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High Energy Interest group accepted by IVOA Executive committee - November 2024 Interoperability meeting
Chair: Bruno Khélifi (APC, Paris) Vice-chair: Janet Evans (Harvard CfA)
Charter:The group shall define requirements for the representation of high energy astrophysics data in the VO through:
Motivation:High energy astrophysics (HEA) typically includes X-ray astrophysics and gamma-ray astrophysics of the GeV range (HE), the TeV range (very high energy, VHE), up to the ultra high energy (UHE) above 100 TeV, VHE neutrino astrophysics, and studies of cosmic rays. High energy astrophysics has several domain-specific requirements that need to be fulfilled if HEA data is to be well-served by the VO. High energy astrophysics observations are based on techniques that are different compared to the optical or radio domains. HEA observatories are generally designed to detect particles, e.g., individual photons, cosmic rays, or neutrinos, with the ability to estimate several characteristics of those particles. This technique is generally named event counting where an event has some probability of being due to the interaction of an astrophysical particle with the detectors. The list of detected events is named an event list and these data sets are typically multi-dimensional and can simultaneously encode event position, time, and spectral information. Instrument Response Functions are required to map the physical properties of the source to the observables, and these mappings are probabilistic and typically not invertible, requiring more complex representations for data sets and their associated calibrations compared to (e.g.) optical data. The groups and projects that have expressed interest to be involved include current and future X-ray facilities, gamma-ray facilities, and neutrino observatories, as well as high energy astrophysics data archives:
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High Energy Interest Group (HEIG)Last updated - 26Nov24 | |||||||||||||||||||
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> > | High Energy Interest group accepted by IVOA Executive committee - November 2024 Interoperability meeting | ||||||||||||||||||
Chair: Bruno Khélifi (APC, Paris) Vice-chair: Janet Evans (Harvard CfA)
Charter:The group shall define requirements for the representation of high energy astrophysics data in the VO through:
Motivation:High energy astrophysics (HEA) typically includes X-ray astrophysics and gamma-ray astrophysics of the GeV range (HE), the TeV range (very high energy, VHE), up to the ultra high energy (UHE) above 100 TeV, VHE neutrino astrophysics, and studies of cosmic rays. High energy astrophysics has several domain-specific requirements that need to be fulfilled if HEA data is to be well-served by the VO. High energy astrophysics observations are based on techniques that are different compared to the optical or radio domains. HEA observatories are generally designed to detect particles, e.g., individual photons, cosmic rays, or neutrinos, with the ability to estimate several characteristics of those particles. This technique is generally named event counting where an event has some probability of being due to the interaction of an astrophysical particle with the detectors. The list of detected events is named an event list and these data sets are typically multi-dimensional and can simultaneously encode event position, time, and spectral information. Instrument Response Functions are required to map the physical properties of the source to the observables, and these mappings are probabilistic and typically not invertible, requiring more complex representations for data sets and their associated calibrations compared to (e.g.) optical data. The groups and projects that have expressed interest to be involved include current and future X-ray facilities, gamma-ray facilities, and neutrino observatories, as well as high energy astrophysics data archives:
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HE IG Goals:
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High Energy Interest Group (HEIG) | |||||||||||||||||||
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Charter:The group shall define requirements for the representation of high energy astrophysics data in the VO through:
