  Accurate age estimation of nearby young moving groups (NYMGs) is important as
they serve as crucial testbeds in various fields of astrophysics, including
formation and evolution of stars, planets, as well as loose stellar
associations. The $\beta$-Pictoris moving group (BPMG), being one of the
closest and youngest NYMGs, has been extensively investigated, and its
estimated ages have a wide range from $\sim$10 to 25 Myr, depending on the age
estimation methods and data used. Unlike other age dating methods, kinematic
traceback analysis offers a model-independent age assessment hence the merit in
comparing many seemingly discordant age estimates. In this study, we determine
the kinematic ages of the BPMG using three methods: probabilistic volume
calculation, mean pairwise distance calculation, and covariance matrix
analysis. These methods yield consistent results, with estimated ages in the
range of 14 to 20 Myr. Implementing corrections to radial velocities due to
gravitational redshift and convectional blueshift increases the ages by
$\sim2-4$ Myr. Conversely, considering data uncertainties decreases the
estimated ages by 1 to 2 Myr. Taken together, our analysis determined the
kinematic age of BPMG to be 16.3$^{+3.4}_{-2.1}$ Myr. This age is significantly
younger than the commonly accepted age of the BPMG ($\sim$24 Myr) determined
primarily from the lithium depletion boundary analysis. This younger kinematic
age may point to the discrepancy between the luminosity evolution and lithium
depletion models or the presence of unaccounted systematic error in the method.
This result underscores the necessity for systematic reevaluations of
age-dating methods for nearby, young moving groups.
