Astronomy & Astrophysics

All Tables

Table 1: Multiplicative factors used to scale the different sub bands of the $\alpha$ Orionis spectrum to the absolute flux level when the latter is either determined by the flux level in band 1d (3rd column) or by requiring the average of the scaling factors to be equal to 1 (4th column). The large deviations from unity in the 1d-referenced scaling suggest that the absolute flux in band 1d might be underestimated. Further evidence supporting this hypothesis is given in Sect. 4.3. The large jumps between some bands can be (partially) attributed to the use of three different filters and apertures and 4 different detector types.
Table 2: The stellar/atmospheric parameters of $\alpha$ Orionis, according to Lambert et al. (1984), for a temperature of 3800 K (their own estimate) and for a temperature of 3600 K (as suggested by other temperature determinations).
Table 3: The grid of layer parameters in which we search for a best fit to both the ISO-SWS spectrum and the interferometric data.
Table 4: Dust shell parameters for the best fit to the ISO-SWS spectrum. The dust shell inner radius corresponds to the measured inner radius of Skinner et al. (1997) and Sloan et al. (1993). The dust to gas ratio is taken from Knapp et al. (1980) and the outflow velocity from Knapp & Morris (1985). Grain shapes are a continuous distribution of ellipsoids (CDE).
Table 5: Stellar and layer parameters for $\alpha$ Orionis, as derived by Jennings & Sada (1998), Tsuji (2000b), Ohnaka (2004b) and Perrin et al. (2004a). The first 2 determinations are purely spectroscopic, the third combines high-resolution spectroscopy and interferometry and the fourth one combines photometry with interferometry (NA = not available).