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The BICEP/Keck (BK) experiment aims to detect the imprint of primordialgravitational waves in the Cosmic Microwave Background polarization, whichwould be direct evidence of the inflation theory. While the tensor-to-scalarratio has been constrained to be r_0.05 < 0.06 at 95% c.l., furtherimprovements on this upper limit are hindered by polarized Galactic foregroundemissions and removal of gravitational lensing polarization. The 30/40 GHzreceiver of the BICEP Array (BA) will deploy at the end of 2019 and willconstrain the synchrotron foreground with unprecedented accuracy within the BKsky patch. We will show the design of the 30/40 GHz detectors and test resultssummarizing its performance. The low optical and atmospheric loading at thesefrequencies requires our TES detectors to have low saturation power in order tobe photon-noise dominated. To realize the low thermal conductivity requiredfrom a 250 mK base temperature, we developed new bolometer leg designs. We willpresent the relevant measured detector parameters: G, Tc, Rn, Psat , andspectral bands, and noise spectra. We achieved a per bolometer NEP includingall noise components of 2.07E-17 W/sqrt(Hz), including an anticipated photonnoise level 1.54E-17 W/sqrt(Hz).

Characterizing the Sensitivity of 40 GHz TES Bolometers for BICEP Array