Pure-Hydrogen White Dwarf Models ("WD-GRID")

NLTE calculations of hot white dwarf (WD) model atmospheres are the cornerstone of modern flux calibrations for the Hubble Space Telescope (HST) and for the CALSPEC database. These theoretical spectral energy distributions (SEDs) provide the relative flux vs. wavelength, and only the absolute flux level remains to be set by reconciling the measured absolute flux of Vega in the visible with the Midcourse Space Experiment (MSX) values for Sirius in the mid-IR. The most recent SEDs calculated by the tlusty and tmap NLTE model atmosphere codes for the primary WDs G191B2B, GD153, and GD71 show improved agreement to 1% from 1500 Angstroms to 30 microns, in comparison to the previous 1% consistency only from 2000 Angstroms to 5 microns. These new NLTE models of hot WDs now provide consistent flux standards from the FUV to the mid-IR. Model grids from both the TLUSTY207 and TMAP2019 NLTE software codes are presented across a range of stellar parameters. Both grids contain 132 models with effective temperature (T_eff) in the range 20,000 - 95,000 K and gravity (logg) between 7.0 and 9.5, with six steps of 0.5. The steps in T_eff are 2,000 K between 20,000 and 40,000 K and 5,000 K between 40,000 and 95,000 K. The wavelengths are presented in Angstroms, measured in vaccuum. The fluxes are Eddington fluxes, with different conversions for the two model sets to needed to convert to physical fluxes. See the Bohlin et al. 2020 paper for important information on how to use and convert the fluxes from these models.