Measurement of gravitational lensing of the cosmic microwave background using SPT-3G 2018 data
Creators
-
Pan, Z.
-
Bianchini, F.
-
Wu, W. L. K.
-
Ade, P. A. R.
- Ahmed, Z.
- Anderes, E.
-
Anderson, A. J.
-
Ansarinejad, B.
-
Archipley, M.
- Aylor, K.
-
Balkenhol, L.
- Barry, P. S.
-
Basu Thakur, R.
- Benabed, K.
-
Bender, A. N.
-
Benson, B. A.
-
Bleem, L. E.
-
Bouchet, F. R.
- Bryant, L.
- Byrum, K.
-
Camphuis, E.
-
Carlstrom, J. E.
- Carter, F. W.
-
Cecil, T. W.
- Chang, C. L.
- Chaubal, P.
- Chen, G.
-
Chichura, P. M.
- Cho, H.-M.
- Chou, T.-L.
-
Cliche, J.-F.
-
Coerver, A.
-
Crawford, T. M.
-
Cukierman, A.
-
Daley, C.
- de Haan, T.
- Denison, E. V.
-
Dibert, K. R.
- Ding, J.
- Dobbs, M. A.
-
Doussot, A.
-
Dutcher, D.
- Everett, W.
- Feng, C.
-
Ferguson, K. R.
- Fichman, K.
-
Foster, A.
- Fu, J.
- Galli, S.
- Gambrel, A. E.
- Gardner, R. W.
- Ge, F.
- Goeckner-Wald, N.
-
Gualtieri, R.
-
Guidi, F.
-
Guns, S.
-
Gupta, N.
-
Halverson, N. W.
- Harke-Hosemann, A. H.
- Harrington, N. L.
- Henning, J. W.
- Hilton, G. C.
-
Hivon, E.
-
Holder, G. P.
-
Holzapfel, W. L.
-
Hood, J. C.
- Howe, D.
- Huang, N.
- Irwin, K. D.
- Jeong, O.
- Jonas, M.
- Jones, A.
-
Kéruzoré, F.
-
Khaire, T. S.
- Knox, L.
-
Kofman, A. M.
- Korman, M.
- Kubik, D. L.
- Kuhlmann, S.
- Kuo, C.-L.
- Lee, A. T.
- Leitch, E. M.
- Levy, K.
-
Lowitz, A. E.
- Lu, C.
- Maniyar, A.
- Menanteau, F.
- Meyer, S. S.
- Michalik, D.
-
Millea, M.
- Montgomery, J.
- Nadolski, A.
- Nakato, Y.
-
Natoli, T.
- Nguyen, H.
-
Noble, G. I.
-
Novosad, V.
-
Omori, Y.
-
Padin, S.
-
Paschos, P.
- Pearson, J.
-
Posada, C. M.
- Prabhu, K.
- Quan, W.
-
Raghunathan, S.
- Rahimi, M.
-
Rahlin, A.
-
Reichardt, C. L.
-
Riebel, D.
-
Riedel, B.
-
Ruhl, J. E.
-
Sayre, J. T.
-
Schiappucci, E.
-
Shirokoff, E.
-
Smecher, G.
-
Sobrin, J. A.
-
Stark, A. A.
- Stephen, J.
- Story, K. T.
- Suzuki, A.
-
Takakura, S.
- Tandoi, C.
- Thompson, K. L.
-
Thorne, B.
-
Trendafilova, C.
-
Tucker, C.
-
Umilta, C.
- Vale, L. R.
- Vanderlinde, K.
- Vieira, J. D.
- Wang, G.
-
Whitehorn, N.
-
Yefremenko, V.
- Yoon, K. W.
- Young, M. R.
- Zebrowski, J. A.
