We rederive the relation between the specific angular momentum j _ { \star } and the mass M _ { \star } of the stellar matter in galaxies of different morphological types .
This is a revision of the j _ { \star } – M _ { \star } diagram presented in our recent comprehensive study of galactic angular momentum .
In that work , we estimated j _ { \star } from kinematic and photometric data that extended to large radii and M _ { \star } from near-infrared luminosities L _ { K } with an assumed universal mass-to-light ratio M _ { \star } / L _ { K } .
However , recent stellar population models show large variations in M _ { \star } / L _ { K } correlated with B - V color .
In the present work , we use this correlation to estimate M _ { \star } / L _ { K } and hence M _ { \star } from the measured B - V and L _ { K } .
Our revised j _ { \star } – M _ { \star } diagram is similar to our previous one ; both disk-dominated and elliptical galaxies follow nearly parallel sequences with j _ { \star } \propto M _ { \star } ^ { \alpha } and \alpha = 0.6 \pm 0.1 .
However , the offset between the sequences is now a factor of about 5 , some 30 % larger than before ( and close to the offset found by Fall in 1983 ) .
Thus , our new results place even tighter constraints on the loss of specific angular momentum by galactic disks over their lifetimes .