Motivation:High energy astrophysics (HEA) typically includes X-ray astrophysics and gamma-ray astrophysics of the GeV range (HE), the TeV range (very high energy, VHE), up to the ultra high energy (UHE) above 100 TeV, VHE neutrino astrophysics, and studies of cosmic rays. High energy astrophysics has several domain-specific requirements that need to be fulfilled if HEA data is to be well-served by the VO. High energy astrophysics observations are based on techniques that are different compared to the optical or radio domains. HEA observatories are generally designed to detect particles, e.g., individual photons, cosmic rays, or neutrinos, with the ability to estimate several characteristics of those particles. This technique is generally named event counting where an event has some probability of being due to the interaction of an astrophysical particle with the detectors. The list of detected events is named an event list and these data sets are typically multi-dimensional and can simultaneously encode event position, time, and spectral information. Instrument Response Functions are required to map the physical properties of the source to the observables, and these mappings are probabilistic and typically not invertible, requiring more complex representations for data sets and their associated calibrations compared to (e.g.) optical data. The groups and projects that have expressed interest to be involved include current and future X-ray facilities, gamma-ray facilities, and neutrino observatories, as well as high energy astrophysics data archives:
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HEIG Group Meetings
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High Energy Interest Group (HEIG)Last updated - 15Nov24Charter:The group shall define requirements for the representation of high energy astrophysics data in the VO through:
Motivation:High energy astrophysics (HEA) typically includes X-ray astrophysics and gamma-ray astrophysics of the GeV range (HE), the TeV range (very high energy, VHE), up to the ultra high energy (UHE) above 100 TeV, VHE neutrino astrophysics, and studies of cosmic rays. High energy astrophysics has several domain-specific requirements that need to be fulfilled if HEA data is to be well-served by the VO. High energy astrophysics observations are based on techniques that are different compared to the optical or radio domains. HEA observatories are generally designed to detect particles, e.g., individual photons, cosmic rays, or neutrinos, with the ability to estimate several characteristics of those particles. This technique is generally named event counting where an event has some probability of being due to the interaction of an astrophysical particle with the detectors. The list of detected events is named an event list and these data sets are typically multi-dimensional and can simultaneously encode event position, time, and spectral information. Instrument Response Functions are required to map the physical properties of the source to the observables, and these mappings are probabilistic and typically not invertible, requiring more complex representations for data sets and their associated calibrations compared to (e.g.) optical data. The groups and projects that have expressed interest to be involved include current and future X-ray facilities, gamma-ray facilities, and neutrino observatories, as well as high energy astrophysics data archives:
Virtual Observatory and High Energy Astrophysics v1.0 - M. Servillat et al.
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High Energy Interest Group (HEIG)Last updated - 15Nov24Charter:The group shall define requirements for the representation of high energy astrophysics data in the VO through:
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Motivation:High energy astrophysics (HEA) typically includes X-ray astrophysics and gamma-ray astrophysics of the GeV range (HE), the TeV range (very high energy, VHE), up to the ultra high energy (UHE) above 100 TeV, VHE neutrino astrophysics, and studies of cosmic rays. High energy astrophysics has several domain-specific requirements that need to be fulfilled if HEA data is to be well-served by the VO. High energy astrophysics observations are based on techniques that are different compared to the optical or radio domains. HEA observatories are generally designed to detect particles, e.g., individual photons, cosmic rays, or neutrinos, with the ability to estimate several characteristics of those particles. This technique is generally named event counting where an event has some probability of being due to the interaction of an astrophysical particle with the detectors. The list of detected events is named an event list and these data sets are typically multi-dimensional and can simultaneously encode event position, time, and spectral information. Instrument Response Functions are required to map the physical properties of the source to the observables, and these mappings are probabilistic and typically not invertible, requiring more complex representations for data sets and their associated calibrations compared to (e.g.) optical data. The groups and projects that have expressed interest to be involved include current and future X-ray facilities, gamma-ray facilities, and neutrino observatories, as well as high energy astrophysics data archives:
Virtual Observatory and High Energy Astrophysics v1.0 - M. Servillat et al.
