Comparison of radio observations and numerical simulations of the radio lobes of Cygnus A

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dc.contributor.author Carvalho, Joel en_US
dc.contributor.author Daly, Ruth en_US
dc.contributor.author Mory, Matthew en_US
dc.contributor.author O'Dea, Christopher en_US
dc.date.accessioned 2006-06-08T20:15:16Z en_US
dc.date.available 2006-06-08T20:15:16Z en_US
dc.date.issued 2005-02-10 en_US
dc.identifier.citation Astrophysical Journal 620 (2005) 126-144 en_US
dc.identifier.issn 1538-4357 en_US
dc.identifier.uri http://hdl.handle.net/1850/1958 en_US
dc.description Also archived in: arXiv:astro-ph/0406212 v2 19 Oct 2004 en_US
dc.description.abstract We present a comparison of radio observations of the archetypal powerful radio galaxy Cygnus A and 2-D numerical hydrodynamical simulations. We characterize some global trends in the observed radio properties and compare them with the properties of a simulated radio source. The numerical results are the following. Jets propagating in a constant density atmosphere will decelerate with time. Thus, the estimated dynamical age of the source will be greater than the actual age of the source. For a source similar to Cygnus A the difference will be about a factor of 2. The second moment gives an accurate representation of the "true" width of the simulated source. The Gaussian FWHM tends to be about 40% larger than the true width and can be systematically in error if the surface brightness exhibits multiple peaks. We suggest that the ratio of the Gaussian FWHM to the second moment may be a diagnostic of the emissivity profile in the lobes. The simulations can qualitatively reproduce the overall observed morphology and the behavior of the cross-sections in surface brightness, the decline in surface brightness with distance from the hot spots, and the width of the lobes. This suggests that the 2-D simulations give a reasonable representation of the properties of Cygnus A. en_US
dc.description.sponsorship JCC acknowledges the financial support of PRONEX/Finep and CNPq and the hospitality of STScI where this work was carried out. This work was supported in part by a grant to C. O’Dea from the Space Telescope Science Institute [STScI] Collaborative Visitor Program which funded visits by JCC to STScI, and by grant AST-0206002 to R. Daly from the U. S. National Science Foundation. en_US
dc.format.extent 1711715 bytes en_US
dc.format.mimetype application/pdf en_US
dc.language.iso en_US en_US
dc.publisher University of Chicago Press: Astrophysical Journal en_US
dc.relation.ispartofseries vol. 620 en_US
dc.relation.ispartofseries no. 1 en_US
dc.relation.ispartofseries part 1 en_US
dc.relation.ispartofseries pps. 126-144 en_US
dc.subject Galaxies-jets en_US
dc.subject Galaxies-intergalactic medium en_US
dc.subject Galaxies-radio continuum en_US
dc.subject Hydrodynamics en_US
dc.title Comparison of radio observations and numerical simulations of the radio lobes of Cygnus A en_US
dc.type Article en_US

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