Interrelations between V il and S tr photometric systems: The luminosity indicator (v - X)

Details Interrelations between V il and S tr photometric systems: The luminosity indicator (v - X) Interrelations between V il and S tr photometric systems: The luminosity indicator (v - X)

Aug 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003a%26a...407..377k&link_type=abstract

Astronomy and Astrophysics, v.407, p.377-384 (2003)

Astronomy and Astrophysics

Astrophysics

1

Methods: Observational, Techniques: Photometric

Scientific paper

Using the largest database of near-IR Ca II Triplet indices currently available (Cenarro et al. \cite{Cenarro01a},b), we confirm our finding about the influence of the Ca II stellar lines on the X magnitude of the Vilnius photometric system. This effect is significant for spectral sub-classes from early F until mid K. For this spectral range there is a linear relation between the v-X index and the strength of the infrared Ca II Triplet, which implies that the Ca II H&K lines should influence the difference in a similar way. For the spectral interval studied, v-X repeats the behavior of the Ca II Triplet with respect to gravity, temperature and metallicity. The Ca II Triplet lines are a powerful diagnostic of the stellar populations in galaxies because of their sensitivity to the main stellar atmospheric parameters. Being much easily achievable observationally and virtually reddening free, the v-X index may find similar applications. v-X is log g sensitive but additional means are required to break the dwarf - giant duplicity. For this purpose we have studied the variation of the v(Strömgren)-B(Johnson) index with gravity, temperature and the equivalent width of the Ca II Triplet. Since v(Strömgren)-B(Johnson) have a none overlapping variation with the Ca II Triplet the dwarfs and giants may be separated and Teff and log g may be estimated. The v(Strömgren)-B(Johnson) index has furthermore the advantage that E(v-B) ~ 0.25E(B-V).
Based on CDS data.

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