Exploring Giant Planet Atmospheres with Habitable Worlds Observatory
Visible and ultraviolet imaging and spectroscopy of Solar System giant planets can set the paradigm for the atmospheric, ionospheric, and magnetospheric processes shaping the diversity of giant exoplanets, brown dwarfs, and their interactions with stellar hosts.
Spectra of their molecular absorptions, aerosol scattering, airglow, and auroral emissions can reveal these dynamic atmospheres in three dimensions. Given that giant planets are extended, bright, moving, and rotating objects, with extreme dynamic range and highly variable appearances, they impose specific mission and instrumentation requirements on future large space-based optical/UV observatories like the proposed Habitable Worlds Observatory (HWO).
We advocate that HWO must have the capability to track non-sidereal targets like the giant planets and their satellites; should be able to view auroras and atmospheres without saturation (e.g., through the use of filters or fast read-out modes); and with a high dynamic range to explore faint objects near bright discs.
HWO should enable spatially-resolved spectroscopy from ∼80 nm to ∼900 nm, capturing H2 Lyman and Werner band series and H Lyman-α in the far-UV; molecular absorptions and scattering in the mid-UV/visible; and deep hydrogen/methane absorptions in the 800-900 nm for cloud characterisation and CH4 mapping.
Imaging should enable time-resolved observations, from seconds to create auroral movies, to hours for cloud tracking and winds, to months and years for atmosphere/ionosphere variability. We advocate that an imager should have sufficient field of view to capture Jupiter (>50\arcsec), and that UV/visible integral field spectrographs be considered with both narrow (3\arcsec) and wide (>10\arcsec) field capabilities to provide efficient mapping of atmospheres and auroras. [Abbr]
Montage of Jupiter spectra from the UV (Melin et al. 2020; Edgington et al. 1999), visible (Karkoschka 1994), and near-infrared (Rayner et al. 2009; Encrenaz 2003), adapted from Fletcher et al. (2023). Key atmospheric absorptions and emissions have been labelled. We define the spectral ranges as follows: extreme UV (50-120 nm); far-UV (121-200 nm), mid-UV (200-300 nm), near-UV (300-400 nm), visible (> 400 nm), near-IR (> 900 nm), and the start of the mid-IR at ∼ 5 µm. — astro-ph.IM
Leigh N. Fletcher, Amy Simon, Michael H. Wong, Jonathan D. Nichols, Nick A. Teanby, Conor A. Nixon, Marina Galand
Comments: 12 pages, this article is an adaptation of a science case document developed for HWO’s Solar System Steering Committee
Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM); Earth and Planetary Astrophysics (astro-ph.EP)
Cite as: arXiv:2510.17926 [astro-ph.IM] (or arXiv:2510.17926v1 [astro-ph.IM] for this version)
https://doi.org/10.48550/arXiv.2510.17926
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From: Leigh Fletcher
[v1] Mon, 20 Oct 2025 09:49:03 UTC (7,927 KB)
https://arxiv.org/abs/2510.17926
Astrobiology, Exoplanet,
