Astrophys. J., 745, 84 (2012/January-3)
Chandra X-ray observations of the redshift 1.53 radio-loud quasar 3C 270.1.
WILKES B.J., LAL D.V., WORRALL D.M., BIRKINSHAW M., HAAS M., WILLNER S.P., ANTONUCCI R., ASHBY M.L.N., AVARA M., BARTHEL P., CHINI R., FAZIO G.G., HARDCASTLE M., LAWRENCE C., LEIPSKI C., OGLE P. and SCHULZ B.
Abstract (from CDS):
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, 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 1.8x 1044 erg/s, 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.
quasars: individual: 3C 270.1 - X-rays: galaxies: clusters
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