Detector Control for the ELT (and the VLT) What we are doing and why?

Transcription

1 Detector Control for the ELT (and the VLT) What we are doing and why? Derek Ives, Leander Mehrgan, Javier Reyes and Gert Finger Pasadena 2015

2 ELT and VLT Detector Requirements Science Detectors AO Detectors CCDs/CMOS NIR (TIS - H2RGs, H4RGs, RVS, SELEX, Other) MIR (H4RGs AQUARIUS) CCDs/CMOS (L3CCDs and NGSD) NIR (SAPHIRA) 2

3 Requirements for Detector controllers Generic system able to support all detector types Bias voltages, large range, 3.3V for CMOS but 12V clocks or 100V biases for CCD Output pixel rates, 50 khz for CCDs, 10 MHz for AOCCD, 3 MHz for MIR, 10 MHz for AONIR Driving mosaics of detectors up to 16 4kx4k NIR arrays for ELT instrument Asynchronous clocking of different detectors (with master synch) (HiPERCAM, 5 x FTCCDs, asynchronously clocked) 64 high speed outputs at 3 MHz pixel rates for some MIR detectors Multiple clocks with highest time resolution (10ns) Real time Fowler/NDR/sub-pixel sampling for AO systems 3

4 Example detectors - CCDs LBNL large format, high resistivity CCDs Vsub ~ 115V for fully depleted 1 uf parallel capacitance 12V clock swing 3 MHz operation 19 clocks 16 video channels Lowest noise requirements Space and temperature constraints Other 4

5 Example Detectors - NIR SELEX SAPHIRA detector for AO 32 outputs (10 MHz) Variable bias voltage/variable avalanche gain Fowler/sub-pixel sampling used, real time processing Sub-windowing programming/readout Teledyne H4RG 66 outputs 100 khz, low noise/5 MHz high speed Sub-windowing programming/readout >1Gbit data rates required 5

6 Example mid-ir detectors - AQUARIUS 64 outputs Operation a 6 K 3 MHz pixel rates 150 Hz frame rates 300 Mbytes/s data rates 5.5V clock levels 7.5V video signal 6

7 Specific Science Instruments ELT first light instruments HARMONI 4 x (2 x 4kx4k NIR) + 4 x (2 x 4kx4k CCDs) MICADO 9-16 x (4kx4k NIR) METIS 1 x 4kx4k (5um) and 1-2 AQUARIUS (1kx1k 10um) HARMONI 7 MICADO

8 VLT next generation instruments MOONS 4 of 4kx4k NIR detectors + 2 of 4kx4k CCDs 4MOST multiple large CCDs (9 of 6kx6k) 8 MOONS

9 Other controller requirements Operation of and synchronization with external shutters Synchronisation of multiple systems to master clock level Operation and synchronization with external choppers (secondary mirror) Commonality across platforms for all detector types, including AO Interfacing to Observatory Control System and Detector controller software (~ 500k lines of software) Operation with external GPS systems Gain and Bandwidth switching 9

10 Controller options for observatory detector control ASICS SIDECAR from TIS IDEAS (Norway) low background version for ESA Commercial Controllers Astro-cam generic for IR or CCD Many CCD/CMOS camera companies, Andor, PCO, STA, IR Labs In-house controller development IRACE for IR, FIERA for CCD Now NGC for all detector types, CCD, CMOS, NIR, MIR etc 10

11 ASIC developments TIS SIDECAR Matches H2RG Good heritage NIRCA Development for ESA 5 inputs with 12 bit ADCs SPI or 8b/10b outputs Cryogenic and radiation hard operation Possibility of future ESO collaboration 11

12 ASICs concerns Not generic, well matched to TIS H*RG family, but not to other detectors from other companies and other detector technology For CCDs, interface circuitry required, but not operational cryogenically Controller/Detector expertise would be lost to ESO Off the shelf cost similar to controller cost Development costs for new ASIC too high for ESO (1-2M Euro minimum) Development cycle time may be too long as well ASIC development risk is high, especially if designing a generic device. In-house electronics effort still required to build test equipment for new ASIC If using ASICs for one detector type and controller for another then support issues, team still required for controllers etc. > 20 year support cycle required 12

13 Integrated Camera Controllers STA Controller ASTROCAM Controller ANDOR controller/camera PCO controller/camera 13

14 Commercial controller Not one generic commercial controller to meet all different detector needs Astro-cam (SDSU) controller now old technology and slow fibre links Loads of good CCD/CMOS integrate camera systems but no IR 20 year support cycle required (Already had issues with commercial camera systems no longer supported) Integrated controllers not useful for IR detectors where detector is at 40K and camera electronics is at RT ESO use cryogenic preamps to solve this 14

