<figure><img src="image_24.png" /><figcaption>**Figure 24.** Simulated spectrum (in blue) of an A star with $T_{\text{eff}} = 9000$ K, $\log g = 4.0$ in the calcium-triplet region, compared with the best fit (in orange and with fewer features) obtained using the method of Harris et al. (2018). The biases in the returned parameters (measured minus input) for $T_{\text{eff}}$, log g, and radial velocity are –11 K, –0.003 dex, and +0.7 km s⁻¹, respectively.</figcaption></figure>

transfer of data from the ‘telescope’ to CASU (Cambridge) were performed at night (i.e. in ‘real time’) to emulate – and hence also to verify – the network traffic in a realistic manner. The resulting data sets were then made available to the QAG and SWG for analysis.

A key aspect of this process is that every step in the data flow should occur automatically, driven only by the observation description and calibration templates in the OB, and by information generated internally within the CPS and APS, which have no prior knowledge of the input target parameters beyond the basic photometric data. Flux calibrations were generated from the white dwarf calibration stars within each field, and the sky and object fibres were subjected to the variations in throughput arising from the non-telecentricity and vignetting in the optical models.

Figs 24–27 provide a few illustrative results from Operational Rehearsal 3b (OpR3b; see also Fig. 17). As the first end-to-end test of the complete CPS and APS pipelines, it was not expected that we would meet our science goals in the output of these systems in OpR3b. Rather, the intention was to stress-test the data-flow set-up and the pipelines themselves, which could then be used to make any necessary improvements. Through the rehearsal, a number of undesirable effects were identified and corrected in both the input fields generated by some of the surveys and in the data-processing and analysis chains, illustrating the value of conducting such an exercise in advance of the instrument commissioning phase. An example of such an effect is the noticeable curvature in the residual log g and microturbulence values as a function of fibre location on the detector arrays for stars observed by the WEAVE GA survey (shown in Fig. 25), symptomatic of an uncorrected spectral-resolution variation with wavelength in the high-resolution spectral mode (cf. Fig. 23, which shows a similar variation as a function of fibre location for the low-resolution spectral mode). On the other hand, Fig. 27 shows that the WEAVE Simulator and the WEAVE exposure time calculator (ETC), developed independently, are on average in excellent agreement for faint (WQ) targets, suggesting that the ETC can be used with some confidence for planning WEAVE observations.

## 6.3 Operational Rehearsal 3c

Operational Rehearsal 3c (OpR3c) was a scheduling exercise covering a virtual period of 18 contiguous months. The 18 months were split into trimesters (named T1–T6), each covering 3 months. These

six periods allowed us to test the SCHEDULER’s OB queue creation with WEAVE’s full complement of observing modes: the LIFU, the mLIFU, and the two MOS plates. In essence, OpR3c was a significantly scaled-up version of OpR3a, taking lessons learnt from both OpR3a and OpR3b and attempting a close-to-reality scheduling simulation for the use of WEAVE on the WHT. As such, we also included a representative sample of OBs belonging to ‘PI time’, which entered the SCHEDULER queue alongside the WEAVE Survey OBs, as will occur during regular Survey operations.

As well as all envisaged observing modes being available for scheduling purposes, the single main difference of OpR3c to OpR3a was in the length of the rehearsal, both in virtual and real time. Two months of ‘Survey time’ were simulated almost every week, with 18 months of virtual observing time scheduled in total. Approximately every two weeks, the OISMT released the outcome of the scheduling exercise of the current trimester to the SWG, offset by one month, e.g. for the first trimester (T1), for which the SWG had submitted fields for months 1–3, the OISMT then released scheduling results for months 1–2 to the SWG, which the SWG then used to decide on their submissions for months 4–6 (i.e. T2). The SWG members were required, in consultation with their STLs and relevant science team members, to make decisions within three to four working days regarding the next set of fields to submit for the following trimester, based on the knowledge of which fields had been observed. While there is an overall observing strategy for the planned five-year WEAVE Survey for every individual survey, making the decision of which fields to prioritize and which specific targets should be contained within those fields requires knowledge of what has or has not – despite the OBs having already been submitted – yet been observed. The actual WEAVE Survey operations will also follow a trimesterly cycle for field submissions by the SWG, making OpR3c a realistic – if somewhat condensed and highly time-pressured – simulation of what is to come. Note that while the intensive and relatively rigid real-time schedule was set up to enable the SWG and STLs to rehearse decision making on realistic timescales, the intervals, and timing offsets later did require some flexibility and shifting at times, primarily due to the availability of those involved in the exercise.

One of the principal aims of OpR3c was to identify any missing pieces in the operational flow for WEAVE operations. The following list provides an example of the types of questions raised and issues identified, some of which were resolved in real time during OpR3c, and all of which require resolving prior to the start of WEAVE operations.

(i) OpR3c allowed science teams to identify which other surveys typically compete for similar observing conditions, modes, and sky positions. This in turn helped us identify new functionalities to be implemented in the SCHEDULER, allowing for a better sampling of OBs from the OB database, thereby creating both a better balance of OBs observed across the different surveys as well as better OB selection within each survey according to its science goals. OpR3c further identified some collisions between surveys whose science requirements call for similar observing conditions, which have now been ameliorated through adjustments made to the relative, inter-survey observation-time allocations in the survey planning.

(ii) The combined effect of the requests in right-ascension distribution, observing conditions, and instrumental set-up by community PI programmes cannot be predicted in advance, and neither, therefore, can the effect that this will have on their interplay with the WEAVE surveys in the OB scheduling process. OpR3c simulated the contribution of PI programmes to the scheduling process by incorporating a wide range of observing requirements (weather
<figure><img src="image_25.png" /><figcaption>**Figure 25.** APS output compared with the input to the WEAVE Simulator for high-resolution green+red GA-HR data in OpR3b in the form of density plots, where yellow indicates regions of highest density and purple the lowest density regions, passing through green and blue for intermediate densities. The panels show the difference (output – input) for the parameters $T_{\text{eff}}$, log g, [M/H], [α/Fe], and microturbulence (in km s⁻¹) from top to bottom, as a function of input value (left), mean S/N between the blue and red arms (middle), and the fibre location on the detector (right). We note that the curvature seen in the right column (as a function of fibre location) in log g and microturbulence results from uncorrected spectral-resolution variation in the APS pipeline, which has since been addressed in an updated version of the pipeline (see Section 6.2).</figcaption></figure>

conditions and observing modes) that was also varied trimesterly. Although no simulation can truly emulate (or help predict) the effect of combining PI programmes and the WEAVE Survey during WEAVE operations, OpR3c has helped us identify ways in which the balancing of these components could be achieved.

(iii) A small number of empty slots were identified in the SCHEDULER output, indicating sky conditions that could not be used by any WEAVE survey. These tended to correspond to poor seeing (>2 arcsec) during bright time (where there were no OBs available from the Survey or simulated PI programmes) and came to a total of 15 one-hour slots (out of a total of ~3500) over the course of 18 months. A PI or WEAVE science programme that can utilize such conditions would therefore be a favourable complement from a scheduling perspective. WL and WQ are amongst the science teams planning to use the WEAVE integral-field spectrographs (mIFU and LIFU) in relatively undersubscribed weather conditions to ameliorate this issue, so that no usable telescope time is left unfilled.

(iv) The weighting of different factors (such as seeing, sky brightness, and moon distance) by the SCHEDULER in choosing which

OB should be queued requires re-evaluation and retesting. Giving higher weight to the seeing at the location of the field (which is affected by its airmass, i.e. its elevation) relative to other factors tends to disfavour those OBs that never reach low airmasses due to their declination. This biasing has been fixed in the most recent version of the SCHEDULER.

(v) OBs should have expiration dates so that the OB database at the OCS (in general) contains only currently observable OBs, and to allow surveys to refresh the content of the OB database in case of changes in their plans. An expiration date of 9 months after ingestion is now set for any OB entering the database. An exception to this rule is if there are OBs in the database belonging to an already started 'chain' (i.e. duplicate OBs to enable a longer total exposure of the field), in which case the remaining OBs have their expiration dates removed.

(vi) There is a need for the ability to retract OBs (prior to them being observed) or data (at different stages of the data-processing and archiving process). Necessary protocols for this within the SPA are now mostly implemented.
<figure><img src="image_25.png" /><figcaption>**Figure 25.** APS output compared with the input to the WEAVE Simulator for high-resolution green+red GA-HR data in OpR3b in the form of density plots, where yellow indicates regions of highest density and purple the lowest density regions, passing through green and blue for intermediate densities. The panels show the difference (output – input) for the parameters $T_{\text{eff}}$, log g, [M/H], [α/Fe], and microturbulence (in km s⁻¹) from top to bottom, as a function of input value (left), mean S/N between the blue and red arms (middle), and the fibre location on the detector (right). We note that the curvature seen in the right column (as a function of fibre location) in log g and microturbulence results from uncorrected spectral-resolution variation in the APS pipeline, which has since been addressed in an updated version of the pipeline (see Section 6.2).</figcaption></figure>

conditions and observing modes) that was also varied trimesterly. Although no simulation can truly emulate (or help predict) the effect of combining PI programmes and the WEAVE Survey during WEAVE operations, OpR3c has helped us identify ways in which the balancing of these components could be achieved.

(iii) A small number of empty slots were identified in the SCHEDULER output, indicating sky conditions that could not be used by any WEAVE survey. These tended to correspond to poor seeing (>2 arcsec) during bright time (where there were no OBs available from the Survey or simulated PI programmes) and came to a total of 15 one-hour slots (out of a total of ~3500) over the course of 18 months. A PI or WEAVE science programme that can utilize such conditions would therefore be a favourable complement from a scheduling perspective. WL and WQ are amongst the science teams planning to use the WEAVE integral-field spectrographs (mIFU and LIFU) in relatively undersubscribed weather conditions to ameliorate this issue, so that no usable telescope time is left unfilled.

(iv) The weighting of different factors (such as seeing, sky brightness, and moon distance) by the SCHEDULER in choosing which

OB should be queued requires re-evaluation and retesting. Giving higher weight to the seeing at the location of the field (which is affected by its airmass, i.e. its elevation) relative to other factors tends to disfavour those OBs that never reach low airmasses due to their declination. This biasing has been fixed in the most recent version of the SCHEDULER.

(v) OBs should have expiration dates so that the OB database at the OCS (in general) contains only currently observable OBs, and to allow surveys to refresh the content of the OB database in case of changes in their plans. An expiration date of 9 months after ingestion is now set for any OB entering the database. An exception to this rule is if there are OBs in the database belonging to an already started ‘chain’ (i.e. duplicate OBs to enable a longer total exposure of the field), in which case the remaining OBs have their expiration dates removed.

