Data Set Overview : The following describes the nature of instrument operation during the various periods for which IES data are available in this submission. In all cases the data are calibrated differential electron and ion energy flux as function of energy, azimuth (direction in the instrument symmetry plane) and elevation (angle above or below the symmetry plane). Post hibernation commissioning: IES turned on 24 march 2014 for Low Voltage checkout, operated ~19:50 to ~20:50 UTC (no useful science data), High Voltage checkout (all times UTC): 22:44:59 to 22:53:31; 25 March: 00:42:51 to 03:37:15, 21:34:35 to 23:56:59; 26 March: 00:41:15 to 01:08:59 and 01:16:27 to 02:09:15 (little useful science data except a small amount of solar wind is evident in the early part of the 25 March 2014 and intermittently in 26 March 2014 files). Approach phase: 9 May 2014 15:23:00 to 20 May 11:25:41. Little useful science except occasional solar wind 11 May, 18:00; 12 May, 08:00; 13, 14, May, intermittently; 15 May from 15:00 to 24:00; 16 May 0:00 to 03:00; 18, 19 May, intermittently; 23 May 0:00 to 24:00; 24 May, 0:00 to 3:30; 26 May, 13:00 to 24:00; 27 May, intermittently from 0:00 to 12:00; 29 May, intermittently, 13:00 to 24:00; 30 May, intermittently from 0:00 to 6:00; 7 June, 23:00 to 24:00; 8 June, 0:00 to 11:00; 11 June, 1:00 to 10:00; 20 June, intermittently; 21 June, 2:00 to 3:00; 22 June, 0:30 to 10:00; 25 June, 15:00 to 17:00; 26 June, intermittently; 27 June, 0:00 to 4:30; 28 June, 19:30 to 20:00; 6 July, 10:00 to 14:00; 7 July, 4:00 to 8:00; 12 July, 3:30 to 7:30; 18 July, 18:00 to 18:30; 20 July, 5:30 to 6:00; 3 August, intermittently between 8:00 and 10:30; 5 August, intermittently after 13:00; 6 August, intermittently after 12:00; 7 August, intermittently between 6:00 and 10:00; 8 August, 3:00 to 5:00; 10 August, 8:00 to 10:30; 11 August, 16:00 to 17:30; 12 August, intermittently; 13 August, 8:30 to 10:30; 14 August, 3:30 to 5:00; 15 August, intermittently; 16 August, intermittently between 13:00 and 24:00; 17 August, between 8:30 and 10:30; 18 August, 0:00 to 2:00. 19 August: Beginning of detection of low energy pickup ions in addition to solar wind (S/C to comet : 78 km, S/C to Sun : 3.5 AU). 20 - 22 August, intermittent solar wind; 24 August, 9:00 to 10:00 solar wind; 25 August, 0:00 to 1:30 solar wind; 26 August, intermittent solar wind; 27 August, intermittent solar wind; 28 August, intermittent solar wind, with possible shock at ~18:00, low energy pickup ions; 29 August, intermittent solar wind, low energy pickup ions; 30 August, intermittent solar wind, low energy pickup ions; 31 August, intermittent solar wind, low energy pickup ions; 1 September, solar wind until ~7:00 followed by the result of interplanetary energetic particles through 2 September. IES was turned off at ~15:45 until 9:00 on 5 September when solar wind was observed; 6 September, intermittent solar wind; 7 September, intermittent solar wind; 8 September, solar wind observed from 0:30 through the remainder of the day; 9 September, solar wind and low energy pickup ions; 10 September, solar wind and low energy pickup ions; 11 September, solar wind and low energy pickup ions and a possible shock at 10:00; 12 September, solar wind and low energy pickup ions (a gap in data occurred around 23:00); 13 September, solar wind and low energy pickup ions; 14 September, solar wind and low energy pickup ions; 15 September, solar wind; 16 September, solar wind; 17 September, solar wind; 18 September, solar wind, with a data gap from ~11:15 to 17:45; 19 September solar wind with low energy pickup ions; 20 September, solar wind with low energy pickup ions, with a data gap ~12:00 to 12:15; 21 September, solar wind with low energy pickup ions, 22 September, solar wind with low energy pickup ions; 23 September, solar wind with low energy pickup ions; 24 September, solar wind; 25 September, intermittent solar wind plus possible penetrating radiation; 26 September, intermittent solar wind plus possible penetrating radiation; 27 September, intermittent solar wind; 28 September, intermittent solar wind; 29 September, intermittent solar