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Fluorescence Imaging Spectrometer (FLORIS) for ESA FLEX Mission

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Fluorescence Imaging Spectrometer (FLORIS) for ESA FLEX Mission remote sensing Article Fluorescence Imaging Spectrometer (FLORIS) for ESA FLEX Mission Peter Coppo 1, Alessio Taiti 1, Lucia Pettinato 1, Michael Francois 2,*, Matteo Taccola 2 and Matthias Drusch 2 1 Leonardo, Via A. Einstein, 35, Campi Bisenzio, 50013 Florence, Italy; [email protected] (P.C.); [email protected] (A.T.); [email protected] (L.P.) 2 ESA ESTEC, Keplerlaan 1, P.O. Box 299, 2200 AG Noordwijk ZH, The Netherlands; [email protected] (M.T.); [email protected] (M.D.) * Correspondence: [email protected] Received: 10 May 2017; Accepted: 18 June 2017; Published: 23 June 2017 Abstract: The Fluorescence Explorer (FLEX) mission has been selected as ESA’s 8th Earth Explorer mission. The primary objectives of the mission are to provide global estimates of vegetation fluorescence, actual photosynthetic activity, and vegetation stress. FLEX will fly in tandem formation with Sentinel-3 providing ancillary data for atmospheric characterization and correction, vegetation related spectral indices, and land surface temperature. The purpose of this manuscript is to present its scientific payload, FLORIS, which is a push-broom hyperspectral imager, flying on a medium size platform. FLORIS will measure the vegetation fluorescence in the spectral range between 500 nm and 780 nm at medium spatial resolution (300 m) and over a swath of 150 km. It accommodates an imaging spectrometer with a very high spectral resolution (0.3 nm), to measure the fluorescence spectrum within two oxygen absorption bands (O2A and O2B), and a second spectrometer with lower spectral resolution to derive additional atmospheric and vegetation parameters. A compact opto-mechanical solution is the current instrument baseline. A polarization scrambler is placed in front of a common dioptric telescope serving both spectrometers to minimize the polarization sensitivity. The telescope images the ground scene onto a double slit assembly. The radiation is spectrally dispersed onto the focal planes of the grating spectrometers. Special attention has been given to the mitigation of stray-light which is a key factor to reach good accuracy of the fluorescence measurement. The absolute radiometric calibration is achieved by observing a dedicated Sun illuminated Lambertian diffuser, while the spectral calibration in flight is performed by means of vicarious techniques. The thermal stabilization is achieved by using two passive radiators looking directly to the cold space, counterbalanced by heaters in a closed loop system. The focal planes are based on custom developed CCDs. The opto-mechanical design is robust, stable vs. temperature and easy to align. The optical quality is very good as recently demonstrated by the latest tests of an elegant breadboard. The scientific data products comprise the Top Of Atmosphere (TOA) radiance measurements as well as fluorescence estimates and higher-level products related to the health status of the vegetation addressing a wide range of applications from agriculture to forestry and climate. Keywords: fluorescence imager; FLEX mission; Sentinel-3 1. Introduction and Objectives Observing the plant functional status from space represents a major interest for farming, forest management, and assessment of the terrestrial carbon budget. The measurement of solar induced chlorophyll fluorescence [1] directly addresses the photosynthetic efficiency of the terrestrial vegetation layer and complements traditional reflectance measurements used to infer parameters like Leaf Area Remote Sens. 2017, 9, 649; doi:10.3390/rs9070649 www.mdpi.com/journal/remotesensing Remote Sens. 2017, 9, 649 2 of 18 Index (LAI) or chlorophyll absorption [2]. Fluorescence estimates provide an early and more direct approach for diagnosis of the functioning and health status of vegetation. In fact the fluorescence emission is in competition with the photochemical conversion and may allow more accurate carbon assimilation estimation and earlier stress detection than is possible from only reflectance data [3]. The FLuorescence EXplorer (FLEX) mission has been selected for the ESA Earth Explorer EE8 program [4]. FLEX will fly in tandem with Sentinel 3 mission, making use of data synergy with other visible reflectance (from OLCI, [5]) and surface temperature data (from SLSTR, [6,7]). The FLuORescence Imaging Spectrometer (FLORIS) is the FLEX payload. It will be mounted on a medium/small size satellite and fly in a Sun synchronous orbit at a height of about 815 Km. Two different spectral channels with high spectral sampling (0.1–2 nm) have been implemented by means of two spectrometers with spatial co-registration enhanced by design using a common fore-optics with ground spatial sampling of 300 m and swath of 150 km. High efficient anti-reflection coatings, super-polished surfaces, tight particle contamination control and holographic gratings are essential to control the spatial and the spectral stray-light, which have a direct impact