MKID Large Format Array Testbed

Ferrari, L.; Yates, S. J. C.; Eggens, Martin; Baryshev, A.; Baselmans, J. J. A.

doi:10.1109/tthz.2018.2871365

Cited by 6 publications

(10 citation statements)

References 18 publications

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“…In Fig. 4a, we give NEP exp (P abs , f = 200 Hz) together with the theoretical value of the photon noise background from the radiation source and obtain a result very similar to those of de Visser et al 18 ,Baselmans et al 12 and Ferrari et al 36 , but with ten times greater sensitivity. For a comparison of the NEP as a function of the absorbed power as shown in Fig.…”

Section: Methodssupporting

confidence: 78%

“…where P is the radiation power, given now by P s , which is the power from the source that can couple to a single mode. P s is calculated from the radiator temperature and the measured filter transmission using the formalism explained in detail in Appendix B of Ferrari et al 36 . Figure 3a shows the phase noise power spectral density S θ ( f ) for one representative device, which has a resonance frequency of 2.74 GHz and an aluminium length of 913 µm.…”

Section: Methodsmentioning

confidence: 99%

“…We can now obtain NEP exp using Eq. 4, and use it to determine the detector coupling efficiency η opt using the photon noise from the radiator as an absolute calibration source 36 . This procedure is only valid if the MKID is photon-noise limited, which is the case for source powers exceeding 5 fW; here the spectrum is white with a single Lorentzian roll-off 38 .…”

Section: Methodsmentioning

confidence: 99%

See 2 more Smart Citations

Ultra-sensitive Super-THz Microwave Kinetic Inductance Detectors for future space telescopes

Baselmans¹,

Facchin²,

Laguna³

et al. 2022

Preprint

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Future actively cooled space-borne observatories for the far-infrared, loosely defined as a 1-10 THz band, can potentially reach a sensitivity limited only by background radiation from the Universe. This will result in an increase in observing speed of many orders of magnitude. A spectroscopic instrument on such an observatory requires large arrays of detectors with a sensitivity expressed as a noise equivalent power NEP = 3 × 10 −20 W/ √Hz. We present the design, fabrication, and characterisation of microwave kinetic inductance detectors (MKIDs) for this frequency range reaching the required sensitivity. The devices are based on thin-film NbTiN resonators which use lens-antenna coupling to a submicron-width aluminium transmission line at the shorted end of the resonator where the radiation is absorbed. We optimised the MKID geometry for a low NEP by using a small aluminium volume of ≈ 1 µm 3 and fabricating the aluminium section on a very thin (100 nm) SiN membrane. Both methods of optimisation also reduce the effect of excess noise by increasing the responsivity of the device, which is further increased by reducing the parasitic geometrical inductance of the resonator. We measure the sensitivity of eight MKIDs with respect to the power absorbed in the detector using a thermal calibration source filtered in a narrow band around 1.55 THz. We obtain a NEP exp (P abs ) = 3.1 ± 0.9 × 10 −20 W/ √Hz at a modulation frequency of 200 Hz averaged over all measured MKIDs. The NEP is limited by quasiparticle trapping. The measured sensitivity is sufficient for spectroscopic observations from future, actively cooled space-based observatories. Moreover, the presented device design and assembly can be adapted for frequencies up to ≈ 10 THz and can be readily implemented in kilopixel arrays.

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Section: Methodssupporting

confidence: 78%

Section: Methodsmentioning

confidence: 99%

Section: Methodsmentioning

confidence: 99%

See 1 more Smart Citation

Ultra-sensitive Super-THz Microwave Kinetic Inductance Detectors for future space telescopes

Baselmans¹,

Facchin²,

Laguna³

et al. 2022

Preprint

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show abstract

“…In this paper we only summarize the experimental setup for this measurement, but it is covered in detail in Davis et al 12 . As an example for the analysis we use data from a lab based reflective optics based large field camera with a base T of 240 mK, see Ferrari et al 13 for more details. An overview of the optics is shown in Fig.…”

Section: Experimental Methodsmentioning

confidence: 99%

Complex Beam Mapping and Fourier Optics Analysis of a Wide-Field Microwave Kinetic Inductance Detector Camera

et al. 2020

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For astronomical instruments, accurate knowledge of the optical pointing and coupling are essential to characterize the alignment and performance of (sub-)systems prior to integration and deployment. Ideally, this requires the phase response of the optical system, which for direct (phase insensitive) detectors was not previously accessible. Here we show development of the phase sensitive complex beam pattern technique using a dual optical source heterodyne technique for a large field of view Microwave Kinetic Inductance Detector camera at 350 GHz. We show here how you can analyze the measured data with Fourier optics, which allows integration into a telescope model to calculate the on sky beam pattern and telescope aperture efficiency prior to deployment at a telescope.

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“…GRASP simulations of the full end-to-end optical system predict a waist size of ≈ 3.25 mm in this focal plane [27]. More details on the cryostat and optics system are presented in [25] and [28].…”

Section: A Test Arraymentioning

confidence: 99%

Complex Field Mapping of Large Direct Detector Focal Plane Arrays

Davis

Yates

Jellema

et al. 2019

IEEE Trans. THz Sci. Technol.

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Complex field mapping is a powerful tool to characterize the optical performance of astronomical instruments, and has become the standard for characterizing heterodyne array cameras. Recently, an adaptation of the heterodyne beam mapping technique was demonstrated on a single pixel of a direct detector instrument. We present a novel measurement apparatus and data acquisition techniques to efficiently reconstruct the complex field pattern of individual pixels across a direct detector focal plane array. These techniques are scalable to high pixel counts as the technology maturation and scientific requirements push to larger arrays. For this demonstration, we used an engineering model of the low-frequency band of the APEX microwave kinetic inductance detector camera with a center frequency of ν = 350 GHz. Amplitude and phase radiation patterns were measured from all 880 pixels of the test array in two orthogonal polarizations. We also discuss an updated postprocessing pipeline using the complex field data to characterize the optical performance of the array. Using the measured complex field pattern, we extract the co-and crosspolarization patterns and Gaussian beam parameters, and propagate the beam from the measurement plane to additional planes of interest across all pixels in the test array. Complex field measurements of direct detectors allow more precise characterization Manuscript ). A. M. Baryshev is with the of beam parameters when compared to thermal measurements, particularly for individualized fitting in postprocessing not reliant on the accuracy of the probe system alignment. These techniques enable high-precision characterization of individualized beam parameters as well as the overall optical system to very large format arrays with modest computational processing power. These results demonstrate the diagnostic power of the presented measurement and analysis techniques.Index Terms-Complex field mapping, Gaussian beam analysis, kinetic inductance detector, near-to-far-field transformation, optical characterization. 2156-342X

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MKID Large Format Array Testbed

Cited by 6 publications

References 18 publications

Ultra-sensitive Super-THz Microwave Kinetic Inductance Detectors for future space telescopes

Ultra-sensitive Super-THz Microwave Kinetic Inductance Detectors for future space telescopes

Complex Beam Mapping and Fourier Optics Analysis of a Wide-Field Microwave Kinetic Inductance Detector Camera

Complex Field Mapping of Large Direct Detector Focal Plane Arrays

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