2.6.0
spase://NASA/NumericalData/IMAGE/EUV/EquatorialMappedImages/ModifiedData/PT10M
IMAGE Extreme UltraViolet (EUV) Imager, Modified Data 2 (M2), 10 min Data
https://doi.org/10.48322/xsb1-nc45
2023-07-30T12:34:56.789
2021-04-27T15:38:11
Only known prior ReleaseDate of the metadata
2023-07-30T12:34:56.789
Added DOI and PublicationInfo minted by LFB, metadata versioned up to SPASE 2.6.0, reviewed by LFB 20230727
The IMAGE extreme ultraviolet (EUV) imager detects resonantly scattered solar EUV photons with a wavelength of 30.4 nm that have been resonantly scattered by singly ionized helium (Sandel et al., 2000). The sizeable database of IMAGE global snapshots from the extreme ultraviolet (EUV) imager provides revolutionary observations of spatial and temporal plasma distributions throughout the plasmasphere. In this study, the IMAGE EUV data have been mapped to the equator using the approach detailed in Gallagher et al. (2005). IMAGE EUV data have been used to create an automated method that locates and extracts the plasmapause. The plasmapause extraction technique searches a set range of possible plasmasphere densities for a maximum gradient in order to identify the magnetic local time, MLT, dependent plasmapause position as a function of time. This description has been adapted from text appearing in Katus et al. (2015).
Please acknowledge the Principal Investigator R.M. Katus for use of the Data
Katus, Roxanne, M.
2023-01-01T00:00:00
NASA Space Physics Data Facility
spase://SMWG/Person/Roxanne.M.Katus
PrincipalInvestigator
spase://SMWG/Person/Robert.M.Candey
MetadataContact
spase://SMWG/Person/Lee.Frost.Bargatze
MetadataContact
IMAGE Extreme Ultraviolet Imager web site, hosted by LPL, Univ. of Arizona
http://euv.lpl.arizona.edu/euv/
Imager for Magnetopause-to-Aurora Global Exploration, IMAGE, satellite Extreme Ultraviolet Imager, instrument information web site, hosted by the Lunar and Planetary Laboratory, University of Arizona
NSSDC Master Catalog
https://nssdc.gsfc.nasa.gov/nmc/experiment/display.action?id=2000-017A-06
General information concerning the Imager for Magnetopause-to-Aurora Global Exploration, IMAGE, Extreme Ultraviolet, EUV, instrument
Katus et al. (2015) IMAGE EUV storm time plasmapause position, Journal of Geophysical Research Space Physics publication
https://doi.org/10.1002/2015JA021225
Katus, R.M., D.L. Gallagher, M.W. Liemohn, A.M. Keesee, and L.K. Sarno-Smith, Statistical Storm Time Examination of MLT dependent Plasmapause Location derived from IMAGE EUV, J. Geophys. Res. Space Phys., 120, 5545-5559, 2015, DOI: 10.1002/2015JA021225
spase://VSPO/NumericalData/IMAGE/EUV/EquatorialMappedImages/ModifiedData/PT10M
spase://SMWG/Repository/NASA/GSFC/SPDF/CDAWeb
Online
Open
FTPS from SPDF (not with most browsers)
ftps://spdf.gsfc.nasa.gov/pub/data/image/fuv/euv_m2/
Access to Data in CDF Format via ftp from SPDF
HTTPS from SPDF
https://spdf.gsfc.nasa.gov/pub/data/image/fuv/euv_m2/
Access to Data in CDF Format via http from SPDF
CDAWeb
https://cdaweb.gsfc.nasa.gov/cgi-bin/eval2.cgi?dataset=IMAGE_M2_EUV&index=sp_phys
IMAGE_M2_EUV
Access to ASCII, CDF, and Plots via NASA/GSFC CDAWeb
CDF
None
Please acknowledge the Principal Investigator R.M. Katus. Please acknowledge the Data Providers and CDAWeb when using these Data.
spase://SMWG/Repository/NASA/GSFC/SPDF/CDAWeb
Online
Open
CDAWeb HAPI Server
https://cdaweb.gsfc.nasa.gov/hapi
IMAGE_M2_EUV
Web Service to this product using the HAPI interface.
