To investigate the dynamical nature of the kinematic asymmetry in the isolated gas-rich dwarf irregular galaxy W LM in the Local Group, we first examine whether an m = 1 perturbation in the halo potential could be a mechanism creating such kinematical asymmetry.
By fitting a theoretical rotational velocity associated with an m = 1 perturbation in the halo potential model to the observed data, we show that such a lopsided halo potential model can explain the asymmetry in the kinematic data reasonably well.
In addition, we study the kinematical classification of the velocity field of WLM with various methods, and 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. Thus, a merger may indeed be one of the possible origins of the dark matter halo lopsidedness for this isolated galaxy.
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