## Contents ##

10 ascii files with MIR and NIR spectra in five regions:
  HII region (HII)
  ionization front (IF)
  atomic neutral region (PDR_atomic)
  dissociation front (DF)
  molecular cloud (PDR_molecular)

## Computations and caveat ##

These spectra have been computed individually for each region, using the Meudon PDR code for the contribution from molecular and atomic lines (Le Petit et al. 2006), the CLOUDY code for the ionized gas (Ferland et al. 1998), the PAHTAT model for the PAH emission (Foschino et al. 2019), and the DUSTEM model and THEMIS coupled to SOC radiative transfer for the contribution from the dust continuum. The physical parameters used for these models correspond to those of the Orion Bar. Absolute calibration of the sum of the resulting spectra of the five regions has been crossed-check with existing observations of the Orion Bar. However, we emphasize that the individual spectra of the different regions, obtained by making simple assumptions, are probably not fully realistic. This could be an issue when trying to interpret the synthetic data from a detailed physical point of view, but this is not a limitation for the data simulation.