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.
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