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Chemical Cartography with APOGEE: Mapping Disk Populations with a Two-Process Model and Residual Abundances

Weinberg, David H.; Holtzman, Jon A.; Johnson, Jennifer A.; Hayes, Christian; Hasselquist, Sten; Shetrone, Matthew; Ting, Yuan-Sen; Beaton, Rachael L.; Beers, Timothy C.; Bird, Jonathan C.; Bizyaev, Dmitry; Blanton, Michael R.; Cunha, Katia; Fernandez-Trincado, Jose G.; Frinchaboy, Peter M.; Garcia-Hernandez, D.A.; Griffith, Emily; Johnson, James W.; Jönsson, Henrik; Lane, Richard R.; Leung, Henry W.; Mackereth, J. Ted; Majewski, Steven R.; Meszaros, Szabolcz; Nitschelm, Christian; Pan, Kaike; Schiavon, Ricardo P.; Schneider, Donald P.; Schultheis, Mathias; Smith, Verne; Sobeck, Jennifer S.; Stassun, Keivan G.; Stringfellow, Guy S.; Vincenzo, Fiorenzo; Wilson, John C.; Zasowski, Gail

Authors

David H. Weinberg

Jon A. Holtzman

Jennifer A. Johnson

Christian Hayes

Sten Hasselquist

Matthew Shetrone

Yuan-Sen Ting

Rachael L. Beaton

Timothy C. Beers

Jonathan C. Bird

Dmitry Bizyaev

Michael R. Blanton

Katia Cunha

Jose G. Fernandez-Trincado

Peter M. Frinchaboy

D.A. Garcia-Hernandez

Emily Griffith

James W. Johnson

Henrik Jönsson

Richard R. Lane

Henry W. Leung

J. Ted Mackereth

Steven R. Majewski

Szabolcz Meszaros

Christian Nitschelm

Kaike Pan

Ricardo P. Schiavon

Donald P. Schneider

Mathias Schultheis

Verne Smith

Jennifer S. Sobeck

Keivan G. Stassun

Guy S. Stringfellow

John C. Wilson

Gail Zasowski



Abstract

We apply a novel statistical analysis to measurements of 16 elemental abundances in 34,410 Milky Way disk stars from the final data release (DR17) of APOGEE-2. Building on recent work, we fit median abundance ratio trends [X/Mg] vs. [Mg/H] with a 2-process model, which decomposes abundance patterns into a "prompt" component tracing core collapse supernovae and a "delayed" component tracing Type Ia supernovae. For each sample star, we fit the amplitudes of these two components, then compute the residuals \Delta[X/H] from this two-parameter fit. The rms residuals range from ~0.01-0.03 dex for the most precisely measured APOGEE abundances to ~0.1 dex for Na, V, and Ce. The correlations of residuals reveal a complex underlying structure, including a correlated element group comprised of Ca, Na, Al, K, Cr, and Ce and a separate group comprised of Ni, V, Mn, and Co. Selecting stars poorly fit by the 2-process model reveals a rich variety of physical outliers and sometimes subtle measurement errors. Residual abundances allow comparison of populations controlled for differences in metallicity and [\alpha/Fe]. Relative to the main disk (R=3-13 kpc, |Z|<2 kpc), we find nearly identical abundance patterns in the outer disk (R=15-17 kpc), 0.05-0.2 dex depressions of multiple elements in LMC and Gaia Sausage/Enceladus stars, and wild deviations (0.4-1 dex) of multiple elements in \omega Cen. Residual abundance analysis opens new opportunities for discovering chemically distinctive stars and stellar populations, for empirically constraining nucleosynthetic yields, and for testing chemical evolution models that include stochasticity in the production and redistribution of elements.

Citation

Weinberg, D. H., Holtzman, J. A., Johnson, J. A., Hayes, C., Hasselquist, S., Shetrone, M., …Zasowski, G. (2022). Chemical Cartography with APOGEE: Mapping Disk Populations with a Two-Process Model and Residual Abundances. The Astrophysical journal. Supplement series, 260(2), Article 32. https://doi.org/10.3847/1538-4365/ac6028

Journal Article Type Article
Acceptance Date Mar 21, 2022
Online Publication Date Jun 17, 2022
Publication Date 2022-06
Deposit Date Mar 12, 2022
Publicly Available Date Mar 28, 2024
Print ISSN 1538-4365
Publisher American Astronomical Society
Peer Reviewed Not Peer Reviewed
Volume 260
Issue 2
Article Number 32
DOI https://doi.org/10.3847/1538-4365/ac6028
Public URL https://hull-repository.worktribe.com/output/3948511

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Publisher Licence URL
http://creativecommons.org/licenses/by/4.0

Copyright Statement
© 2022. The Author(s).
Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.




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