001     600676
005     20250724132657.0
024 7 _ |a 10.22323/1.444.0618
|2 doi
024 7 _ |a 10.3204/PUBDB-2023-08099
|2 datacite_doi
024 7 _ |a arXiv:2309.16488
|2 arXiv
024 7 _ |a openalex:W4385304799
|2 openalex
037 _ _ |a PUBDB-2023-08099
041 _ _ |a English
082 _ _ |a 530
088 _ _ |a arXiv:2309.16488
|2 arXiv
088 _ _ |a CTA-ICRC/2023/26
|2 Other
100 1 _ |a Dominik, Rune Michael
|0 P:(DE-HGF)0
|b 0
|e Corresponding author
111 2 _ |a 38th International Cosmic Ray Conference
|g ICRC2023
|c Nagoya
|d 2023-07-26 - 2023-08-03
|w Japan
245 _ _ |a Interpolation of Instrument Response Functions for the Cherenkov Telescope Array in the Context of pyirf
260 _ _ |a Trieste
|c 2023
|b SISSA
300 _ _ |a 16
336 7 _ |a CONFERENCE_PAPER
|2 ORCID
336 7 _ |a Conference Paper
|0 33
|2 EndNote
336 7 _ |a Journal Article
|0 PUB:(DE-HGF)16
|2 PUB:(DE-HGF)
|m journal
336 7 _ |a INPROCEEDINGS
|2 BibTeX
336 7 _ |a conferenceObject
|2 DRIVER
336 7 _ |a Output Types/Conference Paper
|2 DataCite
336 7 _ |a Contribution to a conference proceedings
|b contrib
|m contrib
|0 PUB:(DE-HGF)8
|s 1707138780_3708075
|2 PUB:(DE-HGF)
336 7 _ |a Contribution to a book
|0 PUB:(DE-HGF)7
|2 PUB:(DE-HGF)
|m contb
490 0 _ |a 2681409
|2 Author
500 _ _ |a Presented at the 38th International Cosmic Ray Conference (ICRC 2023), 2023 (arXiv:2309.08219)
520 _ _ |a The Cherenkov Telescope Array (CTA) will be the next generation ground-basedvery-high-energy gamma-ray observatory, constituted by tens of Imaging AtmosphericCherenkov Telescopes at two sites once its construction and commissioning are finished. Like its predecessors, CTA relies on Instrument Response Functions (IRFs) to relate the observed and reconstructed properties to the true ones of the primary gamma-ray photons. IRFs are needed for the proper reconstruction of spectral and spatial information of the observed sources and are thus among the data products issued to the observatory users. They are derived from Monte Carlo simulations, depend on observation conditions likethe telescope pointing direction or the atmospheric transparency and can evolve with time as hardware ages or is replaced. Producing a complete set of IRFs from simulations for every observation taken is a time-consuming task and not feasible when releasing data products on short timescales. Consequently, interpolation techniques on simulated IRFs are investigated to quickly estimate IRFs for specific observation conditions. However, as some of the IRFs constituents are given as probability distributions, specialized methods are needed. This contribution summarizes and compares the feasibility of multiple approaches to interpolate IRF components in the context of the pyirf python software package and IRFs simulated for the Large-Sized Telescope prototype (LST-1). We will also give an overview of the current functionalities implemented in pyirf.
536 _ _ |a 613 - Matter and Radiation from the Universe (POF4-613)
|0 G:(DE-HGF)POF4-613
|c POF4-613
|f POF IV
|x 0
588 _ _ |a Dataset connected to CrossRef Conference
650 _ 7 |a numerical calculations: Monte Carlo
|2 INSPIRE
650 _ 7 |a atmosphere: transparency
|2 INSPIRE
650 _ 7 |a Cherenkov Telescope Array
|2 INSPIRE
650 _ 7 |a observatory
|2 INSPIRE
650 _ 7 |a spectral
|2 INSPIRE
650 _ 7 |a photon
|2 INSPIRE
650 _ 7 |a programming
|2 INSPIRE
650 _ 7 |a Cherenkov counter
|2 INSPIRE
650 _ 7 |a gamma ray: VHE
|2 INSPIRE
650 _ 7 |a site
|2 INSPIRE
650 _ 7 |a hardware
|2 INSPIRE
650 _ 7 |a imaging
|2 INSPIRE
693 _ _ |0 EXP:(DE-H253)CTA-20150101
|5 EXP:(DE-H253)CTA-20150101
|e Cherenkov Telescope Array
|x 0
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|b 1
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