In progress – view active session
Conference 13092
Space Telescopes and Instrumentation 2024: Optical, Infrared, and Millimeter Wave
16 - 21 June 2024 | Room G303, North - 3F
View Session 
Session 1:
Sustainably Developing Technologies and Careers
16 June 2024 • 09:00 - 10:00 Japan Standard Time | Room G303, North - 3F
13092-1
16 June 2024 • 09:00 - 09:20 Japan Standard Time | Room G303, North - 3F
Show Abstract +
NASA’s Astrophysics Division features annual solicitations to fund technology development for future space flight missions. Two major, repeated calls for proposals are the Astrophysics Research and Analysis (APRA) and the Strategic Astrophysics Technology (SAT) opportunities, and there are occasional solicitations for other technology development programs. We will present the paradigm used in these solicitations, including 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. We will discuss anecdotal aspects of NASA’s technology innovation, maturation, and flight pipeline, and how it supports early-career researchers.
13092-2
16 June 2024 • 09:20 - 09:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Pandora SmallSat mission is a NASA Astrophysics Pioneers mission whose goal is to assess the impact of stellar activity on exoplanet transmission spectroscopy. A secondary goal of both the Pioneers program and the Pandora mission is to provide space mission experience to early career participants with a range of expertise including scientists, engineers, and project managers. Pandora is facilitating the involvement of early career participants from undergrad to post-grad through a variety of formal and informal programs including summer internships, year long graduate student shadow opportunities, post-doctoral programs, and formal mission roles. The success of early career participants within the mission is enabled by pairing them with mentors as well as the identification and assignment of responsibilities that match their capabilities with mission needs. We will discuss the details of these programs, lessons learned, and summarize the best practices Pandora has developed which enable us to contribute to the pipeline of scientists and technologists with space mission experience (while simultaneously developing a SmallSat mission).
13092-3
16 June 2024 • 09:40 - 10:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
This paper describes the development of a new system from the vantage point of our previous experience on Chandra and James Webb. We introduce and define what we call the problem of newness, namely system development with an incomplete understanding of the system performance. We will discuss programmatic and technical approaches to maximize engineering productivity in the development of a new complex system like NASA’s Habitable Worlds Observer or other future flagship missions.
Break
Coffee Break 10:00 - 10:30
Session 2:
Mission Concepts with Small Spacecraft
16 June 2024 • 10:30 - 12:10 Japan Standard Time | Room G303, North - 3F
13092-4
16 June 2024 • 10:30 - 10:50 Japan Standard Time | Room G303, North - 3F
Show Abstract +
To address the need for surveys with high-cadence, large area, and long time baselines to study the transient universe, we intend to launch CuRIOS (CubeSats for Rapid Infrared and Optical Surveys), a constellation of several hundred 16U CubeSats that will provide all-sky, all-the-time observations to a depth of 21 Vega magnitudes in the optical bandpass.
A CuRIOS technology demonstrator, known as the CuRIOS-Exploration Demo (CuRIOS-ED), is slated to launch in 2025 as part of the 12U payload. CuRIOS-ED will be used to space-qualify a commercial camera package—the Atik apx60 with Sony IMX455 CMOS detector—for use on the full CuRIOS payload.
In this presentation, we discuss the CuRIOS-ED mission design with an emphasis on the disassembly, repackaging, and testing of the Atik apx60 for space-based. The testing results will include characterization of the IMX455 detector and Atik electronics performance, as well as preliminary environmental testing results.
13092-5
16 June 2024 • 10:50 - 11:10 Japan Standard Time | Room G303, North - 3F
Show Abstract +
CubeSpec is an in-orbit demonstration CubeSat mission in the ESA technology programme, developed and funded in Belgium. The goal of the mission is to demonstrate high-spectral-resolution astronomical spectroscopy from a 6-unit CubeSat. The technological challenges are numerous. The optical payload, consisting of an off-axis Cassegrain telescope and a compact Echelle spectrometer have been designed to fit in a 10x10x20cm volume. The telescope is built entirely from a composite material to limit defocusing when the spacecraft thermal environment changes. Shielding from the Sun and Earth infrared flux is achieved via deploying Earth and Sun shades. The high resolution spectrograph requires arcsecond-level pointing stability. This is achieved using a performant 3-axis wheel stabilised attitude control system with star tracker augmented with a piezo-actuated 3-axis fine beam steering mechanism in the payload. CubeSpec is now starting the implementation phase, with a planned launch in 2025. A qualification and a flight model are now being constructed and tested. In this contribution we will give an overview of the mission, its technologies and qualification status.
13092-6
16 June 2024 • 11:10 - 11:30 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The CANDLE Engineering Demonstration Unit (EDU) was selected by the 2022 APRA program to develop & demonstrate that we can reach the flux accuracy and range required for an artificial star.
A critical issue in producing accurate and reliable flux calibration is systematic effects; adding
This ETU is on the path to provide an artificial star calibration payload outside Earth’s atmosphere with SI-traceable calibration that enables accurate throughput characterization of astronomical and earth science observatories in space and on the ground. Such a payload could be carried independently on a dedicated platform such as an orbiting satellite, e.g. ORCAS, by a star shade at L2, or some other independent platform to enable accurate end-to-end throughput vs. wavelength
calibration that can be measured repeatedly throughout the operational lifetime of an observatory. Once calibrated, the observatory is enabled to carry out astrophysical programs
whose science objectives demand high accuracy and/or high precision observations. One
specific and immediate application is establishing SI-traceable standard stars beyond the
current limited set.
13092-7
16 June 2024 • 11:30 - 11:50 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Line Imaging Orbiter for Nanosatellite-Enabled Spectrographic Surveys (LIONESS) is a 4U cube satellite mission in development at Columbia University, supported for a 2027 launch by the NASA CubeSat Launch Initiative. The student-driven cubesat will host a narrowband integral field spectrograph with a microlens field slicer, drawing inspiration from, and intending to complement Columbia’s ground-based Circumgalactic H-alpha Spectrograph (CHαS) deployed at MDM Observatory. The circumgalactic medium (CGM) may account for up to 90% of a galaxy's mass, yet its properties are not well understood. LIONESS will observe the diffuse CGM in low-redshift galaxies, imaging hydrogen spectra to extract information about gas distribution, mass, composition, and kinematics, and aiming to provide insights into galactic formation and gas flow between the CGM and disk. As a space-based companion to CHαS, LIONESS will offer comparable narrowband H-alpha imaging over a one-degree field of view, with a significantly lower background. We present results from an initial mission concept study, flight hardware plans, and the development of an at-scale optomechanical prototype of the LIONESS spectrograph.
13092-8
16 June 2024 • 11:50 - 12:10 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The exploration of habitable exoplanets and the detection of potential biosignature represent frontier domains in astronomy and space science. Using Earth as a proxy habitable exoplanet, we propose a micro-satellite mission for spectroscopic observations from deep space orbit to Earth. This mission aims to acquire empirical data to validate the completeness of the observation variable framework and the mapping of observational parameters. Such validation serves as essential support for future endeavors in the detection of habitable exoplanets.
Break
Lunch Break 12:10 - 13:30
Session 3:
Time Domain I: Astrometry and Dynamics
16 June 2024 • 13:30 - 14:30 Japan Standard Time | Room G303, North - 3F
13092-9
16 June 2024 • 13:30 - 13:50 Japan Standard Time | Room G303, North - 3F
Show Abstract +
To investigate the evolution of our Galaxy, we plan to measure the distances and motions of stars in the Galactic center region. Additionally, our goal is to detect planets within the habitable zone around mid-M-type stars using transit phenomena.
To achieve these objectives, we launched the Japan Astrometry Satellite Mission for Infrared Exploration (JASMINE) project, targeting a 40 microarcsecond annual parallax measurement and aiming photometric accuracy of less than 0.3% for mid-M-type stars. A conceptual study of the observation instrument was conducted.
As a result, the telescope is designed with high stability in orbit through carefully chosen materials and a special thermal design. A three-year operation is planned to collect sufficient data for annual parallax measurements. The telescope, with a diameter of 36 cm, covers wavelengths from 1.0 to 1.6 microns using InGaAs detectors. This paper will detail how instrument parameters were selected based on scientific objectives.
13092-10
16 June 2024 • 13:50 - 14:10 Japan Standard Time | Room G303, North - 3F
Show Abstract +
With sub-microsecond angular accuracy, the Theia telescope will be able to reveal the architectures of nearby exoplanetary systems down to the mass of the Earth. This research addresses the challenges inherent in space astrometry missions, focusing on focal plane calibration and telescope optical distortion. We propose to assess in a controlled laboratory environment the future feasibility of large-format detectors (50 to 200 megapixels). The aim is to improve the architecture of the focal plane while ensuring that the specifications are met. The use of field stars as metrological sources for calibrating the optical distortion of the field may help to constrain telescope stability. The paper ends with an attempt to confirm in the laboratory the performance predicted by simulations. We will address also the possibility of using such techniques with a dedicated instrument for the Habitable World Observatory.
13092-11
16 June 2024 • 14:10 - 14:30 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The TOLIMAN mission will fly a low-cost space telescope designed and led from the University of Sydney. Its primary science involves an exhaustive search for temperate-orbit rocky planets around either star in the Alpha Centauri AB binary. By performing narrow-angle astrometric monitoring of the binary at extreme precision, any exoplanets betray their presence by gravitationally, engraving a tell-tale perturbation on the orbit. By implementing significant innovations optical and signal encoding architecture, the TOLIMAN space telescope aims to recover such signals with a telescope aperture of only a 12.5cm. Here we describe the key features of the mission: its optics, signal encoding and the 16U CubeSat spacecraft bus in which the science payload is housed - all of which are now under construction.
Session 4:
Far Infrared Mission Concepts I
16 June 2024 • 14:30 - 15:30 Japan Standard Time | Room G303, North - 3F
13092-12
16 June 2024 • 14:30 - 14:50 Japan Standard Time | Room G303, North - 3F
Show Abstract +
With the end of science operations of the airborne observatory SOFIA, the far-infrared wavelength regime between ~30-300 µm has become mostly inaccessible to the international community for at least the next decade. This regime encompasses a range of key observables across multiple spatial scales, covering astrophysical concepts that are required for a comprehensive interpretation of results from the new generation of observatories like JWST. We will overview SOFIA’s science achievements and present a number of major science cases for continuing observational access to the far-IR. We will outline ongoing efforts to preserve the scientific and technological legacy of SOFIA and bridge the gap to the next generation of far-IR missions. Finally, we will overview technical requirements of such missions from a science perspective, and outline our wishes for a future, open-access astrophysical & observational toolbox exploitable by the entire community.
13092-13
16 June 2024 • 14:50 - 15:10 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Single Aperture Large Telescope for Universe Studies (SALTUS) is a proposed NASA Probe class mission that will provide a powerful far-infrared (far-IR) pointed space observatory to explore our cosmic origins and the possibility of life elsewhere. During its 5 year baseline mission, SALTUS will perform groundbreaking studies towards 1000s of astrophysical targets, including the first galaxies, protoplanetary disks, and numerous solar system objects. SALTUS employs a deployable 14-m aperture, with a sunshield that will radiatively cool the off-axis primary to <45K, along with cryogenic coherent and incoherent detectors that span the 34 to 660 𝜇m far-IR range at both high and moderate spectral resolutions. This spectral range is unavailable to any existing ground or space observatory. SALTUS will have 16x the collecting area and 4x the angular resolution of Herschel and is de-signed for a lifetime ≥5 years. With its large aperture and powerful suite of instruments, SALTUS’s observations will provide a giant leap forward in our capabilities to study the local and distant universe.
13092-14
16 June 2024 • 15:10 - 15:30 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The SAFARI-lite instrument on the SALTUS mission with its large 14 meter diameter aperture, will present the astronomical community with an unprecedented observational capability providing extremely sensitive FarIR spectroscopy at high spatial resolution. With the combination of SALTUS’ large collecting area and an array of sensitive Kinetic Inductance Detectors (KIDs) in a compact grating spectrometer configuration the SAFARI-lite instrument will generate R~300 resolution 34-230 μm spectra reaching sensitivities of order 10-20 W/m2 (5σ/1 hour) – an observing capabilityy in the Far Infra-Red domain with both spatial resolution and sensitivity at levels comparable to JWST. The instrument will provide both point source optimized spectroscopy observing modes, as well as spectroscopic imaging for small fields.
With this breakthrough capability astronomers will be able to fully address many fundamental astrophysical issues like understanding the evolution of galaxies over cosmic time, following the distribution and role of water in the evolution those galaxies, and unveiling the formation history of planetary systems in general and our own solar system in particular.
Break
Coffee Break 15:30 - 16:00
Session 5:
Far Infrared Mission Concepts II
16 June 2024 • 16:00 - 18:00 Japan Standard Time | Room G303, North - 3F
13092-15
16 June 2024 • 16:00 - 16:20 Japan Standard Time | Room G303, North - 3F
Show Abstract +
FIRSST is a far-infrared pointed space-borne observatory led at APL for the 2023 Astrophysics $1B Probe
Class mission competition. FIRSST payload consists of a 1.8m telescope that is cryo-cooled to a temperature
of 4.7K and two instruments that allow sensitive far-infrared spectroscopy between 35 to 600 microns with
resolving powers up to a million. The PI-led science program of FIRSST aims to understand how galaxies grow in
the universe, why super-Earths to mini-Neptunes are the most frequent planets, and what is the source of water
in rocky planets. As required by NASA, 75% of the mission five-year lifetime is left open to be used by the
astronomical community through a time allocation process, similar to the selection of science programs with
Hubble and JWST. This talk will summarize the history of far-infrared astronomy, science objectives and
requirements, and the technical details of FIRSST.
13092-16
16 June 2024 • 16:20 - 16:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Direct Detection Spectrometer Instrument (DDSI) is one of two instruments designed for the Far-IR Spectroscopy Space Telescope (FIRSST) recently proposed to NASA in response to the Astrophysics Probe Explorer call. The DDSI consists of two modules: HR delivering spectra at R~20,000 to 100,000 in three select bands (HR1-3) across 56-184μm, and LR providing broadband spectral coverage at R~100 in four bands (LR1-4) across 35-260 µm. The dispersive element of the HR bands is a compact optical resonator known as a virtually imaged phase array. All DDSI bands use microwave kinetic inductance detector (MKID) arrays cooled to 120mK. The total DDSI MKID pixel count is 2612 pixels.
13092-17
16 June 2024 • 16:40 - 17:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Heterodyne Spectrometer Instrument (HSI) is one of two instruments designed for the Far-IR Spectroscopy Space Telescope (FIRSST) recently proposed to NASA in response to the Astrophysics Probe Explorer call. HSI will be the first THz cryogenic heterodyne array receiver implemented for a space mission. It has extremely high spectral resolving power (R>10^6) in order to allow detailed spectral observations. HSI covers a very wide bandwidth range between 150 and 600 microns in only 3 bands, each equipped with two 5-pixel arrays. HSI enables highly sensitive dual-polarization, multi-pixel and multi-frequency observations on a space telescope, by a careful design and by employing low-heat dissipating, low-power, but high TRL components.
13092-18
16 June 2024 • 17:00 - 17:20 Japan Standard Time | Room G303, North - 3F
Show Abstract +
PRIMA addresses questions about the origins and growth of planets, supermassive black holes, stars, and dust. Much of the radiant energy from these formation processes is obscured and only emerges in the far infrared (IR) where PRIMA observes (24–261 um). PRIMA’s PI science program (25% of its 5-year mission) focuses on three questions and feeds a rich archival Guest Investigator program: How do exoplanets form and what are the origins of their atmospheres? How do galaxies’ black holes and stellar masses co-evolve over cosmic time? How do interstellar dust and metals build up in galaxies over time? PRIMA provides access to atomic (C, N, O, Ne) and molecular lines (HD, H2O, OH), redshifted PAH emission bands, and far-IR dust emission. PRIMA’s 1.8-m, 4.5-K telescope serves two instruments using sensitive KIDs: the Far-InfraRed Enhanced Survey Spectrometer (continuous, high-resolution spectral coverage with over an order of magnitude improvement in spectral line sensitivity and 3-5 orders of magnitude improvement in spectral survey speed) and the PRIMA Imager (hyperspectral imaging, broadband polarimetry). PRIMA opens new discovery space with 75% of the time for General Observers.
13092-19
16 June 2024 • 17:20 - 17:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The PRobe far-Infrared Mission for Astrophysics (PRIMA) is an actively cooled, infrared observatory for the community for the next decade.
On board, an infrared camera, PRIMAger, will provide observers with coverage of mid-infrared to far-infrared wavelengths from about 25 to 264 microns. PRIMAger will offer two imaging modes: the Hyperspectral mode will cover the 25-80 microns wavelength range with a resolution R~10 while the Polarimetric mode will have four broad-band filters, sensitive to polarization, from 80 to 264 microns. These capabilities have been specifically tailored to answer fundamental astrophysical questions such as black hole and star-formation coevolution in galaxies, the evolution of small dust grains over a wide range of redshifts, and the effects of interstellar magnetic fields in various environments, as well as opening a vast discovery space with versatile photometric and polarimetric capabilities.
13092-20
16 June 2024 • 17:40 - 18:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
FIRESS is the multi-purpose spectrometer proposed for the PRobe far-Infrared Mission for Astrophysics (PRIMA). The sensitive spectrometer on the cold telescope provide factors of 1,000 to 100,000 improvement in spatial-spectral mapping speed relative to Herschel, accessing galaxies across the arc of cosmic history via their dust-immune far-infrared spectral diagnostics. FIRESS covers the 24 to 235 micron range with four slit-fed grating spectrometer modules providing resolving power between 85 and 130. The four slits overlap in pairs so that a complete spectrum of any object of interest is obtained in 2 pointings. For higher-resolving-power studies, a Fourier-transform module (FTM) is inserted into the light path in advance of the grating backends. The FTM serves all four bands and boosts the resolving power up to 4,400 at 112 microns, allowing extraction of the faint HD transition in protoplanetary disks. FIRESS uses four 2016-pixel arrays of kinetic inductance detectors (KIDs) which operate at the astrophysical photon background limit. KID sensitivities for FIRESS have been demonstrated, and environmental qualification of prototype arrays is underway.
Monday Plenary Session
17 June 2024 • 08:30 - 10:00 Japan Standard Time | National Convention Hall, 1F
Join us for the Monday morning plenary talks.
Break
Coffee Break 10:00 - 10:20
Session 6:
Wide Field Survey Missions I
17 June 2024 • 10:20 - 12:00 Japan Standard Time | Room G303, North - 3F
13092-21
17 June 2024 • 10:20 - 10:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Euclid is the first stage IV space-based Dark Energy mission and is developed and operated by the European Space Agency. The Euclid satellite was successfully launched on a SpaceX Falcon9 rocket from Florida in July 2023. The first months of the mission was dedicated to the commissioning of the spacecraft and instruments, followed by a phase to verify the scientific performances and to perform the in-orbit calibrations. We present an overview of the expected and unexpected findings during these early phases. The nominal mission started in December 2024 with a 6 months early survey operations phase to closely monitor the performance of the sky survey. In the light of the in-orbit mission performances, we give an outlook of the planning for the remainder of the mission and the data release plan.
13092-22
17 June 2024 • 10:40 - 11:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Euclid is an European Space Agency mission dedicated to the mapping of the geometry of the dark Universe launched the 1st of July 2023. The first images were released the 7th of November 2023. They are the demonstration of the exquisite image quality and performance of the space segment, including the payload module and the pointing stability provided by the service module. To reach such performance the space segment was extensively tested on-ground and underwent a thorough commissioning in-flight. The paper presents the highlights and main results of both test campaigns.
13092-23
17 June 2024 • 11:00 - 11:20 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Launched successfully on July 1st, 2023, Euclid, the M2 mission of the ESA cosmic vision program, aims mainly at understanding the origin of the accelerated expansion of the Universe. Along with a visible imager VIS, it is equipped with the NISP instrument, a Near Infrared Spectrometer and Photometer, bespoke tailored to perform a 3D mapping of the observable Universe. Operating in the the near-infrared spectral range, from 900 nm to 2000 nm with 2 observation modes: As a spectrometer, the NISP instrument will permit measuring millions of galaxy spectroscopic redshift over the Euclid mission 6.5 years lifetime; As a photometer, it will obtain photometric redshifts of billions of galaxy. This talk provides a description of the NISP instrument, its scientific objectives, and offers an assessment of its current performance in flight.
13092-24
17 June 2024 • 11:20 - 11:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Euclid will be subject to a large amount of highly energetic particles over its lifetime. These particles can cause damage to the detectors by creating defects in the silicon lattice that lead to trails in the image data. This can be problematic for the Euclid VIS instrument, which aims to measure the shapes of galaxies to a very high degree of accuracy. Using a special technique called trap pumping, the single defects in the CCDs can be detected and characterised. Being the first instrument in space with this capability, it will provide novel insights into the creation and evolution of radiation-induced defects and give input to the radiation damage correction of the scientific data. We present the status of the radiation damage of the Euclid VIS CCDs and how it has evolved over the first year in space and evaluate how this compares to the on-ground testing of these devices.
13092-25
17 June 2024 • 11:40 - 12:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
In November 2022, the ESA Science Programme Committee (SPC) selected ARRAKIHS as the second Fast-implementation mission (F2) within the Agency’s Scientific Programme, with a launch planned in 2030. ARRAKIHS is designed specifically to explore, at unprecedented depth, the predictions of the Λ-Cold Dark Matter (ΛCDM) cosmological model, and to assess the significance of reported tensions between model and observations in the local Universe. Through multi-band, ultra-low surface brightness imaging of the halos of a statistically representative sample of nearby Milky Way-type galaxies, ARRAKIHS will provide key tests with which to probe both the nature of Dark Matter in the Universe, and baryonic physics currently adopted in state-of-the-art galaxy formation models. This paper describes the ARRAKIHS mission concept and the main design and implementation challenges.
Break
Lunch Break 12:00 - 13:20
Session 7:
Wide Field Survey Missions II
17 June 2024 • 13:20 - 15:20 Japan Standard Time | Room G303, North - 3F
13092-26
17 June 2024 • 13:20 - 13:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Nancy Grace Roman Space Telescope (“Roman”) was prioritized by the 2010 Decadal Survey in Astronomy & Astrophysics and is NASA’s next flagship observatory. Launching no earlier than 2026, it will conduct several wide field and time domain surveys, as well as find exoplanets via microlensing. Roman’s large field of view, agile survey capabilities, and excellent stability enable these objectives, yet present unique challenges. Roman comprises a Spacecraft and the Integrated Payload Assembly (IPA), the latter of which includes the Optical Telescope Assembly (OTA), the primary science Wide Field Instrument, a technology demonstration Coronagraph Instrument, and the Instrument Carrier, which meters the OTA to each instrument. The Spacecraft supports the IPA and includes the Bus, Solar Array Sun Shield, Outer Barrel Assembly, and Deployable Aperture Cover. It provides all required power, attitude control, communications, data storage, and stable thermal control functions as well as shading and straylight protection across the entire field of regard. This paper presents the Observatory as it begins integration and test, as well as describes key test and verification activities.
13092-27
17 June 2024 • 13:40 - 14:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Optical Telescope Assembly (OTA) for the Nancy Grace Roman Space Telescope includes the primary mirror, secondary mirror, and aft optics for guiding light into the Wide Field Instrument and the Coronagraph Instrument. The OTA is nearing completion with the system fully integrated and environmental testing underway. Pictures and descriptions of the integration and test progress are provided, along with performance results. Final environmental and performance tests are continuing, leading into delivery of the completed telescope.
13092-28
17 June 2024 • 14:00 - 14:20 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Wide Field Instrument (WFI) on NASA’s Nancy Grace Roman Space Telescope has just finished its pre-environmental thermal-vacuum testing, where performance of the Cold Module was demonstrated for the first time as a fully integrated instrument. The instrument is hybrid-developed mission between Goddard Space Flight Center and Ball Aerospace. This paper will describe the performance results of the Cold Module, the 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.
13092-29
17 June 2024 • 14:20 - 14:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Surveys in space and time are key to answering outstanding questions in astrophysics. The power to study very large numbers of stars, galaxies, and transient events over large portions of the sky and different time scales has repeatedly led to new breakthroughs. The Nancy Grace Roman Space Telescope (Roman), NASA's next Astrophysics Flagship mission, takes wide field and time domain survey observations to the next level. Roman carries the Wide Field Instrument (WFI), which provides optical to near-IR imaging and spectroscopy with an unprecedented combination of field-of-view, spatial resolution, and sensitivity. When combined with a highly stable observatory and efficient operations, the WFI allows surveys never before possible. These observations will lead to new discoveries in cosmology, exoplanets, and a very wide array of other astrophysics topics ranging from high redshift galaxies to small bodies in the solar system. This paper provides an overview of Roman survey science, connects this science to the design of the WFI, and provides a status update on WFI hardware build and test.
13092-30
17 June 2024 • 14:40 - 15:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Slated for launch in 2025, SPHEREx will be NASA’s next astrophysics explorer mission. Optimized to meet rigorous requirements to precisely map the Universe’s large scale structure, produce deep maps of the diffuse extragalactic background, and to survey the Milky Way’s biogenic ice content, the SPHEREx telescope’s wide-field optical design utilizes a series of custom near infrared linear variable filters to survey the entire sky spectroscopically. This unique instrument has now completed its construction phase and is fully assembled for flight. To precisely focus and calibrate the optical and spectroscopic properties of SPHEREx, a custom optical-cryogenic facility was developed and commissioned. In this overview, we’ll examine the implementation of the recently completed instrument integration and testing campaign, delivering a well characterized imaging spectrometer to be integrated with the rest of the observatory.
13092-31
17 June 2024 • 15:00 - 15:20 Japan Standard Time | Room G303, North - 3F
Show Abstract +
About half a billion years after the Big Bang, the earliest galaxies had formed and grown enough that their ultraviolet light ionized the gas between galaxies, driving the last phase transition for most of the ordinary matter in the universe: cosmological reionization. Key aspects of reionization can only be studied by surveying wide fields of view, because the reionization process was inhomogeneous on large scales.
We are developing the Reionization Explorer--- REX--- as a NASA Astrophysics Small Explorer Mission concept. REX will combine a wide field of view with an unprecedented, flexible narrow-bandpass filter complement, enabling it to identify strong emission line galaxies in the epoch of reionization. Strong line emission identifies the most actively star-forming early galaxies, believed to be drivers of reionization. Moreover, mapping the locations of Lyman alpha emitting galaxies will reveal the distribution of ionized and neutral gas, because neutral gas scatters Lyman alpha light.
Break
Coffee Break 15:20 - 15:50
Session 8:
Wide Field Survey Missions III
17 June 2024 • 15:50 - 17:30 Japan Standard Time | Room G303, North - 3F
13092-32
17 June 2024 • 15:50 - 16:10 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Cosmic Infrared Background Experiment 2 (CIBER-2) is a NASA sounding rocket experiment designed to observe the anisotropy and spectrum of extragalactic background light (EBL) at visible and near-infrared wavelengths with unprecedented accuracy to unveil the near-infrared EBL excess. The instrument comprises a 28.5-cm telescope cooled to 90K, coupling optics, and three HAWAII-2RG detectors equipped with both dual-band filters and linear variable filters. In this paper, we describe the as-rebuilt payload following its second flight, and we report on the status of the instrument for its third flight in early May 2024.
