High-resolution CCD spectra of stars in globular clusters. II - Metals and CNO in M71

Details High-resolution CCD spectra of stars in globular clusters. II - Metals and CNO in M71 High-resolution CCD spectra of stars in globular clusters. II - Metals and CNO in M71

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987aj.....93..338l&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 93, Feb. 1987, p. 338-346. Previously announced in STAR as N87-10789.

Astronomy and Astrophysics

Astronomy

28

Abundance, Charge Coupled Devices, Globular Clusters, Metallicity, Calcium, Carbon 12, Carbon 13, Iron, Sodium, Stellar Spectrophotometry

Scientific paper

Palomar coude CCD spectra of resolution 0.3 and 0.6 has been used to redetermine abundances in five stars of the relatively metal rich globular cluster M71. The (Fe/H) value is restricted to the limits of -0.6 to -1.0. The largest source of uncertainty is a systematic difference in f-values between those derived via the Holweger-Muller (1974) solar model and the Bell et al. (1976) solar model. If we use absolute f-values measured by the Oxford group (Blackwell et al. 1982) we find Fe/H to lie in the range of -0.6 to -0.75, i.e., as given by using the Bell et al. solar model. The relative abundances of the light elements, i.e., Na through Ca and probably including Ti show an average excess relative to iron of 0.4-dex. The effect of this difference on metal indices derived from broad- and narrow- band photometry is discussed. For three stars we find O/H = -0.6 using absolute f-values. For CN an analysis of individual rotational lines of the 2-0 band of the red system yields lines in the (C/H, N/H) plane that are consistent with either an original C/Fe = N/Fe = 0 or a modest increase in N relative to C due to CN burning and mixing. A search for C-13N was not successful and an uncertain lower limit of C-12/C-13 near 10 was obtained.

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