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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



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


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


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



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?


  • 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



Changchun

Urumqi

NAOC

Delingha

PMO

SHAO

YNAO

2005.08.31

7

Xinglong(LAMOST)

Miyun

HuaiRou

Urastai

NIAOT

FAST

Gaomeigu


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



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


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


CASS 2009:new site for small telescopes




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) reserach and developing

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.


Lamost mb with 37 sub mirrors
LAMOST-Mb with 37 sub-mirrors reserach and developing


Lamost ma with 24 sub mirrors
LAMOST-Ma with 24 sub-mirrors reserach and developing


16 low medium resolution spectrographs
16 Low/Medium reserach and developing Resolution 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


Space Solar Telescope (SST) reserach and developing

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“


  • 1 reserach and developing )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


Song china project schedule
SONG-CHINA project schedule reserach and developing


  • May 2010 reserach and developing : 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 ! reserach and developing


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