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7 results for “CTAO”
CTAO Simulation Telescope Models for CORSIKA and sim_telarray - Prod6
<p>The <a href="https://www.cta-observatory.org/">Cherenkov Telescope Array Observatory</a> (CTAO) is the next-generation gamma-ray observatory under construction on the island of La Palma (Spain) and near Paranal (Chile). CTAO will cover a wide energy range and provide substantial improvements in sensitivity, angular resolution and energy resolution in comparison to any existing gamma-ray detector. Detailed Monte Carlo simulations enable the optimization of the instrument configuration and the estimation of observatory performance using realistic models of the telescope design. The CORSIKA air-shower simulation code and the sim_telarray code for simulation of arrays of Cherenkov telescopes are used for all CTAO Monte Carlo simulation productions.</p> <p>This repository provides access to the simulation configuration describing the site parameters and the telescope simulation models required for the generation of the CTAO Instrument Response Functions based on the Prod6 observatory model (to be published).</p> <p>In detail, these are:</p> <ul> <li>telescope simulation models for each telescope type (Prod6 includes models for large-size, medium-size, and small-size telescopes)</li> <li>CORSIKA input files defining (among others) site atmosphere, telescope positions, and interaction models;</li> <li>execution scripts required to run CORSIKA and sim_telarray.</li> </ul> <p>The CORSIKA air-shower simulation code is available from the Institute for Astroparticle Physics (KIT), see <a href="https://www.iap.kit.edu/corsika/index.php" target="_blank" rel="noopener">CORSIKA website</a>. The sim_telarray telescope simulation program, auxilliary libraries, and common configuration files are available at the <a href="https://www.mpi-hd.mpg.de/hfm/~bernlohr/sim_telarray/" target="_blank" rel="noopener">sim_telarray website</a>, with an up-to-date interface to CORSIKA at the <a href="https://www.mpi-hd.mpg.de/hfm/~bernlohr/iact-atmo/" target="_blank" rel="noopener">IACT/ATMO interface website</a>. For installation, copy all relevant tar.gz packages plus the ‘build_all’ script into the same directory and run `./build_all prod6 qgs2` (see `–help` for more options). Note that CORSIKA 7.7550 requires the corsika-77550.patch file available in bernlohr-1.68.tar.gz. Runing without it would lead to run-time errors. Placing the patch file in the top level of the directory structure is enough for the `build_all` script to pick it up.</p> <p>In cases for which the CTAO Simulation Telescope Models are used in a research project, we ask that the following acknowledgement is added in any resulting publication:</p> <p>“This research has made use of the CTAO Simulation Telescope Models provided by the CTAO Central Organisation and Consortium (version prod6 v1.0; [a]).”</p> <p>Please use the following BibTex Entry for [a] in the reference section of your publication: https://zenodo.org/records/14198379/export/bibtex</p> <p>References:</p> <p>[1] K.Bernlöhr, Simulation of imaging atmospheric Cherenkov telescopes with CORSIKA and sim_telarray, Astroparticle Physics 30 (2008) 149–158; <a href="https://arxiv.org/abs/0808.2253" target="_blank" rel="noopener">arXiv:0808.2253</a></p>
CTAO Simulation Telescope Models for CORSIKA and sim_telarray - prod3b
