Subaru Telescope Ground Layer AO System and New Near-IR ...• Need of Competitive NIR Instrument(s)...
Transcript of Subaru Telescope Ground Layer AO System and New Near-IR ...• Need of Competitive NIR Instrument(s)...
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Subaru Telescope Ground Layer AO Systemand New Near-IR Instrument2013/04/15I. Iwata (New Development Group, Subaru Telescope, NAOJ)
photo by Sebastian Egner
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Subaru Next-Gen AO Working Group
• Founded in 2011
• Members:
• M. Akiyama, Y. Ohno (Tohoku Univ.)
• K. Motohara (Univ. of Tokyo)
• NAOJ:
• PI: N. Arimoto
• Y. Hayano, S. Oya, Y. Minowa, M. Hattori
• T. Usuda, T. Kodama, N. Takato, H. Terada, I. Tanaka, T. Hattori, I. Iwata
• H. Takami, M. Iye
• Public Meetings, Publications and Reviews:
• 2011/09: Subaru Next-Gen AO WS @ Osaka Univ.
• 2012/08: Study Report
• 2012/11: Evaluation by Japanese Community (for various projects)
• Science=S、Feasibility=S、Urgency=A
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Ground Layer AO + New NIR Instrument
1. Ground Layer AO with Adaptive Secondary Mirror
2. New Near-IR Instrument (Wide-field Imager + MOS)
• → Seeing Improvement (FWHM 0.4”→0.2”) over FoV >15’
• High Spatial Resolution Competitive to HST
• Higher Sensitivity Equivalent to 2x Telescope Aperture*1
• 6x Wider Field of View*2
• Targeted to Start Operation in 2020
*1For point sources.*2 Relative to MOIRCS
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Science Objectives
• Understanding History of Galaxy Evolution with
Huge Imaging + Spectroscopic Sample of High-z Galaxies• ~Several Thousands of 1<z<3 Galaxies - Morphology, Kinematics, SF Diagnostics,
Environmental Effects etc.
• Detection of the Most Distant Galaxies w/ Narrow-band Imaging• Finding Galaxies at z>7.5, Exploration of the Cosmic Reionization
•→ Unique Samples for TMT
•‘Upgrade’ of Subaru Telescope, Benefit for Various Science Cases
Study Report by Many Contributions:http://www.naoj.org/Projects/newdev/ngao/
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Galaxy Evolution
Distant Galaxies
Galactic Archaeology
Exoplanets
Galactic Center
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Why GLAO+WFNIRIMOS?
• Need of Competitive NIR Instrument(s) - Based on Recommendations by SAC
• ‘Large Survey’ is Subaru’s Strategy in TMT era
• Uniqueness of GLAO + >10’ NIR instrument
• Mauna Kea is Suited for GLAO
• Key Elements of AO for TMT (Tomography, Multiple Laser and WFS, ASM)
• Pathway from Subaru to TMT
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Ground Layer AO for Subaru
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Ground Layer Adaptive Optics (GLAO)
• Adaptive Secondary Mirror (ASM)
• Multiple Laser Guide Stars, Multiple Wavefront Sensors
• Tomography of Earth Atmosphere
• Correct Ground Layer Turbulence with ASM
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0 0.2 0.4 0.6 0.80
0.25
0.5
0.75
1
FWHM (moffat) [arcsec]
Prob
abilit
y
R−band
0 0.2 0.4 0.6 0.80
0.25
0.5
0.75
1
FWHM (moffat) [arcsec]Pr
obab
ility
J−band
0 0.2 0.4 0.6 0.80
0.25
0.5
0.75
1
FWHM (moffat) [arcsec]
Prob
abilit
y
H−band
0 0.2 0.4 0.6 0.80
0.25
0.5
0.75
1
FWHM (moffat) [arcsec]
Prob
abilit
y
K−band
Expected Performance of Subaru GLAO:FWHM Improvement
by S. Oya
10’
Distance from Center
15’ 20’ SeeingGLAO
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0 0.2 0.4 0.6 0.80
0.25
0.5
0.75
1
FWHM (moffat) [arcsec]
Prob
abilit
y
R−band
0 0.2 0.4 0.6 0.80
0.25
0.5
0.75
1
FWHM (moffat) [arcsec]
Prob
abilit
y
J−band
0 0.2 0.4 0.6 0.80
0.25
0.5
0.75
1
FWHM (moffat) [arcsec]
Prob
abilit
y
H−band
0 0.2 0.4 0.6 0.80
0.25
0.5
0.75
1
FWHM (moffat) [arcsec]
Prob
abilit
yK−band
Expected Performance of Subaru GLAO:FWHM Improvement
by S. Oya
10’
Distance from Center
15’ 20’ SeeingGLAO
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0 0.2 0.4 0.6 0.8 10
0.25
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1
Esq.Engy.
