Figure 1:
The phase space picture for the black hole threshold in the presence of a critical point. Every point correspond to an initial data set, that is, a 3metric, extrinsic curvature, and matter fields. (In type II critical collapse these are only up to scale). The arrow lines are solution curves, corresponding to spacetimes, but the critical solution, which is stationary (type I) or selfsimilar (type II) is represented by a point. The line without an arrow is not a time evolution, but a 1parameter family of initial data that crosses the black hole threshold at p = p_{*}. The 2dimensional plane represents an (–1)dimensional hypersurface, but the third dimension represents really only one dimension. 

Figure 2:
A different phase space picture, specifically for type II critical collapse, and two 2dimensional projections of the same picture. In contrast with Figure 1, one dimension of the two representing the (infinitely many) decaying modes has been suppressed. The additional axis now represents a global scale which was suppressed in Figure 1, so that the scaleinvariant critical solution CS is now represented as a straight line (in red). Several members of a family of initial conditions (in blue) are attracted by the critical solution and then depart from it towards black hole formation (A or B) or dispersion (D). Perfectly finetuned initial data asymptote to the critical solution with decreasing scale. Initial conditions starting closer to perfect fine tuning produce smaller black holes, such that the parameter along the line of black hole end states is –ln M_{BH}. Two 2dimensional projections of the same picture are also given. The horizontal projection of this figure is the same as the vertical projection of Figure 1. 

Figure 3:
The spacetime diagram of all generic DSS continuations of the scalar field critical solution, from [157]. The naked singularity is timelike, central, strong, and has negative mass. There is also a unique continuation where the singularity is replaced by a regular centre except at the spacetime point at the base of the CH, which is still a strong curvature singularity. No other spacetime diagram is possible if the continuation is DSS. The lines with arrows are lines of constant adapted coordinate x, with the arrow indicating the direction of towards larger curvature. 

Figure 4:
Conformal diagram of the critical solution matched to an asymptotically flat one (RC: regular centre, S: singularity, SSH: selfsimilarity horizon). Curved lines are lines of constant coordinate , while converging straight lines are lines of constant coordinate x. Let the initial data on the Cauchy surface CS be those for the exact critical solution out to the 2sphere R, and let these data be smoothly extended to some data that are asymptotically flat, so that the future null infinity exists. To the past of the matching surface MS the solution coincides with the critical solution. The spacetime cannot be uniquely continued beyond the Cauchy horizon CH. The redshift from point A to point B is finite by selfsimilarity, and the redshift from B to C is finite by asymptotic flatness. 

Figure 5:
The final event horizon of a black hole is only known when the infall of matter has stopped. Radiation at 1 collapses to form a small black hole which settles down, but later more radiation at 2 falls in to give rise to a larger final mass. Finetuning of a parameter may result in , but the final mass would be approximately independent of . 
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