KPL/IK SERENA Instrument Kernel =========================================================================== This instrument kernel (I-kernel) contains references to mounting alignment, operating modes, and timing as well as internal and FOV geometry for the BepiColombo MPO Search for Exospheric Refilling and Emitted Natural Abundances (SERENA). Version and Date ----------------------------------------------------------------------------- Version 0.0 -- January 15, 2017 -- Marc Costa Sitja, ESAC/ESA First draft. Pending review from the SERENA instrument team and the BepiColombo SGS. References ----------------------------------------------------------------------------- 1. ``Kernel Pool Required Reading'' 2. ``Frames Required Reading'' 3. ``C-Kernel Required Reading" 4. BepiColombo MPO Spacecraft Frames Definition Kernel 5. ``BepiColombo PHEBUS - Instrument User Manual'', PHEB_UM_INST_111107_1_LATMOS, Issue 1, Release 1, Draft 4, 15th October 2015 6. ``SERENA Experiment Interface Document - Part B'', BC-EST-RS-02522, Draft 3, 12th February 2009 Contact Information ----------------------------------------------------------------------------- If you have any questions regarding this file contact SPICE support at ESAC: Marc Costa Sitja (+34) 91-8131-457 mcosta@sciops.esa.int, esa_spice@sciops.esa.int or NAIF at JPL: Boris Semenov (818) 354-8136 Boris.Semenov@jpl.nasa.gov Implementation Notes ----------------------------------------------------------------------------- This file is used by the SPICE system as follows: programs that make use of this frame kernel must "load" the kernel normally during program initialization. Loading the kernel associates the data items with their names in a data structure called the "kernel pool". The SPICELIB routine FURNSH loads a kernel into the pool as shown below: FORTRAN: (SPICELIB) CALL FURNSH ( frame_kernel_name ) C: (CSPICE) furnsh_c ( frame_kernel_name ); IDL: (ICY) cspice_furnsh, frame_kernel_name MATLAB: (MICE) cspice_furnsh ( 'frame_kernel_name' ) PYTHON: (SPICEYPY)* furnsh( frame_kernel_name ) In order for a program or routine to extract data from the pool, the SPICELIB routines GDPOOL, GIPOOL, and GCPOOL are used. See [2] for more details. This file was created and may be updated with a text editor or word processor. * SPICEPY is a non-official, community developed Python wrapper for the NAIF SPICE toolkit. Its development is managed on Github. It is available at: https://github.com/AndrewAnnex/SpiceyPy Naming Conventions ----------------------------------------------------------------------------- Data items are specified using ''keyword=value'' assignments [1]. All keywords referencing values in this I-kernel start with the characters `INS' followed by the NAIF MPO instrument ID code, constructed using the spacecraft ID number (-121) followed by the NAIF three digit ID number for one of the SIXS data item. These IDs are as follows Instrument name ID -------------------- ------ MPO_SERENA_ELENA -121510 MPO_SERENA_MIPA -121520 MPO_SERENA_PICAM -121530 MPO_SERENA_STROFIO+X -121541 MPO_SERENA_STROFIO-X -121542 The remainder of the name is an underscore character followed by the unique name of the data item. For example, the SELENA sensor boresight direction in the MPO_SERENA_ELENA frame (see [2]) is specified by: INS-121510_BORESIGHT The upper bound on the length of the name of any data item identifier is 32 characters. If the same item is included in more than one file, or if the same item appears more than once within a single file, the latest value supersedes any earlier values. Overview ----------------------------------------------------------------------------- From [5] and [6]: The Search for Exospheric Refilling and Emitted Natural Abundances (SERENA) is a single instrument composed by 4 units devoted to the detection of neutral and ionized particles in the Hermean environment. It addresses some of the main scientific objectives of the BepiColombo mission: composition, origin and dynamics of Mercury's exosphere and polar deposits; and structure and dynamics of Mercury's magnetosphere. Each unit is able to operate individually and to achieve its specific scientific objectives. In addition, the opportunity to operate sensors simultaneously greatly improves the success of scientific objectives and allows for additional objectives. The major goals of SERENA are: 1. Exosphere composition and spatial distribution and dynamics 2. Search for exo-ionosphere and its relation with neutral atmosphere 3. Surface release processes. 