CUBES: a UV spectrograph for the future

CUBES: a UV spectrograph for the future

In spite of the advent of extremely large telescopes in the UV/optical/NIR range, the current generation of 8-10m facilities is likely to remain competitive at ground-UV wavelengths for the foreseeable future. The Cassegrain U-Band Efficient Spectrograph (CUBES) has been designed to provide high-eff...

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Veröffentlicht in:arXiv.org 2022-12
Hauptverfasser: Covino, S, Cristiani, S, Alcala', J M, Alencar, S H P, Balashev, S A, Barbuy, B, Bastian, N, Battino, U, Bissell, L, Bristow, P, Calcines, A, Calderone, G, Cambianica, P, Carini, R, Carter, B, Cassisi, S, Castilho, B V, Cescutti, G, Christlieb, N, Cirami, R, Conzelmann, R, Coretti, I, Cooke, R, Cremonese, G, Cunha, K, Cupani, G, da Silva, A R, D'Auria, D, De Caprio, V, De Cia, A, Dekker, H, D'Elia, V, De Silva, G, Diaz, M, P Di Marcantonio, D'Odorico, V, Ernandes, H, Evans, C, Fitzsimmons, A, Franchini, M, Gaensicke, B, Genoni, M, Giribaldi, R E, Gneiding, C, Grazian, A, Hansen, C J, Hopgood, J, Kosmalski, J, La Forgia, F, La Penna, P, Landoni, M, Lazzarin, M, Lunney, D, Maciel, W, Marcolino, W, Marconi, M, Migliorini, A, Miller, C, Modigliani, A, Noterdaeme, P, Oggioni, L, Opitom, C, Pariani, G, Pilecki, B, Piranomonte, S, Quirrenbach, A, Redaelli, E M A, Pereira, C B, Randich, S, Rossi, S, Sanchez-Janssen, R, Schoeller, M, Seifert, W, Smiljanic, R, Snodgrass, C, Squalli, O, Stilz, I, Stuermer, J, Trost, A, Vanzella, E, Ventura, P, Verducci, O, Waring, C, Watson, S, Wells, M, Wright, D, Zafar, T, Zanutta, A, Zins, G
Format: Artikel
Sprache:eng
Schlagworte:
Astrophysics
Beryllium
Cubes
Deuterium
Extremely large telescopes
Galaxies
Heavy elements
Intergalactic media
Line spectra
Project development
Project management
Resolution
Stellar spectra
Ultraviolet radiation
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creator Covino, S
Cristiani, S
Alcala', J M
Alencar, S H P
Balashev, S A
Barbuy, B
Bastian, N
Battino, U
Bissell, L
Bristow, P
Calcines, A
Calderone, G
Cambianica, P
Carini, R
Carter, B
Cassisi, S
Castilho, B V
Cescutti, G
Christlieb, N
Cirami, R
Conzelmann, R
Coretti, I
Cooke, R
Cremonese, G
Cunha, K
Cupani, G
da Silva, A R
D'Auria, D
De Caprio, V
De Cia, A
Dekker, H
D'Elia, V
De Silva, G
Diaz, M
P Di Marcantonio
D'Odorico, V
Ernandes, H
Evans, C
Fitzsimmons, A
Franchini, M
Gaensicke, B
Genoni, M
Giribaldi, R E
Gneiding, C
Grazian, A
Hansen, C J
Hopgood, J
Kosmalski, J
La Forgia, F
La Penna, P
Landoni, M
Lazzarin, M
Lunney, D
Maciel, W
Marcolino, W
Marconi, M
Migliorini, A
Miller, C
Modigliani, A
Noterdaeme, P
Oggioni, L
Opitom, C
Pariani, G
Pilecki, B
Piranomonte, S
Quirrenbach, A
Redaelli, E M A
Pereira, C B
Randich, S
Rossi, S
Sanchez-Janssen, R
Schoeller, M
Seifert, W
Smiljanic, R
Snodgrass, C
Squalli, O
Stilz, I
Stuermer, J
Trost, A
Vanzella, E
Ventura, P
Verducci, O
Waring, C
Watson, S
Wells, M
Wright, D
Zafar, T
Zanutta, A
Zins, G
description In spite of the advent of extremely large telescopes in the UV/optical/NIR range, the current generation of 8-10m facilities is likely to remain competitive at ground-UV wavelengths for the foreseeable future. The Cassegrain U-Band Efficient Spectrograph (CUBES) has been designed to provide high-efficiency (>40%) observations in the near UV (305-400 nm requirement, 300-420 nm goal) at a spectral resolving power of R>20,000, although a lower-resolution, sky-limited mode of R ~ 7,000 is also planned. CUBES will offer new possibilities