TESS and Galactic Science
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1 TESS and Galactic Science! Keivan Stassun!! WFIRST Meeting! 18 November 2014! 1!
2 Preliminary TESS Mission Schedule! Activity! Date! Status! Systems Requirement Review! Feb 2014! Completed! Preliminary Design Review! 8-11 Sep 2014! Completed! Mission Confirmation! 31 Oct 2014! Completed! Launch Vehicle Selection! mid-december 2015! Upcoming! Critical Design Review! May 2015! Upcoming! Systems Integration Review! 4 Oct 2016! Planned! Launch Readiness Review! 2 Aug 2017! Planned! Science Mission Complete! 8 Oct 2020! Planned! Discovering New Earths and Super-Earths in the Solar Neighborhood! 2!
3 Lens Hood Lens Assembly Detector Assembly Entrance pupil diameter! Bandpass! 10.5 cm! nm! Field of view! 24 x 24! Cadence for target stars! Cadence for full frame images! Nominal mag. Range! 2 min! 30 min! I = 4-16!
4 TESS Baseline Science Requirements! u BSR1: TESS shall perform a wide-field sky survey sensitive to transiting planets with orbital periods of less than 10 days. In this survey, TESS shall monitor >200,000 stars spread over the celestial sphere with a photometric sensitivity sufficient to permit detection of transiting planets with a radius 2.5 REarth.! u BSR2: TESS shall perform a concurrent [narrow field] sky survey sensitive to transiting planets with periods of 120 days or more. In this survey, TESS shall monitor >10,000 stars in regions centered on the ecliptic poles with a photometric sensitivity sufficient to permit detection of transiting planets with a radius 2.5 REarth.! u BSR3: The TESS team shall assure that masses of fifty (50) planets with radii less than 4 REarth are determined.! TESS KDP-C Review! 4!
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7 TESS KDP-C Review!
8 Simulated TESS detections! ecliptic coordinates! detectable planets around pre-selected target stars! Sullivan et al., in prep.! detectable planets around other stars in full-frame images!
9 Simulated TESS image (24 x 24 )!
10 2.8! 2.8!
11 Simulated TESS detections! 10 6! 10 5! 10 4! 10 3! 10 2! 10 1! Sullivan et al., in prep.!
12 Ricker et al. (2014)!
13 Opportunities for Galactic Science" days, ppm lightcurves for stars over all sky with I<12 and better than ~0.01 mag for 12<I<16" u Using 2-min cadence! u eclipsing binaries for fundamental parameters! u asteroseismology, mainly for red giants (TESS for nearby stars, WFIRST for distant stars compare stellar properties in different environments?)! u stellar granulation flicker accurate gravities (ages) for many many stars (extend this to IR for WFIRST?)! TESS KDP-C Review!
14 Prospects for p-mode detection!
15 Stellar gravities (ages) from granulation flicker! Stellar log g accurate to ~0.15 dex For dwarfs: ~30 ppm (visible light) For giants: ~500 ppm (visible light) Flicker detectable down to ~20% of shot noise as long as shot noise is well behaved and characterized! Granulation amplitudes probably much lower in the IR (Bastien et al., Nature, 2013)
16 Opportunities for Galactic Science" days, ppm lightcurves for stars over all sky with I<12 and better than ~0.01 mag for 12<I<16" u Using Full Frame Images:! u lightcurves of late type stars - weather and rotation of late M dwarfs and a few L/T dwarfs! u rotation for ~all stars in nearby open clusters! u Better lightcurves for all known variable stars in the sky than ever before, by a lot! u Kepler-level lightcurves for all known EBs except those found by OGLE, et al! TESS KDP-C Review!
17 Opportunities for Galactic Science" A WFIRST coronograph could be a great tool for studying TESSdetected systems. The TESS planets themselves would be too short-period for even a coronograph, but one could:" - look for long-period planets in the TESS systems! - look at the circumstellar environments for dust or debris disks! - eclipsing disks?!! TESS KDP-C Review!
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19 Overall TESS Science Status! " u Emerging Science Case for Full-Frame Images (FFI)! Resource for Broader Astronomical Community" Strongly Complements Large Synoptic Survey Telescope (LSST) " LSST: Stars fainter than 16th magnitude " TESS: Stars brighter than 16th magnitude! LSST! 2021! TESS KDP-C Review!
