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href="https://doi.org/10.1051/0004-6361/202449763">10.1051/0004-6361/202449763 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of a dormant 33 solar-mass black hole in pre-release Gaia astrometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Panuzzo%2C+P">P. Panuzzo</a>, <a href="/search/astro-ph?searchtype=author&query=Mazeh%2C+T">T. Mazeh</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Holl%2C+B">B. Holl</a>, <a href="/search/astro-ph?searchtype=author&query=Caffau%2C+E">E. Caffau</a>, <a href="/search/astro-ph?searchtype=author&query=Jorissen%2C+A">A. Jorissen</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Gavras%2C+P">P. Gavras</a>, <a href="/search/astro-ph?searchtype=author&query=Sahlmann%2C+J">J. Sahlmann</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+U">U. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=Wyrzykowski%2C+%C5%81">艁. Wyrzykowski</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Leclerc%2C+N">N. Leclerc</a>, <a href="/search/astro-ph?searchtype=author&query=Bauchet%2C+N">N. Bauchet</a>, <a href="/search/astro-ph?searchtype=author&query=Bombrun%2C+A">A. Bombrun</a>, <a href="/search/astro-ph?searchtype=author&query=Mowlavi%2C+N">N. Mowlavi</a>, <a href="/search/astro-ph?searchtype=author&query=Seabroke%2C+G+M">G. M. Seabroke</a>, <a href="/search/astro-ph?searchtype=author&query=Teyssier%2C+D">D. Teyssier</a>, <a href="/search/astro-ph?searchtype=author&query=Balbinot%2C+E">E. Balbinot</a>, <a href="/search/astro-ph?searchtype=author&query=Helmi%2C+A">A. Helmi</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a> , et al. (390 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="2404.10486v2-abstract-short" style="display: inline;"> Gravitational waves from black-hole merging events have revealed a population of extra-galactic BHs residing in short-period binaries with masses that are higher than expected based on most stellar evolution models - and also higher than known stellar-origin black holes in our Galaxy. It has been proposed that those high-mass BHs are the remnants of massive metal-poor stars. Gaia astrometry is exp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.10486v2-abstract-full').style.display = 'inline'; document.getElementById('2404.10486v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.10486v2-abstract-full" style="display: none;"> Gravitational waves from black-hole merging events have revealed a population of extra-galactic BHs residing in short-period binaries with masses that are higher than expected based on most stellar evolution models - and also higher than known stellar-origin black holes in our Galaxy. It has been proposed that those high-mass BHs are the remnants of massive metal-poor stars. Gaia astrometry is expected to uncover many Galactic wide-binary systems containing dormant BHs, which may not have been detected before. The study of this population will provide new information on the BH-mass distribution in binaries and shed light on their formation mechanisms and progenitors. As part of the validation efforts in preparation for the fourth Gaia data release (DR4), we analysed the preliminary astrometric binary solutions, obtained by the Gaia Non-Single Star pipeline, to verify their significance and to minimise false-detection rates in high-mass-function orbital solutions. The astrometric binary solution of one source, Gaia BH3, implies the presence of a 32.70 \pm 0.82 M\odot BH in a binary system with a period of 11.6 yr. Gaia radial velocities independently validate the astrometric orbit. Broad-band photometric and spectroscopic data show that the visible component is an old, very metal-poor giant of the Galactic halo, at a distance of 590 pc. The BH in the Gaia BH3 system is more massive than any other Galactic stellar-origin BH known thus far. The low metallicity of the star companion supports the scenario that metal-poor massive stars are progenitors of the high-mass BHs detected by gravitational-wave telescopes. The Galactic orbit of the system and its metallicity indicate that it might belong to the Sequoia halo substructure. Alternatively, and more plausibly, it could belong to the ED-2 stream, which likely originated from a globular cluster that had been disrupted by the Milky Way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.10486v2-abstract-full').style.display = 'none'; document.getElementById('2404.10486v2-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">23 pages, accepted fro publication in A&A Letters. New version with small fixes</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.08859">arXiv:2404.08859</a> <span> [<a href="https://arxiv.org/pdf/2404.08859">pdf</a>, <a href="https://arxiv.org/format/2404.08859">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: Calibrating the lithium-age relation with open clusters and associations. II. Expanded cluster sample and final membership selection </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Albarr%C3%A1n%2C+M+L+G">M. L. Guti茅rrez Albarr谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Montes%2C+D">D. Montes</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=Hern%C3%A1ndez%2C+J+I+G">J. I. Gonz谩lez Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Marfil%2C+E">E. Marfil</a>, <a href="/search/astro-ph?searchtype=author&query=Frasca%2C+A">A. Frasca</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzafame%2C+A+C">A. C. Lanzafame</a>, <a href="/search/astro-ph?searchtype=author&query=Klutsch%2C+A">A. Klutsch</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Korn%2C+A+J">A. J. Korn</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Casey%2C+A">A. Casey</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Damiani%2C+F">F. Damiani</a>, <a href="/search/astro-ph?searchtype=author&query=Feltzing%2C+S">S. Feltzing</a>, <a href="/search/astro-ph?searchtype=author&query=Fran%C3%A7ois%2C+P">P. Fran莽ois</a>, <a href="/search/astro-ph?searchtype=author&query=Esteban%2C+F+J">F. Jim茅nez Esteban</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Morbidelli%2C+L">L. Morbidelli</a>, <a href="/search/astro-ph?searchtype=author&query=Prisinzano%2C+L">L. Prisinzano</a> , et al. (4 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="2404.08859v1-abstract-short" style="display: inline;"> The Li abundance observed in pre-main sequence and main sequence late-type stars is strongly age-dependent, but also shows a complex pattern depending on several parameters, such as rotation, chromospheric activity and metallicity. The best way to calibrate these effects, with the aim of studying Li as an age indicator for FGK stars, is to calibrate coeval groups of stars, such as open clusters (O… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.08859v1-abstract-full').style.display = 'inline'; document.getElementById('2404.08859v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.08859v1-abstract-full" style="display: none;"> The Li abundance observed in pre-main sequence and main sequence late-type stars is strongly age-dependent, but also shows a complex pattern depending on several parameters, such as rotation, chromospheric activity and metallicity. The best way to calibrate these effects, with the aim of studying Li as an age indicator for FGK stars, is to calibrate coeval groups of stars, such as open clusters (OCs) and associations. We present a considerable target sample of 42 OCs and associations, ranging from 1 Myr to 5 Gyr, observed within the Gaia-ESO survey (GES), and using the latest data provided by GES iDR6 and the most recent release of Gaia that was then available, EDR3. As part of this study, we update and improve the membership analysis for all 20 OCs presented in our previous article. We perform detailed membership analyses for all target clusters to identify likely candidates, using all available parameters provided by GES and based on numerous criteria: from radial velocity distributions, to the astrometry and photometry provided by Gaia, to gravity indicators, [Fe/H] metallicity, and Li content. We obtain updated lists of cluster members for the whole target sample, as well as a selection of Li-rich giant contaminants obtained as an additional result of the membership process. Each selection of cluster candidates was thoroughly contrasted with numerous existing membership studies using data from Gaia to ensure the most robust results. These final cluster selections will be used in the third and last paper of this series, which reports the results of a comparative study characterising the observable Li dispersion in each cluster and analysing its dependence on several parameters, allowing us to calibrate a Li-age relation and obtain a series of empirical Li envelopes for key ages in our sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.08859v1-abstract-full').style.display = 'none'; document.getElementById('2404.08859v1-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> 12 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">83 pages, 246 figures. To be published in A&A, accepted January 27, 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/2402.06076">arXiv:2402.06076</a> <span> [<a href="https://arxiv.org/pdf/2402.06076">pdf</a>, <a href="https://arxiv.org/format/2402.06076">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: The DR5 analysis of the medium-resolution GIRAFFE and high-resolution UVES spectra of FGK-type stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Worley%2C+C+C">C. C. Worley</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Frasca%2C+A">A. Frasca</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Montes%2C+D">D. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Feuillet%2C+D+K">D. K. Feuillet</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=Hern%C3%A1ndez%2C+J+I+G">J. I. Gonz谩lez Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Villanova%2C+S">S. Villanova</a>, <a href="/search/astro-ph?searchtype=author&query=Mikolaitis%2C+%C5%A0">艩. Mikolaitis</a>, <a href="/search/astro-ph?searchtype=author&query=Lind%2C+K">K. Lind</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvai%C5%A1ien%C4%97%2C+G">G. Tautvai拧ien臈</a>, <a href="/search/astro-ph?searchtype=author&query=Casey%2C+A+R">A. R. Casey</a>, <a href="/search/astro-ph?searchtype=author&query=Korn%2C+A+J">A. J. Korn</a>, <a href="/search/astro-ph?searchtype=author&query=Bonifacio%2C+P">P. Bonifacio</a>, <a href="/search/astro-ph?searchtype=author&query=Soubiran%2C+C">C. Soubiran</a>, <a href="/search/astro-ph?searchtype=author&query=Caffau%2C+E">E. Caffau</a>, <a href="/search/astro-ph?searchtype=author&query=Guiglion%2C+G">G. Guiglion</a>, <a href="/search/astro-ph?searchtype=author&query=Merle%2C+T">T. Merle</a>, <a href="/search/astro-ph?searchtype=author&query=Hourihane%2C+A">A. Hourihane</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Fran%C3%A7ois%2C+P">P. Fran莽ois</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a> , et al. (20 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="2402.06076v1-abstract-short" style="display: inline;"> The Gaia-ESO Survey is an European Southern Observatory (ESO) public spectroscopic survey that targeted $10^5$ stars in the Milky Way covering the major populations of the disk, bulge and halo. The observations were made using FLAMES on the VLT obtaining both UVES high ($R\sim47,000$) and GIRAFFE medium ($R\sim20,000$) resolution spectra. The analysis of the Gaia-ESO spectra was the work of mult… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.06076v1-abstract-full').style.display = 'inline'; document.getElementById('2402.06076v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.06076v1-abstract-full" style="display: none;"> The Gaia-ESO Survey is an European Southern Observatory (ESO) public spectroscopic survey that targeted $10^5$ stars in the Milky Way covering the major populations of the disk, bulge and halo. The observations were made using FLAMES on the VLT obtaining both UVES high ($R\sim47,000$) and GIRAFFE medium ($R\sim20,000$) resolution spectra. The analysis of the Gaia-ESO spectra was the work of multiple analysis teams (nodes) within five working groups (WG). The homogenisation of the stellar parameters within WG11 (high resolution observations of FGK stars) and the homogenisation of the stellar parameters within WG10 (medium resolution observations of FGK stars) is described here. In both cases, the homogenisation was carried out using a bayesian Inference method developed specifically for the Gaia-ESO Survey by WG11. The WG10 homogenisation primarily used the cross-match of stars with WG11 as the reference set in both the stellar parameter and chemical abundance homogenisation. In this way the WG10 homogenised results have been placed directly onto the WG11 stellar parameter and chemical abundance scales. The reference set for the metal-poor end was sparse which limited the effectiveness of the homogenisation in that regime. For WG11, the total number of stars for which stellar parameters were derived was 6,231 with typical uncertainties for Teff, log g and [Fe/H] of 32~K, 0.05 and 0.05 respectively. One or more chemical abundances out of a possible 39 elements were derived for 6,188 of the stars. For WG10, the total number of stars for which stellar parameters were derived was 76,675 with typical uncertainties for Teff, log g and [Fe/H] of 64~K, 0.15 and 0.07 respectively. One or more chemical abundances out of a possible 30 elements were derived for 64,177 of the stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.06076v1-abstract-full').style.display = 'none'; document.getElementById('2402.06076v1-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> 8 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">31 pages, 19 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/2311.08358">arXiv:2311.08358</a> <span> [<a href="https://arxiv.org/pdf/2311.08358">pdf</a>, <a href="https://arxiv.org/format/2311.08358">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: 3D dynamics of young groups and clusters from GES and Gaia EDR3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wright%2C+N+J">Nicholas J. Wright</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffries%2C+R+D">R. D. Jeffries</a>, <a href="/search/astro-ph?searchtype=author&query=Jackson%2C+R+J">R. J. Jackson</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+G+G">G. G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Arnold%2C+B">Becky Arnold</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Morbidelli%2C+L">L. Morbidelli</a>, <a href="/search/astro-ph?searchtype=author&query=Prisinzano%2C+L">L. Prisinzano</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Worley%2C+C+C">Clare C. Worley</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="2311.08358v2-abstract-short" style="display: inline;"> We present the first large-scale 3D kinematic study of ~2000 spectroscopically-confirmed young stars (<20 Myr) in 18 star clusters and OB associations (hereafter groups) from the combination of Gaia astrometry and Gaia-ESO Survey spectroscopy. We measure 3D velocity dispersions for all groups, which range from 0.61 to 7.4 km/s (1D velocity dispersions of 0.35 to 4.3 km/s). We find the majority of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.08358v2-abstract-full').style.display = 'inline'; document.getElementById('2311.08358v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.08358v2-abstract-full" style="display: none;"> We present the first large-scale 3D kinematic study of ~2000 spectroscopically-confirmed young stars (<20 Myr) in 18 star clusters and OB associations (hereafter groups) from the combination of Gaia astrometry and Gaia-ESO Survey spectroscopy. We measure 3D velocity dispersions for all groups, which range from 0.61 to 7.4 km/s (1D velocity dispersions of 0.35 to 4.3 km/s). We find the majority of groups have anisotropic velocity dispersions, suggesting they are not dynamically relaxed. From the 3D velocity dispersions, measured radii and estimates of total mass we estimate the virial state and find that all systems are super-virial when only the stellar mass is considered, but that some systems are sub-virial when the mass of the molecular cloud is taken into account. We observe an approximately linear correlation between the 3D velocity dispersion and the group mass, which would imply that the virial state of groups scales as the square root of the group mass. However, we do not observe a strong correlation between virial state and group mass. In agreement with their virial state we find that nearly all of the groups studied are in the process of expanding and that the expansion is anisotropic, implying that groups were not spherical prior to expansion. One group, Rho Oph, is found to be contracting and in a sub-virial state (when the mass of the surrounding molecular cloud is considered). This work provides a glimpse of the potential of the combination of Gaia and data from the next generation of spectroscopic surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.08358v2-abstract-full').style.display = 'none'; document.getElementById('2311.08358v2-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </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, 15 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.03199">arXiv:2311.03199</a> <span> [<a href="https://arxiv.org/pdf/2311.03199">pdf</a>, <a href="https://arxiv.org/format/2311.03199">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Quantifying Interstellar Extinction at High Galactic Latitudes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=O%27Callaghan%2C+M">Matthew O'Callaghan</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">Gerry Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Mandel%2C+K+S">Kaisey S. Mandel</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="2311.03199v3-abstract-short" style="display: inline;"> A detailed map of the distribution of dust at high Galactic latitudes is essential for future cosmic microwave background (CMB) polarization experiments because the dust, while diffuse, remains a significant foreground in these regions. We develop a Bayesian model to identify a region of the Hertzsprung-Russell (HR) diagram suited to constrain the single-star extinction accurately at high Galactic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.03199v3-abstract-full').style.display = 'inline'; document.getElementById('2311.03199v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.03199v3-abstract-full" style="display: none;"> A detailed map of the distribution of dust at high Galactic latitudes is essential