transition disks - valentinchristiaensdmawet/meetings/transition-disks---valentin.pdfvalentin...
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![Page 1: Transition disks - ValentinChristiaensdmawet/meetings/transition-disks---valentin.pdfValentin Christiaens Universidad de Chile - Université de Liège Thesis advisors: Simon Casassus](https://reader035.vdocuments.mx/reader035/viewer/2022070823/5f2bc4ebc2261d19572a8a15/html5/thumbnails/1.jpg)
Transition Disks
Vortex yearly meeting - Aug. 15, 2016
Valentin Christiaens Universidad de Chile - Université de Liège
Thesis advisors: Simon Casassus - Olivier Absil
![Page 2: Transition disks - ValentinChristiaensdmawet/meetings/transition-disks---valentin.pdfValentin Christiaens Universidad de Chile - Université de Liège Thesis advisors: Simon Casassus](https://reader035.vdocuments.mx/reader035/viewer/2022070823/5f2bc4ebc2261d19572a8a15/html5/thumbnails/2.jpg)
1. What is a transition(al) disk? Why should we observe them?
2. First results of the AGPM on transition disks
3. Current transition disk programs with the AGPMs
Outline
![Page 3: Transition disks - ValentinChristiaensdmawet/meetings/transition-disks---valentin.pdfValentin Christiaens Universidad de Chile - Université de Liège Thesis advisors: Simon Casassus](https://reader035.vdocuments.mx/reader035/viewer/2022070823/5f2bc4ebc2261d19572a8a15/html5/thumbnails/3.jpg)
Outline1. What is a transition(al) disk? Why should we observe them?
2. First results of the AGPM on transition disks
3. Current transition disk programs with the AGPMs
![Page 4: Transition disks - ValentinChristiaensdmawet/meetings/transition-disks---valentin.pdfValentin Christiaens Universidad de Chile - Université de Liège Thesis advisors: Simon Casassus](https://reader035.vdocuments.mx/reader035/viewer/2022070823/5f2bc4ebc2261d19572a8a15/html5/thumbnails/4.jpg)
—104
t (yrs)
—105
—106
—107
—108
Transition Disks (TDs)
credit: L. Pérez
• Short definition of TD: Protoplanetary disk (still has gas!) showing evidence for a gap/cavity in the dust distribution
• Why are they so interesting? Giant planet formation must occur before the gas in the disk gets dissipated (max. ~10Myr)
TDDebris diskTransition disk
Class I/II (pp.) disk
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First observational identification
Espaillat+14 (PPVI)
:
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pre-Transitional disksGM Aur
Espaillat+07
UX Tau A
Espaillat+11
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Confirmation with resolved images
Espaillat+14 (PPVI)
sub-mm continuum
(large grains)
N-IR polarized light
(small grains)
HD 142527 (Avenhaus+13)
PDS 70 (Hashimoto+12)
LkCa 15 (Thalmann+14)
HD 169142 (Quanz+13)
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Origin?Grain growth Photoevaporation Companion
(Strom & Najita)
D U S T
G A S
So far most observations indicate a shallower gap in the gas than in the dust distribution => hint towards a companion origin
![Page 9: Transition disks - ValentinChristiaensdmawet/meetings/transition-disks---valentin.pdfValentin Christiaens Universidad de Chile - Université de Liège Thesis advisors: Simon Casassus](https://reader035.vdocuments.mx/reader035/viewer/2022070823/5f2bc4ebc2261d19572a8a15/html5/thumbnails/9.jpg)
Additional companion signposts
(Dong+15)
HD 135344 B (Muto+12)
Modelling
(Avenhaus+13)
• Spiral arms
HD 142527
HD 100453 (Wagner+15)(Fukagawa+06)
HD 100546
BUT alternative origins: gravitational instability, recent fly-by, shadowing from inner disk
(Christiaens+14)
(Grady+01) (Boccaletti+13)
(Dong+16)
MWC 758 (Benisty+15)
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A pressure bump or “vortex” (e.g. generated by a planet) can trap large dust grains
(Pinilla+12)
HD 142527 (Casassus+13,+15)
• Spiral arms • Dust traps
BUT alternative origin: any extrema in the surface density profile can trigger instabilities leading to the formation of a vortex and hence to a dust trap
Additional companion signposts
IRS 48 (van der Marel+13)
MWC 758 (Marino+15)
![Page 11: Transition disks - ValentinChristiaensdmawet/meetings/transition-disks---valentin.pdfValentin Christiaens Universidad de Chile - Université de Liège Thesis advisors: Simon Casassus](https://reader035.vdocuments.mx/reader035/viewer/2022070823/5f2bc4ebc2261d19572a8a15/html5/thumbnails/11.jpg)
Outline1. What is a transition(al) disk? Why should we observe them?
