PDS_VERSION_ID = PDS3
RECORD_TYPE = STREAM
LABEL_REVISION_NOTE = "
2010-05-29, W. Kurth (U. IOWA), initial;
2010-05-31, C. Piker (U. IOWA), general revision;
2012-05-30, C. Piker (U. IOWA), changed high-rate data layout;
2012-06-04, C. Piker (U. IOWA), added notes on dataset limitations;
2018-09-23, C. Piker (U. IOWA), added antenna length caution;
2018-03-28, J. Mafi (UCLA), updated for orbits 7 and 8 release;
2018-07-10, J. Mafi (UCLA), updated for orbits 9 and 10 release;
2018-08-02, D. Kazden (UCLA), removed ARCHIVE_STATUS keyword;
2018-10-25, J. Mafi (UCLA), updated for orbits 11 and 12 release;
2019-02-05, J. Mafi (UCLA), updated for orbits 13 and 14 release;
2019-05-22, J. Mafi (UCLA), updated for orbits 15 and 16 release;
2019-09-10, J. Mafi (UCLA), updated for orbits 17 and 18 release;
2019-12-20, J. Mafi (UCLA), updated for orbits 19 and 20 release;
2020-02-03, D. Kazden (UCLA), updated DATA_SET_RELEASE_DATE and
CITATION_DESC;
2020-04-06, J. Mafi (UCLA), updated for orbits 21 and 22 release;
2020-06-24, D. Kazden (UCLA), updated for orbits 23 and 24 release;
2020-11-06, D. Kazden (UCLA), updated for orbits 25 and 26 release;
2020-11-17, C. Piker (U. IOWA), updates to effective antenna length;
2021-02-19, D. Kazden (UCLA), updated for orbits 27 and 28 release;
2021-03-28, C. Piker (U. IOWA), update data_set_id to 2.0;
2021-06-04, D. Kazden (UCLA), updated for orbits 29 and 30 release;
2021-09-20, D. Kazden (UCLA), updated for orbits 31 and 32 release;
2022-01-03, D. Kazden (UCLA), updated for orbits 33 and 34 release;
2022-03-24, D. Kazden (UCLA), updated for orbits 35 and 36 release;
2022-06-21, D. Kazden (UCLA), updated for orbits 37 and 38 release;
2022-09-16, D. Kazden (UCLA), updated for orbits 39 and 40 release;
2022-12-13, D. Kazden (UCLA), updated for orbits 41 and 42 release;
2023-03-08, D. Kazden (UCLA), updated for orbits 43 and 44 release;
2023-06-30, D. Kazden (UCLA), updated for orbits 45, 46 and 47 release;
2023-10-27, D. Kazden (UCLA), updated for orbits 48, 49 and 50 release;
2024-02-02, D. Kazden (UCLA), updated for orbits 51, 52 and 53 release;"
OBJECT = DATA_SET
DATA_SET_ID = "JNO-E/J/SS-WAV-3-CDR-BSTFULL-V2.0"
OBJECT = DATA_SET_INFORMATION
DATA_SET_NAME = "
JUNO E/J/S/SS WAVES CALIBRATED BURST FULL RESOLUTION V2.0"
DATA_SET_COLLECTION_MEMBER_FLG = "N"
DATA_OBJECT_TYPE = TABLE
START_TIME = 2011-08-09T16:56:56
STOP_TIME = 2023-08-18T23:06:14.105
DATA_SET_RELEASE_DATE = 2024-02-02
PRODUCER_FULL_NAME = "DR. WILLIAM S. KURTH"
DETAILED_CATALOG_FLAG = "N"
DATA_SET_TERSE_DESC = "
The Juno Waves calibrated burst waveform full resolution data set
includes all high rate science waveform information calibrated in units
of electric or magnetic field for the entire Juno mission."
ABSTRACT_DESC = "
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."
