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Technology developments for a large-format heterodyne MMIC array at W-band

Published online by Cambridge University Press:  12 April 2012

Matthew Sieth ,
Sarah Church ,
Judy M. Lau ,
Patricia Voll ,
Todd Gaier ,
Pekka Kangaslahti ,
Lorene Samoska ,
Mary Soria ,
Kieran Cleary  and
Rohit Gawande
...Show all authors
Matthew Sieth*
Affiliation:
Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA. Kavli Institute for Particle Astrophysics & Cosmology, MS 29, Stanford, CA 94309, USA.
Sarah Church
Affiliation:
Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA. Kavli Institute for Particle Astrophysics & Cosmology, MS 29, Stanford, CA 94309, USA.
Judy M. Lau
Affiliation:
Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA. Kavli Institute for Particle Astrophysics & Cosmology, MS 29, Stanford, CA 94309, USA.
Patricia Voll
Affiliation:
Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA. Kavli Institute for Particle Astrophysics & Cosmology, MS 29, Stanford, CA 94309, USA.
Todd Gaier
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA.
Pekka Kangaslahti
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA.
Lorene Samoska
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA.
Mary Soria
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA.
Kieran Cleary
Affiliation:
Department of Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA.
Rohit Gawande
Affiliation:
Department of Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA.
Anthony C.S. Readhead
Affiliation:
Department of Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA.
Rodrigo Reeves
Affiliation:
Department of Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA.
Andrew Harris
Affiliation:
Department of Astronomy, University of Maryland, College Park, MD 20742, USA.
Jeffrey Neilson
Affiliation:
SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025, USA.
Sami Tantawi
Affiliation:
SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025, USA.
Dan Van Winkle
Affiliation:
SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025, USA.
*
Corresponding author: M. Sieth Email: [email protected]; Phone: +00 1 650 725 9796
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Abstract

We report on the development of W-band (75–110 GHz) heterodyne receiver technology for large-format astronomical arrays. The receiver system is designed to be both mass producible, so that the designs could be scaled to thousands of receiver elements, and modular. Most of the receiver functionality is integrated into compact monolithic microwave integrated circuit (MMIC) amplifier-based multichip modules. The MMIC modules include a chain of InP MMIC low-noise amplifiers, coupled-line bandpass filters, and sub-harmonic Schottky diode mixers. The receiver signals will be routed to and from the MMIC modules on a multilayer high-frequency laminate, which includes splitters, amplifiers, and frequency triplers. A prototype MMIC module has exhibited a band-averaged noise temperature of 41 K from 82 to 100 GHz and a gain of 29 dB at 15 K, which is the state-of-the-art for heterodyne multichip modules.

Keywords

Hybrid and Multi-chip ModulesLow Noise and Communication Receivers
Type
Research Papers
Information
International Journal of Microwave and Wireless Technologies , Volume 4 , Special Issue 3: European Microwave Week 2011 , June 2012 , pp. 299 - 307
Copyright
Copyright © Cambridge University Press and the European Microwave Association 2012

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References

[1]The CARMA website [online], 2011. Available: http://www.mmarray.org/.Google Scholar
[2]Sieth, M.; Lau, J. M.; Voll, P.; et al. : Development of MMIC receivers for cosmic microwave background interferometry, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conf. Series, vol. 7741, July 2010.Google Scholar
[3]The SEQUOIA website [online], 2011. Available: http://www.astro.umass.edu/fcrao/instrumentation/sequoia/seq.html.Google Scholar
[4]Samtleben, D: Measuring the cosmic microwave background radiation (CMBR) polarization with QUIET, Nuovo Cimento B, 122 (2007), 1353–1358.Google Scholar
[5]Camiade, M.; Dourlens, C.; Serru, V.; Savary, P.; Blanc, J.: Highly integrated and compact w-band front-end for radiometry application, in 17th Annual IEEE, Gallium Arsenide Integrated Circuit (GaAs IC) Symp., 1995. Technical Digest 1995, October 1995, 230–237.Google Scholar
[6]Haydl, W.; et al. : Compact monolithic coplanar 94 GHz front ends, in IEEE MTT-S Int. Microwave Symp. Digest, 1997, vol. 3, June 1997, 1281–1284.Google Scholar
[7]Tessmann, A.; et al. : A compact W-band dual-channel receiver module, in IEEE MTT-S Int. Microwave Symp. Digest, 2006, June 2006, 85–88.Google Scholar
[8]Schellenberg, J.; Chedester, R.McCoy, J.: Multi-channel receiver for an E-band FMCW imaging radar, in IEEE/MTT-S Int. Microwave Symp. 2007, June 2007, 1359–1362.Google Scholar
[9]Sieth, M.; et al. : Technology developments for a scalable heterodyne MMIC array at W-band, in 2011 41st European Microwave Conf. (EuMC), October. 2011, 527–530.Google Scholar
[10]Kangaslahti, P.; et al. : Compact, miniature MMIC receiver modules for an MMIC array spectrograph, NASA Tech. Briefs, no. NPO-46522, December 2009, 14–15.Google Scholar
[11]Leong, Y.-C.; and Weinreb, S.: Full band waveguide-to-microstrip probe transitions, in 1999 IEEE MTT-S Int. Microwave Symp. Digest, vol. 4, 1999, 1435–1438.Google Scholar
[12]Weinreb, S.; Lai, R.; Erickson, N.; Gaier, T.; and Wielgus, J.: W-band InP wideband MMIC LNA with 30 K noise temperature, in 1999 IEEE MTT-S Int. Microwave Symp. Digest, vol. 1, 1999, 101–104.Google Scholar
[13]Samoska, L.; et al. : Cryogenic MMIC low noise amplifiers for W-Band and Beyond, in Int. Symp. on Space Terahertz Technology, Tucson, AZ, April 2011 [online]. Available: http://www.nrao.edu/meetings/isstt/papers/2011/2011193196.pdf.Google Scholar
[14]Parashare, C.; et al. : Millimeter-wave radiometers to correct satellite altimetry for wet-tropospheric path delay in the coastal zone, presented at the 2011 Jet Propulsion Laboratory Postdoctoral Research Day, Pasadena, CA, September 2011.Google Scholar
[15]Pillai, E: Coax via-A technique to reduce crosstalk and enhance impedance match at vias in high-frequency multilayer packages verified by FDTD and MoM modeling, IEEE Trans. Microw. Theory Tech, 45(10) (1997), 1981–1985.Google Scholar