13092-33
17 June 2024 • 16:10 - 16:30 Japan Standard Time | Room G303, North - 3F
Show Abstract +
We describe scientific objective and project status of an astronomical 6U CubeSat mission VERTECS (Visible Extragalactic background RadiaTion Exploration by CubeSat). The scientific purpose of VERTECS is to reveal the star-formation history by measuring the cosmic background radiation in visible wavelength. Detection sensitivity of cosmic background radiation is determined by Etendue, the product of the telescope aperture and the field of view. In VERTECS mission, we develop a 6U CubeSat equipped with a 3U size wide-field telescope to observe the visible cosmic background radiation. The bus system including onboard computer, electric power system, communication, and structure is based on heritage of CubeSats developed at Kyushu Institute of Technology. To accomplish severe requirement of pointing stability, we adopt a 1U unit of high-precision attitude control system. The VERTECS mission was selected for JAXA-Small Satellite Rush Program (JAXA-SMASH Program). We started the satellite development in December 2022 and plan to launch the satellite in early 2025.
13092-34
17 June 2024 • 16:30 - 16:50 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Extragalactic Background Light (EBL) is the integrated emission from all objects outside of our galaxy, with infrared EBL showing an unknown, brighter emission than extragalactic galaxies. Possible sources include first stars and halo brown dwarfs, each with unique spectral characteristics. The VERTECS project plans to reveal these unknowns through continuous visible EBL observations using a 6U CubeSat with a 3U optical telescope. The main feature of this telescope is its lens optics with high-throughput (SΩ > 10^-6 m^2 sr). In addition, it has a wide field of view and filters to capture a range of wavelengths. Observations involve 60-second exposure images, shifting the field incrementally for photometry in four bands. The project was selected by JAXA-SMASH for launch in early 2025, and progress on the engineering model is underway. This presentation covers the visible EBL observation strategy, optical telescope development progress, and future plans.
13092-35
17 June 2024 • 16:50 - 17:10 Japan Standard Time | Room G303, North - 3F
Show Abstract +
GREX-PLUS (Galaxy Reionization EXplorer and PLanetary UniverseSpectrometer) is one of the three candidates of ISAS/JAXA's Strategic L-class mission for 2030s. The 1.2m primary mirror, 50 K cryogenic telescope will have a wide-field camera (WFC) of 1,260 square arcmin field-of-view in the 2-8 micron wavelength band and a high resolution spectrometer (HRS) with a wavelength resolution of 30,000 in the 10-18 micron band. The WFC field-of-view is 130 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. In this talk, I will present the latest status of the concept design of GREX-PLUS, including telescope system, WFC, HRS, cooling system, and spacecraft system.
13092-36
17 June 2024 • 17:10 - 17:30 Japan Standard Time | Room G303, North - 3F
Show Abstract +
SIRMOS (Satellite for Infrared Multi-Object Spectroscopy) is a NASA Small Explorers (SMEX) mission concept to map the universe in 3D over ~ 500 cubic gigaparsecs using 131 million [OIII] and H alpha emission line galaxies at 1 < z < 4. SIRMOS will probe the cosmic origin by placing unprecedented constraints on primordial non-Gaussianity, precisely measure the sum of neutrino masses, and definitively differentiate dark energy and modification of general relativity as the cause for the observed low-redshift cosmic acceleration.
SIRMOS has a 50 cm aperture telescope with 1.6 square degree field of view, and more than 4.4 million micromirrors on 2 digital micro-mirror devices (DMDs) to provide a programmable reflective slit mask allowing slit spectroscopy at R~1300 over the wavelength range of 1.25-2.5 microns. SIRMOS can calibrate and purify data from Euclid and Roman Space Telescopes and accomplish flagship-level stand-alone science at the modest cost of a SMEX mission.
Tuesday Plenary session
18 June 2024 • 08:30 - 10:00 Japan Standard Time | National Convention Hall, 1F
Join us for the Tuesday morning plenary talks.
Break
Coffee Break 10:00 - 10:20
Session 9:
JWST
18 June 2024 • 10:20 - 11:20 Japan Standard Time | Room G303, North - 3F
13092-37
18 June 2024 • 10:20 - 10:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Based on defocused phase retrieval analysis of JWST commissioning, routine maintenance, and science data, we characterize components of the JWST OTE wavefront error (WFE) variations over a wide range of time scales, including the accumulation of segment pose changes (tilt events) over days and weeks of typical wavefront control cycles, smooth drifts over hours and days, oscillation due to thermal cycling of the ISIM Electronics Compartment (IEC) heaters with periods of a few minutes, and mechanical vibration modes with periods ~1 second and less. We extract the spatial and temporal forms of the detected WFE variations and explore correlation with relevant observatory telemetry data, including reaction wheel rotation speeds, IEC heater panel temperatures, and spacecraft attitude.
13092-38
18 June 2024 • 10:40 - 11:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The NIRSpec instrument on the James Webb Space Telescope (JWST) affords the astronomical community an unprecedented space-based Multi-Object Spectroscopy (MOS) capability through the use of a programmable array of micro-electromechanical shutters. Although MOS is only one of the observing modes available to users, the complexity and relative uniqueness of the Microshutter Array (MSA) that enables it has presented a variety of engineering challenges including the appearance of electrical shorts that produce contaminating glow in exposures and specialized anomaly detection and fault response considerations. Despite these challenges, the NIRSpec Multi-Object Spectrograph continues to perform robustly with no discernable degradation or significant reduction in capability.
This paper provides an overview of the NIRSpec microshutter subsystem's state of health and operability, characterizing both routine and contingent operations and presenting some of the developments that have taken place in its operation since the completion of instrument commissioning.
13092-267
18 June 2024 • 11:00 - 11:20 Japan Standard Time | Room G303, North - 3F
Show Abstract +
NIRISS/SOSS is a prime instrument mode of the James Webb Space Telescope unique for its GR700XD grism that disperses light across three diffraction orders spanning a wavelength range from 0.6 to 2.8 𝜇m with moderate spectral resolution. This mode is ideal for exoplanet spectroscopy and Time Series Observations. The NIRISS/SOSS team has made recent advancements in improving the wavelength and photometric calibration, alongside notable updates to essential observer planning tools such as the Exoplanet Characterization ToolKit (ExoCTK). We improved the wavelength calibration for the GR700XD grism and the photometric calibration. We have made functional and user interface upgrades to ExoCTK enabling users to better plan their SOSS observations. Future calibration efforts will be directed towards characterizing the spatial point spread function profiles and noise reduction strategies. We are committed to supplying the community with advanced tools, code, and data models that will assist in observational planning and data reduction.
Session 10:
Exoplanet Time Series Observations I
18 June 2024 • 11:20 - 12:00 Japan Standard Time | Room G303, North - 3F
13092-40
18 June 2024 • 11:20 - 11:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Twinkle telescope is a space-based observatory conceived to study solar system objects, exoplanets, brown dwarfs, protoplanetary disks and stars. The satellite, based on a high-heritage platform, will carry a visible and infrared spectrograph providing simultaneous broad wavelength coverage. Launching into a Sun-synchronous low-Earth polar orbit, Twinkle will operate from a highly stable thermal environment for a baseline lifetime of seven years.
In this presentation, the Twinkle team will highlight the work undertaken to develop the satellite platform and prepare for the extrasolar survey. We will present the latest engineering and programmatic updates, as well as the initial science themes under development. Demonstrating how Twinkle will contribute to other missions and a broad range of astrophysics research in the coming years.
13092-41
18 June 2024 • 11:40 - 12:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Pandora SmallSat is a NASA flight project designed to study the atmospheres of exoplanets. Transmission spectroscopy of transiting exoplanets provides our best opportunity to identify the makeup of planetary atmospheres in the coming decade, and is a key science driver for HST and JWST. Stellar brightness variations due to star spots, however, have been shown to contaminate the observed spectra in these high-precision measurements. Pandora will collect long-duration photometric observations with a visible-light channel and simultaneous spectra with a near-IR channel to constrain star spot covering fractions of exoplanet host stars, enabling star and planet signals to be disentangled in transmission spectra to reliably determine exoplanet atmosphere compositions. Pandora will observe exoplanets with sizes ranging from Earth-size to Jupiter-size and host stars spanning mid-K to late-M spectral types. Pandora was selected in early 2021 as part of NASA’s Astrophysics Pioneers Program. We will provide an update on the mission status, and present the science goals, target selection, observing strategy, and synergies with other ground and space-based facilities.
Break
Lunch Break 12:00 - 13:20
Session 11:
Exoplanet Time Series Observations II
18 June 2024 • 13:20 - 15:00 Japan Standard Time | Room G303, North - 3F
13092-42
18 June 2024 • 13:20 - 13:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
PLATO (PLAnetary Transits and Oscillations) mission is a space-based optical multi-camera photometer mission of the European Space Agency to identify and characterize exoplanets and their hosting stars. Led by ESA and developed as a collaboration between ESA and its industrial contractors and a Consortium of institutes (PLATO Mission Consortium), the satellite entered the development phase in 2017 and it is currently at an advance stage of assembly and testing, with launch scheduled end of 2026. We provide an update of the current status, initial performance results from ground testing, and a review of the lessons learned to date, both on the technical development as on the organizational and programmatic aspects.
13092-43
18 June 2024 • 13:40 - 14:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
PLATO (PLAnetary Transits and Oscillations of stars) is he M3 class ESA mission dedicated to the discovery and study of extrasolar planetary systems by means of planetary transits detection. 8 flight camera were TVAC tested for acceptance and performance verification between June and December 2023 at 3 different test facilities (SRON, IAS and INTA), with the remaining units to be tested in 2024. In this paper, we provide an overview of our serial testing approach, some of the associated challenges, and key performance results, including comparison between models and with subsystem results. An up-to-date status on the remaining planned activities will also be discussed.
13092-295
18 June 2024 • 14:00 - 14:20 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Leonardo SpA is leading an Italian Space Industry Team, funded by ASI, collaborating to the ESA mission PLATO program for the realization of the 26 telescopes, that will fly on a single platform, aimed to discover, observe and analyze exoplanets. The mission is based on a challenging telescope design with peculiar optical performance to be assured at very low operative temperature (-80°C). The “large” number of telescopes, produced in high rate (up to 3 telescopes every 2 months), is quite unusual for the production of scientific payloads. It has imposed a change with respect the prototypical manufacturing and test approach as standard for a few space equipment/instruments, addressing the implementation of smart and fast methodologies for the aligning and focusing of the telescopes, based on simulation of the as-built data. The opto-mechanical design of the telescope was optimized for an industrial approach used for all the manufacturing, assembly, integration and test (MAIT) phases. The number, production rate and the performance result of the flight units so far delivered to the PLATO – Team, is validating the selected design solutions and selected MAIT approach and procedures.
13092-45
18 June 2024 • 14:20 - 14:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Earth 2.0 (ET) space mission has entered its phase B study in China. This mission aims to detect thousands of Earth-sized terrestrial-like planets, including habitable Earth-like planets orbiting solar-type stars (i.e., Earth 2.0s), cold low-mass planets, and free-floating planets. The final design of ET includes six 28 cm diameter transit telescopes, each with a field of view of 550 square degrees, and one 35 cm diameter microlensing telescope with a field of view of 4 square degrees. The transit telescopes will be pointed towards the original Kepler field and its neighboring fields, while the microlensing telescope is directed towards the Galactic bulge region from its Earth-Sun L2 halo orbit. It will continuously monitor these fields for four years to detect planets.
13092-46
18 June 2024 • 14:40 - 15:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
We present a laboratory demonstration of an ultra-stable mid-IR Array Spectrometer for Exoplanet Transits (MIRASET), which includes a calibration system that, as we show, is required to achieve the minimum sensitivity for the detection of atmospheric bio-signatures in habitable-zone planets around M-dwarfs. The spectrometer uses an array of Transition Edge Sensor detectors (TES). These devices are known to be intrinsically very stable and the required detector parameters (sensitivity, dynamic range) for space-based mid-IR transit and phase-curve spectroscopy can be easily met with existing devices. No new detector developments are required. This project includes the development of a high-accuracy calibration system with a stable reference source which itself is monitored by an out-of-band photo diode at a wavelength at which the precision of this measurement exceeds that of an in-band calibration (0.5 um). This scheme allows for real time monitoring of the detector gain, which results in a background-limited performance with the required stability of better than 5 ppm for the detection of bio-signatures in a designated spectrometer for future space missions.
Break
Coffee Break 15:00 - 15:30
Session 12:
Exoplanet Time Series Observations III
18 June 2024 • 15:30 - 17:30 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Ariel, part of the European Space Agency's (ESA) Cosmic Vision program, is a unique medium-class mission designed to study the atmospheres of over 500 transiting exoplanets. It is set for launch in 2029 aboard Ariane 6.2 and will orbit the Sun-Earth system's second Lagrange point. The mission has a four-year lifespan, extendable by two years. The spacecraft hosts a payload provided by the Ariel Mission Consortium (AMC) that consists of an all-aluminium cryogenic telescope, the AIRS and FGS infrared instruments, and a cryocooler. The operational segment includes the Operational Ground Segment at ESOC and Science Ground Segment shared between ESAC and the AMC.
ESA collaborates with the AMC, NASA, and CSA to explore exoplanetary atmospheres and advance our knowledge of distant worlds.
13092-48
18 June 2024 • 15:50 - 16:10 Japan Standard Time | Room G303, North - 3F
Show Abstract +
This paper presents the overall picture of the payload for the Ariel mission. The payload tightly integrates the design and analysis of the various payload elements (including for example the integrated STOP analysis of the Telescope and Common Optics) in order to allow the exacting photometric stability requirements for the mission to be met. The Ariel payload has passed through the Preliminary Design Review (completed in Q2 2023) and is now developing and building prototype models of the Telescope, Instruments and Subsystems (details of which will be provided in other contributions to this conference). This paper will present the current status of the development work and outline the future plans to complete the build and verification of the integrated payload.
13092-49
18 June 2024 • 16:10 - 16:30 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Ariel (Atmospheric Remote-Sensing Infrared Exoplanet Large Survey) is the adopted M4 mission in the framework of the ESA “Cosmic Vision” program. Its purpose is to survey the atmospheres of known exoplanets through transit spectroscopy. The scientific payload consists of an off-axis, unobscured Cassegrain telescope feeding a set of photometers and spectrometers in the waveband 0.5-7.8 µm and operating at cryogenic temperatures (55 K). The Telescope Assembly is based on an innovative fully aluminium design to tolerate thermal variations to avoid impacts on the optical performance; it consists of a primary parabolic mirror with an elliptical aperture of 1.1 m (the major axis), followed by a hyperbolic secondary that is mounted on a refocusing system, a parabolic re-collimating tertiary and a flat folding mirror directing the output beam parallel to the optical bench. The Telescope Assembly is in phase B2 towards the Critical Design Review, and the fabrication of the structural and engineering models has started. This paper aims to update the scientific community on the progress concerning the development, manufacturing and qualification activity of the ARIEL Telescope Assembly.
13092-50
18 June 2024 • 16:30 - 16:50 Japan Standard Time | Room G303, North - 3F
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 (Channel 1) µm 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 cover the opto-mechanical design of the instrument operating in a 60 K environment, up to the detection chain of both channels based on 2 HgCdTe detectors actively cooled down below 42 K.
This overview will present updated information of phase C studies, in particular on the assembly and testing of prototypes that are highly representative of the future engineering model that will be used as an instrument-level qualification model.
13092-51
18 June 2024 • 16:50 - 17:10 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The FGS is one of two scientific instruments on board the ESA ARIEL space telescope that ESA plans to launch in 2029. The aim of the mission is to characterize the atmospheres of several hundred different exoplanets.
The FGS is an opto-electronic instrument – a photometer working in channels 500-600nm, 600-800nm and 800-1100nm and a near infra-red low-resolution spectrometer operating in a range from 1.1 to 1.95 microns. Although FGS stands for Fine Guidance System it has two main goals: 1) to deliver scientific data of observed exoplanets, exactly speaking, their atmospheres, 2) to support the spacecraft’s AOCS with very precise pointing and guiding towards an observation object.
This paper presents the overview of the current FGS design and implementation for ARIEL mission. The instrument is in a middle step between successfully passed iPDR and before upcoming iCDR. Up to now, the team successfully built a prototype of the instrument, and is working on the starting the manufacturing of the engineering and engineering-qualification models.
13092-52
18 June 2024 • 17:10 - 17:30 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Ariel space mission will characterise spectroscopically the atmospheres of a large and diverse sample of hundreds of exoplanets. Targets will be chosen to cover a wide range of masses, densities, equilibrium temperatures and host stellar types to study the physical mechanisms behind the observed diversity in the population of known exoplanets. With a 1-m class telescope, Ariel will detect the atmospheric signatures from the small, <100ppm, modulation induced by exoplanets on the bright host-star signals, using transit, eclipse and phase curve spectroscopy. Three photometric and three spectroscopic channels, with Nyquist sampled focal planes, simultaneously cover the 0.5-7.8 micron region of the electromagnetic spectrum, to maximise observing efficiency and to reduce systematics of astrophysical and instrumental origin. This contribution reviews the predicted Ariel performance as well as the design solutions implemented that will allow Ariel to reach the required sensitivity and control of systematics.
Wednesday Plenary Session
19 June 2024 • 08:30 - 10:00 Japan Standard Time | National Convention Hall, 1F
Join us for the Wednesday morning plenary talks.
Break
Coffee Break 10:00 - 10:20
Session 13:
Exoplanet Imaging I: JWST, Roman, and Technology Roadmaps for HWO
19 June 2024 • 10:20 - 12:00 Japan Standard Time | Room G303, North - 3F
13092-53
19 June 2024 • 10:20 - 10:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The James Webb Space Telescope is the first segmented observatory in space to conduct, among other things, high-contrast direct observations of exoplanetary systems. Such observations are thus to date the more technically akin to the future reconnaissance of nearby habitable zones with the Habitable Worlds Observatory. While JWST coronagraphs are not sensitive to temperate telluric planets, mostly due to the absence of critical Deformable Mirrors that will fly on the Roman Coronagraph Instrument (CGI), their capabilities are have achieved a few milestones relevant to HWO. This paper is part of a series to be presented by the JWST Telescope Scientist Team, JWST-TST. A common theme of these investigations is the desire to pursue and demonstrate science for the astronomical community at the limits of what is made possible by the exquisite op- tics and stability of JWST. The high-contrast programs of TST were crafted to rapidly advance knowledge of high-contrast strategies and best practices with JWST early in the mission. In this paper, we summarize our results and discuss their implications for the ongoing HWO architecture formulation.
13092-54
19 June 2024 • 10:40 - 11:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
In preparation for the operational phase of the Nancy Grace Roman Space Telescope, NASA has created the Coronagraph Community Participation Program (CPP) to plan and execute Coronagraph Instrument technology demonstration observations. The CPP is composed of 7 small, US-based teams, selected competitively via the Nancy Grace Roman Space Telescope Research and Support Participation Opportunity, members of the Roman Project Team, and international partner teams from ESA, JAXA, CNES, and the Max Planck Institute for Astronomy. The primary goals of the CPP are to prepare simulation tools, target databases, and data reduction software for the execution of the Coronagraph Instrument technology demonstration. Here, we present the current status of the CPP and its working groups, along with plans for future CPP activities up through Roman's launch. We also discuss plans to potentially enable future commissioning of currently-unsupported modes.
13092-55
19 June 2024 • 11:00 - 11:20 Japan Standard Time | Room G303, North - 3F
Show Abstract +
NASA’s Habitable Worlds Observatory (HWO) mission is intended to search for biosignatures from ~25 exoplanets in the habitable zones of their host stars using a coronagraph instrument. This requires the coronagraph to directly detect and spectrally analyze photons from planets that are merely ~ 0.1 arcsec from the host star and ~ 10 billion times fainter. Achieving extreme contrast levels at extremely small angular separations is a daunting technological challenge. A working group of 50+ multi-institutional experts has been developing a first cut at a coronagraph technology roadmap to identify key technology gaps and enabling technology developments for HWO’s coronagraph instrument system. This paper will present a summary of the working group’s findings.
13092-56
19 June 2024 • 11:20 - 11:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
NASA’s Habitable Worlds Observatory will consist of a segmented telescope and high contrast coronagraph to characterize exoplanets for habitability. Achieving this objective requires an ultra-stable telescope with wavefront stability of picometers in certain critical modes. The NASA funded Ultra-Stable Large Telescope Research and Analysis – Technology Maturation program has matured key component-level technologies in 10 areas spanning an “ultra-stable” architecture, including active components like segment edge sensors, actuators and thermal hardware, passive components like low distortion mirrors and stable structures, and supporting capabilities like precision metrology. This paper will summarize the final results from the four-year ULTRA-TM program, including advancements in performance and/or path-to-flight readiness, TRL/MRL maturation, and recommendations for future work.
13092-57
19 June 2024 • 11:40 - 12:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Deformable Mirror Technology Roadmap (DMTR) is a working group tasked by NASA’s Exoplanet Program Office to study the path to bring deformable mirror (DM) systems to a Technology Readiness Level 5. DMs, and their drive electronics and harnessing, are the critical component of any exoplanet direct imaging coronagraph, and there is no device that exists today which can meet the ambitious performance goals expected for NASA’s Habitable Worlds Observatory (HWO). Here we present progress on surveying the field of DM technologies, defining a first cut set of device requirements, and recommending a development and verification maturation program.
Break
Lunch Break 12:00 - 13:20
Session 14:
Exoplanet Imaging II: Towards the Habitable Worlds Observatory
19 June 2024 • 13:20 - 15:20 Japan Standard Time | Room G303, North - 3F
13092-58
19 June 2024 • 13:20 - 13:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
This talk will discuss the science activities associated with these studies performed by the Science, Technology, and Architecture Review Team (START) for the Habitable Worlds Observatory, including the team and organization, and with a focus on identifying those key science drivers which inform trades that will lead to architecture choices as the mission enters the Pre-Phase A stage and beyond.
13092-59
19 June 2024 • 13:40 - 14:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
NASA has begun the Great Observatory Maturation Program (GOMAP) with the goal of studying and advancing the Habitable Worlds Observatory (HWO), a large UV/optical/IR space telescope recommended by the Astro 2020 Decadal Survey. Among its many goals, HWO will obtain spectra of at least 25 exo-Earth candidates to search for signs of life and conduct transformative astrophysics at ultraviolet, optical, and near-infrared wavelengths. The observatory, like HST and JWST, will be a powerful general class observatory. This past Fall the GOMAP program stood up two study groups, the Science Technology Architecture Review Team (START) and the Technical Assessment Group (TAG) aimed at helping to study the science, technology and architecture options for this new flagship mission. This talk will discuss the engineering activities associated with these studies including the team and organization, the study plan and the plans to use the Concept Maturity Level (CML) approach. In addition, the talk will discuss the key initial engineering working groups, the key technology gaps, overall engineering plans and opportunities to get involved.
13092-60
19 June 2024 • 14:00 - 14:20 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Modeling played a vital role on the James Webb Space Telescope (JWST) program. From early modeling to aid in requirements development to final verification and on-orbit performance determination, modeling evolved and grew as the program progressed. With the heavy reliance on modeling that large, complex missions like JWST has had and Habitable Worlds Observatory (HWO) will have, enabling accurate and timely modeling results as the design matures is extremely important. This paper will discuss the types of modeling necessary and the lessons learned during the development of JWST that are applicable to HWO.
13092-61
19 June 2024 • 14:20 - 14:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
We present an approach for end-to-end optical alignment and phasing of a segmented space telescope under closed loop rigid body control, from post-launch acquisition and initialization, to hand-off to a metrology-based closed-loop stabilization system capable of preserving picometer-level wavefront stability. This approach builds on the methods used to initialize the James Webb Space Telescope, including heuristic methods to capture and coarsely align the Primary Mirror segments, followed by spectral techniques for establishing global phase, and image-based Phase Retrieval high-precision direct wavefront sensing for fine phasing. It goes beyond JWST by exploiting high-accuracy laser metrology and edge sensors to stabilize the telescope optics, by using White-Light Interferometry instead of Dispersed Fringe methods for global phasing, and by its close integration with out-of-band wavefront sensing and control in the coronagraph instrument. We analyze performance of straw-person HWO architectures, using simulations to show performance vs sensing and control components.
13092-62
19 June 2024 • 14:40 - 15:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Astro2020 Decadal Survey recommends an ambitious mission named Habitable Worlds Observatory (HWO) to explore the universe and search for life on exoplanets. HWO builds upon NASA investments, including the James Webb Space Telescope segmented optical system, Roman Space Telescope coronagraph, as well as large mission concept studies and technology development. Studies continue to drive our understanding of the HWO mission trade spaces, and increase the readiness of relevant technologies. NASA’s Science, Technology, Architecture Review Team (START) will explain how mission architecture decisions impact science yields and improve understanding of the boundaries and opportunities within the mission trade spaces.
13092-63
19 June 2024 • 15:00 - 15:20 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Habitable Worlds Observatory will revolutionize our understanding of the universe by directly detecting biosignatures on extrasolar planets and allow us to answer the question if we are alone in the universe. To accomplish the tight science goals associated with this mission, the development of an ultrastable observatory with a coronagraphic instrument is necessary. The observatory itself may need to stay stable on the order of 10 picometers over a wavefront control cycle, orders of magnitude more stable than what is required on current space missions. The metrology to verify stability requirements must be roughly a factor of ten more stable. The ultrastable laboratory at NASA’s Goddard Space Flight Center has further stabilized its testbed to allow for dynamic measurements on diffuse and specular objects on the order of single picometers, and we are currently measuring drifts on the orders of tens of picometers over different temporal bands. This paper will discuss the mechanical updates to the testbed setup, the analysis performed on several test articles, and the path forward on the road to measuring achieving the required stability for Habitable Worlds Observatory.
Break
Coffee Break 15:20 - 15:50
Session 15:
Exoplanet Imaging III: Emerging Technologies for Photonics and Detectors
19 June 2024 • 15:50 - 17:30 Japan Standard Time | Room G303, North - 3F
13092-64
19 June 2024 • 15:50 - 16:10 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Theoretical ideal coronagraph performance is achieved when the light from an exoplanet can be coherently decomposed into a linear combination of spatial modes indistinguishable from that containing starlight, and an orthogonal mode. The intensity in the exoplanet mode orthogonal from the stellar modes as a function of separation from the star represents theoretical ideal coronagraph performance. Here we introduce a photonic coronagraph architecture capable of achieving this near-ideal exoplanet throughput at small inner working angles. We will review progress at the NASA Jet Propulsion Lab on prototype hardware implementing this photonic coronagraph concept and discuss our progress at device calibration and closed-loop control required for a photonic coronagraph in a changing wavefront environment.
13092-65
19 June 2024 • 16:10 - 16:30 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Habitable Worlds Observatory (HWO) is the leading recommendation of the Astro2020 decadal survey. The HWO flagship, to be launched in the early 2040s, will directly survey ~100 of the nearest stellar systems and their habitable zones with the goal of detecting and spectroscopically characterizing ~25 potentially “Earth-like planets” (or “Exo-Earths”). Photonic-based technologies can subsntially improve technical and science margins by improving coronagraphic efficiency.
We present the architecture of a photonic-integrated circuit-based coronagraph (“AstroPIC”), currently being studied as a near-infrared channel coronagraph that can be adopted as part of a suite of coronagraphs that could be deployed on the HWO. In this hybrid architecture, detection is performed initially in the visible channel with follow-up NIR spectroscopic characterization in at small inner working angles (within 1-3 L/D). We review the system architecture including input/output couplings options, photonic nulling using a Mach-Zehnder Interferometric (MZI) mesh, wavefront control, PIC configurability, bandwidths, and science detection.
