  We study numerically the late-time tails of linearized fields with any spin
$s$ in the background of a spinning black hole. Our code is based on the
ingoing Kerr coordinates, which allow us to penetrate through the event
horizon. The late time tails are dominated by the mode with the least multipole
moment $\ell$ which is consistent with the equatorial symmetry of the initial
data and is equal to or greater than the least radiative mode with $s$ and the
azimuthal number $m$.
