Atmospheric Lidar The Atmospheric Lidar (ATLID) is a high-spectral resolution lidar and will be the first of its type to be flown in space.
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1 EarthCARE mission instruments ESA s EarthCARE satellite payload comprises four instruments: the Atmospheric Lidar, the Cloud Profiling Radar, the Multi-Spectral Imager and the Broad-Band Radiometer. Atmospheric Lidar The Atmospheric Lidar (ATLID) is a high-spectral resolution lidar and will be the first of its type to be flown in space. ATLID transmits linearly polarised laser signals at a wavelength of 355nm in the ultraviolet. The receiver can distinguish between the signal backscattered on atmospheric molecules from the signal backscattered on cloud and aerosol particles. At this wavelength, the molecular backscatter signal is broadened according to the Rayleigh scattering function. Laser light backscattered on particles only has a very small broadening and follows, in the case of backscatter on spherical particles, the Mie scatter functions. The lidar receiver is equipped with a very narrow wavelength filter that separates the spectrally narrow particle backscatter signal from the much broader molecular backscatter signal. This means that the signal extinction of cloud and aerosols can be distinguished from clear air absorption. Beyond the capability to distinguish molecular from particle backscatter signals, it will also gain important information about the type of observed particles. Depending on the structure of the backscattering particle, the polarisation of the incident light changes when back scattered. The receiver is therefore equipped with the additional functionality to measure the degree of change of polarisation of the backscattered signal compared to the emitted, linearly polarised signal. The use of the ultraviolet has strong benefits over laser wavelengths in the visible range. While the visible range is, in principle, technically easier, the ultraviolet has the advantage that the laser beam diverges much less than at visible wavelengths. This allows the reduction the laser footprint on the surface to just a few metres. The advantage of it is that the telescope, which collects the backscattered light, can have a small field of view. This reduces the unwanted contribution from scattered sunlight entering the telescope that would otherwise degrade the quality of the observations on the day-side of the orbit. With its narrow field of view, it is expected that the cloud and aerosol observations on the day-side of the orbit will be very close to the quality on the night-side.
2 The viewing direction of the lidar is slightly tilted away from the nadir direction. This is because ice cloud particles tend to orient themselves horizontally similar to leaves falling off a tree. This can lead to very strong reflections of the lidar signal and, subsequently, misinterpretation of the amount of ice particles. In order to reduce this effect, a 3º shift of the ATLID field of view has been implemented. The instrument points backwards nadir, so that it will be collocated with a tiny shift in time with the observations of the EarthCARE Cloud Profiling Radar. The main components of the instrument are the transmitter system and the receiver. The emitter includes the power laser head and its transmitter electronics, a beam steering mechanism (to keep the laser beam aligned with the receiver telescope field of view) and the beam expanding optics. The back-scattered laser light is collected by a Cassegrain telescope and transmitted to the receiver, which includes a background light filtering stage, a high spectral resolution filter and polarisation filter to measure, separately, molecular backscatter and particle backscatter in two polarisations. Furthermore, the receiver includes a co-alignment sensor that determines and guides the alignment of the transmitting and receiving telescopes. The ATLID instrument is being developed by Astrium SAS (FR) and its subcontractors including Selex-Galileo responsible for the transmitter under contract to Astrium GmbH (DE). Cloud Profiling Radar The Cloud Profiling Radar (CPR) is a millimetre-wave cloud radar. With its very high sensitivity it can retrieve accurately high ice clouds that impact Earth s radiation budget in particular in the upper troposphere where these clouds are abundant. In fact, 98% of radiatively significant ice clouds would be detected. Furthermore it will be able to accurately observe liquid water clouds in the atmospheric boundary layer (about 90% of it over oceans). In addition to its high sensitivity, the instrument will be the first cloud radar in space equipped with the capability to measure the Doppler shift of the backscattered radar signal, allowing the observation of vertical motions of cloud particles to an accuracy of about 1 m/s. This will allow scientists to study vertical updrafts within clouds and particle sedimentation rates. It will also enable global measurements of the fall speed of light rain. This is an important factor in the regulation of the lifetime of low-level clouds and is only poorly represented in today s numerical models.
