In this example the custom data source name is qd1min. Wildcard substitutions can be made for the year (YYYY), month (MM) and day (DD). Future updates willgive more flexibility in data storage model, but currently we assume that allcustom data sources follow a convention in which the data files are daily, andthe files are organized into folders by year. The year, month and day must allbe specified in the filename.
Currently there are some restrictions on the data format for custom data sources. The stored data must currently be stored as JSON-headed ASCII.If data conversions are required, then a valid dictionary of conversionfunctions must be supplied via the convert keyword argument. See readJSONheadedASCII() for details.Additionally, by default this will interpolate the data to the requested time ticks. To return only the actual recorded data values for the specified time range set the keyword argument interp to False.
Energetic particle data sources: Fluxes of protons above 6 energy thresholds (1, 2, 4, 10, 30, 60 Mev) from the IMP 7 and IMP 8 Charged Particle Measurement Experiment (CPME; Principal Investigator S.M. Krimigis, then R.B. Decker) are included in OMNI and OMNI 2 for the period January 1, 1973, through the end of 2005 shortly after which IMP 8 operations terminated. The data were prepared and provided by CPME Co-Investigator T.P. Armstrong and colleagues at U. Kansas and Fundamental Technologies, LLC. The instrument and data are further described at -www.jhuapl.edu/IMP/imp_index.html and at of protons above 1, 10, 30 and 60 MeV for mid-1967 through the end of 1972, from the JHU/APL Solar Proton Monitoring Experiment (SPME) on IMP 4 (1967/150 - 1969/123) and IMP 5 (1969/172 - 1972/358) were added to OMNI 2 shortly after its creation. The fluxes were computed at NSSDC from count rates provided on tape to NSSDC decades earlier. The values are not reliable absolute measures of quiet time galactic fluxes, but are good for solar and shock- accelerated particles. cf. Williams and Bostrom, J. Geophys. Res.,74, 3019, 1969.Fluxes of protons above 10, 30 and 60 MeV, as measured by NOAA's geosynchronous GOES 11 spacecraft for 2006-2010, from GOES 13 for 2011 -2017/11 and from GOES 14 for 2017/12 later; (cf. ),were added to OMNI 2. (The GOES 13 and 14 data added to OMNI 2 are actually averages over the fluxes given at NOAA for eastward-looking and westward looking sensors.) Principal Investigator for the GOES energetic particle instruments is currently T. Onsager, and key responsible NOAA person is D. Wilkinson. Comparisons of IMP 8, GOES 10 and GOES 11 proton flux values obtained between 1999 and 2005 show reasonably good agreement during solar particle flux events; see _ogg.html.8. Spacecraft prioritization A new prioritization on which spacecraft to use for hours with multiple sources. Previously, we prioritized Wind over ACE through the end of 1999, and prioritized ACE thereafter. Now, we have spacecraft priorities for 7 intervals: 1. 1995/001-1998/180 Wind, ACE, IMP8, Geotail 2. 1998/181-1999/129 ACE, Wind, IMP8, Geotail 3. 1999/130-1999/228 Wind, ACE, IMP8, Geotail 4. 1999/229-2002/333 ACE, Wind, IMP8, Geotail 5. 2002/334-2003/222 Wind, ACE 6. 2003/223-2004/119 ACE, Wind, 7. 2004/120-current Wind, ACE These ACE-prioritized intervals are when Wind either makes several magnetospheric incursions or is unusually far (e.g., >200 Re) from the magnetosphere.9. IMF data sources:Table 1 shows the sources of LRO magnetic field data.The parentheses after the spacecraft names show our numeric spacecraft identifiers.
