2026-04-17T03:24:31Zhttps://recercat.cat/oai/request

oai:recercat.cat:2117/4077962026-01-21T09:38:26Zcom_2072_1033col_2072_452950

The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation Jin, Shuanggen Drew, Janet E. Gänsicke, Boris T. Aguado Fernández, Maria Dolores Antoja, T. Babusiaux, C. Battaglia, Giuseppe Hoskin, Matthew Pérez Ràfols, Ignasi Pico, Sandra Raddi, Roberto Ashley, R. P. Bernard, Escudié Bosma, A. Cantat Gaudin, Tristan Castro Ginard, Alfred Casamiquela Floriach, Laia Figueras Siñol, Francesca Greimel, Robert Hughes, Samantha J. Jordi Nebot, Carme Barberá Flichi, Francesc Larsen, Sine Miralda Escudé, Jordi Morelli, Luca Naylor, Tim Hochrainer, M Ramos, Pau Grossi, Emanuele Sanna, Nico Steele, I. A. Vink, J Wilson, Alice Wright, Nicholas Zurita, C Universitat Politècnica de Catalunya. Departament de Física Universitat Politècnica de Catalunya. Departament d'Enginyeria Mecànica Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica Àrees temàtiques de la UPC::Física::Astronomia i astrofísica WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, will see first light in late 2022. WEAVE comprises a new 2-degree field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable ‘mini’ integral field units (IFUs), and a single large IFU. These fibre systems feed a dual-beam spectrograph covering the wavelength range 366-959 nm at R ~ 5000, or two shorter ranges at R ~ 20¿000. After summarising the design and implementation of WEAVE and its data systems, we present the organisation, science drivers and design of a five- to seven-year programme of eight individual surveys to: (i) study our Galaxy’s origins by completing Gaia’s phase-space information, providing metallicities to its limiting magnitude for ~3 million stars and detailed abundances for ~1.5 million brighter field and open-cluster stars; (ii) survey ~0.4 million Galactic-plane OBA stars, young stellar objects and nearby gas to understand the evolution of young stars and their environments; (iii) perform an extensive spectral survey of white dwarfs; (iv) survey ~400 neutral-hydrogen-selected galaxies with the IFUs; (v) study properties and kinematics of stellar populations and ionised gas in z < 0.5 cluster galaxies; (vi) survey stellar populations and kinematics in ~25¿000 field galaxies at 0.3 ¿ z ¿ 0.7; (vii) study the cosmic evolution of accretion and star formation using >1 million spectra of LOFAR-selected radio sources; (viii) trace structures using intergalactic/circumgalactic gas at z > 2. Finally, we describe the WEAVE Operational Rehearsals using the WEAVE Simulator. Postprint (published version) 2023-03-11 Article Jin, S. [et al.]. The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation. "Monthly notices of the Royal Astronomical Society", 11 Març 2023, 0035-8711 https://hdl.handle.net/2117/407796 10.1093/mnras/stad557 eng https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stad557/7076341 http://creativecommons.org/licenses/by-nc-nd/4.0/ Open Access Attribution-NonCommercial-NoDerivatives 4.0 International application/pdf Oxford University Press