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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/2412.03460">arXiv:2412.03460</a> <span> [<a href="https://arxiv.org/pdf/2412.03460">pdf</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> </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/10.1117/12.3018288">10.1117/12.3018288 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CUBES, the Cassegrain U-Band Efficient Spectrograph: towards final design review </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Genoni%2C+M">Matteo Genoni</a>, <a href="/search/astro-ph?searchtype=author&query=Dekker%2C+H">Hans Dekker</a>, <a href="/search/astro-ph?searchtype=author&query=Covino%2C+S">Stefano Covino</a>, <a href="/search/astro-ph?searchtype=author&query=Cirami%2C+R">Roberto Cirami</a>, <a href="/search/astro-ph?searchtype=author&query=Scalera%2C+M+A">Marcello Agostino Scalera</a>, <a href="/search/astro-ph?searchtype=author&query=Bissel%2C+L">Lawrence Bissel</a>, <a href="/search/astro-ph?searchtype=author&query=Seifert%2C+W">Walter Seifert</a>, <a href="/search/astro-ph?searchtype=author&query=Calcines%2C+A">Ariadna Calcines</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">Gerardo Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Stuermer%2C+J">Julian Stuermer</a>, <a href="/search/astro-ph?searchtype=author&query=Ritz%2C+C">Christopher Ritz</a>, <a href="/search/astro-ph?searchtype=author&query=Lunney%2C+D">David Lunney</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+C">Chris Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+S">Stephen Watson</a>, <a href="/search/astro-ph?searchtype=author&query=Waring%2C+C">Chris Waring</a>, <a href="/search/astro-ph?searchtype=author&query=Castilho%2C+B+V">Bruno Vaz Castilho</a>, <a href="/search/astro-ph?searchtype=author&query=De+Arruda%2C+M">Marcio De Arruda</a>, <a href="/search/astro-ph?searchtype=author&query=Verducci%2C+O">Orlando Verducci</a>, <a href="/search/astro-ph?searchtype=author&query=Coretti%2C+I">Igor Coretti</a>, <a href="/search/astro-ph?searchtype=author&query=Oggioni%2C+L">Luca Oggioni</a>, <a href="/search/astro-ph?searchtype=author&query=Pariani%2C+G">Giorgio Pariani</a>, <a href="/search/astro-ph?searchtype=author&query=Redaelli%2C+E+A+M">Edoardo Alberto Maria Redaelli</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ambrogio%2C+M">Matteo D'Ambrogio</a>, <a href="/search/astro-ph?searchtype=author&query=Calderone%2C+G">Giorgio Calderone</a>, <a href="/search/astro-ph?searchtype=author&query=Porru%2C+M">Matteo Porru</a> , et al. (17 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="2412.03460v1-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 instrumental efficiency ( $>$ 37\%) observations in the near UV (305-400 nm requirement, 300-420 nm goal) at a spectral resolving power of R… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.03460v1-abstract-full').style.display = 'inline'; document.getElementById('2412.03460v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.03460v1-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 instrumental efficiency ( $>$ 37\%) 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 $\sim$ 7, 000). With the design focusing on maximizing the instrument throughput (ensuring a Signal to Noise Ratio -SNR- $\sim$ 20 per spectral resolution element at 313 nm for U $\sim$ 17.5 mag objects in 1h of observations), it will offer new possibilities in many fields of astrophysics: i) access to key lines of stellar spectra (e.g. lighter elements, in particular Beryllium), extragalactic studies (e.g. circumgalactic medium of distant galaxies, cosmic UV background) and follow-up of explosive transients. We present the CUBES instrument design, currently in Phase-C and approaching the final design review, summarizing the hardware architecture and interfaces between the different subsystems as well as the relevant technical requirements. We describe the optical, mechanical, electrical design of the different subsystems (from the telescope adapter and support structure, through the main opto-mechanical path, including calibration unit, detector devices and cryostat control, main control electronics), detailing peculiar instrument functions like the Active Flexure Compensation (AFC). Furthermore, we outline the AITV concept and the main instrument operations giving an overview of its software ecosystem. Installation at the VLT is planned for 2028-2029 and first science operations in late 2029. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.03460v1-abstract-full').style.display = 'none'; document.getElementById('2412.03460v1-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> 4 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proceedings Volume 13096, Ground-based and Airborne Instrumentation for Astronomy X; 130967T (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.17542">arXiv:2407.17542</a> <span> [<a href="https://arxiv.org/pdf/2407.17542">pdf</a>, <a href="https://arxiv.org/format/2407.17542">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> </div> </div> <p class="title is-5 mathjax"> End-to-End simulation framework for astronomical spectrographs: SOXS, CUBES and ANDES </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Scaudo%2C+A">A. Scaudo</a>, <a href="/search/astro-ph?searchtype=author&query=Genoni%2C+M">M. Genoni</a>, <a href="/search/astro-ph?searchtype=author&query=Causi%2C+G+L">G. Li Causi</a>, <a href="/search/astro-ph?searchtype=author&query=Cabona%2C+L">L. Cabona</a>, <a href="/search/astro-ph?searchtype=author&query=Landoni%2C+M">M. Landoni</a>, <a href="/search/astro-ph?searchtype=author&query=Campana%2C+S">S. Campana</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">P. Schipani</a>, <a href="/search/astro-ph?searchtype=author&query=Claudi%2C+R">R. Claudi</a>, <a href="/search/astro-ph?searchtype=author&query=Aliverti%2C+M">M. Aliverti</a>, <a href="/search/astro-ph?searchtype=author&query=Baruffolo%2C+A">A. Baruffolo</a>, <a href="/search/astro-ph?searchtype=author&query=Ben-Ami%2C+S">S. Ben-Ami</a>, <a href="/search/astro-ph?searchtype=author&query=Biondi%2C+F">F. Biondi</a>, <a href="/search/astro-ph?searchtype=author&query=Capasso%2C+G">G. Capasso</a>, <a href="/search/astro-ph?searchtype=author&query=Cosentino%2C+R">R. Cosentino</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Alessio%2C+F">F. D'Alessio</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Avanzo%2C+P">P. D'Avanzo</a>, <a href="/search/astro-ph?searchtype=author&query=Hershko%2C+O">O. Hershko</a>, <a href="/search/astro-ph?searchtype=author&query=Kuncarayakti%2C+H">H. Kuncarayakti</a>, <a href="/search/astro-ph?searchtype=author&query=Munari%2C+M">M. Munari</a>, <a href="/search/astro-ph?searchtype=author&query=Santhakumari%2C+K+R">K. Radhakrishnan Santhakumari</a>, <a href="/search/astro-ph?searchtype=author&query=Pignata%2C+G">G. Pignata</a>, <a href="/search/astro-ph?searchtype=author&query=Rubin%2C+A">A. Rubin</a>, <a href="/search/astro-ph?searchtype=author&query=Scuderi%2C+S">S. Scuderi</a>, <a href="/search/astro-ph?searchtype=author&query=Vitali%2C+F">F. Vitali</a>, <a href="/search/astro-ph?searchtype=author&query=Young%2C+D">D. Young</a> , et al. (51 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="2407.17542v1-abstract-short" style="display: inline;"> We present our numerical simulation approach for the End-to-End (E2E) model applied to various astronomical spectrographs, such as SOXS (ESO-NTT), CUBES (ESO-VLT), and ANDES (ESO-ELT), covering multiple wavelength regions. The E2E model aim at simulating the expected astronomical observations starting from the radiation of the scientific sources (or calibration sources) up to the raw-frame data pr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.17542v1-abstract-full').style.display = 'inline'; document.getElementById('2407.17542v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.17542v1-abstract-full" style="display: none;"> We present our numerical simulation approach for the End-to-End (E2E) model applied to various astronomical spectrographs, such as SOXS (ESO-NTT), CUBES (ESO-VLT), and ANDES (ESO-ELT), covering multiple wavelength regions. The E2E model aim at simulating the expected astronomical observations starting from the radiation of the scientific sources (or calibration sources) up to the raw-frame data produced by the detectors. The comprehensive description includes E2E architecture, computational models, and tools for rendering the simulated frames. Collaboration with Data Reduction Software (DRS) teams is discussed, along with efforts to meet instrument requirements. The contribution to the cross-correlation algorithm for the Active Flexure Compensation (AFC) system of CUBES is detailed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.17542v1-abstract-full').style.display = 'none'; document.getElementById('2407.17542v1-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> 24 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </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">19 pages, 17 figures, SPIE Astronomical Telescopes + Instrumentation, Yokohama 2024. arXiv admin note: text overlap with arXiv:2209.07185, arXiv:2012.12684</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.14601">arXiv:2407.14601</a> <span> [<a href="https://arxiv.org/pdf/2407.14601">pdf</a>, <a href="https://arxiv.org/format/2407.14601">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> </div> </div> <p class="title is-5 mathjax"> ANDES, the high resolution spectrograph for the ELT: science goals, project overview and future developments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">A. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+M">M. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/astro-ph?searchtype=author&query=Alberti%2C+V">V. Alberti</a>, <a href="/search/astro-ph?searchtype=author&query=Albrecht%2C+S">S. Albrecht</a>, <a href="/search/astro-ph?searchtype=author&query=Alcaniz%2C+J">J. Alcaniz</a>, <a href="/search/astro-ph?searchtype=author&query=Aliverti%2C+M">M. Aliverti</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez%2C+J+D+A">J. D. Alvarado G贸mez</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+C+S">C. S. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Amado%2C+P+J">P. J. Amado</a>, <a href="/search/astro-ph?searchtype=author&query=Amate%2C+M">M. Amate</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+M+I">M. I. Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Antoniucci%2C+S">S. Antoniucci</a>, <a href="/search/astro-ph?searchtype=author&query=Artigau%2C+E">E. Artigau</a>, <a href="/search/astro-ph?searchtype=author&query=Bailet%2C+C">C. Bailet</a>, <a href="/search/astro-ph?searchtype=author&query=Baker%2C+C">C. Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+V">V. Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Balestra%2C+A">A. Balestra</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+S+A">S. A. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Baron%2C+F">F. Baron</a>, <a href="/search/astro-ph?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+S+M">S. M. