A dark cluster of galaxies at redshift z = 1

M. Hattori (), Y. Ikebe, I. Asaoka, T. Takeshima, H. Böhringer, T. Mihara, D. M. Neumann, S. Schindler, T. Tsuru and T. Tamura#
Additional contact information
M. Hattori: *Max-Planck-Institut für extraterrestrische Physik
Y. Ikebe: †The Institute of Physical and Chemical Research (Riken)
I. Asaoka: *Max-Planck-Institut für extraterrestrische Physik
T. Takeshima: †The Institute of Physical and Chemical Research (Riken)
H. Böhringer: *Max-Planck-Institut für extraterrestrische Physik
T. Mihara: †The Institute of Physical and Chemical Research (Riken)
D. M. Neumann: *Max-Planck-Institut für extraterrestrische Physik
S. Schindler: *Max-Planck-Institut für extraterrestrische Physik
T. Tsuru: Kyoto University
T. Tamura#: University of Tokyo

Nature, 1997, vol. 388, issue 6638, 146-148

Abstract: Abstract The abundance of metals in the hot, gaseous X-ray haloes of galaxy clusters depends crucially on the evolution of the constituent galaxies and their associated stellar populations. The metal abundances in X-ray clusters at high redshifts should therefore provide important insights into the nature and epoch of galaxyformation. Here we report the detection of an extended X-ray source in the direction of the lensed quasi-stellar object MG2016+112 (refs 1, 2). Although deep optical searches have failed to reveal a galaxy cluster at the lens position3,4, the X-ray emission is consistent with thermal bremsstrahlung radiation from a hot metal-rich, diffuse gaseous halo, as observed in nearby galaxy clusters. This is the most distant galaxy cluster discovered in X-rays so far. Furthermore, the mass of the cluster derived from this emission is consistent with that implied by lensing models of the system5. Given that the cluster apparently comprises few galaxies, yet contains a large amount of iron, a new type of astronomical object is implied by our results. A revision of theoretical models of the metal enrichment process in galaxy clusters may therefore be required.

Date: 1997
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DOI: 10.1038/40572

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