From 1348af52150ae580b8b59dd25ee07781911cc0ce Mon Sep 17 00:00:00 2001 From: =?UTF-8?q?Bruno=20Kh=C3=A9lifi?= Date: Thu, 22 Aug 2024 11:59:09 +0200 Subject: [PATCH 1/4] Update HESS and CTA MIME-Version: 1.0 Content-Type: text/plain; charset=UTF-8 Content-Transfer-Encoding: 8bit Signed-off-by: Bruno Khélifi --- VOHE-Note.tex | 46 +++++++++++++++++++++++++++++++++------------- 1 file changed, 33 insertions(+), 13 deletions(-) diff --git a/VOHE-Note.tex b/VOHE-Note.tex index f18ac21..468ddbd 100644 --- a/VOHE-Note.tex +++ b/VOHE-Note.tex @@ -106,35 +106,55 @@ \section{High Energy observatories and experiments} %XMM use case scenario %Données attachées ? data link? -There are various observatories, either from ground- or space-based, that distribute high-energy data with different level of involvement in the VO. We list here the observatories currently represented in the VO HE group. There are also other observatories that are connected to the VO in some way, and may join the group discussions at IVOA. +There are various observatories, either from ground, space or deep-sea based, that distribute high-energy data with +different level of involvement in the VO. We list here the observatories currently represented in the VO HE group. +There are also other observatories that are connected to the VO in some way, and may join the group discussions at IVOA. \subsection{Gamma-ray programs} \subsubsection{CTAO} -The Cherenkov Telescope Array Observatory (CTAO) is the next generation ground-based instrument for gamma-ray astronomy at Very-High Energies (VHE). With tens of telescopes located in the northern and southern hemispheres, the CTAO will be the first open ground-based gamma-ray observatory and the world’s largest and most sensitive instrument to study high-energy phenomena in the Universe. -Building on the technology of current generation ground-based gamma-ray detectors (H.E.S.S., MAGIC and VERITAS), the CTAO will be between five and 10 times more sensitive and have unprecedented accuracy in its detection of high-energy gamma rays. +The Cherenkov Telescope Array Observatory (CTAO) is the next generation ground-based instrument for gamma-ray astronomy +at very high energies (VHE, 10GeV-100TeV). With tens of telescopes located in the northern (La Palma, Canary Island) +and southern (Chili) hemispheres, CTAO will be the first open ground-based VHE gamma-ray observatory and the world’s +largest and most sensitive instrument to study high-energy phenomena in the Universe. Built on the technology of current +generation ground-based gamma-ray detectors (e.g. H.E.S.S., MAGIC and VERITAS), CTAO will be between five and 10 times +more sensitive and have unprecedented accuracy in its detection of VHE gamma rays. -CTAO will distribute data as an open observatory, for the first time in this domain, with calls for proposals and publicly released data after a proprietary period. CTAO will ensure that the data provided will be FAIR: Findable, Accessible, Interoperable and Reusable, by following the FAIR Principles for data management \citep{Wilkinson2016}. In particular, because of the complex data processing and reconstruction step, the provision of provenance metadata for CTAO data has been a driver for the development of a provenance standard in Astronomy. +CTAO will distribute data as an open observatory, for the first time in this domain, with calls for proposals and +publicly released data after a proprietary period. CTAO will ensure that the provided data will be FAIR: Findable, +Accessible, Interoperable and Reusable, by following the FAIR Principles for data management \citep{Wilkinson2016}. +In particular, because of the complex data processing and reconstruction steps, the provision of provenance metadata +for CTAO data has been a driver for the development of a provenance standard in astronomy. -CTAO will also ensure VO compatibility of the distributed data and access systems. CTAO participated to the ESCAPE European Project, and is now part of the ESCAPE Open Collaboration to face common challenges for Research Infrastructure in the context of cloud computing, including data analysis and distribution. +CTAO will also ensure VO compatibility of the distributed data and access systems. CTAO participated to the ESCAPE +European Project, and is now part of the ESCAPE Open Collaboration to face common challenges for Research Infrastructures +in the context