CONCERTO: Instrument model of Fourier transform spectroscopy, white-noise components
| Autor: | Fasano, Alessandro, Ade, Peter, Aravena, Manuel, Barria, Emilio, Beelen, Alexandre, Benoit, Alain, Béthermin, Matthieu, Bounmy, Julien, Bourrion, Olivier, Bres, Guillaume, Calvo, Martino, Catalano, Andrea, De Breuck, Carlos, Désert, François-Xavier, Dubois, Cédric, Durán, Carlos, Fenouillet, Thomas, Garcia, Jose, Garde, Gregory, Goupy, Johannes, Hoarau, Christophe, Hu, Wenkai, Lagache, Guilaine, Lambert, Jean-Charles, Levy-Bertrand, Florence, Lundgren, Andreas, Macías-Pérez, Juan-Francisco, Marpaud, Julien, Monfardini, Alessandro, Pisano, Giampaolo, Ponthieu, Nicolas, Prieur, Leo, Roni, Samuel, Roudier, Sebastien, Tourres, Damien, Tucker, Carol, Van Cuyck, Mathilde |
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| Rok vydání: | 2024 |
| Předmět: | |
| Druh dokumentu: | Working Paper |
| Popis: | Modern astrophysics relies on intricate instrument setups to meet the demands of sensitivity, sky coverage, and multi-channel observations. An example is the CONCERTO project, employing advanced technology like kinetic inductance detectors and a Martin-Puplett interferometer. This instrument, installed at the APEX telescope atop the Chajnantor plateau, began commissioning observations in April 2021. Following a successful commissioning phase that concluded in June 2021, CONCERTO was offered to the scientific community for observations, with a final observing run in December 2022. CONCERTO boasts an 18.5 arcmin field of view and a spectral resolution down to 1.45 GHz in the 130-310 GHz electromagnetic band. We developed a comprehensive instrument model of CONCERTO inspired by Fourier transform spectrometry principles to optimize performance and address systematic errors. This model integrates instrument noises, subsystem characteristics, and celestial signals, leveraging both physical data and simulations. Our methodology involves delineating simulation components, executing on-sky simulations, and comparing results with real observations. The resulting instrument model is pivotal, enabling a precise error correction and enhancing the reliability of astrophysical insights obtained from observational data. In this work, we focus on the description of three white-noise noise components included in the instrument model that characterize the white-noise level: the photon, the generation-recombination, and the amplifier noises. Comment: 8 pages, 1 figure, Proceeding of the SPIE conference Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy XII, SPIE Astronomical Telescopes + Instrumentation 2024 |
| Databáze: | arXiv |
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