SKA Science Data Processing
|
|
|
- Rebecca Ward
- 5 years ago
- Views:
Transcription
1 SKA Science Data Proceing B. Nikolic (SDP Project Engineer) & SDP Conortium Team Atrophyic Group, Cavendih Laboratory, Univerity of Cambridge bn204/ 1 April 2014 AASTCS 2: Exacale Radio Atronomy Monterey, CA, USA
2 Outline
3 SKA1 -Mid SKA1 -Low SKA1 -Survey
4 SKA1 -Mid SKA1 -Low SKA1 -Survey Computer
5 SKA1 -Mid SKA1 -Low SKA1 -Survey Computer
6 SKA Progre Dec 2011 Incorporation of the SKA Organiation a a not-for-profit company regitered in England May 2012 Deciion on ite and cope of SKA-1 March 2013 Iue of the firt Baeline Deign, call for conortia propoal May 2013 Opening of SKA International HQ at Jodrell Bank Sept 2013 Acceptance of conortia, ignature of MoU and CA, fully funded deign phae Nov 2013 Iue of L1 requirement, commencement of the work of conortia March 2014 UK Government announce GBP 100 million for it hare of SKA 1 contruction cot
7 SKA Project Structure
8 Square Kilometre Array Simplified Context SADT Monitor and Control Manager LFAA Wetern Autralia SKA1 Low: Low Frequency Aperture Array Dih SKA1 Survey: Dih Antenna with PAF Central Signal Proceing LFAA Correlator/ Beam Former Survey Correlator Science Data Proceor Science Data Proceor Implementation (Autralia) South Africa SKA1 Mid: Dih Antenna with Single- Pixel feed SKA1 Mid Correlator/ Beam Former Pular Science Data Proceor Implementation (South Africa) Search Proceor
9 Context of the SKA Science Data Proceor Central Signal Proceor Beam Formed Data 1000 km Viibilitie Pular Candidate Control Science Data Proceor km Control Telecope State Monitoring Catalogue Image Cube Telecope Manager Atronomer
10 Outline
11 We can ee the route to SKA 1 -SDP FLOPS: 300 PetaFLOPS Expect won t be at top of Top500 Scratch torage capacity: 100 PetaByte Both dik and olid tate poibility Scratch torage throughput: 20 TByte/ node, lot of inherent parallelim Inget rate 5 TByte/ FDR Infiniband witche almot there now Capital & Operational cot Commoditiation and general drive to low power
12 Rik Convergence with rapidly evolving technology? Unknown apect of data? Implementing the Software? Actual cot of caling up?
13 Outline
14 Data level Catalogue Stacked Image Archive Power Spectra Pular Timing Confirmed Pular Science Ready Image Cube Pular Candidate Calibrated Viibilitie Time erie Raw Viibilitie Raw data
15 Point ource Meaurement Proce Atronomical wavefront Turbulent Ionophere Corrupted wavefront Collector q Ai da E q (x, y, t) W qp i (x, y, t) q Aj da E q (x, y, t) W qp j (x, y, t) Correlator V p ij
16 Major cycle imaging iteration Filter Sky Model Image Plane Correction Combine Predict viibilitie Etimate ky FFT Grid Convolve Subtract Viibilitie Solve Calibration Phae Rotate
17 Outline
18 Data Rate time mearing v V i j = (a + ib) θ rad 1 θ D/λ t int D 8B θ B λ u
19 Data Rate bandwidth mearing v D/λ 2 f f D 8B B λ B 1 λ B 2 λ 3 u
20 Wide-field & three dimenional geometry Incoming wavefront Offaxi wavefront A2 Reference plane λw θ co λw A 1 A 2 λw λw co θ = λw(1 co θ) = = λw(1 1 in 2 θ) = λw(1 1 l 2 )
21 Outline
22 SKA-1 Parameter SKA1-Low SKA1-Mid SKA1-Survey N a t dump N f 256k 256k 256k N beam D S 35 m 15 m 15 m B max 100 km 200 km 50 km N GW Size of the w-projection kernel N AA N facet Tion Size of the anti-aliaing kernel Number of facet (on the ide) Ionopheric timecale
23 inget Input Viibility Rate 2 (N a 1) N a N beam N f t dump SKA1-Low SKA1-Mid SKA1-Survey / / / Input Data Rate 16 (N a 1) N a N beam N f t dump byte SKA1-Low SKA1-Mid SKA1-Survey 7.2 Tbyte 3.3 Tbyte 4.5 Tbyte
24 w-naphot Snaphot Duration (in term of w-kernel ize) D N facet N GW B max SKA1-Low SKA1-Mid SKA1-Survey 9.6 N facet N GW 2.1 N facet N GW 8.3 N facet N GW
25 pixel baed FFT nominal FLOP rate ( ).012 Bmax 3 16 B N beam N f log max 2 D 2 N2 facet log 2 D 3 N facet N GW SKA1-Low SKA1-Mid SKA1-Survey (aume N facet = 1 ) log 2 N GW Op log 2 N GW Op Op log 2 N GW Op Re-projection Rate FLOPS.12 B 3 max N beam N f D 3 N facet N GW Op SKA1-Low SKA1-Mid SKA1-Survey N facet N GW Op N facet N GW Op N facet N GW Op
