Antenna coupled Kinetic Inductance arrays for space and ground based imaging arrays

Yates, S. J. C.; Baselmans, J. J. A.; Baryshev, A. M.; Neto, A.; Gerini, G.; Barends, R.; Lankwarden, Y. J. Y.

doi:10.1063/1.3292301

Cited by 9 publications

(4 citation statements)

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“…The reduction of the Q-factor at a higher blackbody temperature is due to increasing R a and R m . The operation is somewhat similar to a traditional antenna-coupled MKID device [18]. The effective area of L a and R a in the resonator is difficult to calculate directly but mainly confined to the area between the choke filters at two sides.…”

Section: Thz Direct Detectionmentioning

confidence: 94%

Performance improvements of a terahertz direct detector for imaging arrays

Su¹,

Wang²,

Shi³

et al. 2021

Supercond. Sci. Technol.

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We studied and improved the performance of a terahertz (THz) direct detector based on the superconducting NbN hot electron bolometer (HEB) integrated with microwave readout for imaging arrays and other applications. A 6 nm thick NbN microbridge at the feed point of a twin-slot antenna is embedded into a high-Q quarter-wavelength coplanar waveguide (CPW) resonator made from a 350 nm thick NbN film which is weakly coupled to a CPW feedline. THz direct detection was performed at a signal frequency of 0.66 THz at a bath temperature of 4.2 K. When operating at a low input microwave power level, the device acting as a microwave kinetic inductance detector with a kinetic inductance fraction of 0.45 changes the surface impedance of the resonator in response to incident THz radiation. The estimated optical noise equivalent power (NEP) is ∼0.23 pW · Hz−0.5 which shows about one order of magnitude improvement compared to that of the traditional voltage-biased NbN HEBs. The improved performance of the THz direct detectors with lower NEP and easy readout makes them promising in imaging with a large number of the array pixels.

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Section: Thz Direct Detectionmentioning

confidence: 94%

Performance improvements of a terahertz direct detector for imaging arrays

Su¹,

Wang²,

Shi³

et al. 2021

Supercond. Sci. Technol.

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“…Today, MKID arrays are produced in many laboratories (see e.g. [150][151][152] ) and are starting to be operated at large telescopes (see e.g. 153,154 ).…”

Section: Mapping Speedmentioning

confidence: 99%

The cosmic microwave background: observing directly the early universe

Bernardis

Masi

2012

Space Telescopes and Instrumentation 2012: Optical, Infrared, and Millimeter Wave

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The Cosmic Microwave Background (CMB) is a relict of the early universe. Its perfect 2.725K blackbody spectrum demonstrates that the universe underwent a hot, ionized early phase; its anisotropy (about 80 µK rms) provides strong evidence for the presence of photon-matter oscillations in the primeval plasma, shaping the initial phase of the formation of structures; its polarization state (about 3 µK rms), and in particular its rotational component (less than 0.1 µK rms) might allow to study the inflation process in the very early universe, and the physics of extremely high energies, impossible to reach with accelerators. The CMB is observed by means of microwave and mm-wave telescopes, and its measurements drove the development of ultra-sensitive bolometric detectors, sophisticated modulators, and advanced cryogenic and space technologies. Here we focus on the new frontiers of CMB research: the precision measurements of its linear polarization state, at large and intermediate angular scales, and the measurement of the inverse-Compton effect of CMB photons crossing clusters of Galaxies. In this framework, we will describe the formidable experimental challenges faced by ground-based, near-space and space experiments, using large arrays of detectors. We will show that sensitivity and mapping speed improvement obtained with these arrays must be accompanied by a corresponding reduction of systematic effects (especially for CMB polarimeters), and by improved knowledge of foreground emission, to fully exploit the huge scientific potential of these missions.

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“…Even if the KID concept had been proposed more than five years earlier 14 , at that time multiplexed KID hadn't been demostrated yet at a telescope, and the achieved sensitivities on the sky were still rather poor. Despite that, new ideas like the Lumped Element KID (LEKID) proposed by Doyle et al 10 and the encouraging preliminary results concerning antenna-coupled KID 11 convinced us that building such an instrument was possible in a relatively short amount of time. Three European laboratories (Institut Neel, AIG Cardiff, SRON) decided on this base to start an intense phase of development culminated in October 2009, i.e.…”

Section: The Nika Development: 2009-2013mentioning

confidence: 99%

Latest NIKA Results and the NIKA-2 Project

et al. 2013

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NIKA (New IRAM KID Arrays) is a dual-band imaging instrument installed at the IRAM (Institut de RadioAstronomie Millimetrique) 30-meter telescope at Pico Veleta (Spain). Two distinct Kinetic Inductance Detectors (KID) focal planes allow the camera to simultaneaously image a field-of-view of about 2 arc-min in the bands 125 to 175 GHz (150 GHz) and 200 to 280 GHz (240 GHz). The sensitivity and stability achieved during the last commissioning Run in June 2013 allows opening the instrument to general observers. We report here the latest results, in particular in terms of sensitivity, now comparable to the state-of-theart Transition Edge Sensors (TES) bolometers, relative and absolute photometry. We describe briefly the next generation NIKA-2 instrument, selected by IRAM to occupy, from 2015, the continuum imager/polarimeter slot at the 30-m telescope.

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Antenna coupled Kinetic Inductance arrays for space and ground based imaging arrays

Cited by 9 publications

References 0 publications

Performance improvements of a terahertz direct detector for imaging arrays

Performance improvements of a terahertz direct detector for imaging arrays

The cosmic microwave background: observing directly the early universe

Latest NIKA Results and the NIKA-2 Project

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