Dark Energy Survey Year 1 results: Measurement of the galaxy angular power spectrum

H. Camacho; N. Kokron; F. Andrade-Oliveira; R. Rosenfeld; M. Lima; F. Lacasa; F. Sobreira; L. N. Da Costa; S. Avila; K. C. Chan; M. Crocce; A. J. Ross; A. Troja; J. García-Bellido; T. M.C. Abbott; F. B. Abdalla; S. Allam; J. Annis; R. A. Bernstein; E. Bertin; S. L. Bridle; D. Brooks; E. Buckley-Geer; D. L. Burke; A. Carnero Rosell; M. Carrasco Kind; J. Carretero; F. J. Castander; R. Cawthon; C. E. Cunha; C. B. D'Andrea; J. De Vicente; S. Desai; H. T. Diehl; P. Doel; J. Estrada; A. E. Evrard; B. Flaugher; P. Fosalba; J. Frieman; D. W. Gerdes; T. Giannantonio; R. A. Gruendl; J. Gschwend; G. Gutierrez; D. L. Hollowood; K. Honscheid; B. Hoyle; D. J. James; M. W.G. Johnson; M. D. Johnson; S. Kent; D. Kirk; E. Krause; K. Kuehn; N. Kuropatkin; H. Lin; J. L. Marshall; R. Miquel; W. J. Percival; A. A. Plazas; A. K. Romer; A. Roodman; E. Sanchez; M. Schubnell; I. Sevilla-Noarbe; M. Smith; R. C. Smith; M. Soares-Santos; E. Suchyta; M. E.C. Swanson; G. Tarle; D. Thomas; D. L. Tucker; A. R. Walker; J. Zuntz

doi:10.1093/mnras/stz1514

Dark Energy Survey Year 1 results: Measurement of the galaxy angular power spectrum

H. Camacho, N. Kokron, F. Andrade-Oliveira, R. Rosenfeld, M. Lima, F. Lacasa, F. Sobreira, L. N. Da Costa, S. Avila, K. C. Chan, M. Crocce, A. J. Ross, A. Troja, J. García-Bellido, T. M.C. Abbott, F. B. Abdalla, S. Allam, J. Annis, R. A. Bernstein, E. BertinS. L. Bridle, D. Brooks, E. Buckley-Geer, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, R. Cawthon, C. E. Cunha, C. B. D'Andrea, J. De Vicente, S. Desai, H. T. Diehl, P. Doel, J. Estrada, A. E. Evrard, B. Flaugher, P. Fosalba, J. Frieman, D. W. Gerdes, T. Giannantonio, R. A. Gruendl, J. Gschwend, G. Gutierrez, D. L. Hollowood, K. Honscheid, B. Hoyle, D. J. James, M. W.G. Johnson, M. D. Johnson, S. Kent, D. Kirk, E. Krause, K. Kuehn, N. Kuropatkin, H. Lin, J. L. Marshall, R. Miquel, W. J. Percival, A. A. Plazas, A. K. Romer, A. Roodman, E. Sanchez, M. Schubnell, I. Sevilla-Noarbe, M. Smith, R. C. Smith, M. Soares-Santos, E. Suchyta, M. E.C. Swanson, G. Tarle, D. Thomas, D. L. Tucker, A. R. Walker, J. Zuntz

Workflow Systems

Research output: Contribution to journal › Article › peer-review

26 Scopus citations

Abstract

We use data from the first-year observations of the DES collaboration to measure the galaxy angular power spectrum (APS), and search for its BAO feature. We test our methodology in a sample of 1800 DES Y1-like mock catalogues. We use the pseudo-C_l method to estimate the APS and the mock catalogues to estimate its covariance matrix. We use templates to model the measured spectra and estimate template parameters firstly from the C_l's of the mocks using two different methods, a maximum likelihood estimator and a Markov Chain Monte Carlo, finding consistent results with a good reduced χ². Robustness tests are performed to estimate the impact of different choices of settings used in our analysis. Finally, we apply our method to a galaxy sample constructed from DES Y1 data specifically for LSS studies. This catalogue comprises galaxies within an effective area of 1318 deg² and 0.6 < z < 1.0. We find that the DES Y1 data favour a model with BAO at the $2.6 σ C.L. However, the goodness of fit is somewhat poor, with χ²/(d.o.f.) = 1.49. We identify a possible cause showing that using a theoretical covariance matrix obtained from C_l's that are better adjusted to data results in an improved value of χ²/(dof) = 1.36 which is similar to the value obtained with the real-space analysis. Our results correspond to a distance measurement of D_A(z_eff = 0.81)/r_d = 10.65 ± 0.49, consistent with the main DES BAO findings. This is a companion paper to the main DES BAO article showing the details of the harmonic space analysis.

