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Data Access
The SOHO/UVCS Data Search via VSO
MEDOC site
Search:
SOHO Science Archive
SOHO UVCS Data
var authors='The UVCS Consortium: Harvard-Smithsonian Center for Astrophysics (USA); Università di Firenze (Italy); ESA European Space Research and Technology Centre (Netherlands); Università di Torino (Italy); Università di Padova (Italy); Osservatorio Astrofisico di Catania (Italy); Osservatorio Astrofisico di Arcetri (Italy); Max Planck Institut für Aeronomie (Germany); European Southern Observatory (Germany); International Space Science Institute (Switzerland); University of New Brunswick (Canada); University of Maryland (USA); Alenia Spazio (Italy); Officine Galileo (Italy); Brusag (Switzerland); Oerlikon-Contraves (Switzerland); Space Sciences Laboratory (USA); Ball Corporation (USA); NASA/GSFC (USA)';
document.write(authors);
(2013).
SOHO UVCS Data.
[Data set].
Solar Data Analysis Center; European Space Astronomy Centre.
https://doi.org/10.48322/a1pz-bm40. Accessed on document.write(currentDateStr);.
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or other formats, should include the "Accessed on date" to identify the version of the resource being cited in a given publication.
ResourceID
spase://NASA/NumericalData/SOHO/UVCS/PT9M
Description
The primary scientific goals of the UVCS (UltraViolet Coronagraph Spectrometer) are to: (1) locate and characterize the coronal source regions of the solar wind; (2) identify and understand the dominant physical processes that accelerate the solar wind; (3) understand how the coronal plasma is heated in solar wind acceleration regions; and, (4) increase our knowledge of the coronal phenomena that control the physical properties of the solar wind as determined by in situ measurements. The UVCS is intended to determine the primary plasma parameters of the solar corona from its base to as high as 10 Re. It is expected to measure signatures of both thermal and nonthermal processes: electron temperatures, effective temperatures of protons and several minor ions; electron and ion densities of O+5, Mg+9, Si+11, and Fe+11; and flow velocities of the electron/proton plasma and of O+5, Mg+9, and Si+11. The instrument consists of an occulted telescope and a high resolution spectrometer assembly. Three off-axis telescope mirrors focus co-registered images of the extended corona onto the three entrance slits of the spectrometer assembly. The spectrometer assembly consists of three sections. One is optimized for line profile measurements of H I Lyman alpha, with a range of 114.8--128.3 nm, extendable to 113.0 nm and 130.0 nm with grating motions. A second section is optimized for line intensity measurements of O VII (103.2 nm) and is also used to observe Si XII in second order (499 and 521 nm; first order range is 93.2--106.8 nm). The third section is used to measure polarized radiance of the visible corona. A filter with a bandpass of 450.0--600.0 nm is mounted in front of a photomultiplier tube. The EUV spectrometer sections use toroidal concave diffraction gratings in Rowland circle mounts that produce stigmatic imaging at the subject wavelengths. There are entrance slit changing mechanisms on each spectrometer. The detectors for the EUV are multi-anode microchannel arrays, each with 360 x 1024 pixels on 0.025 mm centers. The instantaneous field of view (FOV) of the instrument is the portion of the solar image that passes through the spectrometer entrance slits. Internal mirror motions are used to step the instantaneous FOV across the 141' x 40' FOV defined by the entrance aperture. Offset pointing adjustments can be used to extend the FOV for EUV measurements down to the solar limb, and also onto the solar disk for measurements of absolute spectral line intensities and positions. The UVCS can rotate its FOV about the sun-center to observe any segment of the corona within 10 solar radii. Twelve rotations of 30 degrees would build up a spectroscopic description of the full corona out to 5 solar radii, with additional data out to 10 solar radii. This information was taken from the article ``UVCS - the Ultraviolet Coronagraph Spectrometer for SOHO,'' by J. L. Kohl and G. Noci (Proceedings of the First SOHO Workshop, ESA SP-348, pp. 23-26, November 1992).
