Case for high-resolution mid-IR spectroscopy and imaging ...
Transcript of Case for high-resolution mid-IR spectroscopy and imaging ...
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Case for high-resolution mid-IR spectroscopy and imaging of protoplanetary disks on the E-
ELT
Talk by C.P. DullemondMax-Planck-Institute for Astronomy, Heidelberg
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Billion-Dollar Question:
How were “we” formed4.5 Billion years ago?
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STARDUST sample return missionChondritic meteorite
Messengers from the past
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Extrasolar Planetary Systems
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Study “proto-solar systems”
Image: VLT HAWK, ESO Press Release
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Probing the inner disk regions...
Magn.sph.accretion0.02 AU
Dust inner rim0.07 AU
Habitable zone0.5 - 2 AU
Outer disk
T Tauri star
Hubble Space Telescope
8-10 meter Telescope
Mid-IR VLT interferometry
(sub-)mm interferoNear-IR VLT interferometry
E-ELT imaging(!) and spectroscopy
E-ELT spectro-astrometry
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Probing the inner disk regions...
Magn.sph.accretion0.02 AU
Dust inner rim0.5 AU
Habitable zone4 - 13 AU
Outer disk
Herbig Ae/Be star Hubble Space Telescope
8-10 meter Telescope
Mid-IR VLT interferometry
(sub-)mm interferometryNear-IR VLT interferometry
E-ELT imaging(!) and spectroscopy
E-ELT spectro-astrometry
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Major questions• Structure, formation and evolution of
protoplanetary disks?• How and when is gas lost from disks =>
timescale for giant planet formation?– Mechanisms: photoevaporation, winds, …
• How and when is dust lost from disks?• How and when are planets formed?• How do planets affect their birth-disks?• Chemical composition of material for forming
planets (H2O, biogenic molecules, …)?
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Some highlights ofrecent protoplanetary disk
observations
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Rich features in NIR/MIRboth in dust and in gas
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PAH & [Ne II] in disks: tracers of X-ray/EUV radiation
Geers et al. 2006Lahuis et al. 2007Pascucci et al. 2007
T Cha
Detected in at least 20% of sources.Fluxes consistent with recent models of X-ray irradiated disks.
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[Ne II] at high spectral resolution
Herczeg et al. 2007
FWHM=21 km/s,broader than othernarrow lines =>
- Keplerian rotation at 0.1 AU?
-Photoevaporative flow?
TW Hya
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Water andorganics !
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Carr & Najita 2008
Spitzer
Water and organics in AA Tau
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Water and organics in AS 205
Salyk et al. 2008
H2O spectral featuresbarely seen at R=600;should have boomingline/cont at high R
AS 205 Disk in Ophdata
model
ELT can image emission and kinematics at few AU spatial resolution
data
model
data
model
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What would we gain from METIS?
R=105
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Implications • Water gas is found well inside the ‘snow’ line
(estimated at ~3 AU)• Water is expected to disappear in ~105 yr ⇒
replenishment needed• Inward radial migration or upward mixing of icy
planetesimals, followed by evaporation?• Might be able to characterize the snow line with
ELT by direct spatially resolvingThis is extremely important for planet
formation theories!
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Line profiles,P/V diagrams:
Kinematics of the disk(and wind?)
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Hot HCN and CO blue-shifted by 25 km/s =>-Base of MHD wind?
Keck HCN 3 μm and CO 4.7 μm
Resolving the lines
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High R: Dynamics from line profiles
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Cold gas Hot gas
CO v=1-0 band at 4.7 μm in protoplanetary disks
Blake & Boogert 2004
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Spectro-astrometry with CRIRES
• Slit spectrum• At each wavelength fit
Gauss to spatial emission• Plot centroid of Gauss as a
function of wavelength
• Acquires spatial resolution well in excess of PSF!
• But only for 0th Moment• For ELT: Huge resolution!
Pontoppidan et al. 2008
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Large inner holes...
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Transition disks : Huge inner holes
D’Alessio et al. 2005, Forrest et al. 2004
CoKu Tau 4
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Transition disks : Huge inner holes
Brown et al. 2008
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Transition disks : Huge inner holes
Brown et al. 2008
LkHα330
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Transition disks : Huge inner holes
Brown et al. 2008
40 AULkHα330
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Can photoevaporation explain cavities?
