TY - GEN
T1 - JWST-YSES: a Young Suns Exoplanet Survey to study the demographics of sub-Jovian planets around Sun-like stars and unveil the formation and evolution history of widely separated companions
AU - Kammerer, Jens
AU - Pueyo, Laurent
AU - Balmer, William
AU - Bogat, Ell
AU - Bonavita, Mariangela
AU - Burr, Zach
AU - Carter, Aarynn L.
AU - Chen, Christine
AU - Cugno, Gabriele
AU - Fontanive, Clemence
AU - Ginski, Christian
AU - Girard, Julien
AU - Hinkley, Sasha
AU - Hoch, Kielan K. W.
AU - Kenworthy, Matthew
AU - Manjavacas, Elena
AU - Perrin, Marshall
AU - Rebollido, Isabel
AU - Rickman, Emily
AU - van Capelleveen, Richelle Felicia
PY - 2025/3
Y1 - 2025/3
N2 - As of now, the vast majority of wide separation giant planets around FGK-type hosts have been imaged around stars in the ~10–15 Myr Sco-Cen association or younger. To this date, the origin of this population of widely-separeted massive (>5 MJup) giant planets remains elusive. However, today JWST presents a unique opportunity to resolve this mystery, by probing the giant planet frequency for less massive (0.1-5 MJup) companions which only JWST can detect. This proposal aims to (1) measure the frequency of young long-period sub-Jovian exoplanets which still lacks observational constraints and (2) distinguish between in-situ formation via gravitational instability vs. formation via core accretion closer to the star followed by outward migration/scattering as the origin of the existing massive (>5 MJup) Sco-Cen giant planets. These goals will be achieved by searching for new 0.1-5 MJup giant planets around 30 Sun-like stars in the Sco-Cen association using NIRCam coronagrapy and comparing observations to planet population synthesis simulations. Should the core-accretion+migration scenario prevail, this proposal will uncover a large reservoir of wide separation sub-Jovian planets. On the other hand, if the existing massive Sco-Cen planets formed via gravitaional instability, this proposal will detect no new sub-Jovian planets because in-situ formation is extremely inefficient for these low-mass planets at wide separations from the star. As such, this proposal will provide the first demographic evidence for giant planet migration/scattering - or lack thereof - of giant planets orbiting wider than 10 au, and further populate the age-luminosity diagram for sub-Jovian planets....
AB - As of now, the vast majority of wide separation giant planets around FGK-type hosts have been imaged around stars in the ~10–15 Myr Sco-Cen association or younger. To this date, the origin of this population of widely-separeted massive (>5 MJup) giant planets remains elusive. However, today JWST presents a unique opportunity to resolve this mystery, by probing the giant planet frequency for less massive (0.1-5 MJup) companions which only JWST can detect. This proposal aims to (1) measure the frequency of young long-period sub-Jovian exoplanets which still lacks observational constraints and (2) distinguish between in-situ formation via gravitational instability vs. formation via core accretion closer to the star followed by outward migration/scattering as the origin of the existing massive (>5 MJup) Sco-Cen giant planets. These goals will be achieved by searching for new 0.1-5 MJup giant planets around 30 Sun-like stars in the Sco-Cen association using NIRCam coronagrapy and comparing observations to planet population synthesis simulations. Should the core-accretion+migration scenario prevail, this proposal will uncover a large reservoir of wide separation sub-Jovian planets. On the other hand, if the existing massive Sco-Cen planets formed via gravitaional instability, this proposal will detect no new sub-Jovian planets because in-situ formation is extremely inefficient for these low-mass planets at wide separations from the star. As such, this proposal will provide the first demographic evidence for giant planet migration/scattering - or lack thereof - of giant planets orbiting wider than 10 au, and further populate the age-luminosity diagram for sub-Jovian planets....
M3 - Other contribution
ER -