tokens: We are grateful to the referee, Prof. Michael Shull, for his thorough reading and for useful comments and suggestions that have significantly improved the clarity of the paper. E.L. thanks G. Calderone for having modified the code QSFit to handle low-resolution WFC3 spectra and for feedback and suggestions on the fitting procedure. E.L. is supported by a European Union COFUND/Durham Junior Research Fellowship (under EU grant agreement 609412). M.F. acknowledges support by the Science and Technology Facilities Council (grant ST/P000541/1). This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement 757535). Support for HST Program GO-14127 was provided by NASA through grants from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS526555. M.R. acknowledges support by HST-GO-14127.011 and a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Some of the data presented herein were obtained at the W.M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency’s scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Facilities: HST (WFC3) , Keck:II (ESI). Software: astropy (Astropy Collaboration et al. 2013 ), corner (Foreman-Mackey 2016 ), matplotlib (Hunter 2007 ), emcee (Foreman-Mackey et al. 2013 ), QSFit (Calderone et al. 2017 ).
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