DOI: 10.5281/zenodo.5163272
title: CTAO Instrument Response Functions - version prod3b-v2

description: <strong>CTAO Instrument Response Functions - version prod3b-v2</strong> <strong>**Please check the CTA webpage (https://www.cta-observatory.org/science/cta-performance/)) for the most recent instrument response functions.**</strong> <strong>**Figures and files in this repository are superseded by newer versions and provided for archival reasons.**</strong> 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. - IRF version: prod3b-v2<br> - Telescope model and site configuration: prod3b model<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). Citation and Acknowledgements: 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: “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.” Please use the following BibTex Entry for [citation] in the reference section of your publication:<br> https://zenodo.org/record/5163273/export/hx Description Monte Carlo Simulations: 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. 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. Instrument Response Functions (IRFs): 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. 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). 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. File Naming (examples): - 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 List of files: - 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 ### CTA Science Performance Requirements <strong>**Performance requirements for CTA are currently under review. The attached requirements are preliminary and subject to change.**</strong> 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. - Requirements description (CTA-SPE-SCI-00000-0001_Issue_1_SystemLevelSciencePerformanceReqs.pdf)<br> - CTA-Performance-Requirements.tar.gz (ascii files) ## References - [1] https://www.ikp.kit.edu/corsika/<br> - [2] Bernloehr, K. 2008, Astroparticle Physics, 30, 149 ## Acknowledgements We would like to thank the computing centres that provided resources for the generation of the Instrument Response Functions: - 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