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| Format: | Preprint |
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2025
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| Online Access: | https://arxiv.org/abs/2510.14733 |
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| _version_ | 1866908597927018496 |
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| author | Cheshire, Ishani Armstrong, Joseph J. Tan, Jonathan C. |
| author_facet | Cheshire, Ishani Armstrong, Joseph J. Tan, Jonathan C. |
| contents | Aims: Studying the dynamical evolution of young clusters is crucial for a more general understanding of the star formation process. Methods: We took spectra of >600 candidate pre-main sequence (PMS) stars in several nearby young clusters (NGC 2264 N & S, Collinder 95, and Collinder 359) using MMT/Hectospec. These spectra were analyzed for Hα emission and lithium absorption, features indicative of low-mass young stellar objects (YSOs) still in their PMS evolution. We complemented these samples with YSOs identified via Gaia DR3 variability. In conjunction with Gaia astrometry, these data enable an analysis of cluster structure, kinematics and ages. In particular, we searched for halos of YSOs around our targets to test models of young cluster dynamical evolution. Results: For the NGC 2264 N & S cluster pair we identified 354 YSOs, while for Collinder 95 and 359 we identified 130 and 7 YSOs, respectively. We calculate kinematic "traceback ages" for YSOs in these clusters, which we compare to isochronal ages estimated using several sets of stellar evolution models. We find for NGC 2264 N & S that kinematic ages are generally smaller than their isochronal ages, which may indicate these systems remained bound for a few Myr before their current state of expansion. On the other hand, kinematic ages for Collinder 95 are often significantly larger than isochronal ages, which implies many of these YSOs did not originate from a central, dense region, leading to overestimated kinematic ages. Conclusions: We conclude that NGC 2264 N & S clusters likely formed as initially bound and compact systems, but have been gradually evaporating as cluster members become unbound, forming halos of unbound YSOs surrounding the cluster cores. We conclude that Collinder 95 likely formed initially sparse and substructured and has been dispersing since gas expulsion. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2510_14733 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Expansion kinematics of young clusters. II. NGC 2264 N & S and Collinder 95 with HectoSpec Cheshire, Ishani Armstrong, Joseph J. Tan, Jonathan C. Solar and Stellar Astrophysics Aims: Studying the dynamical evolution of young clusters is crucial for a more general understanding of the star formation process. Methods: We took spectra of >600 candidate pre-main sequence (PMS) stars in several nearby young clusters (NGC 2264 N & S, Collinder 95, and Collinder 359) using MMT/Hectospec. These spectra were analyzed for Hα emission and lithium absorption, features indicative of low-mass young stellar objects (YSOs) still in their PMS evolution. We complemented these samples with YSOs identified via Gaia DR3 variability. In conjunction with Gaia astrometry, these data enable an analysis of cluster structure, kinematics and ages. In particular, we searched for halos of YSOs around our targets to test models of young cluster dynamical evolution. Results: For the NGC 2264 N & S cluster pair we identified 354 YSOs, while for Collinder 95 and 359 we identified 130 and 7 YSOs, respectively. We calculate kinematic "traceback ages" for YSOs in these clusters, which we compare to isochronal ages estimated using several sets of stellar evolution models. We find for NGC 2264 N & S that kinematic ages are generally smaller than their isochronal ages, which may indicate these systems remained bound for a few Myr before their current state of expansion. On the other hand, kinematic ages for Collinder 95 are often significantly larger than isochronal ages, which implies many of these YSOs did not originate from a central, dense region, leading to overestimated kinematic ages. Conclusions: We conclude that NGC 2264 N & S clusters likely formed as initially bound and compact systems, but have been gradually evaporating as cluster members become unbound, forming halos of unbound YSOs surrounding the cluster cores. We conclude that Collinder 95 likely formed initially sparse and substructured and has been dispersing since gas expulsion. |
| title | Expansion kinematics of young clusters. II. NGC 2264 N & S and Collinder 95 with HectoSpec |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2510.14733 |