Recent progress on our understanding of powerful winds from AGN and their potential for mechanical feedback into the host galaxy will be discussed. In particular, detailed case studies of recent large programs on PDS 456, PG 1211+143 and IRAS F11119+3257 will be presented. In PDS 456, the 2013-2014 XMM-Newton and NuSTAR observations have revealed the presence of a fast (0.3c), wide angle, accretion disk wind, originating from within 100 gravitational radii of the black hole and subtending at least 2 pi steradians in total solid angle. The wind has a high duty cycle, being persistent across all observations and the mechanical power of the wind easily exceeds the nominal 5% of Eddington value postulated in black hole vs galaxy feedback models. Similarly, the Ultra Luminous Infra Red Galaxy, IRAS F11119+3257, was also observed to have a fast and powerful disk wind in recent Suzaku observations, with a total covering factor of at least 80%, while Herschel observations also revealed the presence of a massive molecular outflow in OH. The observations imply that the initial fast disk wind is likely responsible for driving the molecular outflow, observed on the wider scale of the host galaxy, through energy conserving feedback. These two cases, given their overall high bolometric luminosities and wind kinetic powers, may be more representative of the feedback which occurs in higher redshift quasars, at the peak of the quasar epoch. Finally the case of PG 1211+143, which was the prototype example of a non-BAL ultra fast X-ray outflow, will be presented. Recent NuSTAR observations appear to cast doubt on the presence of the accretion disk wind in this quasar. However from a series of XMM-Newton observations in 2014, I instead show that the wind in PG 1211+143 is more intermittent (or inhomogeneous) and that the AGN undergoes a rapid absorption event in the soft X-ray band during the XMM-Newton campaign. Overall the implications of the observations on our understanding of accretion disk winds will be discussed.