Probing Cosmic Dark Matter and Dark Energy with Weak Gravitational Lensing Statistics by Masato Shirasaki

Author:Masato Shirasaki
Language: eng
Format: epub
Publisher: Springer Singapore, Singapore

4.2.2 Realistic Forecast of Cosmological Constraints

4.2.2.1 Fisher Analysis

In this section, we perform a Fisher analysis to produce a forecast for parameter constraints on , , and with future weak-lensing surveys.

For a multivariate Gaussian likelihood, the Fisher matrix can be written as

(4.15)

where , , is the data covariance matrix, represents the assumed model, and are the main parameters. Here, we consider only the second term in Eq. (4.15). Because C is expected to scale proportionally inverse to the survey area, the second term will be dominant for a large area survey (see, e.g., Ref. [29]). We model the theoretical template by averaging the MFs over 40 convergence maps with appropriate noises for each CFHTLenS field. Figure 4.9 shows the cosmological dependence of our model MFs thus calculated. We find the clear behavior of the MFs as a function of even in the presence of various observational effects.

Fig. 4.9Variation of the lensing MFs for different cosmological parameters (taken from [33]). Each panel shows the differences of , and with respect to those of our fiducial cosmology. In all of the panels, the thick (thin) black line represents the case of cosmological model with higher (lower) . The thick (thin) red one corresponds to the result of the cosmological model with higher (lower) , and the thick (thin) blue one is for the model with higher (lower) . For reference, the typical statistical errors of , , and at are , , and , respectively, for CFHTLenS

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