Cross-correlation of gravitational lensing from DES Science Verification data with SPT and Planck lensing

D. Kirk; Y. Omori; A. Benoit-Lévy; R. Cawthon; C. Chang; P. Larsen; A. Amara; D. Bacon; T. M. Crawford; S. Dodelson; P. Fosalba; T. Giannantonio; G. Holder; B. Jain; T. Kacprzak; O. Lahav; N. MacCrann; A. Nicola; A. Refregier; E. Sheldon; K. T. Story; M. A. Troxel; J. D. Vieira; V. Vikram; J. Zuntz; T. M.C. Abbott; F. B. Abdalla; M. R. Becker; B. A. Benson; G. M. Bernstein; R. A. Bernstein; L. E. Bleem; C. Bonnett; S. L. Bridle; D. Brooks; E. Buckley-Geer; D. L. Burke; D. Capozzi; J. E. Carlstrom; A. Carnero Rosell; M. Carrasco Kind; J. Carretero; M. Crocce; C. E. Cunha; C. B. D'Andrea; L. N. Da Costa; S. Desai; H. T. Diehl; J. P. Dietrich; P. Doel; T. F. Eifler; A. E. Evrard; B. Flaugher; J. Frieman; D. W. Gerdes; D. A. Goldstein; D. Gruen; R. A. Gruendl; K. Honscheid; D. J. James; M. Jarvis; S. Kent; K. Kuehn; N. Kuropatkin; M. Lima; M. March; P. Martini; P. Melchior; C. J. Miller; R. Miquel; R. C. Nichol; R. Ogando; A. A. Plazas; C. L. Reichardt; A. Roodman; E. Rozo; E. S. Rykoff; M. Sako; E. Sanchez; V. Scarpine; M. Schubnell; I. Sevilla-Noarbe; G. Simard; R. C. Smith; M. Soares-Santos; F. Sobreira; E. Suchyta; M. E.C. Swanson; G. Tarle; D. Thomas; R. H. Wechsler; J. Weller

doi:10.1093/mnras/stw570

Cross-correlation of gravitational lensing from DES Science Verification data with SPT and Planck lensing

D. Kirk, Y. Omori, A. Benoit-Lévy, R. Cawthon, C. Chang, P. Larsen, A. Amara, D. Bacon, T. M. Crawford, S. Dodelson, P. Fosalba, T. Giannantonio, G. Holder, B. Jain, T. Kacprzak, O. Lahav, N. MacCrann, A. Nicola, A. Refregier, E. SheldonK. T. Story, M. A. Troxel, J. D. Vieira, V. Vikram, J. Zuntz, T. M.C. Abbott, F. B. Abdalla, M. R. Becker, B. A. Benson, G. M. Bernstein, R. A. Bernstein, L. E. Bleem, C. Bonnett, S. L. Bridle, D. Brooks, E. Buckley-Geer, D. L. Burke, D. Capozzi, J. E. Carlstrom, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Crocce, C. E. Cunha, C. B. D'Andrea, L. N. Da Costa, S. Desai, H. T. Diehl, J. P. Dietrich, P. Doel, T. F. Eifler, A. E. Evrard, B. Flaugher, J. Frieman, D. W. Gerdes, D. A. Goldstein, D. Gruen, R. A. Gruendl, K. Honscheid, D. J. James, M. Jarvis, S. Kent, K. Kuehn, N. Kuropatkin, M. Lima, M. March, P. Martini, P. Melchior, C. J. Miller, R. Miquel, R. C. Nichol, R. Ogando, A. A. Plazas, C. L. Reichardt, A. Roodman, E. Rozo, E. S. Rykoff, M. Sako, E. Sanchez, V. Scarpine, M. Schubnell, I. Sevilla-Noarbe, G. Simard, R. C. Smith, M. Soares-Santos, F. Sobreira, E. Suchyta, M. E.C. Swanson, G. Tarle, D. Thomas, R. H. Wechsler, J. Weller

