# Data Description

1. Product
2. Repository
3. Instrument
4. Observatory
5. Persons

SPASE version 2.2.1

# Display Data Product: Geotail PWI 2 hour dynamic spectrograms

Resource ID
spase://VWO/DisplayData/Geotail/PWI/DS.PT2H
Name
Geotail PWI 2 hour dynamic spectrograms
Alternate name
Description

Geotail PWI SFA and MCA dynamic spectrogram plots with frequency in Hz on the vertical axis and time in UT on the horizontal axis. Each file contains one spectrogram from the electric field antennas and one from the magnetic field search coils. The electric field spectrograms span the frequency range 5.62 to 24 Hz (the Multi-Channel Analyzer - MCA instrument) and 24 Hz to 800 kHz (the Sweep Frequency Analyzer - SFA instrument). The intensity values are color coded and are expressed in units of dBV/m/root-Hz. The magnetic field spectrograms also combine the MCA and SFA instruments and span the frequency range 5.62 Hz to 12.5 kHz. The intensity values are color coded and are expressed in units of dB nT/root-Hz. Each plot spans 2 hours. Information on the instrument and antenna status is also provided above each spectrogram.

Geotail PWI Instrument Page

Geotail PWI Instrument page maintained by the Research Institute for Sustainable Humanosphere at Kyoto University, Japan with descriptions of PWI, PWI 24 hour plots, PWI 2 hour plots and Geotail PWI publications.

Language
en
Acknowledgement

Before using these data in publications or presentations permission must be obtained from the PI of PWI (Hiroshi Matsumoto). Concerning this permission and questions about the GEOTAIL PWI data contact Hiro Kojima

Contact
Role Person
1. Principal investigator Prof. Hiroshi Matsumoto
2. CoInvestigator

General contact
Dr. Hirotsugu Kojima
3. Project scientist Guan Le
Release date
2012-02-24 17:16:35
Association
Prior ID
spase://VWO/DisplayData/Geotail/PWI/Geotail_PWI_DS_2H
Repository
Name
Geotail PWI Data Repository at RISH, Kyoto University, Japan
Availability
Online
Access rights
Open
URL
Directory of Geotail PWI 2 Hour Dynamic Spectrograms

A directory containing Geotail PWI 2 hour dynamic spectrograms

Language
en
Format
GIF
Encoding
None
Acknowledgement

Before using these data in publications or presentations permission must be obtained from the PI of PWI (Hiroshi Matsumoto). Concerning this permission and questions about the GEOTAIL PWI data contact Hiro Kojima

Instrument
Geotail Plasma Wave Investigation (PWI)
Measurement type
Electric field
Magnetic field
Spectrum
Passive waves
Temporal description
Start date
1992-09-18 00:00:00
Relative stop date
30 days ago
2 hours
Observed regions
Earth.Magnetosphere
Earth.NearSurface.AuroralRegion
Earth.NearSurface.Plasmasphere
Earth.NearSurface.PolarCap
Heliosphere.Inner
Keywords
AKR
Chorus
Dynamic Spectrogram
Spectrogram
TKR

## Parameters

### Parameter #1

Name
Pseudo Electric Intensity
Units
db(V/m/root-Hz)
Wave type
Plasma waves
Quantity
ACElectricField
Qualifier
Magnitude
Pseudo
Frequency range
Spectral range
Low frequency
5.62
High frequency
800000
Units
Hz

### Parameter #2

Name
Pseudo Magnetic Intensity
Units
db(nT/root-Hz)
Wave type
Plasma waves
Quantity
ACMagneticField
Qualifier
Magnitude
Pseudo
Frequency range
Spectral range
Low frequency
5.62
High frequency
12500
Units
Hz

SPASE version 2.1.0

# Instrument: Geotail Plasma Wave Investigation (PWI)

Instrument ID
spase://SMWG/Instrument/Geotail/PWI
Name
Geotail Plasma Wave Investigation (PWI)
Alternate name
Geotail PWI
Description

Description taken from

Matsumoto, H., I. Nagano, R. R. Anderson, H. Kojima, K. Hashimoto, M. Tsutsui, T. Okada, I. Kimura, Y. Omura, and M. Okada, Plasma Wave Observations with GEOTAIL Spacecraft, J. Geomag. Geoelectr., 46, 59-95, 1994.