<p>The <a href="https://www.cta-observatory.org/">Cherenkov Telescope Array Observatory</a> (CTAO) will be the next-generation gamma-ray observatory under construction on the island of La Palma (Spain) and near Paranal (Chile). CTAO will cover a wide energy range and provide substantial improvements in sensitivity, angular resolution and energy resolution in comparison to any existing gamma-ray detector. Detailed Monte Carlo simulations allow us to optimise the instrument configuration and to estimate the observatory performance using realistic models of the telescope design. The CORSIKA air-shower simulation code and the sim_telarray code for simulation of arrays of Cherenkov telescopes are used for all CTAO Monte Carlo simulation productions.</p> <p>This repository provides access to the simulation configuration describing the site parameters and the telescope simulation models required for the generation of the <a href="https://doi.org/10.5281/zenodo.5163272">CTAO Instrument Response Functions - prod3b</a>.</p> <p>In detail, these are:</p> <ul> <li>telescope simulation models for each telescope type (prod3b includes models for large-size, medium-size, and small-size telescopes)</li> <li>CORSIKA input files defining (among others) site atmosphere, telescope positions, and interaction models;</li> <li>execution scripts required to run CORSIKA and sim_telarray.</li> </ul> <p>The CORSIKA air-shower simulation code is available from the Institute for Astroparticle Physics (KIT), see <a href="https://www.iap.kit.edu/corsika/index.php">CORSIKA website</a>. The sim_telarray telescope simulation program, auxilliary libraries, and common configuration files are available at the <a href="https://www.mpi-hd.mpg.de/hfm/~bernlohr/sim_telarray/">sim_telarray website</a>, with an up-to-date interface to CORSIKA at the <a href="https://www.mpi-hd.mpg.de/hfm/~bernlohr/iact-atmo/">IACT/ATMO interface website</a>. For installation, copy all relevant tar.gz packages plus the ‘build_all’ script into the same directory and run ‘./build_all prod3-la-palma qgs2' (see ‘--help’ for more options).</p> <p>In cases for which the CTAO Simulation Telescope Models are used in a research project, we ask that the following acknowledgement is added in any resulting publication:</p> <p>“This research has made use of the CTA Simulation Telescope Models provided by the CTA Observatory and Consortium (version prod3b v1.0; [a]).”</p> <p>Please use the following BibTex Entry for [a] in the reference section of your publication: <a href="https://zenodo.org/record/6219128/export/hx">https://zenodo.org/record/6219128/export/hx</a></p> <p>References:</p> <p>[1] K.Bernlöhr, Simulation of imaging atmospheric Cherenkov telescopes with CORSIKA and sim_telarray, Astroparticle Physics 30 (2008) 149–158; <a href="https://arxiv.org/abs/0808.2253">arXiv:0808.2253</a></p> <p>[2] A. Acharyya, for the CTA Consortium (2019), Monte Carlo studies for the optimisation of the Cherenkov Telescope Array layout, <a href="https://arxiv.org/abs/1904.01426">arXiv:1904.01426</a></p>
CTAO Simulation Telescope Models for CORSIKA and sim_telarray - prod5
<p>The <a href="https://www.cta-observatory.org/">Cherenkov Telescope Array Observatory</a> (CTAO) will be the next-generation gamma-ray observatory under construction on the island of La Palma (Spain) and near Paranal (Chile). CTAO will cover a wide energy range and provide substantial improvements in sensitivity, angular resolution and energy resolution in comparison to any existing gamma-ray detector. Detailed Monte Carlo simulations allow us to optimise the instrument configuration and to estimate the observatory performance using realistic models of the telescope design. The CORSIKA air-shower simulation code and the sim_telarray code for simulation of arrays of Cherenkov telescopes are used for all CTAO Monte Carlo simulation productions.</p> <p>This repository provides access to the simulation configuration describing the site parameters and the telescope simulation models required for the generation of the <a href="https://doi.org/10.5281/zenodo.5499839">CTAO Instrument Response Functions - prod5</a>.</p> <p>In detail, these are:</p> <ul> <li>telescope simulation models for each telescope type (prod5 includes models for large-size, medium-size, and small-size telescopes)</li> <li>CORSIKA input files defining (among others) site atmosphere, telescope positions, and interaction models;</li> <li>execution scripts required to run CORSIKA and sim_telarray.