2024

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: project overview, future developments and science goals

@Alessandro Marconi

ALL members of ANDES Consortium

LONG ABSTRACT (300-words max):
ANDES, the ArmazoNes high Dispersion Echelle Spectrograph, will be the high-resolution spectrograph of the European Extremely Large Telescope at optical and near-infrared wavelengths and is being developed thanks to the efforts of a a large, internation consortium composed of more than 220 scientists and engineers from 33 institutes in 13 countries.
ANDES will consist of three fibre-fed spectrographs providing a spectral resolution of 100,000 with a simultaneous wavelength coverage of 0.4-1.8 µm, with the goal of extending it to 0.35-2.4 µm with the addition of the U and K bands. It will be able to operate in seeing limited conditions but will also include a unique integral field unit in the 1.0-1.8 µm range which, coupled with a SCAO module, will provide diffraction-limited spatially-resolved observations.
ANDES has a wide range of science cases spanning nearly all areas of research in astrophysics and even fundamental physics. Some of the top science cases will be the detection of biosignatures from exoplanet atmospheres, finding the fingerprints of the first generation of stars (PopIII), tests on the stability of Nature's fundamental couplings, and the direct detection of the cosmic acceleration.
I will provide a general overview of the ANDES project, including its main science cases, its status following the successfull completion of the System Architecture Review and the forthcoming steps to construction.

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.

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 Sarajlic, 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.

16 - 21 June 2024

Yokohama, Japan

ANDES, the high resolution spectrograph for the ELT: A novel high performances light distribution system for calibration units

Mirsad Sarajlic

see above

16 - 21 June 2024

Yokohama, Japan

ANDES, the high resolution spectrograph for the ELT: a 30 GHz UB-band astrocomb from 390–470 nm

see above

16 - 21 June 2024

Yokohama, Japan

ANDES, the high-resolution spectrograph for the ELT: RAM strategy during the Preliminary Design Review

Enrico Giro

Enrico Giro

Alessio Zanutta

Paolo Di Marcantonio

Manuel Abreu

Matteo Aliverti

Andrea Balestra

Lorenzo Cabona

Bruno Chazelas

Igor Coretti

Wolfgang Gaessler

Philipp Huke

Domenico Giannone

Marco Landoni

Mike MacIntosh

Ernesto Oliva

Livia Origlia

Giorgio Pariani

Edoardo Maria Alberto Redaelli

Marco Riva

Chiara Selmi

Marco Xompero

Jennifer Zimara

Alessandro Marconi

16 - 21 June 2024

Yokohama, Japan

ANDES, the high-resolution spectrograph for the ELT: project management for the preliminary design phase

Paolo Di Marcantonio

Paolo Di Marcantonio

Eric H.C. Stempels - Eric.Stempels@physics.uu.se –  Department of Physics & Astronomy, Uppsala University, Box 516, 75120 Uppsala, Sweden;

Enrico Giro – enrico.giro@inaf.it - INAF - Osservatorio Astronomico di Padova, Vicolo Dell’Osservatorio 5, I-35122 Padova, Italy;

Valentina Alberti – valentina.alberti@inaf.it - INAF - Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11, I-34143 Trieste, Italy;

Manuel Amate Plasencia - manuel.amate@iac.es - Instituto de Astrofísica de Canarias, C/Vía Láctea, 38205, Tenerife, Spain.

Veronica Baldini - veronica.baldini@inaf.it - INAF - Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11, I-34143 Trieste, Italy;

Lise Christensen - lichrist@nbi.ku.dk  - Cosmic DAWN Center, 2200 Copenhagen N, Denmark and Niels Bohr Institute, University of Copenhagen, Jagtvej 155, 2200 Copenhagen N, Denmar

Frédérique Baron - frederique.baron@umontreal.ca - Université de Montréal - Institut de recherche sur les exoplanètes - Observatoire du Mont-Mégantic, 1375 Avenue Thérèse-Lavoie-Roux, Montréal, QC H2V 0B3, Canada;

Joar Brynnel - jbrynnel@aip.de - Leibniz-Institute for Astrophysics Potsdam (AIP), An der Sternwarte 16, 144 82 Potsdam, Germany

Alexandre Cabral - Alexandre.Cabral@ciencias.ulisboa.pt - Instituto de Astrofísica e Ciências do Espaço, Universidade de Lisboa, Faculdade de Ciências, Campo Grande, PT1749-016 Lisboa, Portugal;

