Final design and progress of WEAVE: the next generation wide-field spectroscopy facility for the William Herschel Telescope

Dalton, Gavin; Trager, S. C.; Abrams, Don Carlos; Bonifacio, P.; Aguerri, J. A. L.; Middleton, Kevin; Benn, Chris; Dee, Kevin; Sayède, Frédéric; Lewis, Ian; Pragt, J.; Picó, Sergio; Walton, N. A.; Rey, Jeurg; Prieto, C. Allende; Peñate, José; Lhomé, Émilie; Agócs, Tibor; Alonso, José L.; Terrett, D. L.; Brock, Matthew; Gilbert, James; Schallig, Ellen; Ridings, Andy; Guinouard, Isabelle; Verheijen, Marc; Tosh, Ian; Rogers, Kevin; Lee, Martin; Steele, I. A.; Stuik, Remko; Tromp, Niels; Jaskó, Attila; Carrasco, E.; Farcas, Szigfrid; Kragt, Jan; Lesman, Dirk; Kroes, Gabby; Mottram, Chris; Bates, Stuart; Rodríguez, L. F.; Gribbin, Frank; Delgado, José Miguel; Herreros, J. M.; Martín, Carlos; Cano, Diego; Navarro, Ramón; Irwin, M. J.; Lewis, Jim; Solares, Eduardo González; Murphy, D. N. A.; Worley, C. C.; Bassom, Richard; O'Mahoney, Neil; Bianco, Andrea; Zurita, Christina; Horst, Rik ter; Molinari, E.; Lodi, M.; Guerra, J.; Martin, Adrian P.; Vallenari, A.; Salasnich, Bernardo; Baruffolo, A.; Jin, Shoko; Hill, V.; Smith, Dan; Drew, J. E.; Poggianti, Bianca M.; Pieri, Matthew M.; Palmero, Lillian Dominquez; Fariña, C.

doi:10.1117/12.2231078

Cited by 41 publications

(29 citation statements)

References 4 publications

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“…The LRS covers the full spectral range of 370 − 950 nm. This is very similar to many of the other survey instruments including WEAVE (Dalton et al (2016)), DESI (DESI collaboration (2016)), LAMOST, and SEGUE. Further details on exposure times and how the resolution varies across each passband can be found in de Jong et al (2016a) andde Jong et al (2016b).…”

Section: A Brief Introduction To the 4most Facilitysupporting

confidence: 76%

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Galactic Archeology with 4MOST

et al. 2017

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4MOST is a new wide-field, high-multiplex spectroscopic survey facility for the VISTA telescope of ESO. Starting in 2022, 4MOST will deploy more than 2400 fibres in a 4.1 square degree field-of-view using a positioner based on the tilting spine principle. In this contribution we give an outline of the major science goals we wish to achieve with 4MOST in the area of Galactic Archeology. The 4MOST Galactic Archeology surveys have been designed to address long-standing and far-reaching problems in Galactic science. They are focused on four major themes: 1) Near-field cosmology tests, 2) Chemo-dynamical characterisation of the major Milky Way stellar components, 3) The Galactic Halo and beyond, and 4) Discovery and characterisation of extremely metal-poor stars.In addition to a top-level description of the Galactic surveys we provide information about how the community will be able to join 4MOST via a call for Public Spectroscopic Surveys that ESO will launch.

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Section: A Brief Introduction To the 4most Facilitysupporting

confidence: 76%

“…WEAVE has three passbands, however, at any given time only two are used. The choice is to have either the blue or the green band, Dalton et al (2016). At the bottom we show the three passbands of the 4MOST HRS.…”

Section: A Brief Introduction To the 4most Facilitymentioning

confidence: 99%

Galactic Archeology with 4MOST

et al. 2017

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“…By combining self-consistent chemical evolution models with the large amount of available and upcoming data (e.g. Dalton et al 2016;Jönsson et al 2018;Buder et al 2018;de Jong et al 2019), we will be able to further test our proposed scenario and put stronger constraints on the complicated timescales of the r-process.…”

