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Conference 13103
X-Ray, Optical, and Infrared Detectors for Astronomy XI
16 - 19 June 2024 | Room G213, North - 2F
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Session 1:
Infrared Detectors I
16 June 2024 • 08:30 - 12:00 Japan Standard Time | Room G213, North - 2F
Session Chair:
Andrew D. Holland, Ctr. for Electronic Imaging (United Kingdom)
13103-1
16 June 2024 • 08:30 - 09:00 Japan Standard Time | Room G213, North - 2F
Show Abstract +
Teledyne Digital Imaging is a leading supplier of high performance visible and infrared focal plane arrays (FPAs) to the scientific community. Teledyne e2v Space Imaging (Chelmsford, UK) supplies visible CCD and CMOS FPAs and Teledyne Imaging Sensors (Camarillo, California) supplies hybrid CMOS infrared FPAs.
This paper will review visible and infrared FPA technologies and the major products used by the scientific community. We then present several of the most recent astronomy facilities and missions served by Teledyne’s FPAs. These include JWST, Euclid Dark Universe mission, Roman Space Telescope, SPHEREx, NEO Surveyor, OSIRIS-REx and ARIEL space missions and the Vera Rubin and ESO ELT ground-based observatories.
13103-2
16 June 2024 • 09:00 - 09:20 Japan Standard Time | Room G213, North - 2F
Show Abstract +
ESA’s Science Payload Validation laboratory is characterising Leonardo’s IBEX detector.
IBEX is new 2kx2k pixels MCT-hybridised detector that relies on avalanche photo-diode to provide effective sub-electron readout noise capabilities and low enough dark current compatible with long integration duration typical of photon-starved astronomy applications.
In this contribution, we provide first an overview of the packaging solution and test setups including our custom readout chain and prototype controller. We then report on functional and performance test results for a bare-ROIC as well as early dark current performance for the hybridised arrays.
13103-3
16 June 2024 • 09:20 - 09:40 Japan Standard Time | Room G213, North - 2F
Show Abstract +
The new imaging system, SIRIS (Short InfraRed Imaging System) is designed around an hybrid CMOS_InGaAs FPA from NIT (New Imaging Technologies). This detector was originally intended for industrial applications, however through innovative controls and new readout methods, it became fully exploitable in scientific applications. The SIRIS camera, manufactured by LYTID, is aimed at cutting-edge applications, like astronomy ones, that can take advantage of all of its improved characteristics to gain in signal to noise ratio, resolution and optimization of acquisition times. SIRIS has been able to confront the observation conditions and take advantage of the high requirements on the astronomical measurement signal, mounted on the Pic du Midi T1m telescope, to improve all its characteristics. This system, with its specific SWIR sensor, will be presented, illustrated through all its recent results.
13103-4
16 June 2024 • 09:40 - 10:00 Japan Standard Time | Room G213, North - 2F
Show Abstract +
Wide-field imaging with large-format detectors is crucial for astronomical surveys, particularly in the time-domain era. While CCD and CMOS detectors have been extensively utilized in optical surveys, there is a scarcity of surveys conducted in the infrared bands due to the expensive nature of HgCdTe detectors. However, the InGaAs camera offers a cost-effective alternative for near-infrared imaging. This paper presents the preliminary testing results of a new 1280 × 1024 infrared camera, providing an overview of its performance. Laboratory tests were conducted to determine dark current, readout noise, non-linearity, bias stability, and other parameters. The camera was also mounted on a small telescope for astronomical observations. The potential application of this camera in future time-domain surveys is discussed.
Coffee Break 10:00 - 10:20
13103-5
16 June 2024 • 10:20 - 10:40 Japan Standard Time | Room G213, North - 2F
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We demonstrate a 64-pixel single-photon imager based on superconducting nanowire single photon detectors (SNSPDs) capable of counting single photons up to a wavelength of 10 microns. This technology could be useful in future space telescopes in applications such as exoplanet transit spectroscopy.
13103-6
16 June 2024 • 10:40 - 11:00 Japan Standard Time | Room G213, North - 2F
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The IRD2007 is a Medium Wave Infrared (MWIR) image sensor developed by Teledyne e2v UK for potential use in the International Mars Ice Mapper mission (I-MIM). Featuring a 640×512 array with 15 µm pixel pitch and a MW cutoff wavelength of 5 µm, the sensor employs Type 2 Supper Lattice (T2SL) technology. The study focuses on characterizing the sensor's quantum efficiency (QE), dark current (DC), and radiation hardness under cryogenic conditions down to 150 K. In-situ measurements were conducted before and after proton irradiation, assessing the sensor's performance while cryogenically cooled, with potential applications for space imaging and resource utilization on Mars.
13103-7
16 June 2024 • 11:00 - 11:20 Japan Standard Time | Room G213, North - 2F
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We present advances to MCT/Si Infrared detector technology, building on previously published results and expanding the scope of characterization to constrain the effects of p-n junction size on various detector performance parameters, such as dark current, read noise, quantum efficiency, persistence, linearity, full-well depth, and crosstalk probability. Results from an observing program with the best of the detectors from the SATIN detector development program are presented, and comparisons to competing technology are made in regards to application, performance, and cost. Finally, we present plans for radiation testing of the SATIN devices to evaluate their radiation hardness for deployment in a space environment.
13103-8
16 June 2024 • 11:20 - 11:40 Japan Standard Time | Room G213, North - 2F
Show Abstract +
The 1/f noise in the readout electronics of the JWST near-IR detectors affects the total noise, the amount of correlated noise, and imprints positive and negative stripes into images in the fast read direction. The relative strength of this noise is decreased with multiple samples up-the-ramp, but even in exposures with 100+ samples, the 1/f is significant. In this paper, we discuss various methods to minimize the effect of the 1/f noise. This includes both routines to remove the 1/f and changes in the readout to sample more reference pixels. We also discuss the pros and cons of the various methods.
13103-9
16 June 2024 • 11:40 - 12:00 Japan Standard Time | Room G213, North - 2F
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A review of the status of Leonardo MCT detectors aimed at the space and astronomy sector, including technology and mission updates. Subjects covered include LmAPDs for wavefront sensors, communication and low flux imaging, very long wave devices for low flux environments, progress on extending MCT into the visible band and an update on recent commercial off the shelf (COTS) devices now in orbit.
Break
Lunch Break 12:00 - 13:20
Session 2:
Cryogenic Detectors
16 June 2024 • 13:20 - 15:40 Japan Standard Time | Room G213, North - 2F
Session Chair:
Gregory Mosby, NASA Goddard Space Flight Ctr. (United States)
13103-10
16 June 2024 • 13:20 - 13:40 Japan Standard Time | Room G213, North - 2F
Show Abstract +
Using disordered superconductors, like β-Ta, TiN, Hf and PtSi, for MKIDs has the potential to improve the photon absorption efficiency, η, over a broad wavelength range. However, the resolving power, R, of these MKIDs is not higher than 20 at 1 µm, while the fundamental Fano limit is around 65. To improve R, the signal-to-noise ratio must be increased.
We measure the single photon pulse response of β-Ta MKIDs and show that the pulse duration is limited by disorder in two ways. First, the initial pulse decay is faster than exponential, which we attribute to slow quasiparticle diffusion. Second, the decay time of the pulse tail is faster due to low energetic, localized quasiparticles. Both these effects do not occur in conventional Al at the same experimental conditions.
These results imply a trade-off between η and R and shows that improving MKIDs by using disordered superconductors is not straightforward.
13103-11
16 June 2024 • 13:40 - 14:00 Japan Standard Time | Room G213, North - 2F
Show Abstract +
One of the major goals of modern astronomy is the atmospheric characterization of small exoplanets to learn about their diversity, habitability and ultimately, whether they harbor life. The Large Interferometer For Exoplanets initiative aims to perform atmospheric characterization of these planets in the mid-infrared (MIR) wavelength regime (4-18.5 micron). Extremely sensitive and highly efficient detectors are required to detect the faint signal from these small exoplanets. Kinetic Inductance Detectors (KIDs) are a promising candidate as they are able to count single photons with no readout noise or dark current. In this work we experimentally show that KIDs are able to do photon counting at 4 wavelengths between 3.8 and 24 micron. We also compare the performance of two KID designs to investigate what design would be optimal across the MIR band.
13103-12
16 June 2024 • 14:00 - 14:20 Japan Standard Time | Room G213, North - 2F
Show Abstract +
Multiple space missions currently under study require high-performing detectors at mid-infrared wavelengths from 2 to 20 µm. However, the future availability of the IBC detectors used for JWST is in doubt, and HgCdTe detectors have difficulties at longer wavelengths. Superconducting detectors are therefore being considered as a solution to fill this technology gap. Superconducting nanowire single-photon detectors (SNSPDs) are particularly advantageous, because they are true photon-counting detectors with digital-like output signals and low dark count rates. These features make them very stable for applications like exoplanet transit spectroscopy and able to operate in photon-starved environments for applications like nulling interferometry. We have recently demonstrated SNSPDs with high internal detection efficiency at wavelengths as long as 29 µm. This talk will provide an overview of the current state of mid-IR SNSPDs and lay out the future steps needed to adapt them for exoplanet science missions.
13103-13
16 June 2024 • 14:20 - 14:40 Japan Standard Time | Room G213, North - 2F
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Here, we introduce the kinetic inductance current sensor (KICS), a novel readout technology based on the nonlinear current dependence of the kinetic inductance in a superconductor. The KICS takes the form of a superconducting resonator with small cross-section inductor, and current input from a TES or similar device causes shifts in the resonant frequency, enabling a sensitive measurement of the TES current. Additionally, the KICS makes use of a superconducting switch, which is used to trap a persistent current in the resonator, reducing noise and bias line pickup and enabling nearly arbitrary frequency tunability. We demonstrate the KICS through the readout of a TES optimized for 1550 nm photon detection, where we measure a resolving power, R, above 5, already matching the performance of a conventional SQUID readout of the same device.
13103-14
16 June 2024 • 14:40 - 15:00 Japan Standard Time | Room G213, North - 2F
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Superconducting detectors have fundamental advantages over conventional optical sensors in terms of noise, sensitivity, energy and time resolution, and radiation tolerance. In this paper, we consider the three most relevant superconducting detector technologies towards the Habitable Worlds Observatory: transition edge sensors (TESs), microwave kinetic inductance detectors (MKIDs), and superconducting nanowire single photon detectors (SNSPDs). We present a reference table providing a quantitative comparison of the three technologies, to help facilitate future trade studies. We also consider instrumental concerns such as low-vibration cryogenics and low-power readout electronics.
13103-15
16 June 2024 • 15:00 - 15:20 Japan Standard Time | Room G213, North - 2F
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The new generation of X-ray and gamma-ray detectors employ cryogenic detectors known as transition-edge sensors (TES) due to their high energy resolution and photon detection rates. These detectors require a refrigeration module that can operate at the transition temperature of the TES’s superconducting film—usually at mK temperatures. DR-TES consists of a novel mini-dilution refrigerator (DR) from Chase Research Cryogenics that can be used in balloon-borne missions to cool detectors to temperatures between 10-100 mK. To test the viability of this DR module, we will be cooling down a SLEDGEHAMMER detector fabricated by the National Institute of Standards and Technology quantum sensor group. The SLEDGEHAMMER microcalorimeter uses TESs coupled to superconducting quantum interference devices which are in turn coupled to microwave resonators to detect X-rays and gamma-rays. We plan to fly the SLEDGEHAMMER detector cooled by the mini-DR on a stratospheric balloon flight in August of 2024 at Fort Sumner, NM. As a follow-up mission, 511-CAM will use a modified version of the detector to map the 511 keV emission from the galactic center region.
13103-16
16 June 2024 • 15:20 - 15:40 Japan Standard Time | Room G213, North - 2F
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The Habitable Worlds Observatory’s (HWO) search for life on exoplanets via direct imaging is fundamentally photon starved. We report on our detector development using superconducting transition-edge sensors (TESs) to achieve the HWO science detector needs: rad-hard, ultra-high QE, energy-resolving, noiseless single photon detector arrays providing increased throughput in both finding and spectrally characterizing exoplanets. Our TES arrays are being developed to operate in the UV, visible, and NIR to provide spectral characterization across a broad bandpass of biosignatures. With the improved capabilities over other detector implementations, spectra of each field point are taken all of the time without penalty, thereby increasing the exoplanet characterization yield and increasing the probability of finding, recognizing, and quantifying life. We also discuss development of ultra-low vibrational cooling to accommodate TES arrays with the low mechanical disturbance required for high contrast imaging.