of cloud computing, including data analysis and distribution. -A focus of CTAO is to distribute in this context their Data Level 3 (DL3) datasets, that correspond to lists of Cherenkov events detected by the telescopes along with the proper IRFs. CTAO is planning an internal and a public Science Data Challenge, which represent opportunities to build "VO inside" solutions. +A focus of CTAO is to distribute in this context their Data Level 3 (DL3) datasets, that correspond to lists of Cherenkov +events detected by the telescopes along with the proper IRFs. CTAO is planning an internal and a public Science Data +Challenges, which represent opportunities to build "VO inside" solutions. \subsubsection{H.E.S.S} \label{sec:hess} -H.E.S.S. is a system of Imaging Atmospheric Cherenkov Telescopes located in Namibia that investigates cosmic gamma rays in the energy range from 10s of GeV to 100s of TeV. It is constituted of four telescopes officially inaugurated in 2004, and a much larger fifth telescope operational since 2012, extending the energy coverage towards lower energies and further improving sensitivity. +The High Energy Steresopic System (H.E.S.S.) experiment is an array of Imaging Atmospheric Cherenkov Telescopes (IACT) +located in Namibia that investigates cosmic gamma rays in the energy range from 10s of GeV to 100s of TeV. It is +constituted of four telescopes officially inaugurated in 2004, and a much larger fifth telescope operational since 2012, +extending the energy coverage towards lower energies and further improving sensitivity. -The H.E.S.S. collaboration operates the telescopes as a private experiment and published mainly high level data, i.e. images, time series and spectra in scientific publications after dedicated analyses. +The H.E.S.S. collaboration operates the telescopes as a private experiment and publishes mainly high level data, +i.e. images, time series and spectra in scientific publications after dedicated analyses. -In September 2018, the H.E.S.S. Collaboration has, for the first time and unique time, released a small subset of its archival data in Flexible Image Transport System (FITS) format, an open file format widely used in astronomy. The release consists of Cherenkov event-lists and IRFs for observations of various well-known gamma-ray sources +In September 2018, the H.E.S.S. collaboration has, for the first time and unique time, released a small subset of its +archival data in Flexible Image Transport System (FITS) format, an open file format widely used in astronomy. The release +consists of Cherenkov event-lists and IRFs for observations of various well-known gamma-ray sources \citep{hess-zenodo.1421098}. -This test data collection has been registered in the VO via a TAP service hosted at the Observatoire de Paris, with a tentative ObsCore description of each dataset. We hope that in the future, the H.E.S.S. legacy archive will be published in a similar way and accessible through the VO. - - +This test data collection has been registered in the VO via a TAP service hosted at the Observatoire de Paris, with a +tentative ObsCore description of each dataset. We hope that, in the future, the H.E.S.S. legacy archive will be published +in a similar way and accessible through the VO. \subsection{X-ray programs} @@ -177,7 +197,7 @@ \subsection{KM3Net and neutrino detection} -%\subsection{Gravitational wave detection} +\subsection{Some other experiments} From edb334be323bfb6450b751b914dd3297b05a754b Mon Sep 17 00:00:00 2001 From: =?UTF-8?q?Bruno=20Kh=C3=A9lifi?= Date: Thu, 22 Aug 2024 15:41:09 +0200 Subject: [PATCH 2/4] Add Gammapy references MIME-Version: 1.0 Content-Type: text/plain; charset=UTF-8 Content-Transfer-Encoding: 8bit Signed-off-by: Bruno Khélifi --- VOHE-Note.bib | 32 +++++++++++++++++++++++--------- 1 file changed, 23 insertions(+), 9 deletions(-) diff --git a/VOHE-Note.bib b/VOHE-Note.bib index 6c6fbe2..bc399f1 100644 --- a/VOHE-Note.bib +++ b/VOHE-Note.bib @@ -12,6 +12,7 @@ @misc{hess-zenodo.1421098 year = {2018}, copyright = {Open Access} } + %reproducible analysis @ARTICLE{2019A&A...625A..10N, author = {{Nigro}, C. and {Deil}, C. and {Zanin}, R. and {Hassan}, T. and {King}, J. and {Ruiz}, J.~E. and {Saha}, L. and {Terrier}, R. and {Br{\"u}gge}, K. and {N{\"o}the}, M. and {Bird}, R. and {Lin}, T.~T.~Y. and {Aleksi{\'c}}, J. and {Boisson}, C. and {Contreras}, J.