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We present the analysis of MOA-2007-BLG-197Lb, the first brown dwarf companion to a Sun-like star detected through gravitational microlensing. The event was alerted and followed-up photometrically by a network of telescopes from the PLANET, MOA, and mu FUN collaborations, and observed at high angular resolution using the NaCo instrument at the VLT. From the modelling of the microlensing light curve, we derived basic parameters such as, the binary lens separation in Einstein radius units (s similar or equal to 1.13), the mass ratio q = (4.732 +/- 0.020) x 10(-2) and the Einstein radius crossing time (t(E) similar or equal to 82 d). Because of this long time scale, we took annual parallax and orbital motion of the lens in the models into account, as well as finite source effects that were clearly detected during the source caustic exit. To recover the lens system’s physical parameters, we combined the resulting light curve best-fit parameters with (J, H, K-s) magnitudes obtained with VLT NaCo and calibrated using IRSF and 2MASS data. From this analysis, we derived a lens total mass of 0.86 +/- 0.04 M-circle dot and a lens distance of D-L = 4.2 +/- 0.3 kpc. We find that the companion of MOA-2007-BLG-197L is a brown dwarf of 41 +/- 2 M-J observed at a projected separation of a(perpendicular to) = 4.3 +/- 0.1 AU, and orbits a 0.82 +/- 0.04 M-circle dot G-K dwarf star. We then placed the companion of MOA-2007-BLG-197L in a mass-period diagram consisting of all brown dwarf companions detected so far through different techniques, including microlensing, transit, radial velocity, and direct imaging (most of these objects orbit solar-type stars). To study the statistical properties of this population, we performed a two-dimensional, non-parametric probability density distribution fit to the data, which draws a structured brown dwarf landscape. We confirm the existence of a region that is strongly depleted in objects at short periods and intermediate masses (P less than or similar to 30 d, M similar to 30-60 M-J), but also find an accumulation of objects around P similar to 500 d and M similar to 20 M-J, as well as another depletion region at long orbital periods (P greater than or similar to 500 d) and high masses (M greater than or similar to 50 M-J). While these data provide important clues on the different physical mechanisms of formation (or destruction) that shape the brown dwarf desert, more data are needed to establish their relative importance, in particular as a function of host star mass. Future microlensing surveys should soon provide more detections, in particular for red dwarf hosts, thus uniquely complementing the solar-type host sample.