Bryan, Sean A.Ade, Peter A. R.Amiri, MandanaBenton, SteveHelson, Kyleet al2022-06-242022-06-242010-07-15Sean A. Bryan, Peter A. R. Ade, Mandana Amiri, Steve Benton, Richard Bihary, James J. Bock, J. Richard Bond, Joseph A. Bonetti, H. Cynthia Chiang, Carlo R. Contaldi, Brendan P. Crill, Daniel O'Dea, Olivier Dore, Marzieh Farhang, Jeffrey P. Filippini, Laura Fissel, Natalie Gandilo, Sunil Golwala, Jon E. Gudmundsson, Matthew Hasselfield, Mark Halpern, Kyle R. Helson, Gene Hilton, Warren Holmes, Viktor V. Hristov, Kent D. Irwin, William C. Jones, Chao Lin Kuo, Carrie J. MacTavish, Peter Mason, Tracy Morford, Thomas E. Montroy, C. Barth Netterfield, Alexandra S. Rahlin, Carl D. Reintsema, Daniel Riley, John E. Ruhl, Marcus C. Runyan, Matthew A. Schenker, Jamil Shariff, Juan Diego Soler, Amy Transrud, Rebecca Tucker, Carole Tucker, Anthony Turner, "Modeling and characterization of the SPIDER half-wave plate," Proc. SPIE 7741, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy V, 77412B (15 July 2010); https://doi.org/10.1117/12.857837https://doi.org/10.1117/12.857837http://hdl.handle.net/11603/25048SPIE Astronomical Telescopes + Instrumentation, 2010, San Diego, California, United StatesAuthors: Sean A. Bryan, Peter A. R. Ade, Mandana Amiri, Steve Benton, Richard Bihary, James J. Bock, J. Richard Bond, Joseph A. Bonetti, H. Cynthia Chiang, Carlo R. Contaldi, Brendan P. Crill, Daniel O'Dea, Olivier Dore, Marzieh Farhang, Jeffrey P. Filippini, Laura Fissel, Natalie Gandilo, Sunil Golwala, Jon E. Gudmundsson, Matthew Hasselfield, Mark Halpern, Kyle R. Helson, Gene Hilton, Warren Holmes, Viktor V. Hristov, Kent D. Irwin, William C. Jones, Chao Lin Kuo, Carrie J. MacTavish, Peter Mason, Tracy Morford, Thomas E. Montroy, C. Barth Netterfield, Alexandra S. Rahlin, Carl D. Reintsema, Daniel Riley, John E. Ruhl, Marcus C. Runyan, Matthew A. Schenker, Jamil Shariff, Juan Diego Soler, Amy Transrud, Rebecca Tucker, Carole Tucker, Anthony TurnerSpider is a balloon-borne array of six telescopes that will observe the Cosmic Microwave Background. The 2624 antenna-coupled bolometers in the instrument will make a polarization map of the CMB with approximately one-half degree resolution at 145 GHz. Polarization modulation is achieved via a cryogenic sapphire half-wave plate (HWP) skyward of the primary optic. We have measured millimeter-wave transmission spectra of the sapphire at room and cryogenic temperatures. The spectra are consistent with our physical optics model, and the data gives excellent measurements of the indices of A-cut sapphire. We have also taken preliminary spectra of the integrated HWP, optical system, and detectors in the prototype Spider receiver. We calculate the variation in response of the HWP between observing the CMB and foreground spectra, and estimate that it should not limit the Spider constraints on inflation.9 pagesen-USThis work was written as part of one of the author's official duties as an Employee of the United States Government and is therefore a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law.Public Domain Mark 1.0Text