for future cosmic microwave background (CMB) polarization experiments because the dust, while diffuse, remains a significant foreground in these regions. We develop a Bayesian model to identify a region of the Hertzsprung-Russell (HR) diagram suited to constrain the single-star extinction accurately at high Galactic latitudes. Using photometry from Gaia, 2MASS and ALLWISE, and parallax from Gaia, we employ nested sampling to fit the model to the data and analyse the posterior over stellar parameters for both synthetic and real data. Charting low variations in extinction is complex due to systematic errors and degeneracies between extinction and other stellar parameters. The systematic errors can be minimised by restricting our data to a region of the HR diagram where the stellar models are most accurate. Moreover, the degeneracies can be reduced by including astrophysical priors and spectroscopic constraints. We show that accounting for the measurement error of the data and the assumed inaccuracies of the stellar models are critical in accurately recovering small variations in extinction. We compare the posterior distribution for individual stars with spectroscopic stellar parameter estimates from LAMOST and Gaia ESO and illustrate the importance of estimating extinction and effective temperature as a joint solution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.03199v3-abstract-full').style.display = 'none'; document.getElementById('2311.03199v3-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </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">24 pages, 13 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.15107">arXiv:2310.15107</a> <span> [<a href="https://arxiv.org/pdf/2310.15107">pdf</a>, <a href="https://arxiv.org/format/2310.15107">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Assembling a high-precision abundance catalogue of solar twins in GALAH for phylogenetic studies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Walsen%2C+K">Kurt Walsen</a>, <a href="/search/astro-ph?searchtype=author&query=Jofr%C3%A9%2C+P">Paula Jofr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Buder%2C+S">Sven Buder</a>, <a href="/search/astro-ph?searchtype=author&query=Yaxley%2C+K">Keaghan Yaxley</a>, <a href="/search/astro-ph?searchtype=author&query=Das%2C+P">Payel Das</a>, <a href="/search/astro-ph?searchtype=author&query=Yates%2C+R">Robert Yates</a>, <a href="/search/astro-ph?searchtype=author&query=Hua%2C+X">Xia Hua</a>, <a href="/search/astro-ph?searchtype=author&query=Signor%2C+T">Theosamuele Signor</a>, <a href="/search/astro-ph?searchtype=author&query=Eldridge%2C+C">Camilla Eldridge</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Arriagada%2C+A">Alvaro Rojas-Arriagada</a>, <a href="/search/astro-ph?searchtype=author&query=Tissera%2C+P">Patricia Tissera</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+E">Evelyn Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilera-G%C3%B3mez%2C+C">Claudia Aguilera-G贸mez</a>, <a href="/search/astro-ph?searchtype=author&query=Zoccali%2C+M">Manuela Zoccali</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">Gerry Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Foley%2C+R">Robert Foley</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="2310.15107v2-abstract-short" style="display: inline;"> Stellar chemical abundances have proved themselves a key source of information for understanding the evolution of the Milky Way, and the scale of major stellar surveys such as GALAH have massively increased the amount of chemical data available. However, progress is hampered by the level of precision in chemical abundance data as well as the visualization methods for comparing the multidimensional… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.15107v2-abstract-full').style.display = 'inline'; document.getElementById('2310.15107v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.15107v2-abstract-full" style="display: none;"> Stellar chemical abundances have proved themselves a key source of information for understanding the evolution of the Milky Way, and the scale of major stellar surveys such as GALAH have massively increased the amount of chemical data available. However, progress is hampered by the level of precision in chemical abundance data as well as the visualization methods for comparing the multidimensional outputs of chemical evolution models to stellar abundance data. Machine learning methods have greatly improved the former; while the application of tree-building or phylogenetic methods borrowed from biology are beginning to show promise with the latter. Here we analyse a sample of GALAH solar twins to address these issues. We apply The Cannon algorithm to generate a catalogue of about 40,000 solar twins with 14 high precision abundances which we use to perform a phylogenetic analysis on a selection of stars that have two different ranges of eccentricities. From our analyses we are able to find a group with mostly stars on circular orbits and some old stars with eccentric orbits whose age-[Y/Mg] relation agrees remarkably well with the chemical clocks published by previous high precision abundance studies. Our results show the power of combining survey data with machine learning and phylogenetics to reconstruct the history of the Milky Way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.15107v2-abstract-full').style.display = 'none'; document.getElementById('2310.15107v2-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </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 in MNRAS journal. Associated catalog of high precision, Cannon-rederived abundances for GALAH solar twins to be made publicly available upon publication and available now upon request. See Manea et al. 2023 for a complementary, high precision, Cannon-rederived abundance catalog for GALAH red giant stars</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.12235">arXiv:2310.12235</a> <span> [<a href="https://arxiv.org/pdf/2310.12235">pdf</a>, <a href="https://arxiv.org/format/2310.12235">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> On the evolutionary history of a simulated disc galaxy as seen by phylogenetic trees </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Silva%2C+D+d+B">Danielle de Brito Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Jofr%C3%A9%2C+P">Paula Jofr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Tissera%2C+P+B">Patricia B. Tissera</a>, <a href="/search/astro-ph?searchtype=author&query=Yaxley%2C+K+J">Keaghan J. Yaxley</a>, <a href="/search/astro-ph?searchtype=author&query=Jara%2C+J+G">Jenny Gonzalez Jara</a>, <a href="/search/astro-ph?searchtype=author&query=Eldridge%2C+C+J+L">Camilla J. L. Eldridge</a>, <a href="/search/astro-ph?searchtype=author&query=Sillero%2C+E">Emanuel Sillero</a>, <a href="/search/astro-ph?searchtype=author&query=Yates%2C+R+M">Robert M. Yates</a>, <a href="/search/astro-ph?searchtype=author&query=Hua%2C+X">Xia Hua</a>, <a href="/search/astro-ph?searchtype=author&query=Das%2C+P">Payel Das</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilera-G%C3%B3mez%2C+C">Claudia Aguilera-G贸mez</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+E+J">Evelyn J. Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Arriagada%2C+A">Alvaro Rojas-Arriagada</a>, <a href="/search/astro-ph?searchtype=author&query=Foley%2C+R">Robert Foley</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">Gerard Gilmore</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="2310.12235v1-abstract-short" style="display: inline;"> Phylogenetic methods have long been used in biology, and more recently have been extended to other fields - for example, linguistics and technology - to study evolutionary histories. Galaxies also have an evolutionary history, and fall within this broad phylogenetic framework. Under the hypothesis that chemical abundances can be used as a proxy for interstellar medium's DNA, phylogenetic methods a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.12235v1-abstract-full').style.display = 'inline'; document.getElementById('2310.12235v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.12235v1-abstract-full" style="display: none;"> Phylogenetic methods have long been used in biology, and more recently have been extended to other fields - for example, linguistics and technology - to study evolutionary histories. Galaxies also have an evolutionary history, and fall within this broad phylogenetic framework. Under the hypothesis that chemical abundances can be used as a proxy for interstellar medium's DNA, phylogenetic methods allow us to reconstruct hierarchical similarities and differences among stars - essentially a tree of evolutionary relationships and thus history. In this work, we apply phylogenetic methods to a simulated disc galaxy obtained with a chemo-dynamical code to test the approach. We found that at least 100 stellar particles are required to reliably portray the evolutionary history of a selected stellar population in this simulation, and that the overall evolutionary history is reliably preserved when the typical uncertainties in the chemical abundances are smaller than 0.08 dex. The results show that the shape of the trees are strongly affected by the age-metallicity relation, as well as the star formation history of the galaxy. We found that regions with low star formation rates produce shorter trees than regions with high star formation rates. Our analysis demonstrates that phylogenetic methods can shed light on the process of galaxy evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.12235v1-abstract-full').style.display = 'none'; document.getElementById('2310.12235v1-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> 18 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </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 ApJ, October 12th 2023</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.06551">arXiv:2310.06551</a> <span> [<a href="https://arxiv.org/pdf/2310.06551">pdf</a>, <a href="https://arxiv.org/format/2310.06551">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202347203">10.1051/0004-6361/202347203 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Focused Product Release: Sources from Service Interface Function image analysis -- Half a million new sources in omega Centauri </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Weingrill%2C+K">K. Weingrill</a>, <a href="/search/astro-ph?searchtype=author&query=Mints%2C+A">A. Mints</a>, <a href="/search/astro-ph?searchtype=author&query=Casta%C3%B1eda%2C+J">J. Casta帽eda</a>, <a href="/search/astro-ph?searchtype=author&query=Kostrzewa-Rutkowska%2C+Z">Z. Kostrzewa-Rutkowska</a>, <a href="/search/astro-ph?searchtype=author&query=Davidson%2C+M">M. Davidson</a>, <a href="/search/astro-ph?searchtype=author&query=De+Angeli%2C+F">F. De Angeli</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J">J. Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Torra%2C+F">F. Torra</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos-Lerate%2C+M">M. Ramos-Lerate</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Crowley%2C+C">C. Crowley</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Lindegren%2C+L">L. Lindegren</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADn-Fleitas%2C+J+M">J. M. Mart铆n-Fleitas</a>, <a href="/search/astro-ph?searchtype=author&query=Palaversa%2C+L">L. Palaversa</a>, <a href="/search/astro-ph?searchtype=author&query=Mieres%2C+D+R">D. Ruz Mieres</a>, <a href="/search/astro-ph?searchtype=author&query=Tisani%C4%87%2C+K">K. Tisani膰</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Barbier%2C+A">A. Barbier</a> , et al. (378 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="2310.06551v2-abstract-short" style="display: inline;"> Gaia's readout window strategy is challenged by very dense fields in the sky. Therefore, in addition to standard Gaia observations, full Sky Mapper (SM) images were recorded for nine selected regions in the sky. A new software pipeline exploits these Service Interface Function (SIF) images of crowded fields (CFs), making use of the availability of the full two-dimensional (2D) information. This ne… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06551v2-abstract-full').style.display = 'inline'; document.getElementById('2310.06551v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.06551v2-abstract-full" style="display: none;"> Gaia's readout window strategy is challenged by very dense fields in the sky. Therefore, in addition to standard Gaia observations, full Sky Mapper (SM) images were recorded for nine selected regions in the sky. A new software pipeline exploits these Service Interface Function (SIF) images of crowded fields (CFs), making use of the availability of the full two-dimensional (2D) information. This new pipeline produced half a million additional Gaia sources in the region of the omega Centauri ($蠅$ Cen) cluster, which are published with this Focused Product Release. We discuss the dedicated SIF CF data reduction pipeline, validate its data products, and introduce their Gaia archive table. Our aim is to improve the completeness of the {\it Gaia} source inventory in a very dense region in the sky, $蠅$ Cen. An adapted version of {\it Gaia}'s Source Detection and Image Parameter Determination software located sources in the 2D SIF CF images. We validated the results by comparing them to the public {\it Gaia} DR3 catalogue and external Hubble Space Telescope data. With this Focused Product Release, 526\,587 new sources have been added to the {\it Gaia} catalogue in $蠅$ Cen. Apart from positions and brightnesses, the additional catalogue contains parallaxes and proper motions, but no meaningful colour information. While SIF CF source parameters generally have a lower precision than nominal {\it Gaia} sources, in the cluster centre they increase the depth of the combined catalogue by three magnitudes and improve the source density by a factor of ten. This first SIF CF data publication already adds great value to the {\it Gaia} catalogue. It demonstrates what to expect for the fourth {\it Gaia} catalogue, which will contain additional sources for all nine SIF CF regions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06551v2-abstract-full').style.display = 'none'; document.getElementById('2310.06551v2-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> 8 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 680, A35 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.06295">arXiv:2310.06295</a> <span> [<a href="https://arxiv.org/pdf/2310.06295">pdf</a>, <a href="https://arxiv.org/format/2310.06295">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey 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/10.1051/0004-6361/202347273">10.1051/0004-6361/202347273 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Focused Product Release: A catalogue of sources around quasars to search for strongly lensed quasars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Krone-Martins%2C+A">A. Krone-Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Ducourant%2C+C">C. Ducourant</a>, <a href="/search/astro-ph?searchtype=author&query=Galluccio%2C+L">L. Galluccio</a>, <a href="/search/astro-ph?searchtype=author&query=Delchambre%2C+L">L. Delchambre</a>, <a href="/search/astro-ph?searchtype=author&query=Oreshina-Slezak%2C+I">I. Oreshina-Slezak</a>, <a href="/search/astro-ph?searchtype=author&query=Teixeira%2C+R">R. Teixeira</a>, <a href="/search/astro-ph?searchtype=author&query=Braine%2C+J">J. Braine</a>, <a href="/search/astro-ph?searchtype=author&query=Campion%2C+J+-+L">J. -F. Le Campion</a>, <a href="/search/astro-ph?searchtype=author&query=Mignard%2C+F">F. Mignard</a>, <a href="/search/astro-ph?searchtype=author&query=Roux%2C+W">W. Roux</a>, <a href="/search/astro-ph?searchtype=author&query=Blazere%2C+A">A. Blazere</a>, <a href="/search/astro-ph?searchtype=author&query=Pegoraro%2C+L">L. Pegoraro</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Barbier%2C+A">A. Barbier</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Guerra%2C+R">R. Guerra</a> , et al. (376 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="2310.06295v1-abstract-short" style="display: inline;"> Context. Strongly lensed quasars are fundamental sources for cosmology. The Gaia space mission covers the entire sky with the unprecedented resolution of $0.18$" in the optical, making it an ideal instrument to search for gravitational lenses down to the limiting magnitude of 21. Nevertheless, the previous Gaia Data Releases are known to be incomplete for small angular separations such as those ex… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06295v1-abstract-full').style.display = 'inline'; document.getElementById('2310.06295v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.06295v1-abstract-full" style="display: none;"> Context. Strongly lensed quasars are fundamental sources for cosmology. The Gaia space mission covers the entire sky with the unprecedented resolution of $0.18$" in the optical, making it an ideal instrument to search for gravitational lenses down to the limiting magnitude of 21. Nevertheless, the previous Gaia Data Releases are known to be incomplete for small angular separations such as those expected for most lenses. Aims. We present the Data Processing and Analysis Consortium GravLens pipeline, which was built to analyse all Gaia detections around quasars and to cluster them into sources, thus producing a catalogue of secondary sources around each quasar. We analysed the resulting catalogue to produce scores that indicate source configurations that are compatible with strongly lensed quasars. Methods. GravLens uses the DBSCAN unsupervised clustering algorithm to detect sources around quasars. The resulting catalogue of multiplets is then analysed with several methods to identify potential gravitational lenses. We developed and applied an outlier scoring method, a comparison between the average BP and RP spectra of the components, and we also used an extremely randomised tree algorithm. These methods produce scores to identify the most probable configurations and to establish a list of lens candidates. Results. We analysed the environment of 3 760 032 quasars. A total of 4 760 920 sources, including the quasars, were found within 6" of the quasar positions. This list is given in the Gaia archive. In 87\% of cases, the quasar remains a single source, and in 501 385 cases neighbouring sources were detected. We propose a list of 381 lensed candidates, of which we identified 49 as the most promising. Beyond these candidates, the associate tables in this Focused Product Release allow the entire community to explore the unique Gaia data for strong lensing studies further. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06295v1-abstract-full').style.display = 'none'; document.getElementById('2310.06295v1-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> 10 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </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">35 pages, 60 figures, accepted for publication by Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 685, A130 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.06051">arXiv:2310.06051</a> <span> [<a href="https://arxiv.org/pdf/2310.06051">pdf</a>, <a href="https://arxiv.org/format/2310.06051">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Gaia Focused Product Release: Radial velocity time series of long-period variables </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Trabucchi%2C+M">M. Trabucchi</a>, <a href="/search/astro-ph?searchtype=author&query=Mowlavi%2C+N">N. Mowlavi</a>, <a href="/search/astro-ph?searchtype=author&query=Lebzelter%2C+T">T. Lebzelter</a>, <a href="/search/astro-ph?searchtype=author&query=Lecoeur-Taibi%2C+I">I. Lecoeur-Taibi</a>, <a href="/search/astro-ph?searchtype=author&query=Audard%2C+M">M. Audard</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Lario%2C+P">P. Garc铆a-Lario</a>, <a href="/search/astro-ph?searchtype=author&query=Gavras%2C+P">P. Gavras</a>, <a href="/search/astro-ph?searchtype=author&query=Holl%2C+B">B. Holl</a>, <a href="/search/astro-ph?searchtype=author&query=de+Fombelle%2C+G+J">G. Jevardat de Fombelle</a>, <a href="/search/astro-ph?searchtype=author&query=Nienartowicz%2C+K">K. Nienartowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Rimoldini%2C+L">L. Rimoldini</a>, <a href="/search/astro-ph?searchtype=author&query=Sartoretti%2C+P">P. Sartoretti</a>, <a href="/search/astro-ph?searchtype=author&query=Blomme%2C+R">R. Blomme</a>, <a href="/search/astro-ph?searchtype=author&query=Fr%C3%A9mat%2C+Y">Y. Fr茅mat</a>, <a href="/search/astro-ph?searchtype=author&query=Marchal%2C+O">O. Marchal</a>, <a href="/search/astro-ph?searchtype=author&query=Damerdji%2C+Y">Y. Damerdji</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Guerrier%2C+A">A. Guerrier</a>, <a href="/search/astro-ph?searchtype=author&query=Panuzzo%2C+P">P. Panuzzo</a>, <a href="/search/astro-ph?searchtype=author&query=Katz%2C+D">D. Katz</a>, <a href="/search/astro-ph?searchtype=author&query=Seabroke%2C+G+M">G. M. Seabroke</a>, <a href="/search/astro-ph?searchtype=author&query=Benson%2C+K">K. Benson</a> , et al. (382 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="2310.06051v1-abstract-short" style="display: inline;"> The third Gaia Data Release (DR3) provided photometric time series of more than 2 million long-period variable (LPV) candidates. Anticipating the publication of full radial-velocity (RV) in DR4, this Focused Product Release (FPR) provides RV time series for a selection of LPVs with high-quality observations. We describe the production and content of the Gaia catalog of LPV RV time series, and the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06051v1-abstract-full').style.display = 'inline'; document.getElementById('2310.06051v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.06051v1-abstract-full" style="display: none;"> The third Gaia Data Release (DR3) provided photometric time series of more than 2 million long-period variable (LPV) candidates. Anticipating the publication of full radial-velocity (RV) in DR4, this Focused Product Release (FPR) provides RV time series for a selection of LPVs with high-quality observations. We describe the production and content of the Gaia catalog of LPV RV time series, and the methods used to compute variability parameters published in the Gaia FPR. Starting from the DR3 LPVs catalog, we applied filters to construct a sample of sources with high-quality RV measurements. We modeled their RV and photometric time series to derive their periods and amplitudes, and further refined the sample by requiring compatibility between the RV period and at least one of the $G$, $G_{\rm BP}$, or $G_{\rm RP}$ photometric periods. The catalog includes RV time series and variability parameters for 9\,614 sources in the magnitude range $6\lesssim G/{\rm mag}\lesssim 14$, including a flagged top-quality subsample of 6\,093 stars whose RV periods are fully compatible with the values derived from the $G$, $G_{\rm BP}$, and $G_{\rm RP}$ photometric time series. The RV time series contain a mean of 24 measurements per source taken unevenly over a duration of about three years. We identify the great most sources (88%) as genuine LPVs, with about half of them showing a pulsation period and the other half displaying a long secondary period. The remaining 12% consists of candidate ellipsoidal binaries. Quality checks against RVs available in the literature show excellent agreement. We provide illustrative examples and cautionary remarks. The publication of RV time series for almost 10\,000 LPVs constitutes, by far, the largest such database available to date in the literature. The availability of simultaneous photometric measurements gives a unique added value to the Gaia catalog (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06051v1-abstract-full').style.display = 'none'; document.getElementById('2310.06051v1-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> 9 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </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">36 pages, 38 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/2304.12197">arXiv:2304.12197</a> <span> [<a href="https://arxiv.org/pdf/2304.12197">pdf</a>, <a href="https://arxiv.org/ps/2304.12197">ps</a>, <a href="https://arxiv.org/format/2304.12197">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</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/10.1093/mnras/stad1293">10.1093/mnras/stad1293 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: Empirical estimates of stellar ages from lithium equivalent widths (EAGLES) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jeffries%2C+R+D">R. D. Jeffries</a>, <a href="/search/astro-ph?searchtype=author&query=Jackson%2C+R+J">R. J. Jackson</a>, <a href="/search/astro-ph?searchtype=author&query=Wright%2C+N+J">Nicholas J. Wright</a>, <a href="/search/astro-ph?searchtype=author&query=Weaver%2C+G">G. Weaver</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Korn%2C+A+J">A. J. Korn</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Casey%2C+A+R">A. R. Casey</a>, <a href="/search/astro-ph?searchtype=author&query=Frasca%2C+A">A. Frasca</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Guiglion%2C+G">G. Guiglion</a>, <a href="/search/astro-ph?searchtype=author&query=Morbidelli%2C+L">L. Morbidelli</a>, <a href="/search/astro-ph?searchtype=author&query=Prisinzano%2C+L">L. Prisinzano</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+G+G">G. G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvai%C5%A1ien%C4%97%2C+G">G. Tautvai拧ien臈</a>, <a href="/search/astro-ph?searchtype=author&query=Worley%2C+C+C">C. C. Worley</a>, <a href="/search/astro-ph?searchtype=author&query=Zaggia%2C+S">S. Zaggia</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="2304.12197v2-abstract-short" style="display: inline;"> We present an empirical model of age-dependent photospheric lithium depletion, calibrated using a large, homogeneously-analysed sample of 6200 stars in 52 open clusters, with ages from 2--6000 Myr and $-0.3<{\rm [Fe/H}]<0.2$, observed in the Gaia-ESO spectroscopic survey. The model is used to obtain age estimates and posterior age probability distributions from measurements of the Li I 6708A equiv… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.12197v2-abstract-full').style.display = 'inline'; document.getElementById('2304.12197v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.12197v2-abstract-full" style="display: none;"> We present an empirical model of age-dependent photospheric lithium depletion, calibrated using a large, homogeneously-analysed sample of 6200 stars in 52 open clusters, with ages from 2--6000 Myr and $-0.3<{\rm [Fe/H}]<0.2$, observed in the Gaia-ESO spectroscopic survey. The model is used to obtain age estimates and posterior age probability distributions from measurements of the Li I 6708A equivalent width for individual (pre) main sequence stars with $3000 < T_{\rm eff}/{\rm K} <6500$, a domain where age determination from the HR diagram is either insensitive or highly model-dependent. In the best cases, precisions of 0.1 dex in log age are achievable; even higher precision can be obtained for coeval groups and associations where the individual age probabilities of their members can be combined. The method is validated on a sample of exoplanet-hosting young stars, finding agreement with claimed young ages for some, but not others. We obtain better than 10 per cent precision in age, and excellent agreement with published ages, for seven well-studied young moving groups. The derived ages for young clusters ($<1$ Gyr) in our sample are also in good agreement with their training ages, and consistent with several published, model-insensitive lithium depletion boundary ages. For older clusters there remain systematic age errors that could be as large as a factor of two. There is no evidence to link these errors to any strong systematic metallicity dependence of (pre) main sequence lithium depletion, at least in the range $-0.29 < {\rm [Fe/H]} < 0.18$. Our methods and model are provided as software -- "Empirical AGes from Lithium Equivalent widthS" (EAGLES). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.12197v2-abstract-full').style.display = 'none'; document.getElementById('2304.12197v2-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> 25 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </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 Monthly Notices of the Royal Astronomical Society. Code available at https://github.com/robdjeff/eagles</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.07720">arXiv:2304.07720</a> <span> [<a href="https://arxiv.org/pdf/2304.07720">pdf</a>, <a href="https://arxiv.org/format/2304.07720">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202345910">10.1051/0004-6361/202345910 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: homogenisation of stellar parameters and elemental abundances </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hourihane%2C+A">A. Hourihane</a>, <a href="/search/astro-ph?searchtype=author&query=Francois%2C+P">P. Francois</a>, <a href="/search/astro-ph?searchtype=author&query=Worley%2C+C+C">C. C. Worley</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Casey%2C+A+R">A. R. Casey</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+G+G">G. G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Recio-Blanco%2C+A">A. Recio-Blanco</a>, <a href="/search/astro-ph?searchtype=author&query=Korn%2C+A+J">A. J. Korn</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=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Blomme%2C+R">R. Blomme</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Walton%2C+N+A">N. A. Walton</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Eck%2C+S">S. Van Eck</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzafame%2C+A">A Lanzafame</a>, <a href="/search/astro-ph?searchtype=author&query=Frasca%2C+A">A. Frasca</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Damiani%2C+F">F. Damiani</a>, <a href="/search/astro-ph?searchtype=author&query=Lind%2C+K">K. Lind</a>, <a href="/search/astro-ph?searchtype=author&query=Bergemann%2C+M">M. Bergemann</a>, <a href="/search/astro-ph?searchtype=author&query=Bonifacio%2C+P">P. Bonifacio</a> , et al. (37 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="2304.07720v1-abstract-short" style="display: inline;"> The Gaia-ESO Survey is a public spectroscopic survey that has targeted $\gtrsim10^5$ stars covering all major components of the Milky Way from the end of 2011 to 2018, delivering its public final release in May 2022. Unlike other spectroscopic surveys, Gaia-ESO is the only survey that observed stars across all spectral types with dedicated, specialised analyses: from O (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.07720v1-abstract-full').style.display = 'inline'; document.getElementById('2304.07720v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.07720v1-abstract-full" style="display: none;"> The Gaia-ESO Survey is a public spectroscopic survey that has targeted $\gtrsim10^5$ stars covering all major components of the Milky Way from the end of 2011 to 2018, delivering its public final release in May 2022. Unlike other spectroscopic surveys, Gaia-ESO is the only survey that observed stars across all spectral types with dedicated, specialised analyses: from O ($T_\mathrm{eff} \sim 30,000-52,000$~K) all the way to K-M ($\gtrsim$3,500~K). The physics throughout these stellar regimes varies significantly, which has previously prohibited any detailed comparisons between stars of significantly different type. In the final data release (internal data release 6) of the Gaia-ESO Survey, we provide the final database containing a large number of products such as radial velocities, stellar parameters and elemental abundances, rotational velocity, and also, e.g., activity and accretion indicators in young stars and membership probability in star clusters for more than 114,000 stars. The spectral analysis is coordinated by a number of Working Groups (WGs) within the Survey, which specialise in the various stellar samples. Common targets are analysed across WGs to allow for comparisons (and calibrations) amongst instrumental setups and spectral types. Here we describe the procedures employed to ensure all Survey results are placed on a common scale to arrive at a single set of recommended results for all Survey collaborators to use. We also present some general quality and consistency checks performed over all Survey results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.07720v1-abstract-full').style.display = 'none'; document.getElementById('2304.07720v1-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> 16 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </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">A&A accepted, minor revision, 36 pages, 38 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 676, A129 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.14132">arXiv:2211.14132</a> <span> [<a href="https://arxiv.org/pdf/2211.14132">pdf</a>, <a href="https://arxiv.org/format/2211.14132">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202245230">10.1051/0004-6361/202245230 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: Probing the lithium abundances in old metal-rich dwarf stars in the Solar vicinity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dantas%2C+M+L+L">M. L. L. Dantas</a>, <a href="/search/astro-ph?searchtype=author&query=Guiglion%2C+G">G. Guiglion</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Romano%2C+D">D. Romano</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Chiappini%2C+C">C. Chiappini</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Nepal%2C+S">S. Nepal</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvai%C5%A1ien%C4%97%2C+G">G. Tautvai拧ien臈</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzafame%2C+A+C">A. C. Lanzafame</a>, <a href="/search/astro-ph?searchtype=author&query=Heiter%2C+U">U. Heiter</a>, <a href="/search/astro-ph?searchtype=author&query=Morbidelli%2C+L">L. Morbidelli</a>, <a href="/search/astro-ph?searchtype=author&query=Prisinzano%2C+L">L. Prisinzano</a>, <a href="/search/astro-ph?searchtype=author&query=Zaggia%2C+S">S. Zaggia</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="2211.14132v2-abstract-short" style="display: inline;"> We test a scenario in which radial migration could affect the Li abundance pattern of dwarf stars in the solar neighbourhood. This may confirm that the Li abundance in these stars can not serve as a probe for the Li abundance in the interstellar medium. We use the high-quality data (including Li abundances) from the 6th internal Data Release of the Gaia-ESO survey. In this sample, we group stars b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.14132v2-abstract-full').style.display = 'inline'; document.getElementById('2211.14132v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.14132v2-abstract-full" style="display: none;"> We test a scenario in which radial migration could affect the Li abundance pattern of dwarf stars in the solar neighbourhood. This may confirm that the Li abundance in these stars can not serve as a probe for the Li abundance in the interstellar medium. We use the high-quality data (including Li abundances) from the 6th internal Data Release of the Gaia-ESO survey. In this sample, we group stars by similarity in chemical abundances via hierarchical clustering. Our analysis treats both measured Li abundances and upper limits. The Li envelope of the previously identified radially migrated stars is well below the benchmark meteoritic value (<3.26 dex); the star with the highest detected abundance has A(Li) = 2.76 dex. This confirms the previous trends observed for old dwarf stars (median ages $\sim$ 8 Gyr), where Li decreases for [Fe/H]$\gtrsim$0. This result acts as supporting evidence that the abundance of Li measured in the upper envelope of old dwarf stars should not be considered a proxy for the interstellar medium Li. Our scenario also indicates that the stellar yields for [M/H]>0 should not be decreased, as recently proposed in the literature. Our study backs the recent studies that claimed that old dwarfs on the hot side of the dip are efficient probes of the ISM abundance of Li, provided atomic diffusion does not lower significantly the initial Li abundance in the atmospheres of metal-rich objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.14132v2-abstract-full').style.display = 'none'; document.getElementById('2211.14132v2-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> 9 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">8 pages, 3 figures. Abridged abstract to fit ArXiv's requirements. Letter published in A&A Letters. Version after the language proofs</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 668, L7 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.15525">arXiv:2210.15525</a> <span> [<a href="https://arxiv.org/pdf/2210.15525">pdf</a>, <a href="https://arxiv.org/format/2210.15525">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1051/0004-6361/202244957">10.1051/0004-6361/202244957 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO survey: mapping the shape and evolution of the radial abundance gradients with open clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Vazquez%2C+C+V">C. Viscasillas Vazquez</a>, <a href="/search/astro-ph?searchtype=author&query=Spina%2C+L">L. Spina</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Romano%2C+D">D. Romano</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Recio-Blanco%2C+A">A. Recio-Blanco</a>, <a href="/search/astro-ph?searchtype=author&query=Nordlander%2C+T">T. Nordlander</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Orazi%2C+V">V. D'Orazi</a>, <a href="/search/astro-ph?searchtype=author&query=Baratella%2C+M">M. Baratella</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Dantas%2C+M+L+L">M. L. L. Dantas</a>, <a href="/search/astro-ph?searchtype=author&query=Pasquini%2C+L">L. Pasquini</a>, <a href="/search/astro-ph?searchtype=author&query=Spitoni%2C+E">E. Spitoni</a>, <a href="/search/astro-ph?searchtype=author&query=Casali%2C+G">G. Casali</a>, <a href="/search/astro-ph?searchtype=author&query=Van+der+Swaelmen%2C+M">M. Van der Swaelmen</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Stonkute%2C+E">E. Stonkute</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+S+F+G+G">S. Feltzing. G. G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Heiter%2C+U">U. Heiter</a>, <a href="/search/astro-ph?