Participating Project Links (add your project and link)
HEIG Group Meetings
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High Energy Interest Group (HEIG)Last updated - 15Nov24Charter:The group shall define requirements for the representation of high energy astrophysics data in the VO through:
Motivation:High energy astrophysics (HEA) typically includes X-ray astrophysics and gamma-ray astrophysics of the GeV range (HE), the TeV range (very high energy, VHE), up to the ultra high energy (UHE) above 100 TeV, VHE neutrino astrophysics, and studies of cosmic rays. High energy astrophysics has several domain-specific requirements that need to be fulfilled if HEA data is to be well-served by the VO. High energy astrophysics observations are based on techniques that are different compared to the optical or radio domains. HEA observatories are generally designed to detect particles, e.g., individual photons, cosmic rays, or neutrinos, with the ability to estimate several characteristics of those particles. This technique is generally named event counting where an event has some probability of being due to the interaction of an astrophysical particle with the detectors. The list of detected events is named an event list and these data sets are typically multi-dimensional and can simultaneously encode event position, time, and spectral information. Instrument Response Functions are required to map the physical properties of the source to the observables, and these mappings are probabilistic and typically not invertible, requiring more complex representations for data sets and their associated calibrations compared to (e.g.) optical data. The groups and projects that have expressed interest to be involved include current and future X-ray facilities, gamma-ray facilities, and neutrino observatories, as well as high energy astrophysics data archives:
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High Energy Interest Group (HEIG)Last updated - 15Nov24Charter:The group shall define requirements for the representation of high energy astrophysics data in the VO through:
Motivation:High energy astrophysics (HEA) typically includes X-ray astrophysics and gamma-ray astrophysics of the GeV range (HE), the TeV range (very high energy, VHE), up to the ultra high energy (UHE) above 100 TeV, VHE neutrino astrophysics, and studies of cosmic rays. High energy astrophysics has several domain-specific requirements that need to be fulfilled if HEA data is to be well-served by the VO. High energy astrophysics observations are based on techniques that are different compared to the optical or radio domains. HEA observatories are generally designed to detect particles, e.g., individual photons, cosmic rays, or neutrinos, with the ability to estimate several characteristics of those particles. This technique is generally named event counting where an event has some probability of being due to the interaction of an astrophysical particle with the detectors. The list of detected events is named an event list and these data sets are typically multi-dimensional and can simultaneously encode event position, time, and spectral information. Instrument Response Functions are required to map the physical properties of the source to the observables, and these mappings are probabilistic and typically not invertible, requiring more complex representations for data sets and their associated calibrations compared to (e.g.) optical data. The groups and projects that have expressed interest to be involved include current and future X-ray facilities, gamma-ray facilities, and neutrino observatories, as well as high energy astrophysics data archives:
Virtual Observatory and High Energy Astrophysics v1.0 - M. Servillat et al.
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High Energy Interest Group (HEIG)Last updated - 15Nov24Charter:The group shall define requirements for the representation of high energy astrophysics data in the VO through:
Motivation:High energy astrophysics (HEA) typically includes X-ray astrophysics and gamma-ray astrophysics of the GeV range (HE), the TeV range (very high energy, VHE), up to the ultra high energy (UHE) above 100 TeV, VHE neutrino astrophysics, and studies of cosmic rays. High energy astrophysics has several domain-specific requirements that need to be fulfilled if HEA data is to be well-served by the VO. High energy astrophysics observations are based on techniques that are different compared to the optical or radio domains. HEA observatories are generally designed to detect particles, e.g., individual photons, cosmic rays, or neutrinos, with the ability to estimate several characteristics of those particles. This technique is generally named event counting where an event has some probability of being due to the interaction of an astrophysical particle with the detectors. The list of detected events is named an event list and these data sets are typically multi-dimensional and can simultaneously encode event position, time, and spectral information. Instrument Response Functions are required to map the physical properties of the source to the observables, and these mappings are probabilistic and typically not invertible, requiring more complex representations for data sets and their associated calibrations compared to (e.g.) optical data. The groups and projects that have expressed interest to be involved include current and future X-ray facilities, gamma-ray facilities, and neutrino observatories, as well as high energy astrophysics data archives:
Virtual Observatory and High Energy Astrophysics v1.0 - M. Servillat et al.
