TY - JOUR
T1 - Strong detection of the CMB lensing and galaxy weak lensing cross-correlation from ACT-DR4, Planck Legacy, and KiDS-1000
AU - Robertson, Naomi Clare
AU - Alonso, David
AU - Harnois-Déraps, Joachim
AU - Darwish, Omar
AU - Kannawadi, Arun
AU - Amon, Alexandra
AU - Asgari, Marika
AU - Bilicki, MacIej
AU - Calabrese, Erminia
AU - Choi, Steve K.
AU - Devlin, Mark J.
AU - Dunkley, Jo
AU - Dvornik, Andrej
AU - Erben, Thomas
AU - Ferraro, Simone
AU - Fortuna, Maria Cristina
AU - Giblin, Benjamin
AU - Han, Dongwon
AU - Heymans, Catherine
AU - Hildebrandt, Hendrik
AU - Hill, J. Colin
AU - Hilton, Matt
AU - Ho, Shuay Pwu P.
AU - Hoekstra, Henk
AU - Hubmayr, Johannes
AU - Hughes, John P.
AU - Joachimi, Benjamin
AU - Joudaki, Shahab
AU - Knowles, Kenda
AU - Kuijken, Konrad
AU - Madhavacheril, Mathew S.
AU - Moodley, Kavilan
AU - Miller, Lance
AU - Namikawa, Toshiya
AU - Nati, Federico
AU - Niemack, Michael D.
AU - Page, Lyman A.
AU - Partridge, Bruce
AU - Schaan, Emmanuel
AU - Schillaci, Alessandro
AU - Schneider, Peter
AU - Sehgal, Neelima
AU - Sherwin, Blake D.
AU - Sifón, Cristóbal
AU - Staggs, Suzanne T.
AU - Tröster, Tilman
AU - Van Engelen, Alexander
AU - Valentijn, Edwin
AU - Wollack, Edward J.
AU - Wright, Angus H.
AU - Xu, Zhilei
N1 - Funding Information:
Acknowledgements. The figures in this work were created with matplotlib (Hunter 2007), making use of the numpy (Oliphant 2006), scipy (Jones et al. 2001), astropy (Astropy Collaboration 2018) and pixell software packages. DA acknowledges support from the Beecroft Trust, and from the Science and Technology Facilities Council through an Ernest Rutherford Fellowship, grant reference ST/P004474. JHD acknowledges support from an STFC Ernest Rutherford Fellowship (project reference ST/S004858/1). HHi acknowledges the European Research Council (ERC) under grant agreement No. 770935 and support from the Deutsche Forschungsgemeinschaft Heisenberg grant Hi 1495/5-1. OD, BDS, FQ and TN acknowledge support from an Isaac Newton Trust Early Career Grant and from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation programme (Grant agreement No. 851274). BDS further acknowledges support from an STFC Ernest Rutherford Fellowship. AK, MCF, and HHo acknowledge support from the Netherlands Organisation for Scientific Research Vici grant 639.043.512. CH, TT, MA, JHD and BG acknowledge support from the ERC under grant agreement No. 647112. CH also acknowledges support from the Max Planck Society and the Alexander von Humboldt Foundation in the frame-work of the Max Planck-Humboldt Research Award endowed by the Federal Ministry of Education and Research and BG from the Royal Society through an Enhancement Award RGF/EA/181006. TT also acknowledges support from the Marie Skłodowska-Curie grant agreement No. 797794. MB acknowledges support from the Polish Ministry of Science and Higher Education through grant DIR/WK/2018/12, and the Polish National Science Center through grants no. 2018/30/E/ST9/00698 and 2018/31/G/ST9/03388. EC acknowledges support from the STFC Ernest Rutherford Fellowship ST/M004856/2 and STFC Consolidated Grant ST/S00033X/1, and from the Horizon 2020 ERC Starting Grant (Grant agreement No 849169). JD is supported by NSF grant number AST-1814971. KK acknowledges support from the Alexander von Humboldt Foundation. SJ is supported by the ERC under grant No. 693024 and the Beecroft Trust. LM is supported by STFC grant ST/N000919/1. KM acknowledges support from the National Research Foundation of South Africa. NS acknowledges support from NSF grant numbers AST-1513618 and AST-1907657. CS acknowledges support from the Agencia Nacional de Investigación y Desarrollo (ANID) through FONDECYT Iniciación grant No. 11191125. ZX is supported by the Gordon and Betty Moore Foundation. The results in this paper are based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 177.A-3016, 177.A-3017, 177.A-3018 and 179.A-2004, and on data products produced by the KiDS consortium. The KiDS production team acknowledges support from: Deutsche Forschungsgemeinschaft, ERC, NOVA and NWO-M grants; Target; the University of Padova, and the University Federico II (Naples). Data processing for VIKING has been contributed by the VISTA Data Flow System at CASU, Cambridge and WFAU, Edinburgh. For ACT, the work was supported by the U.S. National Science Foundation through awards AST-1440226, AST0965625 and AST-0408698 for the ACT project, as well as awards PHY-1214379 and PHY-0855887. Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque Astronómico Atacama in northern Chile under the auspices of the Comisión Nacional de Inves-tigación (CONICYT). The development of multichroic detectors and lenses was supported by NASA grants NNX13AE56G and NNX14AB58G. Colleagues at AstroNorte and RadioSky provide logistical support and keep operations in Chile running smoothly. We also thank the Mishrahi Fund and the Wilkinson Fund
Publisher Copyright:
© ESO 2021.
