| Abstract : | While it is known that, based on radio emission, quasars can be classified into two categories - radio-loud (RL) and radio-quiet (RQ), the underlying mechanism for this dichotomy has long been a matter of debate. In addition to their intrinsic differences, the presence of a radio jet in RL quasars may distinguish them from RQ quasars in how they affect their host galaxies. While there has been many studies modeling Spectral Energy Distributions (SED) of normal and active galaxies, the modeling of quasar-host galaxy SEDs, particularly classified by their radio emission, remains relatively unexplored. In this work, we study the differences in physical properties of quasar-host galaxies using an optically selected (SDSS; Shen et al 2011) sample of RL and RQ quasars which we have further cross-matched with the VLA-FIRST survey catalog. All sources in our sample have broad H-beta and MgII emission lines. We use the state-of-the-art SED modeling code X-CIGALE (Yang et al 2022) to construct SEDs of the quasar-host galaxies using multi-wavelength data from radio to X-ray. We have determined the best fit physical models of the host galaxy SEDs, by constraining their star formation rate (SFR), main sequence stellar mass, and stellar population. We find the distributions of some of these properties to be statistically different for RL and RQ populations, while other properties are statistically similar across both datasets. |
