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Conference 14145
Space Telescopes and Instrumentation 2026: Optical, Infrared, and Millimeter Wave
5 - 10 July 2026 | Room B4-M3
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Session 1:
General Topics
5 July 2026 • 09:00 - 10:00 CEST
Session Chair:
Marshall D. Perrin, Space Telescope Science Institute (United States)
14145-1
5 July 2026 • 09:00 - 09:20 CEST
Show Abstract +
We are in the era of large space telescopes, which will transform our understanding of the cosmos. The ambitious James Webb Space Telescope is making infrared observations with unprecedented sensitivity and has exceeded its performance expectations. The Nancy Grace Roman Space Telescope is approaching its launch and science operations, with observational capabilities that will carry out panoramic wide-field infrared surveys. On the horizon, the Habitable Worlds Observatory will directly image Earth-like exoplanets and search their atmospheres for biosignatures. I will describe how each large space telescope mission strategically builds upon the technological foundations of its predecessors, creating synergies to answer some of humanity’s most profound questions. The path from Webb to Roman to HWO illustrates technological progress and an ambitious strategic vision for space astronomy that promises to deliver transformational discoveries for decades to come.
14145-2
5 July 2026 • 09:20 - 09:40 CEST
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This presentation summarizes he Astrophysics Strategic Technology & Research Accelerator (ASTRA) Initiative and discusses, NASA’s progress in executing the Astro2020 Decadal Survey recommendations, and outlines the strategic steps being undertaken to prepare for future strategic astrophysics missions. Support for the community considers previous efforts – including existing concept studies developed for Astro2020, the current global astronomical environment of existing and planned missions, increased industry capability, and technological advances/investments over the past decade. The discussion will highlight the interplay of technological advancements and mission planning essential for future exploration in astrophysics and astronomy and will emphasize the value and criticality of industry and international partnering.
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The Landolt mission is NASA’s first dedicated on-orbit stellar calibration observatory, designed to establish SI-traceable photometric standards for ground- and space-based astronomy. Landolt uses a thermally stable payload "star", NIST-calibrated photodiodes, and an onboard reference light system to measure bright stellar standards above the atmosphere, improving on the dominant source of uncertainty in absolute flux calibration. The mission provides a new celestial flux ladder supporting cosmology, exoplanet transit measurements, and survey uniformity for facilities such as Rubin, Roman, Keck, and JWST. This presentation will describe the mission architecture, calibration chain, contamination-control design, payload development status, and the expected accuracy improvements, along with connections to recent hybrid optical-calibration demonstrations, including ORKID and the LCRD–ORCAS–Keck experiment. Will be presented on behalf of the Landolt Mission Team
Break
Coffee Break 10:00 - 10:30
Session 2:
Exoplanet Time Series I: Operating and Near Future Missions
5 July 2026 • 10:30 - 12:10 CEST
Session Chair:
Tyler D. Groff, NASA Goddard Space Flight Ctr. (United States)
14145-4
5 July 2026 • 10:30 - 10:50 CEST
Show Abstract +
The Pandora SmallSat is a NASA Pioneers mission designed to disentangle stellar activity from planetary atmospheric signatures in transmission spectroscopy observations through simultaneous visible photometry and near-infrared spectroscopy. Pandora’s baseline mission lifetime includes a one-month commissioning period followed by a prime mission period of 12 months for science observations. Herein, we present a comprehensive post-launch mission update, detailing operational performance and current observational strategy. We will also highlight key operational milestones, challenges encountered during commissioning and early science operations, and solutions implemented. This information provides insight into Pandora's on-orbit capabilities for precision multiwavelength observations that enable reliable determination of exoplanet atmosphere compositions.
Show Abstract +
Pandora is a NASA Pioneers smallsat designed to separate stellar activity from exoplanet atmospheric signals using combined visible photometry and NIR spectroscopy. During its prime mission, Pandora is observing 10 transits of each of the 20 carefully selected K- and M-dwarf systems, targeting a variety of exoplanets. In addition to the prime mission, Pandora also observes auxiliary targets with a wider range of science cases, filling scheduling gaps between prime targets. We will present the target selection strategy, scheduling approach, early science results, and possible extended-mission opportunities.
14145-6
5 July 2026 • 11:10 - 11:30 CEST
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PLATO is the M3 class ESA mission dedicated to the discovery and study of extrasolar planetary systems through the detection of planetary transits. The PLATO Payload Camera units are integrated and vibrated at CSL and then TVAC tested for thermal acceptance and performance verification at SRON, IAS and INTA. Fifteen of the twenty six Flight Cameras were delivered to ESA between June 2023 and June 2024. The remaining eleven Flight Cameras and three Flight Spares, two of which completed TVAC testing, were subsequently integrated and verified, completing the campaign.
This paper provides an update following the end of the full camera test programme, with a focus on the later series models. Representative performance results and an overview of the integration and verification flow are presented, together with a final status of the camera population and key observations from carrying out a serial production style test campaign.
Show Abstract +
The Earth 2.0 (ET) mission in China aims to detect over 4,000 Earth-sized planets, including potentially habitable Earth-sized planets around solar-type stars. ET consists of six 28-cm transit telescopes with 550 deg² fields of view and one 35-cm microlensing telescope with a 4 deg² field of view. The transit survey will observe a 550 square degree field centered on the original Kepler field, while the microlensing telescope will monitor the Galactic bulge from an Earth–Sun L2 orbit. The mission will conduct continuous monitoring for four years with a daily downlink data rate of 2,500 Gb. Mission progress will be reported.
Show Abstract +
The Earth 2.0 (ET) mission will deploy a space observatory consisting of six wide-field transit telescopes and one microlensing telescope into a Sun-Earth L2 halo orbit. It aims to perform ultra-wide-field, high-precision photometry to discover exo-Earths and free-floating terrestrial planets, conduct a large-scale census of such planets, investigate their origins, and advance the search for extraterrestrial life. ET’s scientific payload includes a transit telescope array and a microlensing telescope. The transit telescope array consists of six 28cm diameter telescopes with each field of view of 550 square degrees, while the microlensing telescope is a 35 cm diameter telescope with a field of view of 4 square degrees.
Break
Lunch Break 12:10 - 13:10
Session 3:
Exoplanet Time Series II: Ariel
5 July 2026 • 13:10 - 14:50 CEST
Session Chair:
Christopher J. Evans, European Space Agency (United States)
14145-9
5 July 2026 • 13:10 - 13:30 CEST
Show Abstract +
The Ariel space mission will characterize spectroscopically the atmospheres of a large and diverse sample of hundreds of exoplanets. Ariel is an ESA Medium class science mission (M4) with a Payload provided by a consortium of national funding agencies in ESA member states, plus contributions from NASA, the CSA and JAXA. The payload is based on a 1-meter class telescope operated at below 60K, built all in Aluminium, which feeds two science instruments; a multi-channel guider, photometer and low-resolution spectrometer instrument (the FGS) and a medium resolution spectroscopy instrument (AIRS).
This paper provides an overview of the design of the overall payload for the Ariel mission, with a focus on the design updates of the Payload since the payload PDR in 2023, along with the outcomes and lessons learnt from the build of the payload module Structural Model (pSM) in 2025 and the mechanical environmental testing of this pSM in Q1 2026.
Show Abstract +
Ariel will spectroscopically characterise the atmospheres of a large and diverse sample of hundreds of exoplanets. Targets will be selected to cover a wide range of masses, densities, equilibrium temperatures, and host stellar types, enabling the study of the physical mechanisms driving the observed diversity in the known exoplanet population.
Transmission, emission, and phase-curve spectroscopy of transiting exoplanet atmospheres require the detection of very small (<100 ppm) modulations in the signal of bright host stars. The Ariel mission design incorporates three photometers and three spectrometers simultaneously covering the 0.5–7.8 μm band, and implements solutions optimised to achieve the required sensitivity while controlling systematics of both astrophysical and instrumental origin. This contribution reviews the predicted end-to-end performance that will enable Ariel to reach its sensitivity goals and maintain stringent control over systematic effects.
14145-11
5 July 2026 • 13:50 - 14:10 CEST
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Ariel will conduct a survey of the atmospheres of known exoplanets through transit spectroscopy. The Ariel telescope consists of an off-axis, unobscured Cassegrain telescopein the waveband between 0.5 and 7.8 µm, and operating at cryogenic temperatures.It consists of a primary parabolic mirror with an elliptical aperture of 1.1 m of major axis, followed by a hyperbolic secondary, a parabolic recollimating tertiary and a flat folding mirror. In this article, an update regarding the development of the Telescope is provided, focusing on the critical tests and technological developments, in particular: the first measurement of the WFE of a model of M1 at 0 gravity level with nm level precision, thermal conductance measurement of the mechanical interfaces of M1, details regarding the improvement in the Diamond Turning and, finally, an overview at System Level of the development of the Engineering Model of the Telescope Assembly.
Show Abstract +
The Ariel telescope consists of a primary parabolic mirror (M1), followed by a hyperbolic secondary (M2), a parabolic re-collimating tertiary (M3) and a flat folding mirror (M4). Media Lario is the industrial enabler in charge of the manufacturing development of the M1 mirror; made of aluminium 6061-T651, the M1 is an off-axis parabola with a big elliptical aperture having about 1.1 m major axis and 0.75 m minor axis. Among the manufacturing processes, diamond turning is the baseline process to produce the off-axis shape, followed by deterministic polishing in Media Lario and finally coated with protected silver coating by CILAS (France). The results of the development models of the M1 mirror are presented and discussed in this paper.
14145-13
5 July 2026 • 14:30 - 14:50 CEST
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AIRS is the infrared spectroscopic instrument of ARIEL: Atmospheric Remote‐sensing Infrared Exoplanet Large‐survey mission selected as the Cosmic Vision M4 ESA mission. This mission will perform transit spectroscopy of over a 1000 of exoplanets to complete a statistical survey.
AIRS spectroscopic data will cover the 1.95-3.90 µm (Channel 0) and the 3.90-7.80 µm (Channel 1) wavelength ranges with dispersive elements producing spectrum of low resolutions R>100 in channel 0 and R>30 in channel 1. This instrument overview will mainly cover the avionic and Engineering Models. It will present updated information on the integration and testing activities which thus conduct to start the realization of the flight model.
Break
Coffee Break 14:50 - 15:20
Session 4:
Exoplanet Time Series III: New Concepts
5 July 2026 • 15:20 - 16:00 CEST
Session Chair:
Laura E. Coyle, BAE Systems, Inc. (United States)
14145-14
5 July 2026 • 15:20 - 15:40 CEST
Show Abstract +
We present a modified HgCdTe detector-based laboratory demonstration of an ultra-stable mid-IR array spectrometer for exoplanet transits. The instrument includes a calibration system that enables the 1/f stability required for the detection of atmospheric bio-signatures in habitable-zone planets around M-dwarfs. We have already demonstrated the required stability of 5 ppm with Transition Edge Sensors (TES) over days in an identical spectrometer. However, TES require sub-K cooling. In 2019 Cabrera et al. demonstrated a long-wavelength cut-off of 16.7 μm for a new HgCdTe-based detector, and Mandell et al., 2022, demonstrated that this long-wavelength cutoff would be sufficient to measure surface temperature, radius, and multiple atmospheric tracers. We use this particular array in our demonstration. Here, we provide an overview of the testbed and present first results from ongoing tests and compare these to the performance we achieved with TES detectors.
14145-15
5 July 2026 • 15:40 - 16:00 CEST
Show Abstract +
Exoplanet atmospheric dynamics are best probed with spectroscopic phase curves, which measure how a planet’s flux changes with longitude and orbital position to reveal heat transport. Linked properties—temperature, pressure, winds, composition, and stellar irradiation—shape clouds, hazes, and the hottest and coldest regions. Hot Jupiters, with periods under ~10 days, provide ideal laboratories for atmospheric studies, but current missions cannot obtain full phase curves for planets with periods >5 days. The Multi Telescope Hot Jupiter Survey (MiTHOS), a SMEX-class concept, will address this gap using a constellation of small satellites carrying identical spectrometers spanning 0.5–5 μm. MiTHOS will gather phase curves for over 80 hot Jupiters and use shared calibration stars to remove instrument-specific systematics. Here, we present updated optical designs and throughput estimates demonstrating MiTHOS’s ability to resolve key questions in atmospheric dynamics.
Session 5:
Innovative Optics from Small to Large Missions
5 July 2026 • 16:00 - 17:40 CEST
Session Chair:
Dmitry Savransky, Cornell Univ. (United States)
14145-16
5 July 2026 • 16:00 - 16:20 CEST
Show Abstract +
CubeSpec is an in-orbit demonstration CubeSat mission in the ESA technology programme, developed and funded in Belgium. The programme is now in phase C/D. Environmental qualification is finalising and building, testing and verification of the spacecraft and payload flight model has started. The project is on track for launch readiness end 2026. We present the final design of the mission and the results of test of engineering, qualification and flight models.
CubeSpec will measure high-resolution time series of spectral line profiles in massive stars to probe their internal structure. This requires a spectral resolution R > 50,000 (~0.01 nm) and SNR ≥ 200.
CubeSpec features several technological innovations: a 3-axis fine steering mirror bringing arcsecond level line-of-sight stability, a compact optical payload with fully ceramic 10x20cm cassegrain telescope, a cross-dispersed echelle spectrograph, compact FPGA CMOS sensor readout and a deployabe sun shade.
14145-17
5 July 2026 • 16:20 - 16:40 CEST
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The Line Imaging Orbiter for Nanosatellite-Enabled Spectrographic Surveys (LIONESS) is a 6U CubeSat carrying a microlens-based narrowband integral field spectrograph payload. LIONESS stands to greatly improve our understanding of the circumgalactic medium (CGM), conducting high signal-to-noise observations by leveraging the low sky background in orbit. LIONESS observes the prominent Hα emission line, dispersing narrowband spectra. It aims to locate the missing baryons surrounding galaxies and map the gas kinematics in the CGM. The LIONESS spectrograph utilizes a retro-reflective Offner relay design, with the convex mirror replaced with a convex grating operating near-Littrow. A crucial benefit of this design is its small footprint, keeping the optical components within the packaging of a nanosatellite, and decreasing reflective surfaces that could lose crucial photons. We will discuss this design, the incorporation of new technologies, and its application to future space missions.
14145-18
5 July 2026 • 16:40 - 17:00 CEST
Show Abstract +
This paper presents the advancement of the miniaturized optical telescope assembly (OTA) for exoplanetary astronomy and development of an ultra-sensitive detector system compatible with small satellite constraints. The test results have shown that the OTA achieves low PSF variations across wavelength and temperature ranges over a wide field enabling precision photometric observations of exoplanet transits candidates. The imaging performance and sensitivity of a compact detector compare favorably to that of ground-based Electron Multiplying CCD (EMCCD) and Complementary Metal-Oxide-Semiconductor (CMOS) imaging systems.
14145-19
5 July 2026 • 17:00 - 17:20 CEST
Show Abstract +
The Chinese Space Station Telescope (CSST) is a space-based observatory equipped with a 2-meter astronomical telescope. It is scheduled for launch in 2027. The Optical Telescope Element (OTE) of the CSST is a 2m off-axis three-mirror anastigmat optical system, whose field of view (FOV) is 1.1°×1°. The optical alignment poses a key difficulty for the OTE, due to the combination of non-parallel optical axes of all the three mirrors and the use of a freeform surface for the tertiary mirror. Whole-process deterministic optical alignment has been achieved successfully. The 2-meter-diameter primary mirror and the 4-meter main substrate were integrated with high precision, achieving an angular error of less than 10 arcseconds and a positional error under 0.05 mm. After integration and alignment, the OTE was tested in a vacuum chamber. The average RMS wavefront error over full FOVs was measured to be 0.074λ at 632.8 nm.
14145-20
5 July 2026 • 17:20 - 17:40 CEST
Show Abstract +
Lightweight mirror blanks for space applications must balance volume, weight, and stiffness to enable effective thermomechanical performance within rocket transport space restrictions. Closed back mirrors enable optimal performance at smaller overall Volume and reduced weight. Bonding the back with adhesives might affect the thermomechanical stability of the mirror.
SCHOTT has recently presented closed back ZERODUR® mirror blanks produced with adhesive-free fusing on 480 mm diameter scale. The quality of the fused interface enables a high degree of strength and almost monolithic quality in terms of stress birefringence and CTE homogeneity.
Meanwhile the technology moved forward on the path of maturing, being upscaled to almost meter sized structures and further characterization of properties.
This paper gives an update on the development of adhesive-free fusing of ZERODUR® structures with a focus on light weight closed back mirror blanks.
Monday Plenary
6 July 2026 • 08:30 - 10:00 CEST
Join us for the Monday plenary session.
Break
Coffee Break 10:00 - 10:30
Session 6:
JWST
6 July 2026 • 10:30 - 11:50 CEST
Session Chair:
Marshall D. Perrin, Space Telescope Science Institute (United States)
Show Abstract +
The James Webb Space Telescope (JWST) has achieved spectacular success as an infrared space observatory, marking a new era in astrophysics and planetary science. JWST developed many new technologies and was the first to demonstrate segmented-telescope wavefront sensing in space, providing a path to even larger space telescopes. The observatory's performance has exceeded expectations, delivering unprecedented infrared sensitivity. The science mission has transformed our understanding of the early universe, exoplanet atmospheres, stellar formation, and galaxy evolution. The lessons learned from its design, deployment, and operations provide key insights for the development and implementation of next-generation space telescopes and astronomical instrumentation. This presentation will report on the JWST prime mission highlights and its lasting legacy for space science.
14145-22
6 July 2026 • 10:50 - 11:10 CEST
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The James Webb Space Telescope (JWST) offers unprecedented near-infrared sensitivity and stability, enabling time-series observations (TSO) of bright targets. The NIRCam Dispersed Hartmann Sensor (DHS) introduces a new short-wavelength spectroscopic mode, producing up to 8 spatially-separated spectra per source at R~300, and extending coverage down to 1 μm. This new mode will enable spectroscopy of targets as bright as magnitude 3, opening access to high precision studies of bright stars, transiting exoplanets, and any variable high-flux sources. Up-coming calibration efforts will establish flux and wavelength solutions, evaluate saturation and sensitivity limits in combination with the long-wavelength channels (2.4-5 μm), and define optimal procedures for TSO. This presentation will summarize instrument performance, expected calibration results, and guidelines to help the community exploit this new DHS mode for bright-target time-series spectroscopy, once integrated on-board NIRCam.
Show Abstract +
Massively multiplexed spectroscopy enables efficient, statistically robust surveys of large cosmic volumes. Space-based wide-field slitless spectroscopy reduces cosmic variance by covering extensive sky areas with consistent sensitivity and calibration. In Cycle 5, JWST introduced a new MIRI prime observing mode—Wide Field Slitless Spectroscopy (WFSS)—which utilizes the P750L double prism to deliver low-resolution (R ~ 100) spectroscopy from 5 to 14 μm across an unobstructed 74″ × 113″ field of view. We present the MIRI WFSS calibration plans and their expected accuracy. We utilized established slitless-spectroscopy techniques from HST and JWST, archival P750L and MIRI imaging data, and dedicated calibration observations for flux/trace and wavelength calibration, including adjustments for positional dependencies. We present the most recent calibration reference files used for flat-fielding, background subtraction, and flux and wavelength calibration, and outline improvement plans.
14145-24
6 July 2026 • 11:30 - 11:50 CEST
Show Abstract +
The limiting noise floor in almost all coronagraphic observations is from uncertainty in the field of speckles around a bright star, in which optical aberrations can easily hide a faint planet. Data-driven methods for subtracting this field have been very successful, but the exquisite precision of the James Webb Space Telescope instruments implies much deeper fundamental contrast and resolution limits than are routinely being achieved. Recent advances in differentiable optics models and machine learning have made it possible to simulate and perform phase retrieval on the optical system end-to-end, trained on science data, and provide much more accurate predictive models of the speckle field in the James Webb NIRISS Interferometer. We present the early results of adapting these methods to the NIRCam coronagraph, achieving improvements in wavefront sensing and metrology and a path to deeper coronagraphy with JWST and other space telescopes.
Break
Lunch Break 11:50 - 13:00
Session 7:
Wide Field I: SPHEREX and Roman
6 July 2026 • 13:00 - 15:00 CEST
Session Chair:
Jeanette L. Domber, BAE Systems, Inc. (United States)
14145-25
6 July 2026 • 13:00 - 13:20 CEST
Show Abstract +
The SPHEREx space telescope is the newest NASA MIDEX mission, designed to study the Universe’s large-scale structure, probe the history of galaxy formation, and survey our Milky way for water and other biogenic ices. Full scale science operations began on May 1st, 2025 and two NIR spectroscopic surveys of the entire celestial sphere have been completed in the intervening year. In this update, we present the observatory’s operational status, instrumental performance and demonstrated sensitivity on-sky. The entirety of the spectral image data from these novel surveys will be made available to the community, with initial releases already available for public access.
Show Abstract +
SPHEREx is the all sky near infrared survey launched on March 11 of 2025. We began full sky survey operations on May 1 of 2025 following two months of in orbit commissioning. The mission is designed to map the entire sky in 102 colors from 0.75 to 5 microns four times during the two year planned survey. In this talk I will describe the launch and in orbit commissioning activities. I will then provide an update on the performance of our calibrations and the current observation status. I will also show several examples of the science enabled by the early SPHEREx data release.
14145-27
6 July 2026 • 13:40 - 14:00 CEST
Show Abstract +
The Nancy Grace Roman Space Telescope (“Roman”) is NASA’s next flagship observatory. Launching in 2026, Roman will explore the nature of dark energy as well as expand the census of exoplanets in our galaxy via microlensing. Roman’s large field of view, agile survey capabilities, and excellent stability enable these scientific objectives, yet present unique challenges for the design, test, and verification of its optical system. Roman recently completed a comprehensive thermal vacuum test of the Spacecraft bus + Integrated Payload Assembly (SCIPA), followed by integrating the Outer Barrel Assembly (OBA), Solar Array Sunshield (SASS), and Deployable Aperture Cover (DAC) with SCIPA to complete the Observatory. This paper will present an overview of the thermal vacuum optical testing as well as a status of the optical system performance and verification.
Show Abstract +
The Roman Space Telescope is a three-mirror anastigmat design with a 2.4 m primary mirror, which will provide science information on dark energy and exoplanets via two science instruments. The Optical Telescope Assembly (OTA) collects and conditions light for both the Widefield Instrument (WFI) and Coronagraph Instrument (CGI). Optical stability is a critical performance aspect of the OTA that enables the science objectives of both instruments. The program prioritized optical stability from the beginning through to final delivery, encompassing requirements, design, analysis, model validation, testing, and verification. After completing final optical testing and shipping the OTA to Goddard Space Flight Center in November 2024, final predictions for on-orbit optical stability were made. The OTA is expected to far exceed its optical stability requirements, with analysis predicting sub-nanometer stability over several days.
14145-29
6 July 2026 • 14:20 - 14:40 CEST
Show Abstract +
The Wide Field Instrument (WFI) on NASA’s Nancy Grace Roman Space Telescope was delivered to Goddard Space Flight Center in the summer of 2024 from its testing at BAE Systems Space & Mission Systems in Boulder, Colorado. This paper will describe the development and qualification process of the Cold Module, which consists of a hexapod adjustment mechanism for the focal plane, an optical element select mechanism, the optical metering support structure within WFI, and the two-stage cooling system. The co-development process with Goddard Space Flight Center will be reviewed. The phases of the development, from requirements, design, build, subsystem test, and final integrated instrument test will be discussed. Finally, a summary of challenges and solutions will be reviewed.
14145-30
6 July 2026 • 14:40 - 15:00 CEST
Show Abstract +
Primary science goals of the Roman Space Telescope include measuring the growth and geometry of the universe and developing constraints on dark energy models via complementary cosmological probes of BAO and Type Ia supernova. The Roman Space Telescope will achieve this by employing slitless spectrographs to conduct a high latitude spectroscopic survey using a near-IR grism assembly (1.0-1.93 µm, R = 435−865) and a high latitude time domain survey using a near-IR prism assembly (0.75-1.8 µm, R = 100–180). This publication covers aspects of the optical assembly designs and how the basic Roman science objectives drive the formulation and verification of the hardware’s key and driving technical performance requirements. We describe the calibration and optical metrology methods for determining assembly wavefront error, dispersion, throughput, and bandpass edge characterization. We demonstrate how the Roman Grism and Prism spectrograph designs and as-built performance meet expectations.
Break
Coffee Break 15:00 - 15:30
Session 8:
Exoplanet Imaging I: Roman and Near Future Missions
6 July 2026 • 15:30 - 17:30 CEST
Session Chair:
Dmitry Savransky, Cornell Univ. (United States)
14145-31
6 July 2026 • 15:30 - 15:50 CEST
Show Abstract +
The Coronagraph Instrument onboard the Nancy Grace Roman Space Telescope serves as a crucial technology pathfinder for the Habitable Worlds Observatory, with on-sky verification of high-contrast imaging techniques and the potential to image a Jupiter analog for the first time. Together with the Roman Project Team, the Community Participation Program (CPP) is responsible for target selection, preparatory observations, developing an exposure time calculator, target database, data reduction pipeline, simulation tools, and engagement with the broader community. Here we present an overview of the CPP activities over the past two years with an emphasis on observation planning activities for the initial in-orbit checkout and the first six months of the observation phase. Finally, we present future opportunities for the astronomical community to interact with the data as it becomes public early in the mission.
14145-32
6 July 2026 • 15:50 - 16:10 CEST
Show Abstract +
The upcoming Roman Coronagraph aims to directly image and characterize exoplanetary systems at contrasts higher than 10^-7, a key technological milestone for Habitable Worlds Observatory coronagraph development. Doing so requires alternating observations of science targets and bright reference stars. These reference stars must satisfy strict criteria, including being single star systems. Other reference star attributes may have other impacts on post-processing performance on a case-by-case basis. Only a small number of the brightest stars in the sky are potentially suitable, necessitating precursor observations and simulations to validate their use. We will present the pre-launch list of Roman Coronagraph reference stars informed from an extensive observing campaign. We will also present the results of simulations investigating the impact of reference star properties on post-processing performance. We discuss the importance of reference star selection for scheduling and performance.
14145-33
6 July 2026 • 16:10 - 16:30 CEST
Show Abstract +
The Coronagraph Instrument, technology pathfinder, is ready to fly onboard the Nancy Grace Roman Space Telescope, a NASA flagship mission scheduled to launch before the Spring 2027. The Community Participation Program (CPP) is building a comprehensive observing program for the “Coronagraph” with preparation, calibration and data processing software. Here we describe a sub-program that could be carried out as soon as the instrument is operational and high-order wavefront sensing and control has been exercised successfully. This program would generate the first canonical on-sky dataset of a bright star with an easily recoverable self luminous companion. We show all preparation steps using the whole suite of tools developed by the CPP. This “training” dataset will be precious for the readiness of the technology demonstration at higher contrasts and for our community to subsequently tackle more difficult targets, including giant exoplanets in reflected light.
14145-34
6 July 2026 • 16:30 - 16:50 CEST
Show Abstract +
The Roman Space Telescope Coronagraph Instrument will demonstrate a series of technologies and techniques to enable the direct detection of reflected-light planets with space-based observatories. To characterize and validate the performance of the Coronagraph Instrument, the Community Participation Program is developing corgidrp, an open-source Python-based data reduction pipeline. The pipeline can process data from the required and best-effort observing modes and their associated calibration sequences. We present the software design and implementation of corgidrp. We describe the software architecture, data flow, processing steps, automation tools, testing framework, and development philosophy. We will also outline future development plans in preparation for on-sky data.
14145-35
6 July 2026 • 16:50 - 17:10 CEST
Show Abstract +
With over 6200 exoplanets discovered, none Earth-twin has been confirmed. The high-contrast imaging can directly detect the photons from the planet itself, thus open the window for spectroscopy of the atmosphere of the planet, which is crucial to answer “Are we alone in the universe?”. However, the direct imaging technique remains challenge, due to the larger flux ratio contrast and its location very close to the primary star. In this talk, I will introduce progress & scientific goals of CPI-C on CSST, which is dedicated for the high-contrast imaging and characterization of the “COOL” planet. Meanwhile, I will make a brief introduction of the next generation flagship space program of ELSE (Extraterrestrial Life Signal Explorer), which will focus on the direct imaging & spectroscopy of the Earth-mass exoplanets in the HZ of a solar type star, one of the most significant sciences of human beings in this new era.
Show Abstract +
The Lazuli Space Observatory is a 3m space observatory designed for rapid-response observations and precision astrophysics across optical and near-infrared wavelengths. An off-axis telescope delivers diffraction-limited image quality to three instruments: 1) The Widefield Context Camera (WCC), capable of high-cadence multi-band imaging. 2) The Lazuli Integral Field Spectrograph (IFS), capable of precise spectrophotometry across 400-1700nm at a resolution of R~100-500. 3) The ExtraSolar Coronagraph (ESC), providing high-contrast imaging expected to reach raw contrasts of 1e-8 and post-processed contrasts approaching 1e-9. Operating from a 3:1 lunar-resonant orbit, Lazuli will respond to targets of opportunity in under 4 hours. Lazuli is conceived as a general-purpose facility capable of supporting a wide range of astrophysical investigations with open time for the global community. We describe the observatory architecture and its capabilities in the preliminary design phase.
Tuesday Plenary
7 July 2026 • 08:30 - 10:00 CEST
Join us for the Tuesday plenary session.
