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Probing Cosmic Dark Matter and Dark Energy with Weak Gravitational Lensing Statistics pp 53–83Cite as

Weak Lensing Morphological Analysis

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Abstract

In this chapter, we summarize our studies on the true utility and applicability of weak lensing Minkowski functionals (MFs) in terms of statistical tool for precision cosmology. We extended the previous morphological studies by including various observational effects such as sky masking, systematics associated with shape measurement, photometric redshift errors, and shear calibration correction. We generated a large set of mock cosmic shear data with numerical simulations to study possible systematics in detail one by one. We found that each observational effect could induce the biased parameter estimation in upcoming galaxy imaging surveys. We then applied all the method developed and examined in our previous studies to the real data obtained by Canada-France-Hawaii Telescope Lensing survey (CFHTLenS). As shown in this chapter, we found that lensing MFs can successfully break degeneracies in parameter constraints from lensing data set alone. These works are useful to properly analyze the data and to accurately extract cosmological information from them.

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Notes

  1. 1.

    We generate the Gaussian convergence maps for \(\varLambda \) CDM cosmology. In Gaussian simulation, we use the fitting formula of Ref. [8] to calculate the matter power spectrum P(k; z). We then obtain the convergence power spectrum by integrating the matter power spectrum over redshift z with a weighting function for the source redshift \(z_\mathrm{source} =1\). Each map is defined on \(2048^2\) grid points with an angular grid size of 0.15 arcmin.

  2. 2.

    http://smoka.nao.ac.jp/.

  3. 3.

    For the simulations, the authors in Ref. [16] adopted the cosmological model which is consistent with WMAP three-years results [17].

  4. 4.

    In principle, one can use regions with \(x>3\) as well. Such regions usually correspond to the positions of massive dark matter halos, which are thought to be sensitive to cosmological parameters. On the other hand, such regions are extremely rare, and thus the first derivatives in Eq. (4.16) are not evaluated accurately even with our large number of \({\mathscr {K}}\) maps. We thus do not use high \({\mathscr {K}}\) regions with \(x>3\) in the analysis.

  5. 5.

    We have also examined which MFs (\(V_0, V_1, V_2\)) cause this trend. We have performed likelihood analysis using each MF only. Both \(V_{1}\) and \(V_{2}\) prefer lower \(w_{0}\). The 68 \(\%\) marginalized constraints on \(w_{0}\) using each MF are found to be \(-0.30\pm ^{0.77}_{0.84}\), \(-3.31\pm {0.60}\), and \(-2.48\pm ^{0.91}_{0.84}\) for \(V_{0}\), \(V_{1}\), and \(V_{2}\), respectively.

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  1. The University of Tokyo, Tokyo, Japan

    Masato Shirasaki

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Shirasaki, M. (2016). Weak Lensing Morphological Analysis. In: Probing Cosmic Dark Matter and Dark Energy with Weak Gravitational Lensing Statistics. Springer Theses. Springer, Singapore. https://doi.org/10.1007/978-981-287-796-3_4

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  • DOI: https://doi.org/10.1007/978-981-287-796-3_4

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