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Microwave, Sub-mm, and THz Technology for payloads and space (sub)systems

Radiometer Physics GmbH (RPG), Germany. Microwave, Sub-mm, and THz Technology for payloads and space (sub)systems. Harald Czekala RPG Thomas Rose RPG AchimWalber RPG Hugh Gibson RPG Bertrand Thomas RPG Michael Brandt RPG Oleg Cojocari ACST Byron Alderman STFC RAL.

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Microwave, Sub-mm, and THz Technology for payloads and space (sub)systems

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  1. Radiometer Physics GmbH (RPG), Germany Microwave, Sub-mm, and THz Technologyfor payloads and space (sub)systems Harald Czekala RPG Thomas Rose RPG AchimWalber RPGHugh Gibson RPG Bertrand Thomas RPG Michael Brandt RPG Oleg Cojocari ACST Byron Alderman STFC RAL

  2. RPG Company Profile Microwave, sub-mm, THz Turn-key radiometers, space technology components, design, scientific expertise ■ 4 decades experience ■ 40 employees ■ Radiometers (space) ■ Frontends/Receivers ■ Lab equipment / VNA ■ Components up to THz ■ Design+Manufacturing

  3. RPG Space Heritage • MLS/UARS Microwave Limb Sounder (JPL/USA, 1991)(RPG founders working with JPL on Gunn oscillators/multipliers) • MHS/FY-3 Microwave Humidity Sounder (CNSA / China, 2008)150 and 183 GHz Receiver front ends for MHS • ODIN (SSC, 2001 until today) 8 Gunn Local Oscilaltors plus fudamental mixers • Herschel / HIFI space telescope (ESTEC, 2009)Local Oscillators (480 to 1200 GHz), IF up-converters • SMILES (JAXA, 2008 installed on ISS)PLL Gunn LO chain at 360 GHz

  4. RPG Space Heritage (2) • SAPHIR+MADRAS / MEGHA-TROPIQUES microwave humidity sounder CNES/ISRO • SAPHIR (183 GHz sounder): specially stabilized Gunn resonator (plus contrib. to LO and RF hardware) • MADRAS (18.7, 23.8, 36.5, 89, 157 GHz Imager)Gunn LO, DC conditioning, RF networks (M4/M5, 89/157), OMT • Components…

  5. Space heritage components RF components • (whisker contacted multipliers) • (Gunn oscillators, with PLL / cavity) • Planar Multipliers • Subharmonic mixers • Fundamental mixers • MMIC driver amplifiers • MMIC low noise amps (LNA) • Noise injection (calibration!) • Rapid Dicke switching (4-point cal.) • PA/QA to delivered hardware Waveguide Components passive • Corrugated feed horns • Attenuator • Coupler • RF loads, absorbers • RF power splitter • Isolator (Y-junction circulator/isolator, Faraday isolator) • Waveguide twists • Orthomode Transducers (OMT) • Optical networks (feedclusters, FSS) • Power supply

  6. Current involvements ESA TRP (Technology Research Programme) activities • ESTEC "Integrated Schottky Structures" (664 GHz Front End) tripler-mixer FE with integrated circuit design • ESTEC "Sub-Millimetre Wave Receiver Front-end" (664 GHz Frontend)  doubler-doubler-mixer with discrete Schottky diodes • EU/FP7 "Millimeter-Wave Integrated Diode & Amplifier sources"  over 400 mW (later: 1000) mW @ 100 GHz • Qual/Eval activities aiming at TRL-5 expected soon ESA-ESTEC/EUMETSAT METOP Second Generation („Polar Orbiter“) • "RPG Sat-B CPI coordination and interface definition support" (OHB) • MWI/ICI Receiver Performance & Test Requirements definition (TAS-I) • ESA "Cloud and Precipitation Airborne Radiometer" (118 & 664 GHz FE) • Proposal ESTEC "243 GHz Direct Detection Radiometers"

  7. Quality Control, tests, procedure, … (PA/QA) • RPG offers PA/QA compliant to highest ESA and NASA standards • RPG has demonstrated these capabilities • RPG advises customers on suitable (tailored) approaches

