Aubin, FrançoisAboobaker, Asad M.Bao, ChaoyunGeach, ChristopherHelson, Kyleet al2022-06-242022-06-242017François Aubin et al. "Temperature calibration of the E and B Experiment". The Fourteenth Marcel Grossmann Meeting, pp. 2084-2089 (2017); https://doi.org/10.1142/9789813226609_0229https://doi.org/10.1142/9789813226609_0229http://hdl.handle.net/11603/25042The Fourteenth Marcel Grossmann Meeting, pp. 2084-2089 (2017)Authors: François Aubin, Asad M. Aboobaker, Chaoyun Bao, Christopher Geach, Shaul Hanany, Terry Jones, Jeff Klein, Michael Milligan, Kate Raach, Karl Young, Kyle Zilic, Kyle Helson, Andrei Korotkov, Valerie Marchenko, Gregory S. Tucker, Peter Ade, Enzo Pascale, Derek Araujo, Daniel Chapman, Joy Didier, Seth Hillbrand, Bradley Johnson, Michele Limon, Amber D. Miller, Britt Reichborn-Kjennerud, Stephen Feeney, Andrew Jaffe, Radek Stompor, Matthieu Tristram, Matt Dobbs, Kevin Macdermid, Graeme Smecher, Julian Borrill, Theodore Kisner, Gene Hilton, Johannes Hubmayr, Carl Reintsema, Carlo Baccigalupi, Giuseppe Puglisi, Adrian Lee, Ben Westbrook, Lorne Levinson and Ilan SagivThe 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 ∼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 x2 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 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