Constraints on Cosmological Parameters from the 500 deg<sup>2</sup> SPTPOL Lensing Power Spectrum
F. BianchiniSchool of Physics, University of Melbourne, Parkville, VIC 3010, AustraliaW. L. K. WuKavli Institute for Cosmological Physics, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USAP. A. R. AdeCardiff University, Cardiff CF10 3XQ, UKA. J. AndersonFermi National Accelerator Laboratory, MS209, P.O. Box 500, Batavia, IL 60510, USAJason E. AustermannNIST Quantum Devices Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305, USAJ. S. AvvaDepartment of Physics, University of California, Berkeley, CA 94720, USAJames A. BeallNIST Quantum Devices Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305, USAA. N. BenderHigh Energy Physics Division, Argonne National Laboratory, 9700 S. Cass Avenue, Argonne, IL 60439, USAB. A. BensonFermi National Accelerator Laboratory, MS209, P.O. Box 500, Batavia, IL 60510, USAL. E. BleemKavli Institute for Cosmological Physics, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USAJ. E. CarlstromDepartment of Astronomy and Astrophysics, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USAC. L. ChangKavli Institute for Cosmological Physics, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USAP. ChaubalSchool of Physics, University of Melbourne, Parkville, VIC 3010, AustraliaH. C. ChiangSchool of Mathematics, Statistics & Computer Science, University of KwaZulu-Natal, Durban, South AfricaR. CitronUniversity of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USAC. Corbett MoranTAPIR, Walter Burke Institute for Theoretical Physics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125, USAT. M. CrawfordKavli Institute for Cosmological Physics, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USAA. T. CritesDepartment of Astronomy and Astrophysics, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USAT. de HaanPhysics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USAM. DobbsCanadian Institute for Advanced Research, CIFAR Program in Gravity and the Extreme Universe, Toronto, ON, M5G 1Z8, CanadaW. EverettDepartment of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309, USAJason GallicchioKavli Institute for Cosmological Physics, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USAE. M. GeorgeEuropean Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching bei München, GermanyA. GilbertDepartment of Physics, McGill University, 3600 Rue University, Montreal, Quebec H3A 2T8, CanadaN. GuptaSchool of Physics, University of Melbourne, Parkville, VIC 3010, AustraliaN. W. HalversonDepartment of Physics, University of Colorado, Boulder, CO 80309, USAN. L. HarringtonDepartment of Physics, University of California, Berkeley, CA 94720, USAJ. W. HenningHigh Energy Physics Division, Argonne National Laboratory, 9700 S. Cass Avenue, Argonne, IL 60439, USAG. C. HiltonNIST Quantum Devices Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305, USAG. P. HolderCanadian Institute for Advanced Research, CIFAR Program in Gravity and the Extreme Universe, Toronto, ON, M5G 1Z8, CanadaW. L. HolzapfelDepartment of Physics, University of California, Berkeley, CA 94720, USAJ. D. HrubesUniversity of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USAN. HuangDepartment of Physics, University of California, Berkeley, CA 94720, USAJohannes HubmayrNIST Quantum Devices Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305, USAK. D. IrwinDepartment of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USAL. KnoxDepartment of Physics, University of California, 1 Shields Avenue, Davis, CA 95616, USAA. T. LeePhysics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USAD. LiNIST Quantum Devices Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305, USAA. E. LowitzDepartment of Astronomy and Astrophysics, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USAA. ManzottiKavli Institute for Cosmological Physics, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USAJ. J. McMahonDepartment of Physics, University of Michigan, 450 Church Street, Ann Arbor, MI 48109, USAS. S. MeyerKavli Institute for Cosmological Physics, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USAM. MilleaDepartment of Physics, University of California, Berkeley, CA 94720, USAL. M. MocanuKavli Institute for Cosmological Physics, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USAJ. MontgomeryDepartment