TESS serves as a formidable tool for investigating stellar variability. Nonetheless, the adaptation of methodologies employed in other space missions, such as Kepler, to deduce long stellar rotation periods or solar-like stellar pulsations has been a challenge. The advent of multiple sectors of data for most stars every two years with the extended

Galactic gas contains atomic hydrogen (HI), which is crucial to numerous astrophysical phenomena. Studying the HI atomic gas in and around galaxies is very important to investigate the physical conditions under which massive star formation is quenched throughout cosmic time and to examine the feeding and feedback scenario in the conventional models

Interstellar gas offers advantages when quantifying the structure of the resonances in disc galaxies. The gas is concentrated close to the disc mid-plane, making it easier to determine its in-plane velocity components, and it offers sharp emission lines for good velocity resolution. These properties are shared by atomic, molecular, and ionized gas