Workflow Systems

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

51 Scopus citations

Abstract

We measure the cross-correlation between weak lensing of galaxy images and of the cosmic microwave background (CMB). The effects of gravitational lensing on different sources will be correlated if the lensing is caused by the same mass fluctuations. We use galaxy shape measurements from 139 deg² of the Dark Energy Survey (DES) Science Verification data and overlapping CMB lensing from the South Pole Telescope (SPT) and Planck. The DES source galaxies have a median redshift of z_med ~ 0.7, while the CMB lensing kernel is broad and peaks at z ~ 2. The resulting cross-correlation is maximally sensitive to mass fluctuations at z ~ 0.44. Assuming the Planck 2015 best-fitting cosmology, the amplitude of the DES×SPT cross-power is found to be A_SPT = 0.88 ± 0.30 and that from DES×Planck to be A_Planck = 0.86 ± 0.39, where A = 1 corresponds to the theoretical prediction. These are consistent with the expected signal and correspond to significances of 2.9σ and 2.2σ, respectively. We demonstrate that our results are robust to a number of important systematic effects including the shear measurement method, estimator choice, photo-z uncertainty and CMB lensing systematics. We calculate a value of A = 1.08 ± 0.36 for DES×SPT when we correct the observations with a simple intrinsic alignment model. With three measurements of this cross-correlation now existing in the literature, there is not yet reliable evidence for any deviation from the expected LCDM level of cross-correlation. We provide forecasts for the expected signal-to-noise ratio of the combination of the five-year DES survey and SPT-3G.

Original language	English
Pages (from-to)	21-34
Number of pages	14
Journal	Monthly Notices of the Royal Astronomical Society
Volume	459
Issue number	1
DOIs	https://doi.org/10.1093/mnras/stw570
State	Published - Jun 11 2016

Funding

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 U.S. Department of Energy, the U.S. National Science Foundation, theMinistry of Science and Education of Spain, the Science and Technology FacilitiesCouncil of theUnitedKingdom, theHigher Education Funding Council for England, the NationalCenter 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, Funda\u00E7\u00E3o Carlos Chagas Filho de Amparo `a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cient\u00EDfico e Tecnol\u00F3gico and the Minist\u00E9rio da Ci\u00EAncia, Tecnologia e Inova\u00E7\u00E3o, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the DES. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energ\u00E9ticas, Medioambientales y Tecnol\u00F3gicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgen\u00F6ssische Technische Hochschule (ETH) Z\u00FCrich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ci`encies de l'Espai (IEEC/CSIC), the Institut de F\u00EDsica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universit \u00E4t M\u00FCnchen 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 data management system is supported by the National Science Foundation under Grant Number AST-1138766. 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. This research used resources of the Calcul Quebec computing consortium, part of the Compute Canada network. The SPT programme is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by theNSF Physics Frontier Center grant PHY-0114422 to theKavli 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. OL acknowledges support from a European Research Council Advanced Grant FP7/291329, which also supported DK. ABL thanks CNES for financial support through its post-doctoral programme. PL is funded jointly by the Royal Society ofNewZealand Rutherford Foundation Trust and the Cambridge Commonwealth Trust. CR acknowledges support from the University of Melbourne. ES is supported by DOE grant DE-AC02-98CH10886.

Keywords

Cosmic background radiation
Gravitational lensing: weak
Methods: data analysis

Access to Document

10.1093/mnras/stw570

Cite this

Kirk, D., Omori, Y., Benoit-Lévy, A., Cawthon, R., Chang, C., Larsen, P., Amara, A., Bacon, D., Crawford, T. M., Dodelson, S., Fosalba, P., Giannantonio, T., Holder, G., Jain, B., Kacprzak, T., Lahav, O., MacCrann, N., Nicola, A., Refregier, A., ... Weller, J. (2016). Cross-correlation of gravitational lensing from DES Science Verification data with SPT and Planck lensing. Monthly Notices of the Royal Astronomical Society, 459(1), 21-34. https://doi.org/10.1093/mnras/stw570

