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Availability: Archived at NSSDC, accessible from elsewhere


This description was generated automatically using input from the Planetary Data System.

Data Set Overview

The Juno Waves calibrated burst waveform full resolution data set includes all high rate science electric field waveforms from 50Hz up to 45.25 MHz and magnetic field waveforms from 50Hz to 20kHz with sample rates that depend on the receiver used to obtain the waveforms. This is the complete waveform data set containing all high rate binning mode data and record mode data received from Waves from launch until the end of mission including initial checkout, the Earth flyby, the Jupiter orbits and cruise. Data are acquired from the Waves Low Frequency Receiver (LFR) and High Frequency Receiver (HFR) and are typically losslessly compressed on board. These data are presented in binary SERIES objects. This data set comprises highest temporal resolution data obtained by Waves (or all other Juno instruments, for that matter). Pre-rendered spectrograms generated from these data are included as well to provide the user with a quick view of the content of the data. This data set should be among the last used of any in the Waves archive as it provides highly detailed information on very short isolated intervals in time. The Waves full resolution survey data provide context for these data.


This data set consists of calibrated electric and magnetic field waveforms obtained in the following manner: 1. Magnetic field waveforms from the LFR receiver B Channel sampled at a rate of 50 ksps with 16 bit resolution. 2. Electric field waveforms from the LFR receiver Lo-E Channel sampled at a rate of 50 ksps with 16 bit resolution. 3. Electric field waveforms from the LFR receiver Hi-E Channel sampled at a rate of 375 ksps with 16 bit resolution. 4. Electric field waveforms from an HFR receiver Baseband Channel with a sample rate of 7 Msps with 12 bit resolution. 5. Electric field waveforms from an HFR receiver Paired-Mixer Channel in a selected 1-MHz bandwidth sampled at a rate of 1.3125 Msps with 12 bit resolution. Each set of waveforms are sampled regularly at the rates stated above to comprise a series of samples of at least 1024 samples. Series length may vary by instrument mode, compression efficiency and for other reasons. Because of telemetry limitations, none of the receivers is the sampling continuous in time. After a 1024 sample collection, there will be a time gap of a fraction of a second or more. These gaps are important to understand should the data be Fourier transformed, as including the gaps in a Fourier transform will introduce artifacts into the resulting spectrum. Electric Antenna Length ----------------------Originally Waves Survey electric field data were calibrated using an effective antenna length of 2.41 m based on the geometry of the deployed, physical antenna elements. Starting with release 14 (Sept. 2020) the effective antenna length was revised to 0.5 m and all previously released data product files were regenerated and re-released using the new value. The rationale for this revision is summarized below. In very simple terms, the Waves instrument measures the differential potential between the two elements of the electric antenna. The electric field E is simply: -V/Leff where V is the measured potential and Leff is the effective antenna length. The pre-launch calibration utilized the geometric antenna length which is basically the distance between the mid-points of the two conducting antenna elements, 2.41 m. The second revision calibration modifies this length by two important electrical considerations. These are discussed in detail by Kurth et al. (2017), but the first involves taking the complex and large surrounding spacecraft structure, including the solar panels, into account. This structure is the ground plane for the antenna system. Given the very short antenna elements (2.8 m) in the presence of the spacecraft with ~ 8-m solar panels and associated structure, the spacecraft effectively decreases the effective length of the antenna system. This effect was studied by Sampl et al. (2012; 2016), using both an analog rheometry analysis as well as a surface patch model of the spacecraft. The result is that the antenna has an effective length, after taking into account the complex ground plane of the spacecraft of 1.46 m. The second effect is a capacitive divider effect due to the base capacitance of the antenna and the capacitance of the antenna to space. While the base capacitance is somewhat uncertain, this is effectively a decrease in sensitivity (equivalently, another decrease in effective length) of 8 db. Combining these, we've used an effective antenna length of 0.5 meters for the Juno electric antenna in the second revision calibration tables. Clearly, this means the newly-calibrated electric field associated with a 1-V potential difference is 4.8 times greater than the old one. And, spectral densities that are proportional to E**2 will increase by a factor of about 23.


