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

Jin, Shoko; Trager, S. C.; Dalton, Gavin; Aguerri, J. A. L.; Drew, J. E.; Falcón-Barroso, J.; Gänsicke, B. T.; Hill, V.; Iovino, A.; Pieri, Matthew M.; Poggianti, Bianca M.; Smith, Daniel; Vallenari, A.; Abrams, Don Carlos; Aguado, David S.; Antoja, T.; Aragón-Salamanca, Alfonso; Ascasíbar, Y.; Babusiaux, C.; Balcells, M.; Barrena, R.; Battaglia, G.; Belokurov, V.; Bensby, T.; Bonifacio, P.; Bragaglia, A.; Carrasco, E.; Carrera, R.; Cornwell, Daniel J.; Domínguez-Palmero, Lilian; Duncan, K. J.; Famaey, Benoît; Fariña, C.; González, Óscar; Guest, Steve; Hatch, N. A.; Hess, Kelley M.; Hoskin, Matthew J.; Irwin, Michael R.; Knapen, J. H.; Koposov, Sergey E.; Kuchner, Ulrike; Laigle, C.; Lewis, Jim; Longhett, Marcella; Lucatello, S.; Méndez-Abreu, J.; Mercurio, A.; Molaeinezhad, Alireza; Monguió, M.; Morrison, Sean J.; Murphy, D. N. A.; Arriba, L. Peralta de; Pérez, Isabel; Pérez-Ràfols, Ignasi; Picó, Sergio; Raddi, R.; Romero-Gómez, M.; Royer, F.; Siebert, A.; Seabroke, G. M.; Som, Debopam; Terrett, D. L.; Thomas, Guillaume; Wesson, R.; Worley, C. C.; Alfaro, Emilio J.; Prieto, C. Allende; Alonso-Santiago, J.; Amos, Nicholas J.; Ashley, R. P.; Balaguer-Núñez, L.; Balbinot, E.; Bellazzini, M.; Benn, Chris; Berlanas, S. R.; Bernard, Edouard J.; Best, P. N.; Bettoni, D.; Bianco, Andrea; Bishop, Georgia; Blomqvist, Michael; Boeche, C.; Bolzonella, M.; Bonoli, Silvia; Bosma, A.; Britavskiy, N.; Busarello, G.; Caffau, E.; Cantat-Gaudin, T.; Castro-Ginard, A.; Couto, Guilherme S.; Carbajo-Hijarrubia, J.; Carter, David; Casamiquela, L.; Conrado, Ana M.; Corcho-Caballero, Pablo; Costantin, Luca; Deason, Alis J.; Burgos, Abel de; Grandi, S. De; Matteo, P. Di; Domínguez-Gómez, Jesús; Dorda, R.; Drake, Alyssa B.; Dutta, Rajeshwari; Erkal, Denis; Feltzing, Sofia; Ferré-Mateu, Anna; Feuillet, Diane; Figueras, F.; Fossat, Matteo; Franciosin, Elena; Frasca, A.; Fumagalli, Michele; Gallazzi, Anna; García-Benito, R.; Fusillo, Nicola Gentile; Gebran, M.; Gilbert, James; Gledhill, T. M.; Delgado, R. M. González; Greimel, R.; Guarcello, M. G.; Guerra, José Luiz; Gullieuszik, Marco; Haines, C. P.; Hardcastle, Martin; Harris, Amy; Haywood, M.; Helmi, Amina; Hernández, N.; Herrero, A.; Hughes, Sarah Jane; Iršič, Vid; Jablonka, P.; Jarvis, Matt J.; Jordi, C.; Kondapally, R.; Kordopatis, G.; Krogager, Jens-Kristian; Barbera, Francesco La; Lam, Man I; Larsen, S. S.; Lemasle, B.; Lewis, Ian; Lhomé, Émilie; Lind, Karin; Lodi, M.; Longobardi, A.; Lonoce, I.; Magrin, Laura; Apellániz, J. Maíz; Marchal, Olivier; Marco, A.; Martín, Nicolás F.; Matsuno, Tadafumi; Maurogordato, S.; Merluzzi, P.; Miralda-Escudé, Jordi; Molinari, E.; Monari, Giacomo; Morelli, L.; Mottram, Christopher J.; Naylor, T.; Negueruela, I.; Oñorbe, José; Pancino, E.; Peirani, Sébastien; Peletier, R. F.; Pozzetti, L.; Rainer, M.; Ramos, P.; Read, Shaun C.; Rossi, Elena M.; Röttgering, H. J. A.; Rubiño-Martín, J. A.; Montes, Jose Sabater; Juan, J. San; Sanna, N.; Schallig, Ellen; Schiavon, Ricardo P.; Schultheis, M.; Serra, P.; Shimwell, T. W.; Simón‐Díaz, S.; Smith, Russell J.; Sordo, R.; Sorini, Daniele; Soubiran, C.; Starkenburg, Else; Steele, I. A.; Stott, John P.; Stuik, Remko; Tolstoy, Eline; Tortora, C.; Tsantaki, M.; Swaelmen, M. Van der; Weeren, R. J. van; Vergani, D.; Verheijen, Marc; Verro, Kristiina; Vink, J. S.; Vioque, M.; Walcher, C. Jakob; Walton, N. A.; Wegg, Christopher; Weijmans, Anne-Marie; Williams, W. L.; Wilson, Andrew; Wright, Nicholas J.; Xylakis-Dornbusch, Theodora; Youakim, Kris; Zibetti, S.; Zurita, C.

