Paper plan

Section 1: introduction

• why model supernovae
• need RT
• various considerations: accuracy vs speed
• atomic physics vs detailed explosions models (dimensionality)
• this paper: want to compare various approximations that are made and establish how good/bad some of the common simplifying assumptions are
• nebular approximation, LTE excitation assumption, choice of atomic data, treatment of non-resonance scattering

Section 2:

• methods
• introduce "radiation field model" - J = B [LTE], J = W B [nebular approximation], J = ? [NLTE]
• introduce the code
• keep brief and to the point (refer lots to Lucy papers)
• idea of a simple but flexible and modular approach - will be public and available to build on

Section 3

• atomic input
• source of atomic data (how it's arranged/stored?)
• processes treated

Section 4:

• simple code tests
• pure Si atmosphere - compared to Synow
• pure Fe?
• other tests - parameters similar to one of the abundance tomography cases?
• Lucy 99 parameters?

Section 5: results

• 5.1 reference calculation
• 5.2 treatment of non-resonance scattering - macro atom vs down brach vs pure scattering (mostly a duplication of the Lucy 99 discussion except we have the full macro atom to compare too)
• 5.3 full NLTE for Si, Ca, S? [combinations thereof?] versus, LTE excitation and versus NLTE with Jblues from rad. field model. [the above is giving us for 1 model, with 1 set of atomic data: a grid of 3 x 3 sets of assumptions: [macro atom, down branch, pure scattering] x [full NLTE, NLTE+from rad. field model, LTE] ]