in many fields of astrophysics, providing access to key lines of stellar spectra: a tremendous diversity of iron-peak and heavy elements, lighter elements (in particular Beryllium) and light-element molecules (CO, CN, OH), as well as Balmer lines and the Balmer jump (particularly important for young stellar objects). The UV range is also critical in extragalactic studies: the circumgalactic medium of distant galaxies, the contribution of different types of sources to the cosmic UV background, the measurement of H2 and primordial Deuterium in a regime of relatively transparent intergalactic medium, and follow-up of explosive transients. The CUBES project completed a Phase A conceptual design in June 2021 and has now entered the Phase B dedicated to detailed design and construction. First science operations are planned for 2028. In this paper, we briefly describe the CUBES project development and goals, the main science cases, the instrument design and the project organization and management.
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The Cassegrain U-Band Efficient Spectrograph (CUBES) has been designed to provide high-efficiency (&gt;40%) observations in the near UV (305-400 nm requirement, 300-420 nm goal) at a spectral resolving power of R&gt;20,000, although a lower-resolution, sky-limited mode of R ~ 7,000 is also planned. CUBES will offer new possibilities in many fields of astrophysics, providing access to key lines of stellar spectra: a tremendous diversity of iron-peak and heavy elements, lighter elements (in particular Beryllium) and light-element molecules (CO, CN, OH), as well as Balmer lines and the Balmer jump (particularly important for young stellar objects). The UV range is also critical in extragalactic studies: the circumgalactic medium of distant galaxies, the contribution of different types of sources to the cosmic UV background, the measurement of H2 and primordial Deuterium in a regime of relatively transparent intergalactic medium, and follow-up of explosive transients. The CUBES project completed a Phase A conceptual design in June 2021 and has now entered the Phase B dedicated to detailed design and construction. First science operations are planned for 2028. In this paper, we briefly describe the CUBES project development and goals, the main science cases, the instrument design and the project organization and management.</description><identifier>EISSN: 2331-8422</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Astrophysics ; Beryllium ; Cubes ; Deuterium ; Extremely large telescopes ; Galaxies ; Heavy elements ; Intergalactic media ; Line spectra ; Project development ; Project management ; Resolution ; Stellar spectra ; Ultraviolet radiation</subject><ispartof>arXiv.org, 2022-12</ispartof><rights>2022. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). 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The Cassegrain U-Band Efficient Spectrograph (CUBES) has been designed to provide high-efficiency (&gt;40%) observations in the near UV (305-400 nm requirement, 300-420 nm goal) at a spectral resolving power of R&gt;20,000, although a lower-resolution, sky-limited mode of R ~ 7,000 is also planned. CUBES will offer new possibilities in many fields of astrophysics, providing access to key lines of stellar spectra: a tremendous diversity of iron-peak and heavy elements, lighter elements (in particular Beryllium) and light-element molecules (CO, CN, OH), as well as Balmer lines and the Balmer jump (particularly important for