Chandra X-ray observations of the high redshift ( z =1.532 ) radio-loud quasar 3C 270.1 in 2008 February show the nucleus to have a power-law spectrum , \Gamma = 1.66 \pm 0.08 , typical of a radio-loud quasar , and a marginally-detected Fe K \alpha emission line .
The data also reveal extended X-ray emission , about half of which is associated with the radio emission from this source .
The southern emission is co-spatial with the radio lobe and peaks at the position of the double radio hotspot .
Modeling this hotspot including Spitzer upper limits rules out synchrotron emission from a single power-law population of electrons , favoring inverse-Compton emission with a field of \sim 11 nT , roughly a third of the equipartition value .
The northern emission is concentrated close to the location of a 40 ^ { o } bend where the radio jet is presumed to encounter external material .
It can be explained by inverse Compton emission involving Cosmic Microwave Background photons with a field of \sim 3 nT , roughly a factor of nine below the equipartition value .
The remaining , more diffuse X-ray emission is harder ( HR= -0.09 \pm 0.22 ) .
With only 22.8 \pm 5.6 counts , the spectral form can not be constrained .
Assuming thermal emission with a temperature of 4 keV yields an estimate for the luminosity of 1.8 \times 10 ^ { 44 } erg s ^ { -1 } , consistent with the luminosity-temperature relation of lower-redshift clusters .
However deeper Chandra X-ray observations are required to delineate the spatial distribution , and better constrain the spectrum of the diffuse emission to verify that we have detected X-ray emission from a high-redshift cluster .