LiteBIRD: lite satellite for the study of B-mode polarization and inflation from cosmic microwave background radiation detection

Ishino, H.; Akiba, Y.; Arnold, K.; Barron, Darcy; Borrill, J.; Chendra, R.; Chinone, Yuji; Cho, S.; Cukierman, A.; Haan, T. de; Dobbs, M.; Dominjon, A.; Dotani, Tadayasu; Elleflot, T.; Errard, Josquin; Fujino, T.; Fuke, H.; Funaki, T.; Goeckner-Wald, N.; Halverson, N. W.; Harvey, P.; Hasebe, Takashi; Hasegawa, M.; Hattori, K.; Hattori, Makoto; Hazumi, M.; Hidehira, N.; Hill, Charles A.; Hilton, G. C.; Holzapfel, W. L.; Hori, Y.; Hubmayr, Johannes; Ichiki, Kiyotomo; Imada, Hiroaki; Inatani, Junji; Inoue, M.; Inoue, Yuki; Irie, Fumitoshi; Irwin, K. D.; Ishitsuka, H.; Jeong, O.; Kanai, Hiroaki; Karatsu, K.; Kashima, Shingo; Katayama, N.; Kawano, Isao; Kawasaki, T.; Keating, Brian; Kernasovskiy, S. A.; Keskitalo, R.; Kibayashi, A.; Kida, Yosuke; Kimura, N.; Kimura, Kouji; Kisner, T. S.; Kohri, Kazunori; Komatsu, Eiichiro; Komatsu, Kunimoto; Kuo, Chao-Lin; Kuromiya, S.; Kusaka, A.; Lee, A.; Li, D.; Linder, Eric V.; Maki, M.; Matsuhara, Hideo; Matsumura, Tomotake; Matsuoka, Satoshi; Matsuura, Shuji; Mima, Silvana; Minami, Y.; Mitsuda, Kazuhisa; Nagai, Makoto; Nagasaki, T.; Nagata, Ryo; Nakajima, Makoto; Nakamura, Shōgo; Namikawa, Toshiya; Naruse, Mitsuhide; Nishibori, Toshiyuki; Nishijo, Kunitoshi; Nishino, Hitoshi; Noda, Atsushi; Noguchi, Takashi; Ogawa, H.; Ogburn, W.; Oguri, S.; Ohta, I.; Okada, Nozomi; Okamoto, Atsushi; Okamura, Takahiro; Otani, Chiko; Pisano, G.; Rebeiz, Gabriel M.; Richards, P. L.; Sakai, S.; Sakurai, Y.; Sato, Yoichi; Sato, N.; Segawa, Y.; Sekiguchi, Shigeyuki; Sekímoto, Yutaro; Sekine, Masakazu; Seljak, Uroš; Sherwin, Blake D.; Shimizu, Toshimasa; Shinozaki, Kazuo; Shu, S.; Stompor, R.; Sugai, Hajime; Sugita, Hiroyuki; Suzuki, Junya; Suzuki, Toyoaki; Suzuki, Aritoki; Tajima, O.; Takada, Suguru; Takakura, S.; Takano, Katsuyoshi; Takatori, S.; Takei, Yoh; Tanabe, D.; Tomaru, T.; Tomita, Naohide; Turin, P.; Uozumi, S.; Utsunomiya, Shin; Uzawa, Yoshinori; Wada, Takehiko; Watanabe, H.; Westbrook, B.; Whitehorn, N.; Yamada, Yosuke; Yamamoto, Ryo; Yamasaki, Noriko Y.; Yamashita, T.; Yoshida, Tetsuya; Yoshida, Mitsuhiro; Yotsumoto, Kazuhiko

doi:10.1117/12.2231995

Cited by 28 publications

(29 citation statements)

References 9 publications

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“…The baseline foreground-cleaning results have been obtained based on an eight-dimensional parameterization of the foregrounds, including synchrotron power-law spectral index plus curvature and effective temperature of dust, plus power-law index of dust emissivity for Q and U Stokes parameters, each of which is allowed to vary across the sky. Systematic uncertainties have also been studied [33], including beam systematics [14], instrumental polarization and HWP harmonics, polarization efficiency, relative and absolute gain, pointing, polarization angle, time-correlated noise, cosmic ray glitches, bandpass mismatch [34], transfer function, nonlinearity, and non-uniformity in HWP, with realistic ground/in-flight calibration methods taken into account [e.g., 15,35]. Through all these studies, it has been shown that the Journal of Low Temperature Physics (2020) 199:1107-1117 updated focal-plane designs satisfy LiteBIRD's full success of the total uncertainty in the tensor-to-scalar ratio of less than 0.001, with its uncertainty budgets distributed comparably into a statistical part (including foreground residual and lensing B-mode), a systematic part, and a margin.…”