wind with data gap from ~6:30 to 11:45; 30 September, solar wind and low energy pickup ions with brief data gap ~10:40; 1 - 9 October, solar wind and low energy pickup ions; 10 October, solar wind and low energy pickup ions with data gap ~2:15 - 9:00; 11 - 17 October, solar wind with low energy pickup ions; 18 October, solar wind with low energy pickup ions with short data gaps ~5:00 to 7:00; 19 October, solar wind with low energy pickup ions with short data gap ~ 2:10; 20 October, solar wind and low energy pickup ions; 21 October, solar wind and low energy pickup ions with data gap 1:45 - 15:50 22 October, solar wind with low energy pickup ions; 23 October, solar wind and low energy pickup ions with high-energy pickup ions; 24 - 29 October, solar wind and low energy pickup ions; 30 October, solar wind and low energy pickup ions with data gap ~1:45 - 4:15; 31 October, intermittent solar wind; 1 November, intermittent solar wind with short data gaps 6:45, 15:15, 16:30, and 17:50; 2 - 6 November, intermittent solar wind; 7 - 8 November, intermittent solar wind and pickup ions; 9 - 19 November, intermittent solar wind and pickup ions; Processing : All Rosetta Plasma Consortium (RPC) data packets are transmitted together during downlinks with Rosetta. RPC data are retrieved from the Data Distribution System (DDS) at European Space Operations Centre (ESOC) to a central RPC data server at Imperial College London. Data for IES is copied from the RPC central data server by IESGS at Southwest Research Institute. The pipeline processing software is the IES Ground System (IESGS). IESGS extracts IES CCSDS packets from the RPC collective data files stored on the RPC central data server at Imperial College. These packets are used to build ion and electron data products. The data products are grouped by date and written out to PDS compliant archive data files. One data file is created for each day. IESGS also generates the labels for the archive data files. IES science products, archive and label files, and limited spectrograms are available to team scientists on the IESGS website. Coordinate System : In order to determine IES pointing, attitude data for the Rosetta spacecraft is obtained through SPICE kernels and converted from the J2000 coordinate system to the HGRTN coordinate system. HGRTN is the heliocentric RTN system such that the sun-spacecraft vector defines the positive x-axis and the positive y-axis is the cross-product of the heliographic polar axis and the HGRTN positive x-axis. J2000 is the inertial frame defined by the intersection of the Earth mean equator and the ecliptic plane at the J2000 epoch of January 1, 2000 at noon. The pointing for each bin of IES is thereafter determined by multiplying the converted spacecraft attitude matrix in HGRTN by the vector representation of each particle measurement bin. The resulting vectors represent the flow of particles through the respective particle measurement bins in HGRTN coordinates. SUB_SPACECRAFT_LATITUDE, SUB_SPACECRAFT_LONGITUDE are given in the Cheops reference frame. These parameters are computed at time t:START_TIME. Distances are given in km, angles in degrees.

Confidence Level Overview : This dataset is used by the IES science team after processing. This is done to ensure that the archived data contains good, valid products. Caveat about using IES Level 3 Differential Energy Flux data: The background subtraction technique used in the production of the Level 3 Differential Energy Flux data does not work well for certain modes and as a result, the flux values may be slightly different from nominal. Please contact the IES team before using the data. Once the background subtraction issue is resolved, the IES team will deliver updated data. Review : This archival data set was examined by the IES science team prior to submission to the NASA Planetary Data System (PDS) and ESA Plantetary Science Archive (PSA). It was reviewed by PDS, PSA, and the Rosetta data archive working group. The current set was peer reviewed scientifically in 2016 by external experts and the recommendations and fixes have been implemented. Limitations : None.