Radio interferometry in astronomy: a view into the XXI century
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1 Radio interferometry in astronomy: a view into the XXI century Lecture 1 Introduction and basics of (radio) interferometry Leonid Gurvits Joint Institute for VLBI in Europe, Dwingeloo, The Netherlands Delft University of Technology, Faculty of Aerospace Engineering, The Netherlands
2 Radio telescopes the most sensitive detectors of electro-magnetic waves Chance discovery of cosmic radio emission by Karl Jansky, 1933 XVI IAG/USP School, Itatiba LIG
3 The beginning: 05 May 1933 Karl Jansky XVI IAG/USP School, Itatiba LIG
4 Let s be acquainted... XVI IAG/USP School, Itatiba LIG
5 Joint Institute for VLBI in Europe Founded in 1993 as a central institute of the European VLBI (Very Long Baseline Interferometry) Network (EVN); EVN unifies 14 institutes in 12 countries; JIVE develops and operates the EVN Data Processor a purpose-built digital facility (correlator), the world most advanced VLBI data processor; JIVE provides to the world-wide community of VLBI observers ( users ) JIVE staff conduct cutting edge research in astrophysics and space science
6 State-of-the-art data processing of (very large) data streams (~20 Gbit/s, multi Tbit/experiment) JIVE: areas of expertise Operations and management of (globally) distributed networks of radio astronomy facilities Astrophysics and Space Science Management of (large) international collaborations (incl. FP 2-7 projects) XVI IAG/USP School, Itatiba LIG
7 EVN & JIVE: user-oriented facility Science done by world-wide user community Open sky policy Access to the EVN via peer-reviewed proposals Access by European users supported via EC FP7 programme RadioNet JIVE provides support to (potential) users Proposals Observations Data processing Users are NOT supposed to be black-belt VLBIers! New users are most welcome!
8 The European VLBI Network XVI IAG/USP School, Itatiba LIG
9 JIVE smiles 2011 XVI IAG/USP School, Itatiba LIG
10 In lieu of self-introduction : Aerospace Engineering, (Spaceflight Control & Dynamics) Moscow Aviation Institute : Astrophysics, Moscow State University : Dept of Astrophysics, Space Research Institute, Moscow : Astro Space Center, Lebedev Physical Institute, Moscow : NAIC, Arecibo Observatory Cornell University, Puerto Rico Since 1994: Joint Institute for VLBI in Europe Since 2011: Faculty of Aerospace Engineering, Delft University of Technology XVI IAG/USP School, Itatiba LIG
11 A glimpse of interferometry XVI IAG/USP School, Itatiba LIG
12 Radio interferometry: a one-slide tutorial Michelson & Young, 1890 s: measurements of stars diametres Synthesis of large apertures (by poor and curious people) D D Large aperture high sensitivity B B Large size high angular resolution Very Long Baseline Interferometry (VLBI) the ultimate angular resolution baselines up to 200,000 km XVI IAG/USP School, Itatiba LIG
13 Young s double-slit interferometer, 1895 XVI IAG/USP School, Itatiba LIG
14 Young s experiment 100 years later XVI IAG/USP School, Itatiba LIG
15 Intereferometer fundamentals XVI IAG/USP School, Itatiba LIG
16 History of radio interferometry (a subjective view) Sea interferometer XVI IAG/USP School, Itatiba LIG
17 From interferometer to aperture synthesis Sir Martin Ryle, Nobel Prize in Physics, 1970 XVI IAG/USP School, Itatiba LIG
18 How (VLB) Interferometry works? VLBI in nutshell Observables: Amplitude Phase Delay Delay rate Atomic clock Cross correlation Signal detection Difference in time of arrival Atomic clock telescopes in different locations (countries, continents) data relayed or recorded on magnetic media and transported to a central facility data processed ( correlated ) Data rate: ~1 Gbps per RT; Total: ~ TB per experiment XVI IAG/USP School, Itatiba LIG
19 JIVE: the heart of EVN XVI IAG/USP School, Itatiba LIG
20 From recording to real-time VLBI: e-vlbi In line with ICT developments Boosted with EC FP6 EXPReS and now continues with FP7 NEXPReS Help solve last mile problem at telescopes Work with NRENs on robust connectivity Push to 1 Gb/s/telescope and beyond Transition from EVN to e-evn Now an operational facility Guaranteed 10 x 24 h per year Flexible ways to get into e-vlbi Request e-vlbi for fast response Or for triggered proposals Short requests <2hr Targets of Opportunities Produces excellent science! e-evn an SKA pathfinder Express Production Real-time e-vlbi Service XVI IAG/USP School, Itatiba LIG
21 e-vlbi: the end of traditional VLBI Feb 2010: uninterrupted 24 hours e EVN run with ~8 Gbps incoming rate XVI IAG/USP School, Itatiba LIG