~L. and {Donath}, A. and {Jouvin}, L. and {Kelley-Hoskins}, N. and {Khelifi}, B. and {Kosack}, K. and {Rico}, J. and {Sinha}, A.}, @@ -54,8 +55,6 @@ @INPROCEEDINGS{2017AIPC.1792g0006D adsnote = {Provided by the SAO/NASA Astrophysics Data System} } - - @article{2021-DF, title={Evolution of Data Formats in Very-High-Energy Gamma-Ray Astronomy}, volume={7}, ISSN={2218-1997}, @@ -87,13 +86,6 @@ @ARTICLE{2022A&A...667A..36A adsnote = {Provided by the SAO/NASA Astrophysics Data System} } - - -%OGIP -%GADF - -% a trier -% ex provenance paper @INPROCEEDINGS{2019ASPC..523..313B, author = {{Bonnarel}, Fran{\c{c}}ois and {Louys}, M. and {Mantelet}, G. and {Nullmeier}, M. and {Servillat}, M. and {Riebe}, K. and {Sanguillon}, M.}, title = "{ProvTAP: A TAP Service for Providing IVOA Provenance Metadata}", @@ -145,3 +137,25 @@ @misc{unbehaun2023prospects archivePrefix={arXiv}, primaryClass={astro-ph.HE} } + +% Gammapy +@article{gammapy:2023, + author = {{Donath}, Axel and {Terrier}, R\'egis and {Remy}, Quentin and {Sinha}, Atreyee and {Nigro}, Cosimo and + {Pintore}, Fabio and {Kh\'elifi}, Bruno and {Olivera-Nieto}, Laura and {Ruiz}, Jose Enrique and + {Br\"ugge}, Kai and {Linhoff}, Maximilian and {Contreras}, Jose Luis and {Acero}, Fabio and + {Aguasca-Cabot}, Arnau and {Berge}, David and {Bhattacharjee}, Pooja and {Buchner}, Johannes and + {Boisson}, Catherine and {Carreto Fidalgo}, David and {Chen}, Andrew and {de Bony de Lavergne}, Mathieu and + {de Miranda Cardoso}, Jos\'e Vinicius and {Deil}, Christoph and {F\"u\ss{}ling}, Matthias and + {Funk}, Stefan and {Giunti}, Luca and {Hinton}, Jim and {Jouvin}, L\'ea and {King}, Johannes and + {Lefaucheur}, Julien and {Lemoine-Goumard}, Marianne and {Lenain}, Jean-Philippe and {L\'opez-Coto}, Rub\'en + and {Mohrmann}, Lars and {Morcuende}, Daniel and {Panny}, Sebastian and {Regeard}, Maxime and {Saha}, Lab + and {Siejkowski}, Hubert and {Siemiginowska}, Aneta and {Sip"ocz}, Brigitta M. and {Unbehaun}, Tim + and {van Eldik}, Christopher and {Vuillaume}, Thomas and {Zanin}, Roberta}, + title = {Gammapy: A Python package for gamma-ray astronomy}, + DOI= "10.1051/0004-6361/202346488", + url= "https://doi.org/10.1051/0004-6361/202346488", + journal = {A&A}, + year = 2023, + volume = 678, + pages = "A157", +} \ No newline at end of file From 66eb4ccb194896b90c236bc703cb282cbee98143 Mon Sep 17 00:00:00 2001 From: =?UTF-8?q?Bruno=20Kh=C3=A9lifi?= Date: Thu, 22 Aug 2024 15:41:43 +0200 Subject: [PATCH 3/4] subsections update and text improvements MIME-Version: 1.0 Content-Type: text/plain; charset=UTF-8 Content-Transfer-Encoding: 8bit Signed-off-by: Bruno Khélifi --- VOHE-Note.tex | 144 ++++++++++++++++++++++++++++++++++---------------- 1 file changed, 99 insertions(+), 45 deletions(-) diff --git a/VOHE-Note.tex b/VOHE-Note.tex index 468ddbd..a6c9dc0 100644 --- a/VOHE-Note.tex +++ b/VOHE-Note.tex @@ -113,10 +113,41 @@ \section{High Energy observatories and experiments} \subsection{Gamma-ray programs} +\subsubsection{H.E.S.S} +\label{sec:hess} + +The High Energy Steresopic System (H.E.S.S.) experiment is an array of Imaging Atmospheric Cherenkov Telescopes (IACT) +located in Namibia that investigates cosmic very high energies (VHE) gamma rays in the energy range from 10s of GeV to +100 of TeV. It is constituted of four telescopes officially inaugurated in 2004, and a much larger fifth telescope +operational since 2012, extending the energy coverage towards lower energies and further improving sensitivity. + +The H.E.S.S. collaboration operates the telescopes as a private experiment and publishes mainly high level data, +i.e. images, time series and spectra in scientific publications after dedicated analyses. Using complex algorithms, +private software process the raw data by applying calibration, reconstructing event properties from their Cherenkov +images and purifying the event list by removing as much as possible events induced by atmospheric cosmic rays (CRs). Even +after this purification, events are largely generated by CRs and statistical analyses are required to derive +the astrophysical source properties. To derive them from the event lists, models of background due to the remaining CRs +(generally generated from real observations) are used with the gamma-ray IRFs (PSF, Energy Dispersion, Collection Area) +that are generated by extensive Monte Carlo simulations. These 4 IRFs (background, PSF, Edisp, CollArea) are computed +for each observation of \sim~30min