- the ao modes for harmoni - from classical to laser...
TRANSCRIPT
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- The AO modes for HARMONI -From Classical to Laser-assisted tomographic AO
systems
Benoît Neichel, Thierry Fusco, Carlos M. Correia, Kjetil Dohlen, Leonardo Blanco, Kacem El Hadi, Jean-François Sauvage, Noah Schwartz, Yoshito Ono, Fraser Clarke, Emmanuel Hugot, Miska Le Louarn, Niranjan A. Thatte, Matthias Tecza, Hermine
Schnetler, Ian Bryson, Angus M. Gallie, David M. Henry, Tim J. Morris, Richard M. Myers, Joël Vernet, Jérôme Paufique, Peter Hammersley, Jean-Luc Gach, Alexis Carlotti, Ariadna Calcines, Pascal Vola, Sandrine Pascal, Marc Llored, Dave Melotte,
Olivier Martin, Arlette Pecontal, Andrew Reeves, James Osbron, Matthew Townson
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HARMONI Overview
Partner Associate Partner Responsibilities
University of Oxford STFC – RAL Space Spectrographs & Obs. Prep
STFC – UK ATC Edinburgh Univ. of Durham Cryostat, AIV, Rotator, LTAO
IAC, Tenerife Pre-optics & Electronics
CSIC – CAB (INTA), Madrid Calibration & Sec. guiding
CRAL, Lyon IPAG, GrenobleIRAP, Toulouse
IFU & Software
LAM, Marseille ONERA, ParisIPAG, Grenoble
SCAO, LTAO, High Contrast
HARMONI Consortium
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HARMONI Overview
Partner Associate Partner Responsibilities
University of Oxford STFC – RAL Space Spectrographs & Obs. Prep
STFC – UK ATC Edinburgh Univ. of Durham Cryostat, AIV, Rotator, LTAO
IAC, Tenerife Pre-optics & Electronics
CSIC – CAB (INTA), Madrid Calibration & Sec. guiding
CRAL, Lyon IPAG, GrenobleIRAP, Toulouse
IFU & Software
LAM, Marseille ONERA, ParisIPAG, Grenoble
SCAO, LTAO, High Contrast
HARMONI Consortium
Thanks for hosting us this week !!
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HARMONI Overview
First light ELT instrument
HARMONI = High Angular Resolution - Monolithic - Optical and Near-infrared - Integral field spectrograph
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HARMONI Overview
First light ELT instrumentWorkhorse instrument - visible and near-infrared spectroscopy (0.5–2.4 µm)Integral Field Spectrograph – providing ~ 30 000 spectra per exposure
3D data cube
HARMONI = High Angular Resolution - Monolithic - Optical and Near-infrared - Integral field spectrograph
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Bands Wavelengths
(μm)
R
“V+R” or “I+z+J” or “H+K”0.45-0.8, 0.8-1.35,
1.45-2.45~3000
“I+z” or “J” or “H” or “K”0.8-1.0, 1.1-1.35, 1.45-
1.85, 1.95-2.45~7500
“Z” or “J_high” or “H_high” or “K_high” 0.9, 1.2, 1.65, 2.2
(TBD)
~20000
HARMONI Overview
HARMONI = 3 resolving powers
3D data cube
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HARMONI Overview
6.42” x 9.12”
3.04” x 4.28”
1.5
2”
x 2
.14
”
21
4 x1
52
spaxe
ls
0.61” x 0.86”
60 x 30 mas
20 mas
10 mas
4 mas
HARMONI = 4 spatial scales
3D data cube
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HARMONI Overview
6.42” x 9.12”
3.04” x 4.28”
1.5
2”
x 2
.14
”
21
4 x1
52
spaxe
ls
0.61” x 0.86”
60 x 30 mas
20 mas
10 mas
4 mas
HARMONI = 4 spatial scales
Assisted with
Adaptive Optics
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HARMONI: Two AO modes
High-Performance – Low sky coverage High-Performance & sky coverage
Single Conjugated AO Laser Tomography AO
x6
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HARMONI
HARMONI, SCAO & LTAO implementation
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HARMONI
Nasmyth Platform
Relay
Light from telescope
Telescope Pre-Focal Station
HARMONI Cryostat
Seeing limited
Focal plane
Re-imaged focal plane
HARMONI, SCAO & LTAO implementation
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HARMONI
Nasmyth Platform
Relay
Light from telescope
Telescope Pre-Focal Station
HARMONI Cryostat
Seeing limited
SCAO WFS SCAOSCAO dichroic
Focal plane
HARMONI, SCAO & LTAO implementation
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HARMONI
Nasmyth Platform
Relay
Light from telescope
Telescope Pre-Focal Station
HARMONI Cryostat
Seeing limited
NGS Pick-off SCAOLGS (<0
.6u
m)
LGSWFSModule
LTAO
Truth Pick-off
Dichroic
HARMONI, SCAO & LTAO implementation
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From Telescope
LGSWFS
SCAO & NGS WFS
IFS
HARMONI
HARMONI, SCAO & LTAO implementation
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From Telescope
LGSWFS
SCAO & NGS WFS
IFS
HARMONI
HARMONI, SCAO & LTAO implementation
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HARMONI SCAO
SCAO system baseline is to use a pyramid WFS:
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HARMONI SCAO
SCAO system baseline is to use a pyramid WFS Better performance & better sensitivity
+2 mag.
