TRAPPIST-1 JWST CI Working Groups


Working Group 1: Assessing GTO observations.

The aim of this WG is to combine models from multiple groups to assess the possible scientific output of the GTO observations and identify complementary observations to be proposed in Cycle 1 for planets b, d, e, f (the other planets are not GTO targets). The science assessment will look at what models/environmental characteristics could be discriminated with the planned GTO observations and more extensive observations, including the significance of a null result.



Working Group 2: Complementary observations.

This WG aims to organize the ground- and space-based observations that would complement and optimize JWST observations, including transit timing/TTVs, RVs, stellar variability. These complementary observations could help constrain planetary atmospheric evaporation and photochemistry, and also provide input for photospheric + chromospheric models, as well as stellar contamination analyses. Other possibly useful complementarities include X-ray monitoring of TRAPPIST-1 with Chandra, applying for SWIFT ToO time. Monitoring in high-resolution spectroscopy could also be attempted.



Working Group 3: Planetary Environments and Evolution

This group will work on anticipated/predicted system-wide trends in atmospheric characteristics to help justify observing the entire sequence of 7 planets, rather than just one or two. This is an interdisciplinary group focused on atmospheres, including the modification of atmospheres via atmospheric loss as well as replenishment by outgassing. Specific questions to be addressed include: What can geophysics tell us about the possible atmospheric compositions of the planets, considering different bulk compositions and outgassing scenarios? We are working on a list of possible atmospheric scenarios for the planets, and the observations required to falsify or confirm these hypotheses, with the ultimate goal to develop a global and sequential plan for the atmospheric characterization of the planets. This will enable a detailed comparative study of the whole system, detect outliers, etc. This group is comprised of both forward modellers and those interested in modeling for spectroscopic retrieval.