**ISTP DATA MANAGEMENT PLAN**

Version 4.3

*Table of Contents*

1.0 Introduction 1

2.0 Mission Science Elements 1

2.1 Global Geospace Science Initiative 1

2.2 Collaborative Solar Terrestrial Research Initiative 2

3.0 Mission Science Objectives and Success Criteria 3

4.0 Mission Operation Elements 4

4.1 Central Data Handling Facility 5

4.2 Data Distribution Facility 6

4.3 Special Data Distribution Activities 7

4.4 The Science Planning and Operations Facility 7

4.4.1 SPOF Science Planning Functions 7

4.4.2 SPOF Operations Functions 8

4.4.3 SPOF Science Advancement Functions 8

4.5 SOHO Experimenters Operations Facility 9

4.6 Cluster Joint Science Operations Center 9

5.0 Data Products 10

5.1 SIRIUS Data 10

5.2 Level 0 Data 10

5.3 Key Parameters 10

5.4 Citable Key Parameters 12

5.5 Event Data 12

5.6 Other Data Products 12

5.7 Archival Data Volume 12

5.8 SOHO Data Products 13

5.9 Cluster Data Products 13

5.10 Solar Wind Catalog 14

6.0 Correlative Science Data Management 14

6.1 Campaign Coordination Functions of the SPOF 14

6.2 Inter-Agency Correlative Science Activities 14

6.3 SOHO Solar Data Analysis Center 16

6.4 Cluster Science Data System 16

7.0 Data Archiving and Distribution 16

7.1 Data Archive Products Contents and Disposition 16

7.2 Archive Data Access 16

8.0 Project Data Management Documentation 17

9.0 References 17

Acknowledgments 19

*Table of Contents (Continued)*

Figure Captions 19

**Table 1 - Data Services at the CDHF** 23

**Table 2 - Key Parameter Standards and Conventions** 24

**Table 3 - Wind KP Data Product Summary** 25

**Table 4 - Polar KP Data Product Summary** 26

**Table 4 - Polar KP Data Product Summary** 27

**Table 4 - Polar KP Data Product Summary** 28

**Table 5 - Ground-based Location & KP Data Product Summary** 29

**Table 5 - Ground-based Location & KP Data Product Summary** 30

**Table 6 - Supplementary Missions KP Data Product Summary** 31

**Table 7 - Geotail KP Data Product Summary** 33

**Table 7 - Geotail KP Data Product Summary** 34

**Table 8 - SOHO KP Data Product Summary** 35

**Table 9 - SOHO Science Data Product Summary** 36

**Table 10 - ClusterSummary Parameters Data Products** 37

**Table 11 - Cluster Science Data Centers** 38

**Table 12 - Interball/Aurora Key Parameters** 39

**Table 13 - Interball/Tail** **Key Parameters** 40

**Table 14 - ISTP Data Products and Disposition Overview** 41

**Appendix A - Overview of the Wind Mission Instruments** 42

**Appendix B - Overview of the Polar Mission Instruments** 47

**Appendix C - Rules for Data Rights**

**ISTP/NASA funded Missions** 53

**Appendix D - Rules for Data Rights**

**Geotail Mission** 54

**Appendix E - Rules for Data Rights**

**SOHO Mission** 55

*Table of Contents (Continued)*

**Appendix F - Rules for Data Rights**

**Cluster Mission** 57

**Appendix G - Rules for Data Rights**

**Interball Mission** 59

**Appendix H - IACG Rules for Data Exchange** 60

**Appendix I-Bibliography of ISTP Data Handling Documents** 64

**Appendix J - Acronym List** 69

.c.1.0 Introduction

Solar-terrestrial physics concerns the study of physical processes that
control the flow, distribution and dissipation of mass, momentum, and
energy from the solar wind to the Earth's atmosphere. When the charged
particles in the solar wind reach the Earth, some solar wind particles
enter the magnetosphere directly along open magnetic field lines or
through dynamical coupling processes. These solar wind entry processes
lead to significant influence of the solar wind on the configuration,
dynamics and energetics of the Earth's upper atmosphere.

An international effort that utilizes multi-space agency spacecraft to
achieve a new understanding of solar-terrestrial physics is currently
underway. This effort is called the International Solar Terrestrial
Physics (ISTP) program. The goal of the ISTP is to attain correlative,
inter-comparison of simultaneous measurements taken by the ISTP
spacecraft in different geospace regions and ground observing stations,
and the interpretation of the observations by theoretical modeling
studies to understand the underlying physics of the entire
solar-terrestrial system.

For this effort, the National Aeronautics and Space Administration
(NASA) is providing the Wind and Polar satellites. The Institute of
Space and Astronautical Science (ISAS) in Japan is providing the Geotail
satellite. NASA is also collaborating with the European Space Agency
(ESA) in two additional solar-terrestrial missions, SOHO and Cluster.

Supplementary observations will be made by several existing equatorial
and solar wind spacecraft. The equatorial spacecraft are the
Geosynchronous Operational Environmental Satellite (GOES) of the
National Oceanic and Atmospheric Administration (NOAA) and the Los
Alamos National Laboratory (LANL) spacecraft from the Department of
Energy (DOE). The equatorial satellites will monitor magnetic-field and
particle changes that occur when particles are energized during auroral
events. Additional data from other existing satellites such as NASA's
Interplanetary Monitoring Platform satellite (IMP-8) will also be used.

The combined data sets from the above spacecraft and from complementary
ground-based observations will be used to construct quantitative models
to describe how mass, momentum, and energy carried by the solar wind are
transported across magnetospheric boundaries, stored and energized in
the magnetosphere, and subsequently dissipated into the Earth's
atmosphere. The purpose of this document is to provide the overview data
management plan for the above missions and to set the scene for the data
archiving and distribution.

.c.2.0 Mission Science Elements

The ISTP Program will provide internationally-coordinated scientific
studies of major areas of Geospace by means of remote and *in situ*
spacecraft measurements, ground-based observations, and theoretical
investigations. These studies will use data products produced by the
"core missions," as well as those obtained from other sources, for
correlative purposes. The ISTP core missions are Geotail, Wind, Polar,
SOHO, and Cluster. NASA's participation in the ISTP Program is through
two programs: the Global Geospace Science Initiative, and the
Collaborative Solar Terrestrial Research Initiative.

.c2.2.1 Global Geospace Science Initiative

The Global Geospace Science (GGS) Initiative consists of the Wind,
Polar, and Geotail missions; selected ground-based observing stations;
selected existing supplementary NASA, NOAA and LANL missions; and the
theoretical global modeling effort.

The Wind spacecraft is placed initially in a dayside apogee, double
lunar swingby orbit of 80 to 250 RE at apogee. An overview of the Wind
mission instruments is given in Appendix A. After approximately a year
in orbit, Wind will be re-positioned into a halo orbit about the sunward
(L1) libration point. The Polar spacecraft is placed in an elliptical
orbit of approximately 2 x 9 RE from the Earth's center with an initial
apogee near the north geomagnetic pole. An overview of the Polar mission
instruments is given in Appendix B.

The Wind spacecraft provides essential measurements pertaining to the
solar wind (particle fluxes, composition, density, flow velocity,
electric and magnetic fields). The Polar spacecraft provides essential
observations of the auroral zone (through remote imaging) and the polar
magnetosphere (particle fluxes, composition, density, electric and
magnetic fields). The eight scientific instruments on Wind and the
eleven instruments on Polar all produce measurements that are processed
in the Central Data Handling Facility (CDHF) to key parameter data
products (see below). The rules for the data rights for the Wind and
Polar missions are given in Appendix C.

The Japanese Geotail spacecraft will initially be operated in a
double-lunar swingby orbit having a nightside variable apogee radius of
80 to 220 Earth radii (RE). At a future date, it is to be placed into an
8 x 30 RE near-tail orbit. Geotail observations in the Earth magnetotail
provide essential science data products (hot tail plasmas, high and low
energy particles, magnetic and electric field properties). Seven flight
instruments are used to produce these data products, four of which
include a significant participation by U.S. scientists. Measurements
from Geotail are processed in the ISTP CDHF to key parameter data
products (see below). The rules for the data rights for the Geotail
mission are given in Appendix D.

The data from the three correlative science missions, Wind, Polar, and
Geotail, will be supplemented by data products (in the form of key
parameters, see below) derived from ancillary observations taken by
IMP-8, GOES 6 & 7, and the LANL spacecraft. This data complement will
provide magnetic field and plasma measurements from IMP-8, averaged
magnetic field and energetic particle measurements from GOES 6 & 7, and
particle data from the LANL spacecraft, covering different regions in
the Geospace.

Ground-based investigations will provide scientific measurements of
spatial and temporal variations of ionospheric parameters (such as
electron density, electric fields, magnetospheric energy deposition,
latitude profiles, Joule heating, and derived geophysical parameters).

Theoretical investigations will focus upon 3-D magnetosphere modeling,
kinetic simulations, magnetosphere-ionosphere coupling, MHD (single
fluid), and a thermosphere global circulation model.

.c2.2.2 Collaborative Solar Terrestrial Research Initiative

The missions that are part of the Collaborative Solar Terrestrial
Research (COSTR) initiative are SOHO and Cluster.

SOHO is to be placed into a halo orbit about the sunward (L1) libration
point and maintained in this orbit throughout its operational lifetime.
SOHO will produce science data products pertaining to solar wind plasma
flow characteristics, coronal temperature, density, and velocity and
with solar oscillations to deduce interior structure. Data from the
eleven flight instruments on SOHO will be accessible in the Experiment
Operations Facility (EOF). The scientific and technical aspects of the
instruments on SOHO are extensively discussed in the ESA Special
Publication compiled by Domingo and Guyenne \[1989\]. An overview of
these products is given in Table 9. The rules for the data rights for
the SOHO mission are given in Appendix E.

Cluster has been baselined by ESA to consist of four spin-stabilized
spacecraft, placed into nearly identical elliptical polar orbits
approximately 4 x 22 RE with periods of about 66 hours. The four
spacecraft will be re-positioned to form vertices of a tetrahedron with
spatial separations that can be adjusted during the mission. Cluster
will produce science data pertaining to electric and magnetic field
properties such as currents, plasma waves, plasma densities, high energy
electrons, and energetic ion distributions and composition. The
scientific and technical aspects of the instruments on Cluster are
extensively discussed in the ESA Special Publication compiled by Schmidt
and Goldstein \[1988\].

Each Cluster spacecraft will provide up to eleven flight instrument
systems, including five component parts of the Wave Experiment
Consortium. The Cluster science data is to be captured by ESA and
distributed to the various data centers of the Cluster Science Data
System (CSDS) for processing into scientific data products (referred to
as prime and summary parameters). An overview of these products is given
in Table 10. The rules for the data rights for the Cluster mission are
given in Appendix F.

.c.3.0 Mission Science Objectives and Success Criteria

The science objectives for the Global Geospace Science Initiative (Wind,
Polar, and Geotail spacecraft) are:

> • To evaluate globally the effects of solar activity on the Sun-Earth
> system;
>
> • To understand how individual parts of the closely coupled, highly
> time-dependent geospace system work together;
>
> • TO determine the control exercised by plasma processes in geospace
> of the energy input to the Earth's atmosphere;
>
> • To understand fundamental physical processes that may occur in other
> astrophysical contexts; and
>
> • To provide a comprehensive data set for determining the accuracy and
> prediction capability of geospace models.

The minimum criteria for mission success are:

> • Acquisition and analysis of coordinated data sets from
> multi-spacecraft located in the four critical regions of geospace
> (solar wind, polar auroral magnetosphere, ionosphere, and the
> geomagnetic tail);
>
> • Acquisition and analysis of coordinated geophysical data from
> ground-based facilities to complement the spacecraft measurements; and
>
> • Development of the global theoretical and empirical models to assist
> in the interpretation of measurements.

These minimum success criteria will be met by continuing theory effort,
ground-based measurements, and the successful launch and operation of
the Wind and Polar spacecraft. For the Wind spacecraft, specific minimum
criteria require the instruments to provide a complete set of
measurements that characterize the solar wind input (IMF, flow velocity,
density, and composition) to the magnetosphere at about 1 minute time
resolution. For the Polar spacecraft, specific minimum criteria require
the instruments to make remote imaging observations of the structure and
morphology of the entire aurora zone and *in situ* particle, and
electric and magnetic field measurements at about 1 (or a few) minute
time resolution.

.c.4.0 Mission Operation Elements

The ISTP science initiative encompasses use of Level 0 (telemetry) data
obtained from six active mission elements, correlative data from other
mission sources, as well as ground-based and theory investigations, to
produce key parameters, event data products, PI archive data products
and models.

Figure 1 illustrates telemetry and Level 0 data flow for the ISTP core
missions (Wind, Polar, Geotail, SOHO, and Cluster) and IMP-8. Three
space networks capture science telemetry and provide radiometric
tracking of the spacecraft for orbit determination purposes. The ad hoc
NASA ground tracking network acquires IMP-8 telemetry data. The NASA
Deep Space Network (DSN) acquires Wind, Polar, and SOHO spacecraft
telemetry (real-time and playback), and captures the Geotail tape
recorder playback telemetry. The Japanese ISAS space network acquires
the real time Geotail science telemetry. ESA will use its space network
to acquire Cluster spacecraft telemetry. Telemetry and radiometric data,
initially captured at the network ground stations, are relayed through
communications networks to data capture/orbit/attitude facilities for
conversion to Level 0 data products that include the orbit and attitude
ephemeris files. Command history logs are maintained by the respective
control centers and are incorporated as ancillary files into the Level 0
data products.

Telemetry streams, acquired by the NASA networks, are routed to the data
capture facilities at Goddard Space Flight Center (GSFC) for Level 0
data processing. These telemetry streams from Geotail (playback), Wind,
and Polar, as well as Level 0 quicklook data products from the IMP-8
spacecraft, are electronically transferred to the NASA CDHF at GSFC,
where they are maintained in short duration storage (approximately 2
years after acquisition). Level 0 data for SOHO field and particle
instruments are electronically transferred from the Packet Processing
System (PACOR) to the CDHF and maintained in short duration storage
(approximately 2 years after acquisition). PACOR electronically
transmits SOHO Level 0 data to the Data Distribution Facility (DDF) at
GSFC. The DDF accesses CDHF databases for transfer of other Level 0
data, all of which are processed onto media for mailing distribution
(see below). PACOR also routes pre-processed real-time telemetry, as
well as "quick look" playback telemetry, to the Experiment Operations
Facility (EOF). The EOF electronically accesses SOHO orbit and attitude
ephemeris databases in the CDHF to process summary data products, which
are transferred to CDHF databases. CDHF databases are maintained as
short-term archives and are accessible to authorized ISTP investigators.

As shown in Figure 1, ISAS will acquire the high rate real-time
telemetry data from Geotail and place this data into their Scientific
Information Retrieval Integrated Utilization System (SIRIUS). NASA will
acquire the low rate playback telemetry data from Geotail which is then
written to compact disk at the GSFC data capture facility.

ESA facilities at the European Space Operations Center (ESOC) are used
to produce the Cluster Level 0, orbit/attitude, and command history
ancillary data. The Cluster data products will be distributed on Compact
Disk-Write Once (CD-WO) media and electronically via the ESA SPAN
network to the Cluster Science Data Centers and to the Cluster Principal
Investigators (PIs).

The GSFC Science Planning and Operations Facility (SPOF) provides the
focus for planning of instrument operations on Wind and Polar for NASA.
The Joint Science Operations Center (JSOC) at the Rutherford Appleton
Laboratory (RAL) will be providing similar services for the Cluster
spacecraft. ISAS provides the focus for planning of instrument
operations on Geotail. ESA utilizes the EOF at GSFC for planning of
instrument operations on SOHO. Summary data products will be produced in
the EOF and transferred to the CDHF as key parameter image data.

Figure 2 provides a high level overview of the ISTP science data flow. A
major ingredient of the processed data consists of key parameters (KP)
produced from the Level 0 information. KP data products are generated in
the CDHF for Geotail, Wind, and Polar missions as well as for magnetic
field data from IMP-8, and the particle instruments on SOHO. The KP data
generated in the CDHF are based upon algorithms provided by the
principal investigator teams. These KP data are supplemented by IMP-8 KP
plasma data which are generated by the PI and remotely networked to the
CDHF for inclusion in the database.

Supplementary science data products will be used to augment those
obtained from the active missions. GOES 6 & 7 will provide key parameter
data pertaining to magnetic fields and energetic particle measurements.
In addition, key parameter data from three to five LANL spacecraft will
provide one- to three-minute averages for solar wind plasma and low
energy particles, respectively. The supplementary data will be generated
at the investigator's remote facility, networked to the CDHF, and
maintained in CDHF databases for use by all the ISTP investigators. In
addition, Cluster summary parameter data will be produced in the Cluster
Science Data Centers. NASA will receive this data via RAL placing it
within the CDHF ISTP data base.

Ground-based investigations will produce key parameter datasets based
upon Earth-based observations of the ionosphere, particularly in the
high-latitude regions. These datasets will be electronically transmitted
to the CDHF and maintained in databases for use by the ISTP
investigators. The ISTP science initiative encompasses theory
investigations to produce improved models of the 3-D magnetosphere,
coupling with the ionosphere, thermosphere global circulation, and MHD
simulations. Datasets produced by these models will be maintained in the
CDHF.

On a regular basis, the key parameter datasets will be transferred from
the CDHF and copied, in the GSFC Data Distribution Facility (DDF), onto
storage media (optical disks) that are mailed to the designated
recipients. Media are also used to provide processed data to the
National Space Science Data Center (NSSDC). The NSSDC also receives key
parameter datasets via the local electronic network at GSFC from the
CDHF 2 to 5 days after they are generated. Cluster Science Data System
(CSDS) data products would be received by the NSSDC on suitable media by
agreements with ESA and the respective PIs. Also, for certain data
products, the NSSDC will have electronic access to datasets via the ESA
SPAN and the NSI networks.

The SPOF will provide a focus for quality control monitoring of key
parameter data products, using electronic access to the CDHF databases.
Remote Investigators may interface directly with SPOF or EOF for
planning of instrument command sequences.

Event data products will be produced as part of an ISTP science
initiative campaign activity or as the result of identifying
scientifically interesting "events" from the key parameter datasets.
Campaigns involve multi-mission international collaboration, coordinated
with the Inter-Agency Consultative Group (IACG) for space science,
addressing specific scientific topics.

Generally, identification of "events" from key parameter datasets will
result in further analysis at Remote Investigator facilities of the
associated higher resolution instrument data contained in the Level 0
products. Event data products resulting from these analyses are to be
archived at the NSSDC where they will be made electronically available.

.c2.4.1 Central Data Handling Facility

The Central Data Handling Facility (CDHF) is the centralized computer
system where measurements from the wide variety of geospace
instrumentation, ground-based instrumentation, and theoretical studies
are brought together and subsequently distributed, along with ancillary
data, in a unified fashion, to the ISTP PI and Co-I teams for further
analysis. The combined data sets from the participating spacecraft,
complementary ground-based observations, and theory

investigations will be used to obtain a more complete understanding of
how mass, momentum, and energy from the solar wind are transported
across geospace boundaries, stored and energized in the magnetosphere,
and subsequently dissipated into the Earth's atmosphere.

The CDHF (both hardware and software) has been designed to provide for
flexibility and substantial evolution as the program proceeds, in order
to accommodate the inevitably unforeseen developments. The reader is
referred to Lehtonen, \[1993\] or Mish, *et al.,* \[1993\] for details
on the architecture of the CDHF.

The major data services of the CDHF are summarized in Table 1.
Essentially, the facility ingests the telemetry streams (Level 0 data
and SIRIUS), orbit, attitude, and command history from the Wind, Polar,
Geotail, SOHO, and IMP-8 spacecraft, and KPs from a variety of other
correlative sources, and outputs KP data sets, Level 0, SIRIUS and
ancillary data. In addition, network transfers of most data products can
be scheduled on a recurring basis or done on an ad-hoc basis through the
CDHF data services menu. Section 5.2 discusses key parameter data
content in more detail.

.c2.4.2 Data Distribution Facility

The Data Distribution Facility (DDF) provides the data distribution and
delivery functions for the GSFC's Information Processing Division (IPD).
In this way, IPD saves the expense of building, operating, and
maintaining unique and distinct facilities and procedures for each
mission, while gaining the ability to better serve its customers. The
DDF can be easily upgraded to new distribution technologies as they
mature and are adopted as standard.

The ISTP data are transferred from the CDHF to the DDF over one of
GSFC's local area networks called InfoLAN. From there, it is reproduced
and distributed to the PIs and to the NSSDC.

The DDF is being developed in three phases. Phase I started operations
in 1992, supporting magnetic tape distributions for the Geotail mission.
This work served as a prototype for Phase II and III development. Phase
II allows ISTP distributions to be made on Compact Disk-Write Once
(CD-WO).

Phase III incorporates the latest technologies and standards to provide
an integrated and flexible system for supporting multiple missions with
a range of physical and electronic distribution capabilities, while also
greatly reducing the level of manual operations required. It is intended
that Phase III will be operational before the SOHO launch.

Phase II capabilities reside in three subsystems: a Host Computer
Subsystem (HCS), a Data Recording Subsystem (DRS), and the InfoLAN Mass
Storage System (IMSS). The HCS hardware consists of a VAX-11/785 and a
VAX 6000/410 and their peripherals. The DRS currently consists of three
personal computers connected by a Novell network, magnetic disk storage,
two Phillips CD-Write Drives, other peripherals (printers, diskette
drives, etc.), and software. The DRS and the HCS communicate using DEC's
Pathworks (subset of DECnet). The DRS is designed to be easily
expandable, not only with similar equipment, but with additional types
of recording devices and additional types of computers.

For Geotail, Wind, and Polar, DDF will distribute at least ten distinct
products. Some of these products will be distributed on a nearly daily
basis, while others may be distributed on a quarterly basis, based on
both the capacity of the media (DDF's current CD-WOs have a capacity of
about 650 Mbytes) and the turn-around time needed. Some of these
products will be distributed to only a few investigators, while others
may be distributed to as many as 100 investigators.

The DDF is currently producing approximately 8 CD-WOs per day for ISTP.
After Wind is launched in FY95, this will increase to 35 per day; and
after Polar is launched in FY95/96, this will increase to 53 per day.
These numbers do not include the copies being duplicated at an external
facility, or products being created for other projects.

.c2.4.3 Special Data Distribution Activities

Special data distribution activities have been established to meet the
needs of other Federal Agency programs for near real-time data. For
instance, the magnetic field and plasma KP data from the SWIM experiment
on the Wind spacecraft are computed by the CDHF within several minutes
of real-time acquisition and sent electronically to the Air Force Space
Weather Forecast Center via the Space Environment Laboratory (SEL) and
to the Air Force Phillips Laboratory over the NASA Science Internet.

.c2.4.4 The Science Planning and Operations Facility

The Science Planning and Operations Facility (SPOF) is the component of
the GGS (Wind and Polar) ground system responsible for the development
and coordination of ISTP science planning operations, and operates under
the direction of the ISTP Project Scientist. The SPOF computer system
consists of four UNIX-based workstations, one Macintosh and one personal
computer interfaced via the GSFC Local Area Network with the CDHF and
the GSFC Command Management System (CMS). Figure 3 provides a schematic
view of the SPOF functional interfaces. SPOF is responsible for the
development and coordination of the science plans for ISTP/GGS
spacecraft. In addition, the SPOF provides a communication link between
the PIs and the CMS for the transfer of Wind and Polar instrument
commands. SPOF responsibilities fall logically into three main
functions: (1) science planning activities, (2) operations activities,
and (3) science advancement functions; each of these functions is
explained below. For a more detailed explanation of the SPOF, the reader
is referred to Mish et. al, \[1993\].

.c3.4.4.1 SPOF Science Planning Functions

SPOF science planning functions include: (1) coordination of science
planning for Geotail, Wind, and Polar; coordination and planning efforts
also involve ancillary spacecraft such as IMP-8, GOES, LANL and others
as available; in addition, ground-based and theory elements are included
as necessary through the ISTP Deputy Project Scientist for Theory and
Ground-Based Experiments; (2) coordination of science operations for
Wind and Polar; (3) use of ephemeris and model tools to generate science
plans, including predicted "event" times; (4) generation of the Long
Term Science Plan (LTSP) based on inputs from the GGS Science Working
Group; (5) development of the BiWeekly Science Plan (BWSP) in
coordination with the PIs and the CMS; (6) review and quality control
checks on KP data; and (7) coordination with planning facilities from
other projects on a regular basis and specifically during science
campaigns.

