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• W3045035825 endingPage "3570" @default.
• W3045035825 startingPage "3557" @default.
• W3045035825 abstract "We conduct a quantitative analysis of the star formation history (SFH) of the Milky Way's bulge by exploiting the constraining power of its stellar [Fe/H] and [Mg/Fe] distribution functions. Using APOGEE data, we confirm the previously-established bimodal [Mg/Fe]--[Fe/H] distribution within 3 kpc of the inner Galaxy. Compared to that in the solar vicinity, the high-$alpha$ population in the bulge peaks at a lower [Fe/H]. To fit these observations, we use a simple but flexible star formation framework, which assumes two distinct stages of gas accretion and star formation, and systematically evaluate a wide multi-dimensional parameter space. We find that the data favor a three-phase SFH that consists of an initial starburst, followed by a rapid star formation quenching episode and a lengthy, quiescent secular evolution phase. The metal-poor, high-$alpha$ bulge stars ([Fe/H]<0.0 and [Mg/Fe]>0.15) are formed rapidly (<2 Gyr) during the early starburst. The density gap between the high- and low-$alpha$ sequences is due to the quenching process. The metal-rich, low-$alpha$ population ([Fe/H]>0.0 and [Mg/Fe]<0.15) then accumulates gradually through inefficient star formation during the secular phase. This is qualitatively consistent with the early SFH of the inner disk. Given this scenario, a notable fraction of young stars (age<5 Gyr) is expected to persist in the bulge. Combined with extragalactic observations, these results suggest that a rapid star formation quenching process is responsible for bimodal distributions in both the Milky Way's stellar populations and in the general galaxy population and thus plays a critical role in galaxy evolution." @default.
• W3045035825 created "2020-07-29" @default.
• W3045035825 creator A5003242521 @default.
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• W3045035825 date "2020-07-27" @default.
• W3045035825 modified "2023-09-30" @default.
• W3045035825 title "The Milky Way’s bulge star formation history as constrained from its bimodal chemical abundance distribution" @default.
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