</li> </ul> <p>The CORSIKA air-shower simulation code is available from the Institute for Astroparticle Physics (KIT), see <a href="https://www.iap.kit.edu/corsika/index.php">CORSIKA website</a>. The sim_telarray telescope simulation program, auxilliary libraries, and common configuration files are available at the <a href="https://www.mpi-hd.mpg.de/hfm/~bernlohr/sim_telarray/">sim_telarray website</a>, with an up-to-date interface to CORSIKA at the <a href="https://www.mpi-hd.mpg.de/hfm/~bernlohr/iact-atmo/">IACT/ATMO interface website</a>. For installation, copy all relevant tar.gz packages plus the ‘build_all’ script into the same directory and run ‘./build_all prod5 qgs2’ (see ‘--help’ for more options).</p> <p>In cases for which the CTAO Simulation Telescope Models are used in a research project, we ask that the following acknowledgement is added in any resulting publication:</p> <p>“This research has made use of the CTA Simulation Telescope Models provided by the CTA Observatory and Consortium (version prod5 v1.0; [a]).”</p> <p>Please use the following BibTex Entry for [a] in the reference section of your publication: <a href="https://zenodo.org/record/6218687/export/hx">https://zenodo.org/record/6218687/export/hx</a></p> <p>References:</p> <p>[1] K.Bernlöhr, Simulation of imaging atmospheric Cherenkov telescopes with CORSIKA and sim_telarray, Astroparticle Physics 30 (2008) 149–158; <a href="https://arxiv.org/abs/0808.2253">arXiv:0808.2253</a></p> <p>[2] O.Gueta for the CTA Consortium and the CTA Observatory, The Cherenkov Telescope Array: layout, design and performance, Proceedings of the 37th International Cosmic Ray Conference (ICRC2021), Berlin, Germany; <a href="https://arxiv.org/abs/2108.04512">arXiv:2108.04512</a></p>
CTAO Monte Carlo Simulations - Eventlists on DL2 data level - prod5
<p>Author: Cherenkov Telescope Array Observatory; Cherenkov Telescope Array Consortium<br>Contact: open-data@cta-observatory.org</p> <p>The <a href="https://www.cta-observatory.org/">Cherenkov Telescope Array Observatory (CTAO)</a> will be the next-generation gamma-ray observatory and is currently under construction on the island of La Palma (Spain) and near Paranal (Chile). <br>This repository provides access to reconstructed event information (DL2- and DL1-level, simulation parameters) from Monte Carlo simulations of the CTAO Northern Array (production 5).</p> <p>The Monte Carlo simulations for prod5 are described in <a href="https://arxiv.org/abs/2108.04512">arXiv:2108.04512</a>, the simulation telescopes models used in the telescope simulation program <a href="https://www.mpi-hd.mpg.de/hfm/~bernlohr/sim_telarray/">sim_telarray</a> and the configuration used in the air-shower code <a href="https://www.iap.kit.edu/corsika/index.php">CORSIKA</a> are available from the Zenodo archive for <a href="../record/6218687">CTA Prod5 Telescope Models</a>.</p> <p>MC events are calibrated and reconstructed using the <a href="https://ctapipe.readthedocs.io/">ctapipe</a> package and stored for the following data levels:</p> <ul> <li> R1-MC: simulated raw data (output from sim_telarray)</li> <li> <strong>DL1 (this repository)</strong>: telescope level data including images and image parameters</li> <li> <strong>DL2 (this repository)</strong>: reconstructed event parameters such as energy, <strong>direction</strong>, gamma/hadron discrimination parameters. Note that this repository only contains the direction information.</li> <li>DL3: selected events with associated instrument response functions (IRFs). Preliminary DL3-IRFs are available from [here](https://doi.org/10.5281/zenodo.5499839).</li> </ul> <p>For a description of the file format and data model, <a href="https://ctapipe.readthedocs.io/en/latest/user-guide/data_models/index.html">see ctapipe Data Model</a>.