I first review the history of the measurements of non-Gaussianity from the cosmic microwave background anisotropies in the universe over the past two decades. I then present results from recent (2008) work where we found that the bias of dark matter halos takes strong scale dependence in non-Gaussian cosmological models. Therefore, measurements of scale dependence of clustering of galaxies and other tracers, can - and do - constrain primordial non-Gaussianity about two orders of magnitude better than previously thought possible using the large-scale structure. I will discuss prospects for future constraints on non-Gaussianity using this method. I will also present a brief overview of work studying recent claims that the number of high-redshift, high-mass galaxy clusters (the 'pink elephant' clusters) is in disagreement with the standard cosmological model predictions with Gaussian initial conditions.