Context. Despite their large number in the Galaxy, M dwarfs remain elusive objects and the modeling of their photospheres has long remained a challenge (molecular opacities, dust cloud formation). Aims. Our objectives are to validate the BT-Settl model atmospheres, update the M dwarf Teff-spectral type relation, and find the atmospheric parameters of the stars in our sample. Methods. We compare two samples of optical spectra covering the whole M dwarf sequence with the most recent BT-Settl synthetic spectra and use a � 2 minimization technique to determine Teff. The first sample consists of 97 low-resolution spectra obta ined with NTT at La Silla Observatory. The second sample contains 55 mid-resolution spectra obtained at the Siding Spring Observa tory (SSO). The spectral typing is realized by comparison with already classified M dwarfs. Results. We show that the BT-Settl synthetic spectra reproduce the slope of the spectral energy distribution and most of its featu res. Only the CaOH band at 5570A and AlH and NaH hydrides in the bluepart of the spectra are still missing in the models. The Teff-scale obtained with the higher resolved SSO 2.3 m spectra is consistent with that obtained with the NTT spectra. We compare our Teffscale with those of other authors and to published isochrones using the BT-Settl colors. We also present relations between effective temperature, spectral type and colors of the M dwarfs.
The effective temperature scale of M dwarfs
A. Rajpurohit,C. Reylé,F. Allard,D. Homeier,M. Schultheis,M. Bessell,A. Robin
Published 2013 in Astronomy and Astrophysics
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- Publication year
2013
- Venue
Astronomy and Astrophysics
- Publication date
2013-04-15
- Fields of study
Physics
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