Design and pre-flight performance of SPIDER 280 GHz receivers

Journal Article · Sun Dec 13 00:00:00 EST 2020 · Proceedings of SPIE - The International Society for Optical Engineering

DOI:https://doi.org/10.1117/12.2562941· OSTI ID:1831080

Shaw, E. C. ^[1]; Ade, P. A.R. ^[2]; Akers, S. ^[3]; Amiri, M. ^[4]; Austermann, Jason E. ^[5]; Beall, James A. ^[5]; Becker, D. T. ^[5]; Benton, S. J. ^[6]; Bergman, A. S. ^[6]; Bock, J. J. ^[7]; Bond, J. R. ^[8]; Bryan, S. A. ^[9]; Chiang, H. C. ^[10]; Contaldi, C. R. ^[11]; Domagalski, R. S. ^[8]; Dore, O. ^[7]; Duff, S. M. ^[5]; Duivenvoorden, A. J. ^[6]; Eriksen, H. K. ^[12]; Farhang, M. ^[13] ; Filippini, J. P. ^[14]; Fissel, L. M. ^[15]; Fraisse, A. A. ^[6]; Freese, K. ^[16]; Galloway, M. ^[12]; Gambrel, A. E. ^[17]; Gandilo, N. N. ^[8]; Ganga, K. ^[18]; Grigorian, A. ^[5]; Gualtieri, R. ^[19]; Gudmundsson, J. E. ^[20]; Halpern, M. ^[4]; Hartley, J. ^[8]; Hasselfield, M. ^[21]; Hilton, G. ^[5]; Holmes, W. ^[7]; Hristov, V. V. ^[22]; Huang, Z. ^[8]; Hubmayr, Johannes ^[5]; Irwin, K. D. ^[23]; Jones, W. C. ^[6]; Kahn, A. ^[14]; Kuo, C. L. ^[23]; Kermish, Z. D. ^[6]; Lennox, A. ^[14]; Leung, J. S.-Y. ^[8]; Megerian, K. ^[7]; Li, S. ^[6]; Reintsema, C. ^[5]; Mason, P. V. ^[22]; Runyan, M. C. ^[7]; Moncelsi, L. ^[22]; Morford, T. A. ^[22]; Nagy, J. M. ^[24]; Nie, R. ^[14]; Nolta, M. ^[8]; Netterfield, C. B. ^[8]; Mocanu, L. M. ^[12]; Padilla, I. L. ^[25]; Osherson, B. ^[14]; Rahlin, A. S. ^[26]; Redmond, S. ^[6]; Turner, A. D. ^[7]; Romualdez, L. J. ^[8]; Ruhl, J. E. ^[3]; Shariff, J. A. ^[8]; Shiu, C. ^[6]; Soler, J. D. ^[27]; Song, X. ^[6]; Trangsrud, A. ^[7]; Thommesen, H. ^[12]; Tucker, C. ^[2]; Tucker, R. S. ^[22]; Ullom, Joel ^[5]; van der List, J. F. ^[6]; Van Lanen, Jeff ^[5]; Vissers, M. R. ^[5]; Weber, A. C. ^[7]; Wen, S. ^[3]; Wehus, I. K. ^[12]; Wiebe, D. V. ^[4]; Young, E. Y. ^[28]

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1. Univ. of Illinois at Urbana-Champaign, IL (United States); Univ of Texas, Austin
2. Cardiff University, Cardiff (United Kingdom)
3. Case Western Reserve Univ., Cleveland, OH (United States)
4. Univ. of British Columbia, Vancouver, BC (Canada)
5. National Inst. of Standards and Technology (NIST), Boulder, CO (United States)
6. Princeton Univ., NJ (United States)
7. California Institute of Technology (CalTech), Pasadena, CA (United States). Jet Propulsion Lab. (JPL)
8. Univ. of Toronto, ON (Canada)
9. Arizona State Univ., Tempe, AZ (United States)
10. McGill Univ., Montreal, QC (Canada)
11. Imperial College, London (United Kingdom)
12. Univ. of Oslo (Norway)
13. Shahid Beheshti Univ., Velenjak, Tehran (Iran)
14. Univ. of Illinois at Urbana-Champaign, IL (United States)
15. Queen's Univ., Kingston, ON (Canada)
16. Univ. of Texas, Austin, TX (United States); Stockholm Univ. (Sweden)
17. Univ. of Chicago, IL (United States)
18. Univ. of Paris (France)
19. Argonne National Lab. (ANL), Argonne, IL (United States)
20. Stockholm Univ. (Sweden)
21. Pennsylvania State Univ., University Park, PA (United States)
22. California Institute of Technology (CalTech), Pasadena, CA (United States)
23. Stanford Univ., CA (United States)
24. Washington Univ., St. Louis, MO (United States)
25. Johns Hopkins Univ., Baltimore, MD (United States)
26. Univ. of Chicago, IL (United States); Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)
27. Max-Planck-Institute for Astronomy, Heidelberg (Germany)
28. Stanford Univ., CA (United States). Kavli Institute for Particle Astrophysics & Cosmology

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 information on polarized Galactic dust emission that will help to separate it from the cosmological signal.

• Research Organization: Univ. of Texas, Austin, TX (United States)
• Sponsoring Organization: Canadian Space Agency; National Aeronautics and Space Administration (NASA); National Science Foundation (NSF); Natural Sciences and Engineering Research Council (NSERC); Research Council of Norway; Swedish Research Council; USDOE Office of Science (SC), High Energy Physics (HEP)
• Grant/Contract Number: SC0007859
• OSTI ID: 1831080
• Alternate ID(s): OSTI ID: 1842740
• Journal Information: Proceedings of SPIE - The International Society for Optical Engineering, Journal Name: Proceedings of SPIE - The International Society for Optical Engineering Vol. 11453; ISSN 0277-786X
• Publisher: SPIE
• Country of Publication: United States
• Language: English

Related Subjects

42 ENGINEERING
Spider
cosmic microwave background
cosmology
millimeter wave instrumentation
polarization
scientific ballooning
scientific instrumentation
transition-edge sensor