 Vacuum constraints for gauge-invariant Minkowski perturbations

With the reversed convention in curvature-sign convention in Killing derivative identities, choose the representative $h_{00}=2\Phi$, $h_{0i}=V_i$, $h_{ij}=2\Psi {\delta }_{ij}+h_{ij}^{\mathrm{TT}}$. The linearized Einstein components are $G_{00}^{(1)}=-2\Delta \Psi$, $G_{0i}^{(1)}=-2{\partial }_i\dot{\Psi }-\Delta V_i/2$ and $G_{ij}^{(1)}=({\partial }_i{\partial }_j-{\delta }_{ij}\Delta )(\Phi -\Psi )-2{\delta }_{ij}\ddot{\Psi }-({\partial }_i{\dot{V}}_j+{\partial }_j{\dot{V}}_i)/2+\square h_{ij}^{\mathrm{TT}}/2$. On all space with regular decaying fields, or for nonzero spatial Fourier modes, the vacuum constraints remove the scalar and vector parts, leaving two radiative gravitational wave polarizations. Singular Coulomb fields, spatial boundaries and homogeneous modes are not covered by that removal argument.