Ionized and neutral gas in the peculiar star/cluster complex in NGC 6946

TL;DR

This study investigates the peculiar gas kinematics and structure of a star/cluster complex in NGC 6946, revealing unusual gas motions, a deep velocity minimum, and possible origins involving galaxy interactions or energetic outflows.

Contribution

It provides detailed observations of ionized and HI gas in a unique star/cluster complex, highlighting its peculiar kinematics and proposing multiple hypotheses for its origin.

Findings

Deep velocity minimum centered near the super star cluster

Expansion of HI and HII gas with velocities up to 30 km/s

Presence of shock-excited emission lines in the velocity dip

Abstract

The characteristics of ionized and HI gas in the peculiar star/cluster complex in NGC 6946, obtained with the 6-m telescope (BTA) SAO RAS, the Gemini North telescope, and the Westerbork Synthesis Radio Telescope (WSRT), are presented. The complex is unusual as hosting a super star cluster, the most massive known in an apparently non-interacting giant galaxy. It contains a number of smaller clusters and is bordered by a sharp C-shaped rim. We found that the complex is additionally unusual in having peculiar gas kinematics. The velocity field of the ionized gas reveals a deep oval minimum, ~300 pc in size, centered 7" east of the supercluster. The Vr of the ionized gas in the dip center is 100 km/s lower than in its surroundings, and emission lines within the dip appear to be shock excited. This dip is near the center of an HI hole and a semi-ring of HII regions. The HI (and less certainly, HII) velocity fields reveal expansion, with the velocity reaching ~30 km/s at a distance about 300 pc from the center of expansion, which is near the deep minimum position. The super star cluster is at the western rim of the minimum. The sharp western rim of the whole complex is plausibly a manifestation of a regular dust arc along the complex edge. Different hypotheses about the complex and the Vr depression origins are discussed, including a HVC/dark mini-halo impact, a BCD galaxy merging, and a gas outflow due to release of energy from the supercluster stars.