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Stellar chemical-abundance gradient in the direction of the South Galactic Pole - preliminary results

Published online by Cambridge University Press:  04 August 2017

Ch. F. Trefzger ,
J. W. Pel  and
A. Blaauw
Ch. F. Trefzger
Affiliation:
Astronomical Institute, Basel, Switzerland
J. W. Pel
Affiliation:
Kapteyn Astronomical Institute, Groningen, The Netherlands
A. Blaauw
Affiliation:
Kapteyn Astronomical Institute, Groningen, The Netherlands

Abstract

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Using the Walraven VBLUW photometric system, we have studied the metal content of 89 F and G stars in the Galactic South Pole field SA141. Our sample is based on the Basel survey of RGU photometry in Selected Areas, and it contains all stars in SA141 with VJ <14m.5 and (G-R)<1m.15 (spectral types earlier than about G7). The observations were made with the VBLUW photometer and the 90-cm Dutch Telescope at ESO, La Silla.

For unreddened intermediate-type stars the VBLUW photometry enables us to separate the effects of temperature, gravity, and metallicity (cf. Lub and Pel, 1977). Since reddening is negligible in SA141, we can therefore determine these three parameters for each program star once the photometric indices are calibrated in terms of Teff, log g, and [Fe/H]. The latter calibration was made in a semi-empirical way, using VBLUW observations of stars with spectroscopic analyses in combination with theoretical colors based on the model spectra by Kurucz (1979). We used the Hyades main-sequence as a zeropoint, adopting [Fe/H] = +0.15 for this cluster.

The results in the (V-B)-(B-L) diagram are shown in Fig. 1. This diagram is very sensitive to metallicity, but almost gravity-independent. Fig. 1 indicates that most program stars have metallicities in the range −1 ≦ [Fe/H] ≦ 0. The distribution of the program stars in the gravity-sensitive (V-B)-(L-U) diagram is very narrow, log g =4.2 ± 0.3, which means that these stars are probably all dwarfs, with only very few possible subgiants.

The absolute-magnitude calibration was derived by using the data of Cayrel de Strobel et al. (1980) and of Cayrel de Strobel and Bentolila (1983). From their [Fe/H]-catalogue we took all stars with known distances, and within the parameter range of our program stars, to construct an empirical MV - Teff relation. This relation was used to derive distances for the stars in SA141.

These distances are plotted against [Fe/H] in Fig. 2. The diagram clearly shows the correlation between distance and metallicity, suggesting for this particular sample a gradient of −0.6 in [Fe/H] over the first 500 pc. Similar values were found in the Basel RGU program (cf. Trefzger, 1981) and by Blaauw and Garmany (1975).

Type
PART II: COMPOSITION, STRUCTURE AND KINEMATICS
Information
Symposium - International Astronomical Union , Volume 106: The Milky Way Galaxy , 1985 , pp. 151 - 152
Copyright
Copyright © Reidel 1985 

References

Blaauw, A., Garmany, C.D.: 1975, in “Proceedings of the Third European Astronomical Meeting”, ed. Kharadze, E.K., Tbilisi, p.3.Google Scholar
Cayrel de Strobel, G., Bentolila, C., Hauck, B., Curchod, A.: 1980, Astron. Astrophys. Suppl. 41, 405.Google Scholar
Cayrel de Strobel, G., Bentolila, C.: 1983, Astron. Astrophys. 119, 1.Google Scholar
Kurucz, R.L.: 1979, Astrophys. J. Suppl. 40, 1.CrossRefGoogle Scholar
Lub, J., Pel, J.W.: 1977, Astron. Astrophys. 54, 137.Google Scholar
Trefzger, Ch.F.: 1981, Astron. Astrophys. 95, 184.Google Scholar