Primordial Nucleosynthesis with CMB Inputs: Probing the Early Universe and Light Element Astrophysics

Details Primordial Nucleosynthesis with CMB Inputs: Probing the Early Universe and Light Element Astrophysics Primordial Nucleosynthesis with CMB Inputs: Probing the Early Universe and Light Element Astrophysics

2001-05-22

arxiv.org/abs/astro-ph/0105397v1

Astropart.Phys.17:87-100,2002

Astronomy and Astrophysics

Astrophysics

17 pages, 13 figures, plain LaTeX

Scientific paper

10.1016/S0927-6505(01)00171-2

Cosmic microwave background (CMB) determinations of the baryon-to-photon ratio $\eta \propto \Omega_{\rm baryon} h^2$ will remove the last free parameter from (standard) big bang nucleosynthesis (BBN) calculations. This will make BBN a much sharper probe of early universe physics, for example, greatly refining the BBN measurement of the effective number of light neutrino species, $N_{\nu,eff}$. We show how the CMB can improve this limit, given current light element data. Moreover, it will become possible to constrain $N_{\nu,eff}$ independent of \he4, by using other elements, notably deuterium; this will allow for sharper limits and tests of systematics. For example, a 3% measurement of $\eta$, together with a 10% (3%) measurement of primordial D/H, can measure $N_{\nu,eff}$ to a 95% confidence level of $\sigma_{95%}(N_\nu) = 1.8$ (1.0) if $\eta \sim 6.0\times 10^{-10}$. If instead, one adopts the standard model value $N_{\nu,eff}=3$, then one can use $\eta$ (and its uncertainty) from the CMB to make accurate predictions for the primordial abundances. These determinations can in turn become key inputs in the nucleosynthesis history (chemical evolution) of galaxies thereby placing constraints on such models.

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