LOFAR. The Low-Frequency Array. (tri-talk franglais)
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1 LOFAR The Low-Frequency Array (tri-talk franglais)
2 LOFAR = Interféromètre de Réseaux Phasés Δf = (10) MHz A e ~ m 2, Cœur + Stations (77 total)
3 Caractéristiques techniques : imagerie haute résolution (~1-10 ) grand champ (plusieurs ) multi-fréquences / multi-faisceaux (8 4 MHz) haute sensibilité ( mjy), polarisation complète (4 paramètres de Stokes) résolutions 1 msec 1 khz gain de 1-2 ordres de grandeur en sensibilité & résolution / instruments existants 1 er télescope BF généraliste et 1 er spectro-imageur à f 100 MHz
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6 Objectifs scientifiques : Cosmologie / Réionisation (Groningen) Surveys profonds all-sky/galaxies (Leiden) Transients = Souces variables/sporadiques (Amsterdam) Rayons cosmiques (Nijmegen) Physique solaire & spatiale
7 LOFAR initial test station prototype (ITS) : 500 Second All-Sky Map LOFAR will have 1000 times higher resolution, 100 times higher sensitivity, and 10 5 times more integration time.
8 Septembre 2006 : Core Station # : début opérations 2008 : fonctionnement nominal Formation des SWG : Transients Key Project : (1) Jets (2) Pulsars (3) (exo)planètes (4) Étoiles/Flare stars Expansion Européenne : Allemagne (GLOW), Suède (LOIS), UK, France, Italie?, Pologne?
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10 Jupiter s magnetosphere
11 Jovian high latitude radio emissions
12 Jovian high latitude radiosources
13 Main aurora
14 Io-induced emissions
15 Io-induced emissions
16 Radio imaging of high latitude sources (Jupiter/Ulysses) ~40
17 Radio imaging of high latitude sources (Saturn/Cassini) [Cecconi et al., 2006]
18 Radio imaging of Jupiter with ~1" resolution from Earth Surface magnetic field mapping (maximum cyclotron frequency) Lead angle (physics) of Io-Jupiter interaction Radio beaming angle physics of generation process Direct detection (& energetics) of Ganymede, Europe, Callisto-Jupiter radio emission Electron bunches & electric fields (potential drops) along Io flux tube torus Ne vs longitude via Faraday rotation «modulation lanes» due to diffraction by torus? multi-wavelength correlations (Radio, UV, IR, X)
19 Radio imaging of Jupiter with ~1" resolution from Earth Surface magnetic field mapping (maximum cyclotron frequency) Lead angle (physics) of Io-Jupiter interaction Radio beaming angle physics of generation process Direct detection (& energetics) of Ganymede, Europe, Callisto-Jupiter radio emission Electron bunches & electric fields (potential drops) along Io flux tube torus Ne vs longitude via Faraday rotation «modulation lanes» due to diffraction by torus? multi-wavelength correlations (Radio, UV, IR, X)
20 dipole
21 Radio imaging of Jupiter with ~1" resolution from Earth Surface magnetic field mapping (maximum cyclotron frequency) Lead angle (physics) of Io-Jupiter interaction Radio beaming angle physics of generation process Direct detection (& energetics) of Ganymede, Europe, Callisto-Jupiter radio emission Electron bunches & electric fields (potential drops) along Io flux tube torus Ne vs longitude via Faraday rotation «modulation lanes» due to diffraction by torus? multi-wavelength correlations (Radio, UV, IR, X)
22 The Io-B scenario #2 Observer & source motion
23 Radio imaging of Jupiter with ~1" resolution from Earth Surface magnetic field mapping (maximum cyclotron frequency) Lead angle (physics) of Io-Jupiter interaction Radio beaming angle physics of generation process Direct detection (& energetics) of Ganymede, Europe, Callisto-Jupiter radio emission Electron bunches & electric fields (potential drops) along Io flux tube torus Ne vs longitude via Faraday rotation «modulation lanes» due to diffraction by torus? multi-wavelength correlations (Radio, UV, IR, X)
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25 Radio imaging of Jupiter with ~1" resolution from Earth Surface magnetic field mapping (maximum cyclotron frequency) Lead angle (physics) of Io-Jupiter interaction Radio beaming angle physics of generation process Direct detection (& energetics) of Ganymede, Europe, Callisto-Jupiter radio emission Electron bunches & electric fields (potential drops) along Io flux tube torus Ne vs longitude via Faraday rotation «modulation lanes» due to diffraction by torus? multi-wavelength correlations (Radio, UV, IR, X)
26 adiabatic motion v 2 // = v2 - v 2 = v2 - µ.f ce [Hess et al., 2006] v 2 // 1 kev potential drop f ce
27 Radio imaging of Jupiter with ~1" resolution from Earth Surface magnetic field mapping (maximum cyclotron frequency) Lead angle (physics) of Io-Jupiter interaction Radio beaming angle physics of generation process Direct detection (& energetics) of Ganymede, Europe, Callisto-Jupiter radio emission Electron bunches & electric fields (potential drops) along Io flux tube torus Ne vs longitude via Faraday rotation «modulation lanes» due to diffraction by torus? multi-wavelength correlations (Radio, UV, IR, X)
