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Table 1

Stellar sample information.

Object IRAS Position DBF DPLR Period ϕIR
αJ2000 δJ2000 (kpc) (km s−1) (10−7M yr−1) (d)
R For 02270−2619 02h29m15.s3 − 26°05′56 0.67 0.70 −2 38 9–22 385 0.0
R Lep 04573−1452 04 59 36.4 −14 48 22 0.48 0.47 +16 38 5–20 438 0.5
AI Vol 07454−7112 07 45 02.4 −71 19 46 0.75 0.83 −39 27 51 511 0.1
X Cnc 08525+1725 08 55 22.9 +17 13 52 0.69 −15 20 0.4–8 180a 0.5a
CQ Pyx (RAFGL 5254) 09116−2439 09 13 53.9 −24 51 25 0.42 1.14 0 26 23–120 659 0.6
CW Leo (IRC+10216) 09452+1330 09 47 57.4 +13 16 44 0.12 0.14b −26.5 36 200–400 630c 0.23
X Vel 09533−4120 09 55 26.9 −41 35 15 0.67 −17 17 0.5–3.5
RW LMi (CIT 6) 10131+3049 10 16 02.3 +30 34 19 0.38 0.46 −2 30 26–140 617 0.7
U Hya 10350−1307 10 37 33.3 −13 23 05 0.35 −31 18 1.1–5 183a 0.8a
V Hya 10491−2059 10 51 37.3 −21 15 00 0.33 −16 22 31–35 531 0.3
V358 Lup (RAFGL 4211) 15082−4808 15 11 41.9 −48 20 01 0.67 0.95 −3 42 93 632 0.8
X TrA 15094−6953 15 14 19.0 −70 04 45 0.47 −3 18 0.4–1.6 320
II Lupd 15194−5115 15 23 05.7 −51 25 59 0.47 0.64 −15 46 100e 576 0.4

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 (ϕIR = 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 DPLR value is adopted for the distance, when available. In other cases we use DBF. 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).

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