Break
Coffee Break 15:40 - 16:10
Session 3:
X-Ray Imaging
16 June 2024 • 16:10 - 17:30 Japan Standard Time | Room G213, North - 2F
Session Chair:
Konstantin D. Stefanov, The Open Univ. (United Kingdom)
13103-17
16 June 2024 • 16:10 - 16:30 Japan Standard Time | Room G213, North - 2F
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The sounding rocket experiment FOXSI-4 will conduct the world's first focusing imaging spectroscopic observation of a solar flare in X-rays. It aims to investigate the release of magnetic energy and the conversion mechanism from magnetic to other energies caused by magnetic reconnection in solar flares. The mission will acquire X-ray data with high dynamic range and high spatial, temporal, and energy resolution throughout the entire solar flaring region, offering valuable physical information about high-temperature and non-equilibrium plasmas. For soft X-ray observations at 0.5-10 keV, a non-dispersive type X-ray imaging-spectroscopy, that is, photon counting, will be performed using a back-illuminated CMOS sensor. This sensor has a sensitive layer of fully depleted silicon which is 25 µm thick and can achieve a high-speed continuous exposure at a rate of ~250 fps. We will report on the evaluation results of the photon counting capability and quantum efficiency of the sensor.
13103-18
16 June 2024 • 16:30 - 16:50 Japan Standard Time | Room G213, North - 2F
Show Abstract +
The Auroral X-ray Imaging Spectrometer (AXIS) instrument proposed by the Indian Space Research Organisation’s (ISRO) Space Astronomy Group plans to gather spectral information of the Earth’s aurorae in the 0.3 – 3 keV band from a polar orbit for the first time. Experimental studies of a backside-illuminated (BI) CIS221-X (a prototype CMOS image sensor (CIS) optimised for soft X-ray detection) were conducted at the BESSY II synchrotron, which provided a source of monochromatic X‑rays down to 310 eV for energy resolution measurements to be made. The FWHM at 500 eV was found to be 54 eV, well within the AXIS instrument requirements. Continued studies on the CIS221-X for AXIS include the impact of warmer operating temperatures and different frame rates used. Optimisation of operating conditions has been performed prior to irradiation to later determine performance at end-of-life (EOL). The latest work on this project is presented.
13103-19
16 June 2024 • 16:50 - 17:10 Japan Standard Time | Room G213, North - 2F
Show Abstract +
Interest in X-ray interferometry (XRI) has recently been reignited by the ESA voyage 2050 programme, but large technological challenges still need to be overcome to realise such a groundbreaking telescope. Due to the potentially large time scales for optical and pointing accuracy technology developments, there is scope to develop new detector technologies to meet the strict requirements of XRI. For the proposed ESA THESEUS X-ray astronomy mission, a bespoke CMOS image sensor (CIS) named CIS221-X has been developed which boasts near Fano-limited energy resolution of 130 eV (@5.8 keV) at -40°C. This paper explores future plans for developing the CIS221-X to meet the requirements of XRI.
13103-20
16 June 2024 • 17:10 - 17:30 Japan Standard Time | Room G213, North - 2F
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We are developing monolithic active pixel sensors, X-ray SOIPIXs based on a Silicon-On-Insulator CMOS technology. Its event trigger output function offers a high time resolution better than ~10 usec. (1) In 2022-23, we and evaluated large sensors, XRPIX-X, with a pixel array size of 14mm x 22mm. We report its design and the results of the performance evaluation. (2) We are developing "Digital X-ray SOIPIXs" for satellite use, featuring on-chip ADCs, DACs, and BGRs for noise robustness. An on-chip clock pattern generator is also included to simplify the readout digital circuits. (3) XRPIXs are increasingly being utilized in various scientific applications beyond X-ray astronomy, and a brief introduction will be provided.
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 - 10:30
Session 4:
Infrared Detectors II
17 June 2024 • 10:30 - 12:20 Japan Standard Time | Room G213, North - 2F
Session Chair:
Kyriaki Minoglou, European Space Agency (Netherlands)
13103-21
17 June 2024 • 10:30 - 11:00 Japan Standard Time | Room G213, North - 2F
Show Abstract +
Detectors are a performance limiting component for space instrumentation – the better the detector, the better the instrument performance. Consequently, the European Space Agency (ESA) invests significant resources into the development of high-performance detector solutions for current and future missions. While visible and infrared wavebands are of particular interest, technology developments are by no means limited to these areas. This paper presents a detailed overview of the detector development activities currently being undertaken by ESA in collaboration with European industrial partners.
13103-22
17 June 2024 • 11:00 - 11:20 Japan Standard Time | Room G213, North - 2F
Show Abstract +
The Cassiopée project aims to develop the key technologies that will be used to deploy very high-performance Adaptive Optics for future ELTs. The ultimate challenge is to detect earth-like planets and characterize the composition of their atmosphere. For this, imaging contrasts of the order of 10^9 are required, implying a leap forward in adaptive optics performance, with high density deformable mirrors (120x120 actuators), low-noise cameras and the control of the loop at few kHz. The project brings together 2 industrial partners: First Light Imaging and ALPAO, and 2 academic partners: ONERA and LAM, who will work together to develop a new camera for WFSensing, a new deformable mirror and their implementation in an AO loop. This paper will present the development of the fast large infrared e-APD camera which will be used as tha wavefront sensor of the system.. The camera will integrate the latest 512x512 Leonardo e-APD array and will benefit from the heritage of the first-light imaging's C-RED One camera. The most important challenges for the application are the autonomous operation, compacness, speed and latency.
13103-23
17 June 2024 • 11:20 - 11:40 Japan Standard Time | Room G213, North - 2F
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Ability to detect individual photons in the mid-ir is crucial for many astronomical applications and detector technology is the vital part of instrumentation for future space missions. The search for bio signatures through transiting exoplanet spectroscopy requires an array of detectors covering the spectral range of 2.8 to 20 μm [1].
Superconducting nanowire single-photon detectors (SNSPDs) are highly efficient and low-noise devices ideal for counting and observing low levels of photons. They have near-perfect quantum efficiency and can be combined into arrays for imaging. Here, we report on the development of 36-pixel mid-infrared SNSPD arrays. Detectors are based on optimised ultrathin NbN films, which are grown by both magnetron sputtering and atomic layer deposition (ALD) techniques. For characterisation we assembled a setup based on tuneable optical parametric oscillator (OPO) source to provide picosecond long pulses in the 1.5 – 10 μm spectral region. This work provides an analysis of the electrical, optical, and temporal performance of individual pixels as well as information on pixel performance uniformity across the array.
[1] M. Meixner et al., arXiv:1912.06213 (2019).
13103-24
17 June 2024 • 11:40 - 12:00 Japan Standard Time | Room G213, North - 2F
Show Abstract +
MICADO, a Multi-AO Imaging Camera for Deep Observations, is a first light imager for the European Large Telescope (ELT). It is being designed and built by a consortium of partners from 6 different countries across Europe and led by the Max Planck Institute for Extraterrestrial Physics (MPE) in Garching. The European Southern Observatory (ESO) is responsible for delivering the near infrared detector subsystem to the instrument. This subsystem includes nine Hawaii-4RG-15 (H4RG-15) near infrared detectors (2.5um cut-off) mounted in a compact 3x3 mosaic at the heart of the instrument, operating nominally at 82K. This paper presents an overview of this detector subsystem, including the measured performance of some of the H4RG science detectors already characterised in a custom built test facility at ESO. Special readout modes have been developed for the instrument and also for AO corrections to one of the ELT mirrors and these will be described. The design of the focal plane, its thermal analysis and the focal plane flatness measurement system being setup at ESO will also be presented.
13103-25
17 June 2024 • 12:00 - 12:20 Japan Standard Time | Room G213, North - 2F
Show Abstract +
We present progress towards developing a science-grade, megapixel format linear-mode avalanche photodiode array for low background shortwave (1 - 2.4 um) infrared astronomy. Our latest results show outstanding performance, with dark current <1e-4 electrons/pixel/second and read noise reducing by 30% per volt of bias, reaching less than 1e-/pixel/frame in correlated double-sampling, and able to average down to ~0.3 e-/pixel/frame when using multiple non-destructive reads. We present some on-sky data as well as comment on prospects for photon counting and photon number resolution.
Break
Lunch Break 12:20 - 13:20
Session 5:
CCDs and Single Photon Detectors I
17 June 2024 • 13:30 - 15:30 Japan Standard Time | Room G213, North - 2F
Session Chair:
Roger Smith, Caltech (United States)
13103-26
17 June 2024 • 13:30 - 13:50 Japan Standard Time | Room G213, North - 2F
Show Abstract +
The Soft X-ray Imager (SXI) on SMILE uses two Te2v CCD370s and will be constantly damaged in flight by radiation. This gradually degrades the focal plane device’s performance throughout the mission.
A proton irradiation campaign has been carried out that aimed to understand how the damage impacts soft X-ray detection between 700 eV - 6 keV, which overlaps with the 200 eV – 2 keV science band for the SXI. This has been achieved by measuring the X-ray charge transfer inefficiency using several X-ray fluorescence targets combined with a standard X-ray tube across -130 to -85 °C. Additional trap pumping measurements help understand the underlying mechanisms that affect the charge transfer. The CCD is run in full frame mode and frame transfer with 6x6 binning and demonstrates how utilizing binning enables small signals to remain detectable throughout a 3-year mission.
This paper summarises the results of the device characterisation at beginning and end of life, the impact of charge injection and related requirements on mission operations and outlines the resulting end of life optimised performance.
13103-28
17 June 2024 • 13:50 - 14:10 Japan Standard Time | Room G213, North - 2F
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We present results from characterizing and optimizing an ultra-low noise Skipper CCD focal plane prototype for the SOAR Integral Field Spectrograph (SIFS). We outline an observation strategy that allows to maximize the signal-to-noise by implementing the Skipper CCD’s region of interest capability that allows to readout a selected region of the detector with tunable readout noise. Finally, we will present the first astronomical spectral data results from the Skipper CCD instrument at SOAR and demonstrate the scientific improvements made possible by ultra-low noise detectors.
13103-29
17 June 2024 • 14:10 - 14:30 Japan Standard Time | Room G213, North - 2F
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Skipper CCDs are a mature detector technology that has been suggested for future space telescope instruments requiring sub-electron readout noise, owing to their ability to repeatedly and nondestructively sample the charge in each detector pixel. However, the effect of high doses of ionizing radiation on skipper CCDs (such as those expected in deep space) remains largely unknown. We report preliminary results on the performance of p-channel skipper CCDs (expected to be radiation-hard) following irradiation with 217-MeV protons at the Northwestern Medicine Proton Center. The total nonionizing energy loss (NIEL) experienced by the detectors exceeds 10 years at the Earth-Sun L2 point. Owing to the low readout noise of these detectors, we are able to sensitively characterize the charge transfer inefficiency, dark current, and the density and time constants of charge traps as a function of proton fluence. We conclude with a brief outlook toward future tests of these detectors at other proton and gamma-ray facilities.
13103-30
17 June 2024 • 14:30 - 14:50 Japan Standard Time | Room G213, North - 2F
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Light emission from Skipper Charge-Coupled Devices (CCDs) readout amplifiers has been identified as a potential background source for future ground and space astronomical observations. In this work we study near infrared photon emissions from p-channel Skipper-CCD’s readout amplifiers, comparing different transistor designs and fabrication parameters, to provide recommendations on how future sensors should be built to minimize light emission. We examined a custom sensor, designed at LBNL and manufactured by Teledyne/DALSA, specifically to minimize light emission, alongside sensors from new foundries. We will present the results of the performance of these new CCD’s, along with the characterization of the readout amplifiers to determine which design optimizes light emission without compromising detector noise. Results were also validated via MonteCarlo simulations.
13103-31
17 June 2024 • 14:50 - 15:10 Japan Standard Time | Room G213, North - 2F
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Skipper-CCDs, with their electron-counting capability and low instrumental background, are highly sensitive to faint signals, which is of great interest for certain astronomical applications. Characterizing the instrumental sources of few-e- events in skipper-CCDs is crucial for estimating their scientific reach. In this work I will report on the performance of fully-depleted, p-channel skipper-CCDs, that were fabricated on 8-inch wafers in two new foundries during the R&D of Oscura, a 26 GPix skipper-CCD array designed to search for light dark matter-electron interactions. Results, performed at FNAL, demonstrate a high yield of sensors achieving sub-electron readout noise. Main instrumental sources of few-e- events were identified and characterized, including thermal dark current, spurious charge and charge traps.