PY - 2021/5/1
Y1 - 2021/5/1
N2 - We measured the cross-correlation between galaxy weak lensing data from the Kilo Degree Survey (KiDS-1000, DR4) and cosmic microwave background (CMB) lensing data from the Atacama Cosmology Telescope (ACT, DR4) and the Planck Legacy survey. We used two samples of source galaxies, selected with photometric redshifts, (0.1 < zB < 1.2) and (1.2 < zB < 2), which produce a combined detection significance of the CMB lensing and weak galaxy lensing cross-spectrum of 7.7σ. With the lower redshift galaxy sample, for which the cross-correlation was detected at a significance of 5.3σ, we present joint cosmological constraints on the matter density parameter, ωm, and the matter fluctuation amplitude parameter, σ8, marginalising over three nuisance parameters that model our uncertainty in the redshift and shear calibration as well as the intrinsic alignment of galaxies. We find our measurement to be consistent with the best-fitting flat ΛCDM cosmological models from both Planck and KiDS-1000. We demonstrate the capacity of CMB weak lensing cross-correlations to set constraints on either the redshift or shear calibration by analysing a previously unused high-redshift KiDS galaxy sample (1.2 < zB < 2), with the cross-correlation detected at a significance of 7σ. This analysis provides an independent assessment for the accuracy of redshift measurements in a regime that is challenging to calibrate directly owing to known incompleteness in spectroscopic surveys.
AB - We measured the cross-correlation between galaxy weak lensing data from the Kilo Degree Survey (KiDS-1000, DR4) and cosmic microwave background (CMB) lensing data from the Atacama Cosmology Telescope (ACT, DR4) and the Planck Legacy survey. We used two samples of source galaxies, selected with photometric redshifts, (0.1 < zB < 1.2) and (1.2 < zB < 2), which produce a combined detection significance of the CMB lensing and weak galaxy lensing cross-spectrum of 7.7σ. With the lower redshift galaxy sample, for which the cross-correlation was detected at a significance of 5.3σ, we present joint cosmological constraints on the matter density parameter, ωm, and the matter fluctuation amplitude parameter, σ8, marginalising over three nuisance parameters that model our uncertainty in the redshift and shear calibration as well as the intrinsic alignment of galaxies. We find our measurement to be consistent with the best-fitting flat ΛCDM cosmological models from both Planck and KiDS-1000. We demonstrate the capacity of CMB weak lensing cross-correlations to set constraints on either the redshift or shear calibration by analysing a previously unused high-redshift KiDS galaxy sample (1.2 < zB < 2), with the cross-correlation detected at a significance of 7σ. This analysis provides an independent assessment for the accuracy of redshift measurements in a regime that is challenging to calibrate directly owing to known incompleteness in spectroscopic surveys.
KW - Cosmology: observations
KW - Gravitational lensing: weak
KW - Large-scale structure of Universe
UR - http://www.scopus.com/inward/record.url?scp=85107263813&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85107263813&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/202039975
DO - 10.1051/0004-6361/202039975
M3 - Article
AN - SCOPUS:85107263813
SN - 0004-6361
VL - 649
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A146
ER -