Charting circumstellar chemistry of carbon-rich asymptotic giant branch stars - III. SiO and SiS abundances

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Table 1

Basic source properties.

Source	${\dot{M}}_{H_{2}}$ $Mathematical equation: $\[\dot{M}_{\mathrm{H}_{2}}\]$$ ^(a) (M_⊙ yr⁻¹)	Distance^(b) (pc)	v_sys (LSRK, km s⁻¹)	v_∞ (LSRK, km s⁻¹)	${\dot{M}}_{H_{2}} / v_{\infty}$ $Mathematical equation: $\[\dot{M}_{\mathrm{H}_{2}} / v_{\infty}\]$$ (M_⊙ yr⁻¹ km⁻¹ s)
IRAS 15194–5115	2.2 × 10⁻⁵	696	−15.0	21.5	1.0 × 10⁻⁶
IRAS 15082–4808	2.2 × 10⁻⁵	1050	−3.3	19.5	1.1 × 10⁻⁶
IRAS 07454–7112	8.3 × 10⁻⁶	583	−38.7	13.0	6.4 × 10⁻⁷
AFGL 3068	4.2 × 10⁻⁵	1220	−30.0	14.0	3.0 × 10⁻⁶
IRC +10 216	1.5 × 10⁻⁵	190	−26.5	14.5	1.0 × 10⁻⁶

Notes. ${\dot{M}}_{H_{2}}$ $Mathematical equation: $\[\dot{M}_{\mathrm{H}_{2}}\]$$ is the H₂ mass-loss rate, and v_sys and v_∞ denote the systemic and expansion velocities, respectively. The full list of stellar and CSE properties that are inputs to the RT models is given in Paper II (see their Table 3). ^(a)Paper II; ^(b)Andriantsaralaza et al. (2022).

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