Detalles de publicación
PP 024057
CONCERTO: Instrument model of Fourier transform spectroscopy, white-noise components
Aix Marseille Univ., CNRS, CNES, LAM, Marseille, France
Instituto de Astrofísica de Canarias, Santa Cruz de Tenerife, E-38205 La Laguna, Spain
Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain
Astronomy Instrumentation Group, University of Cardiff, The Parade, CF24 3AA, United Kingdom
Núcleo de Astronomía, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Av. Ejército 441, Santiago, Chile
Univ. Grenoble Alpes, CNRS, Grenoble INP, Institut Néel, 38000 Grenoble, France
Univ. Grenoble Alpes, CNRS, LPSC/IN2P3, 38000 Grenoble, France
European Southern Observatory, Karl Schwarzschild Straße 2, 85748 Garching, Germany
Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile
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.

