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APOGEE Chemical Abundance Patterns of the Massive Milky Way Satellites

Hasselquist, S, Hayes, CR, Lian, J, Weinberg, DH, Zasowski, G, Horta, D, Beaton, R, Feuillet, DK, Garro, ER, Gallart, C, Smith, VV, Holtzman, JA, Minniti, D, Lacerna, I, Shetrone, M, Jonsson, H, Cioni, M-RL, Fillingham, SP, Cunha, K, O'Connell, R , Fernandez-Trincado, JG, Munoz, RR, Schiavon, RP, Almeida, A, Anguiano, B, Beers, TC, Bizyaev, D, Brownstein, JR, Cohen, RE, Frinchaboy, P, Garcia-Hernandez, DA, Geisler, D, Lane, RR, Majewski, SR, Nidever, DL, Nitschelm, C, Povick, J, Price-Whelan, A, Roman-Lopes, A, Rosado, M, Sobeck, J, Stringfellow, G, Valenzuela, O, Villanova, S and Vincenzo, F (2021) APOGEE Chemical Abundance Patterns of the Massive Milky Way Satellites. ASTROPHYSICAL JOURNAL, 923 (2). ISSN 0004-637X

Apogee chemical abundance patterns of the massive milky way satellites.pdf - Accepted Version

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The SDSS-IV Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey has obtained high-resolution spectra for thousands of red giant stars distributed among the massive satellite galaxies of the Milky Way (MW): the Large and Small Magellanic Clouds (LMC/SMC), the Sagittarius Dwarf Galaxy (Sgr), Fornax (Fnx), and the now fully disrupted Gaia Sausage/Enceladus (GSE) system. We present and analyze the APOGEE chemical abundance patterns of each galaxy to draw robust conclusions about their star formation histories, by quantifying the relative abundance trends of multiple elements (C, N, O, Mg, Al, Si, Ca, Fe, Ni, and Ce), as well as by fitting chemical evolution models to the [α/Fe]–[Fe/H] abundance plane for each galaxy. Results show that the chemical signatures of the starburst in the Magellanic Clouds (MCs) observed by Nidever et al. in the α-element abundances extend to C+N, Al, and Ni, with the major burst in the SMC occurring some 3–4 Gyr before the burst in the LMC. We find that Sgr and Fnx also exhibit chemical abundance patterns suggestive of secondary star formation epochs, but these events were weaker and earlier (∼5–7 Gyr ago) than those observed in the MCs. There is no chemical evidence of a second starburst in GSE, but this galaxy shows the strongest initial star formation as compared to the other four galaxies. All dwarf galaxies had greater relative contributions of AGB stars to their enrichment than the MW. Comparing and contrasting these chemical patterns highlight the importance of galaxy environment on its chemical evolution.

Item Type: Article
Uncontrolled Keywords: Astronomy & Astrophysics; DATA RELEASE; DIGITAL SKY SURVEY; GALACTIC HALO; GLOBULAR-CLUSTERS; LOCAL GROUP; MAIN BODY; Physical Sciences; RAM PRESSURE; SAGITTARIUS DWARF GALAXY; Science & Technology; STAR-FORMATION HISTORY; STELLAR POPULATIONS; Science & Technology; Physical Sciences; Astronomy & Astrophysics; STAR-FORMATION HISTORY; SAGITTARIUS DWARF GALAXY; DIGITAL SKY SURVEY; STELLAR POPULATIONS; GLOBULAR-CLUSTERS; GALACTIC HALO; RAM PRESSURE; DATA RELEASE; LOCAL GROUP; MAIN BODY; Astronomy & Astrophysics; 0201 Astronomical and Space Sciences; 0202 Atomic, Molecular, Nuclear, Particle and Plasma Physics; 0306 Physical Chemistry (incl. Structural)
Subjects: Q Science > QB Astronomy
Divisions: Astrophysics Research Institute
Publisher: IOP Publishing Ltd
SWORD Depositor: A Symplectic
Date Deposited: 10 Oct 2022 14:39
Last Modified: 20 Dec 2022 00:50
DOI or ID number: 10.3847/1538-4357/ac25f9
URI: https://researchonline.ljmu.ac.uk/id/eprint/17787
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