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Chandra X-ray observations of the high redshift (z =1.532) radio-loud quasar3C270.1 in 2008 February show the nucleus to have a power-law spectrum, Gamma =1.66 +/- 0.08, typical of a radio-loud quasar, and a marginally-detected FeKalpha emission line. The data also reveal extended X-ray emission, about halfof which is associated with the radio emission from this source. The southernemission is co-spatial with the radio lobe and peaks at the position of thedouble radio hotspot. Modeling this hotspot including Spitzer upper limitsrules out synchrotron emission from a single power-law population of electrons,favoring inverse-Compton emission with a field of ~11nT, roughly a third of theequipartition value. The northern emission is concentrated close to thelocation of a 40 deg. bend where the radio jet is presumed to encounterexternal material. It can be explained by inverse Compton emission involvingCosmic Microwave Background photons with a field of ~3nT, roughly a factor ofnine below the equipartition value. The remaining, more diffuse X-ray emissionis harder (HR=-0.09 +/- 0.22). With only 22.8+/-5.6 counts, the spectral formcannot be constrained. Assuming thermal emission with a temperature of 4 keVyields an estimate for the luminosity of 1.8E44 erg/s, consistent with theluminosity-temperature relation of lower-redshift clusters. However deeperChandra X-ray observations are required to delineate the spatial distribution,and better constrain the spectrum of the diffuse emission to verify that wehave detected X-ray emission from a high-redshift cluster.

Chandra X-ray Observations of the redshift 1.53, radio-loud quasar: 3C 270.1