The Geotail spacecraft was launched from Kennedy SPace Center at 14:26 UT on July 24, 1992. The primary scientific objectives of the PWI are to characterize wave-particle interaction processes and instabilities associated with the dynamics in the different regions of the magnetosphere.

The PWI consists of three different sets of receivers: (1) the Sweep Frequency Analyzer(SFA), (2) the Multi-Channel Analyzer (MCA) and (3) the Wave-Form Capture(WFC). The first two sets of receivers are devoted to measuring wave spectra, while the last one is designed to capture wave forms from two electric and three magnetic field components of the measured wave emissions, simultaneously. The frequency ranges of the electric and the magnetic fields which can be measured range from 5.6 Hz to 800 kHz and from 5.6 Hz to 12.5 kHz, respectively. The frequency range of wave forms which can be captured by the WFC is from 10 Hz to 4 kHz.

PWI observation data are available in three types of telemetry formats called Format 1, 2, and 3. Format 1 includes the SFA and MCA data. These data are recorded onboard magnetic data recorder and played back to NASA Deep Space Network. Format 2 is a real time observation mode supported by Usuda Deep Space Center (UDSC) in Japan. It includes all of PWI observation data with the highest resolution. Format 3 is an unusual observation mode. We mainly use this format, when we need to monitor US SIs' data in real time, because Format 2 does not include any US SIs' data. Format 3 includes all of PWI observation data, however, WFC data quanities are coarse relative to those in Format 2.

Sensors

In order to measure the weak electric and magnetic fields from plasma waves in the geomagnetic tail region, PWI uses two kinds of electric sensors and tri-axial search coils, having taken into account both the most suitable condition for field detection and reduction of spacecraft noise. Two sets of long dipole antennas with a length of 100 m tip-to-tip are dedicated to measuring the electric field. They are wire and probe antennas termed WANT' and PANT', respectively.

Two masts of 6 m in length are used for mounting the magnetic field sensors well away from the spacecraft in an attempt to the reduce the spacecraft noise. One of these masts, called MST-F', mounts two sets of the flux-gate magnetometers which are used by the MGF team. They are dedicated primarily to the measurement of the DC magnetic field. Two sets of search coil and their pre-amplifiers which are used by both the PWI and MGF teams to measure wave magnetic fields or magnetic field fluctuations are mounted on the other mast called MST-S'.

The antenna elements of the WANT and PANT are radially deployed from the spacecraft and orthogonal to each other. Their axes, U and V, deviate by 15 degrees clockwise from the spacecraft X and Y coordinate directions, respectively. The assembly of PWI tri-axial search coils (which is hereafter called PWI-SC) and their pre-amplifiers is mounted on the top of the MST-S. The tri-axial search coils associated with the MGF (MGF-SC) are mounted on the same mast but 2 m inside of the PWI-SC. The PWI-SC is normally connected to the PWI measurement system. However, we can select the MGF-SC by a telemetry command if necessary. The direction of the MST-S (and MST--F) deviates by 45° clockwise from the spacecraft Y (and -Y) axis. The three axes of the PWI search coils are defined in a cylindrical coordinate system as follows: \alpha is in the tangential direction, \beta measures in the radial direction, and \gamma is parallel to the spin Z axis of the spacecraft.

Sweep Frequency Analyzer (SFA)

The SFA provides spectral information on plasma wave amplitudes over the frequency range from 24 Hz to 800 kHz for the electric field and 24 Hz to 12.5 kHz for the magnetic field. The SFA consists of eight independent receivers covering 5 frequency bands for the electric fields and three frequency bands for the magnetic fields. The receiver specifications are listed in Table 1.