doi:10.48550/arxiv.2212.03981

Cited by 13 publications

(19 citation statements)

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“…Detailed modeling of the spatially-resolved morpho-kinematics of the extended metal emission is required to place more robust constraints on the potential physical mechanisms and gas conditions. Larger galaxy surveys such as WEAVE (Jin et al 2022) and4MOST (de Jong et al 2019), and deeper observations of individual systems with MUSE (Bacon et al 2010), KCWI (Morrissey et al 2018), JWST (Gardner et al 2006), ERIS (Davies et al 2018), and future instruments such as VLT/BlueMUSE (Richard et al 2019) and ELT/HARMONI (Thatte et al 2021), will allow us to obtain multiple diagnostics and interpret the physical mechanisms driving the extended emission. ital grant ST/K00042X/1, STFC capital grants ST/H008519/1 and ST/K00087X/1, STFC DiRAC Operations grant ST/K003267/1 and Durham University.…”

Section: Discussionmentioning

confidence: 99%

Metal line emission from galaxy haloes at z~1

Dutta¹,

Fossati²,

Fumagalli³

et al. 2023

Preprint

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We present a study of the metal-enriched halo gas, traced using Mg and [O ] emission lines, in two large, blind galaxy surveys conducted using Multi Unit Spectroscopic Explorer (MUSE) optical integral field unit observations, namely the MUSE Analysis of Gas around Galaxies (MAGG) and the MUSE Ultra Deep Field (MUDF). By stacking a sample of ≈600 galaxies with stellar masses M * ≈ 10 6−12 M (median M * ≈ 2 × 10 9 M ) at redshifts 𝑧 = 0.7 − 1.5 (median 𝑧 ≈ 1), we characterize for the first time the average metal line emission from a general population of galaxy haloes. The Mg and [O ] line emission extends farther out than the stellar continuum emission around galaxies, on average out to ≈25 kpc and ≈45 kpc, respectively, at a surface brightness (SB) level of 10 −20 erg s −1 cm −2 arcsec −2 . The radial profile of the Mg SB is shallower than that of the [O ], suggesting that the resonant Mg emission is affected by dust and radiative transfer effects. The [O ] to Mg SB ratio is ≈ 3 over ≈ 20 − 40 kpc, also indicating a significant in situ origin of the extended metal emission in the inner halo. The average profiles are intrinsically brighter by a factor ≈ 2 − 3 and more radially extended by a factor of ≈ 1.3 at 1.0 < 𝑧 ≤ 1.5 than at 0.7 ≤ 𝑧 ≤ 1.0. The average extent of the metal emission also increases independently with increasing stellar mass and in overdense group environments. When considering individual detections, we find extended [O ] emission up to ≈ 50 kpc around ≈ 30 − 40 percent of the group galaxies, and extended (≈ 30 − 40 kpc) Mg emission around two 𝑧 ≈ 1 quasars in groups, which could arise from outflows or environmental processes.

