvine et al. (1983), H₂S from Minh et al. (1989), SiO from Ziurys et al. (1989), $\rm H_{2}CO$ from Ohishi & Kaifu (1998).
Table 5: Abundances of SO, SO₂, H₂S, SiO and H₂CO with respect to H₂ in the hot core of IRAS 16293. The abundances of SO, SO₂ and H₂S are estimated by the present work observations, assuming a H₂ column density of $7.5 \times 10^{22}~\rm cm^{-2}$ (Ceccarelli et al. 2000a). The SiO and H₂CO abundances are taken from Ceccarelli et al. (2000a,b). References of the other sources: L1157-mm (IRAS 20386+6751): Bachiller & Perez Gutierrez (1997); Orion-KL: SO, SO₂, SiO and H₂CO from Sutton et al. (1995), H₂S from Minh et al. (1990); G10.47, G29.96, G75.78, G9.62, G12.21, G31.41 and G34.26: Hatchell et al. (1998); BF-Class 0: Buckle & Fuller (2003).
Table 6: Abundance ratios in the shocked regions and in the cloud, as derived from the column densities of Table 3. References for other outflows: L1157-B1 and L1157-B2: Bachiller & Perez Gutierrez (1997); CB3: Codella & Bachiller (1999); L1448, B1 and CepA: Martin-Pintado et al. (1992); NGC 2071: Chernin & Masson (1993).
Table 7: Proposed schema of the formation and destruction of SO, SO₂, H₂S, SiO and H₂CO as function of time. The times are indicative and are meant to represent a sequence.