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1.10. The effects of the disk field on the bulge surface brightness

Published online by Cambridge University Press:  25 May 2016

Y.C. Andredakis  and
R.H. Sanders
Y.C. Andredakis
Affiliation:
Kapteyn Institute, P.O. Box 800, 9700 AV Groningen, The Netherlands
R.H. Sanders
Affiliation:
Kapteyn Institute, P.O. Box 800, 9700 AV Groningen, The Netherlands

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After the classical description of bulges by a de Vaucouleurs profile was found to be inadequate, a generalized profile, Sersic's law, was used successfully to describe the surface brightness: (Andredakis et al. 1994 (APB95)). The exponent n was found to vary systematically with the morphological type of the galaxy, from n = 4 for the bulges of S0s to n = 2 for intermediate type spirals and n = 1 (pure exponential) for the late types. (APB95, de Jong 1996). This has been confirmed also by the kinematics (Heraudeau et al 1996). This variation of n has been interpreted in two ways: (i) As the effect of the disk forming around an already developed bulge (APB95) and (ii) as evidence that the bulge originated from secular processes in the galaxy, after the disk was formed (Courteau et al. 1996). This needs to be resolved.

Type
Part I. Stellar Cluster, Star Formation
Information
Symposium - International Astronomical Union , Volume 184: The Central Regions of the Galaxy and Galaxies , 1998 , pp. 35 - 36
Copyright
Copyright © Kluwer 1998 

References

Andredakis, , Peletier, & Balcells, , 1995, MNRAS, 275, 874 (APB95).CrossRefGoogle Scholar
de Jong, R.S., 1996, A&A 313, 45.Google Scholar
Heraudeau, P., Simien, F., Mamon, G.A., 1996, in ESO Proc., ‘Spiral Galaxies in the Near-IR’, Springer-Verlag Berlin, p. 235.Google Scholar
Courteau, S., De Jong, R.S., & Broeils, 1996, ApJ, 457, L73.CrossRefGoogle Scholar