Ram pressure statistics for bent tail radio galaxies

Show simple item record Mguda, Z Faltenbacher, A Van der Heyden, K Gottlöber, S Cress, C Vaisanen, P Yepes, G 2015-05-25T10:55:38Z 2015-05-25T10:55:38Z 2015-01
dc.identifier.citation Mguda, Z,Faltenbacher, A, Van der Heyden, K, Gottlöber, S, Cress, C, Vaisanen, P and Yepes, G. 2015. Ram pressure statistics for bent tail radio galaxies. Monthly Notices of the Royal Astronomical Society Journal, vol. 446, pp 3310–3318 en_US
dc.identifier.issn 0035-8711
dc.description Copyright: 2015 Oxford University Press en_US
dc.description.abstract In this paper we use the MareNostrum Universe Simulation, a large scale, hydrodynamic, non-radiative simulation in combination with a simple abundance matching approach to determine the ram pressure statistics for bent radio sources (BRSs). The abundance matching approach allows us to determine the locations of all galaxies with stellar masses >10(sup11)MSol in the simulation volume. Assuming ram pressure exceeding a critical value causes bent morphology, we compute the ratio of all galaxies exceeding the ram pressure limit (RPEX galaxies) relative to all galaxies in our sample. According to our model 50% of the RPEX galaxies at z=0 are found in clusters with masses larger than 10(sup14.5)MSol the other half resides in lower mass clusters. Therefore, the appearance of bent tail morphology alone does not put tight constraints on the host cluster mass. In low mass clusters, M<10(sup14)MSol, RPEX galaxies are confined to the central 500 kpc whereas in clusters of >10(sup15)Msol they can be found at distances up to 1.5Mpc. Only clusters with masses >10(sup15)MSol are likely to host more than one BRS. Both criteria may prove useful in the search for distant, high mass clusters. en_US
dc.language.iso en en_US
dc.publisher Oxford University Press en_US
dc.relation.ispartofseries Workflow;14569
dc.subject Radio Astronomy en_US
dc.subject N-body simulations en_US
dc.subject Galaxies en_US
dc.title Ram pressure statistics for bent tail radio galaxies en_US
dc.type Article en_US

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