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Beaulieu%2C+M">M. Beaulieu</a>, <a href="/search/astro-ph?searchtype=author&query=Bellido-Tirado%2C+O">O. Bellido-Tirado</a> , et al. (264 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="2407.14601v1-abstract-short" style="display: inline;"> The first generation of ELT instruments includes an optical-infrared high-resolution spectrograph, indicated as ELT-HIRES and recently christened ANDES (ArmazoNes high Dispersion Echelle Spectrograph). ANDES consists of three fibre-fed spectrographs ([U]BV, RIZ, YJH) providing a spectral resolution of $\sim$100,000 with a minimum simultaneous wavelength coverage of 0.4-1.8 $渭$m with the goal of ex… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.14601v1-abstract-full').style.display = 'inline'; document.getElementById('2407.14601v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.14601v1-abstract-full" style="display: none;"> The first generation of ELT instruments includes an optical-infrared high-resolution spectrograph, indicated as ELT-HIRES and recently christened ANDES (ArmazoNes high Dispersion Echelle Spectrograph). ANDES consists of three fibre-fed spectrographs ([U]BV, RIZ, YJH) providing a spectral resolution of $\sim$100,000 with a minimum simultaneous wavelength coverage of 0.4-1.8 $渭$m with the goal of extending it to 0.35-2.4 $渭$m with the addition of a U arm to the BV spectrograph and a separate K band spectrograph. It operates both in seeing- and diffraction-limited conditions and the fibre feeding allows several, interchangeable observing modes including a single conjugated adaptive optics module and a small diffraction-limited integral field unit in the NIR. Modularity and fibre-feeding allow ANDES to be placed partly on the ELT Nasmyth platform and partly in the Coud茅 room. ANDES has a wide range of groundbreaking science cases spanning nearly all areas of research in astrophysics and even fundamental physics. Among the top science cases, there are the detection of biosignatures from exoplanet atmospheres, finding the fingerprints of the first generation of stars, tests on the stability of Nature's fundamental couplings, and the direct detection of the cosmic acceleration. The ANDES project is carried forward by a large international consortium, composed of 35 Institutes from 13 countries, forming a team of almost 300 scientists and engineers which include the majority of the scientific and technical expertise in the field that can be found in ESO member states. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.14601v1-abstract-full').style.display = 'none'; document.getElementById('2407.14601v1-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> 19 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </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 astronomical telescope and instrumentation 2024, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.02979">arXiv:2407.02979</a> <span> [<a href="https://arxiv.org/pdf/2407.02979">pdf</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> </div> </div> <p class="title is-5 mathjax"> Progress on FORS-Up: the first instrument using ELT technologies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Boffin%2C+H+M+J">H. M. J. Boffin</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+V">V. Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Bertocco%2C+S">S. Bertocco</a>, <a href="/search/astro-ph?searchtype=author&query=Calderone%2C+G">G. Calderone</a>, <a href="/search/astro-ph?searchtype=author&query=Cirami%2C+R">R. Cirami</a>, <a href="/search/astro-ph?searchtype=author&query=Conzelmann%2C+R+D">R. D. Conzelmann</a>, <a href="/search/astro-ph?searchtype=author&query=Coretti%2C+I">I. Coretti</a>, <a href="/search/astro-ph?searchtype=author&query=Cumani%2C+C">C. Cumani</a>, <a href="/search/astro-ph?searchtype=author&query=Del+Valle%2C+D">D. Del Valle</a>, <a href="/search/astro-ph?searchtype=author&query=Derie%2C+F">F. Derie</a>, <a href="/search/astro-ph?searchtype=author&query=Rodr%C3%ADguez%2C+P+A+F">P. A. Fuerte Rodr铆guez</a>, <a href="/search/astro-ph?searchtype=author&query=Cheetham%2C+P+G">P. Gutierrez Cheetham</a>, <a href="/search/astro-ph?searchtype=author&query=Kosmalski%2C+J">J. Kosmalski</a>, <a href="/search/astro-ph?searchtype=author&query=Manescau%2C+A+R">A. R. Manescau</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Marcantonio%2C+P">P. Di Marcantonio</a>, <a href="/search/astro-ph?searchtype=author&query=Modigliani%2C+A">A. Modigliani</a>, <a href="/search/astro-ph?searchtype=author&query=Moehler%2C+S">S. Moehler</a>, <a href="/search/astro-ph?searchtype=author&query=Moins%2C+C">C. Moins</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+D">D. Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=Porru%2C+M">M. Porru</a>, <a href="/search/astro-ph?searchtype=author&query=Reyes%2C+J">J. Reyes</a>, <a href="/search/astro-ph?searchtype=author&query=Siebenmorgen%2C+R">R. Siebenmorgen</a>, <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">V. Strazzullo</a>, <a href="/search/astro-ph?searchtype=author&query=Sulich%2C+A">A. Sulich</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="2407.02979v1-abstract-short" style="display: inline;"> ESO is in the process of upgrading one of the two FORS (FOcal Reducer/low dispersion Spectrograph) instruments - a multi-mode (imaging, polarimetry, long-slit, and multi-object spectroscopy) optical instrument mounted on the Cassegrain focus of Unit Telescope 1 of ESO's Very Large Telescope. FORS1 was moved from Chile to Trieste, and is undergoing complete refurbishment, including the exchange of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.02979v1-abstract-full').style.display = 'inline'; document.getElementById('2407.02979v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.02979v1-abstract-full" style="display: none;"> ESO is in the process of upgrading one of the two FORS (FOcal Reducer/low dispersion Spectrograph) instruments - a multi-mode (imaging, polarimetry, long-slit, and multi-object spectroscopy) optical instrument mounted on the Cassegrain focus of Unit Telescope 1 of ESO's Very Large Telescope. FORS1 was moved from Chile to Trieste, and is undergoing complete refurbishment, including the exchange of all motorised parts. In addition, new software is developed, based on the Extremely Large Telescope Instrument Control Software Framework, as the upgraded FORS1 will be the first instrument in operations to use this framework. The new Teledyne e2V CCD has now been procured and is undergoing testing with the New Generation Controller at ESO. In addition, a new set of grisms have been developed, and a new set of filters will be purchased. A new internal calibration unit has been designed, making the operations more efficient. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.02979v1-abstract-full').style.display = 'none'; document.getElementById('2407.02979v1-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> 3 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </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">This paper is dedicated to the memory of our former colleague, Mario Nonino, who passed away prematurely. Proceedings for the SPIE Astronomical Telescopes and Instrumentation 2024</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.12791">arXiv:2212.12791</a> <span> [<a href="https://arxiv.org/pdf/2212.12791">pdf</a>, <a href="https://arxiv.org/format/2212.12791">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> </div> </div> <p class="title is-5 mathjax"> CUBES: a UV spectrograph for the future </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Covino%2C+S">S. Covino</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Alcala%27%2C+J+M">J. M. Alcala'</a>, <a href="/search/astro-ph?searchtype=author&query=Alencar%2C+S+H+P">S. H. P. Alencar</a>, <a href="/search/astro-ph?searchtype=author&query=Balashev%2C+S+A">S. A. Balashev</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+N">N. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=Battino%2C+U">U. Battino</a>, <a href="/search/astro-ph?searchtype=author&query=Bissell%2C+L">L. Bissell</a>, <a href="/search/astro-ph?searchtype=author&query=Bristow%2C+P">P. Bristow</a>, <a href="/search/astro-ph?searchtype=author&query=Calcines%2C+A">A. Calcines</a>, <a href="/search/astro-ph?searchtype=author&query=Calderone%2C+G">G. Calderone</a>, <a href="/search/astro-ph?searchtype=author&query=Cambianica%2C+P">P. Cambianica</a>, <a href="/search/astro-ph?searchtype=author&query=Carini%2C+R">R. Carini</a>, <a href="/search/astro-ph?searchtype=author&query=Carter%2C+B">B. Carter</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</a>, <a href="/search/astro-ph?searchtype=author&query=Castilho%2C+B+V">B. V. Castilho</a>, <a href="/search/astro-ph?searchtype=author&query=Cescutti%2C+G">G. Cescutti</a>, <a href="/search/astro-ph?searchtype=author&query=Christlieb%2C+N">N. Christlieb</a>, <a href="/search/astro-ph?searchtype=author&query=Cirami%2C+R">R. Cirami</a>, <a href="/search/astro-ph?searchtype=author&query=Conzelmann%2C+R">R. Conzelmann</a>, <a href="/search/astro-ph?searchtype=author&query=Coretti%2C+I">I. Coretti</a>, <a href="/search/astro-ph?searchtype=author&query=Cooke%2C+R">R. Cooke</a>, <a href="/search/astro-ph?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">K. Cunha</a> , et al. (64 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="2212.12791v1-abstract-short" style="display: inline;"> 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 r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.12791v1-abstract-full').style.display = 'inline'; document.getElementById('2212.12791v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.12791v1-abstract-full" style="display: none;"> 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. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.12791v1-abstract-full').style.display = 'none'; document.getElementById('2212.12791v1-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> 24 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">Proceedings for the HACK100 conference, Trieste, June 2022. arXiv admin note: substantial text overlap with arXiv:2208.01672</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.07294">arXiv:2209.07294</a> <span> [<a href="https://arxiv.org/pdf/2209.07294">pdf</a>, <a href="https://arxiv.org/format/2209.07294">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> </div> </div> <p class="title is-5 mathjax"> CUBES and its software ecosystem: instrument simulation, control, and data processing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Calderone%2C+G">Giorgio Calderone</a>, <a href="/search/astro-ph?searchtype=author&query=Cirami%2C+R">Roberto Cirami</a>, <a href="/search/astro-ph?searchtype=author&query=Cupani%2C+G">Guido Cupani</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Marcantonio%2C+P">Paolo Di Marcantonio</a>, <a href="/search/astro-ph?searchtype=author&query=Franchini%2C+M">Mariagrazia Franchini</a>, <a href="/search/astro-ph?searchtype=author&query=Genoni%2C+M">Matteo Genoni</a>, <a href="/search/astro-ph?searchtype=author&query=Kaluszy%C5%84ski%2C+M">Mikolaj Kaluszy艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Landoni%2C+M">Marco Landoni</a>, <a href="/search/astro-ph?searchtype=author&query=Rothmaier%2C+F">Florian Rothmaier</a>, <a href="/search/astro-ph?searchtype=author&query=Scaudo%2C+A">Andrea Scaudo</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">Rodolfo Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Stilz%2C+I">Ingo Stilz</a>, <a href="/search/astro-ph?searchtype=author&query=St%C3%BCrmer%2C+J">Julian St眉rmer</a>, <a href="/search/astro-ph?searchtype=author&query=Verducci%2C+O">Orlando Verducci</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="2209.07294v1-abstract-short" style="display: inline;"> CUBES (Cassegrain U-Band Efficient Spectrograph) is the recently approved high-efficiency VLT spectrograph aimed to observe the sky in the UV ground-based region (305-400 nm) with a high-resolution mode (~20K) and a low-resolution mode (~5K). In this paper we will briefly describe the requirements and the design of the several software packages involved in the project, namely the instrument contro… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.07294v1-abstract-full').style.display = 'inline'; document.getElementById('2209.07294v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.07294v1-abstract-full" style="display: none;"> CUBES (Cassegrain U-Band Efficient Spectrograph) is the recently approved high-efficiency VLT spectrograph aimed to observe the sky in the UV ground-based region (305-400 nm) with a high-resolution mode (~20K) and a low-resolution mode (~5K). In this paper we will briefly describe the requirements and the design of the several software packages involved in the project, namely the instrument control software, the exposure time calculator, the end-to-end simulator, and the data reduction software suite. We will discuss how the above mentioned blocks cooperate to build up a "software ecosystem" for the CUBES instrument, and to support the users from the proposal preparation to the science-grade data products. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.07294v1-abstract-full').style.display = 'none'; document.getElementById('2209.07294v1-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> 15 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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</span> </p> </li> <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/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Alcal%C3%A1%2C+J+M">J. M. Alcal谩</a>, <a href="/search/astro-ph?searchtype=author&query=Alencar%2C+S+H+P">S. H. P. Alencar</a>, <a href="/search/astro-ph?searchtype=author&query=Balashev%2C+S+A">S. A. Balashev</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+N">N. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Battino%2C+U">U. Battino</a>, <a href="/search/astro-ph?searchtype=author&query=Calcines%2C+A">A. Calcines</a>, <a href="/search/astro-ph?searchtype=author&query=Calderone%2C+G">G. Calderone</a>, <a href="/search/astro-ph?searchtype=author&query=Cambianica%2C+P">P. Cambianica</a>, <a href="/search/astro-ph?searchtype=author&query=Carini%2C+R">R. Carini</a>, <a href="/search/astro-ph?searchtype=author&query=Carter%2C+B">B. Carter</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</a>, <a href="/search/astro-ph?searchtype=author&query=Castilho%2C+B+V">B. V. Castilho</a>, <a href="/search/astro-ph?searchtype=author&query=Cescutti%2C+G">G. Cescutti</a>, <a href="/search/astro-ph?searchtype=author&query=Christlieb%2C+N">N. Christlieb</a>, <a href="/search/astro-ph?searchtype=author&query=Cirami%2C+R">R. Cirami</a>, <a href="/search/astro-ph?searchtype=author&query=Coretti%2C+I">I. Coretti</a>, <a href="/search/astro-ph?searchtype=author&query=Cooke%2C+R">R. Cooke</a>, <a href="/search/astro-ph?searchtype=author&query=Covino%2C+S">S. Covino</a>, <a href="/search/astro-ph?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">K. Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Cupani%2C+G">G. Cupani</a>, <a href="/search/astro-ph?searchtype=author&query=da+Silva%2C+A+R">A. R. da Silva</a>, <a href="/search/astro-ph?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/2203.15477">arXiv:2203.15477</a> <span> [<a href="https://arxiv.org/pdf/2203.15477">pdf</a>, <a href="https://arxiv.org/format/2203.15477">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> </div> </div> <p class="title is-5 mathjax"> The CUBES Instrument Model and Simulation Tools. Their role in the project Phase A study </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Genoni%2C+M">Matteo Genoni</a>, <a href="/search/astro-ph?searchtype=author&query=Landoni%2C+M">Marco Landoni</a>, <a href="/search/astro-ph?searchtype=author&query=Cupani%2C+G">Guido Cupani</a>, <a href="/search/astro-ph?searchtype=author&query=Franchini%2C+M">Mariagrazia Franchini</a>, <a href="/search/astro-ph?searchtype=author&query=Cirami%2C+R">Roberto Cirami</a>, <a href="/search/astro-ph?searchtype=author&query=Zanutta%2C+A">Alessio Zanutta</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+C">Chris Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Marcantonio%2C+P">Paolo Di Marcantonio</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">Stefano Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Trost%2C+A">Andrea Trost</a>, <a href="/search/astro-ph?searchtype=author&query=Zorba%2C+S">Sonia Zorba</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="2203.15477v1-abstract-short" style="display: inline;"> We present the simulation tools developed to aid the design phase of the Cassegrain U-Band Efficient Spectrograph (CUBES) for the Very Large Telescope (VLT), exploring aspects of the system design and evaluating the performance for different design configurations. CUBES aims to be the 'ultimate' ultraviolet (UV) instrument at the European Southern Observatory (ESO) in terms of throughput, with the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.15477v1-abstract-full').style.display = 'inline'; document.getElementById('2203.15477v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.15477v1-abstract-full" style="display: none;"> We present the simulation tools developed to aid the design phase of the Cassegrain U-Band Efficient Spectrograph (CUBES) for the Very Large Telescope (VLT), exploring aspects of the system design and evaluating the performance for different design configurations. CUBES aims to be the 'ultimate' ultraviolet (UV) instrument at the European Southern Observatory (ESO) in terms of throughput, with the goal to cover the bluest part of the spectrum accessible from the ground (300 nm to 400 nm) with the highest possible efficiency. Here we introduce the End-to-End (E2E) and the Exposure Time Calculator (ETC) tools. The E2E simulator has been developed with different versions to meet the needs of different users, including a version that can be accessed for use by the broader scientific community using a Jupyter notebook. The E2E tool was used by the system team to help define the Phase A baseline design of the instrument, as well as in scientific evaluation of a possible low-resolution mode. The ETC is a web-based tool through which the science community are able to test a range of science cases for CUBES, demonstrating its potential to push the limiting magnitude for the detection of specific UV-features, such as abundance estimates of beryllium in main sequence stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.15477v1-abstract-full').style.display = 'none'; document.getElementById('2203.15477v1-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> 29 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">Accepted for publication in Experimental Astronomy</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.15352">arXiv:2203.15352</a> <span> [<a href="https://arxiv.org/pdf/2203.15352">pdf</a>, <a href="https://arxiv.org/format/2203.15352">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> </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/10.1007/s10686-022-09837-w">10.1007/s10686-022-09837-w <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CUBES Phase A design overview -- The Cassegrain U-Band Efficient Spectrograph for the Very Large Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zanutta%2C+A">Alessio Zanutta</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">Stefano Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Atkinson%2C+D">David Atkinson</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+V">Veronica Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Balestra%2C+A">Andrea Balestra</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">Beatriz Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Macanhan%2C+V+B+P">Vanessa Bawden P. Macanhan</a>, <a href="/search/astro-ph?searchtype=author&query=Calcines%2C+A">Ariadna Calcines</a>, <a href="/search/astro-ph?searchtype=author&query=Calderone%2C+G">Giorgio Calderone</a>, <a href="/search/astro-ph?searchtype=author&query=Case%2C+S">Scott Case</a>, <a href="/search/astro-ph?searchtype=author&query=Castilho%2C+B+V">Bruno V. Castilho</a>, <a href="/search/astro-ph?searchtype=author&query=Cescutti%2C+G">Gabriele Cescutti</a>, <a href="/search/astro-ph?searchtype=author&query=Cirami%2C+R">Roberto Cirami</a>, <a href="/search/astro-ph?searchtype=author&query=Coretti%2C+I">Igor Coretti</a>, <a href="/search/astro-ph?searchtype=author&query=Covino%2C+S">Stefano Covino</a>, <a href="/search/astro-ph?searchtype=author&query=Cupani%2C+G">Guido Cupani</a>, <a href="/search/astro-ph?searchtype=author&query=De+Caprio%2C+V">Vincenzo De Caprio</a>, <a href="/search/astro-ph?searchtype=author&query=Dekker%2C+H">Hans Dekker</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Marcantonio%2C+P">Paolo Di Marcantonio</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Odorico%2C+V">Valentina D'Odorico</a>, <a href="/search/astro-ph?searchtype=author&query=Ernandes%2C+H">Heitor Ernandes</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+C">Chris Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Feger%2C+T">Tobias Feger</a>, <a href="/search/astro-ph?searchtype=author&query=Feiz%2C+C">Carmen Feiz</a>, <a href="/search/astro-ph?searchtype=author&query=Franchini%2C+M">Mariagrazia Franchini</a> , et al. (29 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="2203.15352v1-abstract-short" style="display: inline;"> We present the baseline conceptual design of the Cassegrain U-Band Efficient Spectrograph (CUBES) for the Very Large Telescope. CUBES will provide unprecedented sensitivity for spectroscopy on a 8 - 10 m class telescope in the ground ultraviolet (UV), spanning a bandwidth of > 100 nm that starts at 300 nm, the shortest wavelength accessible from the ground. The design has been optimized for end-to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.15352v1-abstract-full').style.display = 'inline'; document.getElementById('2203.15352v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.15352v1-abstract-full" style="display: none;"> We present the baseline conceptual design of the Cassegrain U-Band Efficient Spectrograph (CUBES) for the Very Large Telescope. CUBES will provide unprecedented sensitivity for spectroscopy on a 8 - 10 m class telescope in the ground ultraviolet (UV), spanning a bandwidth of > 100 nm that starts at 300 nm, the shortest wavelength accessible from the ground. The design has been optimized for end-to-end efficiency and provides a spectral resolving power of R > 20000, that will unlock a broad range of new topics across solar system, Galactic and extraglactic astronomy. The design also features a second, lower-resolution (R \sim 7000) mode and has the option of a fiberlink to the UVES instrument for simultaneous observations at longer wavelengths. Here we present the optical, mechanical and software design of the various subsystems of the instrument after the Phase A study of the project. We discuss the expected performances for the layout choices and highlight some of the performance trade-offs considered to best meet the instrument top-level requirements. We also introduce the model-based system engineering approach used to organize and manage the project activities and interfaces, in the context that it is increasingly necessary to integrate such tools in the development of complex astronomical projects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.15352v1-abstract-full').style.display = 'none'; document.getElementById('2203.15352v1-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> 29 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">Accepted for publication in Experimental Astronomy</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.09227">arXiv:2012.09227</a> <span> [<a href="https://arxiv.org/pdf/2012.09227">pdf</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> </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/10.1117/12.2562244">10.1117/12.2562244 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> FORS-Up: Making the most versatile instrument in Paranal ready for 15 more years of operations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Boffin%2C+H+M+J">H. M. J. Boffin</a>, <a href="/search/astro-ph?searchtype=author&query=Derie%2C+F">F. Derie</a>, <a href="/search/astro-ph?searchtype=author&query=Manescau%2C+A">A. Manescau</a>, <a href="/search/astro-ph?searchtype=author&query=Siebenmorgen%2C+R">R. Siebenmorgen</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+V">V. Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Calderone%2C+G">G. Calderone</a>, <a href="/search/astro-ph?searchtype=author&query=Cirami%2C+R">R. Cirami</a>, <a href="/search/astro-ph?searchtype=author&query=Coretti%2C+I">I. Coretti</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Marcantonio%2C+P">P. Di Marcantonio</a>, <a href="/search/astro-ph?searchtype=author&query=Kolsmanski%2C+J">J. Kolsmanski</a>, <a href="/search/astro-ph?searchtype=author&query=Lilley%2C+P">P. Lilley</a>, <a href="/search/astro-ph?searchtype=author&query=Moehler%2C+S">S. Moehler</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Rupprecht%2C+G">G. Rupprecht</a>, <a href="/search/astro-ph?searchtype=author&query=Silber%2C+A">A. Silber</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="2012.09227v2-abstract-short" style="display: inline;"> The FORS Upgrade project (FORS-Up) aims at bringing a new life to the highly demanded workhorse instrument attached to ESO's Very Large Telescope (VLT). FORS2 is a multimode optical instrument, which started regular science operations in 2000 and since then, together with its twin, FORS1, has been one of the most demanded and most productive instruments of the VLT. In order to ensure that a FORS s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.09227v2-abstract-full').style.display = 'inline'; document.getElementById('2012.09227v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.09227v2-abstract-full" style="display: none;"> The FORS Upgrade project (FORS-Up) aims at bringing a new life to the highly demanded workhorse instrument attached to ESO's Very Large Telescope (VLT). FORS2 is a multimode optical instrument, which started regular science operations in 2000 and since then, together with its twin, FORS1, has been one of the most demanded and most productive instruments of the VLT. In order to ensure that a FORS shall remain operational for at least another 15 years, an upgrade has been planned. This is required as FORS2 is using technology and software that is now obsolete and cannot be put and maintained to the standards in use at the Observatory. The project - carried out as a collaboration between ESO and INAF-Astronomical Observatory of Trieste - aims at bringing to the telescope in 2023/2024 a refurbished instrument with a new scientific detector, an upgrade of the instrument control software and electronics, a new calibration unit, as well as additional filters and grisms. The new FORS will also serve as a test bench for the Extremely Large Telescope (ELT) standard technologies (among them the use of programmable logic controllers and of the features of the ELT Control Software). The project aims at minimising the downtime of the instrument by performing the upgrade on the currently decommissioned instrument FORS1 and retrofitting the Mask Exchange Unit and polarisation optics from FORS2 to FORS1. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.09227v2-abstract-full').style.display = 'none'; document.getElementById('2012.09227v2-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> 14 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </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">Author version of a paper presented at SPIE Ground-based and Airborne Instrumentation for Astronomy VIII; corrected one statement</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proc. SPIE 11447, Ground-based and Airborne Instrumentation for Astronomy VIII, 114477A (13 December 2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.13963">arXiv:2011.13963</a> <span> [<a href="https://arxiv.org/pdf/2011.13963">pdf</a>, <a href="https://arxiv.org/format/2011.13963">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</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/10.1051/0004-6361/202039345">10.1051/0004-6361/202039345 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Fundamental physics with Espresso: Towards an accurate wavelength calibration for a precision test of the fine-structure constant </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Schmidt%2C+T+M">Tobias M. Schmidt</a>, <a href="/search/astro-ph?searchtype=author&query=Molaro%2C+P">Paolo Molaro</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+M+T">Michael T. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Lovis%2C+C">Christophe Lovis</a>, <a href="/search/astro-ph?searchtype=author&query=Cupani%2C+G">Guido Cupani</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">Stefano Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Pepe%2C+F+A">Francesco A. Pepe</a>, <a href="/search/astro-ph?searchtype=author&query=Rebolo%2C+R">Rafael Rebolo</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+N+C">Nuno C. Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+M">Manuel Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Adibekyan%2C+V">Vardan Adibekyan</a>, <a href="/search/astro-ph?searchtype=author&query=Alibert%2C+Y">Yann Alibert</a>, <a href="/search/astro-ph?searchtype=author&query=Aliverti%2C+M">Matteo Aliverti</a>, <a href="/search/astro-ph?searchtype=author&query=Allart%2C+R">Romain Allart</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">Carlos Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+D">David Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+V">Veronica Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Broeg%2C+C">Christopher Broeg</a>, <a href="/search/astro-ph?searchtype=author&query=Cabral%2C+A">Alexandre Cabral</a>, <a href="/search/astro-ph?searchtype=author&query=Calderone%2C+G">Giorgio Calderone</a>, <a href="/search/astro-ph?searchtype=author&query=Cirami%2C+R">Roberto Cirami</a>, <a href="/search/astro-ph?searchtype=author&query=Coelho%2C+J">Jo茫o Coelho</a>, <a href="/search/astro-ph?searchtype=author&query=Coretti%2C+I">Igor Coretti</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Odorico%2C+V">Valentina D'Odorico</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Marcantonio%2C+P">Paolo Di Marcantonio</a> , et al. (34 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="2011.13963v1-abstract-short" style="display: inline;"> Observations of metal absorption systems in the spectra of distant quasars allow to constrain a possible variation of the fine-structure constant throughout the history of the Universe. Such a test poses utmost demands on the wavelength accuracy and previous studies were limited by systematics in the spectrograph wavelength calibration. A substantial advance in the field is therefore expected from… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.13963v1-abstract-full').style.display = 'inline'; document.getElementById('2011.13963v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.13963v1-abstract-full" style="display: none;"> Observations of metal absorption systems in the spectra of distant quasars allow to constrain a possible variation of the fine-structure constant throughout the history of the Universe. Such a test poses utmost demands on the wavelength accuracy and previous studies were limited by systematics in the spectrograph wavelength calibration. A substantial advance in the field is therefore expected from the new ultra-stable high-resolution spectrograph Espresso, recently installed at the VLT. In preparation of the fundamental physics related part of the Espresso GTO program, we present a thorough assessment of the Espresso wavelength accuracy and identify possible systematics at each of the different steps involved in the wavelength calibration process. Most importantly, we compare the default wavelength solution, based on the combination of Thorium-Argon arc lamp spectra and a Fabry-P茅rot interferometer, to the fully independent calibration obtained from a laser frequency comb. We find wavelength-dependent discrepancies of up to 24m/s. This substantially exceeds the photon noise and highlights the presence of different sources of systematics, which we characterize in detail as part of this study. Nevertheless, our study demonstrates the outstanding accuracy of Espresso with respect to previously used spectrographs and we show that constraints of a relative change of the fine-structure constant at the $10^{-6}$ level can be obtained with Espresso without being limited by wavelength calibration systematics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.13963v1-abstract-full').style.display = 'none'; document.getElementById('2011.13963v1-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> 27 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </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">27 pages, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 646, A144 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.12317">arXiv:2011.12317</a> <span> [<a href="https://arxiv.org/pdf/2011.12317">pdf</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> </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/10.18727/0722-6691/5219">10.18727/0722-6691/5219 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HIRES, the high-resolution spectrograph for the ELT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">Alessandro Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+M">Manuel Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Adibekyan%2C+V">Vardan Adibekyan</a>, <a href="/search/astro-ph?searchtype=author&query=Aliverti%2C+M">Matteo Aliverti</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">Carlos Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Amado%2C+P+J">Pedro J. Amado</a>, <a href="/search/astro-ph?searchtype=author&query=Amate%2C+M">Manuel Amate</a>, <a href="/search/astro-ph?searchtype=author&query=Artigau%2C+E">Etienne Artigau</a>, <a href="/search/astro-ph?searchtype=author&query=Augusto%2C+S+R">Sergio R. Augusto</a>, <a href="/search/astro-ph?searchtype=author&query=Barros%2C+S">Susana Barros</a>, <a href="/search/astro-ph?searchtype=author&query=Becerril%2C+S">Santiago Becerril</a>, <a href="/search/astro-ph?searchtype=author&query=Benneke%2C+B">Bjorn Benneke</a>, <a href="/search/astro-ph?searchtype=author&query=Bergin%2C+E">Edwin Bergin</a>, <a href="/search/astro-ph?searchtype=author&query=Berio%2C+P">Philippe Berio</a>, <a href="/search/astro-ph?searchtype=author&query=Bezawada%2C+N">Naidu Bezawada</a>, <a href="/search/astro-ph?searchtype=author&query=Boisse%2C+I">Isabelle Boisse</a>, <a href="/search/astro-ph?searchtype=author&query=Bonfils%2C+X">Xavier Bonfils</a>, <a href="/search/astro-ph?searchtype=author&query=Bouchy%2C+F">Francois Bouchy</a>, <a href="/search/astro-ph?searchtype=author&query=Broeg%2C+C">Christopher Broeg</a>, <a href="/search/astro-ph?searchtype=author&query=Cabral%2C+A">Alexandre Cabral</a>, <a href="/search/astro-ph?searchtype=author&query=Calvo-Ortega%2C+R">Rocio Calvo-Ortega</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+B+L+C">Bruno Leonardo Canto Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Chazelas%2C+B">Bruno Chazelas</a>, <a href="/search/astro-ph?searchtype=author&query=Chiavassa%2C+A">Andrea Chiavassa</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen%2C+L+B">Lise B. Christensen</a> , et al. (77 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="2011.12317v1-abstract-short" style="display: inline;"> HIRES will be the high-resolution spectrograph of the European Extremely Large Telescope at optical and near-infrared wavelengths. It consists of three fibre-fed spectrographs providing a wavelength coverage of 0.4-1.8 mic (goal 0.35-1.8 mic) at a spectral resolution of ~100,000. The fibre-feeding allows HIRES to have several, interchangeable observing modes including a SCAO module and a small dif… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.12317v1-abstract-full').style.display = 'inline'; document.getElementById('2011.12317v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.12317v1-abstract-full" style="display: none;"> HIRES will be the high-resolution spectrograph of the European Extremely Large Telescope at optical and near-infrared wavelengths. It consists of three fibre-fed spectrographs providing a wavelength coverage of 0.4-1.8 mic (goal 0.35-1.8 mic) at a spectral resolution of ~100,000. The fibre-feeding allows HIRES to have several, interchangeable observing modes including a SCAO module and a small diffraction-limited IFU in the NIR. Therefore, it will be able to operate both in seeing and diffraction-limited modes. ELT-HIRES has a wide range of science cases spanning nearly all areas of research in astrophysics and even fundamental physics. Some of the top science cases will be the detection of bio signatures from exoplanet atmospheres, finding the fingerprints of the first generation of stars (PopIII), tests on the stability of Nature's fundamental couplings, and the direct detection of the cosmic acceleration. The HIRES consortium is composed of more than 30 institutes from 14 countries, forming a team of more than 200 scientists and engineers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.12317v1-abstract-full').style.display = 'none'; document.getElementById('2011.12317v1-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> 24 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </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">to appear in the ESO Messenger No.182, December 2020</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.00316">arXiv:2010.00316</a> <span> [<a href="https://arxiv.org/pdf/2010.00316">pdf</a>, <a href="https://arxiv.org/format/2010.00316">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="Earth and Planetary Astrophysics">astro-ph.EP</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/10.1051/0004-6361/202038306">10.1051/0004-6361/202038306 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ESPRESSO@VLT -- On-sky performance and first results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pepe%2C+F">F. Pepe</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Rebolo%2C+R">R. Rebolo</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+N+C">N. C. Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Dekker%2C+H">H. Dekker</a>, <a href="/search/astro-ph?searchtype=author&query=Cabral%2C+A">A. Cabral</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Marcantonio%2C+P">P. Di Marcantonio</a>, <a href="/search/astro-ph?searchtype=author&query=Figueira%2C+P">P. Figueira</a>, <a href="/search/astro-ph?searchtype=author&query=Curto%2C+G+L">G. Lo Curto</a>, <a href="/search/astro-ph?searchtype=author&query=Lovis%2C+C">C. Lovis</a>, <a href="/search/astro-ph?searchtype=author&query=Mayor%2C+M">M. Mayor</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%A9gevand%2C+D">D. M茅gevand</a>, <a href="/search/astro-ph?searchtype=author&query=Molaro%2C+P">P. Molaro</a>, <a href="/search/astro-ph?searchtype=author&query=Riva%2C+M">M. Riva</a>, <a href="/search/astro-ph?searchtype=author&query=Osorio%2C+M+R+Z">M. R. Zapatero Osorio</a>, <a href="/search/astro-ph?searchtype=author&query=Amate%2C+M">M. Amate</a>, <a href="/search/astro-ph?searchtype=author&query=Manescau%2C+A">A. Manescau</a>, <a href="/search/astro-ph?searchtype=author&query=Pasquini%2C+L">L. Pasquini</a>, <a href="/search/astro-ph?searchtype=author&query=Zerbi%2C+F+M">F. M. Zerbi</a>, <a href="/search/astro-ph?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+M">M. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Affolter%2C+M">M. Affolter</a>, <a href="/search/astro-ph?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/astro-ph?searchtype=author&query=Aliverti%2C+M">M. Aliverti</a>, <a href="/search/astro-ph?searchtype=author&query=Allart%2C+R">R. Allart</a> , et al. (75 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="2010.00316v1-abstract-short" style="display: inline;"> ESPRESSO is the new high-resolution spectrograph of ESO's Very-Large Telescope (VLT). It was designed for ultra-high radial-velocity precision and extreme spectral fidelity with the aim of performing exoplanet research and fundamental astrophysical experiments with unprecedented precision and accuracy. It is able to observe with any of the four Unit Telescopes (UT) of the VLT at a spectral resolvi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.00316v1-abstract-full').style.display = 'inline'; document.getElementById('2010.00316v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.00316v1-abstract-full" style="display: none;"> ESPRESSO is the new high-resolution spectrograph of ESO's Very-Large Telescope (VLT). It was designed for ultra-high radial-velocity precision and extreme spectral fidelity with the aim of performing exoplanet research and fundamental astrophysical experiments with unprecedented precision and accuracy. It is able to observe with any of the four Unit Telescopes (UT) of the VLT at a spectral resolving power of 140,000 or 190,000 over the 378.2 to 788.7 nm wavelength range, or with all UTs together, turning the VLT into a 16-m diameter equivalent telescope in terms of collecting area, while still providing a resolving power of 70,000. We provide a general description of the ESPRESSO instrument, report on the actual on-sky performance, and present our Guaranteed-Time Observation (GTO) program with its first results. ESPRESSO was installed on the Paranal Observatory in fall 2017. Commissioning (on-sky testing) was conducted between December 2017 and September 2018. The instrument saw its official start of operations on October 1st, 2018, but improvements to the instrument and re-commissioning runs were conducted until July 2019. The measured overall optical throughput of ESPRESSO at 550 nm and a seeing of 0.65 arcsec exceeds the 10% mark under nominal astro-climatic conditions. We demonstrate a radial-velocity precision of better than 25 cm/s during one night and 50 cm/s over several months. These values being limited by photon noise and stellar jitter show that the performanceis compatible with an instrumental precision of 10 cm/s. No difference has been measured across the UTs neither in throughput nor RV precision. The combination of the large collecting telescope area with the efficiency and the exquisite spectral fidelity of ESPRESSO opens a new parameter space in RV measurements, the study of planetary atmospheres, fundamental constants, stellar characterisation and many other fields. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.00316v1-abstract-full').style.display = 'none'; document.getElementById('2010.00316v1-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> 1 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </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">26 pages, 28 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.06410">arXiv:2007.06410</a> <span> [<a href="https://arxiv.org/pdf/2007.06410">pdf</a>, <a href="https://arxiv.org/format/2007.06410">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/10.1051/0004-6361/202038416">10.1051/0004-6361/202038416 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A precise architecture characterization of the $蟺$ Men planetary system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/astro-ph?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Lovis%2C+C">C. Lovis</a>, <a href="/search/astro-ph?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/astro-ph?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/astro-ph?searchtype=author&query=Demangeon%2C+O+D+S">O. D. S. Demangeon</a>, <a href="/search/astro-ph?searchtype=author&query=Faria%2C+J+P">J. P. Faria</a>, <a href="/search/astro-ph?searchtype=author&query=Lillo-Box%2C+J">J. Lillo-Box</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Pepe%2C+F">F. Pepe</a>, <a href="/search/astro-ph?searchtype=author&query=Rebolo%2C+R">R. Rebolo</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+N+C">N. C. Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Osorio%2C+M+R+Z">M. R. Zapatero Osorio</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J+I+G">J. I. Gonz谩lez Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Amate%2C+M">M. Amate</a>, <a href="/search/astro-ph?searchtype=author&query=Pasquini%2C+L">L. Pasquini</a>, <a href="/search/astro-ph?searchtype=author&query=Zerbi%2C+F+M">F. M. Zerbi</a>, <a href="/search/astro-ph?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+M">M. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Affolter%2C+M">M. Affolter</a>, <a href="/search/astro-ph?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/astro-ph?searchtype=author&query=Aliverti%2C+M">M. Aliverti</a>, <a href="/search/astro-ph?searchtype=author&query=Allart%2C+R">R. Allart</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=%C3%81lvarez%2C+D">D. 脕lvarez</a> , et al. (75 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="2007.06410v1-abstract-short" style="display: inline;"> The bright star $蟺$ Men was chosen as the first target for a radial velocity follow-up to test the performance of ESPRESSO, the new high-resolution spectrograph at the ESO's Very-Large Telescope (VLT). The star hosts a multi-planet system (a transiting 4 M$_\oplus$ planet at $\sim$0.07 au, and a sub-stellar companion on a $\sim$2100-day eccentric orbit) which is particularly appealing for a precis… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.06410v1-abstract-full').style.display = 'inline'; document.getElementById('2007.06410v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.06410v1-abstract-full" style="display: none;"> The bright star $蟺$ Men was chosen as the first target for a radial velocity follow-up to test the performance of ESPRESSO, the new high-resolution spectrograph at the ESO's Very-Large Telescope (VLT). The star hosts a multi-planet system (a transiting 4 M$_\oplus$ planet at $\sim$0.07 au, and a sub-stellar companion on a $\sim$2100-day eccentric orbit) which is particularly appealing for a precise multi-technique characterization. With the new ESPRESSO observations, that cover a time span of 200 days, we aim to improve the precision and accuracy of the planet parameters and search for additional low-mass companions. We also take advantage of new photometric transits of $蟺$ Men c observed by TESS over a time span that overlaps with that of the ESPRESSO follow-up campaign. We analyse the enlarged spectroscopic and photometric datasets and compare the results to those in the literature. We further characterize the system by means of absolute astrometry with Hipparcos and Gaia. We used the spectra of ESPRESSO for an independent determination of the stellar fundamental parameters. We present a precise characterization of the planetary system around $蟺$ Men. The ESPRESSO radial velocities alone (with typical uncertainty of 10 cm/s) allow for a precise retrieval of the Doppler signal induced by $蟺$ Men c. The residuals show an RMS of 1.2 m/s, and we can exclude companions with a minimum mass less than $\sim$2 M$_\oplus$ within the orbit of $蟺$ Men c). We improve the ephemeris of $蟺$ Men c using 18 additional TESS transits, and in combination with the astrometric measurements, we determine the inclination of the orbital plane of $蟺$ Men b with high precision ($i_{b}=45.8^{+1.4}_{-1.1}$ deg). This leads to the precise measurement of its absolute mass $m_{b}=14.1^{+0.5}_{-0.4}$ M$_{Jup}$, and shows that the planetary orbital planes are highly misaligned. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.06410v1-abstract-full').style.display = 'none'; document.getElementById('2007.06410v1-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> 13 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </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">Accepted for publication on A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 642, A31 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.01081">arXiv:2007.01081</a> <span> [<a href="https://arxiv.org/pdf/2007.01081">pdf</a>, <a href="https://arxiv.org/format/2007.01081">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/10.1051/0004-6361/202038187">10.1051/0004-6361/202038187 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterization of the K2-38 planetary system. Unraveling one of the densest planets known to date </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Toledo-Padr%C3%B3n%2C+B">B. Toledo-Padr贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Lovis%2C+C">C. Lovis</a>, <a href="/search/astro-ph?searchtype=author&query=Mascare%C3%B1o%2C+A+S">A. Su谩rez Mascare帽o</a>, <a href="/search/astro-ph?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J+I+G">J. I. Gonz谩lez Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bouchy%2C+F">F. Bouchy</a>, <a href="/search/astro-ph?searchtype=author&query=Osorio%2C+M+R+Z">M. R. Zapatero Osorio</a>, <a href="/search/astro-ph?searchtype=author&query=Rebolo%2C+R">R. Rebolo</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Pepe%2C+F+A">F. A. Pepe</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+N+C">N. C. Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/astro-ph?searchtype=author&query=Tabernero%2C+H+M">H. M. Tabernero</a>, <a href="/search/astro-ph?searchtype=author&query=Lillo-Box%2C+J">J. Lillo-Box</a>, <a href="/search/astro-ph?searchtype=author&query=Bossini%2C+D">D. Bossini</a>, <a href="/search/astro-ph?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/astro-ph?searchtype=author&query=Allart%2C+R">R. Allart</a>, <a href="/search/astro-ph?