and are valid for the field of view. They depend on true energies, positions in the +field of view and sometimes from event classification types. The derivation of astrophysical quantities from +the event lists are now using open libraries, in particular the reference library Gammapy \ref{gammapy:2023}. +%% Need to describe the IRFs like for Chandra? + +In September 2018, the H.E.S.S. collaboration has, for the first time and unique time, released a small subset of its +archival data using the GADF format (\S~\ref{sec:gadf}) serialized into the Flexible Image Transport System (FITS) format, +an open file format widely used in astronomy. The release consists of Cherenkov event-lists and IRFs for observations of +various well-known gamma-ray sources \citep{hess-zenodo.1421098}. + +This test data collection has been registered in the VO via a TAP service hosted at the Observatoire de Paris, with a +tentative ObsCore description of each dataset. We hope that, in the future, the H.E.S.S. legacy archive will be published +in a similar way and accessible through the VO. + \subsubsection{CTAO} +\label{sec:ctao} -The Cherenkov Telescope Array Observatory (CTAO) is the next generation ground-based instrument for gamma-ray astronomy -at very high energies (VHE, 10GeV-100TeV). With tens of telescopes located in the northern (La Palma, Canary Island) +The Cherenkov Telescope Array Observatory (CTAO) is the next generation ground-based IACT instrument for gamma-ray astronomy +at very high energies. With tens of telescopes located in the northern (La Palma, Canary Island) and southern (Chili) hemispheres, CTAO will be the first open ground-based VHE gamma-ray observatory and the world’s largest and most sensitive instrument to study high-energy phenomena in the Universe. Built on the technology of current generation ground-based gamma-ray detectors (e.g. H.E.S.S., MAGIC and VERITAS), CTAO will be between five and 10 times @@ -135,51 +166,68 @@ \subsubsection{CTAO} A focus of CTAO is to distribute in this context their Data Level 3 (DL3) datasets, that correspond to lists of Cherenkov events detected by the telescopes along with the proper IRFs. CTAO is planning an internal and a public Science Data Challenges, which represent opportunities to build "VO inside" solutions. +%% Need to describe the IRFs like for Chandra? -\subsubsection{H.E.S.S} -\label{sec:hess} - -The High Energy Steresopic System (H.E.S.S.) experiment is an array of Imaging Atmospheric Cherenkov Telescopes (IACT) -located in Namibia that investigates cosmic gamma rays in the energy range from 10s of GeV to 100s of TeV. It is -constituted of four telescopes officially inaugurated in 2004, and a much larger fifth telescope operational since 2012, -extending the energy coverage towards lower energies and further improving sensitivity. - -The H.E.S.S. collaboration operates the telescopes as a private experiment and publishes mainly high level data, -i.e. images, time series and spectra in scientific publications after dedicated analyses. - -In September 2018, the H.E.S.S. collaboration has, for the first time and unique time, released a small subset of its -archival data in Flexible Image Transport System (FITS) format, an open file format widely used in astronomy. The release -consists of Cherenkov event-lists and IRFs for observations of various well-known gamma-ray sources -\citep{hess-zenodo.1421098}. - -This test data collection has been registered in the VO via a TAP service hosted at the Observatoire de Paris, with a -tentative ObsCore description of each dataset. We hope that, in the future, the H.E.S.S. legacy archive will be published -in a similar way and accessible through the VO. +The CTAO observatory is complementary to other gamma-ray instruments observing the sky up to ultra high energies (ie PeV). +Detecting directly from ground secondary charged particles of extensive air showers initiated by gamma rays, Water +Cherenkov Detectors (WCD) survey the whole observable sky above the TeV/tens of TeV energy range. The HAWC and LHAASO +detectors are running in the northern hemisphere and the future SWGO observatory will be installed in the southern +hemisphere. Such instruments have similar high-level data structures and it has been already demonstrated that joined +analyses with Gammapy of data from IACTs and WCDs using the GADF format are very powerful \ref{2022A&A...667A..36A}. \subsection{X-ray