Large and kinematically unbiased samples of G- and K-type stars. V - Evolved stars in the selected areas at + 15-deg declination

Details Large and kinematically unbiased samples of G- and K-type stars. V - Evolved stars in the selected areas at + 15-deg declination Large and kinematically unbiased samples of G- and K-type stars. V - Evolved stars in the selected areas at + 15-deg declination

Mar 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990pasp..102..242e&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 102, March 1990, p. 242-298.

Astronomy and Astrophysics

Astronomy

8

Abundance, G Stars, Interstellar Extinction, K Stars, Stellar Spectrophotometry, Tables (Data), H Beta Line, Heavy Elements, Iron, Metallicity, Stellar Evolution, Stellar Luminosity, Photometry: Abundances: G- And K-Type Stars

Scientific paper

Intermediate-band, HI, and DDO photometry of 430 C- and K-type stars in the Selected Areas at 15° are discussed. The reddening is derived from (b-y)0 0.353-0.550(b-y) + 0.722 M1 + 0.826(R - I) as well as from DDO photometry. New DDO photometry is presented for 62 stars. The luminosity calibrations are Mυ = 0.834-5.86(R - I)0 + 4.86[C1] for young disk stars and 0.73 mag fainter for old disk stars of the same (R - I). The bluest old disk objects ((R - I) ≤ 0.29 mag) have adopted values Of Mυ = +3.0 mag. An improved calibration of the heavy element abundance indicator, M1, based on high-dispersion spectroscopic results by Cottrell and Sneden (1986) and McWilliam (1989), leads to P[Fe/H] 3.2 Δ(M1)0 + 0.10, where Δ(M1)0 = (M1)0 - 2.15(R - I)0 + 0.240 for (R - I)0 ≤ 0.425 mag and Δ(M1)0 = (M1)0 - 0.293 - 0.90 (R - I)0 for larger values. The results from the previous calibration, used in Paper IV, should be corrected by P[Fe/H] = 1.6 P[Fe/H] (Paper IV) + 0.10. The assumption that P [Fe/H]δCN = P[Fe/H]ΔM1 leads to reddening values that, at least for the halo population objects, are not always acceptable. The possibility remains that this assumption may be correct for the disk population stars.

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