Disentangling the AGN and star-formation contributions to the
  radio-X-ray emission of radio-loud quasars at $1<z<2$
  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
$1<z\lesssim2$. 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.
