Skip to content
Back to outputs

Universal fitting formulae for baryon oscillation surveys

Research output: Contribution to journalArticlepeer-review

Standard

Universal fitting formulae for baryon oscillation surveys. / Blake, Chris; Parkinson, David; Glazebrook, Karl; Bassett, Bruce A.; Kunz, Martin; Nichol, Robert C.

In: Monthly Notices of the Royal Astronomical Society, Vol. 365, No. 1, 2006, p. 255-264.

Research output: Contribution to journalArticlepeer-review

Harvard

Blake, C, Parkinson, D, Glazebrook, K, Bassett, BA, Kunz, M & Nichol, RC 2006, 'Universal fitting formulae for baryon oscillation surveys', Monthly Notices of the Royal Astronomical Society, vol. 365, no. 1, pp. 255-264. https://doi.org/10.1111/j.1365-2966.2005.09706.x

APA

Blake, C., Parkinson, D., Glazebrook, K., Bassett, B. A., Kunz, M., & Nichol, R. C. (2006). Universal fitting formulae for baryon oscillation surveys. Monthly Notices of the Royal Astronomical Society, 365(1), 255-264. https://doi.org/10.1111/j.1365-2966.2005.09706.x

Vancouver

Blake C, Parkinson D, Glazebrook K, Bassett BA, Kunz M, Nichol RC. Universal fitting formulae for baryon oscillation surveys. Monthly Notices of the Royal Astronomical Society. 2006;365(1):255-264. https://doi.org/10.1111/j.1365-2966.2005.09706.x

Author

Blake, Chris ; Parkinson, David ; Glazebrook, Karl ; Bassett, Bruce A. ; Kunz, Martin ; Nichol, Robert C. / Universal fitting formulae for baryon oscillation surveys. In: Monthly Notices of the Royal Astronomical Society. 2006 ; Vol. 365, No. 1. pp. 255-264.

Bibtex

@article{9e44ac705e2d4127a50edb195688b05c,
title = "Universal fitting formulae for baryon oscillation surveys",
abstract = "The next generation of galaxy surveys will attempt to measure the baryon oscillations in the clustering power spectrum with high accuracy. These oscillations encode a preferred scale which may be used as a standard ruler to constrain cosmological parameters and dark energy models. In this paper we present simple analytical fitting formulae for the accuracy with which the preferred scale may be determined in the tangential and radial directions by future spectroscopic and photometric galaxy redshift surveys. We express these accuracies as a function of survey parameters such as the central redshift, volume, galaxy number density and (where applicable) photometric redshift error. These fitting formulae should greatly increase the efficiency of optimizing future surveys, which requires analysis of a potentially vast number of survey configurations and cosmological models. The formulae are calibrated using a grid of Monte Carlo simulations, which are analyzed by dividing out the overall shape of the power spectrum before fitting a simple decaying sinusoid to the oscillations. The fitting formulae reproduce the simulation results with a fractional scatter of 7% (10%) in the tangential (radial) directions over a wide range of input parameters. We also indicate how sparse-sampling strategies may enhance the effective survey area if the sampling scale is much smaller than the projected baryon oscillation scale",
author = "Chris Blake and David Parkinson and Karl Glazebrook and Bassett, {Bruce A.} and Martin Kunz and Nichol, {Robert C.}",
year = "2006",
doi = "10.1111/j.1365-2966.2005.09706.x",
language = "English",
volume = "365",
pages = "255--264",
journal = "MNRAS",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "1",

}

RIS

TY - JOUR

T1 - Universal fitting formulae for baryon oscillation surveys

AU - Blake, Chris

AU - Parkinson, David

AU - Glazebrook, Karl

AU - Bassett, Bruce A.

AU - Kunz, Martin

AU - Nichol, Robert C.

PY - 2006

Y1 - 2006

N2 - The next generation of galaxy surveys will attempt to measure the baryon oscillations in the clustering power spectrum with high accuracy. These oscillations encode a preferred scale which may be used as a standard ruler to constrain cosmological parameters and dark energy models. In this paper we present simple analytical fitting formulae for the accuracy with which the preferred scale may be determined in the tangential and radial directions by future spectroscopic and photometric galaxy redshift surveys. We express these accuracies as a function of survey parameters such as the central redshift, volume, galaxy number density and (where applicable) photometric redshift error. These fitting formulae should greatly increase the efficiency of optimizing future surveys, which requires analysis of a potentially vast number of survey configurations and cosmological models. The formulae are calibrated using a grid of Monte Carlo simulations, which are analyzed by dividing out the overall shape of the power spectrum before fitting a simple decaying sinusoid to the oscillations. The fitting formulae reproduce the simulation results with a fractional scatter of 7% (10%) in the tangential (radial) directions over a wide range of input parameters. We also indicate how sparse-sampling strategies may enhance the effective survey area if the sampling scale is much smaller than the projected baryon oscillation scale

AB - The next generation of galaxy surveys will attempt to measure the baryon oscillations in the clustering power spectrum with high accuracy. These oscillations encode a preferred scale which may be used as a standard ruler to constrain cosmological parameters and dark energy models. In this paper we present simple analytical fitting formulae for the accuracy with which the preferred scale may be determined in the tangential and radial directions by future spectroscopic and photometric galaxy redshift surveys. We express these accuracies as a function of survey parameters such as the central redshift, volume, galaxy number density and (where applicable) photometric redshift error. These fitting formulae should greatly increase the efficiency of optimizing future surveys, which requires analysis of a potentially vast number of survey configurations and cosmological models. The formulae are calibrated using a grid of Monte Carlo simulations, which are analyzed by dividing out the overall shape of the power spectrum before fitting a simple decaying sinusoid to the oscillations. The fitting formulae reproduce the simulation results with a fractional scatter of 7% (10%) in the tangential (radial) directions over a wide range of input parameters. We also indicate how sparse-sampling strategies may enhance the effective survey area if the sampling scale is much smaller than the projected baryon oscillation scale

U2 - 10.1111/j.1365-2966.2005.09706.x

DO - 10.1111/j.1365-2966.2005.09706.x

M3 - Article

VL - 365

SP - 255

EP - 264

JO - MNRAS

JF - MNRAS

SN - 0035-8711

IS - 1

ER -

ID: 127414