Introduction to Radio Interferometers Mike Garrett (ASTRON/Swinburne)
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1 Introduction to Radio Interferometers Mike Garrett (ASTRON/Swinburne) ERIS School - Bonn - Sep 11, 2007.
2 Overview of Lecture Early radio astronomy what makes radio astronomy "special"! Radio Interferometry early days and motivation Interferometer arrays metre, cm, mm and sub-mm wavelengths Types of object we can study - science The Future is VERY, VERY, VERY bright!
3 Early days of radio astronomy 1932 Discovery of cosmic radio waves (Karl Jansky) v=25mhz; dv=26khz Galactic centre
4 The first radio astronomer (Grote Reber) Built the first radio telescope "Good" angular resolution Good visibility of the sky Detected Milky Way, Sun, Cas-A, Cyg-A, 160 & 480 MHz (ca ). Published his results in ApJ Multi-frequency observations
5 The first radio astronomer (Grote Reber) Built the first radio telescope "Good" angular resolution Good visibility of the sky Detected Milky Way, Sun, Cas-A, Cyg-A, 160 & 480 MHz (ca ). Published his results in ApJ Multi-frequency observations
6 The things that make radio astronomy "special" Reber's multi-frequency observations revealed the non-thermal nature of radio emission (UNEXPECTED!)
7 The things that make radio astronomy "SPECIAL" Rebers multi-frequency observations revealed the non-thermal nature of radio emission (UNEXPECTED!) Dawn of High-energy astrophysics!
8 A new transparent window on the Universe Radio window covers 5 decades of freq/wavelength: SPECIAL: Radio waves largely unaffected by dust... Can observe Day and Night! Studies of the Early Universe possible.
9 Radio Spectral-lines 1944: van der Hulst predicts discrete 1420 MHz (21 cm) emission from neutral Hydrogen (HI). Detected by Ewen & Purcell (1951):
10 SPECIAL - HI - most abundant element in the Universe! Gas DYNAMICS: Scale/Structure of the Milky Way Tracing Dark Matter in other galaxies The Dark Ages...
11 's: Construction of Large Telescopes cm wavelengths: NL UK Aus USA USA R.W. Porcas
12 The need for better ANGULAR RESOLUTION Ang. resolution: arcseconds Human eye: 17 arcsecs Effelsberg 21cm: 440 arcsecs (8 arcmins)
13 The answer RADIO INTERFEROMETRY Ang. resolution: B B = Baseline i.e. telescope separation For 2 telescopes separated by 30 km ==> Ang. resolution: ~ 1 arcsecond - MUCH BETTER! Wave-fronts from distant source perfectly in phase Tex Tex B
14 RADIO INTERFEROMETRY & Correlation
15 RADIO INTERFEROMETRY & Correlation
16 Interferometry tries to sythesise a GIANT telescope from lots of small ones:
17
18 Earth rotation helps too (Ryle): Projected Baseline changes for source
19 Earth rotation helps too (Ryle): Projected Baseline changes for source
20 Earth rotation helps too (Ryle): Projected Baseline changes for source
21 The first radio interferometers Early interferometer arrays pioneered by UK and Australian astronomers: 1-mile telescope (1963) Motivation was to identify radio sources with plausible optical counterparts...
22 3c273 - first AGN (Hazard, Schmidt et al) 1963 Stellar objects???? Redshifted lines z=0.2 => cosmological distance objects 1000 x more luminous that Milky-Way
23 Westerbork Synthesis Radio Telescope 14 x 25 metre telescopes, 91 baselines, 3km baseline. Neutral Hydrogen (HI) Stars
24 The SPECIAL nature of the radio sky Nearly all the bright radio sources are extra-galactic and EXOTIC - AGN (Quasars, radio galaxies etc.) Nearly all are located at cosmological distances (z ~ 1) c.f. optical sky (z=0 for naked-eye objects!) Huge excess of faint sources: ==> first evidence of rapid cosmic evolution...! Non-thermal emission - synchrotron mechanism ==> violent Universe powered by gravitation rather than fusion.
25 Radio sources also discovered to be highly variable on time scales of hours or less: ==> very compact objects - scales ~ solar system. At z=1, 1 arcsecond corresponds to ~ 10 kpc (30,000 lt years). Need for much HIGHER RESOLUTION (baselines ~ Earth diameter, km)
26 Pioneering long-baseline interferometry show many Radio sources unresolved on sub-arcsecond scales
27 1967: Very Long Baseline Interferometry 1000x better resolution than Optical telescopes - its so easy!
28
29 Superluminal motion discovered - Whitney et al AGN models
30 Weighing the black hole in NGC Myoshi et al velocity and motion of water maser gas clouds permit: Mass of Black hole ~ 10^7 Msun. DISTANCE of NGC 4258 => Ho VLBA 22 GHz
