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  • Accepted Manuscript: Performance of a continuously rotating half-wave plate on the POLARBEAR telescope

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

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 {\scshape 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 amore » 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 (ℓ ~ 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.« less
Authors:
 [1] ;  [2] ;  [3] ;  [4] ;  [5] ;  [6] ;  [6] ;  [7] ;  [8] ;  [9] ;  [10] ;  [6] ;  [11] ;  [4] ;  [12] ;  [13] ;  [14] ;  [4] ;  [6] ;  [15] more »;  [16] ;  [17] ;  [18] ;  [19] ;  [4] ;  [20] ;  [21] ;  [6] ;  [11] ;  [11] ;  [4] ;  [8] ;  [8] ;  [22] ;  [23] ;  [19] ;  [4] ;  [4] ;  [4] ;  [11] ;  [4] ;  [24] ;  [4] ;  [25] ;  [22] ;  [5] ;  [26] ;  [9] ;  [4] ;  [6] ;  [16] ;  [16] ;  [4] « less
+ Show Author Affiliations
  1. Osaka Univ., Osaka (Japan); High Energy Accelerator Research Organization (KEK), Ibaraki (Japan)
  2. Univ. de Chile, Santiago (Chile)
  3. SOKENDAI (The Graduate Univ. for Advanced Studies), Kanagawa (Japan); High Energy Accelerator Research Organization (KEK), Ibaraki (Japan)
  4. Univ. of California, San Diego, CA (United States)
  5. International School for Advanced Studies (SISSA), Trieste (Italy); INFN, Trieste (Italy)
  6. Univ. of California, Berkeley, CA (United States)
  7. Pontificia Univ. Catolica de Chile, Santiago (Chile)
  8. Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States); Univ. of California, Berkeley, CA (United States)
  9. Dalhousie Univ., Halifax (Canada)
  10. Univ. of California, Berkeley, CA (United States); The Univ. of Tokyo, Chiba (Japan)
  11. The Univ. of Tokyo, Chiba (Japan)
  12. Sorbonne Univ., Paris (France); CNRS-IN2P3 and Univ. Paris, Paris Cedex (France); Univ. Paris Diderot, Paris Cite (France)
  13. Univ Paris-Sud, Univ. Paris-Saclay, Orsay (France); International School for Advanced Studies (SISSA), Trieste (Italy); INFN, Trieste (Italy)
  14. Yokohama National Univ., Kanagawa (Japan); The Univ. of Tokyo, Chiba (Japan)
  15. Univ. of Colorado, Boulder, CO (United States)
  16. High Energy Accelerator Research Organization (KEK), Ibaraki (Japan); SOKENDAI (The Graduate Univ. for Advanced Studies), Kanagawa (Japan)
  17. National Institute of Advanced Industrial Science and Technology (AIST), Ibaraki (Japan); SOKENDAI (The Graduate Univ. for Advanced Studies), Kanagawa (Japan)
  18. High Energy Accelerator Research Organization (KEK), Ibaraki (Japan); SOKENDAI (The Graduate Univ. for Advanced Studies), Kanagawa (Japan); The Univ. of Tokyo, Chiba (Japan); Institute of Space and Astronautical Science (ISAS), Kanagawa (Japan)
  19. Univ. of California, Berkeley, CA (United States); Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
  20. Academia Sinica, Nankang (Taiwan); High Energy Accelerator Research Organization (KEK), Ibaraki (Japan)
  21. Imperial College London, London (United Kingdom)
  22. International School for Advanced Studies (SISSA), Trieste (Italy)
  23. Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
  24. High Energy Accelerator Research Organization (KEK), Ibaraki (Japan)
  25. Univ. of Sussex, Brighton (United Kingdom)
  26. Univ. of Melbourne, Parkville, VIC (Australia)
Publication Date:
Grant/Contract Number:
AC02-05CH11231
Type:
Accepted Manuscript
Journal Name:
Journal of Cosmology and Astroparticle Physics
Additional Journal Information:
Journal Volume: 2017; Journal Issue: 05; Journal ID: ISSN 1475-7516
Publisher:
Institute of Physics (IOP)
Research Org:
Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
Sponsoring Org:
USDOE Office of Science (SC)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS
OSTI Identifier:
1393232
Citation Formats
Takakura, Satoru, Aguilar, Mario, Akiba, Yoshiki, Arnold, Kam, Baccigalupi, Carlo, Barron, Darcy, Beckman, Shawn, Boettger, David, Borrill, Julian, Chapman, Scott, Chinone, Yuji, Cukierman, Ari, Ducout, Anne, Elleflot, Tucker, Errard, Josquin, Fabbian, Giulio, Fujino, Takuro, Galitzki, Nicholas, Goeckner-Wald, Neil, Halverson, Nils W., Hasegawa, Masaya, Hattori, Kaori, Hazumi, Masashi, Hill, Charles, Howe, Logan, Inoue, Yuki, Jaffe, Andrew H., Jeong, Oliver, Kaneko, Daisuke, Katayama, Nobuhiko, Keating, Brian, Keskitalo, Reijo, Kisner, Theodore, Krachmalnicoff, Nicoletta, Kusaka, Akito, Lee, Adrian T., Leon, David, Lowry, Lindsay, Matsuda, Frederick, Matsumura, Tomotake, Navaroli, Martin, Nishino, Haruki, Paar, Hans, Peloton, Julien, Poletti, Davide, Puglisi, Giuseppe, Reichardt, Christian L., Ross, Colin, Siritanasak, Praween, Suzuki, Aritoki, Tajima, Osamu, Takatori, Sayuri, and Teply, Grant. Performance of a continuously rotating half-wave plate on the POLARBEAR telescope. United States: N. p., Web. doi:10.1088/1475-7516/2017/05/008.
