Table 1.
Sample of the LG systems.
| Galaxy | Morph. Type | N | Method | References |
|---|---|---|---|---|
| Milky Way satellites | ||||
| SMC | dIrr | 3032 | CaT | Dobbie et al. (2014) |
| Fornax (Fnx) | dSph | 822 | CaT | Battaglia & Starkenburg (2012) |
| Leo I | dSph | 813 | SpF | Kirby et al. (2013b) |
| Sculptor (Scl) | dSph | 539 | CaT | Battaglia & Starkenburg (2012) |
| Leo II | dSph | 258 | SpF | Kirby et al. (2013b) |
| Carina (Car) | dSph | 392 | CaT | Koch et al. (2006) |
| Sextans (Sxt) | dSph | 162 | CaT | Battaglia et al. (2011) |
| Antlia II (AntlII) | dSph | 234 | CaT | Ji et al. (2021) |
| Ursa Minor (UMi) | dSph | 718 | SpF | Pace et al. (2020) |
| Draco (Dra) | dSph | 455 | F-SpF | Walker et al. (2015) |
| Canes Venatici I (CVenI) | dSph | 163 | SpF | Kirby et al. (2013b) |
| Crater II (CratII) | dSph | 81 | CaT | Ji et al. (2021) |
| M31 satellites | ||||
| M32 | cE | 64 | CaT | Ho et al. (2015b) |
| NGC 205 (N205) | dE | 224 | CaT | Ho et al. (2015b) |
| NGC 185 (N185) | dE | 321 | CaT | Ho et al. (2015b) |
| NGC 147 (N147) | dE | 230 | CaT | Ho et al. (2015b) |
| Andromeda VII (AndVII) | dSph | 104 | CaT | Ho et al. (2015b) |
| Andromeda II (AndII) | dSph | 300 | CaT | Ho et al. (2015b) |
| Andromeda V (AndV) | dSph | 81 | SpF | Kirby et al. (2020) |
| Local Group Isolated | ||||
| NGC 6822 (N6822) | dIrr | 279 | SpF | Kirby et al. (2013b) |
| IC 1613 | dIrr | 296 | CaT | Taibi et al. (in prep.) |
| WLM | dIrr | 126 | CaT | Leaman et al. (2013) |
| UGC 4879 (VV124) | dTr | 63 | SpF | Kirby et al. (2013a) |
| Leo A | dIrr | 113 | SpF | Kirby et al. (2017) |
| Pegasus-DIG (PegDIG) | dIrr | 95 | SpF | Kirby et al. (2013b) |
| Sagittarius-DIG (SagDIG) | dIrr | 43 | SpF | Kirby et al. (2017) |
| Cetus (Cet) | dSph | 54 | CaT | Taibi et al. (2018) |
| Aquarius (Aqu) | dIrr | 45 | CaT | Hermosa Muñoz et al. (2020) |
| Phoenix (Phx) | dTr | 193 | CaT | Kacharov et al. (2017) |
| Tucana (Tuc) | dSph | 54 | CaT | Taibi et al. (2020) |
Notes. Columns show from left to right the galaxies (with the abbreviations used in the figures), the corresponding morphological type (dwarf spheroidal – dSph; compact or dwarf elliptical – cE or dE; dwarf irregular or transition type – dIrr or dTr), the number of probable member stars within each dataset (for Sextans and Sculptor, we adopt the membership criteria as in Cicuéndez et al. 2018 and Iorio et al. 2019, respectively), the method used to obtain the metallicities (by direct fit of the available Fe I absorption lines – SpF; by full spectral fitting using synthetic spectra – F-SpF; applying the calibration between the equivalent width of the Ca II triplet lines and [Fe/H] – labelled CaT), and references to the original catalogues.
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