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Stars form in the dense interiors of molecular clouds. The dynamics andphysical properties of the atomic interstellar medium (ISM) set the conditionsunder which molecular clouds and eventually stars will form. It is, therefore,critical to investigate the relationship between the atomic and molecular gasphase to understand the global star formation process. Using the high angularresolution data from The HI/OH/Recombination line survey of the Milky Way(THOR), we aim to constrain the kinematic and physical properties of the coldatomic hydrogen gas phase toward the inner Galactic plane. HI self-absorption(HISA) has proven to be a viable method to detect cold atomic hydrogen cloudsin the Galactic plane. With the help of a newly developed self-absorptionextraction routine (astroSABER), we build upon previous case studies toidentify HI self-absorption toward a sample of Giant Molecular Filaments(GMFs). We find the cold atomic gas to be spatially correlated with themolecular gas on a global scale. The column densities of the cold atomic gastraced by HISA are usually of the order of $10^{20}\rm\,cm^{-2}$ whereas thoseof molecular hydrogen traced by $\rm^{13}CO$ are at least an order of magnitudehigher. The HISA column densities are attributed to a cold gas component thataccounts for a fraction of $\sim$5% of the total atomic gas budget within theclouds. The HISA column density distributions show pronounced log-normal shapesthat are broader than those traced by HI emission. The cold atomic gas is foundto be moderately supersonic with Mach numbers of a $\sim$few. In contrast,highly supersonic dynamics drive the molecular gas within most filaments.

Cold atomic gas identified by HI self-absorption. Cold atomic clouds toward giant molecular filaments