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1) IMAGE EUV Key Parameters: Ion Images maxmize
Resource ID:spase://VSPO/DisplayData/IMAGE/EUV/PT600S
Start:2000-03-28 00:00:00 Observatory:IMAGE Cadence:
Stop:2005-12-18 00:00:00 Instrument:Extreme Ultraviolet Imager (EUV) Resource:DisplayData
IMAGE EUV Key Parameters, Ion Images, 10-min resolution

2) IMAGE FUV Substorm Onset Catalog maxmize
Resource ID:spase://VSPO/Catalog/IMAGE/FUV/CATALOG
Start:2000-05-16 00:00:00 Observatory:IMAGE Cadence:
Stop: Instrument:Far Ultraviolet Imager (FUV) Resource:Catalog
This is a table of times of substorm onsets observed by IMAGE/FUV. The raw instrument counts in the FUV image with the greatest number of counts at time of onset, the X and Y pixel numbers for this greatest-count pixel, the onset geographic and geomagnetic latitude and longitude angles and local time, and the geocentric distance of IMAGE are also given for each onset.

3) IMAGE FUV SI plots of O/N2 Ratios maxmize
Resource ID:spase://VEPO/DisplayData/IMAGE/FUV/SI/O_N2_Ratios
Start:2000-05-24 00:00:00 Observatory:IMAGE Cadence:2 minutes
Stop:2005-05-18 23:59:59 Instrument:Far Ultraviolet Imager (FUV) Resource:DisplayData
This data set consists of images of thermospheric O/N2 column density ratios at 2-min resolution during times of strong geomagnetic storms (Dst.LT.-80nT) of 2000-2005. The ratios are generated from dayside airglow observations of the IMAGE Far Ultraviolet (FUV) Spectrographic Imager (SI). The SI has a peak response at the OI 135.6 nm oxygen emission line and a bandpass of 131.0 to 140.0 nm which includes the LBH band from N2 molecules. For each O/N2 plot, there is a plot of the SI image from which the O/N2 plot was generated, and there is an IDL saveset of the content of the O/N2 maps. The Information URL of this descriptor identifies detailed discussions of the derivations of O/N2 rations from the SI images.

4) IMAGE FUV SI plots of O/N2 Ratios maxmize
Resource ID:spase://VSPO/DisplayData/IMAGE/FUV/SI/O_N2_Ratios
Start:2000-05-24 00:00:00 Observatory:IMAGE Cadence:2 minutes
Stop:2005-05-18 23:59:59 Instrument:Far Ultraviolet Imager (FUV) Resource:DisplayData
This data set consists of images of thermospheric O/N2 column density ratios at 2-min resolution during times of strong geomagnetic storms (Dst.LT.-80nT) of 2000-2005. The ratios are generated from dayside airglow observations of the IMAGE Far Ultraviolet (FUV) Spectrographic Imager (SI). The SI has a peak response at the OI 135.6 nm oxygen emission line and a bandpass of 131.0 to 140.0 nm which includes the LBH band from N2 molecules. For each O/N2 plot, there is a plot of the SI image from which the O/N2 plot was generated, and there is an IDL saveset of the content of the O/N2 maps. The Information URL of this descriptor identifies detailed discussions of the derivations of O/N2 rations from the SI images.

5) IMAGE FUV SIE Auroral Images, Key Parameters maxmize
Resource ID:spase://VSPO/DisplayData/IMAGE/FUV/SIE/PT124S
Start:2000-04-25 00:00:00 Observatory:IMAGE Cadence:
Stop:2005-12-18 00:00:00 Instrument:Far Ultraviolet Imager (FUV) Resource:DisplayData
Electron Auroral Images at 1356A, Key Parameters, IMAGE Far UltraViolet (FUV) Spectrographic Imaging camera Electrons (SIE)

6) IMAGE FUV SIP Auroral Images, Key Parameters maxmize
Resource ID:spase://VSPO/DisplayData/IMAGE/FUV/SIP/PT124S
Start:2000-04-25 00:00:00 Observatory:IMAGE Cadence:
Stop:2005-12-18 00:00:00 Instrument:Far Ultraviolet Imager (FUV) Resource:DisplayData
Proton Auroral Images at 1218A, Key Parameters, IMAGE Far UltraViolet (FUV) Spectrographic Imaging camera Protons (SIP)

