Astronomy and Astrophysics – Astrophysics
Scientific paper
2006-11-29
Astronomy and Astrophysics
Astrophysics
13 pages, 18 figures: minor revisions to match version accepted by MNRAS
Scientific paper
10.1111/j.1365-2966.2007.12018.x
Measuring the distribution of mass on galaxy cluster scales is a crucial test of the Lambda CDM model, providing constraints on the nature of dark matter. Recent work investigating mass distributions of individual galaxy clusters using gravitational lensing has illuminated potential inconsistencies between the predictions of structure formation models relating halo mass to concentration and those relationships as measured in massive clusters. However, such analyses typically employ only simple spherical halo models with canonical NFW slopes, while the halos formed in simulations show a range of more complex features. Here we investigate the impact of such expected deviations from the canonical NFW halo profile on mass and parameter estimation using weak gravitational lensing on massive cluster scales. The most important deviation is halo triaxiality because it is impossible even with fiducial weak lensing data to fully resolve the three-dimensional structure of the halo due to lensing's sensitivity only to projected mass. Significant elongation of the halo along the line of sight can cause the mass and concentration to be overestimated by as much as 50% and by a factor of 2, respectively, while foreshortening has the opposite effect. Additionally, triaxial halos in certain orientations are much better lenses than their spherical counterparts of the same mass, indicating that clusters chosen for study because of evident lensing are likely to be drawn from the high-triaxiality end of the halo shape distribution. While the effects of triaxiality alone may not be enough to fully explain the very high concentrations reported for some clusters, they go a long way in easing the tensions between observations and the predictions of the cold dark matter paradigm. (Abridged)
Corless Virginia
King Lindsay
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