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HST has completed a number of surveys for a wide range of exoplanets comma enabling comparative planetology. In the dozens of planets studied thus far comma clouds and hazes have been found to be prevalent comma and are seen to hide spectroscopic features. The atmospheric properties of giant planets are expected to vary substantially as the compositions of their host stars change comma and a host star.s metallicity should be an excellent proxy for the composition of the protoplanetary disk from it formed. Giant planets which formed in sufficiently metal-poor environments should in principle show marked differences in their atmospheric properties. In particular comma planets around metal-poor stars should have preferentially clearer atmospheres and stronger molecular features comma as there is less refractory elements such as Mg or Fe to make condensate clouds. The gas-phase chemistry will also change as key volatile ratios like C-O change. However comma to date no hot Jupiters orbiting metal-poor stars (CORCHETE_OPENFe-HCORCHETE_CLOSE < -0.3) have been targeted by HST comma with the vast majority found in metal-rich environments. Our program takes the next steps in comparative exoplanetology comma targeting exoplants with reliably low stellar metallicities down to a new metal-poor extreme (CORCHETE_OPENFe-HCORCHETE_CLOSE < -0.49). This will provide the very first comprehensive atmospheric constraints for planets around metal-poor stars comma which can then be compared to the plentiful metal-rich sample. A detailed comparison of stellar abundances to the spectral features as seen in the planet could reveal correlations that provide new insights into the atmospheric chemistry of hot Jupiters comma and new insights into the nature of the planet-star metallicity connection.