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HARMONI SCAO
SCAO system baseline is to use a pyramid WFS Better performance & better sensitivity
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HARMONI SCAO
SCAO system baseline is to use a pyramid WFS Better performance & better sensitivity Managing the “Island” effect
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HARMONI SCAO
SCAO system baseline is to use a pyramid WFS Better performance & better sensitivity Managing the “Island” effect
50cm Spiders
See Noah Schwartz talk on Friday
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HARMONI SCAO
SCAO system baseline is to use a pyramid WFS Better performance & better sensitivity Managing the “Island” effect
See Noah Schwartz talk on Friday
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HARMONI SCAO
SCAO system baseline is to use a pyramid WFS Better performance & better sensitivity Managing the “Island” effect
Small modulation provides information on what’s behind the spider
+ Secret ingredient See Noah Schwartz talk on Friday
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HARMONI SCAO
SCAO system baseline is to use a pyramid WFS Better performance & better sensitivity Managing the “Island” effect
Small modulation provides information on what’s behind the spider
+ Secret ingredient See Noah Schwartz talk on Friday
Before After
Residuals less than
50nm
SCAO will provide a SR of >70% in K-band
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HARMONI SCAO
High Contrast :Spectral characterization of young Jupiters around nearby stars in H & K bands at R=3000-20000, with a 10-6 contrast at 200mas.
From A. Carlotti, A. Vigan, D. Mouillet, M. Bonnefois
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HARMONI SCAO
High Contrast :Simulated data of 4 planets w/ 10-6 planets contrast & 51 Eri b-like synthetic spectrum (2h exp. with H=6 star).
From A. Carlotti, A. Vigan, D. Mouillet, M. Bonnefois
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LGSWFS
SCAO & NGS WFS
HARMONI
HARMONI, SCAO & LTAO implementation
“High-Order Loop”
“Low-Order Loop”
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HARMONI LTAO
LTAO Top-Level Specifications:
Strehl K > 60%
Jitter < 2mas
Sky Coverage >10% at the Pole
60 x 30 mas20 mas10 mas4 mas
EE (20mas) > 40%
Jitter < 5mas
Sky Coverage of >50% at the Pole
EE (40mas) > 50%
Jitter < 10mas
Sky Coverage of >90% at the Pole
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HARMONI LTAO
LTAO Top-Level Specifications:
Strehl K > 60%
Jitter < 2mas
Sky Coverage >10% at the Pole
60 x 30 mas20 mas10 mas4 mas
EE (20mas) > 40%
Jitter < 5mas
Sky Coverage of >50% at the Pole
EE (40mas) > 50%
Jitter < 10mas
Sky Coverage of >90% at the Pole
Set requirements on the LGS High-Order Loop
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HARMONI LTAO
LTAO Top-Level Specifications:
Strehl K > 60%
Jitter < 2mas
Sky Coverage >10% at the Pole
60 x 30 mas20 mas10 mas4 mas
EE (20mas) > 40%
Jitter < 5mas
Sky Coverage of >50% at the Pole
EE (40mas) > 50%
Jitter < 10mas
Sky Coverage of >90% at the Pole
Set requirements on the LGS High-Order Loop
Set requirements on the NGS Low-Order Loop
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90km − ZA=0
130km − ZA=45
180km − ZA=60
20 40 60 80
0.2
0.4
0.6
LGS Radius (arcsec)
SR
(K
−B
an
d)
R0 scaled
HARMONI LTAO
Optimal LGS constellation between R=[15-40]”
“Small” constellation greatly helps for tomographic error
Laser constellation
See Thierry Fusco talk on Thursday
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HARMONI LTAO
Sensing on LGS
LLT
Sodium layer
