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Progress of the Chinese SONG Nodes Xiaojun Jiang, Fei Zhao National Astronomical Observatories,...
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Progress of the Chinese SONG Nodes
Xiaojun Jiang, Fei Zhao
National Astronomical Observatories, Chinese Academy of Sciences
2010.03
• Overview of Chinese standard and
customized nodes
• A preliminary design review
• Site information
• Candidate manufacturer(s)
• Project schedule
Overview of Chinese nodesOverview of Chinese nodes
• Two nodes: Standard & Customized
• Chinese Standard SONG Node - Original SONG node + Wide Field 3-color Photometer
• Why a customized node? - General purpose photometric telescope - Monitoring of variable objects
- Ground follow-up observations
- Participating observing campaigns and SONG’s microlensing program
Why a customized node? (ctd.)
Chinese Standard Node
• Aperture : 1m
• Alt-Az
• Classic Cassegrain
• 2 Nasmyth platforms
① Lucky imaging
② HRS + 3-color photometer
• M1 & M2 make an F/37 beam– ~f/6.1 reducer, offers15’x15’ FOV
• Pointing precision : 5” RMS
• Pointing speed : 20°/s Max
• Dome: Φ ≈5.5m
Standard Node - Standard Node - NasmythNasmyth platform 1platform 1
– to lucky imager• F/37 • ADC + optical derotator• Focus monitor• WL split @650nm for
vis/red cameras
Standard Node - Standard Node - NasmythNasmyth platform 2platform 2
– 3-color photometer• split by a folding mirror (M4) with central hole• F/37 – F/6.1 reducer• monitoring field stars around central target by using the 3-color photometer w/ 15’x15’ • 3-color: B 、 V 、 R• iKon-L 936: 2048*2048 (13um)• Mechanical derotator
– HRS• as per standard SONG HRS design
Standard node: 3-color photometer
• FOV :≧ 15’ x 15’
• Focal length≦ 6100mm w/ reducer
• Image quality:Encircled energy (80%)
diameter : Ф40micron (each of the BVR bands)
40micron corresponding to FOV of 1.4” @ F=6100mm
Ovserview of Chinese
Customized Node• 1m, Alt-Az mount
• M1 & M2 make a F/37 beam
• M2& M3 offer a 24’x24’ FOV
• two Nasmyth platforms
① Lucky imager (Same as the Std node)
② CCD photometer with 24’x24’ FOV
• Pointing precision :5”RMS
• Pointing speed : 20°/s Max
• Dome: Φ ≈5.5m
Inner surface of each port between detector and M3
stray light stops
Inner surfaces of the M2&M3 baffle ,Upside of the M1 aperture stop
knife-edged vanes
Surfaces of baffles and M1 enclosure that can be seen by the detector directly
Enhanced black paint
Stray Light control
Optical Design review Optical Design review
• Achieved diffraction limit ( λ/20RMS @633nm ) over Φ6’ FOV with classic Cassegerain design – satisfy the requirement of LI
• Difficulties:
– High-power reducers for both nodes: two
solutions
– Layout of 3-color photometer for standard
node: compromise or not?
High-power reducer: solution 1• 6 elements in 6 groups
• Max clear dia. 194mm (dense crown)
• BFD: 35mm from the rear surface (need to be optimized)
• Fits customized node after optimization
Vignetting less than 30% on the F/6.1 image
High-power reducer: solution 2 Re-image Focal ReducerRe-image Focal Reducer
Intermediate focal plane(Field stop)
Intermediate pupil image(Lyot stop)
Prism as beam splitter(Options for multi -channel photometry)
D=1010
Re-image Focal ReducerRe-image Focal Reducer--F/37 to F/6.1
D=1010
Intermediate focal plane (Field stop)
Folding mirror with central hole
Prism as beam splitter(for multi-channel photometry)
Intermediate pupil image (Lyot stop)
Re-image Focal ReducerRe-image Focal Reducer--F/37 to F/6.1
Sumarry of re-image focal reducer
9 lens in 9 groups
Front lens Φ=192mm, Dense Crown glass
Lens after that:
aperture diameters less than 110mm
Dense Crown and Dense flint glasses
BFD 146mm
80% energy within Φ40um (FOV 15’x15’) in V band
Transmittance will be decreased by ≈30%
3-color photometer’s layout is a critical issue
Summary of preliminary optical designSummary of preliminary optical design
• Optical quality of M1 + M2 meets the requirement of Lucky imaging;
• The design of F/37-to-F/6 reducers for both nodes are feasible, but need further optimization;
• Optical layout of the 3-color photometer in the standard node is a tough job, may need make compromise with astronomers – use 2-color or give up the simultaneity
Site Information in ChinaSite Information in China
