Directly Imaging Extrasolar Planets with the Subaru Coronagraphic

Directly Imaging Extrasolar Planets with the Subaru Coronagraphic Extreme Adaptive Optics Project Thayne Currie (NASA-Ames/Subaru, currie@naoj. org) Olivier Guyon; N. Jeremy Kasdin; Timothy Brandt; Tyler Groff; Julien Lozi; Jeff Chilcote; Taichi Uyama; Eric Nielsen; Sarah Blunt; Christian Marois; Nemanja Jovanovic; Masayuki Kuzuhara; Motohide Tamura + many others

SCEx. AO: A New Advance in Exoplanet Imaging HR 8799 b c b d 1. Keck/NIRC 1997 (no AO) 2. Subaru/CIAO 2002 (SR ~ 0. 2? ) 3. Keck/NIRC 2 2005 -2008 (SR ~ 0. 3 -0. 5) c e d 4. Gemini/GPI 2013 (SR ~ 0. 8? ) c e d 5. Subaru/SCEx. AO 2017 (SR ~ 0. 9) ((1. data from KOA; PI. E. Becklin; 2. Fukagawa et al. 2009; 3. Currie et al. 2012; 4. Ingraham et al. 2014; 5. Currie et al. 2019 unpublished)

SCEx. AO/CHARIS Direct Spectroscopy of kappa And b

kappa And b: A Superjovian Planet or Brown Dwarf? Old Brown Dwarf Porter CHARA interferometry of star P 1640 YJH direct spectroscopy of kappa And b • • Inconclusive spectrum? But … Star’s age= old, kap And b = brown dwarf • • Resolved image of star could be young Kap And b could be lower mass Need new kappa And b spectra to clarify properties… (Hinkley et al. 2013; Jones et al. 2016)

SCEx. AO Observations of kappa And SCEx. AO/CHARIS Strehl Ratio ~0. 9 -0. 92; SNR ~ 210 • • Sharply-peaked H band spectrum suggestive of low gravity (and low mass) Eccentric, wide-separation orbit (> 75 au); may be aligned with the rotation axis of the star (Currie et al. 2018, AJ, 156, 291)

kappa And b: A Likely Low-Gravity Superjovian Planet Old/massive t mass • Most consistent with objects at/below planet-mass limit Young/plane t mass Young/plane Old/massive (Currie et al. 2018, AJ, 156, 291)

HIP 79124 HIP 79977 HD 163296/E. Rich, Wednesday talk 320. 02 D B. Gerard/iposter 164. 01 (Asensio-Torres, Currie, & Janson et al. 2019 in press; Goebel, Currie, & Guyon et al. 2018; Rich, Wisniewski, Currie et al. 2019; Gerard, Marois, Currie et al. 2019)

A Direct Imaging + Radial-Velocity Survey for Exoplanet Discovery SCEx. AO/CHARIS+MEC Direct Imaging (observe in good seeing) IRD/precision RV (observe in below average seeing)

Forming kappa And b Planet formation by Core Accretion (side view) By Disk instability (top view) Up to ~10 -75 AU (Kenyon & Bromley 2009; Lambrechts et al. 2012) Favored model forming Jupiter-like planets. Probably cannot form kappa And b. More than 75 AU (Boley 2009; Rafikov 2005) Can form kappa And b? Simulation from Rice et al.

The Orbit of Kappa And b Old/massive • • • Eccentric likely large semimajor axis (a > 75 au) Possibly aligned with rotation axis of star (Currie et al. 2018)