Data Access
These data cubes contain co-aligned, simultaneous observations taken with the Interface Region Imaging Spectrograph (IRIS) and the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamic Observatory (SDO). These cubes are science-ready, co-aligned, high-resolution observations of photospheric, chromospheric, transition region, and coronal solar features.
RIRIS records spectra in the near-ultraviolet band (NUV) from 278.3 nm to 283.4 nm and in the far-ultraviolet bands from 133.2 nm to 135.8 nm (FUV 1) and 138.9 nm to 140.7 nm (FUV 2). The spectra are obtained every 0.5 s to 60 s along a slit (1/3" wide). IRIS detects solar material at temperatures from 5,000 K to 10 million K. IRIS slit-jaw images (SJI) are taken every 0.5 s to 60 s using filters centered at Mg II k 279.6 nm (SJI 2796), the far Mg II h wing at 283.2 nm (SJI 2832), C II at 133 nm (SJI 1330), and Si IV at 140 nm (SJI 1400). In this way, IRIS provides images of solar features as small as 240 km (150 miles) and allows inference of how much material is present at specific velocities, temperatures and densities. These data can then be used to probe the photosphere, the chromosphere, and the transition region and thus to study energetic and dynamic properties of material throughout the solar atmosphere.
The SDO mission was developed and launched under the NASA Living With a Star (LWS) program. This spacecraft carries three instruments: the Extreme ultraviolet Variability Explorer (EVE), Helioseismic and Magnetic Imager (HMI), and the Atmospheric Imaging Assembly (AIA). EVE measures the EUV spectral irradiance while HMI obtains full-disk, high-cadence Dopplergrams, broadband continuum filtergrams, longitudinal and vector magnetograms. AIA is composed of an array of 4 telescopes, and provides full-Sun images (0.6" pixel size) of the solar photosphere, chromosphere and corona through measurements in multiple EUV and UV passbands (94 Å, 131 Å, 171 Å, 193 Å, 211 Å, 304 Å, 335 Å, 1600 Å, 1700 Å, and white light continuum). The cadence of AIA EUV images is 12 s, while 2 s cadence is possible during flare observations. AIA UV images have a cadence of 24 s.
IRIS and AIA filtergrams are cross-correlated using the XCEN/YCEN and FOVX/FOVY keywords from IRIS level 2 and AIA level 1.5 data. To provide context for the IRIS field of view (FOV), the AIA data cubes have a slightly larger FOV than IRIS (±50" in both x and y directions), and start 10 minutes before the IRIS observations and end 10 minutes later. This way, AIA images cover the entire IRIS observational period and FOV with its surroundings. When necessary, AIA data cubes are corrected for solar rotation tracking and IRIS roll angles. Final AIA data products include the following channels: 94 Å, 131 Å, 171 Å, 193 Å, 211 Å, 304 Å, 335 Å, 1600 Å and 1700 Å. The co-aligned SDO/AIA and IRIS data cubes are formatted in the same way as IRIS level 2 data, and can be analyzed using the IRIS SolarSoft software. The IRIS data is corrected for dark current, flat-field, geometric deformation, and scaled to the same plate-scale. Wavelength calibrations and subtraction of the background light leak in FUV data are also performed. In AIA level 1.5 images bad pixels and cosmic ray spikes are identified and removed. The AIA Level 1.5 data products include geometric corrections with all images sharing common plate scales and centers and rotation angle from the Solar North.
Version:2.5.0
These data cubes contain co-aligned, simultaneous observations taken with the Interface Region Imaging Spectrograph (IRIS) and the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamic Observatory (SDO). These cubes are science-ready, co-aligned, high-resolution observations of photospheric, chromospheric, transition region, and coronal solar features.
RIRIS records spectra in the near-ultraviolet band (NUV) from 278.3 nm to 283.4 nm and in the far-ultraviolet bands from 133.2 nm to 135.8 nm (FUV 1) and 138.9 nm to 140.7 nm (FUV 2). The spectra are obtained every 0.5 s to 60 s along a slit (1/3" wide). IRIS detects solar material at temperatures from 5,000 K to 10 million K. IRIS slit-jaw images (SJI) are taken every 0.5 s to 60 s using filters centered at Mg II k 279.6 nm (SJI 2796), the far Mg II h wing at 283.2 nm (SJI 2832), C II at 133 nm (SJI 1330), and Si IV at 140 nm (SJI 1400). In this way, IRIS provides images of solar features as small as 240 km (150 miles) and allows inference of how much material is present at specific velocities, temperatures and densities. These data can then be used to probe the photosphere, the chromosphere, and the transition region and thus to study energetic and dynamic properties of material throughout the solar atmosphere.
