280 GHz Focal Plane Unit Design and Characterization for the SPIDER-2 Suborbital Polarimeter

TL;DR

This paper details the design, construction, and characterization of 280 GHz bolometric focal plane units for the SPIDER-2 balloon-borne CMB experiment, aiming to detect primordial gravitational waves through B-mode polarization.

Contribution

It introduces a new 280 GHz focal plane design with high yield and uniformity, optimized for balloon-borne CMB polarization measurements, including detailed shielding and cryogenic characterization.

Findings

High array yield up to 95% including wiring/readout defects

Median TES saturation power of ~3 pW at 300 mK with <6% variation

Successful cryogenic characterization demonstrating uniform bolometer parameters

Abstract

We describe the construction and characterization of the 280 GHz bolometric focal plane units (FPUs) to be deployed on the second flight of the balloon-borne SPIDER instrument. These FPUs are vital to SPIDER's primary science goal of detecting or placing an upper limit on the amplitude of the primordial gravitational wave signature in the cosmic microwave background (CMB) by constraining the B-mode contamination in the CMB from Galactic dust emission. Each 280 GHz focal plane contains a 16 x 16 grid of corrugated silicon feedhorns coupled to an array of aluminum-manganese transition-edge sensor (TES) bolometers fabricated on 150 mm diameter substrates. In total, the three 280 GHz FPUs contain 1,530 polarization sensitive bolometers (765 spatial pixels) optimized for the low loading environment in flight and read out by time-division SQUID multiplexing. In this paper we describe the mechanical, thermal, and magnetic shielding architecture of the focal planes and present cryogenic measurements which characterize yield and the uniformity of several bolometer parameters. The assembled FPUs have high yields, with one array as high as 95% including defects from wiring and readout. We demonstrate high uniformity in device parameters, finding the median saturation power for each TES array to be ~3 pW at 300 mK with a less than 6% variation across each array at one standard deviation. These focal planes will be deployed alongside the 95 and 150 GHz telescopes in the SPIDER-2 instrument, slated to fly from McMurdo Station in Antarctica in December 2018.