Exoplanet Science in the 2020s NOAO 2020 Decadal Survey Community Planning Workshop Courtney Dressing Assistant Professor of Astronomy at University of California, Berkeley February 20, 2018
Origins Space Telescope
Space-based assets in the 2020s
TESS (Transiting Exoplanet Survey Satellite) Scheduled for spring launch (NLT June 2018) PI: George Ricker (MIT) Goal: detect planets transiting nearby stars Search >200,000 nearby stars Estimate masses of 50 small planets Telescope 4 wide-field cameras (24 x24 ) 10.5 cm aperture Photometric Survey 2-minute cadence At least 27 days per star https://tess.gsfc.nasa.gov/
TESS will Detect Planets Orbiting Brighter Stars
Lens Hood Lens Assembly Detector Assembly 10.5 cm diameter, 24 x24 field of view TESS Slide from Zach Berta-Thompson Ricker et al. (2014), Sullivan et al. (2015)
TESS Slide from Zach Berta-Thompson 1 simulated images by Zach Berta-Thompson
one CCD: 12 TESS Slide from Zach Berta-Thompson simulated images by Zach Berta-Thompson
FOV from one TESS camera: 24 simulated images by Zach Berta-Thompson
FOV from one TESS camera: 24 constellations by H. A. Rey Slide by Zach Berta-Thompson
TESS Slides from Zach Berta-Thompson Slide from Zach Berta-Thompson Ricker et al. (2014), Sullivan et al. (2015)
Slide from Zach Berta-Thompson ecliptic pole Ricker et al. (2014), Sullivan et al. (2015)
TESS Data will Include 2-min Postage Stamps and 30-min Full-Frame Images https://heasarc.gsfc.nasa.gov/docs/tess/operations.html
TESS will Find Hundreds of Planets Sullivan et al. 2015, 2017
Not All Candidate Signals will be Planets Image Credit: NASA
TESS Pixels are Large (20 x20 ) 2MASS (Scale 1 /px) UKIRT (Scale 0.2 /px) J Keck (Scale 0.01 /px) J Keck (Scale 0.01 /px) J Ks Furlan et al. 2017, AJ, 153, 71
Follow-up Observations Will Be Essential to Identify False Positives https://tess.mit.edu/followup/
Follow-up Observations Will Be Essential to Identify False Positives Light Curves for 200,000 Stars Transit-like Signals (3000 signals) Imaging (2500 survive) Reconnaissance Spectroscopy (1700 survive) Selected RV Targets (100) NASA Level 1 Science Requirement 50 Planets smaller than 4 RE with measured masses
ESA S-class (small) mission; 2019 launch? PI: Willy Benz (University of Bern) CHEOPS (CHaracterising ExOPlanet Satellite) Goal: obtain ultra-precise photometry of planet host stars Measure radii to within 10% accuracy Determine bulk densities of small planets Identify best targets for future study Targets: bright (V 12) planet host stars Telescope aperture: 32 cm Photometer: 0.4 1.1 µm Science Mission: 3.5 years (5 year goal) Community Time: 20% http://sci.esa.int/cheops/ and http://cheops.unibe.ch/
JWST (James Webb Space Telescope) Spring 2019 launch Multiple instruments Exoplanet atmospheres Aperture: 6.5 m Mission: 5-10 years Credit: Penny https://www.jwst.nasa.gov/
FINESSE (Fast Infrared Exoplanet Spectroscopy Survey Explorer) Proposed for 2023 launch PI: Mark Swain, Science Lead: Jacob Bean Goal: spectroscopic characterization of 500+ planets Metallicity C/O ratios Energy budgets Heat redistribution Aerosols 75 cm telescope 0.5 5 µm, R = 80-300 https://www.jpl.nasa.gov/missions/fast-infrared-exoplanet-spectroscopy-survey-explorer-finesse/
PLATO (PLAnetary Transits and Oscillations of stars) ESA M-class (medium) mission selected for 2026 launch PI: Heike Rauer (DLR) Goal: detect terrestrial planets orbiting bright stars (V=11-13) Asteroseismology Planet radii to 3% Planet masses to 10% Cameras 24 normal (25 s cadence, V>8) 2 fast (2.5 s cadence, V=4-8) FOV: 1100 deg 2 Pupil diameter: 12 cm Science Mission: 4 years (6.5 year goal) http://sci.esa.int/plato/
Mid-2020s launch Microlensing survey Coronagraph testbed Aperture: 2.4 m Mission: 6 years WFIRST (Wide Field InfraRed Survey Telescope) Credit: Penny https://wfirst.gsfc.nasa.gov/
Ground-based Extremely Large Telescopes