(vi) There is a need for the ability to retract OBs (prior to them being observed) or data (at different stages of the data-processing and archiving process). Necessary protocols for this within the SPA are now mostly implemented.
<figure><img src="image_26.png" /></figure>

**Figure 26.** Redshift estimation for WL targets from a model WL-DEEP OB observed in OpR3b, targeting 150 MHz sources brighter than 100 µJy. The redshift estimate from the APS [derived using the off-the-shelf redrock code is shown on the vertical axis, as a function of the true redshift (taken from the input simulation)], and colour-coded by the I-band apparent magnitude. While the vast majority of targets are correctly redshifted out to $z = 1$ (93.3 per cent of redshifts are correct to $|z_{APS} - z_{true}| < 0.001$), there is some evidence of emission-line mis-identification (e.g. the linear features away from the 1:1 line) and bright targets with incorrect redshifts, perhaps highlighting the need to fold in photometric redshift priors and to optimize/update the redshifting templates once data begin to arrive in earnest. The redshifting performance for the WL survey will be discussed in more detail in a forthcoming work (Smith et al., in preparation).

<figure><img src="image_27.png" /></figure>

**Figure 27.** Signal-to-noise per Å as a function of apparent magnitude, estimated from simulated WQ data and the WEAVE ETC. Here, magnitude and S/N are both defined in Johnson filters. The results of the WEAVE ETC (v4.2.4, identical red crosses spanning the magnitude range) and the measured OpR3 mock data both per spectrum (filled grey circles) and binned (black crosses) are shown. As the WEAVE Simulator and ETC are completely independent codes, the excellent agreement at the faint end is reassuring for prospective WEAVE users; the deviation at the bright end is likely due to a combination of the variation of throughput with fibre position in the focal plane due to non-telecentricity and from vignetting, and to issues related to precise spectral shape and redshift of the simulated targets, neither of which the ETC takes into account in the current version.

## 6.4 Benefits of the Operational Rehearsals

Interactions between the SPA teams and the Science Team through the work of the SWG and QAG has been – and continues to be – crucial for identifying critical areas requiring further development within the data-processing systems (CPS and APS), while feedback from test users of the archive system has been essential in ensuring that the WAS user interface is simultaneously user friendly and powerful. Within the Science Team, the OpRs have allowed us to identify details of specifics, as well as the order of play, for a multitude of tasks not confined to the following: putting together input target catalogues; how to specify sky positions; how to efficiently manage the configuration of dozens to hundreds of field configurations; the need to create software (codes and scripts) that could, in principle, be run by any individual with sufficient understanding of the process (avoiding single-point failures in manpower); how to deal with fields containing targets from multiple surveys. The OpRs have involved the efforts of more than 70 people, with many processes having been performed under realistic time pressure.

## 7 SUMMARY

In an era of ever-increasing telescope and survey sizes, following up initial observations of large numbers of objects with medium- and high-resolution spectroscopy with modestly sized telescopes has been widely identified as a vital component of modern astrophysical research. In this context, we present WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the WHT. WEAVE comprises a new, 2-deg-diameter field-of-view, prime-focus corrector system with a nearly 1000-multiplex fibre positioner, 20 individually deployable mIFUs, and a single LIFU. The MOS fibres and mIFU fibre bundles are placed by two robots working in tandem at the WHT prime focus. These fibre systems feed a dual-beam spectrograph that covers 366–959 nm at $R \sim 5000$, or two shorter ranges at $R \sim 20000$.

The WEAVE Survey is a spectroscopic survey of the Northern sky, using WEAVE to answer key questions about the evolution of our own Galaxy and other galaxies, dark matter, and dark energy, and is comprised of eight individual surveys.

(i) The WEAVE GA survey will complete Gaia's phase-space information, providing metallicities for nearly three million MSTO and red giant stars, as well as providing detailed abundances for up to 1.5 million brighter stars in four sub-surveys: the high-latitude LR survey, observing more than 1.5 million stars over nearly 9000 deg² of the Northern sky; the disc-dynamics LR survey of more than a million stars along 500 sight-lines through the Galactic disc; the HR chemo-dynamical survey of more than 1.5 million stars across 5650 deg² (non-contiguous) of the Northern sky; and the OCs survey of more than one hundred OCs of a variety of evolutionary states in the HR mode.

(ii) The SCIP survey will observe ~400 000 evolved stars and the ISM in the Galactic plane, covering 1200 deg² in the LR mode and regions in the Cygnus star-forming region and the Galactic Anticentre in the HR mode.

(iii) The WEAVE White Dwarfs survey will be one of the largest spectral surveys of white dwarfs ever undertaken, piggybacking on top of the other WEAVE surveys and targeting more than 50 000 white dwarfs.

(iv) WEAVE-Apertif is an IFU survey of ≈400 neutral-hydrogen-selected galaxies in the LR mode, with detailed follow-up of ~100 of these in the HR mode.
<figure><img src="image_26.png" /><figcaption>**Figure 26.** Redshift estimation for WL targets from a model WL-DEEP OB observed in OpR3b, targeting 150 MHz sources brighter than 100 µJy. The redshift estimate from the APS [derived using the off-the-shelf redrock code is shown on the vertical axis, as a function of the true redshift (taken from the input simulation)], and colour-coded by the I-band apparent magnitude. While the vast majority of targets are correctly redshifted out to $z = 1$ (93.3 per cent of redshifts are correct to $|z_{APS} - z_{true}| < 0.001$), there is some evidence of emission-line mis-identification (e.g. the linear features away from the 1:1 line) and bright targets with incorrect redshifts, perhaps highlighting the need to fold in photometric redshift priors and to optimize/update the redshifting templates once data begin to arrive in earnest. The redshifting performance for the WL survey will be discussed in more detail in a forthcoming work (Smith et al., in preparation).</figcaption></figure>

<figure><img src="image_27.png" /><figcaption>**Figure 27.** Signal-to-noise per Å as a function of apparent magnitude, estimated from simulated WQ data and the WEAVE ETC. Here, magnitude and S/N are both defined in Johnson filters. The results of the WEAVE ETC (v4.2.4, identical red crosses spanning the magnitude range) and the measured OpR3 mock data both per spectrum (filled grey circles) and binned (black crosses) are shown. As the WEAVE Simulator and ETC are completely independent codes, the excellent agreement at the faint end is reassuring for prospective WEAVE users; the deviation at the bright end is likely due to a combination of the variation of throughput with fibre position in the focal plane due to non-telecentricity and from vignetting, and to issues related to precise spectral shape and redshift of the simulated targets, neither of which the ETC takes into account in the current version.</figcaption></figure>

## 6.4 Benefits of the Operational Rehearsals

Interactions between the SPA teams and the Science Team through the work of the SWG and QAG has been – and continues to be – crucial for identifying critical areas requiring further development within the data-processing systems (CPS and APS), while feedback from test users of the archive system has been essential in ensuring that the WAS user interface is simultaneously user friendly and powerful. Within the Science Team, the OpRs have allowed us to identify details of specifics, as well as the order of play, for a multitude of tasks not confined to the following: putting together input target catalogues; how to specify sky positions; how to efficiently manage the configuration of dozens to hundreds of field configurations; the need to create software (codes and scripts) that could, in principle, be run by any individual with sufficient understanding of the process (avoiding single-point failures in manpower); how to deal with fields containing targets from multiple surveys. The OpRs have involved the efforts of more than 70 people, with many processes having been performed under realistic time pressure.

## 7 SUMMARY

In an era of ever-increasing telescope and survey sizes, following up initial observations of large numbers of objects with medium- and high-resolution spectroscopy with modestly sized telescopes has been widely identified as a vital component of modern astrophysical research. In this context, we present WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the WHT. WEAVE comprises a new, 2-deg-diameter field-of-view, prime-focus corrector system with a nearly 1000-multiplex fibre positioner, 20 individually deployable mIFUs, and a single LIFU. The MOS fibres and mIFU fibre bundles are placed by two robots working in tandem at the WHT prime focus. These fibre systems feed a dual-beam spectrograph that covers 366–959 nm at $R \sim 5000$, or two shorter ranges at $R \sim 20000$.

The WEAVE Survey is a spectroscopic survey of the Northern sky, using WEAVE to answer key questions about the evolution of our own Galaxy and other galaxies, dark matter, and dark energy, and is comprised of eight individual surveys.

(i) The WEAVE GA survey will complete Gaia's phase-space information, providing metallicities for nearly three million MSTO and red giant stars, as well as providing detailed abundances for up to 1.5 million brighter stars in four sub-surveys: the high-latitude LR survey, observing more than 1.5 million stars over nearly 9000 deg² of the Northern sky; the disc-dynamics LR survey of more than a million stars along 500 sight-lines through the Galactic disc; the HR chemo-dynamical survey of more than 1.5 million stars across 5650 deg² (non-contiguous) of the Northern sky; and the OCs survey of more than one hundred OCs of a variety of evolutionary states in the HR mode.

(ii) The SCIP survey will observe ~400 000 evolved stars and the ISM in the Galactic plane, covering 1200 deg² in the LR mode and regions in the Cygnus star-forming region and the Galactic Anticentre in the HR mode.

(iii) The WEAVE White Dwarfs survey will be one of the largest spectral surveys of white dwarfs ever undertaken, piggybacking on top of the other WEAVE surveys and targeting more than 50 000 white dwarfs.

(iv) WEAVE-Apertif is an IFU survey of ≈400 neutral-hydrogen-selected galaxies in the LR mode, with detailed follow-up of ~100 of these in the HR mode.
(v) WEAVE Galaxy Clusters is a survey of stellar populations, ionized gas properties, and stellar and ionized gas kinematics in cluster galaxies and their outskirts out to $z \sim 0.5$ using all of WEAVE's fibre modes (MOS, mIFU, and LIFU), split into the Nearby, Wide-Field, and Cosmological Clusters sub-surveys.

(vi) StePS is a survey of detailed stellar populations and stellar kinematics in ~25 000 individual field galaxies, the majority within $0.3 \le z \le 0.7$.

(vii) WL will obtain around one million spectra of sources selected on the basis of their activity from the LoTSS. The survey will have a wedding-cake structure with three tiers ranging from WL-Wide (~9000 deg² of the Northern Sky) to WL-Deep (up to 60 deg² in the LoTSS Deep Fields), together efficiently sampling the luminosity and redshift plane, and observing statistical samples of galaxies and AGNs selected in a manner that is unbiased by dust.

(viii) WQ is a survey of the IGM at $z > 2.1$ and a very sensitive probe of baryonic acoustic oscillations at $z > 2.4$ using absorption lines along the line of sight to ~400 000 quasars.

We have developed new, two-phase, dedicated data-processing pipelines for WEAVE, producing both reduced (via the CPS) and science-ready (via the APS) data, with a modular architecture allowing for additional analysis software to be developed as necessary by the science teams to be incorporated into the APS. Outputs from these pipelines populate a dedicated data archive (WAS), which will also store CDPs. WEAVE also requires a new control system at the Observatory (OCS), enabling queue-based observations, in which user-submitted XML files describing the desired telescope and spectrograph settings with MOS or m/LIFU field configurations are converted into OBs and stored in an OB management system that is sampled by the queue SCHEDULER for use by the telescope operator and/or the support astronomer. The entire data system has been exercised in a series of Operational Rehearsals, starting with the end-to-end WEAVE instrument Simulator, which 'observes' synthetic data that are then passed through the OCS to the CPS and the APS, and finally into the WAS. Many lessons about the data flow, survey design, and observation scheduling have been learnt by simulating periods between three weeks (full simulated images) and 1.5 years (nightly scheduling) of the WEAVE Survey. As an example, we suggest that PI observations using poor seeing (>2 arcsec) conditions in bright time would favourably complement the WEAVE Survey programme.