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Section: Discussionmentioning

confidence: 99%

Metal line emission from galaxy haloes at z~1

Dutta¹,

Fossati²,

Fumagalli³

et al. 2023

Preprint

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“…Our code can serve both as an illustration of where the chemical information is present in a stellar spectrum, but most importantly allows one to optimise i) observational strategies, such as choosing resolution and spectral windows, as well as 2) analysis codes, with the application of masks of high quality. In particular, direct applications for observations using the WEAVE (Jin et al 2022) and4MOST (de Jong et al 2019) facilities (both community and consortium surveys) will benefit largely of the present tool.…”

Section: Discussionmentioning

confidence: 99%

“…We now put ourselves in the framework of a survey design, for instance WEAVE. There exist two WEAVE Galactic archaeology (GA) HR surveys, a HR-chemodynamical survey targeting the thin and thick disc as well as the halo, and an Open Cluster survey, aiming to target roughly a hundred of young and old open clusters in the disc (Jin et al 2022) To set this value, we rely on WEAVE's GA survey plan (WEAVE consortium, private communication) and adopt as a threshold S/N resol = 70, which is the value of the expected S/N peak in the blue setup for the typical selection of the WEAVE GA-HR baseline survey. Other setups are expected to have a higher S/N resol value.…”

Section: Choosing Between Setups: Application To the High-resolution ...mentioning

confidence: 99%

“…for abundance determination), or to visualise how many lines of a specific element or a nucleosynthetic channel are useful for a given instrumental configuration. It therefore has immediate and valuable applications for spectroscopic surveys based on already existing or future spectroscopic facilities or instruments such as APOGEE (Majewski et al 2017), DESI (Abareshi et al 2022), Gaia-RVS (Gaia Collaboration et al 2016;Cropper et al 2018), GALAH (De Silva et al 2015), LAMOST (Deng et al 2012), 4MOST (de Jong et al 2019), WEAVE (Jin et al 2022), MOONS (Cirasuolo et al 2020), MSE (The MSE Science Team et al 2019), PFS (Takada et al 2014), etc. The paper is structured as follows. In Sect.…”

Section: Introductionmentioning

confidence: 99%

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Automatic line selection for abundance determination in large stellar spectroscopic surveys

Kordopatis¹,

Hill²,

Lind³

2023

Preprint

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Context. Over the last years, new multiplex spectrographs having observed or planning to observe several millions of stars have emerged. The optimisation of these instruments (regarding resolution or wavelength range), their associated surveys (choice of instrumental setup), or their parameterisation pipelines require methods that estimate which wavelengths, or pixels, contain useful information.Aims. We propose a method that establishes the usefulness of an atomic spectral line, where usefulness is defined by the purity of the line and its detectability. We show two applications of our code: a) optimising an instrument, by comparing the number of detected useful lines at a given wavelength range and resolution, and b) optimising the line-list for a given setup, in the sense of creating a golden subsample, choosing the least blended lines detectable at different signal-to-noise ratios. Methods. The method compares pre-computed normalised synthetic stellar spectra containing all of the elements and molecules with spectra containing the lines of specific elements alone. Then, the flux ratios between the full spectrum and the element spectrum are computed to estimate the line purities. The method identifies automatically (i) the line's central wavelength, (ii) its detectability based on its depth and a given signal-to-noise threshold and (iii) its usefulness based on the purity ratio defined above. Results. We apply this method to compare the three WEAVE high-resolution setups (Blue: 404−465 nm, Green: 473−545 nm, Red: 595−685 nm), and find that the Green+Red setup both allows one to measure more elements and contains more numerous useful lines. However, there is a disparity in terms of which elements are detected over each of the setups, which we characterise. We also study the performances of high-resolution (R ∼ 20 000) and low-resolution (R ∼ 6 000) spectra covering the entire optical wavelength range. Assuming a purity threshold of 60 per cent, we find that the high-resolution setup contains a much wealthier selection of lines, for any of the considered elements, whereas the low-resolution has a "loss" of 50 to 90 per cent of the lines (depending on the nucleosynthetic channel considered) even when the signal-to-noise is increased. Conclusions. The method presented provides a vital diagnostic of where to focus to get the most out of a spectrograph, and is easy to implement for future instruments that have not decided yet their final configuration, or for pipelines that require line masks.

