a proposal of long slit spectrograph for wso/uv nanjing institute of astronomical optics and...
TRANSCRIPT
A Proposal of Long Slit Spectrograph
for WSO/UV
Nanjing Institute of Astronomical Optics and Technology,National Astronomical Observatory of China, CAS
National WSO/UV Implementation Committee of China
2006-June-28
Zhongwen Hu
Contents
• Team Members Introduction• Requirements and assumption• layout overview of NIAOT LSS • Configurations and performance of LSS • Cooperation Expected• Quotation results of diffraction Gratings• Cross check results of the optics design• Schedule
NIAOT Introduction
• A unique research base in China, specialized in professional astronomical telescopes and instruments – 50 astronomical telescopes and instruments ;
30 exported to the USA, Spain, Japan and South Korea.
• Four main Laboratory– Mirror Technology – Astronomical Spectrum and High Resolution Imaging – Solar Instruments – New Technology Telescope
Team members introduction
• Prof. Yongtian Zhu, director
• Dr. Zhongwen Hu, Optics
• Dr. Yi Chen, FEA
• Ms. Jianing Wang, Electronics
• Mr. Lei Wang, Precision mechanics
Prof. Yongtian Zhu
• Vice Director of NIAOT
• Experience– the Coude Echelle Spectrograph for Chinese
2.16-meter astronomical Telescope– Spectrographs for LAMOST project – Proposed a novel two-mirror system for the so
ft X-ray projection lithograph
• Soft X-ray beamline construction and calibration of a varied angle spherical grating monochromator
(12-120nm)• Echelle spectrograph (200-500nm)• Polychromator ( 31channels) (UV-Visible).
• High precision measurements of grating groove density for VLS concave diffraction gratings (Uncertainty 1x10-5). Especially small curvature radius gratings.
• Expression of groove density (N) and groove function (n) applicable for any gratings
Dr. Zhongwen Hu
Soft x-ray beamline optics
Movements in super high vaccum 3 Gratings could be exchangedGratings rotated to scan wavelengthMirror rotated to compensate defocus
First gas absorption spectrum with resolution 1000
NIAOT contribution to LSS
• Under direction of WIC working group of China• NIAOT responsibilities
– Participate system requirement definition– Design of LSS– Construction of prototype, flight model and test system– Complete instrument level test in China
• Some crosscheck of LSS test in Ukraine ?
– Participate Integration with rest of WSO– Develop Calibration and data reduction methodology
• THE ROWLAND MULTICHANNEL LONG SLIT SPECTROGRAPH FOR THE WSO/UV MISSION ----- R.E. Gershberg ,et.al
• HIRDES Phase A Study -----Dr. Schwarz & Project Team
• Performance of the Long-Slit Spectrograph (LSS) ----V. Terebizh
•
LSS References
New designs of LSS
Possible layouts with various resolution-
wavelength pattern
Optimized space and spectrum resolution with
extended wavelength coverage
Expect better image quality for every point on
slit
Use of special gratings
Diffraction grating typesClassical gratingsVLS concave gratingsHolographic gratings of
the first generationHolographic gratings of
the second generation
How to determine
requirements of the LSS ?
