We introduce a new quantity , the mass flux density of galaxies evolving from the blue sequence to the red sequence .
We propose a simple technique for constraining this mass flux using the volume corrected number density in the extinction-corrected UV-optical color magnitude distribution , the stellar age indexes  H \delta _ { A }  and  D _ { n } ( 4000 )  , and a simple prescription for spectral evolution using a quenched star formation history .
We exploit the excellent separation of red and blue sequences in the NUV-r band Hess function .
The final value we measure , \dot { \rho _ { T } } = 0.033 M _ { \odot } yr ^ { -1 } Mpc ^ { -3 } , is strictly speaking an upper limit due to the possible contributions of bursting , composite , and extincted galaxies .
However , it compares favorably with estimates of the average mass flux that we make based on the red luminosity function evolution derived from the DEEPII and COMBO-17 surveys ( 8 ; 12 ) , \dot { \rho } _ { R } = +0.034 M _ { \odot } yr ^ { -1 } Mpc ^ { -3 } .
We find that the blue sequence mass has remained roughly constant since z=1 ( \dot { \rho _ { B } } \simeq 0.01 M _ { \odot } yr ^ { -1 } Mpc ^ { -3 } , but the average on-going star formation of \dot { \rho } _ { SF } \simeq 0.037 M _ { \odot } yr ^ { -1 } Mpc ^ { -3 } over 0 < z < 1 is balanced by mass flux off the blue sequence .
We explore the nature of the galaxies in the transition zone with particular attention to the frequency and impact of AGNs .
The AGN fraction peaks in the transition zone .
We find circumstantial , albeit weak evidence that the quench rates are higher in higher luminosity AGNs .