sign in sign up
<<
Home , Origins Space Telescope

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-based assets in the 2020s TESS (Transiting Exoplanet Survey Satellite)

• Scheduled for spring launch (NLT June 2018) • PI: George Ricker (MIT) • Goal: detect 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 from Slide TESS one CCD:

Zach Berta Zach 12° - Thompson

simulated images by Zach Berta-Thompson 24° fromFOV camera TESS one :

simulated images by Zach Berta-Thompson 24° fromFOV camera TESS one : 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 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 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 • 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 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 • • 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