English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

This paper compares the chemical evolution of the Large Magellanic Cloud(LMC) to that of the Milky Way (MW) and investigates the relation between thebar and the inner disc of the LMC in the context of the formation of the bar.We obtained high-resolution and mid signal-to-noise ratio spectra withFLAMES/GIRAFFE at ESO/VLT and performed a detailed chemical analysis of 106 and58 LMC field red giant stars (mostly older than 1 Gyr), located in the bar andthe disc of the LMC respectively. We measured elemental abundances for O, Mg,Si, Ca, Ti, Na, Sc, V, Cr, Co, Ni, Cu, Y, Zr, Ba, La and Eu. We find that the{\alpha}-element ratios [Mg/Fe] and [O/Fe] are lower in the LMC than in the MWwhile the LMC has similar [Si/Fe], [Ca/Fe], and [Ti/Fe] to the MW. As for theheavy elements, [Ba,La/Eu] exhibit a strong increase with increasingmetallicity starting from [Fe/H]=-0.8 dex, and the LMC has lower [Y+Zr/Ba+La]ratios than the MW. Cu is almost constant over all metallicities and about 0.5dex lower in the LMC than in the MW. The LMC bar and inner disc exhibitdifferences in their [{\alpha}/Fe] (slightly larger scatter for the bar in themetallicity range [-1,-0.5]), their Eu (the bar trend is above the disc trendfor [Fe/H] > -0.5 dex), their Y and Zr, their Na and their V (offset betweenbar and disc distributions). Our results show that the chemical history of theLMC experienced a strong contribution from type Ia supernovae as well as astrong s-process enrichment from metal-poor AGB winds. Massive stars made asmaller contribution to the chemical enrichment compared to the MW. Theobserved differences between the bar and the disc speak in favour of an episodeof enhanced star formation a few Gyr ago, occurring in the central parts of theLMC and leading to the formation of the bar. This is in agreement with recentlyderived star formation histories.

Chemical abundances in LMC stellar populations. II. The bar sample