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

被引：9

作者：

Iovino, A. ^{[1
]}

Poggianti, B. M. ^{[2
]}

Mercurio, A. ^{[3
,4
]}

Longhetti, M. ^{[1
]}

Bolzonella, M. ^{[5
]}

Busarello, G. ^{[3
]}

Gullieuszik, M. ^{[2
]}

La Barbera, F. ^{[3
]}

Merluzzi, P. ^{[3
]}

Morelli, L. ^{[1
,6
]}

Tortora, C. ^{[3
]}

Vergani, D. ^{[5
]}

Zibetti, S. ^{[7
]}

Haines, C. P. ^{[1
,6
]}

Costantin, L. ^{[8
]}

Ditrani, F. R. ^{[1
,9
]}

Pozzetti, L. ^{[5
]}

Angthopo, J. ^{[1
]}

Balcells, M. ^{[10
,11
,12
]}

Bardelli, S. ^{[5
]}

Benn, C. R. ^{[10
]}

Bianconi, M. ^{[13
]}

Cassara, L. P. ^{[14
]}

Corsini, E. M. ^{[2
,15
]}

Cucciati, O. ^{[5
]}

Dalton, G. ^{[16
,17
]}

Ferre-Mateu, A. ^{[11
,12
]}

Fossati, M. ^{[1
,9
]}

Gallazzi, A. ^{[7
]}

Garcia-Benito, R. ^{[18
]}

Granett, B. ^{[1
]}

Delgado, R. M. Gonzalez ^{[18
]}

Ikhsanova, A. ^{[15
]}

Iodice, E. ^{[3
]}

Jin, S. ^{[16
,19
,20
]}

Knapen, J. H. ^{[11
,12
]}

McGee, S. ^{[13
]}

Moretti, A. ^{[2
]}

Murphy, D. N. A. ^{[21
]}

de Arriba, L. Peralta ^{[8
,21
]}

Pizzella, A. ^{[2
,15
]}

Sanchez-Blazquez, P. ^{[22
,23
]}

Spiniello, C. ^{[3
,16
]}

Talia, M. ^{[5
,24
]}

Trager, S. C. ^{[19
]}

Vazdekis, A. ^{[11
,12
]}

Vulcani, B. ^{[2
]}

Zucca, E. ^{[5
]}

机构：

[1] INAF Osservatorio Astron Brera, Via Brera 28, I-20121 Milan, Italy

[2] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[3] INAF Osservatorio Astron Capodimonte, Via Moiariello 16, I-80131 Naples, Italy

[4] Univ Salerno, Dipartimento Fis ER Caianiello, Via Giovanni Paolo II 132, I-84084 Fisciano, SA, Italy

[5] INAF Osservatorio Astrofis & Sci Spazio, Via P Gobetti 93-3, I-40129 Bologna, Italy

[6] Univ Atacama, Inst Astron & Ciencias Planetarias Atacama INCT, Copayapu 485, Copiapo, Chile

[7] INAF Osservatorio Astrofis Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Italy

[8] Ctr Astrobiol CSIC INTA, Ctra Ajalvir Km 4, Madrid 28850, Spain

[9] Univ Milano Bicocca, Piazza Sci, I-20125 Milan, Italy

[10] Isaac Newton Grp Telescopes ING, La Palma 38700, SC Tenerife, Spain

[11] Inst Astrofis Canarias IAC, Via Lactea S-N, Tenerife 38205, SC Tenerife, Spain

[12] Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38206, SC Tenerife, Spain

[13] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, England

[14] INAF IASF Milano, Via Bassini 15, I-20133 Milan, Italy

[15] Univ Padua, Dipartimento Fis & Astron G Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy

[16] Univ Oxford, Dept Phys, Keble Rd, Oxford OX1 3RH, England

[17] RAL Space, Sci & Technol Facil Council, Didcot OX11 0QX, England

[18] CSIC, Inst Astrofis Andalucia, POB 3004, Granada 18080, Spain

[19] Univ Groningen, Kapteyn Astron Inst, Landleven 12, NL-9747 AD Groningen, Netherlands

[20] SRON Netherlands Inst Space Res, Landleven 12, NL-9747 AD Groningen, Netherlands

[21] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[22] Univ Complutense Madrid, Dept Fis Tierra & Astrofis, Madrid 28040, Spain

[23] Univ Complutense Madrid, Inst Fis Particulas & Cosmos IPARCOS, Madrid 28040, Spain

[24] Univ Bologna, Dept Phys & Astron, Via Gobetti 93-2, I-40129 Bologna, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2023年 / 672卷

基金：

瑞典研究理事会; 英国科学技术设施理事会;

关键词：

galaxies; general; formation; evolution; star formation; stellar content; statistics; STAR-FORMATION HISTORIES; SIMILAR-TO; 0.8; REDSHIFT SURVEY VIPERS; DIGITAL SKY SURVEY; OSCILLATION SPECTROSCOPIC SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; EMISSION-LINE GALAXIES; WIDE-FIELD SURVEY; VLT DEEP SURVEY; DATA RELEASE;

D O I：

10.1051/0004-6361/202245361

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 (similar to 950 fibres distributed across a field of view of similar to 3 square degrees on the sky) in low-resolution mode (R similar to 5000, spanning the wavelength range 3660 - 9590 angstrom).Methods. WEAVE-StePS will obtain high-quality spectra (S/N similar to 10 angstrom(-1) at R similar to 5000) for a magnitude-limited (I-AB=20.5) sample of similar to 25000 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 similar to 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 similar to 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.

引用

页数：15

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