Dynamical Models
![Figure 7. Age and abundances for stars with seismic and spectroscopic information from Kepler and APOGEE. The plot shows the distribution of the sample in the [α/M] versus [M/H] plane. Small white dots represent stars for which ages are not measured (i.e., stars with a mass smaller than 1.2 M☉), and colored dots represent stars younger than 7 Gyr (the color encodes the maximal age of each star).](/4485930/original-1518438323.jpg?t=eyJ3aWR0aCI6ODQ4LCJmaWxlX2V4dGVuc2lvbiI6ImpwZyIsIm9ial9pZCI6NDQ4NTkzMH0%3D--7cea9128b670ba769fe7e3555b0da0e4d7e71236 "Figure 7. Age and abundances for stars with seismic and spectroscopic information from Kepler and APOGEE. The plot shows the distribution of the sample in the [α/M] versus [M/H] plane. Small white dots represent stars for which ages are not measured (i.e., stars with a mass smaller than 1.2 M☉), and colored dots represent stars younger than 7 Gyr (the color encodes the maximal age of each star).")
![Figure 7. Age and abundances for stars with seismic and spectroscopic information from Kepler and APOGEE. The plot shows the distribution of the sample in the [α/M] versus [M/H] plane. Small white dots represent stars for which ages are not measured (i.e., stars with a mass smaller than 1.2 M☉), and colored dots represent stars younger than 7 Gyr (the color encodes the maximal age of each star).](/4485930/original-1518438323.jpg?t=eyJ3aWR0aCI6MjQ2LCJvYmpfaWQiOjQ0ODU5MzB9--31aa9ac5452c008022380f778f8b23f214be9bd4)
Figure 7. Age and abundances for stars with seismic and spectroscopic information from Kepler and APOGEE. The plot shows the distribution of the sample in the [α/M] versus [M/H] plane. Small white dots represent stars for which ages are not measured (i.e., stars with a mass smaller than 1.2 M☉), and colored dots represent stars younger than 7 Gyr (the color encodes the maximal age of each star).
MPIA/Martig et al 2015
![Surface density as a function of radius as measured by SEGUE G-dwarf mono-abundance stellar populations (MAPs). Each point represents a measurement based on the data from one MAP; each MAP measures the surface density Σ(R, |Z| 1.1 kpc) at the radius R where the correlation between the model stellar disk scale length and Σ(R0, |Z| 1.1 kpc) is minimized in the MAP’s PDF. The curve is an exponential fit with Σ(R0, |Z| 1.1 kpc) = 69 M☉ pc−2 and a scale length of 2.5 kpc. Points are color-coded by the [α/Fe] of the MAP bin, from [α/Fe] = 0.025 (dark blue) to [α/Fe] = 0.475 (red/brown).](/4485908/original-1518438323.jpg?t=eyJ3aWR0aCI6MzQxLCJmaWxlX2V4dGVuc2lvbiI6ImpwZyIsIm9ial9pZCI6NDQ4NTkwOH0%3D--e52c5ca63ba60f2512b0bae15cc5f1e293d54045 "Surface density as a function of radius as measured by SEGUE G-dwarf mono-abundance stellar populations (MAPs). Each point represents a measurement based on the data from one MAP; each MAP measures the surface density Σ(R, |Z| 1.1 kpc) at the radius R where the correlation between the model stellar disk scale length and Σ(R0, |Z| 1.1 kpc) is minimized in the MAP’s PDF. The curve is an exponential fit with Σ(R0, |Z| 1.1 kpc) = 69 M☉ pc−2 and a scale length of 2.5 kpc. Points are color-coded by the [α/Fe] of the MAP bin, from [α/Fe] = 0.025 (dark blue) to [α/Fe] = 0.475 (red/brown).")
![Surface density as a function of radius as measured by SEGUE G-dwarf mono-abundance stellar populations (MAPs). Each point represents a measurement based on the data from one MAP; each MAP measures the surface density Σ(R, |Z| 1.1 kpc) at the radius R where the correlation between the model stellar disk scale length and Σ(R0, |Z| 1.1 kpc) is minimized in the MAP’s PDF. The curve is an exponential fit with Σ(R0, |Z| 1.1 kpc) = 69 M☉ pc−2 and a scale length of 2.5 kpc. Points are color-coded by the [α/Fe] of the MAP bin, from [α/Fe] = 0.025 (dark blue) to [α/Fe] = 0.475 (red/brown).](/4485908/original-1518438323.jpg?t=eyJ3aWR0aCI6MjQ2LCJvYmpfaWQiOjQ0ODU5MDh9--d20f4e63e1559c85e16f6f39a481ba76ac46a57f)
Surface density as a function of radius as measured by SEGUE G-dwarf mono-abundance stellar populations (MAPs). Each point represents a measurement based on the data from one MAP; each MAP measures the surface density Σ(R, |Z| 1.1 kpc) at the radius R where the correlation between the model stellar disk scale length and Σ(R0, |Z| 1.1 kpc) is minimized in the MAP’s PDF. The curve is an exponential fit with Σ(R0, |Z| 1.1 kpc) = 69 M☉ pc−2 and a scale length of 2.5 kpc. Points are color-coded by the [α/Fe] of the MAP bin, from [α/Fe] = 0.025 (dark blue) to [α/Fe] = 0.475 (red/brown).
MPIA/Bovy and Rix 2013
Dynamical models characterize the Milky Way gravitational potential based on stellar positions and motions.