The WEAVE Survey will begin observations towards the end of 2023. All processed WEAVE data and CDPs will be released to the worldwide astronomy community through the WAS annually, beginning 2 years after the start of the WEAVE Survey (i.e. late 2025), and astronomers in the WEAVE Survey Consortium will have access to the data soon after the data have been taken and reduced. A Science Verification (SV) campaign immediately preceding the WEAVE Survey will test various aspects of the surveys and carry out more than a dozen programmes submitted by the ING community (astronomers in the UK, The Netherlands, and Spain, plus their collaborators); all SV data are expected to be reduced and released to the ING and WEAVE community within 6 months of the end of the SV campaign.

WEAVE represents a significant next step forward in our understanding of the Universe around us. The planned surveys will provide data that will help answer the questions: How did our Galaxy form and the stars within it evolve? How were other galaxies assembled? What are dark matter and dark energy?

## ACKNOWLEDGEMENTS

We would like to thank the reviewers of the WEAVE Survey Strategy Review held at Observatoire de Paris (2015 October 19–20), M. Bershady, G. Hill, F. Najarro, and R. Schiavon, for their constructive and critical comments on the science and survey cases presented then, and which formed the basis of the cases presented here as well as the subsequent, extensive WEAVE Science Case and Survey Plan, which were reviewed at the WEAVE Survey Readiness Review held at the University of Oxford (2020 January 15–16) by G. Hill, S. Martell, K. Master, and A. McConnachie. We are also very grateful to these reviewers for their constructive and supportive critique. S. C. Trager and G. B. Dalton thank the WEAVE Project Board and ING Board for their strong support for the project and many helpful discussions. S. Jin and S. C. Trager thank Francesco de Gasperin for his careful reading of the draft that helped to improve this paper. The authors would also like to thank the anonymous reviewer for their very careful reading of the manuscript. S. Jin acknowledges financial support from the European Union's Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement no. 665593. S. C. Trager acknowledges funding for WEAVE construction through NWO grant 614.061.612 and ongoing support from NOVA, The Netherlands School for Research in Astronomy. G. B. Dalton acknowledges ongoing support for the WEAVE project from STFC. The WEAVE development work carried out at the Cambridge Astronomical Survey Unit (CASU), at the IoA, Cambridge, has been in part funded through UKRI STFC grant ST/X001857/1 and previously ST/M003175/1, ST/N005805/1, ST/P003486/1, ST/M007626/1, and ST/T003081/1. J. A. L. Aguerri, C. Zurita, J. Méndez-Abreu, and A. Molaeinezhad acknowledge support from the Spanish Ministries of Economía y Competitividad (MINECO) and Ciencia e Innovación (MICIN) through the grants AYA2017-83204-P, AYA2013-43188-P, and PID2020-119342GB-I00. E. J. Alfaro acknowledges financial support from the State Agency for Research of the Spanish MCIU through the 'Center of Excellence Severo Ochoa' award to the Instituto de Astrofísica de Andalucía (CEX2021-001131-S) and from the PY20-00753 grant from Junta de Andalucía, Spain (Autonomic Government of Andalusia, Spain). T. Antoja acknowledges the grant RYC2018-025968-I funded by MCIN/AEI/10.13039/501100011033 and by 'ESF Investing in your future'. This work was partially supported by the Spanish MICIN/AEI/10.13039/501100011033 and by 'ERDF A way of making Europe' by the European Union through grants PID2021-122842OB-C21 and PID2021-125451NA-I00, and the Institute of Cosmos Sciences University of Barcelona (ICCUB, Unidad de Excelencia 'María de Maeztu') through grant CEX2019-000918-M. G. Battaglia acknowledges support from the Agencia Estatal de Investigación del Ministerio de Ciencia en Innovación (AEI-MICIN) and the ERDF under grant number AYA2017-89076-P, the AEI under grant number CEX2019-000920-S and the AEI-MICIN under grant number PID2020-118778GB-I00/10.13039/501100011033. T. Bensby acknowledges financial support by grant no. 2018-04857 from the Swedish Research Council. S. R. Berlanas acknowledges funding by the Spanish Ministerio de Ciencia e Innovación and Agencia Estatal de Investigación (MCIN/AEI/10.13039/501100011033/FEDER, UE) under the Juan de la Cierva – Formación grant (contract FJC 2020-045785-I) and NextGeneration EU/PRTR and MIU (UNI/551/2021) through grant Margarita Salas-Universidad de la Laguna. This research has also received financial support by the MCIN and AEI through grant PID2021-122397NB-C22 and with funding from the European Union NextGenerationEU and Generalitat Valenciana in
(v) WEAVE Galaxy Clusters is a survey of stellar populations, ionized gas properties, and stellar and ionized gas kinematics in cluster galaxies and their outskirts out to $z \sim 0.5$ using all of WEAVE's fibre modes (MOS, mIFU, and LIFU), split into the Nearby, Wide-Field, and Cosmological Clusters sub-surveys.

(vi) StePS is a survey of detailed stellar populations and stellar kinematics in ~25 000 individual field galaxies, the majority within $0.3 \le z \le 0.7$.

(vii) WL will obtain around one million spectra of sources selected on the basis of their activity from the LoTSS. The survey will have a wedding-cake structure with three tiers ranging from WL-Wide (~9000 deg² of the Northern Sky) to WL-Deep (up to 60 deg² in the LoTSS Deep Fields), together efficiently sampling the luminosity and redshift plane, and observing statistical samples of galaxies and AGNs selected in a manner that is unbiased by dust.

(viii) WQ is a survey of the IGM at $z > 2.1$ and a very sensitive probe of baryonic acoustic oscillations at $z > 2.4$ using absorption lines along the line of sight to ~400 000 quasars.

We have developed new, two-phase, dedicated data-processing pipelines for WEAVE, producing both reduced (via the CPS) and science-ready (via the APS) data, with a modular architecture allowing for additional analysis software to be developed as necessary by the science teams to be incorporated into the APS. Outputs from these pipelines populate a dedicated data archive (WAS), which will also store CDPs. WEAVE also requires a new control system at the Observatory (OCS), enabling queue-based observations, in which user-submitted XML files describing the desired telescope and spectrograph settings with MOS or m/LIFU field configurations are converted into OBs and stored in an OB management system that is sampled by the queue SCHEDULER for use by the telescope operator and/or the support astronomer. The entire data system has been exercised in a series of Operational Rehearsals, starting with the end-to-end WEAVE instrument Simulator, which 'observes' synthetic data that are then passed through the OCS to the CPS and the APS, and finally into the WAS. Many lessons about the data flow, survey design, and observation scheduling have been learnt by simulating periods between three weeks (full simulated images) and 1.5 years (nightly scheduling) of the WEAVE Survey. As an example, we suggest that PI observations using poor seeing (>2 arcsec) conditions in bright time would favourably complement the WEAVE Survey programme.

The WEAVE Survey will begin observations towards the end of 2023. All processed WEAVE data and CDPs will be released to the worldwide astronomy community through the WAS annually, beginning 2 years after the start of the WEAVE Survey (i.e. late 2025), and astronomers in the WEAVE Survey Consortium will have access to the data soon after the data have been taken and reduced. A Science Verification (SV) campaign immediately preceding the WEAVE Survey will test various aspects of the surveys and carry out more than a dozen programmes submitted by the ING community (astronomers in the UK, The Netherlands, and Spain, plus their collaborators); all SV data are expected to be reduced and released to the ING and WEAVE community within 6 months of the end of the SV campaign.

WEAVE represents a significant next step forward in our understanding of the Universe around us. The planned surveys will provide data that will help answer the questions: How did our Galaxy form and the stars within it evolve? How were other galaxies assembled? What are dark matter and dark energy?

