Into the UV: The Atmosphere of the Hot Jupiter HAT-P-41b Revealed

摘要: For solar system objects, ultraviolet spectroscopy has been critical in identifying sources of stratospheric heating and measuring the abundances a variety hydrocarbon sulfur-bearing species, produced via photochemical mechanisms, as well oxygen ozone. To date, fewer than 20 exoplanets have probed this wavelength range (0.2–0.4 μm). Here we use data from Hubble's newly implemented WFC3 UVIS G280 grism to probe atmosphere hot Jupiter HAT-P-41b through optical combination with observations at infrared wavelengths. We analyze interpret HAT-P-41b's 0.2–5.0 μm transmission spectrum using broad methodologies including multiple treatments systematics comparisons atmospheric forward, cloud microphysical, retrieval models. Although some analysis interpretation methods favor presence clouds or potentially Na, VO, AlO, CrH explain portions spectrum, find that significant H⁻ opacity provides most robust explanation. obtain constraint for abundance H⁻, log(H⁻) = -8.65 ± 0.62, atmosphere, which is several orders magnitude larger predictions equilibrium chemistry ~1700–1950 K Jupiter. show collisional processes on hydrogen-dominated can readily supply necessary amount H− suggest such are work atmospheres many other Jupiters.