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Thayne Currie, Olivier Guyon, Nemanja Jovanovic,
Julien Lozi, Eugenio Garcia, Taichi Uyama
Imaging and Characterizing Exoplanets (and Disks) with SCExAO:
First Results and Future Prospects
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Directly-‐Imaged Planets
(Marois et al. 2008, 2010; Kalas et al. 2008; Lagrange et al. 2010; Kraus & Ireland 2012; Sallum et al. 2015; Carson et al. 2013; Rameau et al. 2013; Kuzuhara et al. 2013; Currie et al. 2014; Quanz et al. 2013; Currie et al. 2015; Macintosh et al. 2015)
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SCExAO Project: An Extreme AO System on Maunakea
• Extreme AO Imager for Subaru
• S.R. ~ 90+% at H band (by July 2016)
• 1200 modes, 3.5 kHz, 1 ms latency
• AddiQonal Strengths: excepQonal site; small IWA (1-‐3 lambda/D) capability
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Extreme AO vs. Site CondiQons GPIES Contrasts, ASDI, Processed with KLIP (R. DeRosa, J. Wang) Planet DetecQon SensiQve to Atmospheric CondiQons?
(from TMT site tesQng results)
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Extreme AO close to 1 lambda/D
T. Currie 2016, in prep
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SCExAO: Current PSF Quality & Contrast
S.R. ~ 0.7 (0.9 in short exp)
H band/1.6 microns
Emerging Dark Hole (r ~0.45—0.8”)
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SCExAO: First Science Results HD 1160 B:
Young, Low-‐Mass Substellar Companion
Garcia, Currie, & Guyon et al. (2016)
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Garcia, Currie, & Guyon et al. (2016)
HD 1160 B SED Modeling
HD 1160 B SED Modeling • Teff = 3000-‐3100 K, log(g) = 4—4.5, M ~ 30-‐90 Mj • Solar Metallicity
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SCExAO: First Science Results, part 2 The directly-‐imaged planet kappa Andromedae b
SNR ~ 105; IWA ~ 0.37”
(Currie, Guyon, et al. in prog.)
Kappa And b SED Modeling • Teff = 1675—1950 K, log(g) = 3.8—4.25 favored • More consistent with planet interpretaQon, not massive brown dwarf
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SCExAO SNRE ~ 5-‐7 to 0.3”
SEEDS/HiCIAO SNRE ~2-‐5 to 0.5”
SCExAO: First Science Results, part 3 The HIP 79977 Debris Disk
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Future Prospects: Exoplanet/Disk Characterization with SCExAO+CHARIS
JHK integral field spectrograph (delivered to Subaru in April 2016) • Low-‐resoluQon ‘discovery’ mode (R ~15-‐20), full JHK bandpass • High-‐resoluQon ‘characterizaQon’ mode (R ~ 70-‐90); invesQgate
exoplanet clouds (e.g. Currie et al. 2011) or disk composiQon (e.g. Rodigas et al. 2015)
R80
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New Exoplanet Survey (SEEDS v. 2.0?) Direct Imaging + Radial Velocity
SCExAO+CHARIS Direct Imaging (good seeing)
IRD Radial-‐Velocity (below average seeing)
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Speckle Nulling DemonstraQon w/ SCExAO (Goal: 1 kHz acQve speckle control)
-‐ -‐ speckle nulling: -‐ A replacement/complement
to ADI/SDI at small lambda/D
Martinache et al. (2014); Mazin et al. (2013)
Future Prospects: “Next-Generation Extreme AO” Capabilities
-‐ fast, focal plane wavefront sensing MKIDS detector (MEC)
à 1e-‐7 to 1e-‐8 contrasts at several lambda/D
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Future Prospects: Imaging Reflected-‐Light Planets with SCExAO+MEC (early 2020s)
1 Mj at 1 AU around Vega
20 Mj Brown Dwarf/Super Jupiter at 1 AU around Vega
Discovery Space for SCExAO/MEC
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Summary • SCExAO: Subaru’s Extreme-‐AO System:
Key Strengths: best site, small lambda/D sensiQvity
• Performance: closing gap with leading extreme AO systems
• First Science: Characterizing the atmospheres to HD 1160 B and kappa And b; characterizing debris disk around HIP 79977
• Future Prospects: Direct imaging/spectroscopy survey; next-‐gen extreme AO; imaging planets in reflected light