</p> <p>Data set description:</p> <ul> <li>using ctapipe version 0.17 (<a href="https://github.com/cta-observatory/ctapipe/releases/tag/v0.17.0">GitHub release page</a>, <a href="../record/7118605">Zenodo page</a>)</li> <li>CTAO Northern Array on La Palma for the Alpha configuration (4 large-sized telescopes, 9 mid-sized telescopes)</li> <li>Zenith angles of 20 deg, telescope pointing direction north and south</li> <li>Primary particles: photons, protons</li> <li>Contained information: DL1 image and parameter data, DL2 geometry, simulation truths</li> <li>For convenience, the same data is provided in a single, large file per particle type for the whole dataset which do not contain the low-level DL1 image information and a larger number of files including this information.</li> </ul> <p>We explicitly note that the products provided are preliminary and do not reflect the final performance of the CTA Observatory, neither are data structure or formats finalized. We also note that these data products are different to those used for the <a href="../record/5499840">CTAO Instrument Response Functions</a>.<br>In cases in which the data provided in this repository are used in a research project, we ask that the following acknowledgment is added in any resulting publication:</p> <p>"This research has made use of the CTA DL1 and DL2 Event lists provided by the CTA Observatory and Consortium (version prod5-DL2-release1-DL2)" and cite this repository in the reference section of your publication.</p> <p>We would like to thank the computing centers that provided resources for the generation of the Prod5 simulation set,<a href="../record/5499840"> click here for a list of service providers</a>.</p>
CTAO Instrument Response Functions - prod5 version v0.1
<p>CTAO Instrument Response Functions - prod5 version v0.1</p> <p>The CTA Observatory (CTAO) will provide very wide energy range and excellent angular resolution and sensitivity in comparison to any existing gamma-ray detector. Energies down to 20 GeV will allow CTAO to study the most distant objects. Energies up to 300 TeV will push CTAO beyond the edge of the known electromagnetic spectrum, providing a completely new view of the sky. This data repository provides access to performance evaluation and instrument response functions (IRFs) for CTA.</p> <ul> <li>IRF version: prod5 v0.1</li> <li>Telescope model and site configuration: <a href="https://zenodo.org/record/6218687">prod5-model</a></li> <li>Publication date: Sep 2021</li> <li>Archived webpage with performance figures included: <a href="/cta-science/montecarlo-results/public-irfs-zenodo/cta-prod5-zenodo/-/blob/preview/Website.md">CTAO Performance Description (file Website.md)</a></li> <li>Licence: this work is licensed under a <a href="/cta-science/montecarlo-results/public-irfs-zenodo/cta-prod5-zenodo/-/blob/preview/LICENSE">Creative Commons Attribution 4.0 International License</a>.</li> </ul> <p>Please use the contact address open-data@cta-observatory.org for any inquiries.</p> <p>Citation and Acknowledgements:</p> <p>In cases for which the CTA instrument response functions are used in a research project, we ask to add the following acknowledgement in any resulting publication:</p> <p>"This research has made use of the CTA instrument response functions provided by the CTA Consortium and Observatory, see <a href="https://www.cta-observatory.org/science/cta-performance/">https://www.ctao-observatory.org/science/cta-performance/</a> (version prod5 v0.1; [citation]) for more details."