The FeH Wing‐Ford Band in Spectra of M Stars | Zendy

Ricardo P. Schiavon | Zendy; B. Barbuy | Zendy; Patan D. Singh | Zendy

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The FeH Wing‐Ford Band in Spectra of M Stars

Author(s) -

Ricardo P. Schiavon,

B. Barbuy,

Patan D. Singh

Publication year - 1997

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/304332

Subject(s) - surface gravity , metallicity , stars , wing , spectral line , astrophysics , physics , resolution (logic) , effective temperature , giant star , surface (topology) , full width at half maximum , spectral resolution , astronomy , optics , geometry , artificial intelligence , computer science , thermodynamics , mathematics

We study the FeH Wing-Ford band at 9850 - 10200 Angstrons by means of the fitof synthetic spectra to the observations of M stars, employing recent modelatmospheres. On the basis of the spectrum synthesis, we analyze the dependenceof the band upon atmospheric parameters. FeH lines are a very sensitive surfacegravity indicator, being stronger in dwarfs. They are also sensitive tometallicity (Allard & Hauschildt 1995). The blending with CN lines, which arestronger in giants, does not affect the response of the Wing-Ford band tosurface gravity at low resolution (or high velocity dispersions) because CNlines, which are spread all along the spectrum, are smeared out at convolutionsof FWHM $\simgreat$ 3 Angstrons. We conclude that the Wing-Ford band is asuitable dwarf/giant indicator for the study of composite stellar populations.Comment: 23 pages + 11 figures in postscript format + 3 ps figures (Nos. 2, 6 and 7) available under request to ripisc@andromeda.iagusp.usp.br. Accepted for publication in The Astrophysical Journa

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