HST Observations of the Interacting Galaxies NGC 2207 and IC 2163

TL;DR

HST images reveal complex star formation, dust structures, and shock fronts in the interacting galaxies NGC 2207 and IC 2163, illustrating the effects of tidal forces and gas dynamics during a recent galactic encounter.

Contribution

This study provides detailed imaging and analysis of the interaction-induced structures and star formation processes in NGC 2207 and IC 2163, supported by numerical models.

Findings

Tidal forces compressed IC 2163's disk, forming star-forming ridges.

Dust filaments are linked to pre-existing spiral arms and shock fronts.

Evidence of density wave triggering and possible tidal-induced nuclear gas flow.

Abstract

Hubble Space Telescope images of the galaxies NGC 2207 and IC 2163 show star formation and dust structures in a system that has experienced a recent grazing encounter. Tidal forces from NGC 2207 compressed and elongated the disk of IC 2163, forming an oval ridge of star formation. Gas flowing away from this ridge has thin parallel dust filaments transverse to the direction of motion. Numerical models suggest that the filaments come from flocculent spiral arms that were present before the interaction. A dust lane at the outer edge of the tidal tail is a shock front where the flow abruptly changes direction. A spiral arm of NGC 2207 that is backlit by IC 2163 is seen to contain several parallel, knotty filaments that are probably shock fronts in a density wave. Blue clusters of star formation inside these dust lanes show density wave triggering by local gravitational collapse. Spiral arms inside the oval of IC 2163 could be the result of ILR-related orbits in the tidal potential that formed the oval. Their presence suggests that tidal forces alone may initiate a temporary nuclear gas flow and eventual starburst without first forming a stellar bar. Several emission structures resembling jets 100-1000 pc long appear. There is a dense dark cloud with a conical shape 400 pc long and a bright compact cluster at the tip, and with a conical emission nebula of the same length that points away from the cluster in the other direction. This region coincides with a non-thermal radio continuum source that is 1000 times the luminosity of Cas A at 20 cm.