Solar dynamics at high latitudes and deep in the convection zone

For a long time, helioseismic inferences have provided a window into the solar interior. In the last two decades, the development of local helioseismology tools has extended the capability of helioseismology by allowing the study of localized structure changes and dynamics. In particular, it has revealed the subsurface flows and its variation throughout the solar cycle. Both the torsional oscillation and the meridional circulation present interesting patterns leading to solar cycle 24, which continue during the onset of this cycle. Yet, many questions related to the behavior of such flows at high latitudes as well as deep down in the convection zone that are key to solar dynamo models remain unanswered. Long-term helioseismic studies using both Global Oscillation Network Group (GONG) and Michelson Doppler Imager (MDI)data have uncovered the difficulties of properly interpreting data far from disk center due to systematics and solar effects, limiting the helioseismic inferences to only specific areas. The Helioseismic and Magnetic Imager (HMI) instrument on board the Solar Dynamics Observatory (SDO) provides an excellent opportunity to explore the until now unreachable territories thanks to its higher resolution. In addition, newly available artificial data sets offer an unprecedented opportunity for disentangling and modeling the different effects. We present here a review of the main features observed in the subsurface flows in the recent years and discuss future plans to extend the inferences at higher latitudes and deep down in the convection zone.