Measurements of dichroic bow-tie antenna arrays with integrated cold-electron bolometers using YBCO oscillators

• Leonid S. Revin,
• Dmitry A. Pimanov,
• Alexander V. Chiginev,
• Anton V. Blagodatkin,
• Viktor O. Zbrozhek,
• Andrey V. Samartsev,
• Anastasia N. Orlova,
• Dmitry V. Masterov,
• Alexey E. Parafin,
• Victoria Yu. Safonova,
• Anna V. Gordeeva,
• Andrey L. Pankratov,
• Leonid S. Kuzmin,
• Anatolie S. Sidorenko,
• Silvia Masi and
• Paolo de Bernardis

Beilstein J. Nanotechnol. 2024, 15, 26–36, doi:10.3762/bjnano.15.3

• malfunction. Typical closed-cycle sorption 3He cryostats, suitable for space and balloon-borne experiments, are limited by their working temperature to about 300 mK. For example, the LSPE-SWIPE custom-designed 3He cryostat cools the two focal planes down to 0.3 K. The ground-based BICEP Array cryostat with a

• elements of the receiving matrix are connected to each other in parallel. The matrix of receiving elements will be located under the opening of the back-to-back horn, similar to the one used for the LSPE-SWIPE project, with a diameter of 4 mm. Accordingly, the receiving elements of the 210 and 240 GHz

• a voltage bias scheme. In case of the LSPE-SWIPE project power load, our estimations [24] demonstrate that, by aforementioned measurement system improvements, the photon NEP level, which is about 7 × 10−17 W/√Hz, can nearly be achieved. Conclusion We have elaborated and tested the receiving arrays

Numerical modeling of a multi-frequency receiving system based on an array of dipole antennas for LSPE-SWIPE

• Alexander V. Chiginev,
• Anton V. Blagodatkin,
• Dmitrii A. Pimanov,
• Ekaterina A. Matrozova,
• Anna V. Gordeeva,
• Andrey L. Pankratov and
• Leonid S. Kuzmin

Beilstein J. Nanotechnol. 2022, 13, 865–872, doi:10.3762/bjnano.13.77

• Large Scale Polarization Explorer-Short-Wavelength Instrument for the Polarization Explorer (LSPE-SWIPE) back-to-back horn. These results are used for calculating the frequency response of arrays of planar dipole antennas with cold-electron bolometers for 145, 210, and 240 GHz frequencies. For the main

• of 1.1 × 10−16 W/Hz1/2. This was achieved by replacing one of two superconductor–insulator–normal tunnel junctions with a superconductor–normal metal contact. Keywords: cosmic microwave background (CMB); cold-electron bolometer; dichroic antenna; dipole antenna; LSPE-SWIPE; waveguide horn

• consists of two instruments: Strip and Short-Wavelength Instrument for the Polarization Explorer (SWIPE). LSPE-SWIPE is a balloon-borne radio telescope, which will consist of a main and two auxiliary frequency channels. According to the latest requirements [2], the operating frequency of the LSPE-SWIPE