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Bergemann%2C+M">M. Bergemann</a> , et al. (5 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="2210.15525v1-abstract-short" style="display: inline;"> The spatial distribution of elemental abundances and their time evolution are among the major constraints to disentangle the scenarios of formation and evolution of the Galaxy. We used the sample of open clusters available in the final release of the Gaia-ESO survey to trace the Galactic radial abundance and abundance to iron ratio gradients, and their time evolution. We selected member stars in 6… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.15525v1-abstract-full').style.display = 'inline'; document.getElementById('2210.15525v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.15525v1-abstract-full" style="display: none;"> The spatial distribution of elemental abundances and their time evolution are among the major constraints to disentangle the scenarios of formation and evolution of the Galaxy. We used the sample of open clusters available in the final release of the Gaia-ESO survey to trace the Galactic radial abundance and abundance to iron ratio gradients, and their time evolution. We selected member stars in 62 open clusters, with ages from 0.1 to about 7~Gyr, located in the Galactic thin disc at Galactocentric radii from about 6 to 21~kpc. We analysed the shape of the resulting [Fe/H] gradient, the average gradients [El/H] and [El/Fe] combining elements belonging to four different nucleosynthesis channels, and their individual abundance and abundance ratio gradients. We also investigated the time evolution of the gradients dividing open clusters in three age bins. The[Fe/H] gradient has a slope of -0.054 dex~kpc-1. We saw different behaviours for elements belonging to different channels. We found that the youngest clusters in the inner disc have lower metallicity than their older counterpart and they outline a flatter gradient. We considered some possible explanations, including the effects of gas inflow and migration. We suggested that it might be a bias introduced by the standard spectroscopic analysis producing lower metallicities in low gravity stars. To delineate the shape of the `true' gradient, we should limit our analysis to stars with low surface gravity logg>2.5 and xi<1.8 km~s-1. Based on this reduced sample, we can conclude that the gradient has minimally evolved over the time-frame outlined by the open clusters, indicating a slow and stationary formation of the thin disc in the latest Gyr. We found a secondary role of clusters' migration in shaping the gradient, with a more prominent role of migration for the oldest clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.15525v1-abstract-full').style.display = 'none'; document.getElementById('2210.15525v1-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 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">25 pages, 14 figures and 4 tables in the main text, 3 figures and 7 tables in the Appendix. 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 669, A119 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.08510">arXiv:2210.08510</a> <span> [<a href="https://arxiv.org/pdf/2210.08510">pdf</a>, <a href="https://arxiv.org/format/2210.08510">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </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/10.1051/0004-6361/202243667">10.1051/0004-6361/202243667 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: Old super-metal-rich visitors from the inner Galaxy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dantas%2C+M+L+L">M. L. L. Dantas</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Boesso%2C+R">R. Boesso</a>, <a href="/search/astro-ph?searchtype=author&query=Rocha-Pinto%2C+H+J">H. J. Rocha-Pinto</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Guiglion%2C+G">G. Guiglion</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvai%C5%A1ien%C4%97%2C+G">G. Tautvai拧ien臈</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Bergemann%2C+M">M. Bergemann</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Jofr%C3%A9%2C+P">P. Jofr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Zaggia%2C+S">S. Zaggia</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="2210.08510v3-abstract-short" style="display: inline;"> We report the identification of a set of old super metal-rich dwarf stars with orbits of low eccentricity that reach a maximum height from the Galactic plane between ~0.5-1.5 kpc. We discuss their properties to understand their origins. We use data from the internal data release 6 of the Gaia-ESO Survey. We selected stars observed at high resolution with abundances of 21 species of 18 individual e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.08510v3-abstract-full').style.display = 'inline'; document.getElementById('2210.08510v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.08510v3-abstract-full" style="display: none;"> We report the identification of a set of old super metal-rich dwarf stars with orbits of low eccentricity that reach a maximum height from the Galactic plane between ~0.5-1.5 kpc. We discuss their properties to understand their origins. We use data from the internal data release 6 of the Gaia-ESO Survey. We selected stars observed at high resolution with abundances of 21 species of 18 individual elements. We apply hierarchical clustering to group the stars with similar chemical abundances within the complete chemical abundance space. According to their chemical properties, this set of super metal-rich stars can be arranged into five subgroups. Four seem to follow a chemical enrichment flow, where nearly all abundances increase in lockstep with Fe. The fifth subgroup shows different chemical characteristics. All subgroups have the following features: median ages of the order of 7-9 Gyr, Solar or sub-Solar [Mg/Fe] ratios, maximum height between 0.5-1.5 kpc, low eccentricities, and a detachment from the expected metallicity gradient with guiding radius. The high metallicity of our stars is incompatible with a formation in the Solar neighbourhood. Their dynamic properties agree with theoretical expectations that these stars travelled from the inner Galaxy due to blurring and, most importantly, to churning. We suggest that most of this population's stars originated in the Milky Way's inner regions (inner disc and/or the bulge) and later migrated to the Solar neighbourhood. The region from where the stars originated had a complex chemical enrichment history, with contributions from supernovae types Ia and II and possibly asymptotic giant branch stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.08510v3-abstract-full').style.display = 'none'; document.getElementById('2210.08510v3-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 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">18 pages, 13 figures. Accepted for publication in A&A. Version after language proofs. The catalogue remains to be released. Abridged abstract to fit arxiv's requirements</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 669, A96 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.04721">arXiv:2210.04721</a> <span> [<a href="https://arxiv.org/pdf/2210.04721">pdf</a>, <a href="https://arxiv.org/format/2210.04721">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202244854">10.1051/0004-6361/202244854 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: Lithium measurements and new curves of growth </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=de+Laverny%2C+P">P. de Laverny</a>, <a href="/search/astro-ph?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Feuillet%2C+D+K">D. K. Feuillet</a>, <a href="/search/astro-ph?searchtype=author&query=Frasca%2C+A">A. Frasca</a>, <a href="/search/astro-ph?searchtype=author&query=Lind%2C+K">K. Lind</a>, <a href="/search/astro-ph?searchtype=author&query=Prisinzano%2C+L">L. Prisinzano</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvai%C5%A1ien%C4%97%2C+G">G. Tautvai拧ien臈</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzafame%2C+A+C">A. C. Lanzafame</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Guiglion%2C+G">G. Guiglion</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+G+G">G. G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Sanna%2C+N">N. Sanna</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Bonifacio%2C+P">P. Bonifacio</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffries%2C+R+D">R. D. Jeffries</a>, <a href="/search/astro-ph?searchtype=author&query=Micela%2C+G">G. Micela</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a> , et al. (15 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="2210.04721v1-abstract-short" style="display: inline;"> The Gaia-ESO Survey (GES) is a large public spectroscopic survey that was carried out using the multi-object FLAMES spectrograph at the Very Large Telescope. The survey provides accurate radial velocities, stellar parameters, and elemental abundances for ~115,000 stars in all Milky Way components. In this paper we describe the method adopted in the final data release to derive lithium equivalent w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.04721v1-abstract-full').style.display = 'inline'; document.getElementById('2210.04721v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.04721v1-abstract-full" style="display: none;"> The Gaia-ESO Survey (GES) is a large public spectroscopic survey that was carried out using the multi-object FLAMES spectrograph at the Very Large Telescope. The survey provides accurate radial velocities, stellar parameters, and elemental abundances for ~115,000 stars in all Milky Way components. In this paper we describe the method adopted in the final data release to derive lithium equivalent widths (EWs) and abundances. Lithium EWs were measured using two different approaches for FGK and M-type stars, to account for the intrinsic differences in the spectra. For FGK stars, we fitted the lithium line using Gaussian components, while direct integration over a predefined interval was adopted for M-type stars. Care was taken to ensure continuity between the two regimes. Abundances were derived using a new set of homogeneous curves of growth that were derived specifically for GES, and which were measured on a synthetic spectral grid consistently with the way the EWs were measured. The derived abundances were validated by comparison with those measured by other analysis groups using different methods. Lithium EWs were measured for ~40,000 stars, and abundances could be derived for ~38,000 of them. The vast majority of the measures (80%) have been obtained for stars in open cluster fields. The remaining objects are stars in globular clusters, or field stars in the Milky Way disc, bulge, and halo. The GES dataset of homogeneous lithium abundances described here will be valuable for our understanding of several processes, from stellar evolution and internal mixing in stars at different evolutionary stages to Galactic evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.04721v1-abstract-full').style.display = 'none'; document.getElementById('2210.04721v1-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> 10 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">15 pages, 15 figures. Accepted by Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 668, A49 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.08874">arXiv:2208.08874</a> <span> [<a href="https://arxiv.org/pdf/2208.08874">pdf</a>, <a href="https://arxiv.org/format/2208.08874">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1051/0004-6361/202244765">10.1051/0004-6361/202244765 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: Preparing the ground for 4MOST & WEAVE galactic surveys. Chemical evolution of lithium with machine learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nepal%2C+S">S. Nepal</a>, <a href="/search/astro-ph?searchtype=author&query=Guiglion%2C+G">G. Guiglion</a>, <a href="/search/astro-ph?searchtype=author&query=de+Jong%2C+R+S">R. S. de Jong</a>, <a href="/search/astro-ph?searchtype=author&query=Valentini%2C+M">M. Valentini</a>, <a href="/search/astro-ph?searchtype=author&query=Chiappini%2C+C">C. Chiappini</a>, <a href="/search/astro-ph?searchtype=author&query=Steinmetz%2C+M">M. Steinmetz</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosch%2C+M">M. Ambrosch</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffries%2C+R+D">R. D. Jeffries</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Romano%2C+D">D. Romano</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Dantas%2C+M+L+L">M. L. L. Dantas</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Bergemann%2C+M">M. Bergemann</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Jim%C3%A9nez-Esteban%2C+F">F. Jim茅nez-Esteban</a>, <a href="/search/astro-ph?searchtype=author&query=Jofr%C3%A9%2C+P">P. Jofr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Morbidelli%2C+L">L. Morbidelli</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+G+G">G. G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvai%C5%A1ien%C4%97%2C+G">G. Tautvai拧ien臈</a>, <a href="/search/astro-ph?searchtype=author&query=Zaggia%2C+S">S. Zaggia</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="2208.08874v2-abstract-short" style="display: inline;"> With its origin coming from several sources (Big Bang, stars, cosmic rays) and given its strong depletion during its stellar lifetime, the lithium element is of great interest as its chemical evolution in the Milky Way is not well understood at present. To help constrain stellar and galactic chemical evolution models, numerous and precise lithium abundances are necessary for a large range of evolu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.08874v2-abstract-full').style.display = 'inline'; document.getElementById('2208.08874v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.08874v2-abstract-full" style="display: none;"> With its origin coming from several sources (Big Bang, stars, cosmic rays) and given its strong depletion during its stellar lifetime, the lithium element is of great interest as its chemical evolution in the Milky Way is not well understood at present. To help constrain stellar and galactic chemical evolution models, numerous and precise lithium abundances are necessary for a large range of evolutionary stages, metallicities, and Galactic volume. In the age of stellar parametrization on industrial scales, spectroscopic surveys such as APOGEE, GALAH, RAVE, and LAMOST have used data-driven methods to rapidly and precisely infer stellar labels (atmospheric parameters and abundances). To prepare the ground for future spectroscopic surveys such as 4MOST and WEAVE, we aim to apply machine learning techniques to lithium measurements and analyses. We trained a convolution neural network (CNN), coupling Gaia-ESO Survey iDR6 stellar labels (Teff, log(g), [Fe/H], and A(Li)) and GIRAFFE HR15N spectra, to infer the atm parameters and lithium abundances for ~40,000 stars. We show that the CNN properly learns the physics of the stellar labels, from relevant spectral features through a broad range of evolutionary stages and stellar parameters. The Li feature at 6707.8 A is successfully singled out by our CNN, among the thousands of lines. Rare objects such as Li-rich giants are found in our sample. This level of performance is achieved thanks to a meticulously built, high-quality, and homogeneous training sample. The CNN approach is very well adapted for the next generations of spectroscopic surveys aimed at studying (among other elements) lithium, such as the 4MIDABLE-LR/HR (4MOST Milky Way disk and bulge low- and high-resolution) surveys. In this context, the caveats of ML applications should be appropriately investigated, along with the realistic label uncertainties and upper limits for abundances. