The discordance between ‘ low ’ and ‘ high ’ primordial D/H measurements can be considerably reduced if the analysis of the H+D profiles accounts for the correlated velocity field of bulk motion .
We have re-estimated the value of D/H at z = 3.572 towards Q1937–1009 ( ‘ low ’ D/H = ( 3.3 \pm 0.3 ) \times 10 ^ { -5 } [ 3 ] ) and at z = 0.701 towards Q1718+4807 ( ‘ high ’ D/H = ( 2.0 \pm 0.5 ) \times 10 ^ { -4 } [ 15 ] ) and found that a single D/H value from the range ( 3.5 - 5.2 ) \times 10 ^ { -5 } ( 2 \sigma C.L . )
is sufficient to describe both spectra .
This result supports homogeneous models of BBN .
The obtained D/H ratio and the measurements of high ^ { 4 } He abundance in extra-galactic H II regions [ 5 ] and ^ { 7 } Li abundance in metal-poor halo stars [ 2 ] are consistent , within the errors , with the predictions of standard BBN for 3.6 \leq \eta _ { 10 } \leq 5.4 , which corresponds to 0.013 \leq \Omega _ { b } h ^ { 2 } _ { 100 } \leq 0.020 .