HST colors of ESO 137-001 tail stars

ESO 137-001 is known to host a prominent stripped tail detected in many bands from X-rays, H {alpha} 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, H II regions from H {alpha} (MUSE), and dense molecular clouds from CO (ALMA). The correlation between the HST blue star clusters and the H II 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 per cent of the SF rate in the galaxy.