26 viibility baed Gridding FLOPS rate 16 (N a 1) N a N beam N f N 2 facet (N 2 GW +N2 AA) t dump Op SKA1-Low SKA1-Mid SKA1-Survey (aume N facet = 1, N AA = 9 ) ( N 2 GW + 81 ) Op ( N 2 GW + 81 ) Op ( N 2 GW + 81 ) Op
27 combined Combined gridding+fft+reprojection 16 (N a 1) N a N beam N f N 2 facet (N 2 GW +N2 AA) t dump Op + ( ).012 B3 16 B max N beam N f log max 2 D 2 N2 facet log 2 D 3 N facet N GW +.12 B3 max N beam N f D 3 N facet N GW Op Optimied w-kernel ize SKA1-Low SKA1-Mid SKA1-Survey Combined gridding+fft+reprojection SKA1-Low SKA1-Mid SKA1-Survey Op Op Op
28 convolution kernel the convolution kernel ( 128 (N a 1) N a N beam N f Nfacet 2 (NGW 2 +N2 AA) ) log 8 NGW 2 +N2 AA log 2 Tion SKA1-Low SKA1-Mid SKA1-Survey (aume 60 econd ionopheric timecale) Op Op Op Op convolution function over gridding rate 8 t dump log (8 ) NGW log 2 Tion SKA1-Low SKA1-Mid SKA1-Survey 31. Tion 5.2 Tion 19. Tion
29 Scratch torage Capacity 27 (N a 1) N a N beam N f t dump Tbyte SKA1-Low SKA1-Mid SKA1-Survey 154. Pbyte 71. Pbyte 97. Pbyte Chunk Size (10 channel, each naphot) (N a 1) N a t dump Gbyte SKA1-Low SKA1-Mid SKA1-Survey 28. Gbyte 13. Gbyte.49 Gbyte
The Square Kilometre Array & High speed data recording
The Square Kilometre Array & High speed Astrophysics Group, Cavendish Laboratory, University of Cambridge http://www.mrao.cam.ac.uk/ bn204/ CRISP Annual Meeting FORTH, Crete, Greece March 2012 Outline
International Project Update
International Project Update - Mike Garrett (ASTRON & Leiden) Chair SKA Science & Engineering Committee This talk - SKA: a global vision for Radio Astronomy - Science drivers - Pathfinders, Precursors,
SKA Science Data Processing or MAKING SENSE OF SENSOR BIG DATA
SKA Science Data Processing or MAKING SENSE OF SENSOR BIG DATA Bojan Nikolic & SDP Consortium Astrophysics Group, Cavendish Laboratory Project Engineer/Architecture Lead SKA Science Data Processor What
Data analysis of massive data sets a Planck example
Data analysis of massive data sets a Planck example Radek Stompor (APC) LOFAR workshop, Meudon, 29/03/06 Outline 1. Planck mission; 2. Planck data set; 3. Planck data analysis plan and challenges; 4. Planck
High-performance computing and the Square Kilometre Array (SKA) Chris Broekema (ASTRON) Compute platform lead SKA Science Data Processor
High-performance computing and the Square Kilometre Array (SKA) Chris Broekema (ASTRON) Compute platform lead SKA Science Data Processor Radio Astronomy and Computer Science Both very young sciences (1950s)
Determining the Specification of an Aperture Array for Cosmological Surveys
Determining the Specification of an Aperture Array for Cosmological Surveys P. Alexander University of Cambridge, Department of Physics, Cavendish Laboratory, Cambridge, UK. A. J. aulkner Jodrell Bank
Year 3 Workshop London, 15-17th December Wayne Holland (UK ATC) & Giorgio Savini (UCL) On behalf of the FISICA team
Year 3 Workhop London, 15-17th December 2015 Wayne Holland (UK ATC) & Giorgio Savini (UCL) On behalf of the FISICA team With help from: John Lightfoot, Bruce Sibthorpe, Jane Greave, Luigi Spinoglio, Maxime
Overview of the Square Kilometre Array. Richard Schilizzi COST Workshop, Rome, 30 March 2010
Overview of the Square Kilometre Array Richard Schilizzi COST Workshop, Rome, 30 March 2010 The Square Kilometre Array A global program Time line 2000-07 Initial Concept Stage 2008-12 System Design Stage
Square Kilometre Array. Steve Torchinsky
Square Kilometre Array Steve Torchinsky steve.torchinsky@obspm.fr A square kilometre of collecting area for each of three frequency bands SKA Low frequency 50MHz to 450MHz to be built in Western Australia
Reinforcement Learning
Reinforcement Learning Yihay Manour Google Inc. & Tel-Aviv Univerity Outline Goal of Reinforcement Learning Mathematical Model (MDP) Planning Learning Current Reearch iue 2 Goal of Reinforcement Learning
The Future of Radio Astronomy. Karen O Neil
The Future of Radio Astronomy Karen O Neil The Present Arecibo Telescope 305m diameter dish 0.4-10 GHz 7-pixel FPA (1.2-1.5 GHz) -01⁰ < δ < 38⁰ Resolution : 15 (0.3 GHz) 0.4 (10 GHz) 60% of astronomy time
New Zealand Impacts on CSP and SDP Designs