@article{d826ee6415d54234ae6231ab3f5f1c17,

title = "Cross-correlation of gravitational lensing from DES Science Verification data with SPT and Planck lensing",

abstract = "We measure the cross-correlation between weak lensing of galaxy images and of the cosmic microwave background (CMB). The effects of gravitational lensing on different sources will be correlated if the lensing is caused by the same mass fluctuations. We use galaxy shape measurements from 139 deg2 of the Dark Energy Survey (DES) Science Verification data and overlapping CMB lensing from the South Pole Telescope (SPT) and Planck. The DES source galaxies have a median redshift of zmed ~ 0.7, while the CMB lensing kernel is broad and peaks at z ~ 2. The resulting cross-correlation is maximally sensitive to mass fluctuations at z ~ 0.44. Assuming the Planck 2015 best-fitting cosmology, the amplitude of the DES×SPT cross-power is found to be ASPT = 0.88 ± 0.30 and that from DES×Planck to be APlanck = 0.86 ± 0.39, where A = 1 corresponds to the theoretical prediction. These are consistent with the expected signal and correspond to significances of 2.9σ and 2.2σ, respectively. We demonstrate that our results are robust to a number of important systematic effects including the shear measurement method, estimator choice, photo-z uncertainty and CMB lensing systematics. We calculate a value of A = 1.08 ± 0.36 for DES×SPT when we correct the observations with a simple intrinsic alignment model. With three measurements of this cross-correlation now existing in the literature, there is not yet reliable evidence for any deviation from the expected LCDM level of cross-correlation. We provide forecasts for the expected signal-to-noise ratio of the combination of the five-year DES survey and SPT-3G.",

keywords = "Cosmic background radiation, Gravitational lensing: weak, Methods: data analysis",

author = "D. Kirk and Y. Omori and A. Benoit-L{\'e}vy and R. Cawthon and C. Chang and P. Larsen and A. Amara and D. Bacon and Crawford, {T. M.} and S. Dodelson and P. Fosalba and T. Giannantonio and G. Holder and B. Jain and T. Kacprzak and O. Lahav and N. MacCrann and A. Nicola and A. Refregier and E. Sheldon and Story, {K. T.} and Troxel, {M. A.} and Vieira, {J. D.} and V. Vikram and J. Zuntz and Abbott, {T. M.C.} and Abdalla, {F. B.} and Becker, {M. R.} and Benson, {B. A.} and Bernstein, {G. M.} and Bernstein, {R. A.} and Bleem, {L. E.} and C. Bonnett and Bridle, {S. L.} 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 J. Carretero and M. Crocce and Cunha, {C. E.} and D'Andrea, {C. B.} and {Da Costa}, {L. N.} and S. Desai and Diehl, {H. T.} and Dietrich, {J. P.} and P. Doel and Eifler, {T. F.} and Evrard, {A. E.} and B. Flaugher and J. Frieman and Gerdes, {D. W.} and Goldstein, {D. A.} and D. Gruen and Gruendl, {R. A.} and K. Honscheid and James, {D. J.} and M. Jarvis and S. Kent and K. Kuehn and N. Kuropatkin and M. Lima and M. March and P. Martini and P. Melchior and Miller, {C. J.} and R. Miquel and Nichol, {R. C.} and R. Ogando and Plazas, {A. A.} and Reichardt, {C. L.} and A. Roodman and E. Rozo and Rykoff, {E. S.} and M. Sako and E. Sanchez and V. Scarpine and M. Schubnell and I. Sevilla-Noarbe and G. Simard and Smith, {R. C.} and M. Soares-Santos and F. Sobreira and E. Suchyta and Swanson, {M. E.C.} and G. Tarle and D. Thomas and Wechsler, {R. H.} and J. Weller",