Section: Discussionmentioning

confidence: 99%

Evidence for ≳4 Gyr timescales of neutron star mergers from Galactic archaeology

Skúladóttir

Salvadori

2020

A&A

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The nucleosynthetic site of the rapid (r) neutron-capture process is currently being debated. The direct detection of the neutron star merger GW170817, through gravitational waves and electromagnetic radiation, has confirmed such events as important sources of the r-process elements. However, chemical evolution models are not able to reproduce the observed chemical abundances in the Milky Way when neutron star mergers are assumed to be the only r-process site and realistic time distributions of such events are taken into account. Now for the first time, we combine all the available observational evidence of the Milky Way and its dwarf galaxy satellites to show that the data can only be explained if there are (at least) two distinct r-process sites: a quick source with timescales comparable to core-collapse supernovae, t quick 10 8 yr, and a delayed source with characteristic timescales t delayed 4 Gyr. The delayed r-process source most probably originates in neutron star mergers, as the timescale fits well with that estimated for GW170817. Given the short timescales of the quick source, it is likely associated with massive stars, though a specific fast-track channel for compact object mergers cannot be excluded at this point. Our approach demonstrates that only by looking at all the available data will we be able to solve the puzzle that is the r-process.

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“…The thick disk is important because its formation is a seemingly ubiquitous feature of disk galaxy evolution; its rapid formation and old population means that it provides a detailed snap-shot of the conditions in the early Galaxy. Understanding how the thick disk formed and evolved will be central to chemical tagging efforts of current and future high resolution massive spectroscopic surveys such as 4MOST (de Jong et al 2011), Gaia-ESO (Gilmore et al 2012), APOGEE (Majewski et al 2015), GALAH 2 (De Silva et al 2015), and WEAVE (Dalton et al 2016).…”

Section: Introductionmentioning

confidence: 99%

The GALAH survey: properties of the Galactic disc(s) in the solar neighbourhood

Duong

Freeman

Asplund

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Using data from the GALAH pilot survey, we determine properties of the Galactic thin and thick disks near the solar neighbourhood. The data cover a small range of Galactocentric radius (7.9 R GC 9.5 kpc), but extend up to 4 kpc in height from the Galactic plane, and several kpc in the direction of Galactic anti-rotation (at longitude 260 • 280 • ). This allows us to reliably measure the vertical density and abundance profiles of the chemically and kinematically defined 'thick' and 'thin' disks of the Galaxy. The thin disk (low-α population) exhibits a steep negative vertical metallicity gradient, at d[M/H]/dz = −0.18 ± 0.01 dex kpc −1 , which is broadly consistent with previous studies. In contrast, its vertical α-abundance profile is almost flat, with a gradient of d[α/M]/dz = 0.008 ± 0.002 dex kpc −1 . The steep vertical metallicity gradient of the low-α population is in agreement with models where radial migration has a major role in the evolution of the thin disk. The thick disk (high-α population) has a weaker vertical metallicity gradient d[M/H]/dz = −0.058 ± 0.003 dex kpc −1 . The α-abundance of the thick disk is nearly constant with height, d[α/M]/dz = 0.007 ± 0.002 dex kpc −1 . The negative gradient in metallicity and the small gradient in [α/M] indicate that the high-α population experienced a settling phase, but also formed prior to the onset of major SNIa enrichment. We explore the implications of the distinct α-enrichments and narrow [α/M] range of the sub-populations in the context of thick disk formation.

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Final design and progress of WEAVE: the next generation wide-field spectroscopy facility for the William Herschel Telescope

Cited by 41 publications

References 4 publications

Galactic Archeology with 4MOST

Galactic Archeology with 4MOST

Evidence for ≳4 Gyr timescales of neutron star mergers from Galactic archaeology

The GALAH survey: properties of the Galactic disc(s) in the solar neighbourhood

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