13092-66
19 June 2024 • 16:30 - 16:50 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Habitable Worlds Observatory (HWO) aims for high-contrast imaging of exoplanets, targeting 1e-10 contrasts. Current coronagraph designs fall short of the fundamental coronagraphic limit, providing an opportunity for increasing the science yield of HWO. Photonic integrated circuits (PICs) are in theory able to achieve the fundamental limit. However, manufacturing errors in PICs introduce modal crosstalk, degrading contrast. To address this, we use a traditional PIAACMC coronagraph as a pre-filter before injection into the PIC. The entire system is optimized for its coronagraphic performance. We show initial simulations of this hybrid coronagraph for unobscured and obscured telescope pupils, with a focus on circuit design and active tuning algorithms for the PIC.
13092-67
19 June 2024 • 16:50 - 17:10 Japan Standard Time | Room G303, North - 3F
Show Abstract +
High Contrast Imaging systems (HCIs) must simultaneously optimize contrast, throughput, inner working angle, and angular resolution. HCIs must also be resilient to residual wavefront errors (WFEs), which is achieved by coronagraph design (low sensitivity to WFEs), active control (WFEs are suppressed) and self-calibration (the contribution of WFEs to residual starlight is accurately known and numerically removed).
We establish a process for designing optimal HCIs considering resilience to WFEs, from which we derive fundamental performance limits in the presence of wavefront errors. We show that a discretized version of an optimal HCI system can be realized as a photonic nulling chip (PNC), an approach providing more design flexibility than is accessible with coronagraph masks. We demonstrate on-sky self-calibration capability with the PNC-based GLINT instrument at the Subaru Telescope, and discuss future developments for ground and space-based HCI.
13092-68
19 June 2024 • 17:10 - 17:30 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Superconducting detectors present a promising alternative to traditional semiconductor-based detectors for use on future space missions such as the Habitable Worlds Observatory (HWO) where incredibly low-noise is required to achieve the sensitivities necessary to image exo-Earths. We present an analysis using the Error Budget Software (EBS) showing how the enhanced noise properties of superconducting detectors impact the exposure times needed to perform exoplanet imaging with HWO. We then focus on a specific superconducting detector technology, called microwave kinetic inductance detectors (MKIDs), and perform simulations of how these detectors will interface with wavefront sensing and control algorithms using the High-contrast imager for Complex Aperture Telescopes (HiCAT) testbed simulator at STScI.
Thursday Plenary Session
20 June 2024 • 08:30 - 10:00 Japan Standard Time | National Convention Hall, 1F
Join us for the Thursday morning plenary talks.
Break
Coffee Break 10:00 - 10:20
Session 16:
Exoplanet Imaging IV: Technology Testbed Results
20 June 2024 • 10:20 - 12:00 Japan Standard Time | Room G303, North - 3F
13092-69
20 June 2024 • 10:20 - 10:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Deformable Mirrors (DM) are a critical technology to enable coronagraphic direct imaging of exoplanets using space-based telescopes, such as the Habitable Worlds Observatory (HWO), which aims to image exoplanet types ranging from gas giants to Earth analogs. The DM requirements to achieve this are unprecedented, requiring a large actuator count of at least 96x96 actuators, resolution better than 2.5 pm, and 10 pm/hr stability. In this paper, we present the first demonstration of single-picometer wavefront control utilizing new high-resolution, vacuum-compatible DM electronics and a Zernike Wavefront Sensor for measurement.
13092-70
20 June 2024 • 10:40 - 11:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Starlight suppression to levels of contrast of 1e-10 with an internal coronagraph would allow for detection and spectral characterization of Earth-analogs. Many coronagraph architectures have been proposed to address this science case. Among them, the vector vortex coronagraph (VVC) stands out for its exquisite sensitivity especially at small angular separations. However, the VVC has yet to demonstrate 1e-10 contrast in the laboratory. As a matter of fact, only a Lyot Coronagraph architecture has been demonstrated at 4e-10 raw contrast in 10% bandwidth light. The limitation of VVCs with respect to the Lyot Coronagraph has been thought to be the vortex mask. Indeed, the mask fabrication imperfections limit how well the deformable mirrors can suppress starlight in the image during wavefront control. Furthermore, the polarization leakage inherent to the VVC has not been fully addressed as a source of incoherent light that limits this type of coronagraph’s performance. Our new experiments in the Decadal Survey Testbed confirm these suspicions. Here we present the results of these experiments with a comprehensive characterization of our VVC masks.
13092-71
20 June 2024 • 11:00 - 11:20 Japan Standard Time | Room G303, North - 3F
Show Abstract +
We present the final laboratory results on the High-contrast imager for Complex Aperture Telescopes (HiCAT) testbed as part of the Strategic Astrophysics Technology (SAT) NASA program. The HiCAT testbed was developed over the past decade and aims to demonstrate a system level hardware approach for coronagraphy and exoplanet direct imaging with a future segmented space telescope such as the Habitable World Observatory. The objectives of the SAT program were organized in three milestones to reach TRL-4 system-like level demonstration of segmented-aperture coronagraphy from static component demonstration to system-level demonstration at TRL-4 under both natural and artificial disturbances.
13092-72
20 June 2024 • 11:20 - 11:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
We have built a laboratory testbed named the Exoplanet Imaging System Testbed (EXIST) for developing future high-contrast imaging technologies. The EXIST can test various types of coronagraphs as well as wavefront control techniques using a spatial light modulator (SLM). We carried out laboratory demonstration of various phase mask coronagraphs combined with the wavefront control to generate dark holes. As a result, we could clearly observe the dark holes against residual speckles of the coronagraphs, and the results suggested that turbulent air in the laboratory could be one of the limiting factors of the achieved contrasts. In this presentation, we report on the recent experimental results and the perspectives for future technology development at the EXIST.
13092-73
20 June 2024 • 11:40 - 12:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Directly imaging Earth-like exoplanets around Sun-like stars with the future Habitable Worlds Observatory (HWO) will require coronagraphic focal plane masks able to suppress starlight to the 1e-10 contrast levels. Furthermore, for the purposes of spectroscopy this level of contrast must be achieved across a 20% bandwidth. Scalar vortex coronagraph designs show promise as a polarization-independent alternative to polarization-sensitive vector vortex coronagraphs, but still face chromatic limitations. New scalar vortex coronagraph mask designs incorporate radial phase dimples to improve the broadband performance. We present initial results of prototype masks including phase metrology, chromatic characterization, and starlight suppression measurements taken on the High Contrast Spectroscopy Testbed at Caltech. This work aims to advance the technological maturity of scalar vortex coronagraphs as a viable option for consideration for HWO.
Break
Lunch Break 12:00 - 13:20
Session 17:
Exoplanet Imaging V: Technology Testbed Results
20 June 2024 • 13:20 - 15:40 Japan Standard Time | Room G303, North - 3F
13092-74
20 June 2024 • 13:20 - 13:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Space Coronagraph Optical Bench (SCoOB) is a high contrast imaging testbed built to demonstrate starlight suppression techniques at visible wavelengths in a space-like vacuum environment. The testbed is designed to achieve <10^-8 contrast from 3-10 lambda/D in a one-sided dark hole using a liquid crystal vector vortex waveplate and a 1,000-actuator Kilo-C deformable mirror (DM) from Boston Micromachines (BMC). We have recently expanded the testbed to include a field stop for mitigation of scattered light, a precision-fabricated pinhole in the source simulator, a Minus K passive vibration isolation table for jitter reduction, a modified Lyot stop for wavefront control in a self-coherent camera (SCC) configuration, a low-noise vacuum-compatible CMOS sensor, and custom-built low-noise DM electronics. We report the latest contrast performance achieved using implicit and explicit electric field conjugation (EFC) at a vacuum of ~10^-6 Torr and over a range of bandpasses.
13092-75
20 June 2024 • 13:40 - 14:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
We present improved simulations and preliminary in-air testing for the Phase Induced Amplitude Apodization (PIAA)-Vortex coronagraph for on-axis telescope architectures. In previous studies, we demonstrated that the PIAA-Vortex coronagraph has the potential to overcome limitations on coronagraph performance for on-axis telescopes, and can maintain insensitivity to stellar angular diameters on the order of 0.1 lambda/D at a contrast of 10^-10. In this presentation, we describe updated simulations of the PIAA-Vortex on on-axis pupils with struts and segmentation in both the ray-optics and Fresnel regimes. We also describe the in-air laboratory prototype of the PIAA-Vortex currently under planning at the Ames Coronagraph Experiment testbed. The ACE-testbed prototype will study contrast and aberration sensitivity on a centrally obstructed pupil. The PIAA-Vortex coronagraph will enable consideration of obstructed telescope pupils for the Habitable Worlds Observatory that take advantage of previous NASA optical observatory heritage and potentially allow for greater flexibility in observatory design.
13092-76
20 June 2024 • 14:00 - 14:20 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Due to the limited number of photons, directly imaging planets requires long integration times and the wavefront must be stable on the same time scale. A dark zone maintenance (DZM) algorithm has been developed that corrects for quasi-static wavefront error drifts and allows simultaneous estimation and control while using only science images. DZM has been tested on the High-contrast imager for Complex Aperture Telescopes (HiCAT) at the STScI and the In Air Coronagraph Testbed (IACT) at JPL. Drifts are injected using the deformable mirrors and corrected via DZM. A synthetic planet is injected into the testbed images then recovered in post-processing. We demonstrate that DZM works with traditional techniques such as Angular Differential Imaging (ADI) and Reference Differential Imaging (RDI) and introduce two novel techniques that leverage the concurrent estimation of the incoherent and coherent light in the image by DZM. All techniques recover an injected planet at the same contrast of the background (8e-8).
13092-77
20 June 2024 • 14:20 - 14:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Bright stellar light prevents the direct detection of exoplanets. Dark hole control technique can suppress the stellar scattered light (speckles). However, disturbance of wavefront faster than the dark hole control causes fluctuation of speckles and limits the contrast. The fast-fluctuating speckles can be suppressed by the post-processing technique called the Coherent Differential Imaging on Speckle Area Nulling (CDI-SAN) method. We contracted a laboratory experimental system to demonstrate the CDI-SAN method. In initial laboratory experiments of the CDI-SAN method, the contrast at the 1E-8 level has been achieved. To achieve even higher contrast, we are currently verifying the accuracy of wavefront control and improving the experimental system. We will report the progress of the laboratory experiment.
13092-78
20 June 2024 • 14:40 - 15:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Stellar coronagraphs use closed-loop focal-plane wavefront sensing and control algorithms to create high-contrast dark zones suitable for imaging exoplanets and exozodiacal dust clouds around nearby stars. Model-based algorithms are susceptible to model mismatch, wherein a departure of the coronagraph's true optical characteristics from the assumed model causes reduced control loop performance. Here, we report on a collection of techniques, including prediction-error minimization, expectation-maximization, and maximum-likelihood estimation, for empirically tuning the wavefront control Jacobian matrix in a statistically rigorous fashion during closed-loop wavefront control operations. This mitigates model mismatch and recovers near-optimal control loop performance.
13092-79
20 June 2024 • 15:00 - 15:20 Japan Standard Time | Room G303, North - 3F
Show Abstract +
We show a conceptual design for a self-referenced Michelson interferometer modified to measure the full complex field at a plane conjugate to the coronagraph entrance pupil, using direct starlight, or using a much brighter internal light source. In conjunction with metrology of the segmented primary and secondary mirrors, this provides a method for high spatial and temporal bandwidth control of the beam train. It can be used to servo the two Deformable Mirrors (DMs) used to establish the coronagraph “dark hole,” enabling operationally efficient go-to control for initializing or changing coronagraphic observations. We will compare the contrast and the stability performance of two “6 Meter Space Telescope” (6MST) non-deployed, off-axis segmented telescope concept designs, one of which uses a keystone-shaped segmented PM, and the other hexagonal (Webb heritage) segments, in conjunction with a coronagraph equipped with a charge-6 vortex mask and two 64x64 actuator DMs. Performance against a wide range of telescope and coronagraph errors will be discussed.
13092-80
20 June 2024 • 15:20 - 15:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
We present initial results from the ESA-funded SUPPPPRESS project, focusing on the development of high-performance liquid-crystal coronagraphs to directly capture images of Earth-like exoplanets in reflected light. Leveraging the exceptional wavefront error stability of space telescopes, such high-performance coronagraphs can reach optimal contrast (1e-10) with high spatial resolution at very high sensitivity. We utilize newly manufactured liquid-crystal vector vortex coronagraphs (VVCs), specifically exploring two or three-layer grating patterns to reduce polarization leakage. Detailed calibration techniques with polarization microscopes and mueller matrix ellipsometers were employed, enhancing direct-write accuracy. The performance testing of these coronagraph masks is done on the THD2 high-contrast imaging testbed in Paris. We describe the software and hardware upgrades performed for the SUPPPPRESS project, and show the performance and contrast of a standard VVC and first multi-grating prototype on the THD2.
Break
Coffee Break 15:40 - 16:10
Session 18:
Submillimeter Sky Surveys
20 June 2024 • 16:10 - 17:30 Japan Standard Time | Room G303, North - 3F
13092-81
20 June 2024 • 16:10 - 16:30 Japan Standard Time | Room G303, North - 3F
Show Abstract +
LiteBIRD, the next-generation CMB satellite, is set for launch in Japan's fiscal year 2032, marking a major advancement in the exploration of primordial cosmology and fundamental physics. Orbiting the Sun-Earth Lagrangian point L2, this JAXA-led strategic L-class mission will conduct a comprehensive mapping of the CMB polarization across the entire sky. During its three-year mission, LiteBIRD will employ three telescopes within 15 unique frequency bands (34-448 GHz), targeting a sensitivity of 2.2μK-arcmin and a resolution of 0.5° at 100 GHz. Its primary goal is to measure the tensor-to-scalar ratio r with a δr=0.001, including systematic error and margin. If r≥0.01, LiteBIRD expects >5 sigma detections in the ℓ=2..10 and ℓ=11..200 ranges separately, providing crucial insight into the early universe.
Our presentation will cover LiteBIRD's scientific objectives, the application of systems engineering to mission requirements, the anticipated scientific impact, and the operations and scanning strategies vital to minimizing systematics. The presentation will also highlight LiteBIRD's synergies with concurrent CMB projects.
13092-82
20 June 2024 • 16:30 - 16:50 Japan Standard Time | Room G303, North - 3F
Show Abstract +
LiteBIRD is a JAXA-led international project aimed to make high sensitivity measurements of the primordial B-modes through cosmic microwave background (CMB) polarization observations. LiteBIRD is expected to launch in the Japanese fiscal year of 2032. The Low-Frequency Telescope (LFT) is a modified crossed Dragone reflective telescope with a diffraction-limited 18° x 9° field-of-view across its entire observation frequency range of 34-161 GHz. We will report on the characterization and design optimization studies of the LFT near and far sidelobes using optical simulations including the LFT reflectors, baffling, and spacecraft payload module structures.
13092-83
20 June 2024 • 16:50 - 17:10 Japan Standard Time | Room G303, North - 3F
Show Abstract +
JAXA’s Large-class LiteBIRD mission is a rapidly-developing space-borne observatory intended to undertake a full-sky survey of the CMB B-mode polarization to probe cosmological inflation. The facility comprises a suite of three reflective and refractive telescopes on a single platform, covering a 40 402 GHz spectral range with an unprecedented sensitivity. The required specification is attained through the optimum observation strategy, advanced foreground characterisation, innovative design of large detector arrays, and by extremely tight control of the instrument systematics and their mitigation by design and calibration. This paper reports the preliminary results of computational studies which inform the development of efficient multi-physics simulation approaches aimed at the identification of the principal mechanisms and sources of stray-light impairments in the LiteBIRD refractive telescopes and their numerical characterisation. The trade-offs of low-straylight instrument design are discussed, alongside the systematics simulation pipeline from optical impairments to cosmological uncertainties. The utility of microwave absorbers and baffling for mitigation is demonstrated.
13092-84
20 June 2024 • 17:10 - 17:30 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Recent advancements in imaging the magnetic field in the interstellar medium (ISM) have been made using instruments like PILOT, NIKA2, and HAWC+. These instruments, operating in submillimeter and millimeter domains, have revealed that the magnetic field tends to be orthogonal to the filamentary structures in star-forming regions of the ISM. However, further observations with higher spatial resolution are needed to better understand the physical processes in these areas. An upgraded version of the BBOP instrument, initially developed for the SPICA mission, is proposed for future large aperture space observatories. This enhanced BBOP features three bolometer arrays sensitive to 100, 220, and 350-micron spectral bands. These silicon bolometers offer significantly improved sensitivity and polarimetric capabilities. Each pixel can detect two orthogonal polarization components, and the bolometer arrays operate at 50 mK with a differential read-out scheme. This allows simultaneous measurement of both total light intensity and polarization for each pixel. The presentation will cover the instrument's concept, design, estimated performance, and initial laboratory tests.
Session 19:
Time Domain II: High-Energy Transients
21 June 2024 • 09:00 - 10:00 Japan Standard Time | Room G303, North - 3F
13092-85
21 June 2024 • 09:00 - 09:20 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Infra-Red Telescope (IRT) is part of the proposed payload of the THESEUS (Transient High Energy Sky and Early Universe Surveyor) mission, which is one of the three ESA candidates for the next medium sized mission within the Cosmic Vision program, planned for launch in 2037. The IRT is composed by a 0.7 m class telescope and a camera, that will implement photometric and moderate (R~400) spectroscopic capabilities in the 0.7 - 1.8 microns wavelength range. Besides the IRT, THESEUS will carry two high-energy (X- and gamma-ray) telescopes, based on coded mask technology and “Lobtster Eye” micropore optics. The THESEUS payload is optimized for detection, localization and characterization of Gamma-Ray Bursts and other high-energy transients. The main goal of the IRT is to precisely localize the NIR counterparts of the high-energy sources and to spectroscopically measure their distance. Here we present the design of the IRT and its expected performance.
13092-86
21 June 2024 • 09:20 - 09:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The HiZ-GUNDAM is designed to provide alerts of high-redshift GRBs with an ultra-wide field X-ray monitor and a co-onboard 30-cm telescope for immediate photometric follow-up observations in the visible and near-infrared.
The five-band simultaneous observation at 0.5-2.5 µm is realized by a beam splitter and a Kösters prism. The telescope, the beam-splitter, the Kösters prism and the optical detector are cooled down to <200 K, and the infrared detector is additionally cooled down to <120 K by radiation cooling.
In this presentation, we introduce the current status of the development of the telescope onboard HiZ-GUNDAM.
Break
Coffee Break 10:00 - 10:30
Session 20:
Space Interferometry for Gravity Waves and Black Holes
21 June 2024 • 10:30 - 12:30 Japan Standard Time | Room G303, North - 3F
13092-88
21 June 2024 • 10:30 - 10:50 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The study of the universe through gravitational waves will yield a revolutionary new perspective on the universe, which has been intensely studied using electromagnetic waves in many wavelength bands. A space based gravitational wave observatory will enable access to a rich array of astrophysical sources in the measurement band from 0.1 to 100 mHz. A space based mission complements ground based gravitational wave observatories, which typically search for signals at higher frequencies. LISA is a space based gravitational wave mission. Telescopes are one of the technology contributions from NASA to the European Space Agency (ESA) for the Laser Interferometer Space Antenna (LISA) Mission. We will describe the key requirements and interfaces for the flight telescopes. We will also discuss the current status of the technology development effort.
13092-89
21 June 2024 • 10:50 - 11:10 Japan Standard Time | Room G303, North - 3F
Show Abstract +
LISA will be the first space-based gravitational wave observatory, enabling orders of magnitude greater sensitivity than the state-of-the-art LIGO facility. L3Harris is developing an engineering development unit (EDU) telescope in support of NASA, ESA and the LISA Consortium. The LISA EDU telescope validates a flight-like telescope design and reduces risks associated with stability, materials, assembly, integration, and testing. Mission requirements are unlike any other and require picometer-level stability across the entire telescope’s beam path, even in the presence of temperature variation and jitter. As a result, an all-glass telescope design was developed. From 2019-2024, the LISA EDU project has increased manufacturing readiness and technology readiness for the stable optical telescope element. This presentation will provide an overview of the LISA EDU design and why it was chosen, challenges with all-glass telescope development, and assembly of the telescopes.
13092-90
21 June 2024 • 11:10 - 11:30 Japan Standard Time | Room G303, North - 3F
Show Abstract +
We present the motivation and vision for the Black Hole Explorer (BHEX), a mission that will extend submillimeter Very Long Baseline Interferometry (VLBI) to space. BHEX, currently under formulation for a NASA Small Explorer mission, will discover and measure the bright and narrow “photon ring” that is predicted to exist in images of black holes, will reveal the processes that drive supermassive black hole creation and growth, and will connect supermassive black holes to their relativistic jets.
13092-91
21 June 2024 • 11:30 - 11:50 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Black Hole Explorer (BHEX) is a next-generation space very long baseline interferometry (VLBI) mission concept that will extend the ground-based Event Horizon Telescope into space. The Japanese community is poised to make major contributions to the mission, ranging from science to mission-critical instrumentation. Here we present the Japanese vision for the mission. A potential major technical contribution is providing key components for its sensitive tri-band receiving system, including SIS mixers at 230 and 345 GHz and a space-qualified multi-stage 4.5K cryocooler similar to that on JAXA’s Hitomi and XRISM satellites. The Japanese community envisions broad science cases spanning from various black hole physics/astrophysics explored with VLBI to molecular universe explored by the potential single-dish observing mode at radio frequencies to be explored for the first time with the BHEX mission.
13092-92
21 June 2024 • 11:50 - 12:10 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Black Hole Explorer: (BHEX) is a space mission to image radio emissions of black holes
by expanding both the baseline and time resolution of Very Long Baseline Interferometry (VLBI).
This involves integrating a space telescope into an array of ground telescopes, such as the Event
Horizon Telescope (EHT). Ultimately, the EHE will enable transformative science and the mission
goals are well aligned with the Astro 2020 Decadal Survey.
The EHE mission concept study was designed with three major stages: (1) a Science Study which
articulates plausible goals and objectives (2) an Engineering Study which articulates overall feasi-
bility and technological readiness and (3) a Mission Architecture Study which combines the results
of the previous studies to match achievable science goals and objectives with feasible engineering
to yield a plausible mission architecture. This paper review the initial steps taken under stage two of the EHE project.
13092-93
21 June 2024 • 12:10 - 12:30 Japan Standard Time | Room G303, North - 3F
Show Abstract +
We describe the baseline design of the science instrument for the Black Hole Explorer (BHEX), a space very long baseline interferometry (VLBI) mission concept currently in the formulation phase. BHEX will study supermassive black holes to understand fundamental physics, black hole jets, and the growth of black holes in galaxies. By co-observing with ground radio telescopes, BHEX will achieve 3-5 micro-arcsecond resolution from a distance of ~40,000 km. Observations will be conducted in two simultaneous bands between 80-350GHz, using an on-board low-power, low-mass ultra-stable oscillator as the master frequency reference, and the digitized data will be transmitted to the ground through an ultra-wide bandwidth laser downlink.
Break
Lunch Break 12:30 - 13:50
Session 21:
Solar System and the Sun
21 June 2024 • 13:50 - 15:30 Japan Standard Time | Room G303, North - 3F
13092-94
21 June 2024 • 13:50 - 14:10 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Near-Earth Object Mission in the Infra-Red (NEOMIR) is the first ESA's space-based mission fully dedicated to discovering NEOs, with a focus to detect and raise early warning for the smaller obejcts that are coming from the Sun dicection - thus nearly impossible to be detected from the ground. NEOMIR is currently in the early phases of mission study (phase A), with a potential launch date in early 2030s.
13092-95
21 June 2024 • 14:10 - 14:30 Japan Standard Time | Room G303, North - 3F
Show Abstract +
COronal Diagnostic EXperiment (CODEX) is a Heliophysics mission to measure the corona density, temperature, and velocity in order to test theories of solar wind acceleration and sources. The temperature and velocity measurement require much higher signal to noise ratio. The dominant noise for solar coronagraphs is the diffracted light from the Sun. This paper emphasizes on how to further suppress the diffracted sun light that existing coronagraphs currently achieve. The unique step is adding an innovative focal mask at the focus of the telescope. Based on analysis, this reduces the diffraction introduced stray light by ~ an order of magnitude. Furthermore, this paper also presents how the CODEX was aligned – Using the combination of metrology, alignment equipment, and real time diffraction ring monitoring to minimize the diffraction. The test results show that the solar brightness suppression reaches 10-11 level as required by science.
13092-96
21 June 2024 • 14:30 - 14:50 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Understanding the origin of the Martian moons is the main objective of the JAXA MMX (Martian Moons eXploration) mission, that will be launched in September 2024. Among the 13 instruments composing the payload, MIRS is an infrared imaging spectrometer that will map the mineralogy and search for organic compounds on the moons’ surfaces. MIRS will also study the Martian atmosphere, focusing on the spatial and temporal variations of water, dust and clouds. MIRS is operating in the 0.9-3.6 µm spectral range with a spectral resolution varying from 20 nm to 33 nm. The field of view covers 3.3° whereas the instantaneous field of view is 0.35 mrad. This presentation will detail the design and present the end-to-end performance obtained during the final instrument test in a representative thermal environment.
13092-97
21 June 2024 • 14:50 - 15:10 Japan Standard Time | Room G303, North - 3F
Show Abstract +
GrainCams is a suite comprising two cameras: SurfCam and LevCam, which EQM is developed by the Korea Astronomy and Space Science Institute (KASI) for the Commercial Lunar Payload Service (CLPS). SurfCam utilizes a light field camera with a Micro Lens Array (MLA) to capture 3D images of the fairy castle structures on the lunar surface. LevCam is designed to detect dust lofting above the lunar surface. Surviving extreme environments, including launch vibrations, lunar surface temperatures, space radiation, etc., necessitates thorough safety reviews, verification, and reliable ground testing of the system.
This paper presents the comprehensive design of GrainCams, along with the cameras' performance following space environment tests such as Total Induced Dose (TID), Electro-Magnetic Compatibility (EMC), Vibration/Shock, and Thermal-Vacuum tests. Performance test analysis plays a crucial role in ensuring mission success. Our demonstration confirms that GrainCams meet system requirements, and their performance in harsh environments is substantiated by sharing test results.
13092-98
21 June 2024 • 15:10 - 15:30 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Lunar Thermal Mapper (LTM) is a compact multi-band push-broom infrared radiometer on the NASA Lunar Trailblazer mission due to launch in 2024. The LTM optics consists of a fast (F1.5) 5-mirror diamond turned free-form system. The mirrors are machined from lightweighted aluminium blanks with integral mounting flexures. The system is assembled on an athermal aluminium optical bench to maintain alignment through the launch and under the challenging thermal environment of lunar orbit. With this novel optical system LTM achieves high resolution infrared imagery in a compact, low mass instrument. We present the design and model performance of the optics, details of the optomechanical design and manufacture, and results from AIT of an optical breadboard and LTM flight model instrument. As the LTM optical system is seeing reuse for future missions (such as MIRMIS on ESAs Comet Interceptor) we discuss the use of the LTM optical design with higher resolution detectors.
