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Fig. 2.


Stellar fraction as a function of stellar mass for 110 galaxies in the SPARC sample. Top panel (in log-scale): individual measurements with their uncertainties. Bottom panel (in linear-scale): f (orange dashed line) and fbaryons = f + 1.4fHI + fH2 (blue dot-dashed line; see text for details) in bins of log M (shaded areas are the 1σ uncertainties). In both panels, the stellar-to-halo mass relation estimated by Moster et al. (2013) using abundance matching is shown as a black curve, with a shaded area representing its scatter. Points in the top panel are colour-coded by how many standard deviations away the galaxy is from the Moster et al. (2013) relation, i.e. , where σf is the observed uncertainty on f, f⋆,M+13 is the value predicted by the abundance matching model, and σM + 13 is the scatter of the Moster et al. (2013) relation. In both panels, galaxies that have converted all the available baryons in the halo into stars would lie on the long dashed line, whose thickness encompasses uncertainties on fb. As in Fig. 1, also shown is the location of the Milky Way (cross) and the Andromeda galaxy (plus), as given by the modelling by Posti & Helmi (2019) and Corbelli et al. (2010), respectively.

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