7) IMAGE FUV WIC Auroral Images, Key Parameters maxmize
Resource ID:spase://VSPO/DisplayData/IMAGE/FUV/WIC/PT124S
Start:2000-04-25 00:00:00 Observatory:IMAGE Cadence:
Stop:2016-09-14 07:59:48 Instrument:Far Ultraviolet Imager (FUV) Resource:DisplayData
Auroral Images, Key Parameters, IMAGE Far UltraViolet (FUV) Wide-band Imaging Camera (WIC)

8) IMAGE FUV/WIC Auroral Images maxmize
Resource ID:spase://VSPO/DisplayData/IMAGE/FUV/WIC/PT6M
Start:2000-05-19 00:00:00 Observatory:IMAGE Cadence:6 minutes
Stop:2000-12-18 00:00:00 Instrument:Far Ultraviolet Imager (FUV) Resource:DisplayData
Auroral Images in GIF format from the Wideband Imaging Camera (WIC) of the Far Ultraviolet (FUV) experiment on IMAGE, at UCB

9) IMAGE HENA Images, Key Parameters maxmize
Resource ID:spase://VSPO/DisplayData/IMAGE/HENA/124S
Start:2000-04-21 00:00:00 Observatory:IMAGE Cadence:
Stop:2005-12-18 00:00:00 Instrument:High-Energy Neutral Atom Imager (HENA) Resource:DisplayData
IMAGE High Energy Neutral Atom (HENA) images for several energy channels <10 to 60 keV, key parameters,

10) IMAGE Housekeeping Data via CDAWeb maxmize
Resource ID:spase://VSPO/NumericalData/IMAGE/HK/CDAWeb/PT24H
Start:2000-03-25 00:00:00 Observatory:IMAGE Cadence:24 hours
Stop:2005-12-18 07:38:17 Instrument:IMAGE HK - Housekeeping Resource:NumericalData
This set of housekeeping data from the IMAGE mission comes from the Central Interface Data Processor (CIDP) and the interface with the Spacecraft/System Control Unit (SCU). The CIDP provides the following major functions for the Observatory: (1) Instrument data acquisition, processing, and compression. (2) Stored command processing. (3) Command receipt (from the SCU), processing, storage (if a delayed command), and transfer to the instruments. (4) Time/attitude synchronization with the spacecraftÕs Attitude Determination and Control system for generation of the nadir and sun pulse signals sent to the instruments. (5) Deckplate thermal control. (6) Additional EEPROM storage for instrument software or tables. (7) Power switching and current limiting. The SCU provides the following major functions for the Observatory: (1) Ground command receipt, processing, storage (for delayed command execution) and relay to the CIDP. (2) Telemetry data formatting and downlink (3) Spacecraft attitude determination and control. (4) Spacecraft thermal control. (5) Spacecraft power management. (6) Spacecraft housekeeping data acquisition, formatting, and storage. (7) Management of the Mass Memory Module. (8) Management of the engineering and high speed telemetry downlink. (9) Safe/hold management of the Observatory. Products include: IM_HK_ADS: Image Attitude Determination System Housekeeping IM_HK_AST: Image Autonomous Star Tracker Housekeeping IM_HK_COM: Image Communication Systems Housekeeping IM_HK_FSW: Image Flight Software Housekeeping IM_HK_PWR: Image Power Systems Housekeeping IM_HK_TML: Image Thermal Housekeeping

11) IMAGE housekeeping data in UDF, all instruments maxmize
Resource ID:spase://VSPO/NumericalData/IMAGE/HK/UDF/Data
Start:2000-05-01 00:00:00 Observatory:IMAGE Cadence:
Stop:2005-12-18 23:59:59 Instrument:Low-Energy Neutral Atom Imager (LENA) Resource:NumericalData
This is a set of data at multiple processing levels from all IMAGE instruments. Built by a UNIX-afficionado requiring editing .cshrc's, etc., the data are in Universal Data Format (UDF), and at the moment, has no PC install documentation. UDF software is available to read the IMAGE UDF files.

