Development of a Microwave SQUID-Multiplexed TES Array for MUSTANG-2

Stanchfield, Sara; Aguirre, James E.; Brevik, J. A.; Cho, H. M.; Datta, Rahul; Devlin, Mark J.; Dicker, Simon; Dober, B.; Egan, Dennis; Ford, Pam; Hilton, G. C.; Hubmayr, Johannes; Irwin, K. D.; Marganian, P.; Mason, B. S.; Mates, J. A. B.; McMahon, Jeffrey; Sarpa, Marcia; Mroczkowski, Tony; Romero, C.; Tucker, C.; Vale, Leila R.; White, Sarahlouise; Whitehead, Mark; Young, Alexander

doi:10.1007/s10909-016-1570-4

Cited by 20 publications

(14 citation statements)

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“…Examples include the ATIsupported Multiwavelength Sub/millimeter Inductance Camera (MUSIC) 166 that was deployed at the Caltech Submillimeter Observatory, a millimeter wavelength system developed at Columbia University, 167 and the optical instruments DARKNESS and MEC. 102 A transition edge sensor (TES), discussed below, that uses CASPER hardware is the Muliplexed SQUID TES Array at Ninety Gigahertz (MUSTANG-2), 168 which is deployed at the GBT. Hickish et al includes a census of CASPER deployments for radio astronomy as of 2016.…”

Section: Radio Wave Digital Signal Processingmentioning

confidence: 99%

Enabling discoveries: a review of 30 years of advanced technologies and instrumentation at the National Science Foundation

Kurczynski

Milojević

2020

J. Astron. Telesc. Instrum. Syst.

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Over its more than 30-year history, the Advanced Technologies and Instrumentation (ATI) program has provided grants to support technology development and instrumentation for ground-based astronomy. Through a combination of automated literature assessment and indepth literature review, we present a survey of ATI-funded research and its impact on astronomy and society. Award acknowledgment and literature citation statistics for ATI are comparable to a comparison astronomy grant program that does not support technology development. Citation statistics for both NSF-funded programs exceed those of the general astronomical literature. Numerous examples demonstrate the significant, long-term impact of ATI-supported research in astronomy. As part of this impact, ATI grants have provided many early career researchers the opportunity to gain critical professional experience. However, technology development unfolds over a time period that is longer than an individual grant. A longitudinal perspective shows that investments in technology and instrumentation have led to extraordinary scientific progress. © The Authors. Published by SPIE under a Creative Commons Attribution 4.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

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Section: Radio Wave Digital Signal Processingmentioning

confidence: 99%

Enabling discoveries: a review of 30 years of advanced technologies and instrumentation at the National Science Foundation

Kurczynski

Milojević

2020

J. Astron. Telesc. Instrum. Syst.

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“…The GBT has an extremely flexible suite of instrumentation, including single-and dual-feed heterodyne receivers covering 290 MHz to 92 GHz. The telescope is currently equipped with four multi-pixel systems: FLAG, a 19 element, dual-polarization cryogenic PAF operating at 1.4 GHz that was in its commissioning phase at the time of this review (Roshi et al 2018); KFPA, a seven pixel, dual-polarization feed horn array operating at 18 -26 GHz (Morgan et al 2008); ARGUS, a 16-pixel single-polarization feed horn array operating in the 85-116 GHz range (Sieth et al 2014); and MUSTANG-2, a 223-feed horn dual-polarization bolometer camera with 20 GHz bandwidth centered at 90 GHz (Stanchfield et al 2016).…”

Section: Green Bank Telescope (Usa)mentioning

confidence: 99%

An International Survey of Front-end Receivers and Observing Performance of Telescopes for Radio Astronomy

Bolli

Orfei

Zanichelli

et al. 2019

PASP

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This paper presents a survey of microwave front-end receivers installed at radio telescopes throughout the World. This unprecedented analysis was conducted as part of a review of front-end developments for Italian radio telescopes, initiated by the Italian National Institute for Astrophysics in 2016. Fifteen international radio telescopes have been selected to be representative of the instrumentation used for radio astronomical observations in the frequency domain from 300 MHz to 116 GHz. A comprehensive description of the existing receivers is presented and their characteristics are compared and discussed. The observing performances of the complete receiving chains are also presented. An overview of on-going developments illustrates and anticipates future trends in front-end projects to meet the most ambitious scientific research goals.

