Investigating the resolved X-ray jet emission mechanism of radio-loud quasars at z ~ 3

One of the outstanding questions in extragalactic astrophysics is unraveling the interplay between actively accreting supermassive black holes and their host galaxies. A pivotal aspect of this inquiry involves studying energetic jetted outflows, which transport energy from the galactic center to spatial scales spanning from milliparsecs to megaparsecs. While jets are primarily observed at radio wavelengths in nearby quasars, several factors favor X-ray jets at high redshifts. The X-ray emission in relativistic jets is attributed to the inverse Compton scattering of the cosmic microwave background (IC/CMB), which is enhanced by the (1+z) increase in CMB energy density at high redshifts. Conversely, the radio surface brightness undergoes a cosmological dimming of the same factor. Additionally, the electrons responsible for X-ray production via IC/CMB have longer lifetimes compared to electrons emitting GHz synchrotron radiation. The detection of X-ray jets in high-redshift quasars is limited, making the findings of each detection crucial for understanding the trends in jet populations across cosmic time. This study focuses on two z~3 radio-loud quasars that present kiloparsec-scale extended X-ray emission but lack an extended underlying radio jet. Their VLBI observations confirm relativistic jet speeds. I will present the follow-up deeper Chandra X-ray and high- resolution, high-sensitivity Very Large Array 6 GHz radio observations of these quasars. Using the IC/CMB model, I will present the constraints we found on relativistic beaming parameters and magnetic fields, providing insights into the enthalpy flux of these high-redshift quasar jets.