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The Gowdy cosmologies provide a suitable arena to further develop Loop Quantum Cosmology, allowing the presence of inhomogeneities.
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Here, we call physical area that measured by the area operator defined on the kinematical Hilbert space, to distinguish it from the fiducial area
Cited in the paper.
There is a discrepancy in signs between this representation and that of Ref. awe1 because, in the latter, γ \gamma is considered to change sign under internal parity transformations, namely γ = | γ | sgn ( v ) \gamma=|\gamma|\text{sgn}(v) , while we treat γ \gamma just as a positive free parameter, which therefore is unaffected by transformations of the dynamical variables
Cited in the paper.
We understand non-densitized
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This difference is due to the factor 1 / ( 16 π G ) 1/(16\pi G) accompanying the classical action, which is not included in the definition of the constraint in this paper
Cited in the paper.
2009
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D. Brizuela, G.A. Mena Marugán, and T. Pawlowski, Classical Quantum Gravity 27
2010
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