on the fluorescence measurement accuracy within the O2 absorption bands. The operative spectral region is selected by a band pass filter, placed in front of the scrambler. Out of band stray-light is also mitigated by using two additional filters, one for each channel, coated on two folding mirrors placed near the double slit assembly. The developed design is robust, stable versus temperature, easy to align and with good optical quality for the whole field of view including excellent corrections of transverse chromatic aberration and distortions (keystone and smile). A thermally stabilized optical bench and three cooled back-side illuminated high speed CCDs detectors are used to guarantee the required Signal to Noise Ratio (SNR) and stability accuracy (spectral and radiometric) between two consecutive on board calibrations. For the absolute radiometric calibration a dedicated Lambertian diffuser illuminated by the sun can be inserted as first element in the optical path by means of a rotating wheel, while spectral calibration is achieved by observing the atmospheric and/or the sun absorption lines (vicarious technique). The thermo-mechanical layout on a very thermal stable Al6061 alloy Optical Bench (OB) has been chosen in order to minimize volume and mass, thus reducing costs and impact on the satellite interfaces and simplifying the Assembly, Integration and Tests (AIT). All optics, detectors and Front End Electronics (FEEs) are attached with titanium/aluminum supports on the optical bench and there are two radiators in the upper position of the instrument completely in view of the cold space for an effective thermal control. These radiators are needed to dissipate heat from detector units and FEEs. The purpose of this paper is to present the state of art of the FLORIS instrument at the start of the phase B2/C/D. The principal requirements are discussed in Section2 in comparison with the foreseen achievable performance. In Section3 the instrument baseline design is presented, including the optical and the detector architecture. The mechanical layout and in-flight calibration architecture are reported respectively in Sections4 and5, while the on ground calibration/validation activites and the principal performance are described respectively in Sections6 and7. The paper will end with a brief discussion of the elegant breadboard activities (Section7), conclusions (Section8) and outlook (Section9). 2. Main Instrument Requirements The key requirements for the instrument design and sizing are summarized in Tables1 and2. Four spectral bands can be clearly identified in the requirements (Table2): - Low Resolution (LR): (500 nm–677 nm) & (697 nm–740 nm) -O 2-B: (677 nm–697 nm) -O 2-A: (740 nm–780 nm) Two spectrometers have been implemented to cover the required spectral range: the LR (Low Resolution) spectrometer for the Low Resolution bands (range 500–758 nm) with un-binned Spectral Remote Sens. 2017, 9, 649 3 of 18 Sampling Interval (SSI) of 0.6 nm/px and the HR (High Resolution) spectrometer for the two oxygen bands (range 677–697, 740–780 nm) with un-binned SSI of 0.0933 nm/px. A spectral binning ×3 and ×5 can be selected in some specific bands to meet the SSI requirement (Table2). The spectral range 677–697 nm and 740–758 nm is also acquired by the LR spectrometer for HR-LR spectral inter-band co-registration. Table 1. Principal FLORIS specification and performance. SSD = Spatial Sampling Distance, ARA = Absolute Radiometric Accuracy, RSRA = Relative Spectral Radiometric Accuracy, RXRA = Relative Spatial Radiometric Accuracy, ISRF = Instrument Spectral Response Function, FWHM = Full Width Half Maximum, ALT/ACT = ALong/ACross-Track, DOP = Degree Of Polarisation, SEDF = System Energy Distribution Function, p = ACT detector pitch, F = focal length, ts = sampling time, H = satellite altitude, GTO = Ground To Orbit, BOL = Begin Of Life, EOL = End Of Life., TBC = To Be Confirmed. Requirement Specification Performance Comments Mission lifetime 3.5/5 years 5 years - Sun zenith < 75◦, Coverage −56◦ < latitude < 75◦ −56◦ < latitude < 75◦ Observ. zenith < 15◦ Satellite height 805–830 km 805–830 km Sentinel 3 orbit. Swath width >150 km >151 km H > 805 km. <288 m (along-track) H < 830 km, p = 84 µm, SSD <300 m (nadir) <300 m (across-track) ts = 43.5 ms Image Quality <1.2 SSD 1.1 SSD FWHM of SEDF. Spatial co-registration Keystone negligible wrt telescope <0.15 SSD <0.15 SSD (HR or LR) lateral color. HR versus LR spatial <0.1 SSD 0.08 SSD At instrument level. co-registration knowledge Geo-location accuracy <0.4 SSD 0.24 SSD At instrument level. Smile (0.4 SSI) negligible wrt to Spectral co-registration <2 SSI 1.2 SSI O2A-O2B detectors alignment. <±0.1 SSI (orbit) <±0.1 SSI Stabilized optical bench (±1 ◦C) Spectral stability <±1 SSI (lifetime) <±1 SSI and detector (±0.1 ◦C). Incl. on-ground characterization, ISRF knowledge <2% 1.6% GTO and BOL-EOL variations. HR Straylight 0.2 (L0) <0.8 (L0) At 40 SSD from the edge of a bright (mW/m2/sr/nm) 0.04 (L1b) 0.04 (L1b) zone. L1b performance TBC. Absolute and Relative ARA/RSRA/RXRA 5%/1%/0.5% 5%/1%/0.5% Radiometric Accuracy.
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