Fig. 8
Distances and bolometric magnitudes of the 1.5 × 103 halo WDs that can be observed with Gaia, for our standard model. Top panel: distribution of their distances. Right panel: distribution of their bolometric magnitudes, which gives an idea of the statistical errors that are to be expected per luminosity bin of the WDLF for Gaia. The yellow stars, labelled “other”, are pre-WDs that are indistinguishable from MS stars or giants. These are not included in the projected distribution histograms.
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