1.Maintain capabilities for high spatial-resolution imaging of bright, extended sources within our own solar system (UV, visible, IR) in the post-Hubble era.
a.Jupiter and Saturn will be too bright to image with many JWST filters. Saturn could be imaged by JWST/NIRCAM at the very longest wavelengths, but imaging of Jupiter would require a highly specialised mode. Jupiter and Saturn can be imaged using JWST/MIRI neutral density filter, provided specific calibration procedures are adopted. Uranus and Neptune can be observed in both imaging and spectroscopic mode.
b.Provisions should be made in the JWST designs to ensure that outer planets can be observed in both imaging and spectroscopic modes
2.Establish a space-borne telescopic facility for the semi-continuous monitoring of atmospheric dynamics and compositional changes, across a wide range of temporal scales (hours, to weeks, to seasonal variability).
a.Enable a fast response to rapidly evolving phenomena on the gas giants (e.g. asteroidal/cometary impacts, global disturbances).
b.Contextual support for orbiting spacecraft and in situ probes.
c.Imaging and spectroscopic modes across a broad range of frequencies (UV to far-IR) to capture regions of the spectrum inaccessible from the ground.
3.Update ground-based observatories for discovery-class science and support of planned spacecraft missions.
a.Larger primary mirrors (in the 8-10 m range) for IR diffraction-limited resolutions.
b.Investment in new adaptive optics technologies and outfitting existing observatories.
c.Investment in upgraded instrumentation covering mid-IR wavelengths to replace existing technologies, extend wavelength range, improve spatial/spectral resolution.
4.Ongoing support for laboratory studies pertinent to interpretation of outer planet atmospheric measurements.
a.Spectroscopic measurements for species at relevant temperatures and pressures (e.g. high pressures and temperatures for NH3, H2S, H2O for interpretation of Juno microwave spectra).
b.Numerical simulations for general circulation models, radiative models, thermochemical and photochemical models, etc.
c.Geophysical fluid dynamics experiments for simulations of outer planet flow.
d.High-pressure equation of state experiments in the lab for extreme conditions in the centres of the outer planets.
e.Low temperature measurements for the IR opacity of H2-He mixtures pertinent to the ice giants (i.e. below 60 K at pressures around 1 bar).
5.Investment in new technologies for mitigation of extreme environments for visiting spacecraft:
b.Extremes of temperature and pressure for entry probe missions, and ablative materials for heat shield manufacture.
c.Efficient solar-panel technologies for the low-light conditions of the outer solar system.
d.Mini-probes to trace the atmospheric circulation and measure composition at multiple locations.
e.Development of new power sources for outer planet missions to mitigate the depleted stockpiles of Plutonium-238 for RTGs.
f.Development of fast IR detectors with increased sensitivity for detection of low fluxes, prevent image smearing and enable rapid mapping.
g.Low-power instrumentation, particularly for ice giant missions.
6.Inclusion of Outer Planet Atmospheric science as a major component in any satellite-focused mission (flybys or orbiters):
a.Jupiter atmospheric science should be made a major consideration for EJSM, with modifications to satellite-focused instruments (particularly in the visible, near-IR and thermal-IR) to produce high-quality atmospheric science.
b.Provision in designs for Titan/Enceladus missions to study Saturn’s atmosphere.
c.Ensuring Uranus and Neptune missions feature the ice giant atmospheres as a primary mission driver.
7.Ensure mission support structures are maintained and improved for future missions:
a.Upgrades to the Deep Space Network so that data is no longer lost on a regular basis.
b.Increased support for early-career scientists to provide exposure to mission operations and planning during an active mission (e.g. Cassini).
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