Showing papers by "Marzieh Farhang published in 2008"
TL;DR: Spider as discussed by the authors is a balloon-borne experiment that will measure the polarization of the Cosmic Microwave Background over a large fraction of a sky at 1 resolution, using six monochromatic refracting millimeter-wave telescopes with large arrays of antenna-coupled transition-edge superconducting bolometers.
Abstract: Spider is a balloon-borne experiment that will measure the polarization of the Cosmic Microwave Backgroundover a large fraction of a sky at 1 resolution. Six monochromatic refracting millimeter-wave telescopes withlarge arrays of antenna-coupled transition-edge superconducting bolometers will provide system sensitivities of4.2 and 3.1 µ K cmb s at 100 and 150 GHz, respectively. A rotating half-wave plate will modulate the polarizationsensitivity of each telescope, controlling systematics. Bolometer arrays operating at 225 GHz and 275 GHz willallow removal of polarized galactic foregrounds. In a 2- 6 day rst ight from Alice Springs, Australia in 2010,Spider will map 50% of the sky to a depth necessary to improve our knowledge of the reionization optical depthby a large factor. 1. INTRODUCTION Rapid progressin millimeter-wave receiver technology enabled major advances in cosmologyover the past decade.Extremely sensitive receivers measur ed the very faint anisotro pies and polarization of the Cosmic MicrowaveBackground (CMB), which are a mere part in 10
71 citations
TL;DR: Spider as mentioned in this paper is a balloon-borne experiment that will measure the polarization of the Cosmic Microwave Background over a large fraction of a sky at 1 degree resolution using six monochromatic refracting millimeter-wave telescopes with large arrays of antenna-coupled transition-edge superconducting bolometers.
Abstract: Spider is a balloon-borne experiment that will measure the polarization of the Cosmic Microwave Background over a large fraction of a sky at 1 degree resolution. Six monochromatic refracting millimeter-wave telescopes with large arrays of antenna-coupled transition-edge superconducting bolometers will provide system sensitivities of 4.2 and 3.1 micro K_cmb rt s at 100 and 150 GHz, respectively. A rotating half-wave plate will modulate the polarization sensitivity of each telescope, controlling systematics. Bolometer arrays operating at 225 GHz and 275 GHz will allow removal of polarized galactic foregrounds. In a 2-6 day first flight from Alice Springs, Australia in 2010, Spider will map 50% of the sky to a depth necessary to improve our knowledge of the reionization optical depth by a large factor.
15 citations