diff --git a/Instrument/AMDA/ACE/MAG.xml b/Instrument/AMDA/ACE/MAG.xml index 3b86234..19dd1ef 100644 --- a/Instrument/AMDA/ACE/MAG.xml +++ b/Instrument/AMDA/ACE/MAG.xml @@ -11,7 +11,25 @@ ACE MFI 1997-045A-09 2016-11-18T16:00:05Z - The ACE Magnetometer (MAG) experiment consists of two triaxial fluxgate magnetometers mounted remotely on booms extending beyond the spacecraft solar panels at four meters from the spacecraft center. Each identical sensor (M1, M2) has a wide dynamic range of sensitivity at +- 0.004 to +- 65536 nT and measures the three vector components of the magnetic field. Usage of twin magnetometer sensors for measurements of weak interplanetary magnetic fields is a proven approach based on experience from many past space missions. The MAG sensors were originally built as spares for the MFI instrument on the Wind spacecraft and have been given minor modifications for inclusion on ACE. Readout of MAG data includes three data types: (1) average magnetic field vectors from the primary and secondary sensors, (2) "Snap-Shot Memory" data, and (3) Fast Fourier Transform (FFT) data. The average vector readout includes 216 bps corresponding to six vectors per second. These vector readouts can be split between M1 and M2 in the ratios of 3:3, 5:1, or 6:0. The "Snap-Shot Memory" stores field vectors at the maximum sampling rate of 30 vectors per second and is read out at 48 bps. The FFT readout includes 17 seconds accumulation of vector data transformed into spectral matrices of the components and total magnitude at a transmission rate of 32 bps. Prof. Norman F. Ness of the Bartol Research Institute at the University of Delaware is the MAG Experiment Manager. + The ACE Magnetometer (MAG) experiment consists of two triaxial fluxgate magnetometers mounted remotely on booms extending + beyond the spacecraft solar panels at four meters from the spacecraft center. + Each identical sensor (M1, M2) has a wide dynamic range of sensitivity at +- 0.004 to +- 65536 nT and measures the three vector components of + the magnetic field. Usage of twin magnetometer sensors for measurements of weak interplanetary magnetic fields is a proven approach based on + experience from many past space missions. The MAG sensors were originally built as spares for the MFI instrument on the Wind spacecraft and + have been given minor modifications for inclusion on ACE. + + Readout of MAG data includes three data types: + * average magnetic field vectors from the primary and secondary sensors, + * "Snap-Shot Memory" data, + * Fast Fourier Transform (FFT) data. + + The average vector readout includes 216 bps + corresponding to six vectors per second. These vector readouts can be split between M1 and M2 in the ratios of 3:3, 5:1, or 6:0. + The "Snap-Shot Memory" stores field vectors at the maximum sampling rate of 30 vectors per second and is read out at 48 bps. + The FFT readout includes 17 seconds accumulation of vector data transformed into spectral matrices of the components and total magnitude at + a transmission rate of 32 bps. + + Prof. Norman F. Ness of the Bartol Research Institute at the University of Delaware is the MAG Experiment Manager. Please acknowledge the ACE/MAG instrument team and the ACE Science Center diff --git a/NumericalData/AMDA/Cluster/Cluster1/PEACE/clust1-pea-mom.xml b/NumericalData/AMDA/Cluster/Cluster1/PEACE/clust1-pea-mom.xml index d9477f0..fd70ef8 100644 --- a/NumericalData/AMDA/Cluster/Cluster1/PEACE/clust1-pea-mom.xml +++ b/NumericalData/AMDA/Cluster/Cluster1/PEACE/clust1-pea-mom.xml @@ -22,6 +22,7 @@ are used instead for the MOMENTS production (see Mode_DataOrigin_HEEA/LEEA). Choices on the best way to combine data from the two sensors can be made in the moments production software; in the first release the moments are made using LEEA data in the energy overlap region. + In some situations, use of both sensors together may be a better choice, for example in case s where the distribution changes during a spin as the method can resolve time aliasing errors. If resources allow, the Moments @@ -33,6 +34,7 @@ using default values to control the approach to potential correction and photoelectron removal, and has not been systematically human - validated, so some errors may exist. + Specifically, the spacecraft potential, Vsc, is set to be 1 V greater than the measured probe - spacecraft potential provided by the electric field experiment (EFW) and the lower energy cutoff for the moments @@ -41,6 +43,7 @@ may also contain counts due to spacecraft electrons). Sometimes cold electrons are present which can appear in the same energy bin as the spacecraft photoelectrons, therefore both the cold electrons and spacecraft photoelectrons are removed resulting in underestimated electron densities. + Recent work by the EFW team suggests a more accurate determination of from would be a term that increases linearly above ~10 V (Cully et al., 2007) but this has not yet been diff --git a/NumericalData/AMDA/Juno/JEDI/juno-jedi-e090.xml b/NumericalData/AMDA/Juno/JEDI/juno-jedi-e090.xml index fb7a89d..e5211e8 100644 --- a/NumericalData/AMDA/Juno/JEDI/juno-jedi-e090.xml +++ b/NumericalData/AMDA/Juno/JEDI/juno-jedi-e090.xml @@ -105,9 +105,6 @@ TimeSeries - - - -- libgit2 0.21.2