Mapping kiloparsec-scale structures in the extended HI disc of the galaxy UGC 00439 by HI 21-cm absorption

TL;DR

This study maps the small- and large-scale structures of HI gas in the extended disc of galaxy UGC 00439 using 21-cm absorption, revealing patchy cold gas distribution and kinematics consistent with corotation.

Contribution

First detailed mapping of kiloparsec-scale HI structures in the extended disc of UGC 00439 via 21-cm absorption observations.

Findings

Detected HI 21-cm absorption over ~2 kpc^2 towards the southern lobe.

Observed sub-kpc-scale structures and turbulent velocities in the absorbing gas.

No HI emission detected from the absorbing gas, constraining the spin temperature to <~300 K.

Abstract

We study the properties of HI gas in the outer regions (~2r_25) of a spiral galaxy, UGC 00439 (z = 0.01769), using HI 21-cm absorption towards different components of an extended background radio source, J0041$-$0043 (z = 1.679). The radio source exhibits a compact core coincident with the optical quasar and two lobes separated by ~7 kpc, all at an impact parameter ~25 kpc. The HI 21-cm absorption detected towards the southern lobe is found to extend over ~2 kpc^2. The absorbing gas shows sub-kpc-scale structures with the line-of-sight velocities dominated by turbulent motions. Much larger optical depth variations over 4-7 kpc-scale are revealed by the non-detection of HI 21-cm absorption towards the radio core and the northern lobe, and the detection of NaI and CaII absorption towards the quasar. This could reflect a patchy distribution of cold gas in the extended HI disc. We also detect HI 21-cm emission from UGC 00439 and two other galaxies within ~150 kpc to it, that probably form an interacting group. However, no HI 21-cm emission from the absorbing gas is detected. Assuming a linear extent of ~4 kpc, as required to cover both the core and the southern lobe, we constrain the spin temperature <~300 K for the absorbing gas. The kinematics of the gas and the lack of signatures of any ongoing in situ star formation are consistent with the absorbing gas being at the kinematical minor axis and corotating with the galaxy. Deeper HI 21-cm observations would help to map in greater detail both the large- and small-scale structures in the HI gas associated with UGC 00439.