Table 1: Summary of uncertainties attributed to the standard star spectra in the CWW network in the 2-200 $ \mu$m range.
Description Uncertainty Spectral type Wavelength region

$ \bullet$ propagation of systematic errors

      

e.g. due to use of Vega as prime calibrator

      

$ \rightarrow$ absolute flux calibration of Sirius w.r.t. Vega

 1-3% A-M 2-200 $ \mu$m

$ \bullet$ use of Engelke function (Engelke 1992)

 3% A-dwarfs 22-35 $ \mu$m
  8% K-giants 22-35 $ \mu$m

$ \bullet$ creation of "template'' spectrum

      

$ \rightarrow$ molecular features

 up to 8% G-K around 2.3, 4.0, 4.2, 8 $ \mu$m

$ \rightarrow$ continuum

 up to 4% A-M 2-200 $ \mu$m

$ \bullet$ presence of chromosphere/ionised wind

 $ \ga$10% G-M $ \lambda$ > 100 $ \mu$m

presence of circumstellar dust

 $ \ga$10% A-M $ \lambda$ > 2 $ \mu$m

$ \bullet$ systematic difference with new Engelke

      

standards (Engelke et al. 2006)

 4-7% G2-M5 1-4 $ \mu$m


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