2025MNRAS.544.2493Z

RR Lyrae stars have long been considered reliable tracers of old metal-poor populations, primarily due to their prevalence in globular clusters and the Galactic halo. However, the discovery of a metal-rich subpopulation in the Galactic disc, kinematically colder and more rotationally supported, challenges this classical view. Understanding the age of these metal-rich RR Lyrae stars is crucial for constraining their formation pathways and assessing what Galactic populations they are tracing. In this work, we leverage the unprecedented astrometric precision of Gaia DR3 to infer the age distribution of metal-rich RR Lyrae stars through a kinematic comparison with O-rich Mira variables. Mira variables, with their well-established period-age relation, serve as a natural clock, allowing us to transfer age information to RR Lyrae stars via their phase-space properties. By applying this approach across different metallicity bins, we find that the most metal-rich RR Lyrae stars ($[\rm Fe/H] > -0.5$) exhibit kinematics consistent with long-period ($\rm {period}\approx 150\, \rm {d}$) young Mira variable population; their ages correspond to $\sim 6\!-\!7$ Gyr (adopting the period-age relation in H. Zhang & J. L. Sanders 2023), which is significantly younger than typically assumed for RR Lyrae stars. In contrast, those with $-1 < [\rm Fe/H] < -0.5$ show properties more aligned with older ($\approx 9\!-\!11$ Gyr) populations. Interestingly, we also find evidence of a possible double-age population for the most metal-rich RR Lyrae, one younger with ages between 4 and 6 Gyr, and another one older ranging from 8 to 9 Gyr. These results provide strong evidence that metal-rich RR Lyrae stars in the Galactic field do not exclusively trace ancient populations. This finding challenges the current model of RR Lyrae formation and supports alternative formation scenarios, such as binary evolution.