Data Set Overview:  This dataset contains results from the Implanted Ion Sensor (IIS) 4DH mode and the Fast Ion Sensor SW and HAR modes of the Three- Dimensional Particle Analyzer (JPA) experiment on the GIOTTO spacecraft for the mission to comet Halley. The results of the Fast Ion Sensor (FIS - inbound) and IIS (outbound) have been merged with results from other Giotto instruments. In the first submitted table, magnetometer measurements are included. Values are given for protons.   JPA FIS data are from two sources:  - up to March 13, 19:24:55 SCET, data are from the solar wind mode at 8 seconds time resolution. The moments are derived from data in a 45 x 45 degree field of view, centered on the nominal solar wind direction. There is continuous coverage in energy and angle. The peak remains within this reduced field of view.  - March 13, 19:24:55 to 22:38:17 SCET, data are from the HAR mode at 24 second time resolution. This mode has an angular field of view accepting ions from all directions except a 20 deg cone in the ram direction. Energy-angle coverage is not contiguous in this mode so an assumption is made to boost the counts in each bin to make the distribution appear contiguous. The peak of the solar wind flux alternates between the last two 26 deg bins during this period. Moments are calculated for the regions of space sampled by the detector, i.e. up to the 20 deg ram cone, with no assumption to increase the range beyond this.  The following assumptions hold: FIS is an electrostatic analyzer and so cannot distinguish mass - except in the solar wind mode where the protons and alpha particles are cold enough that they separate in energy/charge; in HAR mode the moment is over the full FIS energy range so includes anything (all protons).  The temperature profile from solar winds to HAR mode is not continuous due to the different bin sizes involved, so the sudden temperature jump at 19:24:55 should not be take to be correct.  JPA IIS data is from the 4DH mode. In this mode, the Time of Flight measurement is combined with the energy level information provided by the IIS to separate mass groups, e.g., 0-1.7 amu/q (presumably protons). The moments are derived from data collected during one spacecraft spin, i.e., 128 s, at each of 32 energy levels to obtain a complete distribution. Pickup protons are included in the numbers but this is only a small effect.  The 'JPAMERGE' file includes both FIS and IIS data. The JPA data up to 22:38:17 are from FIS given every 8 s. (At this time the sampling changes to every 64 s; only magnetometer values are listed in this interval.) The JPA data starts again at approx 0104 on March 14 (MJD 13221 or day 73), and is from the IIS 4DH mode. This data has a time resolution of 128 seconds - in the merge file it is combined with 64s magnetometer data, which is why there are two MAG points for every JPA data repeated twice here. (The last 16 lines are again only magnetometer values.)  In the second table, the results from the FIS have been merged with data from the magnetometer, the RPA-Copernic plasma experiment, and the Ion Mass Spectrometer (IMS) HERS instrument to form this file. The original file was called GIOMERGE and its explanation follows below:  The file contains data for the period between March 12, 06:09:30 to March 13, 23:36:34 SCET for the MAG, RPA and IMS/HERS experiments and the JPA experiment, which ended earlier (at approximately 22:38 SCET).   MAG 8s averaged data  RPA 8s averaged data  JPA 8s data up to March 13, 19:24:55, 24s after this time  IMS/HERS 16s proton samples after March 13, 18:30:00 64s averaged alpha data  MAG and RPA data are available for all of the above given intervals.  JPA FIS data are from two sources:  - up to March 13, 19:24:55 SCET, data are from the solar wind mode at 8 seconds time resolution. The moments are derived from data in a 45 x 45 degree field of view, centered on the nominal solar wind direction. There is continuous coverage in energy and angle. The peak remains within this reduced field of view.  - March 13, 19:24:55 to 22:38:17 SCET, data are from the HAR mode at 24 second time resolution. This mode has an angular field of view accepting ions from all directions except a 20 deg cone in the ram direction. Energy-angle coverage is not contiguous in this mode so an assumption is made to boost the counts in each bin to make the distribution appear contiguous. The peak of the solar wind flux alternates between the last two 26 deg bins during this period. Moments are calculated for the regions of space sampled by the detector, i.e. up to the 20 deg ram cone, with no assumption to increase the range beyond this.  The temperature profile from solar winds to HAR mode is not continuous due to the different bin sizes involved, so the sudden temperature jump at 19:24:55 should not be taken to be correct.  IMS proton and alpha data have been processed differently:  - Proton data were obtained during ~1 s intervals every 16 s. Since the measurement intervals happened to fall approximately midway between the 8 s times at which the other data in this file are given, each proton parameter is given twice -- ~4 s before the measurement and ~4 s after the measurement was made. Up until ~1830 on March 13, the solar wind was close to or slightly beyond the proton field of view of the HERS so V[z] could not be determined. We recommend using JPA proton data for this time interval, and so have not included IMS proton data in the merged file for this early period.  - Alpha data were also obtained during ~1 s intervals every 16 s, but the parameters have been calculated for averages over 4 such measurements; each value is therefore repeated 8 times in this data file.

Confidence Level Overview: N/A