We start with an elementary example of a nonsingular configuration using a trivial solution to massive gravity yielding a nonzero initial time step. Then we present a history of the cosmological constant issue from Einstein’s introduction—which did not work because his static universe solution to the Ricci Scalar problem and GR was unstable—to the radius of the universe being proportional to the inverse square root of the cosmological constant. We use two spacetime first integrals to isolate a nonperturbative cosmological constant solution at the surface of the start of expansion of the universe. A phenomenological solution to the cosmological constant involves scaling the radius of the present universe. Our idea is to instead solve the cosmological constant at the surface of the initial spacetime bubble, using the initially derived time step, ∆t, as input for the cosmological constant. This was done in a Zeldovich4 section for dark energy; solving the initial value of the cosmological constant supports one of the models of DE and why the universe reaccelerated a billion years ago. We depend on Katherine Freese’s Zeldovich4 talk of dark stars, which form supermassive black holes, to consume initially created DM, and Abhay Ashtekar’s nonsingular start to the universe as part of a solution to low l values in CMBR data. We conclude with a reference to a multiverse generalization of Penrose’s cyclic conformal cosmology as input to the initial nonsingular spacetime bubble.