13103-27
17 June 2024 • 15:10 - 15:30 Japan Standard Time | Room G213, North - 2F
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The 4-metre Multi-Object Spectrograph Telescope (4MOST), a second-generation instrument for the European Southern Observatory’ Visible and Infrared Survey Telescope for Astronomy (ESO VISTA) in Chile, enables extensive spectroscopic surveys of the night sky. Using over 2400 optical fibers, it captures light from celestial targets, feeding it to three spectrographs with CCD 231-C6 detectors, totaling nine science detectors operated by individual NGCs. During testing, an unexplained image structure of diagonal lines with central-to-edge pathways emerged, resistant to calibration. In this work, we describe, evaluate, and present a removal technique for the unidentified image structure observed in all science detectors of the 4MOST instrument.
Break
Coffee Break 15:30 - 16:00
Session 6:
X-Ray I
17 June 2024 • 16:00 - 17:40 Japan Standard Time | Room G213, North - 2F
Session Chair:
Chiaki Crews, The Open Univ. (United Kingdom)
13103-32
17 June 2024 • 16:00 - 16:20 Japan Standard Time | Room G213, North - 2F
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The MCRC-V1.0 ASIC provides 8 channels of high-speed and low-noise readout electronics with comparable performance to our best discrete implementation but with ten times less power consumption at a fraction of the footprint area. In addition, the chip demonstrates a radiation hardness equal or greater to 25 krad. The next iteration (MCRC-V1.5) will expand the channel count and extend the interfaces to external circuits. This paper will summarize our recent characterization efforts, including the TID radiation campaign and results from the first operation of the MCRC ASIC in combination with a representative MIT-LL CCD.
13103-33
17 June 2024 • 16:20 - 16:40 Japan Standard Time | Room G213, North - 2F
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Future mega-pixel imaging X-ray detectors will require excellent spectral response at soft (E < 1 KeV) X-ray energies while operating at fast frame-rates. We have characterized the sub-keV spectral resolution of several low-noise MIT Lincoln Laboratory CCDs in detail. These devices differ in pixel size, gate structure and output stage design. We report measurements of the shape of the spectral redistribution function as a function of energy for each of these sensor types and compare our measurements with device simulations. We also assess the implications of the observed response functions for scientific performance in deep X-ray imaging and high-resolution spectroscopy applications.
13103-34
17 June 2024 • 16:40 - 17:00 Japan Standard Time | Room G213, North - 2F
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Imaging and spectroscopic performances of CCD+CMOS hybrid sensor are reported. The sensor incorporates the benefits of the two sensors; Back-side illuminated CCD has high quantum efficiency and high-speed column-parallel ADCs are realized using CMOS technique. Test chips with 128(V) x 1024(H) pixels are irradiated with monochromatic X-rays from 109Cd. X-ray events are successfully detected and the energy resolution of Ag Ka is derived to be 1.43 keV (FWHM) in room temperature. Performance variations as a function of temperature, frame rate, readout mode, etc. are going to be reported.
13103-35
17 June 2024 • 17:00 - 17:20 Japan Standard Time | Room G213, North - 2F
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Future X-ray missions of all sizes will demand higher readout rates than current CCDs can handle due to the increased effective area of these missions and the resulting increased significance of pile-up issues. Silicon hybrid CMOS X-ray detectors, or HCDs, have significant advantages over CCDs for use on next-generation X-ray missions due to their fast and flexible readout abilities, inherent radiation hardness, and low power requirements. The Penn State High Energy Astrophysics Detector and Instrumentation Lab, in collaboration with Teledyne Imaging Sensors, is leading the effort to design and develop next-generation X-ray HCDs. We discuss the results of this development effort and present the current testing results of next-generation X-ray HCDs that are suitable for high-throughput and high-angular-resolution X-ray missions of the future.
13103-36
17 June 2024 • 17:20 - 17:40 Japan Standard Time | Room G213, North - 2F
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Current-generation solar observatories utilize CCD image sensors to observe the sun in the soft X-ray (SXR) and extreme ultraviolet (EUV) regimes. Observations of large solar flares in the SXR and EUV spectra are hindered by pixel saturation and charge blooming in CCD image sensors. The Swift Solar Activity X-ray Imager (SSAXI) program is developing CMOS image sensors with low noise and high-speed (>5 Hz) readout for next-generation solar observatories that will enable the observation of large solar flares while minimizing the effects of pixel saturation and charge blooming. To demonstrate the CMOS technology in a space environment, SSAXI-Rocket will be operating a CMOS camera as a sub-payload on board the High-Resolution Coronal Imager (Hi-C) sounding rocket as part of NASA’s 2024 solar flare sounding rocket campaign. We describe the pre-launch laboratory tests performed with the SSAXI-Rocket CMOS image sensor to characterize its linearity, spectral resolution, and quantum efficiency.
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 - 10:30
Session 7:
CMOS Image Sensors
18 June 2024 • 10:30 - 11:00 Japan Standard Time | Room G213, North - 2F
Session Chair:
Kyriaki Minoglou, European Space Agency (Netherlands)
13103-37
Innovations in imaging technology at Teledyne e2v to support future visible, NIR, UV & X-ray applications
(Invited Paper)
18 June 2024 • 10:30 - 11:00 Japan Standard Time | Room G213, North - 2F
Show Abstract +
Teledyne e2v is continuing to invest in CCD and CMOS sensors innovation for ground and space-based astronomy applications. The new upgraded 8 inch process is enabling back-thinning of wafer-scale large area detectors such as the CMOS CIS300 product family. New world class broadband anti-reflecting coatings using novel technology enable high stable QE performance at VUV and UV wavelengths. Teledyne-e2v has also developed a solution to increase drastically QE in near-infrared without losing on MTF nor centroiding.
The presentation will cover large CCD and CMOS developments and measurements including electro-optical performances, QE from ultraviolet to near-infrared and results obtained at cryogenic temperature.
Session 8:
CMOS I
18 June 2024 • 11:00 - 12:20 Japan Standard Time | Room G213, North - 2F
Session Chair:
Michael E. Hoenk, Jet Propulsion Lab. (United States)
13103-38
18 June 2024 • 11:00 - 11:20 Japan Standard Time | Room G213, North - 2F
Show Abstract +
We are realizing a novel hybrid imaging/timing detector consisting of a photocathode, a microchannel-plate and a TimePix3ASIC, originally developed at CERN for particle physics experiments, to detect photons in the 350-700 nm wavelength range with high time resolution, high quantum efficiency and good spatial resolution. A feature of this hybrid detector is the time-tagging of each of the photons coming from the sources in the Field of View under investigation with a resolution better than 20 ns. Due to these special characteristics, this detector can be extremely useful for time-domain astronomy. The testing and data taking are conducted primarily at the OARPAF observatory (80 cm primary mirror) with the aim to apply this technology for the first time in the astronomical field and obtain all the information needed to develop at a later stage an instrument based on this technology for the Telescopio Nazionale Galileo.
13103-39
18 June 2024 • 11:20 - 11:40 Japan Standard Time | Room G213, North - 2F
Show Abstract +
This paper discusses the further development of JPL’s n-type superlattice doping (2D doping) process for sensitivity and stability enhancement of CMOS image sensors with PMOS pixels. We discuss the results of the n-type 2D-doping of SRI’s backside illuminated PMOS 4k x 4k and 8k x 8k imagers. We briefly describe the backside processing parameters for the optimization of the 2D-doping process and antireflection coating design. Performance characterization, including quantum efficiency (QE), dark signal, and modulation transfer function (MTF) as a function of epi type and operating temperature will be discussed. These will be compared with the performance of devices produced using SRI’s standard BSI processes.
13103-40
18 June 2024 • 11:40 - 12:00 Japan Standard Time | Room G213, North - 2F
Show Abstract +
Modern scientific complementary metal-oxide semiconductor (sCMOS) detectors provide a competitive alternative to charge-coupled devices (CCDs). They boast comparable performances with faster frame rates, lower read noise, higher dynamic range and have lower production costs such that industry favours sCMOS production. We characterized several commercially available sCMOS detectors to gauge the state of this technology for use in optical astronomy. This included large-pixel detectors (e.g. Teledyne Prime 95B, Andor Sona-11) comparable to traditional CCDs, along with one quantitative sCMOS detector, the Hamamatsu Orca-Quest C15550-20UP, which has photon-resolving capability. We found low levels of dark current, read noise, faulty pixels, and fixed pattern noise, as well as >98% linearity across all detectors. The Quest, in particular, had a dark current of 0.008 +/- 0.034 e-/s/px (-20C) and a read noise of 0.37 +/- 0.10 e- (in standard scan). We also tested this detector on-sky to evaluate its photometric accuracy. Our tests demonstrated that sCMOS detectors perform superior to CCDs in optical imaging and provide more readily available alternatives for upcoming optical instruments.
13103-41
18 June 2024 • 12:00 - 12:20 Japan Standard Time | Room G213, North - 2F
Show Abstract +
Space radiation causes spurious signals and effects that degrade single-photon sensing detectors performance. We present the development of single-photon sensing and photon number resolving CMOS image sensors. The results reported in this paper build upon a precursor program that exposed the sensor up to 50 krad(Si) of radiation. We present the performance of multiple single-photon sensing CMOS devices from a variety manufactures and present plans for a radiation test program to evaluate the detector performance of the devices in a Jovian-like environment and during heavy ion irradiation.
Break
Lunch/Exhibition Break 12:20 - 13:30
Session 9:
CMOS II
18 June 2024 • 13:30 - 14:50 Japan Standard Time | Room G213, North - 2F
13103-42
18 June 2024 • 13:30 - 13:50 Japan Standard Time | Room G213, North - 2F
Show Abstract +
This paper presents an investigation of a mechanism of dark current generation under the transfer gate in pinned photodiode image sensors. It was discovered that the dark current strongly depends on the interplay between the timing and the biasing of the transfer gate and the sense node during reset. Several methods for the reduction of this dark current are proposed and evaluated. The results could help to find the optimal operating conditions of PPD image sensors used in applications where the dark current performance is important.
13103-43
18 June 2024 • 13:50 - 14:10 Japan Standard Time | Room G213, North - 2F
Show Abstract +
CMOS image sensors offer flexibility in readout operation as pixels can be addressed independently. Interleaved row readout can extend the dynamic range (DR) of image sensors by performing additional row readout and resets in a region that would otherwise be saturated, whilst maintaining the noise characteristics of a single readout and reset in the rest of the array. We demonstrate this on two CMOS image sensors from Teledyne-e2v: a DR increase of 34 dB is achieved with a CIS115 and 54 dB with a CIS120. With this approach peak signal-to-noise ratio is also increased whilst the linearity characteristics of the sensor are preserved. We also discuss applications of interleaved row readout, such as multi-cadence photometry.
13103-44
18 June 2024 • 14:10 - 14:30 Japan Standard Time | Room G213, North - 2F
Show Abstract +
The Astro2020 decadal survey envisions a Habitable Worlds Observatory (HWO) for revolutionary advances in exoplanet science, general astrophysics and time domain astronomy in the UV/visible/near IR spectral range. In a project funded by NASA’s Strategic Astrophysics Technology Program, JPL is partnering with industry and academia to fabricate, characterize, and mature CMOS image sensors using nanoscale surface engineering to address technology gaps identified for HWO science. Initial fabrication of delta-doped detectors has been completed, and performance and environmental tests are underway at JPL and Caltech. Columbia University and JPL are developing a CMOS camera for on-sky observations with an integral field spectrograph at MDM Observatory. The University of Colorado is developing engineering designs for incorporating a delta-doped CMOS image sensor in sounding rocket and cubesat payloads. We will present the latest results of our work in support of NASA’s goals for HWO.
13103-45
18 June 2024 • 14:30 - 14:50 Japan Standard Time | Room G213, North - 2F
Show Abstract +
Photon counting detectors have made large strides in recent years. Quanta image sensor (QIS), the electron-multiplying charge-coupled device (EMCCD), and single photon avalanche diode (SPAD) are three leading single photon counting silicon technologies. An example of each device has been fully characterized and evaluated. Their performance and value add have been determined for future space flight missions.
