Table 1
Amount of He enhancement of M3 BHB stars compared to RHB stars.
| Phase | Teff range [K] | ΔY | % non-variables | % total HB | Main diagnostic |
|
|
|||||
| RHB+V | <7500 | <0.01 | 32 ± 5% | 58 ± 6% | Strömgren (visual) |
| cool BHB | 7500 ↔ 8300 | 0.01 | 21 ± 4% | 13 ± 3% | Strömgren (visual) |
| BHB | 8300 ↔ 9300 | <0.02 | 25 ± 4% | 15 ± 3% | WFPC2 (near UV) |
| hot BHB | 9300 ↔ 10 900 | 0.02 | 16 ± 3% | 10 ± 2% | WFPC2 (near UV) |
| eBHB | >10 900 | ? | 6 ± 2% | 4 ± 1% | |
Notes. Fractions are calculated considering only non-variable stars and that the total HB population follows a relation B:V:R = 0.47:0.37:0.16, where B, V, R stand for the number of blue, variable (RR Lyrae), and red HB stars, respectively (Catelan et al. 2001).
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