Multi-wavelength study of XMMU J2235.3-2557: the most massive galaxy cluster at z > 1

• Published in: Astronomy and astrophysics (Berlin) 2009-12, Vol.508 (2), p.583-591
• Main Authors: Rosati, P., Tozzi, P., Gobat, R., Santos, J. S., Nonino, M., Demarco, R., Lidman, C., Mullis, C. R., Strazzullo, V., Böhringer, H., Fassbender, R., Dawson, K., Tanaka, M., Jee, J., Ford, H., Lamer, G., Schwope, A.
• Format: Article
• Language: English
• Subjects: Astronomy; Earth, ocean, space; Exact sciences and technology; galaxies: clusters: individual: XMMU J2235.3-2557; galaxies: evolution; galaxies: high-redshift; X-rays: galaxies: clusters
• ISSN: 0004-6361; 1432-0746
• DOI: 10.1051/0004-6361/200913099

Context. The galaxy cluster XMMU J2235.3-2557 (hereafter XMM2235), spectroscopically confirmed at $z = 1.39$, is one of the most distant X-ray selected galaxy clusters. It has been at the center of a multi-wavelength observing campaign with ground and space facilities. Aims. We characterize the galaxy populations of passive members, the thermodynamical properties and metal abundance of the hot gas, and the total mass of the system using imaging data with HST/ACS (i775 and z850 bands) and VLT/ISAAC (J and KS bands), extensive spectroscopic data obtained with VLT/FORS2, and deep (196 ks) Chandra observations. Methods. Chandra data allow temperature and metallicity to be measured with good accuracy and the X-ray surface brightness profile to be traced out to 1´ (or 500 kpc), thus allowing the mass to be reliably estimated. Out of a total sample of 34 spectroscopically confirmed cluster members, we selected 16 passive galaxies (without detectable [OII]) within the central 2´ (or 1 Mpc) with ACS coverage, and inferred star formation histories for subsamples of galaxies inside and outside the core by modeling their spectro-photometric data with spectral synthesis models. Results. Chandra data show a regular elongated morphology, closely resembling the distribution of core galaxies, with a significant cool core. We measure a global X-ray temperature of kT = $8.6_{\rm -1.2}^{+1.3}$ keV (68% confidence), which we find to be robust against several systematics involved in the X-ray spectral analysis. By detecting the rest frame 6.7 keV Iron K line in the Chandra  spectrum, we measure a metallicity Z = $0.26^{\rm +0.20}_{-0.16}$ $Z_\odot$. In the likely hypothesis of hydrostatic equilibrium, we obtain a total mass of $M_{\mathrm{tot}}$( 1$, with a baryonic content, both its galaxy population and intracluster gas, in a significantly