Table 1. Specification of SFA

Band Frequency Range Freq. Step Bandwidth Source Sweep
1 24 Hz - 200 Hz 1.3 Hz 2.6 Hz B and E 64sec
2 200 Hz - 1600Hz 10.7 Hz 10 Hz B and E 64sec
3 1.6 kHz - 12.5 kHz 85.4 Hz 85 Hz B and E 8 sec
4 12.5 kHz - 100 kHz 683 Hz 680 Hz E only 8 sec
5 100 kHz - 800 kHz 5.47kHz 5.4 kHz E only 8 sec

Each receiver has a very good frequency resolution of 1/128 of the receiver frequency band although their time resolution (64 sec for Bands 1 and 2, and 8 sec for Bands 3 - 5) is somewhat coarse.

The SFA measures one wave electric field component of either the E_U or E_V component and one wave magnetic field component of either the B_\alpha or B_\gamma component. The selection of which field component is measured is carried out by a telemetry command. Each receiver has an effective dynamic range of ~90 dB. The electric field receivers are placed in the High gain mode by stepping up the level in the Low gain mode by 30 dB.

The SFA has another mode of operation which can be used. Despite its operation as the SFA, we can also fix the measured frequency to one preset value in each frequency band. This mode provides very high time resolution for the observed signals at an arbitrarily selected frequency. The time resolutions in this mode are 0.5 sec for Bands 1 and 2, and 62.5 msec for Bands 3, 4, and 5, respectively. This mode change is also carried out by a telemetry command.

Multi Channel Analyzer (MCA)

This subsystem is provided by the University of Iowa. The MCA contains two spectrum analyzers with fixed frequency channel filters. It provides high time resolution data to complement the coarser time resolution data of the SFA. However, their frequency resolution is coarse because they have only four frequency channels per decade in frequency.

The input signal to the MCA is provided from the output of the common front-end circuit of the PWI system as well as to SFA and WFC receivers. One multi-channel spectrum analyzer is used to measure the electric field and is composed of 20 channels covering the frequency range from 5.62 Hz to 311 kHz. The other spectrum analyzer is used for magnetic field measurements and has 14 channels covering the frequency range from 5.62 Hz to 10 kHz. The bandwidths of the filters are +/- 15% of the channel center frequency in the frequency range below 10 kHz and +/- 7.5% of the center frequency for frequency above 10 kHz. The MCA instrument measures the wave electric field of either the E_U or E_V component (depending on which antenna is used) with a dynamic range of ~110 dB and the wave magnetic field of either the B_\alpha or B_\gamma component with a dynamic range of ~100 dB.

Signals from all channels are sampled simultaneously so that the ratio of the electric to magnetic field strength may be calculated accurately. The signals are sampled once (data acquisition time is 1.037 msec) every 250 msec in Format 2 (and every 500 msec in Format 1). Each channel of the spectrum analyzer has a suitable integration time in the linear detection of signal ranging from 500 msec in the lower frequency channels and decreasing to a few milliseconds for those channel above 3 kHz.

Wave-Form Capture (WFC)

The WFC data are used for the detailed analysis of the wave characteristics, such as determination of the wave vector, polarization, Poynting flux, and antenna sheath impedance. The system has five (two electric and three magnetic) receivers each connected to a sensor through each front end circuit. The WFC has two different operation modes: Memory mode and Direct mode.

In the Memory mode, wave signals are measured simultaneously as E_U, E_V , B_\alpha, B_\beta, and B_\gamma. These are fed to a gain-controller followed by an anti-aliasing filter (LPF) with an upper frequency cutoff of 4 kHz, then through high pass filters (HPF) which have a low frequency cutoff of 10 Hz. An alternate HPF with a low frequency cutoff of 100 Hz can be used with the electric field measurements. Wave forms of the analog signal are sampled then converted into 12 bit data by an A/D converter with a frequency of 12 kHz. The 12 bit digital data are compressed into 8 bit by a quasi-logarithmic compression method. The compressed 8 bit data are then stored into onboard memory with a storage of 512 kBytes for a period of 8.7sec. The stored wave form data are read out of memory and telemetered to the ground using the PCM telemetry during a uninterrupted period of 275 seconds in telemetry Format 2 and 375 seconds in telemetry Format 3. The start timing for initiating wave form capture is controlled by either free running timing pulse (INTER. mode) or when the instrument receives one of eight different sources for triggering signals. The instrument is triggered when one of the following measurements exceeds a preset level:

