X iv : a st ro - p h / 98 05 32 6 v 2 1 0 A ug 1 99 8 The Cosmic Microwave Background and Observational Convergence in the Ω m − Ω Λ Plane

ar X iv : a st ro - p h / 98 05 32 6 v 1 2 7 M ay 1 99 8 The Cosmic Microwave Background and Observational Convergence in the Ω m − Ω Λ Plane

I use the most recent cosmic microwave background (CMB) anisotropy measurements to constrain the leading cold dark matter models in the Ωm − ΩΛ plane. A narrow triangular region is preferred. This triangle is elongated in such a way that its intersection with even conservative versions of recent supernovae, cluster mass-to-light ratios and double radio source constraints, is small and provides ...

ar X iv : a st ro - p h / 98 04 15 8 v 1 1 6 A pr 1 99 8 Constraints on Cosmological Parameters from Existing CMB Data

We use current cosmic microwave background data to constrain cosmological parameters. The results are presented as confidence regions in the (Ω–Ho) – plane for both open and flat geometries, and are based on a χ 2 minimization to the power spectrum. Although such an approach does not strictly apply to power spectrum estimates, the results should nonetheless be indicative. We find that purely op...

ar X iv : a st ro - p h / 99 01 30 3 v 1 2 1 Ja n 19 99 Combining Supernovae and LSS Information with the CMB

Observations of the Cosmic Microwave Background (CMB), large scale structure (LSS) and standard candles such as Type 1a Supernovae (SN) each place different constraints on the values of cosmological parameters. We assume an inflationary Cold Dark Matter model with a cosmological constant, in which the initial density perturbations in the universe are adiabatic. We discuss the parameter degenera...

X iv : a st ro - p h / 98 05 25 2 v 1 1 9 M ay 1 99 8 Open Universes , Inflation , and the Anthropic Principle ∗

Models of open inflation with a variable density parameter Ω provide the most natural way to reconcile an open universe with inflation. The use of anthropic principle is essential to derive observational predictions of such models. I discuss how this principle can be used in a quantitative way to determine the most probable value of Ω. I also comment on recent work by Hawking and Turok on quant...

ar X iv : a st ro - p h / 99 02 29 8 v 2 1 3 A pr 1 99 9 New limits on Ω Λ and Ω M from old galaxies at high redshift