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

year = "2016",

month = jun,

day = "11",

doi = "10.1093/mnras/stw570",

language = "English",

volume = "459",

pages = "21--34",

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

issn = "0035-8711",

publisher = "Oxford University Press",

number = "1",

}

Kirk, D, Omori, Y, Benoit-Lévy, A, Cawthon, R, Chang, C, Larsen, P, Amara, A, Bacon, D, Crawford, TM, Dodelson, S, Fosalba, P, Giannantonio, T, Holder, G, Jain, B, Kacprzak, T, Lahav, O, MacCrann, N, Nicola, A, Refregier, A, Sheldon, E, Story, KT, Troxel, MA, Vieira, JD, Vikram, V, Zuntz, J, Abbott, TMC, Abdalla, FB, Becker, MR, Benson, BA, Bernstein, GM, Bernstein, RA, Bleem, LE, Bonnett, C, Bridle, SL, Brooks, D, Buckley-Geer, E, Burke, DL, Capozzi, D, Carlstrom, JE, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Crocce, M, Cunha, CE, D'Andrea, CB, Da Costa, LN, Desai, S, Diehl, HT, Dietrich, JP, Doel, P, Eifler, TF, Evrard, AE, Flaugher, B, Frieman, J, Gerdes, DW, Goldstein, DA, Gruen, D, Gruendl, RA, Honscheid, K, James, DJ, Jarvis, M, Kent, S, Kuehn, K, Kuropatkin, N, Lima, M, March, M, Martini, P, Melchior, P, Miller, CJ, Miquel, R, Nichol, RC, Ogando, R, Plazas, AA, Reichardt, CL, Roodman, A, Rozo, E, Rykoff, ES, Sako, M, Sanchez, E, Scarpine, V, Schubnell, M, Sevilla-Noarbe, I, Simard, G, Smith, RC, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Wechsler, RH & Weller, J 2016, 'Cross-correlation of gravitational lensing from DES Science Verification data with SPT and Planck lensing', Monthly Notices of the Royal Astronomical Society, vol. 459, no. 1, pp. 21-34. https://doi.org/10.1093/mnras/stw570

TY - JOUR

T1 - Cross-correlation of gravitational lensing from DES Science Verification data with SPT and Planck lensing

AU - Kirk, D.

AU - Omori, Y.

AU - Benoit-Lévy, A.

AU - Cawthon, R.

AU - Chang, C.

AU - Larsen, P.

AU - Amara, A.

AU - Bacon, D.

AU - Crawford, T. M.

AU - Dodelson, S.

AU - Fosalba, P.

AU - Giannantonio, T.

AU - Holder, G.

AU - Jain, B.

AU - Kacprzak, T.

AU - Lahav, O.

AU - MacCrann, N.

AU - Nicola, A.

AU - Refregier, A.

AU - Sheldon, E.

AU - Story, K. T.

AU - Troxel, M. A.

AU - Vieira, J. D.

AU - Vikram, V.

AU - Zuntz, J.

AU - Abbott, T. M.C.

AU - Abdalla, F. B.

AU - Becker, M. R.

AU - Benson, B. A.

AU - Bernstein, G. M.

AU - Bernstein, R. A.

AU - Bleem, L. E.

AU - Bonnett, C.

AU - Bridle, S. L.

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 - Carretero, J.

AU - Crocce, M.

AU - Cunha, C. E.

AU - D'Andrea, C. B.

AU - Da Costa, L. N.

AU - Desai, S.

AU - Diehl, H. T.

AU - Dietrich, J. P.

AU - Doel, P.

AU - Eifler, T. F.

AU - Evrard, A. E.

AU - Flaugher, B.

AU - Frieman, J.

AU - Gerdes, D. W.

AU - Goldstein, D. A.

AU - Gruen, D.

AU - Gruendl, R. A.

AU - Honscheid, K.

AU - James, D. J.

AU - Jarvis, M.

AU - Kent, S.

AU - Kuehn, K.

AU - Kuropatkin, N.

AU - Lima, M.

AU - March, M.

AU - Martini, P.

AU - Melchior, P.

AU - Miller, C. J.

AU - Miquel, R.

AU - Nichol, R. C.

AU - Ogando, R.

AU - Plazas, A. A.

AU - Reichardt, C. L.

AU - Roodman, A.

AU - Rozo, E.

AU - Rykoff, E. S.

AU - Sako, M.

AU - Sanchez, E.

AU - Scarpine, V.

