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Exoplanet Science in the 2020S NOAO 2020 Decadal Survey Community Planning Workshop

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Exoplanet Science in the 2020S NOAO 2020 Decadal Survey Community Planning Workshop 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 Lens Hood 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) Thompson - 1° TESS Slide from Zach Berta-Thompson Berta Zach by images simulated TESS Slide from one CCD: Zach Berta 12° - Thompson simulated images by Zach Berta-Thompson 24° one TESS camera FOV from : simulated images by Zach Berta-Thompson 24° one TESS camera FOV from : 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 J Keck (Scale 0.01”/px) 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 50 Planets smaller than 4 RE Requirement with measured masses CHEOPS (CHaracterising ExOPlanet Satellite) • ESA S-class (small) mission; 2019 launch? • PI: Willy Benz (University of Bern) • 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 deg2 • Pupil diameter: 12 cm • Science Mission: 4 years (6.5 year goal) http://sci.esa.int/plato/ WFIRST (Wide Field InfraRed Survey Telescope) • Mid-2020s launch • Microlensing survey • Coronagraph testbed • Aperture: 2.4 m • Mission: 6 years 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 near- infrared 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) Exoplanet Science Opportunity #11: Atmospheric Dynamics • Heat redistribution • Planet rotation Brogi et al. (2016) Stevenson et al. (2014) Exoplanet Science Opportunity #12: Host Star Abundances • What are the connections between stellar compositions and planetary properties? Host Star Host C/O Star Host C/O Planet Temperature (K) Planet Radius (Jupiter Radii) Teske et al. (2014) 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 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 Credit: T. Abbott and NOAO/AURA/NSF.
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