论文标题
宽场，多路复用，光谱设施编织：调查设计，概述和模拟实施
The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation
论文作者
论文摘要
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.这些光纤系统为覆盖波长范围366 $ - $ 959 \ $ r \ sim5000 $或两个较短的范围的双光束光谱仪366 $ - $ 959 \，nm，$ r \ sim20 \，000 $。在总结了编织及其数据系统的设计和实施之后，我们介绍了五到七年计划的组织，科学驱动因素和设计，该计划通过完成Gaia的相位信息来研究我们的银河的起源，从而为Gaia的相位信息完成，为$ \ sim $ \ sim $ \ sim $ \ sim $ \ simble of Simbulance and oble of Simbullance and oble提供了金属的金属，并为$ \ simbullance oble of sim1.5 $ \ brimbulter提供了金属。 （ii）调查$ \ sim0.4 $ $ $ $ $ $ \ $ \ $ \ $ \ $ \ $ \ $ \ $ \ $ \ $ \ $ \ $ \ $ \ $ \ $ \ $ \ $ \ $ \ $ \ $ \ $ \ $ \ $ \ $ \ $ \ sim0.4 $ \ sim0.4 $ \ sim的恒星和附近的天然气，以了解年轻恒星及其环境的演变； （iii）对白矮人进行广泛的光谱调查； （iv）调查$ \ sim400 $带有IFUS的中性氢化星系； （v）恒星种群和离子气体的研究属性和运动型，$ z <0.5 $集群星系； （vi）$ \ sim25 \，000 $ field Galaxies $ 0.3 \ Lessim Z \ Lessim 0.7 $ 0.7 $; （vii）使用$> 100万美元的Lofar选择的无线电来源研究积聚和恒星形成的宇宙演变； （viii）使用$ z> 2 $的层间/圆形气体使用痕量结构。最后，我们使用编织模拟器来描述编织的操作排练。
WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, will see first light in late 2022. WEAVE comprises a new 2-degree field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable 'mini' integral field units (IFUs), and a single large IFU. These fibre systems feed a dual-beam spectrograph covering the wavelength range 366$-$959\,nm at $R\sim5000$, or two shorter ranges at $R\sim20\,000$. 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 $\sim$3 million stars and detailed abundances for $\sim1.5$ million brighter field and open-cluster stars; (ii) survey $\sim0.4$ 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 $\sim400$ 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 $\sim25\,000$ field galaxies at $0.3\lesssim z \lesssim 0.7$; (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.