Section: Foreground-cleaning and Systematic Uncertainty Studiesmentioning

confidence: 99%

Updated Design of the CMB Polarization Experiment Satellite LiteBIRD

et al. 2020

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Recent developments of transition-edge sensors (TESs), based on extensive experience in ground-based experiments, have been making the sensor techniques mature enough for their application on future satellite cosmic microwave background (CMB) polarization experiments. LiteBIRD is in the most advanced phase among such future satellites, targeting its launch in Japanese Fiscal Year 2027 (2027FY) with JAXA's H3 rocket. It will accommodate more than 4000 TESs in focal planes of reflective low-frequency and refractive medium-and-high-frequency telescopes in order to detect a signature imprinted on the CMB by the primordial gravitational waves predicted in cosmic inflation. The total wide frequency coverage between 34 and 448 GHz enables us to extract such weak spiral polarization patterns through the precise subtraction of our Galaxy's foreground emission by using spectral differences among CMB and foreground signals. Telescopes are cooled down to 5 K for suppressing thermal noise and contain polarization modulators with transmissive half-wave plates at individual apertures for separating sky polarization signals from artificial polarization and for mitigating from instrumental 1/f noise. Passive cooling by using V-grooves supports active cooling with mechanical coolers as well as adiabatic demagnetization refrigerators. Sky observations from the second Sun-Earth Lagrangian point, L2, are planned for 3 years.

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Section: Foreground-cleaning and Systematic Uncertainty Studiesmentioning

confidence: 99%

Updated Design of the CMB Polarization Experiment Satellite LiteBIRD

et al. 2020

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“…10]. Therefore, the CRHWP has the potential to be one of the essential tools for the next-generation CMB experiments, such as CMB-S4 [11], a nextgeneration ground-based experiment, and LiteBIRD, a proposed space mission for full-sky CMB polarization measurements [12].…”

Section: Introductionmentioning

confidence: 99%

“…This method can be applied to optical systems in which all the optical elements between the CRHWP and the sky are reflective 12. We assume that the contribution from the non-ideality of the HWP on n = 4 HWPSS, A(4)0 ⟨I in ⟩ , is small compared to that from the instrumental polarization, here.…”

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confidence: 99%

Performance of a continuously rotating half-wave plate on the POLARBEAR telescope

Takakura

Aguilar

Akiba

et al. 2017

J. Cosmol. Astropart. Phys.

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A continuously rotating half-wave plate (CRHWP) is a promising tool to improve the sensitivity to large angular scales in cosmic microwave background (CMB) polarization measurements. With a CRHWP, single detectors can measure three of the Stokes parameters, I, Q and U , thereby avoiding the set of systematic errors that can be introduced by mismatches in the properties of orthogonal detector pairs. We focus on the implementation of CRHWPs in large aperture telescopes (i.e. the primary mirror is larger than the current maximum half-wave plate diameter of ∼ 0.5 m), where the CRHWP can be placed between the primary mirror and focal plane. In this configuration, one needs to address the intensity to polarization (I→P ) leakage of the optics, which becomes a source of 1/f noise and also causes differential gain systematics that arise from CMB temperature fluctuations. In this paper, we present the performance of a CRHWP installed in the Polarbear experiment, which employs a Gregorian telescope with a 2.5 m primary illumination pattern. The CRHWP is placed near the prime focus between the primary and secondary mirrors. We find that the I→P leakage is larger than the expectation from the physical properties of our primary mirror, resulting in a 1/f knee of 100 mHz. The excess leakage could be due to imperfections in the detector system, i.e. detector non-linearity in the responsivity and time-constant. We demonstrate, however, that by subtracting the leakage correlated with the intensity signal, the 1/f noise knee frequency is reduced to 32 mHz ( ∼ 39 for our scan strategy), which is very promising to probe the primordial B-mode signal. We also discuss methods for further noise subtraction in future projects where the precise temperature control of instrumental components and the leakage reduction will play a key role.

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“…As of now, combined observations from the BICEP2 and Keck Array experiments and from the Planck mission yield an upper limit of r < 0.06 at 95% confidence [7,10]. Proposed future CMB space missions such as the consecutive versions of CORE [11,12], LiteBIRD [13][14][15], PICO [16,17], PIXIE [18], PRISM [19] or ground-based experiments such as CMB-S4 [20,21] target a sensitivity σ(r) of 10 −3 or better, requiring instrumental sensitivity and control of instrumental systematic effects four orders of magnitude better than for observing CMB temperature anisotropies on large scales.…”

Section: Introductionmentioning

confidence: 99%

Bandpass mismatch error for satellite CMB experiments II: correcting for the spurious signal

Banerji

Patanchon

Delabrouille

et al. 2019

J. Cosmol. Astropart. Phys.

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Future Cosmic Microwave Background (CMB) satellite missions aim at using the B-mode polarisation signal to measure the tensor-to-scalar ratio r with a sensitivity σ(r) of the order of ≤ 10 −3 . Small uncertainties in the characterisation of instrument properties such as the spectral filters can lead to a leakage of the intensity signal to polarisation and can possibly bias any measurement of a primordial signal. In this paper we discuss methods for avoiding and correcting for the intensity to polarisation leakage due to bandpass mismatch among detector sets. We develop a template fitting map-maker to obtain an unbiased estimate of the leakage signal and subtract it out of the total signal. Using simulations we show how such a method can reduce the bias on the observed B-mode signal by up to 3 orders of magnitude in power.

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LiteBIRD: lite satellite for the study of B-mode polarization and inflation from cosmic microwave background radiation detection

Cited by 28 publications

References 9 publications

Updated Design of the CMB Polarization Experiment Satellite LiteBIRD

Updated Design of the CMB Polarization Experiment Satellite LiteBIRD

Performance of a continuously rotating half-wave plate on the POLARBEAR telescope

Bandpass mismatch error for satellite CMB experiments II: correcting for the spurious signal

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