Square Kilometre Array Nigel Rix

Transcription

1 Square Kilometre Array Nigel Rix Technology Business Manager, ESP KTN Meet the Buyer Event Heathrow, 27 th September 2011

2 What When Who How

3 ORIGINS Neutral hydrogen in the universe from the Epoch of Re-ionisation to now When did the first stars and galaxies form? How did galaxies evolve? Role of Active Galactic Nuclei Dark Energy, Dark Matter Cradle of Life SKA Key Science Drivers FUNDAMENTAL FORCES Pulsars, General Relativity & gravitational waves Origin & evolution of cosmic magnetism TRANSIENTS (NEW PHENOMENA) Science with the Square Kilometre Array (2004, eds. C. Carilli & S. Rawlings, New Astron. Rev., 48)

4 Discovery of Pulsars Technology-led serendipitous discovery using a phased-array antenna Rapidly rotating neutron-stars Established existence of exceptionally accurate natural clocks Exploited by Taylor and Hulse: discovery of the first binary pulsar led to measure the loss of energy due to gravitational radiation in a binary

5 Great Observatories for the coming decades ALMA mm/sub-mm E-ELT optical JWST infra-red SKA radio IXO Xray

6 Top-level description a large radio telescope for transformational science up to 1 million m 2 collecting area distributed over a distance of km operating at frequencies from 70 MHz to 10 GHz (4m-3cm) with multiple detector technologies connected to a signal processor and high performance computing system by an optical fibre network (sensor network) providing 40 x sensitivity of Expanded Very Large Array, and up to 10,000 x survey speed 67 institutes in 20 countries are participating

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8 Dishes: features and design parameters Antenna diameter and cost Degree of aperture blocking Sky mount, equatorial or alt-az Surface accuracy Pointing accuracy and stability Options for housing feeds MeerKAT RSA ASKAP AU

9 Low-frequency Aperture Array LOFAR

10 Mid-Frequency Aperture Array ~60m Tile Support Bunker Freq range MHz Dense array (Nyquist sampled) ~75,000 Receiver chains New opportunities

11 Full SKA Deployment 250 Dense Aperture Arrays 3000 Dishes 3-Core Central Region AA-low Arrays Artist renditions from Swinburne Astronomy Productions

12 Achieving the specification Three collector technologies with a common processing system Frequency Range (MHz) Collector Type Sensitivity (m 2 K -1 ) Survey Speed (m 2 K -2 deg 2 ) Physical Area (m 2 ) Sparse Aperture Array x10 9 4x10 6 m Dense AA 10,000 2 x x10 5 m m Dish 10,000 4x10 7 3x10 5 m 2 +phased-array feeds 10,000 2x10 8 4x10 5 m 2

13 GHz Wide FoV MHz Wide FoV GHz WB-Single Pixel feeds Dense AA.... Sparse AA SKA system & data flow Aperture Array Station Tile & Station Processing DSP... Central Processing Facility - CPF 16 Tb/s To 250 AA Stations 4 Pb/s Correlator UV s Image formation Archive Data Time Control 20 Gb/s 16 Tb/s Optical Data links AA slice AA slice... Dish & AA+Dish Correlation AA slice 24 Pb/s Tb/s Data switch... Imaging s Tb/s Gb/s Gb/s Control s & User interface Data Archive Science s 15m Dishes DSP Gb/s... Time Standard To 1200 Dishes User interface via Internet

14 What When Who How

15 Top level schedule for the SKA Technical Preparation Phase - Telescope system design and cost Pre-construction phase - Detailed design Phase 1 construction 2016 Advanced Instrumentation Program decision Phase 2 construction 2020 full science operations with Phase full science operations with Phase 2 Programmatic 2011 Establish SKA organisation as a legal entity 2012 Site selection 2014 Construction funding approved for Phase 1-350M 2017 Construction funding approved for Phase M

16 Preparatory Phase Preconstruction Phase SKA 1 Construction SKA Preparatory Phase Phase 1 Pre-Construction Phase Phase 1 Construction, Verification, Commissioning, Acceptance, Integration & First Science Science SKA1 REV DRM Development (Ph 1 part) SKA1 User Tech. Requirements REV Science / Engineering Tradeoffs REV Early Science Proposals Refinement of Early Science Shared Risk Science SKA1 System CoDR Concept Concept dcodr Definition* SRR PDR Preliminary Design CDR Detailed Design Sys Eng & Change management REV REV Continuous Performance Evaluation SKA1 Systems integration SKA1 System Testing PDR SKA2 Early Preliminary Design System Definition (includes non-science requirements) Preliminary Design Science SKA2 REV DRM Development REV Initial SKA2 User Tech. Requirements Extraction of detailed SKA2 requirements REV REV Science / Engineering tradeoffs AIP AIP definition, development and fabrication Demonstration & testing Project Milestones Rev B SKA1 Baseline Design Site decision Costed system design SKA1 construction approval Start of SKA1 Construction AIP Decision Baseline Design for SKA * Includes definition of non-science requirements.