  8. Space Products (II) Space qualified front ends (China, FY-3): 183 GHz (4 channels) water vapour sounder

  9. Space Products (III) • Space qualified front ends (China, FY-3): • 90 GHz dual polarized receiver OMT + LNA + (either Direct Detection or Heterodyne) • 150 GHz dual polarized receiver: OMT + SHM

  10. Examples: Frontends and sub-systems for Space FIRST/HIFI MADRAS • Space qualified local oscillators (Herschel / ESA): • 8 local oscillator chains from 480 GHz to 1100 GHz • Other space projects: • EOS (NASA), ODIN (SSA), FIRST/HIFI, • MARFEQ, SAPHIR (CNES), MLS (NASA), FY-3 (China), …

  11. Outline • Direct detection (MMIC) for frequencies up to 120 GHz • Auto-calibration receivers up to 200 GHz (noise-injection / Dicke sw.) • Improvements in mixer and multiplier designs through close cooperation with Schottky diode suppliers • Schottky technology from ACST (Germany) • Schottky technology from RAL (UK) • Subharmonic mixers at 424 GHz and 664 GHz • InGaAS mixers with reduction of LO power by 10 dB

  12. Direct Detection • Direct detection systems up to 110 GHz (since 8 years now…) • LNA mostly based on MMIC supply from IAF Freiburg, Germany • At 118 / 150 / 183 GHz and above, sub-harmonic mixers still have better performance (at least with high-quality sub-harmonic mixers) • Waveguide filters with high stability and narrow bandwidth (0.25 %) 55 dB Pre-Amplifier Splitter and Filter Section Boosters and Detectors Video Amps, MUX, 16 Bit ADC Noise Injection Coupler 51- 59 GHz 7 Channel Filterbank Receiver 170 mm Corrugated Feedhorn

  13. Direct Detection Receivers Compared to heterodyne systems: • Improved noise figure • Decreased long term stability (larger 1/f noise with InP MMICs) • Much better RFI protection • Compact (integrated) design • No planar filters, all waveguide Low loss Ortho-Mode Transducer Tsys < 600 K (NF: 4.9) 90 GHz dual-pol (FM)

  14. Direct Detection: MMIC mounting • Mounting of all amplifier types • Experience in micromachining • Bonding and soldering to space standards

  15. Auto-calibration receivers: Noise injection, Dicke Switching Uambient+noise Uambient DetectorVoltage Usignal Usignal Repetition: 5 Hz Duty cycle: 45 % (due to 10 ms switch time) 0.05 0.10 0.15 0.20 Time / s Fast calibration with noise diodes and ambient load(gain and Tsys are calibrated) Ambient load / Dicke switch:Isolatorsdriven by switchedmagnetic field Noise diodes:mounted directlyin a waveguidecoupling section Applied to direct detectionas well as heterodynereceivers

  16. Auto-Calibration Receivers (II) • Noise injection calibration up to 200 GHz • 7.000 K signal at 183 GHz with stable noise diode (15 dB ENR) • Magnetically switched isolators:Dicke switching up to 150 GHz with low insertion loss (≤1.0 dB) • Fast switching with low currents (small thermal effects, 100 mA, 0.5 V) ESA-ATPROP 15 / 90 GHz • Allan Variance Stability: 4.000 s • Less dependent on external calibration targets (LN2)!

  17. Auto-calibration receivers (III): 90+150 GHz system Achieved System Noise Temperatures: (incl. noise injection coupler, Dicke switch, isolator) 90 GHz: 750 K 150 GHz: 1200 K Full internal calibrationIsolation > 30 dB Insertion loss @ 90 GHz: 0.7 dB Insertion loss @ 150 GHz: 1.0 dB Allan Variance up to 4000 s

  18. Auto-calibration receivers (IV): 183 GHz system Heterodyne receiver at 183 GHzwith 6 channel Filterbank • Channel centers in IF: 0.6, 1.5, 2.5, 3.5, 5.0, 7.5 GHz • Noise injection for calibration • Tsys=1200 K for complete radiometer • Tsys=380 to 450 K for mixer • Schottky mixer diodeby ACST (Germany) Dome-C, Antarctica 3.300m asl, -25 to -80 °C Close to South-Pole Similar System on HAMP (HALO Microwave Package) for HALO research aircraft

