English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

In an effort to transcend the limitations of differential imaging ofexoplanets in the era of extremely large telescopes (ELTs), the first paper inthis series established a rigorous, fully polarimetric framework fordetermining the science camera (SC) image given a turbulent wavefront andunknown aberrations in multiple planes the optical system. This article buildson the structure developed in Paper I in order to rigorously express thepolarimetric SC image in terms of the field impinging on the wavefront sensor(WFS), thereby providing a direct connection between the measurements made inboth subsystems. This formulation allows the SC image to be written as afunction of the WFS measurements, including the following unknown quantitieswhich can, in principle, be estimated via statistical inference: the non-commonpath aberration (NCPA), WFS gain errors, aberrations downstream of thebeamsplitter, and the planetary image. It is demonstrated that WFS bias erroris mathematically equivalent to NCPA. Thus, with the ability to treat WFS biasand gains, the method should not be overly sensitive to WFS calibrationproblems. Importantly, this formulation includes stochastic processes thatrepresent noisy measurement of the SC image, noisy WFS measurements, andhigh-frequency components of the wavefront to which the WFS is insensitive. Itis shown that wavefront error due to noise in the WFS measurements has aconvenient semi-analytical representation in terms of the WFS measurementoperator's singular functions. Further, the first and second order statisticsof these processes are specified, thereby setting the stage for the applicationof statistical inference methods to be describe in later papers in this series.

A Statistical Framework for Utilization of Simultaneous Pupil Plane and  Focal Plane Telemetry for Exoplanet Imaging, Part II: The Science Camera  Image as a Function of the Wavefront Sensor Field