Data on charged particles in space as measured by instruments of TASPD SINP MSU are presented under this root directory. TASPD SINP MSU stands for Theoretical and Applied Space Physics Division, Skobeltsyn Institute of Nuclear Physics, Moscow State University. The data sets co-reside on server TASPD.NPI.MSU.SU at MSU, Moscow, Russia and on server at NSSDC/GSFC, NASA, USA. The data of this collection have been restored from papers and old tapes. This work has been supported, in its significant part, by NASA, grant NAG5-4656. Data sets are given as ASCII tables and placed to the spacecraft-specific subdirectories. Each subdirectory contains a data file, a descriptor on data/instrument/mission and a GIF-file with overview-plots. Long data sets (from the spacecraft GRANAT and COSMOS-900) use one-year and one-day file formats respectively. Each data file is organized as a table with blank-space separators. Two heading lines provide information identifying the spacecraft/instrument and the data columns. A line "The end." terminates each data file. The column-legends from the 2nd header line are used in a file-descriptor id_descr.txt for addressing the explanations to a particular column. Each data line presents a record of measured parameters with leading time-tag. Everywhere time is universal time (UT) and everywhere a time value corresponds to the end of interval of measurement given in the record. Time format is YYMMDDHHmmSS (YY - year, MM - month, ...). If time resolution is worse than seconds, the respectively truncated form may be used instead. Every data column is given in the exponential format E10.3. Everywhere NODATA-filler is -9.999E+99. Almost all measured data are given in count rates (1/s). Ultra-violet sensor on COSMOS-900 is the only exception. Geometric factors are presented for every data channel in the correspondent id_descr.txt files. They may be used for converting the count rate to intensity. Spacecraft trajectory information is also given if available. Coordinates of a spacecraft are appended to each data record. For far missions, trajectory is given in the Heliographic Inertial Coordinate System (HGI). For the Earth's satellites GRANAT and COSMOS-900, trajectory is presented in a geocentric coordinate system. File sc_coordinates.txt describes the used coordinates. A definition of HGI system is given in the file rah_to_hgi.txt. Trajectory information is not available for the following spacecraft: - four lunar spacecraft (Moon's coordinates may be used instead); - ZOND-1 (no source; Earth's coordinates may be used instead); - MARS-2 for the part when it is in the Mars orbit (Mars' coordinates may used); - VEGA-2 (no source; a very similar trajectory of VEGA-1 may be used); - PHOBOS-2 (no source). Trajectories for old missions were restored from old in-paper plots of low quality, hence accuracy is as low as 5-10% or so. Therefore, these data may be used only as a reference, not for precise analysis of the data from spacecraft situated nearby each other. The trajectory data have been converted to HGI system from another system, see notes on the method of this conversion in the file rah_to_hgi.txt. Where available, a file of spacecraft coordinates in both original and HGI form is provided in addition. Below is a reference table on all data sets included in the collection. In 'Columns', the contents of each data set is presented as an information derived from the dataset's column legends. Notations are as follows. A leading letters: 'p' - proton, 'e' - electron, 'a' - alpha-particle, 'n' - nucleon, 'uv' - ultra-violet. Following digits denote energy range/threshold in MeV (except 'uv' channel on COSMOS-900). Trailing letter denotes direction of where particles come from: '+' - from sunward Sun, '-' - from antiSun, '*' - omni (from all directions), 'n' - perpendicular to sunward direction, 'm','c' - 45 degrees to sunward direction, 'z' - perpendicular to lunar surface, 'a' - field-aligned, 'p' - field-perpendicular, 'e' - from center-of-Earth direction. Legends present only main fraction of the measured fluxes for a particular channel if the measurement is not pure; see notes on this issue in the file