2006/10/17 by Lindsay King, Virginia Corless · 3 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Cluster (spacecraft) #Cold dark matter #Dark matter #Electrical and Electromagnetic Research #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy cluster #Gravitational lens #Halo #Mass distribution #Weak gravitational lensing #astro-ph
paper · pdf · doi:10.1111/j.1745-3933.2006.00260.x
published as Mon.Not.Roy.Astron.Soc.Lett. 374 (2007) L37-L41 · To appear in MNRAS letters, 5 pages, 3 figures
arxiv created 2006/10/17 · openalex publication_date 2006/11/21 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Abstract The distribution of mass on galaxy cluster scales is an important test of structure formation scenarios, providing constraints on the nature of dark matter itself. Several techniques have been used to probe the mass distributions of clusters, sometimes yielding results which are discrepant, or at odds with clusters formed in simulations – for example giving Navarro–Frenk–White (NFW) concentration parameters much higher than expected in the standard cold dark matter (CDM) model. In addition, the velocity fields of some well-studied galaxy clusters reveal the presence of several structures close to the line of sight, often not dynamically bound to the cluster itself. We investigate what impact such neighbouring but unbound massive structures would have on the determination of cluster profiles using weak gravitational lensing. Depending on its concentration and mass ratio to the primary halo, one secondary halo close to the line-of-sight can cause the estimated NFW concentration parameter to be significantly higher than that of the primary halo, and also cause the estimated mass to be biased high. Although it is difficult to envisage how this mechanism alone could yield concentrations as high as reported for some clusters, multiple haloes close to the line-of-sight, such as in the case of Abell 1689, can substantially increase the concentration parameter estimate. Together with the fact that clusters are triaxial, and that including baryonic physics also leads to an increase in the concentration of a dark matter halo, the tension between observations and the standard CDM model is eased. Additionally, we note that if the alignment with the secondary structure is imprecise, then the estimated concentration parameter can also be even lower than that of the primary halo, reinforcing the importance of identifying structures in cluster fields.