Giant Magellan Telescope Commissioning in 2023 24.5-m diameter First-light instruments G-CLEF: visible echelle spectrograph GMACS: Visible Multi-Object Spectrograph Future instruments GMTIFS: Near-IR IFU & Adaptive Optics Imager GMTNIRS: IR Echelle Spectrograph MANIFEST: Facility Fiber Optics Positioner ComCam: Commissioning Camera Credit: GMT, rendering by Mason Media
European Extremely Large Telescope Operations beginning in 2024 39-m diameter First-light instruments MICADO (ELT-CAM): diffraction-limited NIR imager HARMONI (ELT-IFU: single-field nearinfrared wide-band integral field spectrograph MAORY (MCAO): multi-conjugate adaptive optics system Future instruments METIS (ELT-MIDIR): Mid-IR imager & spectrometer ELT-HIRES: high-resolution spectrometer ELT-MOS: multi-object spectrometer Credit:ESO/L. Calçada
Thirty Meter Telescope First Light 2026 30-m Diameter First-light Instruments WFOS: Wide-field Optical Spectrometer IRIS: Infrared Imaging Spectrograph IRMS: Infrared Multi-object Spectrometer NFIRAOS: Narrow Field InfraRed Adaptive Optics System Future Instruments White paper deadline March 21, 2018
Exoplanet Science Opportunity #1: Candidate Validation TESS pixels are ENORMOUS False positive identification is crucial NEID time is valuable. We should use it wisely. Nature ISSN 1476-4687 Ciardi et al. 2015, ApJ, 805, 16
Exoplanet Science Opportunity #2: Stellar Characterization Determine the properties of planet host stars Characterize the full target sample Dressing et al. 2017, ApJ, 836, 167
Exoplanet Science Opportunity #3: Transit Recovery Most TESS targets will be observed for only 27 days Ricker et al. (2014), Sullivan et al. (2015) Ballard et al. (2018)
Exoplanet Science Opportunity #4: Detect Smaller & Harder Planets Bowler et al. (2016)
Exoplanet Science Opportunity #5: Planet Occurrence Multiplicity (stellar & planetary) Mass Metallicity Maturity (age) Mulders et al. (2015) Muirhead et al. (2015)
Exoplanet Science Opportunity #6: Compositional Diversity Design goal < 30 cm/s 380 to 930 nm, R = 100,000
Exoplanet Science Opportunity #7: Eccentricity Determination Necessary for secondary eclipse observations! Holds clues about formation Winn & Fabrycky (2015)
Exoplanet Science Opportunity #8: Detection of Additional Planets Kepler-454 Keck HARPS-N Gettel et al. 2015
Exoplanet Science Opportunity #9: System Architectures Determine inclinations Rossiter-McLaughlin effect RV detections of non-transiting planets Astrometry Measure eccentricities Look for trends in composition with planet position Probe systems at a range of orbital separations by combining multiple search methods Winn & Fabrycky (2015)
Exoplanet Science Opportunity #10: Atmospheric Composition Greene et al. (2016)
Brogi et al. (2016) Stevenson et al. (2014) Exoplanet Science Opportunity #11: Atmospheric Dynamics Heat redistribution Planet rotation
Exoplanet Science Opportunity #12: Host Star Abundances What are the connections between stellar compositions and planetary properties? Host Star C/O Host Star C/O Planet Temperature (K) Teske et al. (2014) Planet Radius (Jupiter Radii)
Exoplanet Science Opportunity #13: Surprises & Unusual Objects Boyajian et al. (2016) Credits: NASA/JPL-Caltech
Flexible Scheduling Distinguishing between stellar activity and planet signal Detecting multiple planets Determining orbital eccentricity
Coordination Thousands of planets to consider Avoid wasting resources on unnecessary duplication of effort while still cross-checking results Combine strengths of multiple facilities
Credit: T. Abbott and NOAO/AURA/NSF Summary New breakthroughs in exoplanet science are on the horizon Ground-based observations are essential to maximize the scientific return from space-based missions Smaller facilities play a key role in vetting candidates and characterizing stellar populations