Design of the observation queue scheduler for WEAVE on the WHT

Fariña, C.; Domínguez-Palmero, Lilian; Benn, Chris; Guest, Steve; Morris, Huw; Picó, Sergio; Abrams, Don Carlos; Aguerri, J. A. L.; Bonifacio, P.; Carrasco, E.; Dalton, Gavin; Middleton, Kevin; Trager, S. C.; Vallenari, A.

doi:10.1117/12.2312538

Cited by 2 publications

References 8 publications

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The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation

Jin

Trager

Dalton

et al. 2023

Monthly Notices of the Royal Astronomical Society

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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.

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The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation

Jin

Trager

Dalton

et al. 2023

Monthly Notices of the Royal Astronomical Society

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The WEAVE observatory control system

Picó

Abrams

Benn

et al. 2018

Observatory Operations: Strategies, Processes, and Systems VII

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WEAVE is the next-generation spectroscopic facility for the William Herschel Telescope (WHT) 1,2 . WEAVE offers multi-object (1000 fibres) and integral-field spectroscopy at two resolutions (R ~ 5000, 20000) over a 2-deg field of view at prime focus and will mainly provide follow up of ground-based (LOFAR) and space-based (GAIA) surveys.The Observatory Control System (OCS) is responsible for providing the software control and feedback framework through which WEAVE will be operated. This paper summarizes the design of the different OCS subsystems and the interfaces between them and other WEAVE components.In the remainder of this paper, Section 2 outlines the other WEAVE systems with which the OCS interacts, Section 3 describes the system architecture, Section 4 comments on system-architecture decisions, Section 5 describes the main components of the OCS, Section 6 outlines the life-cycle of an OCS Observing Block and, finally, Section 7 gives an overview of the OCS testing plan.

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Design of the observation queue scheduler for WEAVE on the WHT

Cited by 2 publications

References 8 publications

The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation

The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation

The WEAVE observatory control system

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