Table 1
Properties of the sample stars.
| Star | V ⋆ | D | Teff | R ⋆ | |
| (km s-1) | (pc) | (K) | (mas) | (AU) | |
|
|
|||||
| S Per | –38.5 |
|
3550 | 3.5 ± 1.5 | 8.0 |
| U Ori | –39.5 | 260 ± 50 | 2570 | 5.7 ± 0.2 | 1.5 |
| U Her | –14.5 |  |
2630 | 4.8 ± 0.2 | 1.3 |
| IK Tau | +34.0 | 250 ± 20 | – | 11.2 ± 1.1 | 2.8 |
| RT Vir | +18.2 | 135 ± 15 | 2924 | 6.2 ± 0.3 | 0.8 |
| References | |||||
| S Per | D87 | M08 | L05 | H94, L05 | |
| U Ori | C91 | C91 | A97 | R06 | |
| U Her | C94 | V07 | A97 | R06 | |
| IK Tau | K87 | 098 | – | M04, R06 | |
| RT Vir | N86 | vL07 | C07 | M04 | |
Notes. The stellar velocity V ⋆ is given in the Local Standard of Rest (LSR) convention. The distances D used in our calculations are 2.3 kpc for S Per, 266 pc for the Miras, IK Tau, U Ori and U Her and 133 pc for the SRb RT Vir, in order to remain consistent with RYC99 and B+03. The values of R ⋆ for the AGB stars were measured using IR interferometry at H and K bands. The radius of S Per is the average of values deduced from spectral fits.
References. A97: Alvarez & Mennessier (1997); C91: Chapman et al. (1991); C94: Chapman et al. (1994); C07: Cenarro et al. (2007); D87: Diamond et al. (1987); H74: Humphreys (1974); K87: Kirrane (1987); L05: Levesque et al. (2005); M04: Monnier et al. (2004); M08: Mayne & Naylor (2008); N86: Nyman et al. (1986); 098: Olofsson et al. (1998); R06: Ragland et al. (2006); V07: Vlemmings & van Langevelde (2007); vL07: van Leeuwen (2007).
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