</p> <p>Please use the following BibTex Entry for [citation] in the reference section of your publication:<br> <a href="https://zenodo.org/record/5499840/export/hx">https://zenodo.org/record/5499840/export/hx</a></p> <p>Description</p> <p>Monte Carlo Simulations:</p> <p>The performance values are derived from detailed Monte Carlo (MC) simulations of the CTA instrument based on the CORSIKA air shower code (v7.71, with the hadronic interaction models QGSjet-II-04 and URQMD, [1]) and telescope simulation tool sim_telarray [2]. A power- law gamma-ray spectrum with photon index 2.62 was assumed in the calculations, although none of the instrument response functions (e.g. differential flux sensitivities, effective areas, angular or energy resolutions) depends on the assumed spectral shape of the gamma-ray source. Background cosmic-ray spectra of proton and electron/positron particle types are modelled according to recent measurements from cosmic-ray instruments.</p> <p>Nominal telescope pointing is assumed, with all telescopes pointing directions parallel to each other (performance estimation for other pointing modes, e.g. divergent pointing will be provided in the future). Performance estimations are available for three zenith angles (20 deg, 40 deg, and 60 deg), and for each zenith angle for two different azimuth angles (corresponding to pointing towards the magnetic North and South). There are significant performance differences found between the two azimuthal pointing directions (especially for the Northern site) as the impact of the geomagnetic field is large enough to influence notably the air shower development. For general studies, the use of the azimuth-averaged instrument response functions is recommended.</p> <p>Instrument Response Functions (IRFs):</p> <p>The analysis has been tuned to maximize the performance in terms of flux sensitivity. The optimal analysis cuts depend on the duration of the observation, therefore the IRFs are provided for 3 different observation times, from 0.5 to 50 h. IRFs are provided as binned histogram or FITS tables. It should be stressed, that the full potential of CTA in terms of angular and energy resolution is not revealed by these IRFS, due to the focus on the optimisation for best flux sensitivity.</p> <p>In general all histograms are binned with a 0.2-binning on the logarithmic energy axis (5 bins per decade); some selected histograms (e.g. effective areas or energy migration matrices) are provided with a finer binning. Effective area and energy migration matrix are available in a double version: one for the case in which there is no a priori knowledge of the true direction of incoming gamma rays (e.g. for the observation of diffuse sources), and another for observations of point-like objects (including among the analysis cuts one on the angle between the true and the reconstructed gamma-ray direction).</p> <p>IRFs are provided in ROOT format and as FITS tables. The FITS tables can be used directly as input to science analysis tools. The values of the IRFs are identical for the different file format, with one exception: the angular point-spread function is approximated by a Gaussian function for the FITS tables, while the ROOT files contain the full distribution.</p> <p>Telescope layouts are preliminary and subject to change. The following array layouts (Alpha configuration) have been assumed:</p> <ul> <li> CTA South with 14 MSTs and 37 SSTs (see [figure](figures/CTA-Performance-prod5-v0.1-South-Alpha-Layout.png))</li> <li> CTA North with 4 LSTs and 9 MSTs (see [figure](figures/CTA-Performance-prod5-v0.1-North-Alpha-Layout.png))</li> </ul> <p>Two zip files are uploaded:</p> <ul> <li>full archive with IRFs in FITS and ROOT format: cta-prod5-zenodo-v0.1.zip</li> <li>partial archive with IRFs in FITS format only: cta-prod5-zenodo-fitsonly-v0.1.zip</li> </ul> <p>File Naming (examples):</p> <ul> <li>Prod5-North-40deg-AverageAz-4LSTs09MSTs.18000s-v0.1.root: IRF for CTA Northern site on La Palma, 40 deg zenith angle, azimuth-averaged pointing, optimised for 5 hours of observation time</li> <li>Prod5-South-20deg-AverageAz-14MSTs37SSTs.180000s-v0.1.fits.gz: IRF for CTA Southern site in Paranal, 20 deg