Original language	English
Pages (from-to)	3870-3883
Number of pages	14
Journal	Monthly Notices of the Royal Astronomical Society
Volume	487
Issue number	3
DOIs	https://doi.org/10.1093/mnras/stz1514
State	Published - Aug 11 2019

Funding

HC is supported by the Conselho Nacional de Desenvolvimento CientíficoeTecnológico(CNPq) undergrantnumber141935/2014-6. ML and RR are partially supported by the Fundac¸ão para o Amparo da Pesquisa no estado de São Paulo (FAPESP) and CNPq. AT is supported by FAPESP. We thank the support of the Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundac¸ão Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovac¸ão, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. Based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes.

Keywords

cosmology: observations
large-scale structure of Universe

Access to Document

10.1093/mnras/stz1514

Cite this

Camacho, H., Kokron, N., Andrade-Oliveira, F., Rosenfeld, R., Lima, M., Lacasa, F., Sobreira, F., Da Costa, L. N., Avila, S., Chan, K. C., Crocce, M., Ross, A. J., Troja, A., García-Bellido, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bernstein, R. A., ... Zuntz, J. (2019). Dark Energy Survey Year 1 results: Measurement of the galaxy angular power spectrum. Monthly Notices of the Royal Astronomical Society, 487(3), 3870-3883. https://doi.org/10.1093/mnras/stz1514

@article{25ce301ce05f44d88cf91b910a35be30,

title = "Dark Energy Survey Year 1 results: Measurement of the galaxy angular power spectrum",

abstract = "We use data from the first-year observations of the DES collaboration to measure the galaxy angular power spectrum (APS), and search for its BAO feature. We test our methodology in a sample of 1800 DES Y1-like mock catalogues. We use the pseudo-Cl method to estimate the APS and the mock catalogues to estimate its covariance matrix. We use templates to model the measured spectra and estimate template parameters firstly from the Cl's of the mocks using two different methods, a maximum likelihood estimator and a Markov Chain Monte Carlo, finding consistent results with a good reduced χ2. Robustness tests are performed to estimate the impact of different choices of settings used in our analysis. Finally, we apply our method to a galaxy sample constructed from DES Y1 data specifically for LSS studies. This catalogue comprises galaxies within an effective area of 1318 deg2 and 0.6 < z < 1.0. We find that the DES Y1 data favour a model with BAO at the $2.6 σ C.L. However, the goodness of fit is somewhat poor, with χ2/(d.o.f.) = 1.49. We identify a possible cause showing that using a theoretical covariance matrix obtained from Cl's that are better adjusted to data results in an improved value of χ2/(dof) = 1.36 which is similar to the value obtained with the real-space analysis. Our results correspond to a distance measurement of DA(zeff = 0.81)/rd = 10.65 ± 0.49, consistent with the main DES BAO findings. This is a companion paper to the main DES BAO article showing the details of the harmonic space analysis.",

keywords = "cosmology: observations, large-scale structure of Universe",

author = "H. Camacho and N. Kokron and F. Andrade-Oliveira and R. Rosenfeld and M. Lima and F. Lacasa and F. Sobreira and {Da Costa}, {L. N.} and S. Avila and Chan, {K. C.} and M. Crocce and Ross, {A. J.} and A. Troja and J. Garc{\'i}a-Bellido and Abbott, {T. M.C.} and Abdalla, {F. B.} and S. Allam and J. Annis and Bernstein, {R. A.} and E. Bertin and Bridle, {S. L.} and D. Brooks and E. Buckley-Geer and Burke, {D. L.} and {Carnero Rosell}, A. and {Carrasco Kind}, M. and J. Carretero and Castander, {F. J.} and R. Cawthon and Cunha, {C. E.} and D'Andrea, {C. B.} and {De Vicente}, J. and S. Desai and Diehl, {H. T.} and P. Doel and J. Estrada and Evrard, {A. E.} and B. Flaugher and P. Fosalba and J. Frieman and Gerdes, {D. W.} and T. Giannantonio and Gruendl, {R. A.} and J. Gschwend and G. Gutierrez and Hollowood, {D. L.} and K. Honscheid and B. Hoyle and James, {D. J.} and Johnson, {M. W.G.} and Johnson, {M. D.} and S. Kent and D. Kirk and E. Krause and K. Kuehn and N. Kuropatkin and H. Lin and Marshall, {J. L.} and R. Miquel and Percival, {W. J.} and Plazas, {A. A.} and Romer, {A. K.} and A. Roodman and E. Sanchez and M. Schubnell and I. Sevilla-Noarbe and M. Smith and Smith, {R. C.} and M. Soares-Santos and E. Suchyta and Swanson, {M. E.C.} and G. Tarle and D. Thomas and Tucker, {D. L.} and Walker, {A. R.} and J. Zuntz",

