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

Iovino, A, Poggianti, BM, Mercurio, A, Longhetti, M, Bolzonella, M, Busarello, G, Gullieuszik, M, La Barbera, F, Merluzzi, P, Morelli, L, Tortora, C, Vergani, D, Zibetti, S, Haines, CP, Costantin, L, Ditrani, FR, Pozzetti, L, Angthopo, J, Balcells, M, Bardelli, S , Benn, CR, Bianconi, M, Cassarà, LP, Corsini, EM, Cucciati, O, Dalton, G, Ferré-Mateu, A, Fossati, M, Gallazzi, A, García-Benito, R, Granett, B, González Delgado, RM, Ikhsanova, A, Iodice, E, Jin, S, Knapen, JH, Mcgee, S, Moretti, A, Murphy, DNA, Peralta De Arriba, L, Pizzella, A, Sánchez-Blázquez, P, Spiniello, C, Talia, M, Trager, SC, Vazdekis, A, Vulcani, B and Zucca, E (2023) WEAVE-StePS: A stellar population survey using WEAVE at WHT. Astronomy and Astrophysics, 672. ISSN 0004-6361

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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.

Item Type: Article
Uncontrolled Keywords: 0201 Astronomical and Space Sciences; Astronomy & Astrophysics
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Publisher: EDP Sciences
SWORD Depositor: A Symplectic
Date Deposited: 26 Jun 2023 12:45
Last Modified: 26 Jun 2023 12:45
DOI or ID number: 10.1051/0004-6361/202245361
URI: https://researchonline.ljmu.ac.uk/id/eprint/20079
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