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Galaxy models predict a tight relation between the clustering of galaxies anddark matter on cosmological scales, but predictions differ notably in thedetails. We used this opportunity and tested two semi-analytic models by theMunich and Durham groups with data from the Canada-France-Hawaii TelescopeLensing Survey (CFHTLenS). For the test we measured the scale-dependent galaxybias factor $b(k)$ and correlation factor $r(k)$ from linear to non-linearscales of $k\approx10\,h\,\rm Mpc^{-1}$ at two redshifts $\bar{z}=0.35,0.51$for galaxies with stellar mass between $5\times10^9$ and$3\times10^{11}\,h_{\rm 70}^{-2}\,{\rm M}_\odot$. Our improved gravitationallensing technique accounts for the intrinsic alignment of sources and themagnification of lens galaxies for better constraints for the galaxy-mattercorrelation $r(k)$. Galaxy bias in CFHTLenS increases with $k$ and stellarmass, it is colour-dependent, revealing the individual footprints of galaxytypes. Despite a reasonable model agreement for the relative change with bothscale and galaxy properties, there is a clear conflict for $b(k)$ with no modelpreference: the model galaxies are too weakly clustered. This may flag a modelproblem at $z\gtrsim0.3$ for all stellar masses. As in the models, however,there is a high correlation $r(k)$ between matter and galaxy density on allscales, and galaxy bias is typically consistent with a deterministic bias onlinear scales. Only our blue and low-mass galaxies of about$7\times10^9\,h_{\rm 70}^{-2}\,{\rm M}_\odot$ at $\bar{z}=0.51$ show, contraryto the models, a weak tendency towards a stochastic bias on linear scales where$r_{\rm ls}=0.75\pm0.14\,{\rm(stat.)}\pm0.06\,{\rm(sys.)}$. This result is ofinterest for cosmological probes, such as $E_{\rm G}$, that rely on adeterministic galaxy bias.

CFHTLenS: Galaxy bias as function of scale, stellar mass, and colour. Conflicts with predictions by semi-analytic models