Fig. 6.
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Radio-IR correlation for the total luminosity (upper panel) and the halo luminosity (bottom panel). The horizontal axis corresponds to the logarithm of the IR luminosity in L⊙ and the vertical axis corresponds to the logarithm of the 1.4 GHz luminosity in W Hz−1. Our sample galaxies are shown as stars and the dotted line corresponds to the linear fit of our data. The fit for the upper panel has a slope of 1.08 ± 0.07 and an intercept of 10.6 ± 0.7, while for the bottom panel, we obtained a slope of 1.1 ± 0.2 and an intercept of 9 ± 2.
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