cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.48322/094z-2d40
title: SDO/AIA 193 Angstrom FITS Data

description: The SDO/AIA 193 Å Level 1 FITS Data. The 193 Å channel observes the Fe xii and Fe xxiv lines from corona (1.3 MK) and hot flare plasma (20 MK), respectively.

The Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) focuses on the evolution of the magnetic environment in the Sun’s atmosphere, and its interaction with embedded and surrounding plasma. The AIA investigation covers a broad range of science objectives that focus on five core research themes that both advance solar and heliospheric physics in general and provide advanced warning of coronal and inner-heliospheric disturbances of interest to the Living With a Star (LWS) program, i.e., global change, space weather, human exploration of space, and technological infrastructure in space and on Earth.

AIA provides the following essential capabilities: i) A view of the entire Sun in 4k x 4k resolution (pixel size of 0.6 arcseconds), with full thermal coverage of the corona; ii) A high signal-to-noise ratio for two- to three-second exposures that reaches 100 in quiescent conditions for the low-temperature coronal-imaging channels and during flaring in the higher-temperature channels, with a dynamic range of up to 10,000; iii) Essentially uninterrupted viewing for months at a temporal cadence of 12 seconds in seven extreme UV (EUV) band passes (94, 131, 171, 193, 211, 304 and 335 Å), and 24 seconds for two UV channels (1600 and 1700 Å) band passes; iv) In special observing modes, AIA can capture images of the Sun at higher cadence while keeping within the instrument allocated telemetry by using a subset of bandpass channels, and/or using a crop table.
DOI: 10.48322/n41j-hy30
title: SDO/AIA 171 Angstrom FITS Data

description: The SDO/AIA 171 Å Level 1 FITS Data .The 171 Å channel observes the Fe ix line from quiet corona and upper transition region (0.63 MK).

The Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) focuses on the evolution of the magnetic environment in the Sun’s atmosphere, and its interaction with embedded and surrounding plasma. The AIA investigation covers a broad range of science objectives that focus on five core research themes that both advance solar and heliospheric physics in general and provide advanced warning of coronal and inner-heliospheric disturbances of interest to the Living With a Star (LWS) program, i.e., global change, space weather, human exploration of space, and technological infrastructure in space and on Earth.

AIA provides the following essential capabilities: i) A view of the entire Sun in 4k x 4k resolution (pixel size of 0.6 arcseconds), with full thermal coverage of the corona; ii) A high signal-to-noise ratio for two- to three-second exposures that reaches 100 in quiescent conditions for the low-temperature coronal-imaging channels and during flaring in the higher-temperature channels, with a dynamic range of up to 10,000; iii) Essentially uninterrupted viewing for months at a temporal cadence of 12 seconds in seven extreme UV (EUV) band passes (94, 131, 171, 193, 211, 304 and 335 Å), and 24 seconds for two UV channels (1600 and 1700 Å) band passes; iv) In special observing modes, AIA can capture images of the Sun at higher cadence while keeping within the instrument allocated telemetry by using a subset of bandpass channels, and/or using a crop table.
DOI: 10.48322/dpmb-xg29
title: SDO/AIA 211 Angstrom FITS Data

description: The SDO/AIA 211 Å Level 1 FITS Data. The 211 Å channel observes the Fe xiv line from active region corona (2.0 MK).  

The Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) focuses on the evolution of the magnetic environment in the Sun’s atmosphere, and its interaction with embedded and surrounding plasma. The AIA investigation covers a broad range of science objectives that focus on five core research themes that both advance solar and heliospheric physics in general and provide advanced warning of coronal and inner-heliospheric disturbances of interest to the Living With a Star (LWS) program, i.e., global change, space weather, human exploration of space, and technological infrastructure in space and on Earth.

AIA provides the following essential capabilities: i) A view of the entire Sun in 4k x 4k resolution (pixel size of 0.6 arcseconds), with full thermal coverage of the corona; ii) A high signal-to-noise ratio for two- to three-second exposures that reaches 100 in quiescent conditions for the low-temperature coronal-imaging channels and during flaring in the higher-temperature channels, with a dynamic range of up to 10,000; iii) Essentially uninterrupted viewing for months at a temporal cadence of 12 seconds in seven extreme UV (EUV) band passes (94, 131, 171, 193, 211, 304 and 335 Å), and 24 seconds for two UV channels (1600 and 1700 Å) band passes; iv) In special observing modes, AIA can capture images of the Sun at higher cadence while keeping within the instrument allocated telemetry by using a subset of bandpass channels, and/or using a crop table.
DOI: 10.48322/asmp-nf13
title: SDO/AIA 335 Angstrom FITS Data

description: The SDO/AIA 335 Å Level 1 FITS Data. The 335 Å channel observes the Fe xvi line from active region corona (2.5 MK).  

The Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) focuses on the evolution of the magnetic environment in the Sun’s atmosphere, and its interaction with embedded and surrounding plasma. The AIA investigation covers a broad range of science objectives that focus on five core research themes that both advance solar and heliospheric physics in general and provide advanced warning of coronal and inner-heliospheric disturbances of interest to the Living With a Star (LWS) program, i.e., global change, space weather, human exploration of space, and technological infrastructure in space and on Earth.

AIA provides the following essential capabilities: i) A view of the entire Sun in 4k x 4k resolution (pixel size of 0.6 arcseconds), with full thermal coverage of the corona; ii) A high signal-to-noise ratio for two- to three-second exposures that reaches 100 in quiescent conditions for the low-temperature coronal-imaging channels and during flaring in the higher-temperature channels, with a dynamic range of up to 10,000; iii) Essentially uninterrupted viewing for months at a temporal cadence of 12 seconds in seven extreme UV (EUV) band passes (94, 131, 171, 193, 211, 304 and 335 Å), and 24 seconds for two UV channels (1600 and 1700 Å) band passes; iv) In special observing modes, AIA can capture images of the Sun at higher cadence while keeping within the instrument allocated telemetry by using a subset of bandpass channels, and/or using a crop table.
DOI: 10.48322/z1ks-mk18
title: SDO/AIA 304 Angstrom FITS Data

description: The SDO/AIA 304 Å Level 1 FITS Data. The 304 Å channel observes the He ii line from chromosphere and transition region (0.50 MK). 

The Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) focuses on the evolution of the magnetic environment in the Sun’s atmosphere, and its interaction with embedded and surrounding plasma. The AIA investigation covers a broad range of science objectives that focus on five core research themes that both advance solar and heliospheric physics in general and provide advanced warning of coronal and inner-heliospheric disturbances of interest to the Living With a Star (LWS) program, i.e., global change, space weather, human exploration of space, and technological infrastructure in space and on Earth.

AIA provides the following essential capabilities: i) A view of the entire Sun in 4k x 4k resolution (pixel size of 0.6 arcseconds), with full thermal coverage of the corona; ii) A high signal-to-noise ratio for two- to three-second exposures that reaches 100 in quiescent conditions for the low-temperature coronal-imaging channels and during flaring in the higher-temperature channels, with a dynamic range of up to 10,000; iii) Essentially uninterrupted viewing for months at a temporal cadence of 12 seconds in seven extreme UV (EUV) band passes (94, 131, 171, 193, 211, 304 and 335 Å), and 24 seconds for two UV channels (1600 and 1700 Å) band passes; iv) In special observing modes, AIA can capture images of the Sun at higher cadence while keeping within the instrument allocated telemetry by using a subset of bandpass channels, and/or using a crop table.
DOI: 10.48322/50td-nz33
title: NWRA AIA Active Region Patches (AARP) Database

description: The "AIA Active Region Patches" comprise an unbiased multi-wavelength set of FITS files of data extracted from SDO/AIA full-disk data. The spatial extractions are based on SDO/HMI "Active Region Patch" (HARP) definitions, and match the HARP numbering. However, the AARPs have extended bounding-boxes to cover the larger visible extent of coronal loops. There is no spatial binning and no additional geometric or regridding performed. The spectral down-sampling comprises the omission of 1700 images; all other filters are included (94, 131, 171, 193, 211, 304, 335, 1600). The temporal sampling consists of 11 images at 72s cadence (13 min) for each wavelength, centered at 15:48, 16:48, 17:48, 18:48, 19:48, 20:48 and 21:48, daily. No AEC-invoked (shorter exposure) data were included; exposure times were consistent but not multiplied through (data are presented in DN). The SSW aia_prep and corrections for time-dependent sensitivity degradation were applied.
DOI: 10.48322/51e0-hf62
title: SDO/AIA FITS Data

description: The SDO/AIA Level 1 FITS Data. 

The Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) focuses on the evolution of the magnetic environment in the Sun’s atmosphere, and its interaction with embedded and surrounding plasma. The AIA investigation covers a broad range of science objectives that focus on five core research themes that both advance solar and heliospheric physics in general and provide advanced warning of coronal and inner-heliospheric disturbances of interest to the Living With a Star (LWS) program, i.e., global change, space weather, human exploration of space, and technological infrastructure in space and on Earth.

AIA provides the following essential capabilities: i) A view of the entire Sun in 4k x 4k resolution (pixel size of 0.6 arcseconds), with full thermal coverage of the corona; ii) A high signal-to-noise ratio for two- to three-second exposures that reaches 100 in quiescent conditions for the low-temperature coronal-imaging channels and during flaring in the higher-temperature channels, with a dynamic range of up to 10,000; iii) Essentially uninterrupted viewing for months at a temporal cadence of 12 seconds in seven extreme UV (EUV) band passes (94, 131, 171, 193, 211, 304 and 335 Å), and 24 seconds for two UV channels (1600 and 1700 Å) band passes; iv) In special observing modes, AIA can capture images of the Sun at higher cadence while keeping within the instrument allocated telemetry by using a subset of bandpass channels, and/or using a crop table.
DOI: 10.48322/v66w-8e77
title: SDO/AIA Carrington Maps

description: Synoptic (or Carrington) Map PNG images created from EUV images observed by the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO). Maps are available for each Carrington Rotation since the beginning of the SDO mission. Meridian maps for AIA illustrate the corresponding structures and long-term changes in the lower atmosphere.
DOI: 10.48322/fwtc-3d78
title: SDO/AIA 1600 Angstrom FITS Data

description: The SDO/AIA 1600 Å Level 1 FITS Data. The 1600 Å channel observes the C iv line and continuum from the transition region and the upper photosphere, respectively. 

The Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) focuses on the evolution of the magnetic environment in the Sun’s atmosphere, and its interaction with embedded and surrounding plasma. The AIA investigation covers a broad range of science objectives that focus on five core research themes that both advance solar and heliospheric physics in general and provide advanced warning of coronal and inner-heliospheric disturbances of interest to the Living With a Star (LWS) program, i.e., global change, space weather, human exploration of space, and technological infrastructure in space and on Earth.

AIA provides the following essential capabilities: i) A view of the entire Sun in 4k x 4k resolution (pixel size of 0.6 arcseconds), with full thermal coverage of the corona; ii) A high signal-to-noise ratio for two- to three-second exposures that reaches 100 in quiescent conditions for the low-temperature coronal-imaging channels and during flaring in the higher-temperature channels, with a dynamic range of up to 10,000; iii) Essentially uninterrupted viewing for months at a temporal cadence of 12 seconds in seven extreme UV (EUV) band passes (94, 131, 171, 193, 211, 304 and 335 Å), and 24 seconds for two UV channels (1600 and 1700 Å) band passes; iv) In special observing modes, AIA can capture images of the Sun at higher cadence while keeping within the instrument allocated telemetry by using a subset of bandpass channels, and/or using a crop table.
DOI: 10.48322/mjpe-e089
title: SDO/AIA Synoptic FITS Data

description: The SDO/AIA Level 1.5 Synoptic FITS Data. 

The AIA Synoptic FITS data are reduced to 1024x1024 2.4 arc-sec pixels by summing with pixel value in DN per original 0.6 arc-sec pixel. The data cadence is 2 minutes. These images are produced approximately 7 days after T_OBS since they are derived from definitive level 1 data.
DOI: 10.48322/4k86-r913
title: SDO/AIA 1700 Angstrom FITS Data

description: The SDO/AIA 1700 Å Level 1 FITS Data. The 1700 Å channel observes the continuum from the 4500 K photosphere (temperature minimum).  

The Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) focuses on the evolution of the magnetic environment in the Sun’s atmosphere, and its interaction with embedded and surrounding plasma. The AIA investigation covers a broad range of science objectives that focus on five core research themes that both advance solar and heliospheric physics in general and provide advanced warning of coronal and inner-heliospheric disturbances of interest to the Living With a Star (LWS) program, i.e., global change, space weather, human exploration of space, and technological infrastructure in space and on Earth.