Interactive procedure between science mission
requirements and technology capability and
availability
Performance of the Long-Slit Spectrograph (LSS)
Preliminary results
V. Terebizh, April 2005
Distance of slit from optical axis 10 49.5 mm
Entrance : Width of slit Length of slit
Rectangular: 1 82 m
75 6.2 mm
Coating of surfaces Al + MgF2
Far Ultraviolet (FUV) Near Ultraviolet (NUV)
1150 1775 Å1750 3000 Å
Refl. at 1150 Å ; 1, /3 surfacesat 1216 Å ; 1 , /3 surfacesat 3000 Å ; 1 , /3 surfaces
60 %, / 21 %82 %, / 55 %87 %, / 66 %
LSS optical layout : Modified Rowland-circle spectrograph with one reflection
Dispersive element Curvature radii Light diameter
Concave gratingR1 and R2 ~ 1 m
110 mm
Approximate size 1050 mm 350 mm
Spectral resolution : FUV NUV
2000 30001500 3000
Spectral resolution for stars ~ 5000
Space resolution 0.40”
Number of detectors 2 4
Requirements
baseline of current
NIAOT design
Optical configuration of LSS and Position
313589
52.7
120
450
Spectrometer case LSS
+Z
+Y
60
462
Unit of LSS mounting to the Optical Bench
UV SpectrometerVUV Spectrometer
LSS
Modified Rowland configuration LSS position in the
instrument bay
A layout by R.E. Gershberg et.al(3 detectors and 6 gratings)
Overview of our layout
Three possible layouts are considered:
Layout 1a, Layout 1b, layout2
Each layout is shown with its resolution-wavelength pattern
3 layouts of NIAOT designLayout 1a Detector 1 Detector 2
Resolution 500 1450 5000 5800 5800
Wavelength range(Å)
1100-3500 1150-1655 2000-2370 2360-2710 2700 -3100
Layout 1b Detector 1 Detector 2
Resolution 500 1450 2500 2000
Wavelength range(Å)
1100-3500 1150-1655 1150-1775 1750-3050
Layout 2 Detector 1 Detector 2 Detector 3
Resolution 500 2500 2000 5000 5800 5800
Wavelength range(Å)
1100-3500
1150-1775
1750-3050
2000-2370
2360-2710
2700 -3100
Resolution-Wavelength pattern Layout 1a(5 gratings, 2 detctors)
1000 1500 2000 2500 3000 35000
1000
2000
3000
4000
5000
6000
Re
solu
tion
Wavelength
Very good image across 1100-3500
Two gratings cover 2360-3100
1150-1655
2000-2370
Resolution-Wavelength patternLayout 1b(4 gratings, 2 detctors)
1000 1500 2000 2500 3000 35000
1000
2000
3000
One grating cover 1750-3050
Res
olut
ion
Wavelength
Very good image across 1100-3500
1150-1775
1150-1655
Resolution-Wavelength pattern Layout 2(6 gratings, 3 detctors)
1000 1500 2000 2500 3000 35000
1000
2000
3000
4000
5000
6000
One grating cover 1750-3050Re
solu
tion
Wavelength
Very good image across 1100-3500
Two gratings cover 2360-3100
1150-1775
2000-2370
R.E. Gershberg’s proposal with 3 detectors and 6 gratings
1000 1500 2000 2500 3000 35000
500
1000
1500
2000
2500
3000
3500
4000
4500
5000
5500
6000
Re
solu
tion
Wavelength
Image quality merely acceptable 1200-3400
3 gratings cover 1200-3500
1385-1575 1788-2032
Layout 1a(2 detectors and 5 gratings) Grating
Detector
Configurations and performance
Optical parameters
Image quality
Resolution achieved
Layout parameters for detector 1.R=500
Detector 1Detector size (mm^2)
Pixel size(um^2)
42.1x6.5 25x12
Grating No. 1( Resolution 500) 10( Resolution 1450)
Wavelength range(Å) 1100 ~3500 1150-1655
Incident Angle(deg) 4.176 6.625
Diffraction Angle(deg) -1.6363 0.814
Detector Tilt(deg) 3.39
Incident Length(mm) 897.737
Detector Position(mm) 895.0517
Detector Radius Infinite
Spot diagram on detector 1 with grating 1. Left is the images for different points on 6.2 mm slit within the related wavelength. Right is RMS spot radius which shows good space and spectrum resolution for varied slit positions.
Resolution test
Slit width is 82 microns along spectrum direction space resolution 32 microns along the entrance slit. Gaussian distribution of image on slit with FWHM equals the slit width is assumed.