Break
Coffee Break 10:00 - 10:30
Session 9:
Astrometry and Interferometry
7 July 2026 • 10:30 - 11:50 CEST
Session Chair:
Sylvestre Lacour, Observatoire de Paris à Meudon (France)
14145-37
7 July 2026 • 10:30 - 10:50 CEST
Show Abstract +
The detection of exoplanets by way of astrometric monitoring of the host star to reveal gravitational reflex motion requires extreme precision in measurement stability for Earth-mass objects. Despite this, astrometry is widely regarded as the most promising technology for the most desired of all targets: true Earth analogues in the solar neighbourhood. Formerly thought to require flagship class investment, recently several smaller concepts such as the TOLIMAN and SHERA missions have shown that detections are possible, at least in principle, from more modest space platforms. A key enabling feature of these missions is narrow-angle astrometry: a binary star provides its own astrometric reference greatly alleviating problems from using distant, faint field stars. However, few nearby star systems are multiple. This paper advances novel optical concepts featuring ultra-stable telescopes of modest (<0.5m) aperture for micro-arcsecond monitoring of isolated single stars.
14145-38
7 July 2026 • 10:50 - 11:10 CEST
Show Abstract +
We are promoting conceptual design and the validation study of the telescope on board the Japan Astrometry Satellite Mission for INfrared Exploration (JASMINE). Precise correction of image distortion, which is a key technical challenge for astrometry, may be complicated by the time variation of point spread function centroids caused by thermal deformation of the telescope due to changing thermal condition in orbit. To assess this effect, we conducted a Structural Thermal Optical Performance analysis.
After correcting image shifts and magnification changes, the time variation of the distortion in the second or higher orders was found to be approximately 1 nm RMS, corresponding to 50 μarcsec RMS in position angle. The time stability is insufficient to achieve the mission requirement of annual parallax estimation with a precision better than 40 μarcsec. This demonstrates the necessity of the correction of time-varying distortions in the second order during post processing.
14145-39
7 July 2026 • 11:10 - 11:30 CEST
Show Abstract +
The French contribution to the LISA Consortium, particularly on the instrumental side, focuses on developing Optical Ground Support Equipment (OGSE) to validate LISA’s performance before launch. More specifically, part of the French community’s mandate is to test and qualify the performance of the Interferometric Detection System (IDS).
The IDS Test Set-Up is currently being developed to verify that picometer-level stability is achieved within the IDS and to characterize the TTL (tilt-to-length) coupling coefficients of the Optical Bench (OB) interferometers (the coupling between the relative angular misalignment of the beams and the interferometric length readout).In this contribution, I will briefly present the operating principles of the overall IDS Test Set-Up.
14145-40
7 July 2026 • 11:30 - 11:50 CEST
Show Abstract +
We introduce the NASA-funded mission STARI (STarlight Acquisition and Reflection toward Interferometry), a two-spacecraft technology demonstrator for future long-baseline interferometers. STARI will perform, to our knowledge, the first in-space transfer of starlight between free-flying spacecraft, a critical step toward kilometer-scale missions. Two propulsive 8U CubeSats in low Earth orbit will fly in formation with separations up to 100 m: one relays a narrow stellar beam to the other, where an off-axis parabola reimages it into a single-mode fiber. Using differential GPS, visible LED beacons, and fast-steering mirrors in closed loop, we aim to sustain diffraction-limited, high-throughput fiber coupling during formation flight. STARI, targeting launch in 2029, is designed to retire key optical and control risks for missions such as the Large Interferometer for Exoplanets (LIFE) that seek to detect atmospheric biomarkers on nearby Earth-like exoplanets.
Break
Lunch/Exhibition Break 11:50 - 13:00
Session 10:
Solar System
7 July 2026 • 13:00 - 15:00 CEST
Session Chair:
Anamparambu N. Ramaprakash, Inter-Univ. Ctr. for Astronomy and Astrophysics (India)
14145-41
7 July 2026 • 13:00 - 13:20 CEST
Show Abstract +
The VenSpec spectrometer suite aboard the EnVision mission to Venus is composed out of three spectrometers that will gather data on various coupled phenomena on our sister planet from the surface to the upper atmosphere. The combined technical system will be able to observe Venus at a variety of wavelengths from UV to IR and will map surface composition and variations in various mesospheric and tropospheric gasses that will enable the common science team to study the coupling between the Venusian surface and atmosphere and enable a comprehensive search for volcanic activity. This paper presents an overview and top-level comparison of the instruments including their common Central Control Unit that provides the electrical interface to the spacecraft. A technical budget overview and key parameters of each unit will be shown. The different design drivers for the different units will be explained, and the particularities of the EnVision mission and their impact on the project delineated.
14145-42
7 July 2026 • 13:20 - 13:40 CEST
Show Abstract +
The concept of the optical objective of the VEM instrument (Venus Mapper under DLR responsibility for VERITAS and EnVision missions) will be shown with the first results of its measured performances.
Academic partners (LIRA and DLR) are associated with industrial partners (Bertin-Winlight, Cilas and MECANO-ID) with the CNES support.
Robust design with 3 lenses and filter all integrated in a mechanical barrel has successfully passed the first review.
The mechanical models and FEA results will be presented.
The whole qualification process and the facilities developed at LIRA will be exposed.
14145-43
7 July 2026 • 13:40 - 14:00 CEST
Show Abstract +
The ACS-NIR spectrometer on TGO (Trace Gas Orbiter) is still being used to probe the Martian atmosphere in the infrared. The solar spectrum can be obtained when the ACS-NIR line-of-sight is above the Martian atmosphere, that is when it is pointed directly at the Sun. This solar spectrum serves as a reference for spectra acquired through the atmosphere and for spectral calibration. The processing chain of the diffraction orders of ACS-NIR must be efficient to construct a high-quality solar spectrum across the entire spectral domain of the instrument. Therefore, calibration data have been recorded for this purpose. This paper first presents ACS-NIR then the calibration data. It then explains how these data are used to develop new techniques for estimating the flat-field and stray light matrices for ACS-NIR. Finally, the paper describes how the spectral contamination matrix is obtained and then used to reconstruct the spectral bands of diffraction orders from those of their neighbors.
14145-44
7 July 2026 • 14:00 - 14:20 CEST
Show Abstract +
The paper introduces the PANCAM Vision System, an integrated panoramic imaging and processing platform designed for future planetary exploration. Developed within the framework of the NewSpace era, the system prioritizes the use of Commercial Off-The-Shelf (COTS) components to minimize size, mass, and power without sacrificing scientific precision. Despite using commercial parts, the system undergoes strict Radiation Hardness Assurance through software simulation (extensive software modelling of particle fluxes and radiation effects (irradiation dose, single event effects) and heritage analysis (Evaluation of component production stability and prior space heritage). The PANCAM Vision System demonstrates that by applying precise engineering and rigorous qualification to COTS technology, space missions can achieve the cost and efficiency benefits of the NewSpace paradigm while maintaining high-level scientific capability.
14145-45
7 July 2026 • 14:20 - 14:40 CEST
Show Abstract +
We aim to obtain two-dimensional, spatially resolved infrared spectra for compact planetary and small-satellite missions. To meet this goal, we developed an imaging FT-IR spectrometer that uses wavefront-division Fourier interferometry and Zernike freeform mirrors. The instrument covers 4–20 µm with 3.8 cm^-1 wavenumber resolution and 34 µm spatial resolution. An uncooled mid-infrared camera records an interferogram and a spectrum at each pixel, so a full 2D spectral map is acquired in one scan. Extended sources reduce spatial coherence and wash out the fringes. We address this by placing a slit-array Wavefront Pre-Selection Mask module (WPSM) at the entrance plane. The WPSM raises the center-burst amplitude of 50 and nearly doubles the fringe contrast. A 960 cm^-1 quantum cascade laser test shows a mean wavenumber offset of 0.05 cm^-1, and polystyrene standard data agree with catalog spectra, showing that this system can provide accurate 2D infrared spectra.
14145-46
7 July 2026 • 14:40 - 15:00 CEST
Show Abstract +
We are planning a new concept OPENS (Outer Planet Exploration by Novel Small Spacecraft) program that will explore the outer planet region with a series of small spacecraft in a shorter development time and at a lower cost than legacy spacecraft. OPENS-0, which was selected as a JAXA Eco & Fast Class candidate, is a technology demonstration mission to Saturn. During its cruise phase, OPENS-0 will provide astronomical science opportunities, including observations of the ZL, EBL, and other diffuse background light, using onboard multipurpose cameras. This paper presents an overview of the OPENS-0's instruments and scientific objectives, as well as an introduction to the OPENS program.
Break
Coffee Break 15:00 - 15:30
Session 11:
Wide Field II
7 July 2026 • 15:30 - 17:30 CEST
Session Chair:
Frank U. Grupp, Univ.-Sternwarte München (Germany)
14145-47
7 July 2026 • 15:30 - 15:50 CEST
Show Abstract +
CuRIOS-ED (CubeSats for Rapid Infrared and Optical Surveys–Exploration Demo) is an optical imaging payload launching on a 12U CubeSat in June 2026 as the first technology demonstration for the CuRIOS constellation concept. The payload uses commercial components, including an Atik apx60 camera with a Sony IMX455 detector. CuRIOS-ED was fully integrated into the spacecraft in November 2025. In addition to camera-level characterization, we performed system-level thermal testing of the CuRIOS-ED payload to quantify thermal gradients and detector cooling behavior under flight-like conditions.
In this talk, we present the expected on-orbit performance of CuRIOS-ED based on these measurements, including predicted noise and thermal stability. Additionally, we outline the commissioning plan and expected science returnables. Early telemetry and images—if available—will be used to validate estimates and demonstrate the viability of low-cost CMOS imagers for future survey missions.
Show Abstract +
The Reionization Explorer, REX, is a mission concept to map the progress of cosmological reionization using the interaction of (redshifted) Lyman alpha light with intergalactic gas.
REX will use a wide-area near infrared camera with unique narrow-bandpass filters to identify the youngest, most actively star forming galaxies at cosmic dawn through Lyman alpha line emission.
Lyman alpha is the strongest emission line of hydrogen, and is resonantly scattered by neutral hydrogen. REX will map neutral and ionized intergalactic gas through the spatial distribution of Lyman alpha sources.
REX's baseline survey is 100 deg^2 in eight narrowband filters with central wavelengths from 0.97 to 1.46 microns, corresponding to redshifts 7-11 for Lyman alpha. This survey will have many other applications, including time domain astrophysics, galaxy evolution, interstellar medium studies, and outer solar system bodies. Still more is possible by using REX hardware for additional observations.
14145-49
7 July 2026 • 16:10 - 16:30 CEST
Show Abstract +
GREX-PLUS (Galaxy Reionization EXplorer and PLanetary Universe Spectrometer) is one of the two candidates of ISAS/JAXA's Strategic L-class mission for 2030s. The 1.0m, 50 K cryogenic telescope will have a wide-field camera (WFC) of 0.5 square degree field-of-view in the 2-8 micron wavelength band. An optional high resolution spectrometer (HRS) with a wavelength resolution of 30,000 in the 10-18 micron band is also under discussion. The WFC field-of-view is 200 times larger than that of the James Webb Space Telescope. Since the wavelength coverage of the similarly wide-field imaging telescopes of Euclid and Roman is limited to less than ~2 micron, the GREX-PLUS coverage of the wavelength longer than 2 micron is complementary and unique. The spectral resolution of the HRS is 10 times higher than that of the James Webb Space Telescope, opening a new window of the mid-infrared high resolution spectroscopy from space. I will present the latest status of the concept study of GREX-PLUS.
14145-50
7 July 2026 • 16:30 - 16:50 CEST
Show Abstract +
The VERTECS mission aims to measure the visible Extragalactic Background Light (EBL), whose near-infrared brightness exceeds the integrated galaxy light by several factors, suggesting contributions from early-universe sources and intrahalo stars. VERTECS employs a 6° × 6° wide-field telescope with four-band photometry from 400–800 nm, a low-dark-current CMOS sensor, and a 3U bus equipped with the XACT-15 attitude control system, deployable solar panels, and a high-speed X-band transmitter. Developed under the JAXA-SMASH program since 2022, we are conducting its flight-model assembly and ground verification tests in 2025. End-to-end communication tests, long-duration tests, thermal-vacuum cycles, and initial-phase contingency tests confirmed system functionality, with several issues identified and corrected during verification. VERTECS is scheduled for launch on H3 Launch Vehicle No. 6, with all preparations for flight and operations planned for completion by March 2025.
14145-51
7 July 2026 • 16:50 - 17:10 CEST
Show Abstract +
SIRMOS is a concept for a NASA Astrophysics MIDEX mission designed to revolutionize our understanding of cosmic inflation, dark energy, and neutrino masses by mapping the large-scale structure of distant galaxies with unprecedented breadth and precision. Leveraging the expansive Euclid imaging covering ~14,000 sq deg, SIRMOS will obtain slit spectra for 100 million galaxies at redshifts from 1 to 4 using a powerful multi-object spectroscopy capability enabled by a 2K×1K Digital Micro-mirror Device (DMD) as described in Robert Content's accompanying paper on the optical design. SIRMOS uniquely exploits Euclid’s deep near-infrared catalog for efficient target selection, collecting high-precision spectra (R>1000) with continuous wavelength coverage from 1.25-2.5 microns to eliminate gaps in redshift measurements and minimizes systematic biases. By leveraging heritage bus and thermal designs, SIRMOS offers a cost-effective path to crucial cosmological measurements.
14145-52
7 July 2026 • 17:10 - 17:30 CEST
Show Abstract +
HiZ-GUNDAM aims to explore the early Universe and advance multi-messenger astrophysics through rapid detection of gamma-ray bursts (GRBs). The MONSTER near-infrared telescope performs five-band imaging from 0.5 to 2.5 µm of GRBs detected by the wide-field X-ray monitor EAGLE and provides photometric redshifts. To ensure high sensitivity, the telescope body and HgCdTe detector must be cooled below 200 K and 120 K by radiative cooling. After GRB detection, the satellite slews toward the GRB, increasing thermal input. We evaluated the thermal worst-case condition, defined as the attitude with maximum heat load at the hottest point, and established a method to compute satellite attitude using rotation matrices based on the Sun’s right ascension and declination. Thermal analysis shows that even in the worst case, the telescope body and detector remain at 171 K and 106 K. In this presentation, we report the development and thermal assessment of the MONSTER telescope onboard HiZ-GUNDAM.
Wednesday Plenary
8 July 2026 • 08:30 - 10:00 CEST
Join us for the Wednesday plenary session.
Break
Coffee Break 10:00 - 10:30
Session 12:
Exoplanet Imaging II: From JWST Towards HWO
8 July 2026 • 10:30 - 12:10 CEST
Session Chair:
Christopher J. Evans, European Space Agency (United States)
14145-53
8 July 2026 • 10:30 - 10:50 CEST
Show Abstract +
NASA’s Astrophysics Division features multiple solicitations to fund technology development for future space flight missions. We will present the paradigm used in these solicitations, a compare-and-contrast between the two, and the process for how technologies have been prioritized for inclusion in the SAT opportunity. We have statistics on selections, including groupings by subject matter and how these have evolved over time. Our focus is on the open APRA and SAT programs, and we will also cover the intramural funding for technology development. Over the years, several selected proposals have led to technologies which have been infused into later flight missions. There are now shifting approaches being used to emphasize technology development for the Habitable Worlds Observatory We will discuss anecdotal aspects of NASA’s technology innovation, maturation, and flight pipeline, and how it supports early-career researchers.
14145-54
8 July 2026 • 10:50 - 11:10 CEST
Show Abstract +
The Habitable Worlds Observatory (HWO) aspires to answer a broad range of key questions in astronomy, including whether life exists beyond Earth. In the global sustainability context of the 2030s and 2040s, the credibility and impact of a space mission will also depend on demonstrating responsibility to the only habitable world we know.
We present a framework to integrate the environmental dimension of sustainability into early HWO development by tracking the carbon footprint of mission activities and treating a carbon budget as a formal engineering constraint, integrated with traditional budgets (e.g. mass, power, and cost) through their natural systems-level interdependencies.
This work identifies actionable practices, pathways to encourage stakeholders and partners, and lessons from other large-scale scientific enterprises. Our approach will position HWO as a technical, scientific, and ethical example: advancing space astronomy and meaningfully contributing to a sustainable future.
14145-55
8 July 2026 • 11:10 - 11:30 CEST
Show Abstract +
High-contrast imaging of exoplanetary systems requires robust post-processing to detect faint companions amidst bright stellar light. We present a model-based coronagraphic phase retrieval method under active development for JWST high contrast imaging observations, validated on simulated datasets and currently applied to JWST NIRCam and NIRISS AMI data, with ongoing work to achieve robust convergence across different observations. The approach leverages a physically informed instrument model to estimate the wavefront and mitigate calibration errors, providing a robust framework for PSF subtraction and post-processing without reliance on traditional reference stars. By integrating instrument modeling directly into the analysis pipeline, this method informs observing strategies, calibration approaches, and post-processing techniques for upcoming missions, including the Roman Coronagraph Instrument and the Habitable Worlds Observatory.
14145-56
8 July 2026 • 11:30 - 11:50 CEST
Show Abstract +
NASA’s Habitable Worlds Observatory (HWO) aims to detect and study Earth-like exoplanets, which will require maintaining some wavefront error mode at a picometric stability over hours. While the James Webb Space Telescope (JWST) achieves sub-nanometer stability, it lacks the advanced coronagraphy and active wavefront control needed for direct imaging of such planets.
To better understand the technology gap to be bridged by HWO, we combine JWST’s segments phasing in-flight data, a modern Apodized Pupil Lyot Coronagraph (APLC) design, and wavefront control techniques from the Roman Space Telescope’s Coronagraph Instrument (CGI) to simulate residual wavefront errors under realistic conditions. We evaluate different system designs, including deformable mirror and sensor configurations, to determine achievable contrast levels. The pairing these simulations with JWST’s stability measurements provides insight of the current technological capabilities for Earth-like planet imaging.
14145-57
8 July 2026 • 11:50 - 12:10 CEST
Show Abstract +
The Habitable Worlds Observatory (HWO) requires unprecedented, picometer-level stability to fulfill one of its driving science requirements of detecting and characterizing Earth-like planets around Sun-like stars. Over the last several years, the Goddard Space Flight Center’s Ultra-Stable Structures Laboratory has been designing and constructing the Mini-Metrology and Ultra-Stable Testbed (Mini-MUST) to test components and systems to these stability levels and advance their technical readiness levels. Mini-MUST recently achieved first light at GSFC and has started testing campaigns to support the ROSES D.19 projects. We present our first light results, including correlation of our measured data with our high-fidelity thermal and structural models.
Break
Lunch/Exhibition Break 12:10 - 13:10
Session 13:
Habitable Worlds Observatory I: Joint Session with Conferences 14145 and 14146
8 July 2026 • 13:10 - 15:10 CEST
Session Chair:
Marshall D. Perrin, Space Telescope Science Institute (United States)
Show Abstract +
The Habitable Worlds Observatory Technology Maturation Project Office (HWO-TMPO) is executing a comprehensive pre-formulation program to mature critical technologies and mission architectures for NASA's next flagship astrophysics mission following Roman. Established in August 2024 in response to the 2020 Decadal Survey's top large mission recommendation, HWO-TMPO has systematically progressed through Concept Maturity Levels while exploring multiple mission architectures via Exploratory Analytic Cases. The presentation will status across three primary technology development tracks: coronagraph systems, ultra-stable telescope technologies, and high-sensitivity UV/visible instrumentation.
This presentation will provide an overview of the technical and programmatic status on HWO-TMPO's progress toward Mission Concept Review.
14145-59
8 July 2026 • 13:30 - 13:50 CEST
Show Abstract +
The Habitable Worlds Observatory is NASA’s next large space telescope, selected by the 2020 Decadal Survey in Astronomy and Astrophysics to search for and characterize habitable exoplanets while enabling a broad range of transformative astrophysics. The HWO Technology Maturation Project Office (TMPO) is exploring the HWO science, technology, and mission architectures toward a Mission Concept Review (MCR) at the end of the decade. A primary deliverable of this effort is a technology development plan that identifies critical technologies that enable the mission, defines a process for assessing the readiness of those technologies, and outlines a strategy for developing those technologies to a Technology Readiness Level (TRL) of 5 before the MCR. In this paper we summarize the HWO technology development plan which comprises three “tracks”: Coronagraph System technologies, Ultra-stable Telescope System technologies, and High-sensitivity Ultraviolet and Visible Instrumentation technologies.
14145-60
8 July 2026 • 13:50 - 14:10 CEST
Show Abstract +
NASA’s Habitable Worlds Observatory (HWO) Technology Maturation Project Office (HTMPO) released a call in 2026 for US-led instrument studies. The instrument concepts should be designed to meet the transformative astrophysics measurement capabilities defined by the Community Science and Instrumentation Team (CSIT) in their analysis of science cases developed by the international astronomical community. The instrument study call defined bounding conditions such as mass, power and volume, as well as a fundamental understanding of the optical, mechanical and thermal interfaces provided by the latest two observatory design concepts. The ultraviolet instrument (UVI) coordination team developed these bounding conditions in 2025 – 2026 with a view to the likely range of capabilities for those instruments. While the NASA-sponsored instrument study call focuses on US-led proposals, NASA fully supports collaborative efforts for instrument studies and designs from international partners.
14146-70
8 July 2026 • 14:10 - 14:30 CEST
Show Abstract +
This talk summarizes current progress by the HWO Community Science and Instrumentation Team (CSIT) to identify and quantify science cases that motivate the capabilities of the UV instrument suite for HWO. Key science drivers currently include the regulation of star formation over cosmic time through galactic feedback, the intergalactic ionizing radiation field, the properties of the first stars, and the evolution of chemical complexity in stars and galaxies, and access to ozone in the atmospheres of potentially habitable planets. We describe select science cases as well as the measurement goals and instrument capabilities they imply for the HWO, ranging from UV high-resolution point-source spectroscopy, multi-object and integral field spectroscopy, and far-UV imaging capabilities. The talk will conclude with a synthesis of these measurement capabilities and a description of the next steps for UV instrument definition through the 2026 call for US HWO instrument studies.
14146-71
8 July 2026 • 14:30 - 14:50 CEST
Show Abstract +
Pollux is a proposed high-resolution spectrograph (R>75,000–100,000) with polarimetry capabilities for NASA’s Habitable Worlds Observatory, covering 100–1888 nm across five echelle spectrographs. It enables simultaneous spectroscopy and polarimetry (Stokes I, Q, U, V), addressing key science: exoplanet atmospheres, star-planet interactions, galactic evolution, and cosmic magnetic fields.
Pollux aligns with HWO’s goals, supporting studies of habitable worlds, stellar magnetism, and intergalactic media. Its design includes UV/NIR polarimeters, advanced gratings, and space-qualified detectors. This paper presents Pollux’s science objectives, instrument architecture, and development roadmap, highlighting its potential as a transformative tool for astrophysics.
14145-61
8 July 2026 • 14:50 - 15:10 CEST
Show Abstract +
The Habitable Worlds Observatory (HWO) is NASA’s planned flagship mission for directly detecting and characterising Earth-like exoplanets around nearby Sun-like stars. A UK Space Agency–funded study is assessing a potential UK-led high-resolution imager (HRI). Science drivers from the HWO Science Case define required performance across the UV–optical–near-IR, including sub-microarcsecond astrometry for exo-Earth mass measurements and support for guiding and wavefront sensing.
Concurrent Design Facility work is evaluating optical architectures, detector options, mass and volume limits, and data-handling needs. Early assessments focus on optical modelling, stability and tolerances, and sensitivity and throughput estimates. Initial results show that high-stability, high-sensitivity HRI designs are feasible, outlining key requirements, technology risks, and a development path toward a mature HWO instrument concept.
Break
Coffee Break 15:10 - 15:40
Session 14:
Habitable Worlds Observatory II: Technologies and Instrumentation
8 July 2026 • 15:40 - 17:40 CEST
Session Chair:
Jeanette L. Domber, BAE Systems, Inc. (United States)
14145-63
8 July 2026 • 15:40 - 16:00 CEST
Show Abstract +
We report on our evaluation of the end-to-end dynamic stability performance achieved on a pathfinder observatory architecture developed by NASA and its partners called EAC1. The optical telescope assembly consists of an off-axis 6-meter inscribed-diameter segmented primary mirror with 19 segments and an unobscured telescope. Our reporting covers a layered control approach to achieving the requisite wavefront stability combining Lockheed Martin’s Disturbance Free Payload (DFP) system for vibration isolation from the host spacecraft to the telescope, and active wavefront sensing and control of the primary mirror segment and the secondary mirror complete with picometer-class metrology and actuation. DFP enables high science observation efficiencies with little-to-no downtime following slews and tight telescope precision pointing control at ~0.6-Hz bandwidth. We discuss the implications for the design of the observatory and its active wavefront sensing and control system.
14145-64
8 July 2026 • 16:00 - 16:20 CEST
Show Abstract +
BAE Systems Space & Mission Systems has led a series of NASA-funded programs under the Ultra-stable Large Telescope Research and Analysis (ULTRA) umbrella performing research and development of key technologies for NASA’s Habitable Worlds Observatory (HWO). One of the highest priority technology gaps for the HWO architecture is limiting the rigid body motion of the telescope optics to achieve the demanding wavefront stability needed by the coronagraph. Thus, a major focus of the current ULTRA program is building a subscale, three segment testbed to demonstrate segment level sensing and control to technology readiness level 4/5 at the fidelity needed for HWO. This paper will discuss component technologies, specifically picometer capable actuators and capacitive sensors, and the status of the multiple-segment testbed that is currently in assembly at BAE Systems SMS in preparation for testing at the Goddard Ultrastable Laboratory in the summer of 2026.
Show Abstract +
We report on progress on the STABLE study, which was awarded on the NASA 2023 ROSES D.19 opportunity. In the study, we are developing technologies for the Habitable Worlds Observatory (HWO) in four areas: Micrometeoroid Impact Mitigation, Telescope Temperature Control, Ultra-Stable Telescope Structure Materials and Modeling, and Improvement of Thermal Expansion Test Capability. This study is a collaboration between Northrop Grumman, Kratos, NeXolve, JPL, STScI, NASA’s White Sands Test Facility, and NASA Goddard’s Ultra-Stable Test Facility. We will also discuss our plans for our follow-on study as part of NASA’s 2024 ROSES D.19. In this study, we will address additional technologies as well as perform analysis of HWO architecture options.
14145-66
8 July 2026 • 16:40 - 17:00 CEST
Show Abstract +
To meet its demanding the Habitable Worlds Observatory (HWO) astrometric goals, a dedicated high-precision instrument is being developed around a gigapixel-class focal plane using Pyxalis’s new 220-MP GigaPyx CMOS sensors and an integrated calibration system. The project addresses three main challenges: validating detector performance, developing space-qualified packaging for a multi-sensor focal plane, and implementing on-board processing capable of reducing data volume by a factor of ~100. The maturation plan includes building a complete end-to-end detection chain to reach TRL 5 by the end of the program for the Mission Consolidation review in 2029.
14145-67
8 July 2026 • 17:00 - 17:20 CEST
Show Abstract +
We present a comprehensive system analysis for an instrument onboard the Habitable Worlds Observatory (HWO), designed for high-precision, high-accuracy differential astrometry. The analysis integrates the definition of the mission profile, the instrumental concept architecture, and an error budget that breaks down the key contributors to the sub-µas precision required for a single measurement. The proposed architecture of the instrument concept is derived from error budget and mission constraints based on a large visible detector array composed of an assembly of multiple CMOS sensor chips resulting in an overall gigapixel focal plane, with a technological maturation plan leading to TRL 5 for the Mission Consolidation review in 2029.
14145-248
8 July 2026 • 17:20 - 17:40 CEST
Show Abstract +
The field of space technology is rapidly changing as we enter the second quarter of the 21st century and enter the pre-formulation period for Habitable Worlds Observer (HWO). This rapid advancement in technologies and operating concepts can even be considered a revolution in our field. We will introduce the idea that this revolution also impacts considerations in the mission architecture of the HWO. The three space ages are defined along with their design paradigms and ethos. The challenge of designing a flagship mission such as HWO as a mission of the current space age is presented and we will show that some of the elements of the new space revolution can relax some of these constraints. Inclusion of these new technologies and concepts is not free, and we will examine how architecting for the new space age is different than for previous missions.
Thursday Plenary
9 July 2026 • 08:30 - 10:00 CEST
Join us for the Thursday plenary session.
Break
Coffee Break 10:00 - 10:30
Session 15:
Exoplanet Imaging III: Missions and Testbeds
9 July 2026 • 10:30 - 12:30 CEST
Session Chair:
Tyler D. Groff, NASA Goddard Space Flight Ctr. (United States)
14145-68
9 July 2026 • 10:30 - 10:50 CEST
Show Abstract +
PICTURE-D is a NASA high-altitude balloon mission to directly image exoplanetary systems with the goal of characterizing the inner debris disks of several nearby stars in reflected visible light. The observatory performed its first balloon flight on October 1, 2025 from the NASA CSBF launch facility in Ft. Sumner, NM. The experiment consists of a 60 cm off-axis telescope coupled with a coronagraph instrument containing high and low-order wavefront control systems, dual BMC MEMS deformable mirrors and a charge 6 vector vortex focal plane mask. During the 20 hour flight, 4 stars were observed: Vega, Altair, Fomalhaut and the Gamma Cassiopeiae binary system. On-sky contrast was limited to the 1e-6 level due to poor EFC dark hole convergence and residual pointing jitter owing to a throughput issue with one of the low-order wavefront sensors. We present the observational results from the flight and a description of the technical performance of the observatory sub-systems.
