Harsh radiation from a mass-accreting super-massive black hole, or an AGN, can change thermal and chemical properties of the surrounding interstellar medium (ISM). Here, given a suggestion that the SMBH and host galaxy have grown while affecting each other, it is expected that the host galaxy has formed stars while being subject to the AGN radiation. Thus, toward the complete understanding of the galaxy growth, the study of AGN radiative effects is important. In this colloquium, I will talk about our recent studies of nearby AGNs that focused on an AGN X-ray radiative impact on the ISM. We utilized Chandra and ALMA. Their combination is ideal for the studies. Chandra can reveal the ISM subject to X-ray radiation from an AGN, and ALMA enables us to constrain thermal and chemical properties of the ISM therein. Also, their sub-arcsec resolutions make it possible to resolve the ISM at quite high resolutions below 100 pc. As an interesting result, we found that molecular gas emission appeared faint in regions likely being subject to AGN X-ray radiation. Motivated by this, we quantitatively discussed the possibility that the molecular gas was dissociated by the X-ray radiation. Based on ALMA data, we constrained the molecular gas densities, and found that they were low enough to be interpreted by the X-ray dissociation. Given a positive correlation between the molecular gas and star-formation surface densities, the result can further suggest that the X-ray radiation has the potential to suppress star formation eventually.