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.08874v2-abstract-full').style.display = 'none'; document.getElementById('2208.08874v2-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 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 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">A&A, accepted 05 December 2022, 23 pages, 23 figures. Codes and trained models available at https://github.com/SamirNepal/Li\_CNN\_2022</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 671, A61 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.08872">arXiv:2208.08872</a> <span> [<a href="https://arxiv.org/pdf/2208.08872">pdf</a>, <a href="https://arxiv.org/format/2208.08872">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1051/0004-6361/202244766">10.1051/0004-6361/202244766 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: Chemical evolution of Mg and Al in the Milky Way with Machine-Learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ambrosch%2C+M">M. Ambrosch</a>, <a href="/search/astro-ph?searchtype=author&query=Guiglion%2C+G">G. Guiglion</a>, <a href="/search/astro-ph?searchtype=author&query=Mikolaitis%2C+%C5%A0">艩. Mikolaitis</a>, <a href="/search/astro-ph?searchtype=author&query=Chiappini%2C+C">C. Chiappini</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvai%C5%A1ien%C4%97%2C+G">G. Tautvai拧ien臈</a>, <a href="/search/astro-ph?searchtype=author&query=Nepal%2C+S">S. Nepal</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Bergemann%2C+M">M. Bergemann</a>, <a href="/search/astro-ph?searchtype=author&query=Morbidelli%2C+L">L. Morbidelli</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+G+G">G. G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Zaggia%2C+S">S. Zaggia</a>, <a href="/search/astro-ph?searchtype=author&query=Jofr%C3%A9%2C+P">P. Jofr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Jim%C3%A9nez-Esteban%2C+F+M">F. M. Jim茅nez-Esteban</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="2208.08872v1-abstract-short" style="display: inline;"> We aim to prepare the machine-learning ground for the next generation of spectroscopic surveys, such as 4MOST and WEAVE. Our goal is to show that convolutional neural networks can predict accurate stellar labels from relevant spectral features in a physically meaningful way. We built a neural network and trained it on GIRAFFE spectra with associated stellar labels from the sixth internal Gaia-ESO… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.08872v1-abstract-full').style.display = 'inline'; document.getElementById('2208.08872v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.08872v1-abstract-full" style="display: none;"> We aim to prepare the machine-learning ground for the next generation of spectroscopic surveys, such as 4MOST and WEAVE. Our goal is to show that convolutional neural networks can predict accurate stellar labels from relevant spectral features in a physically meaningful way. We built a neural network and trained it on GIRAFFE spectra with associated stellar labels from the sixth internal Gaia-ESO data release. Our neural network predicts the atmospheric parameters Teff and log(g) as well as the chemical abundances [Mg/Fe], [Al/Fe], and [Fe/H] for 30115 stellar spectra. The scatter of predictions from eight slightly different network models shows a high internal precision of the network results: 24 K for Teff, 0.03 for log(g), 0.02 dex for [Mg/Fe], 0.03 dex for [Al/Fe], and 0.02 dex for [Fe/H]. The network gradients reveal that the network is inferring the labels in a physically meaningful way from spectral features. Validation with benchmark stars and several scientific applications confirm that our network predictions are accurate for individual stars and recover the properties of different stellar populations in the Milky Way galaxy. Such a study provides very good insights into the application of machine-learning for the spectral analysis of large-scale spectroscopic surveys, such as WEAVE and 4MIDABLE-LR and -HR (4MOST Milky Way disk and bulge low- and high-resolution). The community will have to put a substantial effort into building proactive training sets for machine-learning methods to minimize the possible systematics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.08872v1-abstract-full').style.display = 'none'; document.getElementById('2208.08872v1-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> 18 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">Submitted to 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 672, A46 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.05432">arXiv:2208.05432</a> <span> [<a href="https://arxiv.org/pdf/2208.05432">pdf</a>, <a href="https://arxiv.org/format/2208.05432">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202243134">10.1051/0004-6361/202243134 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Public Spectroscopic Survey: Motivation, implementation, GIRAFFE data processing, analysis, and final data products </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Worley%2C+C+C">C. C. Worley</a>, <a href="/search/astro-ph?searchtype=author&query=Hourihane%2C+A">A. Hourihane</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+G+G">G. G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+J+R">J. R. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Francois%2C+P">P. Francois</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffries%2C+R+D">R. D. Jeffries</a>, <a href="/search/astro-ph?searchtype=author&query=Koposov%2C+S+E">S. E. Koposov</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</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=Blomme%2C+R">R. Blomme</a>, <a href="/search/astro-ph?searchtype=author&query=Korn%2C+A+J">A. J. Korn</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzafame%2C+A+C">A. C. Lanzafame</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Recio-Blanco%2C+A">A. Recio-Blanco</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Eck%2C+S">S. Van Eck</a>, <a href="/search/astro-ph?searchtype=author&query=Zwitter%2C+T">T. Zwitter</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Flaccomio%2C+E">E. Flaccomio</a>, <a href="/search/astro-ph?searchtype=author&query=Irwin%2C+M+J">M. J. Irwin</a> , et al. (143 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="2208.05432v1-abstract-short" style="display: inline;"> The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100,000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.05432v1-abstract-full').style.display = 'inline'; document.getElementById('2208.05432v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.05432v1-abstract-full" style="display: none;"> The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100,000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper (arXiv:2206.02901) introduces the survey results. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. The Gaia-ESO Survey obtained 202,000 spectra of 115,000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.05432v1-abstract-full').style.display = 'none'; document.getElementById('2208.05432v1-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> 10 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">38 pages. A&A in press</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 666, A120 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.00211">arXiv:2208.00211</a> <span> [<a href="https://arxiv.org/pdf/2208.00211">pdf</a>, <a href="https://arxiv.org/format/2208.00211">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1051/0004-6361/202243940">10.1051/0004-6361/202243940 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 3: Summary of the content and survey properties </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Ducourant%2C+C">C. Ducourant</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Guerra%2C+R">R. Guerra</a>, <a href="/search/astro-ph?searchtype=author&query=Hutton%2C+A">A. Hutton</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a>, <a href="/search/astro-ph?searchtype=author&query=Klioner%2C+S+A">S. A. Klioner</a>, <a href="/search/astro-ph?searchtype=author&query=Lammers%2C+U+L">U. L. Lammers</a>, <a href="/search/astro-ph?searchtype=author&query=Lindegren%2C+L">L. Lindegren</a>, <a href="/search/astro-ph?searchtype=author&query=Luri%2C+X">X. Luri</a>, <a href="/search/astro-ph?searchtype=author&query=Mignard%2C+F">F. Mignard</a>, <a href="/search/astro-ph?searchtype=author&query=Panem%2C+C">C. Panem</a>, <a href="/search/astro-ph?searchtype=author&query=Pourbaix%2C+D">D. Pourbaix</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Sartoretti%2C+P">P. Sartoretti</a>, <a href="/search/astro-ph?searchtype=author&query=Soubiran%2C+C">C. Soubiran</a> , et al. (431 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="2208.00211v1-abstract-short" style="display: inline;"> We present the third data release of the European Space Agency's Gaia mission, GDR3. The GDR3 catalogue is the outcome of the processing of raw data collected with the Gaia instruments during the first 34 months of the mission by the Gaia Data Processing and Analysis Consortium. The GDR3 catalogue contains the same source list, celestial positions, proper motions, parallaxes, and broad band photom… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.00211v1-abstract-full').style.display = 'inline'; document.getElementById('2208.00211v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.00211v1-abstract-full" style="display: none;"> We present the third data release of the European Space Agency's Gaia mission, GDR3. The GDR3 catalogue is the outcome of the processing of raw data collected with the Gaia instruments during the first 34 months of the mission by the Gaia Data Processing and Analysis Consortium. The GDR3 catalogue contains the same source list, celestial positions, proper motions, parallaxes, and broad band photometry in the G, G$_{BP}$, and G$_{RP}$ pass-bands already present in the Early Third Data Release. GDR3 introduces an impressive wealth of new data products. More than 33 million objects in the ranges $G_{rvs} < 14$ and $3100 <T_{eff} <14500 $, have new determinations of their mean radial velocities based on data collected by Gaia. We provide G$_{rvs}$ magnitudes for most sources with radial velocities, and a line broadening parameter is listed for a subset of these. Mean Gaia spectra are made available to the community. The GDR3 catalogue includes about 1 million mean spectra from the radial velocity spectrometer, and about 220 million low-resolution blue and red prism photometer BPRP mean spectra. The results of the analysis of epoch photometry are provided for some 10 million sources across 24 variability types. GDR3 includes astrophysical parameters and source class probabilities for about 470 million and 1500 million sources, respectively, including stars, galaxies, and quasars. Orbital elements and trend parameters are provided for some $800\,000$ astrometric, spectroscopic and eclipsing binaries. More than $150\,000$ Solar System objects, including new discoveries, with preliminary orbital solutions and individual epoch observations are part of this release. Reflectance spectra derived from the epoch BPRP spectral data are published for about 60\,000 asteroids. Finally, an additional data set is provided, namely the Gaia Andromeda Photometric Survey (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.00211v1-abstract-full').style.display = 'none'; document.getElementById('2208.00211v1-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> 30 July, 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">23 pages, 2 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/2207.12792">arXiv:2207.12792</a> <span> [<a href="https://arxiv.org/pdf/2207.12792">pdf</a>, <a href="https://arxiv.org/format/2207.12792">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202244112">10.1051/0004-6361/202244112 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO survey: A spectroscopic study of the young open cluster NGC 3293 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Morel%2C+T">T. Morel</a>, <a href="/search/astro-ph?searchtype=author&query=Blaz%C3%A8re%2C+A">A. Blaz猫re</a>, <a href="/search/astro-ph?searchtype=author&query=Semaan%2C+T">T. Semaan</a>, <a href="/search/astro-ph?searchtype=author&query=Gosset%2C+E">E. Gosset</a>, <a href="/search/astro-ph?searchtype=author&query=Zorec%2C+J">J. Zorec</a>, <a href="/search/astro-ph?searchtype=author&query=Fr%C3%A9mat%2C+Y">Y. Fr茅mat</a>, <a href="/search/astro-ph?searchtype=author&query=Blomme%2C+R">R. Blomme</a>, <a href="/search/astro-ph?searchtype=author&query=Daflon%2C+S">S. Daflon</a>, <a href="/search/astro-ph?searchtype=author&query=Lobel%2C+A">A. Lobel</a>, <a href="/search/astro-ph?searchtype=author&query=Nieva%2C+M+F">M. F. Nieva</a>, <a href="/search/astro-ph?searchtype=author&query=Przybilla%2C+N">N. Przybilla</a>, <a href="/search/astro-ph?searchtype=author&query=Gebran%2C+M">M. Gebran</a>, <a href="/search/astro-ph?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/astro-ph?searchtype=author&query=Mahy%2C+L">L. Mahy</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+W">W. Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvai%C5%A1ien%C4%97%2C+G">G. Tautvai拧ien臈</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Bergemann%2C+M">M. Bergemann</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Damiani%2C+F">F. Damiani</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Morbidelli%2C+L">L. Morbidelli</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a> , et al. (2 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="2207.12792v1-abstract-short" style="display: inline;"> We present a spectroscopic analysis of the GIRAFFE and UVES data collected by the Gaia-ESO survey for the young open cluster NGC 3293. Archive spectra from the same instruments obtained in the framework of the `VLT-FLAMES survey of massive stars' are also analysed. Atmospheric parameters, non-LTE chemical abundances for six elements, or variability information are reported for a total of about 160… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12792v1-abstract-full').style.display = 'inline'; document.getElementById('2207.12792v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.12792v1-abstract-full" style="display: none;"> We present a spectroscopic analysis of the GIRAFFE and UVES data collected by the Gaia-ESO survey for the young open cluster NGC 3293. Archive spectra from the same instruments obtained in the framework of the `VLT-FLAMES survey of massive stars' are also analysed. Atmospheric parameters, non-LTE chemical abundances for six elements, or variability information are reported for a total of about 160 B stars spanning a wide range in terms of spectral types (B1 to B9.5) and rotation rate (up to 350 km/s). We take advantage of the multi-epoch observations to detect several binary systems or intrinsically line-profile variables. A deconvolution algorithm is used to infer the current, true (deprojected) rotational velocity distribution. We find a broad, Gaussian-like distribution peaking around 200-250 km/s. Although some stars populate the high-velocity tail, most stars in the cluster appear to rotate far from critical. We discuss the chemical properties of the cluster, including the low occurrence of abundance peculiarities in the late B stars and the paucity of objects showing CN-cycle burning products at their surface. We argue that the former result can largely be explained by the inhibition of diffusion effects because of fast rotation, while the latter is generally in accord with the predictions of single-star evolutionary models under the assumption of a wide range of initial spin rates at the onset of main-sequence evolution. However, we find some evidence for a less efficient mixing in two quite rapidly rotating stars that are among the most massive objects in our sample. Finally, we obtain a cluster age of ~20 Myrs through a detailed, star-to-star correction of our results for the effect of stellar rotation. This is significantly older than previous estimates from turn-off fitting that fully relied on classical, non-rotating isochrones. [abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12792v1-abstract-full').style.display = 'none'; document.getElementById('2207.12792v1-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 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">29 pages, 24 figures, 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 665, A108 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.12174">arXiv:2206.12174</a> <span> [<a href="https://arxiv.org/pdf/2206.12174">pdf</a>, <a href="https://arxiv.org/format/2206.12174">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> </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/10.1051/0004-6361/202243791">10.1051/0004-6361/202243791 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 3: Reflectance spectra of Solar System small bodies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Galluccio%2C+L">L. Galluccio</a>, <a href="/search/astro-ph?searchtype=author&query=Delbo%2C+M">M. Delbo</a>, <a href="/search/astro-ph?searchtype=author&query=De+Angeli%2C+F">F. De Angeli</a>, <a href="/search/astro-ph?searchtype=author&query=Pauwels%2C+T">T. Pauwels</a>, <a href="/search/astro-ph?searchtype=author&query=Tanga%2C+P">P. Tanga</a>, <a href="/search/astro-ph?searchtype=author&query=Mignard%2C+F">F. Mignard</a>, <a href="/search/astro-ph?searchtype=author&query=Cellino%2C+A">A. Cellino</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Muinonen%2C+K">K. Muinonen</a>, <a href="/search/astro-ph?searchtype=author&query=Penttila%2C+A">A. Penttila</a>, <a href="/search/astro-ph?searchtype=author&query=Jordan%2C+S">S. Jordan</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Ducourant%2C+C">C. Ducourant</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Guerra%2C+R">R. Guerra</a>, <a href="/search/astro-ph?searchtype=author&query=Hutton%2C+A">A. Hutton</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a> , et al. (422 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="2206.12174v1-abstract-short" style="display: inline;"> The Gaia mission of the European Space Agency (ESA) has been routinely observing Solar System objects (SSOs) since the beginning of its operations in August 2014. The Gaia data release three (DR3) includes, for the first time, the mean reflectance spectra of a selected sample of 60 518 SSOs, primarily asteroids, observed between August 5, 2014, and May 28, 2017. Each reflectance spectrum was deriv… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.12174v1-abstract-full').style.display = 'inline'; document.getElementById('2206.12174v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.12174v1-abstract-full" style="display: none;"> The Gaia mission of the European Space Agency (ESA) has been routinely observing Solar System objects (SSOs) since the beginning of its operations in August 2014. The Gaia data release three (DR3) includes, for the first time, the mean reflectance spectra of a selected sample of 60 518 SSOs, primarily asteroids, observed between August 5, 2014, and May 28, 2017. Each reflectance spectrum was derived from measurements obtained by means of the Blue and Red photometers (BP/RP), which were binned in 16 discrete wavelength bands. We describe the processing of the Gaia spectral data of SSOs, explaining both the criteria used to select the subset of asteroid spectra published in Gaia DR3, and the different steps of our internal validation procedures. In order to further assess the quality of Gaia SSO reflectance spectra, we carried out external validation against SSO reflectance spectra obtained from ground-based and space-borne telescopes and available in the literature. For each selected SSO, an epoch reflectance was computed by dividing the calibrated spectrum observed by the BP/RP at each transit on the focal plane by the mean spectrum of a solar analogue. The latter was obtained by averaging the Gaia spectral measurements of a selected sample of stars known to have very similar spectra to that of the Sun. Finally, a mean of the epoch reflectance spectra was calculated in 16 spectral bands for each SSO. The agreement between Gaia mean reflectance spectra and those available in the literature is good for bright SSOs, regardless of their taxonomic spectral class. We identify an increase in the spectral slope of S-type SSOs with increasing phase angle. Moreover, we show that the spectral slope increases and the depth of the 1 um absorption band decreases for increasing ages of S-type asteroid families. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.12174v1-abstract-full').style.display = 'none'; document.getElementById('2206.12174v1-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">30 pages, 26 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/2206.06207">arXiv:2206.06207</a> <span> [<a href="https://arxiv.org/pdf/2206.06207">pdf</a>, <a href="https://arxiv.org/format/2206.06207">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1051/0004-6361/202243797">10.1051/0004-6361/202243797 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 3: Mapping the asymmetric disc of the Milky Way </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Drimmel%2C+R">R. Drimmel</a>, <a href="/search/astro-ph?searchtype=author&query=Romero-Gomez%2C+M">M. Romero-Gomez</a>, <a href="/search/astro-ph?searchtype=author&query=Chemin%2C+L">L. Chemin</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos%2C+P">P. Ramos</a>, <a href="/search/astro-ph?searchtype=author&query=Poggio%2C+E">E. Poggio</a>, <a href="/search/astro-ph?searchtype=author&query=Ripepi%2C+V">V. Ripepi</a>, <a href="/search/astro-ph?searchtype=author&query=Andrae%2C+R">R. Andrae</a>, <a href="/search/astro-ph?searchtype=author&query=Blomme%2C+R">R. Blomme</a>, <a href="/search/astro-ph?searchtype=author&query=Cantat-Gaudin%2C+T">T. Cantat-Gaudin</a>, <a href="/search/astro-ph?searchtype=author&query=Castro-Ginard%2C+A">A. Castro-Ginard</a>, <a href="/search/astro-ph?searchtype=author&query=Clementini%2C+G">G. Clementini</a>, <a href="/search/astro-ph?searchtype=author&query=Figueras%2C+F">F. Figueras</a>, <a href="/search/astro-ph?searchtype=author&query=Fouesneau%2C+M">M. Fouesneau</a>, <a href="/search/astro-ph?searchtype=author&query=Fremat%2C+Y">Y. Fremat</a>, <a href="/search/astro-ph?searchtype=author&query=Jardine%2C+K">K. Jardine</a>, <a href="/search/astro-ph?searchtype=author&query=Khanna%2C+S">S. Khanna</a>, <a href="/search/astro-ph?searchtype=author&query=Lobel%2C+A">A. Lobel</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+D+J">D. J. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Muraveva%2C+T">T. Muraveva</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a> , et al. (431 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="2206.06207v3-abstract-short" style="display: inline;"> With the most recent Gaia data release the number of sources with complete 6D phase space information (position and velocity) has increased to well over 33 million stars, while stellar astrophysical parameters are provided for more than 470 million sources, in addition to the identification of over 11 million variable stars. Using the astrophysical parameters and variability classifications provid… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.06207v3-abstract-full').style.display = 'inline'; document.getElementById('2206.06207v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.06207v3-abstract-full" style="display: none;"> With the most recent Gaia data release the number of sources with complete 6D phase space information (position and velocity) has increased to well over 33 million stars, while stellar astrophysical parameters are provided for more than 470 million sources, in addition to the identification of over 11 million variable stars. Using the astrophysical parameters and variability classifications provided in Gaia DR3, we select various stellar populations to explore and identify non-axisymmetric features in the disc of the Milky Way in both configuration and velocity space. Using more about 580 thousand sources identified as hot OB stars, together with 988 known open clusters younger than 100 million years, we map the spiral structure associated with star formation 4-5 kpc from the Sun. We select over 2800 Classical Cepheids younger than 200 million years, which show spiral features extending as far as 10 kpc from the Sun in the outer disc. We also identify more than 8.7 million sources on the red giant branch (RGB), of which 5.7 million have line-of-sight velocities, allowing the velocity field of the Milky Way to be mapped as far as 8 kpc from the Sun, including the inner disc. The spiral structure revealed by the young populations is consistent with recent results using Gaia EDR3 astrometry and source lists based on near infrared photometry, showing the Local (Orion) arm to be at least 8 kpc long, and an outer arm consistent with what is seen in HI surveys, which seems to be a continuation of the Perseus arm into the third quadrant. Meanwhile, the subset of RGB stars with velocities clearly reveals the large scale kinematic signature of the bar in the inner disc, as well as evidence of streaming motions in the outer disc that might be associated with spiral arms or bar resonances. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.06207v3-abstract-full').style.display = 'none'; document.getElementById('2206.06207v3-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> 5 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">35 pages, 27 figures, accepted for publication in A&A special Gaia DR3 issue. V2: abstract completed. V3: complete author list and link to data: https://drive.google.com/drive/u/1/folders/1yOJPjYmM7QK5XVsqaiSOTuwDQNti2LlZ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A37 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.06205">arXiv:2206.06205</a> <span> [<a href="https://arxiv.org/pdf/2206.06205">pdf</a>, <a href="https://arxiv.org/format/2206.06205">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/10.1051/0004-6361/202243880">10.1051/0004-6361/202243880 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 3: External calibration of BP/RP low-resolution spectroscopic data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Montegriffo%2C+P">P. Montegriffo</a>, <a href="/search/astro-ph?searchtype=author&query=De+Angeli%2C+F">F. De Angeli</a>, <a href="/search/astro-ph?searchtype=author&query=Andrae%2C+R">R. Andrae</a>, <a href="/search/astro-ph?searchtype=author&query=Riello%2C+M">M. Riello</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Sanna%2C+N">N. Sanna</a>, <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+M">M. Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Carrasco%2C+J+M">J. M. Carrasco</a>, <a href="/search/astro-ph?searchtype=author&query=Sordo%2C+R">R. Sordo</a>, <a href="/search/astro-ph?searchtype=author&query=Busso%2C+G">G. Busso</a>, <a href="/search/astro-ph?searchtype=author&query=Cacciari%2C+C">C. Cacciari</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+F">F. van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Altavilla%2C+G">G. Altavilla</a>, <a href="/search/astro-ph?searchtype=author&query=Barstow%2C+M+A">M. A. Barstow</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Burgess%2C+P+W">P. W. Burgess</a>, <a href="/search/astro-ph?searchtype=author&query=Castellani%2C+M">M. Castellani</a>, <a href="/search/astro-ph?searchtype=author&query=Cowell%2C+S">S. Cowell</a>, <a href="/search/astro-ph?searchtype=author&query=Davidson%2C+M">M. Davidson</a>, <a href="/search/astro-ph?searchtype=author&query=De+Luise%2C+F">F. De Luise</a>, <a href="/search/astro-ph?searchtype=author&query=Delchambre%2C+L">L. Delchambre</a>, <a href="/search/astro-ph?searchtype=author&query=Diener%2C+C">C. Diener</a> , et al. (24 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="2206.06205v1-abstract-short" style="display: inline;"> Context. Gaia Data Release 3 contains astrometry and photometry results for about 1.8 billion sources based on observations collected by the European Space Agency (ESA) Gaia satellite during the first 34 months of its operational phase (the same period covered Gaia early Data Release 3; Gaia EDR3). Low-resolution spectra for 220 million sources are one of the important new data products included i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.06205v1-abstract-full').style.display = 'inline'; document.getElementById('2206.06205v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.06205v1-abstract-full" style="display: none;"> Context. Gaia Data Release 3 contains astrometry and photometry results for about 1.8 billion sources based on observations collected by the European Space Agency (ESA) Gaia satellite during the first 34 months of its operational phase (the same period covered Gaia early Data Release 3; Gaia EDR3). Low-resolution spectra for 220 million sources are one of the important new data products included in this release. Aims. In this paper, we focus on the external calibration of low-resolution spectroscopic content, describing the input data, algorithms, data processing, and the validation of the results. Particular attention is given to the quality of the data and to a number of features that users may need to take into account to make the best use of the catalogue. Methods. We calibrated an instrument model to relate mean Gaia spectra to the corresponding spectral energy distributions using an extended set of calibrators: this includes modelling of the instrument dispersion relation, transmission, and line spread functions. Optimisation of the model is achieved through total least-squares regression, accounting for errors in Gaia and external spectra. Results. The resulting instrument model can be used for forward modelling of Gaia spectra or for inverse modelling of externally calibrated spectra in absolute flux units. Conclusions. The absolute calibration derived in this paper provides an essential ingredient for users of BP/RP spectra. It allows users to connect BP/RP spectra to absolute fluxes and physical wavelengths. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.06205v1-abstract-full').style.display = 'none'; document.getElementById('2206.06205v1-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">33 pages, 50 figures, accepted for publication by Astronomy and Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.06143">arXiv:2206.06143</a> <span> [<a href="https://arxiv.org/pdf/2206.06143">pdf</a>, <a href="https://arxiv.org/format/2206.06143">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/10.1051/0004-6361/202243680">10.1051/0004-6361/202243680 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 3: Processing and validation of BP/RP low-resolution spectral data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=De+Angeli%2C+F">F. De Angeli</a>, <a href="/search/astro-ph?searchtype=author&query=Weiler%2C+M">M. Weiler</a>, <a href="/search/astro-ph?searchtype=author&query=Montegriffo%2C+P">P. Montegriffo</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Riello%2C+M">M. Riello</a>, <a href="/search/astro-ph?searchtype=author&query=Andrae%2C+R">R. Andrae</a>, <a href="/search/astro-ph?searchtype=author&query=Carrasco%2C+J+M">J. M. Carrasco</a>, <a href="/search/astro-ph?searchtype=author&query=Busso%2C+G">G. Busso</a>, <a href="/search/astro-ph?searchtype=author&query=Burgess%2C+P+W">P. W. Burgess</a>, <a href="/search/astro-ph?searchtype=author&query=Cacciari%2C+C">C. Cacciari</a>, <a href="/search/astro-ph?searchtype=author&query=Davidson%2C+M">M. Davidson</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+D+L">D. L. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Hodgkin%2C+S+T">S. T. Hodgkin</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a>, <a href="/search/astro-ph?searchtype=author&query=Osborne%2C+P+J">P. J. Osborne</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Altavilla%2C+G">G. Altavilla</a>, <a href="/search/astro-ph?searchtype=author&query=Barstow%2C+M+A">M. A. Barstow</a>, <a href="/search/astro-ph?searchtype=author&query=Bailer-Jones%2C+C+A+L">C. A. L. Bailer-Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+M">M. Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Castellani%2C+M">M. Castellani</a>, <a href="/search/astro-ph?searchtype=author&query=Cowell%2C+S">S. Cowell</a>, <a href="/search/astro-ph?searchtype=author&query=Delchambre%2C+L">L. Delchambre</a>, <a href="/search/astro-ph?searchtype=author&query=De+Luise%2C+F">F. De Luise</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="2206.06143v1-abstract-short" style="display: inline;"> (Abridged) Blue (BP) and Red (RP) Photometer low-resolution spectral data is one of the exciting new products in Gaia Data Release 3 (Gaia DR3). We calibrate about 65 billion individual transit spectra onto the same mean BP/RP instrument through a series of calibration steps, including background subtraction, calibration of the CCD geometry and an iterative procedure for the calibration of CCD eff… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.06143v1-abstract-full').style.display = 'inline'; document.getElementById('2206.06143v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.06143v1-abstract-full" style="display: none;"> (Abridged) Blue (BP) and Red (RP) Photometer low-resolution spectral data is one of the exciting new products in Gaia Data Release 3 (Gaia DR3). We calibrate about 65 billion individual transit spectra onto the same mean BP/RP instrument through a series of calibration steps, including background subtraction, calibration of the CCD geometry and an iterative procedure for the calibration of CCD efficiency as well as variations of the line-spread function and dispersion across the focal plane and in time. The calibrated transit spectra are then combined for each source in terms of an expansion into continuous basis functions. Time-averaged mean spectra covering the optical to near-infrared wavelength range [330, 1050] nm are published for approximately 220 million objects. Most of these are brighter than G = 17.65 but some BP/RP spectra are published for sources down to G = 21.43. Their signal- to-noise ratio varies significantly over the wavelength range covered and with magnitude and colour of the observed objects, with sources around G = 15 having S/N above 100 in some wavelength ranges. The top-quality BP/RP spectra are achieved for sources with magnitudes 9 < G < 12, having S/N reaching 1000 in the central part of the RP wavelength range. Scientific validation suggests that the internal calibration was generally successful. However, there is some evidence for imperfect calibrations at the bright end G < 11, where calibrated BP/RP spectra can exhibit systematic flux variations that exceed their estimated flux uncertainties. We also report that due to long-range noise correlations, BP/RP spectra can exhibit wiggles when sampled in pseudo-wavelength. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.06143v1-abstract-full').style.display = 'none'; document.getElementById('2206.06143v1-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">Submitted to A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.06075">arXiv:2206.06075</a> <span> [<a href="https://arxiv.org/pdf/2206.06075">pdf</a>, <a href="https://arxiv.org/format/2206.06075">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1051/0004-6361/202243767">10.1051/0004-6361/202243767 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 3: Pulsations in main sequence OBAF-type stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=De+Ridder%2C+J">J. De Ridder</a>, <a href="/search/astro-ph?searchtype=author&query=Ripepi%2C+V">V. Ripepi</a>, <a href="/search/astro-ph?searchtype=author&query=Aerts%2C+C">C. Aerts</a>, <a href="/search/astro-ph?searchtype=author&query=Palaversa%2C+L">L. Palaversa</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Holl%2C+B">B. Holl</a>, <a href="/search/astro-ph?searchtype=author&query=Audard%2C+M">M. Audard</a>, <a href="/search/astro-ph?searchtype=author&query=Rimoldini%2C+L">L. Rimoldini</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Ducourant%2C+C">C. Ducourant</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Guerra%2C+R">R. Guerra</a>, <a href="/search/astro-ph?searchtype=author&query=Hutton%2C+A">A. Hutton</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a>, <a href="/search/astro-ph?searchtype=author&query=Klioner%2C+S+A">S. A. Klioner</a>, <a href="/search/astro-ph?searchtype=author&query=Lammers%2C+U+L">U. L. Lammers</a>, <a href="/search/astro-ph?searchtype=author&query=Lindegren%2C+L">L. Lindegren</a> , et al. (423 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="2206.06075v2-abstract-short" style="display: inline;"> The third Gaia data release provides photometric time series covering 34 months for about 10 million stars. For many of those stars, a characterisation in Fourier space and their variability classification are also provided. This paper focuses on intermediate- to high-mass (IHM) main sequence pulsators M >= 1.3 Msun) of spectral types O, B, A, or F, known as beta Cep, slowly pulsating B (SPB), del… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.06075v2-abstract-full').style.display = 'inline'; document.getElementById('2206.06075v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.06075v2-abstract-full" style="display: none;"> The third Gaia data release provides photometric time series covering 34 months for about 10 million stars. For many of those stars, a characterisation in Fourier space and their variability classification are also provided. This paper focuses on intermediate- to high-mass (IHM) main sequence pulsators M >= 1.3 Msun) of spectral types O, B, A, or F, known as beta Cep, slowly pulsating B (SPB), delta Sct, and gamma Dor stars. These stars are often multi-periodic and display low amplitudes, making them challenging targets to analyse with sparse time series. All datasets used in this analysis are part of the Gaia DR3 data release. The photometric time series were used to perform a Fourier analysis, while the global astrophysical parameters necessary for the empirical instability strips were taken from the Gaia DR3 gspphot tables, and the vsini data were taken from the Gaia DR3 esphs tables. We show that for nearby OBAF-type pulsators, the Gaia DR3 data are precise and accurate enough to pinpoint them in the Hertzsprung-Russell diagram. We find empirical instability strips covering broader regions than theoretically predicted. In particular, our study reveals the presence of fast rotating gravity-mode pulsators outside the strips, as well as the co-existence of rotationally modulated variables inside the strips as reported before in the literature. We derive an extensive period-luminosity relation for delta Sct stars and provide evidence that the relation features different regimes depending on the oscillation period. Finally, we demonstrate how stellar rotation attenuates the amplitude of the dominant oscillation mode of delta Sct stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.06075v2-abstract-full').style.display = 'none'; document.getElementById('2206.06075v2-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> 16 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A36 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.05870">arXiv:2206.05870</a> <span> [<a href="https://arxiv.org/pdf/2206.05870">pdf</a>, <a href="https://arxiv.org/format/2206.05870">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202243800">10.1051/0004-6361/202243800 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 3: A Golden Sample of Astrophysical Parameters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Sarro%2C+L+M">L. M. Sarro</a>, <a href="/search/astro-ph?searchtype=author&query=Lobel%2C+A">A. Lobel</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Andrae%2C+R">R. Andrae</a>, <a href="/search/astro-ph?searchtype=author&query=Smart%2C+R+L">R. L. Smart</a>, <a href="/search/astro-ph?searchtype=author&query=Clementini%2C+G">G. Clementini</a>, <a href="/search/astro-ph?searchtype=author&query=Heiter%2C+U">U. Heiter</a>, <a href="/search/astro-ph?searchtype=author&query=Korn%2C+A+J">A. J. Korn</a>, <a href="/search/astro-ph?searchtype=author&query=Fouesneau%2C+M">M. Fouesneau</a>, <a href="/search/astro-ph?searchtype=author&query=Fr%C3%A9mat%2C+Y">Y. Fr茅mat</a>, <a href="/search/astro-ph?searchtype=author&query=De+Angeli%2C+F">F. De Angeli</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+D+L">D. L. