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 < 1 M⊙) in t...
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| Autori principali: | , , , , , , , , |
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| Natura: | Article (Journal) |
| Lingua: | inglese |
| Pubblicazione: |
2026 February 5
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| In: |
The astrophysical journal
Year: 2026, Volume: 998, Fascicolo: 1, Pages: 1-21 |
| ISSN: | 1538-4357 |
| DOI: | 10.3847/1538-4357/ae28cf |
| Accesso online: | Verlag, kostenfrei, Volltext: https://doi.org/10.3847/1538-4357/ae28cf Verlag, kostenfrei, Volltext: https://iopscience.iop.org/article/10.3847/1538-4357/ae28cf 
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| Note sull'autore: | Mizna Ashraf, Jessy Jose, Gregory J. Herczeg, Min Fang, Varsha Ramachandran, Carlo F. Manara, Christian Schneider, Megan Reiter, and Kiran Kumar Sunil |
| Riassunto: | 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 < 1 M⊙) in the exceptionally metal-poor cluster Dolidze 25 (Z ≈ 0.2 Z⊙), using Very Large Telescope/MUSE observations to probe accretion processes and disk evolution in a subsolar environment. We identify 132 cluster members using a combination of 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, and luminosities enabling robust estimates of stellar masses and ages. Mass accretion rates () derived from Hα emission span 10−10-10−8 M⊙ yr−1 with a median value of 8 × 10−10 M⊙ yr−1. These rates are comparable to those in solar-metallicity regions of a 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 Teff (by approximately 300 K) and AV (by around 0.5 mag), 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. |
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| Descrizione del documento: | Gesehen am 09.06.2026 |
| Descrizione fisica: | Online Resource |
| ISSN: | 1538-4357 |
| DOI: | 10.3847/1538-4357/ae28cf |