Session 10:
Camera
18 June 2024 • 14:50 - 15:50 Japan Standard Time | Room G213, North - 2F
Session Chair:
Michael E. Hoenk, Jet Propulsion Lab. (United States)
13103-46
18 June 2024 • 14:50 - 15:10 Japan Standard Time | Room G213, North - 2F
Show Abstract +
The Wide Field Survey Telescope (WFST) is a dedicated photometric surveying facility equipped with a 2.5-meter diameter primary mirror, an active optics system, and a mosaic CCD camera with 0.765 gigapixels on the primary focal plane for high quality image capture over a 6.5-square-degree field of view. The mosaic CCD camera is the key device for high precision photometric and high frequency observation and the ‘eye’ of the telescope for deep survey with wide field. The focal plane consists of three kinds of CCD including scientific imaging sensors, wavefront sensors and guiding sensors. In the scientific imaging area, there are 9 back-illuminated full frame scientific CCDs –CCD290-99 from E2V company with pixels of 9K by 9K and pixel size of 10um, which is mosaicked by 3 by 3 with flatness of 20μm PV. The R&D of the camera including the high precision large-scale mosaicking of detectors, detectors’ cryocooling and vacuum sealing, readout and driving with low noise and low power, data acquisition, imaging control, data storage and distribution. In this report, we will present the key technoloy of the primary camera and its development process and give our test results.
13103-47
18 June 2024 • 15:10 - 15:30 Japan Standard Time | Room G213, North - 2F
Show Abstract +
We describe the optimization of the operation of 201 CCD sensors installed for the LSST Camera, which is under construction for installation at the Vera C. Rubin Observatory. The sensors are E2V CCD250 and ITL STA3800 deep-depletion, back-illuminated devices. We conducted electro-optical testing to characterize and optimize the performance of the sensors. We describe performance issues that were found during the testing and mitigations via optimization of operation voltages and clocking.
13103-48
18 June 2024 • 15:30 - 15:50 Japan Standard Time | Room G213, North - 2F
Show Abstract +
The radiation environment at L2 yields a large number of cosmic rays that affect JWST detectors. The vast majority of these events deposit charge in only one or two pixels which the baseline JWST pipeline jump detection step correctly excludes from the rate solution. There is, however, a different population of large radiation events that affect both the near-IR and Mid-Infrared Instrument (MIRI) detectors. These large events (“snowballs” in the near-IR and “showers” in MIRI) contain faint regions with excess counts below the baseline jump detection that are not flagged. Left undetected, the residuals from these large events strongly affect deep exposures. In this paper, We describe both the characteristics of snowballs and showers, the algorithms for detecting the affected regions, and how to flag the affected pixels to prevent them from affecting the flux determination.
Break
Coffee Break 15:50 - 16:20
Session 11:
Infrared Detectors
18 June 2024 • 16:20 - 17:20 Japan Standard Time | Room G213, North - 2F
Session Chair:
Douglas Jordan, Teledyne e2v UK Ltd. (United Kingdom)
13103-49
18 June 2024 • 16:20 - 16:40 Japan Standard Time | Room G213, North - 2F
Show Abstract +
Fine Guidance Sensor tracking data obtained during JWST’s observations of the double asteroid system Didymos / Dimorphos during the impact of the NASA’s Double Asteroid Rendezvous Test (DART) spacecraft are used to evaluate FGS performance. Due to the high motion rate and the large number of observations, the DART tracking data provides an opportunity to examine pixelation effects’ impact on guider performance across a wide area of the 5 µm cutoff H2RG HgCdTe arrays employed in the guiders. For Guider 2 the magnitude of these systematic offsets in the centroid data is as expected, while for Guider 1 it was found to be more variable, likely due to the greater degree of ‘cross-hatching’ on the Guider 1 detector array, although other factors such as charge migration, inter-pixel capacitance and the brighter fatter effect are also considered.
13103-50
18 June 2024 • 16:40 - 17:00 Japan Standard Time | Room G213, North - 2F
Show Abstract +
The Subaru Prime Focus Spectrograph project incorporates 4 bench spectrographs each of which has 3 arms which employ dichroics, gratings, camers, and detectors for the blue, red, and near-IR spectral regions. The NIR arm employs 4Kx4K Teledyne H4RG-15 detectors. The project has received five of these devices, four ``science-grade'' and one ``proto-science grade'', which fails slightly to qualify as science grade. We have constructed a test cryostat with a cold illumination system to minimize thermal background. Four LED types which cover our 940-1260nm NIR band allow investigations of cosmetics, persistence, full well, QE, IPC, linearity, and noise. We report here on the basic properties measured for these devices, and some concerns.
13103-52
18 June 2024 • 17:00 - 17:20 Japan Standard Time | Room G213, North - 2F
Show Abstract +
In the past few years, CEA LETI demonstrated MCT P on N photodiodes arrays achieving high level of detection for very low flux astronomy in the short wave infrared (SWIR), with dark currents values as low as 0.003 e-/s/pixel at 100K and high quantum efficiency. Persistence was also a key element to monitor for the development of this technology, and significant improvements were demonstrated in the frame of ALFA program. From this reference technology, LETI developed a brand new P on N process, focused on decreasing defectiveness and improving low frequency stability for MWIR high operating temperature (>130K) detectors for tactical application. In this spectral range, low noise stability is characterized by Random Telegraph Signal (RTS) and noise distribution tail. In the SWIR range, persistence would be the best signature to probe this low frequency stability. Declining this new generation process for the SWIR range, we present and discuss on dark current and persistence characterization on TV format 15µm pixel pitch study array designed for SWIR low flux application.
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 - 10:30
Session 12:
CCDs and Single Photon Detectors II
19 June 2024 • 10:30 - 12:10 Japan Standard Time | Room G213, North - 2F
Session Chair:
Ralf Kohley, European Space Astronomy Ctr. (Spain)
13103-53
19 June 2024 • 10:30 - 10:50 Japan Standard Time | Room G213, North - 2F
Show Abstract +
Detectors with sub-electron noise open new possibilities for the spectroscopy of Earth-like exoplanets, probing the faintest signatures of dark energy and dark matter with high-redshift galaxies, and observing fast-evolving transients. Multi-amplifier sensing (MAS) charge-coupled devices (CCDs) offer the capability to achieve ultra-low readout noise floors together with a readout rate comparable to current CCDs employed in observatories. This is achieved by distributing a chain of Skipper floating gate amplifiers along the serial register, allowing charge to be read repeatedly, non-destructively, and independently. We show recent progress in optimizing the MAS CCD for use in astronomy. These include reducing noise to sub-electron levels with fast read times, optical characterization results, and a discussion of the range of astronomical science cases and facilities that would be enabled by MAS CCDs.
13103-54
19 June 2024 • 10:50 - 11:10 Japan Standard Time | Room G213, North - 2F
Show Abstract +
We present the first demonstration of the novel Multi-Amplifier Sensing Charge-Coupled Device (MAS-CCD). This device uses multiple non-destructive floating-gate amplifiers in series to perform multiple non-destructive charge measurements and achieve single-photon and single-electron counting with an order of magnitude reduction in readout time relative to conventional Skipper CCDs. The readout speed of the MAS-CCD scales roughly linearly with the number of amplifiers without requiring segmentation of the active area. We will show the noise performance results obtained for thick, fully-depleted silicon detectors with 8 and 16 amplifiers per readout stage together with its efficiency for light collection and particle detection. We will show recent developments for on-package and warm electronics to instrument MAS-CCD with a large number of channels (32 and 64, and scalable for a larger number) that could provide a solution for upcoming terrestrial and space astronomical instruments.
13103-55
19 June 2024 • 11:10 - 11:30 Japan Standard Time | Room G213, North - 2F
Show Abstract +
Thick fully-depleted charge-coupled devices (CCDs) with high-resistivity silicon find widespread application in various scientific domains, spanning from particle detection to astronomical imaging. Leveraging their low noise and high charge collection efficiency, these devices allow us to achieve unprecedented sensitivity to physical processes characterized by low-energy transfers. Skipper-CCDs further improve this sensitivity by performing non-disruptive measurements of the same charge package and, in turn, reducing its read-out noise to subelectron resolution. In this work, I will present advancements in the design of Skipper-CCD sensors tailored for X-ray detection in environments characterized by high optical background levels. In addition, I will discuss methods for assessing the quantum efficiency of back-illuminated skipper-CCDs for visible light using sub-kev X-rays to measure the thickness of the partial charge collection layer.
13103-56
19 June 2024 • 11:30 - 11:50 Japan Standard Time | Room G213, North - 2F
Show Abstract +
The Skipper CCD-in-CMOS image sensor integrates the non-destructive readout capability of skipper Charge Coupled Devices (CCDs) with a high conversion gain pinned photodiode on a CMOS imaging process, while taking advantage of in-pixel signal processing.
We will present the first results of the testing of the first prototype ASIC, fabricated in a commercial 180nm CMOS processes, which integrates a pixel matrix as well as individual test structures. Individual pixels in the test structures of the fabricated devices were instrumented to characterize their charge transfer capability and to study their operation in low readout noise conditions. We were able to operate the pixel in single carrier counting mode with deep sub-electron noise to measure charge packets collected by the photodiode when exposed to low illumination levels. Additionally, we will also report on the status of the custom 65nm ASICs prototypes being developed to achieve high speed, sub-electron noise readout. Work supported by the DOE Office of Science under the Microelectronics Co-Design Research Project “Hybrid Cryogenic Detector Architectures for Sensing and Edge Computing enabled by new Fabrication Processes
13103-57
19 June 2024 • 11:50 - 12:10 Japan Standard Time | Room G213, North - 2F
Show Abstract +
Single electron Sensitive Read Out (SiSeRO) is a novel technology for X-ray detectors with significantly greater responsivity and improved noise performance than traditional charge-coupled device (CCD) readout circuitry. We report progress on our continued development of this new device class, in particular, the unique repetitive non-destructive readout with SiSeROs providing single electron noise sensitivity. We also discuss the preliminary device simulation results for the next generation SiSeRO devices which are optimally designed for RNDR technique and layouts to develop a prototype SiSeRO active pixel matrix.
Break
Lunch/Exhibition Break 12:10 - 13:20
Session 13:
Test and Modeling
19 June 2024 • 13:20 - 15:20 Japan Standard Time | Room G213, North - 2F
Session Chair:
Takeshi Go Tsuru, Kyoto Univ. (Japan)
13103-58
19 June 2024 • 13:20 - 13:40 Japan Standard Time | Room G213, North - 2F
Show Abstract +
Designing a CCD pixel is a way to realize CCD functionality integration in the charge domain with a view to optimizing the critical performance parameters such as full well capacity (FWC) and charge transfer inefficiency (CTI). This paper presents a TCAD-based CCD pixel design technique by extracting design conditions and criteria to achieve CCD performance specifications. This pixel design methodology includes test structure based TCAD simulation approach. In general, this proposed methodology is applicable to all types of CCD pixel-design.
13103-59
19 June 2024 • 13:40 - 14:00 Japan Standard Time | Room G213, North - 2F
Show Abstract +
Charge Coupled Devices and Complementary Metal-Oxide Semiconductor cameras have been widely used in several optical observations. These have a high sensitivity and a wide field of view. However, it is difficult to observe a short time scale phenomenon since the time resolution stays at the most order of a millisecond. Recently, we have developed an optical observation system, Imager of MPPC-based Optical photoN counter from Yamagata (IMONY). IMONY can detect a single photon with a customized Multi-Pixel Photon Counter (MPPC) sensor composed of a monolithic Geiger-mode avalanche photodiode array. The rear stage Field Programmable Gate Array gives a timestamp, obtained with the Global Navigation Satellite System, to the detected photon. The processing clock is 10 MHz so we achieved 100 ns high time resolution. In October 2023, we mounted IMONY for a 3.8 m Seimei telescope as the performance evaluation. We observed the Crab pulsar and got good scientific results. In our talk, we will share our current status of IMONY.
13103-60
19 June 2024 • 14:00 - 14:20 Japan Standard Time | Room G213, North - 2F
Show Abstract +
We have characterised the Brighter Fatter Effect (BFE) in the Teledyne e2v CCD273 and CCD270 by mapping their response to sub-pixel sized spot illumination at a range of intensities and wavelengths. In addition, we derived photon transfer curves from uniform illumination at a range of wavelengths of these devices, and analysed the deviation from linearity of these curves. This provides a measure of the correlation between the pixels, also related to the BFE. Lastly, we directly measured the spatial extent of the BFE by characterising the redistribution of signal observed when uniform illumination is superimposed on a line pattern of injected charge.
The BFE has been simulated in a newly developed model within Pyxel, the opensource python-based framework to simulate images including instrumental effects with a focus on detector modelling. The experimental data are compared with the model results.
