Table 5
Distance modulus for ω Cen from the literature.
| Method | μ0 (mag)a | Reference |
|
|
||
| B and V PL relations for Pop. II stars | 13.53 ± 0.20 | Nemec et al. (1994) |
| High-amplitude δ Sct stars | 14.05 ± 0.10 | McNamara (2000) b |
| Detached eclipsing binary (V212) | 13.68 ± 0.11 | Thompson et al. (2001) |
| Detached eclipsing binary (V212) | 13.72 ± 0.04 | Kaluzny et al. (2002) |
| AV-log P models for RRab stars | 13.64 ± 0.11 | Caputo et al. (2002) |
| MV-log P models for RRc stars | 13.71 ± 0.11 | Caputo et al. (2002) |
| MV − [ Fe / H ] relation (RRL stars) | 13.72 ± 0.11 | Del Principe et al. (2006) c |
| MV − [ Fe / H ] relation (RRL stars) | 13.62 ± 0.11 | Del Principe et al. (2006) d |
| PL−Z(KS) | 13.77 ± 0.07 | Del Principe et al. (2006) e |
| PL-τHB(KS, f = 3, τHB = 0.940) | 13.69 ± 0.06 | Del Principe et al. (2006) |
| PL-τHB(J, f = 3, τHB = 0.940) | 13.70 ± 0.10 | Del Principe et al. (2006) |
| PL-τHB(KS, f = 3, τHB = 0.934) | 13.72 ± 0.06 | Del Principe et al. (2006) f |
| PL-τHB(J, f = 3, τHB = 0.934) | 13.76 ± 0.10 | Del Principe et al. (2006) |
| Cluster dynamics | 13.41 ± 0.14 | van de Ven et al. (2006) |
| MV − [ Fe / H ] relation (RRL stars) | 13.68 ± 0.27 | Weldrake et al. (2007) |
| SX Phe log P − V relation | 13.76 ± 0.06 | McNamara (2011) |
| Optical Period-Wesenheit relations (RRL stars) | 13.71 ± 0.08 | Braga et al. (2016) |
|
|
||
| Weighted average | 13.72 ± 0.13 | |
|
|
||
| Weighted-average PL relations (T2Cs and RRLs) | 13.708 ± 0.035 | This work |
Notes.
Most of the error estimates do not consider the contribution of systematic errors, which in the case of T2Cs and RRL stars can reach values of order ≈0.10 mag.
The listed error was determined considering the internal uncertainties of the mean distance modulus value, ±0.02 mag, and the observational error, ±0.1 mag, as described by McNamara (2000).
Based on the MV-[Fe/H] relation from Bono et al. (2003) and mean V magnitudes from Kaluzny et al. (2004).
Based on the MV-[Fe/H] relation of Catelan et al. (2004) and V magnitudes from Kaluzny et al. (2004).
Based on the semi-empirical J-band PL–Z relation from Bono et al. (2003).
Based on the PL-τHB relations from Catelan et al. (2004).
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