Presentation on theme: "High-contrast imaging with AO Claire Max with help of Bruce Macintosh GSMT Science Working Group December 2002."— Presentation transcript:
High-contrast imaging with AO Claire Max with help of Bruce Macintosh GSMT Science Working Group December 2002
Slide 2 Types of high-contrast AO imaging Point sources near bright stars: images and spectra –Brown dwarfs –Young Jupiters (still shining in IR) –Older Jupiters shining by reflected light –Ultimately, Earth-like planets (?) Disks –Debris disks best observed in thermal IR: good motivation for separate cooled AO system aimed at mid-IR –Protostellar and protoplanetary disks –Have proven to be a challenge for current AO systems –But AO polarimetry is VERY promising
Slide 3 Context All detailed AO simulation results are for 8-10m telescopes Simulations for 30m telescopes still need to be done
Slide 4 Extreme AO Phase Space (Impressionistic chart originally done for 10m telescope)
Slide 6 Point-source sensitivities of Keck AO, NICMOS
Slide 7 Current examples of high contrast images High Dynamic Range at modest separations (~1 arc sec) –Existence supported by disk structures –Confirmation by proper motion essential –Current 8-10m contrast ratios: ~10 6 NICMOS image of HD141569 Showing gap at 250 AU possibly created by wide planet(s) Keck AO image showing a candidate for young extra-solar planet (224 AU, 3-7 M J, if confirmed)
Slide 11 Detection of Jupiters in reflected light Q 30m telescopes
Slide 12 Disk Structures with AO: Role for Thermal IR 3 micron imaging studies 1-2 m NICMOS Study shows colorless scattering Grain growth interpretation ambiguous Simulations for GG Tau L-band (3 m)
Imaging AO polarimetry is central to detecting structure in circumstellar disks Dan Potter, UH
Slide 14 Disk Structures with AO Polarimetry Lick AO Near-infrared polarimetry studies –Measure two orthogonal polarization states simultaneously, subtract to get only polarized light (dust only!) –Dan Potter (UH), Marshall Perrin (UC Berkeley - Lick) LkH 234 IQUP R Mon results
Slide 15 Points to importance of differential detection methods Polarimetry Comparison of different spectral bands –Example: methane vs. non-methane –Integral field AO spectrographs will be inherently very capable for this task
Slide 16 Summary Current state of the art for AO on 8-10m telescopes: –Contrast ratio of ~ 10 6 at separation of ~1 arc sec –Polarimetry, coronagraphy, two-color detection will be very important –“Extreme AO” under active investigation “Extreme AO” on 8-10m telescopes will increase this by factor of 10 - 50 –Can clearly do Jupiters (young and old); Uranus-Neptune Critical issues: –Can Extreme AO on GSMT detect Earthlike planets?? –Specifically how does AO performance affect the various GSMT Science Cases? –How will GSMT performance compare with JWST?
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