## ACKNOWLEDGEMENTS

We would like to thank the reviewers of the WEAVE Survey Strategy Review held at Observatoire de Paris (2015 October 19–20), M. Bershady, G. Hill, F. Najarro, and R. Schiavon, for their constructive and critical comments on the science and survey cases presented then, and which formed the basis of the cases presented here as well as the subsequent, extensive WEAVE Science Case and Survey Plan, which were reviewed at the WEAVE Survey Readiness Review held at the University of Oxford (2020 January 15–16) by G. Hill, S. Martell, K. Master, and A. McConnachie. We are also very grateful to these reviewers for their constructive and supportive critique. S. C. Trager and G. B. Dalton thank the WEAVE Project Board and ING Board for their strong support for the project and many helpful discussions. S. Jin and S. C. Trager thank Francesco de Gasperin for his careful reading of the draft that helped to improve this paper. The authors would also like to thank the anonymous reviewer for their very careful reading of the manuscript. S. Jin acknowledges financial support from the European Union's Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement no. 665593. S. C. Trager acknowledges funding for WEAVE construction through NWO grant 614.061.612 and ongoing support from NOVA, The Netherlands School for Research in Astronomy. G. B. Dalton acknowledges ongoing support for the WEAVE project from STFC. The WEAVE development work carried out at the Cambridge Astronomical Survey Unit (CASU), at the IoA, Cambridge, has been in part funded through UKRI STFC grant ST/X001857/1 and previously ST/M003175/1, ST/N005805/1, ST/P003486/1, ST/M007626/1, and ST/T003081/1. J. A. L. Aguerri, C. Zurita, J. Méndez-Abreu, and A. Molaeinezhad acknowledge support from the Spanish Ministries of Economía y Competitividad (MINECO) and Ciencia e Innovación (MICIN) through the grants AYA2017-83204-P, AYA2013-43188-P, and PID2020-119342GB-I00. E. J. Alfaro acknowledges financial support from the State Agency for Research of the Spanish MCIU through the 'Center of Excellence Severo Ochoa' award to the Instituto de Astrofísica de Andalucía (CEX2021-001131-S) and from the PY20-00753 grant from Junta de Andalucía, Spain (Autonomic Government of Andalusia, Spain). T. Antoja acknowledges the grant RYC2018-025968-I funded by MCIN/AEI/10.13039/501100011033 and by 'ESF Investing in your future'. This work was partially supported by the Spanish MICIN/AEI/10.13039/501100011033 and by 'ERDF A way of making Europe' by the European Union through grants PID2021-122842OB-C21 and PID2021-125451NA-I00, and the Institute of Cosmos Sciences University of Barcelona (ICCUB, Unidad de Excelencia 'María de Maeztu') through grant CEX2019-000918-M. G. Battaglia acknowledges support from the Agencia Estatal de Investigación del Ministerio de Ciencia en Innovación (AEI-MICIN) and the ERDF under grant number AYA2017-89076-P, the AEI under grant number CEX2019-000920-S and the AEI-MICIN under grant number PID2020-118778GB-I00/10.13039/501100011033. T. Bensby acknowledges financial support by grant no. 2018-04857 from the Swedish Research Council. S. R. Berlanas acknowledges funding by the Spanish Ministerio de Ciencia e Innovación and Agencia Estatal de Investigación (MCIN/AEI/10.13039/501100011033/FEDER, UE) under the Juan de la Cierva - Formación grant (contract FJC 2020-045785-I) and NextGeneration EU/PRTR and MIU (UNI/551/2021) through grant Margarita Salas-Universidad de la Laguna. This research has also received financial support by the MCIN and AEI through grant PID2021-122397NB-C22 and with funding from the European Union NextGenerationEU and Generalitat Valenciana in
the call Programa de Planes Complementarios de I+D+i (PRTR 2022, Project HIAMAS, reference ASFAE/2022/017). P. N. Best acknowledges support from STFC under grant ST/V000594/1. S. Bonoli acknowledges financial support from the State Research Agency (AEI-MCINN) of the Spanish Ministry of Science and Innovation under the grants PGC2018-097585-B-C22 and PID2021-124243NB-C21 and the Project of excellence Prometeo/2020/085 from the Conselleria d'Innovació, Universitats, Ciència i Societat Digital de la Generalitat Valenciana. N. Britavskiy acknowledges support by the University of Liege under Special Funds for Research, IPD-STEMA Programme. L. Costantin acknowledges financial support from Comunidad de Madrid under Atracción de Talento grant 2018-T2/TIC-11612 and Spanish Ministerio de Ciencia e Innovación MCIN/AEI/10.13039/501100011033 through grant PGC2018-093499-B-I00. J. Falcón-Barroso and A. Ferré-Mateu acknowledge support from the Spanish Ministries of Economía y Competitividad (MINECO) and Ciencia e Innovación (MICINN) through the grants AYA2016-77237-C3-1-P and PID2019-107427GB-C32. AFM also acknowledges support from RYC2021-031099-I and PID2021-123313NA-I00 of MICIN/AEI/10.13039/501100011033/FEDER, UE, Next Generation EU, PRTR. M. Fumagalli acknowledges support from the ERC under the European Union's Horizon 2020 research and innovation programme (grant agreement no. 757535) and from Fondazione Cariplo, grant no. 2018-2329. B. T. Gänsicke was supported by grant ST/T000406/1 from the STFC. This project has received funding from the ERC under the European Union's Horizon 2020 research and innovation programme (grant agreement no. 101020057). R. García-Benito, A. M. Conrado, and R. González Delgado acknowledge financial support from the grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033 and from PID2019-109067-GB100. C. P. Haines acknowledges support from ANID through Fondecyt Regular 2021 project no. 1211909. N. A. Hatch, S. C. Read, A. Aragon-Salamanca, and U. Kuchner acknowledge support from the UK STFC consolidated grant ST/T000171/1. We acknowledge financial support from a Spinoza prize to A. Helmi. A. Herrero, A. de Burgos, and S. Simón-Díaz acknowledge support from the Spanish Ministry of Science and Innovation (MICINN) through the Spanish State Research Agency through grants PGC-2018-0913741-B-C22, PID2021-122397NB-C21, and the Severo Ochoa Programe 2020-2023 (CEX2019-000920-S). This work has also received financial support from the Canarian Agency for Economy, Knowledge, and Employment and the ERDF/EU, under grant with reference ProID2020010016. K. M. Hess acknowledges financial support from the grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033, from the coordination of the participation in SKA-SPAIN, funded by the Ministry of Science and Innovation (MCIN); and support from the ERC under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement no. 291531 (HISTORYNU). V. Iršič was supported by the Kavli Foundation. J. H. Knapen acknowledges financial support from the State Research Agency (AEI-MCINN) of the Spanish Ministry of Science and Innovation under the grant 'The structure and evolution of galaxies and their central regions' with reference PID2019-105602GB-I00/10.13039/501100011033, and from the ACIISI, Consejería de Economía, Conocimiento y Empleo del Gobierno de Canarias and the ERDF under grant with reference PROID2021010044. S. Lucatello, A. Bragaglia, and M. Bellazzini acknowledge the support from PRIN INAF 2019 grant ObFu 1.05.01.85.14 ('Building up the halo: chemo-dynamical tagging in the age of large surveys', PI. S. Lucatello). J. Maíz Apellániz acknowledges support from the Spanish Government Ministerio

de Ciencia e Innovación and Agencia Estatal de Investigación (10.13039/501100011033) through grant PGC2018-095049-B-C22. J. Mendez Abreu acknowledges support from the Spanish Ministries of Economía y Competitividad (MINECO) and Ciencia e Innovación (MICINN) through the grant PID2021-128131NB-I00, and the support of the Viera y Clavijo Senior programme funded by ACIISI and ULL. I. Negueruela and A. Marco acknowledge the financial support of the Spanish Ministerio de Ciencia e Innovación (MCIN) with funding from the European Union NextGenerationEU and Generalitat Valenciana in the call Programa de Planes Complementarios de I+D+i (PRTR 2022, Project HIAMAS, reference ASFAE/2022/017) and through grant PID2021-122397NB-C22. I. Pérez-Ràfols acknowledges support from the European Union's Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement no. 754510. M. M. Pieri, I. Pérez-Ràfols, S. Morrison, D. Som, and M. Blomqvist were supported by the Programme National Cosmology et Galaxies (PNCG) of CNRS/INSU with INP and IN2P3, co-funded by CEA and CNES, by A*MIDEX project (ANR-11-IDEX-0001-02) funded by the 'Investissements d'Avenir' French Government program, managed by the French National Research Agency (ANR), and by ANR under contract ANR-14-ACHN-0021 and ANR-22-CE31-0026. R. Raddi has received funding from the postdoctoral fellowship programme Beatriu de Pinós, funded by the Secretary of Universities and Research (Government of Catalonia) and by the Horizon 2020 programme of research and innovation of the European Union under the Maria Skłodowska-Curie grant agreement no. 801370. E. M. Rossi acknowledges that this project has received funding from the ERC under the European Union's Horizon 2020 research and innovation programme (grant agreement no. 101002511-VEGA P). J. A. Rubino-Martin acknowledges financial support from the Spanish Ministry of Science and Innovation under the project PID2020-120514GB-I00. D. J. B. Smith, A. B. Drake, and M. J. Hardcastle acknowledge support from the UK STFC under grant ST/V000624/1. R. J. Smith acknowledges support from the UK STFC consolidated grant ST/T000244/1. D. Sorini was supported by the ERC, under grant no. 670193, by the STFC consolidated grant no. RA5496, and by the Swiss National Science Foundation (SNSF) Professorship grant no. 202671. E. Starkenburg acknowledges funding through VIDI grant 'Pushing Galactic Archaeology to its limits' (with project number VI.Vidi.193.093), which is funded by the Dutch Research Council (NWO). G. F. Thomas acknowledge support from the Agencia Estatal de Investigación (AEI) under grant Ayudas a centros de excelencia Severo Ochoa convocatoria 2019 with reference CEX2019-000920-S, and from the Agencia Estatal de Investigación del Ministerio de Ciencia e Innovación (AEI-MCINN) under grant En la frontera de la arqueología galacáctica: evolución de la materia luminoso y obscura de la vía Láctea y las galaxias enenas del Grupo Local with reference PID2020-118778GB-I00. J. S. Vink acknowledges support from the UK STFC grant ST/V000233/1. All INAF researchers are supported by INAF grant 1.05.03.04.05. Funding for the WEAVE facility has been provided by UKRI STFC, the University of Oxford, NOVA, NWO, Instituto de Astrofísica de Canarias (IAC), the Isaac Newton Group partners (STFC, NWO, and Spain, led by the IAC), INAF, CNRS-INSU, the Observatoire de Paris, Région Île-de-France, CONCYT through INAOE, Konkoly Observatory (CSFK), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Lund University, the Leibniz Institute for Astrophysics Potsdam (AIP), the Swedish Research Council, the European Commission, and the University of Pennsylvania. The WEAVE Survey Consortium consists of the ING, its three partners, represented by UKRI STFC, NWO, and the IAC, NOVA, INAF, GEPI, INAOE, and individual WEAVE Participants. Please see the
the call Programa de Planes Complementarios de I+D+i (PRTR 2022, Project HIAMAS, reference ASFAE/2022/017). P. N. Best acknowledges support from STFC under grant ST/V000594/1. S. Bonoli acknowledges financial support from the State Research Agency (AEI-MCINN) of the Spanish Ministry of Science and Innovation under the grants PGC2018-097585-B-C22 and PID2021-124243NB-C21 and the Project of excellence Prometeo/2020/085 from the Conselleria d'Innovació, Universitats, Ciència i Societat Digital de la Generalitat Valenciana. N. Britavskiy acknowledges support by the University of Liege under Special Funds for Research, IPD-STEMA Programme. L. Costantin acknowledges financial support from Comunidad de Madrid under Atracción de Talento grant 2018-T2/TIC-11612 and Spanish Ministerio de Ciencia e Innovación MCIN/AEI/10.13039/501100011033 through grant PGC2018-093499-B-I00. J. Falcón-Barroso and A. Ferré-Mateu acknowledge support from the Spanish Ministries of Economía y Competitividad (MINECO) and Ciencia e Innovación (MICINN) through the grants AYA2016-77237-C3-1-P and PID2019-107427GB-C32. AFM also acknowledges support from RYC2021-031099-I and PID2021-123313NA-I00 of MICIN/AEI/10.13039/501100011033/FEDER, UE, Next Generation EU, PRTR. M. Fumagalli acknowledges support from the ERC under the European Union's Horizon 2020 research and innovation programme (grant agreement no. 757535) and from Fondazione Cariplo, grant no. 2018-2329. B. T. Gänsicke was supported by grant ST/T000406/1 from the STFC. This project has received funding from the ERC under the European Union's Horizon 2020 research and innovation programme (grant agreement no. 101020057). R. García-Benito, A. M. Conrado, and R. González Delgado acknowledge financial support from the grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033 and from PID2019-109067-GB100. C. P. Haines acknowledges support from ANID through Fondecyt Regular 2021 project no. 1211909. N. A. Hatch, S. C. Read, A. Aragon-Salamanca, and U. Kuchner acknowledge support from the UK STFC consolidated grant ST/T000171/1. We acknowledge financial support from a Spinoza prize to A. Helmi. A. Herrero, A. de Burgos, and S. Simón-Díaz acknowledge support from the Spanish Ministry of Science and Innovation (MICINN) through the Spanish State Research Agency through grants PGC-2018-0913741-B-C22, PID2021-122397NB-C21, and the Severo Ochoa Programe 2020-2023 (CEX2019-000920-S). This work has also received financial support from the Canarian Agency for Economy, Knowledge, and Employment and the ERDF/EU, under grant with reference ProID2020010016. K. M. Hess acknowledges financial support from the grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033, from the coordination of the participation in SKA-SPAIN, funded by the Ministry of Science and Innovation (MCIN); and support from the ERC under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement no. 291531 (HISTORYNU). V. Iršič was supported by the Kavli Foundation. J. H. Knapen acknowledges financial support from the State Research Agency (AEI-MCINN) of the Spanish Ministry of Science and Innovation under the grant 'The structure and evolution of galaxies and their central regions' with reference PID2019-105602GB-I00/10.13039/501100011033, and from the ACIISI, Consejería de Economía, Conocimiento y Empleo del Gobierno de Canarias and the ERDF under grant with reference PROID2021010044. S. Lucatello, A. Bragaglia, and M. Bellazzini acknowledge the support from PRIN INAF 2019 grant ObFu 1.05.01.85.14 ('Building up the halo: chemo-dynamical tagging in the age of large surveys', PI. S. Lucatello). J. Maíz Apellániz acknowledges support from the Spanish Government Ministerio

