Characterizing the Low-Mass Pre-Main-Sequence Population in the Low-Metallicity Star-Forming Region Dolidze 25 Using VLT-MUSE

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 ($M<1M_{\odot }$) in the exceptionally metal-poor cluster Dolidze~25 ($Z\approx 0.2Z_{\odot }$), using VLT/MUSE observations to probe accretion processes and disk evolution in a subsolar environment. We identify 132 cluster members using a combination of $\mathit{\text{Gaia}}$ 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, luminosities enabling robust estimates of stellar masses and ages. Mass accretion rates (${\dot{M}}_{\mathrm{a}\mathrm{c}\mathrm{c}}$) derived from H$\alpha$ emission span ${10}^{-10}$–${10}^{-8}{M}_{\odot }{\mathrm{y}\mathrm{r}}^{-1}$ with a median value of $8\times {10}^{-10}{M}_{\odot }{\mathrm{y}\mathrm{r}}^{-1}$. These rates are comparable to those in solar-metallicity regions of 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 $T_{\mathrm{e}\mathrm{f}\mathrm{f}}$ (by approximately $300\mathrm{K}$) and $A_V$ (by around $0.5\mathrm{m}\mathrm{a}\mathrm{g}$), 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.