• It is a primordial disk with some evidence for gap/cavity • Their age and morphology are consistent with the presence of planets • Additional companion signposts have been observed (spirals, dust traps)
=> TDs are prime targets to look for forming planets • Most TDs might reveal remarkable disk features given enough angular
resolution and sensitivity
2. First results of the AGPM on transition disks
3. Current transition disk programs with the AGPMs
![Page 12: Transition disks - ValentinChristiaensdmawet/meetings/transition-disks---valentin.pdfValentin Christiaens Universidad de Chile - Université de Liège Thesis advisors: Simon Casassus](https://reader035.vdocuments.mx/reader035/viewer/2022070823/5f2bc4ebc2261d19572a8a15/html5/thumbnails/12.jpg)
Outline1. What is a transition(al) disk? Why should we observe them?
• It is a primordial disk with some evidence for gap/cavity • Their age and morphology are consistent with the presence of planets • Additional companion signposts have been observed (spirals, dust traps)
=> TDs are prime targets to look for forming planets • Most TDs might reveal remarkable disk features given enough angular
resolution and sensitivity
2. First results of the AGPM on transition disks
3. Current transition disk programs with the AGPMs
![Page 13: Transition disks - ValentinChristiaensdmawet/meetings/transition-disks---valentin.pdfValentin Christiaens Universidad de Chile - Université de Liège Thesis advisors: Simon Casassus](https://reader035.vdocuments.mx/reader035/viewer/2022070823/5f2bc4ebc2261d19572a8a15/html5/thumbnails/13.jpg)
• If photospheric, the L-band mag of these detections would correspond to brown dwarfs (>15-28 MJup)
• The morphology of the disk would be different for such objects
• Very faint H and K band counterparts => Most likely explanation: accreting protoplanets heating circum-planetary disk (e.g. Montesinos+15)
Protoplanet candidates
HD 169142 b (Reggiani+14; Biller+14)
HD 100546 b (Quanz+13,+15; Currie+14)
LkCa 15 b (Kraus & Ireland 12; Sallum+15)
![Page 14: Transition disks - ValentinChristiaensdmawet/meetings/transition-disks---valentin.pdfValentin Christiaens Universidad de Chile - Université de Liège Thesis advisors: Simon Casassus](https://reader035.vdocuments.mx/reader035/viewer/2022070823/5f2bc4ebc2261d19572a8a15/html5/thumbnails/14.jpg)
HD 169142 b
L’-AGPM hunting trophies in TDs
(Reggiani+14)
(Biller+14)
MWC 758
LkCa 15PCA-RDI PCA-ADI
=> disk edge; blob close to expected position
(Absil+in prep)
=> spiral arms; new blob
(Reggiani/Christiaens+ in prep)
PCA-RDI PCA-ADI
(Thalmann+14)
(Benisty+15)
![Page 15: Transition disks - ValentinChristiaensdmawet/meetings/transition-disks---valentin.pdfValentin Christiaens Universidad de Chile - Université de Liège Thesis advisors: Simon Casassus](https://reader035.vdocuments.mx/reader035/viewer/2022070823/5f2bc4ebc2261d19572a8a15/html5/thumbnails/15.jpg)
Outline1. What is a transition(al) disk? Why should we observe them?
