for the AST33 telescope for the Kunlun Infrared Sky Survey KISS Progress Meeting Jon Lawrence 14 August 2015 Project Aims and Objectives Project Personnel Project Roles Jeremy Mould SUT as Lead Investigator ID: 602703
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Slide1
AST3-NIR camera for the AST3-3 telescope for the Kunlun Infrared Sky Survey (KISS)
Progress MeetingJon Lawrence14 August 2015Slide2
Project Aims and ObjectivesSlide3
Project PersonnelProject RolesJeremy Mould (SUT) as Lead Investigator
TBD (SUT) as TBDJon Lawrence (AAO) as Project LeaderJulia Tims (AAO) as Project ManagerNick Staszak (AAO) as Project EngineerJessica Zheng (AAO) as Instrument ScientistVlad Churilov
(AAO) as Mechanical EngineerRoss Zhelem
(AAO) as Optical EngineerNaveen Pai (AAO) as Mechanical Technician Slavko Mali/Rolf Muller (AAO) as Electronics Technician
Don Mayfield (AAO) as Detector Engineer (TBD)TBD (AAO/UNSW) as Electronics EngineerMichael
Ashley (UNSW) as Control System LeadXiangyan Yuan (NIAOT) as Telescope Lead Scientist
LIEF proposal investigatorsJeremy Mould (SUT) as Lead Investigator
Karl Glazebrook (SUT) as Chief InvestigatorMichael Ashley (UNSW) as Chief Investigator
Michael Burton (UNSW) as Chief Investigator
Lifan
Wang (PMO/TAMU) as Partner Investigator
Anna Moore (CIT) as Partner Investigator
Jon Lawrence (AAO) as Partner Investigator
Peter
Tuthill
(
USyd
) as Chief Investigator
Mike Ireland (ANU) as Chief Investigator.Slide4
Outside ScopeSlide5
CRYOSTAT
Systems
Requirements under development: available for review soon
System model and ETC under development
TELESCOPE INTERFACE
PLATO INTERFACE
DETECTOR
& CONTROLLER
OPTO-MECHANICS
CONTROL SYSTEM
SOFTWARE
Subsystem architecture (high-level) developed for cost modelSlide6
Design trades
Telescope
configuration
Pixel scale
Filter bandwidth
Optical design
Instrument interface
Detector/controllerSlide7
Telescope configuration
AST3-3 is an upgraded version of AST3-1 and AST3-2 deployed to Dome A in 2012/2015.
Telescope intended for wide field optical camera – no longer requirement (TBC)
Optical prescription fixed (mirrors already fabricated)
Mechanical design mostly fixed (parts under construction)
ITO front window for de-icing – baseline for first season unless proved
uneccessarySlide8
Pixel scale
Total FHWM =1.2 - 3”
Diffraction limit ~1”
Optics ~0.6”
Seeing
0.2”-
2.5
” (is 0.3”-3.3” @0.5 micron)
Current design
1.35
”/pixel (Teledyne) giving 45’x45’ for HR2G or 23’x23’
H1RG
1.13
”/pixel (Selex) giving 19’x24’ per
chip
~1 pixel per FWHM in best seeing conditions
~2 pixels per FWHM in worst seeing conditions
A
rgument
can be made to re-optimise for median seeing conditions and for wide field (ie survey speed) Slide9
Filter bandwidth
Bandwidth to be
optimised
based on SNR
OH lines at short end have uncertain intensity
Red end should be predictable via atmospheric model
Peter
Tuthill
et al. investigatingSlide10
Optical design
Modelling shows cold stop is required due to complexity of
narcissis
mirror approach
Optical design flows from pixel scale and FOV and telescope optics
Mirror folded due to space constraints
Flat cryostat window to simplify alignment
Design has 4 powered lenses with 1 aspheric surfaceSlide11
Instrument Interface
Interface required for telescope
Cryostat design flows from telescope constraints and optical design:
Internal focus drive
Folded layout
No requirement on filter changer
No requirement on shutter (TBC)Slide12
Detector/controller: Teledyne
H2RG with 1kx1k contiguous region now baseline
Controller is SIDECAR ASIC
Detector mount plate available from GL Scientific
ITAR license still unknown
Could be issue with cut-off wavelengthSlide13
Detector/controller: Selex ES
Selex ES have developed 1kx1k device under contract from ESA – now working on 2kx2k device but wont be ready in time
Integrated controller under development at
Caeleste
but not ready yet
Selex ES do chip development and packaging, UKATC responsible for
characterisation
UKATC could provide leach controller under subcontract
Mosaic possible with mods to assembly board