As a general practice, Level-2 and Level-3 data (denoted (L2 and L3 in file names)
should be used where available while accessing only the highest version numbers.
Current best data are:
L1, L2 and L3 inertial frame data for RBSP-A and -B from 2012-08-31 through 2018-09-30.
QL-uvw data version 3.1 or higher for RBSP-A and -B from 2018-10-01 through 2018-10-22.
Use L1, L2 and L3 data rather than QL when available.
Use highest version from 3.1 to 3.5 or higher that is available.
Note to data users:
Day June 22, 2018 for RBSP-B is significantly incomplete due to downlink issues.
Day April 22, 2017 for RBSP-B is significantly incomplete due to downlink issues.
There is an unrecoverable gap for RBSP-A from July 29, 2016 at 23:14:56 UT to
July 30, 2016 at 00:45:40 UT.
There is an unrecoverable gap for RBSP-A on July 17, 2016 from 15:48:18 to 17:21:36 UT.
There is an unrecoverable gap for RBSP-A spanning June 22 & 23, 2016.
There is an unrecoverable gap for RBSP-A on June 17, 2016 from 01:48:55 to 03:20:19 UT.
Large data gap for RBSP-A on May 11, 2016.
Large data gap for RBSP-B on May 7, 2016. Awaiting more data.
Large data gaps for RBSP-A on April 9 and 11, 2016.
There is a 10% data gap for RBSP-A on February 14, 2016.
There is a significant data gap for RBSP-A on January 11-12, 2016 with lost and
There is a significant data gap for RBSP-A on November 20, 2015 with lost and
There is a significant data gap for RBSP-A on November 7, 2015 with lost and
A single even upset at approximately 19:45 UT on October 9, 2015 triggered a
contingency mode which required a processor reset at 20:41 UT on October 13 to
return to normal operations. During this time the MAG instrument was forced into
Range-3. The resolution of the data was degraded while in Range-3 and cannot be
There is a significant data gap on September 15-16, 2015 due to lost and
The processing code failed to address the June 30, 2015 leap second. There also
appears to have been an less-than-correct ephemeris file used at this time. Data
from June 30 to July 21, 2015 contained discontinuities and have been corrected
with version 3.4 of the data.
Due to storm activity and perhaps other reasons we do not yet fully understand,
calibrations are still rough from March 2015 onward and will be improved.
Production continues for intervals after the above as data becomes available.
A reprocessing of all L1, L2 and L3 data is planned for the near future.
We are working to bring into production new calibration codes that will reduce
the spin tone below current levels. We remind the user that we are already
delivering data at superior accuracy than originally promised and hope that the
new codes will improve our performance.
QL-uvw is processed routinely to keep within a few days of measurement.
Current production codes and kernels include a 1.5 Hz signal that is Spice related
and largely removed at this time, an 11-sec signal that is the spin tone due to less
than ideal calibration that we hope will be removed very soon, and a 5-min nutation
signal that is largely the result of removing the star tracker from the spacecraft.
There is a 14.5 Hz signal on spacecraft A that arises from an aliased heater line.
We now believe that inertial frame data contains significant errors during times of
eclipse from 03/04/2013 through 04/07/2013. Data at these times are suspect with
up to 30 nT errors near apogee and the problem is most evident near the boundaries
of the eclipse. Errors are greatest during times of longest eclipse.
Both QL, L2 and L3 data sets are within the promised accuracy. Examination of the
data has taught us that to obtain good and usable spectra we must exceed the promised
instrument calibration and processing goals. We are working on that now.
New Spice-handling codes have been written and are now being tests with new Spice
production codes by APL. MAG instrument calibration continues and is not yet final.
The above L2 and L3 data will be reprocessed when both Spice processing and cals are
For questions regarding data quality and availability please contact:
Dr. Scott R. Bounds, EMFISIS Project Manager,
Physics Department, University of Iowa, Scott-Bounds@uiowa.edu
Copies of questions can be sent to:
Prof. Craig Kletzing, EMFISIS Principal Investigator,
Physics Department, University of Iowa, Craig-Kletzing@uiowa.edu
Mr. Daniel Crawford, EMFISIS SOC Manager,
Physics Department, University of Iowa, Daniel-Crawford@uiowa.edu
Prof. Charles W. Smith, MAG Data Manager,
Space Science Center, University of New Hampshire, Charles. Smith@unh.edu