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1) Cluster Salsa Digital Wave Processor (DWP) prime parameter data at about 4 sec resolution (spin averaged) in GSE Coordinates maxmize
Resource ID:spase://VMO/NumericalData/Cluster-Salsa/DWP/PrimeParameter/PT4S
Start:2000-11-01 00:00:00 Observatory:Cluster FM6 (Salsa) Cadence:4 seconds
Stop:2009-12-30 23:59:59 Instrument:Digital Wave Processor (DWP) Resource:NumericalData
Cluster Salsa Digital Wave Processor (DWP) data set contains various instrument status and data status flags as well as particle correlator information.

2) Cluster Digital Wave Processor (DWP) summary parameter data at about 60 sec resolution (spin averaged) in GSE Coordinates maxmize
Resource ID:spase://VMO/NumericalData/Cluster/DWP/SummaryParameter/PT60S
Start:2000-11-01 00:00:00 Observatory:Cluster FM5 (Rumba) Cadence:60 seconds
Stop:2009-12-30 23:59:59 Instrument:Digital Wave Processor (DWP) Resource:NumericalData
Cluster Digital Wave Processor (DWP) data set contains various instrument status and data status flags as well as particle correlator information.

3) STEREO WAVES (SWAVES) PDF Dynamic Spectrogram Plots both Ahead and Behind s/c maxmize
Resource ID:spase://VWO/DisplayData/STEREO/SWAVES/DS.Color.PDF.P1D
Start:2006-10-27 20:24:42 Observatory:STEREO A Cadence:1 minute
Stop:2016-05-19 13:23:47 Instrument:STEREO-A Waves (SWAVES) Resource:DisplayData
This dataset contains 24 hour duration dynamic spectrogram plots from the combined STEREO A and B Waves instrument. The plots are provided in several file formats (PNG, Postscript and PDF) and there are renditions in color and grayscale with and without additional lines of time series data indicating the instrument operating status. These plots all reside within the same directory structure subdivided by year. The "new" subdirectory contain plots at a higher resolution but currently are not available for dates early in the mission. These data consist of output from the SWAVES HFR and LFR receivers. ? the High Frequency Receivers (HFR) - for spectral analysis and direction finding of radio noise generated from a few solar radii (16 MHz) to about half an Astronomical Unit (125 kHz) ? the Low Frequency Receiver (LFR) - for spectral analysis and direction finding from about half an Astronomical Unit (160 kHz) to one AU (2.5 kHz).

4) STEREO WAVES (SWAVES) Radio Intensity Spectra, both Ahead and Behind s/c maxmize
Resource ID:spase://VWO/NumericalData/STEREO/SWAVES/DS.Combined.PT1M
Start:2006-10-27 20:24:42 Observatory:STEREO A Cadence:1 minute
Stop:2016-05-19 13:23:49 Instrument:STEREO-A Waves (SWAVES) Resource:NumericalData
The CDF file contains 1 minute averaged radio intensity data from both the Ahead and Behind s/c. A description of the STEREO/WAVES instrument is provided in: Bougeret, J.L, et al. (2008), S/WAVES: The Radio and Plasma Wave Investigation on the STEREO Mission, Space Science Reviews, 136, 487-528. The STEREO / WAVES (SWAVES) instruments provide unique and critical observations for all primary science objectives of the STEREO mission, the generation of CMEs, their evolution, and their interaction with Earth's magnetosphere. SWAVES can probe a CME from lift-off to Earth by detecting the coronal and interplanetary (IP) shock of the most powerful CMEs, providing a radial profile through spectral imaging, determining the radial velocity from ~2 RS (from center of sun) to Earth, measuring the density of the volume of the heliosphere between the sun and Earth, and measuring important in situ properties of the IP shock, magnetic cloud, and density compression in the fast solar wind stream that follows. SWAVES measures the fluctuation electric field present on three orthogonal monopole antennas mounted on the back (anti-sunward) surface of the spacecraft. Each monopole antenna unit is a 6 m long Beryllium-Copper (BeCu) ?stacer? spring. The three units deploy from a common baseplate that also accommodates the preamplifier housing. The 6 m length was chosen to put the antenna quarter-wave resonance near the top of the SWAVES HFR2 frequency band. These data consist of output from the SWAVES HFR and LFR receivers. ? the High Frequency Receivers (HFR) - for spectral analysis and direction finding of radio noise generated from a few solar radii (16 MHz) to about half an Astronomical Unit (125 kHz) ? the Low Frequency Receiver (LFR) - for spectral analysis and direction finding from about half an Astronomical Unit (160 kHz) to one AU (2.5 kHz).

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