2005.08.31 7
Delingha
Urumqi
YNAO
SHAO
Changchun
NAOC
PMO
Xinglong(LAMOST)Miyun HuaiRou
NIAOT
Urastai
FASTGaomeigu
Site information in China
Distribution of clear nightsDistribution of clear nightsGMS + NOAA 1996 -2003, J. Mao et al 2004
Cloud distribution at 2:00BJTCloud distribution at 2:00BJTCMA 2425 stations 1961-2008, Y. Zhang et al
High Vast LandClean Dilute AirLess cloudyCold, DryDark, Quiet
Light pollutionLight pollution
2005.04 Karasu, Xinjiang2005.04 Karasu, Xinjiang
2005.08 Oma, Tibet2005.08 Oma, Tibet
Oma: Oma: N32 32 E83 03, 5100mN32 32 E83 03, 5100m
Karasu: Karasu: N38 10 E74 48, 4500mN38 10 E74 48, 4500m
Oma 5000mOma 5000mKarasu 4500mKarasu 4500m
Site Survey carried out by NAOC
⊙⊙⊙
⊙⊙
⊙⊙
喀什
叶城
物玛阿里
措勤
卡拉苏
拉萨↙↙
airport &train station
↙↙
airport &train station
Kashi-Karasu : 190km ~ 2 hr Oma -Lhasa: 1000km ~ 2 days
airport @2010airport @2010
DIMM seeing DIMM seeing domedome
10m10m tower tower weather stationweather station
40 m CT2 tower40 m CT2 tower
2007.10 Karasu2007.10 Karasu
MIR cloud MIR cloud monitormonitorSBIG seeing SBIG seeing
monitormonitor
SBIG cloud SBIG cloud monitormonitor
Instrument setup & campaignInstrument setup & campaign
40 m CT2 tower40 m CT2 tower
DIMM seeing DIMM seeing domedome
weather station weather station 10m10m towertower
4.5 m antenna 4.5 m antenna Satellite communication Satellite communication
2008.11 Oma Site2008.11 Oma Site
SBIG seeing SBIG seeing monitormonitor
MIR cloud MIR cloud monitormonitor
Renewal Renewal power supplypower supply
CASS CASS 20092009 :: new site for small telescopesnew site for small telescopes
Candidate ManufacturersCandidate Manufacturersin Chinain China
• Nanjing Institute of Astronomical Optics &
Technology (NIAOT)
• Nanjing Astronomical instruments Co.,Ltd
(NAIRC)
• Shanghai Astronomical Observatory (SHAO)
• Changchun Institute of Optics, Fine Mechanics
and Physics (CIOMP)
• Institute of Optics and Electronics (IOE)
• NIAOT is the unique institute in China specialized in reserach and developing astronomical technology, professional astronomical telescopes and instruments.
• Major Projects Involved– LAMOST– FAST– SST– Antarctic Telescopes
Large sky Area Multi Objects Spectra Telescope (LAMOST)Large sky Area Multi Objects Spectra Telescope (LAMOST)
LAMOST is a quasi-meridian reflecting Schmidt telescope laid down on the ground with it’s optical axis fixed in the meridian plane. The effective aperture of LAMOST is 4m. It’s focal plane is 1.75m in diameter, corresponding to a 5 degree field of view, may accommodate as many as 4000 optical fibers. So the light from 4000 celestial objects will be led into 16 spectrographs.
LAMOST-Mb with 37 sub-mirrorsLAMOST-Mb with 37 sub-mirrors
LAMOST-Ma with 24 sub-mirrorsLAMOST-Ma with 24 sub-mirrors
16 Low/Medium16 Low/MediumResolution Resolution
Spectrographs Spectrographs RL = 1000/2000
RM= 5000/10000
4kx4k CCD, 12μ/pixelVPHG (Wasach optics )
Spectral range:
Low blue: 370—590nm
red: 570—900nm
Medium blue: 510nm — 540nm
red: 830nm — 890nm
First of 16 LRS
Space Solar Telescope (SST)Space Solar Telescope (SST)
Main charactersMain characters::0.1" 0.1" 0.15" space resolution for vector 0.15" space resolution for vector magnetic field and velocity field etc.magnetic field and velocity field etc.2D spectrograph2D spectrographmagnetic analyzer with accuracy ~ 10-4 magnetic analyzer with accuracy ~ 10-4 0.5" soft X-ray images at 4 bands 0.5" soft X-ray images at 4 bands simultaneouslysimultaneously
Optical design:Optical design: Diameter: 1 M; Diameter: 1 M; Focal rate : 3.5 to 1, Focal rate : 3.5 to 1, FoV : 2.8 ' x 1.5 ', FoV : 2.8 ' x 1.5 ', Diffraction limit: Diffraction limit: 0.1"0.1"—— 0.15 0.15““
1 ) tube material : INVAR-362) Tube sealed and filled with dry nitrogen3) Tilted window with ITO (snow-removing and deicing)4) Special damping structure for safe transportation
SONG-CHINA project schedule
• May 2010: finish preliminary design of both nodes
• December 2010: past design review ,place order of the
telescopes/instruments
• December 2011: finish site-testing
• April 2012: start construction of enclosures/control rooms
• December 2012 : finish on-site installation and past
acceptance tests, engineering runs
• April 2013: science operations
Thank You !Thank You !