AIA provides the following essential capabilities: i) A view of the entire Sun in 4k x 4k resolution (pixel size of 0.6 arcseconds), with full thermal coverage of the corona; ii) A high signal-to-noise ratio for two- to three-second exposures that reaches 100 in quiescent conditions for the low-temperature coronal-imaging channels and during flaring in the higher-temperature channels, with a dynamic range of up to 10,000; iii) Essentially uninterrupted viewing for months at a temporal cadence of 12 seconds in seven extreme UV (EUV) band passes (94, 131, 171, 193, 211, 304 and 335 Å), and 24 seconds for two UV channels (1600 and 1700 Å) band passes; iv) In special observing modes, AIA can capture images of the Sun at higher cadence while keeping within the instrument allocated telemetry by using a subset of bandpass channels, and/or using a crop table.
DOI: 10.48322/3v9b-4p18
title: SDO/EVE Level 1 Version 8 Data

description: The SDO EVE ESP Level 1 data files are created by the Laboratory for Atmospheric and Space Physics in Boulder, Colorado for the NASA Solar Dynamics Observatory (SDO) Extreme Ultraviolet Variability Experiment (EVE). The Science Processing and Operations Center (SPOC) is responsible for creating and maintaining access to all EVE products. ESP Level 1 data products are generated using software and algorithms created at the Univ. of Southern California Space Sciences Center in Los Angeles, CA. For a high-level introduction to the EVE instrumentation, please visit the following website: https://lasp.colorado.edu/home/eve/science/instrument/.

These Level 1 products are defined to contain 4-Hz integrations from the Extreme ultraviolet SpectroPhotometer (ESP) and began in 2010 day 120 and are continuing. This version change includes updated long-term degradation corrections. This release of EVE ESP Level 1 data products replaces all previous versions.
DOI: 10.48322/xze3-9s15
title: SDO/AIA 4500 Angstrom FITS Data

description: The SDO/AIA 4500 Å Level 1 FITS Data. The 4500 Å channel observes the continuum from the photosphere.  

The Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) focuses on the evolution of the magnetic environment in the Sun’s atmosphere, and its interaction with embedded and surrounding plasma. The AIA investigation covers a broad range of science objectives that focus on five core research themes that both advance solar and heliospheric physics in general and provide advanced warning of coronal and inner-heliospheric disturbances of interest to the Living With a Star (LWS) program, i.e., global change, space weather, human exploration of space, and technological infrastructure in space and on Earth.

AIA provides the following essential capabilities: i) A view of the entire Sun in 4k x 4k resolution (pixel size of 0.6 arcseconds), with full thermal coverage of the corona; ii) A high signal-to-noise ratio for two- to three-second exposures that reaches 100 in quiescent conditions for the low-temperature coronal-imaging channels and during flaring in the higher-temperature channels, with a dynamic range of up to 10,000; iii) Essentially uninterrupted viewing for months at a temporal cadence of 12 seconds in seven extreme UV (EUV) band passes (94, 131, 171, 193, 211, 304 and 335 Å), and 24 seconds for two UV channels (1600 and 1700 Å) band passes; iv) In special observing modes, AIA can capture images of the Sun at higher cadence while keeping within the instrument allocated telemetry by using a subset of bandpass channels, and/or using a crop table.
DOI: 10.48322/6y24-z443
title: SDO/EVE Level 2 Version 8 Data

description: EVE level 2 data files were created at the Laboratory for Atmospheric and Space Physics in Boulder, Colorado for the NASA Solar Dynamics Observatory (SDO) Extreme Ultraviolet Variability Experiment (EVE). The Science Processing and Operations Center (SPOC) is responsible for creating and maintaining access to all EVE products. For a high-level introduction to the EVE instrumentation please visit:
https://lasp.colorado.edu/eve/science/instrument/

Level 2 products are defined to contain 10-second intervals and span the time range from 2010 day 120 through 2018 day 108. The integration rate was changed to 60-seconds so the level 2B products were created to provide future spectra. This release of EVE Level 2 data products replaces all previous versions. We have made significant effort at verification and validation, but if you have any questions or encounter any problems with the data, please let us know about them.

Two types of EVE level 2 products are routinely created: Spectra (EVS) and Lines (EVL). Level 2 spectra are the merged spectral measurements from the two spectrographs, MEGS-A and MEGS-B. The A detector is designed to measure from 6 –17 nm, and 17–37 nm using two filters, while the B detector is designed to measure 37–106. After the MEGS-A anomaly, MEGS-B was extended down to 33.33 nm. 