  19. Schottky Mixer and Multiplier Improvements Anode pillar (contact pad) Air-bridge Membrane- substrate Mesa with anode Cathode pillar (contact pad) Back-side ohmic 25μm 50μm Air-bridges Mesas Membrane- substrate Protection pillars (contact pads) Back-side ohmic RAL Diode • Planar technology • Discrete Schottky devices • Semi-integrated and full integrated structures Two collaborations: • STFC/RAL, UK • ACST, Germany Mandatory improvements for 800 to 1000 GHz circuit mountings: • Reduced Cj0 • Reduced Cstr • Smaller size ESTEC Contract 22032/08/NL/JA: Sub-Millimeter Wave Receiver Front-End (at 664 GHz) ESTEC Contract 21628/08/NL/GLC: Integrated Schottky Structures (at 664 GHz) ACST Diode Quasi-vertical (QVD) single Diode (SD) Anti-parallel (APD) diode

  20. Schottky Mixer and Multiplier Improvements Anode pillar (contact pad) Air-bridge Membrane- substrate Mesa with anode Cathode pillar (contact pad) Back-side ohmic 25μm 50μm Air-bridges Mesas Membrane- substrate Protection pillars (contact pads) Back-side ohmic RAL Diode • Planar technology • Discrete Schottky devices • Semi-integrated and full integrated structures Two collaborations: • STFC/RAL, UK • ACST, Germany Mandatory improvements for 800 to 1000 GHz circuit mountings: • Reduced Cj0 • Reduced Cstr • Smaller size ESTEC Contract 22032/08/NL/JA: Sub-Millimeter Wave Receiver Front-End (at 664 GHz) ESTEC Contract 21628/08/NL/GLC: Integrated Schottky Structures (at 664 GHz) ACST Diode Quasi-vertical (QVD) single Diode (SD) Anti-parallel (APD) diode

  21. Improved Diodes: Vector Network Analyzer Products 50–75 GHz 60 – 90 GHz 75–110 GHz 90 – 140 GHz 110 – 170 GHz 140–220 GHz 220–325 GHz 325–500 GHz (500 – 750 GHz) OEM Network Analyzer Frequency Extenders for Rohde & Schwarz Courtesy of Rohde & Schwarz

  22. Improved Diodes: Tx/Rx Products Transmit / Receive Systems: 90 GHz 183 GHz 220 GHz 324 GHz 502 GHz 640 GHz 870 GHz For compact ranges (antenna measurement facilities, phase + amplitude) Multipixel Array 220 – 325 GHz

  23. Improved Diodes: RPG sub-harmonic mixers

  24. Receiver technology – 183 GHz example 183 GHz feeds and sub-harmonic mixers for ALMA-WVR • Best 183 GHz receivers available • Built in larger numbers • Noise-injection calibration @183(RPG only manufacturer world wide) • All ALMA water vapor radiometers equipped with RPG mixers and feeds

  25. Improved Diodes: RPG sub-harmonic mixers

  26. Sub-Harmonic Mixer: 424 GHz LO Power: 5 mW Tmix=800 to 1200 K Tsys=1800 K (Feed, SHM, IF Amp, Detection) Conversion= –7 dB

  27. Sub-Harmonic Mixer: 664 GHz LO Power: 3 mW Tmix ≈ 1600 K Conversion: –7.5 to –9.5 dB

  28. Further Schottky Diode Optimization: InGaAs Only at ACST:InGaAs Diode • InGaAs built-in voltage (barrier height) significantly lower than GaAs(0.2eV compared to 0.8eV) • Reduced LO power required for SHM at 183 GHz: 0.34 mW (10 dB less!) 183 GHz InGaAs mixer with 0.2 / 0.25 / 0.34 mW LO-power

  29. Technical Study – SWI for EJSM Europa Jupiter System Mission (EJSM, Laplace), NASA / ESA Orbiter: Jupiter Ganymede (JGO) Instrument: Submillimetre-Wave (SWI) Situation distance to Jupiter: 106 km (15 RJ) primary: 300 mm frequency bands: 530 – 590 1090 – 1266 scanning: 2-axis: +/- 4°(limb) 1-axis: +/- 60°(moons) science requirement: 10 m/s (winds in limb) angular resolution: < 2 // pointing knowledge: 11.5 // 4° 65°

  30. Technical Study – SWI for EJSM: Principal Setup electr. + synth. Incoming microwave radiation secondary primary SWI-telescope receivers and optics compartment platform common shielded vault CTS spectro. other instr.