13103-61
19 June 2024 • 14:20 - 14:40 Japan Standard Time | Room G213, North - 2F
Show Abstract +
Charge migration in infrared detectors such as in JWST leads to a 'brighter-fatter effect', where photoelectrons from bright pixels spill to nearby faint pixels and blur the pixel response function at its finest spatial scales - a limiting noise floor for high angular resolution astronomy. We demonstrate an effective forwards model: a nonlinear convolution predicting the effect on every pixel as a polynomial of the pixels in its neighbourhood, learning the coefficients by gradient descent together with a differentiable model of the point spread function. We apply this to the JWST/NIRISS Aperture Masking Interferometer, inferring an accurate model for the BFE in NIRISS; overcoming the main barrier to precise interferometric observations with JWST; and illustrating a simple path to high-quality BFE calibration in other JWST instruments and infrared detectors in general.
13103-62
19 June 2024 • 14:40 - 15:00 Japan Standard Time | Room G213, North - 2F
Show Abstract +
Skipper CCDs offer sub-electron readout noise by repetitive non-destructive measurements of signal interleaved with baseline measurements at a high enough frequency to reduce impact of 1/f noise when the average baseline is subtracted from average signal.
We describe the design of a Multichannel Video Processor (MVP) board that supports 128 differential video channels of the new Skipper CCD from STA,inc. It is compact enough to be located close to the detector and narrow enough to allow detector mosaics to be supported.
Results obtained with a compact prototype of an MVP channel and a Skipper CCDs with several output variants are presented and discussed.
13103-63
19 June 2024 • 15:00 - 15:20 Japan Standard Time | Room G213, North - 2F
Show Abstract +
Large format infrared detectors are at the heart of major ground and space-based astronomical instruments, and the HgCdTe HxRG is the most widely used. The Near Infrared Spectrometer and Photometer (NISP) of the ESA's Euclid mission launched in July 2023 hosts 16 H2RG detectors in the focal plane. Their performance relies heavily on the effect of image persistence, which results in residual images that can remain in the detector for many hours contaminating any subsequent observations.
Deriving a precise model of image persistence is challenging due to the sensitivity of this effect to observation history going back hours or even days. Nevertheless, persistence removal is a critical part of image processing because it limits the accuracy of the derived cosmological parameters.
We will present the empirical model of image persistence derived from ground characterization data, adapted to the Euclid observation sequence and compared with the data obtained during the calibrations of the satellite in-orbit. We will discuss its precision and show how efficiently it detects and masks post-images in Euclid observations.
Break
Coffee Break 15:20 - 15:50
Session 14:
X-Ray II
19 June 2024 • 15:50 - 17:30 Japan Standard Time | Room G213, North - 2F
Session Chair:
Andrew D. Holland, Ctr. for Electronic Imaging (United Kingdom)
13103-64
19 June 2024 • 15:50 - 16:10 Japan Standard Time | Room G213, North - 2F
Show Abstract +
The MIT X-ray Polarimetry Beamline is a facility that we developed for testing components for possible use in X-ray polarimetry. Over the past few years, we have demonstrated that the X-ray source can generate nearly 100% polarized X-rays at energies from 183 eV (Boron K-alpha) to 705 eV (Fe L-alpha) using a laterally graded multilayer coated mirror (LGML) oriented at 45 degrees to the source. The position angle of the polarization can be rotated through a range of about 150 degrees. In a downstream chamber, we can orient a Princeton Instruments MTE1300B CCD camera to observe the polarized light either directly or after reflection at 45 degrees by a second LGML. In support of the REDSoX Polarimeter project, we have tested three other detectors by directly comparing them to the PI camera. One was a CCD camera, a Raptor Eagle XV, and two had sCMOS sensors, the Sydor Wraith with a GSENS 400BSI sensor and a commercial Sony IMX290 sensor. We will show results comparing quantum efficiencies and event images in the soft X-ray band.
This work is supported in part by NASA grant 80NSSC23K0644.
13103-65
19 June 2024 • 16:10 - 16:30 Japan Standard Time | Room G213, North - 2F
Show Abstract +
To meet the scientific needs of future X-ray astrophysics missions, CCDs require continued development, most significantly towards higher frame rates. As CCD support electronics enable higher data rates (such as Stanford’s Multi-Channel Readout Chip), we are designing CCDs which can make optimal use of high speed, multi-channel operation through advancement in sense node design, low capacitance fabrication, and architecture changes in support of parallelization. Taken together these advancements minimize the CCD format’s inherent weakness in frame rate while maintaining the impeccable scientific imaging qualities which have kept CCDs as the detector of choice for scientific applications in X-ray imaging spectroscopy for 30 years.
13103-66
19 June 2024 • 16:30 - 16:50 Japan Standard Time | Room G213, North - 2F
Show Abstract +
In order to take advantage of data rich focal planes of future space UV and soft X-ray missions, large format detectors with excellent spatial resolution and dynamic range are required. This paper presents the development of photon counting detectors where Timepix readouts are used in combination with Microchannel Plate electron amplifiers enabling photon counting with high spatial (~5 µm) and temporal resolution with very large dynamic range (exceeding 10^8 ph/cm^2/s), capable of detection of many simultaneous particles and extended lifetime due to low gain operation. The latest generation of Timepix4 readout is 4-side buttabble enabling high resolution detection of many simultaneous particles (photons, ions, electrons, neutrons) in a large active area.
13103-67
19 June 2024 • 16:50 - 17:10 Japan Standard Time | Room G213, North - 2F
Show Abstract +
The X-ray polarization of compact objects in X-ray binaries allows us to understand the complex spacetimes surrounding these sources. XL-Calibur is a state-of-the-art, balloon-borne telescope that measures the linear polarization of stellar-mass black holes, neutron stars, and nebulae in the 15-80 keV energy band. The selected energy range allows for observing coronal emission from black holes while also enabling us to narrow down on emission models from neutron stars, pulsars, and magnetars. Early in 2024, XL-Calibur will be launched from Kiruna, Sweden for approximately 10 days to observe Cyg X-1 and Cyg X-3, or other sources chosen based on flux levels at the time of flight. Observations might be coordinated with the recently launched Imaging X-ray Polarimetry Explorer mission which measures polarization in the complimentary 2-8 keV band. Combined XL-Calibur and IXPE observations will yield information on both soft and hard X-rays allowing us to decompose the total emission from black holes into thermal disk and coronal. We discuss the characterization of the XL-Calibur CdZnTe detectors, the telescope mirror and truss setup, and preliminary results from our most recent flight.
13103-68
19 June 2024 • 17:10 - 17:30 Japan Standard Time | Room G213, North - 2F
Show Abstract +
We are presenting the status of the HypeX project to develop a large volume, increased field of view Time Projection Chamber for X-ray polarimetry based on a triple-GEM optically readout. We expect a complete 3D reconstruction of photoelectrons from around ten of keV to effectively extend the capability of the current GDP design. This will contribute significantly to X-ray astronomy through enhanced sensitivity and technological advancements.
Session PS1:
Posters-Monday
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13103-69
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
In recent years, an interest in the detection of the Short Wave Infra-Red (SWIR) band has grown. On the ground, the development of telescopes (ELTs) requires the construction of large focal planes in the SWIR for imaging, spectroscopy, or wavefront sensing applications. In space, the SWIR band can have many applications whether for communications or for imaging space and earth. The state-of-the-art III-V detectors in the SWIR are InGaAs photodiodes on InP substrate that are limited by a 1.7 um cut-off wavelength. Superlattice (SL) based detectors, that have been increasingly studied in recent years, make it possible to reach new cut-off wavelengths. Starting from the InGaAs on InP detector technology that has been mastered for more than ten years by THALES, the III-V Lab we propose to extend the detection range beyond 1.7 um by introducing a SL in the active region of an InGaAs photodiode. We will present the results obtained up to 2.6 um, as well as the solutions implemented to limit the carrier localization in the superlattice and the associated QE degradation. We will also discuss the consequence of minority carrier lifetime on the performance and of localization on MTF.
13103-70
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Astronomy is a science problem-oriented, measurement-based and discovery-driven discipline, and the significant improvement of astronomical measurement accuracy and ability will greatly promote human cognition of the universe. Astronomers can use telescopes to observe the universe.
Optical telescope is one of the most important astronomical telescopes, it collects optical information about celestial objects using science-grade image sensors. In modern times, with the rapid development of semiconductor technology, and because CMOS (Complementary Metal Oxide Semiconductor) image sensor has high data transmission rate and high integration, CMOS image sensors have become the main optical imaging image sensors used in astronomical telescopes.
In this presentation, the imaging principle and firmware design of a scientific CMOS camera named PX400 are introduced, and its performance test is conducted for astronomical observation and space target observation. The PX400 uses a scientific image sensor called GSENSE400BSI (hereinafter referred to as GS400) produced by GPIXEL, which has a high data readout rate and a variety of operating modes.
13103-71
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
CIS221-X is a prototype monolithic CMOS image sensor, optimised for soft X-ray astronomy and developed for the proposed ESA THESEUS mission. A comprehensive electro-optical characterisation of the CIS221-X reported low noise (3.3 e− RMS), excellent energy resolution (130 eV FWHM at 5.9 keV) and high X-ray quantum efficiency (>80% for 310 – 1900 eV photons). These results strongly support the consideration of CMOS image sensors for soft X-ray astronomy. One significant advantage of CMOS technology is its resistance to radiation damage. To assess this resistance, three backside-illuminated CIS221-X detectors have been irradiated with protons using the MC40 Cyclotron Facility at the University of Birmingham. The radiation effects on CIS221-X performance, particularly dark current and image lag, have been measured. These results, including a summary of the pre-irradiation CIS221-X electro-optical performance, are presented.
13103-72
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Observations in the near-infrared using large ground-based telescopes are limited by bright atmospheric emission lines, particularly OH lines, which can saturate a spectrograph on the order of minutes. Longer exposures will not contain useful information about the emission lines and also run the risk of detector effects such as bleeding and persistence. If exposure times could be made longer without these issues, signal to noise could be significantly increased by reducing the read noise overhead required for stacking shorter exposures. In order to achieve this, we use guide windows to reset detector regions containing bright lines while the rest of the detector continues integrating. We present the results of this method using a HAWAII-2RG infrared detector on the 1.2-m McKellar Spectrograph at Dominion Astrophysical Observatory in Victoria, Canada.
13103-73
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
The Mid-InfraRed Instrument (MIRI) uses three Si:As impurity band conduction (IBC) detectors. These detectors make use of an arsenic-doped infrared-active layer to excite photo-electrons and an electric potential applied across the layer guide them to the pixels. The electric potential depletes the layer of electron-hole pairs. As charge accumulates this region shrinks, resulting in more photo-electrons recombining and not reaching the pixels, which produces non-linear voltage integration ramps. On top of this, the spatial and spectral information may be blurred by up to 20% due to charge migration, depending on the contrast between pixels. This ’Brighter-Fatter Effect’ (BFE) has been observed in detectors for optical and near-infrared wavelengths as well, though it manifests differently in the mid-infrared IBC detectors. Since both the non-linearity and BFE are dependent on the amount of charge accumulated, we propose a fitting and correction routine that corrects both simultaneously for all MIRI observing modes.
13103-74
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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This paper will show a very precise and easier concept to align CCD sensor packages out of an extremly stiff and precise machined SiC based composite material to assemble numerous sensors on a focal plane with micron precicion. The focal plane structure will be from the same ceramic material therefor the cpomplete focal plane assembly will be manufactured out of a single material having a very low CTE. Such assembly can be skaled for cubesats up to very large scale FPA like 1 x 1 m for ground based applications to allow super precise alignments and high camera resolution.
13103-75
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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Kinetic Inductance Detectors (KIDs) are superconducting microwave resonators with single photon arrival timing and intrinsic energy resolution at visible and near-IR wavelengths. To shrink the KIDs below their current 150 μm pixel pitch, we study microwave resonators based on amorphous, hydrogenated silicon carbide (a-SiC:H) parallel plate capacitors (PPC).
In this work, we investigate how the frequency noise level and microwave loss of PPC-based resonators depend on the PPC's geometry. We have measured the frequency noise and microwave loss of 56 a-SiC:H PPC resonators, which cover a factor 44 in PPC area variation and a factor 4 in dielectric thickness. We observe that both an increased PPC area or thickness reduces the frequency noise. Interestingly, the microwave losses, which should be independent of PPC volume, show an unexpected reduction with increasing thickness, pointing towards surface layers dominating the loss, which are not visible in the noise data.