1. The intensity of Z axis component of the DC magnetic field as measured by the outboard fluxgate magnetometer of the MGF. 2. The amplitude of the plasma turbulence detected by a single probe of the EFD. 3. The magnitude of ion and/or electron moments as measured by the electrostatic analyzers of the LEP-EA. 4. The amplitude of the electric field measured on the 100 kHz channel of the MCA. 5. The amplitude of the electric field measured on the 316 Hz channel of the MCA. 6. The amplitude of the magnetic field measured on the 10 Hz channel of the MCA. 7. The integral amplitude of the electric field over the entire frequency range of Band 1 (frequencies less than 250 Hz) of the SFA. 8. The integral amplitude of the magnetic field over the entire frequency range of both Bands 1 and 2 (frequency less than 1.875 kHz) of the SFA.

The selection among the possible eight triggering sources and its preset level or amplitude is made via telemetry commands. When the WFC instrument is operated in the Memory mode the following three modes of operation are available for storing and reading the data:

1. AFT: Storage of 512 kByte of data after instrument triggering. 2. MID: Storage of two successive 256 kByte sequences of data, one before and the other after instrument triggering. 3. BEF: Storage of 512 kByte of data before instrument triggering.

In the last two modes, a continuous sequence of signal sampling and storage into the memory is repeated until a triggering signal is detected by the instrument.

A common problem of noise interference in the plasma wave instruments on spinning occurs as each group of solar cell circuits cycles on/off when the solar cell surface of the group faces to the sun-lit side then to the shadow side of the spacecraft. This repetition of the circuit from on to off to on again causes radiation of electromagnetic noises. To mitigate this problem, a high pass filter (HPF) with a cutoff frequency of 10 Hz is inserted in the receivers in order to suppress the detection of low frequency noise from the solar cell circuits. For the electric field receivers, we prepared an option for changing the HPF cutoff frequency from 10 Hz to 100 Hz in case the noise extended to higher frequencies then expected. The selection of the lower frequency cutoff is based upon the observed in situ noise level. These noise suppression measures limit frequency range of the observed wave forms to a band from 10 Hz (or 100 Hz) to 4 kHz.

Besides the Memory Mode, the WFC can be operated in a Direct mode, with two possible variations: one is the Single channel mode in which only one field component is measured continuously and telemetered to ground on a real-time basis. In this operation mode the instrument can measure continuous wave forms of one electric or one magnetic component with an upper limit in frequency of 640 kHz in telemetry Format 2 (or 470 Hz in telemetry Format 3). The other method of instrument operation is in the Dual channel mode where two field components are measured and telemetered alternately. In this mode the upper limit in frequency is 320 Hz in telemetry Format 2 (or 235 Hz in telemetry Format 3) for each component. For both of these mode, the data sampling frequency is three times the upper limit in frequency.

The WFC system can measure the wave amplitude with a dynamic range of 66 dB. The receiver gain keeping its dynamic range can be stepped up in the gain controller "H/L" by 40 dB and 20 dB in electric and magnetic channels to amplify the weak signal, respectively.

GEOTAIL Plasma Wave Instrument

Information about the Plasma Wave Investigation (PWI) experiment on the Geotail mission.

NSSDC's Master Catalog

Information about the Plasma Wave Investigation (PWI) experiment on the Geotail mission.

