Optical modeling and polarization calibration for CMB measurements with ACTPol and Advanced ACTPol

Brian Koopman, Jason Austermann, Hsiao Mei Cho, Kevin P. Coughlin, Shannon M. Duff, Patricio A. Gallardo, Matthew Hasselfield, Shawn W. Henderson, Shuay Pwu Patty Ho, Johannes Hubmayr, Kent D. Irwin, Dale Li, Jeff McMahon, Federico Nati, Michael D. Niemack, Laura Newburgh, Lyman A. Page, Maria Salatino, Alessandro Schillaci, Benjamin L. SchmittSara M. Simon, Eve M. Vavagiakis, Jonathan T. Ward, Edward J. Wollack

Research output: Chapter in Book/Report/Conference proceedingConference contribution

8 Citations (Scopus)

Abstract

The Atacama Cosmology Telescope Polarimeter (ACTPol) is a polarization sensitive upgrade to the Atacama Cosmology Telescope, located at an elevation of 5190 m on Cerro Toco in Chile. ACTPol uses transition edge sensor bolometers coupled to orthomode transducers to measure both the temperature and polarization of the Cosmic Microwave Background (CMB). Calibration of the detector angles is a critical step in producing polarization maps of the CMB. Polarization angle offsets in the detector calibration can cause leakage in polarization from E to B modes and induce a spurious signal in the EB and TB cross correlations, which eliminates our ability to measure potential cosmological sources of EB and TB signals, such as cosmic birefringence. We calibrate the ACTPol detector angles by ray tracing the designed detector angle through the entire optical chain to determine the projection of each detector angle on the sky. The distribution of calibrated detector polarization angles are consistent with a global offset angle from zero when compared to the EB-nulling offset angle, the angle required to null the EB cross-correlation power spectrum. We present the optical modeling process. The detector angles can be cross checked through observations of known polarized sources, whether this be a galactic source or a laboratory reference standard. To cross check the ACTPol detector angles, we use a thin film polarization grid placed in front of the receiver of the telescope, between the receiver and the secondary reflector. Making use of a rapidly rotating half-wave plate (HWP) mount we spin the polarizing grid at a constant speed, polarizing and rotating the incoming atmospheric signal. The resulting sinusoidal signal is used to determine the detector angles. The optical modeling calibration was shown to be consistent with a global offset angle of zero when compared to EB nulling in the first ACTPol results and will continue to be a part of our calibration implementation. The first array of detectors for Advanced ACTPol, the next generation upgrade to ACTPol, will be deployed in 2016. We plan to continue using both techniques and compare them to astrophysical source measurements for the Advanced ACTPol polarization calibration.

Original languageEnglish (US)
Title of host publicationMillimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII
EditorsJonas Zmuidzinas, Wayne S. Holland
PublisherSPIE
ISBN (Electronic)9781510602076
DOIs
StatePublished - Jan 1 2016
EventMillimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII - Edinburgh, United Kingdom
Duration: Jun 28 2016Jul 1 2016

Publication series

NameProceedings of SPIE - The International Society for Optical Engineering
Volume9914
ISSN (Print)0277-786X
ISSN (Electronic)1996-756X

Other

OtherMillimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII
CountryUnited Kingdom
CityEdinburgh
Period6/28/167/1/16

Fingerprint

Cosmology
Optical Modeling
Microwave measurement
Polarimeter
Polarimeters
polarimeters
Telescopes
Microwave
cosmology
Telescope
Calibration
Polarization
telescopes
Detectors
microwaves
Angle
Detector
polarization
detectors
Nulling

All Science Journal Classification (ASJC) codes

  • Electronic, Optical and Magnetic Materials
  • Condensed Matter Physics
  • Computer Science Applications
  • Applied Mathematics
  • Electrical and Electronic Engineering