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Th%C3%A9venin%2C+F">F. Th茅venin</a>, <a href="/search/astro-ph?searchtype=author&query=Reyl%C3%A9%2C+C">C. Reyl茅</a>, <a href="/search/astro-ph?searchtype=author&query=Sordo%2C+R">R. Sordo</a>, <a href="/search/astro-ph?searchtype=author&query=Garofalo%2C+A">A. Garofalo</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a> , et al. (423 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="2206.05870v1-abstract-short" style="display: inline;"> Gaia Data Release 3 (DR3) provides a wealth of new data products for the astronomical community to exploit, including astrophysical parameters for a half billion stars. In this work we demonstrate the high quality of these data products and illustrate their use in different astrophysical contexts. We query the astrophysical parameter tables along with other tables in Gaia DR3 to derive the samples… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05870v1-abstract-full').style.display = 'inline'; document.getElementById('2206.05870v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.05870v1-abstract-full" style="display: none;"> Gaia Data Release 3 (DR3) provides a wealth of new data products for the astronomical community to exploit, including astrophysical parameters for a half billion stars. In this work we demonstrate the high quality of these data products and illustrate their use in different astrophysical contexts. We query the astrophysical parameter tables along with other tables in Gaia DR3 to derive the samples of the stars of interest. We validate our results by using the Gaia catalogue itself and by comparison with external data. We have produced six homogeneous samples of stars with high quality astrophysical parameters across the HR diagram for the community to exploit. We first focus on three samples that span a large parameter space: young massive disk stars (~3M), FGKM spectral type stars (~3M), and UCDs (~20K). We provide these sources along with additional information (either a flag or complementary parameters) as tables that are made available in the Gaia archive. We furthermore identify 15740 bone fide carbon stars, 5863 solar-analogues, and provide the first homogeneous set of stellar parameters of the Spectro Photometric Standard Stars. We use a subset of the OBA sample to illustrate its usefulness to analyse the Milky Way rotation curve. We then use the properties of the FGKM stars to analyse known exoplanet systems. We also analyse the ages of some unseen UCD-companions to the FGKM stars. We additionally predict the colours of the Sun in various passbands (Gaia, 2MASS, WISE) using the solar-analogue sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05870v1-abstract-full').style.display = 'none'; document.getElementById('2206.05870v1-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> 12 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">35 pages, (incl 6 pages references, acknowledgements, affiliations), 37 figures, A&A accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A39 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.05681">arXiv:2206.05681</a> <span> [<a href="https://arxiv.org/pdf/2206.05681">pdf</a>, <a href="https://arxiv.org/format/2206.05681">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1051/0004-6361/202243232">10.1051/0004-6361/202243232 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 3: The extragalactic content </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Bailer-Jones%2C+C+A+L">C. A. L. Bailer-Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Teyssier%2C+D">D. Teyssier</a>, <a href="/search/astro-ph?searchtype=author&query=Delchambre%2C+L">L. Delchambre</a>, <a href="/search/astro-ph?searchtype=author&query=Ducourant%2C+C">C. Ducourant</a>, <a href="/search/astro-ph?searchtype=author&query=Garabato%2C+D">D. Garabato</a>, <a href="/search/astro-ph?searchtype=author&query=Hatzidimitriou%2C+D">D. Hatzidimitriou</a>, <a href="/search/astro-ph?searchtype=author&query=Klioner%2C+S+A">S. A. Klioner</a>, <a href="/search/astro-ph?searchtype=author&query=Rimoldini%2C+L">L. Rimoldini</a>, <a href="/search/astro-ph?searchtype=author&query=Bellas-Velidis%2C+I">I. Bellas-Velidis</a>, <a href="/search/astro-ph?searchtype=author&query=Carballo%2C+R">R. Carballo</a>, <a href="/search/astro-ph?searchtype=author&query=Carnerero%2C+M+I">M. I. Carnerero</a>, <a href="/search/astro-ph?searchtype=author&query=Diener%2C+C">C. Diener</a>, <a href="/search/astro-ph?searchtype=author&query=Fouesneau%2C+M">M. Fouesneau</a>, <a href="/search/astro-ph?searchtype=author&query=Galluccio%2C+L">L. Galluccio</a>, <a href="/search/astro-ph?searchtype=author&query=Gavras%2C+P">P. Gavras</a>, <a href="/search/astro-ph?searchtype=author&query=Krone-Martins%2C+A">A. Krone-Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Raiteri%2C+C+M">C. M. Raiteri</a>, <a href="/search/astro-ph?searchtype=author&query=Teixeira%2C+R">R. Teixeira</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a> , et al. (422 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="2206.05681v1-abstract-short" style="display: inline;"> The Gaia Galactic survey mission is designed and optimized to obtain astrometry, photometry, and spectroscopy of nearly two billion stars in our Galaxy. Yet as an all-sky multi-epoch survey, Gaia also observes several million extragalactic objects down to a magnitude of G~21 mag. Due to the nature of the Gaia onboard selection algorithms, these are mostly point-source-like objects. Using data prov… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05681v1-abstract-full').style.display = 'inline'; document.getElementById('2206.05681v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.05681v1-abstract-full" style="display: none;"> The Gaia Galactic survey mission is designed and optimized to obtain astrometry, photometry, and spectroscopy of nearly two billion stars in our Galaxy. Yet as an all-sky multi-epoch survey, Gaia also observes several million extragalactic objects down to a magnitude of G~21 mag. Due to the nature of the Gaia onboard selection algorithms, these are mostly point-source-like objects. Using data provided by the satellite, we have identified quasar and galaxy candidates via supervised machine learning methods, and estimate their redshifts using the low resolution BP/RP spectra. We further characterise the surface brightness profiles of host galaxies of quasars and of galaxies from pre-defined input lists. Here we give an overview of the processing of extragalactic objects, describe the data products in Gaia DR3, and analyse their properties. Two integrated tables contain the main results for a high completeness, but low purity (50-70%), set of 6.6 million candidate quasars and 4.8 million candidate galaxies. We provide queries that select purer sub-samples of these containing 1.9 million probable quasars and 2.9 million probable galaxies (both 95% purity). We also use high quality BP/RP spectra of 43 thousand high probability quasars over the redshift range 0.05-4.36 to construct a composite quasar spectrum spanning restframe wavelengths from 72-100 nm. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05681v1-abstract-full').style.display = 'none'; document.getElementById('2206.05681v1-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> 12 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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 to A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.05595">arXiv:2206.05595</a> <span> [<a href="https://arxiv.org/pdf/2206.05595">pdf</a>, <a href="https://arxiv.org/format/2206.05595">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202243782">10.1051/0004-6361/202243782 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 3: Stellar multiplicity, a teaser for the hidden treasure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Barstow%2C+M+A">M. A. Barstow</a>, <a href="/search/astro-ph?searchtype=author&query=Faigler%2C+S">S. Faigler</a>, <a href="/search/astro-ph?searchtype=author&query=Jorissen%2C+A">A. Jorissen</a>, <a href="/search/astro-ph?searchtype=author&query=Kervella%2C+P">P. Kervella</a>, <a href="/search/astro-ph?searchtype=author&query=Mazeh%2C+T">T. Mazeh</a>, <a href="/search/astro-ph?searchtype=author&query=Mowlavi%2C+N">N. Mowlavi</a>, <a href="/search/astro-ph?searchtype=author&query=Panuzzo%2C+P">P. Panuzzo</a>, <a href="/search/astro-ph?searchtype=author&query=Sahlmann%2C+J">J. Sahlmann</a>, <a href="/search/astro-ph?searchtype=author&query=Shahaf%2C+S">S. Shahaf</a>, <a href="/search/astro-ph?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bauchet%2C+N">N. Bauchet</a>, <a href="/search/astro-ph?searchtype=author&query=Damerdji%2C+Y">Y. Damerdji</a>, <a href="/search/astro-ph?searchtype=author&query=Gavras%2C+P">P. Gavras</a>, <a href="/search/astro-ph?searchtype=author&query=Giacobbe%2C+P">P. Giacobbe</a>, <a href="/search/astro-ph?searchtype=author&query=Gosset%2C+E">E. Gosset</a>, <a href="/search/astro-ph?searchtype=author&query=Halbwachs%2C+J+-">J. -L. Halbwachs</a>, <a href="/search/astro-ph?searchtype=author&query=Holl%2C+B">B. Holl</a>, <a href="/search/astro-ph?searchtype=author&query=Lattanzi%2C+M+G">M. G. Lattanzi</a>, <a href="/search/astro-ph?searchtype=author&query=Leclerc%2C+N">N. Leclerc</a>, <a href="/search/astro-ph?searchtype=author&query=Morel%2C+T">T. Morel</a>, <a href="/search/astro-ph?searchtype=author&query=Pourbaix%2C+D">D. Pourbaix</a>, <a href="/search/astro-ph?searchtype=author&query=Fiorentin%2C+P+R">P. Re Fiorentin</a> , et al. (425 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="2206.05595v1-abstract-short" style="display: inline;"> The Gaia DR3 Catalogue contains for the first time about eight hundred thousand solutions with either orbital elements or trend parameters for astrometric, spectroscopic and eclipsing binaries, and combinations of them. This paper aims to illustrate the huge potential of this large non-single star catalogue. Using the orbital solutions together with models of the binaries, a catalogue of tens of t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05595v1-abstract-full').style.display = 'inline'; document.getElementById('2206.05595v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.05595v1-abstract-full" style="display: none;"> The Gaia DR3 Catalogue contains for the first time about eight hundred thousand solutions with either orbital elements or trend parameters for astrometric, spectroscopic and eclipsing binaries, and combinations of them. This paper aims to illustrate the huge potential of this large non-single star catalogue. Using the orbital solutions together with models of the binaries, a catalogue of tens of thousands of stellar masses, or lower limits, partly together with consistent flux ratios, has been built. Properties concerning the completeness of the binary catalogues are discussed, statistical features of the orbital elements are explained and a comparison with other catalogues is performed. Illustrative applications are proposed for binaries across the H-R diagram. The binarity is studied in the RGB/AGB and a search for genuine SB1 among long-period variables is performed. The discovery of new EL CVn systems illustrates the potential of combining variability and binarity catalogues. Potential compact object companions are presented, mainly white dwarf companions or double degenerates, but one candidate neutron star is also presented. Towards the bottom of the main sequence, the orbits of previously-suspected binary ultracool dwarfs are determined and new candidate binaries are discovered. The long awaited contribution of Gaia to the analysis of the substellar regime shows the brown dwarf desert around solar-type stars using true, rather than minimum, masses, and provides new important constraints on the occurrence rates of substellar companions to M dwarfs. Several dozen new exoplanets are proposed, including two with validated orbital solutions and one super-Jupiter orbiting a white dwarf, all being candidates requiring confirmation. Beside binarity, higher order multiple systems are also found. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05595v1-abstract-full').style.display = 'none'; document.getElementById('2206.05595v1-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">60 pages, 60 figures. Accepted for publication in Astronomy & Astrophysics (2022-06-09). The catalogue of binary masses is available for download from the ESA Gaia DR3 Archive and will be available from the CDS/VizieR service</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A34 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.05534">arXiv:2206.05534</a> <span> [<a href="https://arxiv.org/pdf/2206.05534">pdf</a>, <a href="https://arxiv.org/format/2206.05534">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1051/0004-6361/202243511">10.1051/0004-6361/202243511 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 3: Chemical cartography of the Milky Way </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Recio-Blanco%2C+A">A. Recio-Blanco</a>, <a href="/search/astro-ph?searchtype=author&query=Kordopatis%2C+G">G. Kordopatis</a>, <a href="/search/astro-ph?searchtype=author&query=de+Laverny%2C+P">P. de Laverny</a>, <a href="/search/astro-ph?searchtype=author&query=Palicio%2C+P+A">P. A. Palicio</a>, <a href="/search/astro-ph?searchtype=author&query=Spagna%2C+A">A. Spagna</a>, <a href="/search/astro-ph?searchtype=author&query=Spina%2C+L">L. Spina</a>, <a href="/search/astro-ph?searchtype=author&query=Katz%2C+D">D. Katz</a>, <a href="/search/astro-ph?searchtype=author&query=Fiorentin%2C+P+R">P. Re Fiorentin</a>, <a href="/search/astro-ph?searchtype=author&query=Poggio%2C+E">E. Poggio</a>, <a href="/search/astro-ph?searchtype=author&query=McMillan%2C+P+J">P. J. McMillan</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Lattanzi%2C+M+G">M. G. Lattanzi</a>, <a href="/search/astro-ph?searchtype=author&query=Seabroke%2C+G+M">G. M. Seabroke</a>, <a href="/search/astro-ph?searchtype=author&query=Casamiquela%2C+L">L. Casamiquela</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Antoja%2C+T">T. Antoja</a>, <a href="/search/astro-ph?searchtype=author&query=Bailer-Jones%2C+C+A+L">C. A. L. Bailer-Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Andrae%2C+R">R. Andrae</a>, <a href="/search/astro-ph?searchtype=author&query=Fouesneau%2C+M">M. Fouesneau</a>, <a href="/search/astro-ph?searchtype=author&query=Cropper%2C+M">M. Cropper</a>, <a href="/search/astro-ph?searchtype=author&query=Cantat-Gaudin%2C+T">T. Cantat-Gaudin</a>, <a href="/search/astro-ph?searchtype=author&query=Heiter%2C+U">U. Heiter</a>, <a href="/search/astro-ph?searchtype=author&query=Bijaoui%2C+A">A. Bijaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a> , et al. (425 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="2206.05534v1-abstract-short" style="display: inline;"> Gaia DR3 opens a new era of all-sky spectral analysis of stellar populations thanks to the nearly 5.6 million stars observed by the RVS and parametrised by the GSP-spec module. The all-sky Gaia chemical cartography allows a powerful and precise chemo-dynamical view of the Milky Way with unprecedented spatial coverage and statistical robustness. First, it reveals the strong vertical symmetry of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05534v1-abstract-full').style.display = 'inline'; document.getElementById('2206.05534v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.05534v1-abstract-full" style="display: none;"> Gaia DR3 opens a new era of all-sky spectral analysis of stellar populations thanks to the nearly 5.6 million stars observed by the RVS and parametrised by the GSP-spec module. The all-sky Gaia chemical cartography allows a powerful and precise chemo-dynamical view of the Milky Way with unprecedented spatial coverage and statistical robustness. First, it reveals the strong vertical symmetry of the Galaxy and the flared structure of the disc. Second, the observed kinematic disturbances of the disc -- seen as phase space correlations -- and kinematic or orbital substructures are associated with chemical patterns that favour stars with enhanced metallicities and lower [alpha/Fe] abundance ratios compared to the median values in the radial distributions. This is detected both for young objects that trace the spiral arms and older populations. Several alpha, iron-peak elements and at least one heavy element trace the thin and thick disc properties in the solar cylinder. Third, young disc stars show a recent chemical impoverishment in several elements. Fourth, the largest chemo-dynamical sample of open clusters analysed so far shows a steepening of the radial metallicity gradient with age, which is also observed in the young field population. Finally, the Gaia chemical data have the required coverage and precision to unveil galaxy accretion debris and heated disc stars on halo orbits through their [alpha/Fe] ratio, and to allow the study of the chemo-dynamical properties of globular clusters. Gaia DR3 chemo-dynamical diagnostics open new horizons before the era of ground-based wide-field spectroscopic surveys. They unveil a complex Milky Way that is the outcome of an eventful evolution, shaping it to the present day (abridged). