Radar interferometric imaging for the EISCAT Svalbard Radar
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1 Radar interferometric imaging for the EISCAT Svalbard Radar Tom Grydeland 1,2 Jorge L. Chau 3 César La Hoz 1 1 Department of Physics, University of Tromsø 2 Currently at the University Centre on Svalbard 3 Jicamarca Radio Observatory XXVIII URSI General Assembly, Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
2 Outline 1 Scientific rationale Naturally enhanced ion-acoustic echoes PMSE Meteors 2 Antenna construction and testing 3 Antenna configuration and calibration First deployment ( ) Full deployment Phase calibration 4 Experiences at Jicamarca Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
3 Scientific rationale Naturally enhanced ion-acoustic echoes Associated with Langmuir turbulence in the auroral ionosphere power spectra in db (42m ant), 0.2 second integration, starting at range [km] range [km] frequency [khz] Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
4 Scientific rationale Naturally enhanced ion-acoustic echoes Connection to visible aurora on small spatial and temporal timescales (ODIN auroral imager) upshifted, alt > 529 km b2 downshifted, alt > 529 km Line b upshifted, alt < 529 km c (center) downshifted, alt < 529 km Line a b1 b2 (Grydeland et al., 2004; Blixt et al., 2005) lag time [s] b1 Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
5 Scientific rationale Naturally enhanced ion-acoustic echoes Shown to arise in narrow filaments (Grydeland et al., 2003, 2004) power spectra [db], 42m ant power spectra [db], 32m ant range [km] max structure size vs coherence at different ranges 700 km 500 km 300 km 100 km range [km] coherence cross phase [rad] structure size [km] frequency [khz] frequency [khz] coherence Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
6 Scientific rationale Naturally enhanced ion-acoustic echoes Contributions from imaging in this application disambiguate position for up-/downshifted enhancement pinpoint relation to visible auroral forms decide whether filaments are cylindrical or sheet-like (relation to satellite observations, e.g. by Ørsted) Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
7 Scientific rationale Naturally enhanced ion-acoustic echoes Contributions from imaging in this application disambiguate position for up-/downshifted enhancement pinpoint relation to visible auroral forms decide whether filaments are cylindrical or sheet-like (relation to satellite observations, e.g. by Ørsted) Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
8 Scientific rationale Naturally enhanced ion-acoustic echoes Contributions from imaging in this application disambiguate position for up-/downshifted enhancement pinpoint relation to visible auroral forms decide whether filaments are cylindrical or sheet-like (relation to satellite observations, e.g. by Ørsted) Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
9 Scientific rationale Polar Mesospheric Summer Echoes (PMSE) ESRAD at 52 MHz, Yu et al., (2001) Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
10 Scientific rationale Polar Mesospheric Summer Echoes (PMSE) Contributions from imaging in this application help remove space/time ambiguity shed light on the scattering process? Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
11 Scientific rationale Polar Mesospheric Summer Echoes (PMSE) Contributions from imaging in this application help remove space/time ambiguity shed light on the scattering process? Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
12 Scientific rationale Meteors Jicamarca at 50 MHz, Chau and Woodman (2004) Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
13 Scientific rationale Meteors Contributions from imaging in this application work on arrival angle of meteors done at Jicamarca, close to the equator majority of meteors come from the apex ESR at high latitude sees larger section of the ecliptic plane Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
14 Scientific rationale Meteors Contributions from imaging in this application work on arrival angle of meteors done at Jicamarca, close to the equator majority of meteors come from the apex ESR at high latitude sees larger section of the ecliptic plane Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
15 Scientific rationale Meteors Contributions from imaging in this application work on arrival angle of meteors done at Jicamarca, close to the equator majority of meteors come from the apex ESR at high latitude sees larger section of the ecliptic plane Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
16 Antenna construction and testing 18-element Yagi antennas UHF TV antennas, band db gain impedance matched to 50 Ω Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
17 Antenna construction and testing 18-element Yagi antennas UHF TV antennas, band db gain impedance matched to 50 Ω Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
18 Antenna construction and testing 18-element Yagi antennas UHF TV antennas, band db gain impedance matched to 50 Ω Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
19 Antenna construction and testing Combining elements into an array Created from railing/scaffolding components Inter-element distance 1.2 m, or 2λ Inter-element distance can be varied Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
