Luminous Infrared Galaxies (LIRGs) are key laboratories for studying star formation and feedback under the extreme conditions produced by galaxy interactions. Radio continuum observations provide a dust-unbiased view of these processes, allowing us to probe recent star formation across a wide range of physical environments.

We present a spatially resolved study of the radio spectral energy distribution (SED) of the nearby interacting LIRG Arp 240 (NGC 5257/5258). Using Karl G. Jansky Very Large Array (VLA) observations at 3, 6, 10, 15, 22, and 33 GHz, we construct resolved radio SEDs at a common physical resolution of approximately 160 pc. The broad frequency coverage enables us to characterize the radio continuum emission and measure spectral indices on scales comparable to individual star-forming complexes.

By modeling the resolved radio SEDs, we separate the thermal free-free and non-thermal synchrotron components of the radio continuum emission and investigate how their relative contributions vary throughout the system. These measurements provide insight into the distribution of thermal fractions and radio spectral indices across the galaxies and establish a framework for assessing radio continuum diagnostics of star formation at resolved scales.

Our analysis provides one of the highest-resolution radio continuum studies of Arp 240 to date and contributes to ongoing efforts to refine radio-based star formation rate calibrations in dusty galaxies. These results highlight the power of multi-frequency radio observations for understanding the connection between radio emission and star formation in LIRGs.