Probability
R−band
0 0.2 0.4 0.6 0.8 10
0.25
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Esq.Engy.Probability
J−band
0 0.2 0.4 0.6 0.8 10
0.25
0.5
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1
Esq.Engy.
Probability
H−band
0 0.2 0.4 0.6 0.8 10
0.25
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0.75
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Esq.Engy.
Probability
K−band
Expected Performance of Subaru GLAO:Ensquared Energy Improvement
0.24”
Size
0.36” 0.48”
Seeing GLAO
by S. Oya
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0 0.2 0.4 0.6 0.8 10
0.25
0.5
0.75
1
Esq.Engy.
Probability
R−band
0 0.2 0.4 0.6 0.8 10
0.25
0.5
0.75
1
Esq.Engy.
Probability
J−band
0 0.2 0.4 0.6 0.8 10
0.25
0.5
0.75
1
Esq.Engy.
Probability
H−band
0 0.2 0.4 0.6 0.8 10
0.25
0.5
0.75
1
Esq.Engy.
Probability
K−band
Expected Performance of Subaru GLAO:Ensquared Energy Improvement
0.24”
Size
0.36” 0.48”
Seeing GLAO
by S. Oya
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Adaptive Secondary Mirror On-Source Performance
0 0.5 1 1.5 2 2.5 3 3.5 4 4.5 50
0.1
0.2
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wavelength [µ m]
SRASM, LGSAO188, GLAO
by S. Oya
On-Src
AO188
GLAOStre
hl R
atio
ASM can also be an excellent on-source AO
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Wide-Field NIR Instrument for GLAO
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Wide-Field Instrument for GLAO• Requirements from Science Cases (So far):
• Imaging: Wide-Field Near-IR Camera
• Broad-band + Narrow-Band Filters
• 0.9-2.5μm
• Multi-Object Spectroscopy
• Spectral Resolution R > 2,000
• 0.9-2.5μm
• Multi-Object Integral Field Spectroscopy (IFS)
• (No specific requirement on multiplicity yet)
• Field-of-View: >100 arcmin2
• Spatial Resolution: 0.1-0.2 arcsec
• Other possible instruments:
• Optical spectrograph
• K- and L-band Camera
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Wide-Field NIR Imager+Multi-Object Spectrograph
• So far we have studied the possible optical designs of wide-field Near-IR imager and multi-object spectrograph for the Cassegrain focus of Subaru Telescope.
• Scale-Up version of MOIRCS, a current Subaru instrument (4’x7’ FoV)
• We have explored two possible optical designs:
• A case without splitting FoV
• maximum FoV: 13’x13’-16’x16’, depending on whether we can alter optical parameters of the secondary mirror of the telescope.
• A case with splitting FoV into 4 segments
• maximum total FoV: 17’x17’ - 23’x23’
• We are now examining how FoV is limited with vignetting by telescope structures.
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Wide-Field NIR Imager+Multi-Object Spectrograph(A case without FoV splitting)
• Optical Design by Dr. Yamamuro (Optcraft)
FoV 12.6’
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Wide-Field NIR Imager+Multi-Object Spectrograph(A case with FoV splitting)
Telescope + Cass Instrument Optical LayoutNo modification on mirror shapes
• Optical Design by Dr. Yamamuro (Optcraft)
FoV 17’
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Wide-Field NIR Imager+Multi-Object Spectrograph(A case with FoV splitting)
4 H4RG0.06”/pix
AO Guide Starpick-off area
• Optical Design by Dr. Yamamuro (Optcraft)
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WFNIRIMOS - Specifications under Consideration
Wavelength 0.8-2.5μm
Plate Scale 0.06-0.1”/pix
FoV approx.13‘x13’ Wider with Split FoVs?
