期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 447, 期 1, 页码 858-874出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stu2513
关键词
gravitational lensing: weak; methods: numerical; cosmological parameters; cosmology: theory; dark energy; large-scale structure of Universe
资金
- STFC [ST/H002774/1]
- European Commission
- PRIN MIUR
- PRIN INAF
- [ASI/INAF I/023/12/0]
- STFC [ST/L005573/1, ST/K00090X/1, ST/L000768/1, ST/H002774/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/L000768/1, ST/L005573/1, ST/H002774/1, ST/K00090X/1] Funding Source: researchfish
Dark matter and dark energy are usually assumed to couple only gravitationally. An extension to this picture is to model dark energy as a scalar field coupled directly to cold dark matter. This coupling leads to new physical effects, such as a fifth force and a time-dependent dark matter particle mass. In this work we examine the impact that coupling has on weak lensing statistics by constructing realistic simulated weak lensing maps using ray-tracing techniques through N-body cosmological simulations. We construct maps for different lensing quantities, covering a range of scales from a few arcminutes to several degrees. The concordance Lambda cold dark matter (Lambda CDM) model is compared to different coupled dark energy models, described either by an exponential scalar field potential (standard coupled dark energy scenario) or by a SUGRA potential (bouncing model). We analyse several statistical quantities and our results, with sources at low redshifts are largely consistent with previous work on cosmic microwave background lensing by Carbone et al. The most significant differences from the Lambda CDM model are due to the enhanced growth of the perturbations and to the effective friction term in nonlinear dynamics. For the most extreme models, we see differences in the power spectra up to 40 per cent compared to the Lambda CDM model. The different time evolution of the linear matter overdensity can account for most of the differences, but when controlling for this using a Lambda CDM model having the same normalization, the overall signal is smaller due to the effect of the friction term appearing in the equation of motion for dark matter particles.
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