David Cole, University of Leicester Walter Dehnen; Mark Wilkinson – University of Leicester; Justin Read – ETH Zurich 29 June 2012.
A weak lensing_mass_reconstruction_of _the_large_scale_filament_massive_galaxy_cluster_macsj0717
One tenth solar_abundances_along_the_body_of-the_stream
Clash new multiple-images constraining the inner mass profile of macs j1206.2-0847
N.33 dvorak captured-trojans
Parallelization Strategies for Implementing Nbody Codes on Multicore Architectures
Mapping the three_dimensional_density_of_the_galactic_bulge_with_vvv_red_clump_stars
To measure the brightness distribution of galaxies, we must determine the surface brightness of the resolved galaxy. Surface brightness = magnitude within.
Ryuji Morishima (UCLA/JPL). N-body code: Gravity solver + Integrator Gravity solver must be fast and handle close encounters Special hardware (N 2 ):
Disentangling dynamic and geometric distortions Federico Marulli Dipartimento di Astronomia, Università di Bologna Marulli, Bianchi, Branchini, Guzzo,
Galaxy Clustering Topology : Constraints on Galaxy Formation Models and Cosmological Parameters The CosPA 2009 Meeting, Nov. 18-20, 2009 Changbom Park.
SKA: Synergies with optical and infrared surveys Matt Jarvis University of Hertfordshire.