programs} \subsubsection{Chandra}\label{sec:chandra} -Part of NASA's fleet of ``Great Observatories'', the Chandra X-ray Observatory (CXO) was launched in 1999 to observe the soft X-ray universe in the 0.1 to 10 keV energy band. Chandra is a guest observer, pointed-observation mission and obtains roughly 800 observations per year using the Advanced CCD Imaging Spectrometer (ACIS) and High Resolution Camera (HRC) instruments. Chandra provides high angular resolution with a sub-arcsecond on-axis point spread function (PSF), a field of view up to several hundred square arcminutes, and a low instrumental background. The Chandra PSF varies with X-ray energy and significantly with off-axis angle, increasing to R50 $\sim$25 arcsec at the edge of the field of view. A pair of transmission gratings can be inserted into the X-ray beam to provide dispersed spectra with E/DeltaE $\sim$1000 for bright sources. -The Chandra spacecraft normally dithers in a Lissajous pattern on the sky while taking data, and this motion must be removed from the time-resolved X-ray event lists when constructing X-ray images using the motion of optical guide stars tracked by the Aspect camera. - -The Chandra X-ray Center (CXC) processes the spacecraft data through a set of Standard Data Processing Level 0 through Level 2 pipelines. These pipelines perform numerous steps including decommutating the telemetry data, applying instrument calibrations (e.g., detector geometric, time- dependent gain, and CCD charge transfer efficiency [CTI] corrections, bad and hot pixel flagging), computing and applying the time-resolved Aspect solution to de-dither the motion of the telescope, identifying good time intervals (GTIs), and finally filtering out bad times and X-ray events with bad status. All data products are archived in the Chandra Data Archive (CDA) in FITS format following HEASARC OGIP standards; see also \S~\ref{sec:ogip}. The CDA manages the proprietary data period (currently 6 months, after which the data become public) and provides dedicated interactive and IVOA-compliant interfaces to locate and download datasets. - -The CXC also provides the Chandra Source Catalog, which in the latest release (2.1) includes data for $\sim$407K unique X-ray sources on the sky and more than 2.1 million individual detections and photometric upper limits. For each X-ray source and detection, the catalog provides a detailed set of more than 100 tabulated positional, spatial, photometric, spectral, and temporal properties. An extensive selection of individual observation, stacked-observation, detection region, and master source FITS data products (e.g., RMFs, ARFs, PSFs, spectra, light curves, aperture photometry MPDFs) are also provided that are directly usable for further detailed scientific analysis. - -Finally, the CXC distributes the CIAO data analysis package to allow users to recalibrate and analyze their data. A key aspect of CIAO is to provide users the ability to create instrument responses (RMFs, ARFs, PSFs, instrument and exposure maps, etc.) for their observations using their choice of spectral models and weightings. The Sherpa modeling and fitting package supports N-dimensional model fitting and optimization in Python, and supports advanced Bayesian Markov chain Monte Carlo analyses. - +Part of NASA's fleet of ``Great Observatories'', the Chandra X-ray Observatory (CXO) was launched in 1999 to observe +the soft X-ray universe in the 0.1 to 10 keV energy band. Chandra is a guest observer, pointed-observation mission and +obtains roughly 800 observations per year using the Advanced CCD Imaging Spectrometer (ACIS) and High Resolution Camera +(HRC) instruments. Chandra provides high angular resolution with a sub-arcsecond on-axis point spread function (PSF), +a field of view up to several hundred square arcminutes, and a low instrumental background. The Chandra PSF varies with +X-ray energy and significantly with off-axis angle, increasing to R50 $\sim$25 arcsec at the edge of the field of view. +A pair of transmission gratings can be inserted into the X-ray beam to provide dispersed spectra with E/DeltaE $\sim$1000 +for bright sources. The Chandra spacecraft normally dithers in a Lissajous pattern on the sky while taking data, and +this motion must be removed from the time-resolved X-ray event lists when constructing X-ray images using the motion +of optical guide stars