|
|
1.INTRODUCTIONOnly high orbits (e.g. Geostationary or Geosynchronous) enable quasi-permanent Earth Observation, thus favouring them for military or civil surveillance missions. To be really attractive, quasi-permanence has to be coupled with high resolution (typically metric or decametric) and with sufficiently large field of view. Knowing that the resolution of an observation instrument is roughly proportional to its diameter and to the inverse of the platform altitude, high resolution from high orbits implies very large diameter telescopes (~ 10 m). Such instrument dimensions induce problems of mass, volume and launcher accommodation. In this context “classical” technology clearly shows its limits. Optical Aperture Synthesis (OAS) has been identified as a candidate to access such missions.· OAS has been used for on ground astronomy for several years [1] and we believe that its application to extended sources imagery (e.g. for Earth observation) might be envisaged within 15/20 years [2], [3]. In this study, we have analysed interferometer configurations adapted to a 1.2 m nadir Ground Sampling Distance (GSD) and a 40 × 40 km² field of view (FOV) requirements. The two known types of interferometer have been considered, their main characteristics are briefly recalled in Fig. 1. Fizeau type interferometers behave in the field of view like a classical telescope, apart from aberrations linked to the primary mirror segmentation. Michelson type interferometers, without any particular attention in the design, are not imager instruments. Rules to respect in order to obtain images with such interferometer concepts can be found in [4] and [5]. 2.QUALITY IMAGE CRITERIA AND DIMENSIONING METHODOLOGY FOR OAS INSTRUMENTS2.1Image chain simulationInterferometers are mainly characterized by their synthetic entrance pupil composed of collectors which number, position and diameters have to be defined wrt mission requirements. To perform the synthetic pupil selection, we have developed an image chain simulation detailed in Fig. 2. This simulator generates a raw image, taking into account the Modulation Transfer Function (MTF) related to each acquisition chain component. Perturbations can be injected in the simulation in order to derive the sensitivity of the considered concept. 2.2Image quality criteria determinationThe particular shape of an interferometer MTF has two main consequences. Firstly, the raw image is not directly exploitable. Secondly, “classical” image quality criterion like MTFxSNR are not anymore adapted to the sizing of OAS instruments. That is why the simulator also includes image processing algorithms (deconvolution, denoising) to restore an exploitable image and allows to quantify OAS dedicated Image Quality (IQ) criteria. Comparing this image with an ideal one simulated at the required resolution allows to quantify the contribution of acquisition noise, aliasing and incomplete deconvolution to IQ (see Fig. 3), on sub-regions containing low, middle and high frequencies. The sensitivity to perturbations in the image chain can also be derived with this tool (in particular to estimate the sensitivity to co-phasing errors). 2.3Synthetic pupil selectionThe simulation process presented here above has been used for synthetic pupil selection. The first step consists in establishing the IQ criteria objectives by simulating a monolithic telescope fulfilling classical MTFxSNR criteria given by CNES. Numerical values of the IQ contributors of this monolithic configuration are then derived and used as goal for the OAS configuration ones. A pre-selection of OAS configurations, of which MTF support is compatible with the specified resolution, is performed. A possible approach to optimise the frequency plane coverage is presented in [6]. IQ of each OAS configuration is then simulated in order to estimate the required SNR and thus the related integration time. In case of too large integration time, the tested configuration is rejected or modified by increasing the collecting area. This method is illustrated in Fig. 4. Several pupil configurations, with different numbers of pupils, diameters and positions in the plane have been selected with respect to required IQ criteria (Table 1). All of them are inscribed in a 10 m diameter circle. Table 1Selected pupil configurations. Reference [7] details particular applications of the Multi-instrument configuration A trade off analysis has been performed to select the entrance pupil configuration studied during the optical design phase. The trade-off criteria used are the following:
