期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 474, 期 1, 页码 1116-1134出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stx2837
关键词
gravitational lensing: weak; dark matter; large-scale structure of Universe
资金
- NOVA grant
- NWO-M grant
- Department of Physics AMP
- Astronomy of the University of Padova
- Department of Physics of Univ. Federico II (Naples)
- project 'The Dark Universe' - DFG [TR33]
- DFG [Hi 1495/2-1]
- NSFC of China [11333001, 11173001]
- Chinese Academy of Sciences [XDB09000000]
- China Postdoctoral Science Foundation [2016M591006]
- Vici grant - Netherlands Organisation for Scientific Research (NWO) [639.043.512]
- European Commission under a Marie-Sklodwoska-Curie European Fellowship (EU) [656869]
- European Research Council [647112]
- Alexander von Humboldt Foundation
- European Union under Marie Sklodowska-Curie grant [627288, 664931]
- NSFC [11403035]
- ESO Telescopes at the La Silla Paranal Observatory [177.A-3016, 177.A-3017, 177.A-3018]
- Marie Curie Actions (MSCA) [664931, 656869] Funding Source: Marie Curie Actions (MSCA)
This paper is the first of a series of papers constraining cosmological parameters with weak lensing peak statistics using similar to 450 deg(2) of imaging data from the Kilo Degree Survey (KiDS-450). We measure high signal-to-noise ratio (SNR: nu) weak lensing convergence peaks in the range of 3 < nu < 5, and employ theoretical models to derive expected values. These models are validated using a suite of simulations. We take into account two major systematic effects, the boost factor and the effect of baryons on the mass-concentration relation of dark matter haloes. In addition, we investigate the impacts of other potential astrophysical systematics including the projection effects of large-scale structures, intrinsic galaxy alignments, as well as residual measurement uncertainties in the shear and redshift calibration. Assuming a flat Lambda cold dark matter model, we find constraints for S-8 = sigma(8)(Omega(m)/0.3)(0.5) = 0.746(-0.107)(+0.046) according to the degeneracy direction of the cosmic shear analysis and Sigma(8) = s8(Omega(m)/0.3) 0.38 = 0.696(-0.050)(+0.048) based on the derived degeneracy direction of our high-SNR peak statistics. The difference between the power index of S-8 and in Sigma(8) indicates that combining cosmic shear with peak statistics has the potential to break the degeneracy in sigma(8) and Omega(m). Our results are consistent with the cosmic shear tomographic correlation analysis of the same data set and similar to 2s lower than the Planck 2016 results.
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