Spectroscopic Surveys
![Observed mono-abundance stellar populations (MAPs) in the Milky Way disk. The plot shows the correlation between the radial scale length and the vertical scale height of MAPs, color-coded by [α/Fe]. The size of the points corresponds to the total stellar surface-mass density—corrected for mass and sample selection effects—in each population. MAPs appear to have a simple spatial structure, approximated by a single exponential in the radial and vertical directions.](/4485919/original-1518438323.jpg?t=eyJ3aWR0aCI6ODAwLCJoZWlnaHQiOjYwMCwib2JqX2lkIjo0NDg1OTE5fQ%3D%3D--da48c9adae4c63dad3dd37f829b7766925a74002)
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Observed mono-abundance stellar populations (MAPs) in the Milky Way disk. The plot shows the correlation between the radial scale length and the vertical scale height of MAPs, color-coded by [α/Fe]. The size of the points corresponds to the total stellar surface-mass density—corrected for mass and sample selection effects—in each population. MAPs appear to have a simple spatial structure, approximated by a single exponential in the radial and vertical directions.
Observed mono-abundance stellar populations (MAPs) in the Milky Way disk. The plot shows the correlation between the radial scale length and the vertical scale height of MAPs, color-coded by [α/Fe]. The size of the points corresponds to the total stellar surface-mass density—corrected for mass and sample selection effects—in each population. MAPs appear to have a simple spatial structure, approximated by a single exponential in the radial and vertical directions.
MPIA/Bovy et al 2012
MPIA/Bovy et al 2012
Spectroscopic surveys, such as SDSS-IV, provide stellar parameters, ages, and abundances.
