CMB lensing tomography with the DES Science Verification galaxies

T. Giannantonio; P. Fosalba; R. Cawthon; Y. Omori; M. Crocce; F. Elsner; B. Leistedt; S. Dodelson; A. Benoit-Lévy; E. Gaztañaga; G. Holder; H. V. Peiris; W. J. Percival; D. Kirk; A. H. Bauer; B. A. Benson; G. M. Bernstein; J. Carretero; T. M. Crawford; R. Crittenden; D. Huterer; B. Jain; E. Krause; C. L. Reichardt; A. J. Ross; G. Simard; B. Soergel; A. Stark; K. T. Story; J. D. Vieira; J. Weller; T. Abbott; F. B. Abdalla; S. Allam; R. Armstrong; M. Banerji; R. A. Bernstein; E. Bertin; D. Brooks; E. Buckley-Geer; D. L. Burke; D. Capozzi; J. E. Carlstrom; A. Carnero Rosell; M. Carrasco Kind; F. J. Castander; C. L. Chang; C. E. Cunha; L. N. da Costa; C. B. D'Andrea; D. L. DePoy; S. Desai; H. T. Diehl; J. P. Dietrich; P. Doel; T. F. Eifler; A. E. Evrard; A. Fausti Neto; E. Fernandez; D. A. Finley; B. Flaugher; J. Frieman; D. Gerdes; D. Gruen; R. A. Gruendl; G. Gutierrez; W. L. Holzapfel; K. Honscheid; D. J. James; K. Kuehn; N. Kuropatkin; O. Lahav; T. S. Li; M. Lima; M. March; J. L. Marshall; P. Martini; P. Melchior; R. Miquel; J. J. Mohr; R. C. Nichol; B. Nord; R. Ogando; A. A. Plazas; A. K. Romer; A. Roodman; E. S. Rykoff; M. Sako; B. R. Saliwanchik; E. Sanchez; M. Schubnell; I. Sevilla-Noarbe; R. C. Smith; M. Soares-Santos; F. Sobreira; E. Suchyta; M. E.C. Swanson; G. Tarle; J. Thaler; D. Thomas; V. Vikram; A. R. Walker; R. H. Wechsler; J. Zuntz

doi:10.1093/mnras/stv2678

CMB lensing tomography with the DES Science Verification galaxies

T. Giannantonio, P. Fosalba, R. Cawthon, Y. Omori, M. Crocce, F. Elsner, B. Leistedt, S. Dodelson, A. Benoit-Lévy, E. Gaztañaga, G. Holder, H. V. Peiris, W. J. Percival, D. Kirk, A. H. Bauer, B. A. Benson, G. M. Bernstein, J. Carretero, T. M. Crawford, R. CrittendenD. Huterer, B. Jain, E. Krause, C. L. Reichardt, A. J. Ross, G. Simard, B. Soergel, A. Stark, K. T. Story, J. D. Vieira, J. Weller, T. Abbott, F. B. Abdalla, S. Allam, R. Armstrong, M. Banerji, R. A. Bernstein, E. Bertin, D. Brooks, E. Buckley-Geer, D. L. Burke, D. Capozzi, J. E. Carlstrom, A. Carnero Rosell, M. Carrasco Kind, F. J. Castander, C. L. Chang, C. E. Cunha, L. N. da Costa, C. B. D'Andrea, D. L. DePoy, S. Desai, H. T. Diehl, J. P. Dietrich, P. Doel, T. F. Eifler, A. E. Evrard, A. Fausti Neto, E. Fernandez, D. A. Finley, B. Flaugher, J. Frieman, D. Gerdes, D. Gruen, R. A. Gruendl, G. Gutierrez, W. L. Holzapfel, K. Honscheid, D. J. James, K. Kuehn, N. Kuropatkin, O. Lahav, T. S. Li, M. Lima, M. March, J. L. Marshall, P. Martini, P. Melchior, R. Miquel, J. J. Mohr, R. C. Nichol, B. Nord, R. Ogando, A. A. Plazas, A. K. Romer, A. Roodman, E. S. Rykoff, M. Sako, B. R. Saliwanchik, E. Sanchez, M. Schubnell, I. Sevilla-Noarbe, R. C. Smith, M. Soares-Santos, F. Sobreira, E. Suchyta, M. E.C. Swanson, G. Tarle, J. Thaler, D. Thomas, V. Vikram, A. R. Walker, R. H. Wechsler, J. Zuntz

