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Chemical Cartography with APOGEE: Large-scale Mean Metallicity Maps of the Milky Way | | Michael R. Hayden
; Jon A. Holtzman
; Jo Bovy
; Steven R. Majewski
; Carlos Allende Prieto
; Timothy C. Beers
; Katia Cunha
; Peter M. Frinchaboy
; Ana E. García Pérez
; Léo Girardi
; Fred R. Hearty
; Jennifer A. Johnson
; Young Sun Lee
; David Nidever
; Ricardo P. Schiavon
; Katharine J. Schlesinger
; Donald P. Schneider
; Mathias Schultheis
; Matthew Shetrone
; Verne V. Smith
; Gail Zasowski
; Dmitry Bizyaev
; Diane Feuillet
; Sten Hasselquist
; Karen Kinemuchi
; Elena Malanushenko
; Viktor Malanushenko
; Robert O'Connell
; Kaike Pan
; Keivan Stassun
; | | Date: |
18 Nov 2013 | | Abstract: | We present Galactic mean metallicity maps derived from the first year of the
SDSS-III APOGEE experiment. Mean abundances in different zones of
Galactocentric radius (0 < R < 15 kpc) at a range of heights above the plane (0
< |z| < 3 kpc), are derived from a sample of nearly 20,000 stars with
unprecedented coverage, including stars in the Galactic mid-plane at large
distances. We also split the sample into subsamples of stars with low and
high-[{alpha}/M] abundance ratios. We assess possible biases in deriving the
mean abundances, and find they are likely to be small except in the inner
regions of the Galaxy. A negative radial gradient exists over much of the
Galaxy; however, the gradient appears to flatten for R < 6 kpc, in particular
near the Galactic mid-plane and for low-[{alpha}/M] stars. At R > 6 kpc, the
gradient flattens as one moves off of the plane, and is flatter at all heights
for high-[{alpha}/M] stars than for low-[{alpha}/M] stars. Alternatively,
these gradients can be described as vertical gradients that flatten at larger
Galactocentric radius; these vertical gradients are similar for both low and
high-[{alpha}/M] populations. Stars with higher [{alpha}/M] appear to have a
flatter radial gradient than stars with lower [{alpha}/M]. This could suggest
that the metallicity gradient has grown steeper with time or, alternatively,
that gradients are washed out over time by migration of stars. | | Source: | arXiv, 1311.4569 | | Services: | Forum | Review | PDF | Favorites | |
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