Hα emission line sources from VLT-MUSE in a low-metallicity star forming region—Dolidze 25.

The process of accretion through circumstellar disks in young stellar objects is an integral part of star formation and the H α emission line is a prominent signature of accretion in low-mass stars. We present the detection and characterization of H α emission line sources in the central region of a distant, low-metallicity young stellar cluster Dolidze 25 (at ∼ 4.5 kpc) using medium-resolution optical spectra (4750–9350 Å) obtained with the multi-unit spectroscopic explorer (MUSE) at the VLT. We have identified 14 potential accreting sources within a rectangular region of ( 2 ′ × 1 ′ ) towards the center of the cluster based on the detection of strong and broad emissions in H α as well as the presence of other emission lines, such as [OI] and H β . 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. [ABSTRACT FROM AUTHOR]