A lunar array needs at least ~30,000 Fourier modes and distributed stations to reach σ(α_s)=0.034 on inflation, competitive with Planck, though thermal noise limits high-redshift small-scale access.
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Upper bounds on the dark matter fraction in MACHOs of 10^3 to 10^7 solar masses are derived from limits on distortions to the global 21-cm signal at z~17, z~89, and z>300.
Neutrino invisible decays and a boomerang mechanism transferring particles between visible and dark sectors could resolve cosmological anomalies while predicting an observable effective magnetic moment.
citing papers explorer
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A Designer's Guide to Lunar Far-Side Interferometer Array: Power Spectrum Measurement and Cosmological Constraints from the Dark Ages
A lunar array needs at least ~30,000 Fourier modes and distributed stations to reach σ(α_s)=0.034 on inflation, competitive with Planck, though thermal noise limits high-redshift small-scale access.
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Dark ages bounds on non-accreting massive compact halo objects
Upper bounds on the dark matter fraction in MACHOs of 10^3 to 10^7 solar masses are derived from limits on distortions to the global 21-cm signal at z~17, z~89, and z>300.
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How neutrinos could help solving cosmological anomalies and tensions
Neutrino invisible decays and a boomerang mechanism transferring particles between visible and dark sectors could resolve cosmological anomalies while predicting an observable effective magnetic moment.