**A** new arXiv entry on ways to approximate marginal likelihoods based on MCMC output, by astronomers (apparently). With an application to the 2015 Planck satellite analysis of cosmic microwave background radiation data, which reminded me of our joint work with the cosmologists of the Paris Institut d’Astrophysique ten years ago. In the literature review, the authors miss several surveys on the approximation of those marginals, including our San Antonio chapter, on Bayes factors approximations, but mention our ABC survey somewhat inappropriately since it is not advocating the use of ABC for such a purpose. (They mention as well variational Bayes approximations, INLA, powered likelihoods, if not nested sampling.)

The proposal of this paper is to identify the marginal *m* [actually denoted *a* there] as the normalising constant of an unnormalised posterior density. And to do so the authors estimate the posterior by a non-parametric approach, namely a k-nearest-neighbour estimate. With the additional twist of producing a sort of Bayesian posterior on the constant *m*. [And the unusual notion of number density, used for the unnormalised posterior.] The Bayesian estimation of m relies on a Poisson sampling assumption on the k-nearest neighbour distribution. (Sort of, since k is actually fixed, not random.)

If the above sounds confusing and imprecise it is because I am myself rather mystified by the whole approach and find it difficult to see the point in this alternative. The Bayesian numerics does not seem to have other purposes than producing a MAP estimate. And using a non-parametric density estimate opens a Pandora box of difficulties, the most obvious one being the curse of dimension(ality). This reminded me of the commented paper of Delyon and Portier where they achieve super-efficient convergence when using a kernel estimator, but with a considerable cost and a similar sensitivity to dimension.

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