Table A.1.
Data for the four YHGs used in Fig. 1.
| Star | Time | log Teff | log L/L⊙ | (B − V) |
|---|---|---|---|---|
| RL or BL | interval | range | range | range |
| HR 8752 | ||||
| RL | 1895–1963 | 3.72–3.70 | 5.25–5.38 |
 |
| BL | 1976–2005 | 3.70–3.90 | 5.60–5.36 |
 |
| ρ Cas | ||||
| RL | 1968–1998 | 3.72–3.66 | 5.48–5.54 |
 |
| HR 5171A | ||||
| RL | 1958–1974 | 3.70–3.65 | 5.40–5.30 |
 |
| HD 179821 | ||||
| BL | 1990–2004 | 3.69–3.83 | 5.20–5.10 |
 |
Notes. The distances used are for HR 8752: 1.370 kpc ± 0.480 kpc (Nieuwenhuijzen et al. 2012: based on the HIPPARCOS parallax: van Leeuwen 2007), ρ Cas: 2.5 kpc ± 0.5 kpc (Sect. 2.9), HR 5171A: 1.5 kpc ± 0.5 kpc (Sect. 2.9), and HD 179821: 6 kpc (Sect. 3.3). We preferred to use spectroscopic temperatures if available: the four of HR 8752, and the second of HD 179821. If spectroscopic temperatures were not available, we used temperatures based on the less reliable (B − V) (Sects. 2.4–2.6).
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