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Article Contents
1 Introduction
2 IR observations and data reduction
3 MIR flux measurements and uncertainties
4 Optical observations and data reduction
5 The mid-IR spectrum of Mrk 279
6 The spectral energy distribution
7 The IR variability
8 Optical variability and the H $\vec \beta$ emission-line lag
9 Discussion and concluding remarks
References

Copyright ESO 2001
Published by EDP Sciences