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2013MNRAS.431..781M
Simulations of bent-double radio sources in galaxy groups
Morsony, Brian J. ( Department of Astronomy, University of Wisconsin-Madison, 2535 Sterling Hall, 475 N. Charter Street, Madison WI 53706-1582, USA; ); Miller, Jacob J. ( Department of Astronomy, University of Wisconsin-Madison, 2535 Sterling Hall, 475 N. Charter Street, Madison WI 53706-1582, USA; APS Department, University of Colorado, Boulder, UCB 391, Boulder CO 80309, USA ); Heinz, Sebastian ( Department of Astronomy, University of Wisconsin-Madison, 2535 Sterling Hall, 475 N. Charter Street, Madison WI 53706-1582, USA ); Freeland, Emily ( Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843-4242, USA; Department of Astronomy and Oskar Klein Centre, AlbaNova, Stockholm University, SE-106 91 Stockholm, Sweden ); Wilcots, Eric ( Department of Astronomy, University of Wisconsin-Madison, 2535 Sterling Hall, 475 N. Charter Street, Madison WI 53706-1582, USA ); Brüggen, Marcus ( Jacobs University Bremen, Campus Ring 1, D-28759 Bremen, Germany; Hamburger Sternwarte, University of Hamburg, Gojenbergsweg 112, D-21029 Hamburg, Germany ); Ruszkowski, Mateusz ( Department of Astronomy, The University of Michigan, 500 Church Street, Ann Arbor MI 48109, USA; The Michigan Center for Theoretical Physics, 3444 Randall Lab, 450 Church St, Ann Arbor MI 48109, USA ) show affiliations
Monthly Notices of the Royal Astronomical Society, Volume 431, Issue 1, p.781-792
Published in May 2013
Bent-double radio sources have been used as a probe to measure the density of intergalactic gas in galaxy groups. We carry out a series of high-resolution, three-dimensional simulations of active galactic nucleus (AGN) jets moving through an external medium with a constant density in order to develop a general formula for the radius of curvature of the jets, and to determine how accurately the density of the intra-group medium (IGM) can be measured. Our simulations produce curved jets ending in bright radio lobes with an extended trail of low surface brightness radio emission. The radius of curvature of the jets varies with time by only about 25 per cent. The radio trail seen in our simulations is typically not detected in known sources, but may be detectable in lower resolution radio observations. The length of this tail can be used to determine the age of the AGN. We also use our simulation data to derive a formula for the kinetic luminosity of observed jets in terms of the radius of curvature and jet pressure. In characterizing how well observations can measure the IGM density, we find that the limited resolution of typical radio observations leads to a systematic underestimate of the IGM density of about 50 per cent. The unknown angles between the observer and the direction of jet propagation and direction of AGN motion through the IGM lead to an uncertainty of about ±50 per cent in estimates of the IGM density. Previous conclusions drawn using these sources, indicating that galaxy groups contain significant reservoirs of baryons in their IGM, are still valid when considering this level of uncertainty. In addition, we model the X-ray emission expected from bent-double radio sources. We find that known sources in reasonably dense environments should be detectable in ̃100 ks Chandra observations. X-ray observations of these sources would place constraints on the IGM density and AGN velocity that are complementary to radio observations.
Keywords:
Free Keywords: Astrophysics - Cosmology and Extragalactic Astrophysics; Astrophysics - High Energy Astrophysical Phenomena; galaxies: clusters: intracluster medium; galaxies: groups: general; galaxies: intergalactic medium; galaxies: jets; radio continuum: galaxies
Astronomy: galaxies: clusters: intracluster medium; galaxies: groups: general; galaxies: intergalactic medium; galaxies: jets; radio continuum: galaxies
arXiv: Astrophysics - Cosmology and Extragalactic Astrophysics; Astrophysics - High Energy Astrophysical Phenomena
2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
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