young stellar objects). The UV range is also critical in extragalactic studies: the circumgalactic medium of distant galaxies, the contribution of different types of sources to the cosmic UV background, the measurement of H2 and primordial Deuterium in a regime of relatively transparent intergalactic medium, and follow-up of explosive transients. The CUBES project completed a Phase A conceptual design in June 2021 and has now entered the Phase B dedicated to detailed design and construction. First science operations are planned for 2028. In this paper, we briefly describe the CUBES project development and goals, the main science cases, the instrument design and the project organization and management.</description><subject>Astrophysics</subject><subject>Beryllium</subject><subject>Cubes</subject><subject>Deuterium</subject><subject>Extremely large telescopes</subject><subject>Galaxies</subject><subject>Heavy elements</subject><subject>Intergalactic media</subject><subject>Line spectra</subject><subject>Project development</subject><subject>Project management</subject><subject>Resolution</subject><subject>Stellar spectra</subject><subject>Ultraviolet radiation</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><sourceid>BENPR</sourceid><recordid>eNpjYuA0MjY21LUwMTLiYOAtLs4yMDAwMjM3MjU15mRQdw51cg22UkhUCA1TKC5ITS4pyk8vSizIUEjLL1IoyUhVSCstKS1K5WFgTUvMKU7lhdLcDMpuriHOHroFRfmFpanFJfFZ-aVFeUCpeCNzUwsTUzMDC1Nj4lQBAOgSLr0</recordid><startdate>20221224</startdate><enddate>20221224</enddate><creator>Covino, S</creator><creator>Cristiani, S</creator><creator>Alcala', J M</creator><creator>Alencar, S H P</creator><creator>Balashev, S A</creator><creator>Barbuy, B</creator><creator>Bastian, N</creator><creator>Battino, U</creator><creator>Bissell, L</creator><creator>Bristow, P</creator><creator>Calcines, A</creator><creator>Calderone, G</creator><creator>Cambianica, P</creator><creator>Carini, R</creator><creator>Carter, B</creator><creator>Cassisi, S</creator><creator>Castilho, B V</creator><creator>Cescutti, G</creator><creator>Christlieb, N</creator><creator>Cirami, R</creator><creator>Conzelmann, R</creator><creator>Coretti, I</creator><creator>Cooke, R</creator><creator>Cremonese, G</creator><creator>Cunha, K</creator><creator>Cupani, G</creator><creator>da Silva, A R</creator><creator>D'Auria, D</creator><creator>De Caprio, V</creator><creator>De Cia, A</creator><creator>Dekker, H</creator><creator>D'Elia, V</creator><creator>De Silva, G</creator><creator>Diaz, M</creator><creator>P Di Marcantonio</creator><creator>D'Odorico, V</creator><creator>Ernandes, H</creator><creator>Evans, C</creator><creator>Fitzsimmons, A</creator><creator>Franchini, M</creator><creator>Gaensicke, B</creator><creator>Genoni, M</creator><creator>Giribaldi, R E</creator><creator>Gneiding, C</creator><creator>Grazian, A</creator><creator>Hansen, C J</creator><creator>Hopgood, J</creator><creator>Kosmalski, J</creator><creator>La Forgia, F</creator><creator>La Penna, P</creator><creator>Landoni, M</creator><creator>Lazzarin, M</creator><creator>Lunney, D</creator><creator>Maciel, W</creator><creator>Marcolino, W</creator><creator>Marconi, M</creator><creator>Migliorini, A</creator><creator>Miller, C</creator><creator>Modigliani, A</creator><creator>Noterdaeme, P</creator><creator>Oggioni, L</creator><creator>Opitom, C</creator><creator>Pariani, G</creator><creator>Pilecki, B</creator><creator>Piranomonte, S</creator><creator>Quirrenbach, A</creator><creator>Redaelli, E M A</creator><creator>Pereira, C