HAWK-I imaging of the X-ray luminous galaxy cluster XMMU J2235.3-2557^*

The red sequence at z = 1.39

¹ European Southern Observatory, Alonso de Cordova 3107, Casilla 19001, Santiago, Chile e-mail: clidman@eso.org
² European Southern Observatory, Karl-schwarzschild-Strasse 2, 85748 Garching, Germany
³ National Radio Astronomy Observatory, PO Box O, Socorro, NM 87801, USA
⁴ Department of Physics and Astronomy, John Hopkins University, Baltimore, USA
⁵ Wachovia Corporation, NC6740, 100 N. Main Street, Winston-Salem, NC 27101, USA
⁶ MPI für extraterrestische Physik, Giessenbachsrtasse, 85748 Garching, Germany

Received: 5 July 2008
Accepted: 31 July 2008

Abstract

We use HAWK-I, the recently-commissioned near-IR imager on Yepun (VLT-UT4), to obtain wide-field, high-resolution images of the X-ray luminous galaxy cluster XMMU J2235.3-2557 in the J and Ks bands, and we use these images to build a colour-magnitude diagram of cluster galaxies. Galaxies in the core of the cluster form a tight red sequence with a mean colour of 1.9 (Vega system). The intrinsic scatter in the colour of galaxies that lie on the red sequence is similar to that measured for galaxies on the red sequence of the Coma cluster. The slope and location of the red sequence can be modelled by passively evolving the red sequence of the Coma cluster backwards in time. Using simple stellar population (SSP) models, we find that galaxies in the core of XMMU J2235.3-2557 are, even at , already 3 Gyr old, corresponding to a formation redshift of . Outside the core, the intrinsic scatter and the fraction of galaxies actively forming stars increase substantially. Using SSP models, we find that most of these galaxies will join the red sequence within 1.5 Gyr. The contrast between galaxies in the cluster core and galaxies in the cluster outskirts indicates that the red sequence of XMMU J2235.3-2557 is being built from the dense cluster core outwards.