The FIR/radio correlation in starburst galaxies - constraints on starburst models

This paper presents an analysis of the correlation between the far-infrared (FIR) and the radio emission of starburst galaxies. Data for interacting galaxies, many of which are undergoing a starburst, and for normal galaxies have been analysed and compared in order to test for any influence of the star-formation activity on the ratio between the FIR and the radio emission at 2.4 GHz, $\text{q}24$. No statistically significant indication for such an influence has been found: There is neither a significant difference between $\text{q}24$ of the two samples nor a dependence of this ratio on the starburst strength. This observational fact is unexpected because of the different physical conditions and the short time-scale of the star-formation activity in a starburst. In order to interprete the observations the FIR and the radio emission during a starburst have been modeled. The following conclusions could be drawn from the observed constancy of $\text{q}24$: A strong and fast ($\approx {10}^7$ yr) increase of the magnetic field at the beginning of the starburst is required in order to maintain a constant $\text{q}24$. Otherwise the strong Inverse Compton losses that are due to the intense radiation field in a starburst would lower the synchrotron emission drastically resulting in a value of $\text{q}24$ significantly higher than the observed one. Furthermore, the time-scale of the variation of the star-formation rate has to be longer than some ${10}^7$ yr. For lower values the different time-scales of the FIR and the radio emission produce large fluctuations of $\text{q}24$.