  Ram pressure stripping (RPS) is an important mechanism for galaxy evolution.
In this work, we present results from HST and APEX observations of one RPS
galaxy, ESO 137-002 in the closest rich cluster Abell 3627. The galaxy is known
to host prominent X-ray and H$\alpha$ tails. The HST data reveal significant
features indicative of RPS in the galaxy, including asymmetric distribution of
dust in the galaxy, dust filaments and dust clouds in ablation generally
aligned with the direction of ram pressure, and young star clusters immediately
upstream of the residual dust clouds that suggest star formation (SF) triggered
by RPS. The distribution of the molecular gas is asymmetric in the galaxy, with
no CO upstream and abundant CO downstream and in the inner tail region. A total
amount of $\sim 5.5 \times 10^{9}$ M$_\odot$ of molecular gas is detected in
the galaxy and its tail. On the other hand, we do not detect any active SF in
the X-ray and H$\alpha$ tails of ESO 137-002 with the HST data and place a
limit on the SF efficiency in the tail. Hence, if selected by SF behind the
galaxy in the optical or UV (e.g., surveys like GASP or using the Galex data),
ESO 137-002 will not be considered a ``jellyfish'' galaxy. Thus, galaxies like
ESO 137-002 are important for our comprehensive understanding of RPS galaxies
and the evolution of the stripped material. ESO 137-002 also presents a great
example of an edge-on galaxy experiencing a nearly edge-on RPS wind.
