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arxiv: 2606.31945 · v1 · pith:M5Z2H65Vnew · submitted 2026-06-30 · 🌌 astro-ph.IM

An overview of stray light findings and interpretation during on-sky commissioning of LSSTCam

Gabriele Rodeghiero , Alex Drlica-Wagner , Alessio Taranto , Luca Rosignoli , Hannah Pollek , Aashay Pai , Lynne Jones , Erin Howard
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Sean MacBride John Andrew Douglas Neill Travis Lange Andrew Rasmussen Aaron Roodman Brian Johnson Elana Urbach Parker Fragelius Eli Rykoff Tomislav Vucina Christopher Stubbs Robert Lupton Charles Claver Joshua Meyers Anastasia Alexov Keith Bechtol Lee Kelvin Brian Stalder Pierre Antilogus Alexandre Boucaud Aurelien Marini Alexander Broughton Leanne Guy Tiago Ribeiro Erik Dennihy Bruno Quint Aaron Watkins Alysha Shugart Lukas Eisert Kevin Fanning Marina Pavlovich Yijung Kang Hye Park Paulo Lago Kristopher Mortensen Paulina Venegas Salas Minhee Hyun Karla Pe\~na Ram\'irez David Sanmartim Shuang Liang Gonzalo Aravena Kshitija Kelkar Kate Napier Jacqueline Seron Navarrete Carlos Morales Mar\'in Danica \v{Z}ilkov\'a Narayan Khadka Eric Christensen Yousuke Utsumi Merlin Fisher-Levine Yusra Alsayyad Colin Slater Fritz M\"uller William O'Mullane Enrico Giro Rodolfo Canestrari Guillem Homar Megias Sandrine Thomas Kevin Reil Roberto Tighe Mario Rivera Juan Lopez Claudio Araya Cortes David Jim\'enez Mej\'ias Hern\'an Herrera Freddy Mu\~noz Arancibia Dimitri Buffat Johan Bregeon Jacques Sebag Holger Drass Pablo Zorzi Massimo Brescia
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Pith reviewed 2026-07-01 02:41 UTC · model grok-4.3

classification 🌌 astro-ph.IM
keywords stray lightwide-field telescopecommissioningray tracingimage artifactsmitigationopto-mechanical systemscattered light
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The pith

The commissioning team built tools to track stray light from discovery through ray-tracing simulation to corrective actions.

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

Wide-field telescopes are hard to shield from stray and scattered light that can contaminate images. This paper describes the dedicated test campaign for one such camera that began at first light. The team developed testing and analysis tools to move artifacts from initial discovery to reproduction in observations, then to ray-tracing simulations that locate their origins in the opto-mechanical system, and finally to corrective actions. A sympathetic reader would care because clean images are required for long-term surveys of dark matter, dark energy, transients, and the Milky Way. The work also supplies practical experience for future wide-field facilities.

Core claim

The commissioning team created a series of testing and analysis tools to track stray light artifacts from their initial discovery through reproduction with timely observations, simulation using ray tracing to identify opto-mechanical origins, and finally devising corrective actions.

What carries the argument

The workflow of observation reproduction, ray-tracing simulation of the opto-mechanical system, and corrective-action development.

If this is right

  • Stray light artifacts can be reproduced with targeted observations and traced to specific opto-mechanical sources.
  • Ray-tracing models can locate the origins of complex contamination patterns in the telescope.
  • Corrective actions developed from the simulations reduce the impact of stray light on images.
  • The encountered features supply lessons for shielding designs in future wide-field telescopes.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If the workflow proves repeatable, similar campaigns could shorten commissioning time for other large telescopes.
  • Data-quality gains from reduced stray light would directly benefit statistical measurements in long-duration sky surveys.
  • Unmodeled scattering mechanisms, if present, would require additional diagnostic observations beyond the current simulations.

Load-bearing premise

Ray-tracing simulations of the opto-mechanical system can reliably identify the physical origins of the observed stray light features without significant unmodeled contributions from other sources.

What would settle it

Implementing the corrective actions derived from the simulations produces no measurable reduction in the stray light features seen in later on-sky images.

