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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.
Jin, S., Trager, S., Dalton, G., Aguerri, J., Drew, J., Falcón-Barroso, J., et al. (2023). The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY [10.1093/mnras/stad557].
The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation
Jin, Shoko
;Trager, Scott C;Dalton, Gavin B;Aguerri, J Alfonso L;Drew, J E;Falcón-Barroso, Jesús;Gänsicke, Boris T;Hill, Vanessa;Iovino, Angela;Pieri, Matthew M;Poggianti, Bianca M;Smith, D J B;Vallenari, Antonella;Abrams, Don Carlos;Aguado, David S;Antoja, Teresa;Aragón-Salamanca, Alfonso;Ascasibar, Yago;Babusiaux, Carine;Balcells, Marc;Barrena, R;Battaglia, Giuseppina;Belokurov, Vasily;Bensby, Thomas;Bonifacio, Piercarlo;Bragaglia, Angela;Carrasco, Esperanza;Carrera, Ricardo;Cornwell, Daniel J;Domínguez-Palmero, Lilian;Duncan, Kenneth J;Famaey, Benoit;Fari na, Cecilia;Gonzalez, Oscar A;Guest, Steve;Hatch, Nina A;Hess, Kelley M;Hoskin, Matthew J;Irwin, Mike;Knapen, Johan H;Koposov, Sergey E;Kuchner, Ulrike;Laigle, Clotilde;Lewis, Jim;Longhetti, Marcella;Lucatello, Sara;Méndez-Abreu, Jairo;Mercurio, Amata;Molaeinezhad, Alireza;Monguió, Maria;Morrison, Sean;Murphy, David N A;de Arriba, Luis Peralta;Pérez, Isabel;Pérez-Ràfols, Ignasi;Picó, Sergio;Raddi, Roberto;Romero-Gómez, Mercè;Royer, Frédéric;Siebert, Arnaud;Seabroke, George M;Som, Debopam;Terrett, David;Thomas, Guillaume;Wesson, Roger;Worley, C Clare;Alfaro, Emilio J;Prieto, Carlos Allende;Alonso-Santiago, Javier;Amos, Nicholas J;Ashley, Richard P;Balaguer-Nú nez, Lola;Balbinot, Eduardo;Bellazzini, Michele;Benn, Chris R;Berlanas, Sara R;Bernard, Edouard J;Best, Philip;Bettoni, Daniela;Bianco, Andrea;Bishop, Georgia;Blomqvist, Michael;Boeche, Corrado;Bolzonella, Micol;Bonoli, Silvia;Bosma, Albert;Britavskiy, Nikolay;Busarello, Gianni;Caffau, Elisabetta;Cantat-Gaudin, Tristan;Castro-Ginard, Alfred;Couto, Guilherme;Carbajo-Hijarrubia, Juan;Carter, David;Casamiquela, Laia;Conrado, Ana M;Corcho-Caballero, Pablo;Costantin, Luca;Deason, Alis;de Burgos, Abel;De Grandi, Sabrina;Di Matteo, Paola;Domínguez-Gómez, Jesús;Dorda, Ricardo;Drake, Alyssa;Dutta, Rajeshwari;Erkal, Denis;Feltzing, Sofia;Ferré-Mateu, Anna;Feuillet, Diane;Figueras, Francesca;Fossati, Matteo;Franciosini, Elena;Frasca, Antonio;Fumagalli, Michele;Gallazzi, Anna;García-Benito, Rubén;Fusillo, Nicola Gentile;Gebran, Marwan;Gilbert, James;Gledhill, T M;Delgado, Rosa M González;Greimel, Robert;Guarcello, Mario Giuseppe;Guerra, Jose;Gullieuszik, Marco;Haines, Christopher P;Hardcastle, Martin J;Harris, Amy;Haywood, Misha;Helmi, Amina;Hernandez, Nauzet;Herrero, Artemio;Hughes, Sarah;Irsic, Vid;Jablonka, Pascale;Jarvis, Matt J;Jordi, Carme;Kondapally, Rohit;Kordopatis, Georges;Krogager, Jens-Kristian;Barbera, Francesco La;Lam, Man I;Larsen, Søren S;Lemasle, Bertrand;Lewis, Ian J;Lhomé, Emilie;Lind, Karin;Lodi, Marcello;Longobardi, Alessia;Lonoce, Ilaria;Magrini, Laura;Apellániz, Jesús