Direct N-body simulations of NGC 6397 and its tidal tails

TL;DR

This study combines direct N-body simulations and Gaia DR3 data to analyze the evolution, structure, and tidal tails of the globular cluster NGC 6397, providing insights into its current state and stellar distribution.

Contribution

It presents the first detailed simulation and observational analysis of NGC 6397's tidal tails and structure, matching models with Gaia data without invoking dark matter halos.

Findings

Simulations match observed surface density and velocity dispersion profiles.

Tidal tails extend up to 10 degrees beyond the cluster.

No need for dark remnants or dark matter halos to explain the data.

Abstract

We have performed a series of direct N-body simulations that study the evolution of the Galactic globular cluster NGC 6397 under the combined influence of two-body relaxation, stellar evolution and the Milky Way's tidal field. Our simulations follow the evolution of the cluster over the last several Gyr up to its present-day position in the Milky Way in order to allow us to derive present-day cluster parameters and the distribution of its extra-tidal stars. We have also determined a new density profile of NGC 6397 by selecting stars from Gaia DR3 using Gaia DR3 proper motions, parallaxes and photometry to discriminate cluster members from non-members. This allows us to derive the surface density profile of NGC 6397 and the location of its tidal tails up to 10 degrees of the cluster centre, well beyond the tidal radius of NGC 6397. Our results show that the current state of NGC 6397 in terms of surface density, velocity dispersion profile and stellar mass function can be matched by a cluster model evolving from a standard initial mass function and does not require an additional central cluster of dark remnants. We also find good agreement in the location and absolute number of the extra-tidal stars between our simulations and the observations, making it unlikely that NGC 6397 is surrounded by a dark matter halo.