zenith angle, azimuth-averaged pointing, optimised for 50 hours of observation time</li> </ul> <p>List of files:</p> <p>FITS format:</p> <ul> <li>fits/CTA-Performance-prod5-v0.1-North-20deg.FITS.tar.gz</li> <li>fits/CTA-Performance-prod5-v0.1-North-40deg.FITS.tar.gz</li> <li>fits/CTA-Performance-prod5-v0.1-North-60deg.FITS.tar.gz</li> <li>fits/CTA-Performance-prod5-v0.1-South-20deg.FITS.tar.gz</li> <li>fits/CTA-Performance-prod5-v0.1-South-40deg.FITS.tar.gz</li> <li>fits/CTA-Performance-prod5-v0.1-South-60deg.FITS.tar.gz</li> </ul> <p>ROOT format:</p> <ul> <li>root/CTA-Performance-prod5-v0.1-North-20deg.tar.gz</li> <li>root/CTA-Performance-prod5-v0.1-North-40deg.tar.gz</li> <li>root/CTA-Performance-prod5-v0.1-North-60deg.tar.gz</li> <li>root/CTA-Performance-prod5-v0.1-South-20deg.tar.gz</li> <li>root/CTA-Performance-prod5-v0.1-South-40deg.tar.gz</li> <li>root/CTA-Performance-prod5-v0.1-South-60deg.tar.gz</li> </ul> <p>IRFs for subarrays of e.g., MSTs only are in the files named MSTSubArray (similar for all other telescope types).</p> <p>References</p> <ul> <li>[1] <a href="https://www.ikp.kit.edu/corsika/">https://www.ikp.kit.edu/corsika/</a></li> <li>[2] Bernloehr, K. 2008, Astroparticle Physics, 30, 149</li> </ul> <p>Acknowledgements</p> <p>We would like to thank the computing centres that provided resources for the generation of the Prod 5 Instrument Response Functions (IRFs):</p> <ul> <li>CAMK, Nicolaus Copernicus Astronomical Center, Warsaw, Poland</li> <li>CIEMAT-LCG2, CIEMAT, Madrid, Spain</li> <li>CYFRONET-LCG2, ACC CYFRONET AGH, Cracow, Poland</li> <li>DESY-ZN, Deutsches Elektronen-Synchrotron, Standort Zeuthen, Germany</li> <li>GRIF, Grille de Recherche d’Ile de France, Paris, France</li> <li>IN2P3-CC, Centre de Calcul de l’IN2P3, Villeurbanne, France</li> <li>IN2P3-CPPM, Centre de Physique des Particules de Marseille, Marseille, France</li> <li>IN2P3-LAPP, Laboratoire d Annecy de Physique des Particules, Annecy, France</li> <li>INFN-FRASCATI, INFN Frascati, Frascati, Italy</li> <li>INFN-T1, CNAF INFN, Bologna, Italy</li> <li>INFN-TORINO, INFN Torino, Torino, Italy</li> <li>MPIK, Heidelberg, Germany</li> <li>OBSPM, Observatoire de Paris Meudon, Paris, France</li> <li>PIC, port d’informacio cientifica, Bellaterra, Spain</li> <li>prague_cesnet_lcg2, CESNET, Prague, Czech Republic</li> <li>praguelcg2, FZU Prague, Prague, Czech Republic</li> <li>UKI-NORTHGRID-LANCS-HEP, Lancaster University, United Kingdom</li> </ul>
CTAO DL2 small test files
<p>These files are simple copies of files from https://zenodo.org/records/7298569 but with images removed to create smaller versions usable for tests.</p> <p>All credit goes to https://zenodo.org/records/7298569</p>
CTAO Instrument Response Functions - version prod3b-v2
<p><strong>CTAO Instrument Response Functions - version prod3b-v2</strong></p> <p><strong>**Please check the CTA webpage (<a href="https://www.cta-observatory.org/science/cta-performance/">https://www.cta-observatory.org/science/cta-performance/</a>)) for the most recent instrument response functions.**</strong></p> <p><strong>**Figures and files in this repository are superseded by newer versions and provided for archival reasons.**</strong></p> <p>The CTA Observatory (CTAO) will provide very wide energy range and excellent angular resolution and sensitivity in comparison to any existing gamma-ray detector. Energies down to 20 GeV will allow CTAO to study the most distant objects. Energies up to 300 TeV will push CTAO beyond the edge of the known electromagnetic spectrum, providing a completely new view of the sky.</p> <p>This data repository provides access to performance evaluation and instrument response functions (IRFs) for CTA.