Development of the LTSP is the responsibility of the GGS Science Working
Group (SWG), but SPOF interacts with the SWG to facilitate its
development. During the periodic meetings of the SWG, SPOF presents
results from its planning activities, including predicted crossings for
key boundaries, magnetospheric region occupation reports, and
anticipated magnetic conjunctions between spacecraft and/or ground-based
stations. Duration of the LTSP is approximately six months. The plan is
initially generated prior to launch, and subsequently updated after
periodic meetings of the SWG and the PIs. Records of accomplished
activities are fed back into the plan for accounting purposes. An
up-to-date copy of the LTSP is placed in a SPOF directory on the CDHF to
allow individual investigators to review the LTSP via their network
connection.

SPOF is responsible for the development of the BWSP in coordination with
the PIs and the CMS. Specifically, SPOF insures that the BWSP is free of
science-related conflicts and complies with the

LTSP. Validation with respect to engineering constraints is carried out
at the CMS, and folded into the BWSP by the SPOF. The BWSP is updated by
SPOF on a weekly basis and includes: (1) requests from the Wind and
Polar PIs for instrument activities and/or instrument reconfigurations;
(2) inputs from the Project Scientist and SWG; (3) instrument
coordination procedures; (4) procedures for coordination with other
missions when appropriate; and (5) inputs from GGS-related activities.
As with the LTSP, PIs will have access to a copy of the BWSP via the
CDHF.

.c3.4.4.2 SPOF Operations Functions

SPOF is responsible for the following operations functions: (1)
maintaining a communication link with the RDAFs via the NSI network for
receiving instrument commands; (2) ensuring security of this interface;
(3) receiving all Wind and Polar instrument command requests,
microprocessor loads, and any special scheduling event definitions from
the PIs via the RDAFs; (4) checking commands for compliance with the
science plans, time tagging if required, and resolving any science
conflicts; (5) forwarding all Wind and Polar instrument command requests
and microprocessor loads to the CMS for engineering constraint
validation; (6) obtaining command history, daily mission schedule, and
DSN schedules from the CDHF; (7) accepting validation reports from the
CMS; (8) developing and maintaining the SPOF databases and the
associated reports placed in a SPOF directory on the CDHF, *e.g.*, LTSP,
BWSP.

Instrument command requests (ICRs) transmitted by the PIs to the SPOF
are checked for science conflicts and compliance with the overall
science plan, and subsequently are transmitted to the CMS for validation
with respect to engineering constraints. Upon science and engineering
validation, requests are incorporated into the BWSP and the detailed
operations schedule.

The Interface Control Document (ICD) between the CMS-SPOF-PIs describes
in detail the file formats used for ICRs; command mnemonics are
interpreted using the mnemonic dictionary contained in the project data
base resident on the SPOF.

Microprocessor data, generated by the PIs for their instruments, are
composed of instructions and/or data to be stored in the memory of their
onboard instrument microprocessor. It is the PI's responsibility to
validate the microprocessor data and to segment it into loadable blocks
of bytes. The SPOF performs no value-added functions for microprocessor
loads, but just passes them on to CMS.

.c3.4.4.3 SPOF Science Advancement Functions

SPOF Science Advancement Functions involve active participation of SPOF
scientists in ISTP related research. SPOF researchers are currently
involved with the ISTP/GGS Theory Program, where they are collaborating
with ISTP Theory Investigators, under the direction of the ISTP Deputy
Project Scientist for Theory and Ground-Based Experiments, on the
assessment and comparison of various global magnetospheric models based
on both data as well as MHD simulations, in order to evaluate their
value as quantitative guides in gluing together the ISTP spacecraft
observations. Furthermore, research collaborations with various ISTP
scientists are underway, and it is anticipated that more will emerge as
the project unfolds.

SPOF personnel are active members of the ISTP/GGS Theory Group working
under the direction of the ISTP Deputy Project Scientist for Theory and
Ground Based Experiments. The Theory Group is concentrating on the
comparison and evaluation of global magnetospheric models. Initial tests
involved inter-calibrations between magnetohydrodynamic (MHD)
simulations, and comparisons between empirical magnetic field models and
MHD simulations. The most significant improvement to the MHD simulations
has been the extension of the modeled domain to 300-400 RE in the
tailward direction. Several key tests have been devised to validate
these simulations by the GGS Theory Group. Results from the MHD
simulations will be made available to the ISTP

community via the CDHF; in addition, SPOF will integrate such MHD
results into its scientific visualization mission planning tools.

Global magnetic field models are among the essential tools required for
SPOF operations. The widely used Tsyganenko models \[Tsyganenko 1987,
1989 & 1990\] have been incorporated into the SPOF, and enhancements to
these models are under development. As new models become available and
are validated, they will be incorporated into the suite of tools
available to the SPOF for science planning and data analysis.

Effective mission planning tools are essential to SPOF operations. The
Satellite Situation Center (SSC) software \[Peredo, *et al.,* 1992a;
Parthasarthy, *et al.,* 1992; Aist-Sagara, *et al.,* 1993\] provides a
key baseline capability. SSC applications represent the core set of
ephemeris tools, capable of generating reports of magnetic conjunctions,
region occupancy, boundary crossings, coordinate conversions and limited
graphical displays. The SSC tools have been updated to include the most
recent magnetic field models, up-to-date definitions for key
magnetospheric regions, and to create a graphical user interface. The
SPOF has developed additional visualization analysis tools to compliment
the SSC. These tools are available from the SPOF.

.c2.4.5 SOHO Experimenters Operations Facility

The SOHO EOF functions are described in detail in the document by Poland
and Domingo \[1993\]. The EOF is to be located at NASA/GSFC and will
serve as the focal point for mission science planning and instrument
operations. Most EOF elements will be physically located at the SOHO
Solar Data Analysis Center (see below). From the EOF, experiment PI
representatives will receive real-time and playback flight telemetry
data, process these data to determine instrument commands, and send
commands to their instruments, both in near-real-time and on a delayed
execution basis. They will be able to perform data reduction and
analysis, and have capabilities for data storage. Workstations connected
to an EOF Local Area Network (LAN) will support the Project Scientists
and planning and operations staff in the EOF, and there will be
connections to external facilities to transfer data from GSFC support
elements, remote investigator institutions, other science observatories,
and ESA facilities. The EOF will also have connections to the SOHO
Mission Operations Control Center (SMOCC) and other required elements at
GSFC for scheduling and commanding the SOHO flight experiments.

The functions of the EOF relevant to this Data Management Plan are
detailed in the document by Domingo *et al.,* \[1993\]. Chapter 3 of
this document describes the data sets available in the EOF and at the
different SOHO facilities. NASA will forward real-time Level 0 (=
depacketized) data to the EOF over the LAN to the PI workstations with
no additional front-end processing for quality assessment. Playback data
will be sent to the EOF in the same manner with transmission delays from
DSN (approximately 3 hours) and processing delays to turn the data
around (approximately 2 hours). Level 0 housekeeping data are to be
treated in the same way, and will be available in both raw counts and
engineering units. A data set called ancillary data also will be
collected, consisting of various parameters relating to spacecraft
condition. Some of these ancillary data parameters will be transmitted
to the Data Distribution Facility (DDF) for distribution on hard media
to the PIs.

Summary data will be prepared to be used both to plan observations at
the EOF and to provide an overview of the observations that have been
obtained from SOHO. The EOF also will handle some processed science data
products, but it has not been determined if a central archiving facility
for the processed data products will be developed (at the EOF or NSSDC,
for instance).

.c2.4.6 Cluster Joint Science Operations Center

The Joint Science Operations Centre (JSOC) is located at the Rutherford
Appleton Laboratory in England. The purpose of the JSOC is to optimize
the scheduling of all Cluster instrument plans to

maximize the scientific return. In essence, the JSOC has similar
responsibilities for the Cluster mission as the SPOF does for GGS. (see
section 4.4).

.c.5.0 Data Products

Section 5 discusses the details of the generation and composition of
ISTP data products. Section 7 specifically addresses the accessibility
of the ISTP archival data products. Table 14 provides an overview of the
ISTP archival data products and associated software along with a summary
of their public accessiblity. It is important to note that not all the
data products from all the ISTP instruments will follow the
accessibility overview given in Table 14 due to a variety of funding and
instrument specific calibration processes. Therefore, Table 14 should be
used as a general guide to the ISTP data products.

.c2.5.1 SIRIUS Data

At this time there are no plans for archiving the SIRIUS data at NASA.

.c2.5.2 Level 0 Data

The CD-WOs produced by the DDF conform to the ISO 9660, which defines
both the physical and logical format of the CD-WO. This ensures that
most CD-WO drives on most platforms will be able to read the disk. In
addition, the CD-WOs produced by DDF follow other emerging NASA
standards, guidelines, and practices, especially use of SFDUs, and a
file naming and directory structure which will be compatible with most
platforms.

.c2.5.3 Key Parameters

In order to accomplish the ISTP scientific goals of correlative
analysis, the ability to quickly survey a vast array of scientific data
being gathered by the many spacecraft and ground-based data sources is
essential. The key parameter (KP) data product was designed to
accomplish the survey task. In general, KPs are low resolution time
series (on the order of 1 minute) computed from each instrument.

Both internally- and externally-generated KP data sets adhere to
mutually agreed upon standards and conventions to permit rapid analysis
and comparisons of the over 100 KP data sets from a variety of
instrumentation. The more important of these standards and conventions
are listed in Table 2. All KP data sets are created as Common Data
Format (CDF) files with ISTP Guidelines (see Kessel et al., 1994).

KPs computed internally to the CDHF are based on Level 0 (decommutated
telemetry) or SIRIUS data (full Geotail telemetry stream) as input.
There are also KPs generated externally to the CDHF which are ingested
from a variety of ground-based instruments and non-ISTP spacecraft (see
next sections). In general, each KP data set covers one complete day.
Internally-generated KPs are available within a few days of real-time
acquisition. The delay from real-time for externally-generated KPs can
range from near-real-time to several weeks, depending on their source.
For rapid access, KPs residing on the CDHF are also accessible via
standard computer networks (both DECnet and TCP/IP protocols are
supported) approximately 1 hour after generation or ingestion into the
CDHF.

Software for internally-generated KP production is provided by the PI
team for each instrument and is integrated into the CDHF production
environment prior to the launch (in most cases) of each spacecraft
(Wind, Polar, Geotail, SOHO, and IMP-8). The software and associated
documentation will be archived at the NSSDC.

The KP data product summaries for Wind, Polar, Geotail, and SOHO are
given in Tables 3, 4, 7, and 8, respectively.

The first 6 months after instrument turn-on is a period of time set
aside to allow these PI teams to come to a better understanding of the
on-orbit operation of their instrumentation and thus refine the KP
software appropriately. It is also anticipated that additional
refinement of the KP software will take place over the life of the ISTP
mission, so the CDHF environment has been designed to allow for rapid
update of KP software, and the ability to handle multiple versions of
the same KP data set, which can exist because of reprocessing.

Quality information is available for each KP data set in the CDHF
catalog. Each KP data set has quality flages that are generated and
embedded in the KP data records as part of the routine processing. Once
the PI groups have had a chance to review their KP data, they then put
the additional quality information into the CDHF data set catalog. This
latter quality information may be days to weeks after the KP data files
have been generated, and contains the information on the KP software
version.

The residency time for KP data sets on the CDHF storage is \~ 1 year.
CD-WO disks will be generated by the DDF for distribution to the ISTP
scientific community and NSSDC typically every 90 days. The long time
period is due to the likelihood of reprocessing the KP data after the PI
teams have done their quality evaluations. The DDF will write onto the
CDs the most recent version of the KP data.

The ISTP CD-WOs will use the ISO 9660 Level 1 standard to provide
compatibility across major computing platforms (for more details on
CD-WO formats, see Mish, *et al.,* 1993). In addition to the data files,
each CD contains an ASCII file listing the contents of the CD and a
cumulative index of all files distributed to date on CD.

Level 0, SIRIUS, orbit, attitude and spin phase data are used as input
into the PI-provided software that produces the CDHF
internally-generated KPs. The KPG software, which can be written in "C"
and/or FORTRAN (ANSI 77), does not directly interface with the VAX/VMS
operating system, but resides in a shell that provides some isolation.
Thus, input and output to the KP software is accomplished using various
"ISTP CDHF Software System" (ICSS) "calls" which, in turn, interact with
the operating system. For example, the Level 0, orbit, attitude, and
spin phase data required by a particular set of KPG software would be
obtained via these ICSS calls. Coordinate transformations are also
available via ICSS calls. Output to CDF files is through calls to the
CDF software.

Also ingested by the CDHF are externally-generated KPs from the
Ground-Based Investigations (GBIs), SOHO spacecraft (some SOHO KPG
software execute in the CDHF), Cluster , GOES 6 & 7 spacecraft, LANL89,
LANL90, and LANL91 spacecraft, the IMP-8 spacecraft, and the Interball
mission (only during IACG Campaign times, see section 6.2). These KPs
are sent to the CDHF via NSI.

The KP data product summary for ground-based data and supplementary
missions data are given in Tables 4 and 5, respectively.

Key Parameter data that reside in the CDHF are reviewed by the SPOF both
for monitoring the quality of the KP products, and to identify events of
scientific interest. Identification of unusual values in a KP data set
and/or irregularities will result in electronic mail from SPOF to the
appropriate PI. While the SPOF routinely spot-checks KP quality and
alerts investigators of anomalies, in all instances, the PIs are
responsible for evaluating if individual or global reprocessing of the
KP data is necessary.

Future funding for the U.S. instrument investigators will depend on
their ability to provide open access to KP data from Geotail, Wind, and
Polar. Investigators can choose to provide open access to the science
community at large to their KP data through the World Wide Web (WWW).
These data should be made available within 3 days after they have been
generated in the ISTP/CDHF or SPOF homepages. The non-citability of this
data will be prominently noted in the interface.

.c2.5.4 Citable Key Parameters

It is expected that the quality of the KP data will improve as the
investigators learn more about their instruments from in-orbit
calibrations and therefore improve the algorithms in the CDHF which
generate these data. The creation of additional citable KP data may also
result from reprocessing in the CDHF. Future funding to U.S. principal
investigators will depend on their ability to provide open access and
production of KP data of publishable quality (called citable KP data)
from ground-based instruments, the theory group, Geotail, Wind, and
Polar. All citable KP data sets are also created as ISTP Common Data
Format (CDF) files.

Accessibility to citable KP data by the science community at large will
be at the instrument investigators' discretion and could be made
available over the WWW as the non-citable KP data discussed in the
previous section. Because pre-launch funding for key parameters has been
omitted for most investigators (for Wind), it is recognized that there
will be a significant delay, perhaps up to 18 months, after launch
before citable KP data will be produced for some instruments.

.c2.5.5 Event Data

As mentioned above, the KP data sets will be used to identify
interesting scientific "events." In general, this identification will
result in analysis of the associated higher resolution instrument data
by the PI teams at their remote data analysis facilities (RDAF) using
Level 0 or SIRIUS data. The higher resolution data products generated by
this analysis are called event data. Event data products will also be
created as CDF files and submitted to the CDHF for subsequent joint
analysis and distribution on CD-ROM.

.c2.5.6 Other Data Products

Each of the investigators has facilities at his or her institution that
are used in processing, analyzing, and correlating ISTP data. In some
cases, it is expected that some investigators will routinely generate
additional instrument data products. These products along with
associated documentation and the generation software will be delivered
to the NSSDC for long-term archiving and community-wide distribution.
What these products are and how they will be managed is TBD but
decisions should be made approximately 18 months after launch of Wind
and Polar.

.c2.5.7 Archival Data Volume

Level 0 telemetry data is archived at the NSSDC. The basic science data
rates are estimated at:

[Spacecraft]{.underline} [Science Data Rate]{.underline} [Approximate
archive size]{.underline}

Wind 4.8 kb/s 19 GBytes/year

Polar 51.5 kb/s 202 GBytes/year

Geotail 16 kb/s 63 GBytes/year

When the Wind spacecraft is inside a radial distance of \~60 Earth Radii
(RE) the science data rate will probably be twice the above stated rate.
In addition, the VLF wide-band data rates will be:

Wind 64 kb/s @ 1-4 hours/day (currently planned)

Polar 250 kb/s @ 3.6 hours/day (12 hours/day for 1st month of mission)

It is estimated that once Geotail, Wind, and Polar are fully
operational, including the ground-based data, that approximately 20
megabytes/day of KP or citable KP data will be generated. This will
amount to approximately 10 gigabytes/year to be kept online in the NSSDC
archive (see section 7).

The proprietary data rights for all Wind and Polar data are given in
Appendix C and for Geotail in Appendix D.

.c2.5.8 SOHO Data Products

The SOHO data products are described in more detailed in Domingo *et
al.,* \[1993\]. In brief, the SOHO summary data will consist of three
classes of data. The first two classes will consist of representative
images from each of the imaging experiments (in SFDU/FITS), and key
parameter data from the non-imaging experiments (in SFDU/CDF). Both
these data types are shown in Table 8. The third class will be lists of
observing programs and start/stop times of data sequences. Serving as a
synopsis of solar conditions and the science programs that have been
carried out by SOHO, these summary data will be available on-line in the
EOF for 28 days and will then be transmitted to the DDF for distribution
on hard media (CD-WO) to the PIs. Due to their quick-look, unverified
status, the summary data will not be citable. An event log will be
maintained in the summary data file and be distributed by the DDF, but
the contents of the log will be allowed to change, reflecting revisions
to include events identified by observatories other than SOHO.

The summary data also are to include planned and actual observing
programs, describing the instrument operation modes and heliographic
areas covered. The summary data are to be archived in the permanent SOHO
archive at NSSDC.

Each PI team will transform the Level 0 data and related data into
processed data files, or they will maintain software which is used to
perform direct scientific analysis with Level 0 data. The details of the
archived science data files may be found in the individual experiment
Operations Manuals.

The processed science data files that are expected to be generated are
given in Table 9. In addition to the science data products, various
catalogs are to be compiled in database tables that are to be linked
together using standard relational database techniques. The information
in these database tables includes general information about observing
programs, specific information about the actual observing sequences used
to carry out those observing programs, and information about events that
may be relevant to more than one instrument. A standard query language
(*e.g.*, SQL) will be used to access the databases. These catalogs may
be accessed electronically over the EOF LAN.

All of the data products described in this section are to be accessible
during the lifetime of the SOHO project at the SOHO Solar Data Analysis
Center (see section 6.3 below) and permanently archived at NSSDC.

.c2.5.9 Cluster Data Products

It is expected that a wide scientific community from over 20 nations
will be using Cluster data. The Cluster mission will produce several
types of data products that will be processed and distributed from the
data centers which are part of the Cluster Science Data System (CSDS)
\[see for example, Schmidt, R., and L. J. C. Woolliscroft, 1993\].

The Summary Parameter Database (SPD) is comparable to the KP data
generated in the GGS and Geotail missions. These data are approximately
60 scientific and ancillary parameters at 1 minute resolution from a
single Cluster spacecraft and will be widely accessible for selection of
events. The SPD parameters are listed in Table 10. In addition to the
digital SPD, Summary Data Plots (SDP) will be generated at the Cluster
Science Data Centers and also used for event selection. The SDP are
mainly line plots of the SPDB parameters with temporal resolutions of
between 30 and 60 seconds.

The Prime Parameter Database (PPDB) will be about 60 scientific
parameters at a temporal resolution of about 4 seconds (approximately
one spin period). These data are generated from each instrument on all
four spacecraft and will contain ancillary spacecraft information. The
PPDB will be available to all Cluster Investigators through the CSDS.

The highest resolution data from Cluster will not be part of the ISTP
CDHF (which is also serving as the U.S. Cluster Science Data Center),
but will reside at the PI institutions. The PIs are to respond to
requests from the science community for individual high resolution event
data.

.c2.5.10 Solar Wind Catalog

Detailed knowledge of the solar wind conditions upstream of the
magnetosphere is essential to the understanding of the transfer of
energy across the solar wind-magnetosphere-ionosphere system. As such,
widespread interest in solar wind information is anticipated across the
ISTP and science communities. A collaboration has been established
between SPOF and Dr. R. Lepping to jointly develop a catalog of solar
wind events observed by the IMP-8 and WIND spacecraft. This catalog will
be made available to ISTP scientists through the CDHF to aid in the
correlative analysis and will be archived at the NSSDC.

.c.6.0 Correlative Science Data Management

.c2.6.1 Campaign Coordination Functions of the SPOF

The SPOF is responsible for the science planning and coordination of GGS
campaigns; in addition, SPOF works closely with the science planning
facilities from non-ISTP programs such as those from the Inter-Agency
Consultative Group (IACG) participants (see below) in order to promote
optimal use of resources and effective coordination across these
programs. In the campaign mode, SPOF operates according to its nominal
operations schedule, but with special emphasis on verification that all
instruments operate in modes compatible with campaign goals, unless
there are instrument health/safety issues.

.c2.6.2 Inter-Agency Correlative Science Activities

The IACG for space science was formed in 1981 by the scientific heads
from four space agencies: ESA (European Space Agency) of Europe, IKI
(Institut Kosmicheskikh Issledoranii, *i.e.*, Space Research Institute)
of Russia, ISAS (Institute of Space and Astronautical Science) of Japan,
and NASA of the United States. The main goal of the IACG was to increase
the overall scientific return from their missions through cooperation
among the agencies. In the early 1980s, the IACG coordinated efforts to
study Halley's Comet. The success of the coordinated effort of
observations on Halley's Comet provided the basis for further
cooperation. In 1986, IACG adopted solar-terrestrial science as their
next science focus. In the 1990s, the four member agencies have up to 25
projects involving over 35 spacecraft that are either fully or partially
dedicated to studies of the solar-terrestrial environment. A core set of
spacecraft has been defined to play the major role in coordination
effort. The primary spacecraft to be included in the core group are the
Wind and Polar (from NASA), Geotail (from ISAS), the four Interball
(from IKI), and the SOHO and the

four Cluster spacecraft (from ESA). It is important to note that the
four Interball spacecraft have been added to the ISTP core missions to
make up the IACG core missions.

Implementation plans for the first and the second IACG campaigns have
been completed. The first IACG campaign will focus on the study of
magnetotail energy flow and non-linear dynamics \[see Whipple and
Lancaster, 1992\]. The second campaign plan is on boundaries in
collisionless plasmas \[see Whipple and Lancaster, 1993\]. The third
IACG campaign has been defined as "solar events and their manifestations
in interplanetary space and in the Earth's magnetosphere," but an
implementation plan has not yet been completed. The fourth IACG campaign
is on "solar-heliospheric structures out-of-the ecliptic." An
implementation plan for this last campaign should be completed by April
1994.

For the campaigns to be successful, it is recognized that:

> • The data exchange between mission communities be facilitated by
> harmonized data systems. The exchange of higher-resolution data than
> key or summary parameters for the periods of coordinated measurements
> should be envisaged and is currently being planned.
>
> • The mission-oriented theory and numerical simulation communities be
> involved in the planning and execution of campaigns.
>
> • The individual mission-related ground-based observation programs be
> coordinated and integrated into the ISTP data management activities.
>
> • The agencies' science mission planning facilities be available for
> predictions of the proper spacecraft constellations.

Specific science topics identified for the first campaign included:
definition of structure and energy flow through the boundary layers of
the Earth's magnetosphere, definition of the quiescent extended
configuration of the magnetotail and its dependence on ambient solar
wind plasma and fields, the origin of plasma in the magnetospheric
plasma sheet, mapping the response of the magnetosphere to
externally-driven disturbances, and understanding the physics of
internal magnetospheric instabilities and energy release. The key
spacecraft for this campaign will be Geotail (in the deep tail), Wind
(monitoring the solar wind), Polar and Interball/Aurora (measuring
auroral forms and particle precipitation), and Interball/Tail (in the
near-Earth tail region). Key parameter data from both Interball/Tail
(see Table 12) and Interball/Aurora (see Table 13) will be generated in
Russia and networked to the ISTP/CDHF for data management and accesses.

The SPOF will help coordinate campaign planning by combining spacecraft
ephemeris and model software to predict advantageous times for campaign
intervals. As discussed above, the SPOF uniquely combines spacecraft
ephemeris and model software to predict intervals when the spacecraft
are in advantageous positions for scientific studies, and presents the
results to the IACG Science Working Group Teams for campaign planning.
The SPOF plays an essential coordination role of working closely with
the science planning facilities from the other agencies.

Once the planning is complete and the data have been acquired, the ISTP
key parameter data will be reviewed to identify specific intervals for
detailed investigation. Additional data sets, such as those resident at
NSSDC or at other investigator facilities, will be incorporated into the
event identification and detailed analysis processes in accordance with
agreements between members of the IACG science community. Detailed event
data will be analyzed and inter-compared, obtaining a scientific
understanding that could not be accomplished by one instrument or
spacecraft data alone. The science analysis will be accomplished through
a series of Coordinated Data Analysis Workshops (or CDAWs). It is
envisioned that the CDAWs will be both centralized and

distributed, being hosted by more than one agency. These CDAWs will make
use of existing data centers and facilities necessary to manage and
manipulate the large volumes of data expected. The rules for data rights
for the IACG 1st Campaign are given in Appendix G.

