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Dark Energy Survey Year 1 Results: redshift distributions of the weak-lensing source galaxies

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Dark Energy Survey Year 1 Results: redshift distributions of the weak-lensing source galaxies. / Dark Energy Survey Collaboration; Macaulay, E.; Nichol, R. C.; Ross, A. J.; Capozzi, D.; Thomas, D.

In: Monthly Notices of the Royal Astronomical Society, Vol. 478, No. 1, 21.07.2018, p. 592-610.

Research output: Contribution to journalArticle

Harvard

Dark Energy Survey Collaboration, Macaulay, E, Nichol, RC, Ross, AJ, Capozzi, D & Thomas, D 2018, 'Dark Energy Survey Year 1 Results: redshift distributions of the weak-lensing source galaxies', Monthly Notices of the Royal Astronomical Society, vol. 478, no. 1, pp. 592-610. https://doi.org/10.1093/mnras/sty957

APA

Dark Energy Survey Collaboration, Macaulay, E., Nichol, R. C., Ross, A. J., Capozzi, D., & Thomas, D. (2018). Dark Energy Survey Year 1 Results: redshift distributions of the weak-lensing source galaxies. Monthly Notices of the Royal Astronomical Society, 478(1), 592-610. https://doi.org/10.1093/mnras/sty957

Vancouver

Dark Energy Survey Collaboration, Macaulay E, Nichol RC, Ross AJ, Capozzi D, Thomas D. Dark Energy Survey Year 1 Results: redshift distributions of the weak-lensing source galaxies. Monthly Notices of the Royal Astronomical Society. 2018 Jul 21;478(1):592-610. https://doi.org/10.1093/mnras/sty957

Author

Dark Energy Survey Collaboration ; Macaulay, E. ; Nichol, R. C. ; Ross, A. J. ; Capozzi, D. ; Thomas, D. / Dark Energy Survey Year 1 Results: redshift distributions of the weak-lensing source galaxies. In: Monthly Notices of the Royal Astronomical Society. 2018 ; Vol. 478, No. 1. pp. 592-610.

Bibtex

@article{c065ea5f56ab499e8d167ec52dce34f4,
title = "Dark Energy Survey Year 1 Results: redshift distributions of the weak-lensing source galaxies",
abstract = "We describe the derivation and validation of redshift distribution estimates and their uncertainties for the populations of galaxies used as weak-lensing sources in the Dark Energy Survey (DES) Year 1 cosmological analyses. The Bayesian Photometric Redshift (BPZ) code is used to assign galaxies to four redshift bins between z ≈ 0.2 and ≈1.3, and to produce initial estimates of the lensing-weighted redshift distributions niPZ(z)∝dni/dz for members of bin i. Accurate determination of cosmological parameters depends critically on knowledge of ni, but is insensitive to bin assignments or redshift errors for individual galaxies. The cosmological analyses allow for shifts ni(z)=niPZ(z−Δzi) to correct the mean redshift of ni(z) for biases in niPZ. The Δzi are constrained by comparison of independently estimated 30-band photometric redshifts of galaxies in the Cosmic Evolution Survey (COSMOS) field to BPZ estimates made from the DES griz fluxes, for a sample matched in fluxes, pre-seeing size, and lensing weight to the DES weak-lensing sources. In companion papers, the Δzi of the three lowest redshift bins are further constrained by the angular clustering of the source galaxies around red galaxies with secure photometric redshifts at 0.15 < z < 0.9. This paper details the BPZ and COSMOS procedures, and demonstrates that the cosmological inference is insensitive to details of the ni(z) beyond the choice of Δzi. The clustering and COSMOS validation methods produce consistent estimates of Δzi in the bins where both can be applied, with combined uncertainties of σΔzi=0.015,0.013,0.011,and 0.022 in the four bins. Repeating the photo-z procedure instead using the Directional Neighbourhood Fitting algorithm, or using the ni(z) estimated from the matched sample in COSMOS, yields no discernible difference in cosmological inferences.",
keywords = "RCUK, STFC",
author = "{Dark Energy Survey Collaboration} and B. Hoyle and D. Gruen and Bernstein, {G. M.} and Rau, {M. M.} and J. De Vicente and Hartley, {W. G.} and E. Gaztanaga and J. Derose and Troxel, {M. A.} and C. Davis and A. Alarcon and N. MacCrann and J. Prat and C. S{\'a}nchez and E. Sheldon and Wechsler, {R. H.} and J. Asorey and Becker, {M. R.} and C. Bonnett and Rosell, {A. C.} and D. Carollo and Kind, {M. C.} and Castander, {F. J.} and R. Cawthon and C. Chang and M. Childress and Davis, {T. M.} and A. Drlica-Wagner and M. Gatti and K. Glazebrook and J. Gschwend and Hinton, {S. R.} and Hoormann, {J. K.} and Kim, {A. G.} and A. King and K. Kuehn and G. Lewis and C. Lidman and H. Lin and E. Macaulay and Maia, {M. A. G.} and P. Martini and D. Mudd and A. M{\"o}ller and Nichol, {R. C.} and Ogando, {R. L. C.} and Rollins, {R. P.} and Ross, {A. J.} and D. Capozzi and D. Thomas",
year = "2018",
month = jul,
day = "21",
doi = "10.1093/mnras/sty957",
language = "English",
volume = "478",
pages = "592--610",
journal = "MNRAS",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "1",

}

RIS

TY - JOUR

T1 - Dark Energy Survey Year 1 Results: redshift distributions of the weak-lensing source galaxies

AU - Dark Energy Survey Collaboration

AU - Hoyle, B.

