Wilkes, BelindaLal, Dharam V.Worrall, DianaBirkinshaw, MarkHaas, MartinWillner, StevenAntonucci, RobertAshby, MatthewAvara, MarkBarthel, PeterChini, RolfFazio, GiovanniHardcastle, MartinLawrence, CharlesLeipski, ChristianOgle, PatrickSchulz, Bernhard2017-01-122012Wilkes, Belinda J., Dharam V. Lal, D. M. Worrall, Mark Birkinshaw, Martin Haas, S. P. Willner, Robert Antonucci, et al. 2012. “Chandra X-Ray Observations of the Redshift 1.53 Radio-Loud Quasar 3c 270.1.” The Astrophysical Journal 745 (1) (January 3): 84. doi:10.1088/0004-637x/745/1/84.0004-637Xhttp://nrs.harvard.edu/urn-3:HUL.InstRepos:29921926Chandra 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, Γ = 1.66 ± 0.08, typical of a radio-loud quasar, and a marginally detected Fe Kα 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 hot spot. Modeling this hot spot, including Spitzer upper limits, rules out synchrotron emission from a single power-law population of electrons, favoring inverse Compton emission with a field of ∼11 nT, roughly a third of the equipartition value. The northern emission is concentrated close to the location of a 40◦ bend where the radio jet is presumed to encounter an external medium. It can be explained by inverse Compton emission involving cosmic microwave background photons with a field of ∼3 nT, a factor of 7–10 below the equipartition value. The remaining, more diffuse X-ray emission is harder (HR = −0.09 ± 0.22). With only 22.8 ± 5.6 counts, the spectral form cannot be constrained. Assuming thermal emission with a temperature of 4 keV yields an estimate for the luminosity of 1.8×1044 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.en-USQuasars: individual: 3C 270.1X-rays: galaxies: clustersJournal Article2017-01-1210.1088/0004-637X/745/1/84