Cite this

Koopman, B., Austermann, J., Cho, H. M., Coughlin, K. P., Duff, S. M., Gallardo, P. A., ... Wollack, E. J. (2016). Optical modeling and polarization calibration for CMB measurements with ACTPol and Advanced ACTPol. In J. Zmuidzinas, & W. S. Holland (Eds.), Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII [99142T] (Proceedings of SPIE - The International Society for Optical Engineering; Vol. 9914). SPIE. https://doi.org/10.1117/12.2231912
Koopman, Brian ; Austermann, Jason ; Cho, Hsiao Mei ; Coughlin, Kevin P. ; Duff, Shannon M. ; Gallardo, Patricio A. ; Hasselfield, Matthew ; Henderson, Shawn W. ; Ho, Shuay Pwu Patty ; Hubmayr, Johannes ; Irwin, Kent D. ; Li, Dale ; McMahon, Jeff ; Nati, Federico ; Niemack, Michael D. ; Newburgh, Laura ; Page, Lyman A. ; Salatino, Maria ; Schillaci, Alessandro ; Schmitt, Benjamin L. ; Simon, Sara M. ; Vavagiakis, Eve M. ; Ward, Jonathan T. ; Wollack, Edward J. / Optical modeling and polarization calibration for CMB measurements with ACTPol and Advanced ACTPol. Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII. editor / Jonas Zmuidzinas ; Wayne S. Holland. SPIE, 2016. (Proceedings of SPIE - The International Society for Optical Engineering).
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abstract = "The Atacama Cosmology Telescope Polarimeter (ACTPol) is a polarization sensitive upgrade to the Atacama Cosmology Telescope, located at an elevation of 5190 m on Cerro Toco in Chile. ACTPol uses transition edge sensor bolometers coupled to orthomode transducers to measure both the temperature and polarization of the Cosmic Microwave Background (CMB). Calibration of the detector angles is a critical step in producing polarization maps of the CMB. Polarization angle offsets in the detector calibration can cause leakage in polarization from E to B modes and induce a spurious signal in the EB and TB cross correlations, which eliminates our ability to measure potential cosmological sources of EB and TB signals, such as cosmic birefringence. We calibrate the ACTPol detector angles by ray tracing the designed detector angle through the entire optical chain to determine the projection of each detector angle on the sky. The distribution of calibrated detector polarization angles are consistent with a global offset angle from zero when compared to the EB-nulling offset angle, the angle required to null the EB cross-correlation power spectrum. We present the optical modeling process. The detector angles can be cross checked through observations of known polarized sources, whether this be a galactic source or a laboratory reference standard. To cross check the ACTPol detector angles, we use a thin film polarization grid placed in front of the receiver of the telescope, between the receiver and the secondary reflector. Making use of a rapidly rotating half-wave plate (HWP) mount we spin the polarizing grid at a constant speed, polarizing and rotating the incoming atmospheric signal. The resulting sinusoidal signal is used to determine the detector angles. The optical modeling calibration was shown to be consistent with a global offset angle of zero when compared to EB nulling in the first ACTPol results and will continue to be a part of our calibration implementation. The first array of detectors for Advanced ACTPol, the next generation upgrade to ACTPol, will be deployed in 2016. We plan to continue using both techniques and compare them to astrophysical source measurements for the Advanced ACTPol polarization calibration.",
author = "Brian Koopman and Jason Austermann and Cho, {Hsiao Mei} and Coughlin, {Kevin P.} and Duff, {Shannon M.} and Gallardo, {Patricio A.} and Matthew Hasselfield and Henderson, {Shawn W.} and Ho, {Shuay Pwu Patty} and Johannes Hubmayr and Irwin, {Kent D.} and Dale Li and Jeff McMahon and Federico Nati and Niemack, {Michael D.} and Laura Newburgh and Page, {Lyman A.} and Maria Salatino and Alessandro Schillaci and Schmitt, {Benjamin L.} and Simon, {Sara M.} and Vavagiakis, {Eve M.} and Ward, {Jonathan T.} and Wollack, {Edward J.}",
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Koopman, B, Austermann, J, Cho, HM, Coughlin, KP, Duff, SM, Gallardo, PA, Hasselfield, M, Henderson, SW, Ho, SPP, Hubmayr, J, Irwin, KD, Li, D, McMahon, J, Nati, F, Niemack, MD, Newburgh, L, Page, LA, Salatino, M, Schillaci, A, Schmitt, BL, Simon, SM, Vavagiakis, EM, Ward, JT & Wollack, EJ 2016, Optical modeling and polarization calibration for CMB measurements with ACTPol and Advanced ACTPol. in J Zmuidzinas & WS Holland (eds), Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII., 99142T, Proceedings of SPIE - The International Society for Optical Engineering, vol. 9914, SPIE, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII, Edinburgh, United Kingdom, 6/28/16. https://doi.org/10.1117/12.2231912

Optical modeling and polarization calibration for CMB measurements with ACTPol and Advanced ACTPol. / Koopman, Brian; Austermann, Jason; Cho, Hsiao Mei; Coughlin, Kevin P.; Duff, Shannon M.; Gallardo, Patricio A.; Hasselfield, Matthew; Henderson, Shawn W.; Ho, Shuay Pwu Patty; Hubmayr, Johannes; Irwin, Kent D.; Li, Dale; McMahon, Jeff; Nati, Federico; Niemack, Michael D.; Newburgh, Laura; Page, Lyman A.; Salatino, Maria; Schillaci, Alessandro; Schmitt, Benjamin L.; Simon, Sara M.; Vavagiakis, Eve M.; Ward, Jonathan T.; Wollack, Edward J.

Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII. ed. / Jonas Zmuidzinas; Wayne S. Holland. SPIE, 2016. 99142T (Proceedings of SPIE - The International Society for Optical Engineering; Vol. 9914).

Research output: Chapter in Book/Report/Conference proceedingConference contribution

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AU - Koopman, Brian

AU - Austermann, Jason

AU - Cho, Hsiao Mei

AU - Coughlin, Kevin P.

