haloes in a slice of the Millennium-WMAP7 simulation at $z=0$ and $z=3$, distinguishing between those with early and late formation times and also those with high and low concentrations. Starting with the halo age dependence at $z=0$ (Fig. \[Fig:CW\], top-left double panels), we see that while both early-formed and late-formed haloes trace the same cosmic web, the early-formed haloes present a sharper view of the web and appear somewhat more clustered. The view of the cosmic web when highlighting the extremes of halo concentration at $z=0$ (Fig. \[Fig:CW\], top-right panels) is reminiscent of that using halo formation time, though the clustering differences are slightly less apparent in this case. The bottom half of Fig. \[Fig:CW\] shows the distribution of haloes chosen similarly, but now at $z=3$. As expected, the haloes overall appear less clustered than at $z=0$. The differences between the early-formed and late-formed haloes (bottom-left panels) are much smaller in this case, and interestingly for the concentration (bottom-right panels), it appears that the haloes with low concentration are in fact now more clustered than the ones with high concentration. We quantify all of the trends discussed above shortly below using the CF.

These results are in agreement with those 