.c2.6.3 SOHO Solar Data Analysis Center

The Solar Data Analysis Center (SDAC), currently located at NASA/GSFC,
is intended to become the SOHO mission data analysis center and main
archive site. Originally created to serve the EOF of the Solar Maximum
Mission in 1979, the SDAC currently serves as main distribution center
for CGRO/BATSE solar hard X-ray data, Yohkoh data, and SMM data. Current
plans call for the SDAC to move from its present location in building 21
to building 26 (by January 1995), where it will be co-located with the
ISTP facility there. The SDAC will continue supporting access and
guidance in using solar archive data the SDAC already holds, while
supporting new SOHO observing plans and archiving. That is, the SDAC
will be the site of most SOHO science planning EOF functions, whereas
daily/hourly/near-real-time SOHO operations are to be controlled from
the EOF at GSFC building 3. The SDAC includes workstations, data storage
facilities and personnel to carry out these functions.

.c2.6.4 Cluster Science Data System

There will be eight Cluster data centers which make up the CSDS. Nearly
all of the Cluster data centers are responsible for generating and
distributing a number of data products from specific Cluster
instruments. Each PI is associated with one of these data centers. The
data centers and the associated instruments are listed in Table 11 (see
Daly *et al.,* \[1993\] for more details). Not all the Cluster data
centers offer the same services. For instance, the U.K. data center at
RAL will provide an on-line archive of the summary and prime parameter
datasets, while the German data center at MPE Garching plans to hold
little reduced data on-line, but to hold access software to the Level 0
data. The rules for data rights for the Cluster mission are given in
Appendix F.

.c.7.0 Data Archiving and Distribution

The raw and processed data generated in the CDHF from the NASA/GGS
spacecraft are being routinely archived at the NSSDC for long-term
access. These data products come to the NSSDC in two distinct ways. The
NSSDC receives the CD-WOs generated from the DDF. As discussed earlier,
these CDs contain KPs, decommutated telemetry, and associated ancillary
data. The CD-WO data from the DDF is managed and held in an off-line
archive. The NSSDC also receives, on a daily basis, KP data that exceeds
a few days old from the time they are generated on the CDHF. These KP
data are placed in an on-line archive system and are accessible to
registered ISTP users and IACG campaign participants. These data are
being managed as proprietary data products and will not be released to
the general scientific community until the proprietary period has
expired. The length of the proprietary period is TBD. In addition, the
event data will also be stored in the NSSDC on-line archive facility
when it becomes available.

.c2.7.1 Data Archive Products Contents and Disposition

An overview of the data products generated from Wind, Polar, Geotail and
their disposition is shown in Table 14.

.c2.7.2 Archive Data Access

The NSSDC's on-line archive facility that is being used for the rapid
access to all the archived KP data is called the NASA/NSSDC Data Archive
and Distribution Service, or NDADS. The purpose of the NDADS system is
to manage public data and data that will eventually be made public.
Since

the CDHF's primary purpose is to process and distribute the most recent
ISTP data, it is not designed to manage all the processed and archive
ISTP data. ISTP investigators wanting retrospective ISTP data will then
have to access the NSSDC's archive. NDADS provides archive data services
not only to ISTP scientists, but also to a worldwide science user
community. Access to ISTP data (after the proprietary period) by the
general science community will be through the NDADS system and not
though the CDHF. For more details on the NDADS system architecture, the
reader is referred to Mish, *et al.,* \[1993\].

One of the most important features of the NDADS system is that it
provides the capability for scientists to retrieve data from the archive
by several methods. The public data archive can easily be accessed
through the automated retrieval mail system, or ARMS \[Van Steenberg,
1993\]. Users initiate a data request from their remote machines using a
specifically formatted mail message. Once a request has been initiated,
the data are quickly retrieved from the optical storage system and
placed in a staging disk on NDADS, or sent automatically to the remote
user's location via networks (such as the NSI-DECnet and the TCP/IP
Internet).

For the proprietary ISTP data, interactive accounts are being
established on NDADS to authenticate users. Authorized accounts for
accessing ISTP proprietary data are approved by the NASA/ISTP Science
Office. The interactive NDADS interface for accessing the ISTP data
provides a full help facility, data selection, electronic data ordering,
data browse, and is compatible with VT100-type terminals up to
X-terminals. An interactive interface for accessing and visualizing
various aspects of the public data on NDADS is currently under
development and will be heavily based on the existing ISTP interface.
The NDADS system is operational nearly 24 hours/day, 7 days/week and is
a major archive and data distribution facility on the Space Physics Data
System.

.c.8.0 Project Data Management Documentation

An extensive amount of data management documentation for the ISTP
mission is currently available. Appendix H provides the current list of
ISTP data management documentation.

.c.9.0 References

Daly, P. W., W. Baumjohann, J. Dandonras, K-H. Glabmeier, C. Harvey, S.
Schwartz, K. Tokar, L. J. C. Woolliscroft, "Report of the data products
task group for the Cluster Science Data System," DS-MPA-TN-001,
February, 1993.

Domingo, V., A. Poland, B. Fleck, and T. Appourchaux, "SOHO Science
Operations Plan," Issue 1.1, June 1993.

Domingo, V., and T. D. Guyenne, editors, "The SOHO Mission," ESA
SP-1104, 1989.

Kessel, R. L., R. E. McGuire, H. K. Hills, and N. J. Love, "CDF
Implementation Guidelines for ISTP", Version 2.3, February 7, 1994.

Lehtonen, K., "Architecting the International Solar-Terrestrial Physics
(ISTP) Central Data Handling Facility (CDHF)," GSFC Technical Document,
June 1993.

Mish, W. H., M. Peredo, J. L. Green, and M. G. Reph, "ISTP Science Data
Systems and Products," submitted for publication, 1993.

Poland, A., and V. Domingo, "SOHO Experiment Operations Facility
Functional Requirement Document," Draft Version 1.0, 1993.

Schmidt, R. and M. L. Goldstein, editors, "The Cluster Mission," ESA
SP-1103, 1988.

Schmidt, R., and L. J. C. Woolliscroft, "Cluster Science Data System - A
distributed system to serve a wide international community," 1993.

Whipple, E. C., and H. Lancaster, editors, "Toward A New Era of Global
Solar-Terrestrial Research - The First IACG Campaign: Magnetotail Energy
Flow and Non-Linear Dynamics," Science Applications International
Corporation (SAIC), October 1992.

Whipple, E. C., and H. Lancaster, editors, "Toward A New Era of Global
Solar-Terrestrial Research - The Second IACG Campaign: Boundaries in
Collisionless Plasmas," Science Applications International Corporation
(SAIC), October 1993.

.c.Acknowledgments

Comments by David Batchelor, Evan Eller, Shing Fung, Joseph Gurman, Mona
Kessel, Joseph King, Robert McGuire, William Mish, and Arthur Poland are
gratefully acknowledged. In addition, I would like to gratefully
acknowledge Mauricio Peredo for developing and maintaining the GGS Key
Parameter summary tables used in this report. I would also like to
acknowledge the members on the SAIC staff for their assistance in
compiling the information in the brief instrument descriptions for Wind
and Polar, given in Appendices A and B, respectively.

.c.Figure Captions

Figure 1 - The level 0 data capture facilities for the ISTP mission. The
ESA network is used to track and capture the Cluster spacecraft and
instrument data. The NASA DSN is used to track and capture the Geotail,
Wind, Polar, and SOHO spacecraft and their instrument data. The NASA
STDN system is used to track and capture the IMP-8 spacecraft and
instrument data. The ISAS network tracks and captures the Geotail
spacecraft and high rate data.

Figure 2 - The process data flow for ISTP. KP data from SOHO,
ground-based instruments, IMP-8, GOES 6 & 7, and the LANL equatorial
spacecraft are generated on computer systems external to the CDHF. SOHO
KP data will be processed in the EOF and in the CDHF (three
instruments). The SOHO KP data processes in the EOF will be networked to
the CDHF for data management and distribution. The KP data from the CDHF
is then sent to the DDF and NSSDC facilities. The CSDS will provide
Cluster data to the NSSDC.

Figure 3 - SPOF Functional Interfaces include transmission of instrument
command requests and science coordination plans with the GGS Science
Working Group and PIs at their RDAFs. Wind and Polar commands, command
validation and schedule submissions are exchanged with the CMS. Key
Parameter, ephemeris and ancillary data are extracted from the CDHF,
while SPOF reports are placed on the CDHF for access by the PI teams.
Coordination of science planning activities takes place between SPOF and
the SSC.

.c.**Table 1 - Data Services at the CDHF**

> **Service for accessing and transferring data**
>
> • Provides an electronic interface with the RDAFs for support of
> remote login, file transfer, and electronic mail.
>
> • Data can be marked proprietary.
>
> • Transfers of data can be scheduled to occur at specified times.
>
> • Queries for data can be scheduled to run at regular intervals with
> the data automatically sent to a specified destination.
>
> • On-line, limited plotting of orbit and KP data.
>
> • Quick-look instrument telemetry available in "near real time" over
> network.
>
> **On-line retention of data**
>
> • KPs on-line for at least 1 year.
>
> • Orbit, attitude, and command history on-line for at least 1 year.
>
> • Telemetry data on-line for 8 days.
>
> **Database queries and reports**
>
> • Users can query the CDHF databases for information about ISTP data
> sets.
>
> • Users can generate reports from these databases.
>
> • Authorized users can update database entries to indicate quality of
> KP data.
>
> **Infrastructure support**
>
> • Provides a means of monitoring/accounting for the status of data
> import/export, data processing tasks, and network activity.
>
> • Provides a data store for the SPOF.
>
> • Provides both a KPGS development environment and a KPGS production
> environment.
>
> • Provides a scheduler to handle recurring tasks and recurring network
> activity.
>
> • Provide a computational platform for parameterized theoretical
> models.

.c1.**Table 2 - Key Parameter Standards and Conventions**;

> • KP time resolution is on the order of 1 min (actually, many KPs are
> time tagged using multiples of 1/2 the Major Frame rate of the
> spacecraft. Major Frame rates are: Geotail - 16 sec; Wind - 92 sec or
> 46 sec; Polar - 9.2 sec; IMP 8 - 1.28 sec) and is generally time
> tagged to the middle of the measurement.
>
> • KP time tag is presented in two separate representations in each KP
> record.
>
> \- ISTP Standard Time (Time_PB5) - An intuitive representation (Year,
> Day, & elapsed ms of day).
>
> \- NSSDC Standard Time (Epoch) - A representation easy to use in
> computing and display elapsed ms since AD.
>
> • Missing or bad KPs are represented with standard "fill" values.
>
> • Coordinate systems for KPs are left to the discretion of the PI
> teams - GSE & GSM are common systems used by many of the KPs.
>
> • Externally generated KPs always have spacecraft position and
> attitude embedded in each KP record, if appropriate. Again, the
> particular coordinate system is left to the discretion of the PI team.
>
> • Each KP record contains quality information; also the CDHF catalog
> stores quality information for each individual KP data set.
>
> • Each KP record contains a Post Gap flag that explains, if
> appropriate, the reason a gap in data coverage occurred.
>
> • Generally KP data sets span one day.
>
> • All KP data sets (both external and internal) are presented as CDFs
> with detached SFDUs.
>
> • KP software is written in FORTRAN and C.

.c1. **Table 3 - Wind KP Data Product Summary**;

  --------------- -------------------------------------------- -------------
  Investigation   Key Parameters                               Time
                                                               resolution

  --------------- -------------------------------------------- -------------

  ------------- -------------------------------------------- -------------
  WAVES         Ne, Peak, avg. for **E,B** per freq decade   2 min

  ------------- -------------------------------------------- -------------

+------------+--------------------------------------------+------------+
| SWE        | Bulk velocity: (Vx, Vy, Vz)GSE, (Vx, Vy,   | At least   |
|            | Vz)GSM, (V,Vlong, Vlat)GSE, proton         | every      |
|            | density,                                   |            |
|            |                                            | 2 min      |
|            | 100 \* (alpha part. density/proton         |            |
|            | density)                                   |            |
|            |                                            |            |
|            | Most probable proton thermal speed         |            |
|            |                                            |            |
|            | Delta time (1/2 length of spectra)         |            |
|            |                                            |            |
|            | (X,Y,Z)GSE, (X,Y,Z)GSM, R                  |            |
+------------+--------------------------------------------+------------+

+------------+--------------------------------------------+------------+
| 3-D PLASMA | e flux: 7 energies (0.1-225 keV),          | 46 or 92   |
|            |                                            | sec[^1]    |
|            | ion flux: 7 energies (0.07 - 400 keV)      |            |
|            |                                            |            |
|            | Ne, Ni, **Ve**, **Vi**, Te, Ti, e heat     |            |
|            | flux along **B**, **V**s/c (GSE),          |            |
|            | (X,Y,Z)GSE                                 |            |
+------------+--------------------------------------------+------------+

+------------+--------------------------------------------+------------+
| MFI        | \|\<**B**\>\|, \<\|**B**\|\>, RMS, Num.    | 46 or 92   |
|            | pts. in avg.,                              | sec1       |
|            |                                            |            |
|            | (Bx, By, Bz, B, f, l)GSM; (Bx, By, Bz, B,  |            |
|            | f, l)GSE,                                  |            |
|            |                                            |            |
|            | (X,Y,Z)GSE, (X,Y,Z)GSM, R                  |            |
+------------+--------------------------------------------+------------+

+------------+--------------------------------------------+------------+
| SMS        | PARTICLE FLUXES                            | 2.0 min    |
|            |                                            |            |
|            | Differential Intensity (10-6 - 10-5        | 3.0 min    |
|            | part/cm2-sec-sr-keV/e)                     |            |
|            |                                            | 3.0 min    |
|            | SOLAR WIND PARAMETERS                      |            |
|            |                                            | 3.0 min    |
|            | Solar wind speed:                          |            |
|            |                                            | 3.0 min    |
|            | H+ (150 - 2370 km/sec)                     |            |
|            |                                            |            |
|            | Fe+10 (60 - 1000 km/sec)                   |            |
|            |                                            |            |
|            | Solar wind density (10-6 - 102 cm-3)       |            |
|            |                                            |            |
|            | Solar wind kinetic temperature (104 - 108  |            |
|            | K)                                         |            |
+------------+--------------------------------------------+------------+

+------------+--------------------------------------------+------------+
| TGRS       | Major Frame Number, Instrument Mode, Fast  | 5 min      |
|            | Rate Counter                               |            |
|            |                                            |            |
|            | Major Frame Accumulation, Average Fast     |            |
|            | Rate                                       |            |
+------------+--------------------------------------------+------------+

+------------+--------------------------------------------+------------+
| EPACT      | STEP fluxes:                               | 46 or 92   |
|            |                                            | sec1       |
|            | He3 (80-160 keV/n), He5 (320-640 keV/n),   |            |
|            |                                            |            |
|            | CNO3 (80-160 keV/n), CNO5 (320-640 keV/n), |            |
|            |                                            |            |
|            | Fe3 (80-160 keV/n), Fe6 (320 to 640 keV/n) |            |
|            |                                            |            |
|            | LEMT fluxes:                               |            |
|            |                                            |            |
|            | He (3.2-6.2 keV/n), O (3.2-6.2 keV/n),     |            |
|            |                                            |            |
|            | Fe (3.2-6.2 keV/n)                         |            |
|            |                                            |            |
|            | APE-A fluxes:                              |            |
|            |                                            |            |
|            | Electrons (0.2-2 MeV/n), Protons (4.6-6.6  |            |
|            | MeV/n)                                     |            |
|            |                                            |            |
|            | Protons (6.6-25 MeV/n), He (4.6-6.6        |            |
|            | MeV/n),                                    |            |
|            |                                            |            |
|            | He (6.6-25 MeV/n)                          |            |
|            |                                            |            |
|            | APE-B:                                     |            |
|            |                                            |            |
|            | Electrons (1-10 MeV), Protons (19-28       |            |
|            | MeV/n)                                     |            |
|            |                                            |            |
|            | Protons (28-72 MeV/n), He (19-28 MeV/n)    |            |
|            |                                            |            |
|            | He (28-72 MeV/n)                           |            |
+------------+--------------------------------------------+------------+

  ------------- -------------------------------------------- -------------
  KONUS         n/a                                          

  ------------- -------------------------------------------- -------------

.c1. **Table 4 - Polar KP Data Product Summary**;

**(page 1 of 3)**

  --------------- -------------------------------------------------- ------------
  Investigation   Key Parameters                                     Time
                                                                     resolution

  --------------- -------------------------------------------------- ------------

+---------+--------------------------------------------------+--------+
| TIMAS   | Partial density for H+ (low, med, high energy    | 1 min  |
|         | range), O+ (low, med, high energy range), He+    |        |
|         | (full energy range) and He++ (full energy        |        |
|         | range); Three dimensional velocity for H+ (low,  |        |
|         | full energy range), O+ (low, full energy range), |        |
|         | Temperature (parallel, perpendicular to **B**)   |        |
|         | for H+ (low, full energy range), O+ (low, full   |        |
|         | energy range)                                    |        |
|         |                                                  |        |
|         | NOTE: Energy ranges not final until after        |        |
|         | instrument calibration, but best guess about     |        |
|         | ranges is: density_low_E_range (15 eV to 100     |        |
|         | eV), density_medium_E_range (100 eV to 1 keV),   |        |
|         | density_high_E_range (1 keV to 30 keV),          |        |
|         | vel_temp_low_E_range (15 eV to 1 keV) and        |        |
|         | vel_temp_full_E_range (15 eV to 30 keV)          |        |
+---------+--------------------------------------------------+--------+

  ---------- -------------------------------------------------- ---------
  MFE        POS-GSE, POS-GSM, RAD-DIST, (T,H)=tilt angle of    0.92 min
             dipole axis using dipole moment of date (IGRF with 
             secular correction), B-Total (every 9.2 sec), BSC  
             (**B** in s/c coords., every 9.2 sec), Comp_Delta  
             (compressional standard deviation of the magnetic  
             field in nT calculated over 6 vectors),            
             Trans_Delta (Square root of the sum of the         
             variance in the x, y and z direction less the      
             compressional variance, BTAV (average magnitude of 
             the magnetic field, averaged over 0.92 min from    
             magnitudes taken every 9.2 s, **B**--GSE,          
             **B**-GSM, BTIGRF (IGRF magnetic field magnitude   
             calculated at the epoch of the measurements using  
             the IGRF and secular terms), BCIGRF_GSE            
             (Components of the IGRF magnetic field calculated  
             at the epoch of measurement in GSE coords.),       
             BCIGRF_GSM (Components of the IGRF magnetic field  
             calculated at the epoch of measurement in GSM      
             coords.), BT_Model (Magnitude of the Tsyganenko    
             magnetic field model using the tilt of the dipole  
             and the T89c model for the Kp=3-, 3, 3+ range,     
             calculated every 9.2 sec and averaged over the     
             0.92 min of the observed field), BC_MODEL_GSE (the 
             3 components of the Tsyganenko magnetic field      
             model using the tilt of the dipole and the T89c    
             model for the Kp=3-, 3, 3+ range, calculated every 
             9.2 sec and averaged over the 0.92 min of the      
             observed field; rotated into GSE coordinates;      
             epoch of the measurements is used to calculate     
             model), BC_MODEL_GSM (the 3 components of the      
             Tsyganenko magnetic field model using the tilt of  
             the dipole and the T89c model for the Kp=3-, 3, 3+ 
             range, calculated every 9.2 sec and averaged over  
             the 0.92 min of the observed field; rotated into   
             GSM coordinates; epoch of the measurements is used 
             to calculate model), FOOT_PRINT (the northern      
             geographic longitude and latitude and the southern 
             geographic longitude and latitude respectively of  
             the foot print of the field line that passes       
             through the spacecraft in the model field)         

  ---------- -------------------------------------------------- ---------

  ---------- -------------------------------------------------- ---------
  HYDRA      Mean electron energy, Mean ion energy, Index       \~ 1 min
             indicating detection of statistically significant  
             beam or void in the source/loss cone region,       
             Energy at which the structure in the source/loss   
             cone is inferred to be present                     

  ---------- -------------------------------------------------- ---------

  ---------- -------------------------------------------------- ---------
  EFI        E-spin plane (V12), Erms (V12); Ex, Ey (V12), avg. 9.2 sec
             sigmas (V12); Ex', Ey' (V34), avg. sigmas (V34);   
             s/c potential, band pass filters 1-3, V34          
             potential; probe bias currents (V12, V34, V56)     

  ---------- -------------------------------------------------- ---------

.c1. **Table 4 - Polar KP Data Product Summary**;

**(page 2 of 3)**

  --------------- -------------------------------------------------- ------------
  Investigation   Key Parameters                                     Time
                                                                     resolution

  --------------- -------------------------------------------------- ------------

  ---------- -------------------------------------------------- ---------
  PWI        Dt (half a time interval), fce,p, MLAT, MLT, R     1 min
             (geocentric radial distance), **E** peak, **E**    
             average, **B** peak, **B** average, Freq.,         
             SFR_Mode                                           

  ---------- -------------------------------------------------- ---------

+---------+--------------------------------------------------+--------+
| CAMMICE | Integral Spin Averaged Fluxes: He+ (\~40 keV -   | 96 sec |
|         | \~400 keV), He++ (\~30 keV - \~400 keV), O+      |        |
|         | (\~80 keV - \~400 keV),                          |        |
|         |                                                  |        |
|         | O≥2+ (\~50 keV - \~400 keV), He (\~300 keV -     |        |
|         | \~10 MeV),                                       |        |
|         |                                                  |        |
|         | CNO (\~300 keV - \~15 MeV), \>CNO (2 MeV - \~15  |        |
|         | MeV)                                             |        |
|         |                                                  |        |
|         | Angular Distributions (Anisotropy parameters):   |        |
|         |                                                  |        |
|         | He+, He++ (\~50 - \~ 100/keV/amu),               |        |
|         |                                                  |        |
|         | O+ (\~50 - \~ 200/keV/amu), He, O (\>            |        |
|         | 100/keV/amu)                                     |        |
|         |                                                  |        |
|         | Spectral Fits (Cubic in Log J vs. Log E space):  |        |
|         | He+, He++, O+                                    |        |
+---------+--------------------------------------------------+--------+

  ---------- -------------------------------------------------- ---------
  VIS        1\. Pixels (image pixel counts range from 0 to     5 min
             255); 2,3. Center time (the time assigned to an    
             image is the center time of the integration period 
             within a resolution of 50 msec); 4. Image source   
             (sensor number, 1=low res, 2=med res, 3=Earth      
             sensor); 5. Half integration time; 6. Filter wheel 
             position; 7. Field-stop wheel position; 8.         
             Platform pitch angle; 9,10. Mirror pointing        
             angles - elevation and azimuth in s/c coordinates; 
             11,12. Geographic coordinates every 15th row and   
             every 15th column; 13. Spacecraft position vector  
             in GCI coords. for the image center; 14. Presumed  
             altitude of emissions; 15,16,17. Image-to-GCI      
             rotation matrix; 18. Zenith angle of center        
             line-of-sight at presumed altitude; 19. Sun vector 
             in GCI coords. for the image center time given in  
             KPs 2 and 3; 20. Solar zenith angle at observed    
             point of center line-of-sight; 21,22. Low and high 
             color mapping limits; 23. Display orientation flag 

  ---------- -------------------------------------------------- ---------

  ---------- -------------------------------------------------- ---------
  UVI        Poleward/Equatorward extent of auroral oval,       10 min
             Energy flux in 4 quadrants, sector, Characteristic 
             energy, LBH_long Auroral Image (228 ¥ 200), row    
             number, column number                              

  ---------- -------------------------------------------------- ---------

  ---------- -------------------------------------------------- -----------
  PIXIE      Accumulation half-interval, energy bin endpoints,  10
             energy bin upper limits, energy bin lower limit,   min/image
             energy range specifiers, energy range upper limit, 
             energy range lower limit, X-ray source array,      
             vertical pixel coord., horizontal pixel coord.,    
             X-ray source array - high & low energy, total      
             X-ray flux - high & low energy, location of        
             terminator - markers 1 & 2, pixel coords.,         
             location of Greenwich meridian, location of        
             geographic pole, location of geomagnetic pole,     
             location of sub-satellite point, MLT - markers 0,  
             6, 12 & 18 hrs, geographic long/lat map, MLT map,  
             magnetic lat map, number of sub-images, aperture   
             size                                               

  ---------- -------------------------------------------------- -----------

.c1. **Table 4 - Polar KP Data Product Summary**;

**(page 3 of 3)**

  --------------- -------------------------------------------------- ------------
  Investigation   Key Parameters                                     Time
                                                                     resolution