22 RADIO INTERFEROMETRIC IMAGING OR DOING THE MAGIC...
23 Golden formulae of interferometry & aperture synthesis 1. Van Cittert Zernike theorem (optics analogy): Visibility function Brightness distribution 2. Correlation, convolution and Wiener-Khinchin theorem: r( V ) V lim T 1 2T * V1 T ( t) V2T ( t ) dt F( V ) F( V * 1T 2T Fourier 1T 2T ) XVI IAG/USP School, Itatiba LIG
24 Interferometric imaging basics Interferometer response to a source of brightness distribution I(l,m): Ideally, in 2D-approximation: Difficulties with the above integral: - Incomplete sampling of the uv-plane; - Errors, additive and multiplicative, in measuring V(u,v) XVI IAG/USP School, Itatiba LIG
25 The first recipe of image reconstruction XVI IAG/USP School, Itatiba LIG
26 Fourier inversion 1 XVI IAG/USP School, Itatiba LIG
27 Dirty imaging The dirty image is a sum of harmonic functions with amplitudes and relative phases taken froim the visibility function (as measured). XVI IAG/USP School, Itatiba LIG
28 Deconvolution XVI IAG/USP School, Itatiba LIG
29 Effect of uv-sampling Good (dense) uv-sampling small sidelobes Bad (sparse) uv-sampling large sidelobes XVI IAG/USP School, Itatiba LIG
30 Deconvolution realities Each point seen in the dirty image is a product of the true image feature (a delta function with the correct amplitude) and the properly positioned and scaled dirty beam XVI IAG/USP School, Itatiba LIG
31 A-priori knowledge is always helpful XVI IAG/USP School, Itatiba LIG
32 (A glimpse on) UV-weighting Natural weighting helps to minimize the noise in the dirty image: But, this results in overweighting the uv areas with high sampling density (usually near the origin); in turn it means throwing out the baby long baselines are suppressed Uniform weighting is used to minimize the rms sidelobes of dirty beams i.e. correction for local sampling density): XVI IAG/USP School, Itatiba LIG
33 CLEAN (see TMS and references therein) XVI IAG/USP School, Itatiba LIG
![Closure relations in VLBI Measurables: V ( u, v) A( u, v) exp[ i ( u, v)] but (, v) ( u, v) ( u, v, t); ( u, v, t) 1 m u t Closure phase: 123 123 12 23 31 = invariant(instrumental effects) 1 2 A 12](/docs-images/82/85157702/images/34-0.jpg "23 Closure amplitude: 1234 A A 12 13 A A A = invariant(instrumental effects) 1234 A 34 24 A 13 31 A 14 A 24 4 3 uv-sampling ( uv-coverage ) is incomplete XVI IAG/USP School, Itatiba LIG 05-09.11.")
34 Closure relations in VLBI Measurables: V ( u, v) A( u, v) exp[ i ( u, v)] but (, v) ( u, v) ( u, v, t); ( u, v, t) 1 m u t Closure phase: = invariant(instrumental effects) 1 2 A Closure amplitude: 1234 A A A A A = invariant(instrumental effects) 1234 A A A 14 A uv-sampling ( uv-coverage ) is incomplete XVI IAG/USP School, Itatiba LIG
35 Vivat closure phase (Jennison, 1953) XVI IAG/USP School, Itatiba LIG
36 Practical recipe 2 XVI IAG/USP School, Itatiba LIG
37 Recipe 3 XVI IAG/USP School, Itatiba LIG
38 Selfcalibration XVI IAG/USP School, Itatiba LIG
39 Example (from Wilkinson, VLBI Technologies, Felli & Spencer, 1989) XVI IAG/USP School, Itatiba LIG
40 Selfcalibration (hybrid mapping) XVI IAG/USP School, Itatiba LIG
41 Is a reconstructed image unique? XVI IAG/USP School, Itatiba LIG
42 How does look the final product (of continuum VLBI) The weakest EVN target detected to date: S 1.4 = 1.1 mjy VLBI image (right panel): 770 μjy/beam Frey et al, 2003, 2005, MNRAS XVI IAG/USP School, Itatiba LIG
43 VLBI imaging practice Exercise it; theoretical VLBI imaging is pointless Available software packages: Astronomical Imaging Processing System (AIPS), supported by National Radio Astronomy Observatory (NRAO) Differential Mapping softare (Difmap), supported (voluntarily) by CalTech Both packages are free (requires registration) Get your hands on experience! Ya. Zeldovich: What s the use to study for the future? Find a problem and solve it; this way you will learn something for real. XVI IAG/USP School, Itatiba LIG
44 Useful reading on radio interferometry B. Burke, F. Graham-Smith An introduction to Radio Astronomy A.R. Thompson, J.M. Moran, G.W. Swenson, Interferometry and Synthesis in Radio Astronomy Radio Astronomy from Karl Jansky to Microjansky, eds. L.I. Gurvits, S. Frey, S.Rawlings, EDP Sciences, 2005 K. Rohlfs, T.L. Wilson Tools of Radio Astronomy XVI IAG/USP School, Itatiba LIG
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