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Ulysses GRB Integral 0.5-Second Omnidirectional Counting Rates
var authors='Hurley, Kevin C.';
document.write(authors);
(2025).
Ulysses GRB Integral 0.5-Second Omnidirectional Counting Rates.
[Data set].
Planetary Data System; Space Physics Data Facility; European Space Astronomy Centre.
https://doi.org/10.48322/14fy-2640. Accessed on document.write(currentDateStr);.
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ResourceID
spase://NASA/NumericalData/Ulysses/SCE/GRB/PT1S
Description
This data set contains data and software for integral 0.5-second omnidirectional counting rates from the Ulysses Gamma Ray Burst
(GRB) experiment. It consists of count rates from the sum of two hemispherical detectors convering 4 pi steradians and operating continuously. The detectors
are 3 mm thick CsI scintillators coupled to photomultiplier tubes. The nominal energy range is 25-150 keV, but Table 1 (see below) should be consulted to find
the accurate thresholds for any day of the mission. A more complete description of the instrument may be found in Hurley et al. (1992) and Cotin et al. (1983).
Althoughthe prime objectives of this investigation are the study of solar and cosmic x- and gamma-ray bursts, it should be noted that the experiment is also
sensitive to solar protons and electrons. The former deposit energy directly in the scintillator if they are energetic enough, while the latter may produce x-
radiation locally by bremsstrahlung. Thus although the counting rates are generally stable at about 500 c/s over the long term, there are periods of
weeks to a month or so when the rates increase considerably due to particles. Examples may be found in March 1991 (solar protons) and February 1992
(particles in the Jovian magnetosphere).
The time resolution of the data takes on one of four values depending on the telemetry rate and instrument operating mode: 0.25, 0.5, 1, or 2 seconds. Data
rate changes produce short spikes in the count rates due to a processing artefact. These can in principle be corrected if the data are scanned and the
rate changes are identified; the count rate spikes can then be adjusted to their correct values. There are also short (one sample long) count rate
dropouts, due to an artefact of the onboard software. These may be seen in the sample plots; they cannot be corrected for.
Two figures give examples of solar and cosmic events in the data. The upper panel gives the count rates for day 142, 1993, around 8.24 hours UT. The solar event is evident as a 300 second long increase. Note the count rate dropouts. The bottom panel includes a 20 second long cosmic gamma-ray burst from day 237, 1993 around 8.79 hours UT.
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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Version:2.7.1
NumericalData
ResourceID
spase://NASA/NumericalData/Ulysses/SCE/GRB/PT1S
NamingAuthority
NASA
ResourceType
NumericalData
ResourceHeader
ResourceName
Ulysses GRB Integral 0.5-Second Omnidirectional Counting Rates
DOI
https://doi.org/10.48322/14fy-2640
ReleaseDate
2026-06-26 13:30:40Z
RevisionHistory
RevisionEvent
ReleaseDate
2020-07-07 21:15:49Z
Note
Only known prior ReleaseDate of the metadata
RevisionEvent
ReleaseDate
2025-11-14 16:02:58Z
Note
Added PublicationInfo. Added ResourceType and NamingAuthority. ZCB
RevisionEvent
ReleaseDate
2025-12-04 13:32:21Z
Note
Added MetadataRightsList and RightsList(s). Updated to 2.7.1. ZCB
RevisionEvent
ReleaseDate
2026-06-26 13:30:40Z
Note
Add 'Z' to TemporalDescription:TimeSpan:StartDate, TemporalDescription:TimeSpan:StopDate. ZCB
Description
This data set contains data and software for integral 0.5-second omnidirectional counting rates from the Ulysses Gamma Ray Burst
(GRB) experiment. It consists of count rates from the sum of two hemispherical detectors convering 4 pi steradians and operating continuously. The detectors
are 3 mm thick CsI scintillators coupled to photomultiplier tubes. The nominal energy range is 25-150 keV, but Table 1 (see below) should be consulted to find
the accurate thresholds for any day of the mission. A more complete description of the instrument may be found in Hurley et al. (1992) and Cotin et al. (1983).
Althoughthe prime objectives of this investigation are the study of solar and cosmic x- and gamma-ray bursts, it should be noted that the experiment is also
sensitive to solar protons and electrons. The former deposit energy directly in the scintillator if they are energetic enough, while the latter may produce x-
radiation locally by bremsstrahlung. Thus although the counting rates are generally stable at about 500 c/s over the long term, there are periods of
weeks to a month or so when the rates increase considerably due to particles. Examples may be found in March 1991 (solar protons) and February 1992
(particles in the Jovian magnetosphere).
The time resolution of the data takes on one of four values depending on the telemetry rate and instrument operating mode: 0.25, 0.5, 1, or 2 seconds. Data
rate changes produce short spikes in the count rates due to a processing artefact. These can in principle be corrected if the data are scanned and the
rate changes are identified; the count rate spikes can then be adjusted to their correct values. There are also short (one sample long) count rate
dropouts, due to an artefact of the onboard software. These may be seen in the sample plots; they cannot be corrected for.
Two figures give examples of solar and cosmic events in the data. The upper panel gives the count rates for day 142, 1993, around 8.24 hours UT. The solar event is evident as a 300 second long increase. Note the count rate dropouts. The bottom panel includes a 20 second long cosmic gamma-ray burst from day 237, 1993 around 8.79 hours UT.
Acknowledgement
Please acknowledge the Ulysses team and the National Space Science Data Center.
PublicationInfo
Authors
Hurley, Kevin C.
PublicationDate
2025-11-14 16:02:58Z
PublishedBy
Planetary Data System; Space Physics Data Facility; European Space Astronomy Centre
Contacts
Role
Person
StartDate
StopDate
Note
1.
DataProducer
spase://SMWG/Person/Roger.W.Williams
2.
PrincipalInvestigator
spase://SMWG/Person/Kevin.C.Hurley
InformationURL
Name
Readme file at SPDF
URL
https://spdf.gsfc.nasa.gov/pub/data/ulysses/gamma/grb_1sec/ULYGRB.FMT
PriorIDs
spase://VSPO/NumericalData/Ulysses/GRB_1sec
spase://VSPO/NumericalData/Ulysses/SCE/GRB/PT1S
AccessInformation
RepositoryID
spase://SMWG/Repository/NASA/GSFC/SPDF
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
FTPS from SPDF (not with most browsers)
URL
ftps://spdf.gsfc.nasa.gov/pub/data/ulysses/gamma/grb_1sec/
Description
Via ftp in ASCII from nssdcftp
AccessURL
Name
HTTPS from SPDF
URL
https://spdf.gsfc.nasa.gov/pub/data/ulysses/gamma/grb_1sec/
Description
Via http in ASCII from nssdcftp
Format
Text
InstrumentIDs
spase://SMWG/Instrument/Ulysses/SCE
MeasurementType
EnergeticParticles
TemporalDescription
TimeSpan
StartDate
1990-10-29 00:00:00Z
StopDate
2005-01-31 23:59:59Z
Cadence
PT1S
ObservedRegion
Heliosphere.Outer