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Many galaxy clusters show diffuse cluster-scale emission in the form of radiohalos, showing that magnetic fields and relativistic electrons are mixed inwith the intra-cluster medium (ICM). There is general agreement that the originof radio halos is connected to turbulence, generated during cluster mergers.Statistical studies of large samples of galaxy clusters in the radio band havethe potential to unveil the connection between the properties of radio halosand the mass and dynamics of the host clusters. Previous studies have beenlimited to massive clusters and based on a small number of radio halos. The aimof this paper is to investigate the scaling relation between the radio power ofradio halos and the mass of the host clusters at low frequencies and down tolower cluster masses. We analysed the clusters from the second catalogue ofPlanck Sunyaev Zel'dovich sources that lie within the 5634 sq deg covered bythe second Data Release of the LOFAR Two-meter Sky Survey. We derived thecorrelation between the radio power and the mass of the host clusters and weinvestigated the distribution of clusters without radio halos with respect tothe correlation. We use X-ray observations to classify the dynamical state ofclusters and investigate its role on the power of radio halos. We found acorrelation between the power of radio halos at 150 MHz and the mass of thehost clusters down to 3e14 Msun. This correlation has a large scatter, part ofwhich can be attributed to the different dynamical states of host clusters. Weused two statistical test to show that the distribution of clusters with andwithout (upper limits) radio halos in the mass-radio power diagram is notcompatible with a single correlation and that it is also not compatible withclusters being uniformly distributed below an upper envelope constituted by thecorrelation.

The Planck clusters in the LOFAR sky V. LoTSS-DR2: Mass - radio halo power correlation at low frequency