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Dark Energy Survey Year 1 results: galaxy sample for BAO measurement

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Dark Energy Survey Year 1 results: galaxy sample for BAO measurement. / Dark Energy Survey Collaboration ; Ross, A. J.; Avila, S.; D'Andrea, C. B.; Nichol, R. C.; Percival, W. J.; Thomas, D.

In: Monthly Notices of the Royal Astronomical Society, Vol. 482, No. 2, 11.01.2019, p. 2807–2822.

Research output: Contribution to journalArticlepeer-review

Harvard

Dark Energy Survey Collaboration, Ross, AJ, Avila, S, D'Andrea, CB, Nichol, RC, Percival, WJ & Thomas, D 2019, 'Dark Energy Survey Year 1 results: galaxy sample for BAO measurement', Monthly Notices of the Royal Astronomical Society, vol. 482, no. 2, pp. 2807–2822. https://doi.org/10.1093/mnras/sty2522

APA

Dark Energy Survey Collaboration, Ross, A. J., Avila, S., D'Andrea, C. B., Nichol, R. C., Percival, W. J., & Thomas, D. (2019). Dark Energy Survey Year 1 results: galaxy sample for BAO measurement. Monthly Notices of the Royal Astronomical Society, 482(2), 2807–2822. https://doi.org/10.1093/mnras/sty2522

Vancouver

Dark Energy Survey Collaboration, Ross AJ, Avila S, D'Andrea CB, Nichol RC, Percival WJ et al. Dark Energy Survey Year 1 results: galaxy sample for BAO measurement. Monthly Notices of the Royal Astronomical Society. 2019 Jan 11;482(2):2807–2822. https://doi.org/10.1093/mnras/sty2522

Author

Dark Energy Survey Collaboration ; Ross, A. J. ; Avila, S. ; D'Andrea, C. B. ; Nichol, R. C. ; Percival, W. J. ; Thomas, D. / Dark Energy Survey Year 1 results: galaxy sample for BAO measurement. In: Monthly Notices of the Royal Astronomical Society. 2019 ; Vol. 482, No. 2. pp. 2807–2822.

Bibtex

@article{f9a84afe38e84996a9d1118920542ff0,
title = "Dark Energy Survey Year 1 results: galaxy sample for BAO measurement",
abstract = "We define and characterize a sample of 1.3 million galaxies extracted from the first year of Dark Energy Survey data, optimized to measure baryon acoustic oscillations (BAO) in the presence of significant redshift uncertainties. The sample is dominated by luminous red galaxies located at redshifts z ≳ 0.6. We define the exact selection using colour and magnitude cuts that balance the need of high number densities and small photometric redshift uncertainties, using the corresponding forecasted BAO distance error as a figure-of-merit in the process. The typical photo z uncertainty varies from 2.3 percent to 3.6 percent (in units of 1+z⁠) from z = 0.6 to 1, with number densities from 200 to 130 galaxies per deg2 in tomographic bins of width Δz = 0.1. Next, we summarize the validation of the photometric redshift estimation. We characterize and mitigate observational systematics including stellar contamination and show that the clustering on large scales is robust in front of those contaminants. We show that the clustering signal in the autocorrelations and cross-correlations is generally consistent with theoretical models, which serve as an additional test of the redshift distributions.",
keywords = "astro-ph.CO, RCUK, STFC",
author = "{Dark Energy Survey Collaboration} and M. Crocce and Ross, {A. J.} and I. Sevilla-Noarbe and E. Gaztanaga and J. Elvin-Poole and S. Avila and A. Alarcon and Chan, {K. C.} and N. Banik and J. Carretero and E. Sanchez and Hartley, {W. G.} and C. Sanchez and T. Giannantonio and R. Rosenfeld and Salvador, {A. I.} and M. Garcia-Fernandez and J. Garcia-Bellido and Abbott, {T. M. C.} and Abdalla, {F. B.} and S. Allam and J. Annis and K. Bechtol and A. Benoit-Levy and Bernstein, {G. M.} and Bernstein, {R. A.} and E. Bertin and D. Brooks and E. Buckley-Geer and Rosell, {A. Carnero} and Kind, {M. Carrasco} and Castander, {F. J.} and R. Cawthon and Cunha, {C. E.} and D'Andrea, {C. B.} and Costa, {L. N. da} and C. Davis and Vicente, {J. De} and S. Desai and Diehl, {H. T.} and P. Doel and A. Drlica-Wagner and Eifler, {T. F.} and P. Fosalba and J. Frieman and J. Garcia-Bellido and Gerdes, {D. W.} and Nichol, {R. C.} and Percival, {W. J.} and D. Thomas",
note = "15 pages, 12 figures. Added discussion on photo-z validation and other tests added based on referee's comments. Matches published version in MNRAS",
year = "2019",
month = jan,
day = "11",
doi = "10.1093/mnras/sty2522",
language = "English",
volume = "482",
pages = "2807–2822",
journal = "MNRAS",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "2",

}

RIS

TY - JOUR

T1 - Dark Energy Survey Year 1 results: galaxy sample for BAO measurement

AU - Dark Energy Survey Collaboration

AU - Crocce, M.

