# Kinetic Inductance Detectors and readout electronics for the OLIMPO   experiment

**Authors:** A. Paiella, E. S. Battistelli, M. G. Castellano, I. Colantoni, F., Columbro, A. Coppolecchia, G. D'Alessandro, P. de Bernardis, S. Gordon, L., Lamagna, H. Mani, S. Masi, P. Mauskopf, G. Pettinari, F. Piacentini, G., Presta

arXiv: 1904.01890 · 2019-04-04

## TL;DR

This paper presents the development and validation of LEKID arrays and their readout electronics for the OLIMPO experiment, aimed at astrophysical observations in multiple spectral bands.

## Contribution

It introduces optimized LEKID arrays and a comprehensive readout system tailored for balloon-borne astrophysics applications, demonstrating their suitability in a space-like environment.

## Key findings

- LEKID arrays operate effectively at 0.3 K with high quality factors.
- The readout electronics achieve low noise performance suitable for astrophysical signals.
- Successful characterization and validation of the detector system for OLIMPO.

## Abstract

Kinetic Inductance Detectors (KIDs) are superconductive low$-$temperature detectors useful for astrophysics and particle physics. We have developed arrays of lumped elements KIDs (LEKIDs) sensitive to microwave photons, optimized for the four horn-coupled focal planes of the OLIMPO balloon-borne telescope, working in the spectral bands centered at 150 GHz, 250 GHz, 350 GHz, and 460 GHz. This is aimed at measuring the spectrum of the Sunyaev-Zel'dovich effect for a number of galaxy clusters, and will validate LEKIDs technology in a space-like environment. Our detectors are optimized for an intermediate background level, due to the presence of residual atmosphere and room--temperature optical system and they operate at a temperature of 0.3 K. The LEKID planar superconducting circuits are designed to resonate between 100 and 600 MHz, and to match the impedance of the feeding waveguides; the measured quality factors of the resonators are in the $10^{4}-10^{5}$ range, and they have been tuned to obtain the needed dynamic range. The readout electronics is composed of a $cold$ $part$, which includes a low noise amplifier, a dc$-$block, coaxial cables, and power attenuators; and a $room-temperature$ $part$, FPGA$-$based, including up and down-conversion microwave components (IQ modulator, IQ demodulator, amplifiers, bias tees, attenuators). In this contribution, we describe the optimization, fabrication, characterization and validation of the OLIMPO detector system.

## Full text

_Full body text omitted from this summary view._ Fetch the complete paper as Markdown: https://tomesphere.com/paper/1904.01890/full.md

## Figures

6 figures with captions in the complete paper: https://tomesphere.com/paper/1904.01890/full.md

## References

19 references — full list in the complete paper: https://tomesphere.com/paper/1904.01890/full.md

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Source: https://tomesphere.com/paper/1904.01890