Grid of 3D pure-hydrogen NLTE synthetic spectra

Separate files for log (g) = 5.0, 5.5, 6.0, 6.5, 7.0, 7.5, 8.0, 8.5, 9.0
Grids below log(g) = 7.0 have a different Teff range.

Each model atmosphere was spatially and temporally averaged before calculating
the mean 3D spectra.

1D LTE(<40,000 K) is used outside of the range of the published 3D model grid (see references).
The grid can be appended with 1D NLTE models (>40,000 K) also available on the website 
https://warwick.ac.uk/fac/sci/physics/research/astro/people/tremblay/modelgrids/
NLTE corrections for line cores <20,000 K at high spectroscopic resolution 
are available upon request to the authors.

File format:

 1) Grid of 3747 (6787 from log(g)=7.0 and above) wavelength points in Angstrom
 2) For each model at fixed gravity
    Header
    "Effective temperature =   [value]  gravity =  [value]  y =  0.000E+00"
    Grid of 3747 (6787) Fnu Eddington fluxes in air wavelength 
    (units of erg cm^-2 s^-1 Hz^-1)

Files with H2 molecular lines have instead 62557 wavelength points and are for log(g)>7.0 only.

Main references
Tremblay, P.-E., Ludwig, H.-G., Steffen, M. & Freytag, B. (2013) A&A, 559, A104.
Tremblay, P.-E., Gianninas, A., Kilic, M., et al. (2015) ApJ, 809, 148.

With line profiles from
Tremblay, P.-E. & Bergeron, P. (2009) ApJ, 696, 1755.

Conversion:

The flux at Earth is f = 4*pi*R^2/D^2 * Eddington flux

where R is the white dwarf radius, D the distance and the Eddington flux 
the quantity in the files. The radius can be found from Evolutionary Sequences.
There are several sources including the website below
https://www.astro.umontreal.ca/~bergeron/CoolingModels/

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Physics included in the calculations:

3D hydrodynamics convection
Freytag, B. et al. 2012, JCoPh, 231, 919
Tremblay, P.-E., Ludwig, H.-G., Steffen, M. & Freytag, B. (2013) A&A, 559, A104.
Tremblay, P.-E., Gianninas, A., Kilic, M., et al. (2015) ApJ, 809, 148.

Non-ideal effects from charged and neutral particles 
Hummer, D.G. and Mihalas, D. 1988, ApJ, 331, 794
(Bohr radii of H I and H2 have a free parameter of 0.5; see Tremblay et al. 2010, ApJ, 712, 1345)

H2 molecular lines - *Included optionally in one high-res version of the grid*
Hubeny I., Allende Prieto C., Osorio Y., Lanz T., 2021, arXiv, arXiv:2104.02829

Lyman, Balmer, Paschen, Brackett lines profiles (extended to a total of 60 lines in 2015)
Tremblay, P.-E. & Bergeron, P. (2009) ApJ, 696, 1755

Hydrogen neutral broadening profiles for Lyman alpha, beta, gamma and delta
Allard, N. 2014, public website (https://www.iap.fr/useriap/allard/lymantables.html)
Broadening due to charged particles for these lines is treated from the Tremblay+2009 reference above.

Hydrogen neutral broadening profiles for Lyman alpha from H2-H and H-H collisions
Kowalski, P. M., Saumon D. 2006, ApJ, 651, L137

H2 collision-induced absorption (including high-density corrections from Hare & Welsh 1958)
H2-H2 from Borysow et al. (2001, JQSRT, 68, 235)
H2-H from Hitran database (http://hitran.org/cia/)

H minus bf and ff opacity
John, T. L. 1988, A&A, 193, 189

H2 minus ff opacity
H2+ bf and ff opacity
H bf opacity (>972 Angstrom Hummer & Mihalas pseudo-continuum cut)
H, H2 and H3 ff opacity
Stimulated emission
H, H2 Rayleigh scattering
(Standard references, e.g. Mihalas 1978 Stellar Atmospheres book and Kurucz 1970, Atlas: A Computer Program)