Break
Coffee Break 15:30 - 16:00
Session 22:
Space Astronomy on the Surface of the Moon
21 June 2024 • 16:00 - 17:20 Japan Standard Time | Room G303, North - 3F
13092-99
21 June 2024 • 16:00 - 16:20 Japan Standard Time | Room G303, North - 3F
Show Abstract +
Aim to Japan's participation in the Artemis program in the 2030s in mind, we pursue the feasibility studies of lunar telescope, including astronomical observations. Focusing on the meter-wavelength observations (observing frequency of lower than 50MHz), which cannot be observed in the harsh environments on the ground from the Earth, we plan the meter-wavelength interferometric array as lunar telescope, including the single-dish observations. The main scientific objectives we have studied so far are broadly covering the following three areas: astronomy and astrophysics, planetary science, and lunar science. In this paper, focused on the scientific requirements from the 21 cm global signal (spatial average temperature) observation from the Dark Ages, we will report the design concepts of Lunar Meter-wave Telescope (TSUKUYOMI), including the advanced feasibility studies of antenna, receiver, signal chain and spectrometer that are compared as other studies in US, China and Europe.
13092-100
21 June 2024 • 16:20 - 16:40 Japan Standard Time | Room G303, North - 3F
Show Abstract +
The Dark Ages Explorer (DEX) is the European initiative for a radio interferometry facility on the lunar far side. DEX will focus on performing neutral hydrogen cosmology observations, aiming to obtain the spatial power spectrum of density fluctuations throughout the history of the early Universe. DEX is planned to consist of a large number (>1024) of planar antenna elements deployed onto the lunar surface around the landing site, providing a densely filled aperture. The antenna elements are arranged in a regular grid, making it possible to generate sky snapshots by using the efficiency of a spatial 2D Fourier transform for every frequency bin. This talk introduces the concept design of DEX, shows the expected performance of the array in the presence of lunar regolith and discusses current and future efforts in technology development that are required to realise this design.
13092-101
21 June 2024 • 16:40 - 17:00 Japan Standard Time | Room G303, North - 3F
Show Abstract +
MoonLITE (Lunar InTerferometry Explorer) is an Astrophysics Pioneers proposal to develop, build, fly, and operate the first separated-aperture optical interferometer in space, delivering sub-milliarcsecond science results. MoonLITE will leverage the Pioneers option for utilizing NASA’s Commercial Lunar Payload Services (CLPS), for delivery of an optical interferometer to the lunar surface, enabling unprecedented discovery power by combining high-spatial-resolution from optical interferometry and deep sensitivity from the stability of the lunar surface. MoonLITE combines sub-milliarcsecond spatial resolution with sensitivity to observe targets fainter than 17th magnitude in the visible, exceeding ground-based interferometric sensitivity by many magnitudes, and surpassing space-based optical systems resolution by a factor of 50$\times$. MoonLITE takes advantage of the CLPS opportunity to place an interferometer in space on a stable platform -- the lunar surface -- and delivers an unprecedented combination of sensitivity and angular resolution at the remarkably affordable cost point of Pioneers.
13092-102
21 June 2024 • 17:00 - 17:20 Japan Standard Time | Room G303, North - 3F
Show Abstract +
LuSEE Night is a low frequency radio astronomy experiment that will be delivered to the farside of the Moon by the NASA Commercial Lunar Payload Services (CLPS) program in early 2026. LuSEE Night is designed to characterize the galactic radio foreground with best-yet sensitivity and depth but will also measure solar, planetary, and other astrophysical sources. The payload system under contract and being developed jointly by NASA and the US Department of Energy (DOE) and consists of a 4 channel, 50 MHz Nyquist baseband receiver system and 2 orthogonal ~6m tip-to-tip electric dipole antennas. LuSEE Night will enjoy standalone operations through the lunar night, without the electromagnetic interference (EMI) of an operating lander system and antipodal to our noisy home planet. LuSEE Night will also be supported by a NASA-funded far-field calibration source, in the form of a lunar-orbiting radio transmitter that broadcasts a pseudo-random code sequence; LuSEE Night will correlate against the code and use the signal to calibrate antenna pattern and system spectral chromaticity.
Session PS1:
Posters - Mission Concepts and Technologies for Small Spacecraft
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-103
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Pandora NASA Astrophysics Pioneers SmallSat mission employs a dual-channel observational approach, simultaneously utilizing visible photometry and infrared spectroscopy to assess stellar contamination of exoplanet transmission spectra. Pandora will use a PCO Panda 4.2M sCMOS sensor for the visible-wavelength photometry, while the near-infrared spectroscopy will use a 2.5-micron cutoff Teledyne H2RG detector. Both detectors have undergone thermal-vacuum testing at Lawrence Livermore National Labs to characterize their performance under flight-like conditions. This paper provides an overview of the Pandora detector test plan and the suite of tests conducted to date, shedding light on critical detector properties derived from subsequent analyses. Key parameters include read noise, gain, saturation, and persistence, offering insights into the detectors' capabilities and paving the way for enhanced data interpretation in the pursuit of unraveling the complexities within exoplanetary atmospheres.
13092-104
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Cubespec, a 6-unit CubeSat, serves as a high-resolution stellar spectroscopy demonstrator. The mission analysis involves careful orbit selection, considering avoidance angles around celestial bodies, and determining visibility windows for stars in the input catalogue. A star target scheduler is developed to meet scientific goals while managing ground access and respecting avoidance angles. Regular recalibration is crucial due to the limited accuracy of orbit propagators, ensuring the spacecraft's location accuracy for reliable observations
13092-105
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
CubeSpec is 6U CubeSat, targeting high-resolution optical astronomical spectroscopy, scheduled for launch by the end of 2025. The CubeSpec payload consists of an athermalized Cassegrain telescope with a rectangular aperture filling the surface area of 2 CubeSat units and a prism cross-dispersed echelle spectrograph (R=55000, wavelength range: 420-620nm). The complete optical payload fits in approximately 4 CubeSat units. A fine-guidance system consisting of a fast beam-steering mirror and a fine-guidance sensor, provides arcsec-precise centering of the source image on the entrance slit of the spectrograph. In this contribution, we describe the optical and optomechanical design of the payload, and discuss the challenges imposed by strong volume constraints. We also present the first results obtained with a prototype of the spectrograph.
13092-106
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
KU Leuven's CubeSpec mission is pioneering the use of a CubeSat platform for advanced space-based spectroscopy. This innovation is partly attributed to its payload electronics, which must be space-efficient and power-conscious. To achieve exceptional pointing accuracy, CubeSpec employs a High-Pointing Precision Platform (HPPP) that works in tandem with the onboard Attitude Determination and Control System (ADCS). The HPPP utilizes a Fine Steering Mirror (FSM), controlled by piezo actuators, which directs light precisely onto the spectrograph slit. This setup is controlled in a closed loop system with a Fine Guidance Sensor (FGS) and strain gauges that provide real-time feedback. Both the FGS and the science detector, which captures the spectrograph output, utilize the Gpixel GSENSE2020BSI CMOS sensor. Due to stringent time requirements, a Xilinx Zynq 7000 FPGA manages the detector readout. The design incorporates a DC-DC boost converter and a linear amplifier to meet the high-voltage demands of the piezo actuators.
13092-107
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
A-DOT (Active Deployable Optical Telescope) is a payload prototype of a 6U deployable telescope operating in the visible from 400 to 800 nm with an aperture diameter of 300 mm.
A deployable, single-segment, prototype was designed to demonstrate the mechanical alignment and phasing strategy: tip, tilt and piston are controlled using piezoelectric actuators at three contact points and the segment position measured using capacitive sensors.
Structural-Thermal-Optical-Performance analysis was performed based on several orbital heat loading scenarios. The impact on image quality caused by deformation of the telescope mirrors due to thermal radiation during orbit was assessed.
13092-108
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
In the search for life in our galaxy, and for understanding the origins of our solar system, the direct imaging and characterization of earth-like exoplanets is key. In a step towards achieving these goals, the STARLITE mission (Superluminous Tomographic Atmospheric Reconstruction with Laser-beacons for Imaging Terrestrial Exoplanets) uses five CubeSats in a highly elliptical orbit as artificial guide stars to enable tomographic reconstruction of the atmosphere for extreme multi-conjugate adaptive optics (MCAO). Through the use of current and next-generation extremely-large ground-based telescopes, the STARLITE constellation at its ~350,000km apogee will provide -3 magnitude artificial guide stars from a 10cm launching telescope in a sub-arcminute field of view for up to an hour. Careful selection and design of the ~760nm on-board laser will allow O2 detection and characterization of exoplanet atmospheres. At a size of 12U, each satellite weighs only 32kg and utilizes mostly commercially available off-the-shelf parts to keep costs per satellite around $2M. In this paper we will present the satellite mission concept and early 3D system design for the STARLITE constellation.
13092-109
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We demonstrate the performance of our developing LCTF (Liquid Crystal Tunable Filter), which is an optical bandpass filter consists of several layers of polarizers, wave plates, and liquid crystal cells. Its transmission wavelength can be controlled electronically by changing the voltage applied to the liquid crystal cells. The peak transmittance of the LCTF we developed is approximately 20-40 %, the band width (FWHM; full-width at half maximum) is 10-100 nm depending on the wavelength. This device is compact (37 x 37 x <30 mm3), light-weight (95 g), low power consumption, and can be used in a wide temperature range (0-45 deg). Therefore, it is suitable for multi-spectral or hyper-spectral imaging mounted on small satellites. We have experience in conducting observations on orbit by five small satellites equipped with our LCTFs. We also introduce our patent for the optical arrangement to bring out the performance of LCTFs.
13092-110
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
A new method for the measurement of polarization was thoroughly investigated during the last years, from the theoretical and numerical perspectives. The method employs a new type of optical modulator based on birefringent prisms with different fast axis orientations. The modulator achieves a continuous variation of the polarization state of the transmitted beam in a given direction. Associated to a fixed linear polarizer and a dispersive element, the modulator allows the snapshot measurement of any kind of uniform polarization, without moving components and for a continuous bandwidth. We present the characterization process of the first batch of modulators, the optical experimental setup and the characterization results for several wavelengths. Afterwards, we describe the first results of the measurement of different polarization states at several wavelengths and we compare them to the numerical ones. We conclude with the future developments of this method.
13092-111
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We are developing a new compact and broadband infrared imaging Fourier spectrometer based on the common path wavefront division phase shift interferometry. Based on this principle, a 3-reflector point-to-point optical system with overlapping optical paths was constructed by applying two free-form mirrors and an upside/downside pair of flat mirrors with a height of 35 and a width of 70 mm each. By detailed optimization of the parameters for two free-form mirrors, in which one collimates the beam from the multi-slit, and the other re-focused onto the FPA detector, we find the best structure for the optical system of the IR imaging spectrometer for the wavelength range of 4 - 20μm, employing the commercially available uncooled bolometer camera (640 x 480 pixels with 17 μm unit pixel size). In our design, all optical components can be mounted in an enclosure with 120 x 120 x 80 mm dimensions.
13092-112
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We present the concept for STARI: STarlight Acquisition and Reflection toward Interferometry. If launched, STARI will be the first mission to control a 3-D CubeSat formation to the few mm-level, reflect starlight over 10s to 100s of meter from one spacecraft to another, receive that light and control tip-tilt with sub-arcsecond stability, and validate end-to-end performance by injecting light into single-mode fiber. This will advance the Technology Readiness Levels of the essential subsystems needed for a space interferometer in the near future. We end by outlining prospects for a space interferometer science mission after STARI that would demonstrate formation-flying interferometry for the first time, built around exoplanet and black hole science cases.
13092-113
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
RAFTER (Ring Astrometric Field Telescope for Exo-planets and Relativity) is a TMA telescope concept aimed at astrometric missions, and providing a wide FOV and high optical response uniformity over an annular region around the optical axis.
This paper describes and analyzes the process of miniaturization and implementation of this idea into a Cubesat for technology demonstration purposes, and to evaluate its feasibility by analysing the performance and challenging aspects of different designs, calculating their mechanical tolerances and thermal sensitivity.
We outline the critical aspects of the payload that can be tested and optimized in the framework of a dedicated CubeSat mission, in order to demonstrate the enabling technological contributors crucial to the development of a future larger scale mission.
13092-114
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We present here an STM32 microcontroller based on-board computer designed for use in
small satellites and CubeSat missions that was developed using commercial-off-the-shelf (COTS) electron-
ics components. An on-board computer (OBC) is one of the important subsystems of any CubeSat mission.
An on-board computer is the central brain of a CubeSat or small satellite, responsible for coordinating and
controlling various subsystems to achieve mission objectives efficiently and autonomously. It performs cru-
cial tasks like power management, communication, command and data handling, on-board data processing
and on-board software execution. This paper discusses the development of one such OBC designed for a
spectroscopic mission called Spectroscopic Investigator of Nebular Gas (SING).
13092-115
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Visible Extragalactic background RadiaTion Exploration by CubeSat(VERTECS) is designed for observing Extragalactic Background Light(EBL).
VERTECS mission requires attitude control stability better than 10 arcsec (3σ) per minute and the orbit and attitude to avoid the sun-or earth-shine entering the telescope.
We discuss the software-in-the-loop (SIL) attitude simulator simulation to verify if the current Attitude and Orbit Control System (AOCS) design and the planned orbit can meet the requirements for EBL observations. To perform the simulation, we use the SIL simulator developed by the Intelligent Space System Laboratory. The simulation software calculates the attitude control commands considering the parameters of the AOCS hardware and the expected attitude disturbances in the assumed orbit.
This simulation is expected to show the orbital parameters and AOCS hardware configuration to achieve the attitude stability mentioned in requirement and the sequence of attitude maneuvers to meet the requirement.
13092-116
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The extragalactic background light (EBL) is the integrated emission from out of our Galaxy.
The Visible Extragalactic background RadiaTion Exploration by CubeSat (VERTECS) is an astronomical 6U satellite that observes the EBL in visible wavelength. To observe the EBL, a telescope is equipped within 3U. The remaining 3U is the bus section mainly based on the heritage standard bus design of Kyushu Institute of Technology. This paper describes the structural design and verification of the STM model of the satellite to satisfy the launch and mission requirements. Stress and frequency analysis are performed to verify the satellite’s strength and stiffness under the expected loading conditions. A series of mechanical environmental tests (shock, random, and sinusoidal vibrations) are scheduled to verify the design and analysis results.
13092-117
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
VERTECS (Visible Extragalactic Background Radiation Exploration by CubeSat) is a CubeSAT project aiming to observe the Extragalactic Background Light (EBL), crucial for understanding the universe's history. This satellite (sized at W6U) is equipped with deployable solar array panels (DSAP), and it operates in a sun-synchronous orbit at 500 km altitude. To observe the EBL, high performance payloads are essential, however these components consume a significant amount of power. Therefore, some strategic operational plans are necessary to operate this CubeSAT within the constraints of limited power resources. We have devised some operational scenarios utilizing attitude control and DSAP to meet our mission requirements and constructed a power budget simulation. In this presentation, we describe the operational strategy, subsystems, and the outcomes of power simulations which enable the mission successful.
Session PS2:
Posters - Astrometry
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-184
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The CEntral (field) Three-mirror Anastigmat (CETA) telescope is designed
on the specifications of the proposed Theia mission, aiming at high
precision differential astrometry over a large field, for exo-planetary
system characterization and dark matter /dark energy search through the
dynamics of star clusters.
Usually, Three Mirror Anastigmat designs are either off-axis in terms
of field, or decentered in terms of pupil.
We propose a family of solutions using fully centred optics and a large
on-axis field, at the expense of a non negligible central obscuration.
We analyse in particular a 1 m class compact telescope, with 15 m
effective focal length, i.e. suited to small pixel (4-6 $\micro$m)
CMOS detectors operating in the visible and near IR.
Due to the underlying symmetry, the resulting optical response is quite
good over a 14 arcmin radius field, and it is of special interest to
astrometry applications. Also, manufacturing, alignment and calibration
can be expected to benefit significantly; some basic aspects are
preliminarily considered.
13092-185
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
JASMINE is a Japanese near-infrared space mission with the scientific objectives of ultra-high-precision astrometric observations of stars in the central region of the Galaxy and exploration of terrestrial exoplanets around M-type stars. To achieve these scientific objectives, we are developing a 36-cm aperture diffraction-limited telescope with an emphasis on ultra-low stable telescope structure. The telescope will be equipped with an infrared detector and a bandpass filter for the wavelength range of 1000-1600 nm. For the astrometry, the telescope will have a high optical performance: the Strehl ratio larger than 0.9 at near-infrared wavelengths and is required to have a stable image distortion of less than a few tens micro arcsec during a low Earth sun-synchronous orbital motion. The telescope has an axisymmetric Korsch-type optical system which is easy to be designed to have the high optical performance over a large field-of-view. We present the progress of the telescope optics design, optics alignment/adjustment procedures, and telescope optics evaluation and verification procedures.
13092-186
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
One of the prime science objectives of Japan Astrometry Satellite Mission for INfrared Exploration (JASMINE) is to reveal the central core structure and formation history of the Milky Way galaxy through infrared astrometry at 1.0 – 1.6 micron. For this purpose, the JASMINE telescope is required to be highly stable with an orbital/seasonal variation of the image distortion pattern being less than a few 10 micro arcsec. The stability of the JASMINE telescope system is investigated by performing the Structure, Thermal, and Optical, Performance analysis. The thermal model of the JASEMINE telescope system is utilized to estimate the in-orbit temperature distribution and its variation. This is followed by the structural analysis which evaluates the thermal distortion of the telescope system. Finally, the variation of the image distortion pattern is evaluated from the optical model. It is suggested that the current telescope design possibly meets the JASMINE requirement.
Session PS3:
Posters - Mid- and Far-Infrared Mission Concepts and Technologies
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-230
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
This paper covers Ball’s 4 K Cryocooler, which is comprised of TRL 6-9 subassemblies and meets the needs of multiple future space missions. The 4 K Cryocooler is comprised of a hybrid Stirling Pre-Cooler and a J-T (Joule-Thomson) Cryocooler driven by the MACCE (Modular Advanced Cryocooler Control Electronics). The Stirling Pre-Cooler uses the Ball 2-stage SC-235C 2-stage cryocooler which has flown on the TIRS-1 and TIRS -2 NASA missions. The precooler provides cooling at 15-18 K to precool the J-T Cooler and around 65 K to intercept thermal system heat loads. The J-T Cryocooler uses the TRL 9 flight SC-235/TIRS compressor with reed valves with a J-T cold head (heat exchangers, plumbing, J-T valve, etc.) from the ACTDP TRL 6 Engineering unit that demonstrated cooling to 3.4 K. The MACCE electronics are TRL 8 and have been delivered for flight.
13092-231
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We have developed a robust bandpass filter that is suitable for use in mid- and far-infrared cryogenic space telescopes using simple photolithography. The filter consists of Babinet complementary metamaterial mirrors, which are sub-wavelength holes on a silicon wafer with metalized rim and bottom, and non-metalized side wall. The mirrors work as a “Fabry-Perot interference” type bandpass filter and have a spectral resolving power of R~10. The central wavelength is tunable by adjusting the optical distance between the surface and the bottom. It has higher mechanical toughness compared to conventional metal mesh-filters because of the support of the silicon wafer. It also has higher resistance to thermal cycles compared to conventional multi-layer filters because of its simple structure. The central wavelength can be configured only by the sub-wavelength structure without changing the depth of the holes, so that monolithic filters with different central wavelengths at each position can be fabricated.
13092-232
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The COBE/FIRAS mission observed the Cosmic Microwave Background (CMB) energy distribution, revealing a near-perfect blackbody spectrum to an accuracy of ΔI/I = 10^(-5). These are referred to as spectral distortions. Measurements of these signals are challenging but allow us to access information about the full thermal history of the Universe. High-precision CMB spectroscopy emerges as one the three main focus in the ESA Voyage 2050 program. Several dedicated space missions such as PIXIE, PRISTINE, and FOSSIL have been proposed since 2011. Additionally, a balloon-borne project, BISOU, is being considered as a pathfinder of a future space mission dedicated to CMB spectral distortions.
I will present a new and versatile instrument model for such future projects. In conjunction with a sky emission model, we can then optimize both instrument concept and mission parameters. Additionally, the model aids in investigating potential instrumental systematics for upcoming CMB distortion experiments.
13092-233
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Probe far-Infrared Mission for Astrophysics (PRIMA) contains two instruments: an imager (PRIMAGER) and a multi-band spectrometer (FIRESS). These two instruments require detector cooling to 100 mK and require parts of the optical train to operate at 1.0 K. From a base temperature of 4.5 K, provided by a JWST-like cryocooler, a 5-stage Continuous Adiabatic Demagnetization Refrigerator (CADR) will provide this cooling to both instruments. The PRIMA CADR is based on heritage parts from the Hitomi and the X-Ray Imaging and Spectroscopy Mission (XRISM) ADRs and from recent Strategic Astrophysics Technology (SAT)-developed hardware. The CADR will provide 700 microW of lift at 1.0 K and 9 microW of lift at 100 mK to meet the two instruments (PRIMAGER and FIRESS) cooling requirements with a factor of 2 margin. The CADR is designed to reject a maximum of 8 mW at the 4.5 K cryocooler heat sink. This paper will describe the CADR, its requirements, its operation, and its heritage.
13092-234
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
PRIMA is a cryogenically-cooled, far-infrared observatory for the community for the beginning of the next decade (~2031). It features two instruments, PRIMAger and FIRESS. The PRIMAger instrument will cover the mid-IR to far-IR wavelengths, from about 25 to 260 microns. Hyperspectral imaging can be obtained in 12 medium-resolution bands (R ~ 10) covering the wavelength range from 25 to 80 microns, and broad-band (R ~ 4) photometric and polarimetric imaging can be carried out in four bands between 80 and 260 microns.
PRIMAger’s unique and unprecedented scientific capabilities will enable study, both in PI and GO programs, of black hole and star-formation coevolution in galaxies, the evolution of small dust grains over a wide range of redshift, and the effects of interstellar magnetic fields in various environments, as well as opening up a vast discovery space with its versatile imaging and polarimetric capabilities. One of the most ambitious possibilities is to carry out an all-sky survey with PRIMAger’s hyperspectral mode, creating a rich data set for many investigations. The design of PRIMAger is presented is an accompanying paper (Ciesla et al.)
13092-235
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
SALTUS is a mission concept for a THz observatory proposed for the NASA Astrophysics Probe Explorer Opportunity. This paper will review the architecture and explain the rationale behind the design. The paper will give special attention to the 14 m diameter inflatable primary mirror, its inflation and pressure control and expected lifetime. The choice of a large inflatable primary reflector results in large collection areas at very high mass efficiency enabling the science mission. We describe the spacecraft bus, and the receiver, a heritage design based on the GUSTO balloon heterodyne system and SAFARI. We also discuss the observing strategy and pointing requirements from its planned L2 location. Particular emphasis is placed on challenges to the design, such as momentum management, balancing consumable mass allocations, thermal management, and testing.
13092-236
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Theoretical calculations predict that high-resolution spectroscopy of H2O gas in the mid-infrared region is the most promising method to observationally identify the snow-line, which has been proposed as the critical factor separating gas giants from solid planets in the planetary formation process. This requires the spectroscopic observations from space with R ∼ 30,000. For this purpose, we are proposing a mid-infrared (10-18 micrometers) high-resolution spectrometer to be onboard the GREX-PLUS (Galaxy Reionization EXplorer and PLanetary Universe Spectrometer) mission. To enable high-resolution spectroscopy in space, we are developing "immersion grating" spectroscopy technology. We have chosen CdZnTe as a candidate for the optical material. We report the current status of the development of the CdZnTe immersion grating, including evaluation of its optical properties (absorption rate and refractive index) at cryogenic temperatures, verification of machinability for grating production, and development of an anti-reflection coating with a moth-eye structure for wide-wavelength coverage.
13092-237
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We cryogenically measured the transmittance of high-resistivity CdZnTe, a small absorbance material candidate of Immersion grating (IG) for the next-generation infrared astronomical satellite, GREX-PLUS, which realizes high-spectral dispersion R = λ/∆λ ∼ 30, 000 in 10 – 18 µm aiming for the snowline detection toward protoplanetary nebulae.
We measured the transmittance of high-resistivity CdZnTe in 8-14 μm by employing the new FT-IR imaging spectrometer with common path wavefront division phase shift interference for the cryogenically cooled CdZnTe sample. The transmittance obtained was 0.71±0.01 at the wavelength of 10.6 µm, with no significant temperature dependence in the range 6 – 300 K.
We also developed a new measurement system for transmittance in 10-18 μｍ with cryogenic common-path double beam optics, which enables accurate determination of the absorption coefficient at the cryogenic temperature by considering the effect of the multiple Fresnel reflection at the sample surface.
13092-238
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We’re developing an Immersion Grating (IG) made of CdZnTe designed for a high-dispersion mid-infrared spectrograph (10-18 µm, R = λ / Δλ ~ 30,000) to be onboard the next-generation infrared space telescope GREX-PLUS. The adoption of a IG will reduce the spectrometer size to 1/n (1/n^3 in volume, n: refractive index) compared to conventional diffraction gratings. To determine this absorption coefficient accurately, we need to take the effect of multiple reflection into account that depend on the refractive index. However, accurate the refractive index of CdZnTe (Δn < 10^-4) at 10-18 µm below 20 K has not been measured yet.
Therefore, we’re developing a measurement system of the refractive index at cryogenic temperatures in the mid-infrared range. We adopt the minimum deviation method in this system to measure the refractive index, measuring the apex and deviation angle of the prismatic material.
Session PS4:
Posters - Wide Field Survey Missions
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-239
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Near Infrared Spectrometer and Photometer (NISP) detector system (DS) of the ESA's Euclid mission was successfully commissioned in the second semester of 2023. Here are presented results obtained during this period, focusing on the comparison between the in-orbit and on-ground performances of the near-infrared detectors (H2RGs) and onboard data processing. The final NISP detector configuration presented here includes the onboard software parametrization, and a set of detector's noise sources are examined along with their monitoring over this first phase of Euclid’s activity. Among the highlights of the NISP DS commissioning are the determination of the in-flight detector's thermal pedestal (or baseline), the tuning of a statistical indicator for the goodness of the scientific signal evaluated on-board, and the study of different components of the kTC noise.
13092-240
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Euclid is an ESA wide-field space mission dedicated to the high-precision study of dark energy and dark matter. In July 2023 a Space X Falcon 9 launch vehicle put the spacecraft in its target orbit, located 1.5 million kilometers away from the Earth, for a nominal lifetime of 6.5 years. The survey will be realized by means of a wide field telescope and two channels: a VISible imaging channel (VIS) and a Near Infrared Spectrometer and Photometer (NISP). In this paper, we present an overview of the NISP instrument operations as they are at the end of the instrument calibration phase. The necessary tools, workflows, and organizational structures are described. Finally, we highlight how the concept of an integrated instrument development and verification approach turns out to be vital to address systematic effects and technical issues and to reduce the overall cost of the mission.
13092-241
Estimating optical aberrations of NISP's Instrument through machine learning and Zernike polynomials
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
This study, within the Euclid mission's Near Infrared Spectro-Photometer (NISP), integrates advanced numerical modeling and machine learning to assess optical aberrations in the Point-Spread Function (PSF). Employing Zernike polynomials and neural networks, we showcase the capability of machine learning algorithms to detect and quantify optical aberrations using simulated data. Ongoing efforts involve refining these models with experimental data from ground validation and in-flight calibration phases, contributing to a comprehensive understanding of the NISP instrument's optical performance. Aligned with the Euclid mission's goals, this work advances insights into the NISP instrument and its critical role in probing the mysteries of dark matter and the accelerated expansion of the universe.
13092-242
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Euclid is a space-based optical/near-infrared survey mission of the European Space Agency (ESA) to investigate the nature of dark energy and dark matter. Scientific objectives demand a pointing stability of few tens of milliarcseconds (mas), which is achieved using a Fine Guidance Sensor (FGS) that provides high-precision pointing information as input to the spacecraft Attitude and Orbit Control Subsystem (AOCS). During the Performance Verification Phase, a reconstruction of instantaneous attitude at high precision has been achieved by using science instruments in special operating modes. The pointing jitter derived from these observations is correlated with the FGS/AOCS reported attitude to evaluate consistency. A precision of 2-3 mas is achieved in the reconstructed attitude at 30 ms time resolution in the optical channel, and 3 seconds in the infrared channel. The observation design, data analysis techniques and reconstructed attitude jitter curves are presented.
