  We wish to carry forward to higher dimensions the insightful and novel method
of obtaining the Kerr metric proposed by one of us [Gen. Relativ. Gravit. 45,
2383 (2013)] for deriving the Myers-Perry rotating black hole metric. We begin
with a flat spacetime metric written in oblate spheroidal coordinates
(ellipsoidal geometry) appropriate for the inclusion of rotation, and then
introduce arbitrary functions to introduce a gravitational potential due to
mass, which are then determined by requiring that a massless particle
experiences no acceleration, while a massive particle feels Newtonian
acceleration at large r. We further generalize the method to include the
cosmological constant {\Lambda} to obtain the MyersPerry de Sitter/antide
Sitter black hole metric.