sensors.txt. More details are given in the spacecraft specific files id_descr.txt placed in the spacecraft relevant subdirectories. Spacecraft Instrument Id TimeRes DataStart DataEnd Columns: ---------- ---------- -- ------- --------- ------- -------- ZOND-1 KS-OLD Z1 1d 64/04/02-64/05/16 UT p>30+ ZOND-3 KS-18 Z3 4h 65/07/19-66/01/21 UT p>30+ p1-5n LUNA-17/lk1 RV-2N LG 1d 70/11/10-71/09/14 UT p>30z p1-5z a4-8z LUNA-19 RV-2N-LS LI >1d 71/09/29-72/08/23 UT p>30+ p1-5+ p5-12+ p12-40+ LUNA-21/lk2 RV-2N LK 1d 73/02/14-73/04/20 UT p>30z p1-5z a4-8z LUNA-22 RV-2N-1 LL 4h 74/05/29-75/08/23 UT p1-5+ p5-15+ a5-10+ LUNA-22 RV-2N-1 LS 1d 74/05/29-75/08/26 UT p>30+ MARS-2/crs KS-18-4M M2 4h 71/05/21-71/11/26 UT p>30+ p1-5v+ p1-5+ p5-12+ p1-5v- p1-5- p5-12- p>500* MARS-2/orb KS-18-4M/ga MA 4h 71/11/26-72/06/01 UT p>30+ p1-5+ p5-12+ p1-5- p5-12- e>.3- MARS-2/orb KS-18-4M/gb MB 4h 71/11/26-72/06/01 UT p1-5v+ p1-5v- p>500* e>.3+ e>.05- MARS-4 KS-18-5M M4 4h 73/07/23-73/10/30 UT p>30+ p1-5+ p4-12+ p4-12- p>500* MARS-5 KS-18-5M M5 4h 73/07/26-74/02/08 UT p>30+ p1-5+ p1-5- p4-12+ MARS-7 KS-18-5M M7 4h 73/08/17-74/03/25 UT p>30+ p1-5+ p1-5- p4-12+ p>500* VENERA-2 KS-18M V2 4h 65/11/15-66/01/25 UT p>30+ p1-5n VENERA-3 KS-18M V3 4h 65/11/16-65/12/10 UT p>30+ p1-5n e>.05n VENERA-4 KS-2M V4 4h 67/06/12-67/10/16 UT p>30+ p1-5+ p1-5- e>.05- VENERA-5 KS-3M V5 4h 69/01/05-69/03/09 UT p>30+ p1-4+ p1-4- p1-4n e>.05n VENERA-6 KS-3M V6 4h 69/01/10-69/05/15 UT p>30+ p1-4+ p1-4- p1-4n e>.05n VENERA-7 KS-4M V7 4h 70/08/17-70/12/15 UT p>30+ p1-5+ p1-5- p4-12+ p4-12- VENERA-8 KS-18-4M V8 4h 72/03/27-72/07/22 UT p>30+ p1-5- p5-10+ p>0.3- e>.05+ e>.05- VENERA-9 KS-18-5M V9 4h 75/06/09-76/01/11 UT p>30+ p>800* p4-12- VENERA-10 KS-18-5M VA 4h 75/08/19-76/04/01 UT p>30+ p>500* p4-12- VENERA-11 ASP-8 VB 20m 78/09/11-79/10/04 UT p>30+ p3-5+ p3-5- VENERA-13 ASP-8M VD 20m 81/10/31-83/04/12 UT p>30+ p1-3+ p1-3- VENERA-14 ASP-8M VE 20m 81/11/06-83/03/16 UT p>30+ p1-3+ p1-3- VENERA-13 ASP-8M WD 80m 81/10/31-83/04/12 UT p2-3+ p3-5+ p5-8+ p2-3- p3-5- p5-8- VENERA-14 ASP-8M WE 80m 81/11/06-83/03/16 UT p1-2+ p2-4+ p4-8+ p1-2- p2-4- p4-8- VENERA-16 KS-18-6V VG 4h 83/06/08-85/05/28 UT p>30+ p>60+ p1-65+ p1-11+ p5-8+ a7-24+ p1-70- p1-9- p5-10- a7-22- VEGA-1 VFS-VK A1 20m 84/12/22-86/07/08 UT p>30m p>30c VEGA-2 VFS-VK A2 20m 84/12/28-85/05/03 UT p>30m p>30c PHOBOS-2 VFS-F F2 1h 88/07/13-89/03/23 UT p>30n GRANAT KS-18-M/gr1 G1 20m 89/12/02-95/12/16 UT p>20+ p>6+ p1-20+ p>20- p>6- p1-20- GRANAT KS-18-M/gr2 G2 2m 89/12/01-95/12/16 UT p2-7+ p5-20+ p2-7- p5-20- GRANAT KS-18-M/gr3 G3 20m 89/12/02-94/07/11 UT a12-18+ a12-18- GRANAT KS-18-M/gr4 G4 2m 89/12/01-95/12/16 UT p1-2+ p1-2- GRANAT KS-18-M/gr5 G5 20m 89/12/02-95/11/30 UT p1-2+ p2-3+ p5-6+ p6-30+ p30-100+ a7-12+ n>20+ p1-2- p2-3- p5-6- p6-30- p30-100- a7-12- n>20- GRANAT KS-18-M/gr6 G6 20m 89/12/02-95/12/16 UT p>20+ p>2.4+ p1-6+ a7-28+ a20-90+ p>20- p>2.4- p1-6- a6-40- a20-90- COSMOS-900 DPS-MES-NS-UF C9 5s 77/04/01-79/09/10 UT p.050-.080p p.080-.128p p.128-.206p p.206-.314p p.211-.326a p1-3p e.030-.050a e.030-.050p e.050-.080p e.080-.130p e.130-.210p uv3900e All listed spacecraft except GRANAT and COSMOS-900 are non-geocentric. The two latter are satellites: GRANAT has a high-altitude orbit with its initial apogee ~200000 km and COSMOS-900 has a circular orbit with h=~500 km and i=83 degrees. Since GRANAT spent most of time out of geomagnetosphere, its data sets are split to the subdirectories /heliospheric_data and /magnitospheric_data. Time resolution listed above may be understood differently for different spacecraft. For old non-geocentric spacecraft it may vary from one record to another; the almost smallest value is given in the table. For newer spacecraft, given time resolution is the best that the instruments have provided. The given values are almost constant ones but they may not be exactly equal to 4 hours or 20 minutes, - some small shifting of time grid may be observed. On GRANAT, 2 minute mode has been used only for several channels and mostly in the periods of high intensity of measured fluxes. Please feel free to direct any questions or comments on the data collection to Nick Pavlov: nnpavlov@taspd.npi.msu.su