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  APOGEE Chemical Abundances of the Large Magellanic Cloud

Hasselquist, S., Nidever, D., Hayes, C. R., Anguiano, B., Majewski, S., Sobeck, J., et al. (2019). APOGEE Chemical Abundances of the Large Magellanic Cloud. In American Astronomical Society Meeting Abstracts #233.

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Hasselquist, Sten1, Author
Nidever, David1, Author
Hayes, Christian R.1, Author
Anguiano, Borja1, Author
Majewski, Steve1, Author
Sobeck, Jennifer1, Author
Stringfellow, Guy1, Author
Beers, Timothy C.1, Author
Jonsson, Henrik1, Author
Lian, Jianhui1, Author
Cohen, Roger1, Author
Zasowski, Gail1, Author
Mackereth, John T.1, Author
Battaglia, Giuseppina1, Author
Weinberg, David1, Author
Lane, Richard R.1, Author
Long-Pena, Penelope1, Author
Gallart, Carme1, Author
Villanova, Sandro1, Author
Rix, Hans-Walter1, Author
Andrews, Brett1, AuthorCunha, Katia1, AuthorSmith, Verne1, AuthorChoi, Yumi1, AuthorGeisler, Doug1, AuthorCarrera, Ricardo1, AuthorAlmeida, Andres1, AuthorFernandez-Trincado, Jose G.1, Author more..
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1Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners, ou_2421692              

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 Abstract: To date, the SDSS-IV APOGEE survey has obtained S/N > 70 spectra for over 2,500 red giant stars distributed across much of the Large Magellanic Cloud (LMC), allowing for the characterization of the detailed abundance patterns for 10+ chemical elements. In this project, we interpret the chemical abundance patterns of the LMC by comparing them to the chemical abundance patterns of the Sagittarius Dwarf Galaxy (Sgr) and the Milky Way (MW), as well as by invoking chemical evolution models (such as flexCE and chempy) that include the LMC's star formation history. Preliminary results show that the LMC shares [Ni/Fe] and [Al/Fe] deficiencies with Sgr, but exhibits alpha-element abundances ([O/Fe], [Mg/Fe], and [Si/Fe]) that are near-solar. There is also a correlation with [O/Fe] and [Mg/Fe] with [Fe/H] at [Fe/H] > -1.0. These results suggest that the LMC exhibited low star formation efficiency (as compared to Sgr and the MW) at early times, but has since experienced several starbursts which spawned the stars with [Fe/H] > -1.0. Using these APOGEE chemical abundance patterns as constraints, we use chemical evolution models to better characterize the nature (strength, time, duration, IMF, etc.) of these starbursts.

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 Dates: 2019
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Title: American Astronomical Society Meeting Abstracts #233
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Start-/End Date: 2019

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Title: American Astronomical Society Meeting Abstracts #233
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