Table 1.
Metallicity and absorption in the G band for a sample of GCs and dSphs, obtained by averaging individual values derived by the SOS pipeline for the RR Lyrae stars in these systems.
| Name | [Fe/H]C09 | RRLs | [Fe/H]Gaia | St. dev. [Fe/H]Gaia | RRLs | A(G) | St. dev. [A(G)] | A(G) (*) | Ref. |
|---|---|---|---|---|---|---|---|---|---|
| (dex) | (N1) | (dex) | (dex) | (N2) | (mag) | (mag) | (mag) | ||
| NGC 1261 | −1.27 | 14 | −1.13 | ±0.49 | 12 | 1.32 | ±1.47 | 0.02 | (1) |
| NGC 1851 | −1.18 | 21 | −1.11 | ±0.48 | 18 | 1.27 | ±1.06 | 0.05 | (2) |
| NGC 288 | −1.32 | 1 | −1.24 | ±0.33 | 1 | 0.07 | ±0.08 | 0.08 | (3) |
| NGC 3201 | −1.59 | 73 | −1.27 | ±0.36 | 77 | 0.73 | ±0.30 | 0.62 | (4) |
| NGC 5024 | −2.10 | 25 | −1.66 | ±0.57 | 25 | 0.49 | ±0.69 | 0.05 | (5) |
| NGC 5139-OCen | −1.53 | 36 | −1.42 | ±0.63 | 39 | 0.43 | ±0.36 | 0.31 | (6) |
| NGC 5272-M3 | −1.50 | 125 | −1.38 | ±0.39 | 105 | 0.89 | ±1.52 | 0.01 | (7) |
| NGC 6266-M62 | −1.18 | 105 | −0.73 | ±0.36 | 88 | 2.77 | ±1.81 | 1.23 | (8) |
| IC 4499 | −1.53 | 64 | −1.45 | ±0.48 | 58 | 0.66 | ±0.23 | 0.60 | (9) |
| NGC 7078-M15 | −2.37 | 44 | −1.95 | ±0.54 | 30 | 0.89 | ±0.83 | 0.26 | (10) |
| Sculptor | −1.68 | 289 | −1.64 | ±0.50 | 275 | 0.53 | ±0.63 | 0.05 | (11) |
| Draco | −1.93 | 258 | −1.79 | ±0.67 | 216 | 0.54 | ±0.43 | 0.08 | (12) |
| Ursa Major I | −2.18 | 5 | −2.38 | ±0.43 | 5 | 1.94 | ±2.00 | 0.02 | (13) |
| Ursa Major II | −2.47 | 1 | −2.24 | ±0.45 | 3 | 0.26 | ±0.04 | 0.25 | (14) |
Notes.
A(G)values obtained by transforming the A(V) values in the literature using the following ratio of extinction coefficients A(G)/A(V) = 0.840 from Bono et al. (2019). N1 and N2 are the number of RR Lyrae stars on which the mean [Fe/H]Gaia and A(G) values were computed, with the corresponding standard deviation of the mean in Cols. 5 and 8, respectively.
References. (1) Salinas et al. (2016); (2) Walker (1998); (3) Kaluzny et al. (1997), Arellano Ferro et al. (2013); (4) Layden & Sarajedini (2003), Arellano Ferro et al. (2014); (5) Cuffey (1966), Goranskij (1976), Arellano Ferro et al. (2011); (6) Braga et al. (2018); (7) Benkő et al. (2006); (8) Contreras et al. (2010); (9) Walker & Nemec (1996); (10) Corwin et al. (2008); (11) Martínez-Vázquez et al. (2016);(12) Muraveva et al. (2020); (13) Garofalo et al. (2013); (14) Vivas et al. (2020).
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