The Data for 'Non-thermal Ionization of Kilonova Ejecta: Observable Impacts'

Produced synthetic kilonova spectra for 'Non-thermal Ionization of Kilonova Ejecta: Observable Impacts' 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 simulations 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 (seconds) time_edges - Edges of time bins (seconds) Each kilonova spectra file is named according to QNLTE_n<#>_toy_KN_<lanthanide fraction>X_lan_<characteristic velocity>v_<mass>M_1D_spec_final.h5 where: # represents the index of the outer power law of the density profile (the inner index is always 1) 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