How Other Projects Will Enable JWST Transiting Planet Science David Charbonneau (Harvard) 18 November 2015 Questions for Today Where will our JWST targets originate? What role do current and planned ground- based activities play in JWST transiting exoplanet science? What role do current and planned missions play in JWST transiting planet science? The Current Target List (R p < 5 R Earth ) Figure by Z. Berta-Thompson The Current Target List (R p < 5 R Earth ) Figure by Z. Berta-Thompson The Best Ones Start with the Letter G M Dwarf Properties 0.07 < mass < 0.6 M sun G2 M = 1 M sun R = 1 R sun T = 5800 K M3 M = 0.45 M sun R = 0.45 R sun T = 3500 K M6 M = 0.12 M sun R = 0.18 R sun T = 2900 K Earth --sizes to scale-- Slide by Jacob Bean The MEarth Project David Charbonneau, Jonathan Irwin, Zachory Berta-Thompson, Elisabeth Newton & Jason Dittmann Photo by Jonathan Irwin MEarth Discovers GJ1132b 11 May 2015 Movie & Observatory by Jonathan Irwin (Harvard-Smithsonian CfA) GJ1132b is the Only Spectroscopically Accessible Terrestrial Exoplanet Simulated transmission (top) & emission (bottom) spectra of with JWST, assuming a pure CO 2 atmosphere (Miller-Ricci & Fortney 2010). JWST/NIRISS uncertainties are approximated by scaling from achieved Hubble/WFC3 precision (Kreidberg et al. 2014); JWST/MIRI uncertainties are estimated from expected performance (Cowan et al. 2015; Kendrew et al. 2015). Figure by Z. Berta-Thompson & H. Diamond-Lowe The Current Target List (R p < 5 R Earth ) Figure by Z. Berta-Thompson The Current Target List (R p < 5 R Earth ) Figure by Z. Berta-Thompson Discovered by Radial Velocities & Transits Found from Space The Current Target List (R p < 5 R Earth ) Figure by Z. Berta-Thompson Discovered by Radial Velocities & Transits Found from Space The Current Target List (R p < 5 R Earth ) Figure by Z. Berta-Thompson Discovered by Radial Velocities & Transits Found from Space Many Ongoing / Upcoming Dedicated M-dwarf Planet Surveys SPIROU (RV, CFHT) CARMENES (RV, Calar Alto Observatory) HPF (RV, Hobby Eberly Telescope) APACHE (Transit, Italy) MEarth-N and MEarth-S (Transit, Arizona + Chile) SPECULOOS (Transit, Chile) EXTRA (Transit, Chile) Also, NGTS, HARPS, HARPS-N, HIRES, and others Kepler covered 0.3% of sky K2 might cover 6% of sky Kepler + K2 cannot find the best targets for JWST TESS Simulated Detections Sullivan et al. ApJ 2015 The Figure That Zach Berta-Thompson Made t hat you wont be able to get out of your mind Feasibility of Mass Measurements of TESS Planets Sullivan et al. ApJ 2015 Feasibility of Transit Spectroscopy of TESS Planets Sullivan et al. ApJ 2015 Slide by Z. Berta-Thompson Slide by D. Ehrenreich Slide by A. Sozzetti Hubble Space Telescope M-dwarfs offer overwhelming SNR advantages for study of terrestrial planet atmospheres with JWST. We will be in position of comparing terrestrial exoplanets orbiting M-dwarfs with solar system terrestrial planets. Use HST to gather UV spectra of host stars. Use HST to vet candidates for puffy (i.e. low mean molecular weight atmospheres) and find best candidates for JWST. Yes, HST is now the finderscope. Hubble Space Telescope M-dwarfs offer overwhelming SNR advantages for study of terrestrial planet atmospheres with JWST. We will be in position of comparing terrestrial exoplanets orbiting M-dwarfs with solar system terrestrial planets. Use HST to gather UV spectra of host stars. Use HST to vet candidates for puffy (i.e. low mean molecular weight atmospheres) and find best candidates for JWST. Yes, HST is now the finderscope. Conclusions GJ1132 is a good benchmark for JWST simulations. TESS will find 500 Earths and super-Earths transiting nearby stars, and the majority of small planets targeted by JWST will come from TESS. A robust ground-based program is essentially to confirm TESS planets and measure their densities. We need to have a credible path for targets if TESS fails or is delayed. Ground-based surveys + Spitzer provide a reasonable Plan B. CHEOPS has open time and provides a means to search for transits of RV-detected planets and improve SNR of TESS discoveries. GAIA is on schedule to provide parallaxes for TESS target list and any conceivable JWST exoplanet target. The interaction of a terrestrial planet atmosphere with an illuminating M- dwarf spectrum is a fundamental question for modelers. HST will gather UV spectra of M-dwarf planet hosts and vet mean molecular weight of candidate JWST targets. Conclusions GJ1132 is a good benchmark for JWST simulations. TESS will find 500 Earths and super-Earths transiting nearby stars, and the majority of small planets targeted by JWST will come from TESS. A robust ground-based program is essentially to confirm TESS planets and measure their densities. We need to have a credible path for targets if TESS fails or is delayed. Ground-based surveys + Spitzer provide a reasonable Plan B. CHEOPS has open time and provides a means to search for transits of RV-detected planets and improve SNR of TESS discoveries. GAIA is on schedule to provide parallaxes for TESS target list and any conceivable JWST exoplanet target. The interaction of a terrestrial planet atmosphere with an illuminating M- dwarf spectrum is a fundamental question for modelers. HST will gather UV spectra of M-dwarf planet hosts and vet mean molecular weight of candidate JWST targets. Conclusions GJ1132 is a good benchmark for JWST simulations. TESS will find 500 Earths and super-Earths transiting nearby stars, and the majority of small planets targeted by JWST will come from TESS. A robust ground-based program is essentially to confirm TESS planets and measure their densities. We need to have a credible path for targets if TESS fails or is delayed. Ground-based surveys + Spitzer provide a reasonable Plan B. CHEOPS has open time and provides a means