12) IMAGE LENA Low Images, Key Parameters maxmize
Resource ID:spase://VSPO/DisplayData/IMAGE/LENA/PT124S
Start:2000-05-24 00:00:00 Observatory:IMAGE Cadence:
Stop:2005-12-18 23:59:59 Instrument:Low-Energy Neutral Atom Imager (LENA) Resource:DisplayData
This set of images from IMAGE Low-Energy Neutral Atom (LENA) contains key parameters for several energy channels from 20 to 200 keV.

13) IMAGE MENA Images, Key Parameters maxmize
Resource ID:spase://VSPO/DisplayData/IMAGE/MENA/PT124S
Start:2000-04-04 00:00:00 Observatory:IMAGE Cadence:
Stop:2005-12-18 23:59:59 Instrument:Medium-Energy Neutral Atom Imager (MENA) Resource:DisplayData
This set of images and movies from IMAGE Medium-Energy Neutral Atom (MENA) contains key parameters for several energy channels from 1 to 70 keV.

14) IMAGE Definitive Orbit Data maxmize
Resource ID:spase://VSPO/NumericalData/IMAGE/Orbit/Definitive/PT120S
Start:2000-03-27 00:00:00 Observatory:IMAGE Cadence:120 seconds
Stop:2004-06-21 00:00:00 Instrument:IMAGE Positions Resource:NumericalData
IMAGE Definitive Orbit Data, GSE and GSM Coordinates

15) IMAGE RPI Daily Dynamic Spectrogram Plot maxmize
Resource ID:spase://VWO/DisplayData/IMAGE/RPI/DS.P1D
Start:2000-04-21 20:24:42 Observatory:IMAGE Cadence:5 minutes
Stop:2005-12-18 07:50:00 Instrument:Radio Plasma Imager (RPI) Resource:DisplayData
Collection of RPI Daily Dynamic Spectrogram plots at NASA GSFC, covering complete mission period from 2000-04-21 to 2005-12-18. Dynamic Spectrograms present the time history of natural radio emissions in space between 3 and 1009 kHz while the IMAGE spacecraft orbits the Earth. This operating frequency range was selected by the RPI team to provide an optimal temporal resolution to the wave observations. Each image is a daily plot of the voltage spectral density of received signal (color scale) as function of operating frequency (vertical axis) and time (horizontal axis). Commonly used in the analysis of noise generators, spectral density is a frequency-dependent characteristic that describes how much power is generated by the emission source in a 1 Hz bandwidth. RPI Dynamic Spectograms plot a Voltage Spectral Density, which is root of power spectral density, measured in [V/root-Hz] units. Note that conversion of antenna voltage to electric field strength depends on effective length of receive antennas, and such conversion is not performed here. RPI is capable of detecting input radio emissions above its noise floor of 5 nV/root-Hz, which is determined by the internal white noise of the RPI antenna pre-amplifiers.

