The formation of supermassive black holes (MBH) is thought to be tightly linked to the formation and growth of their host galaxy bulges. MBH mass measurements of local galaxies based on stellar or gaseous motion reveal strong correlations of the MBH mass with bulge properties, such as bulge mass, stellar velocity dispersion and light concentration. However, the black hole sample and its covered mass range are limited, revealing an increased scatter for the high and low mass end of the scaling relations. While it is crucial to expand and constrain these regions in order to investigate on the universality of the scaling relations for different galaxy populations and possible different galaxy formation scenarios, the MBH measurements are challenging due to the need of time-expensive (preferable IFU) data and resolution arguments. I present my dynamical MBH measurements of almost 20 galaxies expanding on both the high and low mass end of the scaling relations. For our measurements we made wide use of IFU data, such as SINFONI, NIFS, MUSE, ALMA, and more. We tooks special care in testing dynamical measurement methods on different tracers (stars vs gas) and other systematics. I will also discuss formation scenarios of galaxies harbouring strongly undermassive black holes or possibly no black holes at all. A strong tool to give implications about the formation and growth of MBHs is the analysis of the galaxy's central orbital distributions. I will conclude my talk with a discussion on what we can learn from examining orbital distributions in galaxy evolution and formation context and how measurement uncertainties are affecting our MBH results.