AU - Schubnell, M.

AU - Sevilla-Noarbe, I.

AU - Simard, G.

AU - Smith, R. C.

AU - Soares-Santos, M.

AU - Sobreira, F.

AU - Suchyta, E.

AU - Swanson, M. E.C.

AU - Tarle, G.

AU - Thomas, D.

AU - Wechsler, R. H.

AU - Weller, J.

PY - 2016/6/11

Y1 - 2016/6/11

N2 - We measure the cross-correlation between weak lensing of galaxy images and of the cosmic microwave background (CMB). The effects of gravitational lensing on different sources will be correlated if the lensing is caused by the same mass fluctuations. We use galaxy shape measurements from 139 deg2 of the Dark Energy Survey (DES) Science Verification data and overlapping CMB lensing from the South Pole Telescope (SPT) and Planck. The DES source galaxies have a median redshift of zmed ~ 0.7, while the CMB lensing kernel is broad and peaks at z ~ 2. The resulting cross-correlation is maximally sensitive to mass fluctuations at z ~ 0.44. Assuming the Planck 2015 best-fitting cosmology, the amplitude of the DES×SPT cross-power is found to be ASPT = 0.88 ± 0.30 and that from DES×Planck to be APlanck = 0.86 ± 0.39, where A = 1 corresponds to the theoretical prediction. These are consistent with the expected signal and correspond to significances of 2.9σ and 2.2σ, respectively. We demonstrate that our results are robust to a number of important systematic effects including the shear measurement method, estimator choice, photo-z uncertainty and CMB lensing systematics. We calculate a value of A = 1.08 ± 0.36 for DES×SPT when we correct the observations with a simple intrinsic alignment model. With three measurements of this cross-correlation now existing in the literature, there is not yet reliable evidence for any deviation from the expected LCDM level of cross-correlation. We provide forecasts for the expected signal-to-noise ratio of the combination of the five-year DES survey and SPT-3G.

AB - We measure the cross-correlation between weak lensing of galaxy images and of the cosmic microwave background (CMB). The effects of gravitational lensing on different sources will be correlated if the lensing is caused by the same mass fluctuations. We use galaxy shape measurements from 139 deg2 of the Dark Energy Survey (DES) Science Verification data and overlapping CMB lensing from the South Pole Telescope (SPT) and Planck. The DES source galaxies have a median redshift of zmed ~ 0.7, while the CMB lensing kernel is broad and peaks at z ~ 2. The resulting cross-correlation is maximally sensitive to mass fluctuations at z ~ 0.44. Assuming the Planck 2015 best-fitting cosmology, the amplitude of the DES×SPT cross-power is found to be ASPT = 0.88 ± 0.30 and that from DES×Planck to be APlanck = 0.86 ± 0.39, where A = 1 corresponds to the theoretical prediction. These are consistent with the expected signal and correspond to significances of 2.9σ and 2.2σ, respectively. We demonstrate that our results are robust to a number of important systematic effects including the shear measurement method, estimator choice, photo-z uncertainty and CMB lensing systematics. We calculate a value of A = 1.08 ± 0.36 for DES×SPT when we correct the observations with a simple intrinsic alignment model. With three measurements of this cross-correlation now existing in the literature, there is not yet reliable evidence for any deviation from the expected LCDM level of cross-correlation. We provide forecasts for the expected signal-to-noise ratio of the combination of the five-year DES survey and SPT-3G.

KW - Cosmic background radiation

KW - Gravitational lensing: weak

KW - Methods: data analysis

UR - http://www.scopus.com/inward/record.url?scp=84970046143&partnerID=8YFLogxK

U2 - 10.1093/mnras/stw570

DO - 10.1093/mnras/stw570

M3 - Article

AN - SCOPUS:84970046143

SN - 0035-8711

VL - 459

SP - 21

EP - 34

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 1

ER -

Cross-correlation of gravitational lensing from DES Science Verification data with SPT and Planck lensing

Abstract

Funding

Keywords

Access to Document

Other files and links

Fingerprint

Cite this