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Charter:The group shall define requirements for the representation of high energy astrophysics data in the VO through:
Motivation:High energy astrophysics (HEA) typically includes X-ray astrophysics and gamma-ray astrophysics of the GeV range (HE), the TeV range (very high energy, VHE), up to the ultra high energy (UHE) above 100 TeV, VHE neutrino astrophysics, and studies of cosmic rays. High energy astrophysics has several domain-specific requirements that need to be fulfilled if HEA data is to be well-served by the VO. | |||||||||||||||
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< < | High energy astrophysics observations are based on techniques that are radically different compared to the optical or radio domains. HEA observatories are generally designed to detect particles, e.g., individual photons, cosmic rays, or neutrinos, with the ability to estimate several characteristics of those particles. This technique is generally named event countingwhere an event has some probability of being due to the interaction of an astrophysical particle with the detectors. The list of detected events is named an event list and these data sets are typically multi-dimensional and can simultaneously encode event position, time, and spectral information. Instrument Response Functions are required to map the physical properties of the source to the observables, and these mappings are probabilistic and typically not invertible, requiring more complex representations for data sets and their associated calibrations compared to (e.g.) optical data. | ||||||||||||||
> > | High energy astrophysics observations are based on techniques that are different compared to the optical or radio domains. HEA observatories are generally designed to detect particles, e.g., individual photons, cosmic rays, or neutrinos, with the ability to estimate several characteristics of those particles. This technique is generally named event counting where an event has some probability of being due to the interaction of an astrophysical particle with the detectors. The list of detected events is named an event list and these data sets are typically multi-dimensional and can simultaneously encode event position, time, and spectral information. Instrument Response Functions are required to map the physical properties of the source to the observables, and these mappings are probabilistic and typically not invertible, requiring more complex representations for data sets and their associated calibrations compared to (e.g.) optical data. | ||||||||||||||
The groups and projects that have expressed interest to be involved include current and future X-ray facilities, gamma-ray facilities, and neutrino observatories, as well as high energy astrophysics data archives:
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> > | High energy astrophysics (HEA) typically includes X-ray astrophysics and gamma-ray astrophysics of the GeV range (HE), the TeV range (very high energy, VHE), up to the ultra high energy (UHE) above 100 TeV, VHE neutrino astrophysics, and studies of cosmic rays. High energy astrophysics has several domain-specific requirements that need to be fulfilled if HEA data is to be well-served by the VO. | ||||||||||||||
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> > | High energy astrophysics observations are based on techniques that are radically different compared to the optical or radio domains. HEA observatories are generally designed to detect particles, e.g., individual photons, cosmic rays, or neutrinos, with the ability to estimate several characteristics of those particles. This technique is generally named event countingwhere an event has some probability of being due to the interaction of an astrophysical particle with the detectors. The list of detected events is named an event list and these data sets are typically multi-dimensional and can simultaneously encode event position, time, and spectral information. Instrument Response Functions are required to map the physical properties of the source to the observables, and these mappings are probabilistic and typically not invertible, requiring more complex representations for data sets and their associated calibrations compared to (e.g.) optical data. | ||||||||||||||
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High Energy Interest Group (HEIG) PageOur meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects. Last updated - 25Sep24Membership - email alias "HEIG"~30 subscribers from major projects in the High Energy regime To be added to the email list, use the following link:Group Goals
DRAFT Note - Virtual Observatory and High Energy Astrophysics - M. Servillat
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High Energy Interest Group (HEIG) PageOur meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects. Last updated - 25Sep24Membership - email alias "HEIG"~30 subscribers from major projects in the High Energy regime To be added to the email list, use the following link:Group Goals
DRAFT Note - Virtual Observatory and High Energy Astrophysics - M. Servillat
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High Energy Interest Group (HEIG) PageOur meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects. Last updated - 25Sep24Membership - email alias "HEIG"~30 subscribers from major projects in the High Energy regime To be added to the email list, use the following link:Group Goals
DRAFT Note - Virtual Observatory and High Energy Astrophysics - M. Servillat
