While represnting only a minor fraction of the interstellar medium (ISM) mass, interstellar dust significantly affects the thermal, chemical, and radiative processes that govern galaxy evolution. By mediating gas cooling, enabling molecule formation, and absorbing and re-emitting stellar radiation in far-infrared and Sub-mm regimes, dust serves as an essential tracer of the physical conditions, offering insights into the interplay of stars, dust and the ISM. With the help of multi-wavelength observations, it is possible to study the different components of the ISM and their relations in a spatially resolved manner across nearby galaxies, on scales of few hundreds to kiloparsecs. In this talk, I present a spatially resolved analysis of dust in spiral galaxies, focusing on two complemetary aspects: dust heating and dust scaling relations. I will show that both young and evolved stellar popluations contribute to dust heating, and examine how dust content related to the gas and metals in the ISM through dust-to-gas and dust-to-metal ratios. These results provide a more complete picture of how dust properties are shaped by both stellar radiation and ISM conditions.