CLASS Data Pipeline and Maps for 40 GHz Observations through 2022
The Cosmology Large Angular Scale Surveyor (CLASS) is a telescope array that observes the cosmic microwave background over 75% of the sky from the Atacama Desert, Chile, at frequency bands centered near 40, 90, 150, and 220 GHz. This paper describes the CLASS data pipeline and maps for 40 GHz observ...
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/acf293 |
| _version_ | 1827789597891887104 |
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| author | Yunyang Li Joseph R. Eimer Keisuke Osumi John W. Appel Michael K. Brewer Aamir Ali Charles L. Bennett Sarah Marie Bruno Ricardo Bustos David T. Chuss Joseph Cleary Jullianna Denes Couto Sumit Dahal Rahul Datta Kevin L. Denis Rolando Dünner Francisco Espinoza Thomas Essinger-Hileman Pedro Fluxá Rojas Kathleen Harrington Jeffrey Iuliano John Karakla Tobias A. Marriage Nathan J. Miller Sasha Novack Carolina Núñez Matthew A. Petroff Rodrigo A. Reeves Karwan Rostem Rui Shi Deniz A. N. Valle Duncan J. Watts Janet L. Weiland Edward J. Wollack Zhilei Xu Lingzhen Zeng CLASS Collaboration |
| author_facet | Yunyang Li Joseph R. Eimer Keisuke Osumi John W. Appel Michael K. Brewer Aamir Ali Charles L. Bennett Sarah Marie Bruno Ricardo Bustos David T. Chuss Joseph Cleary Jullianna Denes Couto Sumit Dahal Rahul Datta Kevin L. Denis Rolando Dünner Francisco Espinoza Thomas Essinger-Hileman Pedro Fluxá Rojas Kathleen Harrington Jeffrey Iuliano John Karakla Tobias A. Marriage Nathan J. Miller Sasha Novack Carolina Núñez Matthew A. Petroff Rodrigo A. Reeves Karwan Rostem Rui Shi Deniz A. N. Valle Duncan J. Watts Janet L. Weiland Edward J. Wollack Zhilei Xu Lingzhen Zeng CLASS Collaboration |
| author_sort | Yunyang Li |
| collection | DOAJ |
| description | The Cosmology Large Angular Scale Surveyor (CLASS) is a telescope array that observes the cosmic microwave background over 75% of the sky from the Atacama Desert, Chile, at frequency bands centered near 40, 90, 150, and 220 GHz. This paper describes the CLASS data pipeline and maps for 40 GHz observations conducted from 2016 August to 2022 May. We demonstrate how well the CLASS survey strategy, with rapid (∼10 Hz) front-end modulation, recovers the large-scale Galactic polarization signal from the ground: the mapping transfer function recovers ∼67% (85%) of EE and BB ( VV ) power at ℓ = 20 and ∼35% (47%) at ℓ = 10. We present linear and circular polarization maps over 75% of the sky. Simulations based on the data imply the maps have a white noise level of $110\,\mu {\rm{K}}\,\mathrm{arcmin}$ and correlated noise component rising at low- ℓ as ℓ ^−2.4 . The transfer-function-corrected low- ℓ component is comparable to the white noise at the angular knee frequencies of ℓ ≈ 18 (linear polarization) and ℓ ≈ 12 (circular polarization). Finally, we present simulations of the level at which expected sources of systematic error bias the measurements, finding subpercent bias for the Λ cold dark matter EE power spectra. Bias from E -to- B leakage due to the data reduction pipeline and polarization angle uncertainty approaches the expected level for an r = 0.01 BB power spectrum. Improvements to the instrument calibration and the data pipeline will decrease this bias. |
| first_indexed | 2024-03-11T17:22:06Z |
| format | Article |
| id | doaj.art-e8b667c09ce4437995a91dea74c45620 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-11T17:22:06Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-e8b667c09ce4437995a91dea74c456202023-10-19T11:08:49ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0195627710.3847/1538-4357/acf293CLASS Data Pipeline and Maps for 40 GHz Observations through 2022Yunyang Li0https://orcid.org/0000-0002-4820-1122Joseph R. Eimer1https://orcid.org/0000-0001-6976-180XKeisuke Osumi2https://orcid.org/0000-0003-2838-1880John W. Appel3https://orcid.org/0000-0002-8412-630XMichael K. Brewer4Aamir Ali5https://orcid.org/0000-0001-7941-9602Charles L. Bennett6https://orcid.org/0000-0001-8839-7206Sarah Marie Bruno7https://orcid.org/0000-0003-2682-7498Ricardo Bustos8https://orcid.org/0000-0001-8468-9391David T. Chuss9https://orcid.org/0000-0003-0016-0533Joseph