Abstract
We present a measurement of gravitational lensing over 1500 deg² of the Southern sky using SPT-3G temperature data at 95 GHz and 150 GHz taken in 2018. The lensing amplitude relative to a fiducial Planck 2018 Lambda cold dark matter (ΛCDM) cosmology is found to be 1.020 ± 0.060, excluding instrumental and astrophysical systematic uncertainties. We conduct extensive systematic and null tests to check the robustness of the lensing measurements, and report a minimum-variance combined lensing power spectrum over angular multipoles of 50 < L < 2000, which we use to constrain cosmological models. When analyzed alone and jointly with primary cosmic microwave background (CMB) spectra within the ΛCDM model, our lensing amplitude measurements are consistent with measurements from SPT-SZ, SPTpol, ACT, and Planck. Incorporating loose priors on the baryon density and other parameters including uncertainties on a foreground bias template, we obtain a 1σ constraint on σ₈Ωₘ^(0.25) = 0.595 ± 0.026 using the SPT-3G 2018 lensing data alone, where σ8 is a common measure of the amplitude of structure today and Ωₘ is the matter density parameter. Combining SPT-3G 2018 lensing measurements with baryon acoustic oscillation (BAO) data, we derive parameter constraints of σ₈ = 0.810 ± 0.033, S₈ ≡ σ₈(Ωₘ/0.3)^(0.5) = 0.836 ± 0.039, and Hubble constant H₀ =68.8^+1.3)_(−1.6) km s⁻¹ Mpc⁻¹. Our preferred S₈ value is higher by 1.6 to 1.8σ compared to cosmic shear measurements from DES-Y3, HSC-Y3, and KiDS-1000 at lower redshift and smaller scales. We combine our lensing data with CMB anisotropy measurements from both SPT-3G and Planck to constrain extensions of ΛCDM. Using CMB anisotropy and lensing measurements from SPT-3G only, we provide independent constraints on the spatial curvature of Ω_K = 0.014^(+0.023)_(−0.026) (95% C.L.) and the dark energy density of Ω_Λ = 0.722^(+0.031)_(−0.026) (68% C.L.). When combining SPT-3G lensing data with SPT-3G CMB anisotropy and BAO data, we find an upper limit on the sum of the neutrino masses of ∑m_ν < 0.30 eV (95% C.L.). Due to the different combination of angular scales and sky area, this lensing analysis provides an independent check on lensing measurements by ACT and Planck.
Copyright and License
© 2023 American Physical Society.
Acknowledgement
We would like to thank Mathew Madhavacheril and Frank Qu for clarifications regarding the ACT DR6 lensing analysis. The South Pole Telescope program is supported by the National Science Foundation (NSF) through the Grant No. OPP-1852617. Partial support is also provided by the Kavli Institute of Cosmological Physics at the University of Chicago. Argonne National Laboratory's work was supported by the U.S. Department of Energy, Office of High Energy Physics, under Contract No. DE-AC02-06CH11357. Work at Fermi National Accelerator Laboratory, a DOE-OS, HEP User Facility managed by the Fermi Research Alliance, LLC, was supported under Contract No. DE-AC02-07CH11359. The Cardiff authors acknowledge support from the UK Science and Technologies Facilities Council (STFC). The IAP authors acknowledge support from the Centre National d'Études Spatiales (CNES). This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (Grant Agreement No. 101001897). The Melbourne authors acknowledge support from the Australian Research Council's Discovery Project scheme (No. DP210102386). The McGill authors acknowledge funding from the Natural Sciences and Engineering Research Council of Canada, Canadian Institute for Advanced Research, and the Fonds de recherche du Québec Nature et technologies. The SLAC authors acknowledge support by the Department of Energy, Contract No. DE-AC02-76SF00515. The UCLA and MSU authors acknowledge support from NSF AST-1716965 and CSSI-1835865. M. A. and J. V. acknowledge support from the Center for AstroPhysical Surveys at the National Center for Supercomputing Applications in Urbana, IL. K. F. acknowledges support from the Department of Energy Office of Science Graduate Student Research (SCGSR) Program. Z. P. was supported by Laboratory Directed Research and Development (LDRD) funding from Argonne National Laboratory, provided by the Director, Office of Science, of the U.S. Department of Energy under Contract No. LDRD-2021-0186. J. V. acknowledges support from the Sloan Foundation. W. L. K. W. is supported in part by the Department of Energy, Laboratory Directed Research and Development program and as part of the Panofsky Fellowship program at SLAC National Accelerator Laboratory, under Contract No. DE-AC02-76SF00515. This research was done using resources provided by the Open Science Grid [116,117], which is supported by the NSF Award No. 1148698, and the U.S. Department of Energy's Office of Science. Some of the computing for this project was performed on the Sherlock cluster. We would like to thank Stanford University and the Stanford Research Computing Center for providing computational resources and support that contributed to these research results.
Files
PhysRevD.108.122005.pdf
Files
(3.8 MB)
| Name | Size | Download all |
|---|---|---|
|
md5:227209dfe3d1108a09a53d7a0b8637f3
|
3.8 MB | Preview Download |
Additional details
Identifiers
- ISSN
- 2470-0029
Funding
- National Science Foundation
- OPP-1852617
- Kavli Institute for Cosmological Physics, University of Chicago
- United States Department of Energy
- DE-AC02-06CH11357
- United States Department of Energy
- DE-AC02-07CH11359
- Science and Technology Facilities Council
- Centre National d'Études Spatiales
- European Research Council
- 101001897
- Australian Research Council
- DP210102386
- Natural Sciences and Engineering Research Council
- Canadian Institute for Advanced Research
- Fonds de Recherche du Québec – Nature et Technologies
- United States Department of Energy
- DE-AC02-76SF00515
- National Science Foundation
- AST-1716965
- National Science Foundation
- OAC-1835865
- National Center for Supercomputing Applications
- Argonne National Laboratory
- LDRD-2021-0186
- Alfred P. Sloan Foundation
- National Science Foundation
- PHY-1148698