Direct Imaging Direct imaging of exoplanets:
Where are Remote sensing of planetary we going? systems and processes Where are we now?
Why is it hard? Katie Morzinski
What’s NASA Sagan Fellow, University of Arizona next?
K. Morzinski Exoplanets & Brown Dwarfs: Mind the Gap 2 Sep. 2013
magao.as.arizona.edu High-contrast imaging with adaptive optics: Removing scattered starlight
Direct Imaging
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K. Morzinski
magao.as.arizona.edu Direct imaging of planets…
Direct Imaging
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magao.as.arizona.edu Voyager 1, NASA, 1990 …has gone beyond our solar system
Direct Imaging
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magao.as.arizona.edu Direct imaging presents our best opportunity to thoroughly characterize exoplanets
Direct Imaging
HR 8799 bcde -- Marois+ 2008, 2010 Where are we going? Fomalhaut b – Kalas+ 2008 Where are we now? 2M 1207 b – Chauvin+ 2004 M Why is it hard?
Beta Pic b – Lagrange+ 2009 What’s next?
K. Morzinski
GJ 504 b – Kuzuhara+ 2013 1RXS 1609 b Kappa And b – Carson+ 2013 Lafreniere+ 2010 HD 95086 b – Rameau+2013 K B A G magao.as.arizona.edu Directly imaged low-mass objects
Directly imaged planets CD-35 2722 b 3.0 2M 0746+202M 2206-20 b b
Direct 1.75 HIP 78530 b Imaging GQ Lup b Oph 11 b 2.0 2M 2140+16 b 1.5 GSC 06214-00210 b UScoCTIOHN Peg b 108 b FU Tau b Where are 1RXS1609 b 1.25 Star Mass[MSol] 2Mkappa 0122-24392M And 0103(AB) b b b we going? CHXR 73 b DH Tau b 1e01 HR 8799HR 8799d c 1 HR 8799 e Where are 9.0 Ross 458(AB) c 8.0 WD 080 we now? Planet Mass [MJup] 2M 044144 b 0.75 7.0 beta Pic b HR 8799 b CFBDS 1458 b 6.0 LKCA 15 b Why is 0.5 it hard? 5.0 HD 95086 b 0.25 4.0 GJ2M1207 504 b b What’s next? 5.0 1e01 5.0 1e02 5.0 1e03 5.0 Semimajor axis [AU] K. Morzinski
magao.as.arizona.edu Jupiter’s SED: reflectivity, deep atmospheric windows, and thermal blackbody emission wavelength / microns Direct 20 10 5 3 2 1.5 1.2 1.0 Imaging
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K. Morzinski Energy balance indicates internal heat source
Gehrels, ed. 1976 Jupiter: studies of the interior, atmosphere, magnetosphere, and satellites magao.as.arizona.edu Where we’d like to be with exoplanets
Direct Imaging
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magao.as.arizona.edu L.N. Fletcher et al. / Icarus 200 (2009) 154–175 Where we’d like to be with exoplanets
Energy balance Direct Energy transport Imaging Winds, storms Composition, clouds Where are we going? Energetic processes
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Zhang 2013 K. Morzinski
magao.as.arizona.edu The New Solar System – Ingersoll Ammonia clouds on Jupiter & Saturn vs. strong methane absorption on Uranus & Neptune
Direct Imaging
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The New Solar System – Ingersoll 1999
magao.as.arizona.edu Four co-eval gas giant planets in the same system
Direct Imaging
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de Pater Planetary Sciences magao.as.arizona.edu Four co-eval gas giant planets in the same system
Direct Imaging
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Oppenheimer et al 2013 magao.as.arizona.edu Equilibrium chemistry models underpredict the HR 8799 planets’ 3.3um fluxes
Direct Imaging
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Skemer et al 2012 magao.as.arizona.edu HR 8799 b fit with inverse model
Direct HR 8799 b Imaging
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Cloud-free with high mean molecular weight OK, or intermediate clouds. K. Morzinski CF = Cloud Free Heavy element enhanced, high C:O. UC = Uniformly Cloudy Radius too small in model. IN = Intermediate Lee et al 2013 magao.as.arizona.edu Clues about formation – Enrichment of C:O ratio in HR 8799 c
Direct Imaging
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Konopacky et al 2013 magao.as.arizona.edu The effect of clouds and non-equilibrium chemistry – 2MASS 1207 b
Direct Imaging
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Barman et al 2011 magao.as.arizona.edu Comparing HR 8799 b, c, and 2M 1207 b
Direct Imaging
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Konopacky et al 2013 magao.as.arizona.edu Searching for planetary systems like our own
Direct Imaging
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K. Morzinski Marois et al 2010
magao.as.arizona.edu Are dust zones signposts of multiple planets in debris disks?
