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arxiv: 2606.12842 · v1 · pith:LVEQ2ISCnew · submitted 2026-06-11 · 🌌 astro-ph.IM · astro-ph.EP

Connecting Polarization to Exoplanet Yield Calculations for HWO

Jaren N. Ashcraft , Scott D. Will , Maxwell A. Millar-Blanchaer , Breann Sitarski , Christopher C. Stark , Ewan S. Douglas , John Krist , Brian Kern
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Manuel Quijada
This is my paper

Pith reviewed 2026-06-27 06:09 UTC · model grok-4.3

classification 🌌 astro-ph.IM astro-ph.EP
keywords polarization aberrationsexoplanet yieldHabitable Worlds Observatorycoronagraphangle of incidencephysical optics modelingHWO designEAC-1
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The pith

Shorter HWO barrel from 16 m to 12 m still reaches 10^{-10} contrast at the inner working angle in visible light despite polarization aberrations.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper links physical optics modeling of polarization aberrations to exoplanet yield calculations to quantify their effect on the number of detectable Earth-like planets for the Habitable Worlds Observatory. It shows how angle-of-incidence variations along the optical path create these aberrations and how they scale with primary-to-secondary mirror separation. A sympathetic reader would care because the findings guide design choices between observatory compactness, mechanical stability, and the total science return from a coronagraph that must suppress starlight by ten billion times. The work reports that the visible band remains sensitive to these effects while the ultraviolet band is less so, and it identifies a limited window for yield-based optimization to offset the aberrations.

Core claim

By connecting open-source physical optics tools to an exoplanet yield optimizer, the authors establish that polarization aberrations induced by angle-of-incidence changes in the EAC-1 design can be quantified and mapped to detection statistics. Decreasing the barrel length from 16 m to 12 m produces approximately 10^{-10} contrast at the inner working angle where exo-Earths are expected in the visible, while the ultraviolet band shows lower sensitivity because exo-Earths lie farther from the inner working angle. The design reference mission admits only a limited range of altruistic yield optimization that compensates for the aberrations, and the authors outline mitigation approaches to reduc

What carries the argument

The linkage between physical optics modeling of polarization aberrations from angle-of-incidence variations and an exoplanet yield optimizer that converts resulting contrast levels into expected detection yields.

Load-bearing premise

The physical optics modeling tools accurately capture the polarization aberrations induced by angle-of-incidence variations in the actual HWO optical train, and the exoplanet yield optimizer correctly maps those contrast levels into detection statistics.

What would settle it

A laboratory measurement of achieved contrast at the inner working angle in a scaled or flight-like HWO coronagraph model using the 12 m barrel configuration, checked against the modeled value of approximately 10^{-10} in the visible.

Figures

Figures reproduced from arXiv: 2606.12842 by Breann Sitarski, Brian Kern, Christopher C. Stark, Ewan S. Douglas, Jaren N. Ashcraft, John Krist, Manuel Quijada, Maxwell A. Millar-Blanchaer, Scott D. Will.

Figure 1
Figure 1. Figure 1: Overview of the simulation pipeline components used in this work. The modeling begins with [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: The reflectivity (left) diattenuation (center) and retardance (right) of the coatings considered in this study. The [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: (Left) Ray diagram of the EAC-1 observatory and coronagraph which is packaged under the primary mirror (M1). [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Azimuthally-averaged PSF profiles for each of the 10 optical designs used in this study, with polarization [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Azimuthally-averaged PSF profiles for each of the 10 optical designs used in this study, with polarization [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Azimuthally-averaged PSF profiles for each of the 10 optical designs used in this study, with polarization [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Yield diagrams showing the difference in HZ Completeness between a polarization aberrated case and the [PITH_FULL_IMAGE:figures/full_fig_p010_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Plot of the degraded normalized intensity averaged over different annuli on the coronagraph focal plane as a [PITH_FULL_IMAGE:figures/full_fig_p011_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Azimuthally averaged focal plane residuals for EAC-4 for the three cases studied. Each design had a slightly [PITH_FULL_IMAGE:figures/full_fig_p012_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Azimuthally-averaged PSF profiles for each of the 10 optical designs used in this study, with polarization [PITH_FULL_IMAGE:figures/full_fig_p014_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Azimuthally-averaged PSF profiles for each of the 10 optical designs used in this study, with polarization [PITH_FULL_IMAGE:figures/full_fig_p015_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Azimuthally-averaged PSF profiles for each of the 10 optical designs used in this study, with polarization [PITH_FULL_IMAGE:figures/full_fig_p016_12.png] view at source ↗
read the original abstract

