Volume 556, August 2013
|Number of page(s)||16|
|Section||Cosmology (including clusters of galaxies)|
|Published online||30 July 2013|
A quasi-Gaussian approximation for the probability distribution of correlation functions ⋆
Argelander-Institut für Astronomie, Universität Bonn,
Auf dem Hügel 71,
e-mail: email@example.com; firstname.lastname@example.org
Accepted: 1 July 2013
Context. Whenever correlation functions are used for inference about cosmological parameters in the context of a Bayesian analysis, the likelihood function of correlation functions needs to be known. Usually, it is approximated as a multivariate Gaussian, though this is not necessarily a good approximation.
Aims. We show how to calculate a better approximation for the probability distribution of correlation functions of one-dimensional random fields, which we call “quasi-Gaussian”.
Methods. Using the exact univariate probability distribution function (PDF) as well as constraints on correlation functions previously derived, we transform the correlation functions to an unconstrained variable for which the Gaussian approximation is well justified. From this Gaussian in the transformed space, we obtain the quasi-Gaussian PDF. The two approximations for the probability distributions are compared to the “true” distribution as obtained from simulations. Additionally, we test how the new approximation performs when used as likelihood in a toy-model Bayesian analysis.
Results. The quasi-Gaussian PDF agrees very well with the PDF obtained from simulations; in particular, it provides a significantly better description than a straightforward copula approach. In a simple toy-model likelihood analysis, it yields noticeably different results than the Gaussian likelihood, indicating its possible impact on cosmological parameter estimation.
Key words: methods: statistical / cosmological parameters / large-scale structure of Universe / galaxies: statistics / cosmology: miscellaneous
Appendices are available in electronic form at http://www.aanda.org
© ESO, 2013
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