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Visible SpectroPolarimeter (ViSP)SWG Meeting Nov. 24, 2010
R. Casini with P. Nelson, A. de Wijn, M. Knölker,
and P. Huang
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ViSP Science Justifications
Science Case: to study the emergence, evolution, and decay of magnetic flux in the solar atmosphere, and the dynamics of solar atmospheric structures
Examples: • formation and decay of active regions• smallscale evolution of quietSun magnetism• magnetic stability of prominences and filaments• magnetic structure of flare and CME precursors• plasma oscillations in the photosphere and chromosphere• kinetic studies of filament eruption• spicules• deposition of mass and kinetic energy from the lower solar atmosphere into
the corona
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ViSP Science Justifications
Methodology: • spectropolarimetric observations of magnetic regions• plasma dynamics from Doppler shifts of spectral lines• modeling of polarized line formation (Zeeman effect; atomic polarization;
radiative transfer in inhomogeneous media; radiationMHD simulations)
Requirements: • Highsensitivity, highcadence (not necessarily simultaneous) spectro
polarimetry• multiple spectral lines simultaneously (improve magnetic inference; sample
different atmospheric heights)• high spatial resolution, 2D maps of solar regions• high spectral resolution
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• Wavelength range: 380 – 900 nm, three lines simultaneously• Spatial resolution: 2£ ATST diffraction limit (0.07 arcsec @ 630nm)• Spatial FOV: 2£2 a rcmin2 [camera format may limit further]• Spectral Resolution: 3.5 pm @ 630 nm (< 1.7 km/s) → R ~ 180,000• Polarimetric Capability: 103 Icont polarimetry in 10 sec @ required
spectral/spatial res. [may not be possible over entire spectral range in all cases]• Simultaneous operation with:
— Visible Broadband Imager (VBI)— DiffractionLimited NearIR SpectroPolarimeter (DLNIRSP)— Visible Tunable Filter (VTF)
[no spectral overlap unless light from slitjaw is “recycled”]
ViSP Science Requirements
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1) Continuous spectral coverage from 380 to 1100 nm2) Meets FOV and spatial resolution requirements [slit height to width is ~4,000:1!]3) Low order gratings (m < 20) allow for large free spectral range:
– observation of wide lines like Ca II H & K, Hα, Ca II IR Triplet [full capability requires 2K px spectral coverage per beam]– observation of multiple lines at different βangles with scientifically useful
spectrograph efficiencies [strongly dependent on grating choice]– reasonable number (~12) of order isolation filters to observe any line from
380 to 1100 nm [filters are relatively inexpensive: ~ 5 K$]4) Multiple gratings (3 to 5) to ensure wavelength diversity with good spectrograph
efficiency [may require custom gratings and associate design effort]5) Automated reconfiguration [a few minutes for three lines]6) Library of photoetched slits [3 provided at first light, corresponding to diffr. limit
@ 450, 650, and 850 nm (respectively: ~16, 23, and 30 µm)]7) Multislit compatible design
ViSP DesignEssential Features
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ViSP Optical Concept
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ViSP Mechanical Overview
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ViSP Table
M8 OAP
M10 DM
BS1
BS2BS3
FM1
Con
text
Cam
Tab
l e
D-K Feed Telescope
(f=7m, F/35)
Context Cam Lens
Collimator Lens
GratingSlit
Counter Scanner
Cam3
Cam2
Cam1
CC
Cam LensPA
ATSTViSP Layout Overview
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From slit
Air-gapped doublet collimator lens (f=2.6m, F/26)
Counter scanning fold mirrors
Air-gapped triplet camera lens1 (f=0.85m) Conic 1st surface
Order sorting filter
ProFlux polarization beam
splitter
FMCMOS detector array
Combiner prism
Collimator/Camera #1Detailed View
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Typical Wavelength Selection(from SWG Use Cases)
Prominences 587.6 He I (D3) 656.3 Hα 854.2 Ca II1083.0 He I
AR Filaments 630.2 Fe I 656.3 854.21083.0
Photo/Chromosphere 517.3 Mg I (b2) 630.2 656.3 849.8 Ca II 854.21083.0
Photosphere517.3525.0 Fe I553.8 Mn I630.2
Weak Fields453.6 Ti I455.4 Ba II460.7 Sr I589.0 Na I (D2)589.6 Na I (D1)
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Other lines of interestOther lines of interest(accessible with versatile gratings in at least one of the beams)
...and more lines, as science and diagnostic capabilities improvebetween now and ATST first light
393.3 Ca II (K)396.8 Ca II (H)486.1 Hβ518.4 Mg I (b1)
617.3 Fe I676.8 Ni I769.9 K I849.8 Ca II
866.2 Ca II 874.1 Mn I1526.0 Mn I1565.0 Fe I
Typical Wavelength Selection(from SWG Use Cases)
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Wavelength Selection(from SWG Use Cases)
Prominences 587.6 He I (D3) 656.3 Hα 854.2 Ca II1083.0 He I
AR Filaments 630.2 Fe I 656.3 854.21083.0
Photo/Chromosphere 517.3 Mg I (b2) 630.2630.2 656.3 849.8849.8 Ca II 854.2854.21083.01083.0
Photosphere517.3525.0 Fe I553.8 Mn I630.2
