= Solution
* \b[Muted near-infrared molecular bands:] <exoplanet transmission spectra> across approximately $1.1$–$1.7\,\mu\mathrm m$, or a broader $1$–$5\,\mu\mathrm m$ interval, can show weak <water> features because an opaque <exoplanet cloud deck> truncates the atmospheric annulus before the gas becomes transparent in the continuum.
* \b[A rising transit radius towards blue wavelengths:] optical <exoplanet transmission spectroscopy> over roughly $0.3$–$1\,\mu\mathrm m$ can show a <Rayleigh scattering> or aerosol slope from small haze particles. Larger particles can instead give a nearly wavelength-independent, grey continuum.
* \b[Enhanced reflected light:] an optical <exoplanet secondary eclipse> or <reflected-light planetary phase curve> observation around $0.4$–$0.9\,\mu\mathrm m$ can indicate a large <geometric albedo> and wavelength-dependent reflection from bright condensate <exoplanet clouds>.
Cloud particles can scatter or absorb, so not every <atmospheric haze> makes a high-albedo planet. Weak molecular bands alone also admit low abundance or high <mean molecular weight>; a consistent spectral combination is stronger evidence than a single signature.
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