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The structure and evolution of a forming galaxy cluster at z = 1.62

journal contribution
posted on 2016-04-18, 08:24 authored by N. A. Hatch, Stuart Iain Muldrew, E. A. Cooke, W. G. Hartley, O. Almaini, C. J. Simpson, C. J. Conselice
We present a comprehensive picture of the Cl 0218.3-0510 protocluster at z = 1.623 across 10 co-moving Mpc. Using filters that tightly bracket the Balmer and 4000Å breaks of the protocluster galaxies we obtain precise photometric redshifts resulting in a protocluster galaxy sample that is 89 ± 5% complete and has a contamination of only 12 ± 5%. Both star forming and quiescent protocluster galaxies are located allowing us to map the structure of the forming cluster for the first time. The protocluster contains 6 galaxy groups, the largest of which is the nascent cluster. Only a small minority of the protocluster galaxies are in the nascent cluster (11%) or in the other galaxy groups (22%), as most protocluster galaxies reside between the groups. Unobscured star forming galaxies predominantly reside between the protocluster's groups, whereas red galaxies make up a large fraction of the groups' galactic content, so observing the protocluster through only one of these types of galaxies results in a biased view of the protocluster's structure. The structure of the protocluster reveals how much mass is available for the future growth of the cluster and we use the Millennium Simulation, scaled to a Planck cosmology, to predict that Cl 0218.3-0510 will evolve into a 2.7^{+3.9}_{-1.7}× 10^{14} M_{⊙} cluster by the present day.

History

Citation

Monthly Notices of the Royal Astronomical Society, 2016, 459(1), pp. 387-401

Author affiliation

/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomy

Version

  • VoR (Version of Record)

Published in

Monthly Notices of the Royal Astronomical Society

Publisher

Oxford University Press (OUP)

issn

0035-8711

eissn

1365-2966

Acceptance date

2016-03-10

Copyright date

2016

Available date

2016-04-18

Publisher version

http://mnras.oxfordjournals.org/content/459/1/387

Language

en

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