Non-Gaussianity and the Cosmic Microwave Background Anisotropies

Figure 1

Shape dependence of the second-order bispectrum from products of the first-order terms (top) and that of the local primordial bispectrum (bottom). We show ℓ₁ℓ₂⟨𝑎_ℓ⁽¹⁾_1𝑚1𝑎_ℓ⁽¹⁾_2𝑚2𝑎_ℓ⁽²⁾_3𝑚3⟩(𝒢^{𝑚1𝑚2𝑚3}_ℓ1ℓ2ℓ3)⁻¹/(2𝜋)²×10²² as a function of ℓ₁/ℓ₃ and ℓ₂/ℓ₃ where ℓ₃=200. Both shapes have the largest signals in the squeezed triangles, ℓ₁≪ℓ₂≈ℓ₃.

(a)

(b)