Characterization of extrasolar planets with SPHERE

Transcript

Characterization of exoplanetary systems
with VLT/SPHERE
Anne-Lise Maire (INAF-Padova) on behalf of the SPHERE Consortium
Jean-Luc Beuzit (PI), Markus Feldt (Co-PI),
David Mouillet (PS), Pascal Puget (PM), Kjetil Dohlen (SE), F. Wildi (AIT),
and numerous participants from 12 European institutes!
Co-Is: G. Chauvin (IPAG, Grenoble), T. Henning (MPIA, Heidelberg), C.
Moutou (LAM, Marseille), A. Boccaletti (LESIA, Paris), S. Udry
(Observatoire de Genève), M. Turatto (INAF, Padova), H.M. Schmid
(ETH, Zurich), F. Vakili (Lagrange, Nice), C. Dominik (UvA, Amsterdam)
T. Fusco (ONERA responsible), M. Kasper (ESO responsible)
Nov. 7th, 2014
La Ricerca dei Pianeti Extrasolari in Italia, Roma
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Designed for planetary system studies
 High contrast detection capability
 Extreme AO
 Advanced coronagraphy
 Differential imaging techniques: angular, simultaneous
spectral (dual-band, multi-wavelength), polarimetric
 for a large sample of bright stars
SPHERE User Manual
 Optimal correction up to R ~ 9-10 (…and up to R>11! )
Nov. 7th, 2014
80%
Spec in H band
for faint star!
>11
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Designed for planetary system studies
 High contrast detection capability
 Extreme AO
 Advanced coronagraphy
 Differential imaging techniques: angular, simultaneous
spectral (dual-band, multi-wavelength), polarimetric
 for a large sample of bright stars
 Optimal correction up to R ~ 9-10 (…and up to R>11! )
 & separations: optimized 0.2–0.8’’, access 0.050–6’’
 Complementary information in VIS & NIR:
 High angular resolution imaging in various filters
 Spectral characterization up to medium resolution
 Polarization & differential imaging in NIR & VIS
Nov. 7th, 2014
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Concept overview
Beam control
(DM, TT, PTT,
derotation)
Polar control
Calibration
Fore
optics
Common Path
High frequency AO correction (41x41 act.)
High stability : image / pupil control
Visible – NIR Refraction correction
FoV = 12.5’’
40x40 SH-WFS in visible
1.2 KHz, RON < 1e-
Extreme
AO
Vis
Coronagraph
NIR
Coronagraph
Pupil apodization
Focal masks: classical Lyot, HW4QPM, APLC
IR-TT sensor for fine centering
Nasmyth platform, static bench,
Temperature control, cleanliness control
Active vibration control
Nov. 7th, 2014
Coronagraphic imaging:
Dual polarimetry, direct BB + NB
λ = 0.5 – 0.9 µm,
λ/2D @ 0.6 µm, FoV = 3.5’’
ZIMPOL
IFS
IRDIS
0.95 – 1.35/1.65 µm
λ/2D @ 0.95 µm,
Spectral resolution:
R = 54 / 33
FoV = 1.77’’
0.95 – 2.32 µm; λ/2D @ 0.95 µm
FoV = 11’’
Direct BB + NB
Differential imaging: 2 filters, R~30
Long slit spectro: R~50 & 400
Differential polarization
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Classical imaging
HR4796A, IRDIS H band, ADI
J. Milli
ESO press release 1417:
http://www.eso.org/public/news/eso1417/
Nov. 7th, 2014
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IRDIFS mode
2,00E-13
ESO press release 1417:
http://www.eso.org/public/news/eso1417/
Flux
1,50E-13
iota Sgr B
1,00E-13
IRDI-H2-H3
M1V
5,00E-14
Very high SNR detection
Δm~9 companion @ 0.24’’
M2.5V
0,00E+00
0,9
R. Gratton
1,1
1,3
1,5
1,7
Wavelength (μm)
A. Vigan
D. Mesa
Simultaneous IRDIS H2-H3 bands & IFS Y-J
Nov. 7th, 2014
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Dual-band imaging

Simultaneous imaging in 2 adjacent spectral filters
- Filter 1: star+planet
- Filter 2: star
Out methane band
Subaru/HiCIAO
Nov. 7th, 2014
In methane band
GJ504 b
Janson et al. (2013)
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Dual-polarization imaging

Disk light polarized, star light usually not
Quanz et al. (2011)
HD100546
Disk morphology
info unseen planets
VLT/NaCo
Nov. 7th, 2014
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Dual-polarization imaging

Disk light polarized, star light usually not
Quanz et al. (2011)
HD100546
Quanz et al. (2013)
Disk
morphology
Protoplanet candidate
info unseen planets
VLT/NaCo L’
VLT/NaCo
Nov. 7th, 2014
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IRDIS long-slit spectroscopy
Brown-dwarf companion @ 0.5’’
separation
A. Vigan
Masked star core
10-5
YJ
H
K
After preprocessing
Dispersed stellar
speckles
wavelength
After differential imaging
LRS (R≈50), 20-min exp, seeing 0.5–0.6’’, companion contrast ΔH≈5.4
Observing mode unique to SPHERE!
Nov. 7th, 2014
SPHERE User Manual
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Color information
β Pic b
Bonnefoy et al. (2013)
VLT/NaCo
HD95086 b
Galicher et al. (2014)
Gemini/GPI
β Pic b
Nov. 7th, 2014
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Spectral information
Molecules
2M1207 b
Variability
Keck
HR8799 c
HR8799 b
Apai et al. (2013)
L/T brown dwarfs
Konopacky et al. (2013)
HST
Vertical structure of atmosphere
HR8799 cd
Skemer et al. (2014) – LBT
Nov. 7th, 2014
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Constraints on formation models
Hot-start
β Pic b
Hot-start
Cold-start
Cold-start
Excluded by RV
constraints
β Pic b
Bonnefoy et al. (2013)
VLT/NaCo
Nov. 7th, 2014
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Astrometry
HR8799
Literature data
SPHERE astrometric precision in lab
Zurlo et al., A&A, in press
http://arxiv.org/abs/1410.1754
IRDIS
IFS
Orbit architecture
A.-L. Maire, S. Desidera
Nov. 7th, 2014
• 3 mas @ SNR=10
• 1 mas @ SNR=50
• <0.5 mas @ SNR>100
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VIS imaging


Nearby (<10 pc) cold/mature giant planets in
polarimetry  dedicated GTO survey
Accreting giant planets in Hα (diffr. limit for seeing 0.6–0.7’’)
Schmid et al. 2006
Titan
Ice giants
MCT/MagAO+VisAO
Gas giants
Solar System’s planets
Nov. 7th, 2014
Close et al. 2014
Low-mass stellar
companion
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Summary






Imaging allows to characterize a large variety of
planets + circumstellar disks
Colors  spectral type, Teff, surface gravity
Spectra  molecules, vertical structure
Astrometry  orbit architecture, dynamical mass
Constraints planetary formation models
SPHERE designed to address these questions for a
large sample of targets
Nov. 7th, 2014
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Characterization of extrasolar planets with SPHERE

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