CITATION_DESC = "Kurth, W.S., and Piker C.W.,
JUNO E/J/S/SS WAVES CALIBRATED BURST FULL RESOLUTION V2.0,
JNO-E/J/SS-WAV-3-CDR-BSTFULL-V2.0, NASA Planetary Data System, 2024,
DOI: 10.17189/1522461."
DATA_SET_DESC = "
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.
Parameters
==========
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)
https://doi.org/10.1007/s11214-017-0396-y, 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) https://doi.org/10.1002/2016RS005954, 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.
Processing
==========
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.
Data
====
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.
Software
========
TBD - We may include software to output these data as ASCII comma
separated values.
Media/Format
============
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."
CONFIDENCE_LEVEL_NOTE = "
Confidence Level Overview
=========================
This data set contains all calibrated waveform data for the Juno Waves
instrument for the interval defined by the START_TIME and STOP_TIME
elements above. Every effort has been made to ensure that all data
returned to the ground from the spacecraft are included and that the
calibration is accurate.
This section will be updated with information on known issues with the
data, such as interference from other spacecraft systems, or other
information needed to use the data with confidence.
Review
======
The Waves calibrated burst waveform data will be reviewed internally by
the Juno Waves team prior to release to the PDS. The data set will also
be peer reviewed by the PDS.
Data Coverage and Quality
=========================
TBD
Limitations
===========
Waves amplitude data from the upper bands of the high frequency
receivers are not collected via a direct sampling of the electric field
in time. Since the A/D converters employed in the instrument are not
capable of sampling at the rates needed for direct measurements, the
incoming 'real-world' signal has been mixed with the output of a local
oscillator. The down-mixed, in-phase and quadrature signals are then
sampled at a fixed 1.3125 MHz rate, regardless of the band of interest.
This produces a set of waveforms with ambiguous frequency components.
Since a simple Fourier Transform of these time domain data will *not*
produce a meaningful spectra we have converted these waveform data
into spectra with unambiguous frequency components. These products
have the filename pattern:
WAV_yyyydddThhmmss_E_NBS_qqq_Vnn.DAT
and contain electric field amplitudes versus frequency. Here the
parameter 'qqq' can read either 'REC' or 'BST'. In this case
the first amplitude of each row is *not* a DC component. Rather these
spectra comprise a roughly 1 MHz band centered on the frequency of the
local oscillator used to down-mix the signal to a measurable range.
This center frequency can change from row to row in an attempt to track
the electron cyclotron frequency. Appendix C in the
DOCUMENT/VOLSIS/VOLSIS.HTM document provides more information on how
spectra are derived from the down-mixed waveforms.
The instrument response across the 1 MHz band is not flat, however
applying frequency corrections artificially inflates background noise
levels within the receiver to the point that these artificial data
exceed the real signal level in many cases. Thus frequency corrections
have not been applied to these products. Persons wishing to apply such
correction may use the calibration file:
WAV_CAL_BST_NBS_FREQ_Vnn.CSV
to normalize the response across the 1 MHz band with the response at
a calibrated frequency.
"
END_OBJECT = DATA_SET_INFORMATION
OBJECT = DATA_SET_TARGET
TARGET_NAME = "EARTH"
END_OBJECT = DATA_SET_TARGET
OBJECT = DATA_SET_TARGET
TARGET_NAME = "JUPITER"
END_OBJECT = DATA_SET_TARGET
OBJECT = DATA_SET_TARGET
TARGET_NAME = "SOLAR_SYSTEM"
END_OBJECT = DATA_SET_TARGET
OBJECT = DATA_SET_HOST
INSTRUMENT_HOST_ID = "JNO"
INSTRUMENT_ID = "WAV"
END_OBJECT = DATA_SET_HOST
OBJECT = DATA_SET_MISSION
MISSION_NAME = "JUNO"
END_OBJECT = DATA_SET_MISSION
OBJECT = DATA_SET_REFERENCE_INFORMATION
REFERENCE_KEY_ID = "NULL"
END_OBJECT = DATA_SET_REFERENCE_INFORMATION
END_OBJECT = DATA_SET
END
|