Direct Imaging
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Su et al 2013 magao.as.arizona.edu Fomalhaut b is not the object sculpting the disk
(if any; Direct see Lyra Imaging et al 2013)
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Kalas et al 2012 magao.as.arizona.edu Beta Pictoris – One of the first stars known to host an analagous system to ours –> Comets
Direct Imaging
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Smith & Terrile 1984 magao.as.arizona.edu The existence of a planet around Beta Pictoris was long suspected, due to the inner disk warp
Direct Imaging
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Where are Lagrange et al 2009 we now?
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magao.as.arizona.edu Magellan adaptive optics imaging of Beta Pic b [3.3]μm PSF Direct Imaging
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Where are we now? Modeled PSF
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K. Morzinski [3.3]μm [3.1]μm
Morzinski et al 2013 in prep magao.as.arizona.edu Cloudy atmosphere, Teff 1700±100 K
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Bonnefoy et al 2013 magao.as.arizona.edu Are wide low-mass (<30 MJup) companions to B and A-type stars over-represented? All confirmed Frequency Direct planets (NASA of Stars Imaging exoplanet archive)
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Where are 2M1207 we now? 2M2140+16 2M2206-20 Why is 2M0122-2439 it hard? GQ Lup 2M044144 LkCa 15 Ross 458 FU Tau What’s AB Pic SR 12 DH Tau next? GSC 06214-00210 Kappa And HR 8799 1RXS 1609 Oph 11 HD 100546 Fomalhaut USco 1610-1913 GJ 504 USco CTIO 108 Hip 77900 Beta Pic USco 1602-2401 HN Peg USco 1602-1800
K. Morzinski CFBDS 1R2149
CT Cha WD 0806-661 2M 0746+20
Hip 78530 HD 95086 Sigma Ori objects
HD 203030 CFBDS 1458 CHXR 73 O B A F G K M L T WD
magao.as.arizona.edu No systems imaged with low mass ratio <50 AU
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Perryman 2011 Exoplanet handbook magao.as.arizona.edu NICI results for companion search around B and A stars find that HR 8799 is a rare system
<20% of B & A Direct stars have Imaging planets >4 MJup beyond Where are 60 AU. we going?
Where are <10% of B & A we now? stars have planets >10 Why is MJup beyond it hard? 40 AU. What’s next?
K. Morzinski
Nielsen et al 2013 magao.as.arizona.edu IDPS results for companion search around A stars find similar results
<20% of A Direct stars have Imaging planets >3 MJup Where are beyond 5 we going? AU.
Where are we now? <10% of A stars have Why is BDs >15 it hard? MJup What’s beyond 5 next? AU.
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Vigan et al 2012 magao.as.arizona.edu Disk mass as a function of stellar mass
Direct Imaging
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magao.as.arizona.edu Survey results – Stars with debris disks
Direct Imaging <13% of 57 stars with debris Where are disks have we going? planets >5 MJup Where are beyond 80 AU we now?
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Wahhaj et al 2013 magao.as.arizona.edu There is a lot of parameter space yet to be observed
Direct Imaging
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magao.as.arizona.edu Oppenheimer & Hinkley 2009 ARA&A L-band contrast curves vs search space
Direct Imaging
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Hinkley 2011 magao.as.arizona.edu H-band contrast vs. guide star magnitude, GPI
Direct Imaging
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McBride et al 2011 magao.as.arizona.edu Dark Hole
Direct Imaging Inner working distance ~3-5 λ/D Where are we going?
Where are Outer working we now? distance ~λ/2d
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What’s next? Fitting error
K. Morzinski
WFS measurement
magao.as.arizona.edu Slide courtesy Bruce A. Macintosh Speckle noise sets a fundamental limit to sensitivity
Direct Imaging
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What’s next? Keck pupil image by Bruce A. Macintosh Typical Keck H-band PSF, circa 2009
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magao.as.arizona.edu MagAO & LBTAO are 2nd-gen. adaptive optics
• Pyramid • Control Direct – Better low-spatial-frequency # #" Imaging performance – Fainter guide stars
• Adaptive Secondary Mirror $%& Where are we going? – Thermal throughput Where are we now?
