Difference: HEGroup (41 vs. 42)

Revision 422024-11-14 - JanetEvans

 
META TOPICPARENT name="IvoaSciencePriorities"
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High Energy Interest Group (HEIG) Page

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High Energy Interest Group (HEIG)

 
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<		Our 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.
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>		Last updated - 14Nov24
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Charter:

 
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<		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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>		The group shall define requirements for the representation of high energy astrophysics data in the VO through:
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  • development of use cases for data discovery, access and visualization;
  • identification of metadata concepts needed by high energy astrophysics data that are not currently supported by the VO;
  • the group will provide a well identified point of contact for high energy astrophysics projects with IVOA, and actively encourage their use of VO standards and protocols;
  • the group will organize sessions focused on high energy astrophysics data at IVOA meetings.

Motivation:

 
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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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Membership - email alias "HEIG"

 
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>		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:
  • Chandra X-ray Observatory;
  • XMM-Newton;
  • Space-based multi-band astronomical Variable Objects Monitor (SVOM);
  • High-Energy Stereoscopic System (HESS);
  • Cherenkov Telescope Array Observatory (CTAO);
  • KM3NeT;
  • NASA High Energy Astrophysics Science Archive Research Center (HEASARC).
By providing the necessary standards, the IVOA can help to ensure that VO protocols can support further developments in the high energy astrophysics community and enable interoperability and data discovery both within high energy astrophysics and between high energy astrophysics and other wavelengths.

Membership - email alias "HEIG"

 ~30 subscribers from major projects in the High Energy regime

To be added to the email list, use the following link:

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Group Goals

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Virtual Observatory and High Energy Astrophysics V1.0 - M. Servillat et al

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  • Connect with IVOA - send an email to IVOA mail group on timeframe of a DRAFT HE Note welcoming participation/feedback to doc
  • Plan to request new IVOA HE IG at Fall Interop in Malta; also planning for a Plenary in coordination with CSP
  • Complete HEIG Note - In progress: see link below

DRAFT Note - Virtual Observatory and High Energy Astrophysics - M. Servillat

 
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Participating Project Links (add your project and link)

HEIG Group Meetings

META FILEATTACHMENT attachment="HEIG_Cube_Review.pdf" attr="" comment="Presentation slides from 20230914 meeting." date="1694785679" name="HEIG_Cube_Review.pdf" path="HEIG_Cube_Review.pdf" size="785863" user="MarkCresitelloDittmar" version="1"
META FILEATTACHMENT attachment="2023-12-20_IVOA_Note___VO_for_High_Energy_astrophysics.pdf" attr="" comment="" date="1715811297" name="2023-12-20_IVOA_Note___VO_for_High_Energy_astrophysics.pdf" path="2023-12-20_IVOA_Note___VO_for_High_Energy_astrophysics.pdf" size="350529" user="MathieuServillat" version="1"
META FILEATTACHMENT attachment="2023-11-10_IVOA_Note___VO_for_High_Energy_astrophysics.pdf" attr="" comment="" date="1715811323" name="2023-11-10_IVOA_Note___VO_for_High_Energy_astrophysics.pdf" path="2023-11-10_IVOA_Note___VO_for_High_Energy_astrophysics.pdf" size="329059" user="MathieuServillat" version="1"
META FILEATTACHMENT attachment="2024-01-31_VOHE-Note-draft.pdf" attr="" comment="" date="1715811445" name="2024-01-31_VOHE-Note-draft.pdf" path="2024-01-31_VOHE-Note-draft.pdf" size="449701" user="MathieuServillat" version="1"
META FILEATTACHMENT attachment="2024-05-16_VOHE-Note-draft.pdf" attr="" comment="" date="1716183463" name="2024-05-16_VOHE-Note-draft.pdf" path="2024-05-16_VOHE-Note-draft.pdf" size="467016" user="MathieuServillat" version="1"
META FILEATTACHMENT attachment="2024-08-30_VOHE-Note-draft.pdf" attr="" comment="" date="1725280896" name="2024-08-30_VOHE-Note-draft.pdf" path="2024-08-30_VOHE-Note-draft.pdf" size="488953" user="MathieuServillat" version="1"
META FILEATTACHMENT attachment="2024-09-27_VOHE-Note-draft.pdf" attr="" comment="" date="1729601545" name="2024-09-27_VOHE-Note-draft.pdf" path="2024-09-27_VOHE-Note-draft.pdf" size="542655" user="MathieuServillat" version="1"
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