Table 1
ATOMIUM sources and their stellar parameters.
| Source | Stellar type | Pulsation type | P (days) | Teff (K) | Diameter(1) (mas) |  (cm) |
MLR(3) (M⊙ yr−1) | vexp (kms−1) | D(4) (pc) |
|---|---|---|---|---|---|---|---|---|---|
| S Pav | M-type | SRa | 381 (a) | 3100 (b) | 12.0 (c) | 1.7E+13 | 1.3E-07 (a) | 13.0 (c) | 190 (d,e,f) |
| RW Sco | M-type | Mira | 389 (g) | 3300 (b) | 4.9 (c) | 2.1E+13 | 1.3E-07 (g) | 18.5 (c) | 560 (e) |
| T Mic | M-type | SRb | 347 (a) | 3300 (b) | 9.3 (c) | 1.2E+13 | 1.4E-07 (a) | 12.7 (c) | 175 (f) |
| R Hya | M-type | Mira | 366 (h) | 2100 (i) | 23.0 (c) | 2.2E+13 | 1.8E-07 (i) | 22.2 (c) | 126 (f) |
| SV Aqr | M-type | LPV | − | 3400 (b) | 4.4 (c) | 1.5E+13 | 2.7E-07 (a) | 15.9 (c) | 445 (f) |
| U Her | M-type | Mira | 402 (h) | 3100 (c) | 11.0 (c) | 2.2E+13 | 3.2E-07 (j) | 19.7 (c) | 266(k,f) |
| U Del | M-type | SRb | 119 (d) | 2800 (c) | 7.9 (c) | 2.0E+13 | 3.7E-07 (a) | 14.6 (c) | 330 (d,e,h) |
| V PsA | M-type | SRb | 148 (a) | 2400 (a) | 13.0 (c) | 2.7E+13 | 4.8E-07 (a) | 18.8 (c) | 278 (d,e) |
| π1 Gru | S-type | SRb | 150 (i) | 2300 (i) | 21.0 (c) | 2.6E+13 | 9.2E-07 (l) | 64.5 (c) | 164 (e) |
| R Aql | M-type | Mira | 268 (h) | 2800 (i) | 12.0 (c) | 2.1E+13 | 1.6E-06 (j) | 12.8 (c) | 230 (d,e,h) |
| GY Aql | M-type | Mira | 468 (h) | 3100 (b) | 21.0 (c) | 6.4E+13 | 2.3E-06 (m) | 15.0 (c) | 410 (f) |
| W Aql | S-type | Mira | 479 (h) | 2800 (c) | 11.0 (c) | 3.1E+13 | 2.7E-06 (n) | 24.6 (c) | 375 (d,e,f) |
| KW Sgr | RSG | SRc | 647 (o) | 3700 (c) | 3.9 (c) | 7.0E+13 | 3.6E-06 (p) | 27.7 (c) | 2400 (q) |
| IRC-10529 | M-type | Mira | 680 (i) | 2700 (i) | 6.5 (c) | 4.5E+13 | 1.0E-05 (i) | 21.8 (c) | 930 (i,f) |
| AH Sco | RSG | SRc | 738 (r) | 3700 (c) | 5.8 (c) | 9.8E+13 | 1.0E-05 (s) | 35.4 (c) | 2260 (t) |
| IRC+10011 | M-type | Mira | 660 (i) | 2700 (i) | 6.5 (c) | 3.6E+13 | 1.9E-05 (i) | 23.1 (c) | 740 (f) |
| VX Sgr | RSG | SRc | 732 (u) | 3500 (c) | 8.8 (c) | 1.0E+14 | 6.0E-05 (i) | 32.9 (c) | 1560 (v) |
Notes. (1)Optical angular diameter. (2)Calculated from the stellar angular diameter and distance. (3)Scaled to the new distance estimate, see Sect. 2.3.(4) Several distances have been updated with respect to the values given in Gottlieb et al. (2022).
References. (a)Olofsson et al. (2002);(b)Marigo et al. (2008); (c)Gottlieb et al. (2022); (d)Gaia Collaboration (2018); (e)Bailer-Jones et al. (2021); (f)Andriantsaralaza et al. (2022); (g)Groenewegen et al. (1999); (h)Perryman et al. (1997); (i)De Beck et al. (2010); (j)Young (1995); (k)Vlemmings & Langevelde (2007); (l)Doan et al. (2017); (m)Loup et al. (1993); (n)Ramstedt et al. (2017); (o)Wittkowski et al. (2017); (p)Mauron & Josselin (2011); (q) Arroyo-Torres et al. (2013); (r)Kiss et al. (2006); (s)Jura & Kleinmann (1990); (t)Chen & Shen (2008);(u)Samus’ et al. (2017); (v)Chen et al. (2007).
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