Acknowledgement
Contact
Role Person
1. Principal investigator Prof. Hiroshi Matsumoto
2. CoInvestigator

General contact
Dr. Hirotsugu Kojima
3. Project scientist Guan Le
4. CoInvestigator Dr. Stanley D. Shawhan
5. CoInvestigator Mr. Minoru Tsutsui
6. CoInvestigator Mr. Joseph K. Alexander, Jr.
7. CoInvestigator Dr. Robert G. Stone
8. CoInvestigator Dr. Edward J. Smith
9. CoInvestigator Prof. Robert A. Helliwell
10. CoInvestigator Dr. Michael C. Kelley
11. CoInvestigator Dr. Iwane Kimura
12. CoInvestigator Dr. Paul J. Kellogg
14. CoInvestigator Dr. Roger R. Anderson
15. CoInvestigator Dr. Paul M. Kintner
16. CoInvestigator Dr. Paul Rodriguez
17. CoInvestigator Dr. Isamu Nagano
18. CoInvestigator Dr. William W. L. Taylor
19. CoInvestigator Dr. William S. Kurth
20. CoInvestigator Mr. Kozo Hashimoto
21. CoInvestigator Dr. Yoshiharu Omura
22. CoInvestigator Dr. Hirotsugu Kojima
23. FormerPI Dr. Frederick L. Scarf
Release date
2012-03-07 11:50:38
Instrument type
Antenna
Long Wire
Search Coil
Investigation name
Plasma Wave Investigation (PWI) on Geotail
Observatory
Geotail

SPASE version 2.2.0

# Observatory: Geotail

Observatory ID
spase://SMWG/Observatory/Geotail
Name
Geotail
Alternate name
1992-044A
GTL
ISTP/Geotail
GGS/Geotail
Geomagnetic Tail Lab
Description

The solar wind draws the Earth's magnetic field into a long tail on the nightside of the Earth and stores energy in the stretched field lines of the magnetotail. During active periods, the tail couples with the near-Earth magnetosphere, sometimes releasing energy stored in the tail and activating auroras in the polar ionosphere. The Geotail mission measures global energy flow and transformation in the magnetotail to increase understanding of fundamental magnetospheric processes. This includes the physics of the magnetopause magnetospheric boundary regions, the lobe and plasma sheet, and reconnection and neutral line formation, i.e., the mechanisms processes of input, transport, storage, release and conversion of mass, momentum and energy in the magnetotail. Geotail, together with Wind, Polar, SOHO, and Cluster projects, constitute a cooperative scientific satellite project designated the International Solar Terrestrial Physics (ISTP) program which aims at gaining improved understanding of the physics of solar-terrestrial relations. Geotail is a spin-stabilized spacecraft utilizing mechanically despun antennas with a design lifetime of about four years. The nominal spin rate of the spacecraft is about 20 rpm around a spin axis maintained between 85-89 degrees to the ecliptic plane. Geotail is cylindrical, approximately 2.2 m in diameter, and 1.6 m high. with It has body-mounted solar cells. Geotail also has and a back-up battery subsystem which that operates when the spacecraft is in the Earth's shadow (limited to 2 hrs). Real-time telemetry data transmitted in X-band are received at the Usuda Deep Space Center (UDSC) in Japan. There are two tape recorders on board, each with a capacity of 450 Mb, which allows daily 24-hour data coverage and are collected in playback mode by the NASA Deep Space Network (DSN). The Geotail mission is divided into two phases. During the two-year initial phase, the orbit apogee was kept on the nightside of the Earth by using the Moon's gravity in a series of double-lunar swing-by maneuvers that result in the spacecraft spending most of its time in the distant magnetotail (maximum apogee about 200 Earth radii) with a period varying from one to four months. Then, in November 1994, there were a series of maneuvers that reduced the apogee to 50 Re. After three more months in the magnetotail the spacecraft was put in a 10 by 30 Re orbit where it has remained except that the perigee was reduced from 10 to 9 Re in June 1997. Details on the Geotail mission and instrumentation are given in the Journal of Geomagnetism and Geoelectricity (Vol. 46, No. 1, 1994); online from JGG at http://www.terrapub.co.jp/journals/EPS/JGG

