Abstract
LiteBIRD is a JAXA-led Strategic Large-Class mission designed to search for the existence of the primordial gravitational waves produced during the inflationary phase of the Universe, through the measurements of their imprint onto the polarization of the cosmic microwave background (CMB). These measurements, requiring unprecedented sensitivity, will be performed over the full sky, at large angular scales, and over 15 frequency bands from 34 GHz to 448 GHz. The LiteBIRD instruments consist of three telescopes, namely the Low-, Medium-and High-Frequency Telescope (respectively LFT, MFT and HFT). We present in this paper an overview of the design of the Medium-Frequency Telescope (89{224 GHz) and the High-Frequency Telescope (166{448 GHz), the so-called MHFT, under European responsibility, which are two cryogenic refractive telescopes cooled down to 5 K. They include a continuous rotating half-wave plate as the first optical element, two high-density polyethylene (HDPE) lenses and more than three thousand transition-edge sensor (TES) detectors cooled to 100 mK. We provide an overview of the concept design and the remaining specific challenges that we have to face in order to achieve the scientific goals of LiteBIRD.
| Original language | English |
|---|---|
| Title of host publication | Space Telescopes and Instrumentation 2020 |
| Subtitle of host publication | Optical, Infrared, and Millimeter Wave |
| Editors | Makenzie Lystrup, Marshall D. Perrin |
| Publisher | SPIE |
| ISBN (Electronic) | 9781510636736 |
| DOIs | |
| Publication status | Published - 2020 |
| Event | Space Telescopes and Instrumentation 2020: Optical, Infrared, and Millimeter Wave - Virtual, Online, United States Duration: 2020 Dec 14 → 2020 Dec 22 |
Publication series
| Name | Proceedings of SPIE - The International Society for Optical Engineering |
|---|---|
| Volume | 11443 |
| ISSN (Print) | 0277-786X |
| ISSN (Electronic) | 1996-756X |
Conference
| Conference | Space Telescopes and Instrumentation 2020: Optical, Infrared, and Millimeter Wave |
|---|---|
| Country/Territory | United States |
| City | Virtual, Online |
| Period | 20/12/14 → 20/12/22 |
Keywords
- Cosmic microwave background
- LiteBIRD
- Polarization measurements
- Space telescopes
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Space Telescopes and Instrumentation 2020: Optical, Infrared, and Millimeter Wave. ed. / Makenzie Lystrup; Marshall D. Perrin. SPIE, 2020. 114432G (Proceedings of SPIE - The International Society for Optical Engineering; Vol. 11443).
Research output: Chapter in Book/Report/Conference proceeding › Conference contribution › peer-review
TY - GEN
T1 - Overview of the medium and high frequency telescopes of the LiteBIRD space mission
AU - Montier, L.
AU - Mot, B.
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AU - Maffei, B.
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AU - Gudmundsson, J. E.
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AU - Beck, D.
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AU - Bersanelli, M.
AU - Bonis, J.
AU - Borrill, J.
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AU - Brilenkov, M.
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AU - Bucher, M.
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AU - Campeti, P.
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AU - Curtis, D.
AU - D'alessandro, G.
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AU - De Petris, M.
AU - Dickinson, C.
AU - Diego-Palazuelos, P.
AU - Dobbs, M.
AU - Dotani, T.
AU - Duband, L.
AU - Duff, S.
AU - Duval, J. M.
AU - Ebisawa, K.
AU - Elleflot, T.
AU - Eriksen, H. K.
AU - Errard, J.
AU - Essinger-Hileman, T.
AU - Finelli, F.
AU - Flauger, R.
AU - Franceschet, C.
AU - Fuskeland, U.
AU - Galloway, M.
AU - Ganga, K.
AU - Gao, J. R.
AU - Genova-Santos, R.
AU - Gerbino, M.
AU - Gervasi, M.
AU - Ghigna, T.
AU - Gjerløw, E.
AU - Gradziel, M. L.
AU - Grain, J.
AU - Grupp, F.
AU - Gruppuso, A.
AU - De Haan, T.
AU - Halverson, N. W.
AU - Hargrave, P.
AU - Hasebe, T.
AU - Hasegawa, M.
AU - Hattori, M.
AU - Hazumi, M.
AU - Herman, D.
AU - Herranz, D.
AU - Hill, C. A.
AU - Hilton, G.
AU - Hirota, Y.
AU - Hivon, E.
AU - Hlozek, R. A.
AU - Hoshino, Y.
AU - De La Hoz, E.
AU - Hubmayr, J.
