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.webp?t=eyJ3aWR0aCI6MTY5NiwiZmlsZV9leHRlbnNpb24iOiJ3ZWJwIiwib2JqX2lkIjo0NDg1OTMwfQ%3D%3D--5f19c5a883ebd47d37690f7f76456ce3479fcd8c "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=eyJ3aWR0aCI6MTM3OCwib2JqX2lkIjo0NDg1OTMwfQ%3D%3D--312e6f017a30adfc1bdb2674e44d3a2463b3150f)
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.webp?t=eyJ3aWR0aCI6OTYwLCJmaWxlX2V4dGVuc2lvbiI6IndlYnAiLCJvYmpfaWQiOjQ0ODU5MDh9--a695afba22b984bebfb63501aeacc735bc762279 "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=eyJ3aWR0aCI6OTY2LCJvYmpfaWQiOjQ0ODU5MDh9--7ec2b19b9f596dc8a555cd9b44c1ebc164827de0)
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.