• It is a primordial disk with some evidence for gap/cavity • Their age and morphology are consistent with the presence of planets • Additional companion signposts have been observed (spirals, dust traps)
=> TDs are prime targets to look for forming planets • Most TDs might reveal remarkable disk features given enough angular
resolution and sensitivity
2. First results of the AGPM on transition disks • L’-AGPM ideal to look for protoplanets • L’-AGPM also allows to probe disk features
3. Current transition disk programs with the AGPMs
![Page 16: Transition disks - ValentinChristiaensdmawet/meetings/transition-disks---valentin.pdfValentin Christiaens Universidad de Chile - Université de Liège Thesis advisors: Simon Casassus](https://reader035.vdocuments.mx/reader035/viewer/2022070823/5f2bc4ebc2261d19572a8a15/html5/thumbnails/16.jpg)
Outline1. What is a transition(al) disk? Why should we observe them?
• It is a primordial disk with some evidence for gap/cavity • Their age and morphology are consistent with the presence of planets • Additional companion signposts have been observed (spirals, dust traps)
=> TDs are prime targets to look for forming planets • Most TDs might reveal remarkable disk features given enough angular
resolution and sensitivity
2. First results of the AGPM on transition disks • L’-AGPM ideal to look for protoplanets • L’-AGPM also allows to probe disk features
3. Current transition disk programs with the AGPMs
![Page 17: Transition disks - ValentinChristiaensdmawet/meetings/transition-disks---valentin.pdfValentin Christiaens Universidad de Chile - Université de Liège Thesis advisors: Simon Casassus](https://reader035.vdocuments.mx/reader035/viewer/2022070823/5f2bc4ebc2261d19572a8a15/html5/thumbnails/17.jpg)
NACO+AGPM (mini-)mini-survey (PI: Christiaens)
• Search for protoplanets using direct imaging in L’-band • Initial plan: mini-survey of 16 transition disks with NACO+AGPM
…but severe streak of bad luck • Targets observed so far:
Source Type Instrument Obs. strategy
PDS 66 TD NACO (+AGPM) RDI
RU Lup TD NACO (+AGPM) ADI
HD 98800B TD or circum-binary gap? NACO BDI
DoAr 21 TD? NACO (+AGPM) ADI+RDI
TWA 7 Debris disk NACO (+AGPM) ADI
gamma doradus Debris disk MagAO/Clio2 ADI
HD 35650 Debris disk MagAO/Clio2 ADI
• Data reduction in progress
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NIRC2+AGPM mini-survey (PI: Ruane)• Search for protoplanets using direct imaging in L’-band
• Beginning of the observations last Saturday • First result:
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First ALES+AGPM images
FOV (1.2”x1.2”)
First AGPM+IFU image (beta Aur) Spectral image cube (2.8 – 4.2 microns, R~20)
LMIRCam+AGPM mini-survey (PI: Defrère)
• Weather loss for TDs => commissioning of ALES+AGPM
![Page 20: Transition disks - ValentinChristiaensdmawet/meetings/transition-disks---valentin.pdfValentin Christiaens Universidad de Chile - Université de Liège Thesis advisors: Simon Casassus](https://reader035.vdocuments.mx/reader035/viewer/2022070823/5f2bc4ebc2261d19572a8a15/html5/thumbnails/20.jpg)
Summary1. What is a transition(al) disk? Why should we observe them?
• It is a primordial disk with some evidence for gap/cavity • Their age and morphology are consistent with the presence of planets • Additional companion signposts have been observed (spirals, dust traps)
=> TDs are prime targets to look for forming planets • Most TDs might reveal remarkable disk features given enough angular
resolution and sensitivity
2. First results of the AGPM on transition disks • L’-AGPM ideal to look for protoplanets • L’-AGPM also allows to probe disk features
3. Current transition disk programs with the AGPMs • VLT: results for the NACO+AGPM mini-survey will arrive soon • Keck: promising start for the NIRC2+AGPM mini-survey • LBT: LMIRCam+AGPM mini-survey delayed