17 SKA 1 baseline design Baseline technologies are mature and demonstrated in the SKA Precursors and Pathfinders Central Region 250 Dishes 50 Sparse Aperture Arrays Single pixel feed Artist renditions from Swinburne Astronomy Productions

18 SKA 2 including AIP technologies 250 Dense Aperture Arrays 3-Core Central Region 2500 Dishes 250 Sparse Aperture Arrays Artist renditions from Swinburne Astronomy Productions

19 SKA 1 An SKA collector summary Freq. Range Collector Sensitivity Number / size Distribution 70 MHz to 450 MHz 300 MHz to 3 GHz AA-low Sparse AA Dishes with single pixel feed 1,000 m 2 /K at 100 MHz 1,000 m 2 /K at 1.4 GHz 50 arrays, Diameter 180 m 70% within 5 km dia., 250 dishes Diameter 15 m 30 % along 3 spiral arms out to 100 km radius SKA 2 Freq. Range Collector Sensitivity Number / size Distribution 70 MHz to 450 MHz 400 MHz to 1.45 GHz 300/1000 MHz to 10 GHz AA-low Sparse AA AA-mid Dense AA Dishes with single pixel feed + PAF 4,000 m 2 /K at 100 MHz 10,000 m 2 /K at 800 MHz 10,000 m 2 /K at 1.4 GHz 250 arrays, Diameter 180 m 250 arrays, Diameter 56 m dishes Diameter 15 m 66% within 5 km dia., 34% along 5 spiral arms out to 180 km radius 50% within 5 km dia, 30% 5km km 20% 180 km-3,000 km.

20 What When Who How

21 April 2011, in Rome Australia, China, France, Germany, Italy, the Netherlands, New Zealand, South Africa, and the UK sign a Letter of Intent in Rome declaring their common ambition to see the SKA built, and to work together to secure funding for the next phase of the project.

22 SKA Organisational Structure SKA Organisation Board of Directors Advisory Committees General Director Advisory Committees SKA Project Office (SPO) Work package Contractor Work package Contractor Work package Contractor Industry POs

23 What When Who How

24 Pre-construction Phase Objectives 1. Bring all SKA 1 subsystems to Critical Design level 2. Close Production Reviews for all SKA 1 subsystems, including contract preparation 3. Manage trade-offs for SKA 2 technology, taking into account the results from the AIP 4. Bring all SKA 2 subsystems to Preliminary Design level

25 Project Execution Plan 11 work packages Proposed funding: 91 M 28 M for SPO staff and operations (30%) 63 M for WP Consortia under contract to SPO (70%) Reviewed by int l panel SKA is ready to transition from science project to big construction project

26 Work Packages in the Project Execution Plan 1. Management 2. System 3. Science 4. Maintenance and support /Operations Plan 5. Site preparation 6. Dishes 7. Aperture arrays 8. Signal transport & networks 9. Signal processing 10.Computing & software 11. Power Work Package Contractors SPO

27 Contact Points: SKA Project Office Phil Crosby UK Principal Investigator Prof Paul Alexander UK Project Engineer Dr Andrew Faulkner UK Industry Cluster Nigel Rix

28 SKA is driving development of new science & technical solutions Dishes, feeds, receivers (N=3000) Low and mid aperture arrays (N=250) ongoing verification programs Signal transport (10 Pbit/s) Signal processing (exa-macs) Software engineering and algorithm development High performance computing (exa-flop capability) Data storage (exa-byte capacity) (Distributed) power requirements ( MW) INDUSTRY ENGAGEMENT IS CENTRAL TO THE SKA

29 Conclusions SKA is a transformational science instrument Addresses major questions in Cosmology, Astrophysics and Physics Technology to realise the SKA is challenging, exciting and has wide interest / applicability to industry SKA is a major ICT infrastructure for the next decade Offers significant opportunities for industry and global collaborations

30 The Challenges of Radio Astronomy The signals are extremely weak. We need large capture area They need to be in special places Astronomers compete with noise From radio, TV, phones, machines, etc From the equipment itself, amplifiers etc Signals are buried in the noise Need smart techniques to resolve This means huge computing power Large amounts of data to handle Pushing boundaries in capacity, speed and storage

31 24-hour coverage is needed, storage is crucial Cost likely to be an issue if not subsidised. Phase 1 (array) ~ 4 MW. Phase 2 = 30-50MW. Stringent EMC / RFI requirements (build & run) Integrated M&C into system Good project for demonstration of scalable solar technology.

32 Little wind, no geothermal, no hydro, great solar. (Concentrated) Solar thermal looks possible, but difficult to up-scale. Photo-voltaics, with Vanadium Redox battery seems most promising.

33 Remote Stations 2,000 PV panels covering 1 hectare will generate 320KW at each of the 15 remote stations. Requires a 100KW VRB with 0.1 mega litres of electrolyte. Will run the station for 24 hours in the absence of full sunshine. Core Site 100,000 PV panels over 40 hectares to give 16 MW (net after losses), to power 3 MW array. Remainder charges the VRB batteries. Needs 5.4 mega litres (or 2 Olympic pools) of electrolyte. Will run the array continuously (including core computing and support), for about 18 hours in the absence of full sunshine. Cost is likely to be US$ million installed.

34 Questions?