31 VLBI Brings the Universe to life...
32 VLBI Brings the Universe to life...
33 The Very Large Array (VLA) Wide Frequency range up to 50 GHz 25-m dimater antennas on rails - Baseline 1-36 km Good sensitivity ~ 6uJy in 12 hrs (8.4 GHz) see
34 Other Interferometer Arrays MERLIN VLBA, EVN & Global and mm-vlbi ATCA IRAM PdB SMA
35 European Radio Telescope Resources (incl. single dishes) )%$15#"# (3=+ (3=+ ;#./E0'F% (GH+ N#/.#"&'"1 (8D+! " # $ % $ # & ' ( $ # ) * + +, % % J7;C (39+ =:'$1%: (3=+ C'"4: ()D+ 3"456% (78+ B#??'"I (3=+ >??#@/&#"A (B>+ ;1< (3=+ D'F#@@ (3=+ P:/-@- <M5 (9>+ P:/-@- <Q5 (9>+!"#$%&' ()*+ 9#/0-: ( &"%IA# (3=+ N#..O#@@ (B>+,-".#&##/.0'#1 (2!+ *'&@#I' (>9+ ;#I%$%:- (HC+ =>K K#&#/ (>9+ H*!; LM5 (>9+ H*!; )IU (G*+ 8'.' (HC+ >S8 -:.#::-/ >S8 -:IT'" ;>*DH8 -:.#::-/ ;>*DH8 -:.#::-/ >S8 -:IT'" /.-:I -@':# /.-:I -@':# -:.#::-/ '" -""-R/
36 Radio Sources in the Solar system Thermal emission from the quiet sun Bi-static radar image of Mercuty VLA VLA-Goldstone Synchrotron emission from Jupiter (before and after comet SL9 impact VLA
37 Galactic Centre Galactic centre completely obscured in optical
38 Galactic PNe, SNRs, Novas, PSRs
39 Other Galactic sources (stars, exo-solar systems, masers X-ray binaries)
40 Nearby Galaxies (cont & HI) - WSRT - Braun et al.
41 HI in Galaxies - emission & Absorption Dynamics of stars, neutral gas (HI) and ionised gas: Morganti et al HI absorption against bright AGN reveals outflow and inflow of gas Morganti et al. 2006
42 The magnetic Universe... Polarised Radio emission: SPECIAL: Just about the only way to study magnetic fields in the ISM, in galaxies, & AGN
43 AGN - Imaging on all scales - M87 an example Kitt Peak 2-m optical mm-vlbi ~ 80kpc VLBI ~ sub-pc
44 Many other examples of powerful radio galaxies Powerful radio galaxies usually associated with Elliptical galaxies
45 Extra-galactic Zoo
46 The silent majority - faint radio sources As you go deeper in the radio, the Universe comes towards you! Mostly moderate redshift star-forming galaxies ==> radio emission powered by massive star formation. AGN monster
47 Resolution still important for these faint sources... Star forming galaxies - radio emission on galactic/sub-galactic scale e.g. M82 x60 Extended emission on kpc scale SNe and SNR on tens of pc.
48 Radio-FIR Spectral Energy Distribution of "Normal" Galaxies (e.g. Milky Way, M82): AGN SF FIR-Radio Correlation Both Radio and FIR (sub-mm at high reshift) are sensitive measures sures of MASSIVE Star formation in the local and distant galaxies. Radio and sub-mm observations closely allied in the study of the DUSTY High-z Universe.
49 Going even deeper... microjy source population A few areas of sky studied at ujy levels (e.g. HDF-N, Muxlow et al. 2005) MicroJy sensitivity Universe begins to move away from us - high-z The fainstest radio sources dust obscured - no optical id - Sub-mm associations - Good ASTROMETRY - SPECIAL
50 Radio Interferometry & Cosmology CMB experiments - interferometry offers many advantages... SPECIAL: Noise is independant for each antenna - disappears during correlation e.g. RFI - Gravitational lensing - Ho High resolution of radio interferometers makes them idea for detecting and imaging resolved gravitational lens phenomena EVN
51 CLASS Gravitational lens surveys Radio surveys ideal for finding lenses... Source population typically at high-z Seperation ~ 1 arcsec Flat spectrum radio sources rare. Gravitational lensing - also MAGNIFIES sources
52 Lenses as giant cosmic magnifying glasses: Magnification permits us to detect comologically distant star forming galaxies e.g. Garrett et al. 2005; Berciano Alba et al. (2007); Garrett et al. (in prep). WSRT 20cm IRAM, Kneib et al Spitzer 24u Total magnification of cluster is x45 Source is a intrinsically faint, z=2.5 SMG & ujy radio source - undetectable without the lens..
![More [lensed] distant star-forming](/docs-images/86/94427610/images/53-2.jpg "galaxies Sub-mm VLA Berciano alba et al.")
53 More [lensed] distant star-forming galaxies Sub-mm VLA Berciano alba et al. (2007)
54 Most luminous Ly-break Galaxy (8 o'clock lens) WSRT 6cm Garrett et al. in prep (2007)
55 The Future... Activity is intense! Many telescope upgrades in progress: EVLA, e-merlin, e-vlbi (2009) Many NEW telescope arrays under construction (pathfinders for the Square Km Array): ATA, LOFAR, MWA, ASKAP, MeerKAT. Key issues are cost and field-of-view: ATA SKA
56 Aperture Arrays - multiple, independent, simultaneous beams (LOFAR)
57 LOFAR (ASTRON) E-LOFAR Expansion of LOFAR into Europe 40 stations Current status: Germany ~12 stations UK ~2-3 stations Italy ~2 stations France ~1 station? Other EVN sites
58 LOFAR first images (see Ger de Bruyn's lecture) Amazing Field of view - superb survey instrument - if we can calibrate it!
59 Understanding the Universe Amazing Field of view - superb survey instrument - if we can calibrate it!
60 Loeb et al Maybe possible to detect leakage radiation from neaby Extra-terrestrial Civilisations...
61 Stacking G-type stars (NVSS) 3uJy noise level ==> leakage from planet >> G-type stars
62 There has never been a better time to do... RADIO ASTRONOMY!
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