15 IRACE, InfraRed Array Control Electronics First light with ISAAC in From 1998 to 2008 IRACE was the ESO standard controller for InfraRed application. This controller was based on Transputer processors. gigabit fiber for data low speed fiber for command

16 FIERA, Fast Imager Electronic Readout Assembly From 1998 to 2008 FIERA was the ESO standard controller for Optical application. This controller was based on DSP processors. FIERA 16 output video channels for NAOS chip

17 FIERA and IRACE are still used by many instruments at ESO telescopes Using IRACE controller Using FIERA controller ISAAC CONICA CRIRES HAWK-I UVES NACO S GIRAFFE SOFI SINFONI VISIR FINITO X-SHOOTER FORS EMMI IRIS PRIMA VINCI VIMOS OmegaCAM X-SHOOTER VISTA

18 ESO detector controller Both controllers have been extremely successful, but various limitations, e.g.: mass (OmegaCAM: ¼ ton), volume, heat dissipation obsolete components voltage range and swing speed, number of channels 2 controller successes (= 2 x costs) Therefore. v Make new design, taking advantage of new technologies v Both groups combined to form one controller group

19 NGC, New General detector Controller In 2004 the NGC team started with a new design. Features of the NGC: No parallel bus system, only high speed serial links Central element on each board is a Xilinx FPGA using latest VIRTEX- 7 for some boards Digital parts, like RAMs, FIFOs, and the sequencer are fully implemented in the FPGA Data and commands time multiplexed transferring System is always detector limited, multiple fibre links allow data rates > 6 Gbit/ s Full monitoring of bias current and voltage levels Variations used for L3CCD AO detector systems

20 Detector specific operation Cryogenic preamplification, means controller can be metres from detector HAWKI - 4 x H2RG detector mount With 4 x 32 channel fully differential Cryogenic preamplifiers H4RG preamp footprint smaller than detector Woven ribbon cables - fully true differential cabling 360 shielding flexible 20

21 Different type of NGCs Ø SCI- NGC: the scientific NGC, which is used for all type of detectors Ø AO- NGC: used to readout the e2v CCD220 detector with a very compact, high speed integrated controller. Ø The same back- end interface is used for both NGC types. Core of the SCI-NGC WFS camera (AO-NGC)

22 Different type of housing Ø The NGC provides different type of housing: Compact (no water cooling) Fanless housing (needed for GRAVITY and MATISSE, water cooling only) Six- slot (with water cooling and fan assist)

23 NGC, New General detector Controller The NGC controller is a modular, customizable system Backplane AQ-32ch module 10 MHz FEB module Transition module Visible NIR MID-IR Visible WFS

24 NGC, New General detector Controller Ø Just like Lego blocks we can combine different modules to cover our needs. Video Basic Videointerface board-10mhz board Basic board Fiber cable Power supply box Power supply cable A system like this PCIexpress has been using to readout the SAPHIRA detector of the GRAVITY instrument LLCU

25 SAPHIRA readout electronics standard 2-slot NGC system: front-end basic board (sequencer, clock &bias ) new 32-channel 10 MHz ADC board & preprocessor in FPGA ADC

26 NGC, New General detector Controller Ø Just like Lego blocks we can combine different modules to cover our needs. MUSE I MUSE II MUSE III MUSE NGC system readouts 24 CCD detectors simultaneously MUSE IV

27 Status of the NGC Ø NGC systems are already being used by many instruments Ø Since 2012 also operational at the telescopes. VISIR GALACSI / GRAAL MATISSE AQUARIUS MID-IR MID-IR AO NIR GRAVITY NIR NGC NIR WFS SAPHIRA NIR Visible WFS Visible Visible SPHERE MUSE

28 The future - NGC v.2.0 NGC can already operate all detector choices for ELT and VLT However :- Already issues over obsolescence, in 10 years - continuous development and upgrades are therefore required New higher speed/multi-port fibre links, > 6.0 Gbit possible (we just add more fibres for higher data rates!!) Smaller, more compact form factor, especially for mosaics of detectors New modes, such as, digital correlated double sampling More integration/real time processing using VIRTEX 7 and higher FPGAs Lower power, more options, e.g. higher current biases, more biases and clocks Even more commercialization manufacture and build done outside ESO 28

29 Conclusions Looked at options for ELT, ASIC, Commercial and In-house Decided to continue with NGC development for ELT Some upgrades required but could build for ELT instruments now Looking at options such as ASIC for cryogenic preamplifier Upfront costs least for this development model Keeps in-house expertise for all aspects of detector operation 29