2026ApJ...998..116A

The metallicity of the star-forming environment is a fundamental parameter shaping the evolution of protoplanetary disks and the formation of planetary systems, yet its influence remains poorly constrained. We present a spectroscopic study of low-mass pre-main-sequence (PMS) stars (M < 1 M_⊙) in the exceptionally metal-poor cluster Dolidze 25 (Z ≈ 0.2 Z_⊙), using Very Large Telescope/MUSE observations to probe accretion processes and disk evolution in a subsolar environment. We identify 132 cluster members using a combination of Gaia astrometry and spectroscopic youth indicators, including lithium absorption and Balmer emission. The stellar parameters are derived using low-metallicity BT-Settl models yielding effective temperatures, extinctions, and luminosities enabling robust estimates of stellar masses and ages. Mass accretion rates (${\dot{M}}_{{\rm{acc}}}$) derived from Hα emission span 10^–10-10^–8M_⊙ yr^–1 with a median value of 8 × 10^–10M_⊙ yr^–1. These rates are comparable to those in solar-metallicity regions of a similar age, such as Lupus and Orion, indicating minimal metallicity dependence in accretion processes. Our analysis shows that using solar-metallicity templates to fit low-metallicity stars leads to systematic overestimations of T_eff (by approximately 300 K) and A_V (by around 0.5 mag), underscoring the importance of employing metallicity-matched models for reliable characterization in low-Z environments. We present flux-calibrated, extinction-corrected spectra of these metal-poor PMS stars as a valuable resource for future investigations of disk evolution in subsolar regimes.