Table 2
Bias-correction due to magnitude cut in the RGB selection.
| Distance bin (kpc) | Metallicity bin | Weight |
|---|---|---|
| 10 < dhc < 22 | −0.5 < [Fe/H] | 2.07 |
| −1.0 < [Fe/H] < -0.5 | 1.69 | |
| −1.5 < [Fe/H] < -1.0 | 1.27 | |
| −2.0 < [Fe/H] < -1.5 | 1.07 | |
| [Fe/H] < -2.0 | 1.00 | |
| 22 < dhc < 45 | −0.5 < [Fe/H] | 3.91 |
| −1.0 < [Fe/H] < -0.5 | 1.95 | |
| −1.5 < [Fe/H] < -1.0 | 1.46 | |
| −2.0 < [Fe/H] < -1.5 | 1.20 | |
| [Fe/H] < -2.0 | 1.00 | |
| 45 < dhc < 101 | −0.5 < [Fe/H] | − |
| −1.0 < [Fe/H] < -0.5 | 6.49 | |
| −1.5 < [Fe/H] < -1.0 | 2.27 | |
| −2.0 < [Fe/H] < -1.5 | 1.32 | |
| [Fe/H] < -2.0 | 1.00 |
Notes. The weights calculated from PARSEC simulated stellar populations, to bias-correct the metallicity bias introduced by binning the sample in distance. Because of our magnitude cut where we only keep stars with G < 17.6 mag, each distance bin probes a limited range in absolute magnitude, which because of the colour cut primarily affects the metal-rich stars, see Figure 13. Within each distance bin, the weights for each metallicity has been normalised to the weight in the [Fe/H] < -2.0 bin. These weights are multiplied to the MDFs to bias-correct them.
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