2025AJ....169..284C

Cold neutral hydrogen (H I) is a crucial precursor for molecular gas formation and can be studied via H I absorption. This study investigates H I absorption in low column density regions of the Small and Large Magellanic Clouds (SMC and LMC) using the Galactic-ASKAP H I (GASKAP-H I) survey, conducted by the Australian Square Kilometer Array Pathfinder (ASKAP). We select 10 SMC directions in the outer regions and 18 LMC directions, with four in the outskirts and 14 within the main disk. Using the radiative transfer method, we decompose the emission and absorption spectra into individual cold neutral medium (CNM) and warm neutral medium (WNM) components. In the SMC, we find H I peak optical depths of 0.09-1.16, spin temperatures of ∼20-50 K, and CNM fractions of 1%-11%. In the LMC, optical depths range from 0.03-3.55, spin temperatures from ∼10-100 K, and CNM fractions from 1%-100%. The SMC's low CNM fractions likely result from its low metallicity and large LOS depth. Additionally, the SMC's outskirts show lower CNM fractions than the main body, potentially due to increased CNM evaporation influenced by the hot Magellanic Corona. Shell motions dominate the kinematics of the majority of CNM clouds in this study and likely supply cold H I to the Magellanic Stream. In the LMC, high CNM fraction clouds are found near supergiant shells, where thermal instability induced by stellar feedback promotes WNM-to-CNM transition. Although no carbon monoxide has been detected, enhanced dust shielding in these areas helps maintain the cold H I.