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Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
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2010 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 718, no 1, 23-30 p.Article in journal (Refereed) Published
Abstract [en]

We present deep J-and K-s-band photometry of 20 high redshift galaxy clusters between z = 0.8 and 1.5, 19 of which are observed with the MOIRCS instrument on the Subaru telescope. By using near-infrared light as a proxy for stellar mass we find the surprising result that the average stellar mass of Brightest Cluster Galaxies (BCGs) has remained constant at similar to 9 x 10(11) M-circle dot since z similar to 1.5. We investigate the effect on this result of differing star formation histories generated by three well-known and independent stellar population codes and find it to be robust for reasonable, physically motivated choices of age and metallicity. By performing Monte Carlo simulations we find that the result is unaffected by any correlation between BCG mass and cluster mass in either the observed or model clusters. The large stellar masses imply that the assemblage of these galaxies took place at the same time as the initial burst of star formation. This result leads us to conclude that dry merging has had little effect on the average stellar mass of BCGs over the last 9-10 Gyr in stark contrast to the predictions of semi-analytic models, based on the hierarchical merging of dark matter halos, which predict a more protracted mass build-up over a Hubble time. However, we discuss that there is potential for reconciliation between observation and theory if there is a significant growth of material in the intracluster light over the same period.

Place, publisher, year, edition, pages
2010. Vol. 718, no 1, 23-30 p.
Keyword [en]
galaxies: clusters: general, galaxies: evolution, galaxies: elliptical and lenticular, cD
National Category
Natural Sciences
URN: urn:nbn:se:su:diva-49709DOI: 10.1088/0004-637X/718/1/23ISI: 000280340800003OAI: diva2:379278
authorCount :17Available from: 2010-12-17 Created: 2010-12-17 Last updated: 2011-05-10Bibliographically approved

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Sahlén, Martin
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