to search for transits of RV-detected planets and improve SNR of TESS discoveries. GAIA is on schedule to provide parallaxes for TESS target list and any conceivable JWST exoplanet target. The interaction of a terrestrial planet atmosphere with an illuminating M- dwarf spectrum is a fundamental question for modelers. HST will gather UV spectra of M-dwarf planet hosts and vet mean molecular weight of candidate JWST targets. Conclusions GJ1132 is a good benchmark for JWST simulations. TESS will find 500 Earths and super-Earths transiting nearby stars, and the majority of small planets targeted by JWST will come from TESS. A robust ground-based program is essentially to confirm TESS planets and measure their densities. We need to have a credible path for targets if TESS fails or is delayed. Ground-based surveys + Spitzer provide a reasonable Plan B. CHEOPS has open time and provides a means to search for transits of RV-detected planets and improve SNR of TESS discoveries. GAIA is on schedule to provide parallaxes for TESS target list and any conceivable JWST exoplanet target. The interaction of a terrestrial planet atmosphere with an illuminating M- dwarf spectrum is a fundamental question for modelers. HST will gather UV spectra of M-dwarf planet hosts and vet mean molecular weight of candidate JWST targets. Conclusions GJ1132 is a good benchmark for JWST simulations. TESS will find 500 Earths and super-Earths transiting nearby stars, and the majority of small planets targeted by JWST will come from TESS. A robust ground-based program is essentially to confirm TESS planets and measure their densities. We need to have a credible path for targets if TESS fails or is delayed. Ground-based surveys + Spitzer provide a reasonable Plan B. CHEOPS has open time and provides a means to search for transits of RV-detected planets and improve SNR of TESS discoveries. GAIA is on schedule to provide parallaxes for TESS target list and any conceivable JWST exoplanet target. The interaction of a terrestrial planet atmosphere with an illuminating M- dwarf spectrum is a fundamental question for modelers. HST will gather UV spectra of M-dwarf planet hosts and vet mean molecular weight of candidate JWST targets. Conclusions GJ1132 is a good benchmark for JWST simulations. TESS will find 500 Earths and super-Earths transiting nearby stars, and the majority of small planets targeted by JWST will come from TESS. A robust ground-based program is essentially to confirm TESS planets and measure their densities. We need to have a credible path for targets if TESS fails or is delayed. Ground-based surveys + Spitzer provide a reasonable Plan B. CHEOPS has open time and provides a means to search for transits of RV-detected planets and improve SNR of TESS discoveries. GAIA is on schedule to provide parallaxes for TESS target list and any conceivable JWST exoplanet target. The interaction of a terrestrial planet atmosphere with an illuminating M- dwarf spectrum is a fundamental question for modelers. HST will gather UV spectra of M-dwarf planet hosts and vet mean molecular weight of candidate JWST targets. Conclusions GJ1132 is a good benchmark for JWST simulations. TESS will find 500 Earths and super-Earths transiting nearby stars, and the majority of small planets targeted by JWST will come from TESS. A robust ground-based program is essentially to confirm TESS planets and measure their densities. We need to have a credible path for targets if TESS fails or is delayed. Ground-based surveys + Spitzer provide a reasonable Plan B. CHEOPS has open time and provides a means to search for transits of RV-detected planets and improve SNR of TESS discoveries. GAIA is on schedule to provide parallaxes for TESS target list and any conceivable JWST exoplanet target. The interaction of a terrestrial planet atmosphere with an illuminating M- dwarf spectrum is a fundamental question for modelers. HST will gather UV spectra of M-dwarf planet hosts and vet mean molecular weight of candidate JWST targets. Conclusions GJ1132 is a good benchmark for JWST simulations. TESS will find 500 Earths and super-Earths transiting nearby stars, and the majority of small planets targeted by JWST will come from TESS. A robust ground-based program is essentially to confirm TESS planets and measure their densities. We need to have a credible path for targets if TESS fails or is delayed. Ground-based surveys + Spitzer provide a reasonable Plan B. CHEOPS has open time and provides a means to search for transits of RV-detected planets and improve SNR of TESS discoveries. GAIA is on schedule to provide parallaxes for TESS target list and any conceivable JWST exoplanet target. The interaction of a terrestrial planet atmosphere with an illuminating M- dwarf spectrum is a fundamental question for modelers. HST will gather UV spectra of M-dwarf planet hosts and vet mean molecular weight of candidate JWST targets. Conclusions GJ1132 is a good benchmark for JWST simulations. TESS will find 500 Earths and super-Earths transiting nearby stars, and the majority of small planets targeted by JWST will come from TESS. A robust ground-based program is essentially to confirm TESS planets and measure their densities. We need to have a credible path for targets if TESS fails or is delayed. Ground-based surveys + Spitzer provide a reasonable Plan B. CHEOPS has open time and provides a means to search for transits of RV-detected planets and improve SNR of TESS discoveries. GAIA is on schedule to provide parallaxes for TESS target list and any conceivable JWST exoplanet target. The interaction of a terrestrial planet atmosphere with an illuminating M- dwarf spectrum is a fundamental question for modelers. HST will gather UV spectra of M-dwarf planet hosts and vet mean molecular weight of candidate JWST targets.