EUV Photoevap: - Weak, but- Works around 1 AU
FUV Photoevap: - Strong, but- Works > 50 AU
Hollenbach et al. 1994Gorti & Hollenbach 2007
1 AU50 AU
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Can photoevaporation explain cavities?
Hollenbach 1994; Clarke et al. 2001Alexander, Clarke & Pringle 2006
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Spatial separation small and large grains
VLT VISIR image + spectra
8.6 PAH 19.8 μm large grains
Geers et al. 2007
IRS48in Oph
- 60 AU radius gap seen in large grains, but NOT in PAHs
7-13 μm spectrum
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Prospects for mid-IR imager/spectromete
for E-ELT
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Clumpiness and asymmetries
in protoplanetary disks
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Disks are clumpy / spiraly / asymmetric
Fukagawa et al. 2004
AB Aurigae
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Formation of planets: clumps, waves
Johansen et al. 2006
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Formation of planets: clumps, waves
Johansen et al. 2007
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Formation of planets: clumps, waves
Rice, Lodato et al. 2004
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Planetary gapsand
deviations from Kepler
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Planet gap opening
Credit: Frederic Masset
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Is the gap really empty?
Minimum Mass Solar Nebula
Surface density
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Is the gap really empty?
Minimum Mass Solar Nebula
Optical depthat Near IR
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Is the gap really empty?
Planet
Gap Spiral wave
The answer is: often not! Only for very massive planets
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Detecting gap by probing Kepler-deviations
Planet
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g g 2 p pforming zone
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g g 2 p pforming zone
-18 km/s
10 A U
3 m H2O hot band lines, 1 M star
Model made with RAD-Liteby Klaus M. Pontoppidanand Cornelis P. Dullemond
Includes gas lines and dust continuum
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g g 2 p pforming zone
-9 km/s
10 A U
3 m H2O hot band lines, 1 M star
Model made with RAD-Liteby Klaus M. Pontoppidanand Cornelis P. Dullemond
Includes gas lines and dust continuum
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g g 2 p pforming zone
0 km/s
10 A U
3 m H2O hot band lines, 1 M star
Model made with RAD-Liteby Klaus M. Pontoppidanand Cornelis P. Dullemond
Includes gas lines and dust continuum
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g g 2 p pforming zone
+9 km/s
10 A U
3 m H2O hot band lines, 1 M star
Model made with RAD-Liteby Klaus M. Pontoppidanand Cornelis P. Dullemond
Includes gas lines and dust continuum
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g g 2 p pforming zone
+18 km/s
10 A U
3 m H2O hot band lines, 1 M star
Model made with RAD-Liteby Klaus M. Pontoppidanand Cornelis P. Dullemond
Includes gas lines and dust continuum
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10 AU 3 m H2O hot band lines
-18 km/s 0 km/s-9 km/s 18 km/s9 km/s
120 pc (
Oph)
56 pc(TW Hya)
0 pc
g g 2 p pforming zone
Resolution: E-ELT 42 meter
Nearly no noise, so even these small “ears” can be analyzed to high precision
with an E-ELT
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Probing mixingand turbulence
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Crystallinity: Measuring Prandtl number
Prandtl number (or better: “Schmidt number”) is:
Sc =vviscos ity
Dturb−mixing
One of the most crucial, but completely unknownparameters in the theory of planet formation!
Links mixing and coagulation to the (measureable)accretion rate in the disk.
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Crystallinity: Measuring Prandtl number
Pavlyuchenkov & Dullemond, 2007
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Crystallinity: Measuring Prandtl number
Pavlyuchenkov & Dullemond, 2007
Strong mixing Weak mixing
InnerDisk
Outer Disk
Predicted N-band spectra as a function of R-coordinate:
1 AU2 AU4 AU8 AU
16 AU32 AU64 AU
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Conclusions• Near- and Mid-Infrared are bonanzas of
diagnostics of protoplanetary disks:– Dust composition in earth-forming region– Rich set of atomic / rovib gas lines. [NeII], Water,
Organics!– Kinematics of earth-forming region. Can we see
planet formation in progress!? • ELT with METIS provides:
– Much higher sensitivity than VLT-I, plus true imaging capability (as opposed to VLT-MIDI / MATISSE)
– Same resolving power as ALMA, but much higher sensitivity
– Higher spatial resolving power than NGST