### 5.13 Loop inspired quantum cosmology

The constructions described so far in this section follow all the steps in the full theory as closely as
possible. Most importantly, one obtains quantum representations inequivalent to those used in a
Wheeler–DeWitt quantization, which results in many further implications. This has inspired investigations
where not all the steps of loop quantum gravity are followed, but only the same type of representation, i.e.,
the Bohr Hilbert space in an isotropic model, is used. Other constructions, based on ADM rather than
Ashtekar variables, are then done in the most straightforward way rather than a way suggested by the full
theory [188].
In isotropic models the results are similar, but already here one can see conceptual differences. Since the
model is based on ADM variables, in particular using the metric and not triads, it is not clear what the
additional sign factor , which is then introduced by hand, means geometrically. In loop quantum
cosmology it arose naturally as an orientation of triads, even before its role in removing the classical
singularity, to be discussed in Section 5.16, had been noticed. (The necessity of having both signs available
is also reinforced independently by kinematical consistency considerations in the full theory [171].) In
homogeneous models the situation is even more complicated since sign factors are still introduced by hand,
but not all of them are removed by discrete gauge transformations as in Section 5.8 (see [230] as
opposed to [14]). Those models are useful to illuminate possible effects, but they also demonstrate
how new ambiguities, even with conceptual implications, arise if guidance from a full theory is
lost.

In particular, the internal time dynamics is more ambiguous in those models and thus not usually
considered. There are then only arguments that the singularity could be avoided through the boundedness
of relevant operators [191], but those statements are not generic in anisotropic models [82] or even the full
theory [120]. Moreover, even if all curvature quantities could be shown to be bounded, the evolution could
still stop (as happens classically where not any singularity is also a curvature singularity). The focus has
shifted to an understanding of horizon dynamics in black hole collapse, where not all properties of the
quantum representation may be crucial [190, 189, 192].