AU - Gruen, D.

AU - Bernstein, G. M.

AU - Rau, M. M.

AU - De Vicente, J.

AU - Hartley, W. G.

AU - Gaztanaga, E.

AU - Derose, J.

AU - Troxel, M. A.

AU - Davis, C.

AU - Alarcon, A.

AU - MacCrann, N.

AU - Prat, J.

AU - Sánchez, C.

AU - Sheldon, E.

AU - Wechsler, R. H.

AU - Asorey, J.

AU - Becker, M. R.

AU - Bonnett, C.

AU - Rosell, A. C.

AU - Carollo, D.

AU - Kind, M. C.

AU - Castander, F. J.

AU - Cawthon, R.

AU - Chang, C.

AU - Childress, M.

AU - Davis, T. M.

AU - Drlica-Wagner, A.

AU - Gatti, M.

AU - Glazebrook, K.

AU - Gschwend, J.

AU - Hinton, S. R.

AU - Hoormann, J. K.

AU - Kim, A. G.

AU - King, A.

AU - Kuehn, K.

AU - Lewis, G.

AU - Lidman, C.

AU - Lin, H.

AU - Macaulay, E.

AU - Maia, M. A. G.

AU - Martini, P.

AU - Mudd, D.

AU - Möller, A.

AU - Nichol, R. C.

AU - Ogando, R. L. C.

AU - Rollins, R. P.

AU - Ross, A. J.

AU - Capozzi, D.

AU - Thomas, D.

PY - 2018/7/21

Y1 - 2018/7/21

N2 - We describe the derivation and validation of redshift distribution estimates and their uncertainties for the populations of galaxies used as weak-lensing sources in the Dark Energy Survey (DES) Year 1 cosmological analyses. The Bayesian Photometric Redshift (BPZ) code is used to assign galaxies to four redshift bins between z ≈ 0.2 and ≈1.3, and to produce initial estimates of the lensing-weighted redshift distributions niPZ(z)∝dni/dz for members of bin i. Accurate determination of cosmological parameters depends critically on knowledge of ni, but is insensitive to bin assignments or redshift errors for individual galaxies. The cosmological analyses allow for shifts ni(z)=niPZ(z−Δzi) to correct the mean redshift of ni(z) for biases in niPZ. The Δzi are constrained by comparison of independently estimated 30-band photometric redshifts of galaxies in the Cosmic Evolution Survey (COSMOS) field to BPZ estimates made from the DES griz fluxes, for a sample matched in fluxes, pre-seeing size, and lensing weight to the DES weak-lensing sources. In companion papers, the Δzi of the three lowest redshift bins are further constrained by the angular clustering of the source galaxies around red galaxies with secure photometric redshifts at 0.15 < z < 0.9. This paper details the BPZ and COSMOS procedures, and demonstrates that the cosmological inference is insensitive to details of the ni(z) beyond the choice of Δzi. The clustering and COSMOS validation methods produce consistent estimates of Δzi in the bins where both can be applied, with combined uncertainties of σΔzi=0.015,0.013,0.011,and 0.022 in the four bins. Repeating the photo-z procedure instead using the Directional Neighbourhood Fitting algorithm, or using the ni(z) estimated from the matched sample in COSMOS, yields no discernible difference in cosmological inferences.

AB - We describe the derivation and validation of redshift distribution estimates and their uncertainties for the populations of galaxies used as weak-lensing sources in the Dark Energy Survey (DES) Year 1 cosmological analyses. The Bayesian Photometric Redshift (BPZ) code is used to assign galaxies to four redshift bins between z ≈ 0.2 and ≈1.3, and to produce initial estimates of the lensing-weighted redshift distributions niPZ(z)∝dni/dz for members of bin i. Accurate determination of cosmological parameters depends critically on knowledge of ni, but is insensitive to bin assignments or redshift errors for individual galaxies. The cosmological analyses allow for shifts ni(z)=niPZ(z−Δzi) to correct the mean redshift of ni(z) for biases in niPZ. The Δzi are constrained by comparison of independently estimated 30-band photometric redshifts of galaxies in the Cosmic Evolution Survey (COSMOS) field to BPZ estimates made from the DES griz fluxes, for a sample matched in fluxes, pre-seeing size, and lensing weight to the DES weak-lensing sources. In companion papers, the Δzi of the three lowest redshift bins are further constrained by the angular clustering of the source galaxies around red galaxies with secure photometric redshifts at 0.15 < z < 0.9. This paper details the BPZ and COSMOS procedures, and demonstrates that the cosmological inference is insensitive to details of the ni(z) beyond the choice of Δzi. The clustering and COSMOS validation methods produce consistent estimates of Δzi in the bins where both can be applied, with combined uncertainties of σΔzi=0.015,0.013,0.011,and 0.022 in the four bins. Repeating the photo-z procedure instead using the Directional Neighbourhood Fitting algorithm, or using the ni(z) estimated from the matched sample in COSMOS, yields no discernible difference in cosmological inferences.

KW - RCUK

KW - STFC

U2 - 10.1093/mnras/sty957

DO - 10.1093/mnras/sty957

M3 - Article

VL - 478

SP - 592

EP - 610

JO - MNRAS

JF - MNRAS

SN - 0035-8711

IS - 1

ER -

ID: 10846701