SIMBAD references

2007AJ....134.1777T - Astron. J., 134, 1777-1789 (2007/November-0)

The uvbyHβ metallicity calibration for G and K dwarfs.


Abstract (from CDS):

The metallicity dependence of the primary indices of the uvby photometric system for cooler dwarfs (Te∼6500-5000 K) is investigated. The database for the analysis is composed of the overlap between a composite catalog of selected, high-dispersion spectroscopic abundances for 1801 stars on the metallicity scale of Valenti & Fischer and a merged catalog of high-precision uvbyHβ photometry for over 35,000 stars. While [Fe/H] for F dwarfs is best estimated from m1, with a modest dependence on c1 as expected, for hotter G dwarfs the pattern reverses, and c1 becomes the dominant index. For cooler G dwarfs and K stars, the c1 dominance continues, but a discontinuity appears such that stars between b-y=0.50 and 0.58 with [Fe/H]≥+0.25 have m1 and c1indices that classify them as subgiants, confirming an earlier result based on a much smaller sample. The reversal in the sensitivity to m1 and c1is traced, in part, to the metallicity sensitivity of the b-y index. Moreover, b-y grows larger in a nonlinear fashion for stars above solar metallicity, leading to an overestimate of the reddening for super-metal-rich stars from some standard intrinsic color relations. Based on successful tests using indices from synthetic spectra and the empirical trends among the observations, metallicity calibrations tied to Hβ rather than b-y have been derived for [Fe/H]≥-1.0, generating dispersions among the residuals ranging from 0.061 to 0.085 dex over the entire temperature range of interest. The new calibrations have the added advantage of being significantly less sensitive to errors in reddening than previous calibrations.

Abstract Copyright:

Journal keyword(s): Stars: Abundances - Techniques: Photometric

Simbad objects: 28

goto Full paper

goto View the reference in ADS

To bookmark this query, right click on this link: simbad:2007AJ....134.1777T and select 'bookmark this link' or equivalent in the popup menu


© Université de Strasbourg/CNRS

    • Contact