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

98 Scopus citations

Abstract

We measure the cross-correlation between the galaxy density in the Dark Energy Survey (DES) Science Verification data and the lensing of the cosmic microwave background (CMB) as reconstructed with the Planck satellite and the South Pole Telescope (SPT). When using the DES main galaxy sample over the full redshift range 0.2 < z_phot < 1.2, a cross-correlation signal is detected at 6σ and 4σ with SPT and Planck, respectively. We then divide the DES galaxies into five photometric redshift bins, finding significant (>2σ) detections in all bins. Comparing to the fiducial Planck cosmology, we find the redshift evolution of the signal matches expectations, although the amplitude is consistently lower than predicted across redshift bins. We test for possible systematics that could affect our result and find no evidence for significant contamination. Finally, we demonstrate how these measurements can be used to constrain the growth of structure across cosmic time. We find the data are fit by a model in which the amplitude of structure in the z < 1.2 universe is 0.73 ± 0.16 times as large as predicted in the A cold dark matter Planck cosmology, a 1.7σ deviation.

Original language	English
Pages (from-to)	3213-3244
Number of pages	32
Journal	Monthly Notices of the Royal Astronomical Society
Volume	456
Issue number	3
DOIs	https://doi.org/10.1093/mnras/stv2678
State	Published - Mar 1 2016
Externally published	Yes

Funding

TG thanks Anthony Challinor and George Efstathiou for comments on a draft version of this paper, and James Fergusson, Martin Kilbinger and Ariel Sánchez for useful discussions. TG acknowledges support from the Kavli Foundation, STFC grant ST/L000636/1, and from the Excellence Cluster 'Universe' of Garching, Germany, as well as the Institut de Ciències de l'Espai, IEEC-CSIC, Universitat Autònoma de Barcelona, for hospitality. PF acknowledges support from the Mare Nostrum supercomputer (BSC-CNS, http://www.bsc.es), grants AECT-2008-1-0009 to 2010-1-0007, Port d'Informació Científica (http://www.pic.es), and the Cosmo-HUB portal (cosmohub.pic.es), where the MICE simulations were run, stored, and distributed, respectively. PF is funded by MINECO, project ESP2013-48274-C3-1-P. FE, BL and HVP were partially supported by the European Research Council under the European Union's Seventh Framework Programme (PP7/2007-2013) / ERC grant agreement no. 306478-CosmicDawn. CR acknowledges support from the University of Melbourne and from the Australian Research Council's Discovery Projects scheme (DP150103208). This paper has gone through internal review by the DES collaboration. We are grateful for the extraordinary contributions of our CTIO colleagues and the DECam Construction, Commissioning and SV teams in achieving the excellent instrument and telescope conditions that have made this work possible. The success of this project also relies critically on the expertise and dedication of the DES Data Management group. Funding for the DES Projects has been provided by the US Department of Energy, the US 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, Fundação 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 Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the DES. The DES data management system is supported by the National Science Foundation under Grant Number AST-1138766. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Enérgeticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l'Espai (IEEC/CSIC), the Institut de Física d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. The SPT programme is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation through Grant GBMF#947 to the University of Chicago.

Funders	Funder number
Centro de Excelencia Severo Ochoa	SEV-2012-0234
Collaborating Institutions are Argonne National Laboratory
Institut de Ciències de l'Espai
Mare Nostrum supercomputer	AECT-2008-1-0009
Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University
NSF Physics Frontier Center	PHY-0114422
Port d'Informació Científica
Science and Technology Facilities Council of the United Kingdom
National Science Foundation	1248097, 1138766, AST-1138766, 1125897, 1311924, 1536171
U.S. Department of Energy
Gordon and Betty Moore Foundation	GBMF#947
Kavli Foundation
University of Illinois at Urbana-Champaign
Stanford University
Fermilab
Lawrence Berkeley National Laboratory
University of California, Santa Cruz
University of Pennsylvania
Ohio State University
University of Chicago
University of Michigan
Texas A and M University	FPA2013-47986, AYA2012-39559, ESP2013-48274
University of Portsmouth
National Centre for Supercomputing Applications
Seventh Framework Programme	PLR-1248097, 240672, 306478, 291329
SLAC National Accelerator Laboratory
Higher Education Funding Council for England
Science and Technology Facilities Council	ST/L000636/1
University College London
European Research Council
University of Nottingham
University of Sussex
University of Edinburgh
Australian Research Council	DP150103208
Deutsche Forschungsgemeinschaft
University of Melbourne
Eidgenössische Technische Hochschule Zürich
Ministerio de Economía y Competitividad	ESP2013-48274-C3-1-P
Ministério da Ciência, Tecnologia e Inovação
Conselho Nacional de Desenvolvimento Científico e Tecnológico
Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro
Financiadora de Estudos e Projetos
Seventh Framework Programme
Ludwig-Maximilians-Universität München
Ministry of Education and Science of Ukraine
Institut de Física d'Altes Energies