New Zealand Impacts on CSP and SDP Designs Dr Andrew Ensor Director HPC Research Laboratory/ Director NZ SKA Alliance Mid-Year Mini SKA Colloquium 2018 12 July 2018 Past, Present, Future Mega-Science Projects
Square Kilometre Array Science Data Challenge 1
Square Kilometre Array Science Data Challenge 1 arxiv:1811.10454v1 [astro-ph.im] 26 Nov 2018 Anna Bonaldi & Robert Braun, for the SKAO Science Team SKA Organization, Jodrell Bank, Lower Withington, Macclesfield,
SKA Industry Update. Matthew Johnson Head of the UK SKA Project Office STFC
SKA Industry Update Matthew Johnson Head of the UK SKA Project Office STFC Square Kilometre Array Rebaselining announced in March 2015 UK selected as HQ host in April 2015 Business case approved by Jo
The Square Kilometre Array Radio Telescope Project : An Overview
Science with the SKA IISER Mohali 19th March The Square Kilometre Array Radio Telescope Project : An Overview Yashwant Gupta NCRA-TIFR Background : what is the SKA? The SKA is the most ambitious Radio
Square Kilometre Array: status. Philip Diamond SKA Director-General 16 th September 2013
Square Kilometre Array: status Philip Diamond SKA Director-General 16 th September 2013 Great Observatories for the coming decades E- ELT E- ELT oop(cal/ p(cal/ir IR Construc(on Construc(on approved approved
Hughes et al., 1998 ApJ, 505, 732 : ASCA. Westerlund, 1990 A&ARv, 2, 29 : Distance to LMC 1 ) ) (ergs s F X L X. 2 s 1. ) (ergs cm
1 SUMMARY 1 SNR 0525-66.1 1 Summary Common Name: N 49 Distance: 50 kpc (distance to LMC, Westerlund(1990) ) Position of Central Source (J2000): ( 05 25 59.9, -66 04 50.8 ) X-ray size: 85 x 65 Description:??
Welcome and SKA Overview Michiel van Haarlem. Interim Director General SKA Organisation 15 February 2012
Welcome and SKA Overview Michiel van Haarlem Interim Director General SKA Organisation 15 February 2012 SKA Concept A large radio telescope for transformational science: up to 1 million m 2 antenna collecting
Project Engineer SKA Science Data Processor Consortium
SKA Science Data Processing Storage Requirements BigStorage Initial Workshop 3 rd March 2016 Bojan Nikolic Astrophysics Group, Cavendish Lab University of Cambridge Email: b.nikolic@mrao.cam.ac.uk Project
Layering as Optimization Decomposition
TLEN7000/ECEN7002: Analytical Foundation of Network Layering a Optimization Decompoition Lijun Chen 11/29/2012 The Internet Compleity i ever increaing Large in ize and cope Enormou heterogeneity Incomplete
The Square Kilometre Array. Richard Schilizzi SKA Program Development Office
The Square Kilometre Array Richard Schilizzi SKA Program Development Office EVN Symposium, Manchester September 2010 1995-00 2000-07 Science 2008-12 SKA Science & Engineering 2013-23 Committee 2020-50+
Transient Cosmic Phenomena and their Influence on the Design of the SKA Radio Telescope
Transient Cosmic Phenomena and their Influence on the Design of the SKA Radio Telescope Research Review Curtin Institute of Radio Astronomy 5 May 2009 ToC Parameter space Discovering phenomena ASKAP &
ECEN620: Network Theory Broadband Circuit Design Fall 2018
ECEN60: Network Theory Broadband Circuit Deign Fall 08 Lecture 6: Loop Filter Circuit Sam Palermo Analog & Mixed-Signal Center Texa A&M Univerity Announcement HW i due Oct Require tranitor-level deign
Chapter 4: Applications of Fourier Representations. Chih-Wei Liu
Chapter 4: Application of Fourier Repreentation Chih-Wei Liu Outline Introduction Fourier ranform of Periodic Signal Convolution/Multiplication with Non-Periodic Signal Fourier ranform of Dicrete-ime Signal
GNSS Solutions: What is the carrier phase measurement? How is it generated in GNSS receivers? Simply put, the carrier phase
GNSS Solution: Carrier phae and it meaurement for GNSS GNSS Solution i a regular column featuring quetion and anwer about technical apect of GNSS. Reader are invited to end their quetion to the columnit,
A Study on Simulating Convolutional Codes and Turbo Codes
A Study on Simulating Convolutional Code and Turbo Code Final Report By Daniel Chang July 27, 2001 Advior: Dr. P. Kinman Executive Summary Thi project include the deign of imulation of everal convolutional