13092-244
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Nancy Grace Roman Space Telescope project is NASA's next flagship astrophysics mission to study dark energy, dark matter, and exoplanets along with the innumerable topics that will be enabled by the infrared survey telescope's instruments. The Wide Field Instrument contains a focal plane of 18 newly developed Teledyne H4RG-10 HgCdTe detectors. Roman's focal plane completed its first system level thermal vacuum test at NASA Goddard in 2022, when an increase in dark current compared to component level testing was observed for several detectors. Roman chartered an anomaly review board (ARB) and in collaboration with Teledyne undertook a testing program to help identify possible root cause and select from Roman's spare inventory suitable replacement detectors for devices that had significantly degraded. A possible root cause was determined by the ARB along with recommendations for how to prevent further degradation. We summarize the initial observation of the detector anomaly, present the detector testing strategy to find suitable spares and provide evidence of root cause, share the general findings of the ARB, and show new data showing the improved dark current performance.
13092-246
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
With a series of custom near infrared linear variable filters, and six HAWAII-2RG detectors, the SPHEREx satellite telescope will study the physics of cosmic inflation, the history of galaxy formation, and the content of biogenic ices in the Milky Way. SPHEREx will fly as a fixed focus system, eliminating the potential single point mechanical failure introduced by a focus mechanism. To precisely characterize and set focus of the SPHEREx optics, we implement a custom collimator system which couples to the telescope, cooled inside of a cryogenic chamber, through a large sapphire vacuum window. A cold filter reduces background thermal infrared loading which would otherwise saturate the detectors. Here, we describe the collimator setup for focus measurements in the laboratory, design details for the test chamber vacuum window and cold filter, calibration of the collimator and coupling optics, sources of measurement error, and results from SPHEREx focus measurements in which we achieve ~6 um statistical and ~15 um systematic error.
13092-247
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The SPHEREx satellite will survey the entire sky between 0.75 - 5.0 micron in over 100 wavelengths with spectral resolving power R = 35 to 130 to study cosmic inflation, the history of galaxy formation, and biogenic ices in the Milky Way. The instrument uses six HAWAII-2RG detectors and linear variable filters (LVF) that sort incoming photons into different wavelengths along one spatial direction of the detectors. To minimize the scattered light produced when sources outside of SPHEREx field of view land on the LVF mounting frame (also known as ``dragon’s breath’’), a scale model was tested to refine a double undercut edge design and coating recipe that halves the ghost size and reduces the ghost’ intensity by 10-fold. We present here the edge design, the scale model experiment, and the characterization of the ghost in the flight telescope.
13092-248
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
SPHEREx is a NASA medium-class explorers (MIDEX) mission planning to launch in early 2025. It is designed to study the origin of the Universe, evolution of galaxies, and surveying water and organic molecules in interstellar ices by producing the first all-sky near infrared spectral survey at 0.75 to 5 micros with spectral resolution ranging from R = 35 - 130.
In this presentation, we will show the SPHEREx spectral design, which is constructed with a dichroic beam splitter, the Linear Variable Filters (LVFs), and the 6x H2RG detectors. We will also present the telescope spectral calibration measurements including the precise in-band transmission and out-of-band blocking of each of the 25millions pixels.
13092-250
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
ARRAKIHS is an ESA mission dedicated to observing dwarf galaxies and stellar streams. Its objective will be to test the standard cosmological model, particularly regarding the nature of dark matter. It will use four telescopes operating in the visible and near infrared spectral ranges. As they will observe ultra-low brightness objects, an extreme level of stray light control is necessary. A large external baffle is necessary to prevent out-of-field light from entering the telescope, with an extreme stray light rejection down to 10-11. This paper will discuss the design of this baffle. We will present the design trade-offs, as different possible baffle architectures were considered. Ultimately, the selected architecture consists in developing one baffle for two telescopes, hence a total of two baffles are used on the payload. A multi-stage baffle is developed, in the heritage of the CoRoT baffle which is seen as one of the best ever designed. Moreover, we will discuss the reflections on the test setup which will be implemented for validating the design on a prototype.
13092-251
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We describe our technical approach to developing a space observatory to survey the large-scale distribution of neutral and ionized intergalactic gas during cosmological reionization (the landmark event of “Cosmic Dawn”) from 400 to 800 million years after the Big Bang. To look this far back in time at the large-scale distributions of ionized gases, we use wide-field, narrow-passband surveys for Lyman alpha light from individual galaxies red-shifted to the near-infrared. Wherever this light can be seen, it implies the presence of ionized gas. We are developing a large FOV (0.5-to-1.0-degree) instrument with plate scale on the order of 0.3”/pixel to obtain a comprehensive view of the reionization process over a representative volume of the early universe.
To maximize science return, the Reionization Explorer (REX) will be placed in a high orbit. Through disciplined application of design-for-cost principles and a thorough searching for existing designs that can achieve our science objectives, we have developed what could be a game changing approach at advancing our understanding of the formation of the universe on a limited Small Explorer (SMEX) budget. By leveraging existing te
Session PS5:
Posters - Manufacturing, Optomechanical, and Electronics Technologies for Space Applications
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-252
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
JWST has been successfully launched and NIRSpec operating as designed with the microshutter arrays assembly as one of the enabling technologies. We have been working on the development of the Next-Generation Microshutter Array (NGMSA) device as a spaceflight-qualified field object selector mask for multi-object spectroscopy (MOS) for the future observatories with the Habitable World Observatory (HWO) as a primary target. The technological goal of this development is defined by the expectation of the strategic space flight missions large format field selector masks. We present the status of the NGMSA large format arrays technology readiness. Our development demonstrated the small format NGMSA devices in the Far-ultraviolet Off Rowland-circle Telescope for Imaging and Spectroscopy (FORTIS) sounding rocket flight. It opened the path to the large format arrays qualified for the next generation of the space borne observatories. We present our current status of the arrays fabrication, functional and optical performance in the UV on the newly developed test facility, integration and the plans to scalability of the individual devices into the focal plane assembly.
13092-253
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The James Webb Space Telescope’s (JWST) Center of Curvature Optical Bench (CoCOB) hexapod was repurposed to enhance NASA Marshall Space Flight Center’s X-Ray & Cryogenic Facility (XRCF) optical metrology capabilities. This upgrade increased test article load capacity, extended measurement ranges of motion, coupled the hexapod with an additional axis of motion, integrated a complementary X-Y-Z translational stage and COTS hexapod, and supported commanding of these enhanced capabilities through a modern control architecture. This paper discusses the justification for re-using the CoCOB by highlighting its unique precision motion control capabilities in a high vacuum and optically clean environment. The design and key component selection for the additional motion stages is presented along with performance test results for all axes. Finally, a summary of the motion control system architecture and its flexibility to address tomorrow’s optical metrology needs are presented.
13092-254
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
DEPFET detectors with repetitive non destructive readout (RNDR) achieve deep-sub electron noise and present a unique technology for high precision measurements with high time resolution. Due to the active pixel sensor concept, the readout process can be fully parallelized and configured with high modularity. Due to the fabrication standards for X-ray spectroscopy, this properties are combined with a fully depleted 450 µm thick bulk, an excellent entrance window and a low dark current. This enables cutting edge applications in direct dark matter detection experiments and photon number resolved measurements down do the near infrared regime.
We will present a performance characterization of different RNDR-DEPFET detectors, combined with results from proton irradiations of DEPFET detectors without repetitive readout. As no lateral charge transfer is needed at DEPFET detectors, an excellent radiation hardness - relevant for space applications - is expected and will be modelled.
13092-256
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Hybrid microwave kinetic inductance detectors based on niobium-titanium-nitride and aluminum are our main workhorse for the far-infrared (FIR) instruments that we develop. We have improved our aluminium patterning route by using electron beam patterning and wet etching, improving feature dimensions to linewidths of 300 nm. We have incorporated measures to limit dewetting effects, and improve reproducibility, quality and yield. This patterning route has been used for detector chips which have been delivered and commissioned on instruments for various ground based telescopes, and is an important novelty in the realization of the prototype chips for the NASA FIR PROBE proposals.
13092-257
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Apertures define the maximum diameter of a light beam that can pass through a telescope. Diaphragms that contain the aperture and are placed in the optical path are called aperture stops. For an efficient reduction of straylight, black aperture stops that absorb non-imaging light are applied.
For space-based applications in particular, the aim is to keep the mass and number of individual elements, integrated into the optical system, as low as possible. In this contribution, we will present how a coated black aperture stop can replace a mechanical aperture. This coated black aperture stop can be combined with anti-reflection coatings (in case of lenses) or highly reflective coatings (in case of mirrors).
The presented black aperture coatings were deposited on top of AR coatings to operate at different wavelength bands between ~ 750 nm and ~ 2100 nm. All coating combinations were qualified for space-based application.
13092-258
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Optomechanical charateristics would be critical to operate at observational site condition. In order to predict optomechanical performances during thermal variations, we simulate under actual boundary condition and prepare laboratory test with 350 mm SiC mirrors using thermal vacuum chamber. In this paper, we will briefly present the current simulation results and the preparation status for the experiment.
13092-259
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Presentation on how collaborative engineering has enabled advancements at Optimax Systems in filter, mirror and anti-reflection coatings for Space and Astronomical applications and their pivotal role in enhancing the performance and durability of spaceborne components. This talk will cover current capabilities as well as future development work.
13092-260
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Cordierite materials can be used as a reflected optical surface for astronomical space and ground-based telescopes due to their high rigidity and low CTE (Coefficient of Thermal Expansion) which is ±1.94×10⁻⁸m/℃. Using Cordierite materials in astronomical telescopes requires polishing techniques to control quantitatively. Therefore, it is essential to study the material removal properties using Tool Influence Function (TIF), which plays an important role in improving optical performance. In this paper, we present the characteristics of initial Tool Influence Function on Cordierite substrates.
13092-261
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Fabrication of ultra-precise CFRP (Carbon Fiber Reinforced Plastic) mirrors without the need for mirror polishing, utilizing replica technology has been studied. Conducted as part of an international collaborative research project between Germany and Japan, we achieved a mirror accuracy of 0.5 µm RMS in shape and 5 nm RMS in surface roughness for a φ300 mm spherical mirror. Despite this accomplishment, challenges remain in meeting the precision requirements for visible light telescopes, with defects such as bubbles and areas of insufficient accuracy.
Post-project investigation led to the identification of molding and replicating conditions for achieving even higher mirror accuracy. The corrective effect of replica technology on mirror surface accuracy was explored and the limitations of improvement achievable through replica processing was investigated. It was found that pre-replication of sand-blast polishing can improve surface roughness to 3 nm. This report details the results of our investigations and improvements in pursuit of superior mirror accuracy.
13092-262
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The use of aluminum substrate for space telescope mirrors is wide spreading in space field. This choice makes conceivable to combine mirror component and its support in one single part.
This study is focused on M2 design case and on performance evaluation of M2 design baseline, in the framework of a reference space mission.
A baseline design of M2 is verified through FEM analyses: modal analysis and static analyses with survival and operative loads. The baseline design is modified to identify the sensitivity of induced surface deformation to design parameters under study. A first trade-off between design alternative options is provided.
13092-263
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Radio telescopes play a crucial role in the study of the universe, allowing us to investigate celestial phenomena and enhance our understanding of astrophysics. This paper proposes the use of lightweight foam material integrated with a reflective thin film that can reflect gigahertz radiation as an alternative to traditional aluminium panels in the construction of radio telescope panels. The primary objective is to highlight the advantages of this panel design, focusing on the potential advancements it offers in terms of reducing weight and cost. Dish deformation due to the self-weight is the major challenge faced by the future giant (above 30m in diameter) submillimetre telescopes. The mirror fabrication and qualification are verified by measuring reflectivity, surface quality (rms) and accelerated aging through fast thermal cycling. The potential applications of the foam-based reflective thin film panels extend beyond their use in radio telescopes. The lightweight characteristics, low cost, and ease of integration make these panels suitable for portable radio antenna and drone observations.
13092-264
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
In the frame of an international R&D project a team from Japan and Germany were developing a replica process to manufacture a CFRP honeycomb mirror for visible application. The main target was to generate the optical surface with minimized effort to achieve a microroughness of better 1 – 2 nm RMS. This technology would enable the team to manufacture cost effective mirrors for larger amounts like for constellations.
In this paper we will present the recent results of this development and a the finally achieve performance of a 300 mm light CFRP We will also present lesson learned for next steps of development to achieve such mirrors with a optical performance not only for microroughness but also for surface accuracy.
13092-265
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Habitable Worlds Observatory (HWO) is the current concept of NASA’s next flagship mission on searching for signatures of life on planets outside our solar system.
LISA, the Laser Interferometer Space Antenna and ESA’s flagship will detect gravitational waves with the help of a gigantic laser systems spanned by triangle of three satellites each 2,5 billion kilometers apart.
Both missions have tremendous requirements on the stability in the picometer range of the materials for the optics, positioning mechanics and optical benches. ZERODUR® has a strong heritage for its extremely low coefficient of thermal expansion and its excellent homogeneity in the single digit ppb/K CTE range over the entire blank volume.
At SCHOTT, several development programs are dedicated to fulfilling the requirements of future space telescope missions. Our glass ceramic material has been analyzed with respect to the low CTE application temperature range and long-time stability. Several geometrical designs are considered to deliver the best trade between stability, stiffness and weight.
This paper presents our material property and design results valuable to realizing picometer stability optics.
Session PS6:
Posters - Exoplanet Time Series Observations: Science Data Processing & Simulations
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-268
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The NIRISS Single Object Slitless Spectroscopy mode makes uses of a cross-dispersed prism to obtain spectra at a resolving power of R=650 covering wavelengths between 0.85 and 2.85 microns across 2 spectral orders. The SOSS mode is primarily used for exoplanet time-series observations, typically integrating light for over 5 hours. This work presents a library of SOSS spectra of planet-hosting stars with extremely high signal-to-noise ratio. The spectrum extraction method, wavelength and flux calibrations are presented.
13092-269
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Ariel is an ESA Medium class science mission due for launch in 2029 and will characterize the atmospheres of a diverse sample of up to 1000 exoplanets. The payload consists of a 1m class mirror with 2 focal plane instruments covering both photometry and spectroscopy over the 0.5-7.8 micrometre range. All spacecraft mission data will be processed at the ESA Science Operations Centre via data processing software provided by the Ariel consortium provided Instrument Operations Science and Data Centre (IOSDC). In addition, high level science data products, including the final exoplanet spectra will be provided to the ESA archive directly from the Ariel consortium. This paper will discuss the current status, and development of the IOSDC Ground Segment up to launch, its role during mission operations and the integration within the ESA Ground Segment environment.
13092-270
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
ExoSim 2 is a modular framework for simulating exoplanet observations, adaptable to various space-based telescopes, with a current focus on the Ariel space mission. This study showcases ExoSim 2's expanded capabilities, particularly in integrating a comprehensive set of noise models that surpass those in the original ExoSim.
This adaptability is key to ExoSim 2's design, allowing for easy customization to different telescopic platforms and the incorporation of additional noise sources. Our simulations for Ariel, enriched with these diverse noise models, provide insights into the telescope's performance and the challenges in detecting exoplanetary signals.
The results demonstrate ExoSim 2's efficacy in realistically mimicking observational conditions, highlighting its importance in mission planning and data analysis for exoplanet studies. Its flexibility and comprehensive approach make ExoSim 2 a crucial tool in advancing our understanding of exoplanets and preparing for future explorations.
Session PS7:
Posters - Exoplanet Time Series Observations: Detectors, electronics, and operations
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-272
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Earth 2.0 (ET) mission is a space mission in China, aimed at detecting thousands of exoplanets, including potentially habitable Earth-like planets around Sun-like stars (i.e. Earth 2.0s), cold low-mass planets and free-floating planets. Six 28 cm telescopes are used for ultra-high precision photometry to detect transiting planets. To verify that transit telescopes can detect the transit event of exoplanets, a photometric signal detection experiment system has been developed to validate the selected CMOS detectors with capability of detecting Earth 2.0’s transit signals (84 ppm photometric variations). and the measurement results are reported.
13092-273
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Earth2.0 is a space telescope mission proposed by Chinese scientists for the exploration of exoplanets. It is anticipated to be launched in 2027 and will be work in the Halo orbit at the Sun-Earth L2 point for a minimum of four years. The payload includes six ∅28 cm, 550-square-degree transit telescopes and one ∅35cm, 4-square-degree microlensing telescope.
Currently, Teledyne e2v's CCD290-99 has been considered as the optional detector for the microlensing telescope with a focal plane composed of a 2x2 array of detectors. To evaluate the performance of CCD290-99, a prototype camera for the microlensing telescope based on CCD290-99 was designed and tested. Additionally, a proton displacement damage irradiation experiment was implemented to study the impact of space radiation on the performance of the CCD290-99 detector.
After accumulating a dose of 3.072x1010 p/cm² and 6.792x1010 p/cm² of 60MeV proton irradiation, CCD290-99 underwent tests for dark current, dark signal non-uniformity, charge transfer efficiency. Test results will be introduced in this article.
13092-274
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The PLATO mission, part of ESA's Cosmic Vision program, is expected to be launched by 2026 and will focus on discovering exoplanets from gas giant down to small rocky planets. Equipped with telescopes and cameras, including 24 normal and 2fast cameras, it mainly aims to find Earth-sized planets in the habitable zone of Sun-type stars. The Data Processing System, comprising DPUs and the ICU, manages payload operations, with an On-Board Control Procedures (OBCP) engine enhancing autonomy and flexibility. Written in OCL, OBCPs are independent procedures loaded into the ICU memory, enabling late-stage modifications and regular re-execution, reducing repetitive uploads and conserving bandwidth.
In this paper, we present a brief overview of the OCL (On-Board Command) language and its features, as well as the capabilities and benefits of having OBCPs.
We also describe the OBCP flight software environment and the OBCP engine implemented in the ASW, along with the features and capabilities of the OBCP for the PLATO mission. Finally, the usage scenario is discussed.
13092-275
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
PLATO (PLAnetary Transits and Oscillations of stars) is ESA's third medium-class mission, adopted in the Cosmic Vision program.
PLATO's Payload consists of 26 telescopes (24 normal, 2 fast) capturing images every 25 seconds and 2.5 seconds, respectively. Each camera comprises four CCDs, yielding 2.11 gigapixels images overall. The onboard Data Processing System (DPS) handles this huge data load, employing Normal and Fast DPUs along with a single Instrument Control Unit (ICU). The ICU manages data compression, overseeing the P/L through a SpaceWire network.
This paper provides a comprehensive overview of the Instrument Control Unit's (ICU) status following the rigorous performance test conducted on the Engineering Model (EM) and its evolution during the development phases of the Qualification Model (EQM) and Proto-Flight Model (PFM).
The content delineates the outcomes derived from the performance test executed on the Engineering Model (EM), detailing the activities undertaken during the Assembly, Integration, and Verification (AIV) processes of the EQM. Additionally, it shows the current status of the Proto-Flight Model (PFM), offering insights into its developmental trajectory.
13092-276
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
PLAnetary Transits and Oscillations of stars (PLATO) is a medium-class mission selected by ESA in the framework of the Cosmic Vision programme. The PLATO Instrument Control Unit (ICU) is responsible for the management of the scientific payload, the communication with the satellite on board computer, the acquisition of housekeeping and scientific data from the 26 PLATO cameras and their processing before the downloading to the satellite mass memory unit.
The data produced by the cameras cannot be transmitted directly to ground as soon as they are acquired but an onboard pre-processing and compression is needed. While the pre-processing stage is in charge of the camera's Data Processing Units (DPUs), the compression is executed on board ICU. Due to the highly demanding science requirements, the compression must be rigorously lossless.
In this paper we will review the overall ICU onboard data processing chain, from the DPUs to the satellite mass memory, presenting the compression strategies implemented in the ICU application software architecture, and the results of the performance test run on the ICU Engineering Model.
13092-277
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Ariel is the fourth medium-class mission (M4) of the ESA’s Cosmic Vision Program adopted in November 2020 by the Agency for a launch opportunity in 2029 and conceived to perform exoplanets atmospheres characterization by means of photometry and primary plus secondary transit spectroscopy in the VL and NIR wavelengths.
The Payload hosts two instruments and a cryocooler to provide active cooling capability to the main spectrometer (AIRS) detectors working at cryogenic temperatures close to 42K. The on-board instrumentation is controlled by means of warm avionic units located in the spacecraft Service Module and electrically interfaced to the Payload cold units hosting optical modules, detectors and their cold front-end electronics. This overview on the electrical and electronic design of the overall Payload will show the selected design and its implementation status during Phase C.
13092-278
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The AIRS infrared spectrometer will study exoplanets’ atmospheres onboard the ARIEL space telescope, scheduled to launch in 2029. It implements two spatial detectors in two channels to observe a broad wavelength range. The creation of a spatial detector acquisition chain is becoming increasingly demanding. It requires low-noise, low-power, radiation-tolerant electronics that can operate at low temperatures, which means we must develop very specific electronics and test benches that can faithfully reproduce spatial conditions. This paper will present how the AIRS team proceeds to meet the needs of the AIRS instrument, by developing high-performance readout electronics and highly representative test benches.
13092-279
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The ARIEL InfraRed Spectrometer (AIRS) on board of the ARIEL space mission to be launched in 2029, will study the exoplanets’ atmosphere in a wavelength range going from 1.95 to 7.8 micrometers. AIRS detection plane is divided into two channels. Each integrated Focal Plane Assembly (iFPA) includes a Cold Front-End Electronic and a Focal Plane Array. The paper will focus on the iFPAs. It will present the different models developed prior to the Engineering Model and Flight model program as well as the test set-up developed for the validation and the characterization of the performances of the iFPAs.
13092-280
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
ARIEL (Atmospheric Remote-sensing Infrared Exoplanet Large-survey) is an ESA mission dedicated to the analysis of the chemical composition and thermal structures of up to a thousand warm and hot transiting exoplanets. AIRS (ARIEL InfraRed Spectrometer), one of the two ARIEL instruments, performs IR spectrometry in two wavelength ranges: 1.95 – 3.9 μm (R = 100) and 3.9 – 7.8 μm (R = 30).
The ICU (Instrument Control Unit) is an electronic box acting as the main interface between AIRS and the Spacecraft (S/C). It performs several tasks: communicates with, collects science data from and provides secondary voltages to the ARIEL Detector Control Units (A-DCU); it controls the TCU (Telescope Control Unit) as well.
This paper reports the ICU status after the Preliminary Design Review (PDR), describing its architecture, the current activities and the development process.
13092-281
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The ARIEL mission has the task of conducting a large, unbiased spectroscopic survey of exoplanets, in order to explore the nature of exoplanet atmospheres and interiors and, through this, the key factors affecting the formation and evolution of planetary systems in our galaxy.
Ariel is composed of two scientific instrument: one is the FGS which provides the Fine Guidance System capabilities and in addition combines a VIS photometer and a NIR low resolution spectrometer.
The other instrument is the Ariel IR Spectrometer (AIRS) which provides spectra with resolution between 30 and 100 on a spectral band between 1.95 and 7.8 micrometers.
This paper will focus on the application SW of the Instrument Control Unit of the Ariel mission, which is in charge of controlling the AIRS instrument as well as the Telescope Control Unit (TCU), which controls the M2 Mirror Mechanism (M2M) and provides the temperatures of the Payload. In particular, we will discuss the design of the ASW and the development status of the SW.
13092-282
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Hawai detectors, known as HxRG have been serving the astrophysics community both ground and space based for the development of scientific instruments in the infra-red. They are notorious for their outstanding electro-optical performances and adaptability to a wide range of wavelength from the near to the long wave infrared. With increasingly demanding scientific instrumentation some readout artefacts that can affect the performances of these detectors have to be scrutinized. Multiplexer glow that is inherent to the architecture of the Hawaii detectors and generally speaking hybrid infra red detectors can limit the signal to noise ratio of an scientific instrument in photon starved observations. We will present our study of mutliplexer glow on three H1RG detectors that have been characterized in the context of the ARIEL mission. We will analyze the root cause of this effect, its consequence on the overall performances of the detectors and paarameters of influence.
Session PS8:
Posters - Exoplanet Time Series Observations: Optics, Optomechanics, and Modeling
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-44
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
A STOP (Structural, Thermal, Optical and Performance) analysis has been conducted on the camera units of the PLATO space mission. The analysis is devoted to the prediction of in-orbit performance metrics that could not be otherwise verified through direct testing. The analysis presented in this paper is restricted to the so-called “static cases” which provide a snapshot of a specified thermal condition. These are intended to evaluate the camera performance over the expected operational temperature range and at zero gravity. We hereby provide a description of the model, the requirements to be tested, the simulation strategy and the performance results.
13092-283
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Earth 2.0 (ET) mission is a space mission in China which will be operated at the Earth-Sun L2 halo orbit. ET’s scientific payload consist of six 28cm diameter transit telescopes with each field of view of 550 square degrees and one 35 cm diameter microlensing telescope with a field of view of 4 square degrees. For transit telescopes, the suppression of straylight will be key to meet the requirement of 34ppm photometric precision for detecting weak transit signals from Earth 2.0s. This paper presents the design and simulation of straylight suppression for transiting telescopes.
13092-284
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Ariel (Atmospheric Remote-Sensing Infrared Exoplanet Large Survey) is the adopted M4 mission of ESA “Cosmic Vision” program. Its purpose is to conduct a survey of the atmospheres of known exoplanets through transit spectroscopy. Launch is scheduled for 2029.
The Primary mirror is a very innovative device made of lightened aluminum. Aluminum mirrors for cryogenic instruments and for space application are already in use, but never before now it has been attempted the creation of such a large mirror made entirely of aluminum: this means that the production process must be completely revised and fine-tuned, finding new solutions, studying the thermal processes and paying a great care to the quality check.
By the way, the advantages are many: thermal stabilization is simpler than with mirrors made of other materials based on glass or composite materials, the cost of the material is negligeable, the shape may be free and the possibility of making all parts of the telescope, from optical surfaces to the structural parts, of the same material guarantees a perfect alignment at whichever temperature.
The results and expectations for the flight model are discussed in this paper.
_
13092-286
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Ariel is the ESA M4 mission and will be launched in 2029. It will aim to survey about 1000 exoplanetary atmospheres.
All mirrors of the telescope will be bare aluminum.
The processing techniques developed for this material and the large dimensions of the primary (1.1X0.7 m) make the Mid-spatial frequency components important as a contribution to the reduction of optical performance. Simulations were carried out in Zemax to quantify this contribution, which is difficult to measure in metrology.
13092-287
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Ariel is the ESA M4 mission and will be launched in 2029. It will aim to survey about 1000 exoplanetary atmospheres.
All mirrors of the telescope will be bare aluminum. Such a low-density material can deform easily, risking compromising the optical performance of the mirror surface. For this, Ariel's mechanical team developed, manufactured and tested the flexure hinges for connection to the optical bench on the primary Structural Model to minimize the effects of torsion and deformation during assembly and reduce mechanical stress on this mirror.
13092-288
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Ariel is the ESA M4 mission and will be launched in 2029. It will aim to survey about 1000 exoplanetary atmospheres.
