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Title: Making maps of cosmic microwave background polarization for B-mode studies: the POLARBEAR example

Abstract

Analysis of cosmic microwave background (CMB) datasets typically requires some filtering of the raw time-ordered data. For instance, in the context of ground-based observations, filtering is frequently used to minimize the impact of low frequency noise, atmospheric contributions and/or scan synchronous signals on the resulting maps. In this paper, we have explicitly constructed a general filtering operator, which can unambiguously remove any set of unwanted modes in the data, and then amend the map-making procedure in order to incorporate and correct for it. We show that such an approach is mathematically equivalent to the solution of a problem in which the sky signal and unwanted modes are estimated simultaneously and the latter are marginalized over. We investigated the conditions under which this amended map-making procedure can render an unbiased estimate of the sky signal in realistic circumstances. We then discuss the potential implications of these observations on the choice of map-making and power spectrum estimation approaches in the context of B-mode polarization studies. Specifically, we have studied the effects of time-domain filtering on the noise correlation structure in the map domain, as well as impact it may haveon the performance of the popular pseudo-spectrum estimators. We conclude that although mapsmore » produced by the proposed estimators arguably provide the most faithful representation of the sky possible given the data, they may not straightforwardly lead to the best constraints on the power spectra of the underlying sky signal and special care may need to be taken to ensure this is the case. By contrast, simplified map-makers which do not explicitly correct for time-domain filtering, but leave it to subsequent steps in the data analysis, may perform equally well and be easier and faster to implement. We focused on polarization-sensitive measurements targeting the B-mode component of the CMB signal and apply the proposed methods to realistic simulations based on characteristics of an actual CMB polarization experiment, POLARBEAR. Finally, our analysis and conclusions are however more generally applicable.« less

Authors:
 [1];  [2];  [1];  [3];  [4];  [2];  [5];  [5];  [6];  [7];  [8];  [5];  [9];  [10];  [11];  [9];  [5];  [5];  [12];  [13] more »;  [14];  [5];  [10];  [15];  [9];  [5];  [16];  [10];  [6];  [6];  [17];  [18];  [10];  [5];  [10];  [10];  [10];  [10];  [2];  [19];  [7];  [10];  [10];  [20];  [1];  [5];  [21];  [10];  [5] « less
  1. Univ. of Paris Diderot, Paris (France)
  2. International School for Advanced Studies (SISSA), Trieste (Italy); National Inst. of Nuclear Physics (INFN), Trieste (Italy)
  3. Univ. of Sussex, Brighton (United Kingdom)
  4. Univ. of Wisconsin, Madison, WI (United States)
  5. Univ. of California, Berkeley, CA (United States)
  6. Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States); Univ. of California, Berkeley, CA (United States)
  7. Dalhousie Univ., Halifax (Canada)
  8. Univ. of California, Berkeley, CA (United States); Univ. of Tokyo, Chiba (Japan)
  9. Imperial College, London (United Kingdom)
  10. Univ. of California, San Diego, CA (United States)
  11. Sorbone Univ. and Univ. of Paris, Paris (France)
  12. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
  13. High Energy Accelerator Research Organization (KEK), Tsukuba (Japan); Graduate University for Advanced Studies (SOKENDAI), Kanagawa (Japan)
  14. High Energy Accelerator Research Organization (KEK), Tsukuba (Japan); Graduate University for Advanced Studies (SOKENDAI), Kanagawa (Japan); Univ. of Tokyo (Japan)
  15. Academia Sinica, Taipei (Taiwan); High Energy Accelerator Research Organization (KEK), Tsukuba (Japan)
  16. Univ. of Tokyo (Japan)
  17. Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
  18. Univ. of California, Berkeley, CA (United States); Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
  19. Univ. of Melbourne (Australia)
  20. California Inst. of Technology (CalTech), Pasadena, CA (United States)
  21. High Energy Accelerator Research Organization (KEK), Tsukuba (Japan)
Publication Date:
Research Org.:
Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
Sponsoring Org.:
USDOE Office of Science (SC)
OSTI Identifier:
1393212
Grant/Contract Number:  
AC02-05CH11231
Resource Type:
Journal Article: Accepted Manuscript
Journal Name:
Astronomy and Astrophysics
Additional Journal Information:
Journal Volume: 600; Journal ID: ISSN 0004-6361
Publisher:
EDP Sciences
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; cosmic background radiation; cosmology observations