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29 Radio imaging of Jupiter with ~1" resolution from Earth Surface magnetic field mapping (maximum cyclotron frequency) Lead angle (physics) of Io-Jupiter interaction Radio beaming angle physics of generation process Direct detection (& energetics) of Ganymede, Europe, Callisto-Jupiter radio emission Electron bunches & electric fields (potential drops) along Io flux tube torus Ne vs longitude via Faraday rotation «modulation lanes» due to diffraction by torus? multi-wavelength correlations (Radio, UV, IR, X)
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31 Radio imaging of Jupiter with ~1" resolution from Earth Surface magnetic field mapping (maximum cyclotron frequency) Lead angle (physics) of Io-Jupiter interaction Radio beaming angle physics of generation process Direct detection (& energetics) of Ganymede, Europe, Callisto-Jupiter radio emission Electron bunches & electric fields (potential drops) along Io flux tube torus Ne vs longitude via Faraday rotation «modulation lanes» due to diffraction by torus? multi-wavelength correlations (Radio, UV, IR, X)
32 Radio imaging of Jupiter with ~1" resolution from Earth Surface magnetic field mapping (maximum cyclotron frequency) Lead angle (physics) of Io-Jupiter interaction Radio beaming angle physics of generation process Direct detection (& energetics) of Ganymede, Europe, Callisto-Jupiter radio emission Electron bunches & electric fields (potential drops) along Io flux tube torus Ne vs longitude via Faraday rotation «modulation lanes» due to diffraction by torus? multi-wavelength correlations (Radio, UV, IR, X) LOFAR fast imaging should provide NEW information about Jupiter's magnetospheric structure and dynamics
33 Radio imaging of Jupiter Radiation Belts [de Pater, P&SS, 2004]
34 Radio imaging of Jupiter Radiation Belts [de Pater, P&SS, 2004] high spatial resolution imaging 240 MHz («low» energy e-) over a large relative bandwidth variation with time and solar wind parameters origin and transport of energetic e- in Jupiter s inner radiation belts : pitch-angle scattering by PW, coulomb scattering, interaction with dust? + emission from Saturn, Uranus, Neptune?
35 Instrumental constraints (for magnetospheric radio emissions) Arcsec (1"-4") resolution imaging of planetary disk environment (~10, including Io s plasma torus). Frequency range = MHz (instantaneous). Spectral resolution = khz. Time integration ~ msec (typical Jovian burst duration). Full polarization. Emission intense, with bursts up to Jy, dynamic range db. Observation sequences of minutes to tens of minutes (Jovian radio «storm» duration, source tracking), at intervals of days/weeks. Partial predictability of Jovian radio emission. RFI mitigation required + quiet ionosphere better.
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37 Radio decameter VLBI tests Target resolution : ~1, 1 msec, 1 30 MHz Aim: LF radioastronomy with high angular resolution Influence of ionosphere : Loss of phase coherency, dispersion in frequency, Faraday rotation, refraction Limitation of coherence time, usable spectral band, self-cal capabilities Previous studies 34 MHz, baseline 4300 km [Dulk, Astrophys. J., 1970] 81.5 MHz, baselines 1500 km [Hartas et al., MNRAS, 1983] 20 & 25 MHz, baseline 900 km [Megn et al., Radio Phys. and Radio Astron., 1997] Problematic : % de feasibility as a function of f, t?
38 Observation of Jupiter s millisecond radio bursts LOFAR-ITS [H. Falcke, A. Nigl, et al.] + NDA [P. Zarka, L. Denis, et al.] (11/2005) MHz, baseline ~750 km, remote control ITS, synchro GPS/crystal, snapshots of 6.7 sec radiosource ~point-like, Jy, sporadic, wave packets ~0.1 msec cross-correlation of dynamic spectra data time-stamping waveforms cross-correlation OK!
39 Instruments: ITS LOFAR Initial Test Station 60 (30x2) dipoles < 40 MHz digitization (80 Msamples) storage (1GB = 6.7s) offline time-beamforming
40 Instruments: NDA Nancay Decametric Array 72 spirals (RH wounded) < 40 MHz analog beamforming digitization (80 Msamples) storage
41 Jupiter - Io Alfvén waves Io Flux Tube s-burst sources angle of lead Io Torus
42 Jupiter - Io: Frequency Window ~10 MHz ionospheric cutoff (cyclotron radiation) 40 MHz cyclotron frequency (synchrotron radiation)
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44 22/6/2004
45 30/11/2005
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53 ~1 ITS time base (can be corrected) submitted
54 Conclusions Prospective en France depuis 2002 Atelier fondateur au CIAS-Meudon, 3/2006 : «LOFAR : Radioastronomie basses fréquences à une résolution de quelques secondes d'arc (Astrophysique, Cosmologie et Astroparticules) Vers une participation française» ~40 participants Argumentaire scientifique FLOW (M. Tagger & al.) Demande INSU 10/2006 pour 1 station à Nançay (M. Tagger & PZ) Études à venir pour une «super-station» TKP : (exo-)planets SWG : PZ, G. Woan, J.-M. Griessmeier, D. Stam, H. Spreeuw, T. Bastian, I. de Pater. Observations VLBI CS-1 / Nançay (soumises)
55 Station : cost ~600 k + optical fiber link 3 Gbps Low Band High Band 60 m 50 m
56 European Expansion Current discussions: Germany ~12 stations UK ~2-3 stations Italy ~2 stations France ~1 station? Poland ~1 station?
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