Galaxy clusters are assembled via merging of smaller structures, in a process that generates shocks and turbulence in the intra cluster medium and produces radio emission in the form of halos and relics. The cluster pair A 399-A 401 represents a special case: both clusters host a radio halo and recent LOFAR observations at 140~MHz revealed the presence of a radio bridge connecting the two clusters and two candidate relics, one South of A 399 and the other in between the two clusters in proximity of a shock front detected in X-ray observations. In this paper we present Westerbork observations at 1.7, 1.4 and 1.2~GHz and 346~MHz of the A 399-A 401 cluster pair. We detected the radio halo in the A 399 cluster at 346~MHz, extending up to $sim 650$~kpc and with a $125 pm 6$~mJy flux density. Its spectral index between 1.4~GHz and 346~MHz and between 140~MHz and 346~MHz is $alpha = 1.47 pm 0.05$, and $alpha = 1.75 pm 0.14$ respectively. The two candidate relics are also seen at 346~MHz and we determined their spectral index to be $alpha = 1.10 pm 0.14$ and $alpha = 1.46 pm 0.14$. The low surface brightness bridge connecting the two clusters is below the noise level at 346~MHz, therefore we constrained the bridge average spectral to be steep, i.e. $alpha > 1.5$ at $2sigma$ confidence level. This result favours the scenario where dynamically-induced turbulence is a viable mechanism to reaccelerate a population of mildly relativistic particles and amplify magnetic fields even in cluster bridges, i.e. on scales of a few Mpcs.
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