13103-77
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
Future strategic X-ray satellite telescopes, such as the probe-class Advanced X-ray Imaging Satellite (AXIS), require excellent soft energy response in their imaging detectors to enable maximum discovery potential. In order to characterize Charge-Coupled Device (CCD) and Single Electron Sensitive Read Output (SiSeRO) detectors in the soft X-ray region, the X-ray Astronomy and Observational Cosmology (XOC) group at Stanford has developed, assembled, and commissioned a 3-meter-long X-ray beamline test system. The beamline is designed to efficiently produce monoenergetic X-ray fluorescence lines in the 0.3-8 keV energy range and achieve detector temperatures as low as 173 K. I will present design and simulation details of the beamline, and the achieved vacuum, cooling, and X-ray fluorescence performance. As a workhorse for future detector characterization at Stanford, the XOC beamline will support detector development for a broad range of future X-ray astronomy instruments.
13103-78
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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We are developing imaging Cadmium Telluride (CdTe) and Cadmium Zinc Telluride (CZT) pixel detectors with potential applications in hard X-ray astrophysical NASA Explorer and Probe-class missions, utilizing wide field and focusing instruments. Our hybrid sensor consists of a CdTe and a CZT detector with segmented anode contacts directly bonded to an ASIC. We have utilized a custom low-noise, low-power ASIC developed for NuSTAR mission. While NuSTAR employed eV Products CZT detectors, for this study, we used a CdTe detector by Acrorad and a CZT detector by Redlen. Both detectors have anode pixels with a 604-micron pitch in a 32 x 32 array. The CdTe detectors have segmented Schottky blocking contacts, whereas the CZT detectors have plain contacts. Understanding the charge sharing and charge loss behavior between the pixels is crucial to achieve good energy resolutions.
In this paper, we report on the study of charge sharing and charge loss effects between the pixels. We will compare the behavior among eV CZT, Redlen CZT, and Acrorad CdTe detectors. Furthermore, we will discuss how these effects might influence smaller pixel pitch detectors for our next-generation prototype ASIC.
13103-79
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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InGaAs detectors, as one of the mainstream detectors in the field of short-wavelength infrared detection, hold a crucial position in the field of infrared astronomy. As the core component of astronomical telescopes, the performance of detectors plays a decisive role in astronomical observation systems. Temperature significantly affects the semiconductor characteristics, including dark current and readout noise, thus impacting the key performance of the detector. In this study, three commercially available InGaAs short-wavelength infrared focal plane array detectors from Chinese manufacturers were selected. A high-performance readout electronics system compatible with these three detectors was designed, and performance tests were conducted on a short-wavelength infrared testing platform under high vacuum and deep cooling conditions. By analyzing the performance of the detectors from -40°C to -160°C, the influence of temperature on detector performance was investigated.
13103-80
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The Mid-Infrared Instrument (MIRI), on-board the James Webb Space Telescope (JWST), was designed to produce a diffraction-limited Point Spread Function (PSF) at the detector image plane in the 5-28 micron wavelength range. For the MIRI Medium-Resolution Spectrometer (MRS), a PSF broadening of 60% down to 10% is observed in the 5-28 micron range. Additionally, 20% of the light is scattered into the wings as an extended component on the detector. The same PSF systematics manifest in the MIRI Imager and Low-Resolution Spectrometer (LRS) data. We use physical optics propagation to propagate a uniform wavefront from the JWST pupil to the MIRI Imager detector plane. The camera F-number and variation of incidence angle across the detector allow us to reproduce the systematics and an observed bending in the extended component, across the detector. This is a significant leap for PSF-weighted photometry. The model can be extended to the LRS and MRS.
13103-81
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
Show Abstract +
ESA’s Science Payload Validation laboratory is developing a new type of detector characterisation bench, designed to cope with new challenges set by future instrument requirements and newly developed detectors. This new bench can accommodate large format detector up to 4kx4k 10um pitch or at least two 2kx2k 15 um pitch side by side, it enables measurement in the 300-4000 nm wavelength range, and can bring the detector temperature down to 20 K. Its concept, based on lessons learned accumulated over the last 10 years, enables light and dark measurements to be performed in a single configuration reducing handling and optimising testing time in test campaigns.
This contribution provides a general overview of the bench concept and main features. It details the main design challenges and describes the corresponding opto-mechanical and thermal design solutions, validated by early commissioning results.
13103-82
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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JASMINE, the near-infrared space telescope for astrometry and exoplanet surveys, is planned for launch in the 2030s. This will be the first time that the InGaAs Infrared 2D image sensor chip manufactured by Hamamatsu Photonics is employed for a space mission. For the space mission, we processed substrate layer thinning to mitigate fluorescence on the image from cosmic rays. In this context, we introduce preliminary reports on the performance testing of the sensor chip, including measurements of dark current and quantum efficiency. Through these experiments, we confirmed fluorescence is significantly reduced over a few minutes of exposure as a result of the substrate removal.
13103-83
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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State-of-the-art X-ray CCDs are close to delivering the key performance metrics for the next generation of X-ray telescopes except the required frame rates. To meet this need, we developed the Multi-Channel Readout Chip (MCRC) which enables fast readout and higher frame rates for MIT-LL JFET (junction field effect transistor) CCDs. We have characterized the MCRC V1.0 performance alone and with an X-ray CCD as well as its TID radiation tolerance. We also report progress on our continued development of the novel SiSeRO (Single electron Sensitive Read Out) technology which is able to deliver exquisitely low noise. Finally our group is developing AI methods to enhance our detector performance, including enhanced particle background screening and improved event characterization.
13103-85
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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With CMOS sensors starting to be utilised in astronomical telescopes, new uses for them are being explored. One such use is the possibility of observing distant, dim objects, which requires long integration times, and therefore low dark current. This work focuses on the dark current characterisation of the CIS220 at very long integration times at a range of temperatures, from +20 to –60 °C, before and after proton and gamma irradiation.
13103-86
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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Under an ESA contract, Leonardo UK developed the IBEX detector also referred to as LAPD for Large-format Avalanche Photo Diode array. Leonardo’s packaging solution relied on a chip-on-board solution incompatible with technical and performance requirements of ESA characterisation campaign and experimental setup. An in-house solution has been developed, with ESA responsible for the design, manufacture, and test. And Leonardo responsible for gluing the device to the carrier and the wire bonding. ESA’s packaging solution relies on Molybdenum carrier and two flexible PCB cables.
This contribution details the mechanical design and test activities for the development of the full solution including carrier, handling jig and transport container.
13103-87
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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In this paper we will present characterization of our Microwave Kinetic Inductance Detectors (MKIDs). The design process involved using Sonnet and LEdit 8.3. In this design, we employed a structure consisting of TiN (3nm)/Ti (10nm)/TiN(3nm) layers covered by a 100nm aluminum layer. This structure provides a kinetic inductance of 100 pH/Sqcm and a critical temperature of 1.1 Kelvin. The MKIDs were fabricated on 5-inch silicon wafers with a resistivity exceeding 15000 ohmcm. The designs cover three frequency regimes: 1-2 GHz, 2-4 GHz, and 3-6 GHz. This variation in frequency ranges allows us to study the improvement of quality factors and provides a range of frequencies for testing our electronics.
13103-88
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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Observing astronomical phenomena in short time-scale such as transients require image sensors with high frame rates. National Astronomical Observatory of Japan (NAOJ) and Hamamatsu Photonics K.K. have been developing large format, high-speed readout and back-illuminated CMOS sensors. NAOJ is aiming to develop a wide-field and high-speed CMOS camera for Subaru Telescope that will cover a similar field of view that Suprime-Cam covered with its CCDs (34' x 27'). The CMOS sensors have 2,560 x 10,000 pixels with 7.5 um pixel square. We will report the progress of the development of the CMOS sensors and the measured basic characteristics such as quantum efficiency, full well and readout noise. We will also introduce the readout electronics which is under development for this CMOS sensors.
13103-89
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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We are developing X-ray Silicon-On-Insulator (SOI) pixel sensors, called “XRPIX” for the next generation X-ray astronomy satellites (Tsuru et al. 2018). In order to use the XRPIX for the X-ray observatories, the sufficient time resolution is required to discriminate non X-ray events using the anti-coincidence method. For this method, a hit trigger of the XRPIX with a short delay and jitter time (~ 10 μs) is required since the typical hitting rate of the high-energy background events on active shields is ~ 10 kHz. Therefore, we have evaluated the trigger performance using the laser-generated pseudo-X-ray instead of X-ray sources. This allows us to easily control the timing, the position, and the energy of the hit events on the XRPIX. Our laser evaluation estimated trigger’s delay and jitter time to be < ~1 μs. Here, we will report on the results of the trigger evaluation and the anti-coincidence system demonstration.
13103-90
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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Specular X-ray reflectometry (XRR) is a widely used experimental technique to characterize thin layer materials. By analysing the reflectivity spectrum, one can obtain information on the material surface and interfacial roughnesses, layer thicknesses and densities.
We have developed an independent open-source Python-based fitting tool has been developed to analyse the data from XRR measurement. The tool is abbreviated XFT, X-ray reflectometry Fitting Tool.
In this paper, we describe the theoretical background for the calculation of specular reflectivity responses from complex mirror structures. We compare optical constants provided by different institutes (LLNL, NIST, CXRO), and present the differential evolution algorithm that allows for a complete free parameter space and performs well for a multi-parametric model space, where parameters may be correlated. In order to validate the XFT, the computed reflectivity spectra are compared against those computed from the IMD software. The complete XFT package is available at GitLab: https://github.com/NisGellert/XFT.
13103-91
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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On-board SVOM to be launched in 2024, the Microchannel X-Ray Telescope (MXT) is equipped with a 256 x 256 pixel pnCCD and two CAMEX ASIC operated at -65°C, and a full-custom front-end electronics box to control the focal plane and extract photon events. Proton irradiation tests were performed on a qualification model of the MXT focal plane and were followed by spectral calibration tests in the SOLEIL synchrotron. The paper will describe the setups of these two campaigns and the performance results, in particular the degradation of charge efficiency transfer and energy resolution by displacement damage dose.
13103-92
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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Recently, InGaAs cameras have been utilized in time-domain astronomical observations in the infrared bands, taking advantage of their improved performance. However, the noise levels of InGaAs cameras remain high compared to CCDs in optical bands, thereby limiting the signal-to-noise ratio. In this study, we will present a comprehensive investigation of the noise from a commercially available InGaAs camera. Then we will develop correction methods for each noise and apply these methods to images obtained from time-domain observations. We will assess the efficacy of these corrections by evaluating the photometric precision of light curves. Finally, we will discuss the potential of InGaAs cameras in infrared time-domain observations.
13103-93
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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Electron-multiplied CCDs are used in a variety of astronomical and space science applications where high speed and low noise are required. It is known that the gain is not completely stable, and In some applications it is necessary to have an accurate estimate of the gain, preferably using on-sky images. In this paper we investigate different approaches to gain estimation using numerical simulations of EM gain, laboratory measurements and real data obtained at the 8m Gemini South telescope.
13103-94
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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MKIDs made from alternating stacks of Ti and TiN have shown impressive results in far-IR and sub-mm detectors to date, which promises improvements for Optical to Near-IR MKIDs. TiN/Ti/TiN tri-layers offer different advantages between sub-stoichiometric and stoichiometric recipes. We will elaborate on the expected effects of using sub-stoichiometric vs. stoichiometric TiN in triple layers on the wavelength signal-to-noise ratio of MKIDs. We characterise the photon detection performance of TiN/Ti/TiN Optical to Near Infrared MKIDs deposited on silicon wafers. We present measurements of resolving power, quasi-particle lifetime and sensitivity to near-infrared photons with differing pixel fabrication procedures and design.
13103-95
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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MKIDs combine unique advantages that are valuable for modern astronomical instrumentation like single photon counting or single pixel wavelength resolution. We will present our efforts to optimize photon counting MKIDs and will discuss the effects of varying fabrication recipes on their general characteristics. We will elaborate on the advantages and disadvantages of different Tc values, substrates and film thicknesses and will demonstrate how controlled annealing can be used to further tweak the detector’s capabilities. We will report on achieved quality factors, QP lifetimes and drive power limitations and intend to demonstrate how to control them with dedicated fabrication procedures.