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Odorico%2C+V">V. D'Odorico</a>, <a href="/search/astro-ph?searchtype=author&query=Figueira%2C+P">P. Figueira</a>, <a href="/search/astro-ph?searchtype=author&query=Lavie%2C+B">B. Lavie</a>, <a href="/search/astro-ph?searchtype=author&query=Curto%2C+G+L">G. Lo Curto</a>, <a href="/search/astro-ph?searchtype=author&query=Mehner%2C+A">A. Mehner</a>, <a href="/search/astro-ph?searchtype=author&query=Micela%2C+G">G. Micela</a> , et al. (68 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="2007.01081v5-abstract-short" style="display: inline;"> We characterized the transiting planetary system orbiting the G2V star K2-38 using the new-generation echelle spectrograph ESPRESSO. We carried out a photometric analysis of the available K2 photometric light curve of this star to measure the radius of its two known planets. Using 43 ESPRESSO high-precision radial velocity measurements taken over the course of 8 months along with the 14 previously… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.01081v5-abstract-full').style.display = 'inline'; document.getElementById('2007.01081v5-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.01081v5-abstract-full" style="display: none;"> We characterized the transiting planetary system orbiting the G2V star K2-38 using the new-generation echelle spectrograph ESPRESSO. We carried out a photometric analysis of the available K2 photometric light curve of this star to measure the radius of its two known planets. Using 43 ESPRESSO high-precision radial velocity measurements taken over the course of 8 months along with the 14 previously published HIRES RV measurements, we modeled the orbits of the two planets through a MCMC analysis, significantly improving their mass measurements. Using ESPRESSO spectra, we derived the stellar parameters, $T_{\rm eff}$=5731$\pm$66, $\log g$=4.38$\pm$0.11~dex, and $[Fe/H]$=0.26$\pm$0.05~dex, and thus the mass and radius of K2-38, $M_{\star}$=1.03 $^{+0.04}_{-0.02}$~M$_{\oplus}$ and $R_{\star}$=1.06 $^{+0.09}_{-0.06}$~R$_{\oplus}$. We determine new values for the planetary properties of both planets. We characterize K2-38b as a super-Earth with $R_{\rm P}$=1.54$\pm$0.14~R$_{\rm \oplus}$ and $M_{\rm p}$=7.3$^{+1.1}_{-1.0}$~M$_{\oplus}$, and K2-38c as a sub-Neptune with $R_{\rm P}$=2.29$\pm$0.26~R$_{\rm \oplus}$ and $M_{\rm p}$=8.3$^{+1.3}_{-1.3}$~M$_{\oplus}$. We derived a mean density of $蟻_{\rm p}$=11.0$^{+4.1}_{-2.8}$~g cm$^{-3}$ for K2-38b and $蟻_{\rm p}$=3.8$^{+1.8}_{-1.1}$~g~cm$^{-3}$ for K2-38c, confirming K2-38b as one of the densest planets known to date. The best description for the composition of K2-38b comes from an iron-rich Mercury-like model, while K2-38c is better described by a rocky model with a H2 envelope. The maximum collision stripping boundary shows how giant impacts could be the cause for the high density of K2-38b. The irradiation received by each planet places them on opposite sides of the radius valley. We find evidence of a long-period signal in the radial velocity time-series whose origin could be linked to a 0.25-3~M$_{\rm J}$ planet or stellar activity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.01081v5-abstract-full').style.display = 'none'; document.getElementById('2007.01081v5-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> 1 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </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">16 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 641, A92 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.12114">arXiv:2005.12114</a> <span> [<a href="https://arxiv.org/pdf/2005.12114">pdf</a>, <a href="https://arxiv.org/format/2005.12114">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey 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="Solar and Stellar Astrophysics">astro-ph.SR</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/10.1051/0004-6361/202037745">10.1051/0004-6361/202037745 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Revisiting Proxima with ESPRESSO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mascare%C3%B1o%2C+A+S">A. Su谩rez Mascare帽o</a>, <a href="/search/astro-ph?searchtype=author&query=Faria%2C+J+P">J. P. Faria</a>, <a href="/search/astro-ph?searchtype=author&query=Figueira%2C+P">P. Figueira</a>, <a href="/search/astro-ph?searchtype=author&query=Lovis%2C+C">C. Lovis</a>, <a href="/search/astro-ph?searchtype=author&query=Damasso%2C+M">M. Damasso</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J+I+G">J. I. Gonz谩lez Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Rebolo%2C+R">R. Rebolo</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiano%2C+S">S. Cristiano</a>, <a href="/search/astro-ph?searchtype=author&query=Pepe%2C+F">F. Pepe</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+N+C">N. C. Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Osorio%2C+M+R+Z">M. R. Zapatero Osorio</a>, <a href="/search/astro-ph?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/astro-ph?searchtype=author&query=Hojjatpanah%2C+S">S. Hojjatpanah</a>, <a href="/search/astro-ph?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Murgas%2C+F">F. Murgas</a>, <a href="/search/astro-ph?searchtype=author&query=Abreo%2C+M">M. Abreo</a>, <a href="/search/astro-ph?searchtype=author&query=Affolter%2C+M">M. Affolter</a>, <a href="/search/astro-ph?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/astro-ph?searchtype=author&query=Aliverti%2C+M">M. Aliverti</a>, <a href="/search/astro-ph?searchtype=author&query=Allart%2C+R">R. Allart</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+D">D. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Amate%2C+M">M. Amate</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+V">V. Baldini</a> , et al. (66 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="2005.12114v2-abstract-short" style="display: inline;"> We aim to confirm the presence of Proxima b using independent measurements obtained with the new ESPRESSO spectrograph, and refine the planetary parameters taking advantage of its improved precision. We analysed 63 spectroscopic ESPRESSO observations of Proxima taken during 2019. We obtained radial velocity measurements with a typical radial velocity photon noise of 26 cm/s. We ran a joint MCMC an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.12114v2-abstract-full').style.display = 'inline'; document.getElementById('2005.12114v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.12114v2-abstract-full" style="display: none;"> We aim to confirm the presence of Proxima b using independent measurements obtained with the new ESPRESSO spectrograph, and refine the planetary parameters taking advantage of its improved precision. We analysed 63 spectroscopic ESPRESSO observations of Proxima taken during 2019. We obtained radial velocity measurements with a typical radial velocity photon noise of 26 cm/s. We ran a joint MCMC analysis on the time series of the radial velocity and full-width half maximum of the cross-correlation function to model the planetary and stellar signals present in the data, applying Gaussian process regression to deal with stellar activity. We confirm the presence of Proxima b independently in the ESPRESSO data. The ESPRESSO data on its own shows Proxima b at a period of 11.218 $\pm$ 0.029 days, with a minimum mass of 1.29 $\pm$ 0.13 Me. In the combined dataset we measure a period of 11.18427 $\pm$ 0.00070 days with a minimum mass of 1.173 $\pm$ 0.086 Me. We find no evidence of stellar activity as a potential cause for the 11.2 days signal. We find some evidence for the presence of a second short-period signal, at 5.15 days with a semi-amplitude of merely 40 cm/s. If caused by a planetary companion, it would correspond to a minimum mass of 0.29 $\pm$ 0.08 Me. We find that the FWHM of the CCF can be used as a proxy for the brightness changes and that its gradient with time can be used to successfully detrend the radial velocity data from part of the influence of stellar activity. The activity-induced radial velocity signal in the ESPRESSO data shows a trend in amplitude towards redder wavelengths. Velocities measured using the red end of the spectrograph are less affected by activity, suggesting that the stellar activity is spot-dominated. The data collected excludes the presence of extra companions with masses above 0.6 Me at periods shorter than 50 days. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.12114v2-abstract-full').style.display = 'none'; document.getElementById('2005.12114v2-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> 26 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2020. </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">25 pages, 26 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 639, A77 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2003.05528">arXiv:2003.05528</a> <span> [<a href="https://arxiv.org/pdf/2003.05528">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/10.1038/s41586-020-2107-1">10.1038/s41586-020-2107-1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Nightside condensation of iron in an ultra-hot giant exoplanet </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ehrenreich%2C+D">David Ehrenreich</a>, <a href="/search/astro-ph?searchtype=author&query=Lovis%2C+C">Christophe Lovis</a>, <a href="/search/astro-ph?searchtype=author&query=Allart%2C+R">Romain Allart</a>, <a href="/search/astro-ph?searchtype=author&query=Osorio%2C+M+R+Z">Mar铆a Rosa Zapatero Osorio</a>, <a href="/search/astro-ph?searchtype=author&query=Pepe%2C+F">Francesco Pepe</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">Stefano Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Rebolo%2C+R">Rafael Rebolo</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+N+C">Nuno C. Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Borsa%2C+F">Francesco Borsa</a>, <a href="/search/astro-ph?searchtype=author&query=Demangeon%2C+O">Olivier Demangeon</a>, <a href="/search/astro-ph?searchtype=author&query=Dumusque%2C+X">Xavier Dumusque</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J+I+G">Jonay I. Gonz谩lez Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Casasayas-Barris%2C+N">N煤ria Casasayas-Barris</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A9gransan%2C+D">Damien S茅gransan</a>, <a href="/search/astro-ph?searchtype=author&query=Sousa%2C+S">S茅rgio Sousa</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+M">Manuel Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Adibekyan%2C+V">Vardan Adibekyan</a>, <a href="/search/astro-ph?searchtype=author&query=Affolter%2C+M">Michael Affolter</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">Carlos Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Alibert%2C+Y">Yann Alibert</a>, <a href="/search/astro-ph?searchtype=author&query=Aliverti%2C+M">Matteo Aliverti</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+D">David Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Amate%2C+M">Manuel Amate</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">Gerardo Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+V">Veronica Baldini</a> , et al. (72 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="2003.05528v1-abstract-short" style="display: inline;"> Ultra-hot giant exoplanets receive thousands of times Earth's insolation. Their high-temperature atmospheres (>2,000 K) are ideal laboratories for studying extreme planetary climates and chemistry. Daysides are predicted to be cloud-free, dominated by atomic species and substantially hotter than nightsides. Atoms are expected to recombine into molecules over the nightside, resulting in different d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.05528v1-abstract-full').style.display = 'inline'; document.getElementById('2003.05528v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.05528v1-abstract-full" style="display: none;"> Ultra-hot giant exoplanets receive thousands of times Earth's insolation. Their high-temperature atmospheres (>2,000 K) are ideal laboratories for studying extreme planetary climates and chemistry. Daysides are predicted to be cloud-free, dominated by atomic species and substantially hotter than nightsides. Atoms are expected to recombine into molecules over the nightside, resulting in different day-night chemistry. While metallic elements and a large temperature contrast have been observed, no chemical gradient has been measured across the surface of such an exoplanet. Different atmospheric chemistry between the day-to-night ("evening") and night-to-day ("morning") terminators could, however, be revealed as an asymmetric absorption signature during transit. Here, we report the detection of an asymmetric atmospheric signature in the ultra-hot exoplanet WASP-76b. We spectrally and temporally resolve this signature thanks to the combination of high-dispersion spectroscopy with a large photon-collecting area. The absorption signal, attributed to neutral iron, is blueshifted by -11+/-0.7 km s-1 on the trailing limb, which can be explained by a combination of planetary rotation and wind blowing from the hot dayside. In contrast, no signal arises from the nightside close to the morning terminator, showing that atomic iron is not absorbing starlight there. Iron must thus condense during its journey across the nightside. