Kinetic Inductance Detectors and readout electronics for the OLIMPO experiment. (arXiv:1904.01890v1 [astro-ph.IM])
<a href="http://arxiv.org/find/astro-ph/1/au:+Paiella_A/0/1/0/all/0/1">A. Paiella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Battistelli_E/0/1/0/all/0/1">E. S. Battistelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castellano_M/0/1/0/all/0/1">M. G. Castellano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Colantoni_I/0/1/0/all/0/1">I. Colantoni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Columbro_F/0/1/0/all/0/1">F. Columbro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coppolecchia_A/0/1/0/all/0/1">A. Coppolecchia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DAlessandro_G/0/1/0/all/0/1">G. D&#x27;Alessandro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernardis_P/0/1/0/all/0/1">P. de Bernardis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gordon_S/0/1/0/all/0/1">S. Gordon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lamagna_L/0/1/0/all/0/1">L. Lamagna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mani_H/0/1/0/all/0/1">H. Mani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Masi_S/0/1/0/all/0/1">S. Masi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mauskopf_P/0/1/0/all/0/1">P. Mauskopf</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pettinari_G/0/1/0/all/0/1">G. Pettinari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piacentini_F/0/1/0/all/0/1">F. Piacentini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Presta_G/0/1/0/all/0/1">G. Presta</a>

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.

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.

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