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High Energy Interest Group (HEIG) PageOur meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects. Last updated - 25Sep24Membership - email alias "HEIG"~30 subscribers from major projects in the High Energy regime To be added to the email list, use the following link:Group Goals
DRAFT Note - Virtual Observatory and High Energy Astrophysics - M. Servillat
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High Energy Interest Group (HEIG) PageOur meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects. Last updated - 25Sep24Membership - email alias "HEIG"~30 subscribers from major projects in the High Energy regime To be added to the email list, use the following link:Group Goals
DRAFT Note - Virtual Observatory and High Energy Astrophysics - M. Servillat
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High Energy Interest Group (HEIG) PageOur meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects. Last updated - 25Sep24Membership - email alias "HEIG"~30 subscribers from major projects in the High Energy regime To be added to the email list, use the following link:Group Goals
DRAFT Note - Virtual Observatory and High Energy Astrophysics - M. Servillat
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High Energy Interest Group (HEIG) PageOur meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects. | |||||||||||||
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High Energy Interest Group (HEIG) PageOur meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects. Last updated - 28Jun24Current EffortsDRAFT Note - Virtual Observatory and High Energy Astrophysics - M. Servillat
Collecting Obscore Use Cases for High EnergyWe're collecting Use Cases for HE data that falls outside of the Obscore basline; add your use cases to a list below
Collecting High Energy Plenary IdeasWe're collecting Plenary Ideas for the Malta meeting (Not 15-17); add your thoughts to a list below
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High Energy Interest Group (HEIG) PageOur meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects. Last updated - 28Jun24Current EffortsDRAFT Note - Virtual Observatory and High Energy Astrophysics - M. Servillat
Collecting Obscore Use Cases for High EnergyWe're collecting Use Cases for HE data that falls outside of the Obscore basline; add your use cases to a list below
Collecting High Energy Plenary IdeasWe're collecting Plenary Ideas for the Malta meeting (Not 15-17); add your thoughts to a list below
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High Energy Interest Group (HEIG) PageOur meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects. Last updated - 28Jun24Current EffortsDRAFT Note - Virtual Observatory and High Energy Astrophysics - M. Servillat
Collecting Obscore Use Cases for High EnergyWe're collecting Use Cases for HE data that falls outside of the Obscore basline; add your use cases to a list below
Collecting High Energy Plenary IdeasWe're collecting Plenary Ideas for the Malta meeting (Not 15-17); add your thoughts to a list below
Group upcoming Goals
Participating Project Links
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Current Membership - email alias "HEIG"
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High Energy Interest Group (HEIG) PageOur meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects. Last updated - 28Jun24Current EffortsDRAFT Note - Virtual Observatory and High Energy Astrophysics - M. Servillat
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Collecting Obscore Use Cases for High EnergyWe're collecting Use Cases for HE data that falls outside of the Obscore basline; add your use cases to a list below
Collecting High Energy Plenary IdeasWe're collecting Plenary Ideas for the Malta meeting (Not 15-17); add your thoughts to a list below
Group upcoming Goals
Participating Project Links
Meetings/Workshops/Presentations
Current Membership - email alias "HEIG"
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High Energy Interest Group (HEIG) PageOur meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects. Last updated - 28Jun24Current EffortsDRAFT Note - Virtual Observatory and High Energy Astrophysics - M. Servillat
Collecting Obscore Use Cases for High EnergyWe're collecting Use Cases for HE data that falls outside of the Obscore basline; add your use cases to a list below
Collecting High Energy Plenary IdeasWe're collecting Plenary Ideas for the Malta meeting (Not 15-17); add your thoughts to a list below
Group upcoming Goals
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High Energy Interest Group (HEIG) PageOur meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects. Last updated - 28Jun24Current Efforts | |||||||||||
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Collecting Obscore Use Cases for High EnergyWe're collecting Use Cases for HE data that falls outside of the Obscore basline; add your use cases to a list below
Collecting High Energy Plenary IdeasWe're collecting Plenary Ideas for the Malta meeting (Not 15-17); add your thoughts to a list below
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High Energy Interest Group (HEIG) PageOur meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects. Last updated - 28Jun24 | |||||||||||
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Current EffortsDRAFT Note - Virtual Observatory and High Energy Astrophysics - M. Servillat
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> > | Collecting High Energy Plenary IdeasWe're collecting Plenary Ideas for the Malta meeting (Not 15-17); add your thoughts to a list below