14145-69
9 July 2026 • 10:50 - 11:10 CEST
Show Abstract +
We report on the ESA-funded SUPPPPRESS project, focused on developing high-performance liquid-crystal coronagraphs for the direct detection and spectral characterization of Earth-like exoplanets. The goal is to improve the contrast and operational spectral bandwidth of the Vector Vortex Coronagraph (VVC). We manufacture regular and multi-grating VVCs (mgVVCs), stacking two or three liquid-crystal masks (LCMs) with vortex and grating patterns to mitigate polarization leakage. This enables full exploitation of the VVC's achromatic and scale-invariant properties. We detail the improved manufacturing of LCMs by ColorLink Japan, Ltd. and their quality assessment using far-field diffraction, polarization microscopy, and zero-order leakage spectroscopy. The individual LCMs are assembled into mgVVCs using a custom jig. We demonstrate their broadband contrast performance on the THD2 testbed, comparing standard VVCs and mgVVCs. Finally, we discuss space environmental qualification of the masks.
14145-70
9 July 2026 • 11:10 - 11:30 CEST
Show Abstract +
We present the first scientific results by the upgraded THD2 high-contrast imaging testbed. First, for the Nancy Grace Roman Space Telescope, we demonstrate how single-actuator probes outperform the baseline sinc probes by reducing non-linearities, supporting higher probe amplitudes, and improving electric-field estimation. These results led to their prioritisation as an enhanced commissioning mode for Roman. Second, within ESA’s SUPPPPRESS project, we test new polarization-independent Vector Vortex Coronagraphs designed to achieve contrasts approaching 1e-10 over >20% bandwidth in simulations. We assess their behavior on the testbed in narrow- and broadband light with active focal-plane wavefront control. Together, these results show how THD2 strengthens Europe’s capability in high-contrast imaging, providing a unique platform reaching contrasts of 1e-8 to 1e-9 for developing next-generation coronagraphic technologies.
14145-71
9 July 2026 • 11:30 - 11:50 CEST
Show Abstract +
Scalar vortex coronagraphs are promising for future high-contrast imaging missions because they provide a true dual-polarization coronagraph solution. Recent demonstrations of the dimpled scalar vortex coronagraph on the In-Air Coronagraph Testbed (IACT) have achieved contrasts at the current testbed floor (~1e-8). To push beyond this limit, we are exploring upgrades to IACT as well as testing the same mask in vacuum with two deformable mirrors (DMs) for full amplitude and phase control. IACT improvements include replacing the DM electronics with a 16-bit system to reduce noise and increase actuator precision, upgrading the broadband light source, and refining electric-field-conjugation parameters to better model the optical setup. We also verify the dimpled vortex performance in fully unpolarized broadband light, ensuring astrophysical relevance. Together, these upgrades define a clear path toward establishing a new broadband contrast record for the scalar vortex coronagraph.
14145-72
9 July 2026 • 11:50 - 12:10 CEST
Show Abstract +
The detection and characterization of Earth-like exoplanets is one of the key scientific goals of future space observatories. Achieving this requires starlight suppression at contrasts of the order of 10-10. Maintaining these contrasts over long integration times is essential to image faint planets. In practice, this is challenging due to the mechanical instabilities and thermal gradients within the telescope that give rise to quasi-static wavefront errors. Dark Zone Maintenance (DZM) techniques can mitigate these effects by stabilizing the wavefront in realtime. We present the results from simulations of an extended Kalman filter (EKF)-based DZM algorithm implemented on a model of SCoOB (a vector vortex coronagraph with a charge-6 vector vortex wave plate and Kilo-C DM) to maintain the contrast at ~10-8 within a one-sided dark hole from 3–10 lambda/D in the presence of injected drifts and the latest results from the testbed.
14145-73
9 July 2026 • 12:10 - 12:30 CEST
Show Abstract +
The ongoing and upcoming space-based planet survey missions, such as TESS, PLATO, and ET, are expected to discover thousands of small- to medium-sized planets, including over 100 potentially habitable rocky planets. To further study these Earth 2.0, the exoplanetary science community has proposed various follow-up missions. However, none of these missions will be able to characterize the atmospheres of Earth-like planets in habitable zones or detect potential biosignatures. China is pushing Tianlin, a 6.6m UV-to-NIR space telescope, projected to begin operations around 2035+ with a mission lifespan exceeding 10 years. Tianlin's primary goal will be the characterization of rocky planets in the habitable zones of nearby stars, with a focus on identifying possible biosignatures. Additionally, this mission aims to significantly enhance our understanding of exoplanet populations, nearby galaxies, and the early universe. International collaborations in multiple disciplines are welcome.
Break
Lunch/Exhibition Break 12:30 - 13:40
Session 16:
Habitable Worlds Observatory III: Extreme Contrast Wavefront Control
9 July 2026 • 13:40 - 15:20 CEST
Session Chair:
Leonid Pogorelyuk, Rensselaer Polytechnic Institute (United States)
14145-74
9 July 2026 • 13:40 - 14:00 CEST
Show Abstract +
To directly image and characterize Earth-like exoplanets, the Habitable Worlds Observatory (HWO) will be required to control or correct for wavefront errors on the order of picometers. Due to the limited flux of these exoplanets, this stability will need to be maintained for tens of hours thus requiring real-time wavefront sensing and control during science observations. Ideally, the observing strategy, dark zone maintenance (DZM) scheme, and post-processing algorithms are optimized together to maximize the potential science yield. Here we discuss a DZM algorithm that uses an extended Kalman filter to estimate the coherent electric field separate from the incoherent intensity in the science images using a single image per iteration. The coherent estimate is then used to determine a deformable mirror shape that will suppress the drift. We demonstrate the DZM closed-loop and post-processed performance with the exploratory analytical concept one (EAC1) in the presence of realistic drifts.
14145-75
9 July 2026 • 14:00 - 14:20 CEST
Show Abstract +
The Habitable Worlds Observatory (HWO) aims to directly detect nearby earth-like exoplanets and search their atmospheres for biomarkers, requiring starlight suppression at 10^10 contrast over ~20% bandpasses—a major technical challenge. Even with an ultra-stable 6–8 m telescope, advanced coronagraphs, and extreme wavefront control, raw contrast alone is unlikely to meet these requirements for long-duration integrations. HWO will therefore depend on continuous focal-plane wavefront sensing to maintain a deep dark hole and post-processing while minimizing detector noise impacts.
I will present a Canadian imager concept optimized for sensitivity and biomarker characterization, compatible with current space-qualified visible detectors and emerging detector technologies. The instrument supports high-SNR focal-plane wavefront sensing/control and is designed to enhance final contrast with post-processing methods.
14145-77
9 July 2026 • 14:20 - 14:40 CEST
Show Abstract +
The Apodized Vortex Coronagraph (AVC) is a leading architecture for high-contrast imaging on segmented telescopes and a key candidate for the Habitable Worlds Observatory (HWO). Building on our previous optimization of the Amplitude-Apodized Vortex Coronagraph (AAVC) for HWO’s Exploratory Cases 1 and 2, we now report progress from modeling to experiment. We present updated apodizer designs, refined sensitivity analyses, and the first laboratory implementation of the AAVC on a high-contrast testbed. Initial measurements show improved contrast performance and validate the expected error-budget trends toward the ~1e-10 requirement. We also provide updated yield estimates from FRIDAY across recent HWO aperture configurations. These results mark a key step in advancing the AAVC toward HWO requirements.
14145-78
9 July 2026 • 14:40 - 15:00 CEST
Show Abstract +
Deformable Mirrors (DMs) are the critical component for the Habitable Worlds Observatory (HWO). A baseline set of device requirements was set for a short feasibility study by some key DM vendors. Included in these requirements are previously untestable tolerances for which a verification plan must be developed. The stability requirements, in particular, are held at unprecedented temporal frequencies. Picometer-level tolerances are levied for both long term drift as well as times scales greater than 10 Hz. This work presents a shift in thinking on how to augment the DM stability requirements via power spectrum specifications, and a concept testbed that is purpose built to directly verify this. Overall, we present the combined progress on our development of the DM verification plan for HWO DM system technologies, and dive into the testbed measurements intended to demonstrate the devices are fit for exo-Earth coronagraphy.
14145-79
9 July 2026 • 15:00 - 15:20 CEST
Show Abstract +
Direct spectroscopy of habitable exoplanets must overcome low source flux and comparatively higher background, requiring exposure times of weeks for the HWO mission. Spectroscopy in the information-rich NIR regime is particularly challenging, as poorer angular resolution exacerbates background mixing, especially near the coronagraph IWA.
We propose to match the post-coronagraph exoplanet electric field to the input of a single-mode spectrograph using a photonic lantern (PL) positioned on the planet location, and feeding a photonic integrated circuit (PIC). We show that the approach offers an order of magnitude gain in exposure time, and extends exoplanet spectroscopy to the NIR regime by enabling a smaller IWA.
We discuss this approach as a NIR spectroscopy module for the HWO mission, and provide an overview of ongoing technology validation activities, including on-sky demonstration of its key elements at the Subaru Telescope.
Break
Coffee Break 15:20 - 15:50
Session 17:
Technology: Telescope Concepts and Wavefront Control
9 July 2026 • 15:50 - 17:30 CEST
Session Chair:
Dmitry Savransky, Cornell Univ. (United States)
14145-80
9 July 2026 • 15:50 - 16:10 CEST
Show Abstract +
Tianlin, which literally means “neighbors in the universe” in Chinese, is a habitable world exploration mission proposed by astronomers from the National Astronomical Observatories of the Chinese Academy of Sciences (NAOC). The mission will involve launching a 6-meter-class UV-optical space telescope with a monolithic aperture to the Earth-Sun L2 (ESL2) orbit. This article briefly describes the telescope’s optical and structural design, scientific instrument configuration, as well as its deployment and long-term on-orbit maintenance methods.
14145-81
9 July 2026 • 16:10 - 16:30 CEST
Show Abstract +
Inflatable membrane reflectors offer a compelling pathway to realizing large-aperture optical systems for far-infrared and millimeter-wave astronomy. Compared with mechanically deployed reflectors, membrane-based systems provide exceptional advantages in mass efficiency, stowage volume, scalability, and structural simplicity. Our work introduces a novel, instrumentation-driven approach that directly addresses these historical limitations. Central to this approach is an optical architecture that pairs an inflatable primary membrane mirror with precision-machined corrective surfaces, enabling compensation for low-order membrane aberrations and improved far-IR wavefront quality. These innovations are being implemented and validated on a 3-meter prototype reflector, which serves as a critical testbed for understanding inflation behavior, tension-load paths, rigidization performance, and metrology-informed surface correction strategies.
14145-82
9 July 2026 • 16:30 - 16:50 CEST
Show Abstract +
This work proposes an optical telescope architecture for intersatellite laser interferometry missions SILVIA, where lossless intersatellite laser ranging is employed.
To simplify link acquisition and reduce reliance on satellite attitude control, we propose a non-cooperative laser link approach. However, this approach poses two major challenges: both retroreflection and mode matching must be simultaneously achieved, and sharing a single telescope for transmission and reception makes independent bidirectional alignment nontrivial.
To overcome these issues, we propose a new telescope design inspired by the cat’s-eye retroreflector and derive its parameters using ray-matrix analysis. Based on this design, we are currently developing an optical breadboard model (BBM). This talk presents the design concept and reports on the current BBM development status.
14145-83
9 July 2026 • 16:50 - 17:10 CEST
Show Abstract +
This work presents the latest technology development and science opportunities for Multi-Star Wavefront Control (MSWC), a method to enable high-contrast imaging of multi-star systems with the Roman Space Telescope and Habitable Worlds Observatory (HWO). MSWC enhances the exoplanet yield and enables new science specific to planets around multi-star systems. In addition, it enables a follow up of the aCenA planet candidate recently reported by JWST. Our laboratory tests are continuing at JPL’s High Contrast Imaging Testbed (HCIT), and at time of this writing, include a demonstration of 9.4e-8 in full MSWC mode for an equivalent aCenAB separation. Scaled to the binary’s actual flux ratio, these performance levels yield equivalent contrasts of 3.7e-8 (aCenA) and 1.8e-7 (aCenB). These results suggest that current performance may already be sufficient to detect planets around aCenA in reflected light, if it can be replicated on sky.
14145-84
9 July 2026 • 17:10 - 17:30 CEST
Show Abstract +
The Tiny Observatory for Telescope Optimization (TOTO) is an optical testbed designed to evaluate the efficacy of autonomously driven alignment algorithms for space-based telescope systems. For space-based missions, active control of the telescope on-orbit offers potential to relax passive alignment requirements and reduce on-ground verification activity. TOTO is used to evaluate and verify simulation work of two primary alignment algorithms, Stochastic Parallel Gradient Descent (SPGD) and focus-diverse phase retrieval. Previous simulation work has confirmed that by using SPGD for coarse alignment followed by focus-diverse phase retrieval for fine alignment, we can reach diffraction-limited performance on-orbit. This paper presents the results of the autonomous alignment algorithm of a TMA using TOTO. We report the current status of TOTO as well as preliminary results from SPGD and phase retrieval on the testbed using monochromatic light source to simulate a natural guide star.
Session 18:
Heliophysics
10 July 2026 • 08:40 - 10:00 CEST
Session Chair:
Shuji Matsuura, Kwansei Gakuin Univ. (Japan)
14145-85
10 July 2026 • 08:40 - 09:00 CEST
Show Abstract +
The ESA Proba-3 mission is a groundbreaking project to demonstrate and validate the concept of precise formation flying, with millimetric accuracy. It involves two spacecraft flying 150 meters apart and together forming a giant solar coronagraph. Following their launch in December 2024, the Proba-3 spacecraft entered routine science operations in July 2025.
This paper presents the achieved formation flying performance of the Proba-3 spacecraft relevant for the coronagraphic observations, gathered from the satellites’ in-flight data. Moreover it describes how the formation flying enables the observation of the poorly explored inner region of the sun corona by minimizing the straylight level. Finally it discusses the main factors influencing the formation flying performance, including the on-board sensors accuracy, the satellites’ specific orbit and the capabilities of the propulsion system.
14145-86
10 July 2026 • 09:00 - 09:20 CEST
Show Abstract +
The Space-weather Solar Coronagraph (SwSCOR) instruments are in development to provide the National Oceanic and Atmospheric Administration (NOAA) Space weather Observations at Lagrange 1 (L1) for Advanced Readiness (SOLAR) program with continuity and resilience of solar wind data and coronal mass ejection (CME) imagery. The SwSCOR project, led by Southwest Research Institute (SwRI), consists of a coronagraph instrument and a set of ground processing algorithms designed to produce space weather imagery. The instrument is a single-stage, externally occulted coronagraph and the camera and electronics are adapted and tailored for the SwSCOR project from versions already developed for NASA’s Polarimeter to Unify the Corona and Heliosphere (PUNCH) Small Explorer mission. SwSCOR is intended to deliver real-time, forecast-quality images of the solar K corona (sunlight scattered by free electrons near the Sun), allowing forecasters to characterize and track space weather as it leaves the Sun.
14145-87
10 July 2026 • 09:20 - 09:40 CEST
Show Abstract +
Metis is the ultraviolet–visible coronagraph on board the ESA Solar Orbiter mission, designed to image the solar corona simultaneously in polarised visible light and in the Lyman-α ultraviolet emission. The instrument can acquire full-frame images on both channels at a very high rate, with a minimum cadence of one second. This capability enables detailed investigations of coronal variability and fluctuations, but also requires an accurate characterisation of the instrument response in both the time and frequency domains.
In this work, we present the methodology adopted to assess the temporal and spectral variability of the response of the Metis detectors. In particular, we identify and analyse the main sources of signal variability due to instrumental effects, with the aim of quantifying their impact on the measurements and decoupling them from the intrinsic physical fluctuations of the solar corona.
14145-88
10 July 2026 • 09:40 - 10:00 CEST
Show Abstract +
Metis, the coronagraph aboard Solar Orbiter, observes the solar corona by measuring linear polarization in visible broadband (580-640 nm) and capturing ultraviolet images (Ly-alpha HI line, 121.6 nm). This study presents a comprehensive analysis of the Metis Point Spread Function (PSF) in the visible channel throughout the mission duration.
We systematically examined PSF characteristics by analyzing stellar images within the Metis Field of View, considering stars with different spectral properties in both unpolarized and polarimetric imaging modes. In-flight PSF measurements were compared with on-ground calibration data and Zemax optical simulations to identify discrepancies and characterize the instrument's optical performance evolution.
Results assess the consistency between predicted and observed PSF behavior as a function of star position and time, providing insights into the long-term stability and performance of the Metis visible light coronagraph in the space environment.
Break
Coffee Break 10:00 - 10:30
Session 19:
Far IR, Sub-MM, and MM
10 July 2026 • 10:30 - 11:50 CEST
Session Chair:
Matthew J. Griffin, Cardiff Univ. (United Kingdom)
Show Abstract +
LiteBIRD is an ISAS/JAXA strategic L-class mission to probe cosmic inflation and the cosmic history of the Universe through full-sky measurements of cosmic microwave background (CMB) polarization. From mid-2024, LiteBIRD undertook a year-long strategic reformation of its mission architecture. This effort included a reassessment of mission requirements, instrument configuration, and the associated procurement plan, while preserving the mission’s scientific objectives and sensitivity targets. The updated LiteBIRD mission places its primary requirement on achieving the necessary map depth, enabling precise extraction of the tensor-to-scalar ratio and ensuring strong capability for a wide range of additional cosmological and astrophysical investigations. LiteBIRD is proceeding toward a planned launch in the 2030s. The mission is scheduled to enter Phase A, following the Mission Design Review (MDR) in 2026. In this presentation, we report an overview of LiteBIRD.
14145-90
10 July 2026 • 10:50 - 11:10 CEST
Show Abstract +
PRIMA is a NASA astrophysics Probe that has recently completed a Phase A concept study. PRIMA’s exciting science case, the observatory design, and the innovative technology that enables it will be summarized.
14145-91
10 July 2026 • 11:10 - 11:30 CEST
Show Abstract +
PRIMA's Far-Infrared Enhanced Survey Spectrometer (FIRESS) provides 24-235 micron spectroscopy with four slit-fed, 1st-order grating modules, each feeding an arrays of kinetic inductance detectors (KIDs). Each band covers a 1:1.8 spectral range, so the four band cover the full range instantaneously. The gratings provide R>85 everywhere, with median value R of 140. Each FIRESS slit is 24 spatial pixels, and each band delivers the dispersed spectrum to a 24 by 84 (spectral) pixel array. Point sources are chopped along the slit with the steering mirror to remove low-frequency detector noise, subtract the background, and provide half-pixel spectral sampling given the hexagonally-packed array. For high-resolution, a Fourier-transform interferometer is engaged to process the light between the telescope and the grating modules, detailed in a separate contribution led by A. Kogut. Here we provide an overview of FIRESS and the detectors, the observing modes, and expected sensitivity.
14145-92
10 July 2026 • 11:30 - 11:50 CEST
Show Abstract +
PRIMA (PRobe far-Infrared Mission for Astrophysics) is an infrared observatory featuring a 1.8 m telescope cooled to 4.5 K, designed to operate for the next decade. Currently in the concept study phase, it includes two instruments, one of which is PRIMAger developed by an European consortium. PRIMAger offers two modes: hyperspectral (24–84 µm, spectral resolution ≥ 8) and polarimetric (4 broad bands from 80 to 264 µm, measuring three polarization orientations). It uses ultra-sensitive KID detectors cooled at 0.12K and an opto-mechanical structure at 1 K. A major challenge is in-flight verification. The paper outlines the technical requirements, design, and development strategy, including a rigorous test plan.
Break
Lunch Break 11:50 - 13:10
Session 20:
Exoplanet Imaging IV: Photonics, Quantum Optics, and Machine Learning
10 July 2026 • 13:10 - 15:10 CEST
Session Chair:
Laura E. Coyle, BAE Systems, Inc. (United States)
14145-94
10 July 2026 • 13:10 - 13:30 CEST
Show Abstract +
Integrated photonics is a promising coronagraph technology option for increasing the Exo-Earth science yield of NASA’s Habitable Worlds Observatory and relaxing key observatory requirements. A photonic integrated circuit (PIC) coronagraph is theoretically capable of achieving extremely high performance because arrays of integrated interferometers can implement any optical transformation, including a near-optimal coronagraph. However, PIC coronagraphs require maturation before use in a space telescope mission. The AstroPIC project is advancing this technology by developing a proof-of-concept silicon-photonic PIC coronagraph in the near-infrared.
In this talk, we will review the design of AstroPIC and present results from laboratory testing of the first set of PIC devices fabricated for the project, including experiments that achieve over 90 dB extinction (<1e-9 contrast) of a single input channel and over 60 dB extinction (<1e-6 contrast) of multiple illuminated inputs.
14145-95
10 July 2026 • 13:30 - 13:50 CEST
Show Abstract +
Despite their scientific value, no space-based, high–spectral-resolution integral field spectrographs currently exist due to their prohibitive cost, size, and complexity. We propose a novel, highly multiplexed astrophotonic integral field spectrograph architecture that overcomes these barriers, enabling large-scale exoplanet atmosphere and biosignature surveys. The concept employs arrays of silicon nitride photonic chips with high-throughput, tunable cross-correlation filter arrays spanning the visible to short-wave infrared (H-band). This design simultaneously measures gas-specific transit curves and achieves high radial velocity precision at moderate spatial resolution, using polarization duplexing for enhanced information content.
14145-96
10 July 2026 • 13:50 - 14:10 CEST
Show Abstract +
We investigate the quantum limits of exoplanet detection and localization around partially resolved stars with finite angular extent. In this model, the density operator describing the state of the incoming optical field has an infinite-dimensional support over the Hilbert space of band-limited square-normalized spatial modes. Therefore, we numerically evaluate two fundamental quantum bounds: (1) The quantum Chernoff exponent which provides an asymptotic lower bound on the minimum achievable probability of error for exoplanet detection, (2) The quantum Cramer-Rao bound which provides a lower bound on the minimum achievable uncertainty for unbiased estimators of the exoplanet orbital position. We subsequently compare the performance of even-order coronagraphs against these bounds and propose a new quantum-optimal coronagraph which can accelerate the rate of exoplanet discovery over the domain of sub-diffraction orbits.
14145-97
10 July 2026 • 14:10 - 14:30 CEST
Show Abstract +
Coherent starlight suppression techniques are tools for enabling direct observations of faint companions near bright stars. These methods are constrained by several fundamental considerations . We discuss these limits in a unified way. One limit is set by spatial coherence. The planet and the star electric fields overlap slightly at the entrance pupil. A coronagraph suppresses the part of the star orthogonal to the planet field, but any shared component cannot be removed without suppressing the planet. This sets a floor that cannot be eliminated by coherent subtraction. Further, nulling the star at one wavelength does not null it at other wavelengths, but a broader bandwidth improves the photon statistics for field estimation. These effects define the true performance limits for any classical coronagraph combined with coherent subtraction. We describe how recent proposals including quantum enhanced optical imaging relate to these fundamental limits and provide new opportunities.
14145-98
10 July 2026 • 14:30 - 14:50 CEST
Show Abstract +
Direct imaging of exoplanets is limited by the extreme contrast between the star and the planets, which is mitigated using a coronagraph.
However, optical aberrations cause starlight leakage through the coronagraph, producing speckles that obscure the planetary signal. Achieving the required contrast levels demands wavefront control with subnanometric precision.
Deep reinforcement learning, offers a promising alternative to traditional wavefront control approaches. In this work, we present a fully data-driven method for post-coronagraphic aberration correction from focal plane images using reinforcement learning. The agent directly controls a deformable mirror in the pupil plane using phase diversity images generated via single actuator probes. The method is validated on simplified simulations of a high-contrast imaging testbed, where it successfully created the first Dark Holes using reinforcement learning.
14145-99
Coherence differential imaging using random forest regression for the direct detection of exoplanets
10 July 2026 • 14:50 - 15:10 CEST
Show Abstract +
Coronagraphic imaging of exoplanets is limited by residual speckles that mimic planets. Advanced post-processing is essential for current and future instruments on the ground or in space.
Current techniques are time-intensive and limited. ADI requires long sequences and is limited at small separation. RDI is also time-consuming and sensitive to speckle evolution, leading to imperfect subtraction. Coherence Differential Imaging (CDI) offers a faster alternative by using the light incoherence between speckles and planets, but its reliance on accurate instrumental models limits performance.
After demonstration on SPHERE, we enhanced CDI with a Random Forest algorithm. This method models the differential signal as a high-dimensional regression problem, optimizing the discrimination between coherent speckle noise and the incoherent planet signal. We validate this enhanced CDI using testbed data reproducing Roman CGI conditions.
Break
Coffee Break 15:10 - 15:40
Session 21:
Technology: Optics
10 July 2026 • 15:40 - 17:00 CEST
Session Chair:
Frank U. Grupp, Univ.-Sternwarte München (Germany)
14145-100
10 July 2026 • 15:40 - 16:00 CEST
Show Abstract +
To spectroscopically resolve molecular vibrational lines from space, we are proposing the High-Resolution Spectrometer (HRS; 10–18 μm, λ/Δλ ~ 30,000) for GREX-PLUS, an ISAS/JAXA mission candidate. To downsize the HRS, we adopt a CdZnTe immersion grating (CZT-IG). CZT has high transparency and refractive index, but its use for IGs remains unexplored. To develop a CZT-IG, we are measuring the cryogenic optical properties, investigating cooling-resistant anti-reflection coatings, and exploring optimal conditions for groove processing. To verify the performance of a CZT-IG, we are developing a spectrometer for ground use. This instrument aims for HRS-level resolution with a CZT-IG. It will be installed on the 1.5-m Kanata telescope in Higashi-Hiroshima, targeting the N-band (8–13 μm). Its fully reflective optics (except for the IG) allow future expansion to the Q-band (16–26 μm) at a suitable site. This design maximizes the opportunity to test a CZT-IG for the HRS.
14145-101
10 July 2026 • 16:00 - 16:20 CEST
Show Abstract +
Existing state-of-the-art wavefront sensing and control setups for the imaging of exoplanets utilize two high-actuator count flat deformable mirrors (DMs) to control both phase and amplitude aberrations. One of the objectives of the Exoplanet Spectroscopy (ExoSpec) project at Goddard Space Flight Center (GSFC) is to improve upon this regime through the development of parabolic deformable mirrors (PDMs), which can address several of the key limitations in existing setups. Specifically, the need for flat DMs to be located in conjugate pupil planes drives unique packaging challenges that can be overcome by allowing the off-axis imaging elements to be controllable as well. In addition, simulations show that the use of deformable powered elements will increase the overall controllable bandwidth, up to 35% over 5-12 Lambda/D. To pursue this effort, the ExoSpec group has worked with Bertin Alpao to produce a first-generation parabolic DM.
14145-102
10 July 2026 • 16:20 - 16:40 CEST
Show Abstract +
Australian Astronomical Optics (AAO) at Macquarie University is leveraging its heritage in astronomical instrumentation to develop space-ready optical systems for navigation and imaging. We review three recent milestones: Malya, a space-qualified thermal imaging payload delivered to Gilmour Space for Earth observation; ALOHA, a precision optical head enabling LiDAR-like navigation for lunar landings; and OWL, a linkage-driven fast steering mirror system for agile pointing of large-aperture imaging payloads. These projects demonstrate AAO’s ability to adapt telescope technologies for space missions through innovative design and qualification. We conclude with future directions, including scalable pointing systems and advanced optical payloads with potential flow-back benefits for next-generation astronomical instrumentation.
14145-103
10 July 2026 • 16:40 - 17:00 CEST
Show Abstract +
We present a preliminary comparison of the SPDT machinability of five aluminum substrates: RSA aluminum, cast Al 6061, 3D-printed Scalmalloy, HIP-treated Scalmalloy, and 3D-printed AlSi10Mg. All samples were machined under identical ultra-precision conditions, followed by form-error measurement, nanometer-scale roughness evaluation, and microstructural inspection. The study compares porosity, print defects, scratches, and surface roughness among the additively manufactured variants against RSA and cast Al 6061, highlighting the improved homogeneity and reduced porosity from HIP treatment. These results support the use of high-strength additively manufactured aluminum for lightweight monolithic optical structures in space applications, reducing reliance on bimetallic thermal-compensation designs and improving thermoelastic stability and system simplicity.
Session PS1:
Posters - Technologies for Small Spacecraft
5 July 2026 • 17:30 - 19:00 CEST
View
Sunday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-104
5 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The A.S.T.R.O.N.A.U.T project is an international initiative led by the Space and Planetary Exploration Laboratory (SPEL, University of Chile) in collaboration with partners from China and France. Its goal is to develop miniaturized satellites equipped with advanced instrumentation for high-precision space observations and long-term planetary exploration. A key component of the project investigates biological processes for future sustainable life-support systems on the Moon and Mars. In March 2026, SPEL will deploy CubeSats to study seed germination and extremophilic microorganisms aboard the International Space Station. Parallel experiments at the Chinese Space Station is highly suitable. In parallel, the project develops nanosatellites optimized for astronomy, targeting transients, exoplanets, and variable stars. A.S.T.R.O.N.A.U.T strengthens China–Chile cooperation while advancing both space biology and ultra-precision space-based astronomy.
Show Abstract +
While internet mega-constellations undesired impact dominate astronomy discourse, a quieter revo-lution in Earth Observation (EO) is in full motion. Feeding from the new satellite commodity echo-system, bold entrepreneurs are committed to bring space-based optical observation to the masses. Heightened international tensions also encouraging intelligence imagery independence, startups and legacy suppliers are now engaged in large-aperture high-resolution or wide-field multi-detectors tele-scope-camera systems. Using relevant project examples, we explore how modern private EO satellites could perform if pointed toward deep-space and review the compromises needed to get to the price point enabling investor’s business cases. This surge of new funding in technologies highly relevant to astronomy instrumentation is changing the space access equation. We aim to demonstrate how these advances directly benefit candidate astronomy missions such as POET, TWINKLE, and CASTOR.