note = "Publisher Copyright: {\textcopyright} 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.",

year = "2019",

month = aug,

day = "11",

doi = "10.1093/mnras/stz1514",

language = "English",

volume = "487",

pages = "3870--3883",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

}

Camacho, H, Kokron, N, Andrade-Oliveira, F, Rosenfeld, R, Lima, M, Lacasa, F, Sobreira, F, Da Costa, LN, Avila, S, Chan, KC, Crocce, M, Ross, AJ, Troja, A, García-Bellido, J, Abbott, TMC, Abdalla, FB, Allam, S, Annis, J, Bernstein, RA, Bertin, E, Bridle, SL, Brooks, D, Buckley-Geer, E, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Castander, FJ, Cawthon, R, Cunha, CE, D'Andrea, CB, De Vicente, J, Desai, S, Diehl, HT, Doel, P, Estrada, J, Evrard, AE, Flaugher, B, Fosalba, P, Frieman, J, Gerdes, DW, Giannantonio, T, Gruendl, RA, Gschwend, J, Gutierrez, G, Hollowood, DL, Honscheid, K, Hoyle, B, James, DJ, Johnson, MWG, Johnson, MD, Kent, S, Kirk, D, Krause, E, Kuehn, K, Kuropatkin, N, Lin, H, Marshall, JL, Miquel, R, Percival, WJ, Plazas, AA, Romer, AK, Roodman, A, Sanchez, E, Schubnell, M, Sevilla-Noarbe, I, Smith, M, Smith, RC, Soares-Santos, M, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Tucker, DL, Walker, AR & Zuntz, J 2019, 'Dark Energy Survey Year 1 results: Measurement of the galaxy angular power spectrum', Monthly Notices of the Royal Astronomical Society, vol. 487, no. 3, pp. 3870-3883. https://doi.org/10.1093/mnras/stz1514

TY - JOUR

T1 - Dark Energy Survey Year 1 results

T2 - Measurement of the galaxy angular power spectrum

AU - Camacho, H.

AU - Kokron, N.

AU - Andrade-Oliveira, F.

AU - Rosenfeld, R.

AU - Lima, M.

AU - Lacasa, F.

AU - Sobreira, F.

AU - Da Costa, L. N.

AU - Avila, S.

AU - Chan, K. C.

AU - Crocce, M.

AU - Ross, A. J.

AU - Troja, A.

AU - García-Bellido, J.

AU - Abbott, T. M.C.

AU - Abdalla, F. B.

AU - Allam, S.

AU - Annis, J.

AU - Bernstein, R. A.

AU - Bertin, E.

AU - Bridle, S. L.

AU - Brooks, D.

AU - Buckley-Geer, E.

AU - Burke, D. L.

AU - Carnero Rosell, A.

AU - Carrasco Kind, M.

AU - Carretero, J.

AU - Castander, F. J.

AU - Cawthon, R.

AU - Cunha, C. E.

AU - D'Andrea, C. B.

AU - De Vicente, J.

AU - Desai, S.

AU - Diehl, H. T.

AU - Doel, P.

AU - Estrada, J.

AU - Evrard, A. E.

AU - Flaugher, B.

AU - Fosalba, P.

AU - Frieman, J.

AU - Gerdes, D. W.

AU - Giannantonio, T.

AU - Gruendl, R. A.

AU - Gschwend, J.

AU - Gutierrez, G.

AU - Hollowood, D. L.

