david cole, walter dehnen, mark wilkinson university of leicester dark matter in clusters, groups...
TRANSCRIPT
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David Cole, Walter Dehnen, Mark WilkinsonUniversity of Leicester
Dark Matter in clusters, groups and galaxiesNottingham-Birmingham extragalactic
workshopNottingham 14/15 September 2011
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The cusp/core problem
log radius
Navarro, Frenk & White 1997 Navarro et al 2010
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Observations
Oh et al 2008IC 2574
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Analytical model
Parabolic orbit
Final halo mass model 1
Final halo mass model 2
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Fiducial runs
t
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Effects on the dark matter halo
r
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Halo shape
r r
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Anisotropy
r
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Satellite orbitsTime evolution of the orbits of satellites representing baryonic clumps for four parabolic satellite orbits decaying in a dark matter halo with isotropic velocity distribution.
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Effect on Dark Matter Halo
Radial profiles of the halo’s pseudo phase-space density ρ/σ3 (top), density ρ (middle), and the change in cumulative halo mass ΔM (bottom) at the end of the simulations shown in the previous slide (colour coding the same).
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Effect of the Removal of the satellite
Radial profiles of the halo’s pseudo phase-space density ρ/σ3 (top), density ρ (middle), and the change in cumulative halo mass ΔM (bottom) for one of the satellites shown in the previous slide but also including the removal of the satellite.
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Effect of satellite Mass
The variation with satellite mass of time to fall in,tinfall, ΔMmax, rmax, r50%, and the maximum of ρ/σ3 after the decay of a circular satellite orbit (red) or after the decay of a parabolic satellite orbit (blue). The lines are power-laws with exponent as indicated.
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Effect of satellite SizeAs previous slide, except that satellite size rs is varied and ms = 0.01 kept constant.
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Sinking clumps – minor mergers
Hubble Interacting Galaxy NGC 695
Hubble Interacting Galaxy IRAS F10565
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Conclusions
Sinking clumps can modify the cuspParabolic orbits have a stronger effectSmaller clumps are more effectiveHalo shape and velocity structure changedExpulsion of the clump material produces
an even greater effect