The Pristine Inner Galaxy Survey (PIGS) IX. The largest detailed chemical analysis of very metal-poor stars in the Sagittarius dwarf galaxy
arxiv(2024)
Abstract
The most metal-poor stars provide valuable insights into the early chemical
enrichment history of a system, carrying the chemical imprints of the first
generations of supernovae. The most metal-poor region of the Sagittarius dwarf
galaxy remains inadequately observed and characterised. To date, only ∼4
stars with [Fe/H] <-2.0 have been chemically analysed with high-resolution
spectroscopy. In this study, we present the most extensive chemical abundance
analysis of 12 low-metallicity stars with metallicities down to [Fe/H] =-3.26
and located in the main body of Sagittarius. These targets, selected from the
Pristine Inner Galaxy Survey, were observed using the MIKE high-resolution
spectrograph at the Magellan-Clay telescope, which allowed us to measure
up to 17 chemical species. The chemical composition of these stars reflects the
imprint of a variety of type II supernovae (SNe II). A combination of low- to
intermediate-mass high-energy SNe and hypernovae (∼10-70) is required
to account for the abundance patterns of the lighter elements up to the
Fe-peak. The trend of the heavy elements suggests the involvement of compact
binary merger events and fast-rotating (up to ∼300) intermediate-mass
to massive metal-poor stars (∼25-120) that are the sources of rapid
and slow processes, respectively. Additionally, asymptotic giant branch stars
contribute to a wide dispersion of [Ba/Mg] and [Ba/Eu]. The absence of an
α-knee in our data indicates that type Ia supernovae did not contribute
in the very metal-poor region ([Fe/H] ≤-2.0). However, they might have
started to pollute the interstellar medium at [Fe/H] >-2.0, given the
relatively low [Co/Fe] in this metallicity region.
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