1996/10/25 by F. Hammer, P. Teyssandier, Hammer, F. +10
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics (astro-ph) #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9610207
12 pages,Latex, available at ftp://gin.obspm.fr/depot/hammer , Submitted to ApJ Letter
arxiv created 1996/10/25 · openalex publication_date 1996/10/25 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
A deep HST image of the MS 2137-2353 core has revealed detailed morphological structures in two arc systems, which are modelled and well reproduced after a complete analysis of the lensing properties of the dark matter component. Latter could have a simple elliptical mass distribution with ellipticity and angular orientation similar to those of the visible and X-ray light, which suggests that the MS 2137-2353 is a relaxed cluster at z=0.313. The predicted density profile (ρ ∼ r-1.56±0.1 with rc ≤ 22.5h50-1 kpc) within 150h50-1 kpc implies increasing M/L ratio with the radius, and could be in agreement with predictions from standard CDM simulations. At least two faint sources (unlensed magnitude, R=23.9 and 26, respectively) are aligned with the cluster core and are responsible of the arc systems. They have been reconstructed with details as small as 0".02 (or 160h50-1 pc in the source assumed at z= 1), one could be a nearly edge-on barred spiral galaxy, and the other has a more complex morphology, which could be related to a close interacting pair and/or to dust. They show strong signs of star formation indicated by compact HII regions well off their center. The observation of giant luminous arcs by HST could even resolve the size of giant HII regions at z∼ 1.