Nancy Grace Roman Space Telescope coronagraph instrument observation calibration plan

Zellem, Robert T.; Nemati, B.; González, Guillermo; Ygouf, Marie; Bailey, Vanessa P.; Cady, Eric; Colavita, M. M.; Hildebrandt, S. R.; Maier, Erin; Mennesson, Bertrand; Payne, Lindsey; Zimmerman, Neil; Belikov, Ruslan; Rosa, Robert J. De; Debes, John H.; Douglas, Ewan S.; Girard, Julien; Groff, Tyler D.; Kasdin, Jeremy; Lowrance, P.; Macintosh, Bruce; Ryan, Daniel; Weisberg, Carey

doi:10.1117/12.2627567

Cited by 4 publications

(3 citation statements)

References 10 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…High contrast imaging with the recently launched JWST 71 and the upcoming Roman Space Telescope coronagraph 72 will in each case demand a new generation of data-driven PSF and detector calibrations beyond those used fruitfully on ground-based data 73 . While we have not attempted this in the present work, ∂Lux can flexibly model aberrations in the multiple intermediate planes of these coronagraphs, and in future work we intend to assess the practical and fundamental limits of multiplane phase retrieval and calibration to improve coronagraphic modelling.…”

Section: Discussionmentioning

confidence: 99%

Differentiable optics with ∂Lux: I—deep calibration of flat field and phase retrieval with automatic differentiation

Desdoigts

Pope

Dennis

et al. 2023

J. Astron. Telesc. Instrum. Syst.

View full text Add to dashboard Cite

.The sensitivity limits of space telescopes are imposed by uncalibrated errors in the point spread function, photon-noise, background light, and detector sensitivity. These are typically calibrated with specialized wavefront sensor hardware and with flat fields obtained on the ground or with calibration sources, but these leave vulnerabilities to residual time-varying or non-common path aberrations and variations in the detector conditions. It is, therefore, desirable to infer these from science data alone, facing the prohibitively high dimensional problems of phase retrieval and pixel-level calibration. We introduce a new Python package for physical optics simulation, ∂ Lux, which uses the machine learning framework Jax to achieve graphics processing unit acceleration and automatic differentiation (autodiff), and apply this to simulating astronomical imaging. In this first of a series of papers, we show that gradient descent enabled by autodiff can be used to simultaneously perform phase retrieval and calibration of detector sensitivity, scaling efficiently to inferring millions of parameters. This new framework enables high dimensional optimization and inference in data analysis and hardware design in astronomy and beyond, which we explore in subsequent papers in this series.

show abstract

Section: Discussionmentioning

confidence: 99%

Differentiable optics with ∂Lux: I—deep calibration of flat field and phase retrieval with automatic differentiation

Desdoigts

Pope

Dennis

et al. 2023

J. Astron. Telesc. Instrum. Syst.

View full text Add to dashboard Cite

show abstract

“…flat-fielding errors. 16 • Simulate calibration/validation procedures 15 • Investigate new wavefront control schemes 41 • Include more advanced data-analysis approaches based on ADI and RDI 20 • Target selection • Ground-support precursor observations…”

Section: Discussionmentioning

confidence: 99%

“…14 The expected performance of this polarimetric mode is limited by calibration and flat-fielding errors, and the expected error on the linear polarization fraction has been estimated to be at the 3% level. 15,16 With careful in-orbit calibration this might be improved. For example, observations of extended sources like Uranus or Neptune can improve flat-field calibration.…”

Section: Introductionmentioning

confidence: 99%

FALCO simulations of high-contrast polarimetry with the Nancy Grace Roman Space Telescope coronagraph instrument

Doelman,

Belaouchi,

Riggs

et al. 2023

Techniques and Instrumentation for Detection of Exoplanets XI

View full text Add to dashboard Cite

The Coronagraph Instrument of the Nancy Grace Roman Space Telescope (Roman Coronagraph) will be capable of both total intensity and polarization measurements of circumstellar disks. The polarimetric performance is impacted by polarization effects introduced by all mirrors before the Wollaston prisms. In this paper, we aim to characterize these effects for the Roman Coronagraph in bands 1 and 4 using the FALCO and PROPER packages. We simulate the effect of polarization aberrations that impact the polarimetric contrast and the instrumental polarization effects to study the polarimetric accuracy. We include spacecraft rolls, but leave out systematic camera noise. We find that polarimetric differential imaging (PDI) improves the contrast by a factor of six. The PDI contrast of ∼ 8 × 10 −11 is limited by polarized speckles from instrumental polarization effects and polarization aberrations. By injecting polarized companions with at various contrast levels and demodulating their polarimetric signal, we recover their source Stokes vector within 2%.

show abstract

Simulation of High-contrast Polarimetric Observations of Debris Disks with the Roman Coronagraph Instrument

Anche,

Douglas,

Milani

et al. 2023

PASP

View full text Add to dashboard Cite

The Nancy Grace Roman Space Telescope Coronagraph Instrument will enable the polarimetric imaging of debris disks and inner dust belts in the optical and near-infrared wavelengths, in addition to the high-contrast polarimetric imaging and spectroscopy of exoplanets. The Coronagraph uses two Wollaston prisms to produce four orthogonally polarized images and is expected to measure the polarization fraction with measurement errors <3% per spatial resolution element. To simulate the polarization observations through the Hybrid Lyot Coronagraph (HLC) and Shaped Pupil Coronagraph (SPC), we model disk scattering, the coronagraphic point-response function, detector noise, speckles, jitter, and instrumental polarization and calculate the Stokes parameters. To illustrate the potential for discovery and a better understanding of known systems with both the HLC and SPC modes, we model the debris disks around Epsilon Eridani and HR 4796A, respectively. For Epsilon Eridani, using astrosilicates with 0.37 ± 0.01 as the peak input polarization fraction in one resolution element, we recover the peak disk polarization fraction of 0.33 ± 0.01. Similarly, for HR 4796A, for a peak input polarization fraction of 0.92 ± 0.01, we obtain the peak output polarization fraction as 0.80 ± 0.03. The Coronagraph design meets the required precision, and forward modeling is needed to accurately estimate the polarization fraction.

show abstract

Nancy Grace Roman Space Telescope coronagraph instrument observation calibration plan

Cited by 4 publications

References 10 publications

Differentiable optics with ∂Lux: I—deep calibration of flat field and phase retrieval with automatic differentiation

Differentiable optics with ∂Lux: I—deep calibration of flat field and phase retrieval with automatic differentiation

FALCO simulations of high-contrast polarimetry with the Nancy Grace Roman Space Telescope coronagraph instrument

Simulation of High-contrast Polarimetric Observations of Debris Disks with the Roman Coronagraph Instrument

Contact Info

Product

Resources

About