14145-106
5 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Freeform-optics-based telescopes are emerging as a key enabling technology for Earth Observation (EO) remote sensing, offering superior performance, wider fields of view and more compact architectures over conventional optical systems.
This work presents the design and analysis of an optimized f/3.5 off-axis reflective positive–negative–positive three-mirror anastigmatic (PNP-TMA) telescope operating in the visible range (400–800 nm), where a freeform surface is applied to the tertiary mirror. The introduction of a sixth-order XY polynomial freeform surface enables diffraction-limited performance over a ±6° field of view, along the X-direction. Considerations on dispersive elements are addressed for hyperspectral imaging applications targeting urban and vegetation monitoring.
14145-107
5 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Monolithic Telescope technology, developed at LLNL and now being commercialized by Starris Space Systems of Optimax, offers an innovative optical architecture for compact, highly stable space payloads. Made from a single piece of fused silica with primary and secondary surfaces polished on opposite sides, the Monolith removes alignment structures while maintaining diffraction-limited performance. Compared to Cassegrain designs, it provides reduced length and mass, excellent optical quality, and strong resilience to vibration, shock, and thermal variation, enabling high-performance imaging on smaller spacecraft with lower SWaP. Several configurations have been space-qualified or flown, demonstrating maturity and manufacturability. This talk reviews the transition from LLNL research to producible systems, including design and manufacturing methods, test results, and efforts to extend the technology to new mission classes and optical configurations.
14145-108
5 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
IACTEC-Space is an IAC initiative for developing advanced instrumentation for small satellites dedicated to astronomy and Earth observation. One of its goal is to monitor Earth’s dynamic processes from orbit with compact, high-performance imaging systems. The first instruments, DRAGO-1 and DRAGO-2, operate in the SWIR range (1.1 µm and 1.6 µm) using an uncooled InGaAs detector based on proprietary design, unique in the market. Launched in 2021 and 2023, respectively, they enabled imaging of the 2021 La Palma eruption and the 2023 Tenerife wildfire. DRAGO-1 provides 300 m resolution, while DRAGO-2 reaches 50 m, improvable to 30 m via non-interpolated super-resolution. An upgraded DRAGO-2 is onboard ALISIO-1, the first Canarian satellite. Current developments include IACSAT ASTRO-1 and DRAGO-3, featuring four NIR/SWIR bands with ~10 m/pixel resolution, enhancing natural disaster detection within the future Canarian Earth-observation constellation.
Show Abstract +
Nano Observatory as a Service (NOaaS):A Cloud-Connected Space/Ground Telescope Network for Real-Time Sky Awareness is a new way of monitoring the sky, using a fleet of small telescopes in space, combined with ground observatories and cloud computing on aws, to deliver real-time insights about what is happening above Earth. Instead of relying only on large, expensive observatories, NOaaS uses multiple compact telescopes in low-Earth orbit working together as a virtual global observatory.
In the age of AI and computing we are building a future by transforming how humanity explores space by monetizing access to cosmic events through Leveraging Space/Ground data from network of multispectral ground and In-Orbit Telescopes with accurate AI models for astronomy, education, and Asset/SSA-adjacent space mapping for making it accessible to researchers, students, space asset operators, Insurance company and enthusiasts worldwide using AWS platform.
Session PS2:
Posters - Exoplanet Time Series I
5 July 2026 • 17:30 - 19:00 CEST
View
Sunday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-110
5 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
This work presents the results of recent simulations in the relevant plasma environments that the Ariel (Atmospheric Remote-sensing Infrared Exoplanet Large-survey) spacecraft will encounter during its early orbit until its operation around L2, including transients between different plasma regimes, where not negligible surface charging phenomenon is expected to occur. The objective of this study is to analyse the effects of these transient conditions to understand how the spacecraft’s surface charges will redistribute.
14145-111
5 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
At payload level, a Structural, Thermal, and Optical Performance (STOP) analysis is carried out to evaluate how thermo-elastic effects may impact the instrument’s optical performance. A STOP analysis integrates structural, thermal, and optical models to predict how temperature variations and mechanically induced deformations propagate through the telescope assembly and ultimately affect key optical metrics such as alignment, wavefront error, and imaging quality. This coupled approach enables the estimation of performance degradation under representative environmental load cases and supports verification of compliance with scientific and engineering requirements.
This document presents the updated results of the optical design analysis performed to predict the in-flight performance for the Telescope Assembly of the ESA M4 mission Ariel according to the operational scenarios defined for Cycle C-2.
Show Abstract +
The finite element model (FEM) for optically processing the
deformation field of a telescope structure allows for the calculation
of all optically relevant data within a single simulation run. This
paper focuses on a method for computing the impact of structural
deformations on ray tracing for the Ariel Space Telescope. These
deformations arise from external factors such as the gravity field
during ground tests and thermal distortions during operational
observations.
Once the ray tracing calculations are completed, the resulting
data is processed to estimate key optical performance metrics,
including the collimated beam, aberrations, spot diagram,
and point spread function. The method presented in this paper,
which is based on a multi-physics approach, effectively addresses
classical geometrical optics challenges once the structural mechanics
solution is obtained. This makes it an ideal tool for a comprehensive
Structural-Thermal-Optical Performance (STOP) analysis.
14145-113
5 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
ARIEL IR Spectrometer (AIRS) is the infrared spectroscopic instrument of the ARIEL mission providing spectroscopy based on two independent channels covering the CH0 [1.95-3.90] µm and the CH1 [3.90-7.80] µm wavelength. The instrument is producing spectrum of low resolutions R>100 in CH0 and R>30 in CH1 on two independent Teledyne H1RG detectors. The Engineering Model is the first model fully representative in terms of performance of the full instrument chain, from optical to detection chain performance. The test bench and the results of the AIRS Engineering Model full instrument characterization of performance are presented in this paper covering the optical and detection chain in a representative environment of the mission.
14145-114
5 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Earth 2.0 (ET) space mission plans to deploy a satellite equipped with six transit telescopes and one microlensing telescope at Sun–Earth L2 halo orbit. The optimal launch window and halo orbit amplitude are analyzed to mitigate stray light interference. The transfer trajectory is optimized to minimize propellant consumption, with a set of orbital parameters obtained initially using backward shooting and refined via differential correction in a forward-design framework. Furthermore, an orbit maintenance strategy is developed, accounting for momentum wheel unloading and solar exclusion constraints. Numerical simulations confirm that the spacecraft can be successfully inserted into the target halo orbit and can maintain operations for more than eight years.
Show Abstract +
The Earth 2.0 (ET) mission is a next-generation Chinese space mission to detect thousands of Earth-sized planets, including habitable Earth-like planets orbiting solar type stars (Earth 2.0s), cold low-mass planets, and free floating planets. The ET mission will enter its Phase C study in 2026. During the Phase B study, detailed design and optimization of the spacecraft system were carried out, and several key aspects were updated to better fulfill the scientific requirements. In particular, the pointing stability requirement has been increased by more than one order of magnitude. This paper presents the progress in the ET spacecraft system design, covering the overall configuration, pointing stability control, scientific data download, and other aspects.
Show Abstract +
The Life 2.0 space mission concept aims to characterize the atmospheres of transiting exoplanets, including Earth-like worlds, in search of biosignatures in the optical. The mission will consist of an array of 900 one-meter space telescopes in Earth orbit, each equipped with a high-throughput (~50%) waveguide-integrated miniature spectrograph (WIMS) and an ultra-low-noise CMOS detector (~0.3 e-). By combining transmission spectra from 900 telescopes, the signal-to-noise of the combined spectrum can reach a similar level as a single 30-meter space telescope, enabling the detection of the faint planetary atmosphere signal, including species such as oxygen, water, ozone; and many other science cases. The array is scalable and mass-producible, enabling low manufacturing and deployment cost for large-scale atmospheric surveys of habitable exoplanets. The mission design and prototype performance will be reported.
14145-117
5 July 2026 • 17:30 - 19:00 CEST
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The PLATO mission requires twenty-four Normal Cameras (NCAMs) to operate coherently for high-precision photometry. To prevent data stream corruption, the Instrument Control Unit (ICU) must align data production to a strict 6.25s acquisition slot. This paper presents a specialized On-Board Control Procedure (OBCP) designed to manage this synchronization. We describe the nominal start-up sequence, utilizing a reference NCAM event to trigger simultaneous observation and hardware compression, ensuring phase coherence. Furthermore, we detail the autonomous FDIR logic executed following an ICU reboot at the L2 Lagrange point. This sequence restores the Payload Configuration Vector (PCV) and re-initializes N-DPUs to re-establish valid data chunking without ground support. Implemented via interpreted OCL scripts, this architecture allows for dynamic decision-making and in-flight updates. We demonstrate how this flexibility ensures robust fault recovery, minimizing scientific downtime.
14145-118
5 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
AIRS is the infrared spectroscopic instrument of ARIEL: Atmospheric Remote‐sensing Infrared Exoplanet Large‐survey mission selected as the Cosmic Vision M4 ESA mission. This mission will perform transit spectroscopy of over a 1000 of exoplanets to complete a statistical survey.
AIRS spectroscopic data will cover the 1.95-3.90 µm (Channel 0) and the 3.90-7.80 µm (Channel 1) wavelength ranges with dispersive elements producing spectrum of low resolutions R>100 in channel 0 and R>30 in channel 1. This article will describe the AIRS optical alignment method and results of the Engineering Model, providing important data for the instrument calibration.
14145-119
5 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
ARIEL, the Atmospheric Remote‐sensing Infrared Exoplanet Large‐survey mission, is ESA’s Cosmic Vision M4 mission and will study the atmospheres of up to 1000 exoplanets. It uses a set of five dichroic filters (D1 to D5) to split the incoming bandwidth of 0.5 to 7.8 μm and will operate between 40 K and 60 K. We will present ongoing efforts of qualification testing of the D1 - D5 dichroics. Our Tests are performed at ambient and cryogenic temperatures and include transmission and reflectivity spectra, the cryogenic shift of the dichroic’s transition wavelength, wave-front error measurements, humidity testing and cryogenic cycling between 37 K and 323 K. We will give a progress report and will elaborate on achieved results, experimental setups and encountered challenges. We will also discuss steps to establish an instrumentation clean room, suitable for flight acceptance testing for in-space instrumentation.
14145-120
5 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The INAF Astronomical Observatory of Palermo has adapted the XACT facility to perform cryogenic testing of the 1-meter primary mirror for ESA’s Ariel mission, which operates at about 55 K. Thermoelastic effects at this temperature require a cryogenic interferometric campaign to recover the WFE and evaluate optical behavior in a representative environment. The facility includes a 2 m × 2 m vacuum chamber with a 1.4 m entrance hatch, a closed-loop helium cryocooler reaching 30 K, and an optical setup based on a 4D interferometer, a hexapod, and a vacuum optical window. The mirror is supported by an isostatic multi-DoF fork mount, with cooling provided through copper plates, heat shields, and thermal straps linked by an aluminum structure. Simulations show thermal gradients below 5 K and mirror temperatures below the required 90 K. The paper presents the setup, test activities, preliminary interferometric results, and related critical issues.
Show Abstract +
Ariel is ESA’s M4 mission dedicated to the large-scale study of exoplanet atmospheres through transit and eclipse spectroscopy, with launch planned for 2031. Its cryogenic payload is built around a fully aluminum, off-axis Cassegrain Telescope Assembly designed for high thermo-mechanical stability at 55 K. The system includes a 1.1-m primary mirror mounted on flexure hinges, a refocusable secondary, and relay optics feeding AIRS and FGS/NIRSpec. The Structural Model has been delivered for the Payload SM Testing Campaign, while the Engineering Model has completed manufacturing and is now in AIV. This paper presents the latest progress in the development, integration, and qualification of the ARIEL Telescope Assembly.
14145-122
5 July 2026 • 17:30 - 19:00 CEST
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To ensure that The Earth 2.0 (ET) transit telescopes achieves the ultra-high-precision photometric capability required for detecting exoplanets, the internal stray light background noise must be suppressed to an extremely low level. This paper aims to complete an efficient stray light suppression design through systematic simulation analysis and verification. Using TracePro optical analysis software, an accurate model of the transit telescope was constructed, incorporating all optical and mechanical components and surface properties (such as the Bidirectional Scattering Distribution Function (BSDF) of black paint coatings). Stray light simulation analysis was conducted using the forward ray-tracing method to identify critical stray light paths. Furthermore, the Point Source Transmittance (PST) values at different off-axis angles of the light source were calculated. The results indicate that the combined effect of multi-stage baffles and highly absorptive coatings significantly suppress
14145-123
5 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The upcoming PLATO mission (Rauer et al., 2025) will, among others, discover and characterize thousands of exoplanets and is designed to reach the regime of Earth-like planets in the habitable zone of solar-type stars. Here we evaluate results of TVAC measurement campaigns performed in three different test houses in comparison to simulations for the characterization of optical ghosts in seven camera flight models and the engineering model. We investigated intensities and geometries of extended and point-like ghosts, emerging from parasitic reflections of incoming light in the optical system, as these can impact the scientific observations of PLATO. We found the ghost intensities to be well within the requirement specifications. The locations and sizes of the ghosts very well agree between the different cameras and with the simulations. Our findings prepare a camera-specific prediction of the ghost intensities and geometries for PLATO in flight.
14145-124
5 July 2026 • 17:30 - 19:00 CEST
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The ARIEL mission's spacecraft employs a bipods structure made of CFRP, titanium, and aluminum to support and thermally isolate the telescope. This paper outlines the current bipod design status at DTU Space. The bipods must combine high stiffness to prevent modal coupling with sufficient flexibility to accommodate thermal distortions. This dual requirement is achieved through cylindrical flexures whose geometry critically affects the mechanical and thermal performance of the bipods. Analysis results evaluating the impact of flexure geometry on stiffness, strength, and thermal conductance are also presented. These results can be used as a guide for future flexure design of optical instrument structures.
14145-125
5 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Correctly estimating the thermal behaviour of surfaces in contact is key to the correct evaluation of the behaviour of an entire assembly. The parameter that describes such behaviour in typical metallic mechanical interfaces is the thermal contact conductance.
In order to thermally evaluate the complex interfaces between Ariel's primary mirror and optical bench - three bolted joints, one of which characterized by a sphere-to-cone interface - a numerical-experimental analysis and correlation had to be carried out. The assembly was analysed at varying preloads in order to obtain a representative TCC vs pressure curve in a wide range of contact pressures.
This paper summarizes the numerical analyses carried out, the experimental setup and test campaign performed to validate them, and the correlation of models.
14145-126
5 July 2026 • 17:30 - 19:00 CEST
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This study addresses the thermal-structural matching challenge faced by the optical system of The Earth 2.0 (ET) Transit Telescope (comprising nine lenses with apertures of 276–344 mm) operating at –15 ℃. An optomechanical design integrating a two-stage flexible support structure with coefficient of thermal expansion (CTE)-matched materials is proposed, coupled with a low-temperature displacement pre-compensation method. By establishing a coupled thermal-structural-optical model, the predicted deformation is used as a feedforward correction in the alignment process to actively compensate for image quality drift under cryogenic conditions. The resulting system achieves an EE90 radius variation of less than 0.5 μm at –15 ℃, significantly enhancing on-orbit stability and providing a valuable reference for the development of similar cryogenic optical systems.
14145-127
5 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Transit Telescope serves as the core payload of the Earth 2.0 (ET) mission, whose scientific capability critically depends on imaging quality. During launch and orbital insertion, the telescope experiences vibration, gravity release, and orbital thermal environments. These loads induce defocus and degradation of imaging quality. Therefore, on-orbit defocus compensation is necessary. This study proposes a thermally driven focus control method to achieve active focusing. Through thermal-structural-optical coupled analysis, a calibration model relating temperature, displacement, and defocus is established. It identifies the structural regions most sensitive to focus changes. And micrometer-level focusing capability can be achieved through thermal control. Simulation results demonstrate that the proposed thermal focusing approach effectively compensates for defocus induced by launch and on-orbit loads. And it meets the imaging accuracy requirements of the Transit Telescope.
14145-128
5 July 2026 • 17:30 - 19:00 CEST
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The ultra-high stability thermal control design for the transit telescope payload of the Space Origin Exploration Program ET2.0. was conducted by leveraging the heat capacity of the controlled system and the heat transfer relationships, the amplitude of temperature fluctuations of the controlled system is gradually reduced to ensure ultra-high precision and excellent temperature stability for both the telescope and the detector. And then a test in the ground simulation system for the space environment was conducted to simulate the real thermal environment of the transit telescope, primary focal plane, and detector, and implemented multi-stage temperature control on the detector substrate. The final test results showed that the temperature fluctuation was controlled within ±3 mK, meeting the index requirement of ±10 mK, and it also exhibited a certain ability to resist environmental temperature fluctuations.
Session PS3:
Posters - Technologies for Detectors and Control Electronics
5 July 2026 • 17:30 - 19:00 CEST
View
Sunday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-129
5 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The InGaAs photodetector used in the VEM and VenSpec-M instruments for NASA’s VERITAS and ESA’s EnVision missions has shown high potential for moderate temperature annealing during our space environment qualification campaign. We propose an annealing scenario that could be applied to the detector and incorporates estimations for galactic cosmic rays (GCR) and solar energetic particles (SEP) events, which are the main causes of increased noise and thus reduced image SNR.
14145-130
5 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
In modern space exploration missions, CMOS detectors are widely used in scenarios such as astronomical observation and deep-space exploration. They need to work stably for a long time in extreme space environments characterized by low temperature, vacuum, and high radiation. When the detector is exposed in the space radiation environment, irradiation by high-energy particles is likely to cause degradation of its performance. Therefore, it is essential to verify performance of the detector through the irradiation test using a CMOS camera with special design. In this talk, we will present the mechanical design of CMOS camera using GS1517 for Irradiation Test, including the vacuum sealing, support structure for the detector inside vacuum Dewar, Titanium Window and Irradiation Shielding.
14145-131
5 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Since its launch, the Hubble Space Telescope’s Advanced Camera for Surveys (ACS) has been exposed to damaging radiation above the atmosphere. We track the degradation of the ACS’ image quality and find the rate of damage to be modulated by 18.5% during an 11-year solar cycle, peaking 430 days after (i.e. out of phase with) solar minimum based on the number of sunspots. We also find that the type of damage is consistent with defects in the silicon lattice that have all stabilised into one of three configurations. To correct for radiation damage in ACS images, we present the Algorithm for Charge Transfer Inefficiency correction (ArCTIc) v7. It models the physical processes that cause radiation damage to manifest in images. By calibrating ArCTIc using the trailing from ‘hot pixels’ and applying it to astronomical images, we correct 99.9 % of trailing in the worst-affected recent data and 99.5% of trailing averaged over the ACS’s lifetime.
14145-132
5 July 2026 • 17:30 - 19:00 CEST
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Rosella delivers the full programmability and performance of traditional large-observatory controllers in a compact, modular, power optimised and radiation-tolerant architecture for space applications. It provides high-speed, low-noise readout of advanced detectors - including Leonardo SAPHIRA eAPD arrays and Teledyne HxRG focal plane arrays - making it a potential detector control solution for small-satellite science missions and future missions like Gaia-NIR. Rosella supports up to 32 video channels with an analog pixel data resolution of 16-bits. Low-noise detector power and bias supplies are provided by a voltage programmable sequencing circuit allowing for control over voltage dependent detector characteristics including avalanche gain. Strategies to enhance tolerance to radiation are discussed. Rosella’s performance characteristic testing results of an engineering model controlling a Leonardo Saphira detector at cryogenic temperatures will be presented.
14145-133
5 July 2026 • 17:30 - 19:00 CEST
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The CubeSpec mission at KU Leuven brings optical spectroscopy to a 12U CubeSat platform to study massive stars, addressing the challenge of integrating advanced instrumentation in a compact, power-limited spacecraft. High pointing stability is achieved through three piezo actuators rotating a Fine Steering Mirror in closed-loop feedback with a Fine Guidance Sensor and actuator strain-gauge readings. The guidance and science detectors use GSENSE2020BSI CMOS sensors, each interfaced by an Artix-7 FPGA and streamed to a Zynq-7000–based payload processor. Additional components include high-voltage piezo drivers, an ADXL355 microvibration experiment, and CSP-based links for onboard communication and science data transfer.
Show Abstract +
We present a technical status on the development of the Power Supply Module (PSM) of the Phasemeter Measurement System (PMS) for LISA. We provide a description of the overall module architecture, input and output connections, updated individual component design, specific progress on housekeeping and OVP/OCP circuitry, and an early design of the custom DC/DC converters necessary for the mission’s high demanding requirements.
14145-135
5 July 2026 • 17:30 - 19:00 CEST
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The Advanced Data Handling Architecture (ADHA) is a collaborative initiative by the European Space Agency, large system integrators, and data handling equipment suppliers to provide a modular and scalable standard for data handling equipment for space applications. The aim of ADHA is to reduce NRE (Non-Recurring Engineering) in flight projects, by providing standard electronics units and modules form-factors, a standard electrical backplane, and a standard procurement and AIT flow -- which is in-line with ESA's objective of reducing spacecraft development time, and promoting faster adoption innovative technologies.
This paper outlines how standardised ADHA-based hardware can be used to realise end-to-end electronics and software designs for different space instrument topologies and classes, including multi-instrument planetary missions, up to large-scale complex deep-space telescopes. The paper also provides example designs, their parameters and performances.
Show Abstract +
The Arrakihs Electronics Box (EBOX), instrument control subsystem for the Arrakihs instrument is presented in this contribution. The EBOX includes redundant Power Supply Units, redundant high-performance quad-core Data Processing Units, redundant milliKelvins stability Thermal Control Units, two Near-Infrared Interfaces to the NIR detector chain processing guide stars windows and full frame pre-processing for non-destructive read-out scheme and a multi-core application software handling the fine-guidance system, multi-accumulation computation and real-time compression.
14145-137
5 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Advanced Data Handling Architecture (ADHA) is an ESA initiative to establish a compact and modular avionics framework for future space missions. Within this architecture, the Payload Interface Controller Unit (PICU) provides centralized instrument control, data handling, and timing distribution. This work presents the design and development efforts of the Payload Controller Module (PCM), a key building block of the PICU responsible for sensor interfacing and payload command management. We outline the PCM’s role within the PICU, the motivation behind its modular design, and the progress toward its engineering model. The work demonstrates how ADHA’s reusable avionics approach can streamline payload development and support a broad range of scientific and Earth-observation missions.
14145-295
5 July 2026 • 17:30 - 19:00 CEST
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We present the characterization results of Nüvü Camēras’ space qualified digital imaging platform, integrated with the Fairchild Imaging’s low noise (<0.25e RMS) HWK4123 9.4-megapixel sCMOS sensor. The imaging system has been designed for challenging missions requiring low read noise and/or high dynamic range, such as SSA, transient imaging or applications requiring daytime and nighttime imaging capability. Environmental testing was performed in TVAC to evaluate performance stability over the imaging system’s full temperature range. In addition, we present radiation response data obtained during a proton irradiation campaign conducted at TRIUMF (British Columbia, Canada), focusing on TID, and single-event phenomena observed in the HWK4123 sensor. These results demonstrate the suitability of the Nüvü Camēras-Fairchild Imaging innovative devices for space missions requiring high-performance wide-field sensing.
Session PS4:
Posters - JWST
6 July 2026 • 17:30 - 19:00 CEST
View
Monday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-138
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The James Webb Space Telescope (JWST) delivers transformative mid-infrared sensitivity for time-series spectroscopy. A new effort is under way to test the performance and scientific potential of the MIRI Low Resolution Spectrometer in fixed-slit mode for time-series observations. Using the slit suppresses the thermal background that currently limits the precision of shallow signals - such as terrestrial exoplanets or faint stars - when using the slitless configuration. A dedicated fixed-slit subarray is also being developed, which could be used to reduce systematics associated with low frame counts in full-array readout mode. Newly acquired full-array calibration data allow direct slit–slitless performance comparisons, identifying regimes where the fixed-slit mode improves the signal-to-noise ratio. This presentation will detail the resulting instrument behavior, key performance gains, and recommended strategies for adopting this new mode once integrated on-board MIRI.
14145-139
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
MIRI, the Mid-Infrared Instrument on the James Webb Space Telescope, provides the only capability longward of 5 µm on the observatory. In this regime, it is providing order-of-magnitude improvements over past facilities in a wavelength range that is challenging or impossible to access from the ground. As such, MIRI occupies a unique parameter space and offers unparalleled capabilities in all areas of astrophysics. Several years into its operational lifetime, we continue to explore the full breadth of MIRI's potential and make operational improvements to MIRI to create new capabilities and enhance its scientific return. In this paper we will describe several such improvements, and their anticipated impact on MIRI and JWST science - focusing on improvements in detector noise performance, improved time-series capabilities, enhanced efficiency and flexibility of coronagraphic imaging, and a wide-field slitless spectroscopy mode.
Session PS5:
Posters - Wide Field and Time Domain Sky Surveys
6 July 2026 • 17:30 - 19:00 CEST
View
Monday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-140
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The HiZ-GUNDAM mission is dedicated to time-domain and multi-messenger astronomy focusing on gamma-ray bursts (GRBs). It is designed to deliver rapid alerts of high-redshift GRBs with photometric redshift provided by MONSTER, a 30-cm visible and near-infrared telescope onboard the satellite. After launch at ambient temperature, MONSTER is cooled to <200 K and its near-infrared detector to <120 K via radiative cooling, enabling high sensitivity in the near-infrared. The telescope employs an athermal design using a single aluminum alloy, ensuring uniform thermal contraction and stable image performance across temperatures. To validate this concept, a breadboard model (BBM) of MONSTER has been built for cryogenic optical testing. Beginning in April 2026, we plan to cool the BBM to operational temperature and conduct optical performance evaluations. This presentation summarizes the current development status of MONSTER, with emphasis on preparations for the BBM cryogenic optical tests.
14145-141
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
HiZ-GUNDAM is a future space mission designed to detect high-redshift gamma-ray bursts (GRBs) using both an X-ray telescope and a five-band visible/near-infrared telescope, MONSTER. Because the satellite’s real-time alert system cannot downlink raw images, image processing must be performed onboard. MONSTER detects roughly one thousand sources in the field of view, one of which is the GRB afterglow. Since transmitting information for all sources may be impossible, the system must identify only a few tens of afterglow candidates. To accomplish this, a lightweight decision-tree algorithm was developed that can run on the onboard computer. Using five-band photometric measurements, it narrows down the candidates to several tens. Using the constructed decision tree, when detector noise is ignored, the true afterglow at z > 6 is included among these selected candidates with nearly 100% probability. In this presentation, I describe the details of this onboard candidate-selection algorithm.
14145-142
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The concept of the HiZ-GUNDAM satellite is to search transients, including gamma-ray bursts (GRBs), with the wide-field X-ray monitor (EAGLE), and then perform autonomous follow-up observations of these objects using the visible and NIR telescope (MONSTER). The MONSTER adopts the Kösters prism for split NIR observation band 0.9-2.5μm into four bands and perform imaging observations simultaneously with a single NIR detector.
We have developed a double Kösters prism and are currently conducting tests and performance evaluations. As a performance evaluation, we tested cooling, irradiation and vibration resistance of adhesive using prism’s bonding points and we designed holding mechanism of prism and detector. Furthermore, we simply measured transmittance of each band of prism. I will describe on the development status and performance evaluation test results of the Kösters prism.
14145-143
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The NASA SPHEREx satellite was launched in 03/2025 to survey the full sky between 0.75 - 5.0 um. The image processing of SPHEREx H2RG detectors includes real-time flagging of transient events during integration. SPHEREx follows a polar orbit passing over the South Atlantic Anomaly (SAA) zone multiple times daily, where the transient counts reach as high as >80% of pixels, depleting the pixel inventory for further calibration. The science pipeline flags for re-observation all exposures taken while in the SAA, as well as any with >10% transients regardless of the spacecraft location. After six months, ~1.5% of the exposures outside of the pre-defined SAA zone were flagged. Most are near the poles; but also adjacent to the edges of the SAA, potentially expanding its boundary. Given the importance of the SAA to designing and operating space instruments, we present here the SAA boundary traced by SPHEREx transient flags as a reference for future missions.
14145-144
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
SPHEREx, NASA’s all-sky spectrophotometric survey mission, maps the sky in 102 spectral channels from 0.75-5 microns at 6.2” resolution from low-Earth orbit using a custom readout of six HAWAII-2RG detectors. The SPHEREx instrument team and Science Data Center have built a robust science data pipeline that includes mitigating image-space artifacts arising from low-level optical and electronic effects. Analysis of first-survey flight data has confirmed predictions for some of these effects, determined differences between the laboratory and flight predictions in others, and even found new artifacts that were unanticipated. This paper will summarize our current understanding of artifacts in SPHEREx images, including image-space artifacts resulting from cosmic rays, crosstalk and unresponsive pixels. We also present mitigation and/or masking strategies implemented to mitigate such effects, and an assessment of the possible implications for other space missions using HAWAII-2RG detectors.