  --------------- -------------------------------------------------- ------------

  ---------- -------------------------------------------------- ---------
  TIDE       First 13 moments of the ion velocity distribution  1 min
             function for each mass species sampled within the  
             period of integration: N1, V1, T1, H1, N2, V2, T2, 
             H2, N3, V3, T3, H3, N4, V4, T4, H4, N5, V5, T5, H5 
             (N=density, V=velocity, T=temperature, H=heat      
             flux)                                              

  ---------- -------------------------------------------------- ---------

+---------+--------------------------------------------------+--------+
| CEPPAD  | Angular Distribution:                            | 96 sec |
|         |                                                  |        |
|         | Proton anisotropy parameters (\>25 keV), error   |        |
|         | of fit (rms)                                     |        |
|         |                                                  |        |
|         | Electron anisotropy parameters (\>25 keV), error |        |
|         | of fit (rms)                                     |        |
|         |                                                  |        |
|         | HIST anisotropy parameters (\>300 keV), error of |        |
|         | fit (rms)                                        |        |
|         |                                                  |        |
|         | Pitch Angle Flux Ratios (spin averaged, \>25     |        |
|         | keV:                                             |        |
|         |                                                  |        |
|         | j(0)/j(90), j(45)/j(90), j(180)/j(90) for        |        |
|         | protons and electrons                            |        |
|         |                                                  |        |
|         | Energy Spectra:                                  |        |
|         |                                                  |        |
|         | Cubic Fit IPS Protons, error of fit (rms), Cubic |        |
|         | Fit IES Electrons, error of fit (rms)            |        |
|         |                                                  |        |
|         | Integral Energetic Particle Fluxes:              |        |
|         |                                                  |        |
|         | Proton flux \> 25 keV, Electron flux \> 30 keV,  |        |
|         | Electron flux \> 300 keV                         |        |
|         |                                                  |        |
|         | Key Parameter Quality Flags:                     |        |
|         |                                                  |        |
|         | IPS (protons), IES (electrons), HIST (electrons) |        |
+---------+--------------------------------------------------+--------+

+---------+--------------------------------------------------+--------+
| CEPPAD/ | Angular distribution (flux)                      | 184    |
|         |                                                  | sec    |
| SEPS    | Electrons (zenith) E\>50keV                      |        |
|         | background,3deg,9deg,15deg,21deg                 |        |
|         |                                                  |        |
|         | Electrons (nadir) E\>50keV                       |        |
|         | background,3deg,9deg,15deg,21deg                 |        |
|         |                                                  |        |
|         | Protons (zenith) E\>50keV background,3deg,9deg   |        |
|         |                                                  |        |
|         | Protons (nadir) E\>50keV background,3deg,9deg    |        |
|         |                                                  |        |
|         | Energy spectra (flux)                            |        |
|         |                                                  |        |
|         | Electrons (zenith) loss cone 50keV,              |        |
|         | 150keV,300keV,1MeV                               |        |
|         |                                                  |        |
|         | Electrons (nadir) source cone 50keV,             |        |
|         | 150keV,300keV,1MeV                               |        |
|         |                                                  |        |
|         | Protons (zenith) loss cone 50keV,                |        |
|         | 150keV,300keV,1MeV                               |        |
|         |                                                  |        |
|         | Protons (nadir) source cone 50keV,               |        |
|         | 150keV,300keV,1MeV                               |        |
+---------+--------------------------------------------------+--------+

.c1. **Table 5 - Ground-based Location & KP Data Product Summary**;

**(page 1 of 2)**

  ---------------- ----------------------------------------- ------------
  Investigation    Key Parameters                            Time
                                                             resolution

  ---------------- ----------------------------------------- ------------

  ---------------- ----------------------------------------- ------------
  CANOPUS/BARS     North & East components of drift          1 min
                   velocity, number of measured vectors,     
                   eccentric dipole field line latitude      

  ---------------- ----------------------------------------- ------------

  ---------------- ----------------------------------------- ------------
  CANOPUS/MARIA    Riometer absorption corrected for         1 min
                   instrument characteristics, CU & CL       
                   indices, CU lat/lon (geodetic) CL lat/lon 
                   (geodetic), site availability, sites,     
                   sites lat/lon                             

  ---------------- ----------------------------------------- ------------

  ---------------- ----------------------------------------- ------------
  CANOPUS/MPA      l5577 intensity (latitude scan for each   5 min
                   photometer, 17 bins each scan)            

  ---------------- ----------------------------------------- ------------

  ---------------- ----------------------------------------- ------------
  CANOPUS/ASI      l5577 image (One 16 x 25 pixel image)     5 min

  ---------------- ----------------------------------------- ------------

  ---------------- ----------------------------------------- ------------
  DARN/PACE        GEO position, half scan time, half range  \~ 100 sec
                   in GEO coords., velocity components       

  ---------------- ----------------------------------------- ------------

  ---------------- ----------------------------------------- ------------
  DARN Goose Bay   GEO position, half scan time, half range  \~ 100 sec
                   in GEO coords., velocity components       

  ---------------- ----------------------------------------- ------------

  ---------------- ----------------------------------------- ------------
  DARN Saskatoon   GEO position, half scan time, half range  \~ 100 sec
                   in GEO coords., velocity components       

  ---------------- ----------------------------------------- ------------

  ---------------- ----------------------------------------- ------------
  DARN Iceland     GEO position, half scan time, half range  \~ 100 sec
  West             in GEO coords., velocity components       

  ---------------- ----------------------------------------- ------------

  ---------------- ----------------------------------------- ------------
  DARN Kapuskasing GEO position, half scan time, half range  \~ 100 sec
                   in GEO coords., velocity components       

  ---------------- ----------------------------------------- ------------

  ---------------- ----------------------------------------- ------------
  SONDRESTROM      Begin/end/half integration time, GEO      10 sec to 5
                   lat/lon, altitude, normalized power, Ne,  min
                   Ti, Te, Ne error, Ti error, Te error,     
                   Vions, Vions error                        

  ---------------- ----------------------------------------- ------------

+---------------+-----------------------------------------+------------+
| SE            | fmin: lowest plasma frequency recorded  | 15 min     |
| SAME/Advanced | (MHz)                                   |            |
| Ionospheric   |                                         |            |
| Sounder       | fEmax: highest plasma frequency         |            |
|               | recorded from E-region (MHz), fFmax:    |            |
|               | highest plasma frequency recorded from  |            |
|               | F-region (MHz)                          |            |
+---------------+-----------------------------------------+------------+

+---------------+-----------------------------------------+------------+
| S             | VLF-1: mean, omni-directional           | 1 min      |
| ESAME/ELF-VLF | logarithmic intensity of 1 kHz signal   |            |
| Logger        | with 1 kHz bandwidth (dB)               |            |
| Investigation |                                         |            |
|               | VLF-3: As above, but for 3 kHz signal   |            |
|               | (dB), 1/2-duration of observation       |            |
+---------------+-----------------------------------------+------------+

+---------------+-----------------------------------------+------------+
| SESAME/Fabry  | US: Horizontal Doppler velocity in      | 30 min     |
| Perot         | geographic South direction (m/s), UE:   |            |
| I             | As above, but for geographic East       | (Apr - Sep |
| nterferometer | direction, indicator to show emission   | only)      |
|               | wavelength                              |            |
+---------------+-----------------------------------------+------------+

+---------------+-----------------------------------------+------------+
| SE            | HDZ_system (components in Cartesian     | 1 min      |
| SAME/Fluxgate | coords.), **B**\_HDZ (Magnetic field    |            |
|               | components H, D, Z in nT; H=Horizontal  |            |
| Magnetometer  | (+) North, (-) South; D=Horizontal (+)  |            |
|               | East, (-) West; Z=Vertical (+) Down)    |            |
+---------------+-----------------------------------------+------------+

  ----------------- ----------------------------------------- ------------
  SESAME/Riometer   Absorption (dB): AN (North), AE (East),   1 min
                    AS (South), AW (West). Note: in each case 
                    direction shifted onto an L-shell-aligned 
                    coordinate system                         

  ----------------- ----------------------------------------- ------------

.c1. **Table 5 - Ground-based Location & KP Data Product Summary**;

**(page 2 of 2)**

+-------------------------------+-------------------+------------------+
| Name                          | Latitude          | Longitude        |
|                               |                   |                  |
|                               | (degrees)         | (degrees)        |
+-------------------------------+-------------------+------------------+

  -------------------------------- -------------------- ------------------
  Sondrestrom                      67                   309.2

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  SESAME                           -75.6                333.23

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  Canopus/Back                     57.7                 265.8

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  Canopus/Contwoyto Lk             65.8                 248.8

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  Canopus/Dawson                   64.1                 220.9

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  Canopus/Eskimo Point             61.1                 266

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  Canopus/Ft Churchill             58.8                 265.9

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  Canopus/Ft McMurray              56.7                 248.8

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  Canopus/Ft Simpson               61.7                 238.8

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  Canopus/Ft Smith                 60                   248.1

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  Canopus/Gillam                   56.4                 265.4

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  Canopus/Island Lake              53.9                 265.3

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  Canopus/Nipawin                  53.5                 256.3

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  Canopus/Pinawa                   50.2                 264

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  Canopus/Rabbit Lake              58.2                 256.3

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  Canopus/Rankin Inlet             62.8                 267.9

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  Canopus/Red Lake                 50.9                 266.5

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  DARN/Goose Bay                   53.32                299.54

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  DARN/PACE                        -75.6                333.23

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  DARN/Saskatoon                   52.16                253.47

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  DARN/Iceland West                64.43                337.99

  -------------------------------- -------------------- ------------------

  -------------------------------- -------------------- ------------------
  DARN/Kapuskasing                 49.41                277.53

  -------------------------------- -------------------- ------------------

.c1. **Table 6 - Supplementary Missions KP Data Product Summary**;

**IMP-8**

  --------------- ---------------------------------------------- ------------
  Investigation   Key Parameters                                 Time
                                                                 resolution

  --------------- ---------------------------------------------- ------------

  ----------- ---------------------------------------------- ------------
  MAG         \|\<**B**\>\|, \<\|**B**\|\>,                  61.4 sec
              magnitude/components RMS (GSE), Bx, By, Bz,    
              \|B\|, B-Lat/Long (GSE & GSM), (x,y,z)GSE&GSM, 
              R, N                                           

  ----------- ---------------------------------------------- ------------

  ----------- ---------------------------------------------- ------------
  PLA         V(RTN), V(GSE), V(GSM), Vpolar(GSE) proton     1 min
              number density, most probable thermal speed,   
              (x,y,z)GSE&GSM, R                              

  ----------- ---------------------------------------------- ------------

**LANL**

  ---------------- ---------------------------------------- -------------
  Investigation    Key Parameters                           Time
                                                            resolution

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  LANL/SOPA        Electrons: 50-225 keV & 315-1500 keV     61.44 sec
                   flux, density, temperature; Protons:     
                   50-400 keV & 1.2-5 MeV flux, density,    
                   temperature; He (0.9-1.3 MeV) flux,      
                   Heavy ions (C, N, O): 5-15 MeV flux,     
                   (lat, lon,R)GEO                          

  ---------------- ---------------------------------------- -------------

+---------------+----------------------------------------+------------+
| LANL/MPA      | Low_Ions (1-130 ev): partial density,  | 172 sec    |
|               | flow velocity, temperature (T\^,       |            |
|               | T\|\|), temperature eigenvalue ratio   |            |
|               | (T\^/Tmid); High_Ions (130-43,000 eV): |            |
|               | partial density, flow velocity,        |            |
|               | temperature (T\^, T\|\|), polar angle  |            |
|               | of symm. axis (rel. to s/c-Earth       |            |
|               | direction), azimuth of symm. axis      |            |
|               | (rel. to North), temperature           |            |
|               | eigenvalue ratio (T\^/Tmid); Electrons |            |
|               | (30-45,000 eV): partial density,       |            |
|               | temperature (T\^, T\|\|), polar angle  |            |
|               | of symm. axis (rel. to s/c-Earth       |            |
|               | direction), azimuth of symm. axis      |            |
|               | (rel. to North), temperature           |            |
|               | eigenvalue ratio (T\^/Tmid), s/c       |            |
|               | potential, background                  |            |
|               |                                        |            |
|               | (lat,lon,altitude)GEO, (mlat,          |            |
|               | mlt,altitude)MAG                       |            |
+---------------+----------------------------------------+------------+

**Table 6 - Supplementary Missions KP Data Product Summary**

**(Continued)**

**GOES-6, 7, (8, 9)**

  --------------- ------------------------------------------ -------------
  Investigation   Key Parameters                             Time
                                                             resolution

  --------------- ------------------------------------------ -------------

  --------------- ------------------------------------------ -------------
  GOES_6/EPS      electron & proton counts, (R,lat,lon)GEO,  5 min
                  (x,y,z)GEO,(x,y,z)GSE, (x,y,z)GSM,         
                  EPS-status                                 

  --------------- ------------------------------------------ -------------

  --------------- ------------------------------------------ -------------
  GOES_6/MAG      **B** (GSE, GSM and SEL coords.),          1 min
                  (R,lat,lon)GEO, (x,y,z)GEO,(x,y,z)GSE,     
                  (x,y,z)GSM, MAG-status                     

  --------------- ------------------------------------------ -------------

  --------------- ------------------------------------------ -------------
  GOES_7/EPS      electron & proton counts, (R,lat,lon)GEO,  5 min
                  (x,y,z)GEO,(x,y,z)GSE, (x,y,z)GSM,         
                  EPS-status                                 

  --------------- ------------------------------------------ -------------

  --------------- ------------------------------------------ -------------
  GOES_7/MAG      **B** (GSE, GSM and SEL coords.),          1 min
                  (R,lat,lon)GEO, (x,y,z)GEO,(x,y,z)GSE,     
                  (x,y,z)GSM, MAG-status                     

  --------------- ------------------------------------------ -------------

  --------------- ------------------------------------------ -------------
  GOES_8/EP8      TBD                                        TBD

  --------------- ------------------------------------------ -------------

  --------------- ------------------------------------------ -------------
  GOES_8/MAG      TBD                                        TBD

  --------------- ------------------------------------------ -------------

  --------------- ------------------------------------------ -------------
  GOES_9/EP8      TBD                                        TBD

  --------------- ------------------------------------------ -------------

  --------------- ------------------------------------------ -------------
  GOES_9/MAG      TBD                                        TBD

  --------------- ------------------------------------------ -------------

.c1. **Table 7 - Geotail KP Data Product Summary**;

**(page 1 of 2)**

+----------+--------------------------------------------------+-------+
| Inves    | Key Parameters                                   | Time  |
| tigation |                                                  |       |
|          |                                                  | resol |
|          |                                                  | ution |
+----------+--------------------------------------------------+-------+

+----------+--------------------------------------------------+-------+
| CPI      | SOLAR WIND ANALYZER                              | 64    |
|          |                                                  | sec   |
|          | Ion number density, avg. energy & bulk flow vel. |       |
|          |                                                  |       |
|          | HOT PLASMA ANALYZER                              |       |
|          |                                                  |       |
|          | Ion number density, avg. energy & bulk flow vel  |       |
|          |                                                  |       |
|          | Electron avg. energy, plasma pressure            |       |
|          |                                                  |       |
|          | COMPOSITION ANALYZER                             |       |
|          |                                                  |       |
|          | H+, He+, He++, O+ flags                          |       |
+----------+--------------------------------------------------+-------+

  ----------- -------------------------------------------------- --------
  EPIC        Spin-averaged ion differential intensities, ICS;   96 sec
              Uncertainties ion differential intensities, ICS;   
              Ion chan energy band, ICS; Ion Channels, ICS; Ion  
              chan energy plus, ICS; Ion chan energy minus, ICS; 
              Spin-averaged proton differential intensities,     
              STICS; Uncertainties proton differential           
              intensities, STICS; H chan energy band, STICS; H   
              channels, STICS; H chan energy plus, STICS; H chan 
              energy minus, STICS; Spin-averaged electron        
              integral intensity (\>34 keV), ICS; Uncertainty    
              electron integral intensity, ICS; e chan energy    
              band, ICS; e channels, ICS; e chan energy plus,    
              ICS; e chan energy minus, ICS;Spin-averaged He/H   
              diff intensity ratios (82 & 233 keV/67 keV), ICS;  
              Uncertainties He/H diff intensity ratios (82 & 233 
              keV/67 keV), ICS; He/H channels, ICS;              
              Spin-averaged O/H diff intensity ratios (203 &     
              1244 keV/67 keV, ICS; Uncertainties O/H diff       
              intensity ratios (203 & 1244 keV/67 keV), ICS; O/H 
              channels, ICS; Spin-averaged He++/H+ diff          
              intensity ratio (9.4 - 212 keV/67 keV), STICS;     
              Uncertainty He++/H+ diff intensity ratio (92 & 233 
              keV/67 keV), STICS; He++/H+ channels, STICS;       
              Spin-averaged O+/H+ diff intensity ratio (9.4 -212 
              keV/67 keV), STICS; O+/H+ diff intensity ratio (82 
              & 233 keV/67 keV), STICS; O+/H+ channels, STICS;   
              \>34 keV electron anisotropy parameters, ICS;      
              uncertainties electron anisotropy parameters, ICS; 
              9.4-212.1 keV/e proton anisotropy parameters,      
              STICS; Uncertainties proton anisotropy parameters, 
              STICS67.0 keV proton anisotropy, ICS;              
              Uncertainties proton anisotropy parameters, ICS;   
              128.7 keV proton anisotropy parameters, ICS;       
              Uncertainties proton anisotropy parameters, ICS    

  ----------- -------------------------------------------------- --------

+----------+--------------------------------------------------+-------+
| HEP      | Electrons J (E \> 20 keV, az = 0˚, 90˚, 180˚,    | 180   |
| LD-spect | 270˚)                                            | sec   |
| rometers |                                                  |       |
|          | Protons J (E \> 20 keV, az = 0˚, 90˚, 180˚,      | 180   |
| HEP      | 270˚)                                            | sec   |
| BD-spect |                                                  |       |
| rometers | Helium J (E \> 20 keV, az = 0˚), Oxygen J (E \>  | 180   |
|          | 50 keV)                                          | sec   |
|          |                                                  |       |
|          | Electrons J (E \> 0.12 MeV, az = 0˚, 90˚, 180˚,  | 180   |
|          | 270˚)                                            | sec   |
|          |                                                  |       |
|          | Protons J (E \> 0.4 MeV, az = 0˚, 90˚, 180˚,     | 180   |
|          | 270˚)                                            | sec   |
+----------+--------------------------------------------------+-------+

  ----------- -------------------------------------------------- --------
  MGF         \|**B**\|, Bx, By, Bz, s (GSE), XGSE, YGSE, ZGSE   64 sec

  ----------- -------------------------------------------------- --------

+----------+--------------------------------------------------+-------+
| EFD      | Sphere Probe: Ex, Ey, Residue, s/c potential,    | 64    |
|          | bias value                                       | sec   |
|          |                                                  |       |
|          | Wire antenna: Ex, Ey, Residue, s/c potential,    |       |
|          | bias value                                       |       |
|          |                                                  |       |
|          | Half-time resolution, XGSE, YGSE, ZGSE           |       |
+----------+--------------------------------------------------+-------+

.c1. **Table 7 - Geotail KP Data Product Summary**;

**(page 2 of 2)**

+----------+--------------------------------------------------+-------+
| Inves    | Key Parameters                                   | Time  |
| tigation |                                                  |       |
|          |                                                  | resol |
|          |                                                  | ution |
+----------+--------------------------------------------------+-------+

+----------+--------------------------------------------------+-------+
| LEP      | e, ion energy spectra per sector,                | 5.6   |
|          |                                                  | min   |
|          | n, T, vel, q, f                                  |       |
|          |                                                  | 2.8   |
|          | avg. H+, O+, counts per sector                   | min   |
|          |                                                  |       |
|          |                                                  | 5.6   |
|          |                                                  | min   |
+----------+--------------------------------------------------+-------+

+----------+--------------------------------------------------+-------+
| PWI      | Peak and average of spectral intensity for the   | 64    |
|          | **E** of the Multi Channel Analyzer (**E** at 10 | sec   |
|          | Hz, 100 Hz, 1 kHz, 10 kHz and 100 kHz),          |       |
|          |                                                  |       |
|          | Peak and average of spectral intensity for the   |       |
|          | **B** of the Multi Channel Analyzer (**B** at 10 |       |
|          | Hz, 100 Hz, 1 kHz, and 10 kHz),                  |       |
|          |                                                  |       |
|          | Peak and average of the spectral intensities for |       |
|          | the Sweep Frequency Analyzer, Frequency          |       |
|          | corresponding to the peak of the spectral        |       |
|          | intensities, XGSE, YGSE, ZGSE                    |       |
+----------+--------------------------------------------------+-------+

.c1. **Table 8 - SOHO KP Data Product Summary**;

  ----------------- --------------------------------------- -------------
  Investigation     Key Parameters                          Time
                                                            resolution

  ----------------- --------------------------------------- -------------

  ----------------- --------------------------------------- -------------
  CELIAS            Solar wind speed, Solar EUV rate (2     5 min
                    values 0., 1. order), heavy ion rate    

  ----------------- --------------------------------------- -------------

  ----------------- --------------------------------------- -------------
  COSTEP            electron flux: 0.2-0.8, 0.8-3, 3-6.4,   5 min
                    6.4-9.6 MeV; proton flux: 0.3-0.8,      
                    0.8-2, 2-5, 5-9, 9-28, 28-44, 44-56     
                    MeV; Helium flux: 4.5-8.3, 8.3-26,      
                    26-42, 42-55 MeV/n                      

  ----------------- --------------------------------------- -------------

  ----------------- --------------------------------------- -------------
  ERNE              electron flux: 4-16, \>16 MeV; proton   1 min
                    flux: 2-4, 4-8, 8-16, 16-32, 32-64,     
                    64-128 MeV; 4He flux: 2-4, 4-8, 8-16,   
                    16-32, 32-64, 64-128 MeV/n; abundance   
                    ratios: deuteron-to-proton (4-8, 32-64  
                    MeV/n), 3He-to-4He (4-8, 32-64 MeV/n)   

  ----------------- --------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  Experiment       Summary Parameters (Imaging)             Time
                                                            Resolution

  ---------------- ---------------------------------------- -------------

+----------------+----------------------------------------+------------+
| MDI            | Full disk magnetogram, 1024 x 1024     | TBD        |
|                |                                        |            |
|                | Full disk continuum, 1024 x 1024       |            |
+----------------+----------------------------------------+------------+

+----------------+----------------------------------------+------------+
| EIT            | Full disk images in lines Fe IX, Fe    | TBD        |
|                | XII, FE XV,                            |            |
|                |                                        |            |
|                | He II, 1024 x 1024                     |            |
+----------------+----------------------------------------+------------+

+----------------+----------------------------------------+------------+
| UVCS           | 1.2 - 10 RS Corona Ly alpha, 256 x 256 | TBD        |
|                |                                        |            |
|                | 1.2 - 10 RS Corona Temperature, 256 x  |            |
|                | 256                                    |            |
+----------------+----------------------------------------+------------+

+----------------+----------------------------------------+------------+
| LASCO          | 1.1 - 30 RS Corona White Light, 1024 x | TBD        |
|                | 1024                                   |            |
|                |                                        |            |
|                | 1.1 - 3 RS Corona in lines Fe XIV, Fe  |            |
|                | X, Ca XV,                              |            |
|                |                                        |            |
|                | 1024 x 1024                            |            |
+----------------+----------------------------------------+------------+

+----------------+----------------------------------------+------------+
| GOLF           | Global Magnetic Field                  | 6-hour     |
|                |                                        | mean       |
|                |                                        |            |
|                |                                        | 1 value    |
|                |                                        | per day    |
+----------------+----------------------------------------+------------+

  ---------------- ---------------------------------------- -------------
  VIRGO            Solar Constant, SPM, LOI for each pixel  1 value per
                                                            day

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  SWAN             Observation sensors 1 and 2              TBD

  ---------------- ---------------------------------------- -------------

.c1. **Table 9 - SOHO Science Data Product Summary**;

  ---------------- ---------------------------------------- -------------
  Experiment       Summary Parameters                       Time
                                                            resolution

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  GOLF             Time series of global velocity field     TBD

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  VIRGO            Time series of irradiance                TBD

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  MDI              Time series of: full disk velocity,      TBD
                   intensity, and magnetogram images;       
                   high-resolution velocity, intensity and  
                   magnetogram images; mode amplitudes, low 
                   resolution velocity, intensity images    

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  SUMER            Time series of images (small and full    TBD
                   Sun), whole solar spectra, solar events  

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  CDS              Time series of images and spectra        TBD

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  EIT              Full disk, portion of solar image taken  TBD
                   in conjunction with CDS and SUMER        
                   observations                             