CSV
Please acknowledge the Principal Investigator R.M. Katus. Please acknowledge the Data Providers and CDAWeb when using these Data.
Calibrated
spase://SMWG/Instrument/IMAGE/EUV
ImageIntensity
2000-05-04T00:00:00.000
2005-12-17T23:59:59.999
PT10M
Epoch Time, TT2000
Epoch
Epoch Time Tags in Terrestrial Time 2000, TT2000
PT10M
ns
1.0e-9>s
Epoch
F12.2
1999-12-31T23:59:58.999995365
2006-01-01T00:00:00.000000000
9999-12-31T23:59:59.999999999
Temporal
Plasmapause L-shell gradient, spectrogram
Time series defined by using: EPOCH
Plasmapause_MLTbin
Plasmapause L-shell, sharpest gradient from IMAGE EUV ion image data mapped to the equatorial plane, 48 MLT half hour bins, spectrogram format
PT10M
Re
6.3712e6>m
Cartesian
SM
Spectrogram
Plasmapause [Lshell] @ 0.5:.5:24 MLT
F12.2
LinearScale
48
Element 1
1
0.500000
Element 2
2
1
Element 3
3
1.50000
Element 4
4
2
Element 5
5
2.50000
Element 6
6
3
Element 7
7
3.50000
Element 8
8
4
Element 9
9
4.50000
Element 10
10
5
Element 11
11
5.50000
Element 12
12
6
Element 13
13
6.50000
Element 14
14
7
Element 15
15
7.50000
Element 16
16
8
Element 17
17
8.50000
Element 18
18
9
Element 19
19
9.50000
Element 20
20
10
Element 21
21
10.5000
Element 22
22
11
Element 23
23
11.5000
Element 24
24
12
Element 25
25
12.5000
Element 26
26
13
Element 27
27
13.5000
Element 28
28
14
Element 29
29
14.5000
Element 30
30
15
Element 31
31
15.5000
Element 32
32
16
Element 33
33
16.5000
Element 34
34
17
Element 35
35
17.5000
Element 36
36
18
Element 37
37
18.5000
Element 38
38
19
Element 39
39
19.5000
Element 40
40
20
Element 41
41
20.5000
Element 42
42
21
Element 43
43
21.5000
Element 44
44
22
Element 45
45
22.5000
Element 46
46
23
Element 47
47
23.5000
Element 48
48
24
0.0001
20.0
-1.0e+31
Component.I
Component.J
Positional
Plasmapause L-shell gradient, from equatorial IMAGE EUV ion images, MLT noon down, dawn right
Time series defined by using: EPOCH
Mapped_Plasmapause_Grid
Plasmapause L-shell, sharpest gradient from IMAGE EUV ion image data mapped to the equatorial plane, MLT noon to the bottom, dawn to the right
PT10M
Cartesian
SM
Plasmapause
I2
241 241
-32768
Component.I
Component.J
Positional
Plasmapause L-shell gradient, from equatorial IMAGE EUV ion images, MLT noon down, dawn left
Time series defined by using: EPOCH
Mapped_Plasmapause_Grid_flip_vert
Plasmapause L-shell, sharpest gradient from IMAGE EUV ion image data mapped to the equatorial plane, flipped, MLT noon to the bottom, dawn to the left
This parameter is virtual. It is calculated by calling the function ALTERNATE_VIEW_FLIP_VERT with the following input parameters: Mapped_Plasmapause_Grid.
PT10M
Cartesian
SM
Plasmapause
I2
241 241
-32768
Component.I
Component.J
Positional
Plasmapause L-shell gradient, from equatorial IMAGE EUV ion images, Movie
Time series defined by using: EPOCH
Mapped_Plasmapause_Grid_Movie
Plasmapause L-shell, sharpest gradient from IMAGE EUV ion image data mapped to the equatorial plane, flipped, MLT noon to the bottom, dawn to the left, Movie format
This parameter is virtual. It is calculated by calling the function ALTERNATE_VIEW_FLIP_VERT with the following input parameters: Mapped_Plasmapause_Grid.