Figures

Figures reproduced from arXiv: 2606.31945 by Aaron Roodman, Aaron Watkins, Aashay Pai, Alessio Taranto, Alexander Broughton, Alexandre Boucaud, Alex Drlica-Wagner, Alysha Shugart, Anastasia Alexov, Andrew Rasmussen, Aurelien Marini, Brian Johnson, Brian Stalder, Bruno Quint, Carlos Morales Mar\'in, Charles Claver, Christopher Stubbs, Claudio Araya Cortes, Colin Slater, Danica \v{Z}ilkov\'a, David Jim\'enez Mej\'ias, David Sanmartim, Dimitri Buffat, Douglas Neill, Elana Urbach, Eli Rykoff, Enrico Giro, Eric Christensen, Erik Dennihy, Erin Howard, Freddy Mu\~noz Arancibia, Fritz M\"uller, Gabriele Rodeghiero, Gonzalo Aravena, Guillem Homar Megias, Hannah Pollek, Hern\'an Herrera, Holger Drass, Hye Park, Jacqueline Seron Navarrete, Jacques Sebag, Johan Bregeon, John Andrew, Joshua Meyers, Juan Lopez, Karla Pe\~na Ram\'irez, Kate Napier, Keith Bechtol, Kevin Fanning, Kevin Reil, Kristopher Mortensen, Kshitija Kelkar, Leanne Guy, Lee Kelvin, Luca Rosignoli, Lukas Eisert, Lynne Jones, Marina Pavlovich, Mario Rivera, Massimo Brescia, Merlin Fisher-Levine, Minhee Hyun, Narayan Khadka, Pablo Zorzi, Parker Fragelius, Paulina Venegas Salas, Paulo Lago, Pierre Antilogus, Robert Lupton, Roberto Tighe, Rodolfo Canestrari, Sandrine Thomas, Sean MacBride, Shuang Liang, Tiago Ribeiro, Tomislav Vucina, Travis Lange, William O'Mullane, Yijung Kang, Yousuke Utsumi, Yusra Alsayyad.

Figure 1
Figure 1. Figure 1: From left to right: optical assembly of Rubin with three powered mirrors, three lenses, and one curved [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Non-sequential simulations in Ansys Zemax OpticStudio [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Top-left: Focal plane mosaic image acquired with ComCam during a dedicated stray light test using [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Examples of diagnostic figures for identifying stray light at Rubin Observatory. Left: Rubin-LSSTCam [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Difference Imaging Analysis (DIA) has been utilized for some stray light searches where the sky area [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Image obtained during dawn twilight with the stenopeic (pinhole) technique for imaging the Rubin [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Example of filter transmission profile ( [PITH_FULL_IMAGE:figures/full_fig_p010_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Top: Example of zones of convergence of the light beam found with the backward propagation path, [PITH_FULL_IMAGE:figures/full_fig_p011_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Left: The stray light optical path that generates the [PITH_FULL_IMAGE:figures/full_fig_p012_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Top-Left: The stray light optical path that generates the [PITH_FULL_IMAGE:figures/full_fig_p013_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Left: stray light optical path generated by the M2 baffle, the rays reflected off M1, hit the M2 baffle, [PITH_FULL_IMAGE:figures/full_fig_p014_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Left: close-up view of the L2 side support pad that can generate [PITH_FULL_IMAGE:figures/full_fig_p015_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Left: Stray light optical path for the brush stroke feature, the rays reflected off the M1 and M2 and hit with a grazing angle the outer body of the LSSTCam before being reflected off the M3 and reaching the LSSTCam focal plane. Centre: Example on-sky of the feature highlighted in red generated by Canopus located at 1. ◦9 off-axis. Right: Feature reproduction with the Ansys Zemax OpticStudio® non-sequenti… view at source ↗
Figure 14
Figure 14. Figure 14: The mid-level baffle extension, in orange, (right) led to the dampening of the most prominent stray [PITH_FULL_IMAGE:figures/full_fig_p017_14.png] view at source ↗
read the original abstract