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Takakura, Satoru, Aguilar, Mario, Akiba, Yoshiki, Arnold, Kam, Baccigalupi, Carlo, Barron, Darcy, Beckman, Shawn, Boettger, David, Borrill, Julian, Chapman, Scott, Chinone, Yuji, Cukierman, Ari, Ducout, Anne, Elleflot, Tucker, Errard, Josquin, Fabbian, Giulio, Fujino, Takuro, Galitzki, Nicholas, Goeckner-Wald, Neil, Halverson, Nils W., Hasegawa, Masaya, Hattori, Kaori, Hazumi, Masashi, Hill, Charles, Howe, Logan, Inoue, Yuki, Jaffe, Andrew H., Jeong, Oliver, Kaneko, Daisuke, Katayama, Nobuhiko, Keating, Brian, Keskitalo, Reijo, Kisner, Theodore, Krachmalnicoff, Nicoletta, Kusaka, Akito, Lee, Adrian T., Leon, David, Lowry, Lindsay, Matsuda, Frederick, Matsumura, Tomotake, Navaroli, Martin, Nishino, Haruki, Paar, Hans, Peloton, Julien, Poletti, Davide, Puglisi, Giuseppe, Reichardt, Christian L., Ross, Colin, Siritanasak, Praween, Suzuki, Aritoki, Tajima, Osamu, Takatori, Sayuri, & Teply, Grant. Performance of a continuously rotating half-wave plate on the POLARBEAR telescope. United States. doi:10.1088/1475-7516/2017/05/008.
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Takakura, Satoru, Aguilar, Mario, Akiba, Yoshiki, Arnold, Kam, Baccigalupi, Carlo, Barron, Darcy, Beckman, Shawn, Boettger, David, Borrill, Julian, Chapman, Scott, Chinone, Yuji, Cukierman, Ari, Ducout, Anne, Elleflot, Tucker, Errard, Josquin, Fabbian, Giulio, Fujino, Takuro, Galitzki, Nicholas, Goeckner-Wald, Neil, Halverson, Nils W., Hasegawa, Masaya, Hattori, Kaori, Hazumi, Masashi, Hill, Charles, Howe, Logan, Inoue, Yuki, Jaffe, Andrew H., Jeong, Oliver, Kaneko, Daisuke, Katayama, Nobuhiko, Keating, Brian, Keskitalo, Reijo, Kisner, Theodore, Krachmalnicoff, Nicoletta, Kusaka, Akito, Lee, Adrian T., Leon, David, Lowry, Lindsay, Matsuda, Frederick, Matsumura, Tomotake, Navaroli, Martin, Nishino, Haruki, Paar, Hans, Peloton, Julien, Poletti, Davide, Puglisi, Giuseppe, Reichardt, Christian L., Ross, Colin, Siritanasak, Praween, Suzuki, Aritoki, Tajima, Osamu, Takatori, Sayuri, and Teply, Grant. 2017. "Performance of a continuously rotating half-wave plate on the POLARBEAR telescope". United States. doi:10.1088/1475-7516/2017/05/008. https://www.osti.gov/servlets/purl/1393232.
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@article{osti_1393232,
title = {Performance of a continuously rotating half-wave plate on the POLARBEAR telescope},
author = {Takakura, Satoru and Aguilar, Mario and Akiba, Yoshiki and Arnold, Kam and Baccigalupi, Carlo and Barron, Darcy and Beckman, Shawn and Boettger, David and Borrill, Julian and Chapman, Scott and Chinone, Yuji and Cukierman, Ari and Ducout, Anne and Elleflot, Tucker and Errard, Josquin and Fabbian, Giulio and Fujino, Takuro and Galitzki, Nicholas and Goeckner-Wald, Neil and Halverson, Nils W. and Hasegawa, Masaya and Hattori, Kaori and Hazumi, Masashi and Hill, Charles and Howe, Logan and Inoue, Yuki and Jaffe, Andrew H. and Jeong, Oliver and Kaneko, Daisuke and Katayama, Nobuhiko and Keating, Brian and Keskitalo, Reijo and Kisner, Theodore and Krachmalnicoff, Nicoletta and Kusaka, Akito and Lee, Adrian T. and Leon, David and Lowry, Lindsay and Matsuda, Frederick and Matsumura, Tomotake and Navaroli, Martin and Nishino, Haruki and Paar, Hans and Peloton, Julien and Poletti, Davide and Puglisi, Giuseppe and Reichardt, Christian L. and Ross, Colin and Siritanasak, Praween and Suzuki, Aritoki and Tajima, Osamu and Takatori, Sayuri and Teply, Grant},
abstractNote = {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 {\scshape 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 (ℓ ~ 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.},
doi = {10.1088/1475-7516/2017/05/008},
journal = {Journal of Cosmology and Astroparticle Physics},
number = 05,
volume = 2017,
place = {United States},
year = {2017},
month = {5}
}
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