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Direct Imaging, PPVII Currie Review - Coggle Diagram
Direct Imaging
7.8 Other imaging concepts
Intensity Interferometry (including CTA; not amplitude interferometry like in radio or CHARA), Fresnel imaging
Future resolved imaging: Even beyond LIFE or Maeyin or Tianlin/HWO, extreme large aperture, or even hypertelescopes with dozens/hundreds elements, or use lensing or nearby stars
Planetary radar: detecting reflected signals, so far only solar system, need something 1e5x Arecibo for exoplanets
GW signatures: 3 types, star-planet single systems, as overall background, and planet-WD binary systems. Only planet-WD binary systems detectable even with LISA.
Beyond diffraction limit: very much conceptual stage and still questionable.
Desirable innovations: see Cunningham 2009
7.9 Searches and surveys
First Generation Instruments
IDPS with Keck, Gemini, VLT (found any?), VLT-NACO, Gemini-NICI (300 stars, no planet), Subaru-SEEDS (5yr, 120 nights, found a few), LBT-LEECH
Second Generation Instruments
VLT-SPHERE: since 2014, found a few
Gemini-GPI: since 2013, found a few
Search around planet hosts: Probing stellar multiplicity; targeting known planets (mostly with early generation instruments? found any?)
Search around binary stars: VLT-NACO SPOTS program found 5 substellars out of 117 binaries
7.10 Discoveries
Overall: 84 planets as of 2025.9.3; first generation 10-30 MJ, new instrument down to 1-2 MJ, now JWST ~0.3 MJ; Debate over planet vs. BD.
Around young stars and statistics
With debris disks
Protoplanetary disks
7.11 Miscellaneous signatures
7.12 Imaging at other wavelengths
PPVII Currie Review
Detections
Taxonomy (classification)
Why 13 MJ is bad (deuterium burning)
exceptions
resonant companions with 20+ MJ
free floating objects with 5MJ
Mass and metallicity dependent
New def: 25 MJ, 300au, q<0.025
Fully formed planets
General properties
Emblematic systems
Protoplanets
Challenges
Confirmation
Estimating mass
long orbit - dynamical mass hard to get / impossible - model dependent
Hot start vs. Cold start: latest results overall support hot start for all types of planets, but also planets were formed with a range of entropy
Planet or disk feature?
Synergies with other techniques
Interferometry (GRAVITY, 130m baseline though small FoV 50 mas, but RV etc. can help predict planet location)
Connecting RV and microlensing and future astrometry discoveries in semimajor axis space
Atmospheric Characterization
Time averaged
Photometry
Spectroscopy
Theoretical inference
Time resolved
Field brown dwarfs and directly imaged planets are all fast rotators! Prot ~ few - 24 hours!
Clear variability in photometry and spectroscopy, more so in planets than BDs
Modeling
1-D Model
Inversion (retrieval)
3-D Model
Connecting abundance to formation/migration
Surveys and Population Stats
Target Selection
Young; bright; disk; stars with acceleration
List of Surveys
Progression: 8m telescope + AO + speckle + coronography
Occurrence and Demographics
Testing Formation
Instrumentation and Methods
Detectability
Reflected light
Thermal emission
Instruments
Wavefront control
Starlight suppression
Data processing
Architecture
Orbits and Dynamics
Planet-Disk Interactions
Future
New tech and facilities
Science focus trend
Introduction
oval shape - Sharon's read