The Habitable Worlds Observatory (HWO) aims to enable the detection and characterization of Earth-like planets around Sun-like stars to search for possible signs of life elsewhere in our universe. This requires an incredibly sensitive coronagraph instrument that suppresses the light from the star by a factor of 10 billion, which must contend with error terms that have not previously limited high-contrast instrumentation at lower levels of starlight suppression. Polarization aberrations are one such source of error that is particularly problematic for coronagraphy on a large space telescope. Optical rays in large, compact astronomical observatories can have large changes in angle of incidence over the beam, which induce polarization aberrations that decrease sensitivities to faint signals at small angular separations. Limiting variation in angles of incidence along the optical path could lead to longer, less stable observatories. This could negatively impact the total number of exo-Earths HWO would be able to detect. This study links open-source physical optics modeling tools to an exoplanet yield optimizer to understand how polarization aberrations influence science return for HWO. We also explore how polarization aberrations scale with change in angle of incidence, which could drive the primary-secondary mirror distance and overall observatory stability. In the visible, we find that decreasing the EAC-1 barrel from 16m to 12m results in $\approx 10^{-10}$ contrast at the IWA where we expect exo-Earths to be. In the UV we appear to be less sensitive to polarization because exo-Earths are farther from the IWA. We also find a limited range over which the design reference mission of EAC-1 can be optimized to compensate for polarization aberrations using altruistic yield optimization. We then report on mitigation strategies to minimize the presence of polarization aberrations in HWO.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 1 minor

Summary. The manuscript links open-source physical optics modeling tools to an exoplanet yield optimizer to quantify the impact of polarization aberrations on HWO contrast performance and science yield. It reports that shortening the EAC-1 barrel length from 16 m to 12 m produces ≈10^{-10} contrast at the IWA in the visible, with reduced sensitivity in the UV, a limited range for altruistic yield optimization of the DRM, and discussion of mitigation strategies for angle-of-incidence-induced polarization effects.

Significance. If the modeling chain is accurate, the results supply quantitative design guidance on the stability-versus-yield trade-off for HWO by showing how barrel length (and thus primary-secondary separation) controls polarization aberrations that limit contrast at small angular separations. The work also demonstrates a practical workflow connecting physical-optics packages to yield codes, which could be reusable for other high-contrast mission concepts.

major comments (2)
  1. [Abstract] Abstract: the central quantitative claim that a 16 m → 12 m barrel change yields ≈10^{-10} contrast at the IWA rests on the unvalidated assumption that the chosen physical-optics package correctly computes the Mueller-matrix aberrations arising from the specific angle-of-incidence map across the shortened EAC-1 optical train; no benchmark against analytic polarization ray tracing, a second code, or a known test optic is described.
  2. [Abstract] Abstract (paragraph on linking tools to optimizer): the mapping from modeled contrast to exo-Earth yield statistics is load-bearing for the science-return conclusions, yet the abstract supplies no error budget, sensitivity analysis, or propagation of polarization-model uncertainties through the optimizer, leaving the quantitative yield impact unsecured.
minor comments (1)
  1. [Abstract] Abstract: the phrase “we appear to be less sensitive to polarization because exo-Earths are farther from the IWA” would benefit from an explicit statement of the IWA values adopted in each band and the corresponding planet separation distribution.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful review and constructive comments on our manuscript. We address each major comment below and indicate where revisions will be made to strengthen the presentation of our modeling validation and uncertainty considerations.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central quantitative claim that a 16 m → 12 m barrel change yields ≈10^{-10} contrast at the IWA rests on the unvalidated assumption that the chosen physical-optics package correctly computes the Mueller-matrix aberrations arising from the specific angle-of-incidence map across the shortened EAC-1 optical train; no benchmark against analytic polarization ray tracing, a second code, or a known test optic is described.

    Authors: We acknowledge that the manuscript does not include explicit new benchmarks of the polarization modeling against analytic ray tracing or independent codes. The open-source physical optics package used is a standard tool in the high-contrast imaging community with documented polarization capabilities in its reference materials and prior applications. Nevertheless, to directly address this concern we will add a dedicated validation subsection (or appendix) that compares the computed Mueller-matrix aberrations for simplified angle-of-incidence cases against analytic polarization ray-tracing results and, where feasible, against output from a second independent code. This addition will be incorporated in the revised manuscript. revision: yes

  2. Referee: [Abstract] Abstract (paragraph on linking tools to optimizer): the mapping from modeled contrast to exo-Earth yield statistics is load-bearing for the science-return conclusions, yet the abstract supplies no error budget, sensitivity analysis, or propagation of polarization-model uncertainties through the optimizer, leaving the quantitative yield impact unsecured.

    Authors: The abstract is constrained by length, but the full manuscript already contains sensitivity studies on how contrast variations propagate to yield estimates and discusses the limited range of altruistic optimization. To make this more visible at the abstract level, we will revise the abstract to include a concise statement noting that the reported yield impacts incorporate sensitivity analyses of the contrast-to-yield mapping. We will also ensure the methods section explicitly outlines the uncertainty propagation steps used in the optimizer. revision: partial

Circularity Check

0 steps flagged

No significant circularity; results from external open-source optics tools linked to yield optimizer.

full rationale

The paper's core derivation connects polarization aberrations (computed via open-source physical optics modeling) to exoplanet yields via an optimizer. Reported values such as ≈10^{-10} contrast at IWA for the 12 m barrel are direct simulation outputs, not fitted parameters renamed as predictions, self-defined quantities, or results justified only by self-citation. No load-bearing uniqueness theorems, ansatzes smuggled via citation, or renaming of known results appear. The chain is self-contained against external benchmarks and tools, consistent with the default expectation of no circularity (score 0-2).

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only; no explicit free parameters, axioms, or invented entities are stated. Modeling presumably rests on standard optical-physics assumptions (ray tracing, Jones calculus) not detailed here.

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discussion (0)

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Reference graph

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