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Fig. 3


Spectral energy distributions of the B[e] supergiants. Panel a): ARDB 54, panel b): N181, panel c): Hen S137, and panel d): Hen S59. The optical UBV photometry for N181, Hen S59, and Hen S137 is taken from Zaritsky et al. (2004); the optical UBVR photometry for ARDB 54 is taken from Massey (2002), the JHK photometry is taken from the 2MASS catalog, and the 3.68.0 μm Spitzer photometry (the 4 longest-wavelength points) is taken from the SAGE survey data (Whitney et al. 2008). The fluxes are corrected for the reddening (see text). Solid lines represent theoretical SEDs from Kurucz (1993). We assumed Teft of 10 000 K for ARDB 54, 16 000 K for N181 and Hen S–137, and 19 000 K for Hen S59. The fluxes are normalized to the V-band flux and shown on a logarithmic scale versus logarithms of wavelengths in microns.

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