The recorded spectra were reduced to the same value of the frequency of SHF quantum, amplification and sample weight.
This was achieved by using a multiple-peak Pawley-type refinement on the recorded spectra.
The study then proved that the recorded spectra reflected physical phenomena taking place on the emitter surface.
To verify this claim, we simulated the PSF for an assortment of reflectance spectra from the Munsell database of 1250 different recorded spectra.
Furthermore, the recorded spectra indicate that additional quantitative species measurements by SRS are feasible in the non-sooting jet.
From the recorded spectra trace gas densities and temperature fields were derived on a very dense spatial grid.
Electrochemical impedance spectroscopy (EIS) was performed and the quality of the recorded spectra was verified by Kramers-Kronig relations.
We derived total column (TC) of a dozen of atmospheric gases from recorded spectra and performed the error analysis of these retrievals.
The peak of the recorded spectra is very close to the actual wavelength of the IR, with a maximum difference of less than 5 nm.
The visible blue emission is emphasized, and recorded spectra indicate that fine spectral structure is superimposed on a broadband continuum extending from the ultraviolet into the visible region.
The recorded spectra have been adjusted one-by-one using Voigt line-shapes in order to retrieve the line positions and the Lorentz widths for the P(40) to R(40) lines.
