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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). Zoom Image
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).
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). Zoom Image
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).

Dynamical models characterize the Milky Way gravitational potential based on stellar positions and motions.

 
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