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

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        1109.4395v2 (PDF, 1Mb)
        Author
        J. Wilkes, Belinda
        V. Lal, Dharam
        Worrall, D. M.
        Birkinshaw, Mark
        Haas, Martin
        Willner, S. P.
        Antonucci, Robert
        Ashby, M. L. N.
        Avara, Mark
        Barthel, Peter
        Chini, Rolf
        Fazio, G.
        Hardcastle, M.J.
        Lawrence, Charles
        Leipski, Christian
        Ogle, Patrick
        Schulz, Bernhard
        Attention
        2299/8061
        Abstract
        Chandra X-ray observations of the high redshift (z =1.532) radio-loud quasar 3C270.1 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 Fe Kalpha 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 ~11nT, roughly a third of the equipartition value. The northern emission is concentrated close to the location of a 40 deg. 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 ~3nT, roughly a factor of nine 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 1.8E44 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.
        Publication date
        2012-01-20
        Published in
        The Astrophysical Journal
        Published version
        https://doi.org/10.1088/0004-637X/745/1/84
        Other links
        http://hdl.handle.net/2299/8061
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