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  UVCS             Level 1: Uncalibrated solar UV images,   TBD
                   blocks of visible light data. Level 2:   
                   Same as level 1, but calibrated (gain    
                   table and intensity calibrations)        

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  LASCO            Time series of coronal images            TBD
                   (brightness, electron densities, %       
                   polarization, magnetic field             
                   orientation, bulk velocity and line      
                   ratios                                   

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  SWAN             Antisolar Ly-alpha intensity, Ly-alpha   TBD
                   maps of the sky                          

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  CELIAS           Particle fluxes and energies for Solar   TBD
                   Wind and Suprathermal particles;         
                   densities, mean velocities, velocity     
                   distributions for Solar Wind             

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  CEPAC            Counting rates and spectra of various    TBD
                   elements or groups of elements,          
                   abundance of isotopes                    

  ---------------- ---------------------------------------- -------------

.c1. **Table 10 - Cluster**[^2]**Summary Parameters Data Products**;

  ---------------- ---------------------------------------- -------------
  Investigation    Summary Parameters[^3]                   Time
                                                            resolution

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  FGM              **B**, d**B**/B, FGM status word         1 min

  ---------------- ---------------------------------------- -------------

+----------------+----------------------------------------+------------+
| STAFF[^4]      | B power: 0.3-10, 10-180, 180-4000 Hz   | 1 min      |
|                |                                        |            |
|                | E power: 10-180, 180-4000 Hz, STAFF    |            |
|                | status word, WEC status word           |            |
+----------------+----------------------------------------+------------+

+----------------+----------------------------------------+------------+
| EFW2           | Edusk, sE, Vps, Iprobe, E power:       | 1 min      |
|                | 0.3-10, 10-180 Hz, EFW status word,    |            |
|                | WEC status word                        |            |
|                |                                        |            |
|                | \[Dawn-dusk electric field, variations |            |
|                | in electric field, probe-s/c voltage,  |            |
|                | and probe current\]                    |            |
+----------------+----------------------------------------+------------+

  ---------------- ---------------------------------------- -------------
  WHISPER4         n(e), quality, E power: 4-80 kHz,        1 min
                   WHISPER status word, WEC status word     

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  WBD4             WBD status word, WEC status word         1 min

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  DWP4             Significance level, DWP status word, WEC 1 min
                   status word                              

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  EDI              **E**, EDI status word                   1 min

  ---------------- ---------------------------------------- -------------

+----------------+----------------------------------------+------------+
| CIS            | n(p), n(O+), n(He+), n(He++), n(HIA),  | 1 min      |
|                | **v**(p), **v**(HIA), **v**(O+), T(p), |            |
|                | T(HIA), CIS status word                |            |
|                |                                        |            |
|                | \[HIA = Hot Ion Analyzer, measures     |            |
|                | most dominant ion species\]            |            |
+----------------+----------------------------------------+------------+

+----------------+----------------------------------------+------------+
| PEACE          | n(e), **v**(e), T\|\|(e), T\^(e),      | 1 min      |
|                | Q\|\|(e), PEACE status word            |            |
|                |                                        |            |
|                | \[electron density, velocity,          |            |
|                | temperature, heat flux\]               |            |
+----------------+----------------------------------------+------------+

+----------------+----------------------------------------+------------+
| RAPID          | Jlow(s), Jhi(s), s= e, p, He, mass \>  | 1 min      |
|                | 4                                      |            |
|                |                                        |            |
|                | A\|\|(e), A\|\|(p), RAPID status word  |            |
|                |                                        |            |
|                | \[J = particle flux, 2 energy ranges,  |            |
|                | 4 species                              |            |
|                |                                        |            |
|                | A = field aligned flux anisotropy, 2   |            |
|                | species\]                              |            |
+----------------+----------------------------------------+------------+

  ---------------- ---------------------------------------- -------------
  ASPOC            Ion current, ASPOC status word           1 min

  ---------------- ---------------------------------------- -------------

+----------------+----------------------------------------+------------+
| Auxiliary      | **R**1, position of s/c 1, D**R**n; n  | 1 min      |
| information    | = 2,3,4, position relative to s/c 1,   |            |
|                | **V**1, velocity of s/c 1, QG, QR,     |            |
|                |                                        |            |
|                | min \|D**R**ij\|, max \|D**R**ij\|,    |            |
|                | \[Tetrahedron quality parameters of    |            |
|                | Glassmeir and Roux\], qSCn, fSCn; n =  |            |
|                | 1-4, spin axes in GSE, GSEÆGSM         |            |
|                | conversion angle, dipole tilt angle,   |            |
|                | spacecraft status word                 |            |
+----------------+----------------------------------------+------------+

.c1.**Table 11 - Cluster Science Data Centers**;

  ---------------- ---------------------------------------- -------------
  DC Name          Location                                 Experiments

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  UKCDC            Rutherford Appleton Laboratory, U.K      DWP, FGM,
                                                            PEACE

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  CFC              Centre National de Etudes Spatiales,     CIS, STAFF,
                   Toulouse, France                         WHISPER, EFW

  ---------------- ---------------------------------------- -------------

+----------------+----------------------------------------+------------+
| MPEDC          | Max-Planck-Institut fur                | EDI        |
|                | Extraterrestrische Physik              |            |
|                |                                        |            |
|                | Garching, Germany                      |            |
+----------------+----------------------------------------+------------+

+----------------+----------------------------------------+------------+
| LINDC          | Max-Planck-Institut fur Aeronomie      | RAPID      |
|                |                                        |            |
|                | Katlenburg-Lindau, Germany             |            |
+----------------+----------------------------------------+------------+

+----------------+----------------------------------------+------------+
| ACDC           | Institut fur Weltraumforschung         | ASPOC      |
|                |                                        |            |
|                | Graz, Austria                          |            |
+----------------+----------------------------------------+------------+

+----------------+----------------------------------------+------------+
| SCD            | Kunliga Tekniska Hogskolan             | EFW        |
|                |                                        |            |
|                | Stockholm, Sweden                      |            |
+----------------+----------------------------------------+------------+

+----------------+----------------------------------------+------------+
| USCSDC         | Goddard Space Flight Center            | WBD        |
|                |                                        |            |
|                | Greenbelt, MD                          |            |
+----------------+----------------------------------------+------------+

+----------------+----------------------------------------+------------+
| HDC            | Central Research Institute for Physics | \--        |
|                |                                        |            |
|                | Budapest, Hungary                      |            |
+----------------+----------------------------------------+------------+

  ---------------- ---------------------------------------- -------------
  ?                **China**?                               \--

  ---------------- ---------------------------------------- -------------

  ---------------- ---------------------------------------- -------------
  ?                **India**?                               \--

  ---------------- ---------------------------------------- -------------

**.c1.Table 12 - Interball/Aurora**[^5] **Key Parameters;**

  -------------------------------------------- --------------- ------------
  Key Parameters                               Contributing    Time
                                               Instrument(s)   resolution

  -------------------------------------------- --------------- ------------

  -------------------------------------------- -------------- -----------
  High-temperature plasma: F(e-), \<Ee\>,      ION, SKA-3,    TBD
  F(H+), \<E H+\>                              PROMICS-3A     

  -------------------------------------------- -------------- -----------

  -------------------------------------------- -------------- -----------
  High-temperature plasma: F(O+), \<E O+\>,    PROMICS-3A     TBD
  azimuth angle O+ and polar angle O+                         

  -------------------------------------------- -------------- -----------

+--------------------------------------------+-------------+----------+
| High-temperature plasma: Flux of ions      | DOK-2A      | TBD      |
| 27-32 keV (1 detector directed from Sun, 2 |             |          |
| directed at angle 45˚ to Sun or in         |             |          |
| scanning mode)                             |             |          |
|                                            |             |          |
| Flow of electrons 27-32 keV (1 detector    |             |          |
| directed from Sun, 2 directed at angle 45˚ |             |          |
| to Sun or in scanning mode)                |             |          |
|                                            |             |          |
| Pitch angle curve                          |             |          |
+--------------------------------------------+-------------+----------+

  -------------------------------------------- -------------- -----------
  Cold plasma: Density of O+ ions, Density of  HYERBOLOID     TBD
  H+ ions, Temperature of O+ ions, Temperature                
  of H+ ions, Velocity of O+ ions (Vx, Vy,                    
  Vz), Velocity of H+ ions (Vx, Vy, Vz)                       

  -------------------------------------------- -------------- -----------

  -------------------------------------------- -------------- -----------
  Cold plasma: Temperature of electrons        KM-7           TBD

  -------------------------------------------- -------------- -----------

  -------------------------------------------- -------------- -----------
  Cold plasma: Plasma density                  AP-3A          TBD

  -------------------------------------------- -------------- -----------

  -------------------------------------------- -------------- -----------
  Cold plasma: Beam current, probe potential   RON            TBD

  -------------------------------------------- -------------- -----------

  -------------------------------------------- -------------- -----------
  Wave investigations: Spectrogram of HF E,    POLRAD         TBD
  Spectrogram of HF B (cyclotron gyrofrequency                
  Fce added)                                                  

  -------------------------------------------- -------------- -----------

  -------------------------------------------- -------------- -----------
  Wave investigations: Spectrogram of HF E,    MEMO           30 sec
  Spectrogram of HF B (cyclotron gyrofrequency                
  Fce added)                                                  

  -------------------------------------------- -------------- -----------

  -------------------------------------------- -------------- -----------
  VLF E, VLF B, ELF/VLF SFA E, ELF/VLF SFA B,  MEMO           30 sec
  Service parameter (SFA) \[SFA = Sweep                       
  Frequency Analyzer\]                                        

  -------------------------------------------- -------------- -----------

  -------------------------------------------- -------------- -----------
  Electric and Magnetic fields: Spectrogram of IESP-2         TBD
  ULF E (orthogonal), Spectrogram of ULF B                    
  (orthogonal), Spectrogram of ULF E                          
  (parallel), Spectrogram of ULF B (parallel)                 

  -------------------------------------------- -------------- -----------

  -------------------------------------------- -------------- -----------
  3 components of magnetic field, total        IMAP-3         TBD
  magnetic field                                              

  -------------------------------------------- -------------- -----------

  -------------------------------------------- -------------- -----------
  2 components of electric field, electric     IESP-2         TBD
  field DC                                                    

  -------------------------------------------- -------------- -----------

  -------------------------------------------- -------------- -----------
  Auroral image                                UVAI           30 min

  -------------------------------------------- -------------- -----------

  -------------------------------------------- -------------- -----------
  Auxiliary information on s/c position (GSE &                every 1-3
  GSM)                                                        hrs

  -------------------------------------------- -------------- -----------

**.c1.Table 13 - Interball/Tail**[^6] **Key Parameters;**

  ------------- ------------------------------------ --------------- ------------
  Descriptors   Key Parameters                       Contributing    Time
                                                     Instrument(s)   resolution

  ------------- ------------------------------------ --------------- ------------

  ----------- ------------------------------------ -------------- --------
  EMFT        Magnetic field: Bx, By, Bz, \|B\|    IMAP, MIF-M    \~ 2 min

  ----------- ------------------------------------ -------------- --------

  ----------- ------------------------------------ -------------- --------
  EMFT        Fluctuations: Electric field (1-8    OPERA          \~ 2 min
              Hz, 530-750 Hz, 20 kHz)                             

  ----------- ------------------------------------ -------------- --------

  ----------- ------------------------------------ -------------- --------
  EMFT        Fluctuations: Magnetic field (1-4    MIF-M/PRAM     \~ 2 min
              Hz, 600-800 Hz)                                     

  ----------- ------------------------------------ -------------- --------

  ----------- ------------------------------------ -------------- --------
  EMFT        Fluctuations: Electron flux (1-4 Hz) IFPE/PRAM      

  ----------- ------------------------------------ -------------- --------

  ----------- ------------------------------------ -------------- --------
  GPPT        Thermal plasma: ne, Te,              ELECTRON       \~ 2 min

  ----------- ------------------------------------ -------------- --------

+----------+------------------------------------+--------------+-------+
| GPPT     | Thermal plasma: ni, **V**i, Ti     | MONITOR      | \~ 2  |
|          |                                    | (solar wind) | min   |
|          |                                    |              |       |
|          |                                    | AP           |       |
|          |                                    | (p           |       |
|          |                                    | lasmasphere) |       |
|          |                                    |              |       |
|          |                                    | EU-1 or      |       |
|          |                                    | CORALL       |       |
|          |                                    | (other       |       |
|          |                                    | regions)     |       |
+----------+------------------------------------+--------------+-------+

  ----------- ------------------------------------ -------------- --------
  EPTP        Oxygen: EO+ FO+,                     PROMICS        \~ 2 min

  ----------- ------------------------------------ -------------- --------

  ----------- ------------------------------------ -------------- --------
  EPTP        Energetic particles: fluxes of ions  DOK-2          \~ 2 min
              and electrons (two directions,                      
              energy ranges TBD)                                  

  ----------- ------------------------------------ -------------- --------

  ----------- ------------------------------------ -------------- --------
  EPTP        Energetic particles: fluxes of ions  SKA-2          \~ 2 min
              (1-5 meV) and electrons 150-500 keV                 

  ----------- ------------------------------------ -------------- --------

  ----------- ------------------------------------ -------------- --------
              Tail probe coordinates                              1 hr

  ----------- ------------------------------------ -------------- --------

  ----------- ------------------------------------ -------------- --------
              PC (polar cap) geomagnetic index                    15 min
              (from Thule and Vostok stations)                    

  ----------- ------------------------------------ -------------- --------

.c1.**Table 14 - ISTP Data Products and Disposition Overview**;

  -------------- --------------- ------- ------- ------- --------- -------------
  **ISTP/GGS**                                                     

  -------------- --------------- ------- ------- ------- --------- -------------

  ---------- --------------- ---------- ---------- ---------- ------------- ------------------
  Data       Purpose/Use     When       Where      When       When Publicly Appropriate Usage
  Product                    Created?   Created?   Archive?   Accessible?   once
                                                                            non-proprietary?

  ---------- --------------- ---------- ---------- ---------- ------------- ------------------

  ---------- ----------------- ------------- ------- ------------- ------------- ----------------
  Level-0    Telemetry-level   \<2 days from CDHF    \<30 days     1 year from   Requires access
             product;          data                  from data     data          to archived
                               acquisition           acquisition   acquisition   PI-supplied s/w;
                                                                                 very often may
                                                                                 require
                                                                                 PI-assistance in
                                                                                 interpretation

  ---------- ----------------- ------------- ------- ------------- ------------- ----------------

+---------+--------------+------+------+------+--------+------------+
| KPs     | Low          | \<3  | CDHF | wi   | once   | n          |
|         | resolution;  | days |      | thin | del    | on-citable |
|         |              | from |      | 5    | ivered |            |
|         | full         | data |      | days | to the |            |
|         | coverage for | acq  |      | a    | NSSDC  |            |
|         | all          | uisi |      | fter |        |            |
|         | instruments; | tion |      | ge   |        |            |
|         | non-citable; |      |      | nera |        |            |
|         | browse       |      |      | tion |        |            |
+---------+--------------+------+------+------+--------+------------+

+---------+--------------+------+------+------+--------+------------+
| "C      | Low          | TBD  | C    | TBD  | TBD;   | Citable    |
| itable" | resolution,  |      | DHF/ |      |        | ;correctly |
| KPs     | full         |      |      |      | re     | and        |
|         | coverage for |      | RDAF |      | leased | ind        |
|         | given        |      |      |      | by     | ependently |
|         | instrument   |      |      |      | sp     | usable     |
|         | in the time  |      |      |      | ecific |            |
|         | period       |      |      |      | inst   |            |
|         | released,    |      |      |      | rument |            |
|         |              |      |      |      | for    |            |
|         | citable      |      |      |      | sp     |            |
|         | browse and   |      |      |      | ecific |            |
|         | synoptic     |      |      |      | time   |            |
|         |              |      |      |      | p      |            |
|         |              |      |      |      | eriods |            |
+---------+--------------+------+------+------+--------+------------+

+---------+--------------+------+------+------+--------+------------+
| Event   | High         | TBD  | RDAF | TBD  | TBD    | Citable    |
| Data    | resolution;  |      |      |      |        | ;correctly |
|         | select times |      |      |      |        | and        |
|         | and for all  |      |      |      |        | ind        |
|         | instruments; |      |      |      |        | ependently |
|         |              |      |      |      |        | usable,    |
|         | citable      |      |      |      |        | app        |
|         | analysis     |      |      |      |        | roximately |
|         | product      |      |      |      |        | 10% of the |
|         |              |      |      |      |        | ISTP       |
|         |              |      |      |      |        | level-0    |
|         |              |      |      |      |        | data       |
+---------+--------------+------+------+------+--------+------------+

+---------+--------------+------+------+------+--------+------------+
| PI      | Various      | \<2  | RDAF | \<2  | 2      | Citable    |
| Archive | resolutions; | y    |      | y    | years  | ;correctly |
| P       | products     | ears |      | ears | from   | and        |
| roducts | vary by      | from |      | from | data   | ind        |
|         | instrument;  | data |      | data | acqui  | ependently |
|         |              | acq  |      | acq  | sition | usable     |
|         | citable      | uisi |      | uisi |        |            |
|         | analysis     | tion |      | tion |        |            |
|         | products     |      |      |      |        |            |
+---------+--------------+------+------+------+--------+------------+

  ------------ --------------- --------- ------- ------- --------- -------------
  Level-0      Used at the     At or     RDAF    TBD     TBD       TBD
  Processing   CDHF for        shortly                             
  s/w          generation of   after                               
               KP data and at  launch                              
               the RDAF for                                        
               generation of                                       
               event data                                          

  ------------ --------------- --------- ------- ------- --------- -------------

  ---------- --------------- --------- ------- ------- --------- -------------
  KPGS s/w   Used at the     At or     CDHF    TBD     TBD       TBD
             CDHF            shortly                             
                             after                               
                             launch                              

  ---------- --------------- --------- ------- ------- --------- -------------

+---------+--------------+------+------+------+--------+------------+
| Citable | Used at the  | Wi   | C    | TBD  | TBD    | TBD        |
| KP s/w  | CDHF         | thin | DHF/ |      |        |            |
|         |              | 18   |      |      |        |            |
|         |              | mo   | RDAF |      |        |            |
|         |              | nths |      |      |        |            |
|         |              | a    |      |      |        |            |
|         |              | fter |      |      |        |            |
|         |              | la   |      |      |        |            |
|         |              | unch |      |      |        |            |
+---------+--------------+------+------+------+--------+------------+

  ------------- --------------- ------- ------- ------- --------- -------------
  **Geotail**                                                     

  ------------- --------------- ------- ------- ------- --------- -------------

  ------------ --------------- ------------- ------- ------------- ---------- -------------
  Sirius Data  Used at the     \<2 days from CDHF    \<30 days     TBD if to  TBD if to be
  (playback)   CDHF            data                  from data     be         released
                               acquisition           acquisition   released   

  ------------ --------------- ------------- ------- ------------- ---------- -------------

.c1.**Appendix A - Overview of the Wind Mission Instruments**;

**Energetic Particle Acceleration, Composition & Transport (EPACT)**

The principal Investigator of EPACT is Dr. T. von Rosenvinge,
NASA/Goddard Space Flight Center, Greenbelt, MD. The EPACT investigation
will provide a comprehensive study of energetic particle acceleration
and transport processes in solar flares, the interplanetary medium, and
planetary magnetospheres, as well as the galactic cosmic rays and the
anomalous cosmic ray component. EPACT measurements will determine
elemental and isotopic abundances for the minor ions making up the solar
wind, with energies in excess of 20 keV. This direct sampling of solar
matter is a way to study events on the solar surface and the
incorporation of solar material into the solar wind. EPACT will also
provide information on shocks in the interplanetary medium, which
accelerate particles from solar-wind energies to several hundred keV.

Measurement Objectives:

> • Energy spectra of electrons and atomic nuclei of different charge
> and isotopic composition, from hydrogen to iron, over an energy range
> extending from 0.1 to 500 MeV/nucleon.
>
> • Isotopic composition of medium energy particles (2 - 50 MeV/nucleon)
> in solar flares, in the anomalous component and in galactic cosmic
> rays, extending up to Z = 90.
>
> • Determination of angular distributions of these fluxes.

The EPACT instrument consists of three integrated telescope/electronics
boxes mounted on the body of the spacecraft. The extensive dynamic range
of particles to be measured is divided between three Low Energy Matrix
Telescopes (LEMT), two Alpha-Proton-Electron Telescopes (APE), an
Isotope Telescope (IT), and a Supra Thermal Energetic Particle Telescope
(STEP). The APE and IT instruments are contained in a single package
known as the Electron Isotope Telescope (ELITE). These solid state
detector telescopes all use the dE/dx by E method of particle
identification, except STEP, which obtains particle mass by measuring
time-of-flight and energy. An onboard recorder allows continuous
observations to be made.

**Russian Gamma-Ray Spectrometer (KONUS)**

The Principal Investigators for the Russian Gamma-Ray Spectrometer,
KONUS, are Dr. T. L. Cline, NASA/Goddard Space Flight Center, Greenbelt,
Maryland and Dr. E. Mazets, IOFFE Physical Technical Institute, St.
Petersburg, Russia. The objective of KONUS is to perform gamma-ray burst
studies similar to the TGRS studies. It will perform event detection and
will measure time history and energy spectra. Although KONUS has lower
resolution than TGRS, it has broader area coverage to complement that of
TGRS so that, when their data are combined, they provide coverage of the
full sky. KONUS is the first Russian instrument to fly on an American
satellite since civil space cooperation between the U.S. and Russia was
resumed in 1987. KONUS will continuously monitor cosmic gamma-ray bursts
and solar flares in the energy range 10 keV to 10 MeV.

Measurement Objectives:

> • Measurement of gamma-ray burst energy spectra over the energy range
> 10 keV to 10 MeV, with energy resolution E/∆E = 15 @ 200 keV.
>
> • Measurement of burst time histories in three energy ranges covering
> 10 to 770 keV.
>
> • High-time-resolution measurement (2 ms resolution) for the
> high-intensity sections of a burst time history.
>
> • Continuous measurement of the gamma- and cosmic-ray background,
> interrupted only to read out bursts.

The KONUS instrument consists of two Russian sensors mounted on the top
and bottom of the spacecraft aligned with the spin axis, a U.S.
interface box, and a Russian electronics package mounted in the
spacecraft body. The sensors, copies of ones successfully flown on the
Soviet COSMOS, VENERA and MIR missions, are identical and
interchangeable NaI scintillation crystal detectors of 200 cm2 area,
shielded by Pb/Sn. The design and location of the two sensors ensure
practically isotropic angular sensitivity. The relative count rates
recorded by the two detectors can provide a burst source locus to within
a few degrees relative to the spin axis. On-board analysis of background
and burst events is performed by four pulse height analyzers, four time
history analyzers, two high resolution time history analyzers, and a
background measurement system.

**Magnetic Field Investigation (MFI)**

The principal investigator for the Magnetic Field Investigation (MFI) is
Dr. R. Lepping of NASA/Goddard Space Flight Center, Greenbelt, Maryland.
MFI will investigate the large-scale structure and fluctuation
characteristics of the interplanetary magnetic field, which influence
the transport of energy and the acceleration of particles in the solar
wind and dynamic processes in the Earth's magnetosphere. The fundamental
observations of solar wind magnetic fields are important to the study of
the solar wind and magnetosphere coupling process and also to the
interpretation of other observational data from WIND.

MFI will measure the large-scale structure and fluctuation
characteristics of the interplanetary magnetic field as functions of
time, and through correlative studies to relate them to the dynamics of
the magnetosphere.

Measurement Objectives:

> • Accurate, high-resolution vector magnetic field measurements in near
> real time on a continuous basis.
>
> • A wide dynamic measuring range, from ±0.004 nT to ±65,536 nT, in
> eight discrete range steps.
>
> • Measurement rates up to 44 vector samples per second for analysis of
> fluctuations.

The MFI instrument consists of dual triaxial fluxgate magnetometers
mounted on a 12-meter radial boom, and a data processing and control
unit within the body of the spacecraft. The magnetometer sensors each
produce analog signals proportional to the strength of the magnetic
field component aligned with the sensor. These signals are then
digitized and processed by a microprocessor-controlled data system.
Mounting the magnetometers at the outboard end and at an inboard
location on the boom helps substantially to reduce contamination of the
measurements by spacecraft-generated magnetic fields. MFI has a very
wide field measurement capability, from ±0.004 nT to ±65,536 nT, with
both automatic and commandable range-change capability. Measurement
rates are: one vector per 92 seconds for key parameter data, 10.9
vectors per second for rapid data for standard analysis, and 44 vectors
per second for Fast Fourier Transform data, and data from the snap-shot
memory which can be triggered automatically for pre-defined field
changes.