de Ciencia e Innovación and Agencia Estatal de Investigación (10.13039/501100011033) through grant PGC2018-095049-B-C22. J. Mendez Abreu acknowledges support from the Spanish Ministries of Economía y Competitividad (MINECO) and Ciencia e Innovación (MICINN) through the grant PID2021-128131NB-I00, and the support of the Viera y Clavijo Senior programme funded by ACIISI and ULL. I. Negueruela and A. Marco acknowledge the financial support of the Spanish Ministerio de Ciencia e Innovación (MCIN) with funding from the European Union NextGenerationEU and Generalitat Valenciana in the call Programa de Planes Complementarios de I+D+i (PRTR 2022, Project HIAMAS, reference ASFAE/2022/017) and through grant PID2021-122397NB-C22. I. Pérez-Ràfols acknowledges support from the European Union's Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement no. 754510. M. M. Pieri, I. Pérez-Ràfols, S. Morrison, D. Som, and M. Blomqvist were supported by the Programme National Cosmology et Galaxies (PNCG) of CNRS/INSU with INP and IN2P3, co-funded by CEA and CNES, by A*MIDEX project (ANR-11-IDEX-0001-02) funded by the 'Investissements d'Avenir' French Government program, managed by the French National Research Agency (ANR), and by ANR under contract ANR-14-ACHN-0021 and ANR-22-CE31-0026. R. Raddi has received funding from the postdoctoral fellowship programme Beatriu de Pinós, funded by the Secretary of Universities and Research (Government of Catalonia) and by the Horizon 2020 programme of research and innovation of the European Union under the Maria Skłodowska-Curie grant agreement no. 801370. E. M. Rossi acknowledges that this project has received funding from the ERC under the European Union's Horizon 2020 research and innovation programme (grant agreement no. 101002511-VEGA P). J. A. Rubino-Martin acknowledges financial support from the Spanish Ministry of Science and Innovation under the project PID2020-120514GB-I00. D. J. B. Smith, A. B. Drake, and M. J. Hardcastle acknowledge support from the UK STFC under grant ST/V000624/1. R. J. Smith acknowledges support from the UK STFC consolidated grant ST/T000244/1. D. Sorini was supported by the ERC, under grant no. 670193, by the STFC consolidated grant no. RA5496, and by the Swiss National Science Foundation (SNSF) Professorship grant no. 202671. E. Starkenburg acknowledges funding through VIDI grant 'Pushing Galactic Archaeology to its limits' (with project number VI.Vidi.193.093), which is funded by the Dutch Research Council (NWO). G. F. Thomas acknowledge support from the Agencia Estatal de Investigación (AEI) under grant Ayudas a centros de excelencia Severo Ochoa convocatoria 2019 with reference CEX2019-000920-S, and from the Agencia Estatal de Investigación del Ministerio de Ciencia e Innovación (AEI-MCINN) under grant En la frontera de la arqueología galacáctica: evolución de la materia luminoso y obscura de la vía Láctea y las galaxias enenas del Grupo Local with reference PID2020-118778GB-I00. J. S. Vink acknowledges support from the UK STFC grant ST/V000233/1. All INAF researchers are supported by INAF grant 1.05.03.04.05. Funding for the WEAVE facility has been provided by UKRI STFC, the University of Oxford, NOVA, NWO, Instituto de Astrofísica de Canarias (IAC), the Isaac Newton Group partners (STFC, NWO, and Spain, led by the IAC), INAF, CNRS-INSU, the Observatoire de Paris, Région Île-de-France, CONCYT through INAOE, Konkoly Observatory (CSFK), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Lund University, the Leibniz Institute for Astrophysics Potsdam (AIP), the Swedish Research Council, the European Commission, and the University of Pennsylvania. The WEAVE Survey Consortium consists of the ING, its three partners, represented by UKRI STFC, NWO, and the IAC, NOVA, INAF, GEPI, INAOE, and individual WEAVE Participants. Please see the
relevant footnotes for the WEAVE website<fnref n="32" /> and for the full list of granting agencies and grants supporting WEAVE.<fnref n="33" /> Abbreviations for ministries, funding agencies, and bodies are as follows – AEI: Agencia Estatal de Investigación (Spanish State Research Agency); ANR: Agencia Nationale de la Recherche (French National Research Agency); CNRS: Centre national de la recherche scientifique (French National Centre for Scientific Research); CSIC: Consejo Superior de Investigaciones Científicas (Spanish National Research Council); DFG: Deutsche Forschungsgemeinschaft (German Research Foundation); ERC: European Research Council; ERDF: European Regional Development Fund; INAF: Istituto Nazionale di Astrofisica (Italian National Institute for Astrophysics; INSU: Institut National des Sciences de l'Univers (National Institute of Sciences of the Universe, France); MICINN: Ministerio de Ciencia e Innovación (Spanish Ministry of Science and Innovation); MINECO: Ministerio de Economía y Competitividad (Spanish Ministry of Economy and Competitiveness, Spain); NOVA: Nederlandse Onderzoeksschool Voor Astronomie (Dutch Research School for Astronomy); NWO: Nederlandse Organisatie voor Wetenschappelijk Onderzoek (Dutch Research Council); STFC: Science and Technologies Research Council (UK); UKRI: UK Research and Innovation (UK). The Digitized Sky Survey (DSS) was produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. This research has made use of 'Aladin sky atlas' (Bonnarel et al. 2000) developed at CDS, Strasbourg Observatory, France. For the purpose of Open Access, the authors have applied a Creative Commons Attribution (CC BY) public copyright licence to any Author Accepted Manuscript version arising from this submission. This paper is dedicated to the memories of Jim Lewis and Dave Carter, both of whom made significant contributions to the WEAVE Project, and who passed away in 2019 and 2021, respectively, and to Jordi Torra, whose support on the WEAVE Project Board was invaluable, and who passed away in 2021.

## DATA AVAILABILITY

The simulated WEAVE Survey data can be made available to interested parties through contact with the first three authors of this paper.

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<footnote n="32">³²https://ingconfluence.ing.iac.es/confluence/display/WEAV/The+WEAVE+Project</footnote>

<footnote n="33">³³https://ingconfluence.ing.iac.es/confluence/display/WEAV/WEAVE+Acknowledgements</footnote>
relevant footnotes for the WEAVE website<fnref n="32" /> and for the full list of granting agencies and grants supporting WEAVE.<fnref n="33" /> Abbreviations for ministries, funding agencies, and bodies are as follows – AEI: Agencia Estatal de Investigación (Spanish State Research Agency); ANR: Agencia Nationale de la Recherche (French National Research Agency); CNRS: Centre national de la recherche scientifique (French National Centre for Scientific Research); CSIC: Consejo Superior de Investigaciones Científicas (Spanish National Research Council); DFG: Deutsche Forschungsgemeinschaft (German Research Foundation); ERC: European Research Council; ERDF: European Regional Development Fund; INAF: Istituto Nazionale di Astrofisica (Italian National Institute for Astrophysics; INSU: Institut National des Sciences de l'Univers (National Institute of Sciences of the Universe, France); MICINN: Ministerio de Ciencia e Innovación (Spanish Ministry of Science and Innovation); MINECO: Ministerio de Economía y Competitividad (Spanish Ministry of Economy and Competitiveness, Spain); NOVA: Nederlandse Onderzoeksschool Voor Astronomie (Dutch Research School for Astronomy); NWO: Nederlandse Organisatie voor Wetenschappelijk Onderzoek (Dutch Research Council); STFC: Science and Technologies Research Council (UK); UKRI: UK Research and Innovation (UK). The Digitized Sky Survey (DSS) was produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. This research has made use of 'Aladin sky atlas' (Bonnarel et al. 2000) developed at CDS, Strasbourg Observatory, France. For the purpose of Open Access, the authors have applied a Creative Commons Attribution (CC BY) public copyright licence to any Author Accepted Manuscript version arising from this submission. This paper is dedicated to the memories of Jim Lewis and Dave Carter, both of whom made significant contributions to the WEAVE Project, and who passed away in 2019 and 2021, respectively, and to Jordi Torra, whose support on the WEAVE Project Board was invaluable, and who passed away in 2021.

## DATA AVAILABILITY

The simulated WEAVE Survey data can be made available to interested parties through contact with the first three authors of this paper.

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## APPENDIX A: ABBREVIATIONS

A list of abbreviations used in this paper is given in Table A1.
Silk J., Mamon G. A., 2012, Res. Astron. Astrophys., 12, 917

Simón-Díaz S., 2010, A&A, 510, A22

Sinha M., Holley-Bockelmann K., 2012, ApJ, 751, 17

Skillen I., Balcells M., Trager S. C., 2016, in Skillen I., Balcells M., Trager S. C., eds, ASP Conf. Ser. Vol. 507, Multi-Object Spectroscopy in the Next Decade: Big Questions, Large Surveys, and Wide Fields. Astron. Soc. Pac., San Francisco, p. 477

Smith G. P., Treu T., Ellis R. S., Moran S. M., Dressler A., 2005, ApJ, 620, 78

Smith D. J. B. et al., 2016, in Reylé C., Richard J., Cambrésy L., Deleuil M., Pécontal E., Tresse L., Vauglin I., eds, SF2A-2016: Proc. Annual Meeting of the French Society of Astronomy and Astrophysics. p. 271

Smith M. W. L. et al., 2017, ApJS, 233, 26

Smith D. J. B. et al., 2021, A&A, 648, A6

Sorini D., Oñorbe J., Hennawi J. F., Lukić Z., 2018, ApJ, 859, 125

Sorini D., Davé R., Anglés-Alcázar D., 2020, MNRAS, 499, 2760

Soubiran C., Le Campion J.-F., Brouillet N., Chemin L., 2016, A&A, 591, A118

Soubiran C., Brouillet N., Casamiquela L., 2022, A&A, 663, A4

Spina L. et al., 2022, A&A, 668, A16

Starkenburg E. et al., 2017, MNRAS, 471, 2587

Steinmetz M. et al., 2006, AJ, 132, 1645

Straatman C. M. S. et al., 2018, ApJS, 239, 27

Tadhunter C. N., Morganti R., Robinson A., Dickson R., Villar-Martin M., Fosbury R. A. E., 1998, MNRAS, 298, 1035

