Survey geometry and the internal consistency of recent cosmic shear measurements

M. A. Troxel; E. Krause; C. Chang; T. F. Eifler; O. Friedrich; D. Gruen; N. MacCrann; A. Chen; C. Davis; J. DeRose; S. Dodelson; M. Gatti; B. Hoyle; D. Huterer; M. Jarvis; F. Lacasa; P. Lemos; H. V. Peiris; J. Prat; S. Samuroff; C. Sánchez; E. Sheldon; P. Vielzeuf; M. Wang; J. Zuntz; O. Lahav; F. B. Abdalla; S. Allam; J. Annis; S. Avila; E. Bertin; D. Brooks; D. L. Burke; A. Carnero Rosell; M. Carrasco Kind; J. Carretero; M. Crocce; C. E. Cunha; C. B. D'Andrea; L. N. Da Costa; J. De Vicente; H. T. Diehl; P. Doel; A. E. Evrard; B. Flaugher; P. Fosalba; J. Frieman; J. García-Bellido; E. Gaztanaga; D. W. Gerdes; R. A. Gruendl; J. Gschwend; G. Gutierrez; W. G. Hartley; D. L. Hollowood; K. Honscheid; D. J. James; D. Kirk; K. Kuehn; N. Kuropatkin; T. S. Li; M. Lima; M. March; F. Menanteau; R. Miquel; J. J. Mohr; R. L.C. Ogando; A. A. Plazas; A. Roodman; E. Sanchez; V. Scarpine; R. Schindler; I. Sevilla-Noarbe; M. Smith; M. Soares-Santos; F. Sobreira; E. Suchyta; M. E.C. Swanson; D. Thomas; A. R. Walker; R. H. Wechsler

doi:10.1093/mnras/sty1889

Survey geometry and the internal consistency of recent cosmic shear measurements

M. A. Troxel, E. Krause, C. Chang, T. F. Eifler, O. Friedrich, D. Gruen, N. MacCrann, A. Chen, C. Davis, J. DeRose, S. Dodelson, M. Gatti, B. Hoyle, D. Huterer, M. Jarvis, F. Lacasa, P. Lemos, H. V. Peiris, J. Prat, S. SamuroffC. Sánchez, E. Sheldon, P. Vielzeuf, M. Wang, J. Zuntz, O. Lahav, F. B. Abdalla, S. Allam, J. Annis, S. Avila, E. Bertin, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Crocce, C. E. Cunha, C. B. D'Andrea, L. N. Da Costa, J. De Vicente, H. T. Diehl, P. Doel, A. E. Evrard, B. Flaugher, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, R. A. Gruendl, J. Gschwend, G. Gutierrez, W. G. Hartley, D. L. Hollowood, K. Honscheid, D. J. James, D. Kirk, K. Kuehn, N. Kuropatkin, T. S. Li, M. Lima, M. March, F. Menanteau, R. Miquel, J. J. Mohr, R. L.C. Ogando, A. A. Plazas, A. Roodman, E. Sanchez, V. Scarpine, R. Schindler, I. Sevilla-Noarbe, M. Smith, M. Soares-Santos, F. Sobreira, E. Suchyta, M. E.C. Swanson, D. Thomas, A. R. Walker, R. H. Wechsler

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Abstract

We explore the impact of an update to the typical approximation for the shape noise term in the analytic covariance matrix for cosmic shear experiments that assumes the absence of survey boundary and mask effects. We present an exact expression for the number of galaxy pairs in this term based on the survey mask, which leads to more than a factor of three increase in the shape noise on the largest measured scales for the Kilo-Degree Survey (KiDS-450) real-space cosmic shear data. We compare the result of this analytic expression to several alternative methods for measuring the shape noise from the data and find excellent agreement. This update to the covariance resolves any internal model tension evidenced by the previously large cosmological best-fitting Χ² for the KiDS-450 cosmic shear data. The best-fitting Χ² is reduced from 161 to 121 for 118 degrees of freedom. We also apply a correction to how the multiplicative shear calibration uncertainty is included in the covariance. This change shifts the inferred amplitude of the correlation function to higher values. We find that this improves agreement of the KiDS-450 cosmic shear results with Dark Energy Survey Year 1 and Planck results.

