To constrain the emission mechanisms responsible for generating the energy powering the active galactic nuclei (AGN) and their host galaxies, it is essential to disentangle the contributions from both as a function of wavelength. Here we introduce a state-of-the-art AGN radio-to-X-ray spectral energy distribution fitting model (ARXSED). ARXSED uses multiple components to replicate the emission from the AGN and their hosts. At radio wavelengths, ARXSED accounts for radiation from the radio structures (e.g., lobes,jets). At near-infrared to far-infrared wavelengths, ARXSED combines a clumpy medium and a homogeneous disk to account for the radiation from the torus. At the optical-UV and X-ray, ARXSED accounts for the emission from the accretion disk. An underlying component from radio to UV wavelengths accounts for the emission from the host galaxy. Here we present the results of ARXSED fits to the panchromatic SEDs of 20 radio-loud quasars from the 3CRR sample at $1<zlesssim2$. We find that a single power-law is unable to fit the radio emission when compact radio structures (core, hot spots) are present. We find that the non-thermal emission from the quasars radio structures contributes significantly ($>70%$) to the submm luminosity in half the sample, impacting the submm-based star formation rate estimates. We present the median intrinsic SED of the radio-loud quasars at $z>1$ and find that the median SED of cite{Elvis1994} is unable to describe the SED of the radio-selected AGN at $z>1$. The AGN torus and accretion disk parameters inferred from our fitting technique agree with those in the literature for similar samples. We find that the orientation of the torus/accretion disk does not line up with the inclination of the radio jets in our sample.
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