The haloes of merger remnants

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dc.creatorMcMillan, P. J.
dc.creatorAthanassoula, E.
dc.creatorDehnen, W.
dc.date2007-01-18
dc.date2007-03-23
dc.date.accessioned2026-07-07T10:21:33Z
dc.date.available2026-07-07T10:21:33Z
dc.descriptionWe perform collisionless N-body simulations of 1:1 galaxy mergers, using models which include a galaxy halo, disc and bulge, focusing on the behaviour of the halo component. The galaxy models are constructed without recourse to a Maxwellian approximation. We investigate the effect of varying the galaxies' orientation, their mutual orbit, and the initial velocity anisotropy or cusp strength of the haloes upon the remnant halo density profiles and shape, as well as on the kinematics. We observe that the halo density profile (determined as a spherical average, an approximation we find appropriate) is exceptionally robust in mergers, and that the velocity anisotropy of our remnant haloes is nearly independent of the orbits or initial anisotropy of the haloes. The remnants follow the halo anisotropy - local density slope (β-γ) relation suggested by Hansen & Moore (2006} in the inner parts of the halo, but βis systematically lower than this relation predicts in the outer parts. Remnant halo axis ratios are strongly dependent on the initial parameters of the haloes and on their orbits. We also find that the remnant haloes are significantly less spherical than those described in studies of simulations which include gas cooling.
dc.description10 pages, 11 figures, MNRAS accepted, edited to correct equation 4
dc.identifierhttps://arxiv.org/abs/astro-ph/0701541
dc.identifierhttp://arxiv.org/abs/astro-ph/0701541
dc.identifierMon.Not.Roy.Astron.Soc.376:1261-1269,2007
dc.identifierdoi:10.1111/j.1365-2966.2007.11516.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/175211
dc.subjectAstrophysics
dc.titleThe haloes of merger remnants
dc.typetext

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