Digital Control System
Digital Control Sytem - A D D A Micro ADC DAC Proceor Correction Element Proce Clock Meaurement A: Analog D: Digital Continuou Controller and Digital Control Rt - c Plant yt Continuou Controller Digital
The Search for Extraterrestrial Intelligence (SETI) What can SETI
The Search for Extraterrestrial Intelligence (SETI) What can SETI Mike Garrett researchers learn Sir Bernard Lovell Chair, Prof. of Astrophysics. from FRBs Director Jodrell Bank Centre for Astrophysics
Wide-Field Imaging: I
Wide-Field Imaging: I S. Bhatnagar NRAO, Socorro Twelfth Synthesis Imaging Workshop 010 June 8-15 Wide-field imaging What do we mean by wide-field imaging W-Term: D Fourier transform approximation breaks
Gamma-ray pulsars in binary systems
Gamma-ray pulsars in binary systems searching the needle in a haystack Henning Fehrmann Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut) Leibniz Universität Hannover Göhren-Lebbin,
Future radio galaxy surveys
Future radio galaxy surveys Phil Bull JPL/Caltech Quick overview Radio telescopes are now becoming sensitive enough to perform surveys of 107 109 galaxies out to high z 2 main types of survey from the
Science Operations with the Square Kilometre Array
Science Operations with the Square Kilometre Array Dr Antonio Chrysostomou Head of Science Operations Planning a.chrysostomou@skatelescope.org Outline Introduction to the SKA Science Programme Operational
Square Kilometre Array Nigel Rix
Square Kilometre Array Nigel Rix Technology Business Manager, ESP KTN nigel.rix@ukskaic.org Meet the Buyer Event Heathrow, 27 th September 2011 What When Who How ORIGINS Neutral hydrogen in the universe
Introduction to Laplace Transform Techniques in Circuit Analysis
Unit 6 Introduction to Laplace Tranform Technique in Circuit Analyi In thi unit we conider the application of Laplace Tranform to circuit analyi. A relevant dicuion of the one-ided Laplace tranform i found
Non-Closing Offsets on the VLA. R. C. Walker National Radio Astronomy Observatory Charlottesville VA.
VLA SCIENTIFIC MEMORANDUM NO. 152 Non-Closing Offsets on the VLA R. C. Walker National Radio Astronomy Observatory Charlottesville VA. March 1984 Recent efforts to obtain very high dynamic range in VLA
Jul 4, 2005 turbo_code_primer Revision 0.0. Turbo Code Primer
Jul 4, 5 turbo_code_primer Reviion. Turbo Code Primer. Introduction Thi document give a quick tutorial on MAP baed turbo coder. Section develop the background theory. Section work through a imple numerical
Radio Transient Surveys with The Allen Telescope Array & the SKA. Geoffrey C Bower (UC Berkeley)
Radio Transient Surveys with The Allen Telescope Array & the SKA Geoffrey C Bower (UC Berkeley) Transient Science is Exploding New Phenomena An Obscured Radio Supernova in M82 Discovered serendipitously
Big-Data as a Challenge for Astrophysics
Big-Data as a Challenge for Astrophysics ESA / Euclid Consortium Hubble deep field, NASA/STScI HESS collaboration, F. Acero and H. Gast ESA/ATG medialab; ESO/S. Brunier Volker Beckmann Institut National
SKA Precursors and Pathfinders. Steve Torchinsky
SKA Precursors and Pathfinders Steve Torchinsky steve.torchinsky@obspm.fr A square kilometre of collecting area for each of three frequency bands SKA Low frequency 50MHz to 450MHz to be built in Western
Wide Field Astronomy with ASKAP. Wide Field Astronomy with ASKAP. ASKAP Specifications ASKAP & SKA
Wide Field Astronomy with ASKAP ASKAP specifications Survey science process & User policy Survey science ASKAP - what next Wide Field Astronomy with ASKAP Carole Jackson ASKAP Project Team 5 November 2009
Radio Telescopes of the Future
Radio Telescopes of the Future Cristina García Miró Madrid Deep Space Communications Complex NASA/INTA AVN Training School HartRAO, March 2017 Radio Telescopes of the Future Characteristics FAST SKA (EHT)
The Search for Extraterrestrial Intelligence (SETI) Director Jodrell Bank Centre for Astrophysics
The Search for Extraterrestrial Intelligence (SETI) Mike Garrett e-merlin & EVN in Sir Bernard Chair, Prof. of Astrophysics. SKA eralovell workshop Director Jodrell Bank Centre for Astrophysics - Introduction.