14145-145
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Weak gravitational lensing requires highly accurate galaxy shape measurements, making geometric distortion a critical systematic in wide-field space telescopes. Korsch TMAs offer excellent low-order aberration control but struggle to achieve the low distortion needed for weak-lensing surveys. This work addresses this challenge via three integrated approaches. First, a machine-learning framework identifies low-distortion solutions within wide-field Korsch design space. Second, an end-to-end observation model based on non-sequential ray tracing simulates intrinsic galaxy structure, weak-lensing shear, optical propagation, and pixel sampling in a unified 3D environment. Third, as-built mirror poses from an Integrated Metrology System generate a realistic distortion model. Comparing ML-derived designs and as-built data enables clearer separation of instrumental distortion from true gravitational shear, supporting distortion-controlled telescope development for future weak-lensing missions.
14145-146
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
CuRIOS-ED (CubeSats for Rapid Infrared and Optical Surveys – Exploration Demo) is a 12U CubeSat payload and pathfinder for the CuRIOS constellation, a fleet of CubeSats for optical monitoring of the transient sky. The payload combines a commercial Simera f/6 telescope with a Sony IMX455 CMOS detector in a custom camera housing. The system delivers a 3° field of view. We present the optical AIT workflow and on-ground performance of the telescope–detector assembly. A metrology-based alignment scheme positions the focal plane within the ±50 µm depth of focus, with a mean focus error <5 µm across the 36×24 mm sensor. End-to-end tests on a clean-room bench, using a custom OAP collimator, yield PSFs with core FWHM ≲1 pixel (<1.5″), consistent with the vendor wavefront map. PSF mapping after qualification-level vibration shows no measurable degradation, indicating that the CuRIOS-ED optical payload meets its image-quality budget and is robust against launch loads.
14145-147
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
SIRMOS (Satellite for Infrared Multi-Object Spectroscopy) is a NASA MIDEX mission concept to map the universe in 3D over ~500 cubic gigaparsecs using 100-million [OIII] and H-alpha emission line galaxies at 1< z<4. SIRMOS will probe the cosmic origin by placing constraints on primordial non-Gaussianity, precisely measure the sum of neutrino masses, and differentiate dark energy and modification of general relativity as the cause for the observed low-redshift cosmic acceleration. SIRMOS has a 60 cm aperture telescope with 0.9 square-degree field, and 2.2-million micromirrors on a digital micro-mirror devices (DMD) to provide a programmable reflective slit mask for spectroscopy at R~1300 over 1.25-2.5 microns. The multiplex advantage is 4000 even if the DMD is only 2048 micromirrors long. An alternate design uses a prism instead of a grating. Another uses a microshutter array instead of a DMD. The SIRMOS mission design is presented in a companion paper by Gregory Wirth.
14145-148
6 July 2026 • 17:30 - 19:00 CEST
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We have developed a compact cryogenic system for high precision refractive index measurements of CdZnTe, aimed at supporting the optical design of the GREX PLUS high resolution spectrograph. The system is based on the minimum deviation method and incorporates improved vacuum rotation mechanics, non contact magnetic torque transfer, a low temperature ceramic thrust bearing, and flexible high purity copper thermal links. Together with narrow band mid infrared illumination and liquid nitrogen cooled InSb/MCT detectors using lock in detection, the setup enables stable angle measurements in the 4–20 K temperature range. The achieved accuracy of ∣δn∣<10^(-3) in the 10–18 µm wavelength region meets the requirements for designing high dispersion immersion gratings for space infrared instrumentation.
14145-149
6 July 2026 • 17:30 - 19:00 CEST
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We are developing a high-resolution mid-infrared spectrograph (HRS) with a cadmium zinc telluride (CdZnTe) immersion grating (IG) for the GREX-PLUS mission. The HRS aims to achieve a resolving power of R∼30,000 over 10–18 µm, requiring a high-index material with sufficiently low absorption at cryogenic temperatures. In our previous work, we demonstrated that high-resistivity CdZnTe (∼10^10 Ωcm) satisfies this requirement at ≤20 K. Building on this result, large (∼6 inch) CdZnTe ingots have recently been fabricated, enabling extraction of IG-sized blanks. We report new transmission measurements of 1 and 10 mm-thick samples cut near the extraction region of a large ingot with the same crystallographic orientation as the IG optical axis. The samples show a resistivity of ∼10^9 Ωcm. We also improved thermal stabilization of the measurement system and investigated the rapid increase in transmittance below ∼10 K, possibly due to freeze out of residual electrons.
14145-150
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The stray-light that a telescope receives from a contaminating source is described by the Normalized Detector Irradiance (NDI) function. NDI defines how much stray-light background will be seen at any point in the detector space from any (or every) source in the sky. NDI depends on the angular distance (R), position (roll, ϕ) angle of the source with respect of the detector axes and for especially wide field instruments like WFI, can vary widely as a function of position at the focal plane. Convolving the NDI with the position and flux of nearby stars directly provides a stray-light background correction.
We present the optical model and ray trace results being used to generate a high-resolution NDI maps for the Nancy Grace Roman Wide Field Instrument, and describe the dominant scattering features associated with the structure seen in the NDI maps. These optical models are the core of ROSALIA (ROman Sky Analyst for Low surface brightness Imaging & Astronomy)
14145-152
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
VERTECS is a CubeSat designed to study the Extragalactic Background Light (EBL). We conducted pre-flight performance tests of the optical multi-band camera module installed in VERTECS. The camera module uses a commercially available CMOS sensor controlled by a custom-made image capture board. The sensor temperature is maintained below 0°C by the radiator during the observation in orbit. Through the tests, the detectability of the EBL was assessed while considering radiation effects. The detector noise evaluation showed that the detector noise was dominated by readout noise below 0°C, and the shot noise due to zodiacal light dominates over the detector noise in most observation sky regions. By comparing the noise during the observation with the signal electron count by the EBL estimated through the spectral responsivity evaluation, it was demonstrated that VERTECS can detect the EBL with the sufficient signal-to-noise ratio.
14145-153
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
VERTECS is a compact visible-light astronomical imaging satellite designed to measure the extragalactic background light (EBL). Accurate EBL estimation requires precise foreground light removal, which in turn demands a PSF model that varies smoothly across the field and remains stable under temperature changes. However, VERTECS’s fast F/2 telescope produces undersampled PSFs, making conventional wavefront-sensing methods unreliable. We developed a two-stage approach that combines a 3D convolutional neural network (3D-CNN) with phase-diversity (PD) optimization. The 3D-CNN provides robust initial estimates of eight primary Zernike coefficients from through-focus images, enabling PD to avoid local minima and converge reliably. The resulting field-dependent, temperature-parameterized wavefront model reproduces laboratory PSFs and supports accurate foreground light removal for VERTECS’s EBL measurement. Details of the simulation techniques are presented in the poster.
14145-154
6 July 2026 • 17:30 - 19:00 CEST
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The InfraRed Telescope (IRT) on the THESEUS ESA M7 mission candidate requires precise radiometric calibration to enable accurate localisation and spectroscopy of high-energy transients. We present the conceptual design of the IRT’s LED-based Calibration Unit, developed to provide highly uniform and temporally stable illumination across five NIR bands, compliant with tight volume and critical alignment requirements. The design builds upon the heritage and demonstrated in-flight performance of the Euclid NISP Calibration Unit, offering valuable guidance for stability, packaging, and long-term behaviour of infrared LEDs in space. The resulting concept targets sub-percent radiometric accuracy, supporting THESEUS’s infrared measurement goals and advancing future space-based NIR instrumentation.
14145-155
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The InfraRed Telescope (IRT) of the ESA THESEUS mission is a 0.7m off-axis three-mirror anastigmat optimized for imaging and spectroscopy in the 0.7–1.8 µm range to enable rapid GRB follow-up. We present the optical design and performance analysis of the M7 baseline. The system achieves diffraction-limited quality across both photometric and spectroscopic fields, as demonstrated by EE, spot quality and MTF results. A comprehensive Monte-Carlo tolerance analysis, including manufacturing, alignment and stability, defines feasible tolerances and compensator strategies that keep EED50/EED80 within requirements.
14145-157
6 July 2026 • 17:30 - 19:00 CEST
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The Lazuli Space Observatory is a 3-meter aperture astronomical facility with a suite of instruments that will be utilized for rapid response observations. It is scheduled for launch in 2028. The Widefield Context Camera (WCC) is a 350–1000 nm multi-field imager spanning 35’ x 12’. This instrument provides both fine guidance and science capabilities. It is a mosaic of 23 commercial CMOS imagers with individual photometric filters. Two rows of Sony IMX 455 CMOS sensors will be used as science detectors, with two sensors defocused for wavefront sensing. One row of BAE HWK 4123 qCMOS sensors will be used for guiding and pointing. The HWK 4123 features a sub-electron readout noise (RON) that is pivotal for reaching >99% guide star availability in the field for rapid closing of the observatory fast-steering mirror (FSM) control loop. There are two instrument apertures within the mosaic, passing light to the ExtraSolar Coronagraph (ESC) and the Integral Field Spectrograph (IFS).
Session PS6:
Posters - Exoplanet Time Series II
6 July 2026 • 17:30 - 19:00 CEST
View
Monday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
Show Abstract +
In this paper we present the Fine Guiding System (FGS), one of two scientific instruments on board ESA’s ARIEL mission, scheduled for launch in 2029. ARIEL will study hundreds of exoplanets to characterize their atmospheres, investigate chemical composition, cloud properties, and weather variability. FGS serves a dual purpose: it delivers dedicated scientific measurements through three photometric channels and a low-resolution near-infrared spectrometer, while also supporting the spacecraft with ultra-precise pointing. Following the instrument Critical Design Review (iCDR), the FGS has entered the phase of engineering qualification model integration and flight model preparation, marking a major step toward mission readiness.
14145-159
6 July 2026 • 17:30 - 19:00 CEST
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This paper aims to present a simple way of using outputs of Zemax raytracing to improve prediction of the point spread function of space telescope outputs on Fine Guidance Sensors. This is done both to evaluate changes caused by different spectral type stars as well as variations potentially caused by known models of pointing jitter.
Macros in ZPL language can easily be coded to provide ray incidence on a given surface at a variety of wavelengths and field positions. This provides a reference grid in which a separate accurate pointing model can navigate by switching to the nearest neighbour spot and produce for a given integration time the resulting spot cloud at the detector.
This code procedure also aims to facilitate and optimise of the M2 mirror positioning on the Ariel satellite telescope during Commissioning phase.
14145-160
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Fine Guiding System (FGS) is a highly advanced optical instrument developed by international Consortium led by CBK PAN in frame of ESA ARIEL space mission. Its goal is to observe atmospheres of exoplanes by providing scientific data using three photometric channels (FGS1, FGS2 and VISPhot) and one low resolution spectrometer (NIRSpec). To characterize the optical parameters of FGS, an advanced OGSE system was developed and verified at CBK PAN. The main parts of the system include: OGSE ILU which is responsible for providing proper wavelength and power level of light that will illuminate FGS; OGSE OMA which is used for integration and alignment of FGS; OGSE OMC which is responsible for beam forming in TVAC. This paper provides details on design and verification of each major OGSE subsystem.
14145-161
6 July 2026 • 17:30 - 19:00 CEST
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The Instituto de Astrofísica de Canarias (IAC) is currently working on the development of IACSAT, which is expected to become the first satellite of the IAC’s future space observatory. IACSAT will be capable of performing high-precision photometry in the VNIR and SWIR bands, primarily aimed at confirming Earth-like exoplanets located within the habitable zone of red dwarf stars.
For high-precision photometry using two-dimensional sensors, pointing stability is critical in order to reduce the impact of detector non-uniformity. This work presents a study of the impact of pointing jitter on photometric performance, including both simulation results and laboratory experiments to validate the proposed mitigation strategies and performance models.
14145-162
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Earth 2.0 (ET) mission, led by China, aims to detect over 50000 exoplanets, including potentially habitable Earth-like planets around Sun-like stars (“Earth 2.0s”), cold low-mass planets, and free-floating planets. The mission will employ six 28-cm telescopes to conduct ultra-high-precision photometric monitoring for the detection of transiting planets. To verify that the telescopes can reliably detect exoplanet transit events, we have developed a high-precision photometry testbed. This system evaluates selected CMOS detectors for their ability to detect Earth 2.0 transit signals, specifically those exhibiting photometric variations at the 84-ppm level. This report presents the laboratory data processing and analysis pipeline. Preliminary results show that, for simulated sources equivalent to a 12.5-mag Sun-like star, a photometric precision of 10 ppm can be achieved over a 6.5-hour timescale. Moreover, we have successfully recovered injected Earth 2.0-like transit signals.
14145-163
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Exoplanet Earth Science Survey Satellite (Earth 2.0) is planned to be deployed in a halo orbit around the Sun–Earth L2 point. It will function as a space observatory consisting of six wide - field transit telescopes and one microlensing telescope. By combining the transit and microlensing methods, it will conduct a large - scale survey of terrestrial planets and free - floating planets. The microlensing CMOS camera is assembled from four 9K×9K detectors tiled together with guiding detectors. When combined with high - precision thermal control and readout electronics, it can achieve highly stable photometry with a single - exposure signal-to-noise ratio ≥ 5 for targets of 20.5 magnitude. The relevant key technologies have been validated using a prototype camera, which demonstrates that they meet the requirements of both scientific observations and engineering implementation.
14145-164
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Earth 2.0 (ET) space mission requires ultra-high photometric precision (~84 ppm) to detect Earth-like planets around Sun-like stars via the transit method. This paper presents a ground-based simulation experiment designed to evaluate whether the GSENSE 1081BSI CMOS detectors can meet the mission’s photometric performance requirements.The evaluation focused on three key performance metrics: long-term photometric precision, temporal stability, and the ability to recover injected 84 ppm transit signals of Earth 2.0s. Simulated transit events were introduced into the data to directly assess detection capability at the required precision level. The results demonstrate that the GSENSE 1081BSI detectors satisfy the photometric performance re
14145-165
6 July 2026 • 17:30 - 19:00 CEST
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The Earth 2.0 (ET) mission requires extreme image quality and photometric stability from its scientific CMOS detector, relying on precise photon transfer curve (PTC) gain calibration. Traditional PTC methods ignores nonlinear response and fixed-pattern noise, which introduces systematic errors—especially under low-light conditions and across the full dynamic range.
To overcome this, we propose an improved PTC-based gain calculation method. A highly stable monochromatic light source first calibrates the nonlinear response, enabling a pre-correction that removes associated bias. Pixel-level temporal variance analysis is also applied to suppress fixed-pattern noise in PTC fitting.
Simulations and experiments confirm that this method significantly improves detector characterization confidence and offers more accurate gain results. The approach provides a reliable theoretical foundation for developing and evaluating ultra-high-precision space imaging systems.
14145-166
6 July 2026 • 17:30 - 19:00 CEST
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The research team carried out the development and performance evaluation of a low-noise, high gain-stability camera for transiting photometry. With China's independently developed CMOS sensors as its cores and in response to the needs of high-precision photometry, the camera adopts a multi-sensor stitching scheme with techniques such as low-noise power supplies, vacuum cooling, precise assembly and alignment. Particularly, it has achieved a high stability of gain by optimizing the gain bias circuit and applying a high-precision temperature control for the sensors. With a high-precision photometric platform, the research team conducted long-term observations of a 12.5-magnitude star with the camera. The results show that both the readout noise and dark current are controlled at expected low levels. The camera’s photometric precision enables effective detection of the varied weak light signals caused by transiting of Earth-sized planets.
14145-167
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
PLATO is ESA's M3 mission to detect and characterise exoplanets around bright solar-type stars using high-precision space photometry. The payload includes 26 cameras: 24 Normal Cameras (N-CAMs) for photometry and 2 Fast Cameras for bright targets and guidance. Each N-CAM hosts four CCDs, each read out on two sides. During thermal-vacuum tests, bias and dark frames are acquired to characterise the read-out noise (RON) of each side. The CCD bias exhibits a Line Start Effect (LSE), a column-dependent offset at line start that leads to a systematic overestimation of pixel-to-pixel noise and can cause RON to exceed its requirement. For each side, an LSE profile is derived by averaging bias frames along rows and subtracted before recomputing RON maps. After presenting the general framework and the analysis concept, in this presentation, we show how the LSE mitigation reducing high-noise tails and restoring compliance with the N-CAM noise requirement.
14145-168
Cryo-harness shielding effectiveness assessment for ARIEL mission of the ESA’s Cosmic Vision Program
6 July 2026 • 17:30 - 19:00 CEST
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A simulation campaign has been carried out to assess the shielding effectiveness for the ARIEL mission. The analysis focuses particularly on the most sensitive cryo-cables, located outside the payload and the service module cavity. For all the instrument cable sets, conducted and radiated susceptibility analyses have been performed, including the evaluation of the transfer impedance (Zₜ). Time-domain analyses are also included to test the harness impulsive susceptibility and its response to transients. Special attention is given to the number of bonding connections and the maximum allowable resistance to the spacecraft reference ground. The simulation campaign has been performed using numerical electromagnetic analysis tools based on the Finite Element Method and Transmission Line Theory. The outcome of this study will be used to define appropriate reference requirements for the payload, ensuring that the harness design meets the necessary EM compatibility and performance.
Show Abstract +
ARIEL is the M4 mission of the ESA’s Cosmic Vision 2015-2025 program, whose aim is to chemically characterise by low-resolution transit spectroscopy the atmospheres of over one thousand exoplanets orbiting nearby stars.
ARIEL hosts two scientific instruments, AIRS (ARIEL IR Spectrometer) and FGS (Fine Guidance Sensor) performing spectroscopy and spectro-photometry in the VIS and NIR range. AIRS is managed by an Instrument Control Unit (ICU), a Spacewire/PUS (Packet Utilization Standard) remote terminal, whose architecture and general status will be provided in this paper, including a summary of the main processing tasks implemented on-board its processor, following the closeout of the Critical Design Review (CDR) and the development and testing of the on-board Application SW (ASW) versions for both the Avionic (AVM) and Engineering (EM) models.
14145-170
6 July 2026 • 17:30 - 19:00 CEST
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In this paper we present the current status of the development of the application software of the Instrument Control Unit of the Ariel mission, which has the objective to obtain spectra for a number of transiting exoplanets. The Instrument Control Unit provides Command and Control functionalities for the AIRS spectrograph and the Telescope Control Unit, which is used to control and move the secondary mirror mechanism and provides the telescope temperatures.
We will illustrate the main functionalities of the software as well as the approach we are using for testing at different level, from static analysis to unit tests, to functional tests.
14145-171
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
ARIEL, ESA’s M4 mission launching in 2031, aims to chemically characterise about one thousand exoplanet atmospheres through low-resolution transit spectroscopy using the AIRS (ARIEL IR Spectrometer) and the Fine Guidance Sensor (FGS). Within this context, dedicated Flight Operations Procedures (FOPs) are being developed for the Instrument Control Unit (ICU), which controls AIRS and the Telescope Control Unit (TCU). These structured and traceable procedures support instrument operations from integration and verification to in-flight use. Their development builds on the Full Functional Tests (FFTs), a set of TCL scripts used to verify requirements. The methodology identifies atomic scripts as building blocks for the FOPs, later converted into procedure-management formats for the final implementation of the needed services in the ICU Application Software, including those needed for the FDIR (Fault Detection, Isolation and Recovery).
14145-172
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
In a few years, the ARIEL space telescope will study the atmosphere of hundreds of exoplanets through the ARIEL Infra-Red Spectrometer (AIRS) developed by a French consortium of laboratories.
The AIRS instrument is composed of two detector control unit (DCU) located in the service module of the satellite driving two integrated focal plane assembly (iFPA), which operates at cryo temperatures in the payload module. Right behind the detectors, cold front-end electronics (CFEE) are in charge of amplifying the signals to decrease their susceptibility to external noises through their way to the DCU located in the service module. Thus, French teams needed to find a very low-noise amplifier that could operate at temperatures down to 37K, in the harsh space environment.
This paper will first present the issue encountered with the initial selection (OPA2350) and more extensively describe the results of the long test campaign organized to validate the selection of the OP2192.
14145-173
6 July 2026 • 17:30 - 19:00 CEST
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The Boot Software (BSW) of space instruments is mission-critical, ensuring safe and reliable transition from power-on to operational state. This paper focuses on the BSW developed for the Instrument Control Unit (ICU) of the ARIEL payload of ESA’s M4 mission. An automated validation framework has been implemented to verify BSW functionalities via TCL test sequences, covering key services such as request verification, housekeeping, event reporting, memory and time management, connection tests, and on-board parameter management. The validation campaign has been executed on the Spacecraft Interface Simulator (SIS) and across multiple instrument models, with the current campaign performed on the ICU Engineering Model (EM). Results show improved repeatability, requirement coverage, early anomaly detection, and reduced manual effort, with methodology reusable for regression campaigns, Full Functional Tests (FFT), and future in-flight verification.
14145-174
6 July 2026 • 17:30 - 19:00 CEST
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The PLATO Instrument Control Unit (ICU), the payload’s on-board computer for data handling and lossless compression, has completed its qualification and reached flight status. Developed by INAF and Kayser Italia with contributions from IWF Graz and the University of Vienna, the ICU has evolved from Engineering Models to the Proto-Flight Model (PFM), now integrated into the payload. We present the final ICU configuration and the key results of the PFM functional, environmental, and EMC test campaigns. Particular emphasis is placed on the performance of the hardware–software compression chain, verification of redundancy and SpaceWire interfaces, and validation of the flight Application Software. The results confirm compliance with PLATO requirements and demonstrate full readiness of the ICU for launch.
14145-175
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The ARIEL space telescope (ESA) will study the atmosphere of hundreds of exoplanets through its infrared spectrometer, named AIRS developed by a French consortium of laboratories. To enable this development, CEA teams have worked on a flexible and reliable solution of EGSE.
The EGSE shall allow the full control and readout of the two acquisition chains of the instrument : communication with the AIRS Detector Control Unit (A-DCU), power supply, images and housekeeping data acquisition and their display in real time, data storage and log of all sent commands.
We have build five EGSEs fully integrated into movable racks that can easily follow AIRS on various testing environments.
The software is made of LabVIEW (NI) for the graphic interfaces and Python to build elaborated sequences of tests.
The modularity and parametrization of these EGSEs would enable to adapt the software to next missions which require the same needs.
14145-176
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
To read telemetry and command the actuators of the ARIEL Telescope Assembly during thermal-vacuum chamber tests, an Electrical Ground Support Equipment (EGSE) has been developed to interface with the Telescope Control Unit (TCU). Nominal communication with the TCU is achieved using an Arduino Due board and a low-voltage differential signaling module housed in a dedicated enclosure. The connection between the EGSE and the TCU relies on a differential-signal interface built on the SPI protocol. As a first step, the communication channel was tested using a second mirrored system capable of receiving commands and returning simulated responses. The final system was assembled and tested using the full TCU simulator at the INAF - Arcetri Astrophysics Observatory. A dedicated communication manager was required to schedule tasks, avoid conflicts, and meet the test requirements.
14145-177
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
This paper presents the software modules developed for the “ARIEL ICU–TCU Interface Emulator” (EGSE), designed to support the thermal-vacuum (TVAC) test campaign of the Telescope Assembly of ESA’s ARIEL mission. The emulator implements the ICU–TCU communication link, enabling decoding of telemetry packets, telecommand handling, and the monitoring and control of the TCU during test operations. The GUI provides an integrated environment for configuration, real-time visualization, actuator motion control, telemetry supervision, and automated test procedures. The system was validated first with a data-packet simulator and later with the full TCU simulator at INAF-Arcetri. The emulator enhances test execution efficiency, data accessibility, and provides a scalable framework for future operational procedures.
14145-178
6 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The ET mission will deliver unprecedented time-domain data sets for exoplanets and stellar astrophysics: six 28-cm transit telescopes downlink full-frame images at 15-minute cadence and postage stamps for selected targets, while a 35-cm microlensing telescope returns 10-minute cadence imaging toward the Galactic bulge. With a total data rate of 2500Gb per day and survey scales of >5 million FGKM dwarfs and >30 million bulge stars, the Ground Data Operation Segment (GDOS) is a critical element that transforms raw telemetry into validated science products and provides reliable, timely access for the community. This paper presents: (1) a science-driven requirements analysis; (2) the end-to-end ground processing flows for both the transit telescope array and the microlensing payload; and (3) the design framework for the science database and user service platform.
Session PS7:
Posters - Exoplanet Imaging with the Roman Coronagraph
7 July 2026 • 17:30 - 19:00 CEST
View
Tuesday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-179
7 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
NASA's Roman Space Telescope carries the Coronagraph Instrument to perform the first high-contrast imaging of exoplanets in space. The instrument’s only top-level requirement is to demonstrate a broadband dark zone. The Community Participation Program (CPP) is planning a range of scientific and engineering activities to perform afterward. To provide realistic simulations of Roman Coronagraph performance in these various modes, the CPP’s Hardware Working Group is developing the corgihowfsc software package. This repository is a wrapper combining several other repositories open-sourced by the Roman Coronagraph project and CPP: corgisim for producing realistic images, cgi-howfsc for performing and high-order wavefront sensing and control (HOWFSC), cgi-eetc for exposure time calculation, and cgi-coralign for performing optical calibrations. By using this collection of official modeling tools, the modeling results from the CPP will be the highest possible fidelity.
14145-180
7 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Coronagraphic Instrument on the Roman Space Telescope has a visible polarimetric mode. Accurate calibration of its polarization response is essential for characterizing debris disks, detecting planetary polarization, and diagnosing polarization aberrations. We will observe two unpolarized standards and two polarized standards with intrinsic polarization angles separated by about 45 degrees. These four stars provide the necessary constraints to solve the Mueller matrix such that the known polarization degrees and angles of the standards are correctly recovered. Standards must be single, bright enough for high S/N without saturating, and sufficiently polarized; visibility and operational constraints also apply. From optical catalogs we identified 72 candidates and began a precursor campaign targeting 21 northern objects. Multi-band HONIR polarimetry on the Kanata 1.5 m telescope measures wavelength dependence and enables Serkowski-law extrapolation to the Roman filters.
14145-181
7 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Coronagraph Instrument (CGI) on the Roman Space Telescope will be the first space-based system to demonstrate closed-loop focal-plane wavefront sensing and control, a key step towards HWO. Beyond the baseline Hybrid Lyot Coronagraph, “enhanced modes” are being developed to improve efficiency and science yield. One such mode uses gaussian probes for electric field probing, extending the linear regime and allowing higher probe amplitudes without estimator bias. This may increase signal-to-noise, reduce exposure time, accelerate dark-hole convergence, and extend operation to stars as faint as V~5. The Coronagraph Community Participation Program’s Hardware Working Group is validating this enhancement using the corgihowfsc control software and a PROPER-based optical model of CGI. We show simulation results where this may show faster convergence and resilience to DM nonlinearities, supporting alternative probing as a low-risk, high-gain improvement for Roman CGI and future missions.
14145-182
7 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
NASA’s Roman Space Telescope will feature a pathfinder Coronagraph Instrument to demonstrate advanced high-contrast imaging from space. Roman Coronagraph could obtain imaging and spectroscopy of Jupiter analogs in reflected visible light for the first time. We present the work of developing an open-source simulation package “corgisim” as part of the Roman Coronagraph Community Participate Program. Built on established optical propagation libraries such as PROPER and CGISim, corgisim provides a publicly available Python framework for end-to-end simulations of Roman-CGI observations. The package produces high-fidelity, format-compliant data for pre-launch calibration, pipeline testing, and community applications such as target planning and selection and observation planning. We will give an overview of corgisim’s infrastructure, and current implementation across planned imaging, polarimetry, and spectroscopy modes. We will also provide guidance on how users can employ the software.
14145-183
7 July 2026 • 17:30 - 19:00 CEST
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The Nancy Grace Roman Space Telescope’s Coronagraph Instrument will, for the first time, demonstrate high-contrast imaging with active wavefront control in visible wavelengths from space. In preparation for the Coronagraph’s commissioning and observing programs, the Roman Coronagraph Community Participation Program has developed a target database and associated ecosystem of publicly accessible tools for observation planning and scheduling. The target database includes planet and disk hosts, calibration stars, reference stars, and engineering program targets. The database is designed to operate in conjunction with a variety of tools, including an exposure time calculator, a pointing and keepout calculator, and dynamic completeness calculators for both indirectly detected planetary companions and previously imaged self-luminous planets. We describe the current schema and contents of the database and demonstrate how it and its associated tools are being used for observation planning.
14145-184
7 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Roman coronagraph community participation program has led the development of a python-based, open source data reduction pipeline (corgidrp) to quantify the performance of the Roman Space Telescope coronagraph instrument and to process its data products. Here, we present the astrometric calibration function within the greater data reduction pipeline, outline the methods for computing critical astrometric calibration measurements, and contextualize this calibration process within corgidrp. Additionally, we discuss the results of end-to-end testing and show that all formal requirements for this calibration step are satisfied.
Show Abstract +
The Roman Space Telescope Coronagraph Instrument (CGI) will demonstrate a series of technologies and techniques to enable the direct detection of reflected-light planets with space-based observatories. Among the several available observing modes and coronagraphic devices embarked in CGI, there is a transmissive Zernike wavefront sensor (ZWFS) that can be used to directly measure optical aberrations in the system. In this work, we advocate for the commissioning of this unique observing mode. We investigate the sensitivity of the ZWFS and demonstrate how it can be used for a full observatory characterisation. We use the CGI simulator and other tools developed and supported by the Roman community participation program (CPP). This type of analysis is crucial for understanding the stability of the Roman observatory and to prepare the path towards HWO.
