https://spie.org/AS24/conferencedetails/astronomy-ground-based-instrumentation?enableBackToBrowse=true&SSO=1 | 16 - 21 June 2024 Yokohama, Japan | ANDES, the high resolution spectrograph for the ELT: System Architecture Design of Phase-B-one | Alessio Zanutta | Zanutta Alessio,
Abreu Manuel, (1,2)
Aliverti Matteo,
Balestra Andrea,
Bellido-Tirado Olga, - obellido@aip.de
Brucalassi Anna,
Cabona Lorenzo,
Cabral Alexandre, (1,2)
Chazelas Bruno,
Coretti Igor,
Di Marcantonio Paolo,
Ebert Monica, (4)
Gaessler Wolfgang, (4)
Gao Xiao, - xiaofeng.gao@stfc.ac.uk
Geers Vincent, – vincent.geers@stfc.ac.uk
Giro Enrico,
Gonzalez Oscar, – oscar.gonzalez@stfc.ac.uk
Huke Philipp,
Landoni Marco,
Laun Werner, (4)
Lee David, – david.lee@stfc.ac.uk
Lehmitz Michael, (4)
Lunney David, – david.lunney@stfc.ac.uk
MacIntosh Mike, - mike.macintosh@stfc.ac.uk
Marconi Alessandro,
Monteiro Manuel, (3)
Montgomery David, – david.montgomery@stfc.ac.uk
Oliva Ernesto,
Origlia Livia,
Pariani Giorgio,
Pinna Enrico,
Redaelli Edoardo,
Riva Marco,
Rohloff Ralf-Rainer, (4)
Santos Diaz Pablo, - pablo.santosdiaz@unige.ch
Scalera Marcello,
Seifert Walter, (5)
Selmi Chiara,
Waring Chris, – chris.waring@stfc.ac.uk
Weber Michael,
Wehbe Bachar, (1,2)
Xompero Marco,
Xu Wenli, (6) | | LONG ABSTRACT (300-words max):
ANDES (ArmazoNes high Dispersion Echelle Spectrograph) is a fibre-fed echelle spectrograph for the ELT with three spectral arms, spanning 0.4-1.8 μm (goal 0.35-2.4 μm) at ~100,000 resolution. It enables sensitive observations of astronomical objects, such as exoplanets, fundamental physics and other frontier science cases. We describe the instrument's design and architecture, emphasizing its unique features.
The design is driven by requirements on resolving power, slit area, spectral coverage and stability. The instrument can operate in seeing-limited or SCAO modes, with options for sky and/or calibration measurements. In SCAO mode, it can use a small IFU with different spaxel scales.
The light from the telescope reaches the Front-End on the Nasmyth platform, which has four insertable modules: two seeing-limited arms, one SCAO arm and one IFU arm. They are connected by fibres or fibre bundles to the Spectrographs in different locations: the Nasmyth Platform and the Coudé room. The wavelength splitting depends on the fibre transparency. The subsystems are placed at different distances from the telescope.
In Phase-B-one, we performed analyses to define the best trade-off for the budgets and architecture. We extended the spectrographs toward the goal ranges as much as possible. ANDES is complex, but its sophisticated and modular design will enable next-generation astronomy research. |
https://spie.org/AS24/conferencedetails/astronomy-modeling-systems-engineering?enableBackToBrowse=true | 16 - 21 June 2024 Yokohama, Japan | ANDES, the high resolution spectrograph for the ELT: Model-Based Systems Engineering approach | Alessio Zanutta | Zanutta A., Scalera M., Riva M., Balestra A., Cabona L., Di Marcantonio P., Marconi A. | | LONG ABSTRACT (300-words max):
ANDES (ArmazoNes high Dispersion Echelle Spectrograph) is one of the second-phase instruments planned for the Extremely Large Telescope (ELT) of ESO. ANDES will provide high-resolution spectroscopy in the visible and near-infrared wavelengths, enabling a wide range of scientific investigations, such as characterizing exoplanet atmospheres, testing fundamental physics, and measuring the cosmic expansion. In this paper, we present the general strategy of the Model-Based Systems Engineering (MBSE) approach that we have used to design the instrument during the Phase B-One, which covers the system architecture review (SAR) successfully completed at end 2023. We describe how we have applied the Cameo Systems Modeler tool to create and manage the system model in compliance with the SysML standard to perform requirements and interfaces management, structure verification and validation, and trade-off analysis. We also emphasize that ANDES is used as a test case for the application of the MBSE methodology in the astronomical field, in order to create a standard of procedures to perform all the actions and tasks that serve to satisfy all the steps in the various design phases of an ESO project. In fact, the inital phases require specific tasks, such as the analysis of requirements, the flow-down of specifications to the subsystems, the tracing of interfaces, the analysis of budgets. Since there is no tool that specifically encompasses all these capabilities in the astronomical field, it is necessary to define a robust methodology that can be taken as an example for future astronomical instrumentation. We discuss the benefits and challenges of using MBSE for ANDES, as well as the lessons learned and best practices that can be useful for other astronomical instrument projects. |
https://spie.org/AS24/conferencedetails/astronomy-ground-based-instrumentation?enableBackToBrowse=true&SSO=1 | 16 - 21 June 2024 Yokohama, Japan | ANDES, the high resolution spectrograph for the ELT: Calibration Unit(s) | Philipp Huke | IAG: Jennifer Zimara, Sebastian Schäfer, Michael Debus, Ansgar Reiners UNIBE: Mirsad Sarajilic, Christopher Broeg (Center for Space and Habitability, University of Bern, Gesellschaftsstrasse 6, 3012 Bern, Switzerland) NCU: Piotr Maslowski HWU: Yuk Shan Cheng, Kamalesh Dadi, Richard A. McCracken and Derryck T. Reid (Institute of Photonics and Quantum Sciences, Heriot-Watt University, Edinburgh EH14 4AS, United Kingdom) IRAP/OMP: Léa Bonhomme, Driss Kouach (Observatoire Midi-Pyrénées, CNRS, Univ. de Toulouse (France)) Claude Le Men (Institut de Recherche en Astrophysique et Planétologie, CNRS (France)) LUPM: Omar Gabella ILO: Philipp Huke (Institute for Laser and Optics, Applied University Emden/Leer) MPIA: Wolfgang Gaessler, Michael Lehmitz UH: Joerg Knoche | | The instrumentation plan for the ELT foresees the ArmazoNes high Dispersion Echelle Spectrograph (ANDES). The ANDES-project and consortium entered phase B in January 2022 and underwent several (internal and external) revisions by now to ensure that the requirements and eventually the challenging goals can be met by the physical design of the spectrograph. Among its main scientific goals are the detection of atmospheres of exoplanets and the determination of fundamental physical constants. For this, high radial velocity precision and accuracy are required. Even though the ANDES-spectrograph is designed for maximum intrinsic stability, a calibration and thus a calibration unit is mandatory. To allow for maximum flexibility and modularity the calibration unit is physically split into three calibration units. We show the physical design of the calibration units and their individual components. This includes the electronics, the mechanics and the software supporting and controlling the light guiding and calibration sources. |