4. Atmosphere/magnetosphere exchange and transport processes 5. Escape, source/sink balance, geochemical cycles ELENA: ~~~~~~ The Emitted Low-Energy Neutral Atoms sensor, namely ELENA, is based on a novel shuttering mechanism to measure low energy particle distributions while keeping high directional and time correlation. This objective well fits with the idea to minimize the particle interaction with the detector up to the final stopping (Micro Channel Plate -MCP) detector element. The ELENA sensor is a Time-of-Flight (TOF) detector, based on the state-of-the art of ultra-sonic oscillating choppers (operated at frequencies up to 100 kHz) and mechanical gratings. The external collimator defines the overall ELENA FOVs and instrument aperture. It is implemented by the S/C skin opening hole surrounded by a scalloped metal shield envelope for minimizing thermal and visible radiation inputs. The collimator will be a part of the ELENA Box and will be flanged on the nadir facing wall of the instrument Integrated to the ELENA box collimator / lateral wall I/F there will be housed a metal mesh to limit the infrared input heat load from the planet albedo. The shuttering element of the ELENA spectrometer consists of two grids, finely patterned which are moved one with respect to the other, thus allowing the passage of the neutral atoms in determined time windows. By assuming 10 m as the typical peak-to-peak amplitude, a qualified ultrasonic piezo engine is able to provide the highest achievable resonance frequencies (i.e. of the order of 50-100kHz The ELENA core sensor is based on a Time-of-Flight (TOF) detector, implemented by the ultra-sonic oscillating choppers and mechanical coupled gratings. The following table provides the principal optical, performance and resolution parameters of the unit: Parameter | Units | Value/Description Remarks -------------------------+--------------+---------------------------- Optics | | | | Aperture | mm | 10 (Square apperture of | | 100 mm^2) Focal length | mm | 100 Focal number | | 10 Field of view | degrees | 4.5 x 76 (across track) Central obstruction | % | 50 Pixel IFOV | microrad | 1210 Spectral range | keV | 0.02+5 Filter bandwidth | nm | Spectral Channels | | 16 Geometry Factor | cm^2*sr | 2.5 * 10^-4 Dynamic range | cts / cm^2 | 10^4 + 10^8 | sr*KeV | | | Sensor (MCPs based) | | | | Pixel lines | # | 1 Pixels per line | # | 38 Pixel pitch | microrad | 4400 Peak quantum | % | > 50% efficiency | | Scale per pixel | | At Periherm | m/px | 1400 Smear | | At Periherm | px/s | 6 Exposure time | ms | 6000 Imaging sequence | s | 30 (Nominal Mode) duration | | Energy Resolution | % | 25 | | Resolution | | | | Spectral resolution | % | delta(E)/E = 25 Angular resolution | microrad/px | 1210 Spatial resolution | | At Periherm | m/pixel | 1400 Dwell Time | | At Periherm | s | 6 At Apoherm | s | 12 | | MIPA: ~~~~~ MIPA (Miniature Ion Precipitation Analyser) is a simple ion mass analyser optimised to provide monitoring of the precipitating ions using as little spacecraft resource as possible. The analyser is, yet, capable to measure all main groups of ions present in the magnetosphere. The energy range and mass range of the analyser is optimised to cover accelerated ionospheric ions. The following table provides the principal optical, performance and resolution parameters of the unit: Parameter | Units | Value/Description Remarks -------------------------+--------------+---------------------------- Optics | | | | Field of view | degrees | 90 x 360 (View across MPO | | track in orbital plane. | | Central axis +/- RAM dir.) Central obstruction | % | 0 Spectral range | keV | 0.01-15 Spectral Channels | | 32 (Energy steps) Geometry Factor | cm^2*sr eV | 0.19 Dynamic range | cts / cm^2 | 10^6 | sr*KeV | | | Sensor (CCEM) | | | | Exposure time | ms | 31.25 (Sampling time per | | step) Imaging sequence | s | 8 (Full energy and duration | | elevations sweep) | | Energy Resolution | % | 7 | | Resolution | | | | Angular resolution | degrees | 4.5 x 22.5 | | PICAM: ~~~~~~ The PICAM (Planetary Ion CAMera) ion mass spectrometer operates as an all-sky camera for charged particles (Vaisberg, 2001) allowing the determination of the 3D velocity distribution and mass spectrum for ions over a full 2% FOV, from thermal up to ~ 3 keV energies and in a mass range extending up to ~ 132 amu (Xenon). The instantaneous 2% FOV coupled with this mass range and a mass resolution better than ~ 100 is a unique capability, which provides to PICAM superior performances in the frame of the MPO mission. The following table provides the principal optical, performance and resolution parameters of the unit: Parameter | Units | Value/Description Remarks -------------------------+--------------+---------------------------- Optics | | | | Field of view | degrees | 90 x 360 (half sphere) Central obstruction | % | 10 Pixel IFOV | microrad | ~ 20 x 20 deg Mirror Grating and | | Striated mirror, Cu2S or Coating | | CuO surface Number of channels | | Controllable (Standard: | | 32 energies x 61 angular | | positions x (1 ... 132) | | masses) Energy range | KeV | 0.001 3 Mass range | amu | 1 ... 132 (Xe) Geometry Factor | cm^2*sr | 2.3 * 10^-4 Dynamic range | cts / cm^2 | 10^8 | sr*KeV | | | Sensor (MCPs based) | | | | Active area | mm^2 | 625 Pixel lines | # | 5 (radial positions) Pixels per line | # | le 16 (azimuthal pos.) Exposure time | ms | 32 to 1000 (typical time | | per energy step) Imaging sequence | s | 10 (typical) duration | | Energy Resolution | % | ~7 | | STROFIO: ~~~~~~~~ STROFIO is a novel type of mass spectrometer, where the mass of the particle is determined by the time of flight through a given region. The start time is imprinted on the trajectory of the particle by a radio frequency electric field, that bends the trajectory in a given plane, and the stop time is the time when the particle reaches the detector. Every particle is analysed by the system, dramatically increasing the total sensitivity of the spectrometer. Moreover, its performances will depend on fast electronics rather than on mechanical tolerances, making this type of sensors mechanical simple and easy to operate. STROFIO comprises of three major components: ionization source; reflectron, and electronics. The ionization source is the upper portion that is exposed above the spacecraft MLI, and the rest of the sensor is mounted beneath the spacecraft deck. The STROFIO sensor is composed of a cylindrical detector head mounted on an optical bench housing the detector proper and readout anodes ("MCP-Anode"); of two electronic boards stacked at the end of the cylinder opposite to the detector assemby: the HVPS; and the LVPS, filament supply and analog processing (PPB). The following table provides the principal optical, performance and resolution parameters of the unit: Parameter | Units | Value/Description Remarks -------------------------+--------------+---------------------------- Optics | | | | Aperture | mm | 10 (2 circular appertures | | of 80 mm^2 each) Focal length | mm | 300 (equivalent TOF) Field of view | degrees | 20 x 20 (RAM and anti-RAM) Pixel IFOV | microrad | 123,000 Spectral range | keV | 0-50 Filter bandwidth | nm | Spectral Channels | | 256 mass channels Geometry Factor | counts/ | 0.14 | cm^2*s | Dynamic range | particle | 10 + 10^9 | cm^3 | | | Sensor (MCPs based) | | | | Pixel lines | # | 1 Pixels per line | # | 960 (pixels spanning mass | | range) Pixel pitch | microrad | 500 Peak quantum | % | > 50% efficiency | | Exposure time | ms | 10000 (Spectrum int. time) | | Resolution | | | | Dwell Time | | At Periherm | s | 10 At Apoherm | s | 20 | | Mounting Alignment ----------------------------------------------------------------------------- Refer to the latest version of the BepiColombo Frames Definition Kernel (FK) [8] for the SERENA reference frame definitions and mounting alignment information. SERENA ELENA Apparent Field-of-View Layout ----------------------------------------------------------------------------- The ELENA unit is located on the -X panel and has a rectangular FOV of 4.5 by 76 degrees. The baffle is pointing along the Nadir direction. This diagram illustrates the SERENA ELENA apparent FOV in the MPO