3. METHOD (I)
- We are using a “template” method:
Accurate photometry: good definition of the spectrum.
? the relative errors are minimised (goal < 2%).
What happens to the colour terms? Does the spec-tral limitation “block” the photometric calibration?
It gives the fluxes for AV and KIII stars between 1 and 30 microns by using the visible and IR magnitudes and models of stellar emission. We obtain full spectra for any spectral resolution.
AV: their atmospheres are well-understood (high resolution)
KIII: the entire spectrum has been observed (low resolution)