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Probing dark energy with future redshift surveys : a comparison of emission line and broad-band selection in the near-infrared.

Orsi, A. and Baugh, C.M. and Lacey, C.G. and Cimatti, A. and Wang, Y. and Zamorani, G. (2010) 'Probing dark energy with future redshift surveys : a comparison of emission line and broad-band selection in the near-infrared.', Monthly notices of the Royal Astronomical Society., 405 (2). pp. 1006-1024.

Abstract

Future galaxy surveys will map the galaxy distribution in the redshift interval 0.5 < z < 2 using near-infrared cameras and spectrographs. The primary scientific goal of such surveys is to constrain the nature of the dark energy by measuring the large-scale structure of the Universe. This requires a tracer of the underlying dark matter which maximizes the useful volume of the survey. We investigate two potential survey selection methods: an emission-line sample based on the Hα line and a sample selected in the H band. We present predictions for the abundance and clustering of such galaxies, using two published versions of the galform galaxy formation model. Our models predict that Hαselected galaxies tend to avoid massive dark matter haloes and instead trace the surrounding filamentary structure; H-band selected galaxies, on the other hand, are found in the highest mass haloes. This has implications for the measurement of the rate at which fluctuations grow due to gravitational instability. We use mock catalogues to compare the effective volumes sampled by a range of survey configurations. To give just two examples: a redshift survey down to HAB= 22 samples an effective volume that is approximately five to 10 times larger than that probed by an Hα survey with log(FHα[erg s−1 cm−2]) > −15.4 and a flux limit of at least log(FHα[erg s−1 cm−2]) =−16 is required for an Hα sample to become competitive in effective volume.

Item Type:Article
Keywords:Methods: numerical, Galaxies: evolution, Galaxies: high-redshift, Dark energy, Large-scale structure of Universe
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Status:Peer-reviewed
Publisher Web site:http://dx.doi.org/10.1111/j.1365-2966.2010.16585.x
Publisher statement:This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2010 The Authors. Journal compilation © 2010 RAS. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Date accepted:No date available
Date deposited:26 November 2014
Date of first online publication:June 2010
Date first made open access:No date available

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