Multifrequency VLBA polarimetry of the Fermidetected quasar 的费多频VLBI偏振探测类星体.pptVIP

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Multifrequency VLBA polarimetry of the Fermidetected quasar 的费多频VLBI偏振探测类星体.ppt

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Multifrequency VLBA polarimetry of the Fermidetected quasar 的费多频VLBI偏振探测类星体

MFPO 2010 Krakow VLBA polarimetry of the Fermi-detected quasar B0954+556: a rare “spine and sheath” polarisation structure Outline B0954+556: a bright quasar Radio observations VLBA Imaging Results # “Spine and sheath” polarisation structure # Nondetection of the radio core Possible scenarios for the polarisation structure # Plasma compression by shocks and interactions # A helical magnetic field wrapped around the jet Summary B0954+556 (4C 55.17, J0957+5522)---Active from radio to Gamma-ray # Bright radio source with Sν 0.5 Jy in 100 MHz – 43 GHz # Optically, a high polarized quasar: p=8.7 %, mv=17.5, z=0.9 (Wills et al. 1992) # Detected by Chandra and ROSAT at X-ray band. (Tavecchio et al. 2007, Sambruna 1997) # Detected by the EGRET at Energy 100 MeV (Hartman et al. 1999) # 24 sigma detection by the Fermi (Abdo et al. 2009) The used radio observations Radio imaging results The “Spine and sheath” polarisation (E) structure # Spine: E || Jet axis at the centre of the jet # Sheath: E ┴ Jet axis on both sides of the spine Magnetic field B ┴ E, if it is optically thin synchrotron emission. ## Spine: B ┴ Jet axis ## Sheath: B || Jet axis Polarization degree distribution Faraday RM distribution # The RM distribution shows a hint of transverse RM gradients in the inner spine. Color map RM distribution Used polarisation position angle map 1.7, 5, 8.4 GHz VLBA images. Contours 8.4 GHz intensity map convolved with the beam of 1.7 GHz VLBA image. The radio core: not seen # There is no compact component detected at 15 GHz (Rossetti et al. 2005). # No fringes detected even on the shortest baseline in our fringe-detecting VLBA observations at 43 and 86 GHz. The half-Jy source is completely resolved. # The radio emission is very stable (5%) over the last 20 years (Fan et al. 2007) # A rare case in the Fermi-detected quasars and blazars (Abdo et al. 2009). The ran