Investigating the timescales traced by dynamical ages in young stellar systems
Abstract
Stars form in clustered environments, and then the stars may congregate into star clusters. The timescale on which individual stars form is not necessarily the same as the timescale on which star clusters assemble. Therefore, developing methods to probe these different timescales is a crucial part of understanding star cluster assembly and early evolution. Dynamical ages can be constructed from the kinematics of individual stars in clusters in the solar neighborhood using Gaia data. Using a star formation simulation, we test five different dynamical age methods. We divide dynamical ages into two approaches: methods which trace the size evolution of the cluster, and methods which trace the trajectories of individual stars. We confirm that size methods cannot accurately derive ages in bound clusters whereas methods tracing individual stars can be applied to both bound and unbound systems. We find that different dynamical age methods trace different epochs of star cluster formation and assembly: The method using stars with the oldest traceback ages provides an upper limit on stellar ages and the method using the median traceback ages is the best proxy for isochronal ages. Methods which trace the size evolution of the cluster best trace the onset of cluster expansion. Our work suggests that the median traceback time of stars moving away from the cluster provides the most reliable proxy for isochronal age, and that this method can be applied to any expanding system.
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BibTeX
@misc{armstrong2026investigating,
title = {{Investigating the timescales traced by dynamical ages in young stellar systems}},
author = {Isabella Armstrong and Alison Sills and Claude Cournoyer-Cloutier},
howpublished = {arXiv},
year = {2026},
month = nov,
doi = {10.48550/arxiv.2611.12594},
eprint = {2611.12594},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2611.12594},
}
RIS
TY - UNPB
TI - Investigating the timescales traced by dynamical ages in young stellar systems
AU - Isabella Armstrong
AU - Alison Sills
AU - Claude Cournoyer-Cloutier
PY - 2026
DA - 2026/11/09
PB - arXiv
DO - 10.48550/arxiv.2611.12594
UR - https://arxiv.org/abs/2611.12594
AB - Stars form in clustered environments, and then the stars may congregate into star clusters. The timescale on which individual stars form is not necessarily the same as the timescale on which star clusters assemble. Therefore, developing methods to probe these different timescales is a crucial part of understanding star cluster assembly and early evolution. Dynamical ages can be constructed from the kinematics of individual stars in clusters in the solar neighborhood using Gaia data. Using a star formation simulation, we test five different dynamical age methods. We divide dynamical ages into two approaches: methods which trace the size evolution of the cluster, and methods which trace the trajectories of individual stars. We confirm that size methods cannot accurately derive ages in bound clusters whereas methods tracing individual stars can be applied to both bound and unbound systems. We find that different dynamical age methods trace different epochs of star cluster formation and assembly: The method using stars with the oldest traceback ages provides an upper limit on stellar ages and the method using the median traceback ages is the best proxy for isochronal ages. Methods which trace the size evolution of the cluster best trace the onset of cluster expansion. Our work suggests that the median traceback time of stars moving away from the cluster provides the most reliable proxy for isochronal age, and that this method can be applied to any expanding system.
ER -