2.4Planar configurationsAfter giving a mark to each configurations, two circular ones, the 6-pupil (D = 2.5 m) and the 9-pupil (D = 1.8m) have been selected. The 6-pupil configuration relaxes significantly the instrumental design and co-phasing complexity, the in-shroud stacking and the deployment. A 35 % pupil weight reduction and a 40 % integration time decrease are foreseen with respect to the 9-pupil configuration ones. However these advantages are mitigated by the technological gap related to the manufacturing of high performance mirrors larger than 1.8 m. Developments of manufacturing and control means for 2.5 m diameter mirrors seems too costly and incompatible with current development plans. The 9-pupil circular configuration (D = 1.8 m) is thus selected as the best compromise wrt design complexity relaxation, reduction of sub-pupil number and realistic sub-pupil diameter. This configuration is retained for the optical concept analyses presented in the following section. Table 2Estimated integration time and required SNR of the selected 9-pupil circular configuration
2.5Linear configurationThe linear configuration is particular since it does not allow to obtain instantaneously the required resolution in all the directions. A full resolution image is reconstructed by combining/deconvolving a set of sub-images acquired during the pupil rotation along the line of sight axis. This particular configuration allows to reduce the required number of pupils and could avoid deployment as far as the linear telescope system is compatible with a vertical in-shroud stacking. Such concepts are patented by Alcatel Alenia Space [8]. However, this solution reveals drawbacks:
This solution, even if potentially interesting, shows a higher level of criticality than planar solutions. We do not mean that it is not conceivable but it would need a particular study in order to reach the same level of confidence than for the other configurations. Linear solution is not retained in the frame of this study. 3.OPTICAL CONFIGURATIONS FOR FIZEAU AND MICHELSON INTERFEROMETERSThe two types of interferometers have been considered for the analyses of the optical configuration. 3.1Michelson configurationThe Michelson configuration is composed of 9 afocal telescopes plus an optical system dedicated to the combination of the beams. The optimization of the afocal configuration has been performed after analyses of the magnification impact on the aberrations and of the required number of optical surfaces. Numerical simulations have shown that a magnification of 9 is compatible with IQ requirements at the FOV edge without vignetting. The analyzed 2-mirror telescopes have shown unacceptable levels of field curvature. A three-mirror Korsch configuration has thus been selected for the afocal telescopes. Centred and Off-axis Korsch configurations have been analyzed. Considering the combiner, no satisfying two-mirror configurations has been found. For the three-mirror configurations, two types have been studied: Korsch and Gregory. The selected one is the Gregory one to its higher level of compactness. It is illustrated in Fig. 6 with one of the afocal telescopes. Optical performance of this configuration is compatible with the required FOV, a Strehl ratio of 97 % (panchromatic) is estimated at the edges of the field. 3.2Fizeau configurationThe Korsch optical layout has been selected in order to have a real pupil inside allowing the introduction of a compensation for the line of sight jitter and the wavefront errors (WFE) residuals. Two alternatives have been considered: These two options have been studied with varying primary-secondary distance from 22 m to 6.5 m. Fig. 7 illustrates an off-axis one. Only the centred option is compatible with a primary-secondary distance lower than 11m and thus has been selected to avoid the deployment of the secondary mirror. The corresponding optical performance is also very good since a 99 % Strehl ratio is estimated at the FOV edge. Note that this level of performance is maintained when increasing the field up to a 80 km x 80km FOV. 4.CO-PHASING APPROACHMulti-pupil telescopes are based on discontinued mirrors which shape or stability cannot be only ensured by the mechanical stiffness of the supporting structure. The main perturbations identified are the line of sight instability, the sub-pupils alignment errors (piston and tip-tilt) and the high order WFE. In order to circumvent these perturbations, a real-time correction by a co-phasing system is required. The following chronogram (Fig. 8) illustrates the proposed correction logic for both Fizeau and Michelson concepts. The logic is similar for both concepts except for the first steps which consist in aligning the secondary and primary mirror segments for Fizeau and the afocal telescopes for Michelson. 4.1Details of the co-phasing approach
