Kinematical asymmetry in the dwarf irregular galaxy WLM and a perturbed halo potential

TL;DR

This study investigates the origin of the asymmetrical rotation curve of the dwarf galaxy WLM, proposing that a lopsided halo potential can explain the kinematic asymmetry and highlighting the galaxy's perturbed velocity field.

Contribution

It demonstrates that an $m=1$ halo perturbation model can account for WLM's kinematic asymmetry and explores its perturbed velocity field and potential transition between disk and merger states.

Findings

Lopsided halo potential explains rotation curve asymmetry

WLM's velocity field is significantly perturbed

Galaxy may be in a transition region between disk and merger

Abstract

WLM is a dwarf irregular that is seen almost edge-on that has prompted a number of kinematical studies investigating its rotation curve and its dark matter content. In this paper, we investigate the origin of the strong asymmetry of the rotation curve, which shows a significant discrepancy between the approaching and the receding side. We first examine whether an $m = 1$ perturbation (lopsidedness) in the halo potential could be a mechanism creating such kinematical asymmetry. To do so, we fit a theoretical rotational velocity associated with an $m = 1$ perturbation in the halo potential model to the observed data via a $\chi-$squared minimization method. We show that a lopsided halo potential model can explain the asymmetry in the kinematic data reasonably well. We then verify that the kinematical classification of WLM shows that its velocity field is significantly perturbed due to both its asymmetrical rotation curve and also its peculiar velocity dispersion map. In addition, based on a kinemetry analysis, we find that it is possible for WLM to lie in the transition region, where the disk and merger coexist. In conclusion, it appears that the rotation curve of WLM diverges significantly from that of an ideal rotating disk, which may significantly affect investigations of its dark matter content.