14145-186
7 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Reflected-light polarimetry of an exoplanet helps constrain and break degeneracies in atmospheric properties, and polarized light observations of debris disks enable exploration of the disk’s dust-grain properties. The best-effort polarimetric mode of the Roman Coronagraph Instrument will be able to perform multi-wavelength observations of planetary systems using the Hybrid Lyot Coronagraph (HLC) and the Shaped Pupil Coronagraph (SPC). In this paper, we demonstrate the capabilities of the polarimetric mode of the Roman Coronagraph for targets chosen in the nominal observing plan. We simulate science target observations and calibration products using the corgisim package and perform data reduction and analysis using the corgidrp, incorporating all noise factors and instrumental polarization effects from modeled Mueller matrices. The final retrieved polarization fraction (p) indicates that the polarimetry mode of the Roman Coronagraph Instrument meets the goal uncertainty of ~ 3%.
14145-187
7 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Roman Coronagraph technology demonstration focuses on achieving <1e-7 contrasts within the instrument's dark hole and our ability to detect and characterize properties of faint companions around bright stars. In this talk, I describe results from a study of potential Roman Coronagraph technology demonstration phase observations focused on these goals, informed by the ongoing OASIS survey at the Subaru Telescope. OASIS provides at least three compelling targets for the technology demonstration phase: HIP 71618 B for the core contrast goal, HIP 54515 b for characterizing the system's performance, and HIP 99770 b for atmospheric characterization.
Session PS8:
Posters - Astrometry
7 July 2026 • 17:30 - 19:00 CEST
View
Tuesday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-188
7 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Detecting Earth-like exoplanets requires micro-arcsecond astrometry, which relies on a precisely calibrated focal plane equipped with high-resolution detectors. Accurate calibration depends on characterizing detector imperfections and systematic effects. Optical benches have been developed to assess the sensor’s behavior: an integrating-sphere setup for electro-optical parameters, an interferometric bench for pixel-level geometry, and a star-field projection system for intrinsic distortion. This work presents the characterization benches built for a 46-MP imaging sensor, based on the same technology as the four 220-MP detectors foreseen for the final focal-plane, and the performance metrics obtained from these setups in the context of NASA’s HWO and ESA’s M-class missions. Upgrades will bring the test environment closer to operational conditions: a second 46-MP sensor will be added for multi-detector tests, plus an adjustable-angle fringe-projection system and improved alignment.
Show Abstract +
Differential astrometry measures the position and motion of celestial objects relative to nearby stars. Missions like Hipparcos and Gaia reached microarcsecond precision, and future missions such as NASA’s HWO and ESA’s Theia aim for sub-microarcsecond accuracy, enabling studies of Galactic dark matter and the detection of Earth-mass exoplanets.
This work presents key elements of a high-precision astrometric instrument and the simulations of the calibrations required to reach this accuracy. We characterize the 46Mpx Gigapyx CMOS detector from Pyxalis, showing its strong potential for future astrometric focal planes. Sub-microarcsecond precision corresponds to 10⁻⁵ (HWO) or 10⁻⁶ (Theia) pixels on the detector. It requires micro-pixel mapping of gigapixel-scale detectors and optical distortion calibration thanks to high-order polynomial models. We introduce the IPAG (Grenoble) testbed enabling these measurements.
14145-190
7 July 2026 • 17:30 - 19:00 CEST
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JASMINE (Japan Astrometry Satellite Mission for INfrared Exploration) aims for ultra-high-precision infrared astrometry. Its onboard instrument requires stringent stability, and the infrared detectors must be maintained at 173 K within a 273 K enclosure. The Detector Box Unit (DBU), under conceptual design at the Advanced Technology Center of the National Astronomical Observatory of Japan, provides the cooling function to keep the infrared detectors at required temperature, using a vibration-free thermo-electric cooler (TEC) and a graphite thermal strap with high conductance connecting the DBU and a radiator. The radiator interface limits heat rejection to 12 W at 200 K, where the functionality of the TEC and thermal strap is not guaranteed. We are conducting device-level tests to evaluate their performance and incorporating the results into the DBU design. This presentation reports the design approach and findings from TEC and thermal strap characterization.
14145-191
7 July 2026 • 17:30 - 19:00 CEST
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The paper presents the current status and technological advancements of OCEAN (Orbit Characterization of near-by exoplanetary systems by Astrometric determinatioN) mission. The mission is conceived as a 36 U Cubesat, aiming at rapid implementation with a compact telescope designed for high stability and low sensitivity to perturbations, ensuring 1-μas systematic floor. The payload relies on a single-aperture, highly-stable space telescope enforcing circular symmetry on the whole optical system, down to the detector populating an annular region of uniform diffraction limited imaging. The payload is compact, light, and cheap. OCEAN represents a transformative step toward democratizing space-based based astrometry and exoplanet discovery. The mission combines scientific ambition with engineering pragmatism. It builds on existing CubeSat heritage while pushing the limits of precision and stability, potentially unlocking a new class of affordable, targeted astronomical observatories.
14145-192
7 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
We present a differentiable Fresnel optical model to derive wavefront and pointing stability requirements for the proposed SHERA (Searching for Habitable Exoplanets with Relative Astrometry) SMEX mission, which will use a diffractive pupil for micro-arcsecond relative astrometry of nearby Sun-like binaries to search for rocky exoplanets. Implemented in the dLux framework, the model propagates between the primary pupil, an intermediate pupil at the secondary mirror, and the detector, capturing spatially varying wavefront error (WFE) and beamwalk across the secondary. We perform parameter inference in the eigenbasis of the Fisher information matrix for the joint parameter space to suppress degeneracies that drive astrometric bias. Simulated observing campaigns then map WFE and pointing jitter into astrometric precision, yielding nominal stability requirements consistent with SHERA’s performance goals.
14145-193
7 July 2026 • 17:30 - 19:00 CEST
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The TOLIMAN space telescope mission targets revolutionary performance in precision astrometric monitoring of binary stars to detect orbiting companions at micro-arcsecond levels of precision. A key enabling technology is a 125mm diameter patterned diffractive transmission plate with precisely aligned liquid crystal (LC) axes. Assembly of the flight-ready LC TOLIMAN poses immediate challenges to maintain optical transmitted wavefront quality. Along with this, LC polarisation degradation due to temperature and UV exposure is not well understood in an Earth orbit context. Using an optical testbed at the University of Sydney, this paper presents methodologies and outcomes in the pathway to furnish a flight-qualified LC diffractive pupil.
Session PS9:
Posters - Interferometry
7 July 2026 • 17:30 - 19:00 CEST
View
Tuesday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
Show Abstract +
The Large Interferometer For Exoplanets (LIFE) is a formation-flying mission for enabling the detection and characterization of potentially dozens of Earth-sized planets at thermal infrared wavelengths. The mission will need to sieve science signals which are many orders of magnitude fainter than competing systematics, and the science detector itself will contribute potentially highly variable noise terms. We present requirements for detector read noise, quantum efficiency, and other detector characteristics, for observations of potential LIFE targets. We compare mission needs with detectors available on the market, or in development, and include a discussion of the ramifications on the surrounding mission design. Expected high-level noise budgets and predicted planet yields based on detector type are presented, and we conclude with a discussion of the most relevant future avenues in detector development and eventual integration.
14145-195
7 July 2026 • 17:30 - 19:00 CEST
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Precise optical path length (OPL) control is essential for formation-flying interferometer mission concepts, where independent spacecraft motion continuously perturbs the optical path between collectors. For dual-tracking architectures, in which the delay line rapidly switches between a reference star and a science target, we demonstrate a compact laboratory five-mirror delay-line system capable of continuous OPL measurement and control over several meters. We integrate a tunable laser, used in conjunction with a quadrature-channel interferometer, to directly measure and validate OPL with sub-100-micron accuracy. Our demonstration shows the elements needed for dual-tracking: a continuously adjustable 1-5 m delay line with sub-100-micron control, and reliable switching between the reference and science channels.
14145-196
7 July 2026 • 17:30 - 19:00 CEST
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Distributed optical and infrared interferometry in space combines light from multiple telescopes to reach the angular resolution of a much larger virtual aperture, opening regimes inaccessible to current monolithic or segmented observatories. This paper reviews the evolution of space-based optical/IR interferometry, from early concepts such as Bracewell’s nulling interferometer and Labeyrie’s hypertelescope to major mission studies including Darwin, TPF, SIM, SI, and ST3/StarLight. We examine their science goals, architectures, and the technological and programmatic challenges that limited their implementation. We then highlight 2010s advances in formation flying, precision metrology, nulling and beam-combining testbeds, and hypertelescope prototypes, as well as synergies with ground-based facilities. Finally, we discuss recent mission concepts such as LIFE, SPIRIT, and SPECS, and outline a staged, technology-driven roadmap toward future pathfinder and flagship space interferometers.
Show Abstract +
The STarlight Acquisition and Reflection toward Interferometry (STARI) is a NASA-funded joint mission to advance technology for future space interferometry with two 8U cubeSATs to collect/transfer starlight between each other using a single mode fiber. We present a lab proof-of-concept for a two satellite system demonstrating fiber-coupling and simulations for starlight transmission between satellites.The first payload is the Pupil Transport (PT) that collects the incoming starlight and reflects it into the other spacecraft. The second is the Fiber Injection and Detection (FID) that injects the reflected starlight into a single-mode fiber on the other spacecraft and uses itself as a reference. In the lab set-up, we achieve a 20% match to the simulation results for optimal coupling efficiency. This level of coupling efficiency can then be used in future missions to collect meteorology data on stars and exoplanets using formation flying fiber coupled systems.
14145-198
7 July 2026 • 17:30 - 19:00 CEST
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The Black Hole Explorer is a new mission that will discover and measure a black hole’s photon ring, capturing light that has orbited a black hole. This paper describes the development of the backend electronics of the Black Hole Explorer (BHEX) instrument, which is called the “Signal Processing and Instrument Control Electronics” (SPICE).The functional and physical architecture are described with motivation for their design, including critical trades and design decisions made to satisfy the established SPICE requirements.
14145-199
7 July 2026 • 17:30 - 19:00 CEST
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We introduce a concept study of an extremely large optical infrared space telescope. The main science mission is (1) to spatially resolve nearby exoplanets with habitable surface environment and (2) to map gaseous disk around the first stars in the early Universe. We require a spatial resolution of at least 1 micro arc-second to distinguish the ocean, land, plants, and volcano on the exoplanets at 10 persec from us. Therefore we require a telescope aperture size of at least 100 km. A combination of magnetically controlled formation flights of pico satellites and multiple diffractive optical elements, will enable us to realize such extremely large-aperture space telescope.
14145-200
7 July 2026 • 17:30 - 19:00 CEST
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We present a historical and technical roadmap tracing the evolution of concepts that lead toward future lunar hypertelescopes for ultra-high-resolution optical astronomy. Building on diluted-aperture and interferometric concepts, we exploit recent progress in formation flying, precision metrology and lunar surface operations. The Moon offers unique advantages: seismically quiet ground, no atmosphere, cold traps for cryogenics, and long-term infrastructure potential. These enable sparse to kilometric baseline arrays far beyond Earth-based limits. We review paths from near-term precursor interferometers (10–100 m class) to large hypertelescope networks achieving milli- to micro-arcsecond resolution for direct imaging of exoplanets, stellar surfaces, and compact objects. Key milestones, scientific drivers, and engineering challenges are identified to evolve from current studies toward permanent lunar optical interferometric facilities.
Session PS10:
Posters - Technologies for Spacecraft Pointing and Guiding
7 July 2026 • 17:30 - 19:00 CEST
View
Tuesday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-201
7 July 2026 • 17:30 - 19:00 CEST
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This work presents a compact, ultra-low-SWaP star tracker achieving sub-arcsecond attitude determination. The system is validated using on-sky data from a 40 mm aperture optical assembly, and is expected to achieve an accuracy better than 1″ in LEO and ~0.2″ in GEO. The tracker derives absolute pointing (RA, Dec, and field rotation) by detecting stellar sources, constructing asterisms, and matching them in real time to a reference catalog. It supports both first-fix operation without prior knowledge and fast continuous tracking using previous solutions as priors. Performance is assessed across dense and sparse fields, the galactic plane, and regions significantly affected by dust extinction. Operational factors for LEO, including daylight-side background and Sun-avoidance constraints, are evaluated. Results show that high-accuracy attitude determination is achievable with unprecedentedly low SWaP, providing a strong sensor input for autonomous pointing control in future missions.
14145-202
7 July 2026 • 17:30 - 19:00 CEST
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The precision image stabilization subsystem of the large space astronomical telescope usually incorporates a fast steering mirror(FSM) and several fine guide sensors (FGS). The Fine Guide Sensor, serving as the detection module of the precision stabilization system, is located at the edge of the main field of view and shares the primary optical system with the main focal plane. The FGS first carries out the high-frame-rate star target extraction and positioning, then calculates these extracted star points to output both relative attitude information (line-of-sight deviation of the space telescope) and absolute attitude information (three-axis orientation of the telescope). The piezoelectric-driven large-aperture fast steering mirror, serving as the actuator in the precision image stabilization system, is responsible for compensating line-of-sight deviations and fine pointing adjustment.
14145-203
7 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The TOLIMAN mission aims to detect rocky, habitable-zone planets around nearby binary star systems using a 125mm diameter telescope onboard a 16U spacecraft in low Earth orbit. Achieving the mission’s science goals requires pointing accuracy better than 2 arcseconds and pointing stability below 1 arcsecond per second. This work presents the design of a novel fine-pointing system to meet these strict pointing requirements. The system will utilise piezo actuators to stabilise and correct the pointing of the telescope throughout imaging.
14145-204
Ultra-high precision fine guidance sensor design and simulation for the Earth 2.0 (ET) Space mission
7 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Ultra-High Precision Fine Guidance Sensor Design and Simulation for the Earth 2.0（ET） Space Mission will be reported
14145-205
7 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
CubeSpec is a 12U CubeSat scheduled for launch in 2027 as an in-orbit demonstrator for high-resolution astrophysical spectroscopy. With a pointing stability expected to be around 1 arcmin, its excellent attitude determination and control system (ADCS) remains to ensure the targets remain focussed in the 2.5 x 6.5 arcsec entrance slit of the spectrograph.
CubeSpec therefore incorporates a secondary pointing subsystem, the High Precision Pointing Platform (HPPP), which employs a closed-loop tip–tilt mirror coupled with a dedicated fine-guidance sensor (FGS). Accurate modelling of the FGS response is essential for predicting the achievable pointing performance.
In this paper, we present an image-simulation tool developed for the FGS, together with a performance assessment of the HPPP. The analysis combines simulated sensor data with hardware test results obtained at both the ADCS and HPPP levels, providing an end-to-end evaluation of the system’s expected on-orbit behaviour.
Show Abstract +
The guide star acquisition process for the Arrakihs Fine Guidance System (FGS) and its performance are presented in this contribution. The acquisition autonomously selects guide stars within the field of view, instead of relying on information pre-prepared on ground. The FGS measurements produced by the Arrakihs Common Data Processing Unit’s (CDPU) Instrument Application Software (IASW) are essential for achieving the unprecedented surface brightness targeted by the mission.
14145-207
7 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
InfraTracker delivers a low-cost, first of its kind visible and infrared light star tracker assembly that increases performance while lowering resource usage for the cutting edge of defense and space research. The mission is focused on designing a compact, low-cost, and reusable star tracker using visible to near infrared light, from primarily COTS components. InfraTracker will utilize a Terrier-Improved Malemute sounding rocket out of NASA Wallops Flight Facility (WFF) as part of the RockSat program, allowing for observations to be made above most of Earth’s atmosphere allowing for flight qualification in space.
Session PS11:
Posters - Solar System Exploration
7 July 2026 • 17:30 - 19:00 CEST
View
Tuesday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-208
7 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
This paper presents a temporal stability analysis of the DRAGO-2 SWIR imager's performance, using imagery of the Moon captured in-orbit. Spatial stability (MTF, FWHM) is tracked via cross-validated slanted-edge and lunar-limb methods. Absolute radiometric stability is quantified using multiple full-moon acquisitions and the LIME model. This work introduces a correction for detector-plane scattering using a K0 Bessel-function model. The analysis provides valuable data on instrument degradation, critical for validating design choices for future SWIR space instrumentation and guaranteeing the fidelity of Level 2 scientific data products.
14145-209
7 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Vibrational Circular Dichroism (VCD), measured through the differential absorption of circularly polarized infrared light, provides structural information inaccessible to classical IR spectroscopy. Although well established in laboratory settings, VCD has never been implemented in space or applied to planetary exploration. We outline early design considerations for a conceptual VCD spectro-polarimeter intended for deployment on planetary landers and assess the enabling optical technologies required to support such measurements. These studies are informed by ongoing VCD measurements on commercial instruments and by CHAIS, our assembled laboratory VCD testbed currently undergoing optimisation. This work defines a pathway toward enabling chiral spectroscopy on future planetary missions.
14145-210
7 July 2026 • 17:30 - 19:00 CEST
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Scientists are working to unlock the Sun’s magnetic secrets by studying how light is polarized in different wavelengths. Earlier experiments with the SOHO satellite showed the technique of extreme ultraviolet (EUV) polarization measurement could reveal magnetic fields in the Sun’s corona, but progress has been limited by the lack of sensitive polarimetric instruments. To address this, we have designed and built a polarimeter prototype using three mirrors arranged in a special design. Tested with aluminum mirrors at visible light, the reflection-based polarimeter shows verified results. Future versions will operate in the EUV range, paving the way for direct measurements of coronal magnetic fields.
14145-211
7 July 2026 • 17:30 - 19:00 CEST
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The paper describes the thermo-mechanical framework developed for the DUSTER breadboard, aimed at integrating EMI-sensitive, high-voltage electronics in a configuration that remains practical for assembly and test. The enclosure is built from stacked aluminium frames supporting the DPU, the low- and high-voltage power supplies, and the sensor front-ends. Connector distribution was arranged to limit cable cross-routing and to keep kilovolt-level bias lines away from low-level analog paths. EMC control relies on conductive gaskets at the critical interfaces, while the thermal design follows a staged approach based on board-level conduction, internal heat links, and external baseplate coupling. This made it possible to introduce thermal improvements during laboratory testing without redesigning the enclosure.
14145-212
7 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
We present a comparative engineering roadmap for optical telescopes designed to operate in extreme environments on Earth and the lunar surface, particularly for investigating small Solar System bodies. Drawing on lessons from high-altitude deserts, polar stations, and remote platforms, we propose solutions for lunar-based telescopes to monitor near-Earth space, increase detectability of near-Earth asteroids (NEAs), and improve follow-up. These telescopes will also observe transient phenomena like gamma-ray bursts, supernovae, and variable stars, while providing data on space weather and radiation. The Moon’s stable platform, lack of atmosphere, and continuous observing windows offer unique advantages for long-term monitoring of NEAs, space debris, and other celestial phenomena. This project outlines engineering concepts for precursor lunar telescopes and discusses milestones for transitioning from Earth-based systems to robust, autonomous lunar implementations for continuous operation.
14145-213
7 July 2026 • 17:30 - 19:00 CEST
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The paper presents "HH-SfM" (Hyper-Hemispherical Structure from Motion) a global structure-from-motion algorithm developed for the ESA Daedalus mission to explore and map Moon caves using a robot with a hyper-hemispherical lens system. The goal is to reconstruct the robot’s trajectory and environment during its descent into a lava tube. The system’s rig consists of four cameras, allowing each cave point to be seen by at least three cameras. The algorithm optimizes the rig's position and triangulated points using a global bundle adjustment, incorporating odometry for scale correction. The resulting geometry enables photogrammetric reconstruction for geological analysis and exploration of Moon channels, with potential applications on Earth.
14145-214
7 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Commercial Lunar Payload Services (CLPS) program, a component of NASA’s Artemis program, supports lunar exploration by enabling the delivery of scientific instruments to the Moon through commercial lander missions. GrainCams is a candidate payload developed by the Korea Astronomy and Space Science Institute (KASI), consisting of SurfCam and LevCam to study micro-scale regolith structures and lofted dust near the lunar surface. This presentation introduces the objectives and system design of GrainCams, highlighting its role in advancing surface science investigations on future lunar exploration missions.
Show Abstract +
Compact sensor systems, such as those used in rover missions, can profit from 3D measurement techniques that are both accurate and resource-efficient. The Depth-from-Focus (DFF) method derives depth information solely from variations in focus and requires no additional hardware beyond a camera system. Compared to classic DFF-approaches Deep Depth-from-Focus (DDFF) methods using Convolutional Neural Networks (CNNs) can reduce the number of images needed for depth estimation. This lowers both energy consumption and memory requirements. In this work, a microscope setup was upgraded with a DDFF capability, demonstrating how DDFF can be applied to the measurement of geological samples. A beam splitter enables the microscope to operate in combination with a spectrometer. One potential application is to use depth information obtained via DDFF to provide contextual data for spectral measurements.
14145-216
7 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Venus Emissivity Mapper (VEM) is an IR-spectrometer designed to measure surface thermal radiation. The VEM’s electrical design is tailored to meet the unique requirements of two distinct missions: NASA/JPL’s VERITAS and ESA’s EnVision. The VEM must accommodate varying interface and environmental demands while maintaining high performance and reliability. This dual-mission approach presents significant challenges, including differing power, data handling interfaces, and electromagnetic compatibility (EMC) environments. This paper discusses the differences between the two instrument variants in terms of interfaces and environmental constraints, provides an overview of the general electronics architecture, and highlights mission-specific adaptations. It further details the key challenges encountered during early development—particularly concerning the detector, FPGA and replacement of the hybrid DC-DC converter—before presenting the results of functional and performance tests.
Show Abstract +
VenSpec-H is an infrared spectrometer, part of the EnVision mission of ESA to planet Venus. The core optical part of the instrument needs to be cooled down to -45 °C with a maximum gradient of 2°C, while other parts must stay relatively warm (around 0 °C). This led to a design based on a so-called cold-box-in-warm-box concept with the cold box suspended on top of blade flexures inside the warm box.
The proof of this concept is shown here, reporting on the vibration and thermal-vacuum tests that have been performed on a representative breadboard model and the good correlation between the physical and the numerical models.
14145-218
7 July 2026 • 17:30 - 19:00 CEST
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We report on the VEM structural and thermal HW models developed for early testing of the instrument. Because of the challenging dynamic, shock load, temperature and sun illumination environment expected during the two Venus missions VERITAS and EnVision, this is of high importance, since any necessary design impact must be identified early to allow for adapting the flight model design. Three models are used for our investigations. An instrument structural model to check the dynamic and shock loads and to derive qualification loads for the subsystems. A Focal Plane Assembly Thermal Model to check the thermal behavior along the FPA chain. Finally, a flight-representative VEM baffle model for thermal qualification against sun illumination.
The test results reported shall confirm the current VEM design or provide design adjustments if needed, such that the engineering qualification model can be prepared for manufacturing. EQM qualification shall be done until summer 2027 before VEM CDR.
14145-219
7 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
CONVERGE (COordinated Network for Venus Exploration and Research with Ground Experiments) is a European mission concept that combines an orbiter, a short-lived lander, and a longer-lived passive seismic node to obtain new in-situ measurements from the surface of Venus. The mission targets a geologically young region such as Imdr Regio, one of the proposed “young volcanic rises,” to investigate recent interior activity, surface evolution, and atmosphere–surface interactions.
The lander would perform mineralogical (XRD/XRF) and elemental analyses, atmospheric profiling during descent, and passive seismic monitoring on the surface. Even with a limited lifetime, these measurements would provide critical ground truth for radar, spectroscopy, and atmospheric retrievals from missions such as DAVINCI, VERITAS, EnVision, Venera-D, and the Venus Orbiter Mission, and would inform models of rocky exoplanets observed by PLATO, ARIEL, and NASA’s Habitable Worlds Observatory.
14145-220
7 July 2026 • 17:30 - 19:00 CEST
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Laser heterodyne radiometry (LHR) is primarily used for remote sensing of atmospheric column and molecular densities, specifically trace gases. The technique utilizes the mixing of two radiations: one is sunlight, and the other is a local oscillator, typically a laser tuned to spectral line transitions of interest. In this paper, we demonstrate a mid-infrared coupled LHR system to quantify molecular rotational-vibrational line transitions of methane and water vapor in the spectral region of 3.7 μm and 6.8 μm. We used integrated wavelength-modulation spectroscopy to discriminate overlapping line transitions, thereby improving the fit of the speed-dependent Hartmann-Tran Profile (HTP) lineshape models. The laboratory-based instrumentation can be field-deployed for earth science and planetary applications by simply modifying the solar tracker modules.
14145-221
7 July 2026 • 17:30 - 19:00 CEST
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Future Earth–Moon optical communication requires a telescope that can maintain diffraction-limited performance despite severe thermal fluctuations, radiation, and launch loads. Fine Cordierite®, developed by Kyocera, offers ultra-low CTE, high stiffness, radiation resistance, and machinability for complex structures, enabling monolithic and highly athermal optical systems. However, large monolithic telescopes made entirely of this brittle ceramic had not been realized due to the difficulty of assembling precision optical and structural components. Leveraging two decades of accumulated manufacturing and assembly expertise, Kyocera has successfully developed the first all–Fine Cordierite® telescope. This paper summarizes its design, fabrication, and optical performance.
Session PS12:
Posters - Exoplanet Imaging Mission Concepts and Science Yields
8 July 2026 • 17:30 - 19:00 CEST
View
Wednesday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-222
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Inflatable starshades offer a path to achieving the large apertures required for direct imaging of Earth-like exoplanets without the mass, volume, and deployment complexity of rigid architectures. We present an inflatable starshade design that integrates petal-based torus geometry, Kapton–resin laminates for post-deployment rigidization, and a simplified inflation system, enabling stowage within standard launch fairings. Recent structural and thermal analyses demonstrate that the inflatable framework can withstand lateral and vertical disturbances with acceptable safety margins, while identifying thermal gradients as the primary driver of dimensional instability. A baseline architecture is used to evaluate edge fidelity, deployment repeatability, mass drivers, and shielding strategies. We discuss requirements, risks, and the path toward sub-millimeter precision needed for 10⁻¹⁰ contrast. This work outlines the feasibility and remaining challenges of inflatable starshade
14145-223
8 July 2026 • 17:30 - 19:00 CEST
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The hybrid integration of ground-based telescopes with space-based optical components has the potential for unprecedented observational precision, opening new horizons for scientific discoveries in astronomy. We focus on the first hybrid ground-space observatory dedicated to the search for life beyond Earth-a top scientific priority in modern astronomy. In this talk, we present, on behalf of the KISS team, the findings of our recent study supported by the Caltech KISS program, which outlines a clear implementation plan, mission architecture and workflow for designing and deploying a shared 99 m orbiting starshade to work with large ground-based telescopes equipped with adaptive optics (AO) such as the 39 m ELT, 30 m TMT, 24 m GMT, and 10 m Keck to directly image the first Earth-like planet around a Sun-like star. This approach provides high-contrast imaging and high-resolution spectroscopy, enabling the search for potential biosignatures such as oxygen and water.
14145-224
8 July 2026 • 17:30 - 19:00 CEST
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China has proposed a space telescope with aperture size of 6.6 meters named Tianlin, which is dedicated for the characterization of rocky planets in the habitable zones (HZ) around nearby GK stars. It will be equipped with a low to high resolution spectrograph and a high contrast coronagraph that should allow the delivery of high quality spectrum of exoplanets. We conduct a preliminary simulation of transmission and reflected spectra for Earth-like planets around G, K type stars and perform retrieval analysis of the detectablity of H2O, a key bio-indicating molecule. Our results show that Tianlin has the ability to constrain H2O abundances in the atmosphere of Earth-like planets in most cases.
14145-225
8 July 2026 • 17:30 - 19:00 CEST
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Direct exoplanet imaging mission studies use dynamic completeness, the probability of detecting a planet given prior observations, to guide scheduling and estimate yield. Computing it is challenging: brute-force Monte Carlo is expensive, and common approximations often miss the true evolution of detectability. We analyze the numerical behavior of dynamic completeness, identifying cost- and accuracy-dominant steps, including repeated Kepler-equation solves and the mapping from orbital elements to observables. We further introduce a reduced-order uncertainty-propagation framework that carries orbital and photometric uncertainties through parameter distributions, enabling efficient, uncertainty-aware completeness estimates for the Roman Space Telescope Coronagraph Instrument.
14145-226
8 July 2026 • 17:30 - 19:00 CEST
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Characterizing the atmospheres of Earth-like planets is a key goal of NASA’s next flagship-class astrophysics mission concept, the Habitable Worlds Observatory (HWO). We simulate HWO observations of an Earth-like exoplanet at varying orbital configurations and perform spectral retrievals to constrain the surface and atmospheric composition. The phase angle, like cloud coverage and surface features, acts as a normalizing factor for the spectra. We explore how including the phase angle as a free parameter affects atmospheric and surface retrievals. We discuss how phase angle, surface spectra, and water clouds can harbor significant degeneracies. This will hinder placing potential biosignature detections into the full context of the planet. Further development of retrieval algorithms is necessary before robust statistical constraints can be achieved for terrestrial planets.
14145-227
8 July 2026 • 17:30 - 19:00 CEST
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The Habitable Worlds Observatory will use a coronagraph to block starlight and reveal faint, potentially Earth-like planets around nearby stars, and to spectrally characterize them in search of oxygen, requiring SNR > 10. Achieving this science goal demands suppressing and subtracting residual starlight to a few parts in 10¹².
The challenge is often framed primarily in terms of telescope and instrument stability, the dominant engineering driver for HWO. However, many coronagraphs capable of 10⁻¹⁰ raw contrast are sensitive to details of the astrophysical scene (stellar angular diameter, hot exozodiacal dust, and starspots), which can introduce residual structure in the PSF potentially limiting starlight subtraction to levels above the required few parts in 10¹² and imposing an astrophysical, rather than instrumental, noise floor.
