1. AST3-NIR camera for the AST3-3 telescope for the Kunlun Infrared Sky Survey (KISS) Progress Meeting Jon Lawrence 14 August 2015

2. Project Aims and Objectives

3. Project Personnel Project Roles Jeremy Mould (SUT) as Lead Investigator TBD (SUT) as TBD Jon Lawrence (AAO) as Project Leader Julia Tims (AAO) as Project Manager Nick Staszak (AAO) as Project Engineer Jessica Zheng (AAO) as Instrument Scientist Vlad Churilov (AAO) as Mechanical Engineer Ross Zhelem (AAO) as Optical Engineer Naveen 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 Engineer Michael Ashley (UNSW) as Control System Lead Xiangyan Yuan (NIAOT) as Telescope Lead Scientist LIEF proposal investigators Jeremy Mould (SUT) as Lead Investigator Karl Glazebrook (SUT) as Chief Investigator Michael 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.

4. Outside Scope

5. 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 model

6. Design trades Telescope configuration Pixel scale Filter bandwidth Optical design Instrument interface Detector/controller

7. 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 uneccessary

8. 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 Argument can be made to re-optimise for median seeing conditions and for wide field (ie survey speed)

9. 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. investigating

10. 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 surface

11. 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)

12. 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 wavelength

13. 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