  When galaxies move through the intracluster medium (ICM) inside galaxy
clusters, the ram pressure of the ICM can strip the gas from galaxies. The
stripped gas forms tails on the trailing side. These galaxies are hence dubbed
``jellyfish galaxies''. ESO 137-001 is a quintessential jellyfish galaxy
located in the nearest rich cluster, the Norma cluster. Its spectacular
multiphase tail has complex morphology and kinematics both from the imprinted
galaxy's interstellar medium (ISM) and as a result of the interactions between
the stripped gas and the surrounding hot plasma, mediated by radiative cooling
and magnetic fields. We study the kinematics of the multiphase tail using
high-resolution observations of the ionized and the molecular gas in the entire
structure. We calculate the velocity structure functions (VSFs) in moving
frames along the tail and find that turbulence driven by Kelvin-Helmholtz (KH)
instability quickly overwhelms the original ISM turbulence and saturates at
$\sim 30$ kpc. There is also a hint that the far end of the tail has possibly
started to inherit pre-existing large-scale ICM turbulence likely caused by
structure formation. Turbulence measured by the molecular gas is generally
consistent with that measured by the ionized gas in the tail but has a slightly
lower amplitude. Most of the measured turbulence is below the mean free path of
the hot ICM ($\sim 11$ kpc). Using warm/cool gas as a tracer of the hot ICM, we
find that the isotropic viscosity of the hot plasma must be suppressed below
0.01 percent Spitzer level.