Here we present estimates of this astrophysical noise floor with the baselined HWO coronagraph (AAVC) and evaluate two subtraction techniques: RDI and ADI.
14145-228
8 July 2026 • 17:30 - 19:00 CEST
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In this paper we discuss the statistics of systematic noise (aka speckles) in high-contrast imaging. We start from first principles and derive the probability density function of speckles stemming from various misalignments (wavefront errors or others) in an astronomical observatory equipped with a coronagraph instrument in various cases.We show that this theoretical formalism matches very well diffractive end-to-end simulations of a few possible instrument configurations of the Habitable Worlds Observatory. We then consider the case of normally distributed wavefront errors and show how this formalism simplifies into a concise analytical model that ties together contrast stability, coronagraph sensitivities (calculated using said diffractive models), and wavefront variance. We demonstrate that this analytical model matches very well end-to-end simulations of hypothetical HWO exoplanet observations that use differential imaging for signal discrimination.
14145-229
8 July 2026 • 17:30 - 19:00 CEST
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Evaluating the end-to-end performance of coronagraph designs for HWO will require simulations that span a full multi-year mission timeline. Such simulations must capture instrument performance, evolving astrophysical scenes, and post-processing, generating data volumes that push the limits of current tools. To address this challenge we have developed a new pipeline by linking a new image simulation tool called coronagraphoto to existing HWO mission simulation tools. We will present images representing a complete, multi-year simulated observing campaign by a preliminary HWO design. The dataset consists of thousands of individual frames over multiple photometric bands, capturing the orbital motion of multi-planet systems and multiple noise sources. This work will provide a vital dataset for testing post-processing algorithms and performing trade studies between HWO coronagraph designs. We plan to make this complete dataset publicly available.
14145-230
8 July 2026 • 17:30 - 19:00 CEST
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Sub-Neptune-sized planets are among the most common in our galaxy, yet it is currently unknown what fraction of sub-Neptune sized planets are rocky planets, water worlds, or gas-dominated mini-Neptunes. In addition to helping understand exoplanet formation and diversity, some larger-than-Earth planets with solid surfaces or oceans could support life. The Habitable Worlds Observatory (HWO) could perform atmospheric characterization to distinguish types of sub-Neptunes. We evaluate exoplanet characterization yields for sub-Neptunes utilizing our framework to perform a significant number of end-to-end yield simulations in a multivariate parameter sweep in the NUV, Visible, and NIR. By exploring the wavelength range and spectral quality over a broad architecture space, the multivariate parameter sensitivity reveals the intricacies within the trade space and helps to inform high level science performance requirements for the HWO Solar Systems in Context Working Group.
14145-231
8 July 2026 • 17:30 - 19:00 CEST
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In this paper we present a suite of representative top-level error budgets for the Habitable Worlds Observatory produced by the ULTRA-CT team. This error budget relates the contrast stability (key to exoplanet detection using differential imaging) to the wavefront variance at the entrance of the coronagraph instrument, integrated over a suite of past temporal scales.
Show Abstract +
The Lazuli Space Observatory, part of the Eric and Wendy Schmidt Observatory System, is a 3-meter class astronomical observatory designed for rapid-response observations and precision astrophysics across visible to near-infrared wavelengths with science capabilities that will be transformative in this decade. Onboard Lazuli is a high-contrast imaging system, the ExtraSolar Coronagraph (ESC), that is designed to enable direct imaging and characterization of exoplanets and circumstellar debris disks around nearby stars. The ESC hosts an ultra-high-contrast adaptive optics (AO) system and vector vortex coronagraph (VVC) to enable high-contrast imaging with raw contrasts of 1e-8 and post-processed contrasts approaching 1e-9. In this presentation, we will provide a technical overview of the ESC design and development underway at the University of Arizona and insight into the unique role Lazuli’s ExtraSolar Coronagraph plays in the current astrophysical landscape.
Session PS13:
Posters - Exoplanet Imaging Technology Testbeds
8 July 2026 • 17:30 - 19:00 CEST
View
Wednesday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-233
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
High-contrast exoplanet imaging requires dedicated laboratory testbeds for coronagraph technology development. The CATKit2-High-Contrast-Imaging (CATKit2-HCI) international collaboration unites groups operating coronagraph testbeds using CATKit2, an open-source Python infrastructure controlling hardware via a fast, C++ Client-Server architecture.
Our goal is to develop and share a common architecture and tools across facilities, fostering collaboration and accelerating progress. A key objective is to avoid duplication of effort and facilitate more direct comparison of results obtained at different testbeds. We are developing a common framework for wavefront sensing and control, standardized file outputs, visualization, and performance metrics. Formalized by a Collaboration Agreement, this initiative also facilitates the exchange of students and postdoctoral researchers, and is open to expand to other high-contrast coronagraph testbeds.
14145-234
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
High-contrast imaging for direct exoplanet detection is limited by stellar brightness and wavefront errors. Coronagraphy and wavefront control help reduce these effects and enable contrast levels compatible with current testbeds and future missions such as the Roman Space Telescope.
Within this framework, the MITHiC testbed at the Laboratoire d’Astrophysique de Marseille is being upgraded with a new Spatial Light Modulator (SLM) used as a deformable mirror. It complements the existing setup, which includes a Classic Lyot Coronagraph and a first SLM enabling phase and amplitude control to optimize the dark-hole region. We also implement the Zernike wavefront sensor (ZELDA) to correct low-order aberrations.
This contribution presents recent progress on the MITHiC upgrade and initial results, highlighting its role as a versatile platform for developing advanced high-contrast imaging techniques.
14145-235
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
We report on recent development in using adjoint electric field conjugation (aEFC) on the University of Arizona’s Space Coronagraph Optical Bench (SCoOB). In its current configuration, SCoOB is a charge-6 vector vortex coronagraph outfitted with a Kilo-C microelectromechanical systems deformable mirror capable of achieving sub-10^-8 dark hole contrast at visible wavelengths. In this work, we discuss ongoing efforts in improving adjoint model calibration. Using this improved model, we give an updated comparison between aEFC and iEFC for dark hole digging on SCoOB. Finally, we provide the first demonstration of aEFC on SCoOB in broadband light.
14145-236
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The space coronagraph optical bench (SCoOB) previously demonstrated ~10^-9 narrowband and ~10^-8 broadband contrast performance. In the last year, the testbed has undergone major upgrades, including a 100%-yield BMC Kilo-C deformable mirror, a black silicon pupil stop, wedged quarter wave plate retarders and polarizers, improved sensor cooling, and a microfabricated field stop. In this work, we present the contrast performance of the testbed after these upgrades for three different coronagraph architectures: a) a vector vortex mask with polarization filtering, b) a triple grating vector vortex mask with and without polarization filtering, and c) a carbon nanotube shaped pupil mask. We report the latest broadband performance of the testbed using multi-band electric field conjugation for improved broadband control and wavefront stabilization via Lyot low-order wavefront sensing and control, as well as our progress in pushing toward bluer wavelengths.
14145-237
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
NASA plans to image terrestrial exoplanets with the Habitable Worlds Observatory (HWO). HWO's large primary mirror will most likely be segmented, which introduces extra diffraction in the image. Apodization, either with deformable mirrors or a dedicated mask, is needed to suppress this diffraction. Reflective apodizers for the Roman Coronagraph were flight qualified and demonstrated 4e-9 contrast in vacuum testbeds. In our current work, we aim to show that black silicon apodizers can provide the 1e-10 contrast needed by HWO. Last year for our first milestone, we showed that the incoherent light contribution from scattering off black silicon is negligible for the HWO contrast budget. Our next milestone is to achieve <5e-10 raw contrast on the Decadal Survey Testbed 2 bench in vacuum with a shaped pupil coronagraph. Here we present our most recent testbed results.
Session PS14:
Posters - Wavefront Sensing and Control
8 July 2026 • 17:30 - 19:00 CEST
View
Wednesday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-238
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
An auxiliary optical module aimed at enhancing multi-band capability of wavefront control has been proposed and developed as part of the technological efforts at the coronagraph testbed EXIST (Murakami et al., Proc. SPIE, 2020 and 2024). We expect this technology to enable efficient spectral characterization of exoplanets across a broad wavelength range, as well as planetary surface mapping via multi-band photometric variations. We performed numerical simulations to validate the concept of this optical module. Although the simulations are simplified and preliminary, the results suggest that very high contrast can be achieved simultaneously and independently across multiple spectral bands separated by more than 20% in bandwidth.
14145-239
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
In order to directly image exoplanets, a dark hole is created in the coronagraph science camera image, which is a region where light speckles are minimized to improve the contrast ratio. Creation of a dark hole normally consists of two independent steps: sensing and correction. During sensing, the electric field (EF) in the focal plane is determined, then during correction, a command is applied to the deformable mirror(s) to minimize the EF. The PICTURE-D balloon mission makes use of the linear EF Conjugation (EFC) algorithm for EF correction. However, this algorithm has two limitations: first, the corrections require a nonlinear model, whereas EFC relies on an inverted matrix, and second, EFC may not properly describe the optical system. Therefore, a neural network (NN) is developed for EF correction on PICTURE-D and will target the issue of nonlinearity. It is shown, in simulation, that a NN can obtain a higher contrast ratio after one iteration when compared with EFC.
14145-240
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Liquid crystal display (LCD) panels repurposed as phase-only spatial light modulators (SLMs) offer a low-cost alternative to deformable mirrors for focal plane wavefront control. Building on prior demonstrations of monochromatic speckle nulling, we present the implementation of broadband Electric Field Conjugation (EFC) using a transmissive LCD SLM integrated into a vector vortex coronagraph testbed operating over a finite spectral band. We present the EFC control model incorporating the coupled phase-amplitude behavior and chromatic retardance of the liquid crystal device. We demonstrate a broadband coronagraphic dark hole and quantify its contrast performance, stability, and convergence behavior. These results establish LCD-based SLMs as viable wavefront control elements for broadband high-contrast imaging and provide a scalable pathway for low-cost laboratory testbeds, technology development, and educational instrumentation.
14145-241
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
PICTURE-D is a NASA balloon mission intended to directly image debris disks in nearby star systems. The observatory floats at altitudes up to 40km, above 99% of Earth’s atmosphere. This greatly reduces the effects of atmospheric turbulence and seeing, allowing for much more stable stellar wavefronts. To counteract turbulence, most modern optical telescopes utilize various adaptive optics (AO) systems. Many AO systems observe the incoming signal with wavefront sensors and aim to correct the effects of atmospheric distortion in near real-time with deformable mirrors. Although greatly reduced by altitude, PICTURE-D must still contend with these distortions as well as effects from thermal and mechanical deformations and imperfections in optical components. During three flights in 2019, 2022 and 2025, the mission has collected a vast amount of wavefront sensor data, detailing exactly what errors were present and at what times. We present an analysis of the wavefront distortions and attempt to connect them to various sources both interior to the instrument and exterior from the atmosphere. Emphasis is placed on atmospheric turbulence and the simulation of atmospheric distortions at high altitudes. The feasibility of AO corrections is also discussed, centering on the size of distortions and the timescale over which they vary.
14145-242
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
We present a thermal, structural and optical performance analysis for the Planetary Imaging Coronagraph Testbed Using a Recoverable Experiment for Debris Disks (PICTURE-D), a NASA balloon-borne observatory designed to image dust and debris disks around nearby stars in reflected visible light. Key components of PICTURE-D include a 60 cm off-axis telescope, a vector vortex coronagraph to suppress stellar light, and two MEMS based deformable mirrors for wavefront sensing and control. The balloon flight environment presents key challenges to the stability of the wavefront required for imaging. Low ambient temperature and pressure induce thermo-mechanical deformation of the observatory and limit the performance of the coronagraph. Using an integrated finite element model of observatory plus the coronagraph, we model the thermo-structural evolution of the observatory and assess the coronagraphic performance of the instrument.
14145-243
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Wavefront sensing and control (WFSC) is one of the key techniques for high-contrast imaging of exoplanets, suppressing scattered stellar light caused by wavefront aberrations to generate a dark hole. Speckle Area Nulling (SAN) method is the WFSC technique that does not require an optical propagation model in the high contrast imaging system. We have been developing the enhanced SAN method that can generate dark holes on both sides in the focal plane using two wavefront control devices, such as deformable mirrors. As a result of numerical simulations, the proposed method successfully generated both-side dark holes and achieved the stellar suppression performance equivalent to that of one-side dark hole generated by the conventional SAN method.
14145-244
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Habitable Worlds Observatory (HWO) aims to directly image Exo-Earths 10 orders of magnitude dimmer than their host star. Algorithms such as dark zone maintenance (DZM) have been proposed to mitigate high-order wavefront drifts and maintain contrast. A modal dark zone maintenance (MDZM) approach, which represents and corrects drifting wavefronts in the deformable mirror (DM) actuator basis, has demonstrated improvement in closed-loop contrast performance by a factor of 5 in simulation in 2.5 in hardware. However, these results were confined to narrowband estimation and control. This work expands the MDZM formulation to use broadband images in simulation using the Decadal Survey Testbed (DST) simulator FALCO and in hardware using the In-Air Coronagraph Testbed (IACT) at NASA JPL. The resulting contrast performance is compared to traditional broadband DZM, as well as narrowband DZM and MDZM, across various drift rates and signal-to-noise ratios inside the dark zone of the speckles.
14145-245
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Astro2020 Decadal Survey has identified exoplanet imaging technologies as a top priority, especially for the design of the Habitable Worlds Observatory (HWO), which must image and characterize Earth-like planets. Achieving this goal requires reaching and maintaining an extreme contrast of 1×10-10. The High Contrast Spectroscopy Testbed (HCST) in the Caltech Exoplanet Technology Laboratory (ETLab) is an in-air coronagraphic imaging demonstration testbed. Using a high-order deformable mirror and a vector vortex coronagraph (VVC), HCST has reached 1×10⁻⁸ contrast in broadband light. A low-order wavefront sensor (LOWFS) placed at the VVC reflection now tracks tip/tilt drift. We present results from implementing a tip/tilt control loop at the VVC reflection for the first time. Our results achieve an over 100x suppression of drift frequencies < 1 Hz.
14145-246
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Phase retrieval techniques are utilized to correct low order aberrations originating from misalignments of the optical system in space based telescope concepts. Traditional phase retrieval involves observation of the Point Spread Function (PSF) and a diversity measurement, usually focus diversity although other measures are possible, to reconstruct the incident wavefront at the science detector. We consider a Machine Learning Phase Retrieval model trained originally on simulated data, and then augmented with real focus diversity data from the Tiny Observatory for Telescope Optimization (TOTO) testbed at the University of Arizona. We then compare the performance of the Machine Learning Phase Retrieval method with a traditional phase retrieval technique and assess the difference in performance.
14145-247
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Habitable Worlds Observatory (HWO) coronagraph contrast stability required to differentiate planets from residual speckles in the dark hole and to detect planets with proper signal-to-noise ratio (SNR) drives very tight tolerances for wavefront variation. The wavefront needs to be stable within 10 pm over 10 minutes and the tip-tilt control needs to be at the sub-milliarcsecond level. Here we describe a Lyot-based low-order wavefront sensor (LLOWFS) for the Exploratory Analytic Case 1 (EAC1) design for the HWO using the scalar vortex coronagraph (SVC) to estimate dynamic low-order wavefront aberrations. The LLOWFS uses rejected starlight from the Lyot stop and slightly defocused images to infer thermally induced low-order aberrations. In this paper, we review the theory of LLOWFS operation, describe the LLOWFS algorithm, and summarize various numerical sensitivity studies on sensor performance.
Session PS15:
Posters - Habitable Worlds Observatory Architecture and Technologies
8 July 2026 • 17:30 - 19:00 CEST
View
Wednesday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-249
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Habitable Worlds Observatory (HWO) is a NASA flagship space telescope designed to identify and characterize habitable zone exoplanets and advance our understanding of the universe through general astrophysics observations. Currently in pre-formulation, the project has defined Exploratory Analytic Cases (EACs) to address demanding science objectives while exploring challenging engineering parameters through architecture and trade space studies.
This paper describes the first three EACs and their lessons learned, discusses the integrated modeling pipeline, and shares key trade study results. These findings have guided EACs 4 and 5, which will further explore the trade space and prepare for the baseline design supporting the Mission Concept Review.
Show Abstract +
This paper presents ongoing investigations into the impact of micrometeoroid impacts on contrast stability for the coronagraph observations of the Habitable Worlds Observatory. We propagate properties of micrometeoroid impacts through precise coronagraph models that capture the spatial, diffractive properties of micrometeoroid-induced wavefront changes, as well as the temporal behavior of the spacecraft after impact. These calculations cover the case of micrometeoroid strikes on the telescope optics—primary or secondary. In the first case, the wavefront perturbation associated with the hypothetical impact will be localized on a primary segment or induce a secondary tilt, yielding a beam shear. In the second case, the observatory pointing will be perturbed.
14145-252
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Habitable Worlds Observatory (HWO) requires an ultra-stable optical telescope. Critical to this need is thermos-optical stability of the primary mirror assembly. To meet this need, MSFC’s Center for Mirror System Characterization and Acceptance Testing has developed and demonstrated a picometer sensitivity milli-kelvin thermal modulation test (TMT) method that can measure a mirror’s thermal response to thermal stimuli with a noise floor of 0.2 to 0.5 picometers per mK. Additionally, MSFC has build an 80-cm mini-PTC (Precision Thermal Control) testbed with 25-zones of active thermal control. This paper reviews the TMT method, mini-PTC capability and presents test results from ULE® and borosilicate mirrors.
14145-253
Initial modeling and testbed feasibility studies of WaveDriver: a laser guide star AO system for HWO
8 July 2026 • 17:30 - 19:00 CEST
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The Habitable Worlds Observatory will require >100× greater wavefront stability than achieved by JWST, pushing conventional telescope architectures to picometer-level performance limits. WaveDriver is a mission concept that relaxes these constraints by employing an external laser guide star (LGS) spacecraft flying in formation with HWO to enable wavefront sensing and control. Early results from the High Contrast Testbed demonstrate feasibility of required stability using coronagraphs, multiple deformable mirrors, and a suite of wavefront sensors. We report initial stability metrics, sensor performance comparisons, and an optical model quantifying anisoplanatic errors from finite LGS separation.
This work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. This document number is LLNL-ABS-2013921.
14145-254
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Habitable Worlds Observatory (HWO) has the ambitious goal of directly imaging and characterizing Exo-earths in search of life in the universe. For HWO to achieve this, the observatory requires a robust wavefront control system (WCS) to maintain wavefront stability to roughly 2 pm over up to 1000 seconds. As part of the larger WCS, HWO will employ a laser metrology truss consisting of many laser metrology gauges to measure the relative pose between the primary mirror segments and the secondary mirror. Lockheed Martin has developed laser metrology gauges with pm-class stability using photonic integrated circuit (PICs) heterodyne interferometers. In this presentation, we report experimental measurements of metrology errors internal to our PIC gauges. We also present an architecture study on placement and orientation of metrology gauges to minimize wavefront error. Additionally, we present a technology readiness level assessment and roadmap for achieving a level 5 for the gauges.
14145-255
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Ultrastable Large Telescopes Research and Analysis (ULTRA) program led by BAE Systems Space & Mission Systems continues to press forward with technology advances and system level insights for NASA’s Habitable Worlds Observatory (HWO). The team continues its dual focus on 1) high-fidelity simulation leveraging models provided by NASA to evaluate their capabilities and risks as potential architectures and 2) hardware demonstrations/studies to address high priority technology gaps in stable mirrors, precision thermal control, and ultrastable sensing and actuation. This presentation will summarize recent achievements by this team and how they support the technology and concept maturation of HWO.
14145-256
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
We present an overview of Lockheed Martin’s Disturbance-Free Payload (DFP) system in the context of its application to Habitable Worlds Observatory (HWO), as well as its unique benefits over conventional vibration isolation systems. Recent advancements and enhancements to the DFP system are emphasized, including reduction of voice coil actuator noise, assessing the performance impact of cables that bridge the DFP interface, development of algorithms to handle contingency operation on orbit, fail-safe relatching mechanisms that hold the spacecraft and payload fixed during servicing of the telescope, and plans for DFP as a system to reach Technology Readiness Level (TRL) 5 by October 2029.
14145-257
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
In this paper, we present the research work of the Laboratory of Space Systems and Optomechanics (LASSO) at the University of Arizona on laser-interferometric metrology technologies aimed at enabling picometer-level dimensional stability sensing and sub-nanoradian angular alignment for large, segmented space telescopes such as the Habitable Worlds Observatory (HWO). Central to this effort is the Optical Truss Interferometer (OTI), a compact and modular Fabry-Perot system that can be distributed across the telescope’s primary and secondary mirrors. Laboratory prototypes have demonstrated sub-picometer displacement sensitivity over representative baselines. Current work focuses on extending this performance to meter-scale cavity lengths while reducing the physical footprint and complexity of the optical heads. Altogether, this research addresses critical technology and metrology developments required for future missions like HWO, contributing toward NASA’s Exoplanet Exploration Program.
14145-258
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Architectures are currently being explored for NASA’s upcoming flagship mission, Habitable Worlds Observatory (HWO). Similar to James Webb Space Telescope, the primary mirrors are being designed as segmented rather than monolithic. This introduces the need for non-sequential ray tracing in an optical model. In order to make this conversion process more efficient, a series of macros can be written in CODE V. The programs will turn surfaces from sequential to non-sequential, insert the appropriate number of segments, and automatically generate the required geometries for each part. Considerations include:
• Segment shape
• Gap size between segments
• Segment numbers & orientation composing the full mirror
Session PS16:
Posters - Habitable Worlds Observatory Science Instrument Concepts
8 July 2026 • 17:30 - 19:00 CEST
View
Wednesday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-62
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Habitable Worlds Observatory (HWO) is NASA's planned flagship space telescope, following the James Webb Space Telescope and the Roman Space Telescope, of which launch is scheduled for the 2040s. The HWO will conduct observations in the ultraviolet (UV) to near-infrared (NIR) wavelength range using a 6-meter-class telescope. One of HWO's science goals is to search for Earth-like exoplanets (including the search for signs of life) using a coronagraph, and will also conduct astrophysical and astronomical observations possible in the UV to near-infrared wavelength range. The HWO is a NASA-led mission with an international partnership. At this moment, Japan is considering contributing to the HWO via science, the coronagraph hardware, and UV hardware. We present possible contributions of Japan to the HWO.
14145-259
8 July 2026 • 17:30 - 19:00 CEST
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The primary mission of the Habitable Worlds Observatory (HWO) is to identify and characterise potentially habitable worlds. Spectra across a wide wavelength range are needed to cover multiple spectral features per molecule of interest. An integral field spectrometer (IFS), fed by a coronograph system, can be used to measure spectra from any planets within the nulled field of the coronograph, while also characterizing the residual speckles as a function of wavelength, enabling the contrast ratio to be further enhanced. We present design trades for an infrared IFS (0.8 to 1.7 µm) for the HWO Coronagraph Instrument, including assessment of the relative merits of lenslet and image slicer based architectures. Key requirements include full sampling of the speckle field at all wavelengths, maximized optical throughput, and control of spectral cross talk and stray light. We identify technology developments needed to advance the instrument design to the required technology readiness level.
14145-260
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Dark matter dominates the universe's mass, yet its fundamental nature remains unknown. Competing theories predict different populations of low-mass subhalos (~10^6-10^7 M_sun), below current detection limits (~10^8 M_sun). The upcoming Habitable Worlds Observatory (HWO) could reach this regime, but only if its point spread function (PSF) quality and stability are tightly controlled. We present HWO-SLAPS, a strong-lensing simulation and analysis pipeline that simulates galaxy-galaxy lenses with embedded subhalos, convolves them with a segmented-mirror PSF containing controlled aberrations and temporal drifts, and adds realistic detector noise. Using Fisher-matrix forecasts, we compute detection significance as a function of subhalo mass and PSF stability. We then map minimum detectable subhalo mass versus PSF wavefront error and drift, deriving quantitative PSF stability and engineering requirements for HWO and a general framework linking optics stability to dark-matter science yield.
14145-261
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The HWO Technology Maturation Project Office (HTMPO) recently released a call for US-led studies for instruments for transformative astrophysics, including a NUV/Optical/NIR high spatial resolution imager (HRI). HRI could have many potential modes, including astrometry, imaging, and low-resolution spectroscopy, while also fulfilling the guiding and some wavefront sensing modes for the entire observatory. The proposed HRI concepts are meant to be responsive to a wide range of astrophysics science cases detailed by the community. The call for instrument studies defines bounding conditions for mass, power, and volume, as well as information about the optical, thermal, and mechanical interfaces for EACs 4 and 5. The HRI Coordination Group developed these bounding conditions while incorporating science and engineering feedback, which we include in this presentation. NASA supports collaborative efforts for instrument studies, both internal to the US and abroad.
14145-262
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Habitable Worlds Observatory (HWO) will be the next NASA-led flagship mission, following HST, JWST and Roman. Through support from UKSA, UK community studies of different instrument options defined in the NASA HWO studies are now underway. One of them is a UV Multi-Object Spectrograph instrument. The work is examining the current requirements for such an instrument in line with its science objectives, identifying the key technical capabilities and TRL levels to achieve them. These evaluations are done also considering the potential of an Integral Field Unit Spectrograph instrument for the mission. This work seeks to establish potential international partnerships to fill technology gaps and identify required activities for raising TRLs to flight levels, to bring such a powerful capabilities in HWO to a reality. This paper reports on this ongoing study and its future plans.
14145-263
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
In combination with a starlight suppression system, integral field spectroscopy is a promising technique for characterizing directly imaged exoplanets. In typical implementations, the region of interest around an occulted star is spatially sampled with a microlens array and spectrally dispersed in collimated space. The dispersed light is focused onto a detector to record a grid of spectra that can be remapped to a data cube. Here we describe reflective designs that improve the efficiency of the IFS cameras baselined by recent mission concept studies. By applying anamorphic magnification with freeform mirrors, the number of detector pixels per resolution element can be halved, significantly reducing the integration times needed to detect atmospheric absorption features. We also summarize plans to demonstrate the first combined operation of an IFS with a coronagraph in a vacuum testbed at contrast levels below 1E-9 over a 20% spectroscopic bandpass.
14145-264
8 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Habitable Worlds Observatory (HWO), NASA’s next Astrophysics Flagship mission, will absolutely revolutionize astrophysics, and has the potential to conduct complementary planetary science. A prime opportunity to understand exo-ocean worlds and their habitability can be found in visible-wavelength spatially resolved spectroscopy of solar system bodies. In the case of Europa, there are several absorption and emission features spanning the optical bandpass that offer unprecedented insight into the moon’s surface features, plume activity, and exosphere. HWO's long operational lifespan enables long-term monitoring of transient phenomena like geyser eruptions and surface composition changes. Such observations will provide breakthrough progression toward understanding the extent of interior-surface material exchange, which is essential for determining if they harbor habitable environments. To this end, we present a preliminary visible wavelength integral field spectrograph for HWO.
Session PS17:
Posters - Heliophysics
9 July 2026 • 17:30 - 19:00 CEST
View
Thursday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-265
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The ESA Vigil mission will monitor solar activity from Lagrange point L5 to support space-weather forecasting and heliophysics research. Its Photospheric Magnetic field Imager (PMI) generates filtergrams that exceed the available telemetry, requiring real-time onboard data reduction. PMI employs FPGA-based processing to convert raw images into calibrated, demodulated science products within strict latency and resource limits. This paper describes the front-end pipeline - Accumulator and Pre-processing modules, which transform filtergrams into calibrated polarimetric spectral line profiles through deterministic, parallel execution. Subsequently, they can be transformed into physical parameter maps. Initial results reported at EDHPC (2025) and ADASS (2025) demonstrated real-time throughput and bit-accurate performance. This contribution extends those findings with updated implementations and ongoing enhancements intended to increase the scientific quality and robustness of mission data.
14145-266
9 July 2026 • 17:30 - 19:00 CEST
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The TRUTHS mission, led by ESA, aims to establish a reference standard for Earth’s radiative state, enabling SI-traceable calibration and improving climate data consistency. A key element of its On-Board Calibration System is the Solar Polychromator (SPC), a tuneable bandpass instrument that filters solar radiation across 320–2400 nm for high-accuracy spectral calibration.
This work presents the design and verification of a prototype SPC, developed to validate the optical concept before flight implementation. Laboratory tests using a monochromator assessed wavelength accuracy, spectral resolution (FWHM), and straylight suppression. Results show strong agreement between measured and predicted filtering behaviour, confirming accurate modelling and alignment. A Structural-Thermal-Optical Performance (STOP) analysis demonstrated stability under orbital thermal conditions.
14145-267
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Vigil is an upcoming ESA satellite mission designed to monitor space weather, with a particular focus on the solar corona and the interplanetary space between the Sun and Earth.
This paper introduces the basic design of a Forward Baffle (FB), currently being developed for the Heliospheric Imager (HI) instrument included in the Vigil spacecraft’s payload to observe very faint coronal mass ejections (CME) across a wide field of view.
The wide-angle FB is one of the key optical components of the HI designed to suppress direct stray-light from the solar disk. It consists of a multi-stage diffractive vanes (MSDV) module involving a pyramidal wedge structure with a high-reflectivity surface coating and a dedicated thermo-mechanically stabilized FB supporting assembly providing the required spatial and angular position of the MSDV relative to two observation cameras of the HI instrument. The FB supporting assembly is designed to meet the accommodation constrains of the HI instrument.
