All Tables

Table 1: Data on telescopes and receivers.
Table 2: The effect on the integrated model SiO intensities (in percent), due to changes in various parameters. Three model stars with mass loss rate and gas expansion velocity characteristics typical for our samples are used. They lie at a distance of 250 pc, and have luminosities of 4000 $L_{\odot }$ (the model stars with mass-loss rates of 10^-7 and 10 $^{-6}~M_\odot$ yr^-1) and 8000 $L_{\odot }$ (the model star with a mass-loss rate of 10 $^{-5}~M_\odot$ yr^-1), and blackbody temperatures of 2500 K. The nominal CSE parameters are h=0.2 (for the lowest mass-loss rate model star) and h=0.5 (for the other two model stars), $r_{\rm i}=2\times 10^{14}$ cm, $v_{\rm t}=0.5$ km s^-1, and $f_{\rm SiO}=5\times 10^{-6}$ . The size of the SiO envelope, $r_{\rm e}$ , is given by Eq. (13) for the given mass-loss rate. The SiO J=2 $\rightarrow$ 1, J=3 $\rightarrow$ 2, J=5 $\rightarrow$ 4, and J=6 $\rightarrow$ 5 lines are observed with beam widths of 57 $\hbox {$^{\prime \prime }$ }$ , 38 $\hbox {$^{\prime \prime }$ }$ , 23 $\hbox {$^{\prime \prime }$ }$ , and 19 $\hbox {$^{\prime \prime }$ }$ , respectively (appropriate for a 15 m telescope). The model integrated line intensities, I in K km s^-1, are given for the nominal parameters. For comparison, also the integrated CO line intensities for the model stars are given [for a 15 m telescope; 45 $\hbox {$^{\prime \prime }$ }$ (J=1 $\rightarrow$ 0; I=0.14, 3.8, and 45 K km s^-1 for 10^-7,10^-6, and 10 $^{-5}~M_\odot$ yr^-1, respectively), 23 $\hbox {$^{\prime \prime }$ }$ (J=2 $\rightarrow$ 1), 15 $\hbox {$^{\prime \prime }$ }$ (J=3 $\rightarrow$ 2), 9 $\hbox {$^{\prime \prime }$ }$ (J=5 $\rightarrow$ 4), 7 $\hbox{$.\!\!^{\prime\prime}$ }$ 5 (J=6 $\rightarrow$ 5)].
Table 3: CO model results for the Mira sample.
Table 4: Source parameters and SiO model results.
Table 5: Source parameters and model results for those objects with double component line profiles.
Table A.1: Observational results of circumstellar SiO radio line emission towards a sample of M-type IRVs and SRVs (Part 1).
Table A.2: Observational results of circumstellar SiO radio line emission towards a sample of M-type IRVs and SRVs (Part 2).
Table A.3: Observational results of circumstellar CO and SiO line emission towards our Mira sample.