Wide-field telescopes are intrinsically difficult to shield from unwanted stray and scattered light, while the search to identify sources of contaminating light is frequently a challenging task. The Vera C.~Rubin Observatory, which achieved its first photon with the LSST Camera (LSSTCam) on April 15, 2025, will initiate a revolutionary era for the study of dark matter, dark energy, the transient sky, the Solar System, and the Milky Way. LSSTCam will provide near seeing-limited images of the sky in six bands ($u,g,r,i,z,y$) over a $3.^\circ 5$-diameter field of view, and over the course of a decade, it will execute the Legacy Survey of Space and Time (LSST). This work provides an overview of the dedicated stray and scattered light test campaign that has been undertaken since the start of Rubin commissioning. In particular, we highlight the processes used to characterize, model, and mitigate stray light present in LSSTCam images. The Rubin commissioning team created a series of testing and analysis tools to track stray light artifacts from their initial discovery through reproduction with timely observations, simulation using ray tracing to identify opto-mechanical origins, and finally devising corrective actions. The complex stray light features encountered by Rubin provide a wealth of experience for the future wide-field and extremely wide-field observatories. This work covers the many stages of a long journey that started with conceiving an innovative and challenging optical design, followed by the engineering and system engineering efforts to build it, to finally delivering an optimized and revolutionary cutting-edge facility.

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

1 major / 1 minor

Summary. The manuscript provides an overview of the stray light test campaign undertaken during on-sky commissioning of LSSTCam at the Vera C. Rubin Observatory. It describes the development of testing and analysis tools to track artifacts from initial discovery through reproduction via targeted observations, identification of opto-mechanical origins via ray-tracing simulations, and implementation of corrective actions, while noting the broader relevance of these experiences for future wide-field facilities.

Significance. If the workflow and attributions hold, the paper supplies a detailed engineering case study on stray-light management in a complex, wide-field system that is directly relevant to achieving the photometric and image-quality requirements of the LSST. The emphasis on an end-to-end process from observation to mitigation offers transferable lessons for other large-aperture, large-field telescopes.

major comments (1)
  1. [ray-tracing simulation and origin identification] The central claim that ray-tracing simulations identify the opto-mechanical origins of observed stray-light features (abstract and workflow description) is load-bearing yet unsupported by any reported quantitative validation metrics such as pixel-by-pixel residuals, feature-shape correlation coefficients, or sensitivity tests to coating BRDF uncertainties. Without these, alternative explanations (e.g., unmodeled scattering) cannot be ruled out.
minor comments (1)
  1. The abstract would be strengthened by naming at least one concrete stray-light feature and its mitigation outcome to give readers an immediate sense of the results obtained.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful reading and for highlighting the importance of quantitative validation for the ray-tracing results. We address the single major comment below and outline the revisions we will make.

read point-by-point responses

  1. Referee: [ray-tracing simulation and origin identification] The central claim that ray-tracing simulations identify the opto-mechanical origins of observed stray-light features (abstract and workflow description) is load-bearing yet unsupported by any reported quantitative validation metrics such as pixel-by-pixel residuals, feature-shape correlation coefficients, or sensitivity tests to coating BRDF uncertainties. Without these, alternative explanations (e.g., unmodeled scattering) cannot be ruled out.

    Authors: We agree that the manuscript does not report quantitative validation metrics for the ray-tracing identifications. The current text relies on visual feature matching, reproduction via targeted observations, and the outcomes of subsequent mitigations. While these elements provide supporting evidence, they do not constitute the pixel-by-pixel residuals, shape correlation coefficients, or BRDF sensitivity tests requested. We will therefore revise the manuscript to add quantitative comparisons (including feature-shape correlation coefficients for representative cases) and a limited sensitivity analysis to coating BRDF uncertainties where the available data permit. A short discussion of remaining validation limitations will also be included. These changes will be made in the revised version. revision: yes

Circularity Check

0 steps flagged

Descriptive engineering report with no derivations or self-referential predictions

full rationale

The paper is an overview of commissioning activities for stray light in LSSTCam. It describes a workflow of discovery, observation, ray-tracing simulation, and mitigation without any equations, fitted parameters, predictions derived from models, or load-bearing self-citations. No derivation chain exists that could reduce to its inputs by construction. The central claim is a factual report of processes used, not a mathematical result.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

This is a technical overview report of observational findings and engineering processes. It contains no mathematical derivations, free parameters, background axioms, or postulated new entities.

pith-pipeline@v0.9.1-grok · 6182 in / 1034 out tokens · 44539 ms · 2026-07-01T02:41:52.226350+00:00 · methodology

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Reference graph

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