Revealing the cold skeleton of the Magellanic clouds and the Magellanic Bridge with ASKAP

We present the GASKAP-HI pilot absorption survey of neutral hydrogen (H i) in the Magellanic system. This survey provides 3219 sightlines across the Large (LMC) and Small Magellanic Clouds (SMC) and the Magellanic Bridge (MB) towards 1.4-GHz continuum sources, representing a 15-fold increase on pre-GASKAP-HI sampling of the Magellanic system. We find 344 candidate detections of cold gas at Magellanic velocities (v$_\text{LSRK} \ge 90$ km s$^{-1}$), with signal-to-noise ratio $\gt 3$ detection rates of 44 per cent (LMC; 192 of 438), 73 per cent (SMC; 85 of 117), and 4 per cent (MB; 35 of 793). We examine the candidate detections within the MB, Gaussian decompose these, and examine the cold gas across the MB. Here we find that the majority of cold gas detections are found closer to the SMC. We also find potential evidence of the recent formation of cold gas on the outskirts of a shell within the MB. We find a mean cold gas fraction of $\overline{f_\text{CNM}} = 0.12 \pm 0.08$ for the MB, which is very similar to the SMC and lower than the LMC value of 0.14. Overall, we reveal cold gas distributed extensively across the Magellanic system, including within the MB, and surmise that the cold gas in the MB is either pulled from the SMC as part of the formation of the MB, or formed in the turbulence of those same interactions.