Article

Antenna-coupled TES bolometer arrays for BICEP2/Keck and SPIDER.

Department of Physics, California Institute of Technology, 91125, Pasadena, CA, USA; Department of Physics and Astronomy, University of British Columbia, V6T 1Z1, Vancouver, British Columbia, Canada; Jet Propulsion Laboratory, 91109, Pasadena, CA, USA; NIST Quantum Devices Group, 325, 80305, Broadway, Boulder, CO, USA; Harvard-Smithsonian Center for Astrophysics, 02138, Cambridge, MA, USA; Department of Physics, Stanford University, 94305, Palo Alto, CA, USA; Kavli Institute for Particle Astrophysics and Cosmology, 94025, Menlo Park, CA, USA; School of Physics and Astronomy, Cardiff University, CF24 3AA, Cardiff, UK
Proc SPIE 09/2010; DOI: 10.1117/12.857914
Source: arXiv

ABSTRACT BICEP2/Keck and SPIDER are cosmic microwave background (CMB) polarimeters targeting the B-mode polar-ization induced by primordial gravitational waves from inflation. They will be using planar arrays of polarization sensitive antenna-coupled TES bolometers, operating at frequencies between 90 GHz and 220 GHz. At 150 GHz each array consists of 64 polarimeters and four of these arrays are assembled together to make a focal plane, for a total of 256 dual-polarization elements (512 TES sensors). The detector arrays are integrated with a time-domain SQUID multiplexer developed at NIST and read out using the multi-channel electronics (MCE) developed at the University of British Columbia. Following our progress in improving detector parameters uniformity across the arrays and fabrication yield, our main effort has focused on improving detector arrays optical and noise performances, in order to produce science grade focal planes achieving target sensitivities. We report on changes in detector design implemented to optimize such performances and following focal plane arrays characterization. BICEP2 has deployed a first 150 GHz science grade focal plane to the South Pole in December 2009.

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Jun 4, 2014