Cut-sky orthogonal mode analyses of the COBE -DMR 53 and 90 GHz sky maps are used to determine the normalization of a variety of open cosmogonical models based on the cold dark matter scenario .
To constrain the allowed cosmological-parameter range for these open cosmogonies , the predictions of the DMR-normalized models are compared to various observational measures of cosmography and large-scale structure , viz .
: the age of the universe ; small-scale dynamical estimates of the clustered-mass density parameter \Omega _ { 0 } ; constraints on the Hubble parameter h , the X-ray cluster baryonic-mass fraction \Omega _ { B } / \Omega _ { 0 } , and the matter power spectrum shape parameter ; estimates of the mass perturbation amplitude ; and constraints on the large-scale peculiar velocity field .

The open-bubble inflation model ( Ratra & Peebles 1994 ; Bucher , Goldhaber , & Turok 1995 ; Yamamoto , Sasaki , & Tanaka 1995 ) is consistent with current determinations of the 95 % confidence level ( c.l . )
range of these observational constraints .
More specifically , for a range of h , the model is reasonably consistent with recent high-redshift estimates of the deuterium abundance which suggest \Omega _ { B } h ^ { 2 } \sim 0.007 , provided \Omega _ { 0 } \sim 0.35 ; recent high-redshift estimates of the deuterium abundance which suggest \Omega _ { B } h ^ { 2 } \sim 0.02 favour \Omega _ { 0 } \sim 0.5 , while the old nucleosynthesis value \Omega _ { B } h ^ { 2 } = 0.0125 requires \Omega _ { 0 } \sim 0.4 .

Small shifts in the inferred COBE -DMR normalization amplitudes due to : ( 1 ) the small differences between the galactic- and ecliptic-coordinate sky maps , ( 2 ) the inclusion or exclusion of the quadrupole moment in the analysis , ( 3 ) the faint high-latitude Galactic emission treatment , and , ( 4 ) the dependence of the theoretical cosmic microwave background anisotropy angular spectral shape on the value of h and \Omega _ { B } , are explicitly quantified .

The DMR data alone do not possess sufficient discriminative 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 quadrupole moment is included in the analysis , the DMR data are most consistent with either \Omega _ { 0 } { } _ { \sim } ^ { < } 0.1 or \Omega _ { 0 } \sim 0.7 ( depending on the model considered ) .
However , when the quadrupole moment is excluded from the analysis , the DMR data are most consistent with \Omega _ { 0 } \sim 0.35 - 0.5 in all open models considered ( with 0.1 \leq \Omega _ { 0 } \leq 1 ) , including the open-bubble inflation model .
Earlier claims ( Yamamoto & Bunn 1996 ; Bunn & White 1996 ) that the DMR data require a 95 % c.l .
lower bound on \Omega _ { 0 } ( \sim 0.3 ) are not supported by our ( complete ) analysis of the four-year data : the DMR data alone can not be used to meaningfully constrain \Omega _ { 0 } .