SKA Dish Array Elements
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1 SKA Dish Array Elements Eduardo Artal (1) Francisco Casas (2) (1) Departamento de Ingeniería de Comunicaciones (DICOM) Universidad de Cantabria. Santander. (2) Instituto de Física de Cantabria (IFCA). CSIC-Universidad de Cantabria. Santander. Workshop SKA: Strategic Position and Future Opportunities for Spanish Industry Madrid, 23 November 2012, Instituto Rocasolano 1
2 Summary! SKA Dish Array! Description! Our projects in radio astronomy! ESA Planck mission! Microwave polarimeters in El Teide! Low noise receivers for radio astronomy! Cryogenic Low Noise Amplifiers (LNA)! Feed-horns, polarizers, Orthomode Transducers (OMT)! Microwave correlators and detectors! Conclusions 2
3 SKA Dish Array - Description Dishes: Receptors of the astronomical signal for frequencies from 450 MHz to 10 GHz Feeds and Low Noise Amplifiers (LNAs): Single Pixel Feeds (part of the SKA1)" " Phased Array Feeds (part of Advanced Instrumentation) Receivers: Receive amplified RF from the feed/lnas 3
4 SKA Dish Array - Description SKA phases SKA1 250 antennas (15 m) Single-pixel feeds Frequency range of GHz SKA2 Depending on the Advanced Instrumentation Program results Inclusion of Phased Array or Ultra-Wide Band Feeds on the dishes Frequency range up to 10 GHz Proposed work on Feed antennas and Receivers Wideband single-pixel feeds Octave-band single-pixel feeds (current default) Phased-array feeds 4
5 Our projects in radio astronomy ESA Planck-LFI radiometers (30 and 44 GHz) 4 K load reference Feed-horn Feed-horn 20K WG Radiometer metro 300K Channel 4 Channel 3 OMT FEM BEM to DAE 20K WG 300K Channel 2 Channel 1 Radiometer 4 K load reference Feed-horn Back End Module: BEM 5
6 One branch of the 30 GHz BEM EBB L 50 mm LNA (MMIC) Detector output Filter Detector DC amplifier 6
7 MMIC amplifiers (LNA) at 44 GHz Two LNA (Low Noise Amplifier): same topology PHEMT LNA (HEMT-Depletion) OMMIC ED02AH Gate Width : 90 µm (6x15µm) Gate Length : 0.18 µm LNA (HEMT-Enhancement) Size: 3x1 mm 2 7
8 30 GHz BEM. Qualification Model (QM) RF channels 8
9 30 GHz BEM. Flight Model (FM) Size: 60 x 65 x 39 mm 3 DC amplifiers 9
10 Planck - LFI integration in the satellite 3 Back End Modules at 44 GHz 2 Back End Modules at 30 GHz 10
11 Microwave polarimeters in El Teide Observatorio de El Teide Izaña site, m First telescope installation at the observatory (QUIJOTE 1st instrument) 11
12 QUIJOTE 1st Instrument 30 GHz pixel Frontal panel of 30 GHz BEM rack 12
13 Polarimeter receiver (26-36 GHz) (2nd instrument) Feedhorn Polarizer OMT Cryo-LNA LNA LNA FEM Gain&Filtering Modules LNA LNA Phase Switches Module F Ph.Switch 180º F Ph.Switch 180º F Ph.Switch 90º F Ph.Switch 90º 180º Hybrid 0º Ph.Shift φ φ 90º Ph.Shift Correlation&Detection Module DC DC V d1 180º Hybrid V d2 DC DC V d3 V d4 Cryostat (T = 20 K) Back-End Module (Room Temperature, T = 298 K) Receiver test bench 13
14 Cryogenic Low Noise Amplifiers 4-12 GHz MMIC LNA 100 nm mhemt (IAF-Fraunhofer) 3-stage (Gate width: 4 30 µm) Chip size: 3 x 1 mm 2 Collaboration: Centro Astronómico de Yebes Fraunhofer - UC 14
15 Cryogenic Low Noise Amplifiers 4-12 GHz MMIC 15K Gain = 31.5 ± 1.8 db Te average = 5.3 K ± 1.4 K DC Pd= 8 mw 15
16 Feed-horns Feedhorn measurements GHz band (db) Directivity Frecuencia (GHz) Input Matching X-polarization (db) φ = 0º φ = 90º θ (deg) Radiation pattern at f = 32 GHz θ -3dB ~ 13º 16
17 Polarizer Measured performance GHz band Reflexión (db) Frecuencia (GHz) Diferencia de Fase (deg) Transmisión (db) Frecuencia (GHz) Phase Imbalance: 90º ± 1º Matching > 25 db Insertion Losses ~ 0.18 db 17
18 Orthomode Transducer (OMT) Units: GHz GHz GHz 18
19 Facilities at Universidad de Cantabria Test equipment from DC to 50 GHz: Gain, Noise temperature, Signal analysis, Spectrum analysis, 1/f noise, at Room temperature (300 K) and at cryogenic temperature (20 K) Cryostats general view Two LNA units installed inside 19
20 Conclusions - Expertise in broadband low noise receivers for radio astronomy - We are able to contribute to SKA preconstruction phase in collaboration with the industry Acknowledgment: QUIJOTE receivers are funded by the Ministerio de Ciencia e Innovación under Astronomy and Astrophysics research program, reference AYA C
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