Table 1
Main properties of the ATOMIUM stellar sample and H2O, OH detection.
| Star | Variability (a) | RA(radio) (b) | Dec(radio) (b) | Distance (c) | Mass-loss rate (d) | 2 R* (e) |  |
 |
H2O, OH (h) |
|---|---|---|---|---|---|---|---|---|---|
| Spect. type | ICRS (h m s) | ICRS (° ′ ″) | (pc) | (M⊙yr−1) | (mas) | (yes/no) | |||
| S Pav | SRa | 19 55 14.0055 | −59 11 45.194 | 174 | 8.0 × 10−8 | (11.6) | −20.0 | −18.2 | y, y |
| M8 | |||||||||
| T Mic | SRb | 20 27 55.1797 | −28 15 39.553 | 186 | 8.0 × 10−8 | (9.3) | 25.3 | 25.5 | y, y |
| M7–8 | |||||||||
| U Del | SRb | 20 45 28.2500 | +18 05 23.976 | 335 | 1.5 × 10−7 | 7.9 | −6.4 | −6.8 | y, n |
| M4–6 | |||||||||
| RW Sco | Mira | 17 14 51.6867 | −33 25 54.544 | 578 | 2.1 × 10−7 | (4.9) | −72.0 | −69.7 | y, y |
| M6e | |||||||||
| V PsA | SRb | 22 55 19.7228 | −29 36 45.038 | 304 | 3.0 × 10−7 | (11.4) | −11.1 | −11.1 | y, n |
| M7–8 | |||||||||
| SV Aqr | LPV | 23 22 45.4003 | −10 49 00.187 | 431 | 3.0 × 10−7 | (5.7) | 8.5 | 6.7 | y, n |
| M8 | |||||||||
| R Hya | Mira | 13 29 42.7021 | −23 16 52.515 | 148 | 4.0 × 10−7 | 23.7 | −11.0 | −10.1 | y, y |
| M6–9e | |||||||||
| U Her | Mira | 16 25 47.4514 | +18 53 32.666 | 271 | 5.9 × 10−7 | 11.2 | −14.5 | −14.9 | y, y |
| M6.5–8e | |||||||||
| π1 Gru | SRb | 22 22 44.2696 | −45 56 53.007 | 162 | 7.7 × 10−7 | 18.4 | −13.0 | −11.7 | n, n |
| S5,7 | |||||||||
| AH Sco | SRc | 17 11 17.0159 | −32 19 30.764 | 2260 | 1.0 × 10−6 | 5.8 | −4.0 | −2.3 | y, y |
| M5Ia–7Ib | |||||||||
| R Aql | Mira | 19 06 22.2567 | +08 13 46.678 | 234 | 1.1 × 10−6 | 10.9 | 47.0 | 47.2 | y, y |
| M6.5-9e | |||||||||
| W Aql | Mira | 19 15 23.3781 | −07 02 50.331 | 374 | 3.0 × 10−6 | 11.6 | −25.0 | −23.0 | n, n |
| S6, 6e | |||||||||
| KW Sgr | SRc | 17 52 00.7282 | −28 01 20.572 | 2400 | 5.6 × 10−6 | 3.9 | 4.0 | −4.4 | y, n |
| M4Ia | |||||||||
| IRC–10529 | OH/IR | 20 10 27.8713 | −06 16 13.740 | 930 | 6.7 × 10−6 | (6.5) | −18.0 | −16.3 | y, n |
| M? | |||||||||
| IRC+10011 | Mira | 01 06 25.9883 | +12 35 52.849 | 740 | 1.9 × 10−5 | (6.5) | 10.0 | 10.1 | y, y |
| M8 | |||||||||
| GY Aql | Mira | 19 50 06.3148 | −07 36 52.189 | 410 | 3.0 × 10−5 | (20.5) | 34.0 | 34.0 | y, n |
| M8 | |||||||||
| VX Sgr | SRc | 18 08 04.0460 | −22 13 26.621 | 1560 | 6.1 ×10−5 | 8.8 | 5.3 | 5.7 | y, y |
| M8.5Ia |
Notes. (a)SR stands for semi-regular pulsations; SRa and SRb are AGB stars with persistent and poorly defined periodicity, respectively; SRc is used for the supergiants. (b)Stellar peak measured in the continuum around 241.8 GHz for the extended configuration (Gottlieb et al. 2022); astrometric accuracy ~5–10 mas (see Sect. 2.2). The position is corrected for proper motion at the time of the observations. (c)See Sect. 2.1 for adopted distances. (d)Mass-loss rate from references in Table 1 of Gottlieb et al. (2022) with a few revisions (see Sect. 2.1). (e)Angular diameter from Table 1 of Montargès et al. (2023). Figures in brackets are for calculated and not measured diameters; the derived optical diameter for GY Aql appears to be too large as our radio continuum (~250 GHz) uniform disk size is 14.0 mas. (f)Local standard of rest velocity used as input for the ATOMIUM observations. (g)Newer LSR velocity derived from a sample of lines with well-behaved line profiles (Gottlieb et al. 2022). (h)y or n indicates detection or not of at least one transition of H2O (first entry) and OH (second entry).
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