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.05528v1-abstract-full').style.display = 'none'; document.getElementById('2003.05528v1-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> 11 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2020. </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">Published in Nature (Accepted on 24 January 2020.) 33 pages, 11 figures, 3 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/1405.7584">arXiv:1405.7584</a> <span> [<a href="https://arxiv.org/pdf/1405.7584">pdf</a>, <a href="https://arxiv.org/ps/1405.7584">ps</a>, <a href="https://arxiv.org/format/1405.7584">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="Databases">cs.DB</span> </div> </div> <p class="title is-5 mathjax"> DAS: a data management system for instrument tests and operations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Frailis%2C+M">Marco Frailis</a>, <a href="/search/astro-ph?searchtype=author&query=Sartor%2C+S">Stefano Sartor</a>, <a href="/search/astro-ph?searchtype=author&query=Zacchei%2C+A">Andrea Zacchei</a>, <a href="/search/astro-ph?searchtype=author&query=Lodi%2C+M">Marcello Lodi</a>, <a href="/search/astro-ph?searchtype=author&query=Cirami%2C+R">Roberto Cirami</a>, <a href="/search/astro-ph?searchtype=author&query=Pasian%2C+F">Fabio Pasian</a>, <a href="/search/astro-ph?searchtype=author&query=Trifoglio%2C+M">Massimo Trifoglio</a>, <a href="/search/astro-ph?searchtype=author&query=Bulgarelli%2C+A">Andrea Bulgarelli</a>, <a href="/search/astro-ph?searchtype=author&query=Gianotti%2C+F">Fulvio Gianotti</a>, <a href="/search/astro-ph?searchtype=author&query=Franceschi%2C+E">Enrico Franceschi</a>, <a href="/search/astro-ph?searchtype=author&query=Nicastro%2C+L">Luciano Nicastro</a>, <a href="/search/astro-ph?searchtype=author&query=Conforti%2C+V">Vito Conforti</a>, <a href="/search/astro-ph?searchtype=author&query=Zoli%2C+A">Andrea Zoli</a>, <a href="/search/astro-ph?searchtype=author&query=Smart%2C+R">Ricky Smart</a>, <a href="/search/astro-ph?searchtype=author&query=Morbidelli%2C+R">Roberto Morbidelli</a>, <a href="/search/astro-ph?searchtype=author&query=Dadina%2C+M">Mauro Dadina</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="1405.7584v1-abstract-short" style="display: inline;"> The Data Access System (DAS) is a metadata and data management software system, providing a reusable solution for the storage of data acquired both from telescopes and auxiliary data sources during the instrument development phases and operations. It is part of the Customizable Instrument WorkStation system (CIWS-FW), a framework for the storage, processing and quick-look at the data acquired from… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.7584v1-abstract-full').style.display = 'inline'; document.getElementById('1405.7584v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1405.7584v1-abstract-full" style="display: none;"> The Data Access System (DAS) is a metadata and data management software system, providing a reusable solution for the storage of data acquired both from telescopes and auxiliary data sources during the instrument development phases and operations. It is part of the Customizable Instrument WorkStation system (CIWS-FW), a framework for the storage, processing and quick-look at the data acquired from scientific instruments. The DAS provides a data access layer mainly targeted to software applications: quick-look displays, pre-processing pipelines and scientific workflows. It is logically organized in three main components: an intuitive and compact Data Definition Language (DAS DDL) in XML format, aimed for user-defined data types; an Application Programming Interface (DAS API), automatically adding classes and methods supporting the DDL data types, and providing an object-oriented query language; a data management component, which maps the metadata of the DDL data types in a relational Data Base Management System (DBMS), and stores the data in a shared (network) file system. With the DAS DDL, developers define the data model for a particular project, specifying for each data type the metadata attributes, the data format and layout (if applicable), and named references to related or aggregated data types. Together with the DDL user-defined data types, the DAS API acts as the only interface to store, query and retrieve the metadata and data in the DAS system, providing both an abstract interface and a data model specific one in C, C++ and Python. The mapping of metadata in the back-end database is automatic and supports several relational DBMSs, including MySQL, Oracle and PostgreSQL. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.7584v1-abstract-full').style.display = 'none'; document.getElementById('1405.7584v1-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> 29 May, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2014. </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">Accepted for pubblication on ADASS Conference Series</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1405.7255">arXiv:1405.7255</a> <span> [<a href="https://arxiv.org/pdf/1405.7255">pdf</a>, <a href="https://arxiv.org/ps/1405.7255">ps</a>, <a href="https://arxiv.org/format/1405.7255">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> </div> </div> <p class="title is-5 mathjax"> CIWS-FW: a Customizable InstrumentWorkstation Software Framework for instrument-independent data handling </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Conforti%2C+V">Vito Conforti</a>, <a href="/search/astro-ph?searchtype=author&query=Trifoglio%2C+M">Massimo Trifoglio</a>, <a href="/search/astro-ph?searchtype=author&query=Bulgarelli%2C+A">Andrea Bulgarelli</a>, <a href="/search/astro-ph?searchtype=author&query=Gianotti%2C+F">Fulvio Gianotti</a>, <a href="/search/astro-ph?searchtype=author&query=Franceschi%2C+E">Enrico Franceschi</a>, <a href="/search/astro-ph?searchtype=author&query=Nicastro%2C+L">Luciano Nicastro</a>, <a href="/search/astro-ph?searchtype=author&query=Zoli%2C+A">Andrea Zoli</a>, <a href="/search/astro-ph?searchtype=author&query=Dadina%2C+M">Mauro Dadina</a>, <a href="/search/astro-ph?searchtype=author&query=Smart%2C+R">Ricky Smart</a>, <a href="/search/astro-ph?searchtype=author&query=Morbidelli%2C+R">Roberto Morbidelli</a>, <a href="/search/astro-ph?searchtype=author&query=Frailis%2C+M">Marco Frailis</a>, <a href="/search/astro-ph?searchtype=author&query=Sartor%2C+S">Stefano Sartor</a>, <a href="/search/astro-ph?searchtype=author&query=Zacchei%2C+A">Andrea Zacchei</a>, <a href="/search/astro-ph?searchtype=author&query=Lodi%2C+M">Marcello Lodi</a>, <a href="/search/astro-ph?searchtype=author&query=Cirami%2C+R">Roberto Cirami</a>, <a href="/search/astro-ph?searchtype=author&query=Pasian%2C+F">Fabio Pasian</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="1405.7255v1-abstract-short" style="display: inline;"> The CIWS-FW is aimed at providing a common and standard solution for the storage, processing and quick look at the data acquired from scientific instruments for astrophysics. The target system is the instrument workstation either in the context of the Electrical Ground Support Equipment for space-borne experiments, or in the context of the data acquisition system for instrumentation. The CIWS-FW c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.7255v1-abstract-full').style.display = 'inline'; document.getElementById('1405.7255v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1405.7255v1-abstract-full" style="display: none;"> The CIWS-FW is aimed at providing a common and standard solution for the storage, processing and quick look at the data acquired from scientific instruments for astrophysics. The target system is the instrument workstation either in the context of the Electrical Ground Support Equipment for space-borne experiments, or in the context of the data acquisition system for instrumentation. The CIWS-FW core includes software developed by team members for previous experiments and provides new components and tools that improve the software reusability, configurability and extensibility attributes. The CIWS-FW mainly consists of two packages: the data processing system and the data access system. The former provides the software components and libraries to support the data acquisition, transformation, display and storage in near real time of either a data packet stream and/or a sequence of data files generated by the instrument. The latter is a meta-data and data management system, providing a reusable solution for the archiving and retrieval of the acquired data. A built-in operator GUI allows to control and configure the IW. In addition, the framework provides mechanisms for system error and logging handling. A web portal provides the access to the CIWS-FW documentation, software repository and bug tracking tools for CIWS-FW developers. We will describe the CIWS-FW architecture and summarize the project status. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.7255v1-abstract-full').style.display = 'none'; document.getElementById('1405.7255v1-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> 28 May, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2014. </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">Accepted for pubblication on ADASS Conference Series</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1401.5918">arXiv:1401.5918</a> <span> [<a href="https://arxiv.org/pdf/1401.5918">pdf</a>, <a href="https://arxiv.org/format/1401.5918">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="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> ESPRESSO: The next European exoplanet hunter </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pepe%2C+F">F. Pepe</a>, <a href="/search/astro-ph?searchtype=author&query=Molaro%2C+P">P. Molaro</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Rebolo%2C+R">R. Rebolo</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+N+C">N. C. Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Dekker%2C+H">H. Dekker</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%A9gevand%2C+D">D. M茅gevand</a>, <a href="/search/astro-ph?searchtype=author&query=Zerbi%2C+F+M">F. M. Zerbi</a>, <a href="/search/astro-ph?searchtype=author&query=Cabral%2C+A">A. Cabral</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Marcantonio%2C+P">P. Di Marcantonio</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+M">M. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Affolter%2C+M">M. Affolter</a>, <a href="/search/astro-ph?searchtype=author&query=Aliverti%2C+M">M. Aliverti</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">C. Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Amate%2C+M">M. Amate</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+V">V. Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Bristow%2C+P">P. Bristow</a>, <a href="/search/astro-ph?searchtype=author&query=Broeg%2C+C">C. Broeg</a>, <a href="/search/astro-ph?searchtype=author&query=Cirami%2C+R">R. Cirami</a>, <a href="/search/astro-ph?searchtype=author&query=Coelho%2C+J">J. Coelho</a>, <a href="/search/astro-ph?searchtype=author&query=Conconi%2C+P">P. Conconi</a>, <a href="/search/astro-ph?searchtype=author&query=Coretti%2C+I">I. Coretti</a>, <a href="/search/astro-ph?searchtype=author&query=Cupani%2C+G">G. Cupani</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Odorico%2C+V">V. D'Odorico</a> , et al. (33 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="1401.5918v1-abstract-short" style="display: inline;"> The acronym ESPRESSO stems for Echelle SPectrograph for Rocky Exoplanets and Stable Spectroscopic Observations; this instrument will be the next VLT high resolution spectrograph. The spectrograph will be installed at the Combined-Coud茅 Laboratory of the VLT and linked to the four 8.2 m Unit Telescopes (UT) through four optical Coud茅 trains. ESPRESSO will combine efficiency and extreme spectroscopi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.5918v1-abstract-full').style.display = 'inline'; document.getElementById('1401.5918v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1401.5918v1-abstract-full" style="display: none;"> The acronym ESPRESSO stems for Echelle SPectrograph for Rocky Exoplanets and Stable Spectroscopic Observations; this instrument will be the next VLT high resolution spectrograph. The spectrograph will be installed at the Combined-Coud茅 Laboratory of the VLT and linked to the four 8.2 m Unit Telescopes (UT) through four optical Coud茅 trains. ESPRESSO will combine efficiency and extreme spectroscopic precision. ESPRESSO is foreseen to achieve a gain of two magnitudes with respect to its predecessor HARPS, and to improve the instrumental radial-velocity precision to reach the 10 cm/s level. It can be operated either with a single UT or with up to four UTs, enabling an additional gain in the latter mode. The incoherent combination of four telescopes and the extreme precision requirements called for many innovative design solutions while ensuring the technical heritage of the successful HARPS experience. ESPRESSO will allow to explore new frontiers in most domains of astrophysics that require precision and sensitivity. The main scientific drivers are the search and characterization of rocky exoplanets in the habitable zone of quiet, nearby G to M-dwarfs and the analysis of the variability of fundamental physical constants. The project passed the final design review in May 2013 and entered the manufacturing phase. ESPRESSO will be installed at the Paranal Observatory in 2016 and its operation is planned to start by the end of the same year. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.5918v1-abstract-full').style.display = 'none'; document.getElementById('1401.5918v1-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> 23 January, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2014. </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">12 pages, figures included, accepted for publication in Astron. Nachr</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0106390">arXiv:astro-ph/0106390</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0106390">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0106390">ps</a>, <a href="https://arxiv.org/format/astro-ph/0106390">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-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/10.1086/342128">10.1086/342128 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Light Isotope Abundances in Solar Energetic Particles measured by the Space Instrument NINA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+NINA+Collaboration"> The NINA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Bakaldin%2C+A">A. Bakaldin</a>, <a href="/search/astro-ph?searchtype=author&query=Galper%2C+A">A. Galper</a>, <a href="/search/astro-ph?searchtype=author&query=Koldashov%2C+S">S. Koldashov</a>, <a href="/search/astro-ph?searchtype=author&query=Korotkov%2C+M">M. Korotkov</a>, <a href="/search/astro-ph?searchtype=author&query=Leonov%2C+A">A. Leonov</a>, <a href="/search/astro-ph?searchtype=author&query=Mikhailov%2C+V">V. Mikhailov</a>, <a href="/search/astro-ph?searchtype=author&query=Murashov%2C+A">A. Murashov</a>, <a href="/search/astro-ph?searchtype=author&query=Voronov%2C+S">S. Voronov</a>, <a href="/search/astro-ph?searchtype=author&query=Bidoli%2C+V">V. Bidoli</a>, <a href="/search/astro-ph?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/astro-ph?searchtype=author&query=De+Pascale%2C+M">M. De Pascale</a>, <a href="/search/astro-ph?searchtype=author&query=Furano%2C+G">G. Furano</a>, <a href="/search/astro-ph?searchtype=author&query=Iannucci%2C+A">A. Iannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Morselli%2C+A">A. Morselli</a>, <a href="/search/astro-ph?searchtype=author&query=Picozza%2C+P">P. Picozza</a>, <a href="/search/astro-ph?searchtype=author&query=Sparvoli%2C+R">R. Sparvoli</a>, <a href="/search/astro-ph?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/astro-ph?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/astro-ph?searchtype=author&query=Cirami%2C+R">R. Cirami</a>, <a href="/search/astro-ph?searchtype=author&query=Vacchi%2C+A">A. Vacchi</a>, <a href="/search/astro-ph?searchtype=author&query=Zampa%2C+N">N. Zampa</a>, <a href="/search/astro-ph?searchtype=author&query=Ambriola%2C+M">M. Ambriola</a>, <a href="/search/astro-ph?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/astro-ph?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a> , et al. (12 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="astro-ph/0106390v1-abstract-short" style="display: inline;"> This article reports nine Solar Energetic Particle events detected by the instrument NINA between October 1998 and April 1999. NINA is a silicon-based particle detector mounted on-board the Russian satellite Resurs-01-N4, which has flown at an altitude of about 800 km in polar inclination since July 1998. For every solar event the power-law He4 spectrum across the energy interval 10--50 MeV/n wa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0106390v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0106390v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0106390v1-abstract-full" style="display: none;"> This article reports nine Solar Energetic Particle events detected by the instrument NINA between October 1998 and April 1999. NINA is a silicon-based particle detector mounted on-board the Russian satellite Resurs-01-N4, which has flown at an altitude of about 800 km in polar inclination since July 1998. For every solar event the power-law He4 spectrum across the energy interval 10--50 MeV/n was reconstructed, and spectral indexes, gamma, from 1.8 to 6.8 extracted. Data of He3 and He4 were used to determine the He3/He4 ratio, that for some SEP events indicated an enrichment in He3. For the 1998 November 7 event the ratio reached a maximum value of 0.33+- 0.06, with spectral indexes of gamma = 2.5 +- 0.6 and gamma = 3.7 +- 0.3 for He3 and He4, respectively. The He3/He4 ratio averaged over the remaining events was 0.011 +- 0.004. For all events the deuterium-to-proton ratio was determined. The average value over all events was (3.9+-1.4) 10^{-5} across the energy interval 9--12 MeV/n. For one event (1998 November 24) this ratio yielded approximately 10 times higher than normal coronal values. Upper limits on the H3/H1 counting ratio for all events were determined. For the 1998 November 14 SEP event the high flux of heavy particles detected made it possible to reconstruct the carbon and oxygen flux. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0106390v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0106390v1-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> 21 June, 2001; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2001. </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">42 pages, 14 figures, submitted to Journal of Geophysical Research</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> Rom2F/2001/23 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 577 (2002) 513-523 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0012286">arXiv:astro-ph/0012286</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0012286">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0012286">ps</a>, <a href="https://arxiv.org/format/astro-ph/0012286">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-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/10.1086/318955">10.1086/318955 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> In-Orbit Performance of the Space Telescope NINA and GCR Flux Measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+NINA+Collaboration"> The NINA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Bidoli%2C+V">V. Bidoli</a>, <a href="/search/astro-ph?searchtype=author&query=Canestro%2C+A">A. Canestro</a>, <a href="/search/astro-ph?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/astro-ph?searchtype=author&query=DePascale%2C+M+P">M. P. DePascale</a>, <a href="/search/astro-ph?searchtype=author&query=Furano%2C+G">G. Furano</a>, <a href="/search/astro-ph?searchtype=author&query=Iannucci%2C+A">A. Iannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Morselli%2C+A">A. Morselli</a>, <a href="/search/astro-ph?searchtype=author&query=Picozza%2C+P">P. Picozza</a>, <a href="/search/astro-ph?searchtype=author&query=Reali%2C+E">E. Reali</a>, <a href="/search/astro-ph?searchtype=author&query=Sparvoli%2C+R">R. Sparvoli</a>, <a href="/search/astro-ph?searchtype=author&query=Bakaldin%2C+A">A. Bakaldin</a>, <a href="/search/astro-ph?searchtype=author&query=Galper%2C+A">A. Galper</a>, <a href="/search/astro-ph?searchtype=author&query=Koldashov%2C+S">S. Koldashov</a>, <a href="/search/astro-ph?searchtype=author&query=Korotkov%2C+M">M. Korotkov</a>, <a href="/search/astro-ph?searchtype=author&query=Leonov%2C+A">A. Leonov</a>, <a href="/search/astro-ph?searchtype=author&query=Mikhailov%2C+V">V. Mikhailov</a>, <a href="/search/astro-ph?searchtype=author&query=Murashov%2C+A">A. Murashov</a>, <a href="/search/astro-ph?searchtype=author&query=Voronov%2C+S">S. Voronov</a>, <a href="/search/astro-ph?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/astro-ph?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/astro-ph?searchtype=author&query=Cirami%2C+R">R. Cirami</a>, <a href="/search/astro-ph?searchtype=author&query=Vacchi%2C+A">A. Vacchi</a>, <a href="/search/astro-ph?searchtype=author&query=Zampa%2C+N">N. Zampa</a>, <a href="/search/astro-ph?searchtype=author&query=Ambriola%2C+M">M. Ambriola</a> , et al. (14 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="astro-ph/0012286v1-abstract-short" style="display: inline;"> The NINA apparatus, on board the Russian satellite Resurs-01 n.4, has been in polar orbit since 1998 July 10, at an altitude of 840 km. Its main scientific task is to study the galactic, solar and anomalous components of cosmic rays in the energy interval 10--200 MeV/n. In this paper we present a description of the instrument and its basic operating modes. Measurements of Galactic Cosmic Ray spe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0012286v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0012286v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0012286v1-abstract-full" style="display: none;"> The NINA apparatus, on board the Russian satellite Resurs-01 n.4, has been in polar orbit since 1998 July 10, at an altitude of 840 km. Its main scientific task is to study the galactic, solar and anomalous components of cosmic rays in the energy interval 10--200 MeV/n. In this paper we present a description of the instrument and its basic operating modes. Measurements of Galactic Cosmic Ray spectra will also be shown. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0012286v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0012286v1-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> 13 December, 2000; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2000. </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">38 pages, 10 figures, accepted for publication in the ApJS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> Rom2f/2000/32 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.Suppl. 132 (2001) 365-375 </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 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 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