Takada M. et al., 2014, PASJ, 66, R1

Tal T. et al., 2014, ApJ, 789, 164

Tamura N. et al., 2018, in Evans C. J., Simard L., Takami H., eds, Proc. SPIE Conf. Ser. Vol. 10702, Ground-Based and Airborne Instrumentation for Astronomy VII. SPIE, Bellingham, p. 107021C

Tasse C., 2014, preprint (arXiv:1410.8706)

Tasse C. et al., 2018, A&A, 611, A87

Tasse C. et al., 2021, A&A, 648, A1

Tempel E., Stoica R. S., Martínez V. J., Liivamägi L. J., Castellan G., Saar E., 2014, MNRAS, 438, 3465

Terrett D. L., Lewis I. J., Dalton G., Abrams D. C., Aguerri J. A. L., Bonifacio P., Middleton K., Trager S. C., 2014, in Chiozzi G., Radziwill N. M., eds, Proc. SPIE Conf. Ser. Vol. 9152, Software and Cyberinfrastructure for Astronomy III. SPIE, Bellingham, p. 91520P

The MSE Science Team, 2019, preprint (arXiv:1904.04907)

Thomas D., Maraston C., Bender R., Mendes de Oliveira C., 2005, ApJ, 621, 673

Tiwari P., Zhao R., Zheng J., Zhao G.-B., Bacon D., Schwarz D. J., 2022, ApJ, 928, 38

Toloba E. et al., 2009, ApJ, 707, L17

Toloba E. et al., 2014, ApJ, 783, 120

Toloba E. et al., 2015, ApJ, 799, 172

Tonry J. L. et al., 2012, ApJ, 750, 99

Toonen S., Hollands M., Gänsicke B. T., Boekholt T., 2017, A&A, 602, A16

Tremblay P.-E., Kalirai J. S., Soderblom D. R., Cignoni M., Cummings J., 2014, ApJ, 791, 92

Tremblay P.-E. et al., 2017, MNRAS, 465, 2849

Tremblay P.-E., Cukanovaite E., Gentile Fusillo N. P., Cunningham T., Hollands M. A., 2019, MNRAS, 482, 5222

Valentini M. et al., 2019, A&A, 627, A173

Vasiliev E., Belokurov V., Erkal D., 2021, MNRAS, 501, 2279

van Cappellen W. A. et al., 2022, A&A, 658, A146

van der Wel A. et al., 2016, ApJS, 223, 29

van Gorkom J., 2013, in Falcón-Barroso J., Knapen J. H., eds, Secular Evolution of Galaxies. XXIII Canary Islands Winter School of Astrophysics. Cambridge Univ. Press, Cambridge, p. 459

van Haarlem M. P. et al., 2013, A&A, 556, A2

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## APPENDIX A: ABBREVIATIONS

A list of abbreviations used in this paper is given in Table A1.
<table><caption>Table A1. Common WEAVE abbreviations.</caption><thead><tr><th></th><th>Commonly used abbreviations in WEAVE</th><th>Section of paper in which defined</th></tr></thead><tbody><tr><td>CDP</td><td>Contributed Data Product</td><td>2.6</td></tr><tr><td>CPS, APS</td><td>Core Processing System, Advanced Processing System</td><td>2.6</td></tr><tr><td>LR, HR</td><td>Low Resolution, High Resolution</td><td>2.3</td></tr><tr><td>mIFU, LIFU</td><td>mini Integral Field Unit, Large Integral Field Unit</td><td>1</td></tr><tr><td>MOS</td><td>Multi-Object Spectroscopy</td><td>2.2</td></tr><tr><td>OB</td><td>Observing Block</td><td>2.5</td></tr><tr><td>OCS</td><td>Observatory Control System</td><td>2.5</td></tr><tr><td>OISMT</td><td>On-Island Survey Management Team</td><td>3.2</td></tr><tr><td>OpR</td><td>Operational Rehearsal</td><td>6</td></tr><tr><td>QAG</td><td>Quality Assessment Group</td><td>3.3</td></tr><tr><td>SPA</td><td>Science Processing and Analysis</td><td>2.6</td></tr><tr><td>STL</td><td>Science Team Lead</td><td>3</td></tr><tr><td>SWG</td><td>Survey Working Group</td><td>3.1</td></tr><tr><td>WAS</td><td>WEAVE Archive System</td><td>2.6</td></tr><tr><td>WASP</td><td>WEAVE Automated Submission Platform</td><td>6</td></tr><tr><td>WEAVE</td><td>WHT Enhanced Area Velocity Explorer</td><td>1</td></tr><tr><td>WHT</td><td>William Herschel Telescope</td><td>1</td></tr></tbody></table>

<footnote n="1">¹Oxford Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK</footnote>

<footnote n="2">²Kapteyn Astronomical Institute, Rijksuniversiteit Groningen, Landleven 12, 9747 AD Groningen, The Netherlands</footnote>

<footnote n="3">³RALSpace, STFC, Harwell, Didcot OX11 0QX, UK</footnote>

<footnote n="4">⁴SRON - Netherlands Institute for Space Research, Landleven 12, 9747 AD Groningen, The Netherlands</footnote>

<footnote n="5">⁵Instituto de Astrofísica de Canarias, Calle Vía Láctea s/n, 38205 La Laguna, Santa Cruz de Tenerife, Spain</footnote>

<footnote n="6">⁶Departamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain</footnote>

<footnote n="7">⁷Centre for Astrophysics Research, University of Hertfordshire, Hatfield, Hertfordshire AL10 9AB, UK</footnote>

<footnote n="8">⁸Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK</footnote>

<footnote n="9">⁹Department of Physics, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL, UK</footnote>

<footnote n="10">¹⁰Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Bd de l'Observatoire, CS 34229, 06304 Nice Cedex 4, France</footnote>

<footnote n="11">¹¹INAF - Osservatorio Astronomico di Brera, Via Brera, 28, 20121 Milano, Italy</footnote>

<footnote n="12">¹²Aix Marseille Univ, CNRS, CNES, LAM, Laboratoire d'Astrophysique de Marseille, 13388 Marseille, France</footnote>

<footnote n="13">¹³INAF - Osservatorio Astronomico di Padova, Vicolo Osservatorio 5, 35122 Padova, Italy</footnote>

<footnote n="14">¹⁴Isaac Newton Group of Telescopes, Apartado 321, 38700 Santa Cruz de la Palma, Tenerife, Spain</footnote>

<footnote n="15">¹⁵Dipartimento di Fisica e Astrofisica, Università degli Studi di Firenze, via G. Sansone 1, 50019 Sesto Fiorentino, Italy</footnote>

<footnote n="16">¹⁶INAF - Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 5, 20125 Firenze, Italy</footnote>

<footnote n="17">¹⁷Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK</footnote>

<footnote n="18">¹⁸Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (UB), Martí Franquès 1, 08028 Barcelona, Spain</footnote>

<footnote n="19">¹⁹Departament de Física Quàntica i Astrofísica (FQA), Universitat de Barcelona (UB), Martí i Franquès 1, 08028 Barcelona, Spain</footnote>

<footnote n="20">²⁰Institut d'Estudis Espacials de Catalunya (IEEC), Gran Capità, 2-4, 08034 Barcelona, Spain</footnote>

<footnote n="21">²¹School of Physics and Astronomy, University of Nottingham, University Park, Nottingham NG7 2RD, UK</footnote>

<footnote n="22">²²Departamento de Física Teórica, Universidad Autónoma de Madrid, 28049 Madrid, Spain</footnote>

<footnote n="23">²³Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France</footnote>

<footnote n="24">²⁴GEPI, Observatoire de Paris, Université PSL, CNRS: 5, place Jules Janssen, 92195 Meudon, France</footnote>

<footnote n="25">²⁵Lund Observatory, Department of Astronomy and Theoretical Physics, Box 43, SE-221 00 Lund, Sweden</footnote>

<footnote n="26">²⁶INAF - Osservatorio di Astrofisica e Scienza dello Spazio, via P. Gobetti 93/3, 40129 Bologna, Italy</footnote>

<footnote n="27">²⁷Instituto Nacional de Astrofísica, Óptica y Electrónica, Luis Enrique Erro 1, Tonantzintla, Puebla C.P. 72840, Mexico</footnote>

<footnote n="28">²⁸Institute for Astronomy, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK</footnote>

<footnote n="29">²⁹Université de Strasbourg, CNRS, Observatoire astronomique de Strasbourg, UMR 7550, 67000 Strasbourg, France</footnote>

<footnote n="30">³⁰UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK</footnote>

<footnote n="31">³¹Instituto de Astrofísica de Andalucía, CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain</footnote>

<footnote n="32">³²ASTRON, Netherlands Institute for Radio Astronomy, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands</footnote>

<footnote n="33">³³Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Merseyside L3 5RF, UK</footnote>

<footnote n="34">³⁴Department of Physics, McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15213, USA</footnote>

<footnote n="35">³⁵Institut d'Astrophysique de Paris, 98bis Bd Arago, 75014 Paris, France</footnote>

<footnote n="36">³⁶Technical University of Munich Institute for Advanced Studies, Lichtenbergstr. 2a, 85748 Garching, Germany</footnote>

<footnote n="37">³⁷INAF - Osservatorio Astronomico di Capodimonte, Salita Moiariello, 16, 80131 Napoli, Italy</footnote>

<footnote n="38">³⁸Department of Astronomy, University of Illinois at Urbana-Champaign, Urbana, IL 61801, USA</footnote>

<footnote n="39">³⁹Instituto de Astronomía y Ciencias Planetarias, Universidad de Atacama, Copayahu 485, Copiapó, Chile</footnote>

<footnote n="40">⁴⁰Instituto Universitario Carlos I de Física Teórica y Computacional, Universidad de Granada, 18071 Granada, Spain</footnote>

<footnote n="41">⁴¹Instituto de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, 08193 Bellaterra, Barcelona, Spain</footnote>

<footnote n="42">⁴²Departament de Física, Universitat Politècnica de Catalunya, c/Esteve Terrades 5, 08860 Castelldefels, Spain</footnote>

<footnote n="43">⁴³Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking RH5 6NT, UK</footnote>

<footnote n="44">⁴⁴Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA</footnote>

<footnote n="45">⁴⁵INAF - Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy</footnote>

