%0 Generic %1 heymans2020kids1000 %A Heymans, Catherine %A Tröster, Tilman %A Asgari, Marika %A Blake, Chris %A Hildebrandt, Hendrik %A Joachimi, Benjamin %A Kuijken, Konrad %A Lin, Chieh-An %A Sánchez, Ariel G. %A Busch, Jan Luca van den %A Wright, Angus H. %A Amon, Alexandra %A Bilicki, Maciej %A de Jong, Jelte %A Crocce, Martin %A Dvornik, Andrej %A Erben, Thomas %A Getman, Fedor %A Giblin, Benjamin %A Glazebrook, Karl %A Hoekstra, Henk %A Joudaki, Shahab %A Kannawadi, Arun %A Lidman, Chris %A Köhlinger, Fabian %A Miller, Lance %A Napolitano, Nicola R. %A Parkinson, David %A Schneider, Peter %A Shan, HuanYuan %A Wolf, Christian %D 2020 %K library %T KiDS-1000 Cosmology: Multi-probe weak gravitational lensing and spectroscopic galaxy clustering constraints %U http://arxiv.org/abs/2007.15632 %X We present a joint cosmological analysis of weak gravitational lensing observations from the Kilo-Degree Survey (KiDS-1000), with redshift-space galaxy clustering observations from the Baryon Oscillation Spectroscopic Survey (BOSS), and galaxy-galaxy lensing observations from the overlap between KiDS-1000, BOSS and the spectroscopic 2-degree Field Lensing Survey (2dFLenS). This combination of large-scale structure probes breaks the degeneracies between cosmological parameters for individual observables, resulting in a constraint on the structure growth parameter $S_8=\sigma_8 Ømega_\rm m/0.3 = 0.766^+0.020_-0.014$, that has the same overall precision as that reported by the full-sky cosmic microwave background observations from Planck. The recovered $S_8$ amplitude is low, however, by $8.3 2.6$ % relative to Planck. This result builds from a series of KiDS-1000 analyses where we validate our methodology with variable depth mock galaxy surveys, our lensing calibration with image simulations and null-tests, and our optical-to-near-infrared redshift calibration with multi-band mock catalogues and a spectroscopic-photometric clustering analysis. The systematic uncertainties identified by these analyses are folded through as nuisance parameters in our cosmological analysis. Inspecting the offset between the marginalised posterior distributions, we find that the $S_8$-difference with Planck is driven by a tension in the matter fluctuation amplitude parameter, $\sigma_8$. We quantify the level of agreement between the CMB and our large-scale structure constraints using a series of different metrics, finding differences with a significance ranging between $\sim\! 3\,\sigma$, when considering the offset in $S_8$, and $\sim\! 2\,\sigma$, when considering the full multi-dimensional parameter space.

@misc{heymans2020kids1000, abstract = {We present a joint cosmological analysis of weak gravitational lensing observations from the Kilo-Degree Survey (KiDS-1000), with redshift-space galaxy clustering observations from the Baryon Oscillation Spectroscopic Survey (BOSS), and galaxy-galaxy lensing observations from the overlap between KiDS-1000, BOSS and the spectroscopic 2-degree Field Lensing Survey (2dFLenS). This combination of large-scale structure probes breaks the degeneracies between cosmological parameters for individual observables, resulting in a constraint on the structure growth parameter $S_8=\sigma_8 \sqrt{\Omega_{\rm m}/0.3} = 0.766^{+0.020}_{-0.014}$, that has the same overall precision as that reported by the full-sky cosmic microwave background observations from Planck. The recovered $S_8$ amplitude is low, however, by $8.3 \pm 2.6$ % relative to Planck. This result builds from a series of KiDS-1000 analyses where we validate our methodology with variable depth mock galaxy surveys, our lensing calibration with image simulations and null-tests, and our optical-to-near-infrared redshift calibration with multi-band mock catalogues and a spectroscopic-photometric clustering analysis. The systematic uncertainties identified by these analyses are folded through as nuisance parameters in our cosmological analysis. Inspecting the offset between the marginalised posterior distributions, we find that the $S_8$-difference with Planck is driven by a tension in the matter fluctuation amplitude parameter, $\sigma_8$. We quantify the level of agreement between the CMB and our large-scale structure constraints using a series of different metrics, finding differences with a significance ranging between $\sim\! 3\,\sigma$, when considering the offset in $S_{8}$, and $\sim\! 2\,\sigma$, when considering the full multi-dimensional parameter space.}, added-at = {2020-07-31T13:35:37.000+0200}, author = {Heymans, Catherine and Tröster, Tilman and Asgari, Marika and Blake, Chris and Hildebrandt, Hendrik and Joachimi, Benjamin and Kuijken, Konrad and Lin, Chieh-An and Sánchez, Ariel G. and Busch, Jan Luca van den and Wright, Angus H. and Amon, Alexandra and Bilicki, Maciej and de Jong, Jelte and Crocce, Martin and Dvornik, Andrej and Erben, Thomas and Getman, Fedor and Giblin, Benjamin and Glazebrook, Karl and Hoekstra, Henk and Joudaki, Shahab and Kannawadi, Arun and Lidman, Chris and Köhlinger, Fabian and Miller, Lance and Napolitano, Nicola R. and Parkinson, David and Schneider, Peter and Shan, HuanYuan and Wolf, Christian}, biburl = {https://www.bibsonomy.org/bibtex/28ae6e0d4abd4f61ef8e9f4b21870f76e/gpkulkarni}, description = {KiDS-1000 Cosmology: Multi-probe weak gravitational lensing and spectroscopic galaxy clustering constraints}, interhash = {019e1e97e7f99d4105c09804853383b2}, intrahash = {8ae6e0d4abd4f61ef8e9f4b21870f76e}, keywords = {library}, note = {cite arxiv:2007.15632Comment: 24 pages, 11 figures, 5 tables, submitted to A&A. This paper is part of the KiDS-1000 series of papers, accompanying Asgari et al. and Hildebrandt et al. appearing on the arXiv today, joining Joachimi et al. (arXiv:2007.01844) and Giblin et al. (arXiv:2007.01845). Online KiDS-1000 talks and seminars can be viewed at http://kids.strw.leidenuniv.nl/KiDS-1000.php}, timestamp = {2020-07-31T13:35:37.000+0200}, title = {KiDS-1000 Cosmology: Multi-probe weak gravitational lensing and spectroscopic galaxy clustering constraints}, url = {http://arxiv.org/abs/2007.15632}, year = 2020 }