During the last few years, one of our main research topics has been developing a new type of spectropolarimeter intended for space applications. Initially analyzed numerically, the instrument has a compact, stable design without rotating components. The entire Stokes vector can be determined in a single shot in a vast spectral range. The simulations proved that the modulation schemes that can be obtained for this instrument are close to the optimal form. The objective of the current research is the experimental validation of this instrument. Here, we present the first results for determining the instrumental matrix and the demodulation results for a series of polarization states. In conclusion, we present the possible further developments of that project.
The number of satellites is rapidly growing, hence the demand for increasingly precise knowledge of the satellites’ orbital parameters is essential to avoid collisions, debris, and efficient use of the orbits. Recognizing, cataloging, and measuring with better confidence are actions crucial to preserve the health of crewed and uncrewed flying objects. Moreover, strategies to distinguish them may vary: TNO is developing suitable optical instrumentation for flying object reconnaissance along these two main paths. The satellite license plate (SLP) is a collaborative method based on a tag mounted on the satellite before launch. This plate consists of retroreflectors and wisely arranged bandpass filters. Therefore, it is passive and needs no power as opposed to an onboard radio beacon. Once a ground-based laser terminal illuminates the tag attached to the satellite, it sends back to Earth a signal encoding a unique identifier in the spectral domain. The current activities of TNO focus on proof-of-principle experiments in relevant environments (free-space tests over 2.5 km distances) and system design.
A novel method for space object identification is proposed, based on full Stokes spectropolarimetry in the visible and near-infrared wavelength range. Space objects that have been previously detected and are illuminated by the sun can be observed with a telescope to simultaneously obtain intensity, spectra, and polarimetry, and compose light curves of these parameters as function of time. The intention is to thus assign a unique identification, or at least a classification to these objects. Single, double, and multiple reflections of sunlight off the space object (natural or artificial objects, including debris) will introduce spectrally dependent polarisation into the scattered light, the spectral signature of which is affected by the complex refractive index of the scattering materials and the geometry. The simultaneous measurement of the full Stokes vector allows separation of the light source unpolarised spectral signatures on the one hand from the polarisation spectral features on the other hand. To illustrate the concept, we have performed a number of simulations for double scattering off a small selection of materials, for a large range of scattering geometries. Examples of individual scattering geometries and statistical summaries of all geometries are presented. A demonstrator spectropolarimeter is being built, we present an overview of the design and the high level planning, as well as some predicted performance parameters.
The cheapest method for an instrument to perform radiometric monitoring in orbit is to compare its radiometric response from a scene to the known radiance of that same scene. This is known as vicarious calibration. The known radiance of this scene comes mostly from other space instruments. The limiting factors of this vicarious calibration approach arise from differences in the acquisition time and illumination/viewing geometry between the two measurements. Earth scenes may change over time, which limits vicarious calibration to quasi stable scenes. The level of stability of these scenes limits the level of accuracy that can be achieved. Likewise, the bi-directional scattering distribution function (BSDF) of the observed scene is likely to cause differences in observed radiance if the illumination and/or viewing geometry changes. If the observation of the scene is at the same time, stability of the scene is no longer an issue, and if the observation is at the same geometry then BSDF effects will cancel, and direct comparison is possible. This is rarely the case unless the instrument is on the same satellite. In this paper we present the design and measurement concept of such a small, on-board calibration instrument; the Absolute Radiometric Reference Instrument (ARRI). We believe this concept will revolutionize the approach to in-orbit absolute reflectance calibration.
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