<footnote n="46">⁴⁶Department of Physics, Lancaster University, Bailrigg, Lancaster LA1 4YB, UK</footnote>
<table><caption>Table A1. Common WEAVE abbreviations.</caption><thead><tr><th></th><th>Commonly used abbreviations in WEAVE</th><th>Section of paper in which defined</th></tr></thead><tbody><tr><td>CDP</td><td>Contributed Data Product</td><td>2.6</td></tr><tr><td>CPS, APS</td><td>Core Processing System, Advanced Processing System</td><td>2.6</td></tr><tr><td>LR, HR</td><td>Low Resolution, High Resolution</td><td>2.3</td></tr><tr><td>mIFU, LIFU</td><td>mini Integral Field Unit, Large Integral Field Unit</td><td>1</td></tr><tr><td>MOS</td><td>Multi-Object Spectroscopy</td><td>2.2</td></tr><tr><td>OB</td><td>Observing Block</td><td>2.5</td></tr><tr><td>OCS</td><td>Observatory Control System</td><td>2.5</td></tr><tr><td>OISMT</td><td>On-Island Survey Management Team</td><td>3.2</td></tr><tr><td>OpR</td><td>Operational Rehearsal</td><td>6</td></tr><tr><td>QAG</td><td>Quality Assessment Group</td><td>3.3</td></tr><tr><td>SPA</td><td>Science Processing and Analysis</td><td>2.6</td></tr><tr><td>STL</td><td>Science Team Lead</td><td>3</td></tr><tr><td>SWG</td><td>Survey Working Group</td><td>3.1</td></tr><tr><td>WAS</td><td>WEAVE Archive System</td><td>2.6</td></tr><tr><td>WASP</td><td>WEAVE Automated Submission Platform</td><td>6</td></tr><tr><td>WEAVE</td><td>WHT Enhanced Area Velocity Explorer</td><td>1</td></tr><tr><td>WHT</td><td>William Herschel Telescope</td><td>1</td></tr></tbody></table>

<footnote n="1">¹Oxford Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK</footnote>

<footnote n="2">²Kapteyn Astronomical Institute, Rijksuniversiteit Groningen, Landleven 12, 9747 AD Groningen, The Netherlands</footnote>

<footnote n="3">³RALSpace, STFC, Harwell, Didcot OX11 0QX, UK</footnote>

<footnote n="4">⁴SRON - Netherlands Institute for Space Research, Landleven 12, 9747 AD Groningen, The Netherlands</footnote>

<footnote n="5">⁵Instituto de Astrofísica de Canarias, Calle Vía Láctea s/n, 38205 La Laguna, Santa Cruz de Tenerife, Spain</footnote>

<footnote n="6">⁶Departamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain</footnote>

<footnote n="7">⁷Centre for Astrophysics Research, University of Hertfordshire, Hatfield, Hertfordshire AL10 9AB, UK</footnote>

<footnote n="8">⁸Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK</footnote>

<footnote n="9">⁹Department of Physics, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL, UK</footnote>

<footnote n="10">¹⁰Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Bd de l'Observatoire, CS 34229, 06304 Nice Cedex 4, France</footnote>

<footnote n="11">¹¹INAF - Osservatorio Astronomico di Brera, Via Brera, 28, 20121 Milano, Italy</footnote>

<footnote n="12">¹²Aix Marseille Univ, CNRS, CNES, LAM, Laboratoire d'Astrophysique de Marseille, 13388 Marseille, France</footnote>

<footnote n="13">¹³INAF - Osservatorio Astronomico di Padova, Vicolo Osservatorio 5, 35122 Padova, Italy</footnote>

<footnote n="14">¹⁴Isaac Newton Group of Telescopes, Apartado 321, 38700 Santa Cruz de la Palma, Tenerife, Spain</footnote>

<footnote n="15">¹⁵Dipartimento di Fisica e Astrofisica, Università degli Studi di Firenze, via G. Sansone 1, 50019 Sesto Fiorentino, Italy</footnote>

<footnote n="16">¹⁶INAF - Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 5, 20125 Firenze, Italy</footnote>

<footnote n="17">¹⁷Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK</footnote>

<footnote n="18">¹⁸Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (UB), Martí Franquès 1, 08028 Barcelona, Spain</footnote>

<footnote n="19">¹⁹Departament de Física Quàntica i Astrofísica (FQA), Universitat de Barcelona (UB), Martí i Franquès 1, 08028 Barcelona, Spain</footnote>

<footnote n="20">²⁰Institut d'Estudis Espacials de Catalunya (IEEC), Gran Capità, 2-4, 08034 Barcelona, Spain</footnote>

<footnote n="21">²¹School of Physics and Astronomy, University of Nottingham, University Park, Nottingham NG7 2RD, UK</footnote>

<footnote n="22">²²Departamento de Física Teórica, Universidad Autónoma de Madrid, 28049 Madrid, Spain</footnote>

<footnote n="23">²³Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France</footnote>

<footnote n="24">²⁴GEPI, Observatoire de Paris, Université PSL, CNRS: 5, place Jules Janssen, 92195 Meudon, France</footnote>

<footnote n="25">²⁵Lund Observatory, Department of Astronomy and Theoretical Physics, Box 43, SE-221 00 Lund, Sweden</footnote>

<footnote n="26">²⁶INAF - Osservatorio di Astrofisica e Scienza dello Spazio, via P. Gobetti 93/3, 40129 Bologna, Italy</footnote>

<footnote n="27">²⁷Instituto Nacional de Astrofísica, Óptica y Electrónica, Luis Enrique Erro 1, Tonantzintla, Puebla C.P. 72840, Mexico</footnote>

<footnote n="28">²⁸Institute for Astronomy, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK</footnote>

<footnote n="29">²⁹Université de Strasbourg, CNRS, Observatoire astronomique de Strasbourg, UMR 7550, 67000 Strasbourg, France</footnote>

<footnote n="30">³⁰UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK</footnote>

<footnote n="31">³¹Instituto de Astrofísica de Andalucía, CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain</footnote>

<footnote n="32">³²ASTRON, Netherlands Institute for Radio Astronomy, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands</footnote>

<footnote n="33">³³Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Merseyside L3 5RF, UK</footnote>

<footnote n="34">³⁴Department of Physics, McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15213, USA</footnote>

<footnote n="35">³⁵Institut d'Astrophysique de Paris, 98bis Bd Arago, 75014 Paris, France</footnote>

<footnote n="36">³⁶Technical University of Munich Institute for Advanced Studies, Lichtenbergstr. 2a, 85748 Garching, Germany</footnote>

<footnote n="37">³⁷INAF - Osservatorio Astronomico di Capodimonte, Salita Moiariello, 16, 80131 Napoli, Italy</footnote>

<footnote n="38">³⁸Department of Astronomy, University of Illinois at Urbana-Champaign, Urbana, IL 61801, USA</footnote>

<footnote n="39">³⁹Instituto de Astronomía y Ciencias Planetarias, Universidad de Atacama, Copayapu 485, Copiapó, Chile</footnote>

<footnote n="40">⁴⁰Instituto Universitario Carlos I de Física Teórica y Computacional, Universidad de Granada, 18071 Granada, Spain</footnote>

<footnote n="41">⁴¹Instituto de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, 08193 Bellaterra, Barcelona, Spain</footnote>

<footnote n="42">⁴²Departament de Física, Universitat Politècnica de Catalunya, c/Esteve Terrades 5, 08860 Castelldefels, Spain</footnote>

<footnote n="43">⁴³Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking RH5 6NT, UK</footnote>

<footnote n="44">⁴⁴Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA</footnote>

<footnote n="45">⁴⁵INAF - Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy</footnote>

<footnote n="46">⁴⁶Department of Physics, Lancaster University, Bailrigg, Lancaster LA1 4YB, UK</footnote>
<footnote n="47">⁴⁷Dpto. de Física Aplicada, Facultad de Ciencias, Universidad de Alicante, Cta. de San Vicente s/n, 03690 San Vicente del Raspeig, Alicante, Spain</footnote>

<footnote n="48">⁴⁸Astrophysics Group, Keele University, Keele ST5 5BG, UK</footnote>

<footnote n="49">⁴⁹INAF – Osservatorio Astronomico di Brera, via Bianchi 46, 23087 Merate (LC), Italy</footnote>

<footnote n="50">⁵⁰Donostia International Physics Center, Paseo Manuel de Lardizabal 4, 20018 San Sebastián, Spain</footnote>

<footnote n="51">⁵¹IKERBASQUE, Basque Foundation for Science, Bilbao, Plaza Euskadi 5, 48009 Bilbao, Spain</footnote>

<footnote n="52">⁵²Leiden Observatory, Leiden University, Niels Bohrweg 2, 2333 CA Leiden, The Netherlands</footnote>

<footnote n="53">⁵³Leibniz-Institut für Astrophysik Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany</footnote>

<footnote n="54">⁵⁴Laboratoire d'astrophysique de Bordeaux, Université de Bordeaux, CNRS, B18N Allée Geoffroy Saint-Hilaire, 33615 Pessac, France</footnote>

<footnote n="55">⁵⁵Departamento de Física Teórica, Universidad Autónoma de Madrid (UAM), Campus de Cantoblanco, 28049 Madrid, Spain</footnote>

<footnote n="56">⁵⁶Australian Astronomical Optics, Macquarie University, 105 Delhi Road, North Ryde, NSW 2113, Australia</footnote>

<footnote n="57">⁵⁷ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia</footnote>

<footnote n="58">⁵⁸Centro de Astrobiología (CAB/CSIC-INTA), Ctra. de Ajalvir km 4, Torrejón de Ardoz, 28850 Madrid, Spain</footnote>

<footnote n="59">⁵⁹Institute for Computational Cosmology, Durham University, Durham DH1 3LE, UK</footnote>

<footnote n="60">⁶⁰Centre for Extragalactic Astronomy, Durham University, Durham DH1 3LE, UK</footnote>

<footnote n="61">⁶¹Departamento de Física Teórica y del Cosmos, Universidad de Granada, Campus de Fuentenueva, 18071 Granada, Spain</footnote>

<footnote n="62">⁶²Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante, Cta. de San Vicente s/n, 03690 San Vicente del Raspeig, Alicante, Spain</footnote>

<footnote n="63">⁶³Dipartimento di Fisica 'G. Occhialini', Università degli Studi di Milano-Bicocca, Piazza della Scienza 3, 20126 Milano, Italy</footnote>

<footnote n="64">⁶⁴Department of Physics, University of Surrey, Guildford, Surrey GU2 7XH, UK</footnote>

<footnote n="65">⁶⁵INAF – Osservatorio Astronomico di Trieste, Via Giambattista Tiepolo, 11, 34131 Trieste (TS), Italy</footnote>

<footnote n="66">⁶⁶Department of Chemistry and Physics, Saint Mary's College, Notre Dame, IN 46556, USA</footnote>

<footnote n="67">⁶⁷Research School of Astronomy & Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston Creek, ACT 2611, Australia</footnote>

<footnote n="68">⁶⁸Institute of Physics, University of Graz, Universitätsplatz 5, A-8010 Graz, Austria</footnote>

<footnote n="69">⁶⁹INAF – Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy</footnote>

<footnote n="70">⁷⁰INAF – Fundación Galileo Galilei, Rambla José Ana Fernández Pérez 7, 38712 Breña Baja, Tenerife, Spain</footnote>

<footnote n="71">⁷¹Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK</footnote>

<footnote n="72">⁷²Department of Physics & Astronomy, University of the Western Cape, Private Bag X17, Bellville, Cape Town 7535, South Africa</footnote>

<footnote n="73">⁷³Centre de Recherche Astrophysique de Lyon UMR5574, Université de Lyon 1, 9 Av. Charles André, 69230 Saint-Genis-Laval, France</footnote>

<footnote n="74">⁷⁴Department of Astrophysics/IMAPP, Radboud University, PO Box 9010, 6500 GL Nijmegen, The Netherlands</footnote>

