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\section{Initial Conditions}
\subsection{Non-neutrino Physics}
\begin{enumerate}
\item Progenitor: $20\,M_\odot$ model from \cite{2015arXiv151004643S}. This model is publicly available from \url{http://www.ucolick.org/~sukhbold/#iii}, and as stated on this website, will be available from ApJ after publication. This openly available, up to date progenitor model is ideal for this study.
\item For mapping the progenitor, we will use density, temperature, and ye. Careful to note the definition of the radial coordinate in the initial model (radial coordinate is the location of the outer edge of the zone, the velocity is also defined at this radius, the remaining required quantities (rho, temperature, ye) are defined as cell averages).
\item Equation of state: The SFHo nuclear equation of state from \cite{Steiner_2013} available from \url{http://phys-merger.physik.unibas.ch/~hempel/eos.html} or \url{http://www.stellarcollapse.org/equationofstate}. This EOS extends down to densities of $1\,\mathrm{g}\,\mathrm{cm}^{-3}$. In this EOS, NSE is assumed down to these densities (which is incorrect for supernovae). However, to eliminate (for now) issues related to low density equations of state and nuclear reaction networks, this study will use only the SFHo equation of state for all densities, temperatures, and ye's.
\item Boundary and Boundary Conditions: The SFHo EOS only goes down to $0.1\,$MeV, therefore the outer boundary must be closer than $1.2\times 10^9\,\mathrm{cm}$. For this comparison, we would like the outer boundary to be taken as $10^9\,\mathrm{cm}$. For the outer boundary conditions, fix the density and velocity so as to maintain a constant mass accretion rate. This is not the most physical boundary condition, but ensures the same condition is used by different groups.
\item For multidimensional simulations, do collapse in 1D up to 15\,ms after bounce, then transition to 2D. Add perturbations via a clearly defined manner.
\item Perform simulations using both Newtonian gravity and some form of general relativistic gravity (either effective potential, true GR).
\end{enumerate}
\subsection{Neutrino Physics}
\begin{enumerate}
\item Use three species, $\nu_e$, $\bar{\nu}_e$, and $\nu_x = \{\nu_\mu$ $\bar{\nu}_\mu$, $\nu_\tau$, and $\bar{\nu}_\tau\}$.
\item Use a clearly defined energy bin structure.
\item The SFHo EOS contains light clusters. For this study, all neutrino interactions (both absorption and scattering) on light clusters is ignored.
\item For scattering on free nucleons, use the \cite{Bruenn_1985} rates. Include weak magnetism and recoil corrections via \cite{Horowitz_2002}.
\item For scattering on heavy nuclei, use the \cite{Bruenn_1985} rate, include corrections via \cite{Burrows_2006}: Ion-ion correlations, electron polarization correction, and a correction for the nuclear form factor.
\item Include inelastic neutrino-electron scattering only in 1D simulations. This will include inelastic scattering during the collapse phase of 2D simulations as up to 15ms postbounce will be done in 1D.
\item For pair processes, include electron-positron annihilation to neutrino pairs (and the reverse). Ignore all other pair processes, nucleon-nucleon Bremsstrahlung and neutrino pair conversion to other neutrino pairs.
\item Use \cite{Bruenn_1985} rates for absorption rates (on nucleons and nuclei). Include weak magnetism and recoil corrections for nucleon rates. Do not include any nucleon potentials.
\end{enumerate}
