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We test the effects of varying the cosmological parameter values used in the strong lens modeling process for the six Hubble Frontier Fields (HFF) galaxy clusters. The standard procedure for generating high fidelity strong lens models includes careful consideration of uncertainties in the output models that result from varying model parameters within the bounds of available data constraints. It is not, however, common practice to account for the effects of cosmological parameter value uncertainties. The convention is to instead use a single fiducial concordance cosmology and generate lens models assuming zero uncertainty in cosmological parameter values. We find that the magnification maps of the individual HFF clusters vary significantly when lens models are computed using different cosmological parameter values taken from recent literature constraints from space- and ground-based experiments. Specifically, the magnification maps have average variances across the best fit models computed using different cosmologies that are comparable in magnitude to - and as much as 2.5 times larger than - the model fitting uncertainties in each best fit model. We also find that estimates of the mass profiles of the cluster cores themselves vary only slightly when different input cosmological parameters are used. We conclude that cosmological parameter uncertainty is a non-negligible source of uncertainty in lens model products for the HFF clusters, and that it is important that current and future work which relies on precision strong lensing models take care to account for this additional source of uncertainty.
Residual errors in shear measurements, after corrections for instrument systematics and atmospheric effects, can impact cosmological parameters derived from weak lensing observations. Here we combine convergence maps from our suite of ray-tracing sim
Upcoming surveys will map the growth of large-scale structure with unprecented precision, improving our understanding of the dark sector of the Universe. Unfortunately, much of the cosmological information is encoded by the small scales, where the cl
We present a finely-binned tomographic weak lensing analysis of the Canada-France-Hawaii Telescope Lensing Survey, CFHTLenS, mitigating contamination to the signal from the presence of intrinsic galaxy alignments via the simultaneous fit of a cosmolo
Strong gravitational lensing is a powerful tool to measure cosmological parameters and to study galaxy evolution mechanisms. However, quantitative strong lensing studies often require mock observations. To capture the full complexity of galaxies, the
Accurate reconstruction of the spatial distributions of the Point Spread Function (PSF) is crucial for high precision cosmic shear measurements. Nevertheless, current methods are not good at recovering the PSF fluctuations of high spatial frequencies