**3-D Plasma and Energetic Particle Analyzer (3-D Plasma)**

The Principal Investigator for the 3-D Plasma and Energetic Particle
Analyzer (3-D Plasma) is Dr. R. Lin, Space Sciences Laboratory,
University of California , Berkeley, CA. The 3-D Plasma investigation
will measure ions and electrons in the interplanetary medium with
energies including that of the solar wind and into the energetic
particle range. This experiment will cover the gap

between the energy ranges covered by SWE and EPACT. It will study
particles in the thermal and suprathermal energy range, upstream of the
bow shock in the foreshock region and the transient particles emitted by
the Sun during solar particle events following solar flares. The 3-D
Plasma instrument was designed to study transport of particles and basic
plasma acceleration processes in the interplanetary medium, and to
measure the particle and plasma input to and output from the Earth's
magnetosphere.

Measurement Objectives:

> • The three-dimensional distribution of plasma and energetic electrons
> and ions over the particle energy range from solar wind to cosmic ray
> energies, a few eV to several MeV.
>
> • Energy resolution of 0.20 (∆E/E) and angular resolution of 5.6° by
> 5.6°, for particles from 3 eV to 30 keV; and energy resolution of 0.3
> (∆E/E) and angular resolution of 22.5° by 36°, for particles from 20
> keV to 11 MeV.
>
> • Perturbations to the electron distribution function, in
> wave-particle interactions.

The 3-D PLASMA instrument consists of two sensor packages mounted on
small radial booms, and an electronics package mounted inside the
spacecraft. One boom-mounted sensor package contains an array of 6
double-ended semiconductor telescopes, each with two or three closely
sandwiched silicon detectors to measure electrons and ions above 20 keV.
One side of each telescope is covered with a thin foil that absorbs ions
below 400 keV. On the other side, the incoming electrons below 400 keV
are swept away by a magnet so that electrons and ions are cleanly
separated. Higher energy electrons (up to \~1 MeV) and ions (up to 11
MeV) are identified by the two double-ended telescopes which have a
third detector. The first sensor package also contains a pair of ion
electrostatic analyzers (PESA-L and -H) for measuring ion fluxes from
\~3 eV to 40 keV. The second sensor package contains a pair of electron
electrostatic analyzers (EESA-L and -H) for measuring electron fluxes
from \~3 eV to 30 keV, and for making input (from EESA-H) to a fast
particle correlator (FPC). The FPC, also using plasma wave data from
WAVES as input, measures perturbations to the electron distribution
function and studies other wave-particle interactions.

**Solar Wind and Suprathermal Ion Composition Experiment (SMS)**

The principal investigator for the solar wind and suprathermal ion
composition experiment (SMS) is Dr. G. Gloeckler from the Institute of
Physical Sciences and Technology and from the Department of Physics at
the University of Maryland. The SMS experiment comprises three major
instruments: Solar Wind Ion Composition Spectrometer (SWICS), High Mass
Resolution Spectrometer (MASS), and Suprathermal Ion Composition
Spectrometer (STICS). This experiment will determine the abundance,
composition and differential energy spectra of solar wind ions, and the
composition, charge state and 3-D distribution functions of suprathermal
ions. These ions and their abundance fluctuations provide information
about events on the solar surface and the formation of the solar wind,
complementing the EPACT and 3D-PLASMA investigations.

Measurement Objectives:

> • Energy, mass and charge composition of major solar wind ions from H
> to Fe, over the energy range from 0.5 to 30 keV/e. (SWICS)
>
> • High mass-resolution elemental and isotopic composition of solar
> wind ions from He to Ni, having energies from 0.5 to 12 keV/e. (MASS)
>
> • Composition, charge state and 3-D distribution functions of
> suprathermal ions (H to Fe) over the energy range from 8 to 230 keV/e.
> (STICS)

The SMS experiment consists of five separate packages mounted on the
spacecraft body. SWICS uses electrostatic deflection, post-acceleration,
and a time-of-flight vs. energy measurement to determine the energy and
elemental charge state composition of solar wind ions. MASS uses

energy/charge analysis followed by a time-of-flight measurement, to
determine solar-wind ion composition with high mass-resolution (M/∆M \>
100), for the first time. STICS, similar to SWICS but not using
post-acceleration, has a large geometric factor and wide-angle viewing
for studies of suprathermal ions. The SMS data processing unit and STICS
analog electronics unit are mounted separately.

**Solar Wind Experiment (SWE)**

The principal investigator for the solar wind experiment (SWE) is Dr. K.
Ogilvie from NASA/Goddard Space Flight Center. SWE will measure ions and
electrons in the solar wind and the foreshock regions (particles whose
energies are in the kiloelectronvolt range). From these measurements,
the solar wind velocity, density, temperature and heat flux can be
deduced. Electron and ion velocity distributions should reveal
properties of the flowing solar wind plasmas and their pivotal role in
the transfer of mass, momentum, and energy from the Sun to the Earth.
Measurements made in the foreshock region will contribute to
understanding the structure of the bow shock.

Measurement Objectives:

> • High time-resolution 3-D velocity distributions of the ion component
> of the solar wind, for ions with energies ranging from 200 eV to 8.0
> keV.
>
> • High time-resolution 3-D velocity distributions of subsonic plasma
> flows including electrons in the solar wind and diffuse reflected ions
> in the foreshock region, with energies ranging from 7 eV to 22 keV.
>
> • High angular-resolution measurements of the "strahl" (beam) of
> electrons in the solar wind, along and opposite the direction of the
> interplanetary magnetic field, with energies ranging from 5 eV to 5
> keV.

The SWE instrument consists of five integrated sensor/electronics boxes
and a data processing unit (DPU). The sensor units are mounted on the
top and bottom shelves of the spacecraft, extending through the top and
bottom surfaces. 3-D velocity distribution measurements of the ion
component in the solar wind are made by a pair of Faraday Cup analyzers,
which provide a wide field-of-view and the capability for flow
characterization within one spin revolution (3 seconds). 3-D velocity
distribution measurements of ions and electrons in plasmas having Mach
numbers \<1 are made using six cylindrical electrostatic deflection
analyzers, called Vector Electron and Ion Spectrometers (VEIS), arranged
in two triaxial sets. A toroidal electrostatic analyzer with
channelplate detectors functions as the strahl sensor, measuring
electron velocity distribution and pitch angle. An ultra-violet
calibration unit for the VEIS is mounted inside the spacecraft with the
DPU.

**Transient Gamma-Ray Spectrometer (TGRS)**

The principal investigator for the Transient Gamma-Ray Spectrometer is
Dr. B. J. Teegarden from NASA/Goddard Space Flight Center. TGRS will
detect transient gamma-ray burst events and will make the first
high-resolution spectroscopic survey of cosmic gamma-ray bursts, and
will also make measurements of gamma-ray lines in solar flares. Cosmic
gamma-ray bursts are among the most violent and energetic processes
known to exist in nature, characteristically emitting most of their
luminosity at gamma-ray wavelengths. The high resolution spectroscopy of
solar flares will contribute to the study of solar flare activities and
help in the understanding of the coupling between the active corona and
photosphere.

Measurement Objectives:

> • Spectroscopic measurements of transient gamma-ray events, in the
> energy range from 15 keV to 10 MeV.
>
> • Energy resolution of 2.0 keV @ 1.0 MeV (E/∆E = 500).
>
> • Monitoring of the time variability of the 511 keV line emission from
> the galactic center, on time scales from \~2 days to \>1 year.

The TGRS instrument consists of four assemblies: detector-cooler
assembly, pre-amp, and analog processing unit, all mounted on a tower on
the +Z end of the spacecraft, and a digital processing unit mounted in
the body of the spacecraft. The detector is a 215 cm3 high purity n-type
germanium crystal of dimensions: 6.7 cm (diameter) by 6.1 cm (length),
radiatively cooled to 85 degrees K. The germanium serves as a reaction
medium for incoming gamma rays, which, depending on their energy, are
either stopped by or passed through the detector crystal. Particle
energy and angle of incidence are calculated based on a number of
primary and secondary interaction processes, including photoelectric,
Compton, pair and bremsstrahlung radiation as well as the ionization
energy losses of secondary electrons. A two-stage cooler surrounds the
detector, providing a field of view of 170˚. Gamma-ray bursts and solar
flares are expected to be detected at a frequency of several per week,
with typical durations between 1 second and several minutes. Between
bursts the instrument is maintained in a waiting mode, measuring
background counting rates and energy spectra. When a burst or flare
occurs, the instrument switches to a burst mode, where each event in the
detector is pulse-height analyzed and time tagged in a burst memory.
Then the instrument switches to a dump mode for reading out the burst
memory.

**Radio and Plasma Wave Experiment (WAVES)**

The principal investigator for the Radio and Plasma Wave experiment
(WAVES) is Dr. J.-L. Bougeret from the Laboratoire de Recherche Spatiale
Observatoire de Paris-Meudon, France. WAVES will provide comprehensive
measurements of the radio and plasma wave phenomena that occur in the
solar wind upstream of the Earth's magnetosphere and in key regions of
the magnetosphere. Analyses of these measurements, in coordination with
the other onboard plasma, energetic particles, and field measurements,
will further the understanding of solar wind and interplanetary plasma
processes.

Measurement Objectives

> • Low-frequency electric waves and low-frequency magnetic fields, from
> DC to 10 kHz.
>
> • Electron thermal noise, from 4 kHz to 256 kHz.
>
> • Radio waves, from 20 kHz to 14 MHz.
>
> • Time-domain waveform sampling, to capture short duration events that
> meet quality criteria set into the WAVES data processing unit (DPU).

The sensor system of the WAVES experiment consists of three electric
antenna systems (two coplanar, orthogonal wire antennas in the
spin-plane and a rigid spin-axis dipole) and a triaxial magnetic search
coil. The longer and shorter spin-plane dipoles have lengths of 100 and
15 m tip-to-tip, respectively, while the spin-axis dipole is 10.56 m
long tip-to-tip. The triaxial magnetic search coil for measuring
low-frequency magnetic fields is mounted at the outboard end of a 12 m
radial boom. There are five main receiver systems: a low frequency (DC
to 10 kHz) Fast Fourier Transform receiver, a broadband (4 kHz to 256
kHz) electron thermal noise receiver, two swept-frequency radio
receivers (20 kHz to 1 MHz, and 1 MHz to 14 MHz), and a time-domain
waveform sampler (up to 120,000 samples per second). The DPU controls
and acquires data from all operations of the experiment, and can be
reprogrammed from the ground. The receiver systems and DPU are housed
within the spacecraft body. WAVES has onboard interconnects with 3-D
PLASMA and with SWE.

.c1.**Appendix B - Overview of the Polar Mission Instruments**;

**Charge and Mass Magnetospheric Ion Composition Experiment (CAMMICE)**

The principal investigator for the Charge and Mass Magnetospheric Ion
Composition Experiment (CAMMICE) is Dr. T. Fritz from Boston College,
Boston. CAMMICE will determine the composition of major ion constituents
in the near-Earth plasma sheet and in the ring current. This
investigation will add to our understanding of the mechanisms that
control the energization, storage, and precipitation of particles in the
high-latitude magnetosphere.

Measurement Objectives:

> • Energy, time-of-flight, and the energy per charge of the incident
> ion flux, over the energy range from 6 keV/Q to 400 keV/Q, to make a
> unique determination of the ion charge state, mass, and incident
> energy.
>
> • Rate of energy loss and incident ion energy for ions, over the
> energy range from 100 keV per ion to 60 MeV per ion, to make a unique
> determination of the ion mass, elemental identification, and incident
> energy.

CAMMICE consists of two sensor systems: the Magnetospheric Ion
Composition Sensor (MICS), and the Heavy Ion Telescope (HIT). The MICS
sensor uses a conically-shaped electrostatic analyzer, a
secondary-electron generation/detection system, and a solid-state
detector, covering the energy range from 6 keV/Q to 400 keV/Q. The HIT
sensor uses a three-element solid-state detector telescope, covering the
energy range from 100 keV per ion to 60 MeV per ion. MICS and HIT are
mounted on the radial surface of the spacecraft, each with a separately
mounted data processing unit.

**Comprehensive Energetic-Particle Pitch-Angle Distribution (CEPPAD)**

The principal investigator for the Comprehensive Energetic-Particle
Pitch-Angle Distribution (CEPPAD) instrument is Dr. B. Blake of the
Space Sciences Laboratory at The Aerospace Corporation, Los Angeles,
California. The CEPPAD investigation will use a variety of techniques to
provide detailed energy spectra and angular distributions of energetic
particles, which in turn will provide quantitative information on the
sources, energization, transport, and losses of energetic particles in
the magnetosphere. The CEPPAD will also measure the rate of particle
precipitation into the Earth's upper atmosphere.

Measurement Objectives:

> • Pitch angle measurements of electrons with energies from 25 keV to 3
> MeV and protons with energies from 10 keV to 17 MeV, with angular
> resolution of 3° in the source/loss cone, and \~12° in other
> directions.
>
> • Identification and pitch angle measurements of alpha particles from
> 300 to 1100 keV/n and CNO nuclei with energies above 300 keV/n.

The CEPPAD consists of three packages: two body-mounted, and one on the
despun platform. One body-mounted package consists of the Imaging
Electron Sensor (IES) and the High Sensitivity Telescope (HIST). IES
measures electrons with energies from 25 to 400 keV using a spectrometer
incorporating a Microstrip Solid Plate Detector (MSSD) with five
elements. HIST, a solid-state detector telescope, measures electrons
with energies to 3 MeV and protons to 17 MeV, also alpha particles and
CNO ions. The second body-mounted package consists of the Imaging Proton
Sensor (IPS) and the digital processing unit (DPU) serving IPS, IES and
HIST. The IPS, functioning similarly to the IES, measures protons from
10 kev to 1 MeV. The despun platform

package is the Source/Loss Cone Energetic Particle Spectrometer (SEPS),
which contains its own DPU. SEPS exploits the pointing of the platform
along the ambient magnetic field to greatly enhance its angular
resolution of energetic particles within the source/loss cone.

**Electric Field Instrument (EFI)**

The principal investigator for the Electric Field Instrument (EFI) is
Dr. F. Mozer of the Space Sciences Laboratory at the University of
California, Berkeley, California. EFI will measure the electric field
strength and thermal electron density in the vicinity of the spacecraft.
These measurements will be used to infer the electric-field structure of
the high-latitude magnetosphere, the cusp, and the plasma mantle; and
will also provide direct evidence for auroral field-aligned electrical
potential drops, which have been previously inferred to occur.

Measurement Objectives:

> • Triaxial components of the ambient vector electric field and the
> thermal electron density, over a frequency range of DC to 20 kHz.
>
> • Electric field measurements over a dynamic range of 0.02 to 1000
> mV/m, and plasma densities from 0.1 to 100 particles per cubic
> centimeter.
>
> • A sampling rate of 40 samples per second in the normal mode, and
> 1000 samples per second in the burst mode.

EFI utilizes six spherical potential sensors, mounted in pairs at the
ends of two coplanar, orthogonal wire booms in the spin plane and on a
rigid boom aligned along the spin axis. An axial boom stabilizer is
provided. The spin-plane sensor pairs have separations of 130 and 100 m,
respectively, while the spin-axis boom sensors are separated by 14 m. An
electronics box is mounted within the spacecraft body. A two megabyte
burst memory allows storage of high-time-resolution field and plasma
density measurements. EFI sensors provide input to PWI, and EFI
interfaces with MFE, TIDE, and Hydra instruments for coordination of
burst-mode measurements.

**Fast Plasma Analyzer (Hydra)**

The principal investigator for the Fast Plasma Analyzer (Hydra) is Dr.
J. Scudder from the Department of Physics and Astronomy at the
University of Iowa, Iowa City, Iowa. Hydra will provide rapid
measurements of the three-dimensional low-energy ion and electron
distribution functions. The low-energy electrons sampled by Hydra will
be especially good tracers of the global magnetic topology when compared
with simultaneous measurements acquired by SWE in the solar wind. Hydra
will also document the electron and ion signatures accompanying
geomagnetic substorms, auroral arcs, field-aligned currents, and
particle precipitation.

Measurement Objectives:

> • Mean energy of electrons and ions between 2 eV and 35 keV, with time
> resolution of 0.5 seconds, for dense coverage over 4π steradians.
>
> • Angular resolution of 1.5° and time resolution of 3 seconds, for
> electrons between 100 eV and 10 keV along and opposed to the magnetic
> field.

Hydra utilizes two types of instruments: a deployment of cylindrical
electrostatic analyzers (ESA) in six pairs, providing 12 simultaneous
samples, and a pair of parallel plate analyzers (PPA) functioning as a
loss/source cone sensor; mounted in four boxes (2- ESA, 2-PPA) on the
spacecraft body, with the sensors protruding through the solar arrays.
Each ESA has a Field of View (FOV) of 10° by 10°; and the PPA covers a
conical FOV of 30° by 30° simultaneously along and opposed to the
magnetic field, providing angular resolution in 1.5° by 1.5° pixels. The
data processing unit is mounted inside the spacecraft body. Hydra
receives magnetic field raw data

from MFE, and is linked to EFI and TIDE to ensure coordinated high-time
resolution "burst mode" measurements.

**Magnetic Fields Experiment (MFE)**

The principal investigator for the Magnetic Fields Experiment (MFE) is
Dr. C. Russell from the Institute of Geophysics at the University of
California Los Angeles, Los Angeles, California. MFE will measure
accurately the magnetic fields in the high and low altitude polar
magnetosphere. These measurements will furnish data both to other
instruments on board the spacecraft and to the ground investigator team,
while at the same time, providing a state-of-the-art research tool for
furthering the understanding of magnetospheric processes.

Measurement Objectives:

> • Accurate vector magnetic field measurements over the frequency range
> from 0 to 50 Hz, at field strengths from 10¯6 to 0.6 gauss.
>
> • Measurement rates up to 100 vector samples per second with onboard
> processing, allowing burst-mode telemetry at that rate, or economical
> data compression and distribution.

The MFE instrument consists of two triaxial fluxgate magnetometers
mounted on a 6-meter radial boom, and an electronics package mounted
inside the spacecraft. The magnetometer sensors each produce analog
signals proportional to the strength of the magnetic field component
aligned with the sensor. One magnetometer is mounted at the outboard end
of the radial boom and the other at one-third the length of the boom,
helping to significantly reduce contamination of the measurements by
spacecraft-generated magnetic fields. Onboard processing allows direct
broadcast to other instruments on the spacecraft, and telemetry data
transmission at 10 samples per second in the standard mode, or 100
samples per second in the burst mode. The design provides a fully
redundant instrument.

**Polar Ionospheric X-Ray Imaging Experiment (PIXIE)**

The principal investigator for the Polar Ionospheric X-Ray Imaging
Experiment (PIXIE) is Dr. W. Imhoff from the Lockheed Palo Alto Research
Laboratory in Palo Alto, California. Using a pin-hole camera concept,
PIXIE will measure the X-ray emissions from the Earth's atmosphere. The
morphology and spectra of energetic electron precipitation and the
effects upon the atmosphere will be derived from these measurements.
These measurements can be used to estimate the total electron energy
deposition rate and the energy distribution of the precipitating
electrons, and thus to compute the altitude profile of ionization and
electrical conductivity.

Measurement Objectives:

> • Images of atmospheric bremsstrahlung X-rays, with ±21° by ?
> field-of-view for global coverage, over the energy range from 3 to 60
> keV, and with sufficient spatial and time resolution (a few minutes)
> to generate movies of dynamic variations in auroral luminosities and
> associated effects.
>
> • Up to 64 channels energy resolution, and spatial resolution of ?,
> over a detector area of 18 by 18 cm, for image construction.

The PIXIE instrument is a multiple pinhole X-ray camera mounted on the
despun platform, with its electronics unit. The number and size of the
pinholes are selectable, using two aperture plates, thus enabling
field-of-view and sensitivity to change as POLAR moves around its highly
eccentric orbit. The focal plane detector uses a multiwire
position-sensing gas proportional counter to measure the energy and
position of each X-ray event, with shielding from cosmic X-rays and

active rejection of other charged particle backgrounds. The electronics
unit includes low and high voltage power supplies, an analog signal
processor for the detector, a digital section that controls event
processing, and a data processing unit that routes data to telemetry and
controls the apertures. Data on each valid X-ray event is telemetered to
the ground, where it is processed into images.

**Plasma Wave Investigation (PWI)**

The principal investigator for the Plasma Wave Investigation (PWI) is
Dr. D. Gurnett from the Department of Physics and Astronomy, University
of Iowa in Iowa City, Iowa. PWI will provide comprehensive measurements
of plasma wave phenomena in the high latitude auroral zones, in the
dayside cusp regions, and in the plasmasphere and plasmasheet. PWI will
sample the electric-field noise above the highest EFI frequencies, and
will sample the magnetic fluctuations above the highest frequencies
detectable by MFE. These measurements will help in the study of plasma
behavior and wave-particle processes. These wave-particle processes
mediated by the electromagnetic turbulence are thought to play a central
role in momentum transfer in the geospace system.

Measurement Objectives:

> • Comprehensive measurements of spectral power and wave vector
> characteristics of electromagnetic and electrostatic plasma waves over
> the frequency range from 0.1 Hz to 800 kHz for wave electric and
> magnetic fields.
>
> • Measurement of spectral and wave vector characteristics of
> electromagnetic and electrostatic plasma waves generated by
> ground-based active experiments.

PWI uses the sensor system of EFI for electric field measurements,
consisting of spherical sensors on two coplanar, orthogonal wire booms
in the spin-plane and on a rigid spin-axis boom. The longer and shorter
spin-plane antennas have lengths of 130 and 100 m tip-to-tip,
respectively, while the spin-axis boom is 14 m tip-to-tip. For magnetic
field measurements, PWI uses a triaxial magnetic search coil and a loop
antenna, both mounted at the outboard end of a 6-m radial boom. There
are five main receiver systems mounted on the spacecraft body: a low
frequency AC receiver (0.1 Hz to 25 Hz); a wideband receiver with
selectable 11, 22, or 90 kHz bandwidths, with lower band edge at 0, 125,
250 or 500 kHz; a narrow-band swept-frequency receiver covering the
range 26 Hz to 808 kHz; a high-time-resolution multi-channel analyzer
with ranges of 5.6 Hz to 311 kHz for electric fields and 5.6 Hz to 10
kHz for magnetic fields; and a waveform receiver covering the range from
20 Hz to 16 kHz.

**Thermal Ion Dynamics Experiment (TIDE)**

The principal investigator for the Thermal Ion Dynamics Experiment
(TIDE) is Dr. T. Moore at Marshall Space Flight Center, Huntsville
Alabama. TIDE will sample ions escaping from the ionosphere. Low-energy
ions from 0.1 to 100 eV per charge will be the focus of TIDE; such ions
can be remotely diagnosed by their relatively low ionization state as
compared with ions of solar-wind origin. These measurements will be used
to track the outflow of ionospheric plasma throughout the magnetosphere.
To make possible the measurement of such low-energy ions, TIDE will use
a Plasma Source Instrument (PSI) which, on command, emits xenon plasma
to neutralize spacecraft charge build-up.

Measurement Objectives:

> • 3-D low energy (0 to 300 eV) measurements differential in energy and
> angle as well as mass.
>
> • 96% unit sphere coverage per spin, with angular coverage of 10° by
> 157.5° for each of 7 simultaneous sectors, and angular resolution of
> 10° by 22.5°.
>
> • Time resolution of 0.188 sec. for 2-D measurements, and 6 sec. for
> 3-D.

TIDE consists of an integrated sensors-electronics unit mounted on the
spacecraft body, with the sensor head exposed to space, having a wide
field-of-view with one edge aligned with the spin axis. TIDE utilizes 7
separate channels (angular sectors), each comprising a collimator,
electrostatic mirrors and retarding potential analyzer (RPA), coupled
with a time-of-flight mass analyzer system. The PSI, separately
body-mounted with an external exit aperture, consists of a 20,000 hour
xenon plasma source, a gas feed system and an electronics system for
powering and monitoring. PSI is operated on command to regulate the
spacecraft at a few tenths of a volt positive relative to the space
plasma. The high time-resolution mode is triggered by data from EFI and
Hydra.

**Toroidal Imaging Mass-Angle Spectrograph (TIMAS)**

The principal investigator for the Toroidal Imaging Mass-Angle
Spectrograph (TIMAS) is Dr. E. Shelley of the Lockheed Palo Alto
Research Laboratory in Palo Alto, California. TIMAS will sample ions of
resolved mass that are either stored particles of solar-wind origin or
energized ions of ionospheric origin. TIMAS will characterize the
principal source regions for entry of solar wind plasma and the hot
ionospheric plasma into the magnetosphere. TIMAS data will be combined
with data from TIDE and from the SMS/SWICS instrument on WIND to
determine the ultimate origin of mass in the high-latitude
magnetosphere.

