... coefficients

The masking coefficient is simply 1 in regions kept for power spectrum computations, 0 in regions masked, and between 0 and 1 in the transitions.

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... sizes)

Small patches contain few modes, hence empirical correlations are stronger, as discussed in Appendix A.

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... emission

In reality, it is likely that the CMB map actually is somewhat correlated to the foreground emissions (extragalactic point sources and SZ effect), because of the ISW effect. The implication of this is not studied further in the present paper.

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... exact

Or almost exact, for all practical purposes.

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... channel

A noise weighted average beam is obtained from the W1 W2 W3 W4 beam coefficients provided by the WMAP team.

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... options

See http://www.apc.univ-paris7.fr/APC_CS/Recherche/Adamis/ in the ``outreach'' section.

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... site

http://www.apc.univ-paris7.fr/APC_CS/Recherche/Adamis/cmb_wmap-en.php

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... Model

http://www.apc.univ-paris7.fr/APC_CS/Recherche/Adamis/PSM/psky-en.php

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...

We warn the reader that some authors fail to make a clear distinction between the statistical (ensemble average) correlation, which is a deterministic quantity, and the ``empirical correlations'' computed, assuming some kind of ergodicity, as averages over finite sets of samples as in Eq. (A.3).

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... anisotropies

Certainly the CMB is not correlated to galactic components. Small correlations with large scale structure, and hence with SZ effect and emission from outer galaxies, may exist because of the integrated Sachs-Wolfe effect. We neglect this effect in the present discussion.

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