AU - Duff, Shannon M.

AU - Gallardo, Patricio A.

AU - Hasselfield, Matthew

AU - Henderson, Shawn W.

AU - Ho, Shuay Pwu Patty

AU - Hubmayr, Johannes

AU - Irwin, Kent D.

AU - Li, Dale

AU - McMahon, Jeff

AU - Nati, Federico

AU - Niemack, Michael D.

AU - Newburgh, Laura

AU - Page, Lyman A.

AU - Salatino, Maria

AU - Schillaci, Alessandro

AU - Schmitt, Benjamin L.

AU - Simon, Sara M.

AU - Vavagiakis, Eve M.

AU - Ward, Jonathan T.

AU - Wollack, Edward J.

PY - 2016/1/1

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N2 - The Atacama Cosmology Telescope Polarimeter (ACTPol) is a polarization sensitive upgrade to the Atacama Cosmology Telescope, located at an elevation of 5190 m on Cerro Toco in Chile. ACTPol uses transition edge sensor bolometers coupled to orthomode transducers to measure both the temperature and polarization of the Cosmic Microwave Background (CMB). Calibration of the detector angles is a critical step in producing polarization maps of the CMB. Polarization angle offsets in the detector calibration can cause leakage in polarization from E to B modes and induce a spurious signal in the EB and TB cross correlations, which eliminates our ability to measure potential cosmological sources of EB and TB signals, such as cosmic birefringence. We calibrate the ACTPol detector angles by ray tracing the designed detector angle through the entire optical chain to determine the projection of each detector angle on the sky. The distribution of calibrated detector polarization angles are consistent with a global offset angle from zero when compared to the EB-nulling offset angle, the angle required to null the EB cross-correlation power spectrum. We present the optical modeling process. The detector angles can be cross checked through observations of known polarized sources, whether this be a galactic source or a laboratory reference standard. To cross check the ACTPol detector angles, we use a thin film polarization grid placed in front of the receiver of the telescope, between the receiver and the secondary reflector. Making use of a rapidly rotating half-wave plate (HWP) mount we spin the polarizing grid at a constant speed, polarizing and rotating the incoming atmospheric signal. The resulting sinusoidal signal is used to determine the detector angles. The optical modeling calibration was shown to be consistent with a global offset angle of zero when compared to EB nulling in the first ACTPol results and will continue to be a part of our calibration implementation. The first array of detectors for Advanced ACTPol, the next generation upgrade to ACTPol, will be deployed in 2016. We plan to continue using both techniques and compare them to astrophysical source measurements for the Advanced ACTPol polarization calibration.

AB - The Atacama Cosmology Telescope Polarimeter (ACTPol) is a polarization sensitive upgrade to the Atacama Cosmology Telescope, located at an elevation of 5190 m on Cerro Toco in Chile. ACTPol uses transition edge sensor bolometers coupled to orthomode transducers to measure both the temperature and polarization of the Cosmic Microwave Background (CMB). Calibration of the detector angles is a critical step in producing polarization maps of the CMB. Polarization angle offsets in the detector calibration can cause leakage in polarization from E to B modes and induce a spurious signal in the EB and TB cross correlations, which eliminates our ability to measure potential cosmological sources of EB and TB signals, such as cosmic birefringence. We calibrate the ACTPol detector angles by ray tracing the designed detector angle through the entire optical chain to determine the projection of each detector angle on the sky. The distribution of calibrated detector polarization angles are consistent with a global offset angle from zero when compared to the EB-nulling offset angle, the angle required to null the EB cross-correlation power spectrum. We present the optical modeling process. The detector angles can be cross checked through observations of known polarized sources, whether this be a galactic source or a laboratory reference standard. To cross check the ACTPol detector angles, we use a thin film polarization grid placed in front of the receiver of the telescope, between the receiver and the secondary reflector. Making use of a rapidly rotating half-wave plate (HWP) mount we spin the polarizing grid at a constant speed, polarizing and rotating the incoming atmospheric signal. The resulting sinusoidal signal is used to determine the detector angles. The optical modeling calibration was shown to be consistent with a global offset angle of zero when compared to EB nulling in the first ACTPol results and will continue to be a part of our calibration implementation. The first array of detectors for Advanced ACTPol, the next generation upgrade to ACTPol, will be deployed in 2016. We plan to continue using both techniques and compare them to astrophysical source measurements for the Advanced ACTPol polarization calibration.

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Koopman B, Austermann J, Cho HM, Coughlin KP, Duff SM, Gallardo PA et al. Optical modeling and polarization calibration for CMB measurements with ACTPol and Advanced ACTPol. In Zmuidzinas J, Holland WS, editors, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII. SPIE. 2016. 99142T. (Proceedings of SPIE - The International Society for Optical Engineering). https://doi.org/10.1117/12.2231912