AGN spins, where the AGNs were selected by mass and Eddington ratio. Triangles: MBH masses . Squares: MBH masses . Top: QSOs accreting at the high accretion rate (in Eddington units) f _Edd > 0.1. Bottom: AGNs accreting at all accretion rates f _Edd > 0.001. Left: chaotic accretion during the decline of the quasar phase. Right: coherent accretion during the decline of the quasar phase. The signature of feedback in the angular momentum of nuclear gas is strongest in high mass MBHs (compare the right and left panels). In general, AGN spins tend to decrease at late cosmic times.