Classification Spectroscopy of M Dwarfs from 0.6 to 2.4 Microns

  • J. Davy Kirkpatrick
Part of the ESO Astrophysics Symposia book series (ESO)


A powerful tool in the study of cool stars and brown dwarfs is broad wavelength spectroscopy. Recently, a spectral sequence was established between 6300 and 9000 Å for dwarfs ranging in type from K5 to M9. With today’s technology, classification spectra can also be obtained with relative ease in the region near peak flux (0.9 – 2.4μm). A re-establishment of spectral types in the infrared will allow very red dwarfs to be classified using shorter integration times at smaller telescopes. In particular, the resulting 0.6 – 2.4 μm spectra will provide important physical information for the latest M dwarfs and for brown dwarf candidates.


Spectral Sequence Spectral Type Main Sequence Cool Star Spectral Classification 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.


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Copyright information

© Springer-Verlag Berlin Heidelberg 1995

Authors and Affiliations

  • J. Davy Kirkpatrick
    • 1
  1. 1.McDonald ObservatoryUniversity of TexasAustinUSA

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