The massive galaxy cluster XMMU J1230.3+1339 at z ∼ 1: colour-magnitude relation, Butcher-Oemler effect, X-ray and weak lensing mass estimates★

2010/09/20 by M. Lerchster, S. Seitz, F. Brimioulle +8
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Brightest cluster galaxy #Cluster (spacecraft) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy cluster #Gravitational lens #Spectroscopy #Strong gravitational lensing #Weak gravitational lensing #astro-ph.CO

paper · pdf · doi:10.1111/j.1365-2966.2010.17874.x

29 pages, 34 figures, 6 tables, full resolution pdf-file available at http://www.usm.uni-muenchen.de/people/mike/XMMUJ1230_MNRAS.pdf, submitted to MNRAS, shortened abstract

arxiv created 2010/09/20 · openalex publication_date 2011/01/28 · arxiv updated 2015/05/20 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05

Abstract

We present results from the multi-wavelength study of XMMU J1230.3+1339 at z ~ 1. We analyze deep multi-band wide-field images from the Large Binocular Telescope, multi-object spectroscopy observations from VLT, as well as space-based serendipitous observations, from the GALEX and Chandra X-ray observatories. We apply a Bayesian photometric redshift code to derive the redshifts using the FUV, NUV and the deep U, B, V, r, i, z data. We achieve an accuracy of triangle z/(1+z) = 0.07 (0.04) and the fraction of catastrophic outliers is \η = 13 (0)%, when using all (secure) spectroscopic data, respectively. The i - z against z colour-magnitude relation of the photo-z members shows a tight red-sequence with a zero point of 0.935 mag, and slope equal to -0.027. We observe evidence for a truncation at the faint end of the red-cluster-sequence and the Butcher-Oemler effect, finding a fraction of blue galaxies f_b \≈ 0.5. Further we conduct a weak lensing analysis of the deep 26' \× 26' r-band LBC image. The observed shear is fitted with a Single-Isothermal-Sphere and a Navarro-Frenk-White model to obtain the velocity dispersion and the model parameters, respectively. Our best fit values are, for the velocity dispersion \σ_SIS = 1308 \± 284, concentration parameter c = 4.0⁺¹⁴_-2 and scale radius r_s = 345⁺⁵⁰_-57 kpc. Combining our mass estimates from the kinematic, X-ray and weak lensing analyses we obtain a total cluster mass of M^tot₂₀₀ = (4.56 \± 2.3) \× 10¹⁴ M _sun. This study demonstrates the feasibility of ground based weak lensing measurements of galaxy clusters up to z ~ 1.

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