Bayesian isochrone fitting and stellar ages
arXiv:1607.03000 · doi:10.1051/eas/1465006
Abstract
Stellar evolution theory has been extraordinarily successful at explaining the different phases under which stars form, evolve and die. While the strongest constraints have traditionally come from binary stars, the advent of asteroseismology is bringing unique measures in well-characterised stars. For stellar populations in general, however, only photometric measures are usually available, and the comparison with the predictions of stellar evolution theory have mostly been qualitative. For instance, the geometrical shapes of isochrones have been used to infer ages of coeval populations, but without any proper statistical basis. In this chapter we provide a pedagogical review on a Bayesian formalism to make quantitative inferences on the properties of single, binary and small ensembles of stars, including unresolved populations. As an example, we show how stellar evolution theory can be used in a rigorous way as a prior information to measure the ages of stars between the ZAMS and the Helium flash, and their uncertainties, using photometric data only.
43 pages, Proceedings of the Evry Schatzman School of Stellar Astrophysics "The ages of stars", EAS Publications Series, Volume 65
References in corpus (20)
- Bayes in the sky: Bayesian inference and model selection in cosmology
- New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey
- Basic physical parameters of a selected sample of evolved stars
- The accretion origin of the Milky Way's stellar halo
- Structure and Evolution of Nearby Stars with Planets II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog
- Radius determination of solar-type stars using asteroseismology: What to expect from the Kepler mission
- The Distances to Open Clusters from Main-Sequence Fitting. III. Improved Accuracy with Empirically Calibrated Isochrones
- A maximum likelihood method for fitting colour-magnitude diagrams
- Ground-based CCD astrometry with wide field imagers. II. A star catalogue for M67: [email protected] MPG/ESO astrometry, FLAMES@VLT radial velocities
- Fitting the young main-sequence; distances, ages and age spreads
- Recovering the star formation rate in the solar neighborhood
- Inverting Color-Magnitude Diagrams to Access Precise Star Cluster Parameters: A Bayesian Approach
- Metallicities for 13 nearby open clusters from high-resolution spectroscopy of dwarf and giant stars. Stellar metallicity, stellar mass, and giant planets
- Models of alpha Centauri A and B with and without seismic constraints: time dependence of the mixing-length parameter
- Modelling the components of binaries in Hyades: The dependence of the mixing-length parameter on stellar mass
- A robust statistical estimation of the basic parameters of single stellar populations. I. Method
- Structure Through Colour: A Pixel Approach Towards Understanding Galaxies
- New Techniques to Determine Ages of Open Clusters Using White Dwarfs
- A new level of photometric precision: WIRE observations of eclipsing binary stars
- Restoring Color-magnitude Diagrams with the Richardson-Lucy Algorithm