The Future: Ultra Wide Band Feeds and Focal Plane Arrays
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1 The Future: Ultra Wide Band Feeds and Focal Plane Arrays Germán Cortés-Medellín NAIC Cornell University 1-1
2 Overview Chalmers Feed Characterization of Chalmers Feed at Arecibo Focal Plane Arrays for Arecibo Conclusions 1-2
3 Chalmers Feed Developed by Rikard Olsson and Per-Simon Kildal for the US-SKA Bandwidth 1:10 Small Size ~ 0.5 to 0.7 λmax Phase Center independent of Frequency 1-3
4 Chalmers Feed Input Matching Characteristics From: R. Olson and P.S. Kildal, A Novel Low-Profile Log-Periodic Ultra Wideband Feed for the Dual-Reflector Antenna of US-SKA. IEEE Antennas and Propagation International Symposium,
5 Chalmers Feed Input Matching Characteristics Input Matching Efficiency = 75% From: R. Olson and P.S. Kildal, A Novel Low-Profile Log-Periodic Ultra Wideband Feed for the Dual-Reflector Antenna of US-SKA. IEEE Antennas and Propagation International Symposium,
6 Evaluation of Chalmers Feed for Arecibo From 1.5 to 12.0 GHz 1-6
7 Evaluation of Chalmers Feed for Arecibo Spherical Wave Expansion (SWE) of Chalmers feed data patterns from 150 MHz to 1.2 GHz Scaled SWE by a factor of 10: yielding 1.5 to 12.0 GHz Radiation Patterns: 1-7
8 Chalmers Feed Radiation Patterns 0 Frequency Scaled x10 for Arecibo Analysis 1.5 GHz 2.0 GHz 1-8
9 Chalmers Feed Radiation Patterns 1 Frequency Scaled x10 for Arecibo Analysis 1.5 GHz 2.0 GHz -15dB
10 Chalmers Feed Radiation Patterns 2 Frequency Scaled x10 for Arecibo Analysis 3.0 GHz 4.0 GHz -15dB
11 Chalmers Feed Radiation Patterns 3 Frequency Scaled x10 for Arecibo Analysis 5.0 GHz 6.0 GHz -15dB
12 Chalmers Feed Radiation Patterns 4 Frequency Scaled x10 for Arecibo Analysis 7.0 GHz 8.0 GHz -15dB
13 Chalmers Feed Radiation Patterns 5 Frequency Scaled x10 for Arecibo Analysis 9.0 GHz 10.0 GHz -15dB
14 Chalmers Feed Radiation Patterns 6 Frequency Scaled x10 for Arecibo Analysis 11.0 GHz 12.0 GHz -15dB
15 Calculated Arecibo Antenna Performance with Chalmers Feed 1-15
16 Calculated Antenna Performance Antenna Sensitivity Antenna Noise Temperature System Noise Temperature 1-16
17 Calculated Antenna Sensitivity 14 Antenna Sensitivity [K/Jy] Chalmers Feed L-Band Wide ALFA, Pix-0 ALFA, Ave C-Band Feed X-Band Feed Frequency [GHz] 1-17
18 35 Calculated Antenna Noise Temperature 30 Antenna Temperature [K] Chalmers Feed L-Band Wide ALFA C-Band Feed X-Band Feed Frequency [GHz] 1-18
19 Calculated System Temperature I Tsys [K] Un-cooled Chalmers ALFA L-Band Wide C-Band Feed X-Band Feed Frequency 1-19
20 Calculated System Temperature II Tsys [K] Un-cooled Chalmers Cooled Chalmers (70K) ALFA L-Band Wide C-Band Feed X-Band Feed Frequency 1-20
21 Calculated Antenna Performance Antenna Sensitivity Antenna Noise Temperature System Noise Temperature Beam radiation Patterns Cross-Polarization Levels 1-21
22 Arecibo Antenna Beam Pattern with Chalmers Feed Freq= 3.0 GHz 11 x11 11 x db db db Co-Polar Beam Pattern db db X-Polar Beam Pattern db 1-22
23 Arecibo Antenna Beam Pattern with Chalmers Feed Freq= 6.0 GHz 5.5 x x db db db Co-Polar Beam Pattern db db X-Polar Beam Pattern db 1-23
24 Arecibo Antenna Beam Pattern with Chalmers Feed Freq= 9.0 GHz 3.7 x x db db db Co-Polar Beam Pattern db db X-Polar Beam Pattern db 1-24
25 Cross-Polarization Level Chalmers Feed L-Band Wide ALFA C-Band Feed X-Band Feed Cross-Pol Level [db] Frequency [GHz] 1-25
26 Conclusions: Chalmers Feed Great Bandwidth, and compact size Antenna Sensitivity less than current systems Antenna Cross-Pol level better that 19 db, compared with 25 db Large Spillover yields Higher Antenna Noise Temperature. Moderate High Tsys. By cooling the feed to 70K, Tsys reduces from 43K to 33K 1-26
27 Focal Plane Arrays for Arecibo 1-27
28 Enabling Feed Technologies Feed Band width Input Noise Imaging Technology Current Feasible Matching Perform. Config. [db] Corrugated Feed Horns 1.55:1 2: GOOD Single/Array Quad-Ridge Feed Horn 2:1 3: GOOD Single/Array ATA Feed 20: FAIR Single/Array? Chalmers Feed 10: POOR Single/Array? Vivaldi Feed 3:1 5: FAIR Phase Array 1-28
29 Possible Focal Plane Arrays Configurations for Arecibo TE11 mode Focal Plane Arrays Chalmers/Ingerson Feed based Focal Plane Arrays Vivaldi Focal Phased Arrays Others: Quad-Ridge 1-29
30 Arecibo Gregorian Optics Scanning Losses and Field of View Scanning Loss [db] Yscn, GHz ALFA -1.4 Yscn, GHz Yscn, GHz -1.6 Yscn, GHz Yscn, GHz Displacement along X/Y Axis [cm] 1-30
31 Chalmers/Ingerson Feed based Focal Plane Arrays Element Separation 0.5 to 0.7λmax Max. Scanning loss across the band: 1.0 db Dimensions in mm 1-31
32 Arecibo Gregorian Optics Scanning Losses and Field of View Scanning Loss [db] Yscn, GHz ALFA -1.4 Yscn, GHz Yscn, GHz -1.6 Yscn, GHz Yscn, GHz Displacement along X/Y Axis [cm] 1-32
33 TE11 Mode Horns based Focal Plane Arrays Element Separation 1.19λ Max. Scanning loss across the band: 1.0 db Dimensions in mm 1-33
34 Vivaldi Feed Based Focal Phased Arrays Element Separation 0.5λmin Dimensions in mm 1-34
35 Focal Plane Arrays Possibilities 1-35
36 Conclusions Cont Bandwidth of Focal Plane Array at Arecibo is determined by the scanning Losses in the FOV Un-cooled Chalmers Feeds are better suited for single pixel applications than for Focal Plane Array applications due to poor input matching and cooling requirements to reduce Tsys. Vivaldi type Phased Arrays could be located in away from the Gregorian Focal Plane A 19 element X-Band TE11 mode focal plane array is feasible 1-36
37 End 1-37
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