Kernasovskiy, S.Ade, P. A. R.Aikin, R. W.Amiri, M.Benton, S.Bischoff, ColinBock, J. J.Bonetti, J. A.Brevik, J. A.Burger, B.Davis, G.Dowell, C. D.Duband, L.Filippini, J. P.Fliescher, S.Golwala, S. R.Halpern, M.Hasselfield, M.Hilton, G.Hristov, V. V.Irwin, K.Kovac, JohnKuo, C. L.Leitch, E.Lueker, M.Netterfield, C. B.Nguyen, H. T.O, R.Ogburn, R. W.Pryke, CReintsema, C.Ruhl, J. E.Runyan, M. C.Schwarz, R.Sheehy, C. D.Staniszewski, Z.Sudiwala, R.Teply, G.Tolan, J. E.Turner, A. D.Vieregg, A.Wiebe, D. V.Wilson, P.Wong, C. L.2017-07-142012Kernasovskiy, S., P. A. R. Ade, R. W. Aikin, M. Amiri, S. Benton, C. Bischoff, J. J. Bock et al. 2012. "Optimization and sensitivity of the Keck Array." In Proceedings International Society for Optics and Photonics (SPIE) Astronomical Telescopes+ Instrumentation, San Fransisco, CA, January 21-26, 2012: 84521B-84521B.9780819491534http://nrs.harvard.edu/urn-3:HUL.InstRepos:33445979The Keck Array (SPUD) began observing the cosmic microwave background’s polarization in the winter of 2011 at the South Pole. The Keck Array follows the success of the predecessor experiments Bicep and Bicep2,1 using five on-axis refracting telescopes. These have a combined imaging array of 2500 antenna-coupled TES bolometers read with a SQUID-based time domain multiplexing system. We will discuss the detector noise and the optimization of the readout. The achieved sensitivity of the Keck Array is 11.5 µKCMB√ s in the 2012 configuration.en-USCosmic Microwave BackgroundpolarizationinflationKeck ArrayBicep2TESdetector noiseConference Paper2017-02-1320122017-07-1410.1117/12.926934