2007/08/09 by Aneta Siemiginowska, D. E. Harris, Siemiginowska, Aneta +13
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics (astro-ph) #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #Gamma-ray bursts and supernovae #astro-ph
paper · pdf · doi:10.48550/arxiv.0708.1312
5 pages, 5 figures. To be published in the proceedings of "Extragalactic Jets: Theory and Observation from Radio to Gamma Ray" ASP Conference Series, T. A. Rector and D. S. De Young (eds.)
arxiv created 2007/08/09 · openalex publication_date 2007/08/09 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The complex X-ray morphology of the 300 kpc long X-ray jet in PKS1127-145 (z=1.18 quasar) is clearly discerned in a ~100 ksec Chandra observation. The jet X-ray surface brightness gradually decreases by an order of magnitude going out from the core. The X-ray spectrum of the inner jet is relatively flat with alphaX=0.66+/-0.15 and steep in the outer jet with alphaX=1.0+/-0.2. The X-ray and radio jet intensity profiles are strikingly different, with the radio emission peaking strongly at the two outer knots while the X-ray emission is strongest in the inner jet region. We discuss the constraints implied by these data on the X-ray emission models and conclude that ``one-zone'' models fail and that at least a two-component model is needed to explain the jet's broadband emission. We propose that the X-ray emission originates in the jet proper while the bulk of the radio emission comes from a surrounding jet sheath. We also consider intermittent jet activity as a possible cause of the observed jet morphology.