Table 4.
Summary of derived parameters for M80 based on isochrone fitting.
| Data source | Color transform | Age (Gyr) ( ⋆ ) | [Fe/H] (dex) | Comments |
|---|---|---|---|---|
| Alcaino et al. (1998) | UBVRI | 12 − 17 | −1.7 ± 1 | Adjustments to the distance modulus and both |
| extinction coefficients are required (see Fig. 18) | ||||
| PS1 DR2 | PanSTARRS | 14 ± 1(±3) | −2.0 ± 0.1 | Higher metallicities require high ages; ex. [Fe/H]=−1.8 |
| and 17 Gyr; adjustment not strictly required | ||||
| Gaia DR2 | Gaia DR2 | 13 ± 1(±3) | −1.8 ± 0.1 | Older ages are better fit by lower metallicities; |
| adjustment to ABP is required for alignment | ||||
| Gaia EDR3 | Gaia DR2 | 14 ± 1(±3) | −1.75 ± 0.15 | Adjustment to extinction coeffs not strictly required |
Notes. ( ⋆ ) the uncertainties quoted for isochrone-based ages (e.g., 1 Gyr) are a rough reflection of uncertainty due to ambiguity in the best-fitting isochrone, among those presented, by visual fit only. Global uncertainties for isochrone-based age determinations for even the most well-studied and well-constrained globular clusters are likely 2 or 3 Gyr (see, e.g., Joyce et al. 2023). This is reflected parenthetically, e.g., ±1(3) Gyr.
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