B</creator><creator>Randich, S</creator><creator>Rossi, S</creator><creator>Sanchez-Janssen, R</creator><creator>Schoeller, M</creator><creator>Seifert, W</creator><creator>Smiljanic, R</creator><creator>Snodgrass, C</creator><creator>Squalli, O</creator><creator>Stilz, I</creator><creator>Stuermer, J</creator><creator>Trost, A</creator><creator>Vanzella, E</creator><creator>Ventura, P</creator><creator>Verducci, O</creator><creator>Waring, C</creator><creator>Watson, S</creator><creator>Wells, M</creator><creator>Wright, D</creator><creator>Zafar, T</creator><creator>Zanutta, A</creator><creator>Zins, G</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope></search><sort><creationdate>20221224</creationdate><title>CUBES: a UV spectrograph for the future</title><author>Covino, S ; Cristiani, S ; Alcala', J M ; Alencar, S H P ; Balashev, S A ; Barbuy, B ; Bastian, N ; Battino, U ; Bissell, L ; Bristow, P ; Calcines, A ; Calderone, G ; Cambianica, P ; Carini, R ; Carter, B ; Cassisi, S ; Castilho, B V ; Cescutti, G ; Christlieb, N ; Cirami, R ; Conzelmann, R ; Coretti, I ; Cooke, R ; Cremonese, G ; Cunha, K ; Cupani, G ; da Silva, A R ; D'Auria, D ; De Caprio, V ; De Cia, A ; Dekker, H ; D'Elia, V ; De Silva, G ; Diaz, M ; P Di Marcantonio ; D'Odorico, V ; Ernandes, H ; Evans, C ; Fitzsimmons, A ; Franchini, M ; Gaensicke, B ; Genoni, M ; Giribaldi, R E ; Gneiding, C ; Grazian, A ; Hansen, C J ; Hopgood, J ; Kosmalski, J ; La Forgia, F ; La Penna, P ; Landoni, M ; Lazzarin, M ; Lunney, D ; Maciel, W ; Marcolino, W ; Marconi, M ; Migliorini, A ; Miller, C ; Modigliani, A ; Noterdaeme, P ; Oggioni, L ; Opitom, C ; Pariani, G ; Pilecki, B ; Piranomonte, S ; Quirrenbach, A ; Redaelli, E M A ; Pereira, C B ; Randich, S ; Rossi, S ; Sanchez-Janssen, R ; Schoeller, M ; Seifert, W ; Smiljanic, R ; Snodgrass, C ; Squalli, O ; Stilz, I ; Stuermer, J ; Trost, A ; Vanzella, E ; Ventura, P ; Verducci, O ; Waring, C ; Watson, S ; Wells, M ; Wright, D ; Zafar, T ; Zanutta, A ; Zins, G</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-proquest_journals_27584560853</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2022</creationdate><topic>Astrophysics</topic><topic>Beryllium</topic><topic>Cubes</topic><topic>Deuterium</topic><topic>Extremely large telescopes</topic><topic>Galaxies</topic><topic>Heavy elements</topic><topic>Intergalactic media</topic><topic>Line spectra</topic><topic>Project development</topic><topic>Project management</topic><topic>Resolution</topic><topic>Stellar spectra</topic><topic>Ultraviolet radiation</topic><toplevel>online_resources</toplevel><creatorcontrib>Covino, S</creatorcontrib><creatorcontrib>Cristiani, S</creatorcontrib><creatorcontrib>Alcala', J M</creatorcontrib><creatorcontrib>Alencar, S H P</creatorcontrib><creatorcontrib>Balashev, S A</creatorcontrib><creatorcontrib>Barbuy, B</creatorcontrib><creatorcontrib>Bastian, N</creatorcontrib><creatorcontrib>Battino, U</creatorcontrib><creatorcontrib>Bissell, L</creatorcontrib><creatorcontrib>Bristow, P</creatorcontrib><creatorcontrib>Calcines, A</creatorcontrib><creatorcontrib>Calderone, G</creatorcontrib><creatorcontrib>Cambianica, P</creatorcontrib><creatorcontrib>Carini, R</creatorcontrib><creatorcontrib>Carter, B</creatorcontrib><creatorcontrib>Cassisi, S</creatorcontrib><creatorcontrib>Castilho, B