Fix typo + Complete BEPI/MIA description

Benjamin Renard
1 parent e247382e
Showing 3 changed files with 22 additions and 9 deletions Show diff stats
Instrument/CDPP-AMDA/BepiColombo/Mio/MEA1.xml
Instrument/CDPP-AMDA/BepiColombo/Mio/MEA2.xml
Instrument/CDPP-AMDA/BepiColombo/Mio/MIA.xml
@@ -20,7 +20,7 @@
       toroidal electrostatic analyzers, microchannel plates (MCPs), high-voltage power supplies and power supply units. 
       The analyzer selects energies of electrons from 3 eV/q up to 26 keV/q depending on the operation modes.
  
-      ==== Data Procucts: ====
+      ==== Data Products: ====
  
       MEA includes versatile and easily programmable operating modes and data processing routines for optimizing the data collection for specific scientific studies and widely varying plasma regimes. Depending on the telemetry mode, MEA can transmit several data products, including those listed below.
         * Full 3D electron distribution (3D, only for MEA1). The instrument transmits a complete angular-energy spectrum accumulated for a minimum of 1/4 of the spacecraft spin.
@@ -20,7 +20,7 @@
       toroidal electrostatic analyzers, microchannel plates (MCPs), high-voltage power supplies and power supply units. 
       The analyzer selects energies of electrons from 3 eV/q up to 26 keV/q depending on the operation modes.
  
-      ==== Data Procucts: ====
+      ==== Data Products: ====
  
       MEA includes versatile and easily programmable operating modes and data processing routines for optimizing the data collection for specific scientific studies and widely varying plasma regimes. Depending on the telemetry mode, MEA can transmit several data products, including those listed below.
         * Full 3D electron distribution (3D, only for MEA1). The instrument transmits a complete angular-energy spectrum accumulated for a minimum of 1/4 of the spacecraft spin.
@@ -14,14 +14,27 @@
       These sensors measure plasma, high-energy particles and energetic neutral atoms with sufficiently high time resolution, 
       wide energy and dynamic range, wide angle coverage, and high mass resolution.
  
-      Mercury Ion Analyzer (MIA), one of MPPE sensors onboard Mio, measures both the 3D distribution function of solar wind ions 
-      around Mercury and the planet’s magnetospheric ions to understand the structure and plasma dynamics of Mercury’s magnetosphere, 
-      Mercury-solar wind interaction, atmospheric abundances, structures, and generation/loss processes, and the solar wind at Mercury’s 
-      position. MIA consists of a top-hat type electrostatic analyzer with toroidal deflectors, microchannel plates (MCPs), 
-      high-voltage power supplies. The analyzer selects energies of ions from 10 eV/q up to 30 keV/q depending on the operation modes with 64 
-      spin angle sectors.
+      Mercury Ion Analyzer (MIA), one of MPPE sensors onboard Mio, measures both intense solar wind ions and tenuous Mercury magnetospheric ions. 
+      To measure both solar wind ions without saturation and Mercury magnetospheric ions with sufficient counting statistics, MIA includes an 
+      attenuation grid with 10% transmission placed at limited channels of the entrance part of the analyzer. 
+      In addition, MIA includes a function for reducing the geometrical factor electrically for solar wind ion measurement. 
+      The sensitivity of the analyzer can be reduced to ~ 1/50 by applying positive high voltage to the “top-cap” insulated from the surrounding structures. 
+
+      MIA has six different energy sweep modes. Energy sweep mode 0 and 1 are used mainly for solar wind ion observation. The energy range between ~ 100 eV/q and ~ 10 keV/q 
+      is exponentially divided into 128 energy steps. The difference between energy sweep modes 0 and 1 is that the sensitivity control function is either OFF or ON. 
+      Energy sweep mode 2 is referred to as the MCP protection mode, which is used for protecting part of the MCP that detects ions from the analyzer azimuthal 
+      sector with no mechanical attenuation grid. The energy range is determined not to measure intense main component of the solar wind. 
+      Energy sweep modes 3, 4, and 5 are used mainly for magnetospheric ion observation. Energy sweep mode 3, 4, 5 covers the energy range between ~ 20 eV/q and ~ 25 keV/q, 
+      between ~20 eV/q and ~5 keV/q and between ~ 5 keV/q and ~ 25 keV/q, respectively, with 32 exponentially divided steps. 
+
+      Mission Data Processor 1 (MDP1) controls MIA and is responsible for processing the data sent from MIA. In addition, it formats the telemetry data, calculates the velocity moments (VMs), 
+      and reduces the quantity of data by adding, selecting, or compressing the data. Depending on the total telemetry rate of the Mio spacecraft, 
+      three different data rates of high (H-mode), medium (M-mode), and low (L-mode) are defined. The L-mode data are continuously available. 
+      MIA produces VMs of ions (density, velocity, temperature), and compressed E-t spectrograms with limited angle, mass, energy, and time resolution as L-mode data. 
+      The M-mode data are available during about 25% of the entire observation period. MIA produces 3D counts with selected angle and time resolution as M-mode data. 
+      Although full 3D counts are produced as H-mode data, this mode is available only during limited periods.
  
-      ==== Data Procucts: ====
+      ==== Data Products: ====
  
       MIA LEVEL1 CDF files consist of three sub-levels:
       * l1: Raw data with minimal processing for an archive purpose. Not useful for most users. Logarithmically compressed counts of E-t products are not uncompressed. Onboard velocity moments are stored as CDF_UNIT2 and are not converted to physical units.