of Physics, McGill University, 3600 Rue University, Montreal, Quebec H3A 2T8, CanadaAndrew NadolskiAstronomy Department, University of Illinois at Urbana-Champaign, 1002 W. Green Street, Urbana, IL 61801, USAT. NatoliDepartment of Astronomy and Astrophysics, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USAJ. P. NibargerNIST Quantum Devices Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305, USAG. I. NobleDepartment of Physics, McGill University, 3600 Rue University, Montreal, Quebec H3A 2T8, CanadaV. NovosadMaterials Sciences Division, Argonne National Laboratory, 9700 S. Cass Avenue, Argonne, IL 60439, USAY. OmoriKavli Institute for Particle Astrophysics and Cosmology, Stanford University, 452 Lomita Mall, Stanford, CA 94305, USAS. PadinDepartment of Astronomy and Astrophysics, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USAS. PatilSchool of Physics, University of Melbourne, Parkville, VIC 3010, AustraliaC. PrykeSchool of Physics and Astronomy, University of Minnesota, 116 Church Street S.E. Minneapolis, MN 55455, USAC. L. ReichardtSchool of Physics, University of Melbourne, Parkville, VIC 3010, AustraliaJ. E. RuhlPhysics Department, Center for Education and Research in Cosmology and Astrophysics, Case Western Reserve University, Cleveland, OH 44106, USAB. R. SaliwanchikPhysics Department, Center for Education and Research in Cosmology and Astrophysics, Case Western Reserve University, Cleveland, OH 44106, USAJ. T. SayreDepartment of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309, USAK. K. SchafferLiberal Arts Department, School of the Art Institute of Chicago, 112 S. Michigan Avenue, Chicago, IL 60603, USAC. SieversUniversity of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USAG. SimardDepartment of Physics, McGill University, 3600 Rue University, Montreal, Quebec H3A 2T8, CanadaG. SmecherThree-Speed Logic, Inc., Vancouver, B.C., V6A 2J8, CanadaA. A. StarkHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAK. T. StoryDepartment of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USAC. TuckerCardiff University, Cardiff CF10 3XQ, UKK. VanderlindeDepartment of Astronomy & Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON, M5S 3H4, CanadaTodd VeachDepartment of Astronomy, University of Maryland College Park, MD 20742, USAJ. D. VieiraAstronomy Department, University of Illinois at Urbana-Champaign, 1002 W. Green Street, Urbana, IL 61801, USAG. WangHigh Energy Physics Division, Argonne National Laboratory, 9700 S. Cass Avenue, Argonne, IL 60439, USAN. WhitehornDepartment of Physics and Astronomy, University of California, Los Angeles, CA 90095, USAV. YefremenkoHigh Energy Physics Division, Argonne National Laboratory, 9700 S. Cass Avenue, Argonne, IL 60439, USA
2020en
ABI
Аннотация
Abstract We present cosmological constraints based on the cosmic microwave background (CMB) lensing potential power spectrum measurement from the recent 500 deg 2 SPTpol survey, the most precise CMB lensing measurement from the ground to date. We fit a flat ΛCDM model to the reconstructed lensing power spectrum alone and in addition with other data sets: baryon acoustic oscillations (BAO), as well as primary CMB spectra from Planck and SPTpol . The cosmological constraints based on SPTpol and Planck lensing band powers are in good agreement when analyzed alone and in combination with Planck full-sky primary CMB data. With weak priors on the baryon density and other parameters, the SPTpol CMB lensing data alone provide a 4% constraint on . Jointly fitting with BAO data, we find , , and , up to away from the central values preferred by Planck lensing + BAO. However, we recover good agreement between SPTpol and Planck when restricting the analysis to similar scales. We also consider single-parameter extensions to the flat ΛCDM model. The SPTpol lensing spectrum constrains the spatial curvature to be and the sum of the neutrino masses to be eV at 95% C.L. (with Planck primary CMB and BAO data), in good agreement with the Planck lensing results. With the differences in the signal-to-noise ratio of the lensing modes and the angular scales covered in the lensing spectra, this analysis represents an important independent check on the full-sky Planck lensing measurement.
Перевод пока недоступен
Идентификаторы
Цитирования и источники
Цитирований: 3Использованных источников: 0