All mirrors of the telescope will be bare aluminum. Such a low-density material can deform easily, risking compromising the optical performance of the mirror surface. For this, Ariel's mechanical team developed, manufactured, and tested the flexure hinges for connection to the optical bench on the primary Structural Model to minimize the effects of torsion and deformation during assembly and reduce mechanical stress on this mirror.
13092-289
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Optically processing the deformation field of a telescope structure
finite element model allows to calculate in a single simulation run
all the optical relevant data. In this paper we will focus on a method
able to compute the modification of the ray tracing of the Ariel space
telescope when its structure is deformed by some external inputs,
such as the gravity field during the ground test and the thermal
distortions during the operational observations. Once the computation
of the ray tracing is performed, this output is processed in order to
calculate all the data required to estimate the optical performances
of the optical system, such as the collimated beam, the aberrations,
the spot diagram, and the point spread function. The method discussed
in this paper, based on a multi-physics approach, demonstrates its
capability to address classical geometrical optics problems once
the solution to the structural mechanics problem is obtained, making
it well-suited for a comprehensive STOP (Structural-Thermal-Optical
Performance) analysis.
13092-290
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
PAOS is an open-source Python package implementing physical optics propagation (POP) in Fresnel approximation and paraxial ray tracing to analyze complex waveform propagation through both generic and off-axes optical systems, enabling the generation of realistic Point Spread Functions across various wavelengths and focal planes.
PAOS offers extensive customization, a generic input system, and a graphical user interface for seamless user interaction. PAOS provides the community with a fast, reliable, and modern tool for optical studies, enhancing the assessment of system performance and accessibility of advanced simulations.
13092-291
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Ariel is the fourth medium-class mission (M4) of the ESA’s Cosmic Vision Program. Its launch is planned for 2029.
Ariel will observe a large and well selected sample of transiting gas giants, neptunes and super-earths around a wide range of host star types, with the objective to study planetary atmospheres and to understand composition and evolving processes of the planetary systems.
Ariel will perform primary and secondary transit spectroscopy in the 1.10 to 7.80 μm spectral range and broad-band photometry in the Optical (0.50 - 0.80 μm) and Near IR (0.80 - 1.10 μm) ranges with an off-axis Cassegrain telescope having a 1.1x0.7 m primary mirror and two main instruments AIRS, the Ariel Infrared Spectrometer, and the Fine Guidance System (FGS).
A Structural, Thermal, and Optical Performance (STOP) analysis is conducted at Payload level to estimate the thermo-elastic induced degradation of the system performance for a number of selected environmental load cases.
In particular, this document presents the approach used and the results of the optical design analysis performed to predict the performance of the Ariel Telescope Assembly for the In-Flight operational cases during Phase C.
Session PS9:
Posters - Exoplanet Time Series Observations: Assembly, Integration and Test Results
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-292
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Pandora is a first-of-its-kind ESPA Grande small satellite with an all aluminum half-meter class, relayed Cassegrain telescope, dual channel infrared spectroscopy and visible photometry. As a NASA Pioneers class astrophysics mission, Pandora’s goal is to disentangle transmission spectra signals from exoplanets and their host stars by obtaining the first dataset of simultaneous, multiband visible and near-infrared (400-650 nm and 1,000 – 1,700 nm), long-baseline observations. The focus of this paper is on the characterization of payload during assembly, integration, and testing. Results will include structural and thermal finite element analysis for key subsystems (telescope, detector assemblies, and thermal transport). Emphasis will be placed on the telescope alignment procedures and optical characterization, comparing Monte Carlo simulations with as-measured figures of merit, such as surface roughness, wavefront error, throughput, and encircled energy.
13092-293
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The FPA in optics is the unit located at the focal plane position of the different optical instruments. Each FPA hosts the detectors on support structures and associated interfaces (Ifs). Some of these flexibles Ifs cause difficulties in the alignment of the detectors with respect to the nominal optical/mechanical reference system.
The number of FPAs already integrated, aligned and verified at INTA exceeds dozen from small CCDs to large detector arrays. Due to the critical repeatability aspect of the different models in the space missions, each FPA must be identical with very stringent specifications, which includes strict opto-mechanical positioning tolerances. They only can be reached under a special industrialization of alignment processes and an automatic metrology verification thanks to a high-precision non-contact vision dimensional measurement system with micrometric or even better accuracy.
The verification carried out before and after the acceptance test campaigns of FPAs has been successfully passed and several FMs have been assembled by the AIV Team from INTA following ECSS policy.
13092-294
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
PLATO is a European Space Agency medium class mission, whose launch is foreseen for 2026.
Its primary goal is to discover and characterize terrestrial exoplanets orbiting the habitable zone of their host stars. This goal will be reached with a set of 26 wide field-of-view cameras mounted on a common optical bench.
The PLATO camera flight models (FMs) are being tested at three different test-houses, namely the Netherlands Institute for Space Research (SRON), Institut d'Astrophysique Spatiale (IAS) and Instituto Nacional de Técnica Aeroespacial (INTA).
Here we present the results of autocompatibility testing obtained during cryogenic-vacuum tests campaigns on the PLATO Camera 'Normal' FMs.
The autocompatibility testing aims to analyse possible interferences on the CCD readout signal due to camera operations.
Camera operations that could be potential causes of interference are identified in the Thermal control system (TCS) heater lines pulses, and multiple CCD readouts (relevant for PLATO 'Fast' Cameras only).
13092-296
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We present a thermal vacuum chamber that is developed for the performance verification of cameras of ESA’s PLATO mission. All aspects of its performance will be detailed as well as the embedding in the PLATO project and camera test results.
13092-297
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
LEONARDO SpA is leading an Italian Space Industry Team, funded by ASI, collaborating to the ESA mission PLATO (PLAnetary Transits and Oscillation of stars). Its aim is the study of extrasolar planetary systems, with a focus on the discovery of exo-planets hosted by bright, nearby stars. PLATO is composed by 26 fully dioptric designed cameras, each composed of a telescope optical unit (TOU) and a focal plane array (FPA). The FPA is integrated with the TOU at ambient temperature by other Partners of the PLATO CAM-Team, although we determine the best image plane (BIP) of each TOU during test at cryo-vacuum operative conditions. This poses a metrology challenge at TOU manufacturing and testing facilities, with relatively high production rate of the flight units. At cold temperature (-80°C), the orientation and location of the FPA is found out as the BIP, meanwhile at ambient temperature, them are co-registered by using Hartmann masks. The results of this approach show a correspondence between the two analysis methods and give an input for subsequent FPA integration at PLATO CAM level.
13092-298
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
PLATO is a European Space Agency medium class mission, whose launch is foreseen for 2026. Its primary goal is to discover and characterize terrestrial exoplanets orbiting the habitable zone of their host stars. This goal will be reached with a set of 26 wide field-of-view cameras mounted on a common optical bench.
Here we present results obtained during cryogenic-vacuum tests campaigns done at three different test-houses (SRON, IAS, INTA) on the PLATO camera flight models (FMs). As of end of 2023, eight Cameras will be tested, and more than half of the total number of 26 is expected to be completed by the time of this SPIE conference.
In particular, I will present the PSF properties of the first PLATO FM cameras at the nominal focus temperature over all the field of view, focusing on the ensquared energy fractions. I will compare the PSFs of the different cameras and their performances vs. temperature.
I will also present an alternative method to derive the BFT of the Cameras based on transient PSFs, without stabilized temperature measurements.
13092-299
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
In this paper, the set-up preparation for the PLATO telescopes (CAMs) calibration and testing at INTA details are reported on, including design and fabrication. The 26 CAMs that will be mounted on the PLATO (Planetary transits and oscillations of starts) platform will be used for Exoplanets detection and partial characterization together to the associated star activity evaluation through its astroseismology. The results on the first model tested at INTA, the engineering model (EM) are summarized
13092-300
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
In this paper, a brief summary on the main details of the tests carried out at INTA on the PLATO CAM flight model (FM) number 3 are reported on. The different institutes (IAS, SRON and INTA at France, Netherlands and Spain, respectively) involved in the calibration and testing PLATO telescopes will receive at least 9 models for such purpose. The preliminary results obtained together to the rest of the consortium and related to the telescopes capabilities are included for the particular case of such first flight model tested at INTA.
13092-301
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Ariel is ESA’s M4 mission of the “Cosmic Vision” program, with launch scheduled for 2029. Its purpose is to conduct a survey of the atmospheres of known exoplanets through transit spectroscopy.
Ariel is based on a 1 m class telescope optimized for infrared spectroscopy, operating at cryogenic temperatures.
The Ariel Telescope is an off-axis, unobscured Cassegrain design, with a parabolic recollimating tertiary mirror and a flat folding mirror.
The mirrors and supporting structures are all realized in an aerospace-grade aluminum alloy T6061 for ease of manufacturing and thermalization. The low stiffness of the material however, poses unique challenges to integration and alignment.
This paper describes the Assembly, Integration and Test (AIT) plan for the Ariel telescope, and gives an overview of the analyses and reasoning that led to the specific choices and solutions adopted.
13092-302
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
In this proceeding, we present the development of the optical ground support equipment (OGSE) used for payload-level testing of the Ariel space mission. Since PDR, there have been substantial revisions to the OGSE architecture. In this proceeding, we describe the evolution of the OGSE architecture. The updated OGSE design will then be presented.
13092-303
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The future ARIEL Space Mission aims achieving a photometric precision down to the parts-per-million (ppm) level, over periods longer than ten hours. This required level of sensitivity is crucial to obtain valuable information about the properties of the exoplanet and its atmosphere. The Institute of Astrophysics and Space Sciences is responsible for the development of the visible and near-infrared (Vis-NIR) illumination sub-system, integrated in ARIEL’s Optical Ground Support Equipment (OGSE). This study presents an in-depth analysis of two main component of the Vis-NIR illumination sub-system: a Quartz Tungsten-Halogen (QTH) calibration light source and an extended Indium Gallium Arsenide (InGaAs) reference detector, tested under cryogenic conditions. It is shown that these two components are compliant with the ARIEL's requirements, allowing the mission to obtain spectroscopic and photometric time series with the stability needed to identify signal variations from 20 ppm to 100 ppm, over a 10-hour observation period.
Session PS10:
Posters - Exoplanet Time Series Observations: Thermal Control & Space Environment
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-119
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Ariel is the M4 mission of the ESA Cosmic Vision Programme. During its 4-years survey, Ariel will probe spectroscopically the chemistry and physics of a large sample of exoplanets to extend our knowledge of how planetary systems form and evolve.
The cryogenic payload thermal control architecture is based on a passive and active cooling approach. Passive cooling design is mainly based on a V-Groove shields system design that exploits the L2 orbit favorable thermal conditions. The IR spectroscopic channel detectors require a lower operating temperature, provided by an active cooling system based on a Neon Joule-Thomson cold end, fed by a mechanical compressor.
We report about the present status of the PLM thermal architecture design and development during Phase C, together with thermal modeling results and performance predictions.
13092-120
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
ARIEL, the Atmospheric Remote-sensing Infrared Exoplanet Large-survey, is an M-class ESA mission whose purpose is to analyze the chemical composition and thermal structures of up to a thousand warm and hot transiting exoplanets.
The all-Aluminum 1-m class primary mirror, the optics and the instruments are kept at cryogenic temperatures (below 55K) by means of an Active Cooling System and the temperature is accurately measured by a Thermal Monitoring System (based on Cernox™ thermistors).
This paper reports the design process of the Thermal Monitoring System and of the Decontamination System (heaters and sensors) that fall under INAF responsibility, prior the Preliminary Design Review.
13092-121
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Ariel space mission will characterise the atmospheres of a sample of large exoplanets spectroscopically. It is an ESA Medium class science mission (M4) with a payload based on a 1-meter class telescope. To maximise the quality of the science it is necessary to have information about the changes in the telescope, mostly associated with the temperature gradients. This implies the measurement of temperature on nearly 40 points in the telescope structure using thermistors. This cryogenic temperature measurement must provide an accuracy better than +/-25mK.
This paper presents the description, analysis and first results of the Ariel Temperature Sensing system housed in the Telescope Control Unit, which is able to provide an accuracy better than +/-15mK even with a thermistor uncertainty around +/-10mK.
13092-122
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
ARIEL is the ESA's Cosmic Vision M4 mission, whose aim is to chemically characterise by low-resolution transit spectroscopy the atmospheres of over one thousand exoplanets orbiting nearby stars.
The operational orbit of the spacecraft is baselined as a large amplitude halo orbit around the Sun-Earth L2 point, as it offers the possibility of long uninterrupted observations in a fairly stable radiative and thermo-mechanical environment.
A direct escape injection with a single passage through the radiation belts is foreseen.
The space environment presents significant design challenges to all spacecraft, including the effects of interactions with Sun radiation and charged particles owning to the surrounding plasma environment, potentially leading to dielectrics charging and following discharging phenomena endangering the Payload operations and its data integrity.
Here, we present some consolidated analyses about Payload dielectrics charging (both surface and bulk) along the transfer orbit from launch to L2.
Session PS11:
Posters - Exoplanet Imaging: JWST
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-123
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
NIRCam Coronagraphy was declared ready for science in the early summer 2022. Several impactful science results have since been obtained using the NIRCam coronagraphs, mainly on known exoplanetary systems. In this contribution we give an update on all improvements we have implemented to make this mode more efficient and perform better. With tight timing constraints in commissioning, we focused on the long wawvelengths occulter MASK335R. Here we describe how we improved the target acquisition for all five masks, the distortion correction and global alignment, the absolute flux calibration, etc. We also implemented the default dual channel operations mid-Cycle 1 (simultaneous short and long wavelengths). While not trivial, this new capability improves the efficiency and the impact NIRCam Coronagraphy can have in the field of exoplanets. We discuss the current on-sky contrasts and astrometric performances which are now better understood and can be compared to other high contrast facilities. We demonstrate that NIRCam Coronagraphy is transformative in characterizing known objects but also discovering colder and/or more mature exoplanets.
13092-124
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Direct imaging observations have proven to be a method not only of detection but also of characterization of the atmospheres of planets in wide orbits. This is possible thanks to the use of high angular resolution instruments, coronagraphs, and post-processing techniques used to subtract the diffracted starlight, reaching the necessary contrast for detecting these planets. However, the contrast performance is limited by two detection regimes: 1) a speckle-dominated regime at short separations from the star, and 2) a regular noise-dominated regime at large separations. The first is restricted to our ability to suppress starlight, while the second is dominated by classical imaging noise limits. Here we present our preliminary studies and results on both regimes to establish the fundamental sensitivity limits of JWST/NIRCam coronographic observations in the F444W band and the transition separation between the two detection regimes.
13092-125
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
JWST’s MIRI & NIRCam coronagraphic modes continually demonstrate strong high-contrast imaging capabilities. However, subtraction of the residual stellar PSF is required to maximize the contrast performance of the available modes. A common JWST subtraction method is through Reference Differential Imaging (RDI), which utilizes comparable observations of a separate reference target. Despite RDI advantages, any off-axis sources around the reference star can contaminate reference images & degrade the achievable contrast. Yet, it's not easy for observers to determine if the presence of sources at a given position & magnitude will significantly impact the achievable contrast. In this paper we use PanCAKE, a high-contrast imaging JWST simulation tool, to explore the influence of sources at varying ranges of separations, position angles, and magnitudes for both the NIRCam & MIRI coronagraphic high-contrast imaging modes. Loss of contrast due to a given source is measured across the 2D image plane, enabling a determination of its impact both globally, and relative to a given image position. We expect these results to serve as a guide for observers when choosing suitable reference sources.
13092-126
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The origin of the observed diversity of exoplanet systems is still a
matter of debate. High spectral resolution imaging can help us in our
understanding of the physical and chemical properties of
imaged exoplanets.
The wide-orbit planet-mass companion CT Cha b observed with JWST/MIRI MRS is a perfect candidate for constraining theories of giant planet formation. Moreover, the previously measured high mass accretion rate of CT Cha b together with the high extinction is a strong indication for the presence of a circumplanetary disk signatures of which may be probed with a MIR spectrum.
I will show a spectrum of CT Cha b obtained after subtracting the PSF of the star. I will then present a comparison of the extracted spectrum with planet atmosphere models, and test the presence of a circumplanetary disk
Session PS12:
Posters - Exoplanet Imaging: the Roman Coronagraph
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-127
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Coronagraphic Instrument onboard the Nancy Grace Roman Space Telescope is an important stepping stone towards the characterization of habitable, rocky exoplanets. In a technology demonstration phase conducted during the first 18 months of the mission (expected to launch in 2027), novel starlight suppression technology may enable direct imaging of a Jupiter analog in reflected light. Here we summarize the current activities of the Observation Planning working group formed as part of the Community Participation Program. This working group is responsible for target selection and observation planning of both science and calibration targets in the technology demonstration phase of the Roman Coronagraph. We will discuss the ongoing efforts to expand target and reference catalogs, and to model astrophysical targets (exoplanets and circumstellar disks) within the Coronagraph’s expected sensitivity. We will also present preparatory observations of high priority targets.
13092-128
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Nancy Grace Roman Space Telescope’s Coronagraph Instrument will for the first time demonstrate active wavefront sensing and control for a space-based coronagraph, a key milestone in achieving this challenging goal, and may image the first planet in reflected light. The Community Participation Program has been created to engage members of the broader scientific community in the preparation for its planned launch in 2027. Here we will present the on-going work of the Data Reduction and Simulations working group, one of the three working groups within the Community Participation Program. The working group is charged with the development of the data reduction and post-processing pipeline for the on-sky data and the development of a simulation suite to aid in the preparation and planning of Roman Coronagraph observations. We will report on the architecture and functionality of the data reduction pipeline and the expansion of previous simulation tools.
13092-129
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
High-contrast polarimetric observations of debris disks help constrain the scattering properties in addition to improving the contrast ratio. The upcoming Nancy Grace Roman Telescope Coronagraph is expected to measure the linear polarization fraction of disks greater than 0.3 with an uncertainty of 0.03. One of the critical problems with polarimetric observations is the polarization aberrations generated due to the telescope and polarimetric optics, which introduces errors in measuring fainter polarization disk signals. A modeling pipeline was previously developed to simulate the polarization observations of brighter debris disks similar to HR4796A without accounting for polarization aberrations. Here, we present the simulated polarimetric disk images of fainter debris disks ($<$0.1mJy/arcsec2) through the Roman telescope and the HLC and SPC coronagraphs, performing photon-counting in EMCCD, incorporating polarization aberrations, jitter, detector, and speckle noise. Finally, we compare the recovered polarization fraction of the debris disk with the input to demonstrate the polarimetric capability of the Roman Coronagraph.
13092-130
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
RST-CGI will be the first space facility equipped with deformable mirrors (DMs). Those will lead to reach a contrast of 1e-8 or better in a dark hole between 3λ/D and 9λ/D. Post-processing techniques play an important role in increasing the contrast limits.
Our work investigates how DMs can be used to calibrate the instrument response to controlled wavefront error maps and to improve the post-processing performance.
We coded a simulator which reproduces the hybrid Lyot coronagraph optical structure.
With it, we mimic an RST-CGI observing sequence. We generate PSF libraries by modulating the DMs on a reference star and we compute the PCA model. We subtract it to the science target data to remove the residual starlight. We inject planets and compare their detection over those obtained with classical techniques (RDI).
Here we show the first results, comparing the performance gain obtained with the modulated-DM reference library over standard approaches.
13092-131
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Nancy Grace Roman Space Telescope, NASA's next flagship mission in astrophysics, will be launched in the mid-2020s with an onboard Coronagraph Instrument which will serve as a technology demonstrator for exoplanet direct imaging. The Roman Coronagraph will be capable of detecting and characterizing exoplanets and circumstellar disks in visible light at an unprecedented contrast level of ~10-8 or better at small separations. The instrument is equipped with six precision alignment mechanisms (PAMs) which enable ultra-stable, sub-micrometer positioning of optical elements such as coronagraphic masks, optical filters and polarizers.In order to achieve contrast level, which are 2 to 3 orders of magnitude better than state-of-the-art visible or near-infrared coronagraphs, the mechanisms need to be stable at sub-microradian levels during a typically 10 hour long science observation. We report here about the development of these mechanisms and present their performance test results from the qualification/flight acceptance test program. All flight models were already delivered and integrated into the CGI flight instrument which is currently undergoing functional testing at JPL.
Session PS13:
Posters - Exoplanet Imaging: Starshades
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-132
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Astronomical objectives for solar and stellar coronagraphs are respectively the study of the solar corona and the detection of exoplanets. Both coronagraphs use external occulters that block most of the unwanted light before it enters the telescope. They share similar concepts, but are actually very different from each other because of geometric characteristics.
We discuss choices of various solar and stellar externally occulted coronagraphs from geometric and Fourier optics points of view.
13092-133
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We will present the results of the Starshade Exoplanetary Data Challenge and discuss the noise budget of exoplanet direct imaging using a starshade vis-a-vis realistic tests of background subtraction.
13092-134
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Starshades are ambitious space projects that will allow very high contrast imaging of the vicinity of stars,
opening the road to direct imaging and spectroscopy of exoplanets.
Their design relies on very precise computations of Fresnel diffraction of external, binary occulters.
Such computations have been dealt with in two ways in the past: either using contour integrals with field dependent
phase terms (à la Maggi-Rubinowicz), or using bidimensional discrete Fourier transforms, which require very high
resolution to achieve the required control of aliasing.
We propose a new method taking advantage of both approaches. Convolution with the Fresnel kernel is done in Fourier
space as in the bidimensional discrete method. Here, aliasing is controlled by computing the continuous Fourier transform of a polygonal approximation of the occulter, which is implemented as a contour integral.
In contrast to the Maggi-Rubinowicz method, computations on the occulter and the Fresnel kernel are done separately, with the wavelength dependence lying in the kernel only, therefore processing of the occulter needs to be done only once, leading to a cost effective solution.
13092-135
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
NASA’s Habitable Worlds Observatory addresses the challenging goal of characterizing numerous Earth-like exoplanets orbiting nearby stars. While the baseline approach is to carry out the observations with a coronagraph, current planning calls for the observatory to be “starshade ready” so that it can take advantage of the superior throughput, working angle, contrast, and bandwidth when the telescope is paired with a starshade. We describe the instrumentation that works to acquire the starshade position, measures the lateral formation flying position once aligned, and communicates with the starshade. We also describe several starshade designs that enable imaging in the UV, visible, and NIR bands, as well as configurations that combine the starshade with the coronagraph to enable the high-contrast study of binary stars. We present observational yield estimates for these configurations.
Session PS14:
Posters - Pathways to Great Observatories
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-136
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Astronomy is data and observation driven. We have presented in a recent series of papers idea, that we think are necessary to make the second next generation of space telescopes possible.
With this paper we want to present that the ideas and fields of improvement identified in the previous studies are also applicable to allow for faster, less costly and less risky medium and small size missions.
This is already a reality for CubeSat programs, where system components and even payload parts can be bought off the shelf. It is nevertheless not yet a commonly used approach for missions of medium scale and development times between 5 and 15 years.
We will show, that the re-use of concepts and components, as well as the design of components for later re-use, are a time- and cost-efficient way forward. And that this approach will even allow the design and implementation of scientific missions that would else not be possible.
13092-137
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The recent decadal survey advocated for the development of three flagship-class missions, also referred to as the “Next Great Observatories” as fundamental to advancement of the field. Trends in the cadence and cost of development of such missions hint at the lack of sustainability and timeliness of these missions as historically conceived and developed. In this paper, we explore a different architecture for Flagship development. We will examine the opportunities for increasing the cadence of mission development by the adoption of a more strategic vision of flagship-class development and incorporating recent trends in launch capability and servicing into the design.
13092-138
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Commercial satellite servicing has been demonstrated in Geosynchronous orbit and will become a standard feature of orbits from low Earth to lunar in the coming decade. Currently operating and future planned large astrophysical observatories will operate around the Sun-Earth L2 point and far from commercial logistics capabilities. This paper introduces our first look at the considerations for servicing in these science rich orbits. Further we share our investigations into the opportunities for the systems designer that considers servicing in their future concepts. We will review the systems and system of systems considerations for implementation of a cost effective logistic network for these science missions.
Session PS15:
Posters - Habitable Worlds Observatory
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-139
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Habitable Worlds Observatory (HWO) will need unprecedented stability in order to achieve the desired science performance. Achieving this stability will push the state of the art in structural damping, environmental shielding, thermal sensing and heater control, control architecture, etc. and will even involve consideration of effects that were previously negligible such as low-energy micrometeorites and bulk charging of mirrors.
In this paper, we explore the interactions between basic architectural trades and the ability of the observatory to meet the stability requirements. As an example, we discuss how the need for an ultra-stable structure translates to requirements on an environmental shield. We then look at options for the architecture of such a shield and interactions between these possible shield configurations and other design considerations such as verifiability, manufacturability, mass, risk, serviceability, and lifetime.
13092-141
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Habitable Worlds Observatory (HWO) imposes the highest level of temporal and spatial stability requirements on the mirror segments that will comprise its entrance pupil. Some questions of ultrastability realization are addressed by simple models of lightweighting cells and response timescales to thermal stimulus. Closed Back (CB) lightweighted segments are attractive from the eigenfrequency and areal density perspectives but have a long thermal time constant associated with applied thermal stimulus changes, radiated from a heater plane behind the mirror. Open Back (OB) lightweighted segments enjoy a rapid thermal time constant but are not presently meeting the eigenfrequency and areal density of the CB. Thus, neither CB nor OM appears to be optimal for HWO stability. We explore a third option, Partially Closed Back PCB lightweighted segments. PCB segments appear to exhibit eigenfrequencies approaching that of the CB, with thermal time constant characteristics close to those of the OB, thus the best of both forms. We explore preliminary questions of ultrastability for HWO inclusive of these three segment models.
13092-142
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We describe a technique for fine phasing of a segmented primary for the Habitable Worlds Observatory. Our wavefront sensing approach relies on the modified Gerberch-Saxton (MGS) algorithm, which uses focus diversity to perform phase retrieval. We will describe important image processing steps to maximize the accuracy of phase retrieval. This approach only requires a narrow band filter and the ability to produce a repeatable defocus perturbation. Our wavefront control approach incorporates the estimated wavefront error, the estimated pose, and calibration information; as well as a control strategy based on the effectiveness of each degree of freedom in terms of their ability to efficiently minimize the wavefront error.
13092-143
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Roman Coronagraph is a technology demo that is very relevant for the Habitable Worlds Observatory (HWO), including the system engineering approach, Flux Ratio Noise (FRN) error budget, and its sophisticated field interaction model. The field interaction model in turn makes use of separate integrated modeling to calculate sensitivities to the most important types of disturbances. This methodology, shown during CGI's development to be valid at the 10% level, enables a wide range of essential system engineering including the rejection of unfeasible designs, the assessment of impact of imperfections or disturbances. By employing this methodology, HWO can immediately benefit from well-designed initial architecture trades and early decisions, critical to NASA's goal of producing a scientifically credible and feasible mission. We present the approach, the important lessons learned, the immediate implications of the application of this approach into the design trade space, and a proposed initial error budget for HWO.
13092-144
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The search for Exo-Earth biosignatures is the ultimate, and most challenging, scientific objective of the Habitable Worlds Observatory. The Exoplanet Spectroscopy Technologies Project (abbreviated ExoSpec) is dedicated to maturing three subsystem technologies that can enable the characterization of directly imaged exoplanets: integral field spectrographs (IFS), radiation tolerant photon counting CCD detectors, and parabolic deformable mirrors (PDMs). While we advance these subsystem technologies through separate laboratory prototype demonstrations, we are also assessing their impact in terms of scientific yield at the system level through science-based end-to-end modeling and spectral retrieval simulations. This modeling pipeline provides a framework to guide engineering trades. This presentation will report on the status of the ExoSpec effort, key technology demonstrations planned, current testbed configuration, and technological progress to date.