3 Furthermore, the fall speed of ice particles, which is a critical parameter for the global occurrence of ice clouds, can be observed with the radar s Doppler measurement capability, as well as vertical motion inside convective clouds. This is crucial for the understanding of vertical transport of heat, moisture and momentum in tropical circulation and in the formation of convective precipitation. The CPR operates at a frequency of 94.05GHz, with a pulse width of 3.3 µs and a pulse repetition frequency of 6100Hz to 7500Hz. Its high accuracy offset antenna has an aperture diameter of 2.5m. The vertical resolution of the observations will be 500m and the horizontal resolution about 750m with a sampling of 500m. The minimum sensitivity is -35dBZ. The Doppler range is ±10m/s with an accuracy of 1m/s. The CPR is a contribution of JAXA in collaboration with the National Institute of Information and Communications Technology (NICT). Multi-Spectral Imager The primary objective of the Multi-Spectral Imager (MSI) is to provide imagery in support to the two profiling instruments ATLID and CPR. While ATLID and CPR provide vertical profiles along the satellite flight direction, the MSI provides images of clouds and aerosols in the across-track direction, i.e. perpendicular to the ATLID and CPR profiles. With the combination of ATLID, CPR and MSI observations it will be possible to construct three-dimensional scenes of clouds and aerosols. The scene information derived from the MSI will be an important input to the algorithms estimating the top-of-the-atmosphere radiative fluxes from the Broad- Band Radiometer measurements. The MSI takes images with a fixed nadir-viewing direction and swath of 150 km and a pixel size of 500 m. The swath is slightly tilted eastwards (on the day-side) to minimize regions contaminated by sun glint. It covers 35 km on one side to 115 km to the other side of the ATLID and CPR observations. The instrument has seven channels: four solar channels operating in the visible, near-infrared and short-wave infrared capturing reflected solar light on the day-side of the orbit, and three channels measuring the emitted thermal radiation of Earth (thermal infrared channels).
4 Spectral Channels Centre Wavelength Bandwidth (50%) Visible 0.67 m 20 nm Near Infra-Red m 20 nm Short-Wave Infra-Red m 50 nm Short-Wave Infra-Red m 0.1 m Thermal Infra-Red m 0.9 m Thermal Infra-Red m 0.9 m Thermal Infra-Red m 0.9 m The MSI instrument consists primarily of two optical heads or cameras, one dedicated to the four solar channels and one for the three thermal infrared channels, mounted on a common optical bench. The instrument includes the required calibration sun port for the visible channels and blackbody for the infrared channels. The MSI instrument is being developed by Surrey Satellite Technology (SSTL, UK) and its subcontractors, under contract to Astrium GmbH (DE). The optical head for the solar channels is provided by TNO (NL) under contract to SSTL. Broad-Band Radiometer While ATLID, CPR and MSI observations will be used for the retrieval of cloud and aerosol content and three-dimensional structure of an observed scene, the Broad- Band Radiometer (BBR) will measure the solar radiative power (solar flux) reflected back to space by the scene and the scene s emitted thermal radiative power (thermal flux). This observation will ultimately allow to link clouds and aerosols to radiation, which is the overarching objective of the EarthCARE mission. The area over which the flux is being observed by the BBR shall be collocated with the observations of the other EarthCARE instruments. The flux is defined by the radiation that leaves an area in all skyward directions. However, an instrument can only observe a part of this flux, namely the fraction that is being emitted into the direction of the instrument s field-of-view, called the radiance. If the emitted radiation is spatially homogeneous, the flux can be accurately calculated from radiance observations. If the scene is inhomogeneous, for example, in the case of inhomogeneous cloud scenes, the radiance-to-flux conversion is much more complicated and uncertain. To reduce this uncertainty, the BBR includes three independent, fixed telescopes. One telescope looks forward in the satellite flight direction and observes each scene before the satellite passes over it. A second telescope observes the scene in nadir when the satellite is right above it. Afterwards, a backwards looking telescope observes the scene for the third time under the same angle as the
5 forward-looking telescope, but this time from the other side. So each scene will be observed from three different directions. The combination of these three observations gives a much better estimate of the actual fluxes than using only one single radiance observation. Further significant improvement of the flux estimates will be achieved in the on-ground data processing taking into account scene inhomogeneity information from the MSI imagery. Each of the three BBR field-of-views measures the total radiation from 0.25µm to larger than 50µm in the Total Wave (TW) channel and, by temporarily switching a short-wave filter into the optical path, the short-wave part of the radiation in the Short Wave (SW) channel (0.25 µm to 4.0 µm). The Long Wave (LW) signal is calculated by subtraction of the SW signal from the TW signal. The actual solar signal and thermal signal (also referred to as the unfiltered radiances ) will be retrieved in the data processing by removing the effect of the instrument filter functions. The three telescopes of the instrument are oriented towards nadir, +50 and -50º, which, projected to Earth s surface results in an observation zenith angle of 55 º for the fore- and aft-view. The footprint size for each field-of-view is 10km by 10 km and the spatial sampling distance is approximately 1 km. The radiometric calibration is done using onboard hot and cold black bodies and, for the SW channel, with a solar calibration unit. The SW radiance radiometric accuracy requirement is 2.5Wm -2 sr -1, the LW requirement is 1.5Wm -2 sr -1. The BBR instrument is being developed by Systems Engineering & Assessment Ltd. (SEA, UK) and its subcontractors, under contract to Astrium GmbH (DE).
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