Design and pre-flight performance of SPIDER 280 GHz receivers

E. C. Shaw (1); P. A. R. Ade (2); S. Akers (3); M. Amiri (4); J.; Austermann (5); J. Beall (5); D. T. Becker (5); S. J. Benton (6); A. S.; Bergman (6); J. J. Bock (7; 8); J. R. Bond (9); S. A. Bryan (10); H. C.; Chiang (11); C. R. Contaldi (12); R. S. Domagalski (13); O. Dor\'e (7; 8),; S. M. Duff (5); A. J. Duivenvoorden (6); H. K. Eriksen (14); M. Farhang (15),; J. P. Filippini (1; 16); L. M. Fissel (17); A. A. Fraisse (6); K. Freese; (18; 19); M. Galloway (14); A. E. Gambrel (20); N. N. Gandilo (13); K.; Ganga (21); A. Grigorian (5); R. Gualtieri (22); J. E. Gudmundsson (19); M.; Halpern (4); J. Hartley (13); M. Hasselfield (23); G. Hilton (5); W. Holmes; (8); V. V. Hristov (7); Z. Huang (9); J. Hubmayr (5); K. D. Irwin (24 and; 25); W. C. Jones (6); A. Kahn (1); C. L. Kuo (24); Z. D. Kermish (6); A.; Lennox (1); J. S.-Y. Leung (13; 26); S. Li (6); P. V. Mason (7); K.; Megerian (8); L. M. Mocanu (14); L. Moncelsi (7); T. A. Morford (7); J. M.; Nagy (27; 28); R. Nie (1); C. B. Netterfield (13; 29; 26); M. Nolta; (9); B. Osherson (1); I. L. Padilla (29; 30); A. S. Rahlin (20; 31); S.; Redmond (32); C. Reintsema (5); L. J. Romualdez (33); J. E. Ruhl (3); M. C.; Runyan (8); J. A. Shariff (9); C. Shiu (6); J. D. Soler (34; 35); X. Song; (6); H. Thommesen (14); A. Trangsrud (7; 8); C. Tucker (2); R. S. Tucker; (7); A. D. Turner (8); J. Ullom (5); J. F. van der List (6); J. Van Lanen; (5); M. R. Vissers (5); A. C. Weber (8); S. Wen (3); I. K. Wehus (14); D. V.; Wiebe (4); E. Y. Young (24; 36) ((1) Department of Physics; University of; Illinois at Urbana-Champaign; (2) School of Physics; Astronomy; Cardiff; University; (3) Physics Department; Case Western Reserve University; (4); Department of Physics; Astronomy; University of British Columbia; (5); National Institute of Standards; Technology; (6) Department of Physics,; Princeton University; (7) Division of Physics; Mathematics; Astronomy,; California Institute of Technology; (8) Jet Propulsion Laboratory; (9); Canadian Institute for Theoretical Astrophysics; University of Toronto; (10); School of Electrical; Computer; and Energy Engineering; Arizona State; University; (11) Department of Physics; McGill University; (12) Blackett; Laboratory; Imperial College London; (13) Department of Astronomy and; Astrophysics; University of Toronto; (14) Institute of Theoretical; Astrophysics; University of Oslo; (15) Department of Physics; Shahid Beheshti; University; (16) Department of Astronomy; University of Illinois at; Urbana-Champaign; (17) Department of Physics; Engineering Physics and; Astronomy; Queen's University; (18) Department of Physics; The University of; Texas at Austin; (19) The Oskar Klein Centre for Cosmoparticle Physics,; Department of Physics; Stockholm University; (20) Kavli Institute for; Cosmological Physics; University of Chicago; (21) Universit\'e de Paris,; CNRS; AstroParticule et Cosmologie; (22) HEP; Argonne National Laboratory,; (23) Department of Astronomy; Astrophysics; Pennsylvania State University,; (24) Department of Physics; Stanford University; (25) SLAC National; Accelerator Laboratory; (26) Dunlap Institute for Astronomy; Astrophysics,; University of Toronto; (27) Department of Physics; Washington University in; St. Louis; (28) McDonnell Center for the Space Sciences; Washington; University in St. Louis; (29) Department of Physics; University of Toronto,; (30) Department of Physics; Astronomy; Johns Hopkins University; (31); Fermi National Accelerator Laboratory; (32) Department of Mechanical and; Aerospace Engineering; Princeton University; (33) University of Toronto; Institute for Aerospace Studies; (34) Max-Planck-Institute for Astronomy,; (35) Laboratoire AIM; Paris-Saclay; CEA/IRFU/SAp - CNRS - Universit\'e Paris; Diderot; (36) Kavli Institute for Particle Astrophysics; Cosmology,; Stanford University)

arXiv:2012.12407·astro-ph.IM·December 24, 2020

Design and pre-flight performance of SPIDER 280 GHz receivers

E. C. Shaw (1), P. A. R. Ade (2), S. Akers (3), M. Amiri (4), J., Austermann (5), J. Beall (5), D. T. Becker (5), S. J. Benton (6), A. S., Bergman (6), J. J. Bock (7, 8), J. R. Bond (9), S. A. Bryan (10), H. C., Chiang (11), C. R. Contaldi (12), R. S. Domagalski (13)

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TL;DR

This paper details the design, characterization, and pre-flight testing of new 280 GHz receivers for the Spider telescope, enhancing its capability to study polarized Galactic dust emission and primordial B-mode signals.

Contribution

It introduces the design and testing of three new 280 GHz receivers with over 1500 sensors, improving Spider’s multi-frequency polarization mapping capabilities.

Findings

01

Successful pre-flight laboratory characterization of detectors.

02

Optical performance meets design specifications.

03

Receivers ready for deployment in upcoming flight.

Abstract

In this work we describe upgrades to the Spider balloon-borne telescope in preparation for its second flight, currently planned for December 2021. The Spider instrument is optimized to search for a primordial B-mode polarization signature in the cosmic microwave background at degree angular scales. During its first flight in 2015, Spider mapped ~10% of the sky at 95 and 150 GHz. The payload for the second Antarctic flight will incorporate three new 280 GHz receivers alongside three refurbished 95- and 150 GHz receivers from Spider's first flight. In this work we discuss the design and characterization of these new receivers, which employ over 1500 feedhorn-coupled transition-edge sensors. We describe pre-flight laboratory measurements of detector properties, and the optical performance of completed receivers. These receivers will map a wide area of the sky at 280 GHz, providing new…

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