AU - Honscheid, K.

AU - Hoyle, B.

AU - James, D. J.

AU - Johnson, M. W.G.

AU - Johnson, M. D.

AU - Kent, S.

AU - Kirk, D.

AU - Krause, E.

AU - Kuehn, K.

AU - Kuropatkin, N.

AU - Lin, H.

AU - Marshall, J. L.

AU - Miquel, R.

AU - Percival, W. J.

AU - Plazas, A. A.

AU - Romer, A. K.

AU - Roodman, A.

AU - Sanchez, E.

AU - Schubnell, M.

AU - Sevilla-Noarbe, I.

AU - Smith, M.

AU - Smith, R. C.

AU - Soares-Santos, M.

AU - Suchyta, E.

AU - Swanson, M. E.C.

AU - Tarle, G.

AU - Thomas, D.

AU - Tucker, D. L.

AU - Walker, A. R.

AU - Zuntz, J.

PY - 2019/8/11

Y1 - 2019/8/11

N2 - We use data from the first-year observations of the DES collaboration to measure the galaxy angular power spectrum (APS), and search for its BAO feature. We test our methodology in a sample of 1800 DES Y1-like mock catalogues. We use the pseudo-Cl method to estimate the APS and the mock catalogues to estimate its covariance matrix. We use templates to model the measured spectra and estimate template parameters firstly from the Cl's of the mocks using two different methods, a maximum likelihood estimator and a Markov Chain Monte Carlo, finding consistent results with a good reduced χ2. Robustness tests are performed to estimate the impact of different choices of settings used in our analysis. Finally, we apply our method to a galaxy sample constructed from DES Y1 data specifically for LSS studies. This catalogue comprises galaxies within an effective area of 1318 deg2 and 0.6 < z < 1.0. We find that the DES Y1 data favour a model with BAO at the $2.6 σ C.L. However, the goodness of fit is somewhat poor, with χ2/(d.o.f.) = 1.49. We identify a possible cause showing that using a theoretical covariance matrix obtained from Cl's that are better adjusted to data results in an improved value of χ2/(dof) = 1.36 which is similar to the value obtained with the real-space analysis. Our results correspond to a distance measurement of DA(zeff = 0.81)/rd = 10.65 ± 0.49, consistent with the main DES BAO findings. This is a companion paper to the main DES BAO article showing the details of the harmonic space analysis.

AB - We use data from the first-year observations of the DES collaboration to measure the galaxy angular power spectrum (APS), and search for its BAO feature. We test our methodology in a sample of 1800 DES Y1-like mock catalogues. We use the pseudo-Cl method to estimate the APS and the mock catalogues to estimate its covariance matrix. We use templates to model the measured spectra and estimate template parameters firstly from the Cl's of the mocks using two different methods, a maximum likelihood estimator and a Markov Chain Monte Carlo, finding consistent results with a good reduced χ2. Robustness tests are performed to estimate the impact of different choices of settings used in our analysis. Finally, we apply our method to a galaxy sample constructed from DES Y1 data specifically for LSS studies. This catalogue comprises galaxies within an effective area of 1318 deg2 and 0.6 < z < 1.0. We find that the DES Y1 data favour a model with BAO at the $2.6 σ C.L. However, the goodness of fit is somewhat poor, with χ2/(d.o.f.) = 1.49. We identify a possible cause showing that using a theoretical covariance matrix obtained from Cl's that are better adjusted to data results in an improved value of χ2/(dof) = 1.36 which is similar to the value obtained with the real-space analysis. Our results correspond to a distance measurement of DA(zeff = 0.81)/rd = 10.65 ± 0.49, consistent with the main DES BAO findings. This is a companion paper to the main DES BAO article showing the details of the harmonic space analysis.

KW - cosmology: observations

KW - large-scale structure of Universe

UR - http://www.scopus.com/inward/record.url?scp=85072252876&partnerID=8YFLogxK

U2 - 10.1093/mnras/stz1514

DO - 10.1093/mnras/stz1514

M3 - Article

AN - SCOPUS:85072252876

SN - 0035-8711

VL - 487

SP - 3870

EP - 3883

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

Dark Energy Survey Year 1 results: Measurement of the galaxy angular power spectrum

Abstract

Funding

Keywords

Access to Document

Other files and links

Fingerprint

Cite this