FIG 6 - available via license: Creative Commons Attribution 4.0 International
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Correlation coefficient of the total covariance matrix (Gaussian + SSC). The axis labels show the values of .
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Weak gravitational lensing is one of the few direct methods to map the dark-matter distribution on large scales in the Universe, and to estimate cosmological parameters. We study a Bayesian inference problem where the data covariance $\mathbf{C}$, estimated from a number $n_{\textrm{s}}$ of numerical simulations, is singular. In a cosmological cont...
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Context 1
... where we insert y from Eq. (26) for the "signal" C . For the SSC term, we use the one derived in Barreira, Krause and Schmidt (2018b), and parameterize the SSC contribution scaled by the weak-lensing power spectrum, see Fig. 3 in Barreira, Krause and Schmidt (2018b). The correlation matrix of the total covariance (Gaussian + SSC) is plotted in Fig. ...
Context 2
... set to σ ε = 0.31. 14), which ignores the correlation in the data. The acf of one of the n r = 25 realizations of the observations y sim is displayed in Fig. 5. After a sharp drop from zero lag, the correlation stays above zero. This represents the correlation between small and large scales (large ∆ t ), which can be seen in the covariance matrix (Fig. 6). The acf can thus capture some of the correlation information of the data vector, to be used in the distance function. Fig. 7 shows ABC under the non-Gaussian covariance model (G+SSC) with the acf distance Eq. (18). In all cases the ABC parameter estimates are consistent with the true values. The results are summarized in Table 2 for ...
