Table 2
Observational parameters of the sources.
| Source | Variability (a) type | p(a) (days) | Spectral (b) type | Composition (b) type | Lbol (c) (L⊙) | E(B-V) (ISM) (d) (mag) |
|---|---|---|---|---|---|---|
| AT Dra | LB | – | M4III D | O | 1900 ± 400 | <0.0018 |
| BC Cmi | SRB | 34.13 | M4/5III D | O | 720 ± 130 | 0.0 |
| BD Cam | LB | – | S3.5/2 B | S | 2600 ± 600 | <0.04 |
| BY Boo | LB | – | M4.5IIIB | O | 1800 ± 400 | 0.0 |
| CG Uma | LB | – | M4IIIa D | O | 2000 ± 400 | 0.13 ± 0.05 |
| DF Leo | SRB | 70 | M4III C | O | 900 ± 200 | 0.040 ± 0.019 |
| EY Hya | SRA | 182.7 | M7 D | O | 6400 ± 1900 | 0.080 ± 0.007 |
| FH Vir | SRB | 70 | M6III C | O | 1500 ± 400 | 0.090 ± 0.017 |
| IN Hya | SRB | 65 | M3/4IIID | O | 1200 ± 200 | 0.040 ± 0.005 |
| OME Vir | LB | – | M4.5:III C | O | 1900 ± 500 | <0.005 |
| R Lmi | M | 372.19 | M6.5-9e B | O | 3100 ± 900 | <0.014 |
| R Uma | M | 301.62 | M5-8e B | O | 5400 ± 1300 | 0.090 ± 0.009 |
| RR Eri | SRB | 97 | M5III C | O | 4000 ± 1000 | 0.060 ± 0.012 |
| RR Umi | SRB | 43.3 | M4.5IIIC | O | 1300 ± 300 | 0.0 |
| RT Cnc | SRB | 89.8 | M5III C | O | 2900 ± 600 | 0.06 ± 0.016 |
| RU Her | M | 484.83 | M6-7e B | O | 20000 ± 7000 | 0.110 ± 0.007 |
| RW Boo | SRB | 209 | M5III: D | O | 2000 ± 400 | <0.0018 |
| RZ Uma | SRB | 115 | M8 D | O | 5000 ± 1300 | 0.110 ± 0.005 |
| ST Uma | SRB | 110 | M4III C | O | 2800 ± 600 | 0.0 |
| SV Peg | SRB | 144.6 | M7 D | O | 8000 ± 2000 | 0.130 ± 0.008 |
| T Dra | M | 421.62 | C6,2e C | C | 9000 ± 3000 | 0.020 ± 0.007 |
| TU And | M | 316.8 | M6e B | O | 6600 ± 1900 | 0.020 ± 0.007 |
| UY Leo | LB | – | M7III: D | O | 2400 ± 500 | <0.018 |
| V Eri | SRC | 97.0 | M7+II: C | O | 5800 ± 1500 | 0.070 ± 0.018 |
| VY Uma | LB | – | C-N5 B | C | 5300 ± 1100 | <0.007 |
| W Peg | M | 345.5 | M6.5-7.5eB | O | 5300 ± 1400 | 0.120 ± 0.007 |
| Y Crb | SRB | 300 | M8III: D | O | 4100 ± 1000 | <0.005 |
| Y Gem | SRB | 160 | M8 D | O | 7000 ± 2000 | 0.040 ± 0.005 |
| Z Cnc | SRB | 95.4 | M6III C | O | 3700 ± 800 | 0.040 ± 0.005 |
Notes. Column (1): source, Col. (2): variability type, Col. (3): expansion period when the source has a stable period, Col. (4): spectral type, Col. (5): composition (O for O-rich stars or C for C-rich stars), Col. (6): bolometric luminosity, Col. (7): reddening produced by the ISM. (a) From the General Catalogue of Variable Stars (GCVS, Samus’ et al. 2017). (b) From the SIMBAD astronomical database (Wenger et al. 2000). (c) From integration of the extinction-corrected spectral energy distributions (SEDs; see Appendix B).(d) Interstellar medium reddening has been obtained with GALEXtin (see Amôres et al. 2021) with the extinction map from Bayestar19 (see Green et al. 2019).
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