tracked by the Aspect camera. + +% Are the analysis step description made below in necessary? for the homogenity between instruments +The Chandra X-ray Center (CXC) processes the spacecraft data through a set of Standard Data Processing Level 0 through +Level 2 pipelines. These pipelines perform numerous steps including decommutating the telemetry data, +applying instrument calibrations (e.g., detector geometric, time- dependent gain, and CCD charge transfer efficiency +(CTI) corrections, bad and hot pixel flagging), computing and applying the time-resolved Aspect solution to de-dither +the motion of the telescope, identifying good time intervals (GTIs), and finally filtering out bad times and X-ray events +with bad status. All data products are archived in the Chandra Data Archive (CDA) in FITS format following HEASARC +OGIP standards; see also \S~\ref{sec:ogip}. The CDA manages the proprietary data period (currently 6 months, after +which the data become public) and provides dedicated interactive and IVOA-compliant interfaces to locate and download +datasets. + +The CXC also provides the Chandra Source Catalog, which in the latest release (2.1) includes data for $\sim$407K unique +X-ray sources on the sky and more than 2.1 million individual detections and photometric upper limits. For each X-ray +source and detection, the catalog provides a detailed set of more than 100 tabulated positional, spatial, photometric, +spectral, and temporal properties. An extensive selection of individual observation, stacked-observation, detection +region, and master source FITS data products (e.g., RMFs, ARFs, PSFs, spectra, light curves, aperture photometry MPDFs) +are also provided that are directly usable for further detailed scientific analysis. + +% According to https://heasarc.gsfc.nasa.gov/docs/heasarc/caldb/docs/memos/cal_gen_92_002/cal_gen_92_002.html#tth_sEc2.1, +% RMF, ARF and PSF does not depend on spectral models +Finally, the CXC distributes the CIAO data analysis package to allow users to recalibrate and analyze their data. A key +aspect of CIAO is to provide users the ability to create instrument responses (RMFs, ARFs, PSFs, etc) for their +observations. The Sherpa modeling and fitting package supports N-dimensional model fitting and optimization in Python, +and supports advanced Bayesian Markov chain Monte Carlo analyses. \subsubsection{XMM-Newton} -The European Space Agency's (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched in 1999. XMM-Newton is ESA's second cornerstone of the Horizon 2000 Science Program. It carries 3 high throughput X-ray telescopes with an unprecedented effective area, and an optical monitor, dedicated to the study of celestial X-ray sources. +The European Space Agency's (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched in 1999. XMM-Newton is ESA's +second cornerstone of the Horizon 2000 Science Program. It carries 3 high throughput X-ray telescopes with an +unprecedented effective area, and an optical monitor, dedicated to the study of celestial X-ray sources. \todo[inline]{To be completed: XMM catalogs, data... and VO access.} \subsubsection{SVOM} -The SVOM mission (Space-based multi-band astronomical Variable Objects Monitor) is a Franco-Chinese mission dedicated to the study of the most distant explosions of stars, the gamma-ray bursts. It is to be launched in 2024. +The SVOM mission (Space-based multi-band astronomical Variable Objects Monitor) is a Franco-Chinese mission dedicated +to the study of the most distant explosions of stars, the gamma-ray bursts. It is to be launched in 2024. \todo[inline]{To be completed} @@ -187,19 +235,25 @@ \subsubsection{SVOM} \subsection{KM3Net and neutrino detection} -The KM3NeT neutrino detectors are an array of water-based Cherenkov detectors currently under construction in the deep Mediterranean Sea. With its two sites off the French and Italian coasts the KM3NeT collaboration aims at single particle neutrino detection for neutrino physics with the more densely instrumented ORCA detector in the GeV to TeV range, and high-energy astrophysics with the ARCA detector in the TeV range and above. - -Using Earth as a shield from atmospheric particle interference by searching for upgoing particle tracks in the detectors, the measurement of astrophysical neutrinos can be performed almost continuously for a wide field of view that covers the full visible sky. For these