Building gas rings and rejuvenating S0 galaxies through minor mergers

TL;DR

This study uses simulations to show how minor mergers can create long-lasting gas rings in S0 galaxies, influencing their structure and star formation, and providing insights into galaxy rejuvenation.

Contribution

It demonstrates that minor mergers can produce long-lived, inclined gas rings in S0 galaxies without requiring bar resonances, and links ring properties to satellite orbits.

Findings

Gas rings form at 6-13 kpc with ~10^7 Msun mass.

Ring longevity depends on orbital orientation, lasting over 6 Gyr in some cases.

Star formation persists for over 6 Gyr in the galaxy's central regions.

Abstract

We investigate the effects of minor mergers between an S0 galaxy and a gas-rich satellite galaxy, by means of N-body/smoothed particle hydrodynamics (SPH) simulations. The satellite galaxy is initially on a nearly parabolic orbit and undergoes several periapsis passages before being completely stripped. In most simulations, a portion of the stripped gas forms a warm dense gas ring in the S0 galaxy, with a radius of ~6-13 kpc and a mass of ~10^7 solar masses (Msun). The ring is generally short-lived (<~3 Gyr) if it forms from prograde encounters, while it can live for more than 6 Gyr if it is born from counter-rotating or non-coplanar interactions. The gas ring keeps memory of the initial orbit of the satellite galaxy: it is corotating (counter-rotating) with the stars of the disc of the S0 galaxy, if it originates from prograde (retrograde) satellite orbits. Furthermore, the ring is coplanar with the disc of the S0 galaxy only if the satellite's orbit was coplanar, while it lies on a plane that is inclined with respect to the disc of the S0 galaxy by the same inclination angle as the orbital plane of the satellite galaxy. The fact that we form polar rings as long-lived and as massive as co-planar rings suggests that rings can form in S0 galaxies even without strong bar resonances. Star formation up to 0.01 Msun yr^-1 occurs for >6 Gyr in the central parts of the S0 galaxy as a consequence of the interaction. We discuss the implications of our simulations for the rejuvenation of S0 galaxies in the local Universe.