<footnote n="75">⁷⁵Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr. 12-14, 69120 Heidelberg, Germany</footnote>

<footnote n="76">⁷⁶ESA – ESTEC, MMO, Keplerlaan 1, PO Box 299, 2200 AG Noordwijk, The Netherlands</footnote>

<footnote n="77">⁷⁷Department of Astronomy, AlbaNova University Centre, Stockholm University, SE-106 91 Stockholm, Sweden</footnote>

<footnote n="78">⁷⁸Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany</footnote>

<footnote n="79">⁷⁹Department of Physics and Astronomy, Uppsala University, Box 516, SE-751 20 Uppsala, Sweden</footnote>

<footnote n="80">⁸⁰Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA</footnote>

<footnote n="81">⁸¹Centro de Astrobiología (CAB/CSIC-INTA), ESAC campus, Camino bajo del castillo s/n, Villanueva de la Cañada, 28692 Madrid, Spain</footnote>

<footnote n="82">⁸²Institució Catalana de Recerca i Estudis Avançats, Passeig Lluís Companys 23, 08010 Barcelona, Spain</footnote>

<footnote n="83">⁸³INAF – Osservatorio Astronomico di Cagliari, Via della Scienza 5, 09047 Selargius (CA), Italy</footnote>

<footnote n="84">⁸⁴School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL, UK</footnote>

<footnote n="85">⁸⁵Facultad de física, Universidad de Sevilla, Avda. Reina Mercedes s/n, Campus Reina Mercedes, 41012 Sevilla, Spain</footnote>

<footnote n="86">⁸⁶National Astronomical Observatory of Japan, Mitaka-shi, Tokyo 181-8588, Japan</footnote>

<footnote n="87">⁸⁷NOVA Optical-Infrared Instrumentation Group at ASTRON, PO Box 2, 7990 AA Dwingeloo, The Netherlands</footnote>

<footnote n="88">⁸⁸Département de Physique Théorique, Université de Genève, 24 quai Ernest Ansermet, CH-1211 Genève 4, Switzerland</footnote>

<footnote n="89">⁸⁹Dipartimento di Fisica 'E.R. Caianiello', Università degli Studi di Salerno, Via Giovanni Paolo II 132, 84084 Fisciano (SA), Italy</footnote>

<footnote n="90">⁹⁰Armagh Observatory and Planetarium, College Hill, Armagh BT61 9DG, UK</footnote>

<footnote n="91">⁹¹Joint ALMA Observatory, Alonso de Córdova 3107, Vitacura, Santiago 763-0355, Chile</footnote>

<footnote n="92">⁹²National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA</footnote>

<footnote n="93">⁹³School of Physics and Astronomy, Sir William Henry Bragg Building, University of Leeds, Leeds LS2 9JT, UK</footnote>

<footnote n="94">⁹⁴School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK</footnote>

<footnote n="95">⁹⁵Zentrum für Astronomie der Universität Heidelberg, Landessternwarte, Königstuhl 12, 69117 Heidelberg, Germany</footnote>

<footnote n="96">⁹⁶School of Architecture – Universidad Europea de Canarias, C. Inocencio García, 1, 38300 La Orotava, Tenerife, Spain</footnote>

<footnote n="97">⁹⁷GAPHE Institut d'Astroph. et de Géoph., Université de Liège, Allée du 6 Août 19c, B-4000 Sart Tilman, Liège, Belgium</footnote>

<footnote>This paper has been typeset from a TEX/LATEX file prepared by the author.</footnote>
<footnote n="47">⁴⁷Dpto. de Física Aplicada, Facultad de Ciencias, Universidad de Alicante, Cta. de San Vicente s/n, 03690 San Vicente del Raspeig, Alicante, Spain</footnote>

<footnote n="48">⁴⁸Astrophysics Group, Keele University, Keele ST5 5BG, UK</footnote>

<footnote n="49">⁴⁹INAF – Osservatorio Astronomico di Brera, via Bianchi 46, 23087 Merate (LC), Italy</footnote>

<footnote n="50">⁵⁰Donostia International Physics Center, Paseo Manuel de Lardizabal 4, 20018 San Sebastián, Spain</footnote>

<footnote n="51">⁵¹IKERBASQUE, Basque Foundation for Science, Bilbao, Plaza Euskadi 5, 48009 Bilbao, Spain</footnote>

<footnote n="52">⁵²Leiden Observatory, Leiden University, Niels Bohrweg 2, 2333 CA Leiden, The Netherlands</footnote>

<footnote n="53">⁵³Leibniz-Institut für Astrophysik Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany</footnote>

<footnote n="54">⁵⁴Laboratoire d'astrophysique de Bordeaux, Université de Bordeaux, CNRS, B18N Allée Geoffroy Saint-Hilaire, 33615 Pessac, France</footnote>

<footnote n="55">⁵⁵Departamento de Física Teórica, Universidad Autónoma de Madrid (UAM), Campus de Cantoblanco, 28049 Madrid, Spain</footnote>

<footnote n="56">⁵⁶Australian Astronomical Optics, Macquarie University, 105 Delhi Road, North Ryde, NSW 2113, Australia</footnote>

<footnote n="57">⁵⁷ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia</footnote>

<footnote n="58">⁵⁸Centro de Astrobiología (CAB/CSIC-INTA), Ctra. de Ajalvir km 4, Torrejón de Ardoz, 28850 Madrid, Spain</footnote>

<footnote n="59">⁵⁹Institute for Computational Cosmology, Durham University, Durham DH1 3LE, UK</footnote>

<footnote n="60">⁶⁰Centre for Extragalactic Astronomy, Durham University, Durham DH1 3LE, UK</footnote>

<footnote n="61">⁶¹Departamento de Física Teórica y del Cosmos, Universidad de Granada, Campus de Fuentenueva, 18071 Granada, Spain</footnote>

<footnote n="62">⁶²Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante, Cta. de San Vicente s/n, 03690 San Vicente del Raspeig, Alicante, Spain</footnote>

<footnote n="63">⁶³Dipartimento di Fisica 'G. Occhialini', Università degli Studi di Milano-Bicocca, Piazza della Scienza 3, 20126 Milano, Italy</footnote>

<footnote n="64">⁶⁴Department of Physics, University of Surrey, Guildford, Surrey GU2 7XH, UK</footnote>

<footnote n="65">⁶⁵INAF – Osservatorio Astronomico di Trieste, Via Giambattista Tiepolo, 11, 34131 Trieste (TS), Italy</footnote>

<footnote n="66">⁶⁶Department of Chemistry and Physics, Saint Mary's College, Notre Dame, IN 46556, USA</footnote>

<footnote n="67">⁶⁷Research School of Astronomy & Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston Creek, ACT 2611, Australia</footnote>

<footnote n="68">⁶⁸Institute of Physics, University of Graz, Universitätsplatz 5, A-8010 Graz, Austria</footnote>

<footnote n="69">⁶⁹INAF – Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy</footnote>

<footnote n="70">⁷⁰INAF – Fundación Galileo Galilei, Rambla José Ana Fernández Pérez 7, 38712 Breña Baja, Tenerife, Spain</footnote>

<footnote n="71">⁷¹Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK</footnote>

<footnote n="72">⁷²Department of Physics & Astronomy, University of the Western Cape, Private Bag X17, Bellville, Cape Town 7535, South Africa</footnote>

<footnote n="73">⁷³Centre de Recherche Astrophysique de Lyon UMR5574, Université de Lyon 1, 9 Av. Charles André, 69230 Saint-Genis-Laval, France</footnote>

<footnote n="74">⁷⁴Department of Astrophysics/IMAPP, Radboud University, PO Box 9010, 6500 GL Nijmegen, The Netherlands</footnote>

<footnote n="75">⁷⁵Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr. 12-14, 69120 Heidelberg, Germany</footnote>

<footnote n="76">⁷⁶ESA – ESTEC, MMO, Keplerlaan 1, PO Box 299, 2200 AG Noordwijk, The Netherlands</footnote>

<footnote n="77">⁷⁷Department of Astronomy, AlbaNova University Centre, Stockholm University, SE-106 91 Stockholm, Sweden</footnote>

<footnote n="78">⁷⁸Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany</footnote>

<footnote n="79">⁷⁹Department of Physics and Astronomy, Uppsala University, Box 516, SE-751 20 Uppsala, Sweden</footnote>

<footnote n="80">⁸⁰Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA</footnote>

<footnote n="81">⁸¹Centro de Astrobiología (CAB/CSIC-INTA), ESAC campus, Camino bajo del castillo s/n, Villanueva de la Cañada, 28692 Madrid, Spain</footnote>

<footnote n="82">⁸²Institució Catalana de Recerca i Estudis Avançats, Passeig Lluís Companys 23, 08010 Barcelona, Spain</footnote>

<footnote n="83">⁸³INAF – Osservatorio Astronomico di Cagliari, Via della Scienza 5, 09047 Selargius (CA), Italy</footnote>

<footnote n="84">⁸⁴School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL, UK</footnote>

<footnote n="85">⁸⁵Facultad de física, Universidad de Sevilla, Avda. Reina Mercedes s/n, Campus Reina Mercedes, 41012 Sevilla, Spain</footnote>

<footnote n="86">⁸⁶National Astronomical Observatory of Japan, Mitaka-shi, Tokyo 181-8588, Japan</footnote>

<footnote n="87">⁸⁷NOVA Optical-Infrared Instrumentation Group at ASTRON, PO Box 2, 7990 AA Dwingeloo, The Netherlands</footnote>

<footnote n="88">⁸⁸Département de Physique Théorique, Université de Genève, 24 quai Ernest Ansermet, CH-1211 Genève 4, Switzerland</footnote>

<footnote n="89">⁸⁹Dipartimento di Fisica 'E.R. Caianiello', Università degli Studi di Salerno, Via Giovanni Paolo II 132, 84084 Fisciano (SA), Italy</footnote>

<footnote n="90">⁹⁰Armagh Observatory and Planetarium, College Hill, Armagh BT61 9DG, UK</footnote>

<footnote n="91">⁹¹Joint ALMA Observatory, Alonso de Córdova 3107, Vitacura, Santiago 763-0355, Chile</footnote>

<footnote n="92">⁹²National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA</footnote>

<footnote n="93">⁹³School of Physics and Astronomy, Sir William Henry Bragg Building, University of Leeds, Leeds LS2 9JT, UK</footnote>

<footnote n="94">⁹⁴School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK</footnote>

<footnote n="95">⁹⁵Zentrum für Astronomie der Universität Heidelberg, Landessternwarte, Königstuhl 12, 69117 Heidelberg, Germany</footnote>

<footnote n="96">⁹⁶School of Architecture – Universidad Europea de Canarias, C. Inocencio García, 1, 38300 La Orotava, Tenerife, Spain</footnote>

<footnote n="97">⁹⁷GAPHE Institut d'Astroph. et de Géoph., Université de Liège, Allée du 6 Août 19c, B-4000 Sart Tilman, Liège, Belgium</footnote>

<footnote>This paper has been typeset from a TEX/LATEX file prepared by the author.</footnote>