3.1 The Revised Simplex Algorithm. 3 Computational considerations. Thus, we work with the following tableau. Basic observations = CARRY. ... m.
3 Computational conideration In what follow, we analyze the complexity of the Simplex algorithm more in detail For thi purpoe, we focu on the update proce in each iteration of thi procedure Clearly, ince,
Radio Interferometry Fundamentals. John Conway Onsala Space Obs and Nordic ALMA ARC-node
Radio Interferometry Fundamentals John Conway Onsala Space Obs and Nordic ALMA ARC-node So far discussed only single dish radio/mm obs Resolution λ/d, for D=20m, is 30 at mm-wavelengths and 30 (diameter
Progress in multigigabit Point to Point Connectivity between South Africa and GEANT.
Progress in multigigabit Point to Point Connectivity between South Africa and GEANT. Applications to Radio Astronomy M J Gaylard 1, J F H Quick 1, B. Becker 2 1 HartRAO, P. O. Box 443, Krugersdorp 1740,
Apertif. Paolo Serra. Tom Oosterloo (PI) Marc Verheijen (PI) Laurens Bakker George Heald Wim van Cappellen Marianna Ivashina
Netherlands Institute for Radio Astronomy Apertif Tom Oosterloo (PI) Marc Verheijen (PI) Laurens Bakker George Heald Wim van Cappellen Marianna Ivashina ASTRON is part of the Netherlands Organisation for
LOFAR for Pulsar. Ben Stappers ASTRON/UvA
LOFAR for Pulsar Ben Stappers ASTRON/UvA Outline: LOFAR a short introduction Pros and cons of low-frequency observation How to find new pulsars with LOFAR Studying individual Pulsars average pulse profiles
Astronomy of the Next Decade: From Photons to Petabytes. R. Chris Smith AURA Observatory in Chile CTIO/Gemini/SOAR/LSST
Astronomy of the Next Decade: From Photons to Petabytes R. Chris Smith AURA Observatory in Chile CTIO/Gemini/SOAR/LSST Classical Astronomy still dominates new facilities Even new large facilities (VLT,
Very Large Array Sky Survey
1 Very Large Array Sky Survey Technical Implementation & Test Plan Casey Law, UC Berkeley Galactic Center (Survey) Multiwavelength Image Credit: X-ray: NASA/UMass/D.Wang et al., Radio: N RAO/AUI/NSF/NRL/N.Kassim,
7.4. The Inverse of a Matrix. Introduction. Prerequisites. Learning Outcomes
The Inverse of a Matrix 7.4 Introduction In number arithmetic every number a 0has a reciprocal b written as a or such that a ba = ab =. Similarly a square matrix A may have an inverse B = A where AB =
Principles of Interferometry. Hans-Rainer Klöckner IMPRS Black Board Lectures 2014
Principles of Interferometry Hans-Rainer Klöckner IMPRS Black Board Lectures 2014 acknowledgement Mike Garrett lectures James Di Francesco crash course lectures NAASC Lecture 5 calibration image reconstruction
The international SKA project
The international SKA project - Towards a giant global radio telescope - Wim van Driel Paris Observatory - GEPI 3 rd MCCT SKADS School, Paris, 24/08/2009 SKA - Square Kilometre Array Necessary for a breakthrough
The Pulsation Properties of the Double-Mode RR Lyrae Variable V79 in Messier 3
336 The Pulsation Properties of the Double-Mode RR Lyrae Variable V79 in Messier 3 Christine M. Clement Department of Astronomy and Astrophysics, University of Toronto, Toronto, ON, M5S 3H8, Canada Mike
Software, Computing and Data Storage for the
Software, Computing and Data Storage for the Square Kilometre Array Duncan Hall XLDB 2009 2009 August 28 Outline SKA: What are the drivers? How does radio astronomy work? What are the SKA s prime characteristics?