13103-96
17 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The final read of each Mid-InfraRed Instrument (MIRI) integration exhibits a systematic offset in expected absolute data (DN) levels. This offset is row-dependent, resulting in a ~6% and 1% difference from expected absolute data-number (DN) levels on odd and even rows respectively. This offset is mostly caused by the nature of the read-reset being performed in the final frame of each integration. While the effect is stable and repeatable, an empirical correction has been elusive due to the lack of adequate data to model the full parameter-space of the effect. In this work, we report the results of a calibration program aimed specifically at deriving a correction of this effect using a unique dataset.
Session PS2:
Posters-Tuesday
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
13103-97
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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Future space-based missions require detectors with exceptionally low readout noise and minimal intrinsic background. We explore the rate of single-electron events (SEEs) induced by Cherenkov radiation in silicon detectors, a critical phenomena when dealing with intense radiation environments. We employ laboratory data and GEANT4 simulations to estimate the SEE background attributable to Cherenkov radiation produced by high-energy particles in low Earth orbit (LEO) and at the L2 Lagrange point. Our results indicate that cosmic-ray-induced Cherenkov radiation is a non-negligible background source that should be considered for future space missions attempting to achieve single photon counting in the optical/near-infrared.
13103-98
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The Polarimeter to Unify the Corona and Heliosphere (PUNCH) mission is a four spacecraft observatory designed for low earth orbit observations of the Sun to understand better the solar wind. Each of the four observatories carries a Teledyne e2V 230-82 CCD controlled by a Rutherford Appleton Laboratories (RAL) detector controller and a filter wheel that allows for the selection of different polarization vectors and a blank off in order to monitor detector health. The CCD is 2kx4k pixels and has a store shield covering half the device to serve as a charge storage region. The CCDs are operated in pseudo frame transfer mode. We present here the laboratory optical calibration data for the four flight detector systems. We have measured the read noise, dark current, linearity, global and local pixel response nonuniformity, and quantum efficiency across the visible bandpass.
13103-99
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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Persistence effects in HgCdTe infrared detectors cause significant artifacts that can impact the quality of science observations for up to many hours after exposure to bright/saturating sources. This problem will have a substantially greater impact on viable observing modes for infrared cameras on future ELTs due to the leap in sensitivities that is expected. In this paper we present new results from an updated test system that was previously used to prototype "on-detector guide windows" to provide fast T/T feedback to AO systems, interleaved with simultaneous (slow) full-frame readouts for science. We now explore the possibility of continuously resetting these small regions of the detector that are illuminated with a compact source as a strategy for mitigating persistence.
13103-100
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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As part of the OSCURA experiment, we are developing the readout system for a ~30 GigaPixel Skipper-CCD array. This work describes the design of a scalable multiplexed readout cold electronics system based on the newly designed MIDNA ASIC, which is optimized for low-noise readout of skipper-CCDs. We will present the performance demonstrated in recently built small prototypes of this readout system, along with the current development for the full-size detector array.
13103-101
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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We report recent progress on microchannel plate (MCP) sealed, high-vacuum devices and open-face architectures with 25 cm2 active areas. These can be configured with UV transmissive windows, bi-alkali or alkali-halide opaque photocathodes and atomic layer deposited (ALD) MCPs. Detectors with 100cm2 XS readouts are currently under development and we discuss our results with newly fabricated hermetic, high temperature co-fired ceramic (~10 x 10 cm) XS anodes. We employ event driven electronics and make initial performance assessment of these new sensing elements. We also discuss the implementation of a first generation GRAPH ASIC that couples charge sensitive amplification and digitization for XS signal conversion in a low power, small format. The approaches shared serve as candidates for creating large focal planes that can meet the requirements of future flagship UV missions. They also constitute a tailorable option for the community and can support smaller missions with a variety of detector formats.
13103-102
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The Australian National University (ANU) is actively advancing cryogenic preamplifier systems for infrared detectors, addressing challenges in systems with extensive cable runs. This innovation counters radio frequency (RF) noise interference by converting the detector's signal into a differential signal before transmission, enhancing signal cleanliness. Acting as a buffer for the Readout Integrated Circuit (ROIC), the cryogenic preamplifier allows low-noise instrument amplifiers near detectors, isolating the readout path from external interference. The approach significantly boosts infrared array sensitivity, improving frame rates and signal-to-noise ratios in astronomical observations. Laboratory tests demonstrate the cryogenic preamplifier's effectiveness in suppressing external interference noise, showcasing its critical role in ANU's detector and control system for both ground-based and space-based applications.
13103-103
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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This work details the development of the Adiabatic Demagnetization Refrigerator (ADR) control electronics for X-IFU instrument, of ESA's newAthena observatory. The ADR operates in a closed loop using a PID system, where the voltage bias is regulated based on the temperature measurements. The core of this work involves the design and development of two electronics board prototypes, a differential low noise amplifier and a power supply board, addressing the unique space constraints and operational requirements.
The ultra-low noise amplifier is designed to readout a 50mK resistive sensor. We have achieved a noise level of 2nV/rtHz which is critical for addressing the challenges of thermal stability (0.9µK RMS at 50mK), essential to achieve the instrument's target resolution of 2.5eV. Primely results of the ADR cooler's performance and its control electronics will be presented, emphasizing the temperature regulation achievements during the observation phase.
13103-104
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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We present our VASC system, which can test and calibrate UV to NIR detectors in their spatial/angular sensitivity, linearity, spectral response and response to polarized light. We present a few examples of measurements performed by VASC, such as the QE of CMOS detectors, calibration of photodiodes to NIST / PTB standards with less than 0.1% uncertainties, and the measurement of optical components like filters, mirrors and dichroics. We also describe the latest upgrade to VASC relative to SPIE doi:10.1117/12.2629448, using all-reflecting off-axis Schwarzschild relay optics, producing less scattered light, and mounted in a 3D printed closed-box to provide much better environmental stability.
13103-105
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The METIS instrument is designed for mid-infrared observation (3.5 to 13.5μm) with four focal planes, comprising two high-contrast imager/spectroscopy channels, a very high-resolution spectrograph, and single conjugate adaptive optics. It incorporates five H2RG detectors, one SAPHIRA detector, and a GEOSNAP detector. Controlled by the NGCII detector controller, the detectors operate with a new cryogenic preamplifier for minimized crosstalk and high-speed functionality. The paper discusses the challenges in developing these detector systems, covering design, system performance, and the necessary preparations for integration into the METIS instrument.
13103-106
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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Ground based astronomical observatories often require electrical equipment to reside out in the open air close to the telescope and instrument optics. The telescope and instrument optics are extremely sensitive to air currents caused by the warm electronics operating in domes open to the cool night air. In order to avoid these air currents, the ANU in collaboration with ESO has developed a MTCA.4 compliant conduction cooled chassis, backplane and clamshells to accommodate the electronics modules developed by ESO for the ESO NGC II detector controller.
ESO have been developing a MTCA.4 air cooled detector controller to replace the highly successful ESO NGC. The conduction cooled ESO NGC II controller uses the same electronics modules and is interchangeable with air-cooled controller. MTCA.4 does not support conduction cooling and the aim to is to eventually have the PICMG consortium who set the MTCA standard adopt the design concepts developed by the ANU and extend the standard to include conduction cooling.
13103-107
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The first generation of ELT instruments includes an optical-infrared High Resolution Spectrograph, ANDES (ArmazoNes high Dispersion Echelle Spectrograph. It covers a wide spectral range that goes from U to IZ . A common model of detector is planned for the two visible spectrographs. A total of 5 detectors will cover the latter spectral range. A common detector unit design has been developed based on ELT's standard components and inspired by the previous successful detector units designed for HARPS and ESPRESSO. It consists of a 9k x 9k CCD detector, a differential vacuum cryostat that keeps the detector in its dedicated vacuum chamber and a cryocooler that cools down the detector to minimise the dark noise. The required temperature, mechanical and pressure stabilities drive the design of the detector unit
13103-108
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The traditional readout system for Microwave Kinetic Inductance Detectors (MKIDs) often utilized Field-Programmable Gate Arrays (FPGAs) for nearly all its digital processing tasks. However, the cost of such FPGA development is high and the design must be conducted carefully to fit the limited FPGA resource. To cope with this challenge, a hybrid readout system emerged as a viable solution, integrating both FPGA and CPU/GPU components. In this configuration, the FPGA handles the hard real-time and high-throughput processing, while a soft CPU/GPU sub-system receives the phase data and executes more sophisticated algorithms. Details of this FPGA firmware and the corresponding CPU/GPU system software developed at Durham University will be presented.
13103-109
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The MARVEL instrument is an array of four 80cm telescopes feeding a high-resolution echelle spectrograph designed to provide high precision radial-velocity measurement and is being led by KU Leuven (Belgium). The UK ATC is responsible for the delivery of the detector work package; a fully characterised STA1600LN optical CCD housed in a custom cryostat. As a large image area detector, the STA1600LN has been used in a variety of astronomy applications for imaging. This paper will detail the characterisation testing done by the UK ATC Electronics and Detectors group, to verify that this detector meets the requirements for a high-resolution spectrograph of this type. Testing includes measures of read noise, dark current, and the effects of the dither clocking on detector performance and stability, among others.
13103-110
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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With the widespread integration of infrared (IR) instruments in astronomical missions, accurate per-pixel flux estimation for near-infrared (NIR) hybrid detectors has become critical to the success of these missions. This study, based on CPPM's involvement in both SVOM/Colibri and Euclid, proposes universally applicable methods and framework for characterizing IR hybrid detectors. The characterization framework, applied to the ALFA detector and Euclid H2RG, not only validates the proposed methods but also unravels subtle behaviors intrinsic to these detectors.
13103-111
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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ESA’s Science Payload Validation laboratory is responsible for the characterization of detectors under technology development or foreseen to be used in ESA’s science mission. In this context, ESA’s Science Payload Validation laboratory has developed COMODOR (ESA’s COntroller for cMOs DetectOR), a new CMOS detector controller focused on controlling and reading out new and future large format infrared and visible CMOS imaging sensors. A prototype for COMODOR has been developed and is currently in use to characterize Leonardo’s IBEX 2kx2k pixels MCT-hybridised detector. The design of COMODOR version 2 is underway and will add more flexibility by integrating the ability to control and readout digital CMOS detectors such as the future Teledyne E2V CIS120 and CIS300. The paper will describe architecture, and test results on performance, and an outlook towards v2.0.
13103-112
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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We introduce MKIDGen3, a scalable and cost-efficient RFSoC-based readout system for UVOIR-sensitive Microwave Kinetic Inductance Detectors (MKIDs). MKIDGen3 not only doubles readout bandwidth, but also reduces power consumption and costs by 80% and 50%, respectively. The system features a central control node which facilitates array-level setup, data storage, image synthesis, and UI server functionality connected to a cluster of of low-cost RFSoC boards, each responsible for a 2 kilopixel sub-array. This open-source platform is tailored for smaller research groups lacking dedicated FPGA staff, offering ease of maintenance and adaptability. A notable innovation in MKIDGen3 is its system-level performance simulator, designed to eliminate guesswork in the development of optical MKID readouts and facilitating informed decision-making for DSP and device setup algorithms, a significant advancement. We discuss the development and demonstrated performance of the readout and simulator, highlighting their application to detectors in the laboratory and on sky.
13103-113
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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Microchannel plate (MCP) detectors have been used on many ultraviolet
(UV) space based observatories. Future NASA missions would benefit
from scaled designs with larger areas, higher spatial resolution, and
high counting rate capability. These prospects are being successfully
demonstrated with cross strip (XS) anode readouts, but the electronics
that read out such detectors would require reduction in size, weight,
and power. The GRAPH ASIC was developed as an efficient high bandwidth
solution to read out cross strip anodes for MCP detectors. First
generation GRAPH ASICs have been wire bonded to circuit boards and
initial testing and characterization have been done. Firmware and
software have been implemented to process XS anode events producing
X-Y photon positions. To further test and characterize performance of
the GRAPH ASIC a GRAPH board is being used to read out photon events
from an MCP detector with a cross strip anode. We present preliminary
results on GRAPH design and operation. In addition we demonstrate
photon detection with position and pulse height analysis and a
description of the firmware currently being used to carry out these
tests.
13103-114
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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CAGIRE is the near infrared camera of the Colibri robotic telescope designed for the follow-up of SVOM alerts and the quick imaging of sky regions where transient sources are detected by the satellite. CAGIRE is based on the Astronomical Large Format Array (ALFA) detector from the Lynred French Company.
