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Maury had divided stars based on the widths of their spectral lines with her class c identifying stars with the narrowest lines. Nevertheless very hot main-sequence stars are still sometimes called dwarfs even though they have roughly the same size and brightness as the giant stars of that temperature.

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In 1897 Antonia C.

. Supergiant stars can be identified on the basis of their spectra with distinctive lines sensitive to high luminosity and low surface gravity. Although it was not known at the time these were the most luminous stars. For the hottest stars the difference is not directly observable and for these stars the terms dwarf and giant refer to differences in spectral lines which indicate whether a star is on or off the main sequence.

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