Performance of the pre-production band 3 (84-116 GHz) receivers for ALMA

Claude, S.; Jiang, Frank; Niranjanan, Pat; Dindo, P.; Erickson, Darren; Yeung, K.; Derdall, D.; Duncan, David L.; Garcia, Dominic; Leckie, Brian; Pfleger, Michael; Rodrigues, G.; Szeto, Kei; Welle, P.; Wood, I.; Caputa, K.; Lichtenberger, A. W.; Pan, S. K.

doi:10.1117/12.788128

Cited by 13 publications

(3 citation statements)

References 4 publications

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“…In this article we present an overview of the observing modes available for interferometric solar observations with the Band 3 and Band 6 receivers (Claude et al, 2008;Ediss et al, 2004) of ALMA in Cycle 4. A companion article by White et al (2017) presents techniques developed for rapidly mapping the Sun using the TP antennas.…”

Section: Introductionmentioning

confidence: 99%

Observing the Sun with the Atacama Large Millimeter/submillimeter Array (ALMA): High-Resolution Interferometric Imaging

et al. 2017

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Observations of the Sun at millimeter and submillimeter wavelengths offer a unique probe into the structure, dynamics, and heating of the chromosphere; the structure of sunspots; the formation and eruption of prominences and filaments; and energetic phenomena such as jets and flares. High-resolution observations of the Sun at millimeter and submillimeter wavelengths are challenging due to the intense, extended, lowcontrast, and dynamic nature of emission from the quiet Sun, and the extremely intense and variable nature of emissions associated with energetic phenomena. The Atacama Large Millimeter/submillimeter Array (ALMA) was designed with solar observations in mind. The requirements for solar observations are significantly different from observations of sidereal sources and special measures are necessary to successfully carry out this type of observations. We describe the commissioning efforts that enable the use of two frequency bands, the 3 mm band (Band 3) and the 1.25 mm band (Band 6), for continuum interferometric-imaging observations of the Sun with ALMA. Examples of high-resolution synthesized images obtained using the newly commissioned modes during the solar commissioning campaign held in December 2015 are presented. Although only 30 of the eventual 66 ALMA antennas were used for the campaign, the solar images synthesized from the ALMA commissioning data reveal new features of the solar atmosphere that demonstrate the potential power of ALMA solar observations. The ongoing expansion of ALMA and solar-commissioning efforts will continue to enable new and unique solar observing capabilities.

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Section: Introductionmentioning

confidence: 99%

Observing the Sun with the Atacama Large Millimeter/submillimeter Array (ALMA): High-Resolution Interferometric Imaging

et al. 2017

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“…Systems of this type are referred to as dual sideband (2SB) and are used for bands 3-8. To minimize losses, compact designs have been developed in which the RF hybrid and a local oscillator (LO) power divider are in the form of waveguide circuits in a single split metal block, within which all the elements of the 2SB mixer are mounted, see, e.g., [21], [22] or [23]. As the wavelength becomes shorter, it is increasingly difficult to produce such compact designs and above 600 GHz, for the top two bands, double sideband (DSB) mixers without sideband separation are used, see, e.g., [24].…”

Section: The Alma Receiving Systemmentioning

confidence: 99%

Atacama Large Millimeter/Submillimeter Array

2015

Encyclopedia of Astrobiology

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Abstract-The Atacama Large Millimeter/submillimeter Array (ALMA) is an international radio telescope under construction in the Atacama Desert of northern Chile. ALMA is situated on a dry site at 5000 m elevation, allowing excellent atmospheric transmission over the instrument wavelength range of 0.3 to 10 mm. ALMA will consist of two arrays of high-precision antennas. One, of up to 64 12-m diameter antennas, is reconfigurable in multiple patterns ranging in size from 150 meters up to ∼15 km. A second array is comprised of a set of four 12-m and twelve 7-m antennas operating in one of two closely packed configurations ∼50 m in diameter. The instrument will provide both interferometric and total-power astronomical information on atomic, molecular and ionized gas and dust in the solar system, our Galaxy, and the nearby to high-redshift universe. In this paper we outline the scientific drivers, technical challenges and planned progress of ALMA.

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Section: The Alma Receiving Systemmentioning

confidence: 99%

The Atacama Large Millimeter/submillimeter Array

Wootten,

Thompson

2009

Preprint

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The Atacama Large Millimeter/submillimeter Array (ALMA) is an international radio telescope under construction in the Atacama Desert of northern Chile. ALMA is situated on a dry site at 5000 m elevation, allowing excellent atmospheric transmission over the instrument wavelength range of 0.3 to 10 mm. ALMA will consist of two arrays of high-precision antennas. One, of up to 64 12-m diameter antennas, is reconfigurable in multiple patterns ranging in size from 150 meters up to ∼15 km. A second array is comprised of a set of four 12-m and twelve 7-m antennas operating in one of two closely packed configurations ∼50 m in diameter. The instrument will provide both interferometric and total-power astronomical information on atomic, molecular and ionized gas and dust in the solar system, our Galaxy, and the nearby to high-redshift universe. In this paper we outline the scientific drivers, technical challenges and planned progress of ALMA.

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Performance of the pre-production band 3 (84-116 GHz) receivers for ALMA

Cited by 13 publications

References 4 publications

Observing the Sun with the Atacama Large Millimeter/submillimeter Array (ALMA): High-Resolution Interferometric Imaging

Observing the Sun with the Atacama Large Millimeter/submillimeter Array (ALMA): High-Resolution Interferometric Imaging

Atacama Large Millimeter/Submillimeter Array

The Atacama Large Millimeter/submillimeter Array

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