Citation Formats

Poletti, Davide, Fabbian, Giulio, Le Jeune, Maude, Peloton, Julien, Arnold, Kam, Baccigalupi, Carlo, Barron, Darcy, Beckman, Shawn, Borrill, Julian, Chapman, Scott, Chinone, Yuji, Cukierman, Ari, Ducout, Anne, Elleflot, Tucker, Errard, Josquin, Feeney, Stephen, Goeckner-Wald, Neil, Groh, John, Hall, Grantland, Hasegawa, Masaya, Hazumi, Masashi, Hill, Charles, Howe, Logan, Inoue, Yuki, Jaffe, Andrew H., Jeong, Oliver, Katayama, Nobuhiko, Keating, Brian, Keskitalo, Reijo, Kisner, Theodore, Kusaka, Akito, Lee, Adrian T., Leon, David, Linder, Eric, Lowry, Lindsay, Matsuda, Frederick, Navaroli, Martin, Paar, Hans, Puglisi, Giuseppe, Reichardt, Christian L., Ross, Colin, Siritanasak, Praween, Stebor, Nathan, Steinbach, Bryan, Stompor, Radek, Suzuki, Aritoki, Tajima, Osamu, Teply, Grant, and Whitehorn, Nathan. Making maps of cosmic microwave background polarization for B-mode studies: the POLARBEAR example. United States: N. p., 2017. Web. doi:10.1051/0004-6361/201629467.
Poletti, Davide, Fabbian, Giulio, Le Jeune, Maude, Peloton, Julien, Arnold, Kam, Baccigalupi, Carlo, Barron, Darcy, Beckman, Shawn, Borrill, Julian, Chapman, Scott, Chinone, Yuji, Cukierman, Ari, Ducout, Anne, Elleflot, Tucker, Errard, Josquin, Feeney, Stephen, Goeckner-Wald, Neil, Groh, John, Hall, Grantland, Hasegawa, Masaya, Hazumi, Masashi, Hill, Charles, Howe, Logan, Inoue, Yuki, Jaffe, Andrew H., Jeong, Oliver, Katayama, Nobuhiko, Keating, Brian, Keskitalo, Reijo, Kisner, Theodore, Kusaka, Akito, Lee, Adrian T., Leon, David, Linder, Eric, Lowry, Lindsay, Matsuda, Frederick, Navaroli, Martin, Paar, Hans, Puglisi, Giuseppe, Reichardt, Christian L., Ross, Colin, Siritanasak, Praween, Stebor, Nathan, Steinbach, Bryan, Stompor, Radek, Suzuki, Aritoki, Tajima, Osamu, Teply, Grant, & Whitehorn, Nathan. Making maps of cosmic microwave background polarization for B-mode studies: the POLARBEAR example. United States. doi:10.1051/0004-6361/201629467.
Poletti, Davide, Fabbian, Giulio, Le Jeune, Maude, Peloton, Julien, Arnold, Kam, Baccigalupi, Carlo, Barron, Darcy, Beckman, Shawn, Borrill, Julian, Chapman, Scott, Chinone, Yuji, Cukierman, Ari, Ducout, Anne, Elleflot, Tucker, Errard, Josquin, Feeney, Stephen, Goeckner-Wald, Neil, Groh, John, Hall, Grantland, Hasegawa, Masaya, Hazumi, Masashi, Hill, Charles, Howe, Logan, Inoue, Yuki, Jaffe, Andrew H., Jeong, Oliver, Katayama, Nobuhiko, Keating, Brian, Keskitalo, Reijo, Kisner, Theodore, Kusaka, Akito, Lee, Adrian T., Leon, David, Linder, Eric, Lowry, Lindsay, Matsuda, Frederick, Navaroli, Martin, Paar, Hans, Puglisi, Giuseppe, Reichardt, Christian L., Ross, Colin, Siritanasak, Praween, Stebor, Nathan, Steinbach, Bryan, Stompor, Radek, Suzuki, Aritoki, Tajima, Osamu, Teply, Grant, and Whitehorn, Nathan. Thu . "Making maps of cosmic microwave background polarization for B-mode studies: the POLARBEAR example". United States. doi:10.1051/0004-6361/201629467. https://www.osti.gov/servlets/purl/1393212.
@article{osti_1393212,
title = {Making maps of cosmic microwave background polarization for B-mode studies: the POLARBEAR example},
