Beecroft Institute for Particle Astrophysics and Cosmology

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A measurement of Omega from the North American test flight of BOOMERANG

(1999)

Authors:

A Melchiorri, PAR Ade, P de Bernardis, JJ Bock, J Borrill, A Boscaleri, BP Crill, G De Troia, P Farese, PG Ferreira, K Ganga, G de Gasperis, M Giacometti, VV Hristov, AH Jaffe, AE Lange, S Masi, PD Mauskopf, L Miglio, CB Netterfield, E Pascale, F Piacentini, G Romeo, JE Ruhl, N Vittorio

The spectral appearance of primeval galaxies

(1999)

Authors:

B Guiderdoni, JEG Devriendt

Tensor Microwave Anisotropies from a Stochastic Magnetic Field

(1999)

Authors:

R Durrer, PG Ferreira, T Kahniashvili

A Bayesian estimate of the skewness of the Cosmic Microwave Background

(1999)

Authors:

CR Contaldi, PG Ferreira, J Magueijo, KM Gorski

A Bayesian estimate of the skewness of the Cosmic Microwave Background

Astrophys.J. 534 (1999) 25-25

Authors:

CR Contaldi, PG Ferreira, J Magueijo, KM Gorski

Abstract:

We propose a formalism for estimating the skewness and angular power spectrum of a general Cosmic Microwave Background data set. We use the Edgeworth Expansion to define a non-Gaussian likelihood function that takes into account the anisotropic nature of the noise and the incompleteness of the sky coverage. The formalism is then applied to estimate the skewness of the publicly available 4 year Cosmic Background Explorer (COBE) Differential Microwave Radiometer data. We find that the data is consistent with a Gaussian skewness, and with isotropy. Inclusion of non Gaussian degrees of freedom has essentially no effect on estimates of the power spectrum, if each $C_\ell$ is regarded as a separate parameter or if the angular power spectrum is parametrized in terms of an amplitude (Q) and spectral index (n). Fixing the value of the angular power spectrum at its maxiumum likelihood estimate, the best fit skewness is $S=6.5\pm6.0\times10^4(\muK)^3$; marginalizing over Q the estimate of the skewness is $S=6.5\pm8.4\times10^4(\muK)^3$ and marginalizing over n one has $S=6.5\pm8.5\times10^4(\muK)^3$.