NSSDC's Master Catalog

Contact
Role Person
1. Project scientist Guan Le
2. Project scientist Prof. Masaki Fujimoto
Release date
2010-08-05 18:19:18
Location
Region
Earth.Magnetosphere
Heliosphere.NearEarth

SPASE version 2.2.0

# Person: Prof. Hiroshi Matsumoto

Name
Prof. Hiroshi Matsumoto
Organization
Kyoto University
Person ID
spase://SMWG/Person/Hiroshi.Matsumoto

SPASE version 2.2.0

# Person: Dr. Hirotsugu Kojima

Name
Dr. Hirotsugu Kojima
Organization
Kyoto University
Email
kojima@rish.kyoto-u.ac.jp
Person ID
spase://SMWG/Person/Hirotsugu.Kojima

SPASE version 2.2.0

# Person: Guan Le

Name
Guan Le
Organization
NASA Goddard Space Flight Center
Code 674, Greenbelt, MD 20771, USA
Email
guan.le@nasa.gov
Phone
+1 301 286 1087
Person ID
spase://SMWG/Person/Guan.Le
Release date
2010-08-05 17:35:46

SPASE version 2.2.0

# Person: UNKNOWN

Name
UNKNOWN
Organization
UNKNOWN
Person ID
spase://SMWG/Person/UNKNOWN
Release date
2010-08-05 17:35:47

SPASE version 2.2.0

# Person: Dr. Leonard N. Garcia

Name
Dr. Leonard N. Garcia
Organization
NASA Goddard Space Flight Center
Code 605, Greenbelt, MD 20771, USA
Email
Leonard.N.Garcia@nasa.gov
Person ID
spase://SMWG/Person/Leonard.N.Garcia
Release date
2010-08-05 17:35:47

SPASE version 2.2.0

# Person: Dr. Stanley D. Shawhan

Name
Dr. Stanley D. Shawhan
Organization
Deceased - formerly at NASA Headquarters
Person ID
spase://SMWG/Person/Stanley.D.Shawhan
Release date
2010-10-01 18:53:39

SPASE version 2.2.0

# Person: Mr. Minoru Tsutsui

Name
Mr. Minoru Tsutsui
Organization
Kyoto Sangyo University
Person ID
spase://SMWG/Person/Minoru.Tsutsui

SPASE version 2.2.0

# Person: Mr. Joseph K. Alexander, Jr.

Name
Mr. Joseph K. Alexander, Jr.
Organization
GSFC-Code 600
Person ID
spase://SMWG/Person/Joseph.K.Alexander.Jr

SPASE version 2.2.0

# Person: Dr. Robert G. Stone

Name
Dr. Robert G. Stone
Organization
GSFC-Code 690
Person ID
spase://SMWG/Person/Robert.G.Stone

SPASE version 2.2.0

# Person: Dr. Edward J. Smith

Name
Dr. Edward J. Smith
Organization
Jet Propulsion Laboratory
Email
edward.j.smith@jpl.nasa.gov
Phone
+1 818 354 2248
Person ID
spase://SMWG/Person/Edward.J.Smith
Release date
2010-08-05 17:35:46

SPASE version 2.2.0

# Person: Prof. Robert A. Helliwell

Name
Prof. Robert A. Helliwell
Organization
Stanford University
Person ID
spase://SMWG/Person/Robert.A.Helliwell

SPASE version 2.2.0

# Person: Dr. Michael C. Kelley

Name
Dr. Michael C. Kelley
Organization
Cornell University
School of Electrical Engineering Cornell University 318 Rhodes Hall Ithaca NY 14853
Email
mikek@ee.cornell.edu
Phone
+1-607-254-5331
Person ID
spase://SMWG/Person/Michael.C.Kelley
Release date
2010-08-05 17:35:47

SPASE version 2.2.0

# Person: Dr. Iwane Kimura

Name
Dr. Iwane Kimura
Organization
Kyoto University
Person ID
spase://SMWG/Person/Iwane.Kimura