author = {Poletti, Davide and Fabbian, Giulio and Le Jeune, Maude and Peloton, Julien and Arnold, Kam and Baccigalupi, Carlo and Barron, Darcy and Beckman, Shawn and Borrill, Julian and Chapman, Scott and Chinone, Yuji and Cukierman, Ari and Ducout, Anne and Elleflot, Tucker and Errard, Josquin and Feeney, Stephen and Goeckner-Wald, Neil and Groh, John and Hall, Grantland and Hasegawa, Masaya and Hazumi, Masashi and Hill, Charles and Howe, Logan and Inoue, Yuki and Jaffe, Andrew H. and Jeong, Oliver and Katayama, Nobuhiko and Keating, Brian and Keskitalo, Reijo and Kisner, Theodore and Kusaka, Akito and Lee, Adrian T. and Leon, David and Linder, Eric and Lowry, Lindsay and Matsuda, Frederick and Navaroli, Martin and Paar, Hans and Puglisi, Giuseppe and Reichardt, Christian L. and Ross, Colin and Siritanasak, Praween and Stebor, Nathan and Steinbach, Bryan and Stompor, Radek and Suzuki, Aritoki and Tajima, Osamu and Teply, Grant and Whitehorn, Nathan},
abstractNote = {Analysis of cosmic microwave background (CMB) datasets typically requires some filtering of the raw time-ordered data. For instance, in the context of ground-based observations, filtering is frequently used to minimize the impact of low frequency noise, atmospheric contributions and/or scan synchronous signals on the resulting maps. In this paper, we have explicitly constructed a general filtering operator, which can unambiguously remove any set of unwanted modes in the data, and then amend the map-making procedure in order to incorporate and correct for it. We show that such an approach is mathematically equivalent to the solution of a problem in which the sky signal and unwanted modes are estimated simultaneously and the latter are marginalized over. We investigated the conditions under which this amended map-making procedure can render an unbiased estimate of the sky signal in realistic circumstances. We then discuss the potential implications of these observations on the choice of map-making and power spectrum estimation approaches in the context of B-mode polarization studies. Specifically, we have studied the effects of time-domain filtering on the noise correlation structure in the map domain, as well as impact it may haveon the performance of the popular pseudo-spectrum estimators. We conclude that although maps produced by the proposed estimators arguably provide the most faithful representation of the sky possible given the data, they may not straightforwardly lead to the best constraints on the power spectra of the underlying sky signal and special care may need to be taken to ensure this is the case. By contrast, simplified map-makers which do not explicitly correct for time-domain filtering, but leave it to subsequent steps in the data analysis, may perform equally well and be easier and faster to implement. We focused on polarization-sensitive measurements targeting the B-mode component of the CMB signal and apply the proposed methods to realistic simulations based on characteristics of an actual CMB polarization experiment, POLARBEAR. Finally, our analysis and conclusions are however more generally applicable.},
doi = {10.1051/0004-6361/201629467},
journal = {Astronomy and Astrophysics},
number = ,
volume = 600,
place = {United States},
year = {Thu Mar 30 00:00:00 EDT 2017},
month = {Thu Mar 30 00:00:00 EDT 2017}
}

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