SERENA ELENA (MPO_SERENA_ELENA) reference frame. ^ +Yelena (across track) | | | +-|-+ --- | | | ^ ---->| | |<---- 4.5 degrees | | | | | | | | | | | | | | | | | | | | | | | | | | | | | +Xelena (along track) | | | | <------------x | | 76 degrees | | | | | | | | | | | | | | | | | | | | | <--------- | | | direction |___| _v_ of flight Boresight (+Zelena) is out of the page FOV Definitions --------------------------------------------------------------------------- This section contains assignments defining the SERENA Units FOVs. These definitions are based on the spectrometer parameters provided in the previous sections and are provided in a format consistent with/required by the SPICE TOOLKIT function GETFOV. SERENA ELENA FOV: ~~~~~~~~~~~~~~~~~ The ELENA unit is located on the -X panel and has a rectangular FOV of 4.5 by 76 degrees. The baffle is pointing along the Nadir direction. Please note that the FOV reference and cross angles are defined with half angle values. The following FOV definition corresponds to the NAIF Body Name: MPO_PHEBUS. \begindata INS-121510_FOV_FRAME = 'MPO_SERENA_ELENA' INS-121510_FOV_SHAPE = 'RECTANGLE' INS-121510_BORESIGHT = ( 0.000 0.0000 1.000 ) INS-121510_FOV_CLASS_SPEC = 'ANGLES' INS-121510_FOV_REF_VECTOR = ( 0.000 1.0000 0.000 ) INS-121510_FOV_REF_ANGLE = ( 38.000000 ) INS-121510_FOV_CROSS_ANGLE = ( 2.250000 ) INS-121510_FOV_ANGLE_UNITS = 'DEGREES' \begintext SERENA MIPA FOV: ~~~~~~~~~~~~~~~~~ The MIPA unit is located behind the radiator in the -X panel, below PICAM unit. MIPA FOV is a half sphere pointing along the -X axis. Its FOV is partially obstructed by SERENA MIPA, the MGA and the magnetometer boom. Please note that the FOV reference and cross angles are defined with half angle values. The following FOV definition corresponds to the NAIF Body Name: MPO_SERENA_MIPA. \begindata INS-121520_FOV_FRAME = 'MPO_SERENA_MIPA' INS-121520_FOV_SHAPE = 'CIRCLE' INS-121520_BORESIGHT = ( 0.000, 0.000, 1.000 ) INS-121520_FOV_CLASS_SPEC = 'ANGLES' INS-121520_FOV_REF_VECTOR = ( 1.000, 0.000, 0.000 ) INS-121520_FOV_REF_ANGLE = ( 90.0 ) INS-121520_FOV_ANGLE_UNITS = 'DEGREES' \begintext SERENA PICAM FOV: ~~~~~~~~~~~~~~~~~ The SPICAM unit is located behind the radiator in the -X panel and its FOV is nearly a half sphere, pointing along the -X axis. Please note that the FOV reference and cross angles are defined with half angle values. The following FOV definition corresponds to the NAIF Body Name: MPO_SERENA_PICAM. \begindata INS-121530_FOV_FRAME = 'MPO_SERENA_PICAM' INS-121530_FOV_SHAPE = 'CIRCLE' INS-121530_BORESIGHT = ( 0.000, 0.000, 1.000 ) INS-121530_FOV_CLASS_SPEC = 'ANGLES' INS-121530_FOV_REF_VECTOR = ( 1.000, 0.000, 0.000 ) INS-121530_FOV_REF_ANGLE = ( 90.0 ) INS-121530_FOV_ANGLE_UNITS = 'DEGREES' \begintext SERENA STROFIO FOV: ~~~~~~~~~~~~~~~~~~~ The STROFIO unit is located in +X panel. STROFIO has two baffles, one pointing along the X-axis and other along the -X axis, both have a FOV of 10 degrees half cone. Please note that the FOV reference and cross angles are defined with half angle values. The following FOV definition corresponds to the NAIF Body Name: MPO_SERENA_STROFIO. \begindata INS-121541_FOV_FRAME = 'MPO_SERENA_STROFIO+X' INS-121541_FOV_SHAPE = 'CIRCLE' INS-121541_BORESIGHT = ( 0.000, 0.000, 1.000 ) INS-121541_FOV_CLASS_SPEC = 'ANGLES' INS-121541_FOV_REF_VECTOR = ( 1.000, 0.000, 0.000 ) INS-121541_FOV_REF_ANGLE = ( 10.0 ) INS-121541_FOV_ANGLE_UNITS = 'DEGREES' INS-121542_FOV_FRAME = 'MPO_SERENA_STROFIO-X' INS-121542_FOV_SHAPE = 'CIRCLE' INS-121542_BORESIGHT = ( 0.000, 0.000, 1.000 ) INS-121542_FOV_CLASS_SPEC = 'ANGLES' INS-121542_FOV_REF_VECTOR = ( 1.000, 0.000, 0.000 ) INS-121542_FOV_REF_ANGLE = ( 10.0 ) INS-121542_FOV_ANGLE_UNITS = 'DEGREES' \begintext Optical Parameters ----------------------------------------------------------------------------- [TBW] Detector Parameters ----------------------------------------------------------------------------- [TBW] Platform ID ----------------------------------------------------------------------------- This number is the NAIF instrument ID of the platform on which the channels are mounted. For all channels this platform is the spacecraft. \begindata INS-121710_PLATFORM_ID = ( -121000 ) \begintext End of IK file.