Multi Constrained Optimization model of Supply Chain Based on Intelligent Algorithm Han Juan School of Management Shanghai University
5th nternational Conference on Advanced Material and Computer cience (CAMC 206) Multi Contrained Optimization model of upply Chain Baed on ntelligent Algorithm Han Juan chool of Management hanghai Univerity
CS 179: LECTURE 16 MODEL COMPLEXITY, REGULARIZATION, AND CONVOLUTIONAL NETS
CS 179: LECTURE 16 MODEL COMPLEXITY, REGULARIZATION, AND CONVOLUTIONAL NETS LAST TIME Intro to cudnn Deep neural nets using cublas and cudnn TODAY Building a better model for image classification Overfitting
Large Field of View Radio Astronomy; relevant for many KSP s
Large Field of View Radio Astronomy; relevant for many KSP s SKA Key Science Drivers ORIGINS Probing the Dark Ages When & how were the first stars formed? Cosmology and Galaxy Evolution Galaxies, Dark
To describe a queuing system, an input process and an output process has to be specified.
5. Queue (aiting Line) Queuing terminology Input Service Output To decribe a ueuing ytem, an input proce and an output proce ha to be pecified. For example ituation input proce output proce Bank Cutomer
Linear Imperfections Oliver Bruning / CERN AP ABP
Linear Imperfection CAS Fracati November 8 Oliver Bruning / CERN AP ABP Linear Imperfection equation of motion in an accelerator Hill equation ine and coine like olution cloed orbit ource for cloed orbit
From LOFAR to SKA, challenges in distributed computing. Soobash Daiboo Paris Observatory -LESIA
From LOFAR to SKA, challenges in distributed computing Soobash Daiboo Paris Observatory -LESIA Overview LOFAR telescope Data processing with LOFAR NenuFar SKA Summary LOFAR science drivers Key science
Chapter 2: Problem Solutions
Chapter 2: Solution Dicrete Time Proceing of Continuou Time Signal Sampling à 2.. : Conider a inuoidal ignal and let u ample it at a frequency F 2kHz. xt 3co000t 0. a) Determine and expreion for the ampled
A Method for Assessing Customer Harmonic Emission Level Based on the Iterative Algorithm for Least Square Estimation *
Engineering, 203, 5, 6-3 http://dx.doi.org/0.4236/eng.203.59b002 Publihed Online September 203 (http://www.cirp.org/journal/eng) A Method for Aeing Cutomer Harmonic Emiion Level Baed on the Iterative Algorithm
The high angular resolution component of the SKA
The high angular resolution component of the SKA Tingay, S. 1, Bignall, H. 1, Colegate, T. 1, Aben, G. 2, Nicolls, J. 2 & Weston, S. 3 Prof. Steven Tingay SKA2010 Deputy Director, ICRAR March 22 25, 2010
Sequence Obs ID Instrument Exposure uf Exposure f Date Observed Aimpoint (J2000) (ks) (ks) (α, δ)
1 SUMMARY 1 G120.1+01.4 1 Summary Common Name: Tycho s Distance: 2.4 kpc ( Chevalier et al., 1980 ) Center of X-ray emission (J2000): ( 00 25 19.9, 64 08 18.2 ) X-ray size: 8.7 x8.6 Description: 1.1 Summary
Roadmap for Discrete-Time Signal Processing
EE 4G Note: Chapter 8 Continuou-time Signal co(πf Roadmap for Dicrete-ime Signal Proceing.5 -.5 -..4.6.8..4.6.8 Dicrete-time Signal (Section 8.).5 -.5 -..4.6.8..4.6.8 Sampling Period econd (or ampling
E-MERLIN and EVN/e-VLBI Capabilities, Issues & Requirements
E-MERLIN and EVN/e-VLBI Capabilities, Issues & Requirements e-merlin: capabilities, expectations, issues EVN/e-VLBI: capabilities, development Requirements Achieving sensitivity Dealing with bandwidth,
Deconvolving Primary Beam Patterns from SKA Images
SKA memo 103, 14 aug 2008 Deconvolving Primary Beam Patterns from SKA Images Melvyn Wright & Stuartt Corder University of California, Berkeley, & Caltech, Pasadena, CA. ABSTRACT In this memo we present
τ ), respectively. Then
Downloaded /0/ to 9.7.47.34. Reditribution ubject to SEG licene or copyright; ee Term of Ue at http://library.eg.org/ Quality factor affect channel wave propagation in 3D iotropic vicoelatic medium Hui
Atmospheric phase correction for ALMA with water-vapour radiometers
Atmospheric phase correction for ALMA with water-vapour radiometers B. Nikolic Cavendish Laboratory, University of Cambridge January 29 NA URSI, Boulder, CO B. Nikolic (University of Cambridge) WVR phase
Comparison of independent process analytical measurements a variographic study
WSC 7, Raivola, Ruia, 15-19 February, 010 Comparion of independent proce analytical meaurement a variographic tudy Atmopheric emiion Watewater Solid wate Pentti Minkkinen 1) Lappeenranta Univerity of Technology
Delivering SKA Science
Delivering SKA Science P.J.Quinn 1,2, T. Axelrod 3, I. Bird 4, R. Dodson 2, A. Szalay 5, A. Wicenec 2 2 International Centre for Radio Astronomy Research (ICRAR), 3 LSST Project, 4 LHC Computing Grid Project,
SKA-NL Roadmap: SaDT and VLBI. Arpad Szomoru, JIVE
SKA-NL Roadmap: SaDT and VLBI Arpad Szomoru, JIVE JIVE - Joint Institute for VLBI ERIC Promote and advance the use of VLBI for astronomy Central correlation for European VLBI Network Operational feedback
CHAPTER 8 OBSERVER BASED REDUCED ORDER CONTROLLER DESIGN FOR LARGE SCALE LINEAR DISCRETE-TIME CONTROL SYSTEMS
CHAPTER 8 OBSERVER BASED REDUCED ORDER CONTROLLER DESIGN FOR LARGE SCALE LINEAR DISCRETE-TIME CONTROL SYSTEMS 8.1 INTRODUCTION 8.2 REDUCED ORDER MODEL DESIGN FOR LINEAR DISCRETE-TIME CONTROL SYSTEMS 8.3
A simple Concept for the Performance Analysis of Cluster-Computing
A simple Concept for the Performance Analysis of Cluster-Computing H. Kredel 1, S. Richling 2, J.P. Kruse 3, E. Strohmaier 4, H.G. Kruse 1 1 IT-Center, University of Mannheim, Germany 2 IT-Center, University
ACIS ( , ) Total e e e e-10 4.