AU - Ichiki, K.
AU - Iida, T.
AU - Imada, H.
AU - Ishimura, K.
AU - Ishino, H.
AU - Jaehnig, G.
AU - Kaga, T.
AU - Kashima, S.
AU - Katayama, N.
AU - Kato, A.
AU - Kawasaki, T.
AU - Keskitalo, R.
AU - Kisner, T.
AU - Kobayashi, Y.
AU - Kogiso, N.
AU - Kogut, A.
AU - Kohri, K.
AU - Komatsu, E.
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AU - Konishi, K.
AU - Krachmalnicoff, N.
AU - Kreykenbohm, I.
AU - Kuo, C. L.
AU - Kushino, A.
AU - Lanen, J. V.
AU - Lattanzi, M.
AU - Lee, A. T.
AU - Leloup, C.
AU - Levrier, F.
AU - Linder, E.
AU - Louis, T.
AU - Luzzi, G.
AU - Maciaszek, T.
AU - Maino, D.
AU - Maki, M.
AU - Mandelli, S.
AU - Martinez-Gonzalez, E.
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AU - Matsumura, T.
AU - Mennella, A.
AU - Migliaccio, M.
AU - Minami, Y.
AU - Mitsuda, K.
AU - Morgante, G.
AU - Murata, Y.
AU - Murphy, J. A.
AU - Nagai, M.
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AU - Nagasaki, T.
AU - Nagata, R.
AU - Nakamura, S.
AU - Namikawa, T.
AU - Natoli, P.
AU - Nerval, S.
AU - Nishibori, T.
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AU - O'sullivan, C.
AU - Ogawa, H.
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AU - Oguri, S.
AU - Ohsaki, H.
AU - Ohta, I. S.
AU - Okada, N.
AU - Okada, N.
AU - Pagano, L.
AU - Paiella, A.
AU - Paoletti, D.
AU - Patanchon, G.
AU - Peloton, J.
AU - Piacentini, F.
AU - Polenta, G.
AU - Poletti, D.
AU - Puglisi, G.
AU - Rambaud, D.
AU - Raum, C.
AU - Realini, S.
AU - Reinecke, M.
AU - Remazeilles, M.
AU - Ritacco, A.
AU - Roudil, G.
AU - Rubino-Martin, J. A.
AU - Sakurai, H.
AU - Sakurai, Y.
AU - Sandri, M.
AU - Sasaki, M.
AU - Scott, D.
AU - Seibert, J.
AU - Sekimoto, Y.
AU - Sherwin, B.
AU - Shinozaki, K.
AU - Shiraishi, M.
AU - Shirron, P.
AU - Signorelli, G.
AU - Smecher, G.
AU - Stompor, R.
AU - Sugai, H.
AU - Sugiyama, S.
AU - Suzuki, A.
AU - Suzuki, J.
AU - Svalheim, T. L.
AU - Switzer, E.
AU - Takaku, R.
AU - Takakura, H.
AU - Takakura, S.
AU - Takase, Y.
AU - Takeda, Y.
AU - Tartari, A.
AU - Taylor, E.
AU - Terao, Y.
AU - Thommesen, H.
AU - Thorne, B.
AU - Toda, T.
AU - Tomasi, M.
AU - Tominaga, M.
AU - Trappe, N.
AU - Tristram, M.
AU - Tsuji, M.
AU - Ullom, J.
AU - Vermeulen, G.
AU - Vielva, P.
AU - Villa, F.
AU - Vissers, M.
AU - Vittorio, N.
AU - Wehus, I.
AU - Weller, J.
AU - Wilms, J.
AU - Winter, B.
AU - Wollack, E. J.
AU - Yamasaki, N. Y.
AU - Yoshida, T.
AU - Yumoto, J.
AU - Zannoni, M.
AU - Zonca, A.