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Fernando Quiros-Pacheco, Arcetri magao.as.arizona.edu Magellan adaptive optics imaging of Beta Pic b [3.3]μm PSF Direct Imaging
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Where are we now? Modeled PSF
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Morzinski et al 2013 in prep magao.as.arizona.edu Diffraction suppression with a coronagraph
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magao.as.arizona.edu Oppenheimer & Hinkley 2009 Why is it hard? –Kepler’s laws: Planets orbit their stars.
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magao.as.arizona.edu Males, Close, & Skemer 2013 Extreme AO around the world
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magao.as.arizona.edu New surveys link first-generation imaging surveys with on-going r.v. surveys
Direct Imaging
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What’s • GPI – Gemini Planet Imager – Gemini South, Chile next? • LEECH – LBTI Exozodi-Exoplanet Common Hunt – LBT, Arizona • NaCo/NIRI – IDPS – International Deep Planet Survey – VLT, Chile & Gemini N, Hawaii K. Morzinski
Skemer et al 2013 magao.as.arizona.edu %""& #$&$" Young stars: Direct t <100 Myr Imaging d <75 pc
Where are we going? Adolescent stars: t <300 Myr Where are d <35 pc we now?
Why is it hard? McBride et al 2011 What’s next?
K. Morzinski
magao.as.arizona.edu Modern instrumentation for exoplanet surveys and characterization missions
Direct • Ground • Space Imaging – MagAO – JWST
• VisAO – NWO Where are – LBTI we going? – TPF/Darwin/AFTA… – GPI Where are we now? – SPHERE
Why is – CHARIS it hard? • ELTs What’s next? – E-ELT – GMT
K. Morzinski – TMT
magao.as.arizona.edu Observations and data areas of advancement
• System and Direct Imaging population statistics – Architecture of planetary systems Where are we going? – Frequency of planets
Where are • Atmospheric we now? characterization
Why is – Constituents it hard? – Thermal balance
What’s – Winds, dynamics next? – Variability
K. Morzinski Echo
magao.as.arizona.edu Theory and modeling areas of advancement
• Opacities, model • Formation models Direct Imaging atmospheres – Pebble accretion – Unidentified lines – Migration – Pressure broadening – Population synthesis Where are we going? – Temperature-intensity anomalies Where are we now? • Where observers
Why is should be looking it hard? – spectrally
What’s – spatially next?
K. Morzinski
magao.as.arizona.edu Summary – Surveys for directly-imaged planets • Imaging results have found ~ <10-20% of Direct stars host wide massive planets Imaging – Have not yet probed solar-system-like parameter
Where are space we going? – Kepler: ~15% stars have an Earth-size planet in
Where are the habitable zone we now? – Microlensing: ~17% stars host Jupiter-mass Why is planets it hard?
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K. Morzinski
magao.as.arizona.edu Summary – Remote sensing of exoplanets • 2M 1207 b Direct – Thick clouds, low gravity effects Imaging • HR 8799 – b – Little CH4, non-equilibrium chemistry. Where are Thick mixed clouds? Or cloud-free with high mean- we going? molecular weight atmosphere? Or what? Where are – c – High C:O, core accretion we now? • Beta Pic b – Is it an early-L brown dwarf? Is it a Why is planet that is similar to the early-L dwarfs? it hard? – Further characterization, and formation modeling What’s – Orbital analysis – Disk warp, also upper limit on mass from next? r.v. • Fomalhaut b – what is it? K. Morzinski – Is there another object in there responsible for the disk?
magao.as.arizona.edu Conclusions • We are still in a data-driven discovery space Direct – Modeling is crucial but data is critical to improve Imaging models too
Where are – Finally the r.v. and direct imaging search spaces we going? are starting to overlap. Kepler and microlensing
Where are too – Diverse ways to probe planetary systems will we now? help improve understanding
Why is – New instrumentation and new techniques will it hard? continue to provide big payoff What’s next? MagAO/VisAO: Diffraction-limited visible-light imaging – Close et al 2013
K. Morzinski
magao.as.arizona.edu