We present a detailed analysis of the structural parameters of the globular cluster M 15 using g- and i-band photometric data from Pan-STARRS1 DR2. The central coordinates ($X_{ \rm{ C}}, Y_{ \rm{ C}}$), ellipticity ($\epsilon$), and position angle (PA) are derived via two independent methods: ellipse fitting of the two-dimensional stellar number isodensity distribution and Markov Chain Monte Carlo (MCMC) sampling. Our analysis of 38 stellar density intervals reveals a cluster center offset by only $4\,.\!\!^{ \prime\prime}1\pm9\,.\!\!^{ \prime\prime}6$ from the commonly accepted in the literature value, a good agreement on the order of our map resolution. We find a radial variation in the ellipticity, with a mean value of $\epsilon=0.09\pm0.02$ for the inner region ($R\leq4\,.\!\!^{ \prime}5$) and $\epsilon=0.04\pm0.02$ for the outer region ($R>4\,.\!\!^{ \prime}5$), where the errors correspond to $1\sigma$. The MCMC analysis of 75 datasets yields a mean $\epsilon=0.022\pm0.005$ for the entire cluster. The PA remains constant with increasing distance from the cluster center, $\rm{ PA}=44\,.\!\!{ \rm{ ^\circ}}4\pm16\,.\!\!{ \rm{ ^\circ}}2$, and the MCMC method providing a consistent value of $\rm{ PA}=46\,.\!\!{ \rm{ ^\circ}}6\pm7\,.\!\!{ \rm{ ^\circ}}1$. Our results are in agreement with some recent studies but challenge others, suggesting that a single $\epsilon$ value may be insufficient to fully characterize the overall oblateness of M 15 due to incompleteness and crowding effects in its core.
Categories: astro-ph.GA