Layout parameters for detector 2 (1150 Å ~ 3050 Å, two gratings). R=2500
Detector 2 (alternative)
Detector size (mm^2) Pixel size(um^2)
93.5 x6.5 25x12
Grating No. 2 (Resolution 2500) 3 (Resolution 2000)
Wavelength range(Å) 1150~1775 1750~3050
Incident Angle(deg) 12 10.725
Diffraction Angle(deg) 0.1253 -1.1456
Detector Tilt(deg) 8.3755
Incident Length(mm) 1035
Detector Position(mm)
1022
Detector Radius(mm) 1037.832
Layout parameters for detector 3(2000 Å ~ 3500 Å, three gratings). R=5000
Detector 3
Detector size(mm^2)
Pixel size (um^2)
76 x6.5 25x16
Grating No.4
(R= 5000)5
(R= 5800)6
(R= 5800)
Wavelength range(Å) 2000~2370 2360~2710 2700 ~3100
Incident Angle(deg) 21.486 22.982 23
Diffraction Angle(deg)
8.532 10.0267 10.0445
Detector Tilt(deg) 0
Incident Length(mm) 1035
Detector Position(mm)
953.471
Detector Radius(mm) 902.776
Mechanical interface problem
+Z
+YUV SpectrometerVUV Spectrometer
LSS
1.Gratings enter into spaces of UV and VUV chamber--- Space resolution and detector pixel dimension
2.How many detectors mechanically available---with or without folding mirrors?---Interference with FC ?
International cooperation expected
• Detectors– The detector unit (with the High Voltage syste
m) could be supplied by Britain?
• Electronics– Digital process unit provided by Germany?
• other
Detectors available?
– Curved surfacedetector surface could be a flat plane
– Rectangular pixel Square pixel
degraded space resolution,two point sampling
– Maximum available pixels– Mechanical dimensions
Possible vendors of gratings
• Jobin Yvon (France), Bruno Touzet • Spectra-physics (U.S.), Doug Buerkle • Carl Zeiss(Germany), Klaus Heidemann • Shimadzu(Japan), Shinn Takada
Grating has a diameter 115mm. Gratings could be one of the following type.
a. spherical gratings fabrcated by aspheric opticsb. asperical grating available
Grating parameters(Recording wavelength 310nm.)
Grating No.1 2
3 4 56
Tangential Radii
900 1023.2781026.626 987.6782 982.812
982.336
Sagital Radii 895.917 1001.634 1005.007 990.4428 994.145 994.602
Y of P1-
53.4717-217.144
-131.237 178.386 294.7175387.576
Z of P1-
897.115-976.88
-1022.002 -692.005 -1043.679-1043.92
Y of P2 0.1468 244.80492.791 2974.360
52755.836
2577.349
Z of P2-
895.451-1042.999
-1060.278 607.54 -780.765-827.065
Gratings, Reply from Jobin Yvon (France),
– They can make our gratings on a custom substrate• difficult for them to fabricate the toroidal substrate
close to a sphere
– They made their own calculations use the same layout parameters with modified recording wavelength
Comparison (110nm~350nm resolution 500)
---by Jobin Yvon
NIAOT 310nm recording wavelength
Jobin Yvon with a different wavelength
Grating 1 (resolution 500)
Grating 10 (resolution 1450)
Summary of NIAOT design (1)
The incident, the diffracted angles and the positions of
detectors could be tuned to meet the space mechanically
available for LSS
Very good image quality with extended wavelength range
or increased resolution through points along the entrance slit.
Show the possibility to integrates some merits of several
previous designs.
Summary of NIAOT design (2)
For resolution 500 on detector 1
Very good image quality is obtained across wavelength
interval 1100 Å ~ 3500 Å through points on the slit.
No auxiliary reflecting mirror needed in principle.
─It depends on mechanical space available for LSS
Summary of NIAOT design (3)
For resolution ~2500, detector 2
the wavelength range is covered by two gratings like Willem
Wamsteker’s proposal,
yet it has the image quality similar to that described in R.E.
Gershberg’s four gratings mode or double gratings mode with
resolution 1500.
resolution ~5000 on detector 3
Notes
• Optical designs show improvements of the LSS performance.
• Yet it is not the finalized form considering the uncertainties in detectors and science mission requirements.
• System requirements concerning wavelength intervals and their resolution should be to optimized and balanced for newly claimed scientific mission
Schedule
• 2006.02-2007.03: Phase 0+A: Functional Requirements. Feasibility study. Initialization of procurement of component.
• 2006.12-2007.11: Phase B: Requirement specifications, Engineering environment set-up and preliminary design.
• 2007.11-2008.09: Phase C: Detailed design.
• 2008.09~2009.09: Phase D: Production of Flight Model. Ground qualification testing.
• 2009.09~2010.03: Assembling, Integration, and Verification, with the spacecraft.
• 2010.03~2010.09: Pre-launch testing
• 2010.10: Launch
Thank you !