WALLABY Pilot Survey: kNN identification of perturbed galaxies through HI morphometrics

TL;DR

This study uses a k-nearest Neighbor algorithm on HI morphometric parameters to identify perturbed galaxies in the WALLABY survey, achieving 70-80% accuracy, and compares their properties to unperturbed galaxies.

Contribution

It introduces a kNN-based method for identifying perturbed galaxies using HI morphometrics in large HI surveys, demonstrating its effectiveness.

Findings

kNN classifier achieves 70-80% accuracy in identifying perturbed galaxies

Perturbed and unperturbed galaxies show similar scaling relations in some properties

HI-stellar mass relation is flatter for perturbed galaxies

Abstract

Galaxy morphology in stellar light can be described by a series of "non-parametric" or "morphometric" parameters, such as concentration-asymmetry-smoothness, Gini, $M_{20}$, and Sersic fit. These parameters can be applied to column density maps of atomic hydrogen (HI). The HI distribution is susceptible to perturbations by environmental effects, e.g. inter-galactic medium pressure and tidal interactions. Therefore, HI morphology can potentially identify galaxies undergoing ram-pressure stripping or tidal interactions. We explore three fields in the WALLABY Pilot HI survey and identify perturbed galaxies based on a k-nearest Neighbor (kNN) algorithm using an HI morphometric feature space. For training, we used labeled galaxies in the combined NGC 4808 and NGC 4636 fields with six HI morphometrics to train and test a kNN classifier. The kNN classification is proficient in classifying perturbed galaxies with all metrics -- accuracy, precision and recall -- at 70-80%. By using the kNN method to identify perturbed galaxies in the deployment field, the NGC 5044 mosaic, we find that in most regards, the scaling relations of perturbed and unperturbed galaxies have similar distribution in the scaling relations of stellar mass vs star formation rate and the Baryonic Tully-Fisher relation, but the HI and stellar mass relation flatter than of the unperturbed galaxies. Our results for NGC 5044 provide a prediction for future studies on the fraction of galaxies undergoing interaction in this catalogue and to build a training sample to classify such galaxies in the full WALLABY survey.