Low-mass galaxy groups are the most common environments for galaxies in the Universe, providing a crucial link between cosmology and galaxy evolution. Due to the low mass and sparse population of these groups, there is no strict division between the intra-group medium (IGrM) and the circumgalactic medium (CGM). These groups contain highly virialized, high-temperature gas, being the bridge between CGM and the larger-scale cluster halos. The properties of the IGrM can significantly influence the brightest central galaxy and vice versa. In this talk, I will demonstrate the efficiency of X-ray spectral stacking as a method to study X-ray faint galaxy groups identified from major optical spectroscopic surveys such as SDSS, GAMA, and DESI, and observed by the eROSITA All-Sky Survey. The stacking results from eRASS1 will be compared with predictions from eROSITA mock observations based on hydrodynamical simulations like Magneticum and IllustrisTNG. This approach not only probes the properties of the IGrM gas in groups down to scales comparable to Milky Way-sized halos but also extends and validates existing X-ray scaling relations to the CGM. Furthermore, it traces the influence of AGN feedback on baryon distribution within groups, offering insights into their internal dynamics on galactic scales.