20 TESS Working Groups! Working group! Planet simulations! Target star selection! Follow-up observations! Asteroseismology! Serendipitous science! Atmospheric characterization! Habitability! Eclipsing binaries! Chairs! Josh Winn! Keivan Stassun, Josh Pepper! Dave Latham! Jørgen Christensen-Dalsgaard, Hans Kjeldsen! Peter McCullough, Garrett Jernigan! Jacob Bean! Lisa Kaltenegger! Bill Welsh, Nader Haghighipour!
21 Conference at MIT:! Science with TESS! 30 Sep 2 Oct 2015!! SOC Chair: Sara Seager! LOC Chair: Zach Berta! Heighten General Astronomical Interest in TESS "Especially for non-exoplanet community! 21!
22 TESS KDP-C Review!
23 TESS Science Objectives! u OBJECTIVE 1: Identify a diverse sample of transiting exoplanets with radii less than 2.5 REarth and orbital periods of up to 10 days orbiting the brightest stars in the solar neighborhood.! u OBJECTIVE 2: Identify a sample of transiting exoplanets with radii less than 2.5 REarth and orbital periods 120 days or more orbiting bright stars situated near the ecliptic poles, locations that are optimal for JWST followup.! u OBJECTIVE 3: Establish the masses of a sample of TESSlocated transiting planets with radii less than 4 REarth by means of analytical techniques* and/or precise radial velocity (PRV)** measurements.! ** PRV measurements require TESS-committed ground-based assets.! * Analytical techniques include asteroseismology, transit time variations,...! TESS KDP-C Review! 23!
24 TESS Level One Baseline Requirements! Objectives! Baseline Science Requirements! Baseline Technical Requirements! Baseline Data Requirements! Objective 1: Find planets with radius R<2.5RE and periods P<10 days! BSR 1: Monitor 200,000 stars over celestial sphere with sensitivity to find exoplanets with R=2.5RE and P 10 days! BTR 1: Two-year mission after two-month checkout! BDR 1: 95% of data collected delivered to the SOC! Objective 2: Find planets with R<2.5RE and P<120 days in JWST CVZ! BSR 2: Monitor 10,000 stars near ecliptic poles with sensitivity to find exoplanets with R=2.5RE and P 120 days! BTR 2: Collect data from each star for 20 days! BDR 2: Deliver processed data to MAST every 4 months! Objective 3: Measure the masses of a sample of exoplanets with R<4RE! BSR 3: Measure the masses of 50 planets with R<4RE! BTR 3: Instrument effective area Aeff 50 cm 2 in nm bandpass! BDR 3: Final delivery of processed data to MAST at end of Phase F! BTR 4: Systematic error floor of 60 ppm for I=8 in one hour! BDR 4: No proprietary period for data at archive! BTR 5: Temporal resolution 2 minutes! BTR 6: Data processing and ground follow-up sufficient to measure masses of 50 planets with R<4RE! TESS KDP-C Review! 24!
25 TESS Level One Threshold Requirements! Objectives! Threshold Science Requirements! Threshold Technical Requirements! Threshold Data Requirements! Objective 1: Find planets with radius R<2.5RE and periods P<10 days! TSR 1: Monitor 100,000 stars over celestial sphere with sensitivity to find exoplanets with R=2.5RE and P 10 days! TTR 1: Mission designed to execute survey of 100,000 stars! TDR 1: 95% of data collected delivered to the SOC! Objective 2: Find planets with R<2.5RE and P<120 days in JWST CVZ! TSR 2: Monitor 5,000 stars near ecliptic poles with sensitivity to find exoplanets with R=2.5RE and P 120 days! TTR 2: Collect data from each star for 20 days! TDR 2: Deliver processed data to MAST every 4 months! Objective 3: Measure the masses of a sample of exoplanets with R<4RE! TSR 3: Measure the masses of 35 planets with R<4RE! TTR 3: Instrument effective area Aeff 40 cm 2 in nm bandpass! TDR 3: Final delivery of processed data to MAST at end of Phase F! TTR 4: Systematic error floor of 80 ppm for I=8 in one hour! TDR 4: No proprietary period for data at archive! TTR 5: Temporal resolution 5 minutes! TTR 6: Data processing and ground follow-up sufficient to measure masses of 35 planets with R<4RE! TESS KDP-C Review! 25!
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