Primordial Non-Gaussianity and Bispectrum Measurements in the Cosmic Microwave Background and Large-Scale Structure

Figure 18

(a), (b) Predicted errors on galaxy bias parameters (a) and (b) as a function of the maximum wavenumber considered for the sum defining the Fisher matrix, (187). The analysis corresponds to an ideal geometry survey of volume and a galaxy number density of . Dashed (red) lines assume a mean redshift of , while continuous (blue) lines assume . Both assume that Gaussian initial conditions; that is, . The vertical lines correspond to the value of determined as the inverse of the distance scale defined by the condition . (c), (d) Predicted errors on the non-Gaussian parameters (c) and (d), marginalized over the bias parameters, as a function of . The effect of shot noise is evident only at very high values of , while for realistic surveys one can expect a more significant effect at lower . The relatively high value has been chosen here just for illustrative purposes, from the study by Sefusatti and Komatsu in [197].

(a)

(b)

(c)

(d)