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High Energy Interest Group (HEIG) PageOur meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects. | |||||||||||
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DRAFT Note - Virtual Observatory and High Energy Astrophysics - M. Servillat
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High Energy Interest Group (HEIG) PageOur meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
Current EffortsDRAFT Note - Virtual Observatory and High Energy Astrophysics - M. Servillat
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< < | Our first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects. | |||||||
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High Energy Interest Group (HEIG) PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
Current EffortsDRAFT Note - Virtual Observatory and High Energy Astrophysics- M Servillat
Collecting Obscore Use Cases for High EnergyWe're collecting Use Cases for HE data that falls outside of the Obscore basline; add your use cases to a list below
Group upcoming Goals
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High Energy Interest Group (HEIG) PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
Current EffortsDRAFT Note - Virtual Observatory and High Energy Astrophysics- M Servillat
Collecting Obscore Use Cases for High EnergyWe're collecting Use Cases for HE data that falls outside of the Obscore basline; add your use cases to a list below
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High Energy Interest Group (HEIG) PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
Current EffortsDRAFT Note - Virtual Observatory and High Energy Astrophysics- M Servillat
Collecting Obscore Use Cases for High EnergyWe're collecting Use Cases for HE data that falls outside of the Obscore basline; add your use cases to a list below
Project Links
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High Energy Interest Group (HEIG) PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
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High Energy Interest Group (HEIG) PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
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High Energy Interest Group (HEIG) PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
Current DRAFT of HEIG Note to the IVOA - M Servillat
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High Energy Interest Group (HEIG) PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
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Current DRAFT of HEIG Note to the IVOA - M Servillat
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Event list formats for your project & Good time interval informationList the event list & GTI format for your data
Whether an Obscore extension for High Energy data should be consideredCurrent issues associated with Obscore for your project; What Keywords do you propose?? What data product is needed for High Energy data??Outline use cases to provide examples of interoperability issuesUse cases that are provide examples of issues ...Misc Links
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High Energy Interest Group (HEIG) PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
Current DRAFT of HEIG Note to the IVOA - M Servillat
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High Energy Interest Group (HEIG) PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
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High Energy Interest Group (HEIG) PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects. | ||||||||
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High Energy Interest Group (HEIG) PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
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Related workshops and presentations
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Event list formats for your project & Good time interval informationList the event list & GTI format for your data
Whether an Obscore extension for High Energy data should be consideredCurrent issues associated with Obscore for your project; What Keywords do you propose?? What data product is needed for High Energy data??Outline use cases to provide examples of interoperability issuesUse cases that are provide examples of issues ...Misc Links
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High Energy Interest Group (HEIG) PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
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< < | Our first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. This page is meant to be a place to identify and build synergy among the projects. | |||||||
> > | Our first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. We welcome all projects with a High Energy interest (e.g., X-ray, Gamma-Ray, Neutrino). This page is meant to be a place to identify and build synergy among the projects. | |||||||
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> > | What data product is needed for High Energy data?? | |||||||
Outline use cases to provide examples of interoperability issuesUse cases that are provide examples of issues ...Misc Links
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High Energy Interest Group (HEIG) PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
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High Energy Interest Group (HEIG) PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
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High Energy Interest Group (HEIG) PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