PT10M
Cartesian
SM
Plasmapause
I2
LinearScale
241 241
-32768
Component.I
Component.J
Positional
Plasmapause data quality index
Time series defined by using: EPOCH
Quality_Flag
Plasmapause data quality rating index: 1=Low, 2=Medium, 3=High
PT10M
TimeSeries
Quality Flag
I2
LinearScale
1
3
-32768
Velocity
Magnetic Local Time bins
MLTbin
Magnetic Local Time, MLT, 48 half hour bins
PT10M
h
3600>s
MLT [hours]
F12.2
LinearScale
48
0.0
100.0
-1.0e+31
DirectionAngle.AzimuthAngle
Other
X-axis coordinates on the equatorial plane
X_Axis
X-axis coordinates on the equatorial plane, used to define the dependent grid
PT10M
Re
6.3712e6>m
X Axis [Re]
F12.2
241
-1.0e+31
Component.I
Other
Y-axis coordinates on the equatorial plane
Y_Axis
Y-axis coordinates on the equatorial plane, used to define the dependent grid
PT10M
Re
6.3712e6>m
Y Axis [Re]
F12.2
241
-1.0e+31
Component.J
Other
IMAGE EUV images mapped to the equatorial plane, MLT noon down, dawn right
Time series defined by using: EPOCH
Equatorial_EUV_Grid
IMAGE EUV images mapped to the equatorial plane, MLT noon to the bottom, dawn to the right
PT10M
cm^-3
1.0e6>m^-3
Cartesian
SM
IMAGE EUV mapped to z=0
F12.2
LinearScale
241 241
-1.0e+31
Electromagnetic
Magnitude
Intensity
IMAGE EUV images mapped to the equatorial plane, MLT noon down, dawn left
Time series defined by using: EPOCH
Equatorial_EUV_Grid_flip_vert
IMAGE EUV images mapped to the equatorial plane, flipped, MLT noon to the bottom, dawn to the left
This parameter is virtual. It is calculated by calling the function ALTERNATE_VIEW_FLIP_VERT with the following input parameters: Equatorial_EUV_Grid.
PT10M
cm^-3
1.0e6>m^-3
Cartesian
SM
IMAGE EUV mapped to z=0
F12.2
LinearScale
241 241
-1.0e+31
Electromagnetic
Magnitude
Intensity
IMAGE EUV images mapped to the equatorial plane, MLT noon down, dawn left, Movie
Time series defined by using: EPOCH
Equatorial_EUV_Grid_Movie
IMAGE EUV images mapped to the equatorial plane, flipped, MLT noon to the bottom, dawn to the left, Movie format
This parameter is virtual. It is calculated by calling the function ALTERNATE_VIEW_FLIP_VERT with the following input parameters: Equatorial_EUV_Grid.
PT10M
cm^-3
1.0e6>m^-3
Cartesian
SM
IMAGE EUV mapped to z=0
F12.2
LinearScale
241 241
-1.0e+31
Electromagnetic
Magnitude
Intensity
IMAGE EUV images mapped to the equatorial plane, log scale, MLT noon down, dawn left
Time series defined by using: EPOCH
Equatorial_EUV_Grid_log
IMAGE EUV images mapped to the equatorial plane, log scale, flipped, MLT noon to the bottom, dawn to the left
This parameter is virtual. It is calculated by calling the function CONVERT_LOG10_FLIP_VERT with the following input parameters: Equatorial_EUV_Grid.
PT10M
log(cm^-3)
(log(cm^-3)+6)>log(m^-3)
Cartesian
SM
IMAGE EUV mapped to z=0
F12.2
LinearScale
241 241
-1.0e+31
Electromagnetic
Magnitude
Intensity
IMAGE EUV images mapped to the equatorial plane, log scale, MLT noon down, dawn left, Movie
Time series defined by using: EPOCH
Equatorial_EUV_Grid_log_Movie
IMAGE EUV images mapped to the equatorial plane, log scale, flipped, MLT noon to the bottom, dawn to the left, Movie format
This parameter is virtual. It is calculated by calling the function CONVERT_LOG10_FLIP_VERT with the following input parameters: Equatorial_EUV_Grid.
PT10M
log(cm^-3)
(log(cm^-3)+6)>log(m^-3)
Cartesian
SM
IMAGE EUV mapped to z=0
F12.2
LinearScale
241 241
-1.0e+31
Electromagnetic
Magnitude
Intensity