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dc.contributor.authorPerlman, Eric S.
dc.contributor.authorGeorganopoulos, Markos
dc.contributor.authorMay, Emily M.
dc.contributor.authorKazanas, Demosthenes
dc.date.accessioned2013-08-23T15:31:53Z
dc.date.available2013-08-23T15:31:53Z
dc.date.issued2010-01-01
dc.identifier.citationPerlman, E. S., Georganopoulos, M., May, E. M., & Kazanas, D. (2010). Chandra Observations of the Radio Galaxy 3C 445 and the Hot Spot X-Ray Emission Mechanism. The Astrophysical Journal, 708(1), 1.en_US
dc.identifier.urihttp://hdl.handle.net/11141/68
dc.description.abstractWe present new Chandra observations of the radio galaxy 3C 445, centered on its southern radio hot spot. Our observations detect X-ray emission displaced upstream and to the west of the radio–optical hot spot. Attempting to reproduce both the observed spectral energy distribution and the displacement excludes all one-zone models. Modeling of the radio–optical hot spot spectrum suggests that the electron distribution has a low-energy cutoff or break approximately at the proton rest mass energy. The X-rays could be due to external Compton scattering of the cosmic microwave background coming from the fast (Lorentz factor Γ ≈ 4) part of a decelerating flow, but this requires a small angle between the jet velocity and the observer’s line of sight (θ ≈ 14◦). Alternatively, the X-ray emission can be synchrotron from a separate population of electrons. This last interpretation does not require the X-ray emission to be beamed.en_US
dc.language.isoen_USen_US
dc.rightsThis published article is available in accordance with the publisher's policy. It may be subject to U.S. copyright law.en_US
dc.rights.urihttp://aas.org/publications/aas-copyright-policyen_US
dc.titleChandra observations of the radio galaxy 3C 445 and the hot spot x-ray emission mechanismen_US
dc.typeArticleen_US
dc.identifier.doi10.1088/0004-637X/708/1/1


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