20 Antenna construction and testing Combining elements into an array Created from railing/scaffolding components Inter-element distance 1.2 m, or 2λ Inter-element distance can be varied Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
21 Antenna construction and testing Combining elements into an array Created from railing/scaffolding components Inter-element distance 1.2 m, or 2λ Inter-element distance can be varied Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
22 Antenna construction and testing Combining elements into an array Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
23 Antenna construction and testing Measuring the antenna diagram Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
24 Antenna construction and testing Measuring the antenna diagram From this, the beam width (FWHM) is 7.1, in both polarizations Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
25 Antenna construction and testing Surveying the site Photo by A. P. van Eyken Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
26 Antenna construction and testing Analog electronics Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
27 First deployment ( ) one antenna, 4 4 array of 18-element Yagi antennas 15.5 db gain per antenna, 25.5 db gain total First light March 2005 Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
28 First deployment ( ) one antenna, 4 4 array of 18-element Yagi antennas 15.5 db gain per antenna, 25.5 db gain total First light March 2005 Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
29 First deployment ( ) one antenna, 4 4 array of 18-element Yagi antennas 15.5 db gain per antenna, 25.5 db gain total First light March 2005 Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
30 First deployment ( ) Antenna configuration and visibility samples Positions, 1 antenna, uniform Vis. samples, 1 antenna, uniform Metres North Metres East Metres North Metres East Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
31 First deployment ( ) Satellite echo in three antennas Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
32 Full deployment Antenna configuration and visibility samples Positions, 5 antennas, complete uniform Vis. samples, 5 antennas, complete uniform Metres North Metres East Metres North Metres East Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
33 Full deployment Simulated images Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
34 Phase calibration For what we have done so far, phase calibration does not matter For imaging, phase calibration is very important when running in conjunction with cameras, satellites can be used for calibration (work underway at RAL, Sullivan et al., 2005) For daytime/summertime operations, other solutions must be found (radio stars, beacons, suggestions welcome) Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
35 Phase calibration For what we have done so far, phase calibration does not matter For imaging, phase calibration is very important when running in conjunction with cameras, satellites can be used for calibration (work underway at RAL, Sullivan et al., 2005) For daytime/summertime operations, other solutions must be found (radio stars, beacons, suggestions welcome) Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
36 Phase calibration For what we have done so far, phase calibration does not matter For imaging, phase calibration is very important when running in conjunction with cameras, satellites can be used for calibration (work underway at RAL, Sullivan et al., 2005) For daytime/summertime operations, other solutions must be found (radio stars, beacons, suggestions welcome) Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
37 Phase calibration For what we have done so far, phase calibration does not matter For imaging, phase calibration is very important when running in conjunction with cameras, satellites can be used for calibration (work underway at RAL, Sullivan et al., 2005) For daytime/summertime operations, other solutions must be found (radio stars, beacons, suggestions welcome) Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
38 Experiences at JRO (May June 2005) Imaging of non-specular meteor trails Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
39 Experiences at JRO (May June 2005) Preliminary results Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
40 Some Further Reading Blixt, E. M., T. Grydeland, N. Ivchenko, T. Hagfors, C. La Hoz, B. S. Lanchester, U. P. Løvhaug, and T. S. Trondsen, Dynamic rayed aurora and enhanced ion-acoustic radar echoes, Ann. Geophys., 23(1), 3 11, Chau, J. L., and R. F. Woodman, Observations of meteor-head echoes using the Jicamarca 50 MHz radar in interferometer mode, Atmos. Chem. Phys., 4(2), , Grydeland, T., C. La Hoz, T. Hagfors, E. M. Blixt, S. Saito, A. Strømme, and A. Brekke, Interferometric observations of filamentary structures associated with plasma instability in the auroral ionosphere, Geophys. Res. Lett., 30(6), 1338, doi: /2002gl016362, Grydeland, T., E. M. Blixt, U. P. Løvhaug, T. Hagfors, C. La Hoz, and T. S. Trondsen, Interferometric radar observations of filamented structures due to plasma instabilities and their relation to dynamic auroral rays, Ann. Geophys., 22(4), , Grydeland, T., J. Chau, C. La Hoz, and A. Brekke, An imaging interferometry capability for the EISCAT Svalbard Radar, Ann. Geophys., 23(1), , Grydeland et al. (UiT/UNIS/JRO) Interferometric imaging for the ESR URSI / 26
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