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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.01672">arXiv:2208.01672</a> <span> [<a href="https://arxiv.org/pdf/2208.01672">pdf</a>, <a href="https://arxiv.org/format/2208.01672">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> CUBES, the Cassegrain U-Band Efficient Spectrograph </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/physics?searchtype=author&query=Alcal%C3%A1%2C+J+M">J. M. Alcal谩</a>, <a href="/search/physics?searchtype=author&query=Alencar%2C+S+H+P">S. H. P. Alencar</a>, <a href="/search/physics?searchtype=author&query=Balashev%2C+S+A">S. A. Balashev</a>, <a href="/search/physics?searchtype=author&query=Bastian%2C+N">N. Bastian</a>, <a href="/search/physics?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/physics?searchtype=author&query=Battino%2C+U">U. Battino</a>, <a href="/search/physics?searchtype=author&query=Calcines%2C+A">A. Calcines</a>, <a href="/search/physics?searchtype=author&query=Calderone%2C+G">G. Calderone</a>, <a href="/search/physics?searchtype=author&query=Cambianica%2C+P">P. Cambianica</a>, <a href="/search/physics?searchtype=author&query=Carini%2C+R">R. Carini</a>, <a href="/search/physics?searchtype=author&query=Carter%2C+B">B. Carter</a>, <a href="/search/physics?searchtype=author&query=Cassisi%2C+S">S. Cassisi</a>, <a href="/search/physics?searchtype=author&query=Castilho%2C+B+V">B. V. Castilho</a>, <a href="/search/physics?searchtype=author&query=Cescutti%2C+G">G. Cescutti</a>, <a href="/search/physics?searchtype=author&query=Christlieb%2C+N">N. Christlieb</a>, <a href="/search/physics?searchtype=author&query=Cirami%2C+R">R. Cirami</a>, <a href="/search/physics?searchtype=author&query=Coretti%2C+I">I. Coretti</a>, <a href="/search/physics?searchtype=author&query=Cooke%2C+R">R. Cooke</a>, <a href="/search/physics?searchtype=author&query=Covino%2C+S">S. Covino</a>, <a href="/search/physics?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/physics?searchtype=author&query=Cunha%2C+K">K. Cunha</a>, <a href="/search/physics?searchtype=author&query=Cupani%2C+G">G. Cupani</a>, <a href="/search/physics?searchtype=author&query=da+Silva%2C+A+R">A. R. da Silva</a>, <a href="/search/physics?searchtype=author&query=De+Caprio%2C+V">V. De Caprio</a> , et al. (52 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2208.01672v1-abstract-short" style="display: inline;"> 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 lowe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.01672v1-abstract-full').style.display = 'inline'; document.getElementById('2208.01672v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.01672v1-abstract-full" style="display: none;"> 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. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.01672v1-abstract-full').style.display = 'none'; document.getElementById('2208.01672v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">SPIE proceedings, SPIE Astronomical Telescopes + Instrumentation 2022, Montr茅al, Canada; 20 pages, 13 figures, 2 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.02205">arXiv:2102.02205</a> <span> [<a href="https://arxiv.org/pdf/2102.02205">pdf</a>, <a href="https://arxiv.org/format/2102.02205">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Atomic Physics">physics.atom-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.2562497">10.1117/12.2562497 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Stellar astrophysics in the near UV with VLT-CUBES </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Ernandes%2C+H">H. Ernandes</a>, <a href="/search/physics?searchtype=author&query=Evans%2C+C+J">C. J. Evans</a>, <a href="/search/physics?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/physics?searchtype=author&query=Castilho%2C+B">B. Castilho</a>, <a href="/search/physics?searchtype=author&query=Cescutti%2C+G">G. Cescutti</a>, <a href="/search/physics?searchtype=author&query=Christlieb%2C+N">N. Christlieb</a>, <a href="/search/physics?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/physics?searchtype=author&query=Cupani%2C+G">G. Cupani</a>, <a href="/search/physics?searchtype=author&query=Di+Marcantonio%2C+P">P. Di Marcantonio</a>, <a href="/search/physics?searchtype=author&query=Franchini%2C+M">M. Franchini</a>, <a href="/search/physics?searchtype=author&query=Hansen%2C+C">C. Hansen</a>, <a href="/search/physics?searchtype=author&query=Quirrenbach%2C+A">A. Quirrenbach</a>, <a href="/search/physics?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2102.02205v1-abstract-short" style="display: inline;"> Alongside future observations with the new European Extremely Large Telescope (ELT), optimised instruments on the 8-10m generation of telescopes will still be competitive at 'ground UV' wavelengths (3000-4000 A). The near UV provides a wealth of unique information on the nucleosynthesis of iron-peak elements, molecules, and neutron-capture elements. In the context of development of the near-UV CUB… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.02205v1-abstract-full').style.display = 'inline'; document.getElementById('2102.02205v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.02205v1-abstract-full" style="display: none;"> Alongside future observations with the new European Extremely Large Telescope (ELT), optimised instruments on the 8-10m generation of telescopes will still be competitive at 'ground UV' wavelengths (3000-4000 A). The near UV provides a wealth of unique information on the nucleosynthesis of iron-peak elements, molecules, and neutron-capture elements. In the context of development of the near-UV CUBES spectrograph for ESO's Very Large Telescope (VLT), we are investigating the impact of spectral resolution on the ability to estimate chemical abundances for beryllium and more than 30 iron-peak and heavy elements. From work ahead of the Phase A conceptual design of CUBES, here we present a comparison of the elements observable at the notional resolving power of CUBES (R~20,000) to those with VLT-UVES (R~40,000). For most of the considered lines signal-to-noise is a more critical factor than resolution. We summarise the elements accessible with CUBES, several of which (e.g. Be, Ge, Hf) are now the focus of quantitative simulations as part of the ongoing Phase A study. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.02205v1-abstract-full').style.display = 'none'; document.getElementById('2102.02205v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proceedings of the SPIE, Volume 11447, id. 1144760 11 pp. (2020) </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 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