13092-145
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The proposed Habitable Worlds Observatory (HWO) aims to study the atmospheres of Earth-like exoplanets with direct imaging. Understanding an individual Earth-like planet could require weeks of observation time split over multiple visits. The mission concepts studies that inspired HWO, HabEx and LUVOIR, both suggested that precursor science, or detecting the planets with indirect methods prior to the mission's launch, can significantly reduce the time required per planet and should be a priority. The radial velocity method is currently thought to be the most capable of finding Earth-like exoplanets, and has a number of surveys planned and underway. In this work we investigate how different designs for HWO can affect the usefulness of precursor science. We focus on how the size of HWO's field of regard, primarily determined by the pitch requirements, impacts our ability to schedule observations of planets potentially detectable by the current radial velocity surveys.
13092-146
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Habitable Worlds Observatory (HWO) will search for biosignatures from Earth-size exoplanets in the habitable zones of nearby stars. The challenge of the NUV is the drop in flux of host stars. In the NIR, the challenge is the geometric access to the habitable zone due to the wavelength dependency of the inner working angle limit of coronagraphs. Thus, some instrument parameters are more critical for improving NUV and NIR yields than others. In this paper, we evaluate the NUV and NIR spectral characterization yield sensitivity to instrument parameters such as aperture diameter, optical system throughput, starlight suppression system core throughput, contrast, contrast stability, and inner working angle and to the astrophysical parameter of exozodi brightness and exozodi calibration residual. We consider a coronagraph-only architecture as well as a hybrid coronagraph + starshade architecture.
Session PS16:
Posters - Wavefront Sensing and Segment Phasing
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-147
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Developing Earth observation capabilities in low Earth orbit requires a balance between high angular resolution and frequent revisit times. The AZIMOV project addresses this challenge through a 6U CubeSat with a 30 cm aperture deployable telescope. Despite Cubesat constraints, achieving optimal telescope performance involves precise phasing of the primary mirror. Conventional wavefront sensing methods are impractical, leading us to explore focal plane sensing. Our research focuses on leveraging Convolutional Neural Networks to correct aberrations in the primary mirror's segments. The proposed method shows robustness against noise and higher order aberrations, surpassing classical iterative techniques in terms of speed, accuracy, and reliability. Our findings indicate consistent diffraction-limited performance, particularly when imaging a point source or an unknown extended objects on Earth's surface.
13092-148
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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. Being an extremely thin structure for an optical element an active shape correction is required. Utilizing a thermal control of the surface via radiative coupling, localized phase changes are imprinted into the membrane telescope. In this paper we show a detailed modeling of the radiative adaptive optics and compare the FEM calculations to practical results from the demonstrator testbed.
13092-149
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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 membranes allows to roll the mirror and compactly store them upon launch.
In this presentation the evaluation of a mounting structure for the membrane mirror will be presented. As the mirror is a thin membrane only, a stress free mounting need to be realized taking the gravity release into account.
The mounting structure must take the membrane unfolding and radiatively controlled surface optimization into account, requiring special attend on the radiation management. Regarding a telescope structure to finalize a complete optical system has to be discussed in that respect.
13092-150
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
A-DOT (Active Deployable Optical Telescope) is a payload prototype project of a 6U segmented deployable telescope with an aperture diameter of 300 mm currently in the design phase. In this paper, we investigate 2 different strategies for phasing a deployable segmented telescope. The first method is based on a classical optimisation approach (image sharpness) and the second on deep learning techniques. For both methods, we demonstrate excellent phasing control, identifying large phasing errors (microns of PTT) and reducing errors down to the desired performance level (typically below 15 nm in the visible) using a point-source.
13092-151
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Current approaches for phasing of segmented space telescopes have required complex dedicated optics and mechanisms, such as Dispersed Hartmann sensors or grisms. These methods do not scale well as the number of segments increases. The broadband phasing approach used at the Keck Observatory does scale well and can work on space telescopes without the need for any additional hardware. We show that this method implemented as white light interferometry (WLI), using a standard imaging detector and filters, has a capture range limited only by the range of the segment actuators and can easily phase the mirrors to within the capture range of single wavelength phasing methods. An analysis of the Keck broadband phasing performance is presented and used to develop a formula for implementation of WLI on other segmented telescopes. As an example, a WLI implementation for the NASA Habitable Worlds Observatory telescope is developed and demonstrated via detailed wave-optics simulations. The implementation, performance and limitations of the proposed WLI method are discussed in detail in the paper.
13092-153
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We propose an approach for coarse alignment of a segmented space telescope using science instrument images. The recommended steps go from arbitrarily large post launch rigid body misalignments to within the capture range of coarse phasing where segment piston error is the predominant residual wavefront error. These steps include five data collection and analysis methods comprising of segment capture, segment identification, coarse focusing, segment stacking, and fine alignment using a parametric phase retrieval approach.
Using a proposed architecture for the NASA Habitable Worlds Observatory we describe the details of each telescope alignment step. We then present statistics for how well the alignment approach works keeping track of number of telescope data collections, commands applied, and residual alignment errors. This model-based demonstration establishes that the recommended coarse alignment sequence performs adequately, in a cost-effective manner, handing off to coarse and fine phasing activities further along the telescope commissioning process.
Session PS17:
Posters - Exoplanet Imaging: Photonics and Integrated optics
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-154
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We present instrument requirements and a design for an optical single photon counting photonic spectrograph (SPCPS) as determined by simulated observations of an Earth-like exoplanet atmosphere. The SPCPS uses a single photon counting CMOS detector and an on-chip photonic spectrograph. Both are nascent, compact technologies that may provide a smaller and lighter instrument than traditional spectrographs. Using the Earth’s atmosphere as a basis for the simulated observation of the exoplanet atmosphere, we select the spectral signal-to-noise ratio as the key criterion to optimize the parameters of the SPCPS system for. This work will assess the design requirements for the SPCPS for dim spectroscopic applications such as exoplanet atmosphere characterization.
13092-155
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Observations of Earth-like exoplanet atmospheres with the Habitable Worlds Observatory (HWO) will require spectroscopic observations at contrasts of 1E-10. To reduce the number of individual observations needed for characterization, it is beneficial that the coronagraph operates over a bandwidth of 20% or greater. Laboratory demonstrations have shown that these bandwidths are difficult to achieve in practice. Placing a single-mode optical fiber (SMF) in the coronagraphic focal plane offers a way to transfer planet light to a spectrograph, while the selectivity of the fiber’s mode structure also improves starlight rejection. Previous laboratory work has shown that a modified Electric Field Conjugation (EFC) algorithm can be used with an SMF to obtain a contrast of 1E-8 at a bandwidth of 20%. This result was likely limited by the presence of thermal and mechanical disturbances as well as atmospheric turbulence. In this work, we demonstrate EFC with an SMF and a classical Lyot coronagraph in a low-disturbance vacuum environment in the High-Contrast Imaging Testbed (HCIT) at NASA’s Jet Propulsion Laboratory (JPL). We show improved contrast results at a bandwidth of 20%.
13092-156
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Habitable Worlds Observatory aims to detect and characterize Earth-like exoplanets orbiting around Sun-like stars. Current coronagraph technology is not yet capable of reaching the required 10-10 contrasts; however, photonics may be able to fill this gap. One significant challenge in astrophotonics is the efficient coupling of light into the device. We have manufactured a photonic device incorporating a spatial array of photonic lanterns, designed to couple light at a focal plane into the device in the presence of aberrations. We have constructed a testbed for the free-space coupling of light into photonic devices, equipped with a segmented deformable mirror (DM), and a Zernike wavefront sensor (ZWFS). We describe the development of the testbed, the preliminary characterization of the photonic lantern array, and present preliminary results of the coupling efficiencies into the device in the presence of an aberrated wavefront. These results demonstrate a low sensitivity to wavefront aberrations, indicating significant potential for future astrophotonic applications in exoplanet detection.
13092-157
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Space borne nulling interferometry in the mid-infrared waveband is one of the most promising techniques for discovering life markers in the atmosphere of extra-solar planets. One of its main difficulties is to control free-flying telescope spacecrafts orbiting around a central combiner within accuracy better than one micrometer typically. Moreover, the whole array must be reconfigured regularly in order to observing different parent stars, thus increasing the risk of loosing one or more spacecrafts and aborting the mission before its end. In this paper is described a simplified optical configuration based on non-rotating, tip-tilted telescopes arranged along a linear array. The central combiner is made of compact integrated optics chip located close to the detection plane. This leads to considerable simplification with respect to the previously described designs. Numerical simulations confirm that typical contrasts about 10-6 are achievable.
13092-158
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
This thesis adresse the challenge of phase sensitivity in nulling interferometry techniques, using a four-telescopes architecture called "Kernel-Nuller", placing signals in phase quadrature. By utilizing an integrated optical component with electronically controlled phase shifters, the architecture allow to actively corrects optical path differences caused by manufacturing defects. This correction involve developing an algorithm to optimize device performance, evaluated through simulations and lab experiments, with ambition to test it in real conditions using the futur VLTI Nuller mode. Subsequent analysis focuses on intensity distributions produced by the Kernel-Nuller, with statistical tests and machine learning applied to detect exoplanets. Preliminary results are presented, showcasing advancements in overcoming phase aberrations for enhanced exoplanet detection.
Session PS18:
Posters - Exoplanet Imaging: Coronagraphs, Optics, and Deformable Mirrors
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-159
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Direct imaging of Earth-like exoplanets in reflected starlight demands advanced high-contrast imaging systems, such as coronagraphs, capable of suppressing starlight to levels better than 1e-10 across a wide spectral range. This exceptional precision can only be achieved using wavefront control techniques such as electric-field conjugation or speckle nulling, where deformable mirrors (DMs) play a crucial role. State-of-the-art high-actuator count DMs are usually controlled by bulky external electronics, employing about a hundred commercial high-voltage amplifier chips. To enhance the overall system's form factor, there is a pressing need for the development of new technologies. The present work focuses on the electrical and optical testing of three DM drivers designed for space applications. These drivers leverage either Application Specific Integrated Circuit (ASIC) or thin-film-transistor technology (TFT). These technologies substantially reduce the mass of the electronics, overall cost, complexity and minimize the required number of wires and chips by orders of magnitude.
13092-160
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
For the Habitable Worlds Observatory, it is essential to broaden the controllable wavelength bandwidth for high-contrast imaging and spectroscopy to increase the exoEarth yield and characterization. The Parabolic Deformable Mirrors (PDM) under the NASA Headquarters directed ExoSpec Work package is specifically tailored to do so.
A PDM is an off-axis imaging element (off-axis parabola) that is controllable. We have successfully procured a generation 1 (Gen 1) PDM device and completed in-depth characterization of the device. This robust evaluation has become instrumental in informing subsequent stages of development, particularly in shaping the design and specifying requirements for the next generation, Gen2, PDM device.
We have built a testbed in an environmentally controlled cleanroom to experimentally demonstrate the use of a parabolic DM in a coronagraph instrument as well an integral field spectrograph (IFS). This versatile testbed is designed to test different DM architectures, various low-order wavefront schemes, and a lenslet based IFS.
13092-161
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Habitable World Observatory (HWO) is a NASA strategic mission recommended by 2020 astronomical decadal survey. Integral spectrometers play an important role to verify if the observed exoplanet is habitable. The traditional lenslet array based Integral Field Spectrometer (IFS) has the advantage of simplicity and compactness. However, it does not use detector pixels efficiently in order to prevent wavelength crosstalk among adjacent spectra. The efficient lenslet/mirrorlet IFS combines the advantages from both lenslet based and imager slicer based IFSes—keeping lenslet IFS’s simplicity and compactness, concurrently adding slicer IFS’s detector efficiency. This paper discusses the principle of efficient lenslet/mirrorlet IFS, design philosophy, and efficient spectral trace layout ideals. It uses HWO NIR IFS requirement as an example to provide an efficiency mirrorlet IFS optical design. The high detector efficiency not only reduces Needed detector pixel numbers, but also reduce the high communication rate demanding for much a large multiple instrument mission.
13092-162
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
An integral field spectrograph (IFS) camera may help fulfill the exoplanet characterization goals of a future Habitable Worlds Observatory. The Roman Space Telescope Coronagraph Instrument Project established the laboratory performance baseline of a combined coronagraph and IFS system with the Prototype Imaging Spectrograph for Coronagraphic Exoplanet Studies (PISCES). New demonstrations are needed to expand on this milestone in terms of contrast, bandwidth, and field of view towards the requirements of the next flagship mission. Here we present the design of a successor to PISCES that can observe a 20 lambda/D field of view with a 30% instantaneous bandwidth at visible wavelengths with a resolving power of 70. The instrument will interface with the coronagraph on the Decadal Survey Testbed 2 located in the High Contrast Imaging Testbed 2 vacuum chamber at NASA's Jet Propulsion Laboratory, to support demonstrations of broadband wavefront sensing and control and data post-processing techniques.
13092-163
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Future space observatories will likely have segmented primaries, causing diffraction effects that reduce coronagraph performance. Reflective binary pupil apodizer masks can mitigate these, with the metamaterial black silicon (BSi) showing promise as a strong absorber. To bring contrast ratios to the 10^-10 level as needed to observe Earth-like exoplanets, feature sizes on these BSi masks will need to be less than 5 microns when paired with MEMS deformable mirrors. As scalar diffraction cannot reliably model this feature size, we developed a Finite-Difference Time-Domain (FDTD) model of BSi masks using MEEP software. We characterize the polarization aberrations the BSi induces and its specular reflection to develop a contrast budget. Using the physical optics Python software HCIPy, we simulate a shaped pupil Lyot coronagraph based on the FDTD model of BSi masks. Finally, we compare the point spread functions (PSFs) from the FDTD modeled BSi masks with the lab measurements.
13092-164
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Direct detection of earth-like planets using an internal coronagraph will require telescope wavefront stability on the order of ~ 10 picometers over a time scale of ~ 10 minutes. Passive wavefront stability of a space telescope at this level has never been demonstrated, yet active sensing and control is feasible. However, the sensing must be done during the science observation, and with a minimum of non-common path errors. The sensing and control must be done where it matters most – at the location of the focal plane mask. We have architected such a device, that will enable both of these capabilities.
There are three key components of this optical element: 1) the coronagraphic field stop 2) the Zernike phase dimple and 3) the dielectric coating/antireflection surface. We will discuss the design and engineering of these key components, with an emphasis on the first iteration of the actual devices. We will also provide characterization of these devices in our metrology setup. Status of the testing and characterization of these devices in the vacuum, high-contrast optical testbed will also be discussed.
13092-166
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Near Angle Scatter is caused by spatially correlated surface structure and uncorrelated microstructure. This paper investigates the impact of these phenomena on coronagraph flux ratio and derives surface specifications to mitigate near-angle scatter effects.
13092-167
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
In this work, we experimentally demonstrate the performance of the Dispersion Leverage Coronagraph (DLC). The novel DLC coronagraph utilizes primary objective gratings for optical leverage by nulling across an entire spectrum in the focal plane. The unique nulling architecture of DLC allows for the spectral resolvance of the grating, rather than the typical diffraction limited angular resolution of the focusing optics, to be the primary determining factor of the effective inner working angle. With the use of an end-to-end DLC optical system constructed at RPI, we evaluate coronagraphic metrics such as the null depth, inner working angle, point-like source leakage, and the sensitivity to residual OPD errors and pointing jitter. These experimental results are ultimately compared with previously published theoretical estimates of the performance of DLC.
13092-169
19 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
NASA is about to embark on an ambitious program to develop a Habitable Worlds Observatory (HWO) flagship mission to directly image ~25 potentially Earth-like planets and spectroscopically characterize them for signs of life. A critical capability of the HWO mission is starlight suppression. In this paper, we present the results of a survey of potential coronagraph designs suitable for HWO, ranging from the relatively mature technologies to emerging ones. Our results consist of a database of designs from the world-wide community, their assessments against criteria such as expected science yield and maturity, modeling tools to facilitate such assessments in the future, and summary of key findings.
Session PS19:
Posters - Exoplanet Imaging: Sensing, Control, Algorithms, and Data Processing
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-170
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Dynamic completeness--the probability of detecting an exoplanet on the $i$th observation of a particular target star--is an invaluable tool for exoplanet mission simulation and analysis. The evaluation of this quantity requires the marginalization of the propagation of a particular sample of planetary parameters. This process is either approximated via Monte Carlo, or by a much coarser approximation that assumes a near-constant value for the dynamic completeness after some characteristic settling time after the initial observation. The former approach is computationally costly, whereas the latter approach is frequently not sufficiently accurate for simulating realistic observing scenarios, and, depending on the population of planets being investigate, the characteristic settling time may actually be longer than the mission duration. Here, we discuss alternative techniques for computing dynamic completeness, including semi-analytical techniques for evaluating the conditional density function of the true anomaly at arbitrary points in time. We present error analyses for various approximations, along with execution time analyses for the different approaches considered.
13092-171
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We present a control loop based on a mid-order wavefront sensor (MOWFS) to correct for fine cophasing errors in exoplanet imaging with future large segmented aperture space telescopes.
Thermo-mechanical drifts in these observatories lead to small misalignments of the telescope mirror segments and contrast degradation in the coronagraphic image of an observed star. We propose a wavefront control approach based on a Zernike sensor to address these fine cophasing errors. With the HiCAT testbed and its IrisAO deformable mirror, we first characterize the segment discretization steps and the actuator cross-talks using the MOWFS. We then focus on the study and validation of the MOWFS control loop with random drifts on the IrisAO. These results will give insights for exo-Earth observations with the Habitable Worlds Observatory.
13092-172
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Maintaining incoming wavefront stability while directly imaging exoplanets over long exposure times requires robust high-order wavefront sensing and control systems. This paper analyzes the performance of dark zone maintenance (DZM) for maintaining high-contrast levels by performing a parameter scan on the signal-to-noise ratio (SNR) of shot noise injected dark zone images and the wavefront error drift rate through hardware validation. These parameters are prescribed on the High-contrast Imager for Complex Aperture Telescopes (HiCAT) testbed. The testbed results are compared to theoretical model-based contrasts and HiCAT simulator results.
13092-173
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
One of the primary scientific goals of the upcoming Habitable Worlds Observatory (HabWorlds) is to take spectra of reflected light from nearby Exo-Earths. High-contrast integral field spectroscopy (IFS) instrumentation offers one promising avenue to obtain these observations. Aside from taking low-resolution spectra of directly imaged exoplanets, IFS cameras provide multi-wavelength images of residual starlight speckles and deformable mirror actuator probes. This year we restored the functionality of the Prototype Imaging Spectrograph for Coronagraphic Exoplanet Studies (PISCES) and integrated it with the ExoSpec coronagraph testbed at Goddard Space Flight Center. We will use the PISCES IFS to conduct in-air tests of broadband, high-order wavefront sensing and control techniques with a shaped pupil coronagraph.
13092-174
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The High Contrast Spectroscopy Testbed (HCST) within the Caltech Exoplanet Technology laboratory serves as an in-air coronagraphic testbed demonstrator, integrating a high order deformable mirror for wavefront control and a vector vortex coronagraph (VVC). HCST has demonstrated excellent in-air contrast performance, achieving 1×10^−8 raw contrast in broadband light, for both the apodized off-axis segmented pupil configuration and using single mode fiber planet injection. By introducing a tip/tilt sensor that utilizes the out-of-band reflected light from the VVC, coupled with a tip/tilt mirror, our objective is to address dynamic errors, thereby enhancing the wavefront stability of the experiment.
13092-175
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Among the new technical challenges for high-contrast coronagraphy with the Habitable Worlds Observatory (HWO) is the active low-order stabilization of the optical wavefront with a minimum of residual high-order errors. We will explore, through modeling and experiment, the advantages of separating the wavefront control system into (a) an active closed-loop stabilization of low spatial frequencies followed by (b) the iterative control of the high spatial frequencies and open-loop maintenance of the high-contrast coronagraph dark field.
We describe the implementation of a new low-order wavefront control (LOWFC) element for the active correction of wavefront errors associated with telescope line-of-sight jitter, thermal distortions, and alignment drift. Incorporated into a laboratory testbed and used in concert with a Hybrid Lyot Coronagraph (HLC) and Zernike wavefront sensor (ZWFS), this hardware will test the concept at high levels of contrast in a dynamic testbed environment, thereby providing confidence that sources of error have been unambiguously identified and effectively controlled or mitigated.
13092-176
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Lyot-style coronagraphs, with wavefront sensing and control, resiliently handle challenging apertures like the hexagonally segmented primary mirror for the Habitable Worlds Observatory. In the apodized pupil Lyot coronagraph (APLC), rejected light by the focal plane mask enables a highly photon-efficient Zernike wavefront sensor (ZWFS) to measure low-order aberrations. Tuning control strategies on the High-contrast imager for Complex Aperture Telescopes (HiCAT) testbed in broadband light, we achieve robust concurrent operation of low-order and dark hole (DH)-related control loops. In our analysis, we address the handling of loop interruptions during sequential wavelength scans, and the mitigation of the chromatic offsets coming from non-common path aberrations in the low-order optical train.
13092-177
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Direct imaging of exoplanets increasingly relies on focal plane wavefront sensing algorithms. These techniques use the science detector to estimate the static and quasi-static aberrations in the instrument. While Pair-wise probing is the most common wavefront sensor for space-based applications, Borde & Traub forerunner algorithm allows theoretically the recording of less images for the same purpose. In this work, we revisit the Borde & Traub focal plane wavefront sensor and present its performance on coronagraphic testbeds at JPL as well as a first on-sky control of non-common path aberrations with such method on VLT/SPHERE.
13092-178
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Phase Shifting Interferometry (PSI) is routinely used to measure the surface figure error and wavefront error for a wide range of optics. It provides a large dynamic range and naturally suppresses numerous internal errors in the system. In high contrast imaging, it is necessary to measure and stabilize the entire complex E-field to produce and maintain a “dark hole” in which an exoplanet can be directly imaged. In this paper, we present new data processing techniques that enable estimation of the full complex E-field from PSI data. With these techniques, changes to the wavefront amplitude caused by components such as the second deformable mirror (DM) in a coronagraph can be sensed. We also present further extensions to PSI data processing which enable direct reconstruction of the change in the complex E-field. These allow reliable sensing of dynamics ≤ 1 λ without the use of a phase unwrapping algorithm, even when the absolute phase is >> 1 λ. Through numerical modeling, we investigate the performance of this promising metrology technique in the context of a Six Meter Space Telescope (6MST) and coronagraph in family to concepts for the future Habitable Worlds Observatory (HWO).
13092-179
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
This study assesses the performance of high order wavefront sensing and control (HOWFSC) algorithms when run on computationally limited embedded processors analogous to those typically used for deep space missions. We test the performance of spaceflight-relevant CPUs and FPGAs when computing matrix operations and discrete fourier transforms in support of HOWFSC operations like Electric Field Conjugation (EFC) and Fourier optical modeling. We interface the embedded processors with a software model of a telescope and coronagraph to perform processor-in-the-loop testing of HOWFSC algorithms running on embedded processors. We test a range of telescope and HOWFSC algorithm configurations that are relevant to the design of future space missions like the Habitable Worlds Observatory (HWO).
13092-180
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Exoplanet imaging requires the minimization of starlight residuals in an area of interest in the focal plane called the dark hole. State-of-the art wavefront control methods require several iterations to minimize the intensity in the dark hole, which limit the overall contrast performance. This study aims to develop a data-driven method to achieve contrast maximization in coronagraphic images in as few iterations as possible. For this purpose, we train a model-free, deep reinforcement learning agent to learn a control strategy to maximize the contrast in the dark hole. The agent takes several focal plane images with phase diversity as input and outputs control voltages for the deformable mirror, and is trained with simulated coronagraphic images. The results are compared with classical model-based methods.
13092-181
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The search for biosignatures in potentially habitable exoplanets is one of the major drivers for the coming decades, and the prime science case of the HWO NASA mission. Ahead of this, the RST mission will demonstrate critical technologies to reach 1e-8 contrast limits using active wavefront sensing and control (WFC) for the first time in space.
Given the stringent constraints required to achieve the exoEarths 1e-10 contrast levels, observing strategies and post-processing techniques must also be optimized along with hardware and WFC technologies. With ESCAPE (2022-2027 ERC program), we will explore how the wavefront sensor telemetry, deformable mirrors, and data accumulated over time can be used to optimize detection limits for space high-contrast imaging.
In this presentation, we will introduce the ESCAPE project and detail the methodology adopted to investigate observing strategies and post-processing techniques for active space telescopes and advocate for an on-sky demonstration on the RST CGI instrument.
13092-182
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Roman Space Telescope will be a critical mission to demonstrate high-contrast imaging technologies allowing for the characterization of exoplanets in reflected light. It will demonstrate 1e-8 contrast limits or better at 3-9 lambda/D separations with active wavefront control for the first time in space.
The detection limits for RST-CGI are expected to be set by wavefront variations between the science target and the reference star observations. We are investigating methods to use the DMs to methodically probe the impact of such variations onto the coronagraphic PSF, generating a PSF library during observations of the reference star to optimize the starlight subtraction at postprocessing.
We are collaborating with STScI to test and validate these methods in lab using the HiCAT tested, a high-contrast imaging lab platform dedicated to system level developments for future space missions. In this presentation, we will present the first applications of these methods on HiCAT.
13092-183
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
JWST is probing circumstellar environments at an unprecedented sensitivity. However, the performance of high-contrast imaging instruments is limited by the residual light from the star at close separations (<2-3”), where the incidence of exoplanets increases rapidly. There is currently no solution to completely get rid of the residual light down to the photon noise level at those separations. We are further developing and implementing a post-processing method built on a Bayesian framework that provides a more robust determination of faint astrophysical structures around a bright source. This approach uses a model of high-contrast imaging instrument that takes advantage of prior information, such as data from wavefront sensing, to estimate simultaneously instrumental aberrations and the circumstellar environment. Our goal is to further improve the contrast gain over the contrast that can be achieved, starting with NIRCam imaging and coronagraphic imaging from our Cycle 1 calibration program. This work will inform operations and design of future space-based missions such as the Roman Space Telescope Coronagraph Instrument and the Habitable Worlds Observatory.
Session PS20:
Posters - Exoplanet Imaging: Polarization
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-187
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
High-contrast imaging in the next decade aims to image exoplanets at smaller angular separations and deeper contrasts than ever before. A problem that has recently garnered attention for telescopes equipped with high-contrast coronagraphs is polarization aberration arising from the optics. These aberrations manifest as low-order aberrations of different magnitudes for orthogonal polarization states and spread light into the dark hole of the coronagraph that cannot be fully corrected. The origin of polarization aberrations has been modeled at the telescope level. However, we don't fully understand how polarization aberrations arise at the instrument level. To directly measure this effect, we construct a dual-rotating-retarder polarimeter around the SCoOB high-contrast imaging testbed to measure its Mueller matrix. With this matrix, we directly characterize the diattenuation, retardance, and depolarization of the instrument as a function of position in the exit pupil. We measure the polarization aberrations in the Lyot plane, both with and without the Vector Vortex Coronagraph, to understand how polarization couples into high-contrast imaging residuals.
13092-188
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The spectroscopic study of mature giant planets and low mass planets (Neptune-like, Earth-like) requires instruments capable of achieving very high contrasts (1E9, 1e10) at short angular separations. To achieve such high performance on a real instrument, many limitations must be eliminated or minimized: complex component defects (coronagraph, deformable mirror), optical aberrations and scattering, mechanical vibrations and drifts, polarization effects, etc.