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Whether an Obscore extension for High Energy data should be consideredCurrent issues associated with Obscore for your project; What Keywords do you propose??Outline use cases to provide examples of interoperability issuesUse cases that are provide examples of issues ...Misc Links | ||||||||
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High Energy Interest Group (HEIG) PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
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Event list formats for your project & Good time interval informationList the event list & GTI format for your data Chandra Data Descriptions - Event list, GTIWhether an Obscore extension for High Energy data should be consideredCurrent issues associated with Obscore for your project; What Keywords do you propose??Outline use cases to provide examples of interoperability issuesUse cases that are provide examples of issues ...Misc Links |
High Energy Interest Group (HEIG) PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
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Event list formats for your project & Good time interval informationList the event list & GTI format for your data Chandra Data Descriptions - Event list, GTIWhether an Obscore extension for High Energy data should be consideredCurrent issues associated with Obscore for your project; What Keywords do you propose??Outline use cases to provide examples of interoperability issuesUse cases that are provide examples of issues ...Misc Links | ||||||||
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High Energy Interest Group (HEIG) PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
Project Links
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Event list formats for your project & Good time interval informationList the event list & GTI format for your data Chandra Data Descriptions - Event list, GTIWhether an Obscore extension for High Energy data should be consideredCurrent issues associated with Obscore for your project; What Keywords do you propose??Outline use cases to provide examples of interoperability issuesUse cases that are provide examples of issues ...Misc Links | ||||||||
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High Energy Interest Group (HEIG) PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
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Project Links
Event list formats for your project & Good time interval informationList the event list & GTI format for your data Chandra Data Descriptions - Event list, GTIWhether an Obscore extension for High Energy data should be consideredCurrent issues associated with Obscore for your project; What Keywords do you propose??Outline use cases to provide examples of interoperability issuesUse cases that are provide examples of issues ...Misc Links |
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> > | High Energy Interest Group (HEIG) Page | |||||||
Our first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. This page is meant to be a place to identify and build synergy among the projects.
Current Membership - email alias "HEIG"
Project Links
Event list formats for your project & Good time interval informationList the event list & GTI format for your data | ||||||||
Added: | ||||||||
> > | Chandra Data Descriptions - Event list, GTI | |||||||
Whether an Obscore extension for High Energy data should be consideredCurrent issues associated with Obscore for your project; What Keywords do you propose??Outline use cases to provide examples of interoperability issuesUse cases that are provide examples of issues ...Misc Links | ||||||||
Added: | ||||||||
> > |
High Energy Data Group PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
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> > |
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Project Links
Event list formats for your project & Good time interval informationList the event list & GTI format for your dataWhether an Obscore extension for High Energy data should be consideredCurrent issues associated with Obscore for your project; What Keywords do you propose??Outline use cases to provide examples of interoperability issuesUse cases that are provide examples of issues ...Misc Links |
High Energy Data Group PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
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> > |
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Project Links
Event list formats for your project & Good time interval informationList the event list & GTI format for your dataWhether an Obscore extension for High Energy data should be consideredCurrent issues associated with Obscore for your project; What Keywords do you propose??Outline use cases to provide examples of interoperability issuesUse cases that are provide examples of issues ...Misc Links | ||||||||
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< < |
High Energy Data Group PageOur first meeting at the May 2023 Interop in Bologna led to a informal group of High Energy project coordinating on topics related to IVOA support and usage. This page is meant to be a place to identify and build synergy among the projects.Current Membership - email alias "HEIG"
Project Links
Event list formats for your project & Good time interval informationList the event list & GTI format for your dataWhether an Obscore extension for High Energy data should be consideredCurrent issues associated with Obscore for your project; What Keywords do you propose??Outline use cases to provide examples of interoperability issuesUse cases that are provide examples of issues ...Misc Links |