The project "TArget PrioritizAtion routineS for CHEOPS observations" (TAPAS4CHEOPS) is funded by the Austrian Research Promotion Agency (FFG) under the ASAP12 scheme and as part of the Austrian contribution to the CHEOPS mission.
Both exoplanet missions and ground-based facilities revealed the existence of a great variety of planets, particularly of intermediate-mass (sub-Neptune, super-Earth) with masses between 2 and 14 MEarth, which present a large spread in density. These planets are the primary target of CHEOPS, the first S-class ESA mission, which aim is the detection of shallow transits of low- and intermediate-mass planets orbiting bright stars. Typical CHEOPS targets will be systems hosting planets already detected by radial velocity, for which CHEOPS will search for transits, and systems hosting planets detected with the transit method by other facilities (e.g., NGTS and TESS), but for which the measurement of the radius requires a considerable improvement. Hundreds of possible CHEOPS targets are foreseen, but the time constrained nature of CHEOPS observations will not allow to observe them all. It is therefore necessary to construct a target prioritization strategy.
The primary aim of this project is to produce the currently missign piece of information to provide a tool for a fast target prioritisation. We have built a method and tool capable of providing a fast rough planet characterisation, based on theoretical models, for CHEOPS targets. We developed a method that allows one to provide a first characterisation of the atmosphere of an intermediate-mass planet provided only its transit radius. The method allows one also to infer the minimum planetary mass, while the maximum mass can be inferred from considerations on planetary density and formation. Our routines further constrain the past rotation history of planet hosts.
We have computed a large grid of hydrodynamic models of the upper atmosphere of planets considering a parameter space composed by: planetary mass, radius, equilibrium temperature, and stellar high-energy input flux. We used the grid of models, together with available predictions of the atmospheric masses to compute planet atmospheric evolution tracks, taking into account a range of realistic levels for the initial high-energy stellar flux. We used the grids to design a characterisation scheme for the planets discovered with the radial velocity method and with transits detected by CHEOPS.
The project ended in November 2018.
Luca Fossati (PI)
Darya Kubyshkina (main project postdoc)
Helmut Lammer (support)
Monika Lendl (support)
The grid of planetary upper atmosphere models and interpolation routine presented by Kubyshkina et al. (2018) can be downloaded here.
This is still work in progress and to properly use the data/information contained in the tar file, please, contact us at daria.kubyshkina AT oeaw.ac.at or luca.fossati AT oeaw.ac.at
HD 219666 b: a hot-Neptune from TESS Sector 1.
Esposito, M.; et al. (2019); A&A.
Grid of upper atmosphere models for 1-40 ME planets: application to CoRoT-7 b and HD 219134 b,c.
Kubyshkina, D.; et al. (2018); A&A.
Overcoming the Limitations of the Energy-limited Approximation for Planet Atmospheric Escape.
Kubyshkina, D.; et al. (2018); ApJL.
Young planets under extreme UV irradiation. I. Upper atmosphere modelling of the young exoplanet K2-33b.
Kubyshkina, D.; et al. (2018); A&A.
TESS's first planet. A super-Earth transiting the naked-eye star pi Mensae.
Gandolfi, D.; et al. (2018); A&A.
Super-Earth of 8 ME in a 2.2-day orbit around the K5V star K2-216.
Persson, C.; et al. (2018); A&A.