Given opto-mechanical perturbations representative of launch, deployment and in-orbit injection conditions as well as thermo-elastic effects, it has been shown that the proposed co-phasing approach is able to bring back the optical system to the required alignment level. 5.TRADE-OFF ANALYSISAfter the investigation of each interferometer type, a trade-off analysis has been perform to select the more adapted concept for the foreseen mission. Trade-off criteria selected for this exercise are:
Table 3Trade-off criteria notation for the two configurations As a result to this trade-off analysis, the Fizeau type interferometer has been selected in the framework of this study. The following architecture phase of this study has lead to an original opto-mechanical concept not presented here as patent pending. 6.CONCLUSIONGiven a set of IQ criteria, quantified in order to answer the mission specified by CNES, 12 pupil configurations have been proposed in the frame of this study. After a first trade-off, the 9 circular sub-pupil configuration has been selected (∅pupil = 1.8 m, ∅base ≈ 10m). This selected configuration has been used to analyze optical configurations for each interferometer type (Fizeau and Michelson). The Fizeau configuration is a 3-mirror Korsch configuration where each sub-pupil is a segment of the primary mirror. The Michelson configuration is made of afocal collectors (Korsch centred with a magnification of 9) which output beams are injected in a 3-mirror combiner (Gregory type). In parallel to this optical configuration study, co-phasing and line of sight stabilization systems have been analyzed. A control logic has been proposed, from the in-orbit injection to the fine stabilization during acquisition, in accordance with the mission requirements. Phase diversity has been selected to measure the WFE and corrections are ensured: either by a deformable mirror and the M1 segments for the Fizeau, or by piston and tip-tilt mirrors for the Michelson. Given these pupil configurations, optical analyses, co-phasing strategies and adding mechanical architecture criteria, a trade-off has been performed between the Fizeau and Michelson interferometers. Result of this trade-off shows a significant advantage of the Fizeau, mainly for optical, mechanical aspects and control complexity in the case of the Michelson. 7.7.REFERENCESQuirrenbach A.,
“Optical Interferometry,”
Annu. Rev. Astron. Astrophys, 39 353
–401
(2001). Google Scholar
Blanc P., Thomas E., Falzon F.,
“Imagerie de la Terre à Haute Résolution par Synthèse d’Ouverture Optique,”
Bulletin Bibliographique POLOQ, Délégation Générale pour l’Armement, Groupe de Prospective Orientée sur les Lasers et l’OptroniQue,
(2004). Google Scholar
Mugnier., L., Cassaing., F., Sorrente, B., Baron, F., Velluet, M.-T., Michau, V., Rousset., G.,
“Multi aperture optical telescopes: some key issues for earth observation from a geo orbit,”
in International Conference on Space Optics,
(2004). Google Scholar
Harvey J.E., Ftaclas, C.,
“Field-of-view limitations of phased telescope arrays,”
App. Opt, 34 25
(1995). Google Scholar
Traub W.A.,
“Combining beams from separated telescopes,”
App. Opt, 25
(4),
(1986). Google Scholar
Nguyen T., Boissonnat J-D., Blanc P., Falzon F., Thomas E.,
“Pupil Configuration for Extended Source Imaging with Optical Interferometry: a Computational Geometry Approach,”
in To be published in the proceedings of ICASSP,
(2006). Google Scholar
Thomas, E., Blanc P., Falzon F.,
“A new concept of synthetic aperture instrument for high resolution Earth observation from high orbits,”
in proceedings of the Symposium Disruption in Space,
4
–6
(2005). Google Scholar
Blanc P., Thomas E., Falzon F.,
“Instrument d’observation à Synthèse d’Ouverture Optique en mouvement et procédé associé,”
(2003). Google Scholar
Baron, F., Cassaing, F., Blanc A., Laubier, D.,
“Cophasing a wide field multi-aperture array by phase diversity: influence of aperture redundancy and dilution,”
SPIE, 4852 663
–673
(2003). Google Scholar
|
