• Milky Way
• star formation history
• stellar evolution
• Thin Disk
• white dwarf

A crucial aspect of understanding the Milky Way’s formation and evolution is determining its Star Formation History (SFH). Despite the exceptional data quality provided by Gaia, the SFH of the Thin Disk of the Milky Way remains highly uncertain. To address this, we developed a technique that aims to validate a specific SFH of the Thin Disk using the local population of white dwarfs (WDs) observed by the third Gaia data release within 40 pc from the Sun. For this task, we created a new Python code that, for the first time, generates synthetic color-magnitude diagrams simulating stars in all evolutionary phases, from the Pre-Main Sequence to the WD phase. Our code is highly flexible, enabling the use of various WD cooling models, which describe the WD evolution and its cooling processes, and different Initial-to-Final Mass Relations (IFMRs), which connect the initial mass of the progenitor star to the final mass of the resulting WD. The procedure confirmed the reliability of the overall shape of three independent SFH solutions from recent literature, derived from stars up to the AGB phase, and placed additional constraints on the ancient part of the SFHs, which remain highly uncertain. From this perspective, our work indicates that the Thin Disk of the Milky Way is likely no older than approximately 11 Gyr.