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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.

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progress of the chinese song nodes

Progress of the Chinese SONG Nodes

Xiaojun Jiang, Fei Zhao

National Astronomical Observatories, Chinese Academy of Sciences

2010.03

slide2
Overview of Chinese standard and customized nodes
  • A preliminary design review
  • Site information
  • Candidate manufacturer(s)
  • Project schedule
overview of chinese nodes
Overview 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
slide4

Why a customized node? (ctd.)

- Ground follow-up observations

- Participating observing campaigns and SONG’s microlensing program

chinese standard node
Chinese Standard Node
  • Aperture:1m
  • Alt-Az
  • Classic Cassegrain
  • 2Nasmythplatforms
    • Lucky imaging
    • 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 nasmyth platform 1
Standard Node - Nasmythplatform 1
  • to lucky imager
    • F/37
    • ADC + optical derotator
    • Focus monitor
    • WL split @650nm for vis/red cameras
standard node nasmyth platform 2
Standard Node - Nasmythplatform 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
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
Ovserview of Chinese Customized Node
  • 1m, Alt-Az mount
  • M1 & M2 make a F/37 beam
  • M2& M3 offer a 24’x24’ FOV
  • two Nasmythplatforms
    • Lucky imager (Same as the Std node)
    • CCD photometer with 24’x24’ FOV
  • Pointing precision:5”RMS
  • Pointing speed :20°/s Max
  • Dome: Φ ≈5.5m
slide10

Stray Light control

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

slide12

Achieved diffraction limit(λ/20RMS @633nm)over Φ6’ FOV with classic Cassegerain design – satisfy the requirement of LI

slide13
Difficulties:
    • High-power reducers for both nodes: two solutions
    • Layout of 3-color photometer for standard node: compromise or not?
slide14

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
high power reducer solution 2 re image focal reducer
High-power reducer: solution 2Re-image Focal Reducer

Intermediate pupil image

(Lyot stop)

Prism as beam splitter

(Options for multi -channel photometry)

Intermediate focal plane

(Field stop)

D=1010

re image focal reducer
Re-image Focal Reducer

Re-image Focal Reducer

--F/37 to F/6.1

--F/37 to F/6.1

Intermediate pupil image (Lyot stop)

Prism as beam splitter

(for multi-channel photometry)

D=1010

Intermediate focal plane (Field stop)

Folding mirror with central hole

sumarry of re image focal reducer
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 design
Summary 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
slide23

Changchun

Urumqi

NAOC

Delingha

PMO

SHAO

YNAO

2005.08.31

7

Xinglong(LAMOST)

Miyun

HuaiRou

Urastai

NIAOT

FAST

Gaomeigu

slide24

Site information in China

High Vast Land

Clean Dilute Air

Less cloudy

Cold, Dry

Dark, Quiet

Cloud distribution at 2:00BJT

CMA 2425 stations 1961-2008, Y. Zhang et al

Distribution of clear nights

GMS + NOAA 1996 -2003, J. Mao et al 2004

slide26

Karasu: N38 10 E74 48, 4500m

2005.04 Karasu, Xinjiang

airport &

train station

Kashi-Karasu : 190km ~ 2 hr

Oma -Lhasa: 1000km ~ 2 days

喀什

Oma 5000m

Karasu 4500m

卡拉苏

Oma: N32 32 E83 03, 5100m

叶城

airport &

train station

2005.08 Oma, Tibet

物玛

阿里

airport @2010

措勤

拉萨

Site Survey carried out by NAOC

slide27

2007.10 Karasu

2008.11 Oma Site

40 m CT2 tower

10mtower

weather station

DIMM seeing

dome

40 m CT2 tower

4.5 m antenna

Satellite communication

weather station

10mtower

DIMM seeing

dome

MIR cloud

monitor

MIR cloud

monitor

SBIG seeing

monitor

SBIG cloud

monitor

SBIG seeing

monitor

Renewal power supply

Instrument setup & campaign

slide30
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)
slide31
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

slide32

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. Theeffective 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.

16 low medium resolution spectrographs
16 Low/MediumResolution Spectrographs

RL = 1000/2000

RM= 5000/10000

4kx4k CCD, 12μ/pixel

VPHG (Wasach optics )

First of 16 LRS

Spectral range:

Low blue: 370—590nm

red: 570—900nm

Medium blue: 510nm — 540nm

red: 830nm — 890nm

slide36

Space Solar Telescope (SST)

Main characters:

0.1"  0.15" space resolution for vector magnetic field and velocity field etc.

2D spectrograph

magnetic analyzer with accuracy ~ 10-4

0.5" soft X-ray images at 4 bands simultaneously

Optical design:

Diameter: 1 M;

Focal rate : 3.5 to 1,

FoV : 2.8 \' x 1.5 \',

Diffraction limit:

0.1"— 0.15“

slide37

1)tube material:INVAR-36

  • Tube sealed and filled with dry nitrogen
  • Tilted window with ITO (snow-removing and deicing)
  • Special damping structure for safe transportation
slide39
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
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