N1 - Funding Information: This work is supported in Japan by ISAS/JAXA for Pre-Phase A2 studies, by the acceleration program of JAXA research and development directorate, by the World Premier International Research Center Initiative (WPI) of MEXT, by the JSPS Core-to-Core Program of A. Advanced Research Networks, and by JSPS KAKENHI Grant Numbers JP15H05891, JP17H01115, and JP17H01125. The Italian LiteBIRD phase A contribution is supported by the Italian Space Agency (ASI Grants No. 2020-9-HH.0 and 2016-24-H.1-2018), the National Institute for Nuclear Physics (INFN) and the National Institute for Astrophysics (INAF). The French LiteBIRD phase A contribution is supported by the Centre National d’Etudes Spatiale (CNES), by the Centre National de la Recherche Scientifique (CNRS), and by the Commissariat à l’Energie Atomique (CEA). The Canadian contribution is supported by the Canadian Space Agency. The US contribution is supported by NASA grant no. 80NSSC18K0132. Norwegian participation in LiteBIRD is supported by the Research Council of Norway (Grant No. 263011). The Spanish LiteBIRD phase A contribution is supported by the Spanish Agencia Estatal de Investigación (AEI), project refs. PID2019-110610RB-C21 and AYA2017-84185-P. Funds that support the Swedish contributions come from the Swedish National Space Agency (SNSA/Rymdstyrelsen) and the Swedish Research Council (Reg. no. 2019-03959). The German participation in LiteBIRD is supported in part by the Excellence Cluster ORIGINS, which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy (Grant No. EXC-2094 - 390783311). This research used resources of the Central Computing System owned and operated by the Computing Research Center at KEK, as well as resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy. European collaborators acknowledge support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement Nos. 772253, 819478, and 849169). The European Space Agency (ESA) has led a Concurrent Design Facility study, focused on the MHFT and Sub-Kelvin coolers, and funded Technology Research Programmes for “Large radii Half-Wave Plate (HWP) development” (contract number: 4000123266/18/NL/AF) and for the ‘Development of Large Anti-Reflection Coated Lenses for Passive (Sub)Millimeter-Wave Science Instruments” (contract number: 4000128517/19/NL/AS). Publisher Copyright: © COPYRIGHT SPIE. Downloading of the abstract is permitted for personal use only.
PY - 2020
Y1 - 2020
N2 - LiteBIRD is a JAXA-led Strategic Large-Class mission designed to search for the existence of the primordial gravitational waves produced during the inflationary phase of the Universe, through the measurements of their imprint onto the polarization of the cosmic microwave background (CMB). These measurements, requiring unprecedented sensitivity, will be performed over the full sky, at large angular scales, and over 15 frequency bands from 34 GHz to 448 GHz. The LiteBIRD instruments consist of three telescopes, namely the Low-, Medium-and High-Frequency Telescope (respectively LFT, MFT and HFT). We present in this paper an overview of the design of the Medium-Frequency Telescope (89{224 GHz) and the High-Frequency Telescope (166{448 GHz), the so-called MHFT, under European responsibility, which are two cryogenic refractive telescopes cooled down to 5 K. They include a continuous rotating half-wave plate as the first optical element, two high-density polyethylene (HDPE) lenses and more than three thousand transition-edge sensor (TES) detectors cooled to 100 mK. We provide an overview of the concept design and the remaining specific challenges that we have to face in order to achieve the scientific goals of LiteBIRD.
AB - LiteBIRD is a JAXA-led Strategic Large-Class mission designed to search for the existence of the primordial gravitational waves produced during the inflationary phase of the Universe, through the measurements of their imprint onto the polarization of the cosmic microwave background (CMB). These measurements, requiring unprecedented sensitivity, will be performed over the full sky, at large angular scales, and over 15 frequency bands from 34 GHz to 448 GHz. The LiteBIRD instruments consist of three telescopes, namely the Low-, Medium-and High-Frequency Telescope (respectively LFT, MFT and HFT). We present in this paper an overview of the design of the Medium-Frequency Telescope (89{224 GHz) and the High-Frequency Telescope (166{448 GHz), the so-called MHFT, under European responsibility, which are two cryogenic refractive telescopes cooled down to 5 K. They include a continuous rotating half-wave plate as the first optical element, two high-density polyethylene (HDPE) lenses and more than three thousand transition-edge sensor (TES) detectors cooled to 100 mK. We provide an overview of the concept design and the remaining specific challenges that we have to face in order to achieve the scientific goals of LiteBIRD.
KW - Cosmic microwave background
KW - LiteBIRD
KW - Polarization measurements
KW - Space telescopes
UR - http://www.scopus.com/inward/record.url?scp=85099887594&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85099887594&partnerID=8YFLogxK
U2 - 10.1117/12.2562243
DO - 10.1117/12.2562243
M3 - Conference contribution
AN - SCOPUS:85099887594
T3 - Proceedings of SPIE - The International Society for Optical Engineering
BT - Space Telescopes and Instrumentation 2020
A2 - Lystrup, Makenzie
A2 - Perrin, Marshall D.
PB - SPIE
T2 - Space Telescopes and Instrumentation 2020: Optical, Infrared, and Millimeter Wave
Y2 - 14 December 2020 through 22 December 2020
ER -