Detector fabrication development for the LiteBIRD satellite mission

Westbrook, Ben; Raum, Christopher; Lee, A. T.; Farias, Nicole; Sasse, Trevor; Suzuki, Aritoki; Kane, E. D.; Austermann, J. E.; Beall, James A.; Duff, Shannon M.; Hubmayr, Johannes; Hilton, G. C.; Lanen, Jeff Van; Vissers, Michael; Link, Moritz; Halverson, N. W.; Jaehnig, Greg; Tommaso, Ghinga,; Stever, S.; Minami, Y.; Thompson, K. L.; Russell, M.; Arnold, K.; Seibert, Joseph; Silva-Feaver, Maximiliano

doi:10.1117/12.2562978

Cited by 15 publications

(9 citation statements)

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“…Detailed descriptions, including important systematics of sinuous antennas, can be found in previous reports. 1,16 We chose this technology for the LFT and MFT as its broadband nature is well suited to cover the frequency ranges required by LiteBIRD. For this application we describe the specific antenna used to fabricate a LF-4 prototype as shown in Figure 2.…”

Section: Sinuous Antennamentioning

confidence: 99%

“…The standard fabrication flow of sinuous antenna bolometers at MNL UC Berkeley is well described in previous technology development papers for LiteBIRD. 11,16 These proceedings describes the initial 'pre-processing' fabrication steps we took to coat the back side of the wafers with palladium for cosmic ray mitigation.…”

Section: Device Wafer Fabricationmentioning

confidence: 99%

“…A detailed discussion of the experimental setup for creating a hot cosmic ray environment can be found in a previous SPIE proceedings. 16 2. There is good agreement between the two measurement systems.…”

Section: Cosmic Ray Testingmentioning

confidence: 99%

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Development of the low frequency telescope focal plane detector modules for LiteBIRD

Westbrook¹,

Raum²,

Lee³

et al. 2022

Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy XI

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LiteBIRD is a JAXA-led strategic large-class satellite mission designed to measure the polarization of the cosmic microwave background and Galactic foregrounds from 34 to 448 GHz across the entire sky from L2 in the late 2020s. The scientific payload includes three telescopes which are called the low-, mid-, and high-frequency telescopes each with their own receiver that covers a portion of the mission's frequency range. The low frequency telescope will map synchrotron radiation from the Galactic foreground and the cosmic microwave background. We discuss the design, fabrication, and characterization of the low-frequency focal plane modules for low-frequency telescope, which has a total bandwidth ranging from 34 to 161 GHz. There will be a total of 4 different pixel types with 8 overlapping bands to cover the full frequency range. These modules are housed in a single low-frequency focal plane unit which provides thermal isolation, mechanical support, and radiative baffling for the detectors. The module design implements multi-chroic lenslet-coupled sinuous antenna arrays coupled to transition edge sensor bolometers read out with frequencydomain mulitplexing. While this technology has strong heritage in ground-based cosmic microwave background experiments, the broad frequency coverage, low optical loading conditions, and the high cosmic ray background of the space environment require further development of this technology to be

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Section: Sinuous Antennamentioning

confidence: 99%

Section: Device Wafer Fabricationmentioning

confidence: 99%

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Development of the low frequency telescope focal plane detector modules for LiteBIRD

Westbrook¹,

Raum²,

Lee³

et al. 2022

Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy XI

Self Cite

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“…Concerning measurement noise, the described technique relies upon coherent detection of the received signal [27], where the (complex) waveform is preserved, after frequency down-conversion to complex baseband, for further post-processing (correlation between fundamental and high order mode), as opposed to non-coherent detection where only the power of the incoming signal is detected. The implication is that state-of-the-art non-coherent detectors with ultimate noise performance like Superconducting Transition Edge Sensor (TES) bolometers (planned for LiteBIRD [28]) or emerging Microwave Kinetic Inductance Detector (MKID) technology [29], are not applicable to the presented approach. Coherent and non-coherent detection might be not mutually exclusive, because non coherent detection of the fundamental signal and coherent correlation of fundamental and high order mode may co-exist on different paths, however the practical feasibility of such architecture is not verified in this account.…”

Section: Implementation Aspectsmentioning

confidence: 99%

New observables of the cosmic microwave background

Lanucara

Daddato

2022

Exp Astron

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“…In this paper we present the system we have developed for an initial assessment of the magnetic field sensitivity of an AlMn TES prototype. The prototype tested for this paper came from an early fabrication run and does not fully meet LiteBIRD specifications, in particular we measured T c ∼ 220 mK and P sat ∼ 4 pW, while T c ∼ 170 mK and P sat ∼ 1 pW are the target 23,24 (more design and measured parameters of the TES tested are reported in Table 1). Nevertheless, we decided to report these results given the scarcity of data about TES magnetic field sensitivity in the literature.…”

Section: Introductionmentioning

confidence: 99%

Testing magnetic interference between TES detectors and the telescope environment for future CMB satellite missions

Ghigna

Hoang²,

Hasebe

et al. 2022

Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy XI

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The two most common components of several upcoming CMB experiments are large arrays of superconductive TES (Transition-Edge Sensor) detectors and polarization modulator units, e.g. continuously-rotating Half-Wave Plates (HWP). A high detector count is necessary to increase the instrument raw sensitivity, however past experiments have shown that systematic effects are becoming one of the main limiting factors to reach the sensitivity required to detect primordial B-modes. Therefore, polarization modulators have become popular in recent years to mitigate several systematic effects. Polarization modulators based on HWP technologies require a rotating mechanism to spin the plate and modulate the incoming polarized signal. In order to minimize heat dissipation from the rotating mechanism, which is a stringent requirement particularly for a space mission like LiteBIRD, we can employ a superconductive magnetic bearing to levitate the rotor and achieve contactless rotation. A disadvantage of this technique is the associated magnetic fields generated by those systems. In this paper we investigate the effects on a TES detector prototype and find no detectable T c variations due to an applied constant (DC) magnetic field, and a non-zero TES response to varying (AC) magnetic fields. We quantify a worst-case TES responsivity to the applied AC magnetic field of ∼ 10 5 pA/G, and give a preliminary interpretation of the pick-up mechanism.

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Detector fabrication development for the LiteBIRD satellite mission

Cited by 15 publications

References 0 publications

Development of the low frequency telescope focal plane detector modules for LiteBIRD

Development of the low frequency telescope focal plane detector modules for LiteBIRD

New observables of the cosmic microwave background

Testing magnetic interference between TES detectors and the telescope environment for future CMB satellite missions

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