Weak Fields453.6 Ti I455.4 Ba II460.7 Sr I589.0 Na I (D2)589.6 Na I (D1)
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Multiple Gratings for Spectral Diversity
Newport RGL53*451E316 l/mm63° blaze
204£408 mm2
α = 71.9°β−α=(29.9°,3.6°)
Scalar Efficienciescalculation
600 650 700 750 800 850 900 950 1000 1050 1100
0
0.05
0.1
0.15
0.2
0.25
0.3
0.35
0.4
0.45
0.5
Wavelength vs Order for a Fixed Alpha
5 6 7 8 9 10 11 12 13 14
Wavelength, nm
Esti
ma
ted
Eff
icie
nc
y
0 10 20 30 40 50 60 70 80 90 100
0
0.05
0.1
0.15
0.2
0.25
0.3
0.35
0.4
0.45
0.5
Estimated Efficiency vs. Order
5 6 7 8 9 10 11 12 13 14
Beta
Esti
mat
ed
Eff
icie
ncy
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Multiple Gratings for Spectral Diversity
TE & TM Efficiencieswith MRCWA
(Rathgen 2008)
Newport RGL53*451E316 l/mm63° blaze
204£408 mm2
α = 71.9°β−α=(29.9°,3.6°)
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ViSP Grating Optimization
Iterative search ofoptimal gratings
(both stockand custom)
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Prominence Use Case Grating: 254.8 l/mm, blaze = 67.2˚, = 68.7˚α
Wavelength (nm) Diffr. Order ( )˚α β Approx. Efficiency
He I D3 587.6 12 8.8 0.61
Ha 656.3 11 3.5 0.58
Ca II 854.2 8 14.7 0.55
He I 1083.0 6 22.3 0.59
AR Filament Use Case Grating: 305.6 l/mm, blaze = 67.8˚, = 67.8˚α
Wavelength (nm) Diffr. Order ( )˚α β Approx. Efficiency
Fe I 630.2 9 14.0 0.57
Ha 656.3 9 6.3 0.61
Ca II 854.2 7 3.5 0.57
He I 1083.0 5 21.0 0.62
Photo/Chromosphere Use Case Grating: 301.5 l/mm, blaze = 58.3˚, = 65.5˚α
Wavelength (nm) Diffr. Order ( )˚α β Approx. Efficiency
Mg I b2 517.3 11 11.9 0.48
Fe I 630.2 9 12.4 0.48
Ca II 849.8 7 3.5 0.34
Ca II 854.2 6 26.1 0.34
He I 1083.0 5 19.3 0.57
ViSP Grating Optimization
Some use cases, and corresponding optimized custom gratings(not closed; gratings still untested for TE/TM efficiency)
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Some Examples ofViSP Configurability
Prominence Use Case – Grating: 213.3 l/mm, blaze = 61.7˚, = 67.4˚α
Ha 656.3
He I D3 587.6
He I 1083.0
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Some Examples ofViSP Configurability
AR Filament Use Case – Grating: 305.6 l/mm, blaze = 67.8˚, = 67.8˚α
He I 1083.0
Fe I 630.2
Ca II 854.2
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Some Examples ofViSP Configurability
Photo/Chromosphere Use Case – Grating: 267.4 l/mm, blaze = 60.3˚, = 67.2˚α
Ca II 854.2
Ca II 849.8
Fe I 630.2
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Air-gapped triplet context camera lens
(f=0.51m, M=0.16)
Conic 1st surface
Bandpass filter at exit pupil
CMOS detector array
From BS3FM1
Feed-M2
Context CameraDetailed View
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Center
Slit end
FOV right edge
FOV right corner FOV left corner
FOV left edge
Context CameraOptical Performance
Airy disk@ 630 nm
5 pi
xels
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Spectrograph Ch1Optical Performance (NIR)
F = 0.85 m
Center
Slit end
FOV right edge
FOV right corner FOV left corner
FOV left edge5
pixe
ls
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Spectrograph Ch1Optical Performance (Vis)
F = 0.85 m
Center
Slit end
FOV right edge
FOV right corner FOV left corner
FOV left edge5
pixe
ls
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Spectrograph Ch1Optical Performance (UV)
F = 0.85 m
Center
Slit end
FOV right edge
FOV right corner FOV left corner
FOV left edge5
pixe
ls
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Spectrograph Ch2Optical Performance (NIR)
F = 1.10 m
Center
Slit end
FOV right edge
FOV right corner FOV left corner
FOV left edge5
pixe
ls
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Spectrograph Ch2Optical Performance (Vis)
F = 1.10 m
Center
Slit end
FOV right edge
FOV right corner FOV left corner
FOV left edge5
pixe
ls
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Spectrograph Ch2Optical Performance (UV)
F = 1.10 m
Center
Slit end
FOV right edge
FOV right corner FOV left corner
FOV left edge5
pixe
ls
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Spectrograph Ch3Optical Performance (NIR)
F = 1.40 m
Center
Slit end
FOV right edge
FOV right corner FOV left corner
FOV left edge5
pixe
ls
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Spectrograph Ch3Optical Performance (Vis)
F = 1.40 m
Center
Slit end
FOV right edge
FOV right corner FOV left corner
FOV left edge5
pixe
ls
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Spectrograph Ch3Optical Performance (UV)
F = 1.40 m
Center
Slit end
FOV right edge
FOV right corner FOV left corner
FOV left edge5
pixe
ls
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• ViSP design meets or exceeds science requirements:– Continuous wavelength coverage over 380 – 1100 nm– Good spectrograph efficiency over entire spectral range
(needs multiple, and likely custom, gratings)– Spatial, spectral resolution, FOV requirements met (camera
format my limit the FOV further)– Quickly reconfigurable– Multislit compatible
• Design is well understood and is relatively low risk – Design heritage from ASP/SPINOR
ViSP Instrument Summary