16) RPI Dynamic Spectrogram data in CDF at NASA CDAWeb maxmize
Resource ID:spase://VWO/NumericalData/IMAGE/RPI/DS.PT5M
Start:2000-04-21 20:24:42 Observatory:IMAGE Cadence:5 minutes
Stop:2005-12-18 07:50:00 Instrument:Radio Plasma Imager (RPI) Resource:NumericalData
RPI passive wave measurement capturing voltage spectral density of the radio emissions in space as a function of frequency, typically between 3 and 1009 kHz. This operating frequency range was selected by the RPI team to provide optimal temporal resolution of the wave observations. Commonly used in the analysis of noise generators, spectral density is a frequency-dependent characteristic that describes how much power is generated by the emission source in a 1 Hz bandwidth. The original description of emissions was done in terms of thermal noise measurements, though the same approach also applies to non-thermal emissions such as AKR. CDF_DS_PT5M stores calibrated data from all three RPI antennas X, Y, and Z individually and a combined X+Y antenna channel. The data are presented as the Voltage Spectral Density (VSD), which is the root of power spectral density, measured in [V/root-Hz] units. Note that conversion of antenna voltage to electric field strength depends on the effective length of the receive antenna, and such conversion is not performed here. (See spase://SMWG/Instrument/IMAGE/RPI for a time history of the lengths of the three mutually orthogonal RPI dipole antennas.) RPI is capable of detecting input radio emissions above its noise floor of 5 nV/root-Hz, which is determined by the internal white noise of the RPI antenna pre-amplifiers. The VSD in RPI spectrogram data is presented in dB relative to 1 V/root-Hz (logarithmic scale), units of dB(V/root-Hz). The RPI instrument noise floor is 5 nV/root-Hz = -166 dB(V/root-Hz) at the receiver input. Software suggested by the science team for CDF file visualization: (1) Plotting tool at the CDAWeb portal, (2) For analysis beyond static image inspection, including color scale optimization, zooming, text export, alternative data representations in physical units, detailed frequency and time information, overlaid model fpe and fce graphs, and EPS quality figures, use BinBrowser software at UML, http://ulcar.uml.edu/rpi.html

17) RPI Plasmagram Full Resolution Binary Data maxmize
Resource ID:spase://VWO/NumericalData/IMAGE/RPI/PGM.CCSDS.PT5M
Start:2000-04-21 20:24:42 Observatory:IMAGE Cadence:5 minutes
Stop:2005-12-11 02:43:10 Instrument:Radio Plasma Imager (RPI) Resource:NumericalData
RPI plasmagram full resolution data (received signal strength in the frequency-range frame), uncalibrated. Presented as instrument packets wrapped in the standard CCSDS headers. Description of the RPI instrument-level data model can be found at http://ulcar.uml.edu/RPI/RPITelemetryDataFormat_V2.8.pdf. Data are viewed/calibrated/edited by BinBrowser software, see http://ulcar.uml.edu/rpi.html for download and users' guide. RPI plasmagrams are visualized by plotting images in which received signal strength (color scale) is a function of echo delay (range in vertical scale) and radio-sounder frequency (horizontal scale) of the radar pulses. Echoes from important magnetospheric structures, such as the magnetopause and the plasmapause, appear as traces on plasmagrams. Plasmagram traces are intermixed with vertical signatures corresponding to the locally excited plasma resonances and various natural emissions propagating in space.

18) RPI Plasmagram data in CDF at NASA CDAWeb maxmize
Resource ID:spase://VWO/NumericalData/IMAGE/RPI/PGM.CDF.PT5M
Start:2000-03-26 07:51:50 Observatory:IMAGE Cadence:5 minutes
Stop:2005-12-18 07:40:47 Instrument:Radio Plasma Imager (RPI) Resource:NumericalData
Software suggested by the science team for CDF file visualization: (1) Plotting tool at the CDAWeb portal, (2) For analysis beyond static image inspection, including color scale optimization, zooming, text export, alternative data representations in physical units, detailed frequency and time information, overlaid model fpe and fce graphs, and EPS quality figures, use BinBrowser software at UML, http://ulcar.uml.edu/rpi.html

19) IMAGE RPI Plasmagram Plots maxmize
Resource ID:spase://VWO/DisplayData/IMAGE/RPI/PGM.PT5M
Start:2000-04-21 20:24:42 Observatory:IMAGE Cadence:5 minutes
Stop:2005-12-18 07:50:00 Instrument:Radio Plasma Imager (RPI) Resource:DisplayData
Collection of RPI Plasmagram images at University of Massachusetts Lowell, covering complete mission period from 2000-04-21 to 2005-12-18. Access to images is arranged via a webpage containing a query form with the time period of interest and options for search of expert-annotated plasmagrams. The query returns a list of qualifying plasmagrams with URLs pointing to images. RPI plasmagrams are visualized by plotting images in which received signal strength (color scale) is a function of echo delay (range in vertical scale) and radio-sounder frequency (horizontal scale) of the sounder pulses. Echoes that can be used to derive remote, long-range, magnetospheric electron-density profiles, appear as discrete traces on plasmagrams. These plasmagram traces are intermixed with vertical signatures with greater intensity at shorter ranges, corresponding to locally excited plasma resonances, and other vertical signatures that cover the entire listening period, i.e., the entire virtual-range scale, corresponding to various natural and/or man-made emissions propagating in space and/or local interference.