1 SUMMARY 1 G21.5-0.9 1 Summary Distance: 5 kpc ( Safi-Harb et al., 2001 ) Position of Central Source (J2000): ( 18 33 34.0, -10 34 15.3 ) X-ray size: 4.7 x4.6 Description: 1.1 Summary of Chandra Observations
Observational methods for astrophysics. Pierre Hily-Blant
Observational methods for astrophysics Pierre Hily-Blant IPAG pierre.hily-blant@univ-grenoble-alpes.fr, OSUG-D/306 2016-17 P. Hily-Blant (Master2 APP) Observational methods 2016-17 1 / 323 VI Spectroscopy
Inferring source polarisation properties from SKA observations. Joern Geisbuesch
Inferring source polarisation properties from SKA observations In collaboration with Paul Alexander, Rosie Bolton, Martin Krause April 2008 University of Cambridge Department of Physics Motivation and
Mike Garrett. Sir Bernard Lovell Chair, Prof. of Astrophysics. Director Jodrell Bank Centre for Astrophysics
The Search for Extraterrestrial Intelligence (SETI) All-sky Radio Mike Garrett SETI Sir Bernard Lovell Chair, Prof. of Astrophysics. Director Jodrell Bank Centre for Astrophysics Mike Garrett Sir Bernard
Finding the location of switched capacitor banks in distribution systems based on wavelet transform
UPEC00 3t Aug - 3rd Sept 00 Finding the location of witched capacitor bank in ditribution ytem baed on wavelet tranform Bahram nohad Shahid Chamran Univerity in Ahvaz bahramnohad@yahoo.com Mehrdad keramatzadeh
Lecture 9: Speckle Interferometry. Full-Aperture Interferometry. Labeyrie Technique. Knox-Thompson Technique. Bispectrum Technique
Lecture 9: Speckle Interferometry Outline 1 Full-Aperture Interferometry 2 Labeyrie Technique 3 Knox-Thompson Technique 4 Bispectrum Technique 5 Differential Speckle Imaging 6 Phase-Diverse Speckle Imaging
Chapter Landscape of an Optimization Problem. Local Search. Coping With NP-Hardness. Gradient Descent: Vertex Cover
Coping With NP-Hardne Chapter 12 Local Search Q Suppoe I need to olve an NP-hard problem What hould I do? A Theory ay you're unlikely to find poly-time algorithm Mut acrifice one of three deired feature
Lab. 1. Entanglement and Bell inequalities
Lab.. Entanglement and Bell inequalitie In quantum mechanic, two particle are called entangled if their tate cannot be factored into ingle-particle tate: Ψ Ψ Ψ Meaurement performed on the firt particle
Data Reduction and Analysis Techniques. Continuum - Point Sources On-Off Observing
Data Reduction and nalysis echniques Ronald J. Maddalena www.nrao.edu/~rmaddale/education Continuum - oint ources On-Off Observing Noise Diode ignal ignal Observe blank sky for 10 sec Move telescope to
CHAPTER 4 DESIGN OF STATE FEEDBACK CONTROLLERS AND STATE OBSERVERS USING REDUCED ORDER MODEL
98 CHAPTER DESIGN OF STATE FEEDBACK CONTROLLERS AND STATE OBSERVERS USING REDUCED ORDER MODEL INTRODUCTION The deign of ytem uing tate pace model for the deign i called a modern control deign and it i
Real-Time Identification of Sliding Friction Using LabVIEW FPGA
Real-Time Identification of Sliding Friction Uing LabVIEW FPGA M. Laine Mear, Jeannie S. Falcon, IEEE, and Thoma R. Kurfe, IEEE Abtract Friction i preent in all mechanical ytem, and can greatly affect
Search Strategies. Basic Problem: where to look? Possible Scenarios Powerful, omnidirectional beacons
Communication, 2. Search Strategies Basic Problem: where to look? Possible Scenarios Powerful, omnidirectional beacons Implies very advanced civilization Seeking to attract attention of new civilizations
A FUNCTIONAL BAYESIAN METHOD FOR THE SOLUTION OF INVERSE PROBLEMS WITH SPATIO-TEMPORAL PARAMETERS AUTHORS: CORRESPONDENCE: ABSTRACT
