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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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WEAVE-StePS A stellar population survey using WEAVE at WHT.pdf - Published Version Available under License Creative Commons Attribution. Download (5MB) | Preview |
Abstract
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 Identification number: | 10.1051/0004-6361/202245361 |
| URI: | https://researchonline.ljmu.ac.uk/id/eprint/20079 |
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