We describe seven exoplanets transiting stars of brightness V = 10.1-12.4. WASP-130b is a 'warm Jupiter' having an orbital period of 11.6 d around a metal-rich G6 star. Its mass and radius (1.23 plus or minus 0.04 M sub( Jup) and 0.89 plus or minus 0.03 R sub( Jup)) support the trend that warm Jupiters have smaller radii than hot Jupiters. WASP-131b is a bloated Saturn-mass planet (0.27 M sub( Jup) and 1.22 R sub( Jup)). Its large scaleheight and bright (V = 10.1) host star make it a good target for atmospheric characterization. WASP-132b (0.41 M sub( Jup) and 0.87 R sub( Jup)) is among the least irradiated and coolest of WASP planets, having a 7.1-d orbit around a K4 star. WASP-139b is a 'super-Neptune' akin to HATS-7b and HATS-8b, being the lowest mass planet yet found by WASP (0.12 M sub( Jup) and 0.80 R sub( Jup)). The metal-rich K0 host star appears to be anomalously dense, akin to HAT-P-11. WASP-140b is a 2.4-M sub( Jup) planet in an eccentric (e = 0.047 plus or minus 0.004) 2.2-d orbit. The planet's radius is large (1.4 R sub( Jup)), but uncertain owing to the grazing transit (b = 0.93). The 10.4-d rotation period of the K0 host star suggests a young age, and the time-scale for tidal circularization is likely to be the lowest of all known eccentric hot Jupiters. WASP-141b (2.7 M sub( Jup), 1.2 R sub( Jup) and P = 3.3 d) and WASP-142b (0.84 M sub( Jup), 1.53 R sub( Jup) and P = 2.1 d) are typical hot Jupiters orbiting metal-rich F stars. We show that the period distribution within the hot-Jupiter bulge does not depend on the metallicity of the host star.