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

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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 (US)
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

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

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

Access to Document

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{1943a4c067bc40058882130ce8d108ca,

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 (US)",

volume = "456",

pages = "3213--3244",

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

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

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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

UR - http://www.scopus.com/inward/citedby.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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