particle events, extensive Monte Carlo simulations are performed to evaluate the statistical significance towards the various theoretical assumptions for galactic or cosmic neutrino signals. - -During the construction phase, the KM3NeT collaboration develops its interfaces for open science and builds on the data gathered by its predecessor ANTARES, from which neutrino event lists have already been published on the KM3NeT VO server as TAP service. However, reproducibility of the searches for point-like sources require information derived from simulations like background estimate, point spread function and detector acceptance which require linking to the actual event list and interpretation for a given observation, usually as neutrino flux limits for non-significant detection attributable to background rather than an observation. - -With multiple detectors targeting high-energy neutrinos like IceCube, ANTARES, KM3NeT, Baikal and future projects, the chance to detect a significant amount of cosmic and galactic neutrinos increases, requiring an integrated approach to link event lists with instrument responses and to correctly interpret observation time and flux expectations. - - - -\subsection{Some other experiments} - - +The KM3NeT neutrino detectors are arrays of water-based Cherenkov detectors currently under construction in the deep +Mediterranean Sea. With its two sites off the French and Italian coasts, the KM3NeT collaboration aims at single particle +neutrino detection for neutrino physics with the more densely instrumented ORCA detector in the GeV to TeV range, and +VHE astrophysics with the ARCA detector in the TeV range and above. + +Using Earth as a shield from atmospheric particle interference by searching for upgoing particle tracks in the detectors, +the measurement of astrophysical neutrinos can be performed almost continuously for a wide field of view that covers the +full visible sky. For these particle events, extensive Monte Carlo simulations are performed to evaluate the +statistical significance towards the various theoretical assumptions for galactic or cosmic neutrino signals. + +During the construction phase, the KM3NeT collaboration develops its interfaces for open science and builds on the data +gathered by its predecessor ANTARES, from which neutrino event lists have already been published on the KM3NeT VO server +as TAP service. However, {\bf reproducibility of the searches for point-like sources -> computation of astrophysical quantities} +require information derived from simulations like background estimate, PSF and detector acceptance which require linking +to the actual event list and interpolation for a given observation. + +With multiple detectors targeting high-energy neutrinos like IceCube, ANTARES, KM3NeT, Baikal and future projects, the +chance to detect a significant amount of cosmic and galactic neutrinos increases, requiring an integrated approach to +link event lists with instrument responses and to correctly interpret observation time and flux expectations. % mireille : what is specific for the community in terms of data interpretation and computation steps From 44e0ca0a23cd9ab579bbe9eb44cddd1600d91e14 Mon Sep 17 00:00:00 2001 From: =?UTF-8?q?Bruno=20Kh=C3=A9lifi?= Date: Mon, 26 Aug 2024 16:03:58 +0200 Subject: [PATCH 4/4] Fix typo --- VOHE-Note.tex | 2 +- 1 file changed, 1 insertion(+), 1 deletion(-) diff --git a/VOHE-Note.tex b/VOHE-Note.tex index a6c9dc0..fb7a3c1 100644 --- a/VOHE-Note.tex +++ b/VOHE-Note.tex @@ -129,7 +129,7 @@ \subsubsection{H.E.S.S} the astrophysical source properties. To derive them from the event lists, models of background due to the remaining CRs (generally generated from real observations) are used with the gamma-ray IRFs (PSF, Energy Dispersion, Collection Area) that are generated by extensive Monte Carlo simulations. These 4 IRFs (background, PSF, Edisp, CollArea) are computed -for each observation of \sim~30min and are valid for the field of view. They depend on true energies, positions in the +for each observation of $\sim$~30min and are valid for the field of view. They depend on true energies, positions in the field of view and sometimes from event classification types. The derivation of astrophysical quantities from the event lists are now using open libraries, in particular the reference library Gammapy \ref{gammapy:2023}. %% Need to describe the IRFs like for Chandra?