Measurement Objectives:

> • Full 3-D velocity distribution functions of all major magnetospheric
> ion species, with time resolution of 3 seconds, and 11° by ? angular
> resolution, over the energy per charge range of 15 eV/e to 32 keV/e.
>
> • Simultaneous measurements of all mass/charge components from 1 AMU/e
> to greater than 32 AMU/e over nearly 360° by 10° instantaneous
> field-of-view, in 20 milliseconds.

The TIMAS instrument is a double-focusing (angle and energy) mass
spectrograph, utilizing two toroidal electrostatic analyzers in tandem.
A toroidal magnetic field then disperses the particles by momentum,
leading to an image pattern of rings on a microchannel plate detector,
representing mass spectrum dispersed radially and incident direction
dispersed in azimuth. The instrument is mounted on the radial surface of
the spacecraft, sweeping out a 4π solid angle image in a half
spin-period. Fast-settling internal power supplies provide controlled
high voltages to the electrostatic analyzers for various energy levels,
and sequential processing through two SA-3300 microprocessors corrects,
prioritizes, and compresses data for telemetry transmission.

**Ultraviolet Imager (UVI)**

The principal investigator for the Ultraviolet Imager (UVI) is Dr. G.
Parks from the University of Washington, Seattle, Washington. UVI will
image both dayside and nightside aurorae in the far ultraviolet (FUV)
range. Improvements over previous imagers will allow the instrument to
provide simultaneous global imaging from orbital positions greater than
6 Earth radii. UVI images will provide spatial and temporal descriptions
of the aurorae, total particle energy flux, characteristic energy,
thermospheric neutral composition, and ionospheric conductances. These
images will be used to map the temporal and spatial evolution of
electric fields, needed for global modeling of the thermosphere at the
lower end of the solar-terrestrial chain.

Measurement Objectives:

> • 2-D images of the global auroral oval, spectrally resolved for four
> key FUV wavelengths between 1300 Å and 1900 Å.
>
> • Field-of-view of 8°, providing angular resolution of about ?, with
> ground resolution from 5 to 50 km, dependent upon altitude.

The UVI is an intensified charge coupled device (CCD) used in
conjunction with a fast reflective optical system. The instrument is
mounted on the despun platform, permitting simultaneous imaging of the
entire auroral oval throughout 9 hours of each 18 hour orbit. Five
wheel-mounted interference filters, each combining both transmission and
reflective elements, serve the purpose of passing the FUV wavelengths of
interest, while blocking long wavelength (primarily visible) scattered
sunlight. The CCD detector has an active area of 244 by 550 pixels,
formatted to produce an oval image frame of 200 by 228 effective pixels.
A data processing unit, separately mounted on the despun platform,
integrates the images over a standard frame time of 37 seconds, for
telemetry to the ground.

**Visible Imaging System (VIS)**

The principal investigator for the Visible Imaging System (VIS) is Dr.
Louis Frank from the Department of Physics and Astronomy at the
University of Iowa, Iowa City, Iowa. VIS will image the global aurora at
visible wavelengths, with sufficient spatial and temporal resolution to
resolve the principal dynamical features of auroral phenomena. Data from
VIS and from theory investigations will be used to assess the
dissipation of magnetospheric energy into the auroral ionosphere, and to
develop a model of the energy flow within the magnetosphere.

Measurement Objectives:

> • Auroral images with 12 filters for narrow passbands including N2+ at
> 391.4 nm, OI at 557.7 and 630.0 nm, HI at 656.3 nm, and OII at 732.0
> nm.
>
> • Low-resolution images covering 5.6° by 6.3°, and moderate-resolution
> images covering 2.8° by 3.3°, with images integrated over 256 by 256
> pixels, and with corresponding resolution at Earth's surface of 21 km
> and 11 km, respectively, from 8 RE.

VIS is a set of three low-light-level cameras, all mounted in a single
package on the despun platform. Two of these cameras share primary and
some secondary optics and are designed to provide low- and
moderate-resolution images of the nighttime aurora oval, from the POLAR
orbit at 1 to 8 RE distance. These cameras produce auroral images with
12 narrow passband filters at visible wavelengths, at a frame rate of 12
seconds. A third camera (the Earth camera) is used to monitor the
directions of the fields-of-view of the auroral cameras to ensure that
they are correctly pointed and protected from extremely bright sources
such as the Sun and sunlit Earth. All three cameras use charge coupled
device (CCD) detectors, with optically-coupled image intensifiers.

.c.**Appendix C - Rules for Data Rights: ISTP/NASA funded Missions**

**and Instruments**

Approved: March 15, 1996

Revised: November 14, 1996 (Level 0 Policy added)

[Preamble]{.underline}

The ISTP program is predicated on the concept of placing a constellation
of satellites at key positions within the Sun-Earth connected system to
obtain simultaneous, comprehensive and closely coordinated data. The
accomplishment of the scientific objectives of the program is dependent
upon the availability of these coordinated data sets for analysis by
members of the mission science teams, their co-investigators,
associates, and students, and as quickly as possible, by scientists
selected as guest investigators and by the general scientific community.
The purpose of this document is to set forth the rights and obligations
of the Principal Investigators with the various missions and the various
associates and collaborators who wish access to the data.

[Missions, Instruments and Investigations Covered]{.underline}

The ISTP/NASA funded missions, instruments and investigations consist of
the spacecraft in the Global Geospace Science program (GGS): Wind,
Polar, and collaborating spacecraft, plus the associated ground-based
investigations and theory investigations; the instruments on Geotail:
CPI and EPIC; the WBD (NASA portion) instrument on Cluster; the MDI,
LASCO and UVCS instruments on SOHO, and ground-based investigations.

[Data Rights and Rules for Data Use]{.underline}

1\. The NASA funded missions and instruments have an \"open\" data
policy.

2\. Key Parameter digital data will be non-proprietary and publicly
available to identify possible scientifically interesting events or
intervals. The Key Parameters are not intended for analysis or
publication purposes, and should not be used in that manner.

3\. All GGS PIs and/or PI teams will contribute relevant digital
processed data for any special events or intervals that are selected for
study by the GGS SWG and for the IACG Campaigns in a timely and
responsive fashion. All NASA Campaign data will be archived and
publically available.

4\. During a validation period of up to three months after data
acquisition, all use of the data for scientific investigations must be
approved by the PI whose data are being used. PIs can release their own
validated data at any time but may not release data that are in their
possession from other instruments.

5\. Higher level processed instrument and theory data products, along
with their associated documentation and all relevant software (in source
code form), will be publically available immediately after validation.
These data products, along with Level 0 data will be archived at the
National Space Science Data Center (NSSDC) within a year of generation.

The scientific community is encouraged to exercise and demonstrate
professional courtesy, appreciation, and prudence in utilizing the
openness of the data policy. This would be accomplished, along with
greater scientific certainty in the use and interpretation of the data,
by engaging the PI and members of the investigative team to collaborate
on the planned studies leading to co-authored abstracts and/or
publications.

[Policy with respect to Level 0 Data Distribution]{.underline}

NSSDC has been designated as the deep archive for the ISTP Level 0 data.
In general they only receive and archive the \"All Product\" CD-ROMs.
Because of its nature, Level 0 data is proprietary to the PI team for
one year - after one year it is open to the public. Thus Level 0 data
less than one year old requested by someone other than a member of the
PI team requires written permission from the PI. Level 0 data over and
above the initial distribution will be provided only on a charge back
basis to requesters.

.c.**Appendix D - Rules for Data Rights: Geotail Mission**

As of June 1989

1\. Key parameters and Overview data should not be used for actual
analyses or publication by investigators of any category. The only
possible exception may be the PI's usage of these data derived from
his/her own instrument.

2\. At ISAS, the data in the SIRIUS file (namely, BPB, BRT, SRT data)
are to be regarded as raw data.

3\. Scientific analysis of the Japanese experiment data in Japan is to
be based on CPB and CRT. Until the agreed-on time after the acquisition
of data, the PI has the right to the data and governs the analysis and
publication programs. When more than one PI is involved in a study, the
priority is to be determined by negotiation between the PIs concerned.
The PI's right to the data is accompanied by his responsibility to
produce best scientific outcome from the data.

Where:

> BPB - Basic data file (level 0 uncalibrated) derived from the
> play-back data
>
> BRT - Basic data file derived from the real-time data
>
> SRT - SIRIUS data file derived from the real-time data
>
> CPB - Calibrated and sorted data derived from the play-back data
>
> CRT - Calibrated and sorted data derived from the real-time data

.c1.**Appendix E - Rules for Data Rights: SOHO Mission**;

From the SOHO Science Operations Plan

Issue 1.1

June 1993

**1.3 Use of SOHO data**

1.3.1 Data rights

The objective of a coherent policy on these aspects should be to ensure
the maximum exploitation of the SOHO data in order to extract the best
scientific output from the mission. For this purpose, it is necessary to
find a just equilibrium between two conflicting strategies. These are:

> a\) to open up free access to the widest possible community, thereby
> making available special capabilities and expertise from outside the
> SOHO teams, and
>
> b\) to protect the interests of the PI teams who have invested so much
> personal effort, and through rewards for this effort to motivate them
> to continue to work for the collective scientific interest.

Leadership in applying such a policy rests with the PIs, who have a
moral responsibility for maximizing the science from the mission, as
well as the structure and authority within their teams for applying a
well-defined strategy. However, since the joint exploitation of combined
data sets is a key objective of SOHO, it is important to seek joint PI
or SWT agreements on this policy.

1.3.2 Data access

The term Data Access defined in this section refers to the right to have
access to the data, to survey them in evaluating possible use, but NOT
to carry out analysis with a view to publication.

It is proposed that data access rights be accorded by all SOHO PIs to
all other SOHO PIs for the purpose of operations planning during the
mission. Access rights defined in the above manner may serve many other
useful functions, *e.g.,* to allow potential investigators to verify the
availability of required data sets before finalizing a proposition.

1.3.3 SOHO Science projects

SOHO differs greatly from a classical ground-based telescope or
observatory satellites such as IUE, in may respects. For SOHO, it is
inappropriate (with a few exceptions) to identify a scientific proposal
with a specific observing slot. It is necessary to define science
projects using SOHO in a more flexible form. A proposed project should
consist of a clear scientific objective, together with the proposed
means for its accomplishment. It might or might not include the need for
new observations, the definition of new observing sequences, cooperation
between SOHO instruments or with non-SOHO space or ground-based
observations. It could be based upon analysis of synoptic data over long
periods, recorded primarily for completely different objectives. It
could involve the use of a new analysis or theoretical techniques to
analyze existing data. In spite of flexibility in the form, science
projects should be closely defined. Otherwise, approval to follow one
research aspect could be interpreted to cover a very wide range of
activities.

1.3.4 Responsibilities

It is suggested that PI individual responsibilities should include:

> a\) To manage, in the broadest sense the attribution of science
> projects amongst their team scientist and CoIs.
>
> b\) To advise on the selection of Guest Investigator (GI) proposals
> which concern their instrument.
>
> c\) To consider how wider access with appropriate controls could help
> in stimulating outside (GI) participation.
>
> d\) To define, and announce publicly a Publication Policy. This should
> include a policy for Initial Publications; *i.e.,* a declared number
> of early papers, formally authored, which can also give rewards for
> those involved in technical or engineering effort. An On-going
> Publications Policy should indicate the approval or vetting procedure
> (if any), authorship policy, etc.

Collective PI or SWT agreements and responsibilities include:

> a\) Data access policy, as suggested above.
>
> b\) The establishment and managing of joint science projects.
>
> c\) Advice on the selection of GI joint science proposals.
>
> d\) To encourage a common strategy for the PI (Individual) policy.

1.3.5 Guest Investigators

A SOHO Guest Investigator program is foreseen for the EOF. The Guest
Investigators program must start one year before launch. It is thought
that ESA and NASA will issue an Announcement of Opportunity in due time.
The SOHO SWT will recommend the conditions under which the guest
investigators will be recruited and will participate in the SOHO
research program.

.c1.**Appendix F - Rules for Data Rights: Cluster Mission**;

**DRAFT**

September 9, 1993

• Access to raw data requires authorization by the Principal
Investigator (PI) or his/her delegate

• Access to Summary Parameters is, in principle, unrestricted

• Access to Prime Parameters is restricted to the Cluster community

• Neither Summary Parameters nor Prime Parameters are certified for
publication

• Publications ensuing from the usage of Cluster instrument data require
the consent by the PI or his/her delegate (expiration time: TBD)

These rules are subject to endorsement by the PIs (both in their wording
and completeness).

**RULES GOVERNING ACCESS AND USE OF THE**

**CLUSTER/GROUND-BASED DATABASE**

**DRAFT**

April 5, 1995

Preamble: Certain projects operate under a set of rules (*e.g.,* the
CDAW, DE and ISEE Rules of the Road) which identify obligations of
investigators and researchers with regard to data provided by other
investigators. Because the activities of and principal publications by
members of the Cluster/Ground-Based (CLGB) Coordination are, by design,
collaborative efforts which greatly exploit interchange of data within
the research community, the following rules are adopted.

\[If a conflict is identified between these rules and the rules
governing a data set provided to the Cluster/Ground-based data center
the project rule is adopted and an amended copy of the CLGB rules will
be forwarded to each member of the CLGB coordination project.\]

1\. Access to the CLGB database will be granted to established,
participating members of the CLGB Coordination. Members who withdraw
from participation in the project are obligated to continue to respect
the rules established here.

CLGB members are those scientists belonging to institution- specific
research teams providing data to the CLGB database, and/or belonging to
modeling/theory teams whose participation is invited by the CLGB Working
Group. CLGB members are also those other individuals who, through
attendance at regularly scheduled workshops, make significant
contributions to organizing, reformatting, and interpreting data in the
database.

2\. Members of the CLGB Coordination may share data with members of
their research team, but are not entitled to further distribute data
provided by other investigators. The CLGB member is

responsible to CLGB for ensuring that these rules are followed by
members of his/her research team.

3\. The CLGB database is established primarily for identification of
suitable correlative studies by members of the CLGB. Access to the
database and support software provides individual members of CLGB the
means of correlating the summary data sets for the purpose of event
identification. Preparation of summary data sets is the responsibility
of the investigator who supplies the data, and is not to be undertaken
by other members of the CLGB, unless agreed upon by the principal
investigator in question.

4\. If an investigator's summary data can be used in the more detailed
analysis of an event, the investigator responsible for providing these
data should be kept informed of what it is being used for, and should be
given the opportunity to update the preliminary dataset with more
refined data. He should be invited at an early and appropriate time to
participate in the correlative analysis, and must be invited to
participate as a co-author of any resulting publication or presentation,
including abstracts. All co-authors of a research paper or abstract must
be given a reasonable opportunity to review that work prior to
submission for publication. If an investigator chooses to decline
co-authorship after reviewing the work, that investigator is still
encouraged to provide a critical review of the principal author if a
disagreement exists concerning the interpretation of that investigator's
data.

5\. If an investigator declines co-authorship of a paper, an
acknowledgment of that investigator's participation shall be provided.
Authors are also requested to give acknowledgment to the joint efforts
of the CLGB working group and the WDC at RAL, as this will help in
making these efforts more visible to the research community and
supporting agencies, and may assist in establishing and enhancing future
joint activities. A short, standard wording of an acknowledgment will be
offered as a suggestion.

6\. New CLGB members will be welcome at any time, and in particular
after the first major (series of) publications of CLGB results. These
new members will abide by these rules of the road. Access of the
database according to these rules of the road will be granted until, in
the first instance, December 1999. Extension of this period would be
desirable and will be discussed by CLGB members in the light of gained
experience. (After this period the database may be opened without
restrictions, however, individual investigators will be given the
opportunity to withdraw their data from the CLGB database prior to a
public release.)

7\. Access to this database will be restricted by computer name to a
list of institutes, approved by the CLGB working group. A log of all
retrievals of a subset of the database will be sent to the relevant data
provider.

8\. Submission of data to RAL for CLGB Coordination by an investigator
does not constitute submission of data to the CLGB as part of any
contractual obligation.

9\. Unless declared otherwise, the summary data in the CLGB database at
RAL are provided to identify scientifically interesting periods. They
are designed to support data analysis efforts only, and are not to be
used for any other purpose without the specific authorization of the
appropriate Principal Investigators. Any of the summary datasets can
contain unverified data.

.c1.**Appendix G - Rules for Data Rights: Interball Mission**;

**INTERBALL KEY PARAMETERS**

**RULES OF THE ROAD**

Key Parameters (KP) are fast and reliable data set on main plasma, wave,
energetic particle and geomagnetic characteristics. Documentation on KP
and sample KP are open, full KP are available according to these Rules
of the Road.

**Access Rights**

All INTERBALL participants will have free access to all KP from all
mission experiments. The password to the archive will be given to PIs
and/or their Co-PIs in IKI RAN after the launch. It is the
responsibility of PI to distribute the password among his/her Co-Is.

For the selected time intervals (e.g. during international campaigns) KP
will be available to the part of the scientific community, involved in
the campaign. INTERBALL community for these periods of time will have an
access to appropriate KP or their analog of partner missions. This
procedure is supposed to facilitate background for further more extended
and detailed data analysis on PI-to-PI basis.

Other interested researches must apply to the INTERBALL Scientific
Committee.

After three years all KP will have unrestricted access.

**Publication Rights**

KP are intended mainly for planning, event selection and preliminary
studies. Explicit use of the KP data in the publication must be agreed
with the PI at an early and appropriate time.

.c1.**Appendix H - IACG Rules for Data Exchange**;

**RULES GOVERNING ACCESS AND USE OF THE**

**IACG 1st CAMPAIGN DATABASE**

DRAFT 1/26/94

5/13/95

**[Preamble]{.underline}**

The overall scientific objectives of the IACG 1st Campaign are discussed
in detail in the publication edited by Whipple and Lancaster \[Toward a
New Era of Global Solar-Terrestrial Research: 1st IACG Campaign on
Magnetotail Energy Flow and Non-linear Dynamics, SAIC, October 1992\].
It is the responsibility of the IACG Working Group-3 to prepare the
appropriate orbit analysis and for IACG Working Group-1 to select the
times when the IACG spacecraft are in the most favorable positions for
the correlative analysis thereby defining the time interval of the 1st
IACG Campaign. The IACG Working Group-2 provides support for
facilitating data exchange including networks, formats, and data
visualization tools.

Nearly all spacecraft and ground-base projects operate under a set of
data exchange rules that identify obligations of researchers about data
provided by other science research investigators. Because the scientific
aim of the IACG 1st Campaign is, by design, multi-mission collaborative
efforts, which greatly extends this interchange of data within the
international research community, the following rules are adopted for
use in the IACG 1st Campaign. For the 1st Campaign, the IACG core
missions are Geotail, Wind, Polar, and the four Interball spacecraft.
Ancillary data are also being used in the IACG 1st Campaign and include
selected instruments on (but are not limited to) IMP-8, GOES 6 & 7, the
Los Alamos National Laboratory equatorial spacecraft, and a variety of
ground based radar and other instruments.

These \"Rules of the Road\" apply only to the first IACG Campaign and do
not impose any limitation on any principal investigator to distribute
his/her data, or to exchange and to cooperate with other scientists and
scientific groups as he/she sees fit.

**[Mission Rules and KP distribution]{.underline}**

Each of the core IACG missions and relevant ancillary data sources are
generating various levels of data products. In general, the key
parameter data (referred to as KP or key physical parameter plots
(KPPP), or Summary Parameters) are being generated by all the IACG core
missions and other ancillary data sources in a common format.

During Campaign periods the key parameter data are freely exchanged and
accessible to all principal investigators (PI) and co-investigators
(Co-I) on the IACG \"core\" missions and ancillary data instruments in
accordance with the IACG rules. IACG rules state that the key parameter
data will be used for multi-spacecraft event identification and are not
citable or publishable unless explicit certification is given by the
appropriate instrument PI. This rule will also apply to the IACG 1st
Campaign.

**[Campaign Rules]{.underline}**

These \"Rules of the Road\" govern access to and use of data contributed
to the IACG 1st Campaign database and data analysis effort. The IACG 1st
Campaign databases may include any database which may be created for the
correlative analysis of data from intervals corresponding to the IACG
1st Campaign and may be assembled to contribute to any of the 1st
Campaign science objectives. It is expected that these databases will
contain a number of different data products such as: PI certified KP
data (data which can be published), event data, high time resolution
data, etc.

Strict adherence to these rules by all participants, and those applying
to participate, is expected. It is the responsibility of each
participant to ensure that data taken by them from the IACG 1st Campaign
database in whatever form (plots, listings, electronic files, etc.) are
held and used according to these Rules. Any member who withdraws from
participation in the IACG 1st Campaign is obligated to continue to
respect the rules established here.

**[Membership (IACG Mission Scientists)]{.underline}**

All PIs and Co-Is from IACG core missions and ancillary instruments who
wish to participate in multi-mission campaign database must provide a
\"statement of research intent\" to the 1st Campaign Coordination
Committee. This statement should include the scientific approach, data
required (including his/her own), expected analysis techniques, and a
list of all investigators involved. This statement is required by the
Campaign Workshop Organization Committee for the better preparation of
the campaign science workshops. The statement of intent should not
exceed one or two pages.

**[Membership (non- IACG Mission Scientists)]{.underline}**

Access to the IACG 1st Campaign database will be granted to established,
participating members of the IACG 1st Campaign. Membership for other
scientists wishing to contribute, but who are not PI or Co-Is from the
IACG core missions or ancillary instruments, will be approved through a
peer reviewed proposal process. Campaign members are those scientists
who are named in the approved proposals. Proposal instructions are given
in the attachment to these rules.

All Campaign members are responsible to the IACG 1st Campaign
Coordination Committee for ensuring that these rules are followed. The
IACG 1st Campaign Coordination Committee consists of A. Nishida (ISAS),
M. Acuna (NASA), R. Schmidt (ESA), and L. Zelenyi (IKI) with J. Green
(NASA) as lead coordinator.

**[Sharing of Data]{.underline}**

For the IACG 1st Campaign, key parameter data are routinely exchanged
between campaign members and are used to support the identification of
events. Members of the IACG 1st Campaign may share higher level campaign
data products with members of their research team, but are not entitled
to further distribute the Campaign data provided by other investigators.
Distribution of detailed instrument data is the responsibility of the
instrument Principal Investigator.

**[Data Set Preparations]{.underline}**

The IACG 1st Campaign database will be established solely for
correlative studies by members of the Campaign. Access to the database
and support software will provide individual members of

the Campaign the means of correlating the established data sets.
Preparation of an established data set is the responsibility of the
investigator who supplies the data. It is envisioned that several 1st
Campaign databases will be constructed. It is desirable that the
campaign databases be located at several central organizations such as
NASA, ISAS, etc. However, the database location is a decision that is
collectively made by the teams of scientists working on the 1st Campaign
science objectives.

**[Authorship]{.underline}**

When an investigator\'s data (such as PI certified key parameter data or
any other processed data product) is used in the analysis of an event,
the investigator who provided these data should be kept informed of what
they are being used for, should be invited at an early and appropriate
time to participate in the correlative analysis, and would normally have
the option of being a co-author of any resulting publication or
presentation, including abstracts. Authors are reminded that
acknowledgments of the joint efforts of the Campaign participants and
the IACG assist in making these efforts more visible to the research
community and supporting agencies, and assist in establishing and
enhancing future joint activities.

**[Public Release of Data]{.underline}**

Unrestricted access of the database will be granted at the conclusion of
the Campaign. Non-NASA Investigators will be given the opportunity to
withdraw their data from the IACG 1st Campaign database before this
public release.

Approved by:

![](media/image1.pct){width="2.513888888888889in"
height="0.5138888888888888in"} ![](media/image2.pct){width="1.375in"
height="0.9305555555555556in"}

A. Nishida, ISAS R. Schmidt, ESA

![](media/image3.pct){width="2.2222222222222223in"
height="1.0972222222222223in"}
![](media/image4.pct){width="1.6527777777777777in"
height="0.5555555555555556in"}

M. Acuna, NASA L. Zelenyi, IKI

**ATTACHMENT TO THE IACG 1ST CAMPAIGN**

**PROPOSAL INSTRUCTIONS FOR NON-IACG MISSION SCIENTISTS**

**[Evaluation and Content]{.underline}**

All IACG 1st Campaign proposals will be sent to the Science Working
Groups (SWG) of the respective missions for evaluation and
prioritization by the lead Campaign Coordinator. In addition, a copy of
the proposal must be sent to the Campaign Coordinator. This is necessary
for determining compatibility with instrument capabilities and resource
limitations.

