COBE-DMR-NORMALIZED OPEN COLD DARK-MATTER COSMOGONIES

Cut-sky orthogonal mode analyses of the COBE-DMR 53 and 90 GHz sky map s are used to determine the normalization of a variety of open cosmogo nical models based on the cold dark matter scenario. To constrain the allowed cosmological parameter range for these open cosmogonies, the p redictions of the DMR-normalized models are compared to various observ ational measures of cosmography and large-scale structure, viz., the a ge of the universe; small-scale dynamical estimates of the clustered-m ass density parameter Omega(0); constraints on the Hubble parameter h, the X-ray cluster baryonic-mass fraction Omega(B)/Omega(0), and the m atter power spectrum shape parameter; estimates of the mass perturbati on amplitude; and constraints on the large-scale peculiar velocity hel d. The open-bubble inflation model (Ratra & Peebles; Bucher, Goldhaber , & Turok; Yamamoto, Sasaki, & Tanaka) is consistent with current dete rminations of the 95% confidence level (c.l.) range of these observati onal constraints, provided 0.3 < Omega(0) less than or similar to 0.6 (similar to 95% c.l.). More specifically, for a range of h, the model is reasonably consistent with recent high-redshift estimates of the de uterium abundance that suggest Omega(B)h(2) similar to 0.007, provided Omega(0) similar to 0.35; recent high-redshift estimates of the deute rium abundance that suggest Omega(B)h(2) similar to 0.02 favor Omega(0 ) similar to 0.5, while the old nucleosynthesis value Omega(B)h(2) = 0 .0125 requires Omega(0) similar to 0.4. Small shifts in the inferred C OBE-DMR normalization amplitudes due to (1) the small differences betw een the galactic-and ecliptic-coordinate sky maps, (2) the inclusion o r exclusion of the quadrupole moment in the analysis, (3) the faint hi gh-latitude Galactic emission treatment, and (4) the dependence of the theoretical cosmic microwave background anisotropy angular spectral s hape on the value of h and Omega(B), are explicitly quantified. Corres ponding variations in the likelihood fits of models to the DMR data th en imply that the DMR data alone do not possess sufficient discriminat ive power to prefer any values for Omega(0), h, or Omega(B), at the 95 % c.l. for the models considered. At a lower c.l., and when the quadru pole moment is included in the analysis, the DMR data are most consist ent with either Omega(0) less than or similar to 0.1 or Omega(0) simil ar to 0.7 (depending on the model considered). However, when the quadr upole moment is excluded from the analysis, the DMR data are most cons istent with Omega(0) similar to 0.35-0.5 in all open models considered (with 0.1 less than or equal to Omega(0) less than or equal to, 1), i ncluding the open-bubble inflation model. Earlier claims (Yamamoto & B unn; Bunn & White) that the DMR data require a 95% c.l. lower bound on Omega(0) (similar to 0.3) are not supported by our (complete) analysi s of the 4 year data: the DMR data alone cannot be used to constrain O mega(0) meaningfully.