AST 3 NIR camera for the AST 3

AST 3 -NIR camera for the AST 3 -3 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 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.

Outside Scope

Systems • Subsystem architecture (high-level) developed for cost model CRYOSTAT OPTOMECHANICS DETECTOR & CONTROLLER CONTROL SYSTEM SOFTWARE TELESCOPE INTERFACE PLATO INTERFACE • Requirements under development: available for review soon • System model and ETC under development

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

Telescope configuration • AST 3 -3 is an upgraded version of AST 3 -1 and AST 3 -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)

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’x 45’ for HR 2 G or 23’x 23’ H 1 RG – 1. 13”/pixel (Selex) giving 19’x 24’ 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)

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

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

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)

Detector/controller: Teledyne • H 2 RG with 1 kx 1 k 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

Detector/controller: Selex ES • Selex ES have developed 1 kx 1 k device under contract from ESA – now working on 2 kx 2 k 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