Temperature calibration of the E and B experiment

• Main Authors: Aubin, Francois, Aboobaker, Asad M., Ade, Peter, Araujo, Derek, Baccigalupi, Carlo, Bao, Chaoyun, Borrill, Julian, Chapman, Daniel, Didier, Joy, Dobbs, Matt, Feeney, Stephen, Geach, Christopher, Hanany, Shaul, Helson, Kyle, Hillbrand, Seth, Hilton, Gene, Hubmayr, Johannes, Jaffe, Andrew, Johnson, Bradley, Jones, Terry, Kisner, Theodore, Klein, Jeff, Korotkov, Andrei, Lee, Adrian, Levinson, Lorne, Limon, Michele, Macdermid, Kevin, Marchenko, Valerie, Miller, Amber D., Milligan, Michael, Pascale, Enzo, Puglisi, Giuseppe, Raach, Kate, Reichborn-Kjennerud, Britt, Reintsema, Carl, Sagiv, Ilan, Smecher, Graeme, Stompor, Radek, Tristram, Matthieu, Tucker, Gregory S., Westbrook, Ben, Young, Karl, Zilic, Kyle
• Format: Report
• Language: unknown
• Published: arXiv 2016
• Subjects: Instrumentation and Methods for Astrophysics astro-ph.IM; Cosmology and Nongalactic Astrophysics astro-ph.CO; FOS Physical sciences; Antarc*; Antarctica
• Online Access: https://dx.doi.org/10.48550/arxiv.1601.07923; https://arxiv.org/abs/1601.07923

The E and B Experiment (EBEX) is a balloon-borne polarimeter designed to measure the polarization of the cosmic microwave background radiation and to characterize the polarization of galactic dust. EBEX was launched December 29, 2012 and circumnavigated Antarctica observing $\sim$6,000 square degrees of sky during 11 days at three frequency bands centered around 150, 250 and 410 GHz. EBEX was the first experiment to operate a kilo-pixel array of transition-edge sensor bolometers and a continuously rotating achromatic half-wave plate aboard a balloon platform. It also pioneered the use of detector readout based on digital frequency domain multiplexing. We describe the temperature calibration of the experiment. The gain response of the experiment is calibrated using a two-step iterative process. We use signals measured on passes across the Galactic plane to convert from readout-system counts to power. The effective smoothing scale of the EBEX optics and the star camera-to-detector offset angles are determined through \c{hi}2 minimization using the compact HII region RCW 38. This two-step process is initially performed with parameters measured before the EBEX 2013 flight and then repeated until the calibration factor and parameters converge. : 6 pages, 3 figures, Proceedings of the 14th Marcel Grossman Conference