20) IMAGE RPI Monthly Electron Density Values maxmize
Resource ID:spase://VSPO/NumericalData/IMAGE/RPI/PT1M
Start:2001-01-01 00:00:00 Observatory:IMAGE Cadence:1 minute
Stop:2005-12-01 00:00:00 Instrument:Radio Plasma Imager (RPI) Resource:NumericalData
The electron density values listed in this file are derived from the IMAGE Radio Plasma Imager (B.W. Reinisch, PI) data using an automatic fitting program written by Phillip Webb with manual correction. The electron number densities were produced using an automated procedure (with manual correction when necessary) which attempted to self-consistently fit an enhancement in the IMAGE RPI Dynamic Spectra to either 1) the Upper Hybrid Resonance band, 2) the Z-mode or 3) the continuum edge. The automatic algorithm works by rules determined by comparison of the active and passive RPI data [Benson et al., GRL, vol. 31, L20803, doi:10.1029/2004GL020847, 2004]. The manual data points are not from frequencies chosen freely by a human. Rather the human specifies that the computer should search for a peak or continuum edge in a certain frequency region. Thus even the manual points are determined, in part, by the automatic algorithms. Of course that does not guarantee that the data points are right, but it does eliminate some human bias.

21) IMAGE RPI Plasmagram/Echogram Key Parameters maxmize
Resource ID:spase://VSPO/NumericalData/IMAGE/RPI/PT24H
Start:2000-03-26 00:00:00 Observatory:IMAGE Cadence:24 hours
Stop:2005-12-18 00:00:00 Instrument:Radio Plasma Imager (RPI) Resource:NumericalData
This set of daily plasmagrams/echograms comes from the IMAGE Radio Plasma Imager that studies the Earth's magnetophere in the 3 kHz to 3 MHz frequency range. RPI plasmagrams are visualized by plotting images in which received signal strength (color scale) is a function of echo delay (range in vertical scale) and radio-sounder frequency (horizontal scale) of the sounder pulses. Echoes that can be used to derive remote, long-range, magnetospheric electron-density profiles, appear as discrete traces on plasmagrams. These plasmagram traces are intermixed with vertical signatures with greater intensity at shorter ranges, corresponding to locally excited plasma resonances, and other vertical signatures that cover the entire listening period, i.e., the entire virtual-range scale, corresponding to various natural and/or man-made emissions propagating in space and/or local interference.

22) IRIS Calibrated Images and Spectra Data maxmize
Resource ID:spase://VSPO/NumericalData/IRIS/IRIS/PT1S
Start:2013-09-15 00:00:01 Observatory:Interface Region Imaging Spectrograph (IRIS) Cadence:1 second
Stop:2016-09-14 07:59:51 Instrument:Interface Region Imaging Spectrograph (IRIS) Resource:NumericalData
This data set contains calibrated level-2 images and spectra data from the Interface Region Imaging Spectrograph (IRIS). UV images from IRIS telesccope record observations of features as small as 240 km (150 miles) on the sun every five to ten seconds at specific temperatures, ranging from 5,000 K and 65,000 K (and up to 10 million K during solar flares). This range is tailored to observe material traveling on the surface of the sun, called the photosphere, and in the lowermost layers of the atmosphere, called the chromosphere and transition region. Spectra are obtained every one to two seconds along a slit (1/3 arcsec wide) of solar material at temperatures from 5,000 K to 10 million K, providing information on exactly how much light is visible from any specific wavelength. This corresponds to how much material is present at specific velociites, temperatures and densities. The level-2 data is corrected for dark current, flat-field, and geometric deformation, scaled to the same plate-scale, and packaged into timeseries of slitjaw images and spectral raster scans. The calibration is preliminary and will improve in the coming months.

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