Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 411, Issue 3, Pages 2009-2018Publisher
OXFORD UNIV PRESS
DOI: 10.1111/j.1365-2966.2010.17828.x
Keywords
galaxies: clusters: individual: XMMU J2235.3-2557; galaxies: evolution; galaxies: fundamental parameters; galaxies: high-redshift; galaxies: star formation
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Funding
- National Science Foundation (United States)
- Science and Technology Facilities Council (United Kingdom)
- National Research Council (Canada)
- CONICYT (Chile)
- Australian Research Council (Australia)
- Ministerio da Ciencia e Tecnologia (Brazil)
- Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina)
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We present the first results of a narrow-band photometric study of the massive galaxy cluster XMMU J2235.3-2557 at z = 1.39. We obtained deep H narrow-band imaging with the Near InfraRed Imager and Spectrometer on Gemini North, corresponding to Ha emission at the cluster's redshift. Our sample consists of 82 galaxies within a radius of similar to 500 kpc, 10 of which are spectroscopically confirmed cluster members. 16 galaxies are identified as excess line-emitters. Among just the excess line-emitting galaxies, we find an average star formation rate (SFR) of 3.6 +/- 1.3M(circle dot) yr(-1). For spectroscopically confirmed cluster members, we find a correlation between H broad-band magnitude and SFR such that brighter galaxies have lower SFRs. The probability that the SFR and magnitude of confirmed members are uncorrelated is 0.7 per cent. We also find a correlation between the SFR and distance from the cluster centre for both confirmed and excess line-emitting candidate members, with a probability of 5 per cent for there to be no correlation among confirmed members. All excess line-emitting candidate cluster members are located outside a radius of 200 kpc. We conclude that star formation is effectively shut off within the central 200 kpc radius (R-QUENCH similar to 200 kpc) of this massive galaxy cluster at z = 1.39, when the Universe was only 4.5 Gyr old.
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