  The Simons Observatory is a ground-based cosmic microwave background survey
experiment that consists of three 0.5 m small-aperture telescopes and one 6 m
large-aperture telescope, sited at an elevation of 5200 m in the Atacama Desert
in Chile. SO will deploy 60,000 transition-edge sensor (TES) bolometers in 49
separate focal-plane modules across a suite of four telescopes covering 30/40
GHz low frequency (LF), 90/150 GHz mid frequency (MF), and 220/280 GHz
ultra-high frequency (UHF). Each MF and UHF focal-plane module packages 1720
optical detectors spreading across 12 detector bias lines that provide voltage
biasing to the detectors. During observation, detectors are subject to varying
atmospheric emission and hence need to be re-biased accordingly. The re-biasing
process includes measuring the detector properties such as the TES resistance
and responsivity in a fast manner. Based on the result, detectors within one
bias line then are biased with suitable voltage. Here we describe a technique
for re-biasing detectors in the modules using the result from bias-step
measurement.
