Table 1
Properties of the sample stars.
| Star | Position | Type | V⋆ | Distance | D | R⋆ | P | Ṁ | Previous imaging | ||
| (J2000) | (km s-1) | (pc) | (pc) | (AU) | (d) | (M⊙ yr-1) | |||||
|
|
|||||||||||
| VX Sgr | 18 08 04.05 –22 13 26.6 | RSG | –5.3 |
|
1700 | 7.4 ± 0.7 | 732 | 7.2 × 10-5 | C86, B93, M98, M03, V05 | ||
| S Per | 02 22 51.71 +58 35 11.4 | RSG | –38.5 |
|
2300 | 8 ± 3 | 822 | 3.8 × 10-5 | D87, Y94, R99, M98, V01, | ||
| A10 | |||||||||||
| U Ori | 05 55 49.17 +20 10 30.7 | Mira | –39.5 |
|
266 | 1.5 ± 0.1 | 368 | 2.3 × 10-7 | B88, Y94, B94, B03, V05 | ||
| U Her | 16 25 47.47 +18 53 32.9 | Mira | –14.5 |
|
266 | 1.3 ± 0.1 | 406 | 3.4 × 10-7 | Y94, B94, M98, C00, B03, | ||
| V02, V05 | |||||||||||
| IK Tau | 03 53 28.89 +11 24 21.9 | Mira | +34.0 |
|
266 | 2.8 ± 0.3 | 470 | 2.6 × 10-6 | L87, B93, Y94, M98, B03 | ||
| RT Vir | 13 02 37.98 +05 11 08.4 | SRb | +18.2 |
|
133 | 0.8 ± 0.04 | 158 | 1.3 × 10-7 | Y94, B93, B94, B03, I03 | ||
| W Hya | 13 49 02.00 –28 22 03.4 | SRb | +40.6 |
|
98 | 2.1 ± 0.2 | 375 | 2.3 × 10-7 | R90, B93 | ||
| References | |||||||||||
| VX Sgr | vL07 | C86 | C07 | M04 | S11 | D10 | |||||
| S Per | vL07 | D87 | M08 | H94, L05 | S11 | vL05 | |||||
| U Ori | vL07 | C91 | C91 | R06 | S11 | K98 | |||||
| U Her | vL07 | C94 | V07 | R06 | S11 | Y95 | |||||
| IK Tau | C06 | K87 | 098 | M04, R06 | S11 | O98, B00 | |||||
| RT Vir | vL07 | N86 | vL07 | M04 | S11 | K98, K99 | |||||
| W Hya | vL07 | N96 | V03 | Z11 | S11 | K98 | |||||
Notes. The stellar velocity V⋆ is given in the Local Standard of Rest (LSR) convention. The positions given are for epoch 2000, see Sect. 2.2 for more on astrometry. The most recent distances are given along with those used in our calculations, D, in order to remain consistent with M03, R99 and B03. 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. The stellar period P is complex, changeable and/or uncertain for some objects, see Figs. 1 to 3. The mass loss rates Ṁ are adjusted to our adopted distances. The final column gives some of the previous interferometric 22-GHz H2O maser images which have been published.
References. in the table are: A10 Asaki et al. (2010); B88 Bowers & Johnston (1988); B93 Bowers et al. (1993); B94 Bowers & Johnston (1994); B00 Bieging et al. (2000); B03 Bains et al. (2003); C86 Chapman & Cohen (1986); C91 Chapman et al. (1991); C94 Chapman et al. (1994); C00 Colomer et al. (2000); C06 Carlsberg Meridian Catalog 14 (2006); C07 Chen et al. (2007); D87 Diamond et al. (1987); I03 Imai et al. (2003); K87 Kirrane (1987); K98 Knapp et al. (1998); K99 Kerschbaum & Olofsson (1999); L87 Lane et al. (1987); L05 Levesque et al. (2005); M98 Marvel et al. (1998); M03 Murakawa et al. (2003) M04 Monnier et al. (2004); M08 Mayne & Naylor (2008); N96 Neufeld et al. (1996); N86 Nyman et al. (1986); O98 Olofsson et al. (1998); R90 Reid & Menten (1990); R99 Richards et al. (1999); R06 Ragland et al. (2006); S11 Samus et al. (2011) (GCVS); V01 Vlemmings et al. (2001); V02 Vlemmings et al. (2002); V03 Vlemmings et al. (2003); V05 Vlemmings et al. (2005); V07 Vlemmings & van Langevelde (2007); vL05 van Loon et al. (2005); vL07 van Leeuwen (2007); Y94 Yates & Cohen (1994); Z11 Zhao-Geisler et al. (2011).
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