Table 1.
Methodology used for the spatial and Colour-Magnitude (CM) of the likelihood for stars in the dwarf galaxy (Sect. 4.1).
Spatial | CM | Galaxies |
---|---|---|
Exp | Emp | Carina, Draco, Fornax, Leo I, Leo II, |
Sculptor, Sextans, Ursa Minor | ||
Exp | Syn | All those not listed in the other rows |
Emp | Box | IC 1613, NGC 6822, WLM |
NGC 3109, Sextans A, Sextans B, M33 | ||
Exp | Box | Leo A, Peg-dIrr, Sg-dIrr, UGC 4879 |
Notes. In the column “Spatial”, “Exp” indicates that an exponential profile was used for the surface number density distribution and “Emp” that the spatial distribution was determined empirically. In the column, “CM”, “Emp” indicates that the probability distribution on the CM plane was determined empirically (from within 1 half-light radius), “Syn” that the synthetic CMD was used and “Box” that a uniform probability was given to stars within regions of the CMD compatible with hosting massive blue stars and red super-giants.
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