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Prokhodtsov A, An P, Kovalyuk V, Zubkova E, Golikov A, Korneev A, et al. Optimization of on-chip photonic delay lines for telecom wavelengths. In: J. Phys.: Conf. Ser. Vol 1124.; 2018. 051052.
Abstract: In this work, we experimentally studied optical delay lines on silicon nitride platform for telecomm wavelength (1550 nm). We modeled the group delay time and fabricated spiral optical delay lines with different waveguide widths and radii as well as measured their transmission. For the half etched rib waveguides we achieved the losses in the range of 3 dB/cm.
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Korneev A, Kovalyuk V, An P, Golikov A, Zubkova E, Ferrari S, et al. Superconducting single-photon detector for integrated waveguide spectrometer. In: EPJ Web Conf. Vol 190.; 2018. 04009.
Abstract: We present our recent achievements in the development of an on-chip spectrometer consisting of arrayed waveguide grating made of Si3N4 waveguides and NbN superconducting single-photon detector.
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Zubkova E, An P, Kovalyuk V, Korneev A, Goltsman G. Integrated Bragg waveguides as an efficient optical notch filter on silicon nitride platform. In: Proc. SPBOPEN.; 2017. p. 449–50.
Abstract: We modeled and fabricated integrated optical Bragg waveguides on a silicon nitride (Si3N4) platform. Transmission spectra of the integrated notch filter has been measured and attenuation at the desired wavelength of 1550 nm down to -43 dB was observed.
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Kooi JW, Baselmans JJA, Hajenius M, Gao JR, Klapwijk TM, Dieleman P, et al. IF impedance and mixer gain of NbN hot electron bolometers. J. Appl. Phys.. 2007;101(4):044511.
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Griffin MJ, Abergel A, Abreu A, Ade PAR, André P, Augueres J-L, et al. The Herschel-SPIRE instrument and its in-flight performance. A&A. 2010;518:7.
Abstract: The Spectral and Photometric Imaging REceiver (SPIRE), is the Herschel Space Observatory`s submillimetre camera and spectrometer. It contains a three-band imaging photometer operating at 250, 350 and 500 μm, and an imaging Fourier-transform spectrometer (FTS) which covers simultaneously its whole operating range of 194-671 μm (447-1550 GHz). The SPIRE detectors are arrays of feedhorn-coupled bolometers cooled to 0.3 K. The photometer has a field of view of 4Â´× 8´, observed simultaneously in the three spectral bands. Its main operating mode is scan-mapping, whereby the field of view is scanned across the sky to achieve full spatial sampling and to cover large areas if desired. The spectrometer has an approximately circular field of view with a diameter of 2.6´. The spectral resolution can be adjusted between 1.2 and 25 GHz by changing the stroke length of the FTS scan mirror. Its main operating mode involves a fixed telescope pointing with multiple scans of the FTS mirror to acquire spectral data. For extended source measurements, multiple position offsets are implemented by means of an internal beam steering mirror to achieve the desired spatial sampling and by rastering of the telescope pointing to map areas larger than the field of view. The SPIRE instrument consists of a cold focal plane unit located inside the Herschel cryostat and warm electronics units, located on the spacecraft Service Module, for instrument control and data handling. Science data are transmitted to Earth with no on-board data compression, and processed by automatic pipelines to produce calibrated science products. The in-flight performance of the instrument matches or exceeds predictions based on pre-launch testing and modelling: the photometer sensitivity is comparable to or slightly better than estimated pre-launch, and the spectrometer sensitivity is also better by a factor of 1.5-2.
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