Original language	English
Pages (from-to)	4998-5004
Number of pages	7
Journal	Monthly Notices of the Royal Astronomical Society
Volume	479
Issue number	4
DOIs	https://doi.org/10.1093/mnras/sty1889
State	Published - Oct 1 2018

Funding

EK thanks the Centro de Ciencias Pedro Pascual in Benasque, Spain for hospitality during the workshop Understanding cosmological observations, where some of this work originated. Funding for the DES Projects has been provided by the DOE and NSF(USA), MEC/MICINN/MINECO(Spain), STFC(UK), HEFCE(UK). NCSA(UIUC), KICP(U. Chicago), CCAPP(Ohio State), MIFPA(Texas A&M), CNPQ, FAPERJ, FINEP(Brazil), DFG(Germany) and the Collaborating Institutions in the DES. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. This work also used resources at the Ohio Supercomputing Center (OSC 1987). Some of the results in this paper have been derived using the HEALPIX (Górski et al. 2005) package. The DES Data Management System is supported by the NSF 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 Gen-eralitat 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, and the Brazilian Instituto Nacional de Ciênciae Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). We thank O. Doré, G. Efstathiou, C. Heymans, H. Hildebrandt, C. Hirata, B. Joachimi, S. Joudaki, and K. Kuijken for comments, and the KiDS Collaboration for providing their weak lensing data to the community. Part of this research was supported from NASA grant 15-WFIRST15-0008 Cosmology with the High Latitude Survey WFIRST Science Investigation Team. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration and is supported by NASA ROSES ATP 16-ATP16-0084 grant and by NASA ROSES 16-ADAP16-0116. PL acknowledges support from an Isaac Newton Studentship at the University of Cambridge and from the Science and Technologies Facilities Council. 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

Gravitational lensing: weak
Methods: data analysis
Methods: statistical

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10.1093/mnras/sty1889

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Troxel, M. A., Krause, E., Chang, C., Eifler, T. F., Friedrich, O., Gruen, D., MacCrann, N., Chen, A., Davis, C., DeRose, J., Dodelson, S., Gatti, M., Hoyle, B., Huterer, D., Jarvis, M., Lacasa, F., Lemos, P., Peiris, H. V., Prat, J., ... Wechsler, R. H. (2018). Survey geometry and the internal consistency of recent cosmic shear measurements. Monthly Notices of the Royal Astronomical Society, 479(4), 4998-5004. https://doi.org/10.1093/mnras/sty1889

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title = "Survey geometry and the internal consistency of recent cosmic shear measurements",

abstract = "We explore the impact of an update to the typical approximation for the shape noise term in the analytic covariance matrix for cosmic shear experiments that assumes the absence of survey boundary and mask effects. We present an exact expression for the number of galaxy pairs in this term based on the survey mask, which leads to more than a factor of three increase in the shape noise on the largest measured scales for the Kilo-Degree Survey (KiDS-450) real-space cosmic shear data. We compare the result of this analytic expression to several alternative methods for measuring the shape noise from the data and find excellent agreement. This update to the covariance resolves any internal model tension evidenced by the previously large cosmological best-fitting Χ2 for the KiDS-450 cosmic shear data. The best-fitting Χ2 is reduced from 161 to 121 for 118 degrees of freedom. We also apply a correction to how the multiplicative shear calibration uncertainty is included in the covariance. This change shifts the inferred amplitude of the correlation function to higher values. We find that this improves agreement of the KiDS-450 cosmic shear results with Dark Energy Survey Year 1 and Planck results.",

keywords = "Gravitational lensing: weak, Methods: data analysis, Methods: statistical",

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note = "Publisher Copyright: {\textcopyright} 2018 The Author(s). Published by Oxford University Press on behalf of The Royal Astronomical Society.",

year = "2018",

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Troxel, MA, Krause, E, Chang, C, Eifler, TF, Friedrich, O, Gruen, D, MacCrann, N, Chen, A, Davis, C, DeRose, J, Dodelson, S, Gatti, M, Hoyle, B, Huterer, D, Jarvis, M, Lacasa, F, Lemos, P, Peiris, HV, Prat, J, Samuroff, S, Sánchez, C, Sheldon, E, Vielzeuf, P, Wang, M, Zuntz, J, Lahav, O, Abdalla, FB, Allam, S, Annis, J, Avila, S, Bertin, E, Brooks, D, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Crocce, M, Cunha, CE, D'Andrea, CB, Da Costa, LN, De Vicente, J, Diehl, HT, Doel, P, Evrard, AE, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruendl, RA, Gschwend, J, Gutierrez, G, Hartley, WG, Hollowood, DL, Honscheid, K, James, DJ, Kirk, D, Kuehn, K, Kuropatkin, N, Li, TS, Lima, M, March, M, Menanteau, F, Miquel, R, Mohr, JJ, Ogando, RLC, Plazas, AA, Roodman, A, Sanchez, E, Scarpine, V, Schindler, R, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Thomas, D, Walker, AR & Wechsler, RH 2018, 'Survey geometry and the internal consistency of recent cosmic shear measurements', Monthly Notices of the Royal Astronomical Society, vol. 479, no. 4, pp. 4998-5004. https://doi.org/10.1093/mnras/sty1889

TY - JOUR

T1 - Survey geometry and the internal consistency of recent cosmic shear measurements

AU - Troxel, M. A.

AU - Krause, E.

AU - Chang, C.

AU - Eifler, T. F.

AU - Friedrich, O.