Level 2 processing stitches these pieces to form one spectrum. This version includes all measured wavelengths. The file spans 3.01-106.99 nm, but this extends beyond where there is no signal on the detectors, so there will be fill values at the extreme ends of the range. All level 2 irradiances are adjusted to 1 AU. Level 2 lines files contain selected lines derived from the level 2 spectra, ESP diode values and bands that correspond to other SDO instruments and some derived proxies.
DOI: 10.48322/fsck-0y31
title: SDO/EVE Level 2B Version 8 Data

description: EVE level 2B data files were created at the Laboratory for Atmospheric and Space Physics in Boulder, Colorado for the NASA Solar Dynamics Observatory (SDO) Extreme Ultraviolet Variability Experiment (EVE). The Science Processing and Operations Center (SPOC) is responsible for creating and maintaining access to all EVE products.

Version 8 includes two new header-data units, explained in detail in later sections, to report line irradiance from each of the three channels: MEGS-A slit 1, MEGS-A slit 2, and MEGS-B. This allows lines to be compared from each channel where there’s overlap in the bandpass. Some new emission lines have been added in the Version 8 level 2B lines data product. This version change also includes updated long-term degradation corrections for MEGS-B and ESP. This is a new release of EVE Level 2B data products.
DOI: 10.48322/tc3q-qk29
title: SDO/EVE Level 3 Version 8 Mission-Long Data

description: EVE level 3 data files were created at the Laboratory for Atmospheric and Space Physics in Boulder, Colorado for the NASA Solar Dynamics Observatory (SDO) Extreme Ultraviolet Variability Experiment (EVE). The Science Processing and Operations Center (SPOC) is responsible for creating and maintaining access to all EVE products. For a high-level introduction to the EVE instrumentation please visit:
https://lasp.colorado.edu/home/eve/science/instrument/

Level 3 products are defined to contain daily averages beginning on 2010, day 120, April 30. This version change includes updated long-term degradation corrections for MEGS-B and ESP. A small dark adjustment was applied to MEG-B and large degradation changes were applied based on SDO EVE sounding rocket measurements. The MEGS-P (Lyman-alpha) diode processing has been updated to replace the Kalman filter with a Fourier transform filter, and the calibration has been updated to match SORCE SOLSTICE version 17.

The mission length merged datasets are provided at three sampling sizes for user convenience; specifically, native level 2 sampling (0.02nm), 1 angstrom, and 1 nm. The optical resolution is about 0.1 nm, so the 0.02nm spectra contain 5 samples per resolution element.
DOI: 10.48322/qnr8-jw83
title: SDO/EVE Level 3 Version 8 Data

description: EVE level 3 data files were created at the Laboratory for Atmospheric and Space Physics in Boulder, Colorado for the NASA Solar Dynamics Observatory (SDO) Extreme Ultraviolet Variability Experiment (EVE). The Science Processing and Operations Center (SPOC) is responsible for creating and maintaining access to all EVE products. For a high-level introduction to the EVE instrumentation please visit:
https://lasp.colorado.edu/home/eve/science/instrument/

Level 3 products are defined to contain daily averages beginning on 2010, day 120, April 30. This version change includes updated long-term degradation corrections for MEGS-B and ESP. A small dark adjustment was applied to MEG-B and large degradation changes were applied based on SDO EVE sounding rocket measurements. The MEGS-P (Lyman-alpha) diode processing has been updated to replace the Kalman filter with a Fourier transform filter, and the calibration has been updated to match SORCE SOLSTICE version 17.
DOI: 10.48322/jdkz-xv95
title: SDO/HMI Continuum, 45-Second Data

description: The HMI continuum data refers to map of the continuum intensity of the solar spectrum in the region of the Fe I absorption line at 6173 Å on the surface of the sun.

HMI samples the Fe I absorption line at 6173.3 Å at six points. Assuming that the "pure" solar Fe I line profile is a Gaussian, and the HMI filter filter transmission profiles are delta functions, the first and second Fourier coefficients of the of the Fe I line can be calculated and an estimate of the Doppler Velocity can be made. An estimate (proxy) for the continuum intensity Ic is obtained by "reconstructing" the solar line from the estimates of the Doppler shift λo, the linewidth σ, and the linedepth Id. More details can be found at http://jsoc.stanford.edu/relevant_papers/observables.pdf.