An avenue for understanding cosmological galaxy formation is to compare morphometric parameters in observations and simulations of galaxy assembly. In this second paper of the ASymba: Asymmetries of HI in SIMBA Galaxies series, we measure atomic gas HI asymmetries in spatially-resolved detections from the untargetted WALLABY survey, and compare them to realizations of WALLABY-like mock samples from the SIMBA cosmological simulations. We develop a Scanline Tracing method to create mock galaxy HI datacubes which minimizes shot noise along the spectral dimension compared to particle-based methods, and therefore spurious asymmetry contributions. We compute 1D and 3D asymmetries for spatially-resolved WALLABY Pilot Survey detections, and find that the highest 3D asymmetries A3D>0.5 stem from interacting systems or detections with strong bridges or tails. We then construct a series of WALLABY-like mock realizations drawn from the SIMBA 50 Mpc simulation volume, and compare their asymmetry distributions. We find that the incidence of high A3D detections is higher in WALLABY than in the SIMBA mocks, but that difference is not statistically significant (p-value = 0.05). The statistical power of quantitative comparisons of asymmetries such as the one presented here will improve as the WALLABY survey progresses, and as simulation volumes and resolutions increase.
@article{arxiv.2501.09547,
title = {WALLABY Pilot Survey & ASymba: Comparing HI Detection Asymmetries to the SIMBA Simulation},
author = {Mathieu Perron-Cormier and Nathan Deg and Kristine Spekkens and Mark L. A. Richardson and Marcin Glowacki and Kyle A. Oman and Marc A. W. Verheijen and Nadine A. N. Hank and Sarah Blyth and Helga Dénes and Jonghwan Rhee and Ahmed Elagali and Austin Xiaofan Shen and Wasim Raja and Karen Lee-Waddell and Luca Cortese and Barbara Catinella and Tobias Westmeier},
journal= {arXiv preprint arXiv:2501.09547},
year = {2025}
}