As of 2014, Wind and ACE data were being periodically added to LRO. The current latest date of magnetic field data in LRO is given at _data.html.Table 1-----------SpacecraftKey personsData time spanReferences---------- ----------- ----------------- ----------------IMP 1 (18) Ness 11/27/63-02/15/64 Ness et al, 1964IMP 3 (28) Ness 06/01/65-01/29/67 Ness et al, 1964AIMP 1 (33) Ness 07/04/66-07/13/68 Behannon et al, 1968IMP 4 (34) Ness 05/26/67-12/27/68 Fairfield, 1969AIMP 2 (35) Ness 07/26/67-11/10/69 Ness et al, 1967HEOS (1) Hedgecock 12/11/68-10/28/75Hedgecock, 1975IMP 5 (41) Ness 06/21/69-10/26/72 Fairfield & Ness, 1972IMP 6 (43) Ness 03/14/71-07/21/74 Fairfield, 1974IMP 7 (47) Ness 09/26/72-04/03/73 Mish & Lepping, 1976IMP 8 (50) Ness, Szabo 10/30/73-05/12/00 Mish & Lepping, 1976ISEE 3 (13) E.Smith 08/14/78-12/21/82 Frandsen et al, 1978Prognoz 10 (10) Yeroshenko 04/27/85-11/04/85 Styazhkin et al, 1985Wind (51) Lepping, Szabo 11/21/94-current Lepping et al, 1995ACE (71) Smith 02/06/98-current Smith et al, 1998.Geotail (60) Nagai 05/08/95-12/31/06 ----------- ------ ----------------- ------------------ Full citations for these references are given at: _doc_addition.html#references.
Hourly resolution versions of data from these magnetometers are available from:
and
The web pages of the IMP 8, Geotail, Wind and ACE magnetometer teams are to be found at:
IMP 8:
Wind:
ACE:
Geotail: special relevance to LRO preparation is an FTPBrowser-accessible merged hourly IMP8-Geotail-Wind-ACE IMF data set at _iwa.html from which one may make overlapping time-series plots. A second interface at _iwa_s2.html enables one to make scatter plots and linear regression fits of user-selected parameter pairs and time span. Results of analyses of these data, with this latter tool, are reported below. A third interface at _iwa_d.html enables one to determine distributions, means and their standard deviations, and medians of any IMF parameter from any of the spacecraft named, for any time span. 10. Plasma data sources: Most of the solar wind plasma data used in LRO are from the MIT Faraday Cups ( PI is Bridge in Table 2) or the Los Alamos National Laboratory (LANL) electrostatic analyzers ( PI is Bame in Table 2). The data were mainly provided to NSSDC or SPDF and used in OMNI as 1-hour averages. Exceptions are:
1. The IMP 1, Vela and HEOS data which were provided as 3-hour averages and were assigned to each of three successive one-hour records in OMNI,
2. The ISEE 3, Wind and ACE data whose 1-hour averages were computed at SPDF from time-shifted higher-resolution and
3. The LANL IMP 6, 7 and 8 data whose 1-hour averages were computed at SPDF from higher-resolution data.At present time, Wind and ACE data were being periodically added to OMNI.
Information on current latest date of plasma data in OMNI is given at _data.htmlTable 2--------Spacecraft Key personsTime spanComments, Reference---------- ----------- ---------------- --------------------IMP 1 (18) Bridge 11/27/63-02/22/64 Bridge et al, 1965Merged Vela (97) Bame 07/21/64-03/18/71 Bame et al, 1971Vela 3 (3) Bame 07/26/65-11/13/67 Hundhausen et al, 1967AIMP 1 (33) Bridge 07/06/66-09/23/69 Lyon et al, 1968IMP 4 (34) Ogilvie 06/03/67-12/16/67 Ogilvie et al, 1968AIMP 2 (35) Bridge 07/28/67-07/03/68 Lyon et al, 1967OGO 5 (5) Neugebauer 03/05/68-04/29/71 Neugebauer, 1970HEOS 1 (1) Bonetti 12/11/68-04/15/70 Bonetti et al, 1969IMP 6 (43) Bame 03/18/71-07/21/74 Feldman et al, 1973IMP 7 (44) Bame 10/06/72-09/29/78 Asbridge et al, 1976IMP 7 (47) Bridge 01/03/75-09/20/78 Lazarus et al, 1998IMP 8 (45) Bame 11/04/73-07/16/00 Asbridge et al, 1976IMP 8 (50) Bridge 12/05/73-07/26/01Lazarus et al, 1998ISEE 1 (11) Bame 10/30/77-12/19/79 Bame et al, 1978bISEE 3 (13) Bame 08/16/78-10/12/82 Bame et al, 1978aWind (51) Lazarus and Kasper 01/01/95-current Kasper, 2002ACE (71) McComas, R. Skoug 02/05/98-current McComas et al, 1998Geotail (60) L.Frank 05/08/95-12/07/06 Additional key scientists contributing to IMP 8 plasma data are have been J. Gosling and J. Steinberg at LANL and A. Lazarus, K. Paularena and J. Richardson at MIT.