SPASE version 2.2.0

# Person: Dr. Paul J. Kellogg

Name
Dr. Paul J. Kellogg
Organization
University of Minnesota
Person ID
spase://SMWG/Person/Paul.J.Kellogg

SPASE version 2.2.0

Name
Organization
Toyama Prefectural University
Person ID

SPASE version 2.2.0

# Person: Dr. Roger R. Anderson

Name
Dr. Roger R. Anderson
Organization
University of Iowa
Person ID
spase://SMWG/Person/Roger.R.Anderson

SPASE version 2.2.0

# Person: Dr. Paul M. Kintner

Name
Dr. Paul M. Kintner
Organization
Cornell University
Person ID
spase://SMWG/Person/Paul.M.Kintner

SPASE version 2.2.0

# Person: Dr. Paul Rodriguez

Name
Dr. Paul Rodriguez
Organization
US Naval Research Laboratory
Person ID
spase://SMWG/Person/Paul.Rodriguez

SPASE version 2.2.0

# Person: Dr. Isamu Nagano

Name
Dr. Isamu Nagano
Organization
Kanazawa University
Person ID
spase://SMWG/Person/Isamu.Nagano

SPASE version 2.2.0

# Person: Dr. William W. L. Taylor

Name
Dr. William W. L. Taylor
Organization
GSFC-Code 612.4
Person ID
spase://SMWG/Person/William.W.L.Taylor

SPASE version 2.2.0

# Person: Dr. William S. Kurth

Name
Dr. William S. Kurth
Organization
University of Iowa
Person ID
spase://SMWG/Person/William.S.Kurth

SPASE version 2.2.0

# Person: Mr. Kozo Hashimoto

Name
Mr. Kozo Hashimoto
Organization
Kyoto University
Person ID
spase://SMWG/Person/Kozo.Hashimoto

SPASE version 2.2.0

# Person: Dr. Yoshiharu Omura

Name
Dr. Yoshiharu Omura
Organization
Kyoto University
Person ID
spase://SMWG/Person/Yoshiharu.Omura

SPASE version 2.2.0

# Person: Dr. Frederick L. Scarf

Name
Dr. Frederick L. Scarf
Organization
Deceased - formerly at TRW, CA
Person ID
spase://SMWG/Person/Frederick.L.Scarf
Release date
2010-10-01 18:53:39

SPASE version 2.2.0

# Person: Prof. Masaki Fujimoto

Name
Prof. Masaki Fujimoto
Organization
Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency
3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
Email
fujimoto@stp.isas.jaxa.jp
Fax number
+81 42 759 8456
Person ID
spase://SMWG/Person/Masaki.Fujimoto
Release date
2010-08-05 17:35:47

SPASE version 2.2.0

# Person: Jan Merka

Name
Jan Merka
Organization
NASA Goddard Space Flight Center
Code 672, Greenbelt, MD 20771, USA
Email
jan.merka@nasa.gov
Phone
+1 301 286 8751
Person ID
spase://SMWG/Person/Jan.Merka
Release date
2010-08-05 17:35:46

SPASE version 2.1.0

# Repository: Geotail PWI Data Repository at RISH, Kyoto University, Japan

Repository ID
spase://SMWG/Repository/RISH
Name
Geotail PWI Data Repository at RISH, Kyoto University, Japan
Alternate name
Geotail PWI Data Repository at Radio Atmospheric Science Center, Kyoto University, Japan
Description

Geotail PWI data repository at the Research Institute for Sustainable Humanosphere, Kyoto University, Japan

Contact
Role Person
1. General contact UNKNOWN
2. Metadata contact Dr. Leonard N. Garcia
Release date
2010-07-29 19:28:50
Access URL
GEOTAIL Plasma Wave Instrument

Geotail PWI repository for 24 Hour and 2 Hour Dynamic Spectrograms plus instrument descriptions and publication lists