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“…The WEAVE-Stellar Population Survey (WEAVE-StePS in short) is one of the eight surveys (five of which are extragalactic) that will be performed by the WEAVE spectroscopic facility, using a total of approximately 1150 nights over five years of WHT time (see Jin et al 2022, for more details on the planning of WEAVE operations). WEAVE-StePS will use ∼ 3% of this total budget of nights and aims to take full advantage of the WEAVE capabilities to obtain high-quality (S /N ∼ 10 Å −1 at R ∼ 5000) spectra of ∼ 25, 000 galaxies, the vast majority in the redshift range 0.3 ≤ z ≤ 0.7.…”

Section: Introductionmentioning

confidence: 99%

WEAVE-StePS: A stellar population survey using WEAVE at WHT

Iovino¹,

B.²,

Mercurio³

et al. 2023

A&A

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Context. The upcoming new generation of optical spectrographs on four-meter-class telescopes will provide valuable opportunities for forthcoming galaxy surveys through their huge multiplexing capabilities, excellent spectral resolution, and unprecedented wavelength coverage. Aims. WEAVE is a new wide-field spectroscopic facility mounted on the 4.2 m William Herschel Telescope in La Palma. WEAVE-StePS is one of the five extragalactic surveys that will use WEAVE during its first five years of operations. It will observe galaxies using WEAVE MOS (∼950 fibres distributed across a field of view of ∼3 square degrees on the sky) in low-resolution mode (R ∼ 5000, spanning the wavelength range 3660 − 9590 Å). Methods. WEAVE-StePS will obtain high-quality spectra (S/N ∼ 10 Å−1 at R ∼ 5000) for a magnitude-limited (IAB = 20.5) sample of ∼25 000 galaxies, the majority selected at z ≥ 0.3. The survey goal is to provide precise spectral measurements in the crucial interval that bridges the gap between LEGA-C and SDSS data. The wide area coverage of ∼25 square degrees will enable us to observe galaxies in a variety of environments. The ancillary data available in each of the observed fields (including X-ray coverage, multi-narrow-band photometry and spectroscopic redshift information) will provide an environmental characterisation for each observed galaxy. Results. This paper presents the science case of WEAVE-StePS, the fields to be observed, the parent catalogues used to define the target sample, and the observing strategy that was chosen after a forecast of the expected performance of the instrument for our typical targets. Conclusions. WEAVE-StePS will go back further in cosmic time than SDSS, extending its reach to encompass more than ∼6 Gyr. This is nearly half of the age of the Universe. The spectral and redshift range covered by WEAVE-StePS will open a new observational window by continuously tracing the evolutionary path of galaxies in the largely unexplored intermediate-redshift range.

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

Cited by 13 publications

References 0 publications

Metal line emission from galaxy haloes at z~1

Metal line emission from galaxy haloes at z~1

Automatic line selection for abundance determination in large stellar spectroscopic surveys

WEAVE-StePS: A stellar population survey using WEAVE at WHT

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