Protoclusters with evolved populations around radio galaxies at z ∼ 2.5

Masaru Kajisawa, Tadayuki Kodama, Ichi Tanaka, Toru Yamada, Richard Bower

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45 Citations (Scopus)

Abstract

We report the discovery of protocluster candidates around high-redshift radio galaxies at z ∼ 2.5 on the basis of clear statistical excess of colour-selected galaxies around them seen in the deep near-infrared imaging data obtained with CISCO on the Subaru Telescope. We have observed six targets, all at similar redshifts at z ∼ 2.5, and our data reach J = 23.5, H = 22.6 and K = 21.8 (5σ) and cover a 1.6 × 1.6 arcmin 2 field centred on each radio galaxy. We apply colour cuts in JHK bands in order to exclusively search for galaxies located at high redshifts, z > 2. Over the magnitude range of 19.5 < K < 21.5, we see a significant excess of red galaxies with J - K > 2.3 by a factor of 2 around the combined radio galaxies fields compared to those found in the general field of the Great Observatories Origins Deep Survey-South (GOODS-S). The excess of galaxies around the radio galaxies fields becomes more than a factor of 3 around 19.5 < K < 20.5 when the two-colour cuts are applied with JHK bands. Such overdensity of the colour-selected galaxies suggests that those fields tend to host high-density regions at high redshifts, although there seems to be the variety of the density of the colour-selected galaxies in each field. In particular, two radio galaxies fields out of the six observed fields show very strong density excess and these are likely to be protoclusters associated with the radio galaxies which would evolve into rich clusters of galaxies dominated by old passively evolving galaxies.

Original languageEnglish
Pages (from-to)577-582
Number of pages6
JournalMonthly Notices of the Royal Astronomical Society
Volume371
Issue number2
DOIs
Publication statusPublished - 2006 Sep

Keywords

  • Galaxies: clusters: general
  • Galaxies: evolution
  • Galaxies: high-redshift

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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