V</creatorcontrib><creatorcontrib>Cescutti, G</creatorcontrib><creatorcontrib>Christlieb, N</creatorcontrib><creatorcontrib>Cirami, R</creatorcontrib><creatorcontrib>Conzelmann, R</creatorcontrib><creatorcontrib>Coretti, I</creatorcontrib><creatorcontrib>Cooke, R</creatorcontrib><creatorcontrib>Cremonese, G</creatorcontrib><creatorcontrib>Cunha, K</creatorcontrib><creatorcontrib>Cupani, G</creatorcontrib><creatorcontrib>da Silva, A R</creatorcontrib><creatorcontrib>D'Auria, D</creatorcontrib><creatorcontrib>De Caprio, V</creatorcontrib><creatorcontrib>De Cia, A</creatorcontrib><creatorcontrib>Dekker, H</creatorcontrib><creatorcontrib>D'Elia, V</creatorcontrib><creatorcontrib>De Silva, G</creatorcontrib><creatorcontrib>Diaz, M</creatorcontrib><creatorcontrib>P Di Marcantonio</creatorcontrib><creatorcontrib>D'Odorico, V</creatorcontrib><creatorcontrib>Ernandes, H</creatorcontrib><creatorcontrib>Evans, C</creatorcontrib><creatorcontrib>Fitzsimmons, A</creatorcontrib><creatorcontrib>Franchini, M</creatorcontrib><creatorcontrib>Gaensicke, B</creatorcontrib><creatorcontrib>Genoni, M</creatorcontrib><creatorcontrib>Giribaldi, R E</creatorcontrib><creatorcontrib>Gneiding, C</creatorcontrib><creatorcontrib>Grazian, A</creatorcontrib><creatorcontrib>Hansen, C J</creatorcontrib><creatorcontrib>Hopgood, J</creatorcontrib><creatorcontrib>Kosmalski, J</creatorcontrib><creatorcontrib>La Forgia, F</creatorcontrib><creatorcontrib>La Penna, P</creatorcontrib><creatorcontrib>Landoni, M</creatorcontrib><creatorcontrib>Lazzarin, M</creatorcontrib><creatorcontrib>Lunney, D</creatorcontrib><creatorcontrib>Maciel, W</creatorcontrib><creatorcontrib>Marcolino, W</creatorcontrib><creatorcontrib>Marconi, M</creatorcontrib><creatorcontrib>Migliorini, A</creatorcontrib><creatorcontrib>Miller, C</creatorcontrib><creatorcontrib>Modigliani, A</creatorcontrib><creatorcontrib>Noterdaeme, P</creatorcontrib><creatorcontrib>Oggioni, L</creatorcontrib><creatorcontrib>Opitom, C</creatorcontrib><creatorcontrib>Pariani, G</creatorcontrib><creatorcontrib>Pilecki, B</creatorcontrib><creatorcontrib>Piranomonte, S</creatorcontrib><creatorcontrib>Quirrenbach, A</creatorcontrib><creatorcontrib>Redaelli, E M A</creatorcontrib><creatorcontrib>Pereira, C B</creatorcontrib><creatorcontrib>Randich, S</creatorcontrib><creatorcontrib>Rossi, S</creatorcontrib><creatorcontrib>Sanchez-Janssen, R</creatorcontrib><creatorcontrib>Schoeller, M</creatorcontrib><creatorcontrib>Seifert, W</creatorcontrib><creatorcontrib>Smiljanic, R</creatorcontrib><creatorcontrib>Snodgrass, C</creatorcontrib><creatorcontrib>Squalli, O</creatorcontrib><creatorcontrib>Stilz, I</creatorcontrib><creatorcontrib>Stuermer, J</creatorcontrib><creatorcontrib>Trost, A</creatorcontrib><creatorcontrib>Vanzella, E</creatorcontrib><creatorcontrib>Ventura, P</creatorcontrib><creatorcontrib>Verducci, O</creatorcontrib><creatorcontrib>Waring, C</creatorcontrib><creatorcontrib>Watson, S</creatorcontrib><creatorcontrib>Wells, M</creatorcontrib><creatorcontrib>Wright, D</creatorcontrib><creatorcontrib>Zafar, T</creatorcontrib><creatorcontrib>Zanutta, A</creatorcontrib><creatorcontrib>Zins, G</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science &amp; Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Covino, S</au><au>Cristiani, S</au><au>Alcala', J M</au><au>Alencar, S H P</au><au>Balashev, S A</au><au>Barbuy, B</au><au>Bastian, N</au><au>Battino, U</au><au>Bissell, L</au><au>Bristow, P</au><au>Calcines, A</au><au>Calderone, G</au><au>Cambianica, P</au><au>Carini, R</au><au>Carter, B</au><au>Cassisi, S</au><au>Castilho, B V</au><au>Cescutti, G</au><au>Christlieb, N</au><au>Cirami, R</au><au>Conzelmann, R</au><au>Coretti, I</au><au>Cooke, R</au><au>Cremonese, G</au><au>Cunha, K</au><au>Cupani, G</au><au>da