Testing Kerr-CFT Conjecture for QN modes Calculation

The Kerr black hole solution is one of the most widely used models for astrophysical
rotating blackholes. In recent years, gravitational radiation due to a massive object (e.g
stars) plunging into a black hole has been investigated using the conjectured Kerr-CFT
correspondence. Quasi-normal modes (QNMs) for gravitational radiation can also be
computed numerically by solving Tequlosky equation with high precision. In this work,
we have compared QNMs of gravitational radiation derived from numerical techniques
with those predicted by the Kerr-CFT correspondence for near-extremal Kerr black
holes.