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“…The current generation of sub-arcminute resolution experiments also includes the Large APEX Bolometer Camera (LABOCA, Siringo et al 2009) at the Atacama Pathfinder Experiment (APEX) 12-m telescope, which covers a 12 diameter FOV at 345 GHz at an angular resolution of about 19 ; AzTEC at the 50-m Large Millimeter Telescope, which operates with a single bandpass centred at either 143, 217, or 270 GHz (Wilson et al 2008), and which has a beam FWHM of 5, 10, or 18 , respectively; the Submillimetre Common User Bolometer Array Two (SCUBA-2, Holland et al 2013;Dempsey et al 2013) on the 15-m James Clerk Maxwell Telescope, which simultaneously images a FOV of about 7 at 353 GHz and 666 GHz with a main-beam FWHM of 13 and 8 in the two frequency channels, respectively; MUSTANG-2 at the 100-m Green Bank telescope, which maps a 4.35 FOV at 90 GHz with 9 resolution (Dicker et al 2014;Stanchfield et al 2016). Therefore, NIKA2 is unique in combining an angular resolution better than 20 , an instantaneous FOV of a diameter of 6.5 , and multi-band observation capabilities at 150 and 260 GHz.…”

Section: Introductionmentioning

confidence: 99%

Calibration and performance of the NIKA2 camera at the IRAM 30-m Telescope

Perotto

Ponthieu

Macías-Pérez

et al. 2020

A&A

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Context. NIKA2 is a dual-band millimetre continuum camera of 2 900 kinetic inductance detectors, operating at 150 and 260 GHz, installed at the IRAM 30-m telescope in Spain. Open to the scientific community since October 2017, NIKA2 will provide key observations for the next decade to address a wide range of open questions in astrophysics and cosmology. Aims. Our aim is to present the calibration method and the performance assessment of NIKA2 after one year of observation. Methods. We used a large data set acquired between January 2017 and February 2018 including observations of primary and secondary calibrators and faint sources that span the whole range of observing elevations and atmospheric conditions encountered by the IRAM 30-m telescope. This allowed us to test the stability of the performance parameters against time evolution and observing conditions. We describe a standard calibration method, referred to as the “Baseline” method, to translate raw data into flux density measurements. This includes the determination of the detector positions in the sky, the selection of the detectors, the measurement of the beam pattern, the estimation of the atmospheric opacity, the calibration of absolute flux density scale, the flat fielding, and the photometry. We assessed the robustness of the performance results using the Baseline method against systematic effects by comparing results using alternative methods. Results. We report an instantaneous field of view of 6.5′ in diameter, filled with an average fraction of 84%, and 90% of valid detectors at 150 and 260 GHz, respectively. The beam pattern is characterised by a FWHM of 17.6″ ± 0.1″ and 11.1″ ± 0.2″, and a main-beam efficiency of 47%±3%, and 64%±3% at 150 and 260 GHz, respectively. The point-source rms calibration uncertainties are about 3% at 150 GHz and 6% at 260 GHz. This demonstrates the accuracy of the methods that we deployed to correct for atmospheric attenuation. The absolute calibration uncertainties are of 5%, and the systematic calibration uncertainties evaluated at the IRAM 30-m reference Winter observing conditions are below 1% in both channels. The noise equivalent flux density at 150 and 260 GHz are of 9 ± 1 mJy s1/2 and 30 ± 3 mJy s1/2. This state-of-the-art performance confers NIKA2 with mapping speeds of 1388 ± 174 and 111 ± 11 arcmin2 mJy−2 h−1 at 150 and 260 GHz. Conclusions. With these unique capabilities of fast dual-band mapping at high (better that 18″) angular resolution, NIKA2 is providing an unprecedented view of the millimetre Universe.

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Development of a Microwave SQUID-Multiplexed TES Array for MUSTANG-2

Cited by 20 publications

References 5 publications

Enabling discoveries: a review of 30 years of advanced technologies and instrumentation at the National Science Foundation

Enabling discoveries: a review of 30 years of advanced technologies and instrumentation at the National Science Foundation

An International Survey of Front-end Receivers and Observing Performance of Telescopes for Radio Astronomy

Calibration and performance of the NIKA2 camera at the IRAM 30-m Telescope

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