CUBES, the Cassegrain U-Band Efficient Spectrograph
In the era of Extremely Large Telescopes, the current generation of 8-10m facilities are 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 n...
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| creator | Cristiani, S Alcalá, J. M Alencar, S. H. P Balashev, S. A Bastian, N Barbuy, B Battino, U Calcines, A Calderone, G Cambianica, P Carini, R Carter, B Cassisi, S Castilho, B. V Cescutti, G Christlieb, N Cirami, R Coretti, I Cooke, R Covino, S Cremonese, G Cunha, K Cupani, G da Silva, A. R De Caprio, V De Cia, A Dekker, H D'Elia, V De Silva, G Diaz, M Di Marcantonio, P D'Auria, D D'Odorico, V Fitzsimmons, A Ernandes, H Evans, C Franchini, M Genoni, M Gänsicke, B Giribaldi, R. E Gneiding, C Grazian, A Hansen, C. J La Forgia, F Landoni, M Lazzarin, M Lunney, D Maciel, W Marcolino, W Marconi, M Migliorini, A Miller, C Noterdaeme, P Opitom, C Pariani, G Pilecki, B Piranomonte, S Quirrenbach, A Redaelli, E. M. A Pereira, C. B Randich, S Rossi, S Sanchez-Janssen, R Seifert, W Smiljanic, R Snodgrass, C Stilz, I Stürmer, J Vanzella, E Ventura, P Verducci, O Waring, C Watson, S Wells, M Wright, D Zafar, T Zanutta, A |
| description | In the era of Extremely Large Telescopes, the current generation of 8-10m
facilities are 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 (with a lower-resolution, sky-limited mode of R ~ 7,000). With the
design focusing on maximizing the instrument throughput (ensuring a Signal to
Noise Ratio (SNR) ~20 per high-resolution element at 313 nm for U ~18.5 mag
objects in 1h of observations), it 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 detailed design and construction phase. First
science operations are planned for 2028. |
| doi_str_mv | 10.48550/arxiv.2208.01672 |
| format | Article |
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facilities are 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 (with a lower-resolution, sky-limited mode of R ~ 7,000). With the
design focusing on maximizing the instrument throughput (ensuring a Signal to
Noise Ratio (SNR) ~20 per high-resolution element at 313 nm for U ~18.5 mag
objects in 1h of observations), it 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 detailed design and construction phase. First
science operations are planned for 2028.</description><identifier>DOI: 10.48550/arxiv.2208.01672</identifier><language>eng</language><subject>Physics - Instrumentation and Detectors ; Physics - Instrumentation and Methods for Astrophysics</subject><creationdate>2022-08</creationdate><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,776,881</link.rule.ids><linktorsrc>$$Uhttps://arxiv.org/abs/2208.01672$$EView_record_in_Cornell_University$$FView_record_in_$$GCornell_University$$Hfree_for_read</linktorsrc><backlink>$$Uhttps://doi.org/10.48550/arXiv.2208.01672$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Cristiani, S</creatorcontrib><creatorcontrib>Alcalá, J. M</creatorcontrib><creatorcontrib>Alencar, S. H. P</creatorcontrib><creatorcontrib>Balashev, S. A</creatorcontrib><creatorcontrib>Bastian, N</creatorcontrib><creatorcontrib>Barbuy, B</creatorcontrib><creatorcontrib>Battino, U</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>Coretti, I</creatorcontrib><creatorcontrib>Cooke, R</creatorcontrib><creatorcontrib>Covino, S</creatorcontrib><creatorcontrib>Cremonese, G</creatorcontrib><creatorcontrib>Cunha, K</creatorcontrib><creatorcontrib>Cupani, G</creatorcontrib><creatorcontrib>da Silva, A. R</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>Di Marcantonio, P</creatorcontrib><creatorcontrib>D'Auria, D</creatorcontrib><creatorcontrib>D'Odorico, V</creatorcontrib><creatorcontrib>Fitzsimmons, A</creatorcontrib><creatorcontrib>Ernandes, H</creatorcontrib><creatorcontrib>Evans, C</creatorcontrib><creatorcontrib>Franchini, M</creatorcontrib><creatorcontrib>Genoni, M</creatorcontrib><creatorcontrib>Gänsicke, B</creatorcontrib><creatorcontrib>Giribaldi, R. E</creatorcontrib><creatorcontrib>Gneiding, C</creatorcontrib><creatorcontrib>Grazian, A</creatorcontrib><creatorcontrib>Hansen, C. J</creatorcontrib><creatorcontrib>La Forgia, F</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>Noterdaeme, P</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>Seifert, W</creatorcontrib><creatorcontrib>Smiljanic, R</creatorcontrib><creatorcontrib>Snodgrass, C</creatorcontrib><creatorcontrib>Stilz, I</creatorcontrib><creatorcontrib>Stürmer, J</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><title>CUBES, the Cassegrain U-Band Efficient Spectrograph</title><description>In the era of Extremely Large Telescopes, the current generation of 8-10m
