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A number of different types of interesting objects may be distinguished in the DFBS. It is possible to select objects by comparison of their blue and red parts of the spectrum, follow the spectral energy distribution (SED), and notice a number of broad spectral lines, such as the Balmer (and sometimes, HeI) absorption lines at white dwarfs and some subdwarfs, broad emission lines of QSOs and Seyferts, strong emission lines of cataclysmic variables (CV) and planetary nebulae (PN), as well as absorption bands at late-type stars (M, C).

Sample spectra for stars of different spectral types (A-F-G-K).

The following main types of objects have been selected by means of the FBS spectra so far