Bruno Chazelas - Bruno.Chazelas@unige.ch - Observatoire de Genève, University of Geneva, 51 chemin de Pegasi 1290 Versoix, Switzerland

Izan de Castro Leão - izan@fisica.ufrn.br - Departamento de Física Teórica e Experimental, Universidade Federal do Rio Grande do Norte, Campus Universitário, Natal, RN, 59072-970, Brazil

Christine Füßlein - cfuesslein@aip.de  - Leibniz-Institute for Astrophysics Potsdam (AIP), An der Sternwarte 16, 144 82 Potsdam, Germany

Wolfgang Gaessler - gaessler@mpia.de - Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany;

Elena Gallo - egallo@umich.edu - Department of Astronomy, University of Michigan, 1085 S University, Ann Arbor, MI 48104, USA

Philipp Huke - philipp.huke@hs-emden-leer.de - Institut für Astrophysik und Geophysik, Georg-August-Universität, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany and Institute for Laser and Optics, Hochschule Emden/Leer, Constantiaplatz 4, 26723 Emden, Germany;

Driss Kouach - driss.kouach@obs-mip.fr - Observatoire Midi-Pyrénées, CNRS, Université Paul Sabatier, 14 V. Ed. Belin 31400 Toulouse, France

David Lunney - david.lunney@stfc.ac.uk - ^lSTFC – United Kingdom Astronomy Technology Centre (UK ATC), Blackford Hill, Edinburgh, EH9 3HJ, United Kingdom

Alessandro Marconi - alessandro.marconi@inaf.it  - INAF- Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy;  and Dipartimento di Fisica e Astronomia, Università di Firenze via G. Sansone 1, I-50019, Sesto Fiorentino (Firenze), Italy

Piotr Masłowski - pima@fizyka.umk.pl - Institute of Physics, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University in Torun, ul. Grudziadzka 5, 87-100 Torun, Poland

Manuel Monteiro - Manuel.Monteiro@astro.up.pt - Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, PT4150-762 Porto, Portugal;

Enrico Pinna - enrico.pinna@inaf.it - INAF- Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy;

Chiara Selmi - chiara.selmi@inaf.it - INAF- Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy;

Francesca Sortino - francesca.sortino@inaf.it - INAF- Osservatorio Astronomico di Brera, via Brera 28, 20121 Milano, Italy;

Rossella Spiga - rossella.spiga@inaf.it - INAF- Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy;

Andrea Tozzi - andrea.tozzi@inaf.it - INAF- Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy;

Bachar Wehbe - bachar.wehbe@astro.up.pt - Instituto de Astrofísica e Ciências do Espaço, Universidade de Lisboa, Faculdade de Ciências, Campo Grande, PT1749-016 Lisboa, Portugal;

Alessio Zanutta - alessio.zanutta@inaf.it ^- INAF- Osservatorio Astronomico di Brera, via Brera 28, 20121 Milano, Italy;

Jennifer Zimara - jennifer.zimara@uni-goettingen.de - Institut für Astrophysik und Geophysik, Georg-August-Universität, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany;

The ESO/ELT ANDES (ArmazoNes high Dispersion Echelle Spectrograph) project successfully completed the system architecture review and is currently finalizing its preliminary design phase. ANDES is the high-resolution spectrograph for the ELT (ESO Extremely Large Telescope) capable of reaching a resolution of R ~ 100,000 simultaneously, in a wavelength range between 0.35 -2.4 µm (goals included), characterized by high-precision and extreme calibration accuracy suitable to address a variety of flagship scientific cases across a wide range of astronomical domains. To fulfill the required specifications the proposed design adopts a modular approach where the instrument is split in four individual spectrographs, each fiber-fed, and thermally and vacuum stabilized. A dedicated front-end which host a single conjugated adaptive optics module, collects either the light from the telescope or from a calibration unit feeding in turn the individual spectrographs. To master the described complexity the same modularity is reflected also at the project management level: each of the 9 subsystems (counting also the software as a standalone subsystem) is under direct responsibility of different teams coordinated by the ANDES project office. The high distribution and the large community involvement, consisting of 24 institutes from 13 countries, represent certainly a challenge from the project management point of view.

In this paper we present the project management approach we envisaged to master successfully all the ANDES project phases from the finalization of the preliminary design up to commissioning on-sky; in particular we will describe in detail the risk management and PA/QA activities we have foreseen to assure appropriate risk mitigation and an overall high quality standard required for the ANDES project.