Maíz;Marchal, Olivier;Marco, Amparo;Martin, Nicolas F;Matsuno, Tadafumi;Maurogordato, Sophie;Merluzzi, Paola;Miralda-Escudé, Jordi;Molinari, Emilio;Monari, Giacomo;Morelli, Lorenzo;Mottram, Christopher J;Naylor, Tim;Negueruela, Ignacio;Onorbe, Jose;Pancino, Elena;Peirani, Sébastien;Peletier, Reynier F;Pozzetti, Lucia;Rainer, Monica;Ramos, Pau;Read, Shaun C;Rossi, Elena Maria;Röttgering, Huub J A;Rubi no-Martín, Jose Alberto;Montes, Jose Sabater;Juan, José San;Sanna, Nicoletta;Schallig, Ellen;Schiavon, Ricardo P;Schultheis, Mathias;Serra, Paolo;Shimwell, Timothy W;Simón-Díaz, Sergio;Smith, Russell J;Sordo, Rosanna;Sorini, Daniele;Soubiran, Caroline;Starkenburg, Else;Steele, Iain A;Stott, John;Stuik, Remko;Tolstoy, Eline;Tortora, Crescenzo;Tsantaki, Maria;Van der Swaelmen, Mathieu;van Weeren, Reinout J;Vergani, Daniela;Verheijen, Marc A W;Verro, Kristiina;Vink, Jorick S;Vioque, Miguel;Walcher, C Jakob;Walton, Nicholas A;Wegg, Christopher;Weijmans, Anne-Marie;Williams, Wendy L;Wilson, Andrew J;Wright, Nicholas J;Xylakis-Dornbusch, Theodora;Youakim, Kris;Zibetti, Stefano;Zurita, Cristina
2023
Abstract
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.
Jin, S., Trager, S., Dalton, G., Aguerri, J., Drew, J., Falcón-Barroso, J., et al. (2023). The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY [10.1093/mnras/stad557].
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/10281/473793
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simulazione ASN
Il report seguente simula gli indicatori relativi alla propria produzione scientifica in relazione alle soglie ASN 2023-2025 del proprio SC/SSD. Si ricorda che il superamento dei valori soglia (almeno 2 su 3) è requisito necessario ma non sufficiente al conseguimento dell'abilitazione. La simulazione si basa sui dati IRIS e sugli indicatori bibliometrici alla data indicata e non tiene conto di eventuali periodi di congedo obbligatorio, che in sede di domanda ASN danno diritto a incrementi percentuali dei valori. La simulazione può differire dall'esito di un’eventuale domanda ASN sia per errori di catalogazione e/o dati mancanti in IRIS, sia per la variabilità dei dati bibliometrici nel tempo. Si consideri che Anvur calcola i valori degli indicatori all'ultima data utile per la presentazione delle domande.
La presente simulazione è stata realizzata sulla base delle specifiche raccolte sul tavolo ER del Focus Group IRIS coordinato dall’Università di Modena e Reggio Emilia e delle regole riportate nel DM 598/2018 e allegata Tabella A. Cineca, l’Università di Modena e Reggio Emilia e il Focus Group IRIS non si assumono alcuna responsabilità in merito all’uso che il diretto interessato o terzi faranno della simulazione. Si specifica inoltre che la simulazione contiene calcoli effettuati con dati e algoritmi di pubblico dominio e deve quindi essere considerata come un mero ausilio al calcolo svolgibile manualmente o con strumenti equivalenti.