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In this work we measure and study the cross-correlation signal between aforeground sample of GAMA galaxies with spectroscopic redshifts in the range$0.2<z<0.8$, and a background sample of H-ATLAS galaxies with photometricredshifts $\gtrsim1.2$. It constitutes a substantial improvement over thecross-correlation measurements made by Gonzalez-Nuevo et al. (2014) withupdated catalogues and wider area (with $S/N\gtrsim 5$ below 10' and reaching$S/N\sim 20$ below 30"). The better statistics allow us to split the sample indifferent redshift bins and to perform a tomographic analysis (with $S/N\gtrsim3$ below 10 arcmin and reaching $S/N\sim 15$ below 30"). Moreover, we implementa halo model to extract astrophysical information about the background galaxiesand the deflectors that are producing the lensing link between the foreground(lenses) and background (sources) samples. In the case of the sources, we findtypical mass values in agreement with previous studies: a minimum halo mass tohost a central galaxy, $M_{min}\sim 10^{12.26} M_\odot$, and a pivot halo massto have at least one sub-halo satellite, $M_1\sim 10^{12.84} M_\odot$. However,the lenses are massive galaxies or even galaxy groups/clusters, with minimummass of $M_{min}^{lens}\sim 10^{13.06} M_\odot$. Above a mass of$M_1^{lens}\sim 10^{14.57} M_\odot$ they contain at least one additionalsatellite galaxy which contributes to the lensing effect. The tomographicanalysis shows that, while $M_1^{lens}$ is almost redshift independent, thereis a clear evolution of increase $M_{min}^{lens}$ with redshift in agreementwith theoretical estimations. Finally, the halo modeling allows us to identifya strong lensing contribution to the cross-correlation for angular scales below30". This interpretation is supported by the results of basic but effectivesimulations.

H-ATLAS/GAMA: Magnification Bias Tomography. Astrophysical constraints above $\sim1$ arcmin