The TRUCE Collaboration


We are a collaboration of several institutions whose purpose is to design and test exciting next-generation millimeter wave pixels for studies of the Cosmic Microwave Background (CMB).  Optimized for observations at 150 GHz, each pixel contains two optically coupled transition edge sensor (TES) bolometers, both sensitive to orthogonal polarization modes.  The pixels also boast band-defining filters built into the device.  These pixels are slated for use in several upcoming next-generation CMB polarization experiments, including the Atacama B-Mode Search (ABS), the Atacama Cosmology Telescope (ACT)pol, and South Pole Telescope (SPT)pol experiments.  To learn more about what our pixels are and how they operate, take a look at the papers below.



University of Chicago

University of Colorado, Boulder

University of Michigan, Ann Arbor

National Institute of Standards and Technology, Boulder

Princeton University

NASA Goddard Space Flight Center

About Truce

Papers by TRuce

    Low Temperature Detectors (LTD) 13 Proceedings Papers:

        Appel, et al. - Characterizing and Modeling the Noise and Complex Impedance of Feedhorn-Coupled TES Polarimeters.

        Austermann, et al.  - Measurements of Bolometer Uniformity for Feedhorn Coupled TES Polarimeters.

        Bleem, et al.  - Optical Properties of Feedhorn-Coupled TES Polarimeters for CMB Polarimetry.

        Britton, et al.  - Corrugated Feedhorn Arrays in Silicon.

        McMahon, et al.  - Planar Orthomode Transducers for Feedhorn-Coupled TES Polarimeters.

        Yoon, et al.  - Feedhorn-Coupled TES Polarimeters for Next-Generation CMB Instruments.

   SPIE Astronomical Telescopes and Instrumentation 2010 Proceedings Papers:

        Britton, et al. - Corrugated Silicon Platelet Feed Horn Array for CMB Polarimetry at 150 GHz.

        Henning, et al. - Optical Efficiency of Feedhorn-Coupled TES Polarimeters for Next-Generation CMB Instruments.


    This material is based upon work at the University of Colorado at Boulder supported by the National Science Foundation under Grant No. 0705302.  Work at NIST is supported by the NIST Innovations in Measurement Science program.  Work at the University of Chicago is supported by the NSF through grant ANT- 0638937 and the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago.  It also receives generous support from the Kavli Foundation and the Gordon and Betty Moore Foundation.  Work at Princeton University is supported by Princeton University and the NSF through grants PHY-0355328 and PHY-085587.

Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation.