  We present the results from the HST WFC3 and ACS data on an archetypal galaxy
undergoing ram pressure stripping (RPS), ESO 137-001, in the nearby cluster
Abell 3627. ESO 137-001 is known to host a prominent stripped tail detected in
many bands from X-rays, Halpha to CO. The HST data reveal significant features
indicative of RPS such as asymmetric dust distribution and surface brightness
as well as many blue young star complexes in the tail. We study the correlation
between the blue young star complexes from HST, HII regions from Halpha (MUSE)
and dense molecular clouds from CO (ALMA). The correlation between the HST blue
star clusters and the HII regions is very good, while their correlation with
the dense CO clumps are typically not good, presumably due in part to
evolutionary effects. In comparison to the Starburst99+Cloudy model, many blue
regions are found to be young (< 10 Myr) and the total star formation (SF) rate
in the tail is 0.3 - 0.6 M_Sun/yr for sources measured with ages less than 100
Myr, about 40% of the SF rate in the galaxy. We trace SF over at least 100 Myr
and give a full picture of the recent SF history in the tail. We also
demonstrate the importance of including nebular emissions and a nebular to
stellar extinction correction factor when comparing the model to the broadband
data. Our work on ESO 137-001 demonstrates the importance of HST data for
constraining the SF history in stripped tails.
