CHARACTERIZING EXOPLANETS WITH HIGH DISPERSION CORONAGRAPHY ON TMT DIMITRI MAWET, CALTECH, NOVEMBER 2017 HDC TEAM @ 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
HIGH DISPERSION CORONAGRAPHY Wang et al. 2017, Mawet et al. 2017
HIGH RESOLUTION SPECTROSCOPIC CHARACTERIZATION OF EXOPLANETS Unambiguous identification of molecules such as CO, CH 4, CO 2, O 3, O 2
PROOF OF CONCEPT AT MEDIUM RESOLUTION WITH OSIRIS AND HR8799 Marois et al. 2008 (2010)
HR8799c Konopacky et al. 2013
HR8799b Barman et al. 2015
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
MEASURE PLANET SPIN a Relative position ( ) 1.0 0.5 0.0 0.5 Snellen et al. 2014 (CRIRES@VLT) Stellar velocity Star position Planet position b CC signal 1.0 60 40 20 0 20 40 100 50 0 50 Velocity (km s 1 ) Velocity (km s 1 ) Bryan et al. 2017 (NIRSPEC @ Keck)
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
DOPPLER MAPPING OF GIANT PLANETS Crossfield et al. 2014
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
ELTs GPI/SPHERE HDC CONTRAST GAINS N lines
ASTROBIOLOGIST S FLOWCHART TO CHAMPAGNE S. Domagal-Goldman (GSFC)
BIOSIGNATURES AT HIGH R Wang J., Mawet D., Hu R., Benneke B. 2017
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
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
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
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
PSI strawman concept PSI-Blue Vis WFS PSI-Red IR WFS Woofer DM Cold Coronagraph Coronagraph Tweeter DM 8-13 μm Imager 0.6-1.8 μm IFU/Imager 0.6-1.8 μm High-Res Cold Coronagraph 2-5 μm High-Res 2-5 μm IFU/Imager
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
HIGH DISPERSION CORONAGRAPHY DEMONSTRATOR IN THE CALTECH EXOPLANET TECHNOLOGY LAB Mawet et al. 2017
HIGH DISPERSION CORONAGRAPHY SCIENCE DEMONSTRATOR WITH KPIC Keck Planet Imager and Characterizer
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
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: KPIC @ Keck/NIRSPEC SCExAO @ Subaru/IRD HiRISE @ VLT/CRIRES PARVI @ Palomar
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