Anisotropic CMB distortions from non-Gaussian isocurvature perturbations
  We calculate the CMB $\mu$-distortion and the angular power spectrum of its cross-correlation with the temperature anisotropy in the presence of the non-Gaussian neutrino isocurvature density (NID) mode. While the pure Gaussian NID perturbations give merely subdominant contribution to $<\mu>$ and vanishing $< \mu T>$, the latter quantity can be large enough to be detected in the future when the NID perturbations $\mathcal S(\mathbf x)$ are proportional to the square of a Gaussian field $g(\mathbf x)$, i.e. $\mathcal S({\mathbf x})\propto g^2({\mathbf x})$. In particular, large $< \mu T>$ can be realized since Gaussian-squared perturbations can yield a relatively large bispectrum, satisfying the constraints from the power spectrum of CMB anisotropies, i.e. $\mathcal{P}_\mathcal{SS}(k_0) \sim\mathcal{P}_g^2(k_0)\lesssim10^{-10}$ at $k_0=0.05$ Mpc$^{-1}$. We also forecast constraints from the CMB temperature and E-mode polarisation bispectra, and show that $\mathcal{P}_g(k_0)\lesssim10^{-5}$ would be allowed from Planck data. We find that $< \mu >$ and $|l(l+1)C^{\mu T}_l|$ can respectively be as large as $10^{-9}$ and $10^{-14}$ with uncorrelated scale-invariant NID perturbations for $\mathcal{P}_g(k_0)=10^{-5}$. When the spectrum of the Gaussian field is blue-tilted (with spectral index $n_g \simeq 1.5$), $< \mu T>$ can be enhanced by an order of magnitude. 
Atsuhisa Ota, Toyokazu Sekiguchi, Yuichiro Tada and Shuichiro Yokoyama
astro-ph.CO gr-qc hep-ph hep-th