  The process of accretion through circumstellar disks in young stellar objects
is an integral part of star formation and the $H\alpha$ emission line is a
prominent signature of accretion in low-mass stars. We present the detection
and characterization of $H\alpha$ emission line sources in the central region
of a distant, low-metallicity young stellar cluster - Dolidze 25 (at $\sim$ 4.5
kpc) - using medium-resolution optical spectra (4750-9350 \r{A} ) obtained with
the Multi-Unit Spectroscopic Explorer (MUSE) at the VLT. We have identified 14
potential accreting sources within a rectangular region of (2$'$ x 1$'$)
towards the center of the cluster based on the detection of strong and broad
emissions in $H\alpha$ as well as the presence of other emission lines such as
[OI] and $H\beta$. Based on their positions in both photometric color-magnitude
and color-color diagrams, we have also confirmed that these objects belong to
the pre-main sequence phase of star formation. Our results were compared with
the disk and diskless members of the cluster previously identified by Guarcello
et al. (2021) using near-IR colors, and all sources they had identified as
disks were confirmed to be accreting based on the spectroscopic
characteristics.
