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Searching for Planets orbiting M Dwarfs with the TripleSpec Exoplanet Discovery Instrument (TEDI)

Searching for Planets orbiting M Dwarfs with the TripleSpec Exoplanet Discovery Instrument (TEDI). Philip Muirhead (me, Cornell) James Lloyd (my Advisor, Cornell) Jerry Edelstein (Berkeley) David Erskine (LLNL) Jason Wright (Penn State) Matthew Muterspaugh (Tenn State)

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Searching for Planets orbiting M Dwarfs with the TripleSpec Exoplanet Discovery Instrument (TEDI)

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  1. Searching for Planets orbiting M Dwarfs with theTripleSpec Exoplanet Discovery Instrument (TEDI) Philip Muirhead (me, Cornell) James Lloyd (my Advisor, Cornell) Jerry Edelstein (Berkeley) David Erskine (LLNL) Jason Wright (Penn State) Matthew Muterspaugh (Tenn State) Berkeley Undergraduates: Tony Mercer, Aga Czeszumska, Sam Halverson, Danny Mondo

  2. Vega Sun M Dwarfs 1000x fainter than Sun-like stars in the visible M Dwarfs dominate the Galaxy by number

  3. Exoplanet Host Stars Discovered by Doppler Method Gl 581 Gl 317 HD 41004B V < 12

  4. Exoplanet Host Stars Discovered by Doppler Method Gl 581 Gl 317 HD 41004B K < 12 V < 12

  5. Exoplanet Host Stars Discovered by Doppler Method Gl 581 Gl 317 HD 41004B K < 12 V < 12 Dwarfs culled using Proper Motion Lepine & Shara 2005 Nutzman & Charbonneau 2007

  6. Exoplanet Host Stars Discovered by Doppler Method Gl 581 Gl 317 HD 41004B K < 12 V < 12 Infrared Doppler Survey Science Targets Dwarfs culled using Proper Motion Lepine & Shara 2005 Nutzman & Charbonneau 2007

  7. Precise Doppler Methods in Optical Multi-mode Hi Res (moving parts OK) Single-mode Hi Res (moving parts not OK) Graphic from Eggenberger & Udry 2009

  8. Precise Doppler Methods in Near-IR? Multi-mode Hi Res (moving parts OK) Single-mode Hi Res (moving parts not OK) Graphic from Eggenberger & Udry 2009

  9. Precise Doppler Methods in Near-IR? Multi-mode Hi Res (moving parts OK) Single-mode Hi Res (moving parts not OK) Graphic from Eggenberger & Udry 2009

  10. Precise Doppler Methods in Near-IR? Multi-mode Hi Res (moving parts OK) $$$$ Single-mode Hi Res (moving parts not OK) Graphic from Eggenberger & Udry 2009

  11. Our Method: TEDI Single-Mode, NIR Moderate-res Spectrograph Michelson-Morley Interferometer with adjustable opticalDELAY Interferometer fully adjustable (NOT monolithic) Erskine 2003, Ge 2006 Mirrors Beam Splitter Etalon (Glass)

  12. Our Method: TEDI Single-Mode, NIR Moderate-res Spectrograph Michelson-Morley Interferometer with imposedopticalDELAY Interferometer fully adjustable (NOT monolithic) Erskine 2003, Ge 2006 Mirrors Beam Splitter Etalon (Glass)

  13. Our Method: TEDI Single-Mode, NIR Moderate-res Spectrograph Michelson-Morley Interferometer with imposedopticalDELAY Interferometer fully adjustable (NOT monolithic) Erskine 2003, Ge 2006 Mirrors Beam Splitter Etalon (Glass)

  14. One TripleSpec Pixel

  15. 1 km/s Doppler Shift

  16. Advantages of the Method • The Doppler signal is shifted from a pixel-to-pixel flux change to a flux change within a pixel • Highly insensitive to pixel-to-pixel calibration • Extremely sensitive to delay calibration • Delay is simultaneously calibrated with overlapped ThAr lamp emission lines. • Moderate Resolution Spectrograph allows for broad simultaneous wavelength coverage • 0.9 to 2.5 microns, JHK

  17. GJ 411 M2V, K=3.3, vsini < 1km/s, δRV < 5m/s

  18. Modeled and Removed ThAr Line Examine Line Core GJ 411 M2V, K=3.3, vsini < 1km/s, δRV < 5m/s

  19. GJ 411 M2V, K=3.3, vsini < 1km/s, δRV < 5m/s

  20. σφ = 10° = 300 m/s in ONE PIXEL With 1000s of pixels that’s σ<φ>= 10 m/s GJ 411 M2V, K=3.3, vsini < 1km/s, δRV < 5m/s

  21. Challenges • Wavelength Dependent Systematics • Telluric Contamination (calibration promising) • Wavelength dependent delay, related to focus changes (calibration also promising) • Throughput Below Spec • 10m/s in 6 min on K=3.3, the same as • 30m/s in 1 hour on K=8.3 (science targets) • Factor of 10 in throughput loss yet unaccounted for

  22. Summary • TEDI designed to detect planets orbiting M dwarfs with the Doppler technique in NIR. • Potential for detecting habitable worlds. • Uses an interferometer and moderate-res spectrograph for precise radial velocimetry. • Currently achieving ~10 m/s of photon-limited precision on bright M dwarf. • However, currently limited by systematic effects, but calibration is promising.

  23. 5ME Planet with RV > 3m/s on host star Gl 581c Gl 581d Kasting & Catling 2003

  24. TSPEC Hawaii 2K, HgCaTe

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