AU - Gruen, D.

AU - MacCrann, N.

AU - Chen, A.

AU - Davis, C.

AU - DeRose, J.

AU - Dodelson, S.

AU - Gatti, M.

AU - Hoyle, B.

AU - Huterer, D.

AU - Jarvis, M.

AU - Lacasa, F.

AU - Lemos, P.

AU - Peiris, H. V.

AU - Prat, J.

AU - Samuroff, S.

AU - Sánchez, C.

AU - Sheldon, E.

AU - Vielzeuf, P.

AU - Wang, M.

AU - Zuntz, J.

AU - Lahav, O.

AU - Abdalla, F. B.

AU - Allam, S.

AU - Annis, J.

AU - Avila, S.

AU - Bertin, E.

AU - Brooks, D.

AU - Burke, D. L.

AU - Carnero Rosell, A.

AU - Carrasco Kind, M.

AU - Carretero, J.

AU - Crocce, M.

AU - Cunha, C. E.

AU - D'Andrea, C. B.

AU - Da Costa, L. N.

AU - De Vicente, J.

AU - Diehl, H. T.

AU - Doel, P.

AU - Evrard, A. E.

AU - Flaugher, B.

AU - Fosalba, P.

AU - Frieman, J.

AU - García-Bellido, J.

AU - Gaztanaga, E.

AU - Gerdes, D. W.

AU - Gruendl, R. A.

AU - Gschwend, J.

AU - Gutierrez, G.

AU - Hartley, W. G.

AU - Hollowood, D. L.

AU - Honscheid, K.

AU - James, D. J.

AU - Kirk, D.

AU - Kuehn, K.

AU - Kuropatkin, N.

AU - Li, T. S.

AU - Lima, M.

AU - March, M.

AU - Menanteau, F.

AU - Miquel, R.

AU - Mohr, J. J.

AU - Ogando, R. L.C.

AU - Plazas, A. A.

AU - Roodman, A.

AU - Sanchez, E.

AU - Scarpine, V.

AU - Schindler, R.

AU - Sevilla-Noarbe, I.

AU - Smith, M.

AU - Soares-Santos, M.

AU - Sobreira, F.

AU - Suchyta, E.

AU - Swanson, M. E.C.

AU - Thomas, D.

AU - Walker, A. R.

AU - Wechsler, R. H.

PY - 2018/10/1

Y1 - 2018/10/1

N2 - We explore the impact of an update to the typical approximation for the shape noise term in the analytic covariance matrix for cosmic shear experiments that assumes the absence of survey boundary and mask effects. We present an exact expression for the number of galaxy pairs in this term based on the survey mask, which leads to more than a factor of three increase in the shape noise on the largest measured scales for the Kilo-Degree Survey (KiDS-450) real-space cosmic shear data. We compare the result of this analytic expression to several alternative methods for measuring the shape noise from the data and find excellent agreement. This update to the covariance resolves any internal model tension evidenced by the previously large cosmological best-fitting Χ2 for the KiDS-450 cosmic shear data. The best-fitting Χ2 is reduced from 161 to 121 for 118 degrees of freedom. We also apply a correction to how the multiplicative shear calibration uncertainty is included in the covariance. This change shifts the inferred amplitude of the correlation function to higher values. We find that this improves agreement of the KiDS-450 cosmic shear results with Dark Energy Survey Year 1 and Planck results.

AB - We explore the impact of an update to the typical approximation for the shape noise term in the analytic covariance matrix for cosmic shear experiments that assumes the absence of survey boundary and mask effects. We present an exact expression for the number of galaxy pairs in this term based on the survey mask, which leads to more than a factor of three increase in the shape noise on the largest measured scales for the Kilo-Degree Survey (KiDS-450) real-space cosmic shear data. We compare the result of this analytic expression to several alternative methods for measuring the shape noise from the data and find excellent agreement. This update to the covariance resolves any internal model tension evidenced by the previously large cosmological best-fitting Χ2 for the KiDS-450 cosmic shear data. The best-fitting Χ2 is reduced from 161 to 121 for 118 degrees of freedom. We also apply a correction to how the multiplicative shear calibration uncertainty is included in the covariance. This change shifts the inferred amplitude of the correlation function to higher values. We find that this improves agreement of the KiDS-450 cosmic shear results with Dark Energy Survey Year 1 and Planck results.

KW - Gravitational lensing: weak

KW - Methods: data analysis

KW - Methods: statistical

UR - http://www.scopus.com/inward/record.url?scp=85051517642&partnerID=8YFLogxK

U2 - 10.1093/mnras/sty1889

DO - 10.1093/mnras/sty1889

M3 - Article

AN - SCOPUS:85051517642

SN - 0035-8711

VL - 479

SP - 4998

EP - 5004

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 4

ER -

Survey geometry and the internal consistency of recent cosmic shear measurements

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