Silva, A R</au><au>D'Auria, D</au><au>De Caprio, V</au><au>De Cia, A</au><au>Dekker, H</au><au>D'Elia, V</au><au>De Silva, G</au><au>Diaz, M</au><au>P Di Marcantonio</au><au>D'Odorico, V</au><au>Ernandes, H</au><au>Evans, C</au><au>Fitzsimmons, A</au><au>Franchini, M</au><au>Gaensicke, B</au><au>Genoni, M</au><au>Giribaldi, R E</au><au>Gneiding, C</au><au>Grazian, A</au><au>Hansen, C J</au><au>Hopgood, J</au><au>Kosmalski, J</au><au>La Forgia, F</au><au>La Penna, P</au><au>Landoni, M</au><au>Lazzarin, M</au><au>Lunney, D</au><au>Maciel, W</au><au>Marcolino, W</au><au>Marconi, M</au><au>Migliorini, A</au><au>Miller, C</au><au>Modigliani, A</au><au>Noterdaeme, P</au><au>Oggioni, L</au><au>Opitom, C</au><au>Pariani, G</au><au>Pilecki, B</au><au>Piranomonte, S</au><au>Quirrenbach, A</au><au>Redaelli, E M A</au><au>Pereira, C B</au><au>Randich, S</au><au>Rossi, S</au><au>Sanchez-Janssen, R</au><au>Schoeller, M</au><au>Seifert, W</au><au>Smiljanic, R</au><au>Snodgrass, C</au><au>Squalli, O</au><au>Stilz, I</au><au>Stuermer, J</au><au>Trost, A</au><au>Vanzella, E</au><au>Ventura, P</au><au>Verducci, O</au><au>Waring, C</au><au>Watson, S</au><au>Wells, M</au><au>Wright, D</au><au>Zafar, T</au><au>Zanutta, A</au><au>Zins, G</au><format>book</format><genre>document</genre><ristype>GEN</ristype><atitle>CUBES: a UV spectrograph for the future</atitle><jtitle>arXiv.org</jtitle><date>2022-12-24</date><risdate>2022</risdate><eissn>2331-8422</eissn><abstract>In spite of the advent of extremely large telescopes in the UV/optical/NIR range, the current generation of 8-10m facilities is likely to remain competitive at ground-UV wavelengths for the foreseeable future. The Cassegrain U-Band Efficient Spectrograph (CUBES) has been designed to provide high-efficiency (&gt;40%) observations in the near UV (305-400 nm requirement, 300-420 nm goal) at a spectral resolving power of R&gt;20,000, although a lower-resolution, sky-limited mode of R ~ 7,000 is also planned. CUBES will offer new possibilities in many fields of astrophysics, providing access to key lines of stellar spectra: a tremendous diversity of iron-peak and heavy elements, lighter elements (in particular Beryllium) and light-element molecules (CO, CN, OH), as well as Balmer lines and the Balmer jump (particularly important for young stellar objects). The UV range is also critical in extragalactic studies: the circumgalactic medium of distant galaxies, the contribution of different types of sources to the cosmic UV background, the measurement of H2 and primordial Deuterium in a regime of relatively transparent intergalactic medium, and follow-up of explosive transients. The CUBES project completed a Phase A conceptual design in June 2021 and has now entered the Phase B dedicated to detailed design and construction. First science operations are planned for 2028. In this paper, we briefly describe the CUBES project development and goals, the main science cases, the instrument design and the project organization and management.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><oa>free_for_read</oa></addata></record>
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subjects Astrophysics
Beryllium
Cubes
Deuterium
Extremely large telescopes
Galaxies
Heavy elements
Intergalactic media
Line spectra
Project development
Project management
Resolution
Stellar spectra
Ultraviolet radiation
title CUBES: a UV spectrograph for the future
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