In a vacuum, the gravitational field equations take the form RR(X,Y)−12tr(RR(e,e))g(X,Y)+Λg(X,Y)=0
By taking the trace reverse they can be written as
RR(X,Y)=Λg(X,Y)
so any vacuum solution with a cosmological constant is a Riemann-Einstein metric. As user AzureSea states the deSitter-Schwartzchild solution is a spherically symmetric example.