All Tables

Table 1: PRONAOS/SPM bands characteristics. $\lambda _{\rm eff,dust}$ is the effective wavelength for a standard 30 K dust spectrum with a $\lambda ^{-2}$ emissivity law and $\lambda _{\rm eff,SZ}$ is the effective wavelength for the Sunyaev-Zel'dovich thermal effect (Lamarre et al. 1998). The definitions of $\lambda _{\rm ref}$ and $\lambda _{\rm eff}$ are detailed in Sect. 3.1.2.
Table 2: Color correction factors to be taken into account in order to transform the PRONAOS flux intensities from a (T=30 K, $\beta =2$ ) spectrum to a (T, $\beta$ ) or Rayleigh-Jeans (RJ) spectrum.
Table 3: PRONAOS/SPM transmission computed in the PRONAOS/SPM photometric bands and their 3 $\sigma$ errors.
Table 4: Beam characteristics for the geometric optical conjugate of the cold stop (geometrical beam), the Saturn observations (main beam), and a combination of the Saturn observations and a telescope model (full beam).
Table 5: PRONAOS/SPM calibration error budget: absolute and band to band relative errors
Table 6: Noise Equivalent Flux Densities of the PRONAOS/SPM experiment measured in flight.
Table 7: Summary of the Saturn model: Rayleigh-Jeans brightness temperature of the Saturn sub-Earth point and the different contributions we have taken into account. The predictions of the model are compared with the PRONAOS/SPM observations.
Table 8: List of the PRONAOS observations (second flight) used in the intercalibration with COBE/DIRBE and ISO/ISOPHOT .
Table 9: Integrated fluxes of M 82 measured by PRONAOS and DIRBE in Jy. The flux convention is $\nu \times I_{\nu } = \rm cste.$ in both cases.
Table 10: Fit parameters for the M 82 spectrum using PRONAOS data and PRONAOS +DIRBE data.
Table 11: Ratio of the PRONAOS to DIRBE average brightnesses on extended sources. The average value is weighted using 1/ $\sigma ^2$ .
Table 12: Ratio of the PRONAOS to ISOPHOT average brightnesses on extended sources. The average value is weighted using 1/ $\sigma ^2$ .