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Table 3:

The MDF of the Galactic halo field stars as constructed from the sample of 1638 HES with available spectroscopic follow-up observations, by means of scaling to the full candidate sample of 3439 stars (for details see text).
[Fe/H] -4.50 -4.30 -4.10 -3.90 -3.70 -3.50 -3.30 -3.10 -2.90 -2.70 -2.50 -2.30 -2.10
N 0 0 2 0 0 12 45 73 160 198 281 337 399
[Fe/H] -1.90 -1.70 -1.50 -1.30 -1.10 -0.90 -0.70 -0.50 -0.30 -0.10 +0.10 +0.30 +0.50
N 313 231 229 209 308 268 178 109 45 33 3 6 0

Note that for a proper comparison with the MDFs predicted by theoretical models, or the MDFs of other stellar populations, the selection efficiency of the HES as a function of [Fe/H] and (B-V)0 must be taken into account (see Table 4). Note also that the HES sample is increasingly contaminated with thin- and thick-disk stars as [Fe/H] approaches 0.0.


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