Filters Broad+Narrow
MOS Multi Slit Mask
λ Dispersion 2000(TBD) Under Investigation
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Subaru MOIRCS
Subaru GLAO
TMT IRIS HST WFC3/IR JWST NIRCam
TelescopeAperture
8.2m 8.2m 30m 2.4m 6.5m
Wavelength Coverage 0.9-2.5μm 0.9-2.5μm 0.84-2.4μm 0.9-1.7μm
0.9-2.3μm / 2.4-5.0μm
Spatial Resolution
0.117”/pix0.4”@2μm
~0.1”/pix0.2”@2μm
4 mas10mas@1μm
0.13”/pixFWHM~ 0.25”
32 mas /64 mas
Field of View 28 □’ ~180 □’ 0.075 □’ 4.65 □’ 9.7 □’
Comparison: Imaging
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Subaru MOIRCS
Subaru GLAO
TMT IRIS HST WFC3/IR JWST NIRSpec
Wavelength Coverage 0.9-2.5μm 0.9-2.5μm 0.84-2.4μm 0.9-1.7μm 0.6-5μm
Spatial Resolution
0.117”/pix0.4”@2μm
~0.1”/pix0.2”@2μm
4 - 50 mas0.13”/pix
FWHM~ 0.25”0.2”x0.45”
Field of View ~25 □’ ~120 □’ 0.2-10 □” 4.65 □’12.24 □’(MSA)
3”x3”(IFS)
FunctionsSingle-Slit
MOSIFS
MOSMulti-IFS?
IFS SlitlessSlits
MicroshuttersIFS
Spectral Resolution
600-3000 -2000? 4000-10000 TBW 100, 1000, 2700
Comparison: Spectroscopy
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How fine can we resolve them?
1kpc
100 pc
GLAO
Seeing
JWST NIRCam
TMT IRIS
@ 2μm
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1kpc
100 pc
GLAO
Seeing
JWST NIRCam
TMT IRIS
@ 2μm
How fine can we resolve them?
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1e40 erg
1e39 erg
GLAO
Seeing
JWST NIRSpec
TMT IRIS
Emission-Line Sensitivities
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1e40 erg
1e39 erg
GLAO
Seeing
JWST NIRSpec
TMT IRIS
Emission-Line Sensitivities
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Schedule and Resources
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Schedule
2012 13 14 15 16 17 18 19 2020
Concept Design
Prelim Design
Detail Design
Fabrication
Telescope Modification
Integration and Test
Science Operation
Review
FL
TMT
PFS
HSC
AO188/LGS
Review
Review
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Budget
Item Cost (USD)
Adaptive Secondary Mirror 5-10M
Laser System 4-8M
Wavefront Sensor System ~3.5M
Computers ~0.2M
Telescope Modifications 15-25M
Instruments 5-15M
(Additional) Human Resources ~2M
Total 35-60M
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Issues
• Are Science Cases Strong Enough?
• Instrument: MOS or Multi-IFS (KMOS-like)?
• Funding
• Grant-in-Aid: 15M max.
• Telescope Modification by NAOJ Budget?
• International Partnership
• Human Resources
• Conflict with Resources for TMT?
• International Collaborations?
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Current Activities and Plans for 2013• Conceptual Study
• Feasibility of WFNIRIMOS• Compatibility with Subaru Telescope Structure
• Opt-Mechanical Design
• GLAO Development Plan• ASM - based on R&D for VLT
• Laser system, WFS, RTC
• More Detailed Simulations for GLAO and Observations
• GLAO Science WS: 2013/6/13-14 in Sapporo
• Internal Review in Summer 2013• Review Points: Scientific Importance, Technical Feasibility, Funding, Consistency with
Overall Roadmap of NAOJ / Subaru Telescope / TMT