Fig. 14
Left: dependence of SSFRs on galaxy stellar mass for paired galaxies (squares) and for the control sample (crosses). The solid line is the result given by Brinchmann et al. (2004), modified for initial mass function (IMF) and H0. Right: similar to left, but divided into UV (small symbols) and dust (large symbols) parts. The dotted line shows the linear regression of the SSFRs-mass relation for spirals in paired galaxies, and the dashed line for control galaxies.
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