Optical design of the EPIC-IM crossed Dragone telescope

Tran, Hung V.; Johnson, B. R.; Dragovan, M.; Bock, J. J.; Aljabri, A. S.; Amblard, A.; Bauman, Daniel J.; Betoule, M.; Chui, Talso; Colombo, L. P. L.; Cooray, Asantha; Crumb, Dustin; Day, Peter; Dickenson, Clive; Dowell, Darren; Golwala, S. R.; Górski, K. M.; Hanany, Shaul; Holmes, W. A.; Irwin, K. D.; Keating, Brian; Kuo, C. L.; Lee, Adrian V.; Lange, A. E.; Lawrence, C. R.; Meyer, Steve; Miller, Nate; Nguyen, Hien; Pierpaoli, E.; Puget, J.; Raab, J.; Richards, P. L.; Satter, Celeste M.; Seiffert, Mike; Shimon, Meir; Williams, Brett; Žmuidzinas, J.

doi:10.1117/12.857423

Cited by 9 publications

(8 citation statements)

References 3 publications

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“…The F#3.0 and the crossing angle of optical axes of 90 degrees are chosen after an extensive study of stray light. We found that "clipped" side lobe 29 or triple reflection 15 of the crossed Dragone optics can be avoided with this configuration. Primary and secondary mirrors have rectangular shape (∼ 900 mm ×800 mm) with serrations to reduce diffraction pattern from the edges of mirrors.…”

Section: Low Frequency Telescope (Lft)mentioning

confidence: 86%

Concept design of the LiteBIRD satellite for CMB B-mode polarization

Sekímoto¹,

Ade²,

Arnold³

et al. 2018

Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave

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LiteBIRD is a candidate for JAXA s strategic large mission to observe the cosmic microwave background (CMB) polarization over the full sky at large angular scales. It is planned to be launched in the 2020s with an H3 launch vehicle for three years of observations at a Sun-Earth Lagrangian point (L2). The concept design has been studied by researchers from Japan, U.S., Canada and Europe during the ISAS Phase-A1. Large scale measurements of the CMB B-mode polarization are known as the best probe to detect primordial gravitational waves. The goal of LiteBIRD is to measure the tensor-to-scalar ratio (r) with precision of δr < 0.001. A 3-year full sky survey will be carried out with a low frequency (34-161 GHz) telescope (LFT) and a high frequency (89-448 GHz) telescope (HFT), which achieve a sensitivity of 2.5 µK-arcmin with an angular resolution of ∼ 30 arcminutes around 100 GHz. The concept design of LiteBIRD system, payload module (PLM), cryo-structure, LFT and verification plan is described in this paper.

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Section: Low Frequency Telescope (Lft)mentioning

confidence: 86%

Concept design of the LiteBIRD satellite for CMB B-mode polarization

Sekímoto¹,

Ade²,

Arnold³

et al. 2018

Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave

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“…Multiple reflections of crossed-Dragone antennas have been described earlier. 26 A crossed-Dragone antenna of LFT has been designed with anamorphic aspherical surfaces 27 to achieve the specifications listed in Table 2. The anamorphic aspherical surface is described with the following equation for both the primary mirror (PM) and the secondary mirror (SM):…”

Section: Antenna Designmentioning

confidence: 99%

Concept design of low frequency telescope for CMB B-mode polarization satellite LiteBIRD

Sekímoto

Ade

Adler

et al. 2020

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

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LiteBIRD has been selected as JAXA's strategic large mission in the 2020s, to observe the cosmic microwave background (CMB) B-mode polarization over the full sky at large angular scales. The challenges of LiteBIRD are the wide field-of-view (FoV) and broadband capabilities of millimeter-wave polarization measurements, which are derived from the system requirements. The possible paths of stray light increase with a wider FoV and the far sidelobe knowledge of −56 dB is a challenging optical requirement. A crossed-Dragone configuration was chosen for the low frequency telescope (LFT : 34-161 GHz), one of LiteBIRD's onboard telescopes. It has a wide field-of-view (18 • × 9 • ) with an aperture of 400 mm in diameter, corresponding to an angular resolution of about 30 arcminutes around 100 GHz. The focal ratio f/3.0 and the crossing angle of the optical axes of 90 • are chosen after an extensive study of the stray light. The primary and secondary reflectors have rectangular shapes with serrations to reduce the diffraction pattern from the edges of the mirrors. The reflectors and structure are made of aluminum to proportionally contract from warm down to the operating temperature at 5 K. A 1/4 scaled model of the LFT has been developed to validate the wide field-of-view design and to demonstrate the reduced far sidelobes. A polarization modulation unit (PMU), realized with a half-wave plate (HWP) is placed in front of the aperture stop, the entrance pupil of this system. A large focal plane with approximately 1000 AlMn TES detectors and frequency multiplexing SQUID amplifiers is cooled to 100 mK. The lens and sinuous antennas have broadband capability. Performance specifications of the LFT and an outline of the proposed verification plan are presented.

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“…The resulting very clean beam pattern is vital to enable the faint Hi signal to be efficiently separated from the bright Galactic foreground emission, whose signal is about 4 orders of magnitude brighter than Hi. Our adopted crossed-Dragone configuration has been a common choice for many Cosmic Microwave Background (CMB) experiments in the last 15 years (see, e.g., [15,16,17]).…”

Section: Requirements and Optical Designmentioning

confidence: 99%

Baryon acoustic oscillations from Integrated Neutral Gas Observations: Broadband corrugated horn construction and testing

et al. 2020

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The Baryon acoustic oscillations from Integrated Neutral Gas Observations (BINGO) telescope is a 40-m class radio telescope under construction that has been designed to measure the large-angular-scale intensity of Hi emission at 980-1260 MHz and hence to constrain dark energy parameters. A large focal plane array comprising of 1.7-metre diameter, 4.3-metre length corrugated feed horns is required in order to optimally illuminate the telescope. Additionally, very clean beams with low sidelobes across a broad frequency range are required, in order to facilitate the separation of the faint Hi emission from bright Galactic foreground emission. Using novel construction methods,

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Optical design of the EPIC-IM crossed Dragone telescope

Cited by 9 publications

References 3 publications

Concept design of the LiteBIRD satellite for CMB B-mode polarization

Concept design of the LiteBIRD satellite for CMB B-mode polarization

Concept design of low frequency telescope for CMB B-mode polarization satellite LiteBIRD

Baryon acoustic oscillations from Integrated Neutral Gas Observations: Broadband corrugated horn construction and testing

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