In this presentation, we will focus on the polarization effects that are present on the our high contrast test bench in Paris (THD2) which creates differential aberrations between the two polarization states. These could be linked to the Goos-Hänchen and Imbert-Fedorov effects, both of which cause spatial shifts and angular deviations, longitudinal and transverse respectively.
After describing the THD2 bench, we will present the protocol we used to measure the effects of polarization on the light beam. These measurements will be compared with the predicted values. We will also present solutions for minimizing these effects on THD2, but also more generally for all high-contrast instruments.
13092-189
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Polarization aberrations originating from the telescope and high-contrast imaging instrument optics introduce polarization-dependent speckles and associated errors in the image plane, affecting the measured exoplanet signal. Understanding this effect is critical for future space-based high-contrast imaging instruments that aim to image the Earth analogs with 10^(-10) raw contrast and characterize their atmospheres. We present end-to-end modeling of the polarization aberrations for a 6m-class telescope with a high-contrast imaging instrument with wavefront control and sensing. We use a Vector Vortex Coronagraph as the focal plane mask and incorporate polarization filtering. We compare the raw contrast obtained for a 6m on-axis three-mirror anastigmat (TMA) with an off-axis segmented TMA design using a protected aluminum coating for the telescope mirrors and the off-axis parabolas in the high-contrast imaging instrument. We find the dominant polarization aberrations in the system are retardance defocus and tilt, and the contrast estimated for an off-axis TMA is an order of magnitude better than an on-axis TMA incorporating polarization aberrations.
Session PS21:
Posters - Exoplanet Imaging: Polarization
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-190
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
High angular resolution astronomy in far-infrared using intensity interferometry is discussed together with experimental status of a laboratory demonstrator of intensity interferometry. Using fast SIS photon detectors near the gap frequencies of superconductor enable fast measurement of photon bunches, which enables delay time measurements for aperture synthesis imaging. Photon counting detectors will enable background limited observation for long baseline intensity interferometry. Optical experiment using the laboratory demonstrator is on-going and their results will be presented. A roadmap toward space-borne far-infrared interferometer including Antarctic terahertz intensity interferometers will be discussed.
13092-191
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We present a new concept study of an extremely large optical infrared space telescope comprising formation-flying ultra-small satellites. The science mission is (1) to spatially resolve the surface environments of nearby Earth-like exoplanets and (2) to map the gaseous disk around the first stars in the early Universe. We require a spatial resolution of at least 2 micro arc-seconds to distinguish the ocean, land, plants, and volcano on the exoplanets at 10 parsec from us. Therefore we require a telescope aperture size of at least 75 km. In order to realize such extremely large-aperture space telescope, we propose a new telescope concept with a combination of multiple diffractive optical elements and electromagnetic formation flight.
13092-193
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We present a baseline science operations plan for the Black Hole Explorer (BHEX), a space mission concept aiming to confirm the existence of the predicted sharp “photon ring” resulting from strongly lensed photon trajectories around black holes, as predicted by general relativity, and to measure its size and shape to determine the black hole's spin. The BHEX radio antenna will co-observe with a ground-based very long baseline interferometric (VLBI) array, providing unprecedented high resolution with the extension to space that will enable photon ring detection and studies of active galactic nuclei. Here we outline the concept of operations for the hybrid observatory coordinating both a VLBI network and an optical downlink terminal network, the available observing modes, the proposal and observation planning process, and data delivery to achieve the BHEX mission goals and meet mission requirements.
13092-194
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The photon ring is a narrow ring-shaped feature (predicted by general relativity, but not yet observed) that appears in black hole images. It is caused by the extreme bending of light within a few Schwarzschild radii of the event horizon and provides a direct probe of the unstable bound photon orbits of the Kerr black hole geometry. The precise shape of the observable photon ring is remarkably insensitive to the details of the astronomical source and can therefore be used as a precise probe of strong-field gravity. The Black Hole Explorer (BHEX) is a proposed space-based experiment targeting the supermassive black holes M87* and Sgr A* with radio-interferometric observations at frequencies of 86 through 345 GHz and from an orbital distance of ~40,000km. We forecast that its design will enable a measurement of the photon rings around M87* and Sgr A* and confirm the Kerr nature of these two sources.
13092-195
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Black Hole Explorer (BHEX), is an orbiting, multi-band, millimeter radio-telescope, in hybrid combination with millimeter terrestrial radio-telescopes, designed to discover and measure the thin photon ring around the supermassive black holes M87* and Sgr A*. In order to guide the mission design for the BHEX instruments, this paper explores various aspects of the photon ring, like the spin-induced changes to its shape, or the intricate flow of light around a spinning black hole, by tracking, through visual simulations, photons as they course along geodesics. Ultimately, the aim of these visualizations is to advance the foundational aims of the EHE instrument, and through this experiment to articulate spacetime geometry via the photon ring.
13092-196
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
In this presentation, we describe the baseline design of a large, light weight, space borne antenna achieving high efficiency operation at mm/sub-mm wavelengths, for the Black Hole Explorer (BHEX) mission concept. BHEX targets fundamental black hole physics enabled by the detection of the finely structured image feature around black holes known as the photon ring, theoretically expected due to light orbiting the black hole before reaching the observer. Interferometer baselines much longer than an earth diameter are needed to attain the required spatial resolution to achieve detection. The science goals require high sensitivity observations at mm/sub-mm wavelengths, placing stringent constraints on antenna performance. The baseline design described seeks to balance the antenna aperture, volume and mass constraints of prospective mission opportunity profiles and the desired high performance.
13092-197
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We present two receiver designs for the Black Hole Explorer mission, which would extend the current Event Horizon Telescope into space. Plan A employs a tri-band receiver: an 86 GHz HEMT receiver and a pair of SIS receivers centered at 230 and 345 GHz. These receivers feature a state-of-the-art dual polarized sideband separating (2SB) architecture. In plan B, the 345 GHz receiver is removed and a simpler Double-Side-Band (DSB) architecture is adopted. This design represents a compromise between sensitivity and requirements on resources. We will report on the trade-off study of these two plans.
13092-198
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Black Hole Explorer (BHEX) is a space-VLBI mission that will extend the Event Horizon Telescope into space. The cryogenic receivers must be cooled down to 4.5K. A cryogenic system consisting of two Stirling cryocoolers and a Joule-Thomson cooler has been explored which consists of a 20K and a 4.5K cold stage in order to cool a combined heat load of approximately 250mW. The integration challenges of the cryocooling system with the receivers and broader instrument are explored, where power, mass, and thermal challenges require careful considerations and trade-off. This study presents a feasible cryocooling design that reaches the cold temperature requirements of the BHEX instrument.
13092-199
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We present studies of terrestrial versions of signal processing elements for the Black Hole Explorer (BHEX) space telescope. The first stage is a heterodyne system that performs a frequency translation from IF to baseband and conditions it for digitization. The second stage is the digitizer and digital processor. The output from the digitizer interfaces with the optical downlink sub-system. The terrestrial pre-production unit is a functional test of the design. We describe our staged approach to TRL maturation for a mission proposal in 2025.
13092-200
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Event Horizon Explorer (EHE) is a mission concept that can dramatically improve state-of-the-art astronomical very long baseline interferometry (VLBI) imaging resolution by extending baseline distances to space. To support these scientific goals, a high data rate downlink is required from space to ground. Laser communications is a promising option for realizing these high data rate, long-distance space-to-ground downlinks with smaller space/ground apertures. Here, we present a scalable laser communications downlink design and initial test results.
13092-201
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Event Horizon Explorer (EHE) is a space VLBI mission concept, which can probe the black hole spacetime and the plasma properties including the magnetic fields of the accretion flows and relativistic jets. We propose scientific inquiries anticipated to be addressed by EHE, primarily through the imaging of microarcsecond-scale signatures in target sources. An appearance of a crescent-shaped shadow in a bright state of the M87 will enable us to constrain the magnitude of the black hole spin (Kawashima et al. 2019). A possible appearance of the plasma injection region in the vicinity of the black hole results in the formation of the multiple ring structure and may enable us to understand the jet formation processes (Kawashima et al. 2021, and Ogihara et al. submitted to ApJ). In addition, the reversal of the sign of the circular polarization and the separation of linear and circular polarization flux peaks will constrain the magnetic field structure and the thermal properties of the electrons, respectively (Tsunetoe et al. 2021, 2022). Other topics, including potential scientific inquiries of luminous active galactic nuclei, will be also discussed.
Session PS22:
Posters - Time Domain: High Energy Transients
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-202
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The payload Terzina is one of the 2 payloads on bord the mission NUSES.
Scientific Aim is the Astrophysical neutrinos and cosmic rays through space-based detection of the atmospheric Cherenkov emission.
In the paper it will be explained the logical trade off process followed in the optical design and will be described the instrument performances.
13092-203
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
In 2022-23, a conseptual change of the optical train around the focus of the infrared telescope of HiZ-GUNDAM project has been developed: a double Koester prism is newly introduced as a key optical component to devide the incident near-infrared beam (0.9-2.5um) into four wave-bands, enabling to focus four band images simultaneously onto the 1k MCT sensor array. It will greatly reduce the tocal cost compared with the previous design where three 1k MCT sensors were used. The prism consists of four pieces of triangular columuns made of anhydrous fused silica glued on the base plate made of fused silica. We carefully selected the glue which is durable against the vibration during launch as well as the harmful environment onboard. We will show the design, our simulation of structure/vibration analysis and the fabrication of the BBM model of the double Koester prism.
Session PS23:
Posters - Submillimeter, millimeter, and Radio
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-204
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Making use of the API feature in the Zemax Opticstudio software which allows for rapid raytracing computations, we consider the JAXA LiteBIRDbird CMB High frequency telescope (166-448 GHz) as a study case and perform a parametric study of the position of its infrared rejecting filters by looking at the output from multiple configurations within a python script. By manipulating the resulting intermediate products of ray incidence distribution we determine the optimal position of the filters that will minimize ghost features on the focal plane (or define some competing configurations based on desired outcomes). We characterize the variation of spectral response across the focal plane caused by the impact angle distribution on the optical coatings and finally the distribution of thermal (out of band) rejected light reflected by the filters on the optical baffles.
13092-205
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
LiteBIRD is a space mission aimed at searching for the primordial gravitational waves through polarization observations of the cosmic microwave background radiation. It will conduct all-sky observations from an L2 orbit in the millimeter-wave frequency range (34-448 GHz) by using two types of telescopes.
One of the challenges faced by the LFT, one of the telescopes on LiteBIRD, is the issue of infrared radiation entering the telescopes. We are exploring the deliberate roughening of the reflector surfaces to scatter the infrared radiation on the reflector as a potential solution.
In this conference, we will provide an update on the progress of these efforts.
13092-206
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
LiteBIRD is a JAXA strategic L-Class mission whose objective is the study of B-mode polarization from the cosmic background radiation detection (CMB). Observations need to be conducted over a wide frequency range (34 GHz – 448 GHz) by three telescopes (the Low-Frequency Telescope and the Middle and High-Frequency Telescopes). We describe the electrical architecture of these instruments and the architecture of the Digital Processing Unit of the payload. The DPU is composed of a new SRAM based FPGA component called NG-ULTRA (4 x R52 ARM processor + FPGA on a chip). We present more particularly the science data streams, the science on-board processing pipeline and the use of an embedded space-qualified hypervisor called Xtratum XNG.
13092-207
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
LiteBIRD is a JAXA-led space mission for cosmic microwave background (CMB) polarimetry. One of the challenges in terms of the telescope optics is to characterize and suppress the far sidelobes in its antenna beam patterns, which contaminate the CMB signals with Galactic foreground radiation. For the Low-Frequency Telescope (LFT; 34 - 161 GHz) aboard LiteBIRD, the requirements include the far-sidelobe knowledge of −56 dB. On the other hand, the LFT has a wide field of view (18° × 9°) and will operate at 5 K. In this presentation, we report the devleopment of a near-field antenna pattern measurement setup in a cryogenic chamber. We implement a cryogenic-compatible millimeter-wave circuit and motorized stages inside a chamber. In this way, we can scan the aperture of the LFT, which is fully encased and cryogenically cooled in the chamber. As the development of the LFT is in the design phase, we will present our latest measurement results of a 1/4-scaled LFT.
13092-208
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The LiteBIRD space mission is a next generation microwave telescope array which aims to detect the primordial B-mode signal in the Cosmic Microwave Background (CMB). LiteBIRD will consist of three telescopes (low, mid, and high frequency) sensitive to frequencies from 40 - 402 GHz. The low and mid frequency telescopes (LFT and MFTs) will utilize lenslet-coupled planar antennas and transition edge sensor (TES) bolometers, while the high frequency telescope (HFT) will use horn-coupled ortho-mode transducers (OMTs).
A number of mechanical, optical, and thermal considerations must be made in order to effectively integrate these detector wafers into the telescope. We present the current detailed designs for the LFT and MFT detector sub-assemblies, as well as the current status of mechanical simulations and prototype testing to ensure launch survival and adequate optical performance.
13092-209
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
LiteBIRD is a JAXA strategic L-Class mission designed to search for the existence of primordial gravitational waves produced during the inflationary phase of the Universe. This objective involves measuring the large-scale B-mode polarization pattern in the cosmic microwave background (CMB).To fulfill this objective, observations have to be made over a wide frequency range, which is accomplished by three telescopes: the Low-Frequency Telescope (LFT-[34GHz-161GHz]) led by JAXA and the Middle & High-Frequency Telescopes (MHFT-[89GHz-448GHz]) under European responsibility and led by CNES. An extensive measurement campaign was conducted for the MHFT optical prototype, involving both near-field and holographic phase-retrieval measurements. The main goal of this RF characterization campaign is to demonstrate the reliability and the accuracy of such measurements techniques applied in characterizing a refractive type system like MHFT. This paper describes the measurement setups and presents the initial results and conclusions derived from near-field and holographic phase-retrieval measurements conducted on the optical and RF prototype of the MHFT.
13092-210
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The LiteBIRD experiment is an international spaceborne telescope, led by JAXA, to observe cosmic microwave background (CMB) radiation. The instrument will be deployed to measure and characterize the signature of the primordial gravitational waves from cosmic inflation in the B-mode polarization of the CMB radiation. These observations and measurements will take place over 15 separate bands in the range of 34 to 448 GHz. This paper will describe the process flow developed to fabricate the lowest bands of the detectors, namely in the range of 34 to 99 GHz. The detector wafer itself will be further divided into two process flows - one covering the cosmic ray mitigation structures and the other describing the trichroic polarization sensitive sinuous antenna, coupled to the transition-edge sensor (TES) detectors fabricated on the device side of the wafer. Building on the process flow previously developed for detector wafers in the adjacent higher low-frequency bands, these wafers will also incorporate Pd based cosmic ray mitigation structures, of different thicknesses, on both the skyside and device side.
13092-211
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Future optical systems in the sub-mm range require a large field of view and high angular resolution, for which axial refractive systems are a solution.
Instruments require cryogenic cooling of their refractive optics. Thus, the characterization of precise dimensional and refractive index changes with temperature is critical. We have studied the optical properties of ultra-high molecular weight polyethylene, polypropylene, and high resistivity float-zone silicon in the temperature range 300K-4K, covering a frequency range of 60–600 GHz.
We have developed processes for broadband multi-layer AR coatings for lenses and optical components. We present initial results from a study that investigates optical and mechanical properties as a function of the number of annealing cycles. This ensures that the coating process will not affect the required properties of the component substrate.
We then present demonstrated performance for multilayer coatings on polymers and machined coatings on silicon substrates.
13092-212
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The terahertz wave spectrum is considered crucial for a better understanding of the early universe. Integrated superconducting spectrometers (ISSs) such as the Deep Spectroscopic High-redshift Mapper (DESHIMA) use tightly packed bandpass filter structures to accurately measure the redshift of dusty star-forming galaxies over a wide range. Fabricating these filter structures relies on state-of-the-art nanofabrication techniques, where nanometer-size variations in the filter structures can result in blind spots in the observed redshift spectrum, eliminating the mapping of potentially large timeframes in the early universe.
Here we report a significant enhancement in the performance of DESHIMA filter banks by addressing limitations in the electron-beam lithography processing. By comparing the performance of multiple iterations of DESHIMA devices we were able to show an average reduction of 34% in the frequency variance among the filters, thereby, closing the gaps in the redshift spectrum and providing valuable insights into the development of the next-generation ISSs.
Session PS24:
Posters - Astronomy on the Surface of the Moon
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-213
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
We have planned the Lunar observatory project, TSUKUYOMI aiming to meter-wavelength observations on the Moon. One of the scientific objectives is to observe the 21 cm global signal from the dark ages using the 1–50 MHz observing frequency range. The receiving system must have a noise temperature sufficiently lower than the foreground noise and also requires the flat bandpass response. To cover the ultra-wide bandwidth, an electrically-short dipole antenna and a preamplifier with high input impedance will be employed. This paper focuses on a feasibility study of the system performance. The environment of and around the observation site, such as the lunar surface dielectric constant and temperature, affects the bandpass response because it alters important parameters such as the antenna beam pattern and impedance. The investigation results of relationship between the surrounding environment and the bandpass response will be also reported.
13092-214
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Low-frequency radio observations of below 10 MHz on the Moon are free from several radio interference, allowing for the study before cosmic reionization, which is impossible from the Earth. Our lunar observatory project, TSUKUYOMI aims to observe the 21cm global signal from the Dark Ages, requiring wideband observations covering 1-50MHz to spot absorption features of ~40 mK relative to the CMB. Considering the radiation from the Milky Way, which is the main noise source, and the reception characteristics of the short dipole antenna, a pre-amplifier with noise lower than 2nV/sqrt(Hz) will result in a system noise well below this main noise over the entire bandwidth and a roughly flat wideband response. Managing the input/floating capacitance and using a lumped constant circuit is crucial for wideband performance. This paper outlines the wideband system and delves into the system performance requirements.
13092-215
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Lunar Surface Electromagnetics Explorer at Night (LuSEE-Night) is a joint initiative between NASA and DOE that is anticipated to launch at the end of 2025. It aims to make sensitive measurements across two decades in frequency between ~0.5 MHz and ~50 MHz from the radio-quiet far side of the moon with four orthogonal monopole antennas. The performance and sensitivity of the antennas are critical aspects to making the project a success. This talk will delve into the design, modeling, and testing of the antenna module.
Session PS25:
Posters -Solar System and Heliophysics
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13092-216
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
In-flight calibrations for space-based optical instruments are crucial to ensure the reliability of the acquired data. This work presents in-flight simulations applied to the Metis coronagraph of the Solar Orbiter spacecraft. This study introduces a simulation method for predicting the visibility of stars in the instrument field of view. Another complementary simulation process is also presented, which integrates stellar and instrumental characteristics to predict the expected digital numbers on the detector. This second step offers additional valuable information on the behaviour of the instrument considering the input source conditions. This research contributes to effective in-flight calibrations, ensuring the precision of scientific observations in the challenging Metis solar environment.
13092-217
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Space-weather Solar Coronagraph (SwSCOR) is an externally occulted, space-based solar coronagraph that is being developed at Southwest Research Institute for scientific or operational deployment to observe space weather systems such as coronal mass ejections and solar wind stream interaction regions. We will present the design and predicted performance of the coronagraph inclusive of the data reduction pipeline that SwRI is creating. Our design has an external occulter in a baffled vestibule feeding an optical lens assembly onto a CCD detector. The occulter is designed with SwRI Fresnel diffraction codes and provides excellent attenuation performance. The optical lens assembly is radiation resistant for long on-orbit lifetime as is athermally constructed. The CCD and readout electronics are direct copies from the SMEX mission PUNCH providing high QE, low dark noise, low read noise, and a pseudo-frame transfer for shuttering the exposures. Our design directly incorporates the data analysis pipeline from the start of the design to ensure the final data product is suitable for space weather predictions.
13092-218
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Obtaining the infrared solar spectrum from the ground is difficult outside the observation windows allowed by the Earth's atmosphere. Observations over 10 months with the Near InfraRed (NIR) spectrometer on the Atmospheric Chemistry Suite (ACS) platform of the Trace Gas Orbiter (TGO) mission orbiting MARS were used to overcome this limitation. Indeed, the line of sight of the spectrometer ACS-NIR observing the Sun gradually crosses the atmosphere of MARS as the satellite moves in its orbit. The high-resolution solar spectrum is then directly obtained when the line of sight is above the atmosphere. The main concerns for recovering the solar spectrum is spectral contamination of orders. We first present how we processed the order images to obtain the solar spectrum in the 0.7-1.7 µm band. We show that the use of 3 off-centre images of the same order allows to avoid spectral contamination and to improve the detection of solar lines where the intensity is low in the order image. We then compare the solar spectrum obtained with that of Toon taken as a reference. We end by addressing the parts of the spectrum which present solar lines located in spectral bands not observable from Earth.
13092-219
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The ESA mission Solar Orbiter was successfully launched in February 2020. The Photospheric and Helioseismic Imager (PHI) provides measurements of the photospheric solar magnetic field at high solar latitudes with high polarimetric accuracy. The required pointing precision is achieved by an image stabilisation system (ISS) that compensates for spacecraft jitter. The ISS consists of a high-speed correlation tracker camera (CTC) and a fast steerable tip-tilt mirror operated in closed loop.
We will present the results of the calibration measurements and performance tests from ground measurements, during commissioning and science phase. In addition, the correlation tracker was used to directly measure the pointing stability of the satellite.
13092-220
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Upon reflection on a surface, light can undergo a change in its polarization, which can reveal key information about a surface’s structure and composition. We introduce here a novel laboratory ellipsometer that combines polarimetry with spectroscopy to access a new dimension of information about the surface properties. The instrument is designed to measure linear and circular polarization changes over the visible and near-infrared spectral ranges. It will also have movable and fully controllable arms for goniometric studies to investigate the effect of viewing geometry. Spectro-polarimetric investigations of small bodies and planetary surfaces analogues are of interest for the compositional characterization of planetary objects, with an emphasis on asteroids, comets and icy moons.
13092-221
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Martian Moons eXplorer (MMX) is a sample-return mission of Phobos, the larger moon of Mars. To achieve the mission, a high-resolution 3D model of Phobos is essential, which requires a large number of high-resolution images must be sent back to Earth with enough quality before carrying out the landing activity.
To realize this, the data transfer bandwidth is the bottleneck, and we adopt CCSDS 122.0-B-1 image compression, a variation of data compression based on the DWT method.
With this method, we can select only one output quality for one image compression. On the other hand, the data transfer strategy shall be to transfer minimum-quality images first for quick looks and full-quality ones later. To realize this with the least computing power, we modified the method to output a low-quality full image and two supplemental data sets to better quality. This work is based on the CCSDS 122.0-B-1 implementation by a group of the University of Nebraska–Lincoln, available at http://hyperspectral.unl.edu/.
13092-222
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
JANUS is a multi-filter optical camera part of the JUICE ESA Mission, that has been launched last April from the French Guiana towards the Giovian system, where it will arrive in 2031. During the design phase of the instrument an extensive Straylight Analysys has been carried on, but after AIV the need to update the analysis on the base of the 'as built' system has become desiderable, to better interpretate the calibration data and prepare for science phase.
We here report about this update, covering the rationale of the update, the used methodology and the obtained results.
13092-223
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
In this paper we provide a detailed description of a bifocal panoramic lens (BPL), which allows recording a 360°x100° field and, simultaneously, a 20° circular field at a higher resolution. The BPL optical design has been specifically optimized for space environment operations. Furthermore, we describe the results of the tolerance and ghost analyses conducted on the camera, highlighting the challenges arising when dealing with such a wide-field objective due to entrance pupil aberrations and distortions.
13092-225
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Comet Interceptor mission aims to enhance our understanding of comets and the formation of the Solar System by exploring and encountering a Dynamically New Comet or an Interstellar Object.
EnVisS (Entire Visible Sky) is an all-sky camera aboard the mission designed to study the radiance and polarization properties of the comet coma in the visible spectrum.
The Institute for Photonics and Nanotechnologies (CNR-IFN) and Leonardo SpA are responsible for designing the filter package for EnVisS, which consists of three strips, glued side by side: a central high transmission broadband filter, and two linear polarization filters.
In the CNR-IFN laboratories different types of polarizers have been tested to establish which one has the most fitting properties for EnVisS’s purposes. For each type of polarizer, the transmissivity and reflectivity have been measured and compared with the other filters’ ones and with the characteristics provided by the manufacturer.
The Moxtek UBB01A polarizer has been identified as the best candidate for EnVisS due to its optimal performance and fused silica substrate.
13092-226
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The work will describe the activities performed to realize a laboratory set-up to test a prototype of the EnVisS fish-eye camera.
EnVisS is an all-sky camera specifically designed for Comet Interceptor, an ESA Fast mission foreseen to launch in 2029 to study a dynamically new comet.
At the CNR-IFN premises in Padova-Italy, the ad-hoc laboratory test bench has been devised and set-up.
In this paper, the requirements for the set-up and the solutions adopted for its realization will be presented together with an overview of the results obtained during its commissioning.
13092-227
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Dragonfly Geophysics and Meteorology (DraGMet) instrument on NASA’s Dragonfly mission to the Saturnian moon Titan includes a novel methane humidity sensor. This sensor will be used to collect in-situ data at multiple landing sites and during powered flights of the rotorcraft to contribute to our understanding of Titan’s methane hydrologic cycle, which is a primary science objective for the Dragonfly mission. This paper discusses the technical development and laboratory testing of the DraGMet methane sensor.
13092-228
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
In this article, a new model is developed to simulate images of small impacts on an asteroid's surface from cameras onboard probes. Observing the ejecta dust following the impact enables the examination of the body’s physical characteristics. The model’s potential is demonstrated by a comparison with actual photographs of the Hayabusa2 impact and the simulated ones in terms of dust position and magnitude. To achieve the object, the model implements the characteristics of the camera used in the Hayabusa2 mission from the same location as the real camera in the impact instant. The results show a very good match between the real and simulated images, proving that the model can be useful for testing the performance of present and future cameras for ejecta dust observation.
13092-229
20 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The COronal Diagnostic EXperiment (CODEX) is a two-stage externally occulted solar coronagraph that will observe the linearly polarized K-corona within the wavelength range 380-440nm from the International Space Station (ISS). A two fold mirror system is used for achieving a compact design. To measure the coronal light, CODEX is equipped with a polarization image sensor manufactured by Sony, the IMX253MZR, that spatially modulates the incoming light. It is crucial to understand how the instrument modifies the incoming polarized light, to derive with an acceptable level of uncertainty the desired physical quantities of the solar corona from observations. We describe the polarimetric characterization of the CODEX coronagraph, providing an estimate of the instrumental polarization, and a description of the obtained results.
Program Committee
Lab. d'Etudes Spatiales et d'Instrumentation en Astrophysique (France)
Program Committee
Inter-Univ. Ctr. for Astronomy and Astrophysics (India)
Additional Information
View call for papers
What you will need to submit
- Presentation title
- Author(s) information
- Speaker biography (1000-character max including spaces)
- Abstract for technical review (200-300 words; text only)
- Summary of abstract for display in the program (50-150 words; text only)
- Keywords used in search for your paper (optional)
- Check the individual conference call for papers for additional requirements (i.e. extended abstract PDF upload for review or instructions for award competitions)
Related Courses
Courses at Astronomical Telescopes + Instrumentation
-
See courses on topics related to Space Telescopes and Instrumentation 2024: Optical, Infrared, and Millimeter Wave.
-
Pre-registration is required for SPIE Courses.