Primordial Non-Gaussianity in the Large-Scale Structure of the Universe

Figure 6

Non-Gaussian bias correction (33) for the local, equilateral and folded primordial bispectrum as a function of wavenumber. Results are shown at 𝑧=0 for a smoothing radius 𝑅=5h⁻¹Mpc and a nonlinear parameter 𝑓^X_NL=1. The dotted line represent an analytic approximation, (35), which is valid at large-scales 𝑘≪1. Note that while the magnitude of Δ𝑏_𝜅(𝑘,𝑓^loc_NL) does not change with 𝑅, Δ𝑏_𝜅(𝑘,𝑓^eq_NL) and Δ𝑏_𝜅(𝑘,𝑓^fol_NL) strongly depends on the smoothing radius (see text).