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\section{Steady vs Eruptive Massloss}  To help constrain mass-loss theory, we first need to understand the mass-loss history of massive stars. In particular, we need to know the mass-loss rate ($\dot{M}$) and velocity as a function of time before explosion.    The mass loss rates during the last few hundred years of evolution of some core collapse supernova progenitors seem to violate the maximum values allowed by line-driven winds \citep[$\dot{M} \sim 10^{-4}$M$_\odot$yr$^{-1}$][see also Fig.~\ref{fig}]{Smith_2006}. 10^{-4}$M$_\odot$yr$^{-1}$][]{Smith_2006}.  %($\dot{M} \sim 10^{-4}$M$_\odot$yr$^{-1}$, \citet{Smith_2006}, see also Fig.~\ref{fig}).   Intense stellar mass loss during the final years before core collapse could be caused by