Data products for this data set were generated by the CDR data production pipeline as described in section 3.3.2 of the VOLSIS document found under the DOCUMENTS sub directory. The inputs to the processing are: 1. Science and housekeeping packets from the Waves Level 2 data set. 2. Calibration tables located on this volume. 3. NAIF Juno mission SPICE kernels. 4. A listing of mission phase names and orbit number by UTC. The result of the processing is one file per receiver band per burst interval. The WAVES_CAL document in the DOCUMENT directory provides details of the calibration process. These data are calibrated using the best calibration tables and algorithms available at the time the data were archived. Should a significant improvement in calibration become available, an erratum will be noted in the erratum section. Initial calibrations of the electric field waveforms from an HFR receiver in a selected 1-MHz bandwidth (data set 5 above) are currently being reanalyzed and improved. Later versions of the products will contain better calibrations. The calibration for these data are performed, basically, by applying a multiplicative factor to the waveform based on the receiver gain (including any gain/attenuation settings) at the center of the receiver band. An alternate method of calibrating these data is to Fourier transform the data, apply the frequency response of the receiver (convoluted with the preamp, where necessary), apply the gain factor, and then perform an inverse Fourier transform. The information required to perform this type of calibration, starting from the EDR data set is provided in the calibration documentation on this volume, however, it is not the intention of the Waves team to archive data using this calibration method.


The Waves calibrated burst waveform data set includes files from each of the receiver/sensor combinations from which there are waveform data for the burst interval. These include magnetic field waveforms the LFR-LO receiver, and electric field waveforms from both the LFR-LO and LFR-HI, the baseband of an HFR as well as one or more of the upper spectrum paired-mixer bands of an HFR. Each file contains a fixed number of fields containing the measurement initiation times by spacecraft clock and UTC, a flag to indicate the employment of on-board noise mitigation techniques, a column indicating the count of data samples (as opposed to fill) in the row, as well as one field, with an item for each waveform sample.

Ancillary Data

Ancillary data included with the data set collection include a series of files that describe the Waves operating modes as a function of time and provide a time-ordered listing of the Instrument Expanded Block (IEB) trigger commands (WAV_MAJOR_MODE) (the mode by which Waves is reconfigured). Also a detailed description of each of the modes (or IEBs) is provided. Other data which are ancillary to this data set, but which are archived separately from this collection are the Navigation and Ancillary Information Facility's SPICE kernels describing the position and attitude of Juno and various solar system bodies as a function of time.

Coordinate Systems

The data in this data set are measurements of electric and magnetic field waveforms measured by the Waves electric and magnetic sensors. These fields are presented as detected by the sensors and are not rotated into any other coordinate system. If desired the SPICE kernels can be used with the SPICE toolkit to convert from the spacecraft frame to virtually any frame which may be of use in analyzing these data. However, for many purposes, because of the broad beam of the dipole-like sensors, the waveforms are extremely useful and may be entirely adequate with no coordinate transformations at all.


TBD - We may include software to output these data as ASCII comma separated values.


This data set is provided to the Planetary Data System electronically as part of a volume level 'tarball' file, though the standards for file names, directory names and path lengths follow the guidelines provided in the 'Planetary Data System Standards Reference', version 3.8, under section 10.1.3, 'Specification for Files Delivered Electronically'. The 'tarball' file contains all files for a release of this volume in a single GNU Tar file that has then been compressed via the GNU gzip utility. The tar file preserves the relative directory path for each file so when unpacked the original volume directory structure is recreated. See Section 4 of the VOLSIS for more details on the data transfer methods.

These data are available on-line from the Planetary Data System (PDS) at:

Alternate Names



  • Planetary Science: Fields and Particles

Additional Information



Questions and comments about this data collection can be directed to: Dr. David R. Williams



NameRoleOriginal AffiliationE-mail
Dr. William S. KurthGeneral ContactUniversity of
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