TY - GEN
T1 - Simulations of polarimetric observations of debris disks through the Roman Coronagraph Instrument
AU - Anche, Ramya M.
AU - Douglas, Ewan S.
AU - Milani, Kian
AU - Ashcraft, Jaren
AU - Debes, John
N1 - Funding Information:
Portions of this work were supported by the WFIRST Science Investigation team prime award #NNG16PJ24 and the Arizona Board of Regents Technology Research Initiative Fund (TRIF). The authors would like to thank Dr. Max Miller-Blanchaer (UCSB) for the useful discussions and Dr. Bertrand Mennesson (JPL) for generating the Mueller matrices.
Publisher Copyright:
© 2022 SPIE.
PY - 2022
Y1 - 2022
N2 - The Roman coronagraph instrument will demonstrate high-contrast imaging technology, enabling the imaging of faint debris disks, the discovery of inner dust belts, and planets. Polarization studies of debris disks provide additional information on dust grains' size, distribution, and shape. The Roman coronagraph uses a polarization module comprising two Wollaston prism assemblies to produce four orthogonally polarized images (I0, I90, I45, and I135), each measuring 3.2 arcsecs in diameter and separated by 7.5 arcsecs in the sky. The expected RMS error in the linear polarization fraction measurement is 1.66% per resolution element of 3 by 3 pixels. We present a mathematical model to simulate the polarized intensity images through the Roman CGI, including the instrumental polarization and other uncertainties. We use disk modeling software, MCFOST, to model q, u, and polarization intensity of the debris disk, Epsilon-Eridani. The polarization intensities are convolved with the coronagraph throughput incorporating the PSF morphology. We include model uncertainties, detector noise, speckle noise, and jitter. The final polarization fraction of 0.4±0.0251 is obtained after post-processing and speckle noise removal.
AB - The Roman coronagraph instrument will demonstrate high-contrast imaging technology, enabling the imaging of faint debris disks, the discovery of inner dust belts, and planets. Polarization studies of debris disks provide additional information on dust grains' size, distribution, and shape. The Roman coronagraph uses a polarization module comprising two Wollaston prism assemblies to produce four orthogonally polarized images (I0, I90, I45, and I135), each measuring 3.2 arcsecs in diameter and separated by 7.5 arcsecs in the sky. The expected RMS error in the linear polarization fraction measurement is 1.66% per resolution element of 3 by 3 pixels. We present a mathematical model to simulate the polarized intensity images through the Roman CGI, including the instrumental polarization and other uncertainties. We use disk modeling software, MCFOST, to model q, u, and polarization intensity of the debris disk, Epsilon-Eridani. The polarization intensities are convolved with the coronagraph throughput incorporating the PSF morphology. We include model uncertainties, detector noise, speckle noise, and jitter. The final polarization fraction of 0.4±0.0251 is obtained after post-processing and speckle noise removal.
KW - Debris disks
KW - Polarimetric calibration
KW - Polarization observations
KW - Roman CGI
KW - coronagraphs
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U2 - 10.1117/12.2629497
DO - 10.1117/12.2629497
M3 - Conference contribution
AN - SCOPUS:85146685431
T3 - Proceedings of SPIE - The International Society for Optical Engineering
BT - Space Telescopes and Instrumentation 2022
A2 - Coyle, Laura E.
A2 - Matsuura, Shuji
A2 - Perrin, Marshall D.
PB - SPIE
T2 - Space Telescopes and Instrumentation 2022: Optical, Infrared, and Millimeter Wave
Y2 - 17 July 2022 through 22 July 2022
ER -