</p> <p>- IRF version: prod3b-v2<br> - Telescope model and site configuration: <a href="https://zenodo.org/record/6219128">prod3b model</a><br> - Publication date: April 2019<br> - Archived webpage with performance figures included: [CTAO Performance Description (file Website.md)](Website.md)<br> - Licence: his work is licensed under a [Creative Commons Attribution 4.0 International License](LICENSE).</p> <p>Citation and Acknowledgements:</p> <p>In cases for which the CTA instrument response functions are used in a research project, we ask to add the following acknowledgement in any resulting publication:</p> <p>“This research has made use of the CTA instrument response functions provided by the CTA Consortium and Observatory, see https://www.cta-observatory.org/science/cta-performance/ (version prod3b-v2; [citation]) for more details.”</p> <p>Please use the following BibTex Entry for [citation] in the reference section of your publication:<br> <a href="https://zenodo.org/record/5163273/export/hx">https://zenodo.org/record/5163273/export/hx</a></p> <p>Description</p> <p>Monte Carlo Simulations:</p> <p>The performance values are derived from detailed Monte Carlo (MC) simulations of the CTA instrument based on the CORSIKA air shower code (v6.9+, with the hadronic interaction models QGSjet-II-04 and URQMD, [1]) and telescope simulation tool sim\_telarray [2]. A power-law gamma-ray spectrum with photon index 2.62 was assumed in the calculations, although none of the instrument response functions (e.g. differential flux sensitivities, effective areas, angular or energy resolutions) depends on the assumed spectral shape of the gamma-ray source. Background cosmic-ray spectra of proton and electron/positron particle types are modelled according to recent measurements from cosmic-ray instruments.</p> <p>Nominal telescope pointing is assumed, with all telescopes pointing directions parallel to each other (performance estimation for other pointing modes, e.g. divergent pointing will be provided in the future). Performance estimations are available for two zenith angles (20 deg and 40 deg), and for each zenith angle for two different azimuth angles (corresponding to pointing towards the magnetic North and South). There are significant performance differences found between the two azimuthal pointing directions (especially for the Northern site) as the impact of the geomagnetic field is large enough to influence notably the air shower development. For general studies, the use of the azimuth-averaged instrument response functions is recommended.</p> <p>Instrument Response Functions (IRFs):</p> <p>The analysis has been tuned to maximize the performance in terms of flux sensitivity. The optimal analysis cuts depend on the duration of the observation, therefore the IRFs are provided for 3 different observation times, from 0.5 to 50 h. IRFs are provided as binned histogram or FITS tables. It should be stressed, that the full potential of CTA in terms of angular and energy resolution is not revealed by these IRFS, due to the focus on the optimisation for best flux sensitivity.</p> <p>In general all histograms are binned with a 0.2-binning on the logarithmic energy axis (5 bins per decade); some selected histograms (e.g. effective areas or energy migration matrices) are provided with a finer binning. Effective area and energy migration matrix are available in a double version: one for the case in which there is no a priori knowledge of the true direction of incoming gamma rays (e.g. for the observation of diffuse sources), and another for observations of point-like objects (including among the analysis cuts one on the angle between the true and the reconstructed gamma-ray direction).</p> <p>IRFs are provided in ROOT format, as FITS tables, and for some on-axis IRFs also as simple ASCII files. The FITS tables can be used directly as input to science analysis tools. The values of the IRFs are identical for the different file format, with one exception: the angular point-spread function is approximated by a Gaussian function for the FITS tables, while the ROOT files contain the full distribution.