Astronomy and Astrophysics – Astronomy
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21832718s&link_type=abstract
American Astronomical Society, AAS Meeting #218, #327.18; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
Four viable explanations for the development of the characteristic morphology of X-shaped radio galaxies (XRGs) have been presented in the literature. These established models involve: backflowing material from relativistic jets deflected off the host galaxy ISM; over-pressured cocoons leading to outflow along a galaxy's minor axis; rapid jet reorientation (spin-flip), presumably involving the merger of two supermassive black holes; or the interaction of jets with stellar and gaseous shells that arise from the merger of two galaxies. None of these models appears to be able to account for the morphology of all observed XRGs, but images of these sources can be used to decide which of these models provide good fits to individual XRGs. We have examined a sample of 100 XRG candidates and tabulated several different measured parameters based on their morphology and power. The key morphology parameters are the lengths and widths of the primary and secondary lobes. We then classified the XRGs in this sample as to the most likely model or models able to explain their characteristics. Our main conclusion is that the spin-flip and jet interaction with shells models provide better fits to the majority of sources than do the backflow or over-pressured cocoon models.
Sobczak Robert
Starr Jason
Wiita Paul J.
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