Metadata Rights
CC0-1.0:
Creative Commons Zero v1.0 Universal
Note
CC0 1.0 Universal is the Creative Commons license applicable to all publicly available SPASE metadata descriptions. The actual data/software may be subject to a different license.
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Details
Version:2.7.1
NumericalData
ResourceID
spase://NASA/NumericalData/SOHO/UVCS/PT9M
NamingAuthority
NASA
ResourceType
NumericalData
ResourceHeader
ResourceName
SOHO UVCS Data
DOI
https://doi.org/10.48322/a1pz-bm40
ReleaseDate
2026-07-21 12:07:16Z
RevisionHistory
RevisionEvent
ReleaseDate
2020-07-07 21:15:19Z
Note
Only known prior ReleaseDate of the metadata
RevisionEvent
ReleaseDate
2024-08-13 00:08:46Z
Note
Updated Contacts; Updated PublicationInfo
RevisionEvent
ReleaseDate
2025-09-18 12:12:33Z
Note
Added ResourceType and NamingAuthority. Changed http to https in top-level schemaLocation attribute. Fixed version number separator in top-level schemaLocation attribute. Matched version number in schemaLocation attribute to updated value in Version tag. ZCB
RevisionEvent
ReleaseDate
2025-10-03 11:24:33Z
Note
Updated PublishedBy name to match ROR Registry. ZCB
RevisionEvent
ReleaseDate
2025-12-04 13:31:30Z
Note
Added MetadataRightsList and RightsList(s). Updated to 2.7.1. ZCB
RevisionEvent
ReleaseDate
2026-04-03 18:30:01Z
Note
Added DOI. tlk
RevisionEvent
ReleaseDate
2026-06-26 13:28:06Z
Note
Add 'Z' to RevisionEvent:ReleaseDate(s), PublicationDate, TemporalDescription:TimeSpan:StartDate, TemporalDescription:TimeSpan:StopDate. ZCB
RevisionEvent
ReleaseDate
2026-07-21 12:07:16Z
Note
Added HelioData InformationURL. JWL
Description
The primary scientific goals of the UVCS (UltraViolet Coronagraph Spectrometer) are to: (1) locate and characterize the coronal source regions of the solar wind; (2) identify and understand the dominant physical processes that accelerate the solar wind; (3) understand how the coronal plasma is heated in solar wind acceleration regions; and, (4) increase our knowledge of the coronal phenomena that control the physical properties of the solar wind as determined by in situ measurements. The UVCS is intended to determine the primary plasma parameters of the solar corona from its base to as high as 10 Re. It is expected to measure signatures of both thermal and nonthermal processes: electron temperatures, effective temperatures of protons and several minor ions; electron and ion densities of O+5, Mg+9, Si+11, and Fe+11; and flow velocities of the electron/proton plasma and of O+5, Mg+9, and Si+11. The instrument consists of an occulted telescope and a high resolution spectrometer assembly. Three off-axis telescope mirrors focus co-registered images of the extended corona onto the three entrance slits of the spectrometer assembly. The spectrometer assembly consists of three sections. One is optimized for line profile measurements of H I Lyman alpha, with a range of 114.8--128.3 nm, extendable to 113.0 nm and 130.0 nm with grating motions. A second section is optimized for line intensity measurements of O VII (103.2 nm) and is also used to observe Si XII in second order (499 and 521 nm; first order range is 93.2--106.8 nm). The third section is used to measure polarized radiance of the visible corona. A filter with a bandpass of 450.0--600.0 nm is mounted in front of a photomultiplier tube. The EUV spectrometer sections use toroidal concave diffraction gratings in Rowland circle mounts that produce stigmatic imaging at the subject wavelengths. There are entrance slit changing mechanisms on each spectrometer. The detectors for the EUV are multi-anode microchannel arrays, each with 360 x 1024 pixels on 0.025 mm centers. The instantaneous field of view (FOV) of the instrument is the portion of the solar image that passes through the spectrometer entrance slits. Internal mirror motions are used to step the instantaneous FOV across the 141' x 40' FOV defined by the entrance aperture. Offset pointing adjustments can be used to extend the FOV for EUV measurements down to the solar limb, and also onto the solar disk for measurements of absolute spectral line intensities and positions. The UVCS can rotate its FOV about the sun-center to observe any segment of the corona within 10 solar radii. Twelve rotations of 30 degrees would build up a spectroscopic description of the full corona out to 5 solar radii, with additional data out to 10 solar radii. This information was taken from the article ``UVCS - the Ultraviolet Coronagraph Spectrometer for SOHO,'' by J. L. Kohl and G. Noci (Proceedings of the First SOHO Workshop, ESA SP-348, pp. 23-26, November 1992).