</p> <p> </p> <p>File Naming (examples):</p> <p>- CTA-Performance-prod3b-v2-North-20deg-average-50h.root: IRF for CTA Northern site on La Palma, 20 deg zenith angle, azimuth-averaged pointing, optimised for 50 hours of observation time<br> - CTA-Performance-prod3b-v2-South-20deg-average-50h.root: IRF for CTA Southern site in Paranal, 20 deg zenith angle, azimuth-averaged pointing, optimised for 50 hours of observation time<br> - CTA-Performance-prod3b-v2-South-40deg-S-30m.root: RF for CTA Southern site, 40 deg zenith angle, South pointing, optimised for 30 minutes of observation time</p> <p>List of files:</p> <p>- fits/CTA-Performance-prod3b-v2-FITS.tar.gz - IRFs in FITS format (making use of the HEASARC’s caldb indexing) - includes IRFs for 20 deg, 40 deg, and 60 deg zenith angle, average, north and south pointing<br> - root/CTA-Performance-prod3b-v2-20deg-ROOT.tar.gz - IRFs in ROOT format for 20 deg zenith angle, azimuth-averaged, north and south pointing<br> - root/CTA-Performance-prod3b-v2-40deg-ROOT.tar.gz - IRFs in ROOT format for 40 deg zenith angle, azimuth-averaged, north and south pointing<br> - root/CTA-Performance-prod3b-v2-60deg-ROOT.tar.gz - IRFs in ROOT format for 60 deg zenith angle, azimuth-averaged, north and south pointing<br> - ascii/CTA-Performance-prod3b-v2-20deg-ASCII.tar.gz - (selected) IRFs in ASCII format for 20 deg zenith angle, azimuth-averaged, north and south pointing<br> - ascii/CTA-Performance-prod3b-v2-40deg-ASCII.tar.gz - (selected) IRFs in ASCII format for 40 deg zenith angle, azimuth-averaged, north and south pointing<br> - ascii/CTA-Performance-prod3b-v2-60deg-ASCII.tar.gz - (selected) IRFs in ASCII format for 60 deg zenith angle, azimuth-averaged, north and south pointing</p> <p>### CTA Science Performance Requirements</p> <p><strong>**Performance requirements for CTA are currently under review. The attached requirements are preliminary and subject to change.**</strong></p> <p>The following documents summarise the science performance requirements for CTA. These requirements correspond to the baseline implementation of CTA. Values for the requirements on differential sensitivity, angular and energy resolution are provided in plain text files.</p> <p>- Requirements description (CTA-SPE-SCI-00000-0001_Issue_1_SystemLevelSciencePerformanceReqs.pdf)<br> - CTA-Performance-Requirements.tar.gz (ascii files)</p> <p>## References</p> <p>- [1] https://www.ikp.kit.edu/corsika/<br> - [2] Bernloehr, K. 2008, Astroparticle Physics, 30, 149</p> <p>## Acknowledgements</p> <p>We would like to thank the computing centres that provided resources for the generation of the Instrument Response Functions:</p> <p>- CAMK, Nicolaus Copernicus Astronomical Center, Warsaw, Poland<br> - CETA-GRID, Resource Center CETA-CIEMAT, Trujillo, Spain<br> - CIEMAT-LCG2, CIEMAT, Madrid, Spain<br> - CYFRONET-LCG2, ACC CYFRONET AGH, Cracow, Poland<br> - DESY-ZN, Deutsches Elektronen-Synchrotron, Standort Zeuthen, Germany<br> - GRIF, Grille de Recherche d’Ile de France, Paris, France<br> - IN2P3-CC, Centre de Calcul de l’IN2P3, Villeurbanne, France<br> - IN2P3-CPPM, Centre de Physique des Particules de Marseille, Marseille, France<br> - IN2P3-LAPP, Laboratoire d Annecy de Physique des Particules, Annecy, France<br> - INFN-FRASCATI, INFN Frascati, Frascati, Italy<br> - INFN-T1, CNAF INFN, Bologna, Italy<br> - INFN-TORINO, INFN Torino, Torino, Italy<br> - MPIK, Heidelberg, Germany<br> - M3PEC, Mesocentre Aquitain, Bordeaux, France<br> - OBSPM, Observatoire de Paris Meudon, Paris, France<br> - PIC, port d’informacio cientifica, Bellaterra, Spain<br> - prague_cesnet_lcg2, CESNET, Prague, Czech Republic<br> - praguelcg2, FZU Prague, Prague, Czech Republic<br> - SE-SNIC-T2, The Swedish WLCG Tier 2 InitiativeStockholm, Sweden</p> <p> </p>
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