"BOSZ" stellar atmosphere models are based on ATLAS-APOGEE ATLAS9 (Mészáros et al. 2012) and cover a broad range of effective temperature, surface gravity, metallicity, carbon abundance, and alpha-element abundance. Versions at different instrumental broadenings are provided. See the table in the description section for parameter ranges. Our new BOSZ LTE models have been fit to O,B,A,F,G stars observed with HST/STIS, and those results are compared to fits for the LTE grid from Castelli & Kurucz (2004). The name "BOSZ" comes from a combination of letters in the first and second authors' names.
Two version of the files are available, an ASCII text table zipped using "bzip2", and a FITS version with the data stored in a binary FITS table. The files are organized into subdirectories based on parameter grouping as follows:
<u> is either "ascii" or "fits", depending on the data format
<w> is a 6-digit, zero-padded instrumental broadening
<x> is the metallicity value, including '+' or '-'
<y> is the carbon abundance value, including '+' or '-'
<z> is the alpha-element value, including '+' or '-'
For example, ASCII models with an instrumental broadening R of 200, solar metalicity, solar carbon abundance, and solar alpha-element abundance can be found in:
The format for each part of the file name is described in detail in the Appendix of Bohlin et al. 2017, since, for example, decimals are avoided and some values are rounded in the file names. An example file name is:
mm13 → [M/H] = -1.25
cp00 → [C/H] = 0.00
op00 → [α/H] = 0.00
t3500 → Teff = 3500 K
g45 → log(g) = 4.5 K
v20 → Microturbulent velocity = 2.0 km/s
rt0 → Rotational broadening = 0.0 km/s
b50000 → Spectral resolution = 50,000
The models include wavelengths from 1000 Å < λ < 32 μm. The ASCII files are zipped with "bzip2", and contain the wavelengths in vacuum in Å, surface brightness (H_BOSZ), and theoretical continuum level. If you need to decompress the files, use the "bunzip2" command. The FITS files have these data in the first FITS extension, in columns called "WAVELENGTH", "SPECIFICINTENSITY", and "CONTINUUM". Note that to convert from surface brightness to flux, use the equation:
F = π * H_BOSZ
where H_BOSZ is the surface brightness in the file. Normally the equation includes a factor of 4*π, but the BOSZ models are already four times larger, so it is only necessary to multiply the surface brightness values by π to convert to flux in erg cm-2 s-1 Å-1.