The SDO mission was developed and launched under the NASA Living With a Star (LWS) program. This spacecraft carries three instruments: the Extreme ultraviolet Variability Explorer (EVE), Helioseismic and Magnetic Imager (HMI), and the Atmospheric Imaging Assembly (AIA). EVE measures the EUV spectral irradiance while HMI obtains full-disk, high-cadence Dopplergrams, broadband continuum filtergrams, longitudinal and vector magnetograms. AIA is composed of an array of 4 telescopes, and provides full-Sun images (0.6" pixel size) of the solar photosphere, chromosphere and corona through measurements in multiple EUV and UV passbands (94 Å, 131 Å, 171 Å, 193 Å, 211 Å, 304 Å, 335 Å, 1600 Å, 1700 Å, and white light continuum). The cadence of AIA EUV images is 12 s, while 2 s cadence is possible during flare observations. AIA UV images have a cadence of 24 s.
IRIS and AIA filtergrams are cross-correlated using the XCEN/YCEN and FOVX/FOVY keywords from IRIS level 2 and AIA level 1.5 data. To provide context for the IRIS field of view (FOV), the AIA data cubes have a slightly larger FOV than IRIS (±50" in both x and y directions), and start 10 minutes before the IRIS observations and end 10 minutes later. This way, AIA images cover the entire IRIS observational period and FOV with its surroundings. When necessary, AIA data cubes are corrected for solar rotation tracking and IRIS roll angles. Final AIA data products include the following channels: 94 Å, 131 Å, 171 Å, 193 Å, 211 Å, 304 Å, 335 Å, 1600 Å and 1700 Å. The co-aligned SDO/AIA and IRIS data cubes are formatted in the same way as IRIS level 2 data, and can be analyzed using the IRIS SolarSoft software. The IRIS data is corrected for dark current, flat-field, geometric deformation, and scaled to the same plate-scale. Wavelength calibrations and subtraction of the background light leak in FUV data are also performed. In AIA level 1.5 images bad pixels and cosmic ray spikes are identified and removed. The AIA Level 1.5 data products include geometric corrections with all images sharing common plate scales and centers and rotation angle from the Solar North.
| Role | Person | StartDate | StopDate | Note | |
|---|---|---|---|---|---|
| 1. | PrincipalInvestigator | spase://SMWG/Person/Bart.De.Pontieu |
At the IRIS LMSAL site
IRIS Data User's Guide
Definition of IRIS Data Levels
Select IRIS data from today or past dates
Recent IRIS Observations
Planned Observations for IRIS
IRIS records spectra in the near-ultraviolet band (NUV) from 278.3 nm to 283.4 nm and in the far-ultraviolet band from 133.2 nm to 135.8 nm (FUV 1), and from 138.9 nm to 140.7 nm (FUV 2). Spectra are obtained every 0.5 s to 60 s along a slit (1/3" wide). It detects solar material at temperatures from 5,000 K to 10 million K. IRIS slit-jaw images (SJI) are taken every 0.5 s to 60 s using filters centered on Mg II k 279.6 nm (SJI 2796), the far Mg II h wing at 283.2 nm (SJI 2832), C II 133 nm (SJI 1330), and Si IV 140 nm (SJI 1400). In this way IRIS provides images of solar features as small as 240 km (150 miles), and allows inference of how much material is present at specific velocities, temperatures and densities.
SDO/AIA is composed of an array of 4 telescopes, and provides full-Sun images (0.6" pixel size) of the solar photosphere, chromosphere and corona through measurements in multiple EUV and UV passbands (94 Å, 131 Å, 171 Å, 193 Å, 211 Å, 304 Å, 335 Å, 1600 Å, 1700 Å, and white light continuum). The cadence of AIA EUV images is 12 s, while 2 s cadence is possible during flare observations. AIA UV images have a cadence of 24 s.