Non-circular flows in HIghMass galaxies in a test of the late accretion hypothesis

TL;DR

This study uses H-alpha velocity maps to investigate whether late gas accretion explains the large atomic gas reservoirs in HIghMass galaxies, finding limited evidence for outer disk flows but some inner noncircular motions.

Contribution

It provides the first detailed kinematic analysis of HIghMass galaxies to test the late accretion hypothesis using integral field spectroscopy.

Findings

No outer disk radial flows detected in most galaxies

Inner noncircular motions suggest possible bar or radial flows

UGC 7899 shows the strongest candidate for late accretion evidence

Abstract

We present H-alpha velocity maps for the HIghMass galaxies UGC 7899, UGC 8475, UGC 9037 and UGC 9334, obtained with the SITELLE Imaging Fourier Transform Spectrometer on the Canada-France-Hawaii Telescope, to search for kinematic signatures of late gas accretion to explain their large atomic gas reservoirs. The maps for UGC 7899, UGC 9037, and UGC 9334 are amenable to disk wide radial flow searches with the DiskFit algorithm, and those for UGC 7899 and UGC 9037 are also amenable to inner-disk kinematic analyses. We find no evidence for outer disk radial flows down to Vr ~ 20 km/s in UGC 9037 and UGC 9334, but hints of such flows in UGC 7899. Conversely, we find clear signatures of inner (r ~ 5 kpc) noncircularities in UGC 7899 and UGC 9037 that can be modelled as either bisymmetric (which could be produced by a bar) or radial flows. Comparing these models to the structure implied by photometric disk-bulge-bar decompositions, we favour inner radial flows in UGC 7899 and an inner bar in UGC 9037. With hints of outer disk radial flows and an outer disk warp, UGC 7899 is the best candidate for late accretion among the galaxies examined, but additional modelling is required to disentangle potential degeneracies between these signatures in H I and H-alpha velocity maps. Our search provides only weak = constraints on hot-mode accretion models that could explain the unusually high H I content of HIghMass galaxies.