Past and current laser altimeter instruments in planetary research have high requirements in terms of mass, power and volume. We present a novel less resource-demanding concept based on single-photon counting techniques. The instrument concept was utilized in a flight campaign of which the setup and the data analysis is presented. A small-satellite mission to the Moon is outlined as well as further potential for miniaturization of the instrument concept.
A new setup for detector characterization consisting of a cryostat, tunable collimated light source, and versatile data acquisition system is currently being commissioned. The setup enables testing optical and infrared sensors in the 400 to 14000 nm wavelength range and the devices under test can be cooled to cryogenic temperatures of down to 50 K under vacuum condition. 32 spectral band passes with bandwidths of λ{ΔΛ ≥ 50 are available for spectral characterization, covering the full range from 400 to 14000 nm. The setup can be used to characterize responsivity, detectivity, noise equivalent temperature difference, dark current, linearity, dynamic range, well depth, and pixel response non-uniformity. We report on first results for the characterization of imaging sensors using Teledyne’s CCD47-20 as the device under test for which camera gain, linearity error, full well capacity, read noise, dark noise, and quantum efficiency have been determined. Furthermore, the performance of the light source and cryostat system will be discussed.
Both NASA’s VERITAS and ESA’s EnVision missions to Venus incorporate a Venus Emissivity Mapper (VEM) to characterize the surface and distinguish basalt from more felsic rock types. Though Venus’ optically dense atmosphere makes direct observations of the surface challenging, five windows in the CO2 spectrum near 1 μm will be exploited by the VEM instrument. In preparation for these missions, an analog of the VEM instrument (VEMulator2.0) was constructed for field measurements. It was used in a two-week field campaign at Venus-analog sites in Iceland in August 2023 as part of a VERITAS field campaign to collect multi-frequency reflectance measurements of volcanic rocks of varying age and surface conditions, as well as to measure emission from recently erupted lava with hot spots up to ~400°C. The goal of the work was to train scientists and to help assess the capability of the VEM instrument to detect differences in surface composition in a wide variety of volcanic rocks in the field with the limited spectral information provided by six bands. In addition, samples of the imaged regions were collected to be analyzed in detail at the Planetary Spectroscopy Laboratory at DLR in Berlin. Comparing field and laboratory spectra gives insights into the efficacy and limitations of the analog instrument. This paper describes the emulator design and calibration procedure as well as first results from field and laboratory measurements.
One of the main objectives of the NASA's VERITAS and the ESA's EnVision missions is to characterize the composition and origin of the major geologic terrains on Venus. Both missions carry the Venus Emissivity Mapper (VEM) – a multispectral imager - which will be able to observe the surface of Venus through five atmospheric windows with six bands, around the 1μm spectral range. This will enable the spectral characterization of the Venusian surface, as well as deduce the type of lava and likely alteration processes, providing new insights into the evolution of Venus. To improve our knowledge of the mineralogical information obtained from the 1μm spectral range, we are developing a series of "VEM emulator" (aka VEMulator). The first one was based on a commercial Raspberry PI HQ 12MP camera, containing the Sony IMX477 sensor, with a 35mm lens. Four filters with wavelengths of 860, 910, 990, 1100 nm could be attached in front of the lens similar to four of the six VEM mineralogy spectral bands. This instrument was deployed in summer 2022 on the Vulcano island in southern Italy as Venus analog site. Vulcano rocks display a diverse compositional variation from basaltic to rhyolitic, which makes this site an attractive analog to Venus. Currently, a new version of the VEMulator is being developed using the SCD Cardinal 1280 InGaAs detector – similar to the detector used in the VEM flight model. This VEMulator 2.0 will be used in Iceland, in 2023, for a VERITAS field campaign.
KEYWORDS: Microbolometers, Photodiodes, Spectral response, Dark current, Signal to noise ratio, Light sources, Data acquisition, Collimators, Quantum sensors, CMOS sensors
We report on the design of a new laboratory setup for testing the performance of optical and thermal sensors at temperatures ranging from 50 K to 350 K and pressures ranging from ambient atmospheric pressures down to 10-5 mbar. The system will be built around a closed-cycle cooled cryostat which houses the device under test. Optical stimuli will be provided by a calibrated selectable light source which provides collimated light from an integrating sphere or a cavity blackbody. Bandpass filters as well as imaging targets can be selected for determining the spectral response and modular transfer function. Data acquisition from the device under test will be accomplished using an automated test bench based on a custom-made FPGA interface adaption board.
The Fast Front End Electronic (F-FEE) is a unit of the payload for the PLATO ESA mission. PLATO aims at finding and characterising a large number of extra solar planetary systems. In order to achieve its scientific objectives, PLATO relies on the analysis of continuous time series of high precision photometric measurements of stellar fluxes. The scientific payload of PLATO is based on a multi-telescope approach, involving a set of 24 ”normal” cameras working at a cadence of 25 s optimized to monitor stars fainter than magnitude 8 (photometry on saturated stars down to magnitude 4 will be possible), plus two ”fast” cameras working at a cadence of 2.5 s, and observing stars in the V range from 4 to 8. Beside providing star brightness measurements for bright stars, the ”fast” cameras also work as fine guidance sensors for the attitude control system of the Spacecraft. Each ”fast” camera is equipped with 4 CCDs with 4510 × 2255 light sensitive pixels each, working in frame transfer mode. In view of the instrument development an Engineering Model (EM) of the F-FEE has been manufactured, assembled and tested. The performance tests have been conducted using artificially generated CCD signals as well as real CCDs, proving the capability of the electronics to satisfy the demanding requirements to fine guidance but also science requirements of the PLATO mission.
K. Enya, M. Kobayashi, K. Ishibashi, S. Kobayashi, N. Namiki, H. Araki, S. Tazawa, H. Noda, S. Oshigami, S. Kashima, M. Utsunomiya, J. Kimura, K. Touhara, T. Yamawaki, S. Iwamura, N. Fujishiro, Y. Matsumoto, T. Iida, H. Nakagawa, H. Imai, O. Kirino, C. Hatakeyama, T. Yokozawa, Y. Sato, K. Kojima, N. Matsui, K. Tanimoto, M. Fujii, C. Althaus, S. Del Togno, J. Jänchen, B. Borgs, T. Behnke, H. G. Lötzke, R. Kallenbach, K. Lingenauber, H. Hussmann
The Jupiter Icy Moons Explorer (JUICE) mission of the European Space Agency to be launched in 2022 will provide an opportunity for a dedicated exploration of the Jovian system including its icy moons. The Ganymede Laser Altimeter (GALA) has been selected as one of the ten payloads of JUICE. GALA will enable unique studies of the topography and shape, tidal and rotational state, and geology of primarily Ganymede but also Europa and Callisto. The GALA project is an ongoing international collaboration led by Germany, together with Switzerland, Spain, and Japan. This paper presents the optical and mechanical design of the focal plane receiver, the Japanese part of GALA.
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