Cleary10https://orcid.org/0000-0002-7271-0525Jullianna Denes Couto11https://orcid.org/0000-0002-0552-3754Sumit Dahal12https://orcid.org/0000-0002-1708-5464Rahul Datta13https://orcid.org/0000-0003-3853-8757Kevin L. Denis14https://orcid.org/0000-0002-3592-5703Rolando Dünner15https://orcid.org/0000-0003-3892-1860Francisco Espinoza16https://orcid.org/0000-0002-1052-0339Thomas Essinger-Hileman17https://orcid.org/0000-0002-4782-3851Pedro Fluxá Rojas18https://orcid.org/0000-0002-2061-0063Kathleen Harrington19https://orcid.org/0000-0003-1248-9563Jeffrey Iuliano20https://orcid.org/0000-0001-7466-0317John Karakla21Tobias A. Marriage22https://orcid.org/0000-0003-4496-6520Nathan J. Miller23https://orcid.org/0000-0002-2245-1027Sasha Novack24https://orcid.org/0000-0001-7196-2520Carolina Núñez25https://orcid.org/0000-0002-5247-2523Matthew A. Petroff26https://orcid.org/0000-0002-4436-4215Rodrigo A. Reeves27https://orcid.org/0000-0001-5704-271XKarwan Rostem28https://orcid.org/0000-0003-4189-0700Rui Shi29https://orcid.org/0000-0001-7458-6946Deniz A. N. Valle30https://orcid.org/0000-0003-3487-2811Duncan J. Watts31https://orcid.org/0000-0002-5437-6121Janet L. Weiland32https://orcid.org/0000-0003-3017-3474Edward J. Wollack33https://orcid.org/0000-0002-7567-4451Zhilei Xu34https://orcid.org/0000-0001-5112-2567Lingzhen Zeng35https://orcid.org/0000-0001-6924-9072CLASS CollaborationThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.eduThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.eduThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.eduThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.eduThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.eduThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.eduThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.eduThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.eduDepartamento de Ingeniería Eléctrica, Universidad Católica de la Santísima Concepción , Alonso de Ribera 2850, Concepción, ChileDepartment of Physics, Villanova University , 800 Lancaster Avenue, Villanova, PA 19085, USAThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.eduThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.eduThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.edu; NASA Goddard Space Flight Center , 8800 Greenbelt Road, Greenbelt, MD 20771, USAThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.edu; Department of Astronomy and Astrophysics, University of Chicago , 5640 South Ellis Avenue, Chicago, IL 60637, USANASA Goddard Space Flight Center , 8800 Greenbelt Road, Greenbelt, MD 20771, USAInstituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile , Avenida Vicuña Mackenna 4860, 7820436, Chile; Centro de Astro-Ingeniería, Facultad de Física, Pontificia Universidad Católica de Chile , Avenida Vicuña Mackenna 4860, 7820436, ChileDepartamento de Ingeniería Eléctrica, Universidad Católica de la Santísima Concepción , Alonso de Ribera 2850, Concepción, ChileNASA Goddard Space Flight Center , 8800 Greenbelt Road, Greenbelt, MD 20771, USAInstituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile , Avenida Vicuña Mackenna 4860, 7820436, Chile; Centro de Astro-Ingeniería, Facultad de Física, Pontificia Universidad Católica de Chile , Avenida Vicuña Mackenna 4860, 7820436, ChileDepartment of Astronomy and Astrophysics, University of Chicago , 5640 South Ellis Avenue, Chicago, IL 60637, USA; High Energy Physics Division, Argonne National Laboratory , 9700 S. Cass Avenue, Lemont, IL 60439, USAThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.edu; Department of Physics and Astronomy, University of Pennsylvania , 209 South 33rd Street, Philadelphia, PA 19104, USAThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.eduThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.eduThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.edu; NASA Goddard Space Flight Center , 8800 Greenbelt Road, Greenbelt, MD 20771, USAThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.edu; Department of Astrophysical and Planetary Sciences, University of Colorado , 2000 Colorado Avenue, Boulder, CO 80309, USAThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.eduCenter