On non-Gaussianity in the Cosmic Microwave Background
arXiv:astro-ph/0006097
Abstract
We consider a cosmological model with non-Gaussian initial perturbations, which in principle could be generated in non-standard inflationary scenarios with two or more scalar fields. In particular we focus our attention on the model proposed by Linde & Mukhanov (1997) perturbations are quadratic in a Gaussian field. These perturbations, if they exist, have to be observable as a non-Gaussian distribution of the CMB signal on the sky. In order to efficiently pick up the non-Gaussian signal in CMB maps of degree resolution, one can use Minkowski Functionals and peak statistics. Our paper contains the theoretical predictions of the properties for Minkowski Functionals and distributions of peaks of the CMB anisotropy in the model with "squared" Gaussian statistics. Likelihood comparison of the four-year COBE DMR data to this non-Gaussian model and the standard Gaussian model does not select any of them as most likely. We also suggest an efficient algorithm for fast simulation of CMB maps on the whole sky. Using a cylindrical partition of the sphere, we rewrite the spherical harmonics analysis as a Fourier transform in flat space, which makes the problem accessible to numerically advantageous FFT methods.
10 pages, 7 figures, accepted for publication in Astronomy and Astrophysics
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- Tensor Minkowski Functionals: first application to the CMB
- Sojourn measures of Student and Fisher-Snedecor random fields
- Characteristic Angular Scales in Cosmic Microwave Background Radiation
- The extended empirical process test for non-Gaussianity in the CMB, with an application to non-Gaussian inflationary models
- Morphology of CMB fields -- effect of weak gravitational lensing
- Sojourn functionals for spatiotemporal random fields with long-memory