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Measuring redshift-space distortions using photometric surveys

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Measuring redshift-space distortions using photometric surveys. / Ross, Ashley; Percival, Will; Crocce, M.; Cabre, A.; Gaztanaga, E.

In: Monthly Notices of the Royal Astronomical Society, Vol. 415, No. 3, 08.2011, p. 2193-2204.

Research output: Contribution to journalArticle

Harvard

Ross, A, Percival, W, Crocce, M, Cabre, A & Gaztanaga, E 2011, 'Measuring redshift-space distortions using photometric surveys', Monthly Notices of the Royal Astronomical Society, vol. 415, no. 3, pp. 2193-2204. https://doi.org/10.1111/j.1365-2966.2011.18843.x

APA

Ross, A., Percival, W., Crocce, M., Cabre, A., & Gaztanaga, E. (2011). Measuring redshift-space distortions using photometric surveys. Monthly Notices of the Royal Astronomical Society, 415(3), 2193-2204. https://doi.org/10.1111/j.1365-2966.2011.18843.x

Vancouver

Ross A, Percival W, Crocce M, Cabre A, Gaztanaga E. Measuring redshift-space distortions using photometric surveys. Monthly Notices of the Royal Astronomical Society. 2011 Aug;415(3):2193-2204. https://doi.org/10.1111/j.1365-2966.2011.18843.x

Author

Ross, Ashley ; Percival, Will ; Crocce, M. ; Cabre, A. ; Gaztanaga, E. / Measuring redshift-space distortions using photometric surveys. In: Monthly Notices of the Royal Astronomical Society. 2011 ; Vol. 415, No. 3. pp. 2193-2204.

Bibtex

@article{05094eb3c3e045309377a7c715769e71,
title = "Measuring redshift-space distortions using photometric surveys",
abstract = "We outline how redshift-space distortions (RSD) can be measured from the angular correlation function, w(θ), of galaxies selected from photometric surveys. The natural degeneracy between RSD and galaxy bias can be minimized by comparing results from bins with top-hat galaxy selection in redshift, and bins based on the radial position of galaxy pair centres. This comparison can also be used to test the accuracy of the photometric redshifts. The presence of RSD will be clearly detectable with the next generation of photometric redshift surveys. We show that the Dark Energy Survey (DES) will be able to measure f(z)σ8(z) to a 1σ accuracy of (17 ×b) per cent, using galaxies drawn from a single narrow redshift slice centred at z= 1. Here b is the linear bias, and f is the logarithmic rate of change of the linear growth rate with respect to the scalefactor. Extending to measurements of w(θ) for a series of bins of width 0.02(1 +z) over 0.5 < z < 1.4 will measure to a 1σ accuracy of 0.25, given the model f=Ωm(z), and assuming a linear bias model that evolves such that b= 0.5 +z (and fixing other cosmological parameters). The accuracy of our analytic predictions is confirmed using mock catalogues drawn from simulations conducted by the Marenostrum Institut de Ci{\`e}ncies de l'Espai Simulations (MICE) collaboration.",
author = "Ashley Ross and Will Percival and M. Crocce and A. Cabre and E. Gaztanaga",
year = "2011",
month = "8",
doi = "10.1111/j.1365-2966.2011.18843.x",
language = "English",
volume = "415",
pages = "2193--2204",
journal = "MNRAS",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "3",

}

RIS

TY - JOUR

T1 - Measuring redshift-space distortions using photometric surveys

AU - Ross, Ashley

AU - Percival, Will

AU - Crocce, M.

AU - Cabre, A.

AU - Gaztanaga, E.

PY - 2011/8

Y1 - 2011/8

N2 - We outline how redshift-space distortions (RSD) can be measured from the angular correlation function, w(θ), of galaxies selected from photometric surveys. The natural degeneracy between RSD and galaxy bias can be minimized by comparing results from bins with top-hat galaxy selection in redshift, and bins based on the radial position of galaxy pair centres. This comparison can also be used to test the accuracy of the photometric redshifts. The presence of RSD will be clearly detectable with the next generation of photometric redshift surveys. We show that the Dark Energy Survey (DES) will be able to measure f(z)σ8(z) to a 1σ accuracy of (17 ×b) per cent, using galaxies drawn from a single narrow redshift slice centred at z= 1. Here b is the linear bias, and f is the logarithmic rate of change of the linear growth rate with respect to the scalefactor. Extending to measurements of w(θ) for a series of bins of width 0.02(1 +z) over 0.5 < z < 1.4 will measure to a 1σ accuracy of 0.25, given the model f=Ωm(z), and assuming a linear bias model that evolves such that b= 0.5 +z (and fixing other cosmological parameters). The accuracy of our analytic predictions is confirmed using mock catalogues drawn from simulations conducted by the Marenostrum Institut de Ciències de l'Espai Simulations (MICE) collaboration.

AB - We outline how redshift-space distortions (RSD) can be measured from the angular correlation function, w(θ), of galaxies selected from photometric surveys. The natural degeneracy between RSD and galaxy bias can be minimized by comparing results from bins with top-hat galaxy selection in redshift, and bins based on the radial position of galaxy pair centres. This comparison can also be used to test the accuracy of the photometric redshifts. The presence of RSD will be clearly detectable with the next generation of photometric redshift surveys. We show that the Dark Energy Survey (DES) will be able to measure f(z)σ8(z) to a 1σ accuracy of (17 ×b) per cent, using galaxies drawn from a single narrow redshift slice centred at z= 1. Here b is the linear bias, and f is the logarithmic rate of change of the linear growth rate with respect to the scalefactor. Extending to measurements of w(θ) for a series of bins of width 0.02(1 +z) over 0.5 < z < 1.4 will measure to a 1σ accuracy of 0.25, given the model f=Ωm(z), and assuming a linear bias model that evolves such that b= 0.5 +z (and fixing other cosmological parameters). The accuracy of our analytic predictions is confirmed using mock catalogues drawn from simulations conducted by the Marenostrum Institut de Ciències de l'Espai Simulations (MICE) collaboration.

U2 - 10.1111/j.1365-2966.2011.18843.x

DO - 10.1111/j.1365-2966.2011.18843.x

M3 - Article

VL - 415

SP - 2193

EP - 2204

JO - MNRAS

JF - MNRAS

SN - 0035-8711

IS - 3

ER -

ID: 106593