for Astrophysics , Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USACePIA, Astronomy Department, Universidad de Concepción , Casilla 160-C, Concepción, ChileNASA Goddard Space Flight Center , 8800 Greenbelt Road, Greenbelt, MD 20771, USAThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.eduThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.eduInstitute of Theoretical Astrophysics, University of Oslo , P.O. Box 1029 Blindern, N-0315 Oslo, NorwayThe William H. Miller III Department of Physics and Astronomy, Johns Hopkins University , 3701 San Martin Drive, Baltimore, MD 21218, USA ; yunyangl@jhu.eduNASA Goddard Space Flight Center , 8800 Greenbelt Road, Greenbelt, MD 20771, USADepartment of Physics and Astronomy, University of Pennsylvania , 209 South 33rd Street, Philadelphia, PA 19104, USA; MIT Kavli Institute, Massachusetts Institute of Technology , 77 Massachusetts Avenue, Cambridge, MA 02139, USACenter for Astrophysics , Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USAThe Cosmology Large Angular Scale Surveyor (CLASS) is a telescope array that observes the cosmic microwave background over 75% of the sky from the Atacama Desert, Chile, at frequency bands centered near 40, 90, 150, and 220 GHz. This paper describes the CLASS data pipeline and maps for 40 GHz observations conducted from 2016 August to 2022 May. We demonstrate how well the CLASS survey strategy, with rapid (∼10 Hz) front-end modulation, recovers the large-scale Galactic polarization signal from the ground: the mapping transfer function recovers ∼67% (85%) of EE and BB ( VV ) power at ℓ = 20 and ∼35% (47%) at ℓ = 10. We present linear and circular polarization maps over 75% of the sky. Simulations based on the data imply the maps have a white noise level of $110\,\mu {\rm{K}}\,\mathrm{arcmin}$ and correlated noise component rising at low- ℓ as ℓ ^−2.4 . The transfer-function-corrected low- ℓ component is comparable to the white noise at the angular knee frequencies of ℓ ≈ 18 (linear polarization) and ℓ ≈ 12 (circular polarization). Finally, we present simulations of the level at which expected sources of systematic error bias the measurements, finding subpercent bias for the Λ cold dark matter EE power spectra. Bias from E -to- B leakage due to the data reduction pipeline and polarization angle uncertainty approaches the expected level for an r = 0.01 BB power spectrum. Improvements to the instrument calibration and the data pipeline will decrease this bias.https://doi.org/10.3847/1538-4357/acf293Astronomy data analysisCosmic microwave background radiationObservational cosmologyEarly universe |
| spellingShingle | Yunyang Li Joseph R. Eimer Keisuke Osumi John W. Appel Michael K. Brewer Aamir Ali Charles L. Bennett Sarah Marie Bruno Ricardo Bustos David T. Chuss Joseph Cleary Jullianna Denes Couto Sumit Dahal Rahul Datta Kevin L. Denis Rolando Dünner Francisco Espinoza Thomas Essinger-Hileman Pedro Fluxá Rojas Kathleen Harrington Jeffrey Iuliano John Karakla Tobias A. Marriage Nathan J. Miller Sasha Novack Carolina Núñez Matthew A. Petroff Rodrigo A. Reeves Karwan Rostem Rui Shi Deniz A. N. Valle Duncan J. Watts Janet L. Weiland Edward J. Wollack Zhilei Xu Lingzhen Zeng CLASS Collaboration CLASS Data Pipeline and Maps for 40 GHz Observations through 2022 The Astrophysical Journal Astronomy data analysis Cosmic microwave background radiation Observational cosmology Early universe |
| title | CLASS Data Pipeline and Maps for 40 GHz Observations through 2022 |
| title_full | CLASS Data Pipeline and Maps for 40 GHz Observations through 2022 |
| title_fullStr | CLASS Data Pipeline and Maps for 40 GHz Observations through 2022 |
| title_full_unstemmed | CLASS Data Pipeline and Maps for 40 GHz Observations through 2022 |
| title_short | CLASS Data Pipeline and Maps for 40 GHz Observations through 2022 |
| title_sort | class data pipeline and maps for 40 ghz observations through 2022 |
| topic | Astronomy data analysis Cosmic microwave background radiation Observational cosmology Early universe |
| url | https://doi.org/10.3847/1538-4357/acf293 |
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