All citations may be found at: _doc_addition.html#references.
The plasma parameters included in the early-period OMNI-input data sets (i.e., the first 8 rows of data sets of Table 2) are identified in the original OMNI documentation, available through OMNIWeb, and will not be repeated here. For the middle and later periods, we have used the following in OMNI 2 from the various input data sets:NVT phi-V theta-V alpha/protIMP 6 xxxx xIMP7 (LANL)xxxx xIMP7 (MIT)xIMP8 (LANL)xxxx xIMP8 (MIT)xxxxxISEE 1xISEE3 (protons)xxxxISEE3 (electrons)xxWind/SWExxxxx xACE/SWEPAMxxxxx xGeotail xxxxxWind SWE plasma parameter data are available in three separate data sets created by the Principal Investigator team.
These are:
1. KP- key parameter data determined by taking linear fits of assumed-isotropic convecting Maxwellian distribution functions,
2. NLF- parameters based on on anisotropic non-linear fitting of bimaxwellian convecting distributions,
3. MOM - parameters based on taking moments of observed distributions.
The Wind/SWE/NLF plasma data set was chosen as the baseline wasthe result of analysis at MIT (Kasper, 2006, see )and discussed in details in the "Data set intercomparisons and parameter normalizations" section below. Previously we used cross-normalized Wind/SWE KP to the definitiveSWE/NLF data, and we used cross-normalized ACE data thereafter. Now ( as 2019-03-31), we use for 1995-current the Wind definitine NLF SWE data and cross-normalized SWE KP data thereafter. and at the third priority we used cross-normalized ACE data.92s proton and alpha particle NLF parameters, and proton MOM parameters, are available for solar wind intervals only, at _swe_2m.html, and at _swe_2mp.html for all orbit phases.Protons-only KP data are available for solar wind intervals only, at _swe_kp.html and at _kp_unspike/ The ACE/SWEPAM parameters provided by the SWRI/LANL plasma team were determined by taking moments over distribution functions. Additional interfaces for comparing Wind/SWE NLF and KP data to each other and to ACE/SWEPAM, IMP 8 (LANL and MIT) and Geotail are at _iwa.html time series plots, lists _iwa_s2.html 2-spacecraft scatter plots _iwa_s3.html sctr plots, log N&T _iwa_d.html statistics w. filteringReaders interested in the differences between the Wind moments-based and NLF-fits-based parameter-determination approaches may access _swe2m_s.htmlThe LANL plasma instruments on ISEE 3 measured ions and electrons separately. The ion instrument failed February 19, 1980. Electron-based flow speeds and densities were used in OMNI 2 afterthe ion instrument failure until late 1982, but neither electron-based temperatures nor flow direction angles were included into OMNI 2. (This was also done for OMNI years ago.) It should be noted that on two days (July 4,1979, and July 31, 1979), ISEE 3 measured densities so low that for each of several hours, the hourly averaged density was less than 0.05/cc. Given OMNI's use of F6.1 format for densities, this yields an apparentdensity of 0.0 in OMNI for these few hours.Only flow speeds are provided from IMP 7 (MIT) and from ISEE 1. In the former case, this limitation to flow speed was at the suggestion of A. Lazarus at MIT. In the case of ISEE 1, there were too few hours (
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