CPPM is responsible for the characterization of the scientific performance of the ALFA detector. During the tests, ALFA has been tuned in order to optimize its response for CAGIRE with regards to linear dynamics, readout noise, and linearity and its performance parameters such as dark current, readout noise, linearity, inter-pixel capacitance and latency have been evaluated in both J and H bands. First results of these tests will be presented in the light of the project science requirements.
13103-115
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The Little Ultraviolet Camera (LUVCamera) is a low-cost, high-performance UV/optical camera system designed for space-based astronomical facilities. Enabling LUVCamera is a GSENSE 4040-BSI scientific CMOS (sCMOS) sensor, similar to those found in commercial-off-the-shelf (COTS) cameras. Given the intended application, it is crucial to understand not only the performance of the sensor, but also the performance degradation due to radiation damage. Here, we detail the characterization results of a SBIG Aluma AC4040 which uses this sensor, as well as a SBIG Aluma AC2020 (based on the smaller GSENSE 2020-BSI) which has been exposed to radiation. We describe the procedures used for sensor characterization and the associated measurements of the read noise (RN), dark current (DC), and absolute quantum efficiency (QE), along with changes to those quantities post-radiation in the AC2020. Our findings affirm the suitability of COTS sCMOS sensors like these for applications in space-based missions.
13103-116
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The Rubin Observatory LSST Camera exhibits novel crosstalk between CCD amplifier segments that does not scale linearly with intensity as we would expect from capacitive coupling alone. Illuminating with realistic satellite streaks and stars, we create realistic crosstalk sources and images in science-grade LSST CCDs. We use a custom-made electronics board that simulates the load of a CCD to inject proxy video signals directly into Rubin LSST Camera readout electronics board to isolate the sources and shape of crosstalk and its nonlinearity. We discuss possible mechanisms for nonlinear crosstalk in the camera and how it may be partially corrected in the main survey using on-sky data.
13103-117
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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Determining the conversion factor between the observed counts in the MIRI imager and actual number of electrons is inhibited by non-ideal characteristics of the detector. In addition to nonlinearity of the detector, the electronic correlation between pixels, or Inter-Pixel Capacitance (IPC), causes an effective smoothing of the image. This decreases the noise and thus leads to an overestimation of the number of detected electrons. In this work we measure the IPC in the
MIRI imager at a significant level by means of the Pearson Product-Moment Correlation Coefficient (PPMCC). We also demonstrate how IPC influences the MIRI point-spread function and discuss the implications.
13103-118
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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We discuss new methods developed for characterizing CMOS detectors. They are applied and tested on data obtained with the 1kx1k LmAPD NIR arrays developed at the Institute for Astronomy, UH in partnership with Leonardo Company. First, the full IPC (interpixel capacitance) kernel is recovered using a Bayesian technique based on a probabilistic model directly representing the IPC coupling between neighboring pixels as correlations between pairs of random variables. Uncertainties on the IPC kernel terms are estimated by MCMC. We also carried out an analytical study validated by simulations to evaluate the systematic error due to inter-pixel variability and affecting the conversion gain determined by PTC (photon transfer curve) based on spatial averaging. Finally, the combination of high APD gains and multisampling+averaging enables sub-electron readout noise (RN~0.3e-) to be achieved, opening up the possibility of photon number resolving (PNR). The analysis method used to extract the system parameters (conversion gain, readout noise, excess noise factor), and estimate their uncertainties, from the PNR histograms obtained with our LmAPD arrays, is presented.
13103-119
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The LSST Beam Simulator is a wide field f/1.2 re-imaging system that recreates the optical beam of the LSST Camera and is capable of illuminating a single CCD with realistic astronomical scenes. We describe the software and hardware upgrades to the imaging system to replace our previous commercial SAO electronics controller with the custom-built Readout Electronics Board (REB5) and Data Acquisition system (DAQ) used by the LSST Camera, to more accurately replicate the on-sky operation of the CCDs. Basic characterization of two LSST Camera CCDs was done using bias, dark, and flat images to calculate electro-optical properties. We used images of spots and streaks to simulate realistic astronomical objects like stars and satellites respectively for the purpose of studying additional sensor effects such as the brighter-fatter effect and non-linear electronic crosstalk.
13103-120
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The Wide-Field Infrared Transient Explorer (WINTER) is a robotic infrared time-domain survey instrument at the Palomar Observatory, commissioned in June 2023. We present the characterization of the WINTER InGaAs detectors and results from the first year of observing with WINTER.
13103-122
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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We present the design and initial tests of the High-speed Array Controller (HIAC) developed at NRC to operate high-speed multi-channel imaging detectors. Originally developed to operate the large SAPHIRA infrared APD array, which required 64 channels at 10Mpx/s each, it is also being used in other projects, including tests of a large format CMOS imager for the CASTOR space telescope.
13103-123
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The HISPEC tracking camera is a key part of the HISPEC front end instrument (FEI) that ensures the AO-corrected beam from the Keck telescope is optimally coupled into HISPEC’s single mode fibers. We present here an implementation of an Archon Controller with low latency and high cadence (1kHz) capabilities that fulfill real time requirements of the tracking loop.
13103-124
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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Microchannel plates-based detectors have been for a long time the detectors of choice for astronomical applications in the FUV/EUV, due to their photon counting capability and the possibility of solar blindness.
In the framework of R&D for future astronomical FUV/EUV spectrographs, we are developing a new readout system to allow unprecedented dynamic range. The goal is to realize a photon counting, solar blind, UV detector, based on a MCP read out with a 2D anode array integrated in a custom designed Read Out Integrated Circuit (MIRA - Microchannel plate Readout ASIC), able to reach unprecedented performance in terms of dynamic range combined with spatial resolution close to 30 µm. Each pixel contains an anode to collect the electrons emitted by the MCP, a low noise amplifier and filter to maximize the SNR, a comparator to recognize and count single photon events, logic to correct for charge sharing among pixels (CSCL) and two counters.
Results of the characterization of the first prototype, based on a demonstrator of the MIRA ASIC, 32×32 pixels, 35×35 μm2 size, for a total chip area of 2×2 mm2, integrated into a standard demountable MCP intensifier, will be presented.
13103-125
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The Lobster Eye telescope's wide field capability renders it an optimal tool for detecting transients across a vast range of objects in the X-ray band. However, due to the unique structure of the telescope observer, the observed image is modulated by the point spread function, which spreads photons from the point light source into cross-structured images. The current detection algorithm compresses the data observed by the telescope into two-dimensional images for detection. While this strategy can detect sources with obvious cross structure with acceptable performance, it performs worse for sources with fewer photons. In this paper, we consider both the energy and spatial distribution of photons and develop a source detection algorithm based on a 3D detection neural network. Our results demonstrate that our method outperforms contemporary 2D detection algorithms. In addition, we also extracted and accurately classified the source light curve after the source detection, which provides the basis for the further in-depth x-ray astronomical observation research.
13103-126
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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Metis, one of the instruments of the ESA mission Solar Orbiter (launched on February 10th, 2020, from Cape Canaveral), is a coronagraph with 2 channels, capable of performing broadband polarization imaging in the visible range (580-640 nm), and narrow-band imaging in UV (HI Lyman-α 121.6 nm).
It is equipped with two detectors based on CMOS APS sensors: a custom sensor for the VL channel, and a CMOS Star1000 coupled to an intensifier for the UV channel.
Dark subtraction is a crucial step in the data reduction pipeline, thus requiring careful in-flight monitoring and characterization of the dark signal. Since it is not possible to directly acquire dark images with the visible detector, as the door of the instrument is not light-tight, an ad hoc procedure has been designed to estimate the correction to be applied. In the case of the UV detector, however, it is possible to acquire dark frames by turning off the intensifier. Due to small fluctuations occurring on the bias signal level even on short timescales, an algorithm has been developed to correct the dark matrix frame by frame. The results of the correction procedures for both detectors are presented.
13103-127
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The ANU Rosella system is a compact (approx. 0.5U) and configurable, high speed, video readout system that is a miniaturised version of the electronics required to operate scientific detectors. Rosella provides customisable 'clock' and 'bias' signals to drive virtually any CMOS-based sensor array and supports device specific functionality such as reference channels and area-of-interest readout (windowing). In addition, the system can be configured for a range of data interfaces to suit various standard camera and spacecraft bus protocols.
13103-128
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The deployment of ELTs will revolutionize astronomy owing to incredible spatial resolution, light gathering power, and a host of extremely capable instruments. METIS on the ELT, with its high-contrast imager and high-resolution spectrograph, will enable breakthroughs in exoplanets, planet-forming disks, and other areas of astrophysics. Ahead of its deployment, we must verify the performance of its detector, GeoSnap, including its quantum efficiency and 1/f noise. We will test the METIS GeoSnap in the MITTEN Cryostat at the University of Michigan which was previously used to characterize the University of Michigan GeoSnap deployed in MIRAC-5. We have used a reference detector to calculate the flux of the source in order to calculate quantum efficiency for METIS Geosnap. We will present our test results and show that the GeoSnap meets all performance requirements. The successful verification of the METIS GeoSnap will define a new detector of choice for future ground-based mid-IR instruments.
13103-129
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The Keck-NIRC2 electronics underwent an upgrade in the fall of 2023 that dramatically increased the readout efficiency in the mid infrared (3-5 µm). We present an updated analysis of how this upgrade improved the sensitivity of Keck-NIRC2 in the modes most commonly used by the exoplanet direct imaging community. We provide on-sky testing results of the throughput measurements of the vector vortex coronagraph and an evaluation of the thermal background dynamical timescale. Our goal in this proceeding is to provide Keck-NIRC2 users with knowledge and recommendations for how the recent NIRC2 upgrade affects the optimal observing strategies in the mid-infrared high-contrast imaging application.
13103-130
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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We present a technique to identify a thermal light source via testing for Siegert relation violation, using photon correlation of photoevents detected at the output ports of an asymmetric Mach-Zehnder interferometer. Using this method, we show that laser light scattering off a rotating ground glass violates the Siegert relation and hence not a source of thermal light. Conversely, light from a mercury vapor lamp is shown to obey Siegert relation.
13103-131
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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The PRime-focus Infrared Microlensing Experiments (PRIME) camera is part of the joint NASA-JAXA project supporting the Nancy Grace Roman Space Telescope engineering and science studies. It is installed on the 1.8 m PRIME telescope with a ~1.5 square degree FOV dedicated to the project. The instrument is equipped with multiple broad band and narrow band filters between 0.9 µm to 1.8 µm. The instrument is installed at the South African Astronomical Observatory and has been in continuous operation since October 2022. PRIME is currently surveying the Galactic bulge for microlensing events, GW and GRB studies and other science objectives, in advance of the Roman Space Telescope (RST) mission. After 1.5 years of on-sky operation, we present the use, performance and lessons learned operating RST’s yield demonstration lot H4RG-10 detectors as part of the PRIME camera based on the data processing and analysis tools that we have developed. With the large field of view in the near infrared bands this instrument is a powerful tool in the Southern hemisphere and a compliment to the instruments in the North and in the visible.
13103-132
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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Infrared astronomy is an important branch of astronomical observation and astrophysics. Due to the absorption of the infrared ray by the atmosphere, there is only a limited band window for infrared observation on the ground. In order to observe the L (3.6um) and M (5um) bands, it is necessary to develop an infrared camera which is photosensitive to medium-wave infrared. According to the requirement of infrared detection, a medium-wave infrared camera is designed, including readout system as well as its testing system, thus realizing the high precision readout of medium-wave infrared detector. The medium-wave infrared camera electronic system mainly consists of a pre-amplifier board and a main board. The pre-amplifier board provides power supply and output signal amplification for the detector, while the main board provides the readout, control and communication functions. To verify the feasibility of the medium-wave infrared camera in the aspect of astronomical observation, the corresponding test platform is built, then the performance parameters of the detector such as readout noise, quantum efficiency, nonlinearity and crosstalk are tested.
13103-133
18 June 2024 • 17:30 - 19:00 Japan Standard Time | Room G5, North - 1F
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We combine the recent release of the Gaia Synthetic Photometry Catalog (GSPC) with the ability of scientific complimentary metal-oxide-detectors (sCMOS) to do high dynamic range imaging in a project to photometrically observe the brightest stars in the night sky. By stacking exposures on the order of milliseconds to avoid saturation of the primary target, the signal of GSPC catalog entries in the field-of-view rises sufficiently above background noise levels to measure photometrically. We obtain better than 2% photometry on the bright targets, despite a difference in magnitudes between target and standards of 10 or greater.
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