16 - 21 June 2024

Yokohama, Japan

ANDES, the high resolution spectrograph for the ELT: Opto-mechanical design of the cameras for the YJH spectrograph

Étienne Artigau, Frédérique Baron, Denis Brousseau, René Doyon, Jonathan St-Antoine, Simon Thibault, Philippe Vallée, + other to be defined

TBC

16 - 21 June 2024

Yokohama, Japan

ANDES, the high resolution spectrograph for the ELT: The Exposure Time Calculator

Nicoletta Sanna

Bruno Canto, Allan Martins, Ernesto Oliva, Izan Leao, Alessio Turchi

16 - 21 June 2024

Yokohama, Japan

ANDES, the high resolution spectrograph for the ELT: UBV Spectrograph Preliminary Design

@Michael Weber

Michael Weber, Manfred Woche, Daniel Sablowski,
Katja Poppenhäger, Klaus Strassmeier, Julián David Alvarado-Gómez, Svend-Marian Bauer, Olga Bellido-Tirado, Joar Brynnel, Frank Dionies, Christine Füßlein, Domenico Giannone, Arto Järvinen, Silva Järvinen, Jonathan Kern, Hakan Önel, Jörg Weingrill,
Bruno Chazelas, Audrey Lanotte, Pablo Santos Diaz, Ludovic Genolet, Michael Sordet, Ian Hughes, Christophe Lovis, Manuel Amate, José Peñate Castro, Afrodisio Vega Moreno, Jonay I. González Hernández, María Rosa Zapatero Osorio, Rocío Calvo Ortega, Roberto Varas González, Wolfgang Gaessler, Michael Lehmitz, Adrian Kaminski, Ingo Stilz

submitted

Symposium: AS24

16 - 21 June 2024

Yokohama, Japan

ANDES, the high resolution spectrograph for the ELT: Extending to the K-Band

@Wolfgang Gaessler

W. Gaessler, Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany, gaessler@mpia.de

F. Baron, Département de physique Université de Montréal, Complexe des Sciences, PO Box 6128 Centre-Ville STN, Montreal QC H3C 3J7, Canada, frederique.baron@astro.umontreal.ca
W. Brandner, Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany, brandner@mpia.de
R. Doyon, Département de physique Université de Montréal, Complexe des Sciences, PO Box 6128 Centre-Ville STN, Montreal QC H3C 3J7, Canada, doyon@astro.umontreal.ca
M. Ebert, Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany, ebert@mpia.de
A. Kaminski, Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Königstuhl 12, D-69117 Heidelberg, Germany,
akaminsk@lsw.uni-heidelberg.de
L. Kreidberg, Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany, kreidberg@mpia.de
W. Laun, Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany, laun@mpia.de
M. Lehmitz, Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany, lehmitz@mpia.de
P. Mollière, Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany, molliere@mpia.de
A. Quirrenbach, Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Königstuhl 12, D-69117 Heidelberg, Germany,
A.Quirrenbach@lsw.uni-heidelberg.de
R-R. Rohloff, Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany, rohloff@mpia.de
W. Seifert, Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Königstuhl 12, D-69117 Heidelberg, Germany,
wseifert@lsw.uni-heidelberg.de
J. Stuermer, Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Königstuhl 12, D-69117 Heidelberg, Germany,
jstuermer@lsw.uni-heidelberg.de
J. St-Antoine, Département de physique Université de Montréal, Complexe des Sciences, PO Box 6128 Centre-Ville STN, Montreal QC H3C 3J7, Canada, jonathan.st-antoine@umontreal.ca
W. Xu, Optical System Engineering, Kirchenstr. 6, D-74937 Spechbach, Germany, w.xu@wenlixu-ose.de

ANDES is a high resolution spectrograph for the ELT, with the goal of providing simultaneous spectra with R~100000 from 0.35 to 2.4 micrometer. The baseline of the instrument covers 0.4 -1.8 micron. Here we present the study on the extension into the K-band (1.95 to 2.45 micron) with its scientific motivation and the technical solution. The spectrograph design is constrained by external limits, but a solution is found that enables key science cases in this wavelength range and closes the gap in ELT high resolution spectroscopy between the ANDES baseline and the METIS instrument. The spectrograph design is throughput-optimized and is fed by the diffraction-limited input from the ANDES SCAO system. We summarize the preliminary optical and cryo-mechanical design. But, as the available mass is one of the critical parameters, we also look into an alternative implementation of the spectrograph with carbon fiber vessels.