\(H\alpha \) emission line sources from VLT-MUSE in a low-metallicity star forming region—Dolidze 25

Abstract

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 Å) obtained with the multi-unit spectroscopic explorer (MUSE) at the VLT. We have identified 14 potential accreting sources within a rectangular region of (\(2' \times 1'\)) 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.