Abstract
Since the baryon-to-photon ratio η 10 is in some doubt at present, we ignore the constraints on η 10 from big bang nucleosynthesis (BBN) and fit the three key cosmological parameters (h, ΩM, η 10) to four other observational constraints: Hubble parameter (h o), age of the universe (t o), cluster gas (baryon) fraction (f o ≡ f G h 3/2), and effective shape parameter (Γ0). We consider open and flat CDM models and flat ∧CDM models, testing goodness of fit and drawing confidence regions by the Δχ2 method. CDM models with Ωm = 1 (SCDM models) are accepted only because we allow a large error on h o, permitting h < 0.5. Open CDM models are accepted only for ΩM ≳0.4. ∧CDM models give similar results. In all of these models, large η l0(≳ 6) is favored strongly over small η 10(≲2), supporting reports of low deuterium abundances on some QSO lines of sight, and suggesting that observational determinations of primordial 4He may be contaminated by systematic errors. Only if we drop the crucial Γ0. constraint are much lower values of ΩM and η 10 permitted.
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Steigman, G., Hata, N., Felten, J.E. (1998). Non-BBN Constraints on the Key Cosmological Parameters. In: Prantzos, N., Tosi, M., Von Steiger, R. (eds) Primordial Nuclei and Their Galactic Evolution. Space Sciences Series of ISSI, vol 4. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-5116-0_3
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