2006/11/02 by A. Halkola, S. Seitz, M. Pannella · 48 citations
Physics and Astronomy · #Abell 2744 #Astronomy and Astrophysical Research #Brightest cluster galaxy #Cluster (spacecraft) #Dark matter #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy cluster #Halo #Interacting galaxy #Scientific Research and Discoveries #Type-cD galaxy #Velocity dispersion #astro-ph
paper · pdf · doi:10.1086/510555
published in The Astrophysical Journal 656(2), 739-745 (IOP Publishing) · 12 pages, 4 figures. Accepted for publication in the ApJ
arxiv created 2006/11/02 · openalex publication_date 2007/02/14 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
The multiple images observed in the galaxy cluster Abell 1689 provide strong constraints not only on the mass distribution of the cluster, but also on the ensemble properties of the cluster galaxies. Using parametric strong-lensing models for the cluster, and by assuming well-motivated scaling laws between the truncation radius s and the velocity dispersion σ of a cluster galaxy, we are able to derive the sizes of the dark matter halos of cluster galaxies. For the scaling law expected for galaxies in the cluster environment ( s ∝ σ), we obtain s = 64 (σ/220 km s -1 ) kpc. For the scaling law used for galaxies in the field with s ∝ σ 2 , we find s = 66 (σ/220 km s -1 ) 2 kpc. Compared to halos of field galaxies, the cluster galaxy halos in Abell 1689 are strongly truncated.