A FUNCTIONAL BAYESIAN METHOD FOR THE SOLUTION OF INVERSE PROBLEMS WITH SPATIO-TEMPORAL PARAMETERS AUTHORS: Zenon Medina-Cetina International Centre for Geohazard / Norwegian Geotechnical Intitute Roger
Lattice Boltzmann simulations on heterogeneous CPU-GPU clusters
Lattice Boltzmann simulations on heterogeneous CPU-GPU clusters H. Köstler 2nd International Symposium Computer Simulations on GPU Freudenstadt, 29.05.2013 1 Contents Motivation walberla software concepts
A High Throughput String Matching Architecture for Intrusion Detection and Prevention
A Hig Trougput tring Matcing Arcitecture for Intruion Detection and Prevention Lin Tan, Timoty erwood Appeared in ICA 25 Preented by: aile Kumar Dicuion Leader: Max Podleny Overview Overview of ID/IP ytem»
The Square Kilometre Array and the radio/gamma-ray connection toward the SKA era
The Square Kilometre Array and the radio/gamma-ray connection toward the SKA era Marcello Giroletti INAF Istituto di Radioastronomia 12th AGILE Workshop Roma, 8/5/2014 What s in this talk: SKA basics and
Real-time identification of sliding friction using LabVIEW FPGA
Clemon Univerity TigerPrint Publication Automotive Engineering 6-26 Real-time identification of liding friction uing LabVIEW FPGA Laine Mear Clemon Univerity, mear@clemon.edu Jeannie S. Falcon IEEE Thoma
2.7.2 Limits to Parallelism
Chapter 2 Exercie 53 The 1990 will find a broader ue of multiproceor a the peed of individual proceor reache the limit of metal interconnection. The highet utainable clock rate for metal interconnection
Learning Multiplicative Interactions
CSC2535 2011 Lecture 6a Learning Multiplicative Interaction Geoffrey Hinton Two different meaning of multiplicative If we take two denity model and multiply together their probability ditribution at each
Spring 2014 EE 445S Real-Time Digital Signal Processing Laboratory. Homework #0 Solutions on Review of Signals and Systems Material
Spring 4 EE 445S Real-Time Digital Signal Proceing Laboratory Prof. Evan Homework # Solution on Review of Signal and Sytem Material Problem.. Continuou-Time Sinuoidal Generation. In practice, we cannot
HERA Memo 51: System Noise from LST Di erencing March 17, 2017
HERA Memo 51: System Noise from LST Di erencing March 17, 2017 C.L. Carilli 1,2 ccarilli@aoc.nrao.edu ABSTRACT I derive the visibility noise values (in Jy), and the system temperature for HERA, using di
Reliability Analysis of Embedded System with Different Modes of Failure Emphasizing Reboot Delay
International Journal of Applied Science and Engineering 3., 4: 449-47 Reliability Analyi of Embedded Sytem with Different Mode of Failure Emphaizing Reboot Delay Deepak Kumar* and S. B. Singh Department
The Square Kilometre Array: An international project to realize the world s
The Square Kilometre Array: An international project to realize the world s The The Square Square The Kilometre Square Kilometre Kilometre Array: Array: An Array international An largest radio telescope
ALMA Development Program
ALMA Development Program Jeff Kern CASA Team Lead Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array Opportunities for Software
The type 3 nonuniform FFT and its applications
Journal of Computational Phyic 206 (2005) 1 5 Short Note The type 3 nonuniform FFT and it application June-Yub Lee a, *, Lelie Greengard b a Department of Mathematic, Ewha Woman Univerity, 11-1 Daehyundong,
e e-03. which is distributed with standard chandra processing. visual inspection are included.
1 SUMMARY 1 SNR 0505-67.9 1 Summary Common Name: DEM L71 Distance: 50 kpc (distance to LMC, Westerlund(1990) ) Center of X-ray emission (J2000): ( 05 05 42.0, -67 52 39.8 ) X-ray size: 86 x 74 Description: