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A G-band cryogenic MMIC heterodyne receiver module for astronomical applications

Published online by Cambridge University Press:  12 March 2012

Patricia Voll ,
Lorene Samoska ,
Sarah Church ,
Judy M. Lau ,
Matthew Sieth ,
Todd Gaier ,
Pekka Kangaslahti ,
Mary Soria ,
Sami Tantawi  and
Dan Van Winkle
Patricia Voll*
Affiliation:
Department of Physics, Stanford University, Stanford, CA 94305, USA. Phone: +1 650 725 9796. Kavli Institute for Particle Astrophysics and Cosmology, Stanford, CA 94309, USA.
Lorene Samoska
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.
Sarah Church
Affiliation:
Department of Physics, Stanford University, Stanford, CA 94305, USA. Phone: +1 650 725 9796. Kavli Institute for Particle Astrophysics and Cosmology, Stanford, CA 94309, USA.
Judy M. Lau
Affiliation:
Department of Physics, Stanford University, Stanford, CA 94305, USA. Phone: +1 650 725 9796. Kavli Institute for Particle Astrophysics and Cosmology, Stanford, CA 94309, USA.
Matthew Sieth
Affiliation:
Department of Physics, Stanford University, Stanford, CA 94305, USA. Phone: +1 650 725 9796. Kavli Institute for Particle Astrophysics and Cosmology, Stanford, CA 94309, USA.
Todd Gaier
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.
Pekka Kangaslahti
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.
Mary Soria
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.
Sami Tantawi
Affiliation:
SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA.
Dan Van Winkle
Affiliation:
SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA.
*
Corresponding author: P. Voll Email: pvoll@stanford.edu
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Abstract

We report cryogenic noise temperature and gain measurements of a prototype heterodyne receiver module designed to operate in the atmospheric window centered on 150 GHz. The module utilizes monolithic microwave integrated circuit (MMIC) InP high electron mobility transistor (HEMT) amplifiers, a second harmonic mixer, and bandpass filters. Swept local oscillator (LO) measurements show an average gain of 22 dB and an average noise temperature of 87 K over a 40 GHz band from 140 to 180 GHz when the module is cooled to 22 K. A spot noise temperature of 58 K was measured at 166 GHz and is a record for cryogenic noise from HEMT amplifiers at this frequency. Intermediate frequency (IF) sweep measurements show a 20 GHz IF band with less than 94 K receiver noise temperature for a fixed LO of 83 GHz. The compact housing features a split-block design that facilitates quick assembly and a condensed arrangement of the MMIC components and bias circuitry. DC feedthroughs and nano-miniature connectors also contribute to the compact design, so that the dimensions of the moduleare approximately 2.5 cm per side.

Keywords

Multi-Chip ModulesLow Noise Amplifier (LNA)Low Noise ReceiverMMICHEMT
Type
Research Papers
Information
International Journal of Microwave and Wireless Technologies , Volume 4 , Special Issue 3: European Microwave Week 2011 , June 2012 , pp. 283 - 289
Copyright
Copyright © Cambridge University Press and the European Microwave Association 2012