The SWG(s) will review the proposals for:

> \- Potential contribution to the Scientific Objectives of the 1st
> Campaign
>
> \- IACG missions to be used and how
>
> \- Impact on instrument operations
>
> \- Proposer\'s ability to complete the investigation
>
> \- Additional data (ground-based, etc.) brought to the campaign by the
> proposer or other type of contribution.
>
> \- Prior approval from the PIs whose data are required

These prioritized proposals will be forwarded from the SWG to the IACG
Campaign Coordination Committee for final approval. The IACG 1st
Campaign Coordination Committee consists of A. Nishida (ISAS), M. Acuna
(NASA), R. Schmidt (ESA), and L. Zelenyi (IKI) with J. Green (NASA) as
lead coordinator.

The proposals are not to exceed 4 typed pages and have the following
structure:

> \- Title
>
> \- Lead Investigator and other Co-Investigator(s) names and addresses
>
> \- Scientific objectives
>
> \- Precise definition of the data products needed
>
> \- Research Plan and analysis methods
>
> \- Special Requirements on instrument modes or other operations
>
> \- Experience of the Team and their contribution.

Prior endorsements from the IACG mission instrument investigators whose
data would be involved are required.

**[Funding]{.underline}**

The role of the IACG is not to fund scientists for participation within
the campaign process but to facilitate the coordination among the IACG
missions, to acquire the data necessary to meet the campaign science
objectives, and to promote the correlative data analysis.

Scientists who seek to be members of the 1st Campaign and who submit
proposals must provide their own resources for their proposed research.
Therefore, no budget information needs to be part of the science
proposal.

**[Contact]{.underline}**

All questions concerning any aspect of the proposal or status of the
review should be directed to the lead Campaign Coordinator.

James L. Green

Space Science Data Operations Office, Code 630

NASA/Goddard Space Flight Center

Greenbelt, MD 20771

.c1. **Appendix I-Bibliography of ISTP Data Handling Documents**;

(In time order within topic)

*CLUSTER SCIENCE DATA SYSTEM (CSDS) - (abbreviated list)*

Schmidt, R. and M. L. Goldstein, editors, "The Cluster Mission," ESA
SP-1103, 1988.

Cluster Science Data System: Final Report of the CSDS Working Group,
ESA-CL-EST-RP-001, February 1990.

Study of Requirements for a Cluster Science Data Analysis Support
Centre, RAL and IC Consultants Ltd., December 1991.

Cluster Science Data System Requirements Specifications,
ESA-DS-EST-RS-001, January 31, 1993.

Daly, P. W., W. Baumjohann, J. Dandonras, K-H. Glabmeier, C. Harvey, S.
Schwartz, K. Tokar, L. J. C. Woolliscroft, "Report of the data products
task group for the Cluster Science Data System," DS-MPA-TN-001, February
1993.

Daly, P. W., *et al.,* "Report of the data products task group for the
Cluster Science Data System," Issue 2, Revision 1, June 21, 1994.

U.S. Cluster Science Data Center Architectural Design Document, CSC,
September 1993.

Schmidt, R., and L. J. C. Woolliscroft, "Cluster Science Data System - A
distributed system to serve a wide international community," submitted
for publication, 1994.

*CENTRAL DATA HANDLING FACILITY (CDHF)*

Hardware Performance Specification for the ISTP Program Central Data
Handling Facility (CDHF), Preliminary Draft, May 1988.

ISTP Program Central Data Handling Facility (CDHF) System Requirements
Review (SRR) Material, July 14, 1988.

ADPE Acquisition Plan 1649 for the ISTP CDHF, Computer Sciences Corp.,
Contract NAS5-31500, November 1988.

ISTP Program Central Data Handling Facility (CDHF) Software
Specification Review (SSR) Material, February 21, 1989.

ISTP Program Central Data Handling Facility (CDHF) Preliminary Design,
Prepared under Contract NAS5-31500, Computer Sciences Corp.,
CSC/SD-89/6206, October 1989.

ISTP Program Central Data Handling Facility (CDHF) Operations Concept,
Revision 1, May 1990.

Detailed Design Specification for the ISTP Program Central Data Handling
Facility (CDHF), Computer Sciences Corp., Contract NAS5-31500,
CSC/SD-90/6153, August 1990.

ISTP Central Data Handling Facility (CDHF) Critical Design Review (CDR)
Material, August 30 and 31, 1990.

Data Format Control Document (DFCD) between the ISTP Program Information
Processing Division (IPD) Ground Data Processing System and the ISTP
Mission Investigators. This document describes Level Zero (LZ) & SIRIUS
telemetry files, orbit files, attitude files, command history files, and
spin phase files which comprise the input to the KP software, along with
information on SFDUs and ISTP/CDFs.

ISTP CDHF Software System Programming Guide to Key Parameter Generation
Software. This document describes the CDHF KP support routines (the
so-called ICSS routines) used to interface KP software to the CDHF
environment. This document also discusses ISTP/CDFs.

ISTP CDHF Simulated Instrument Data Set (SIDS). This document describes
how KP test data is to be provided into the CDHF environment so that
this test data can be mapped into LZ files and thus be used for testing
of the KP software.

ISTP CDHF Software System User's Guide. This document describes the CDHF
user services, such as query to the CDHF catalog; the transfer of data
sets from the CDHF to the RDAFs; and updating quality information
concerning KPs.

ADPE Acquisition Plan 1649 for the ISTP CDHF, Computer Sciences Corp.,
Contract NAS5-31500, updated by W. H. Mish, July 1991.

Whitman, R., ISTP Project Briefing Material, March 26, 1992.

ISTP Program Central Data Handling Facility (CDHF) System Requirements
Specification, Revision 3, October 1992.

Lehtonen, K., "Architecting the International-Solar Terrestrial Physics
(ISTP) Central Data Handling Facility (CDHF) 1992-2001," Technical
Reference Library, Information Processing Division, Goddard Space Flight
Center, Code 562.7, Greenbelt, MD 20771, June, 1993.

*COMMON DATA FORMAT (CDF)*

CDF User\'s Guide, Version 2.5, NSSDC/WDC-A-R&S 94-11, NASA/Goddard
Space Flight Center, December 1994.

CDF C Reference Manual, Version 2.5, NSSDC/WDC-A-R&S 94-12, NASA/Goddard
Space Flight Center, December 1994.

CDF Fortran Reference Manual, Version 2.5, NSSDC/WDC-A-R&S 94-13,
NASA/Goddard Space Flight Center, December 1994.

Goucher, G. W., and G. J. Mathews, \"A Comprehensive Look at CDF\",
NSSDC/WDC-A-R&S 94-07, NASA/Goddard Space Flight Center, August 1994.

Kessel, R. L., R. E. McGuire, H. K. Hills, and N. J. Love, "CDF
Implementation Guidelines for ISTP", Version 2.3, February 7, 1994.

*DATA CAPTURE FACILITY (DCF)*

ISTP Program Data Capture Facility (DCF) System Requirements
Specification, August 1989.

Software Requirements Specification for the ISTP Program Data Capture
Facility, September 1989.

*DATA DISTRIBUTION ON CD-ROM*

Kulkarni, R., R. Whitman, "ISTP/CDHF Data Distribution System Design
Concept," May 11, 1992.

Rykowski, T., "Minutes of recent file naming convention/CD-ROM
distribution meeting of July 29, 1992," August 7, 1992.

Sawyer, D. and L. Reich, "Proposal for changes to the VOLDESC.SFD file
on the test DDF CD-ROM, and other matters," August 11, 1992.

Reich, L. and D. Sawyer, "Directory/Filename Mapping Requirements and
Objects. NOST/NSSDC," Greenbelt, MD, June 1992.

*DATA DISTRIBUTION FACILITY (DDF)*

Data Distribution Facility Support of the ISTP Program System
Requirements Review Material, Mission Support Systems Branch,
Information Processing Division, May 5, 1989.

Preliminary Design Specification for Data Distribution Facility (DDF)
Support of ISTP Program, Contract NAS5-31500, Computer Sciences Corp.,
CSC/TM-89/6145, November 1989.

Data Distribution Facility Support of the ISTP Program, Preliminary
Design Review Material, Mission Support Systems Branch, Information
Processing Division, December 11, 1989.

Workload Analysis for DDF Support of ISTP, Computer Sciences Corp.,
September 1989.

Media Analysis Report for DDF Support of ISTP, Computer Sciences Corp.,
November 1989.

Preliminary Design Specification (PDR) for DDF Support of ISTP, Computer
Sciences Corp., November 1989.

Operations Concept for Data Distribution Facility (DDF) Support of the
International Solar-Terrestrial Physics (ISTP) Program, Information
Processing Division, January 1990.

System Requirements Specification for DDF Support of the International
Solar Terrestrial Physics (ISTP) Program, Information Processing
Division, January 1990.

Mission Operations and Data Systems Directorate (MO&DSD) Operational
Development Network (MODNET) Configuration Handbook, LORAL AEROSYS/541,
April 1990.

Detailed Design Specification for Data Distribution Facility (DDF)
Support of the ISTP Program (Geotail Prototype), Contract NAS5-31500,
Computer Sciences Corp., CSC/SD- 90/6124, June 1990.

Data Distribution Facility Support of the ISTP Program (Geotail
Prototype) Material, Mission Support System Branch, Information
Processing Division, July 19, 1990.

Detailed Design Specification for DDF Support of ISTP Program (GEOTAIL
Prototype), Computer Sciences Corp., July 1990.

Distribution Media Analysis for ISTP, Information Processing Division,
August 1990.

McCusker, T., "CD-ROM Production Power," Datamation, February 1991.

Phase III DDF Concept Feasibility Report, Computer Technology Assoc.,
August 1991.

Phase III DDF Functional and Performance Requirements, Computer
Technology Assoc., August 1991.

Data Recording Subsystem Reference and Operations Manual, Version 1.1,
IHS, June 1992.

Interface Control Document (ICD) Between the Institute of Space and
Astronautical Science (Japan) and Goddard Space Flight Center (U.S.) for
the Transfer of ISTP/GEOTAIL Data, Computer Sciences Corp., April 1992.

DDF Phase III Operations Concept, Computer Sciences Corp., July 1992.

DDF Phase III System Requirements Document, Computer Technology Assoc.,
July 1992.

Statement of Work and Specification for a Data Recording Subsystem,
Information Processing Division, July 1992.

DDF Phase III System Design Specification, Computer Technology Assoc.,
August 1992..

Data Distribution Facility Phase II CDR Material, Mission Support System
Branch, Information Processing Division, October 15, 1992.

DDF Phase II Detailed Design Specification, Computer Sciences Corp.,
October 1992.

DDF Phase III Preliminary Design Specification, Computer Sciences Corp.,
February 1993.

DDF Phase III Database Design Specification, Computer Sciences Corp.,
February 1993.

*END-TO-END DATA SYSTEM*

ISTP Project Collaborative Solar-terrestrial Research (COSTR)
Initiative: Systems & Operation Requirements Document for Geotail
(SORD), 501-212/Geotail, Draft - March 1990.

Wind Mission Operations Review Material, October 21-22, 1991.

Polar Mission Operations Review Material, March 10-11, 1993.

Mish, W. H., M. Peredo, J. L. Green, and M. G. Reph, "ISTP Science Data
Systems and Products," accepted for publication, 1995.

*INTER-AGENCY CONSULTATIVE GROUP (IACG)*

Toward A New Era of Global Solar-Terrestrial Research - The First IACG
Campaign: Magnetotail Energy Flow and Non-Linear Dynamics, E. C. Whipple
and H. Lancaster, editors, Science Applications International
Corporation (SAIC), October 1992.

Toward A New Era of Global Solar-Terrestrial Research - The Second IACG
Campaign: Boundaries in Collisionless Plasmas, Science Applications
International Corporation (SAIC), October 1993.

*IMP-8*

Mish, W. H., R. P. Lepping, "Magnetic Field Experiment Data Processing
Systems: Explorers 47 and 50," NASA/GSFC X-694-76-158, August 1976.

Whitaker, M. P., Minutes of IMP-8 Meeting, January 7, 1992.

Presentation to the Information Processing Division CCB, "IMP-8
Quicklook Processing in the ISTP-Era," January 16, 1992.

Memorandum of Understanding between the ISTP Projects, the IMP-8 Project
and the Information Processing Division (IPD) for Expedited Quicklook
Processing of Magnetometer and Solar Plasma Telemetry Data, May 5, 1992.

*KEY PARAMETERS (KPS)*

Mish, W. H. (Editor), "ISTP Key Parameter Generation Software (KPGS)
Standards & Conventions," NASA/GSFC, Version 1.3, March 1994.

*LANL S/C*

Mccomas, D. J., R. D. Belian, "Proposal to the National Aeronautics and
Space Administration for Los Alamos Geosynchronous Orbit Data for ISTP
to be Performed by the Los Alamos National Laboratory," Los Alamos, NM,
November 1991.

Briefing Material from ISTP Meeting at Los Alamos, February 25, 1992.

Memorandum of Agreement between the NASA Office of Space Science and
Applications Space Physics Division and the LANL for MPA and SOPA Data
Exchange in Support of the NASA GGS and the ISTP Program, June 1992.

*NSSDC*

Satellite Situation Center: Comprehensive User's Guide, Version 2.1,
December 1993.

Van Steenberg, C., "NDADS Automated Retrieval Mail System Users' Guide,"
NSSDC/WDC-A-R&S, 93-19, May 15, 1993.

Memorandum of Understanding between the ISTP Science Initiative Office
and the Space Science Data Operations Office, April 1993.

*SEL/GOES S/C*

Cruickshank, C. M., editor, "Space Environment Laboratory Data
Acquisition and Display System II," Space Environment Laboratory,
Boulder, Colorado, March 1988.

Memorandum of Agreement Between the National Aeronautics and Space
Administration (NASA) Office of Space Science and Applications Space
Physics Division and the National Oceanic and Atmospheric Administration
(NOAA) Space Environmental Laboratory (SEL) and the National Geophysical
Data Center (NGDC) for Geostationary Operational Environmental Satellite
(GOES) Data Exchange in Support of the NASA Global Geospace Science
(GGS) Program, June 1992.

*SCIENCE PLANNING AND OPERATION FACILITY (SPOF)*

Peredo, M., "Science Planning and Operations Facility (SPOF)," March
1992.

Peredo, M., "Requirements Document for the ISTP WIND/POLAR Science
Planning and Operations Facility (SPOF)," February 1992.

Peredo, M., C. C. Goodrich, D. McNabb, R. Kulkarni, C. Mesztenyi,
"Interactive Tools for ISTP: Science Planning and Data Analysis," SPOF
Movie, Version 1.0, October 1992.

Interface Control Document Between the International Solar-Terrestrial
Physics (ISTP) WIND/POLAR Command Management System (CMS) and the
Science Planning Operations

Facility (SPOF) and the Principal Investigators (PIs), Prepared under
Contract NAS5-31500, Computer Sciences Corp., CSC/TR-90/6126, November
1992.

Peredo, M., C. C. Goodrich, D. McNabb, R. Kulkarni, C. Mesztenyi,
"Interactive Tools for ISTP: Science Planning and Data Analysis," SPOF
Movie, Version 2.0, January 1993.

Peredo, M., C. C. Goodrich, D. McNabb, R. Kulkarni, C. Mesztenyi,
"Interactive Tools for ISTP: Science Planning and Data Analysis," SPOF
Movie, Version 2.1, February 1993.

*SOLAR HELIOSPHERIC OBSERVATORY (SOHO) - (abbreviated list)*

Domingo, V., and T. D. Guyenne, editors, "The SOHO Mission," ESA
SP-1104, 1989.

Solar Oscillations Investigation- Michelson Doppler Imager (SOI-MDI)
Instrument Data Management Plan, Draft V1.4, April 15, 1991.

SOHO Science Operations Plan, Issue 1.1, June 1993.

Poland, A., and V. Domingo, "SOHO Experiment Operations Facility
Functional Requirement Document," Draft Version 1.0, 1993.

Domingo, V., A. Poland, B. Fleck, and T. Appourchaux, "SOHO Science
Operations Plan," Issue 1.1, June 1993.

SOHO Data Archive Requirements, V2.0, January 25, 1994.

*SOLAR WIND INTERPLANETARY MEASUREMENTS (SWIM)*

Whitman, R., "ISTP CDHF Near Real Time Subsystem," Computer Sciences
Corp., February 19, 1991.

Memorandum of Agreement between the DOD Space Test Program (SSD/CLP) and
NASA space Physics Division (NASA) for the Support of Geophysics
Laboratory (GL) Experiment GL-804 (SWIM), April 12, 1991.

SWIM Preliminary and Critical Design Review Material, Computer Sciences
Corp., September 17, 1991 & February 27, 1992.

Whitaker, M. P., Minutes of Design Review for NRT Generation of SWIM
KPGS, May 27, 1992.

*STANDARD FORMATTED DATA UNITS (SFDUs)*

Space Data Systems Operations with SFDU: System and Implementation
Aspects, CCSDS 610.0-G-5, CCSDS Panel 2 Green Book, Issue 5, February
1987.

SFDU - Structure and Construction Rules, CCSDS 620.0-B-1, CCSDS Panel 2
Blue Book, Issue 1, February 1988.

Drexler, M., D. Sawyer and G. Smith, "CCSDS Standard Formatted Data
Units - Standards for Data Understanding," AIAA: Proceedings of the AIAA
Second International Symposium on Space Information Systems,
AIAA-90-5045, 1990.

McGuire, R. E., D. Sawyer, "A Simplified Overview of Standard Formatted
Data Units (SFDUs) and their Proposed Application in the GGS/ISTP
Program."

SFDU - Structure and Construction Rules, CCSDS 620.0-R-1.4, CCSDS Panel
2 Red Book, Issue 1.4 - Draft Recommendation, March 1991. \[This draft,
upon final agency approvals, will become an Issue 2 Blue Book that
incorporates and replaces the February 1988 document\].

Standard Formatted Data Units - A Tutorial, CCSDS 621.0-G-1, Green Book,
May 1992.

Parameter Value Language Specification (CCSD0006), CCSDS 641.0- B-1,
Blue Book, May 1992.

Parameter Value Language - A Tutorial, CCSDS 641.0-G-1, Green Book, May
1992.

.c1. **Appendix J - Acronym List**;

AF - Air Force

ASCII - American Standard Code for Information Exchange -

CA - Control Authority

CAMMICE - Charge & Mass Magnetospheric Ion Composition Experiment (Polar
S/C)

CCB - Configuration Control Board

CCSDS - Consultative Committee for Space Data Systems

CDAWs - Coordinated Data Analysis Workshops run by NSSDC

CDF - Common Data Format - developed by NSSDC

CDHF - Central Data Handling Facility

CDR - Critical Design Review

CD-WO - Compact Disk - Write Once

CEPPAD - Comprehensive Energetic Particle Pitch Angle Distribution
Experiment (Polar S/C)

CMS - Command Management System

CoI - Co-investigator

CANOPUS - Ground Based Investigation of high latitude ionosphere

COSTR - Collaborative Solar Terrestrial Research (initiative)

CPI - Comprehensive Plasma Composition Instrument on Geotail

CPU - Central Processing Unit

CSDS - Cluster Science Data System

DARN - Dual Auroral Radar Network (a GBI)

DCF - Data Capture Facility

DDF - Data Distribution Facility

DEC - Digital Equipment Corp.

DECnet - Networking Protocol developed by DEC

DFCD - Data Formats Control Document

DOE - Department of Energy

DOS - Disk Operating System for IBM or IBM compatible PCs.

DSN - Deep Space Network

EFD - Electric Field Instrument (Geotail S/C)

EFI - Electric Field Instrument (Polar S/C)

EPACT - Energetic Particle: Acceleration, Composition & Transport
Instrument (Wind S/C)

EPIC - Energetic Particles & Ion Composition Instrument (Geotail S/C)

EOF - Experiment Operations Facility for SOHO

EPS - Energetic Particle Sensor (GOES S/C)

ESA - European Space Agency

ESIS - European Space Information System

FDF - Flight Dynamics Facility

GBI - Ground Based Investigations

GCI - Geocentric Celestial Inertial Coordinate System

GSE - Geocentric Solar Ecliptic Coordinate System

GSM - Geocentric Solar Magnetospheric Coordinate System

GGS - Global Geospace Science (Program)

GOES - Geostationary Operational Environmental Satellite

GSFC - Goddard Space Flight Center

HEP - High-Energy Particles Instrument (Geotail S/C)

HSC - DEC Hierarchical Storage Controller

HYDRA - Fast Plasma Analyzer (Polar S/C)

IACG - Inter-Agency Consultative Group

I/O - Input/Output

ICSS - ISTP CDHF Software System

IMP-8 - Interplanetary Monitoring Platform-8 (a series of these were
flown in the 1960's and 70's.)

IMSL - International Mathematical and Statistics Library

IPD - Information Processing Division

ISAS - The Japanese Institute of Space and Astronautical Sciences

ISTP - International Solar-Terrestrial Physics (Program)

JSOC - Joint Science Operations Center

KPs - Key Parameters

KPGS - Key Parameter Generation Software

LACN - Local Area Computer Network

LANL - Los Alamos National Laboratory

LEP - Low-Energy Particles Instrument (Geotail S/C)

MAG - Magnetic Field Instrument

MGF - Magnetic Field Instrument (Geotail S/C)

MIT - Massachusetts Institute of Technology

MF - Major Frame of telemetry

MFE - Magnetic Field Experiment (Polar S/C)

MFI - Magnetic Field Instrument (Wind S/C)

MO&DA - Mission Operations and Data Analysis

MPA - Magnetospheric Plasma Analyzer (LANL S/C)

NAG - Numerical Algorithms Group

NASA - National Aeronautics and Space Administration

Nascom - NASA Communication Network that links DSN to GSFC

NGDC - NOAA National Geophysical Data Center

NOAA - National Oceanic and Atmospheric Administration

NRT - Near Real-Time System used in SWIM

NSI - NASA Science Internet

NSSDC - National Space Science Data Center

PACOR - Packet Processor

PC - Personal Computer (usually an IBM or IBM-compatible running the DOS
or OS/2 operating system)

PDR - Preliminary Design Review

PI - Principal Investigator

PIXIE - Polar Ionospheric X-Ray Imaging Experiment (Polar S/C)

PLA - Plasma Instrument

POCC - Payload Operations and Control Center

PPDB - Prime Parameter Database (Cluster)

PWI - Plasma Wave Instrument

QL - Quicklook - Telemetry that is used to monitor health and safety of
S/C and instruments.

RAL - Rutherford Appleton Laboratory

RDAF - Remote Data Analysis Facility

RE - Earth Radii

Rs - Sun Radii

SDP - Summary Data Plots (Cluster)

SEL - NOAA Space Environment Laboratory

SESAME - Satellite Experiments Simultaneous with Antarctic MEasurements
(a GBI)

SFDU - Standard Formatted Data Units

SIDS - Simulated Instrument Data Set

SIRD - Support Instrumentation Requirements Document

SIRIUS - Scientific Information Retrieval Integrated Utilization System

SOHO - Solar & Heliospheric Observatory

SOPA - Synchronous Orbit Particle Analyzer (LANL S/C)

SORD - Systems & Operations Requirements Document

SPDB - Summary Parameter Data Base (Cluster)

SPOF - ISTP Science Planning and Operations Facility

SRR - Software Requirements Review

SWE - Solar Wind Experiment (Wind S/C)

SWICS/STICS - Solar Wind & Suprathermal Ion Composition Experiment (Wind
S/C)

SWIM - Solar Wind Interplanetary Measurements

TAE - Transportable Applications Executive

TCP/IP - Transmission Control Protocol/Internet Protocol

TGRS - Transient Gamma-Ray Spectrometer (Wind S/C)

TDS - Time Domain Sampler (part of Wind WAVES inst)

TIDE - Thermal Ion Dynamics Experiment (Polar S/C)

TIMAS - Toroidal Imaging Mass-Angle Spectrograph (Wind S/C)

UVI - Ultraviolet Imager (Polar S/C)

VAX/VMS - DEC VAX computer operating system

VIS - Visible Imaging System (Polar S/C)

WAVES - Radio/Plasma Waves Instrument (Wind S/C)

3D-P - 3-D Plasma Analyzer (Wind S/C)

[^1]: Time resolution changes from 46 sec (when the spacecraft is within
    60 RE) to 92 sec (when the radial distance exceeds 60 RE) because of
    the change in bit rate.

[^2]: Information extracted from: "Report of the Data Products Task
    Group for the Cluster Science Data System," Issue 2, Revision 1,
    June 21, 1994.

[^3]: All vector quantities are given in GSE coordinates, except the
    electric field Edusk which is given in the spacecraft spin plane and
    is nearly parallel to the Y-GSE axis.

[^4]: These experiments are collectively referred to as WEC, the Wave
    Experiment Consortium

[^5]: Note that individual KPs for the Interball/Aurora spacecraft are
    computed with contributions from one or more instruments

[^6]: Note that individual KPs for the Interball/Tail spacecraft are
    computed with contributions from one or more instruments. EMFT =
    Electro Magnetic Fields Tail, GPPT = General Plasma Parameters Tail,
    EPTP = Energetic Particles Tail Probe.