PublicationInfo
Authors
The UVCS Consortium: Harvard-Smithsonian Center for Astrophysics (USA); Università di Firenze (Italy); ESA European Space Research and Technology Centre (Netherlands); Università di Torino (Italy); Università di Padova (Italy); Osservatorio Astrofisico di Catania (Italy); Osservatorio Astrofisico di Arcetri (Italy); Max Planck Institut für Aeronomie (Germany); European Southern Observatory (Germany); International Space Science Institute (Switzerland); University of New Brunswick (Canada); University of Maryland (USA); Alenia Spazio (Italy); Officine Galileo (Italy); Brusag (Switzerland); Oerlikon-Contraves (Switzerland); Space Sciences Laboratory (USA); Ball Corporation (USA); NASA/GSFC (USA)
PublicationDate
2013-10-01 00:00:00Z
PublishedBy
Solar Data Analysis Center; European Space Astronomy Centre
Contacts
Role
Person
StartDate
StopDate
Note
1.
FormerPI
spase://SMWG/Person/John.L.Kohl
2.
PrincipalInvestigator
spase://SMWG/Person/Leonard.Strachan
InformationURL
Name
The SOHO/UVCS Website
URL
https://lweb.cfa.harvard.edu/uvcs/
InformationURL
Name
The SOHO/UVCS Instrument paper
URL
https://doi.org/10.1007/BF00733433
InformationURL
Name
HelioData
URL
https://helio.data.nasa.gov/dataset/SOHO_UVCS_PT9M
Description
The HelioData dataset page provides an overview of the dataset with access links, associated variables, and more.
PriorIDs
spase://VSPO/NumericalData/P_SOHO_HDR_UVCS
spase://VSPO/NumericalData/SOHO/UVCS/PT9M
AccessInformation
RepositoryID
spase://SMWG/Repository/SDAC
Availability
Online
AccessRights
Open
RightsList
Rights
SchemeURI
https://spdx.org/licenses/
RightsIdentifierScheme
SPDX
RightsIdentifier
CC0-1.0
RightsURI
https://spdx.org/licenses/CC0-1.0.html
RightsName
Creative Commons Zero v1.0 Universal
Note
CC0 1.0 Universal is the Creative Commons license applicable to all publicly available NASA Heliophysics data products
AccessURL
Name
The SOHO/UVCS Data Search via VSO
URL
https://sdac.virtualsolar.org/cgi/search?time=1&inst_only=1&version=current&build=1&instrument=UVCS
Format
FITS
AccessInformation
RepositoryID
spase://SMWG/Repository/MEDOC
Availability
Online
AccessRights
Open
AccessURL
Name
MEDOC site
URL
http://idoc-medoc.ias.u-psud.fr/sitools/client-user/index.html?project=Medoc-Solar-Portal
Format
FITS
AccessInformation
RepositoryID
spase://ESA/Repository/SOHOScienceArchive
Availability
Online
AccessRights
Open
AccessURL
Name
SOHO Science Archive
URL
https://ssa.esac.esa.int/ssa/#/pages/search
Style
Search
Format
FITS
ProviderProcessingLevel
CALIBRATED
InstrumentIDs
spase://SMWG/Instrument/SOHO/UVCS
MeasurementType
ImageIntensity
TemporalDescription
TimeSpan
StartDate
1996-01-02 00:00:00Z
StopDate
2013-01-19 18:46:16Z
Cadence
PT9M
ObservedRegion
Sun
ObservedRegion
Sun.Corona