2009/08/26 by M. J. Jee, M. James Jee, P. Rosati +11
Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Brightest cluster galaxy #Cluster (spacecraft) #Cosmology #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy cluster #Gamma-ray bursts and supernovae #Gravitational lens #Physics #Redshift #Sigma #Weak gravitational lensing #astro-ph.CO
paper · pdf · doi:10.1088/0004-637x/704/1/672
Accepted to ApJ for publication. 40 pages and 14 figures
arxiv created 2009/08/26 · openalex publication_date 2009/09/24 · arxiv updated 2015/05/14 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We present a weak-lensing analysis of the z ≃ 1.4 galaxy cluster XMMU J2235.3 − 2557, based on deep Advanced Camera for Surveys images. Despite the observational challenge set by the high redshift of the lens, we detect a substantial lensing signal at the ≳8σ level. This clear detection is enabled in part by the high mass of the cluster, which is verified by our both parametric and non-parametric estimation of the cluster mass. Assuming that the cluster follows a Navarro–Frenk–White mass profile, we estimate that the projected mass of the cluster within r = 1 Mpc is (8.5 ± 1.7) × 10 14 M ☉ , where the error bar includes the statistical uncertainty of the shear profile, the effect of possible interloping background structures, the scatter in concentration parameter, and the error in our estimation of the mean redshift of the background galaxies. The high X-ray temperature 8.6 +1.3 −1.2 keV of the cluster recently measured with Chandra is consistent with this high lensing mass. When we adopt the 1σ lower limit as a mass threshold and use the cosmological parameters favored by the Wilkinson Microwave Anisotropy Probe 5-year ( WMAP5 ) result, the expected number of similarly massive clusters at z ≳ 1.4 in the 11 square degree survey is N ∼ 5 × 10 −3 . Therefore, the discovery of the cluster within the survey volume is a rare event with a probability ≲1% and may open new scenarios in our current understanding of cluster formation within the standard cosmological model.