Notes. Information on our sample of observed stars. Columns are (from left to right) the star name (alternative name), IRAS point source catalog designation, J2000 right ascension and declination, distance derived from bolometric flux, distance derived from Mira period-luminosity relation, stellar centroid LSR velocity, twice the terminal velocity (i.e., the full velocity range covered by spectral lines) of the star’s CSE, range of mass-loss rates (see Sect. 2), variability period, and the infrared phase at the time of our APEX observations, i.e., 2015 May 28. For AGB stars the IR light has its maximum (ϕ_IR = 0) at a visual phase of ≈0.1. The periods and phases are based mainly on data in Whitelock et al. (2006, see Sect. 2 and also Appendix A). All our positions agree to within 2^″ with the 2MASS positions of the stars, which themselves have an absolute accuracy of better than 0.′′ 1 (Cutri et al. 2003). For our discussion, the D^PLR value is adopted for the distance, when available. In other cases we use D^BF. The LSR and terminal velocities were taken from Loup et al. (1993), who in general compile multiple literature values for these quantities mostly based on CO= J = 1 →0, 2 → 1 or HCN J = 1 →0 spectra. Our adopted values are averages of the higher-quality entries and should have uncertainties < 2 km s⁻¹. ^(a) Period and phase derived from visual data available through the web site of AAVSO’s International Variable Star Index. ^(b) Menten et al. (2012) proposed a distance of 0.13 kpc for this star. ^(c) Combined value from JHKL IR light curves (Menten et al. 2012). ^(d) For this star, its IRAS name is frequently used in the literature. ^(e) Ryde et al. (1999).