The grid compiles ~20000 spectra of six prominent UV resonant lines resulting from radiative transfer through idealised galactic wind models and contains 5760 different wind configurations. The winds correspond to spherical (expanding or static) thick shells extending from the inner radius $R_{\rm in}$ to the outer radius $R_{\rm out}$.
A full description of the radiative transfer simulations, the wind models, and the grid of spectra is given in Garel et al. (2024).
They are described by six physical parameters :
- gas column density $N$ (atoms/cm2; in log10)
- density profile $\large{\alpha}_{\large{{\rm D}}}$
- maximum wind velocity $V_{\rm max}$ (km/s)
- velocity profile $\large{\alpha}_{\large{{\rm V}}}$
- Doppler parameter $b$ (km/s)
- dust opacity $\large{\tau_{\rm d}}$
Spectral lines
- HI Lyα λ1216
- Si II λλ1190,1193 + fluorescence
- Si II λ1260 + fluorescence
- C II λ1334 + fluorescence
- Fe II λλ2586,2600 multiplet + fluorescence
- Mg II λλ2796,2803 doublet
Outputs
Integrated spectra with or without LSF convolution (FWHM_LSF = 0.2 A) : all spectra are normalised to the continuum and wavelengths are in the rest-frame (in A).Additional outputs are available (e.g. individual photons’ wavelength, position, number of scatterings, etc) and can be provided upon reasonable request (mailto: thibault.garel[at]unige.ch).
More details on the simulations, wind models/parameters and UV lines can be found in the README.