The Geneva-Copenhagen Survey of the Solar neighbourhood II. New uvby calibrations and rediscussion of stellar ages, the G dwarf problem, age-metallicity diagram, and heating mechanisms of the disk

TL;DR

This paper refines uvby photometric calibrations for F and G stars, reassesses stellar ages and metallicities, and discusses implications for galactic disk evolution, including the G-dwarf problem and disk heating mechanisms.

Contribution

It improves temperature and metallicity calibrations, provides reliable age determinations, and offers new insights into the chemical and dynamical evolution of the Galactic disk.

Findings

Revised G-dwarf metallicity distribution remains incompatible with closed-box models.

Age-metallicity relation for the thin disk is nearly flat with significant scatter.

Disk heating continues throughout the disk's lifetime, affecting stellar velocities.

Abstract

Ages, metallicities, space velocities, and Galactic orbits of stars in the Solar neighbourhood are fundamental observational constraints on models of galactic disk evolution. We aim to consolidate the calibrations of uvby photometry into Te, [Fe/H], distance, and age for F and G stars and rediscuss the results of the Geneva-Copenhagen Survey (Nordstrom et al. 2004; GCS) in terms of the evolution of the disk. We substantially improve the Te and [Fe/H] calibrations for early F stars, where spectroscopic temperatures have large systematic errors. Our recomputed ages are in excellent agreement with the independent determinations by Takeda et al. (2007), indicating that isochrone ages can now be reliably determined. The revised G-dwarf metallicity distribution remains incompatible with closed-box models, and the age-metallicity relation for the thin disk remains almost flat, with large and real scatter at all ages (sigma intrinsic = 0.20 dex). Dynamical heating of the thin disk continues throughout its life; specific in-plane dynamical effects dominate the evolution of the U and V velocities, while the W velocities remain random at all ages. When assigning thick and thin-disk membership for stars from kinematic criteria, parameters for the oldest stars should be used to characterise the thin disk.