The M supergiants in NGC 300

Details The M supergiants in NGC 300 The M supergiants in NGC 300

Mar 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986aj.....91..522h&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 91, March 1986, p. 522-529.

Mathematics

Logic

13

Astronomical Spectroscopy, M Stars, Spiral Galaxies, Supergiant Stars, Infrared Photometry, Spectral Line Width, Stellar Color, Stellar Luminosity

Scientific paper

The authors have surveyed the nearby Sc spiral NGC 300 for its brightest red stars and have confirmed six of the brightest candidates to be definite M supergiants. The authors have used far-red spectroscopy and the strength of the Ca II triplet (≈λ8500) as a luminosity discriminant between supergiants and foreground red dwarfs, plus near-infrared (JHK) photometry to derive accurate extinction and bolometric luminosities. Adopting Graham's (1984) true distance modulus of 26.1 mag for NGC 300 it is found that its brightest M supergiants have Mv near -8 mag and MBol ≤ -9.5 mag. A comparison with the brightest red supergiants in the morphologically similar galaxies M33 and NGC 2403 suggests that these galaxies have very similar populations of evolved massive stars.

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