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ALMA BAND 2 EVALUATION RECEIVER AT THE 12 m TELESCOPE

ALMA BAND 2 EVALUATION RECEIVER AT THE 12 m TELESCOPE. David Forbes, Thomas Folkers , Robert Freund, Eugene Lauria , Martin McColl, Mark Metcalfe, George Reiland , Lucy Ziurys Arizona Radio Observatory Tucson, AZ. ARO 12m Antenna. Objective.

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ALMA BAND 2 EVALUATION RECEIVER AT THE 12 m TELESCOPE

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  1. ALMA BAND 2 EVALUATION RECEIVER AT THE 12 m TELESCOPE David Forbes, Thomas Folkers, Robert Freund, Eugene Lauria, Martin McColl, Mark Metcalfe, George Reiland, Lucy Ziurys Arizona Radio Observatory Tucson, AZ

  2. ARO 12m Antenna

  3. Objective • Evaluate the performance of the latest cryogenic MIC/MMIC amplifier technology as compared to the well established SIS technology for the 4mm band • Provide a direct comparison of each of the technologies with observational data • Done by constructing an insert for each type of amplifier (MIC/MMIC) and installing each opposite of an insert using an SIS mixer • These mixers have been used at the 12 m over the past 20 yrs. • Deep integrations done at the J = 1→0 H2CO line at 72.8 GHz

  4. Receiver Architecture SIS SIS MIC MMIC

  5. Receiver Architecture 4-8 GHz 1st IF USB E-band downconverter 1.5 GHz 2nd IF downconverter Needed for MMIC LSB Amplifier SB selector switch 1.5 GHz IF to Backends LO SIS LO 1.5 GHz IF to Backends SIS Mixer IF Amplifier • SIS mixer channel operates in single-sideband mode • Amplifier channel utilizes sideband-separating mode Dewar Boundary

  6. Legacy 68 - 90 GHz 12 m Insert • SIS mixer • Uses (2) backshorts to provide SSB operation • 1.5 GHz IF

  7. RF Amplifier-Based Inserts

  8. E-band Downconverter Architecture WR-12 Quadrature hybrid coupler MAC Tech. C7256 4-12 GHz quad. hybrid coupler Millitech MCA-12-120187 USB Front end signal from amplifier 4 – 8 GHz IF LSB LO Millitech MCA-12-120187 WR-12 Y junction power splitter

  9. Test Bench Setup

  10. Image Rejection Performance for Each Mixer Pair

  11. Pairs Used on Inserts } MMIC } MIC

  12. Complete E-band Downconverter Assy.

  13. Receiver Testing in Lab

  14. Receiver Temperatures at the Telescope* Frequency: 72.8 GHz, LSB, 1st IF = 5 GHz *Noise temperature measured with Y-factor method, using hot / cold loads at the window of each receiver.

  15. Observations: SIS / MIC SIS MIC Object: IRC+10216 Frequency: 72.8 GHz Integration time: 10hrs, 42min Tsys: 403 K (SIS), 303 (MIC), Trec = 64 K (SIS), 56 K (MIC)

  16. Observations: SIS / MMIC SIS MMIC Object: IRC+10216 Frequency: 72.8 GHz Integration time: 10hrs, 42min Tsys: 264 K (SIS), 333 (MIC), Trec: 64 K (SIS), 78 (MMIC)

  17. Conclusions • Amplifier technology has shown comparable noise performance as compared to SIS mixer technology which has been the benchmark for the state-of-the-art over the past 20+ years. • Use of cooled amplifiers reduces the number of cooled components and complexity of the receiver dewar. • Increase reliability • Moves image separating mixer outside the dewar • 1/f stability may still be an issue: • Increases with the number of stages in an amplifier • Typically worse in amplifiers, especially when gate widths become shorter • Important for continuum observations but may not be as much as an issue for spectral line work since a narrower bandwidth is utilized • E-band downconverter needs improvement to meet the ALMA spec. of better than 10 dB of IR, further improvement is needed for single-dish observations.

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