| Authors: | M. Ashraf 1, J. Jose 1, G. Herczeg 2, M. Fan 3 |
| Affiliations: | (1) Indian Institute of Science Education and Research Tirupati, Tirupati, India; (2) Kavli Institute of Astronomy and Astrophysics, China; (3) Purple Mountain Observatory, China |
| Accepted by: | Journal of Astrophysics and Astronomy |
| URL: | https://ui.adsabs.harvard.edu/abs/2023arXiv230405019A/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 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.
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