SWIPE multi-mode pixel assembly design and beam pattern measurements at cryogenic temperature

23 Jul 2019, 12:00
15m
Auditorium G. Testori (Milano)

Auditorium G. Testori

Milano

Piazza Città di Lombardia, 1, 20124 Milano MI
Oral Presentation Low Temperature Detector fabrication techniques and materials Orals LM 003

Speaker

Fabio Columbro (ROMA1)

Description

Detecting the polarization of the cosmic microwave background (CMB) represents the best technique to study physical phenomena happening a split-second within the big bang, thus testing the standard cosmological model. In this framework the Short Wavelength Instrument for the Polarization Explorer (SWIPE) aims at the measurement of CMB polarization at the largest angular scales, where cosmic inflation left its imprint in the form of B-modes and E-modes patterns of the linear polarization field.

SWIPE is a cryogenic large aperture polarimeter which will observe 25\% of sky during a two-weeks-long circumpolar stratospheric balloon mission, thanks to 326 multi-mode bolometers cooled to 0.3 K and covering 3 frequency bands centered at 140 GHz, 220 GHz and 240 GHz.

The detectors are fed by a single large-diameter (500 mm) plano-convex lens, cooled at 1.6 K, coincident with the cold aperture stop. The lens is coupled to multi-mode feed horns (28° FWHM), collecting a total of 8800 modes on the bolometers. The bolometer thermistors are Transition Edge Sensors (TES) made of a Ti/Au bilayer with $T_c$ tuned to operate in the 500-550 mK range. The TESs are thermally coupled to a large (10 mm diameter) spider-web absorber, made of Bi/Au coated $Si_3N_4$ wires, with a mesh size of 250 $\mu$m.

The pixel assembly has been tested at the bolometer base temperature of 350 mK, inside a custom cryogenic testbed, looking at a Gunn oscillator (140 GHz) in the far field.
We have developed custom cryogenic neoprene absorbers, in addition to a stack of standard metal meshes low-pass filters, so that the background on the detector is reduced at a level similar to the in-flight one, allowing to measure the full antenna beam. Once corrected for vignetting, the measured FWHM is consistent with the expected one.

Student (Ph.D., M.Sc. or B.Sc.) Y
Less than 5 years of experience since completion of Ph.D Y

Primary author

Co-authors

Elia Stefano Battistelli (Sapienza University of Rome, INFN Roma1) Michele Biasotti (GE) Alessandro Coppolecchia (Sapienza University of Rome, INFN Roma1) Giuseppe D'Alessandro (Sapienza University of Rome, INFN Roma1) Paolo de Bernardis (Sapienza University of Rome, INFN Roma1) Flavio Gatti (GE) Daniele Grosso (Università di Genova, Dipartimento di Fisica) Luca Lamagna (Sapienza University of Rome, INFN Roma1) Paolo Gennaro Madonia (Sapienza University of Rome, INFN Roma1) Silvia Masi (Sapienza University of Rome, INFN Roma1) Lorenzo Mele (Sapienza University of Rome, INFN Roma1) Alessandro Paiella (Sapienza University of Rome, INFN Roma1) Francesco Piacentini (Sapienza University of Rome, INFN Roma1) Giuseppe Presta (Sapienza University of Rome, INFN Roma1) Beatrice Siri (GE)

Presentation Materials