CHARACTERIZING EXOPLANETS WITH HIGH DISPERSION CORONAGRAPHY ON TMT

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1 CHARACTERIZING EXOPLANETS WITH HIGH DISPERSION CORONAGRAPHY ON TMT DIMITRI MAWET, CALTECH, NOVEMBER 2017 HDC CALTECH/JPL: J. WANG, J. JOVANOVIC, J-R DELORME, J. LLOP, N. KLIMOVICH, Y. XIN, W. XUAN, J. WALLACE, J. FUCIK, G. RUANE EXOPLANET ATMOSPHERES: B. BENNEKE (NOW AT U. MONTREAL), R. HU (JPL), S. DOMOGAL-GOLDMAN (GSFC), G. ARNEY (GSFC), J. FORTNEY KPIC HDC COLLABORATORS: M. FITZGERALD (UCLA), FROM WMKO: P. WIZINOWICH, S. CETRE, B. FEMENIA, S. LILLEY, E. WETHERELL, S. RAGLAND

2 HIGH DISPERSION CORONAGRAPHY Wang et al. 2017, Mawet et al. 2017

3 HIGH RESOLUTION SPECTROSCOPIC CHARACTERIZATION OF EXOPLANETS Unambiguous identification of molecules such as CO, CH 4, CO 2, O 3, O 2

4 PROOF OF CONCEPT AT MEDIUM RESOLUTION WITH OSIRIS AND HR8799 Marois et al (2010)

5 HR8799c Konopacky et al. 2013

6 HR8799b Barman et al. 2015

7 HIGH RESOLUTION SPECTROSCOPIC CHARACTERIZATION OF EXOPLANETS Unambiguous identification of molecules such as CO, CH 4, CO 2, O 3, O 2 Line broadening: => spin measurements => planet accretion history => final mass and atmospheric composition => formation of moons and rings

8 MEASURE PLANET SPIN a Relative position ( ) Snellen et al (CRIRES@VLT) Stellar velocity Star position Planet position b CC signal Velocity (km s 1 ) Velocity (km s 1 ) Bryan et al Keck)

9 HIGH RESOLUTION SPECTROSCOPIC CHARACTERIZATION OF EXOPLANETS Unambiguous identification of molecules such as CO, CH 4, CO 2, O 3, O 2 Line broadening: => spin measurements => planet accretion history => final mass and atmospheric composition => formation of moons and rings Time Domain Analysis of line profile: => Doppler imaging => Global circulation => Cloud coverage and weather

10 DOPPLER MAPPING OF GIANT PLANETS Crossfield et al. 2014

11 HIGH RESOLUTION SPECTROSCOPIC CHARACTERIZATION OF EXOPLANETS Unambiguous identification of molecules such as CO, CH 4, CO 2, O 3, O 2 Line broadening: => spin measurements => planet accretion history => final mass and atmospheric composition => formation of moons and rings Time Domain Analysis of line profile: => Doppler imaging => Global circulation => Cloud coverage and weather Contrast gains: => gains α N lines (# lines resolved) => Sidesteps chromatic speckle noise present and inevitable at low res

12 ELTs GPI/SPHERE HDC CONTRAST GAINS N lines

13 ASTROBIOLOGIST S FLOWCHART TO CHAMPAGNE S. Domagal-Goldman (GSFC)

14 BIOSIGNATURES AT HIGH R Wang J., Mawet D., Hu R., Benneke B. 2017

15 DETECTING BIO-SIGNATURE GASES WITH HDC ON TMT SNR contour map SNR contour map M dwarf planet at 5 pc CO2 Proxima Cen b O2 planet signal is ~10-8 Wang et al. 2017

16 DETECTING BIO-SIGNATURE GASES WITH HDC AT TMT SNR contour map SNR contour map M dwarf planet at 5 pc CO2 Proxima Cen b O2 planet signal is ~10-8 Wang et al. 2017

17 DETECTING BIO-SIGNATURE GASES WITH HDC AT TMT SNR contour map SNR contour map M dwarf planet at 5 pc CO2 Proxima Cen b O2 planet signal is ~10-8 Wang et al. 2017

18 BOTTOM LINE HDC might be the only way to tease out biomarkers from Earth-like and super-earth exoplanets HDC enables detailed characterization from optical to infrared: composition, spin, cloud mapping Strong synergies with transit spectroscopy and RV: fiber-fed diffraction limited high-resolution spectrographs

19 PSI strawman concept PSI-Blue Vis WFS PSI-Red IR WFS Woofer DM Cold Coronagraph Coronagraph Tweeter DM 8-13 μm Imager μm IFU/Imager μm High-Res Cold Coronagraph 2-5 μm High-Res 2-5 μm IFU/Imager

20 HRS CONCEPTUAL DESIGN (MODIUS) 9-channel Multiplexing using H4RG, 25-channel possible (reduced bw) Echelle Gra*ng Fiber Ap. Stop Coll OAP CX Prism Camera M2 H4RG Detector Camera M1 RV ready J. Fucik (COO) Camera M3

21 HIGH DISPERSION CORONAGRAPHY DEMONSTRATOR IN THE CALTECH EXOPLANET TECHNOLOGY LAB Mawet et al. 2017

22 HIGH DISPERSION CORONAGRAPHY SCIENCE DEMONSTRATOR WITH KPIC Keck Planet Imager and Characterizer

23 KPIC HDC MODULE 2nd relay Tip-Tilt mirror Fiber port 1 Fiber port 2 FIU dichroic #2 MEMS DM FIU dichroic #1 Tracking camera AO focus 1st relay Up

24 PERSPECTIVES Theoretical studies/numerical simulations: Refine HDC simulators (exo-zodis, telescope/system emissivity, speckle chromaticity) Refine theoretical models of exoplanet atmospheres Better spectroscopic templates Capture diversity of planets Archean Earth modeling HDC science demonstrators: Keck/NIRSPEC Subaru/IRD VLT/CRIRES Palomar

25 COLLABORATORS Caltech: J. Wang, N. Jovanovic, G. Ruane, J.-R. Delorme, R. Dekany, J. Fucik, N. Klimovich, J. Llop, R. Riddle, K. Matthews JPL: J.K. Wallace, E. Serabyn, G. Vasisht, R. Bartos, M. Bottom, AJ Riggs W.M. Keck Observatory: P. Wizinowich, S. Cetre, B. Femenia, S. Lilley, E. Wetherell, S. Ragland University of Hawaii: M. Chun, C. Bond, C. Baranec, D. Hall, D. Atkinson, S. Goebel, C. Lockhart, E. Warmbier University of Liege: O. Absil, E. Huby*, B. Carlomagno, C. Gomez, A. Jolivet, J. Surdej, S. Habraken, C. Delacroix** Uppsala University: E. Vargas, P. Forsberg, M. Karlsson UCLA: M. Fitzgerald Subaru: O. Guyon LAM: T. Fusco Arcetri: S. Esposito, C. Plantet ANU: F. Rigault (*) ULg -> ObsPM (**) ULg -> Cornel