The Data for 'Impact of Systematic Modeling Uncertainties on Kilonova Property Estimation'

Produced synthetic kilonova spectra for 'Impact of Systematic Modeling Uncertainties on Kilonova Property Estimation' using the Sedona radiative transfer code. Each model is an h5 file with the following groups:

• Lnu - Array of length # of timesteps by # of frequency bins that contains the spectral sequence of each kilonova model in cgs units (erg/s/Hz)
• click - Array of length # of timesteps by # of frequency bins for the number of Monte Carlo particles that make up Lnu
• mu - Center of polar angular bins (not useful since simulations are 1D)
• mu_edges - Edges of polar angular bins (not useful since simualtions are 1D)
• nu - Array of length # of frequency bins that are the central frequencies of a bin (Hz)
• nu_edges - Array of length # of frequency bins +1 that are the edges of each frequency bin (Hz)
• phi - Center of azimuthal angular bins (not useful since simulations are 1D)
• phi_edges - Edges of azimuthal angular bins (not useful since simulations are 1D)
• time - Times at which each spectrum was generated (Days)
• time_edges - Edges of time bins (Days)

Each kilonova spectra file is named according to <atomic dataset>_<thermalization prescription>_KN_<lanthanide fraction>X_lan_<characteristic velocity>v_<mass>M_1D_spec.h5 where:

• atomic dataset is one of: HULLAC, ATOMIC, or Autostructure
• thermalization prescription is one of: local or global
• lanthanide fraction is the fraction of lanthanides in the ejecta by mass
• characteristic velocity is the kinetic velocity of the ejecta in units of the speed of light
• mass is the mass of the ejecta in units of solar masses