facilities are 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 (with a lower-resolution, sky-limited mode of R ~ 7,000). With the
design focusing on maximizing the instrument throughput (ensuring a Signal to
Noise Ratio (SNR) ~20 per high-resolution element at 313 nm for U ~18.5 mag
objects in 1h of observations), it 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 detailed design and construction phase. First
science operations are planned for 2028.</description><subject>Physics - Instrumentation and Detectors</subject><subject>Physics - Instrumentation and Methods for Astrophysics</subject><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><sourceid>GOX</sourceid><recordid>eNotzr1OwzAUhmEvDKhwAUz1BTTBv6kztlGgSJU6tJ2jY_scaomGyIkQ3D2lZfqGT3r1MPYkRWmcteIZ8nf6KpUSrhSyWqp7ppvjut0v-HRC3sA44nuG1PNjsYY-8pYohYT9xPcDhil_Xt7h9MDuCD5GfPzfGTu8tIdmU2x3r2_NalvAJV1QFT3JQEIERQGsXtY6uAqUV-iipbr2xjoBsYpUB6MjEUgC4yUa9B71jM1v2au6G3I6Q_7p_vTdVa9_AZy9P4c</recordid><startdate>20220802</startdate><enddate>20220802</enddate><creator>Cristiani, S</creator><creator>Alcalá, J. M</creator><creator>Alencar, S. H. P</creator><creator>Balashev, S. 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B</creatorcontrib><creatorcontrib>Randich, S</creatorcontrib><creatorcontrib>Rossi, S</creatorcontrib><creatorcontrib>Sanchez-Janssen, R</creatorcontrib><creatorcontrib>Seifert, W</creatorcontrib><creatorcontrib>Smiljanic, R</creatorcontrib><creatorcontrib>Snodgrass, C</creatorcontrib><creatorcontrib>Stilz, I</creatorcontrib><creatorcontrib>Stürmer, J</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><collection>arXiv.org</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Cristiani, S</au><au>Alcalá, J. M</au><au>Alencar, S. H. P</au><au>Balashev, S. A</au><au>Bastian, N</au><au>Barbuy, B</au><au>Battino, U</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>Coretti, I</au><au>Cooke, R</au><au>Covino, S</au><au>Cremonese, G</au><au>Cunha, K</au><au>Cupani, G</au><au>da Silva, A. R</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>Di Marcantonio, P</au><au>D'Auria, D</au><au>D'Odorico, V</au><au>Fitzsimmons, A</au><au>Ernandes, H</au><au>Evans, C</au><au>Franchini, M</au><au>Genoni, M</au><au>Gänsicke, B</au><au>Giribaldi, R. E</au><au>Gneiding, C</au><au>Grazian, A</au><au>Hansen, C. J</au><au>La Forgia, F</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>Noterdaeme, P</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>Seifert, W</au><au>Smiljanic, R</au><au>Snodgrass, C</au><au>Stilz, I</au><au>Stürmer, J</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><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>CUBES, the Cassegrain U-Band Efficient Spectrograph</atitle><date>2022-08-02</date><risdate>2022</risdate><abstract>In the era of Extremely Large Telescopes, the current generation of 8-10m
facilities are 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 (with a lower-resolution, sky-limited mode of R ~ 7,000). With the
design focusing on maximizing the instrument throughput (ensuring a Signal to
Noise Ratio (SNR) ~20 per high-resolution element at 313 nm for U ~18.5 mag
objects in 1h of observations), it 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 detailed design and construction phase. First
science operations are planned for 2028.</abstract><doi>10.48550/arxiv.2208.01672</doi><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext_linktorsrc |
| identifier | DOI: 10.48550/arxiv.2208.01672 |
| ispartof | |
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| language | eng |
| recordid | cdi_arxiv_primary_2208_01672 |
| source | arXiv.org |
| subjects | Physics - Instrumentation and Detectors Physics - Instrumentation and Methods for Astrophysics |
| title | CUBES, the Cassegrain U-Band Efficient Spectrograph |
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