AU - Ross, A. J.

AU - Sevilla-Noarbe, I.

AU - Gaztanaga, E.

AU - Elvin-Poole, J.

AU - Avila, S.

AU - Alarcon, A.

AU - Chan, K. C.

AU - Banik, N.

AU - Carretero, J.

AU - Sanchez, E.

AU - Hartley, W. G.

AU - Sanchez, C.

AU - Giannantonio, T.

AU - Rosenfeld, R.

AU - Salvador, A. I.

AU - Garcia-Fernandez, M.

AU - Garcia-Bellido, J.

AU - Abbott, T. M. C.

AU - Abdalla, F. B.

AU - Allam, S.

AU - Annis, J.

AU - Bechtol, K.

AU - Benoit-Levy, A.

AU - Bernstein, G. M.

AU - Bernstein, R. A.

AU - Bertin, E.

AU - Brooks, D.

AU - Buckley-Geer, E.

AU - Rosell, A. Carnero

AU - Kind, M. Carrasco

AU - Castander, F. J.

AU - Cawthon, R.

AU - Cunha, C. E.

AU - D'Andrea, C. B.

AU - Costa, L. N. da

AU - Davis, C.

AU - Vicente, J. De

AU - Desai, S.

AU - Diehl, H. T.

AU - Doel, P.

AU - Drlica-Wagner, A.

AU - Eifler, T. F.

AU - Fosalba, P.

AU - Frieman, J.

AU - Garcia-Bellido, J.

AU - Gerdes, D. W.

AU - Nichol, R. C.

AU - Percival, W. J.

AU - Thomas, D.

N1 - 15 pages, 12 figures. Added discussion on photo-z validation and other tests added based on referee's comments. Matches published version in MNRAS

PY - 2019/1/11

Y1 - 2019/1/11

N2 - We define and characterize a sample of 1.3 million galaxies extracted from the first year of Dark Energy Survey data, optimized to measure baryon acoustic oscillations (BAO) in the presence of significant redshift uncertainties. The sample is dominated by luminous red galaxies located at redshifts z ≳ 0.6. We define the exact selection using colour and magnitude cuts that balance the need of high number densities and small photometric redshift uncertainties, using the corresponding forecasted BAO distance error as a figure-of-merit in the process. The typical photo z uncertainty varies from 2.3 percent to 3.6 percent (in units of 1+z⁠) from z = 0.6 to 1, with number densities from 200 to 130 galaxies per deg2 in tomographic bins of width Δz = 0.1. Next, we summarize the validation of the photometric redshift estimation. We characterize and mitigate observational systematics including stellar contamination and show that the clustering on large scales is robust in front of those contaminants. We show that the clustering signal in the autocorrelations and cross-correlations is generally consistent with theoretical models, which serve as an additional test of the redshift distributions.

AB - We define and characterize a sample of 1.3 million galaxies extracted from the first year of Dark Energy Survey data, optimized to measure baryon acoustic oscillations (BAO) in the presence of significant redshift uncertainties. The sample is dominated by luminous red galaxies located at redshifts z ≳ 0.6. We define the exact selection using colour and magnitude cuts that balance the need of high number densities and small photometric redshift uncertainties, using the corresponding forecasted BAO distance error as a figure-of-merit in the process. The typical photo z uncertainty varies from 2.3 percent to 3.6 percent (in units of 1+z⁠) from z = 0.6 to 1, with number densities from 200 to 130 galaxies per deg2 in tomographic bins of width Δz = 0.1. Next, we summarize the validation of the photometric redshift estimation. We characterize and mitigate observational systematics including stellar contamination and show that the clustering on large scales is robust in front of those contaminants. We show that the clustering signal in the autocorrelations and cross-correlations is generally consistent with theoretical models, which serve as an additional test of the redshift distributions.

KW - astro-ph.CO

KW - RCUK

KW - STFC

U2 - 10.1093/mnras/sty2522

DO - 10.1093/mnras/sty2522

M3 - Article

VL - 482

SP - 2807

EP - 2822

JO - MNRAS

JF - MNRAS

SN - 0035-8711

IS - 2

ER -

ID: 12755004