Keywords

Cosmic background radiation
Gravitational lensing: Weak
Large-scale structure of Universe

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10.1093/mnras/stv2678

Cite this

Giannantonio, T., Fosalba, P., Cawthon, R., Omori, Y., Crocce, M., Elsner, F., Leistedt, B., Dodelson, S., Benoit-Lévy, A., Gaztañaga, E., Holder, G., Peiris, H. V., Percival, W. J., Kirk, D., Bauer, A. H., Benson, B. A., Bernstein, G. M., Carretero, J., Crawford, T. M., ... Zuntz, J. (2016). CMB lensing tomography with the DES Science Verification galaxies. Monthly Notices of the Royal Astronomical Society, 456(3), 3213-3244. https://doi.org/10.1093/mnras/stv2678

@article{01933b2239944387b38e73d71bf0911a,

title = "CMB lensing tomography with the DES Science Verification galaxies",

abstract = "We measure the cross-correlation between the galaxy density in the Dark Energy Survey (DES) Science Verification data and the lensing of the cosmic microwave background (CMB) as reconstructed with the Planck satellite and the South Pole Telescope (SPT). When using the DES main galaxy sample over the full redshift range 0.2 < zphot < 1.2, a cross-correlation signal is detected at 6σ and 4σ with SPT and Planck, respectively. We then divide the DES galaxies into five photometric redshift bins, finding significant (>2σ) detections in all bins. Comparing to the fiducial Planck cosmology, we find the redshift evolution of the signal matches expectations, although the amplitude is consistently lower than predicted across redshift bins. We test for possible systematics that could affect our result and find no evidence for significant contamination. Finally, we demonstrate how these measurements can be used to constrain the growth of structure across cosmic time. We find the data are fit by a model in which the amplitude of structure in the z < 1.2 universe is 0.73 ± 0.16 times as large as predicted in the A cold dark matter Planck cosmology, a 1.7σ deviation.",

keywords = "Cosmic background radiation, Gravitational lensing: Weak, Large-scale structure of Universe",

author = "T. Giannantonio and P. Fosalba and R. Cawthon and Y. Omori and M. Crocce and F. Elsner and B. Leistedt and S. Dodelson and A. Benoit-L{\'e}vy and E. Gazta{\~n}aga and G. Holder and Peiris, {H. V.} and Percival, {W. J.} and D. Kirk and Bauer, {A. H.} and Benson, {B. A.} and Bernstein, {G. M.} and J. Carretero and Crawford, {T. M.} and R. Crittenden and D. Huterer and B. Jain and E. Krause and Reichardt, {C. L.} and Ross, {A. J.} and G. Simard and B. Soergel and A. Stark and Story, {K. T.} and Vieira, {J. D.} and J. Weller and T. Abbott and Abdalla, {F. B.} and S. Allam and R. Armstrong and M. Banerji and Bernstein, {R. A.} and E. Bertin and D. Brooks and E. Buckley-Geer and Burke, {D. L.} and D. Capozzi and Carlstrom, {J. E.} and {Carnero Rosell}, A. and {Carrasco Kind}, M. and Castander, {F. J.} and Chang, {C. L.} and Cunha, {C. E.} and {da Costa}, {L. N.} and D'Andrea, {C. B.} and DePoy, {D. L.} and S. Desai and Diehl, {H. T.} and Dietrich, {J. P.} and P. Doel and Eifler, {T. F.} and Evrard, {A. E.} and {Fausti Neto}, A. and E. Fernandez and Finley, {D. A.} and B. Flaugher and J. Frieman and D. Gerdes and D. Gruen and Gruendl, {R. A.} and G. Gutierrez and Holzapfel, {W. L.} and K. Honscheid and James, {D. J.} and K. Kuehn and N. Kuropatkin and O. Lahav and Li, {T. S.} and M. Lima and M. March and Marshall, {J. L.} and P. Martini and P. Melchior and R. Miquel and Mohr, {J. J.} and Nichol, {R. C.} and B. Nord and R. Ogando and Plazas, {A. A.} and Romer, {A. K.} and A. Roodman and Rykoff, {E. S.} and M. Sako and Saliwanchik, {B. R.} and E. Sanchez and M. Schubnell and I. Sevilla-Noarbe and Smith, {R. C.} and M. Soares-Santos and F. Sobreira and E. Suchyta and Swanson, {M. E.C.} and G. Tarle and J. Thaler and D. Thomas and V. Vikram and Walker, {A. R.} and Wechsler, {R. H.} and J. Zuntz",

