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Thousands of transiting exoplanets have been discovered, but spectralanalysis of their atmospheres has so far been dominated by a small number ofexoplanets and data spanning relatively narrow wavelength ranges (such as 1.1to 1.7 {\mu}m). Recent studies show that some hot-Jupiter exoplanets have muchweaker water absorption features in their near-infrared spectra than predicted.The low amplitude of water signatures could be explained by very low waterabundances, which may be a sign that water was depleted in the protoplanetarydisk at the planet's formation location, but it is unclear whether this levelof depletion can actually occur. Alternatively, these weak signals could be theresult of obscuration by clouds or hazes, as found in some optical spectra.Here we report results from a comparative study of ten hot Jupiters coveringthe wavelength range 0.3-5 micrometres, which allows us to resolve both theoptical scattering and infrared molecular absorption spectroscopically. Ourresults reveal a diverse group of hot Jupiters that exhibit a continuum fromclear to cloudy atmospheres. We find that the difference between the planetaryradius measured at optical and infrared wavelengths is an effective metric fordistinguishing different atmosphere types. The difference correlates with thespectral strength of water, so that strong water absorption lines are seen inclear-atmosphere planets and the weakest features are associated with cloudsand hazes. This result strongly suggests that primordial water depletion duringformation is unlikely and that clouds and hazes are the cause of weakerspectral signatures.

A continuum from clear to cloudy hot-Jupiter exoplanets without primordial water depletion