CHICAGO — The 2020 MQ cosmology paper proposed geometric interpretations of selected cosmic microwave background features. Its treatment of observational domains and peak coordinates opened a research direction that later source material develops as an exploration of geometry, rather than a completed calculation of the microwave sky.

The current CMB preprint makes the distinction explicit. Domain fractions describe referenceability relative to an observer under MQ premises. Candidate coordinates add prescriptions for locating possible features. Neither step alone specifies the temperature-power height, width or correlation of an observed acoustic peak. Figure 1 separates the three tasks.

The distinction matters for the dark-domain coordinate. The current construction gives a dimensionless index near 214.766864. Its numerical proximity to an angular feature does not establish a detected dark-domain peak. A directly received CMB signal belongs to the observable description, while the MQ dark domain is defined as never observable relative to the specified observer.

Other candidate positions use a metric differential factor with an explicitly stated direction of rescaling. The current manuscript leaves the coordinate-to-multipole correspondence and power normalization to be established. Its public introductory graphic projects numerical markers under declared conventions; those markers are not independently measured MQ peaks or a fitted MQ temperature spectrum.

A full CMB test requires more than selected positions. The evolution of radiation, matter and metric perturbations determines the temperature and polarization signals, while propagation, lensing, foregrounds, instrumental effects and covariance enter their comparison with observations. The current sources do not establish a completed joint numerical spectrum likelihood for MQ.

Mean CMB temperature and radiation-density consistency belong to a different level of comparison. They do not predict angular correlations simply because they describe the same radiation background. Likewise, similar numerical values for MQ domain fractions and conventional cosmological density parameters do not establish identical physical definitions.

The companion Brief supplies the domain equations, a reproducible coordinate table and two explanatory graphics. It distinguishes the historical publication from later calibration and terminology, and identifies the further physical mapping required before a peak claim can become a quantitative sky-spectrum test.

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