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Gersten [Phys. Rev. Lett. 26, 1000 (1971]. In Table I, the value of m 6 should be given as 962 MeV 0 On page 1003, in the formula for P -A, h{6) should be starred, i.e., P -The formula at the bottom of page 1003 which relates the time-reversal violating amplitude t(0) to the scattering T matrix is incorrect and should be replaced byThe correct formula for t{6) was used in all calculations of experimental observables, hence our tables and graphs stand correct as published. However, the sequence of inequalities at the top of page 1004 should be replaced by

Contents 1. Introduction . 2. Motives , 2.1. Unacceptable difficulties in unquantized general relativity . 2.2. T h e basic tenets of contemporary physics demand that the gravitational field be quantized . 2.3. Quantum general relativity raises questions of measurement and interpretation which may contribute to an improved understanding of quantum theory . 2.4. Quantum general relativity promises rich rewards. 3.1, Geometrical background . 3.2. Action principle, field equations and Bianchi identities . 3.3. Benefits of separating time and space . 4.1. The nature of canonical formalism . 4.2. Lapse and shift functions as Lagrange multipliers for taking 4.3, Asymptotic isometries and energy-momentum 5.1. Canonical quantization.5.2. Sum over histories: a computational procedure . 5.3.History vectors: a unified approach to quantization 5.4. Source theory .6. Graviton scattering: current results and prospects 6.1. T h e generalized Green functions 6.2. The reduction formalism .6.3, Covariance, unitarity and fictitious particles .6.4. Operators and time-ordering . 6.5. Divergences . 7.1. The frozen formalism problem of generally covariant theories 7.2. The superspace representations of generally covariant closed universe quantization . 7.3. Hamilton-Jacobi quantization . 7.4. Model theories. 8.1. What is superspace ? , 8.2. What good is superspace ? . 8.3. Metrics for superspace , 8.4. What physics is there in superspace ? . . 3. Einstein's theory in rCsumC .

Einstein’s vacuum field equations are solved for spacetimes with two−parameter spacelike symmetry, a space−reflection symmetry, and space sections homeomorphic to either S1×S2 or S3. All integrals are evaluated, and the spacetime metrics are presented in analytic form.