We use joint likelihood analyses of combinations of fifteen cosmic microwave background ( CMB ) anisotropy data sets from the DMR , UCSB South Pole 1994 , Python I–III , ARGO , MAX 4 and 5 , White Dish , OVRO , and SuZIE experiments to constrain cosmogonies .
We consider open and spatially-flat- \Lambda cold dark matter cosmogonies , with nonrelativistic-mass density parameter \Omega _ { 0 } in the range 0.1–1 , baryonic-mass density parameter \Omega _ { B } in the range ( 0.005–0.029 ) h ^ { -2 } , and age of the universe t _ { 0 } in the range ( 10–20 ) Gyr .

Marginalizing over all parameters but \Omega _ { 0 } , the data favor \Omega _ { 0 } \simeq 0.9–1 ( 0.4–0.6 ) flat- \Lambda ( open ) models .
The range in deduced \Omega _ { 0 } values is partially a consequence of the different combinations of smaller-angular-scale CMB anisotropy data sets used in the analyses , but more significantly a consequence of whether the DMR quadrupole moment is accounted for or ignored in the analysis .
While the open model is difficult to reconcile with the results of less exact analyses of more recent CMB anisotropy data , the lower values of \Omega _ { 0 } found in this case are more easily reconciled with dynamical estimates of this parameter .
For both flat- \Lambda and open models , after marginalizing over all other parameters , a lower \Omega _ { B } h ^ { 2 } \simeq 0.005–0.009 is favored .
This is also marginally at odds with estimates from more recent CMB anisotropy data and some estimates from standard nucleosynthesis theory and observed light element abundances .
For both sets of models a younger universe with t _ { 0 } \simeq 12–15 Gyr is favored , consistent with other recent non-CMB indicators .
We emphasize that since we consider only a small number of data sets , these results are tentative .
More importantly , the analyses here do not rule out the currently favored flat- \Lambda model with \Omega _ { 0 } \sim 0.3 , nor the larger \Omega _ { B } h ^ { 2 } values favored by some other data .