note = "Publisher Copyright: {\textcopyright} 2016 The Authors.",

year = "2016",

month = mar,

day = "1",

doi = "10.1093/mnras/stv2678",

language = "English",

volume = "456",

pages = "3213--3244",

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

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Giannantonio, T, Fosalba, P, Cawthon, R, Omori, Y, Crocce, M, Elsner, F, Leistedt, B, Dodelson, S, Benoit-Lévy, A, Gaztañaga, E, Holder, G, Peiris, HV, Percival, WJ, Kirk, D, Bauer, AH, Benson, BA, Bernstein, GM, Carretero, J, Crawford, TM, Crittenden, R, Huterer, D, Jain, B, Krause, E, Reichardt, CL, Ross, AJ, Simard, G, Soergel, B, Stark, A, Story, KT, Vieira, JD, Weller, J, Abbott, T, Abdalla, FB, Allam, S, Armstrong, R, Banerji, M, Bernstein, RA, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Capozzi, D, Carlstrom, JE, Carnero Rosell, A, Carrasco Kind, M, Castander, FJ, Chang, CL, Cunha, CE, da Costa, LN, D'Andrea, CB, DePoy, DL, Desai, S, Diehl, HT, Dietrich, JP, Doel, P, Eifler, TF, Evrard, AE, Fausti Neto, A, Fernandez, E, Finley, DA, Flaugher, B, Frieman, J, Gerdes, D, Gruen, D, Gruendl, RA, Gutierrez, G, Holzapfel, WL, Honscheid, K, James, DJ, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Lima, M, March, M, Marshall, JL, Martini, P, Melchior, P, Miquel, R, Mohr, JJ, Nichol, RC, Nord, B, Ogando, R, Plazas, AA, Romer, AK, Roodman, A, Rykoff, ES, Sako, M, Saliwanchik, BR, Sanchez, E, Schubnell, M, Sevilla-Noarbe, I, Smith, RC, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Thaler, J, Thomas, D, Vikram, V, Walker, AR, Wechsler, RH & Zuntz, J 2016, 'CMB lensing tomography with the DES Science Verification galaxies', Monthly Notices of the Royal Astronomical Society, vol. 456, no. 3, pp. 3213-3244. https://doi.org/10.1093/mnras/stv2678

TY - JOUR

T1 - CMB lensing tomography with the DES Science Verification galaxies

AU - Giannantonio, T.

AU - Fosalba, P.

AU - Cawthon, R.

AU - Omori, Y.

AU - Crocce, M.

AU - Elsner, F.

AU - Leistedt, B.

AU - Dodelson, S.

AU - Benoit-Lévy, A.

AU - Gaztañaga, E.

AU - Holder, G.

AU - Peiris, H. V.

AU - Percival, W. J.

AU - Kirk, D.

AU - Bauer, A. H.

AU - Benson, B. A.

AU - Bernstein, G. M.

AU - Carretero, J.

AU - Crawford, T. M.

AU - Crittenden, R.

AU - Huterer, D.

AU - Jain, B.

AU - Krause, E.

AU - Reichardt, C. L.

AU - Ross, A. J.

AU - Simard, G.

AU - Soergel, B.

AU - Stark, A.

AU - Story, K. T.

AU - Vieira, J. D.

AU - Weller, J.

AU - Abbott, T.

AU - Abdalla, F. B.

AU - Allam, S.

AU - Armstrong, R.

AU - Banerji, M.

AU - Bernstein, R. A.

AU - Bertin, E.

AU - Brooks, D.

AU - Buckley-Geer, E.

AU - Burke, D. L.

AU - Capozzi, D.

AU - Carlstrom, J. E.

AU - Carnero Rosell, A.

AU - Carrasco Kind, M.