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References

REFERENCES

[1]Voll, P. et al. : A G-band cryogenic MMIC heterodyne receiver module for astronomical applications, Proc. 41st European Microwave Conf. Manchester, UK, October 2011, 523–526.Google Scholar
[2]Ade, P.A.R. et al. : Planck Collaboration: Planck early results: the Planck mission. Astron. and Astrophys., 536 (A1) (2011), 1–16.Google Scholar
[3]Sunyaev, R.A.; Zeldovich, Y.B.: Formation of clusters of galaxies; protocluster fragmentation and intergalactic gas heating. Astron. Astrophys., 20 (1972), 189–200.Google Scholar
[4]Sunyaev, R.A.; Zeldovich, Y.B.: Microwave background radiation as a probe of the contemporary structure and history of the universe. Annu. Rev. Astron. Astrophys., 18 (1980), 537–560.Google Scholar
[5]Samoska, L.; Pukala, D.; Soria, M.; Sadowy, G.: A G-band multi-chip MMIC T/R module for radar applications, 33rd Int. Conf. on Infrared, Millimeter and Terahertz Waves, Pasadena, CA, 2008.Google Scholar
[6]Tessmann, A. et al. : 220 GHz low-noise amplifier modules for radiometric imaging applications, in Proc. 1st European Microwave Integrated Circuits Conf., Manchester, UK, 2006, 137–140.Google Scholar
[7]Tessmann, A. et al. : Metamorphic HEMT MMICs and modules for use in a high-bandwidth 210 GHz radar. IEEE J. Solid-State Circuits, 43, (2008) (10) 2194–2205.Google Scholar
[8]Kangaslahti, P. et al. : Miniature MMIC Low Mass/Power Radiometer modules for the 180 GHz GeoSTAR array, Earth Science Technology Forum, Washington, DC, 2010.Google Scholar
[9]Kallfass, I.; Tessmann, A.; Massler, H.; Pahl, P.; Leuther, A.: An all-active MMIC-based chip set for a wideband 260–304 GHz receiver, in Proc. 5th European Microwave Integrated Circuits Conf., Paris, France, September 2010, 53–56.Google Scholar
[10]Schellenberg, J.; Chedester, R.; McCoy, J.: Multi-channel receiver for an E-band FMCW imaging radar, IEEE/MTT-S Int. Microwave Symp., Honolulu, III, June 2007, 1359–1362.Google Scholar
[11]Khaikin, V.B.; Zakamov, V.R.; Shashkin, V.I.; Kuzmin, S.E.; Radzikhovsky, V.N.: A wideband receiver-module for passive mm wave imaging array: optimization and test results, in Int. Kharkov Symp. Physics and Engineering of Microwaves, Millimeter and Submillimeter Waves (MSMW), Kharkiv, Ukraine, June 2010, 1–3.Google Scholar
[12]Cleary, K.: Coherent polarimeter modules for the QUIET experiment, in Proc. SPIE, Astronomical Telescopes and Instrumentation, San Diego, CA, 2010. 7741, (2010) no. 77412H, 1–9.Google Scholar
[13]Sieth, M. et al. : Development of MMIC receivers for cosmic microwave background interferometry, in Proc. SPIE, Astronomical Telescopes and Instrumentation, San Diego, CA, 2010. 7741, (2010) no. 77412I, 1–12.Google Scholar
[14]Kangaslahti, P.; Pukala, D.; Gaier, T.; Deal, W.; Mei, X.; Lai, R.: Low noise amplifier for 180 GHz frequency band, in IEEE MTT-S Int. Microwave Symp. Dig., Atlanta, GA, 2008, 451–454.Google Scholar
[15]Kangaslahti, P.; Deal, W.R.; Mei, X.; Lai, R.: Broadband characterization of a 100 to 180 GHz amplifier, in IEEE Aerospace Conf. Digest, Big Sky, MT, 2008, 1–6.Google Scholar
[16]Kangaslahti, P.: Recent developments in 180 GHz MMIC LNA and receiver technology, in 11th Specialist Meeting on Microwave Radiometry and Remote Sensing of the Environment, Washington, DC, 2010, 272–275.Google Scholar
[17]Leong, Y.; Weinreb, S.: Full band waveguide-to-microstrip probe transitions, in IEEE MTT-S Int. Microwave Symp. Digest, Anaheim, CA, 1999, 1435–1438.Google Scholar
[18]Voll, P. et al. : Development of a 150 GHz MMIC module prototype for large-scale CMB radiation experiments, in Proc. SPIE, Astronomical Telescopes and Instrumentation, San Diego, CA, 2010. 7741 (2010) no. 77412J, 1–10Google Scholar
[19]Samoska, L.: An overview of solid state integrated circuit amplifiers in the submillimeter-wave and THz regime, IEEE Trans. Terahertz Sci Technol., 1 (3) (2011), 9–24.CrossRefGoogle Scholar
[20]Samoska, L. A. et al. : Cryogenic MMIC low noise amplifiers for W-band and beyond, in Int. Symp. Space Terahertz Technology, Tucson, AZ, April 2011, 193–196.Google Scholar