Abstract
The Pristine survey uses narrow-band photometry to derive precise metallicities down to the extremely metal-poor regime ( [Fe/H] < -3),and currently consists of over 4 million FGK-type stars over a sky area of ∼ 2500 deg^2. We focus our analysis on a subsample of ∼80 000main-sequence turn-off stars with heliocentric distances between 6 and20 kpc, which we take to be a representative sample of the inner halo.The resulting metallicity distribution function (MDF) has a peak at[Fe/H] =-1.6, and a slope of Δ(LogN)/Δ [Fe/H] = 1.0 ±0.1 in the metallicity range of -3.4 < [Fe/H] < -2.5. This agrees well with a simple closed-box chemical enrichment model in this range, but is shallower than previous spectroscopic MDFs presented in the literature, suggesting that there may be a larger proportion of metal-poor stars in the inner halo than previously reported. We identify the Monoceros/TriAnd/ACS/EBS/A13 structure in metallicity space in a low-latitude field in the anticentre direction, and also discuss the possibility that the inner halo is dominated by a single, large merger event, but cannot strongly support or refute this idea with the current data. Finally, based on the MDF of field stars, we estimate the number of expected metal-poor globular clusters in the Milky Way halo to be 5.4for [Fe/H] < -2.5 and 1.5 for [Fe/H] < -3, suggesting that the lack of low-metallicity globular clusters in the Milky Way is not due simply to statistical undersampling.
Original language | English |
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Pages (from-to) | 4986-5002 |
Number of pages | 17 |
Journal | Monthly Notices of the Royal Astronomical Society |
Volume | 492 |
Issue number | 4 |
DOIs | |
Publication status | Published - Mar-2020 |
Externally published | Yes |
Keywords
- stars: abundances
- Galaxy: abundances
- Galaxy: evolution
- Galaxy: formation
- Galaxy: halo
- galaxies: dwarf