AU - Castander, F. J.

AU - Chang, C. L.

AU - Cunha, C. E.

AU - da Costa, L. N.

AU - D'Andrea, C. B.

AU - DePoy, D. L.

AU - Desai, S.

AU - Diehl, H. T.

AU - Dietrich, J. P.

AU - Doel, P.

AU - Eifler, T. F.

AU - Evrard, A. E.

AU - Fausti Neto, A.

AU - Fernandez, E.

AU - Finley, D. A.

AU - Flaugher, B.

AU - Frieman, J.

AU - Gerdes, D.

AU - Gruen, D.

AU - Gruendl, R. A.

AU - Gutierrez, G.

AU - Holzapfel, W. L.

AU - Honscheid, K.

AU - James, D. J.

AU - Kuehn, K.

AU - Kuropatkin, N.

AU - Lahav, O.

AU - Li, T. S.

AU - Lima, M.

AU - March, M.

AU - Marshall, J. L.

AU - Martini, P.

AU - Melchior, P.

AU - Miquel, R.

AU - Mohr, J. J.

AU - Nichol, R. C.

AU - Nord, B.

AU - Ogando, R.

AU - Plazas, A. A.

AU - Romer, A. K.

AU - Roodman, A.

AU - Rykoff, E. S.

AU - Sako, M.

AU - Saliwanchik, B. R.

AU - Sanchez, E.

AU - Schubnell, M.

AU - Sevilla-Noarbe, I.

AU - Smith, R. C.

AU - Soares-Santos, M.

AU - Sobreira, F.

AU - Suchyta, E.

AU - Swanson, M. E.C.

AU - Tarle, G.

AU - Thaler, J.

AU - Thomas, D.

AU - Vikram, V.

AU - Walker, A. R.

AU - Wechsler, R. H.

AU - Zuntz, J.

PY - 2016/3/1

Y1 - 2016/3/1

N2 - We measure the cross-correlation between the galaxy density in the Dark Energy Survey (DES) Science Verification data and the lensing of the cosmic microwave background (CMB) as reconstructed with the Planck satellite and the South Pole Telescope (SPT). When using the DES main galaxy sample over the full redshift range 0.2 < zphot < 1.2, a cross-correlation signal is detected at 6σ and 4σ with SPT and Planck, respectively. We then divide the DES galaxies into five photometric redshift bins, finding significant (>2σ) detections in all bins. Comparing to the fiducial Planck cosmology, we find the redshift evolution of the signal matches expectations, although the amplitude is consistently lower than predicted across redshift bins. We test for possible systematics that could affect our result and find no evidence for significant contamination. Finally, we demonstrate how these measurements can be used to constrain the growth of structure across cosmic time. We find the data are fit by a model in which the amplitude of structure in the z < 1.2 universe is 0.73 ± 0.16 times as large as predicted in the A cold dark matter Planck cosmology, a 1.7σ deviation.

AB - We measure the cross-correlation between the galaxy density in the Dark Energy Survey (DES) Science Verification data and the lensing of the cosmic microwave background (CMB) as reconstructed with the Planck satellite and the South Pole Telescope (SPT). When using the DES main galaxy sample over the full redshift range 0.2 < zphot < 1.2, a cross-correlation signal is detected at 6σ and 4σ with SPT and Planck, respectively. We then divide the DES galaxies into five photometric redshift bins, finding significant (>2σ) detections in all bins. Comparing to the fiducial Planck cosmology, we find the redshift evolution of the signal matches expectations, although the amplitude is consistently lower than predicted across redshift bins. We test for possible systematics that could affect our result and find no evidence for significant contamination. Finally, we demonstrate how these measurements can be used to constrain the growth of structure across cosmic time. We find the data are fit by a model in which the amplitude of structure in the z < 1.2 universe is 0.73 ± 0.16 times as large as predicted in the A cold dark matter Planck cosmology, a 1.7σ deviation.

KW - Cosmic background radiation

KW - Gravitational lensing: Weak

KW - Large-scale structure of Universe

UR - http://www.scopus.com/inward/record.url?scp=84969913853&partnerID=8YFLogxK

U2 - 10.1093/mnras/stv2678

DO - 10.1093/mnras/stv2678

M3 - Article

AN - SCOPUS:84969913853

SN - 0035-8711

VL - 456

SP - 3213

EP - 3244

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

CMB lensing tomography with the DES Science Verification galaxies

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