Exploring the chemo-kinematics of the solar neighbourhood with Gaia DR3

When did the first planets form in the galaxy? The first few generations of stars were too metal-poor to form any planets. As the metallicity of the ISM and the stars in the Galaxy progressively increases, rocky Earth-like planets are formed first. However, for the formation of Jupiter-like planets, a 10-15 Earth-mass core that is relatively rich in iron needs to form first. Therefore, Jupiter-like gas giants are likely to have formed much later when the Galactic metallicity has increased significantly. But it's challenging to measure the ages of main-sequence stars. However, using the dispersion in the peculiar velocities of stars, it is possible to measure the average ages of the stars.  In this contribution, we present our results from the chemo-kinematics study of the solar neighborhood using data from Gaia DR3. We compare the abundance and age distribution for a sample of field stars, debris disk, and exoplanet host stars. Our analysis shows that Jupiter-like planets only formed in the last 5-6 Gyr after significant enrichment of the galactic ISM with metals. We further find that debris disks are also young yet they are metal-poor.  I will discuss these results in the context of disk evolution and planet formation.