BOSS + eBOSS galaxy clustering favors a featureless, quasi-scale-invariant primordial spectrum, with a reconstructed spectral index n_s = 0.976 ± 0.021.
On the Dependence of the Spectra of Fluctuations in Inflationary Cosmology on Trans-Planckian Physics
3 Pith papers cite this work, alongside 218 external citations. Polarity classification is still indexing.
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abstract
We calculate the power spectrum of metric fluctuations in inflationary cosmology starting with initial conditions which are imposed mode by mode when the wavelength equals some critical length $\ell_{_{\rm C}}$ corresponding to a new energy scale $M_{_{\rm C}}$ at which trans-Planckian physics becomes important. In this case, the power spectrum can differ from what is calculated in the usual framework (which amounts to choosing the adiabatic vacuum state). The fractional difference in the results depends on the ratio $\sigma_0$ between the Hubble expansion rate $H_{\rm inf}$ during inflation and the new energy scale $M_{_{\rm C}}$. We show how and why different choices of the initial vacuum state (stemming from different assumptions about trans-Planckian physics) lead to fractional differences which depend on different powers of $\sigma_0$. As we emphasize, the power in general also depends on whether one is calculating the power spectrum of density fluctuations or of gravitational waves.
fields
astro-ph.CO 3years
2026 3representative citing papers
Using combined CMB and LSS observations, the analysis sets 95% CL upper limits on oscillatory amplitudes at approximately 2% of A_s and a MAP value of 0.034 for the particle production coupling constant, finding no statistical preference for the extended models.
Finite recombination thickness introduces Gaussian smoothing in ln k to the primordial power spectrum, producing non-trivial differences between TT and EE spectral indices that may be detectable in future CMB data.
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Primordial power spectrum reconstructions from BOSS + eBOSS
BOSS + eBOSS galaxy clustering favors a featureless, quasi-scale-invariant primordial spectrum, with a reconstructed spectral index n_s = 0.976 ± 0.021.
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Constraining primordial oscillations and inflationary particle production with Planck, ACT DR6, and DESI DR2
Using combined CMB and LSS observations, the analysis sets 95% CL upper limits on oscillatory amplitudes at approximately 2% of A_s and a MAP value of 0.034 for the particle production coupling constant, finding no statistical preference for the extended models.
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Recombination Thickness as an Uncertainty in Inflationary Observables
Finite recombination thickness introduces Gaussian smoothing in ln k to the primordial power spectrum, producing non-trivial differences between TT and EE spectral indices that may be detectable in future CMB data.