Detectorplane
T ~ 20km
H ~ 80km
Distance from launch site
Pupilplane
Predicted spot elongation pattern
LLT
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HARMONI LTAO
LLT
Detectorplane
Distance from launch site
Pupilplane
Dealing with spot elongation
25”
1”
Ideally, we need subapertureswith 25x25 pixels of ~1”
For 80x80 subapertures, we need 2000 x 2000 pixels
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HARMONI LTAO
LLT
Detectorplane
Distance from launch site
Pupilplane
Dealing with spot truncation
Most likely, we will have no more than 10x10 pixels
Strong truncation
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HARMONI LTAO
Dealing with spot truncation
Truncation induces biases that are
projected on-axis by the Tomography
See Leo Blanco talk on Thursday
x6
Up to 300nm
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HARMONI LTAO
Dealing with spot truncation
One way to reduce this impact is to reject the
truncated measurements
See Leo Blanco talk on Thursday
x6
Down to 80nm
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Temporal frequency [Hz]10
-210
-110
010
110
2
|Y(f
)|2/H
z
10-10
10-5
Single-Sided Amplitude Spectrum of y(t)
PSD ATM
PSD WS
HARMONI LTAO
Sensing on NGS
Main offender is the telescope Windshake
Atmosphere = 15 masWindshake = 263 mas
But windshake is isoplanatic:
we can use the telescope WFS
to reduce it
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HARMONI LTAO
Sensing on NGS
2x2 Shack-Hartmann8 mas / pixel
125 pixel / subap.500 Hz
1.2 to 2.2 microns
Jitter control strategy:• Use “bright but far” stars to compensate windshake with
telescope WFS • Use “faint but close” star to compensate atmospheric jitter
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HARMONI LTAO
Sensing on NGS
2x2 Shack-Hartmann8 mas / pixel
125 pixel / subap.500 Hz
1.2 to 2.2 microns
Jitter control strategy:• Use “bright but far” stars to compensate windshake with
telescope WFS • Use “faint but close” star to compensate atmospheric jitter
0 5 100.0
0.2
0.4
0.6
0.8
jitter (mas)
Sky C
ov.
10% Sky Cov. for 2mas
South galactic Pole
50% Sky Cov. for 5mas
90% Sky Cov. for 10mas
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Sensing on NGS
HARMONI LTAO See Carlos Correia poster on Thursday
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Cosmos Field
LTAO 1NGS
−0.1 0.0 0.1 0.2
0.1
0.2
0.3
0
1
2
3
4
6
7
8
9
10
11
jitt
er
[ma
s]
RA + 150.05 [deg]
DE
C +
2.1
7 [
deg
]
Sensing on NGS
HARMONI LTAO
GoodS Field
LTAO 1NGS
Old ESO profile
0.0 0.1 0.20.0
0.1
0.2
0
1
2
3
4
5
6
7
9
10
11
12
13
14
15
16
jitt
er
[ma
s]
RA + 53.00 [deg]
DE
C +
−2
7.9
4 [
de
g]
See Carlos Correia poster on Thursday
The NGS strategy fulfills the science requirements for all observations
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Conclusion: HARMONI schedule
12/2017
PDR
2019
FDR
2023
MAIT
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2024: integration at the telescope
Dr. Frans Snik
2024: 1st light !
Conclusion: HARMONI schedule
12/2017
PDR
2019
FDR
2023
MAIT
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- The AO modes for HARMONI -
1 more slide beforeCoffee Break !
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Register now, for the 2 to 4 October 2017 in Padova, Italy
https://www.ict.inaf.it/indico/event/521/
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Register now, for the 2 to 4 October 2017 in Padova, Italy
https://www.ict.inaf.it/indico/event/521/
Marseille 2016
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HARMONI SCAO
SCAO system baseline is to use a pyramid WFS Better performance & better sensitivity
151397 17