Hostname: page-component-cd9895bd7-hc48f Total loading time: 0 Render date: 2024-12-12T14:21:14.114Z Has data issue: false hasContentIssue false
  • English
  • Français

Visual–IR Color Gradients in Elliptical Galaxies

Published online by Cambridge University Press:  04 August 2017

R. F. Peletier ,
E. A. Valentijn  and
R. F. Jameson
R. F. Peletier
Affiliation:
Kapteyn Astronomical Institute, Groningen, the Netherlands
E. A. Valentijn
Affiliation:
Kapteyn Astronomical Institute, Groningen, the Netherlands
R. F. Jameson
Affiliation:
Department of Astronomy, University of Leicester, United Kingdom

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Dissipational formation theories (e.g. Larson 1974) predict a metallicity change with distance from the center in elliptical galaxies. Several authors have reported small color gradients in visual colors like B–V and B–R. The interpretation of these data is not easy, due to uncertainties caused by the short wavelength–baseline, and by the presence of a hot stellar population suggested by IUE–data (e.g. Burstein et al. 1986). Simultaneous measurements of visual and visual-infrared colors provide the means to determine both the average temperature of the giant branch and the turnoff–temperature of the main sequence. This allows to model fractional contributions of different populations, including age– and metallicity–effects. The required continuity of solutions at different radii provides a strong constraint in selecting a more unique overall population model, and relieves the ambiguous interpretation of single measurements.

Type
Posters
Information
Symposium - International Astronomical Union , Volume 127: Structure and Dynamics of Elliptical Galaxies , 1987 , pp. 443 - 444
Copyright
Copyright © Reidel 1987 

References

REFERENCES

Burstein, D., Bertola, F., Buson, F., Faber, S.M., & Lauer, T.R., 1986. in Stellar Populations, eds Tosi, M., & Norman, C., (Baltimore).Google Scholar
Davies, R.L., & Sadler, E.M., 1986. in Stellar Populations, eds Tosi, M., & Norman, C., (Baltimore).Google Scholar
Efstathiou, G., & Gorgas, J., 1985. M.N.R.A.S., 215, 37P.Google Scholar
Jedrezejewski, R., 1987. This volume, p. 37.Google Scholar
Larson, R.B., 1974. M.N.R.A.S., 166, 585.CrossRefGoogle Scholar
Peletier, R.F., Davies, R.L., Illingworth, G.D., Davis, L.E., & Cawson, M., 1987, in preparation.Google Scholar
Strom, S.E., Strom, K.M., Goad, J.W., Vrba, F.J., & Rice, W., 1976. Astroph. J., 204, 684.Google Scholar
Tinsley, B.M., 1978, Astroph. J., 222, 14.Google Scholar
Valentijn, E.A., & Moorwood, A.F.M., 1985. Astron. Astroph., 143, 46.Google Scholar