SKA Dish Array Elements

Size: px

Start display at page:

Download "SKA Dish Array Elements"

Judith Beasley
8 years ago
Views:

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) Instituto de Física de Cantabria (IFCA). CSIC-Universidad de Cantabria. Santander.

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

Low noise receivers for radio astronomy! Cryogenic Low Noise Amplifiers (LNA)!

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

(LNAs): Single Pixel Feeds (part of the SKA1)" " Phased Array Feeds (part

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

Ultra-Wide Band Feeds on the dishes Frequency range up to 10 GHz Proposed work on Feed antennas and

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

metro 300K Channel 4 Channel 3 OMT FEM BEM to DAE 20K WG 300K

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

Switch 90º 180º Hybrid 0º Ph.Shift φ φ 90º Ph.

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

Matching X-polarization (db) 30 20 10 0-10 -20-30 -40-50 φ = 0º φ = 90º -60-180

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

Frecuencia (GHz) Diferencia de Fase (deg) Transmisión (db) 0-0.1-0.2-0.3-0.4-0.5-0.6-0.

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

analysis, 1/f noise, at Room temperature (300 K) and at cryogenic

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

Acknowledgment: QUIJOTE receivers are funded by the Ministerio de Ciencia e

Low noise millimeter wave receivers for Cosmic Microwave Background radiometers

Low noise millimeter wave receivers for Cosmic Microwave Background radiometers Eduardo Artal, Beatriz Aja, Luisa de la Fuente, Juan Luis Cano, Enrique Villa, Jaime Cagigas (1) Enrique Martínez-González,