Concept design of low frequency telescope for CMB B-mode polarization satellite LiteBIRD
Concept design of low frequency telescope for CMB B-mode polarization satellite LiteBIRD
复制标题
CMB B模偏振卫星LiteBIRD低频望远镜概念设计
DOI:
10.1117/12.2561841
复制
发表时间:
2020
期刊:
影响因子:
--
通讯作者:
et al.
中科院分区:
文献类型:
--
作者:
Sekimoto Yutaro;et al.
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° x 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.
登录
查看更多内容
影响因子:
3.2
作者:
Takakura Hayato;Sekimoto Yutaro;Inatani Junji;Kashima Shingo;Imada Hiroaki;Hasebe Takashi;Kaga Toru;Takeda Yoichi;Okada Norio
通讯作者:
Okada Norio
DOI:
10.1117/12.857423
发表时间:
2010
期刊:
--
影响因子:
--
作者:
H. Tran;Brad L. Johnson;M. Dragovan;J. Bock;A. Aljabri;A. Amblard;D. Bauman;M. Betoule;T. Chui;L. Colombo;A. Cooray;D. Crumb;P. Day;C. Dickenson;D. Dowell;S. Golwala;K. Gorski;S. Hanany;W. Holmes;K. Irwin;B. Keating;C. Kuo;Adrian T. Lee;A. Lange;C. Lawrence;S. Meyer;N. Miller;Hien Nguyen;E. Pierpaoli;N. Ponthieu;J. Puget;J. Raab;P. Richards;C. Satter;M. Seiffert;M. Shimon;B. Williams;J. Zmuidzinas
通讯作者:
J. Zmuidzinas
DOI:
--
发表时间:
2012
期刊:
Other Conferences
影响因子:
--
作者:
M. Hazumi;J. Borrill;Y. Chinone;M. Dobbs;H. Fuke;A. Ghribi;M. Hasegawa;K. Hattori;M. Hattori;W. Holzapfel;Y. Inoue;K. Ishidoshiro;H. Ishino;K. Karatsu;N. Katayama;I. Kawano;A. Kibayashi;Y. Kibe;N. Kimura;K. Koga;E. Komatsu;Adrian T. Lee;H. Matsuhara;T. Matsumura;S. Mima;K. Mitsuda;H. Morii;S. Murayama;M. Nagai;R. Nagata;S. Nakamura;K. Natsume;H. Nishino;A. Noda;T. Noguchi;I. Ohta;C. Otani;P. Richards;S. Sakai;N. Sato;Y. Sato;Y. Sekimoto;A. Shimizu;K. Shinozaki;H. Sugita;A. Suzuki;T. Suzuki;O. Tajima;S. Takada;Y. Takagi;Y. Takei;T. Tomaru;Yoshinori Uzawa;Hiroki Watanabe;N. Yamasaki;M. Yoshida;T. Yoshida;K. Yotsumoto
通讯作者:
K. Yotsumoto
DOI:
10.1117/1.jatis.5.4.044002
发表时间:
2019
期刊:
Journal of Astronomical Telescopes, Instruments, and Systems
影响因子:
--
作者:
Hasebe Takashi;Sekimoto Yutaro;Dotani Tadayasu;Mitsuda Kazuhisa;Shinozaki Keisuke;Yoshida Seiji
通讯作者:
Yoshida Seiji
DOI:
--
发表时间:
2018
期刊:
影响因子:
--
作者:
Z. Qin;Y. Wang;F. L. Fan;S. W. Cao;H. Haba;Y. Komori;S. Yano;D. Kaji;and K. Morimoto;Michinori Ishiwata;吉村浩明;Yuki Sakurai et. al.
通讯作者:
Yuki Sakurai et. al.