Volume 634, February 2020
|Number of page(s)||22|
|Published online||04 February 2020|
Wideband 67−116 GHz receiver development for ALMA Band 2
European Southern Observatory (ESO), Garching, Germany
e-mail: email@example.com, firstname.lastname@example.org
2 Group for Advanced Receiver Development (GARD), Chalmers University of Technology, Gothenburg, Sweden
3 Jodrell Bank Centre for Astrophysics, School of Physics & Astronomy, The University of Manchester (UoM), Manchester, UK
4 School of Electrical & Electronic Engineering, The University of Manchester (UoM), Manchester, UK
5 Istituto Nazionale di Astrofisica (INAF/OAS), Bologna, Italy
6 Observatorio de Yebes, Guadalajara, Spain
7 National Astronomical Observatory of Japan (NAOJ), Mitaka, Tokyo, Japan
8 Universidad de Chile (UdC), Santiago, Chile
9 Istituto Nazionale di Astrofisica (INAF/OAA), Arcetri, Italy
10 Dipartimento di Fisica, Universita degli Studi di Milano, Milano, Italy
11 Radiometer Physics GmbH (RPG), Meckenheim, Germany
12 University of Michigan, Department of Physics, Ann Arbor, MI, USA
13 Academia Sinica, Institute of Astronomy & Astrophysics (ASIAA), Taipei, Taiwan
14 Institute of Applied Physics, University of Bern, Bern, Switzerland
15 Istituto Nazionale di Astrofisica/Istituto di Radioastronomia (INAF/IRA), Bologna, Italy
16 Low Noise Factory (LNF), Gothenburg, Sweden
Accepted: 20 December 2019
Context. The Atacama Large Millimeter/submillimeter Array (ALMA) has been in operation since 2011, but it has not yet been populated with the full suite of its planned frequency bands. In particular, ALMA Band 2 (67−90 GHz) is the final band in the original ALMA band definition to be approved for production.
Aims. We aim to produce a wideband, tuneable, sideband-separating receiver with 28 GHz of instantaneous bandwidth per polarisation operating in the sky frequency range of 67−116 GHz. Our design anticipates new ALMA requirements following the recommendations of the 2030 ALMA Development Roadmap.
Methods. The cryogenic cartridge is designed to be compatible with the ALMA Band 2 cartridge slot, where the coldest components – the feedhorns, orthomode transducers, and cryogenic low noise amplifiers – operate at a temperature of 15 K. We use multiple simulation methods and tools to optimise our designs for both the passive optics and the active components. The cryogenic cartridge is interfaced with a room-temperature (warm) cartridge hosting the local oscillator and the downconverter module. This warm cartridge is largely based on GaAs semiconductor technology and is optimised to match the cryogenic receiver bandwidth with the required instantaneous local oscillator frequency tuning range.
Results. Our collaboration has resulted in the design, fabrication, and testing of multiple technical solutions for each of the receiver components, producing a state-of-the-art receiver covering the full ALMA Band 2 and 3 atmospheric window. The receiver is suitable for deployment on ALMA in the coming years and it is capable of dual-polarisation, sideband-separating observations in intermediate frequency bands spanning 4−18 GHz for a total of 28 GHz on-sky bandwidth per polarisation channel.
Conclusions. We conclude that the 67−116 GHz wideband implementation for ALMA Band 2 is now feasible and that this receiver provides a compelling instrumental upgrade for ALMA that will enhance observational capabilities and scientific reach.
Key words: instrumentation: interferometers
© ESO 2020
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