development of 150 mhz to 4 ghz inverted conical sinuous ...€¦ · sinuous feed for 140 ft radio...
TRANSCRIPT
![Page 1: Development of 150 MHz to 4 GHz Inverted Conical Sinuous ...€¦ · Sinuous Feed for 140 Ft Radio Telescope •Rohit Gawande •PhD Student, Electrical and Computer Engineering Dept,](https://reader036.vdocuments.us/reader036/viewer/2022062402/5fbd355f2e85ee43da5f0ca1/html5/thumbnails/1.jpg)
Atacama Large Millimeter/submillimeter ArrayExpanded Very Large Array
Robert C. Byrd Green Bank TelescopeVery Long Baseline Array
Development of 150 MHz to 4 GHz Inverted Conical Sinuous Feed for 140 Ft Radio Telescope
Rohit GawandePhD Student, Electrical and Computer Engineering Dept, University of Virginia
Dr. Richard F. BradleyScientist / Research Engineer, National Radio Astronomy Observatory, Charlottesville, VA
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Outline
• Motivation• Antenna Assembly• Antenna Characterization• Low Noise Amplifier• System Noise Measurement• Cryogenic and low frequency versions
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Motivation
• Sweeping Large Frequency ranges• Frequency Agility• Detection of short duration pulses• Multi frequency imaging• Simultaneous observation of several spectral lines• Increasing interest in wideband feeds for future radio telescopes
– Frequency Agile Solar Radiotelescope (FASR)– Square Kilometer Array (SKA)– Green Bank Lunar Interferometer for Neutrino Transients (GLINT)
• MIT LL / NRAO Bi-static Radar Collaboration to Study Earth’s Ionosphere (140 Ft Radio Telescope in Green Bank)
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Planar Sinuous Antenna
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Antenna Assembly and WorkingLaboratory version for modeling and measurements
500 MHz to 3 GHz for tests on 140 Ft telescope in GB
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• In order to eliminate the back-lobe, sinuous pattern projected onto a cone, and a ground plane is placed directly behind the cone’s apex.
• Each sinuous resonator a quarter wavelength above the ground plane.• Lightweight feed due to foam support structure
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Simulated Input Reflection Coefficient
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• S11 better than 9 dB over the whole frequency range.
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Measured E Plane and H Plane Far Field Pattern in Green Bank anechoic chamber
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Measured Co and Cross Polarization in 45 degree plane
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Simulated on axis directivity from 1 to 4GHz.
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Simulated sub - efficiencies using BOR1 components as a function of parabola flare angle.
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• BOR1 efficiency=0.94• Aperture efficiency better than 0.7 over 43 to 57 degrees
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Pseudo Differential Amplifier
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• A single ended LNA attached to each of the four arms. The outputs of the LNAs in opposing arms combined using 1800 hybrid
• Avoids any crossover before the LNAs• Provides low impedance path for even mode.
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Low Noise Amplifier Assembly
Inventor drawing of chassis holderPhotograph of the LNA
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Gain and Noise for 50 Ohm inputDevice: 280um gate width Fujitsu FHX45XVd = 1V, Id = 20mA for 300 K Optimal Bias
Noise temperature drops from 35K to 6K when cooled from 300K to 15K around 2 GHz.
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System Noise measurement using Sky and absorber methodMeasured and modeled system noise
Noise Measurement Setup in Green Bank
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Next Step: Cold version to improve the sensitivity
Photograph of the DewarInventor Drawing showing interior of the Dewar
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Next Step: Extending Frequency range down to 150 MHz
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Front End Box
High FrequencySection
Ground Plane Extensions
Pourable Foam Support for Low Frequency Outriggers
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Atacama Large Millimeter/submillimeter ArrayExpanded Very Large Array
Robert C. Byrd Green Bank TelescopeVery Long Baseline Array
Development of 150 MHz to 4 GHz Sinuous Feed for 140 Ft Radio Telescope
•Rohit Gawande•PhD Student, Electrical and Computer Engineering Dept, University of Virginia
•Dr. Richard F. Bradley•Scientist / Research Engineer, National Radio Astronomy Observatory, Charlottesville, VA
Thank You!
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Decade Bandwidth LNA optimized for higher antenna impedance 100 Ohm
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Pulsar Data Using 140 Ft from 800 –1600 MHz
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