14145-268
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Coronal Diagnostic Experiment (CODEX), a solar coronagraph developed by NASA-Goddard Space Flight Center in collaboration with the Korea Astronomy and Space Science Institute (KASI) and the Italian National Institute for Astrophysics (INAF), was successfully operational on-board the International Space Station (ISS) from December 2024 to September 2025. During its nine months of operation, CODEX executed four dedicated radiometric campaigns. These campaigns were crucial for performing in-flight radiometric calibrations, a fundamental step required to convert the measured raw data (counts) into meaningful physical units. The calibration was achieved by repeatedly targeting a select number of bright stars within the instrument’s pointing range, for which well-characterized spectra were available. This presentation describes and analyzes the dataset, methodology, and results of this essential radiometric calibration effort
Session PS18:
Posters - Far Infrared Observatories and Instruments
9 July 2026 • 17:30 - 19:00 CEST
View
Thursday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-269
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
In this presentation, we report on our technical efforts to evaluate and mitigate artifacts that have hindered accurate spectral extraction in AKARI Infrared Camera (IRC) LG2 slit spectroscopy. The AKARI/IRC LG2 slit spectroscopic data suffer from artifacts such as contamination by zeroth- and second-order light in the edge regions of the aperture mask, as well as scattered light produced by the incident beam within the field of view.
To establish a standardized procedure for deriving reliable LG2 slit spectra, we investigate the efficiencies of the zeroth-, first-, and second-order light, the slit properties, the geometry of the aperture mask, and the characteristics of the scattered light. Through these analyses, we develop a robust data-reduction method that eliminates previously uncorrected artifacts and enables accurate extraction of LG2 slit spectra, particularly for diffuse sources.
Show Abstract +
PRIMA is an actively cooled infrared observatory designed to provide the astrophysics community with mid- to far-infrared coverage from 24–265 µm. Its camera, PRIMAger, features a hyperspectral mode (24–84 µm, R ≈ 8) using an LVF and a polarimetric mode with four broadband, polarization-sensitive filters. We present expected detector performance, NEP estimates, filter and LVF characterization, and optical design simulations, along with observing modes and mapping strategies. These results will guide the community in preparing guest observer proposals (75% of PRIMA’s observing time).
14145-271
9 July 2026 • 17:30 - 19:00 CEST
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PRobe far-Infrared Mission for Astrophysics (PRIMA), is an infrared observatory for the next decade, with a 1.8 m telescope actively cooled to 4.5 K, currently in mission concept study of Probe Explorers part of Explorer Program.
PRIMAger, one of two instruments, will provide two channels, hyperspectral from 24 to 84 μm with a spectral resolution R ≥ 8 and polarimetric from 80 to 264 μm.
The Laboratoire d’Astrophysique de Marseille is in charge of the system engineering, of the delivery of the opto-mechanical assembly as well as the integration of the instrument. In this paper we will describe the opto-mechanical design based on off-axis freeform Aluminium mirrors. The mechanical design will be also presented including the carbon fiber bi-pods that allow to maintain and thermally isolate the 1K structure from the 4.5K metering payload structure.
We will present the development plan strategy as well as the overall verification strategy especially the optical alignment and tests.
14145-272
9 July 2026 • 17:30 - 19:00 CEST
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We describe the Engineering Development Unit (EDU) of a novel cryogenic scanning mirror mechanism designed and built by ABB Inc. for SPICA and adopted for the Phase Delay Mechanism (PDM) of the Far-InfraRed Enhanced Survey Spectrometer (FIRESS) instrument on PRIMA. We report on TRL-5 demonstration results from the cryogenic EDU test campaign conducted by Blue Sky Spectroscopy Inc. (BSS) at the University of Lethbridge, verifying the compliance to the challenging SPICA and PRIMA requirements at 4 K (linear stroke, position and velocity stability, low heat dissipation, low magnetic emission, ultra-low photon leakage). The EDU was also integrated into a cryogenic far-infrared post-dispersed polarizing Fourier transform spectrometer designed and built by BSS and successfully tested at the University of Lethbridge to validate the scanning mechanism design.
14145-273
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Earth-like planets emit thermal radiation predominantly in the mid- to far-infrared, spanning roughly 4 μm to 100 μm, with a peak near 11 μm. Despite the scientific importance of this spectral region for habitable world surveys, there are currently very few spectrometers capable of operating in this regime. To address this gap, we present the design, fabrication, and experimental characterization of an air-gapped, silicon-based virtually imaged phased array (VIPA) optimized for mid-IR spectroscopy. The device consists of a 1″ wide, 3″ tall high-purity silicon plate pair with two coating configurations, gold (Au) and titanium nitride (TiN). Using quantum cascade lasers at wavelengths of 14 μm and 17 μm, paired with a THz microbolometer detector array, we characterize the VIPA’s dispersion and evaluate its resolving power. We also develop computational models to simulate the VIPA’s dispersion and expected resolving power, enabling direct comparison with the measured performance.
Session PS19:
Posters - Millimeter and Radio Observatories and Instruments
9 July 2026 • 17:30 - 19:00 CEST
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Thursday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-274
9 July 2026 • 17:30 - 19:00 CEST
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Future space-borne telescopes operating at 5 K and equipped with thousands of bolometers are being developed for CMB polarimetry. To characterize the antenna patterns for each detector, including far sidelobes at −60 dB level, we have studied a two–phase-step phase-retrieval method “PSH-id” (R. Takahashi et al. 2024. SPIE. 13102. 663-676). Applying this method to a scaled LiteBIRD prototype antenna - a crossed Dragone antenna with a 100 mm aperture - at 140-220 GHz, we demonstrated that the differences between the far sidelobes derived from the retrieved field and those obtained from vector near-field measurements below −60 dB.
We present the accuracy of the proposed method by comparing it with other phase-retrieval techniques. We also demonstrate its applicability at 330-500 GHz and on a 200 mm-aperture antenna. From these results, we discuss the factors that affect its accuracy and the systematic effects to which it is more susceptible compared with vector near-field measurements.
14145-275
9 July 2026 • 17:30 - 19:00 CEST
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An astronomical signal can be addressed as a normal random number that follows a Gaussian distribution of its amplitude. The signal is finally sampled, quantized and digitized before spectroscopic or correlation processing at radio telescope. The quantization efficiency is maximized by adjusting the input power to digitizer. The input power to digitizer has been designed to be within the range where the quantization efficiencies meet the sensitivity requirement in radio astronomical observations. However, we must consider not only the sensitivity maximum but also the accuracy or distortion of waves in digitizing. In this paper, we will report the verification tests about the quantization efficiency and the linearity of the input-output response in digitizing. To meet the high precise observation requirement, the digitizer’s input power should be designed to be much lower than the input power at the highest quantization efficiency by taking into consideration the linearity response.
14145-276
9 July 2026 • 17:30 - 19:00 CEST
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Future sub-millimetre optical systems require low-loss, low-reflectance, broadband anti-reflection (AR) coatings, for which interspersed polymer layers with matched refractive indices are a proven option. However, hot-press bonding can change refractive index and deform the optic substrate, degrading lens performance. We address this by annealing the substrate before machining, relieving internal stresses and stabilizing optical properties so the AR-coating process does not distort the lens. We investigate cast polypropylene (CPP) and porous PTFE (pPTFE) as coating materials for UHMWPE optics and identify an optimal annealing cycle enabling reliable fabrication and characterization. Using spectroscopy and an MCMC-based transfer-matrix model, we extract refractive index and loss from 60–900 GHz. These measurements inform optimized 3- and 5-layer AR-coating designs validated on 70 mm pucks and demonstrated on a full-size two-lens system operating over 166–448 GHz.
Session PS20:
Posters - Exoplanet Imaging with Photonics Technologies
9 July 2026 • 17:30 - 19:00 CEST
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Thursday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-277
9 July 2026 • 17:30 - 19:00 CEST
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We are developing coronagraphic segmented phase masks designed for the direct detection and spectral characterization of Earth-like exoplanets. We expect that the segmented phase masks can achieve relatively high core throughput and a small inner working angle (IWA). We have performed numerical simulations to evaluate the core throughput and IWA for segmented phase masks of various orders. Additionally, we simulated observed images for target stars at different distances and spectral types, assuming Earth-like planets in their habitable zones. Development of the phase masks is also underway. We are iteratively designing and prototyping broadband phase masks using three-layer photonic crystals optimized for the visible and near-infrared regimes, and the fabricated masks are evaluated in the laboratory. In this presentation, we will report on the recent activities of our ongoing simulations and mask development efforts.
14145-278
9 July 2026 • 17:30 - 19:00 CEST
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Technology development for the Habitable Worlds Observatory (HWO), particularly coronagraph wavefront measurement and control, remains key for achieving the high contrast imaging and spectroscopy needed to search for and characterize exoplanets. We present simulations of the Photonic-Enabled ExoPlanet Spectroscopic Sensor (PEEPSS), a combined wavefront sensor and science channel which uses a set of photonic lanterns to couple light from the dark hole in the coronagraph focal plane into single-mode fibers and the spectrograph. PEEPSS uses rejected host starlight to aid in wavefront sensing; performing the sensing in the coronagraph focal plane helps eliminate non-common-path errors between the wavefront sensing and science channels. Initial simulations show the lanterns have high coupling efficiency (>=90%) to both the dark hole and off-axis PSFs fed through a simulated coronagraph. Each lantern also acts as a spatial modal filter, aiding in the rejection of unwanted starlight.
14145-279
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Photonic coronagraphy has the potential to dramatically improve our ability to target faint, small-separation exoplanets with future missions such as the Habitable Worlds Observatory. A practical photonic integrated circuit (PIC) coronagraph will need to create a dark zone in multiple output channels (to provide spatial about detected exoplanets) and have finite spectral bandwidth. Previous simulations show that a PIC with a small number of channels can create a ~2% spectral band with ~10^-10 contrast in a single output channel and can create a monochromatic dark zone in multiple output channels in the presence of realistic directional coupler biases. We extend these results to the lab with the AstroPIC Cycle 1 experiment. We first dig a single-channel dark zone with AstroPIC for a 2% band at 1550 nm. We then dig a monochromatic dark zone in 6 simultaneous output channels. We quantify the impacts of noise and model uncertainty on contrast for both scenarios.
14145-280
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Habitable Worlds Observatory (HWO), identified as the top priority flagship for astrophysics in the 2020 Decadal Survey, requires a coronagraph instrument reaching ten orders of magnitude starlight suppression to directly image Earth-like planets. Coronagraphs based on Photonic integrated circuits (PICs) offer potentially game-changing advantages for this mission by combining the efficiency and aggressive inner working angles of advanced nulling architectures with the compactness and reconfigurability of integrated photonics.
This third paper in the series provides an overview of technology development efforts for AstroPIC, a near-infrared photonic integrated coronagraph concept for HWO. We review the design and recent high contrast results for AstroPIC, which reached better than 1e-9 contrast ratios with our silicon PIC prototype, including functional system-level demonstrations with a free-space coupling system. We outline the near-infrared science enabled including compati
14145-281
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Photonic integrated circuits (PICs) can act as coronagraphs by routing telescope light through Mach–Zehnder interfermeter meshes whose phase shifters direct starlight away from the nulled channels. However, imperfections in the PIC limit performance. We investigate hybrid photonic coronagraphs that place a bulk-optic coronagraph upstream, suppressing most starlight before injection and substantially relaxing PIC tolerance requirements.
We test this concept by integrating a NASA Ames AstroPIC device into the UCSC SEAL testbed, performing free-space injection of focal-plane light using a microlens array aligned to on-chip grating couplers . We outline the prototype’s optical, mechanical, and thermal design and report initial throughput, contrast, and stability measurements, comparing direct and hybrid injection. These results probe the feasibility of hybrid photonic coronagraphy for next-generation high-contrast imagers for both ground- and space-based telescopes.
14145-282
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The Habitable Worlds Observatory (HWO) requires an unprecedented contrast of 1e-10 to characterize Exo-Earth atmospheres. Conventional free-space optics struggle with the stability and wavefront error correction needed for this high-contrast imaging, jeopardizing the mission’s exoplanet yield. Integrated photonics (PICs) offer a critical solution, providing superior stability, control, and compactness to boost coronagraph performance.
However, efficiently injecting light collected from the free-space telescope into the micron-scale PIC remains a major technical hurdle that directly limits system throughput. At NASA Ames, the AstroPIC laboratory is dedicated to optimize this injection efficiency. Our research progresses from single-fiber coupling to using a microlens arrays to maximize fill factor. Future efforts include utilizing wavefront information derived from the photonic coronagraph to drive a deformable mirror for active injection optimization into the PIC
Session PS21:
Posters - Exoplanet Imaging: Optics and Deformable Mirrors
9 July 2026 • 17:30 - 19:00 CEST
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Thursday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-283
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
We propose a two-stage coronagraph for high-contrast imaging. The first stage, a Lyot mask coronagraph, reflects the light for tip-tilt control and eliminates most of the light, minimizing scattered light generated by downstream optical elements. The second stage is a vortex phase mask coronagraph equipped with two deformable mirrors. The attenuated electric field from the first stage effectively improves the phase resolution of the deformable mirrors, enabling higher contrast control than conventional single-stage systems.
14145-284
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Diffraction artifacts from aperture segmentation will degrade contrast well above the 10^-10 requirement of the Habitable Worlds Observatory coronagraph instruments. Shaped pupil coronagraphs can theoretically meet this contrast by extinguishing select pupil regions while passing the rest. JPL developed reflective aluminum-coated silicon masks cryo-etched to produce black silicon, a highly absorptive metamaterial. The Roman Space Telescope will flight-qualify these masks at ~10^-8 contrast. Achieving 10^-10 contrast may require mask features only a few wavelengths wide, where mask optical behavior becomes anisotropic and polarization aberrations at reflective–absorptive boundaries cause leakage. We use FDTD simulations to characterize polarization aberrations induced by black silicon masks. We then estimate the resulting contrast degradation, establishing a lower limit on feature size and beam diameter, and explore geometry-tuning strategies to minimize polarization-induced leakage.
14145-285
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The vortex coronagraph offers an efficient solution to starlight suppression: it provides high starlight suppression while maintaining excellent throughput for off-axis sources. The leading approach to fabricate a vortex coronagraph mask relies on liquid crystal polymers (LCPs), producing what is known as the vector vortex coronagraph (VVC). The main limitation of the VVC arises from mask fabrication errors, which result in a contrast floor above the requirements of HWO. Here, we report recent progress at JPL’s Microdevices Laboratory (MDL) toward fabricating VVC masks for HWO.
14145-287
9 July 2026 • 17:30 - 19:00 CEST
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Deformable mirrors (DMs) are critical for coronagraph operations on ground-based telescopes and future missions like HWO and Roman CGI. They enable wavefront control to create a high-contrast “dark zone” (DZ) for detecting faint companions. Achieving contrasts <1e-8 requires precise DM actuator-gain calibration, as picometer-level errors degrade DZ digging efficiency, increase overheads, and tighten stability requirements. Because DM gain varies with stroke, rapid in situ recalibration is needed. Zernike wavefront sensors (ZWFS) offer picometer sensitivity and will likely be onboard HWO, but their use for DM calibration remains unproven and has major operational implications. We present HiCAT testbed results calibrating gain maps for two 952-actuator BMC MEMS DMs with both a Fizeau interferometer and a ZWFS. We show that the ZWFS achieves sub-nm sensitivity and supports gain maps using local linear or quadratic models with implications for final DZ contrast and digging efficiency.
14145-288
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The scientific cases of interest for next-generation space telescopes result in challenging requirements for resolution, contrast and wavefront stability, which must be matched with an effective mission risk and cost mitigation. The integration of a deformable primary mirror with contactless actuators can address these needs by enabling active wavefront control, vibration rejection and weight reduction through the use of lighter materials.
The present work aims to provide a parametric integrated model to simulate the effects of the orbital environment on a space telescope equipped with an active segmented primary mirror. The simulator will compute thermal deformations on the support, disturbance propagation to the optics and the wavefront correction to deliver at the focal plane. Through a trade-off study of orbital and system parameters, the goal of the tool is to investigate the attractiveness of the contactless deformable mirror technology in terms of mission cost and performance.
Show Abstract +
A novel approach to deformable mirror (DM) actuation is presented that overcomes challenges common in current state-of-the-art approaches. DMs are typically actuated by voltage-driven means. The proposed DM utilizes discrete, radiantly heated, thermal expansion pistons as actuators. Multiple thermal expansion pistons sit between a thin mirror and a reaction structure, which also functions as a heatsink. There are "holes" below each piston, allowing radiant heat to be directed to the piston, inducing local thermal expansion. Heat is drained from the piston through physical connection to the reaction structure. The balance between heat input and dissipation rate controls the temperature of the piston, and thus its height. DM sensitivity, response, and recovery time can be tailored by material selection (CTE, specific heat, emissivity, and thermal conductivity) and geometry (thickness shape, and interface cross-section) to optimize performance for the desired application.
14145-290
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Contactless DM systems are widely the state-of-the art for adaptive optics systems of large format ground telescopes, yet their application to space telescopes (for a large format, segmented primary mirror with active optics) remains largely unstudied.
In this contribution present the calibration and laboratory characterization of a contactless deformable mirror prototype for a space telescope segment. The prototype is LATT, the optical surface a 1 mm thick Zerodur mirror with 19 non-contact actuators over its 40 cm diameter. The system is calibrated by adapting existing ground-based calibration techniques for the prototype. The main innovation is in the validation of these techniques in a novel environment: the system is placed in a vacuum chamber and operated in low pressure conditions, in full magnetic levitation, free of any mechanical constraints.
14145-291
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Active mirrors are considered key components for future large aperture space telescopes such as the HWO. Recently, a technology based on contactless active mirrors, developed for ground based observatory, has been proposed and preliminary tested in the lab. In a contactless active mirror, the optical surface is a thin Zerodur glass shell controlled by voice coil actuators and monitored by capacitive sensors; as a result, the optical surface is mechanically decoupled from the support. Such point has relevant implications from a system-wise perspective, as the support structure has no optical specifications any longer: in particular, the support may be extremely light-weighted, while having little to no print-through on the optical surface. The concept has been preliminary demonstrated on a 40 cm diameter prototype with 19 actuators, featuring an areal density as low as 18 kg/m2. In this work we discuss the as-build mass budget and present a roadmap to further improve the mass budget.
Session PS22:
Posters - Exoplanet Imaging: Data Processing and Detectors
9 July 2026 • 17:30 - 19:00 CEST
View
Thursday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
Show Abstract +
Direct imaging of exoplanets requires starlight suppression, which can nominally be done using coronagraphs and deformable mirrors. However, starlight suppression is not perfect and residual speckles still challenge traditional post-processing methods. Recent work has shown that AI-based algorithms, particularly Convolutional Neural Networks (CNNs), can improve exoplanet detection. We extend prior efforts that combined a focal plane wavefront sensor (FPWFS) with an augmented EKF and CNN to detect very dim planets in conditions similar to the Habitable Worlds Observatory. The CNN learns to discriminate noise from injected planetary signals, leveraging drift information captured by the EKF, using the Decadal Survey Testbed. We present the preliminary results and compare performance against traditional high-contrast imaging methods.
14145-293
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Forward-modeling postprocessing approaches use wavefront information to estimate the aberrated stellar PSF, which can be subtracted from a coronagraph image to reduce residual starlight. We simulated a forward-modeling approach that uses a nonlinear optimizer, L-BFGS, to solve for the wavefront phase that will minimize the error between the resulting PSF estimate and the target image. We implemented a bootstrapping method that cycles between optimizing for aberration coefficients, and for pixel-by-pixel phase. This approach kept the solution from straying too far from a realistic wavefront error, and it resulted in a higher planet SNR than point-by-point optimization alone. Our simulations so far show a similar performance to that of ADI and RDI, despite not requiring additional images or moving the telescope.
14145-294
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
The search for biosignatures in potentially habitable exoplanets is one of the major astrophysics’ drivers for the coming decades. It is the prime science case of HWO, a large space telescope that will be equipped with state-of-the art capabilities to directly characterize Earth-like planets in the 2040s. Ahead of this, the Roman Space Telescope will demonstrate critical technologies to reach 1e-8 contrast limits, using wavefront control and optimized coronagraphs for the first time in space.
Given the stringent constraints on wavefront stability required to achieve these unprecedented contrast levels, new observing strategies and data post-processing techniques need to be developed to optimize detection capabilities with these missions.
Here, we introduce the ESCAPE project, which explore new observing strategies that make use of the deformable mirrors to systematically sample wavefront variations during reference star observations to optimize the detection limits at postprocessing.
14145-296
9 July 2026 • 17:30 - 19:00 CEST
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An EMCCD will be used for faint companion detection in the Roman Telescope’s coronograph instrument. As the EM gain increases, the chance of clock-induced charge (CIC) production in the gain register increases, which affects the intended multiplication of charge. I have improved the EMCCD detector simulator used for the Roman Telescope, emccd_detect, so that it accounts for this effect. I demonstrate through maximum likelihood estimation that EMCCD data conform better to the modified probability distribution which accounts for this effect. The use of the modified distribution would in principle improve EMCCD calibration and the accuracy of signal extraction from a frame. I discuss the implementation of this as well as other high-gain phenomena in emccd_detect and demonstrate the enhanced accuracy of the simulator.
Session PS23:
Posters - Optical Technologies and Manufacturing
9 July 2026 • 17:30 - 19:00 CEST
View
Thursday Poster Session schedule and event details
Each day includes a unique set of posters. Poster groupings are listed below by topic.
14145-297
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
In-space assembly of mirrors via the scale-invariant technology of fluidic shaping can enable the paradigm shift from space-borne to space-assembled telescopes, to be iteratively scaled up at a lower cost. Starting from a minimal pathfinder fluidic telescope, we explore some of the potential exo-world science cases made observationally accessible by larger architectures. In particular, we propose to study the feasibility of a dedicated fluidic telescope with an aperture of 3+ m---having assessed the detection limits of the Roman Space Telescope---to conduct a relative-astrometry monitoring campaign on the directly-imaged habitable-zone giant exoplanet candidate α Centauri Ab, in search of Earth-like exomoons. Then, we review the possible discovery and characterization returns of follow-up missions to the Habitable Worlds Observatory (HWO): from variations on the Large UV/Optical/IR Surveyor (LUVOIR) concept to even larger fluidic-telescope architectures.
Show Abstract +
We explore a concept for a giant telescope manufactured in space to enable a primary mirror of 100m diameter. This is combined with a module containing a secondary mirror, correction optics and a prime focus instrumentation, flying in formation at about 1000m from the primary mirror. We assume that deployment of such a large primary mirror in space would require that a large fraction of the system would need to be manufactured in space in order to minimise launch costs, although that trade-off may now be changing with potential advances in heavy-lift capabilities. The enormous challenges of such a project mean that it would be many decades before the technology is possible, but when it is we could have unprecedented angular resolution and sensitivity and consequent breakthroughs in many areas, with exoplanet characterisation being the stand out application. Potential technical solutions are presented, leading to discussion of the potential scientific capability.
Show Abstract +
Membrane mirror technology offers the prospect for future extremely large space telescopes. Utilizing a thin parabolic membrane as primary mirror base, very low aerial weights can be achieved. The flexible nature of those mirrors allows to roll those up for launch un unwrap in orbit. In this paper we will show a proposed foldable structure that can be compactly stared with the mirror in a launcher and deployed in space. With a scaled prototype model, we illustrate the system’s compact stowage and deployment character.
14145-300
9 July 2026 • 17:30 - 19:00 CEST
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We present a 2 meter Silicon Carbide (SiC) Optical Telescope Assembly (OTA) basic design, hosting an active secondary mirror. We show compliance for this design with the scientific performance requirements of both flavors of the mission: Theon and Theon*. Furthermore, we show that the OTA complies with the ESA M-class mission boundaries with respect to mass, volume, and mechanical loads. The OTA weight, including the active secondary mirror, is projected to be less than 400 kg.
Simulations show that the SiC OTA is strong enough to be launched (in a vertical configuration) on both, an Ariane-6-2 and a Falcon 9 - Block 5 launch vehicle.
We finally link this analysis to a split test concept presented in another paper of this conference, and how this concept allows a cost and time optimized manufacturing sequence, minimizing schedule-related risks. [Grupp, et al. 2026 this conference]
Show Abstract +
The Fluidic Telescope (FLUTE) concept enables large-aperture space observatories, overcoming scaling limitations of segmented mirrors by using thin liquid films that naturally form smooth spherical mirrors in microgravity. The ultimate goal is a 50-meter class observatory. We report on the conceptual design for FLUTE-1, a 1-meter aperture technology demonstration mission designed for Low Earth Orbit. The paper presents the conceptual design for the spherical aberrations corrector and the core instrumentation: a Shack-Hartmann wavefront sensor to characterize the fluidic mirror's optical performance, and an imaging camera to obtain the first images and assess imaging performance. FLUTE-1 is a crucial step toward validating fluidic optics for large-scale space astronomy.
14145-302
9 July 2026 • 17:30 - 19:00 CEST
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The Multi-Channel Imager (MCI) is a panchromatic imager that will be deployed in the China Space Station Telescope. It is a powerful near-ultraviolet (NUV) and visible imager on CSST, with a wavelength coverage spanning 255nm to 1000 nm. The MCI high sensitivity, high spatial resolution, and. large field-of-view (FOV) will provide the astronomer with a set of tools for astrophysical. The MCI consists of three imaging channels, which are the NUV channel, the Optical-blue channel and the Optical-red channel, each with its own complement of filters. Each channel of the MCI uses a 9kx9k e2v CCD to cover a 7.5′×7.5′ field of view (FOV). The filter complement, which includes broad, medium, and narrow band filters, naturally reflects the diversity of astronomical programs to be targeted with MCI.
14145-303
9 July 2026 • 17:30 - 19:00 CEST
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We present a concept based on Computer Generated Holograms (CGH) that enables independent testing of the primary mirror (M1) and of the optical path from the Gregorian primary focus, through the secondary, to the final focus behind M1. Although the tests are carried out separately, the CGH configuration and a central reference system link both test lines, allowing highly accurate predictions of the overall Optical Telescope Assembly (OTA) performance. This decoupling of component tests greatly reduces schedule risk and cost. In addition, early use of both paths with the central reference enables rapid creation of CGH-based "as-built" telescope simulators, allowing instruments to be tested individually and early, without needing the OTA itself. The concept aligns with the "new paradigm" proposed by Arenberg, Grupp, and Kellermann [2020, 2022, 2024], which applies modular industrial building-block strategies to space optics to reduce complexity, cost, and risk.
Show Abstract +
On-board infrared calibration sources are essential for space telescopes, but traditional thermal emitters require high power and impose significant heat loads on cryogenic instruments. NIR LEDs offer a low-impact alternative that enables simpler calibration-unit designs suitable for integration near cryogenic detectors. As future infrared astronomy and space instrumentation increasingly rely on highly stable detectors, qualified NIR LED sources will become important for meeting strict calibration requirements. Although Euclid demonstrated the feasibility of LEDs in the 940-1870 nm range, their behaviour under cryogenic, radiation and long-duration conditions still require further characterization to meet space-qualification requirements defined by ESA standards. Selected 700-2500 nm LEDs are characterised through spectroradiometric, radiometric, stability and environmental testing, providing data that will support the qualification of LED-based calibration sources for future missions.
14145-305
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
ZERODUR® is now in its successful 6th decade of continuously controlled production, and the non-proprietary history of these mirrors in space has been published. Over 13 years ago, SCHOTT presented in a conference exhibit, a highly lightweighted 1.2m diameter specimen mirror, 88% lightweighted with a first eigenfrequency of 212Hz. Extreme lightweighting of large ZERODUR® mirrors is available from SCHOTT, augmented by a dedicated 5,000 m2 facility with state-of-the-art environmental controls and machines. In this facility, mirror substrates greater than 4 meters in diameter are produced. ZERODUR®'s material strength has been exhaustively studied, yielding extensive Weibull Statistics consistent with large spaceborne mirrors of other materials. Evidence-based design is possible with SCHOTT's full publication of latest material data on strength, thermal characteristics and environmental resilience plus statistics of 949 1.5-m diameter ZERODUR® mirror blanks for ELT.
14145-306
9 July 2026 • 17:30 - 19:00 CEST
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We introduce a compact hyperspectral camera based on the time-domain Fourier-transform approach, equipped with an ultrastable birefringent interferometer. The time-domain approach enables hyperspectral imaging with shorter acquisition times and higher spectral accuracy compared to standard dispersive optics. We provide experimental proofs of the camera capability by performing remote-sensing measurements in the visible and near-infrared range. Recently we extended the spectral range to the thermal infrared, where vibrational transitions associated with chemical bonds have their absorption. Due to its compactness, lightweight and extreme stability even in harsh environments, the camera is a unique enabling technology for remote unambiguous chemical identification.
14145-307
9 July 2026 • 17:30 - 19:00 CEST
Show Abstract +
Hadamard Transform Spectral Imaging (HTSI) is a signal multiplexing technique used to obtain spectra at every spatial point in the field of view of an instrument, similar to an Integral Field Unit (IFU) spectrograph. The spectra are projected along the rows of a sensing matrix, in this case a Hadamard matrix, by use of multi-slit masks placed at the aperture, which encode the spectra. Taking the inverse Hadamard transform of the resulting observations recovers the spectra. Its main advantage is to provide a signal-to-noise (SNR) increase over direct measurements within the same observation time, where the multiplex advantage is realized. The theory behind HTSI is tested with real world data sets obtained from a laboratory setup and the Southern Astrophysical Research Telescope (SOAR) observatory, and alternative optimal transformations are derived and explored, as well as methods to recover missing data.
Program Committee
Lab. d'Etudes Spatiales et d'Instrumentation en Astrophysique (France)
Program Committee
Inter-Univ. Ctr. for Astronomy and Astrophysics (India)
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