  31. Technical Study – SWI for EJSM Mechanical Design secondary primary along-track scanning optics compartment pusher rotation axis cross-track scanning

  32. hot load receiver feeds 1200 GHz receiver chain IF-LNAs telescope beam calibration flip mirror beam splitter Optics Compartment: 600 GHz receiver chain • low-loss Gaussian Telescope beam path • small overall size (170 x 290 mm2) • thermally stabilized mixer, PA, hot load • classical enclosed housing • good radiation shielding

  33. Technical Study – SWI for EJSM: Mass Budget Electr. + Synth Surface primary mirror (Mg) 750 g actuators (all) 680 g receivers (both) 280 g telescope structure 1370 g optics plate 1130 g sum: 4210 g Vault spectrometers (CTS) 1500 g electronics 1000 g synthesizers 300 g common shielded vault other instr. sum: 2800 g CTS Spectro. total: 7010 g

  34. Conclusion / Summary • Direct detection with superior performance (over heterodyne) up to 120 GHz (until better MMIC LNA technology becomes available) • Auto-calibration receivers up to 200 GHz • Cooperation with Schottky diode manufacturers for improved devices • Development of improved mixers and multipliers up to 900 GHz, leading to: • VNA extenders covering all bands to 500 GHz (and soon even further) • Transmit/Receive systems up to 900 GHz • Excellent sub-harmonic mixers • Outstanding performance at 183 GHz, 424 GHz, 664 GHz Further steps: ■ Substrate Transfer ■ High-Power varactors (driver stages for THz) ■ Film Diode Technology ■ Continuing reduction of capacities and size Results partly supported by: ESTEC Contract 22032/08/NL/JA: Sub-Millimeter Wave Receiver Front-End @ 664 GHz ESTEC Contract 21628/08/NL/GLC: Integrated Schottky Structures @ 664 GHz Thank you!

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  39. RPG ESA/ESTEC/EU current activities • Ongoing ESA and Space application activities: • ESTEC “Integrated Schottky Structures” (664 GHz FE, ICI) • ESTEC “Sub-Millimetre Wave Receiver Front-end” (664 GHz FE, ICI) • EU/FP7 “Millimeter-Wave Integrated Diode & Amplifier sources” (100 GHz) • ESTEC/EUMETSAT Metop Second Generation: • „RPG Sat-B CPI coordination and interface definition support” (OHB) • MWI/ICI Receiver Performance & Test Requirements definition (TAS-I) • ESA “Cloud and Precipitation Airborne Radiometer” (118 & 664 GHz FE) • Proposal ESTEC„243 GHz Direct Detection Radiometers“ MHS from the FY-3 satellite / China

  40. ESTEC & RPG Dreamteam Schedule Now T 0 T0 +7 T0+14 T0+22 T0+50? Phase 0 (MetOp SG Req.) A1 A2 B1 B2 (PDR) C (CDR) D (AI&T) Technology Development Technology Pre-Evaluation Eval & LAT ICI AI&T 2 Development contracts (ongoing) Qualified Instuments ESTEC ESTEC ESTEC ESTEC Pre Evaluation Results LAT Results Instrument Design Component Requirements Design & Test Results RPG Consultancy RPG AI & T RPG Pre-Eval. RPG Eval & LAT RPG ? AI & T ITT: Development & sample man. Component Requirements Qualified Components ACST Diode -manufacturing ACST Diode -manufacturing Diodes Diodes RAL/Teratec Diode -manufacturing RAL/Teratec Diode -manufacturing Diodes Diodes

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