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05534v1-abstract-full').style.display = 'none'; document.getElementById('2206.05534v1-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">Astronomy and Astrophysics (accepted, in press)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A38 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.02901">arXiv:2206.02901</a> <span> [<a href="https://arxiv.org/pdf/2206.02901">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </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/10.1051/0004-6361/202243141">10.1051/0004-6361/202243141 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Public Spectroscopic Survey: Implementation, data products, open cluster survey, science, and legacy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+G+G">G. G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Jackson%2C+R+J">R. J. Jackson</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffries%2C+R+D">R. D. Jeffries</a>, <a href="/search/astro-ph?searchtype=author&query=Worley%2C+C+C">C. C. Worley</a>, <a href="/search/astro-ph?searchtype=author&query=Hourihane%2C+A">A. Hourihane</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=V%C3%A0zquez%2C+C+V">C. Viscasillas V脿zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+J+R">J. R. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E+J">E. J. Alfaro</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=Blomme%2C+T+B+R">T. Bensby R. Blomme</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Flaccomio%2C+E">E. Flaccomio</a>, <a href="/search/astro-ph?searchtype=author&query=Fran%C3%A7ois%2C+P">P. Fran莽ois</a>, <a href="/search/astro-ph?searchtype=author&query=Irwin%2C+M+J">M. J. Irwin</a>, <a href="/search/astro-ph?searchtype=author&query=Koposov%2C+S+E">S. E. Koposov</a>, <a href="/search/astro-ph?searchtype=author&query=Korn%2C+A+J">A. J. Korn</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzafame%2C+A+C">A. C. Lanzafame</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Recio-Blanco%2C+A">A. Recio-Blanco</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a> , et al. (139 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="2206.02901v1-abstract-short" style="display: inline;"> In the last 15 years different ground-based spectroscopic surveys have been started (and completed) with the general aim of delivering stellar parameters and elemental abundances for large samples of Galactic stars, complementing Gaia astrometry. Among those surveys, the Gaia-ESO Public Spectroscopic Survey (GES), the only one performed on a 8m class telescope, was designed to target 100,000 stars… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.02901v1-abstract-full').style.display = 'inline'; document.getElementById('2206.02901v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.02901v1-abstract-full" style="display: none;"> In the last 15 years different ground-based spectroscopic surveys have been started (and completed) with the general aim of delivering stellar parameters and elemental abundances for large samples of Galactic stars, complementing Gaia astrometry. Among those surveys, the Gaia-ESO Public Spectroscopic Survey (GES), the only one performed on a 8m class telescope, was designed to target 100,000 stars using FLAMES on the ESO VLT (both Giraffe and UVES spectrographs), covering all the Milky Way populations, with a special focus on open star clusters. This article provides an overview of the survey implementation (observations, data quality, analysis and its success, data products, and releases), of the open cluster survey, of the science results and potential, and of the survey legacy. A companion article (Gilmore et al.) reviews the overall survey motivation, strategy, Giraffe pipeline data reduction, organisation, and workflow. The GES has determined homogeneous good-quality radial velocities and stellar parameters for a large fraction of its more than 110,000 unique target stars. Elemental abundances were derived for up to 31 elements for targets observed with UVES. Lithium abundances are delivered for about 1/3 of the sample. The analysis and homogenisation strategies have proven to be successful; several science topics have been addressed by the Gaia-ESO consortium and the community, with many highlight results achieved. The final catalogue has been released through the ESO archive at the end of May 2022, including the complete set of advanced data products. In addition to these results, the Gaia-ESO Survey will leave a very important legacy, for several aspects and for many years to come. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.02901v1-abstract-full').style.display = 'none'; document.getElementById('2206.02901v1-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> 6 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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 Astronomy and Astrophysics. 30 pages, 30 figures, 4 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/2205.05045">arXiv:2205.05045</a> <span> [<a href="https://arxiv.org/pdf/2205.05045">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey 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/10.1038/s41550-022-01664-5">10.1038/s41550-022-01664-5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A spectroscopic quadruple as a possible progenitor of sub-Chandrasekhar Type Ia supernovae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Merle%2C+T">T. Merle</a>, <a href="/search/astro-ph?searchtype=author&query=Hamers%2C+A+S">A. S. Hamers</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Eck%2C+S">S. Van Eck</a>, <a href="/search/astro-ph?searchtype=author&query=Jorissen%2C+A">A. Jorissen</a>, <a href="/search/astro-ph?searchtype=author&query=Van+der+Swaelmen%2C+M">M. Van der Swaelmen</a>, <a href="/search/astro-ph?searchtype=author&query=Pollard%2C+K">K. Pollard</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Pourbaix%2C+D">D. Pourbaix</a>, <a href="/search/astro-ph?searchtype=author&query=Zwitter%2C+T">T. Zwitter</a>, <a href="/search/astro-ph?searchtype=author&query=Traven%2C+G">G. Traven</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Hourihane%2C+A">A. Hourihane</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+G">G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Worley%2C+C+C">C. C. Worley</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="2205.05045v1-abstract-short" style="display: inline;"> Binaries have received much attention as possible progenitors of Type Ia supernova (SNIa) explosions, but long-term gravitational effects in tight triple or quadruple systems could also play a key role in producing SNIa. Here we report on the properties of a spectroscopic quadruple (SB4) found within a star cluster: the 2+2 hierarchical system HD 74438. Its membership in the open cluster IC 2391 m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.05045v1-abstract-full').style.display = 'inline'; document.getElementById('2205.05045v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.05045v1-abstract-full" style="display: none;"> Binaries have received much attention as possible progenitors of Type Ia supernova (SNIa) explosions, but long-term gravitational effects in tight triple or quadruple systems could also play a key role in producing SNIa. Here we report on the properties of a spectroscopic quadruple (SB4) found within a star cluster: the 2+2 hierarchical system HD 74438. Its membership in the open cluster IC 2391 makes it the youngest (43 My) SB4 discovered so far and among the quadruple systems with the shortest outer orbital period. The eccentricity of the 6 y outer period is 0.46 and the two inner orbits, with periods of 20.5 d and 4.4 d, and eccentricities of 0.36 and 0.15, are not coplanar. Using an innovative combination of ground-based high resolution spectroscopy and Gaia/Hipparcos astrometry, we show that this system is undergoing secular interaction that likely pumped the eccentricity of one of the inner orbits higher than expected for the spectral types of its components. We compute the future evolution of HD 74438 and show that this system is an excellent candidate progenitor of sub-Chandrasekhar SNIa through white dwarf (WD) mergers. Taking into account the contribution of this specific type of SNIa better accounts for the chemical evolution of iron-peak elements in the Galaxy than considering only near Chandrasekhar-mass SNIa. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.05045v1-abstract-full').style.display = 'none'; document.getElementById('2205.05045v1-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> 10 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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 Nature 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/2204.12574">arXiv:2204.12574</a> <span> [<a href="https://arxiv.org/pdf/2204.12574">pdf</a>, <a href="https://arxiv.org/format/2204.12574">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </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/10.1051/0004-6361/202243483">10.1051/0004-6361/202243483 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Early Data Release 3: The celestial reference frame (Gaia-CRF3) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Klioner%2C+S+A">S. A. Klioner</a>, <a href="/search/astro-ph?searchtype=author&query=Lindegren%2C+L">L. Lindegren</a>, <a href="/search/astro-ph?searchtype=author&query=Mignard%2C+F">F. Mignard</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J">J. Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos-Lerate%2C+M">M. Ramos-Lerate</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+U">U. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Bombrun%2C+A">A. Bombrun</a>, <a href="/search/astro-ph?searchtype=author&query=de+Torres%2C+A">A. de Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Gerlach%2C+E">E. Gerlach</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+R">R. Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Hilger%2C+T">T. Hilger</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+D">D. Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Lammers%2C+U+L">U. L. Lammers</a>, <a href="/search/astro-ph?searchtype=author&query=McMillan%2C+P+J">P. J. McMillan</a>, <a href="/search/astro-ph?searchtype=author&query=Steidelm%C3%BCller%2C+H">H. Steidelm眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Teyssier%2C+D">D. Teyssier</a>, <a href="/search/astro-ph?searchtype=author&query=Raiteri%2C+C+M">C. M. Raiteri</a>, <a href="/search/astro-ph?searchtype=author&query=Bartolom%C3%A9%2C+S">S. Bartolom茅</a>, <a href="/search/astro-ph?searchtype=author&query=Bernet%2C+M">M. Bernet</a>, <a href="/search/astro-ph?searchtype=author&query=Casta%C3%B1eda%2C+J">J. Casta帽eda</a>, <a href="/search/astro-ph?searchtype=author&query=Clotet%2C+M">M. Clotet</a>, <a href="/search/astro-ph?searchtype=author&query=Davidson%2C+M">M. Davidson</a>, <a href="/search/astro-ph?searchtype=author&query=Fabricius%2C+C">C. Fabricius</a> , et al. (426 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="2204.12574v2-abstract-short" style="display: inline;"> Gaia-CRF3 is the celestial reference frame for positions and proper motions in the third release of data from the Gaia mission, Gaia DR3 (and for the early third release, Gaia EDR3, which contains identical astrometric results). The reference frame is defined by the positions and proper motions at epoch 2016.0 for a specific set of extragalactic sources in the (E)DR3 catalogue. We describe the c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.12574v2-abstract-full').style.display = 'inline'; document.getElementById('2204.12574v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.12574v2-abstract-full" style="display: none;"> Gaia-CRF3 is the celestial reference frame for positions and proper motions in the third release of data from the Gaia mission, Gaia DR3 (and for the early third release, Gaia EDR3, which contains identical astrometric results). The reference frame is defined by the positions and proper motions at epoch 2016.0 for a specific set of extragalactic sources in the (E)DR3 catalogue. We describe the construction of Gaia-CRF3, and its properties in terms of the distributions in magnitude, colour, and astrometric quality. Compact extragalactic sources in Gaia DR3 were identified by positional cross-matching with 17 external catalogues of quasars (QSO) and active galactic nuclei (AGN), followed by astrometric filtering designed to remove stellar contaminants. Selecting a clean sample was favoured over including a higher number of extragalactic sources. For the final sample, the random and systematic errors in the proper motions are analysed, as well as the radio-optical offsets in position for sources in the third realisation of the International Celestial Reference Frame (ICRF3). The Gaia-CRF3 comprises about 1.6 million QSO-like sources, of which 1.2 million have five-parameter astrometric solutions in Gaia DR3 and 0.4 million have six-parameter solutions. The sources span the magnitude range G = 13 to 21 with a peak density at 20.6 mag, at which the typical positional uncertainty is about 1 mas. The proper motions show systematic errors on the level of 12 $渭$as yr${}^{-1}$ on angular scales greater than 15 deg. For the 3142 optical counterparts of ICRF3 sources in the S/X frequency bands, the median offset from the radio positions is about 0.5 mas, but exceeds 4 mas in either coordinate for 127 sources. We outline the future of the Gaia-CRF in the next Gaia data releases. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.12574v2-abstract-full').style.display = 'none'; document.getElementById('2204.12574v2-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> 30 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 667, A148 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.05820">arXiv:2204.05820</a> <span> [<a href="https://arxiv.org/pdf/2204.05820">pdf</a>, <a href="https://arxiv.org/format/2204.05820">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</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/10.1093/mnras/stac1245">10.1093/mnras/stac1245 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: Constraining evolutionary models and ages for young low mass stars with measurements of lithium depletion and rotation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Binks%2C+A+S">A. S. Binks</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffries%2C+R+D">R. D. Jeffries</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+G+G">G. G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Jackson%2C+R+J">R. J. Jackson</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+L">L. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Bergemann%2C+M">M. Bergemann</a>, <a href="/search/astro-ph?searchtype=author&query=Bonito%2C+R">R. Bonito</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Jimin%C3%A9z-Esteban%2C+F">F. Jimin茅z-Esteban</a>, <a href="/search/astro-ph?searchtype=author&query=Morbidelli%2C+L">L. Morbidelli</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Roccatagliata%2C+V">V. Roccatagliata</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Zaggia%2C+S">S. Zaggia</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="2204.05820v1-abstract-short" style="display: inline;"> A growing disquiet has emerged in recent years that standard stellar models are at odds with observations of the colour-magnitude diagrams (CMDs) and lithium depletion patterns of pre main sequence (PMS) stars in clusters. In this work we select 1,246 high probability K/M-type constituent members of 5 young open clusters (5--125\,Myr) in the Gaia-ESO Survey to test a series of models that use stan… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05820v1-abstract-full').style.display = 'inline'; document.getElementById('2204.05820v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.05820v1-abstract-full" style="display: none;"> A growing disquiet has emerged in recent years that standard stellar models are at odds with observations of the colour-magnitude diagrams (CMDs) and lithium depletion patterns of pre main sequence (PMS) stars in clusters. In this work we select 1,246 high probability K/M-type constituent members of 5 young open clusters (5--125\,Myr) in the Gaia-ESO Survey to test a series of models that use standard input physics and others that incorporate surface magnetic fields or cool starspots. We find that: standard models provide systematically under-luminous isochrones for low-mass stars in the CMD and fail to predict Li-depletion of the right strength at the right colour; magnetic models provide better CMD fits with isochrones that are $\sim 1.5-2$ times older, and provide better matches to Li depletion patterns. We investigate how rotation periods, most of which are determined here for the first time from Transiting Exoplanet Survey Satellite data, correlate with CMD position and Li. Among the K-stars in the older clusters we find the brightest and least Li-depleted are the fastest rotators, demonstrating the classic "Li-rotation connection" for the first time at $\sim 35$ Myr in NGC 2547, and finding some evidence that it exists in the early M-stars of NGC 2264 at $<10\,$Myr. However, the wide dispersion in Li depletion observed in fully-convective M-dwarfs in the $纬$ Vel cluster at $\sim 20$ Myr appears not to be correlated with rotation and is challenging to explain without a very large ($>10$ Myr) age spread. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05820v1-abstract-full').style.display = 'none'; document.getElementById('2204.05820v1-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> 12 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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 Monthly Notices of the Royal Astronomical Society: 28 pages, 14 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/2203.14991">arXiv:2203.14991</a> <span> [<a href="https://arxiv.org/pdf/2203.14991">pdf</a>, <a href="https://arxiv.org/format/2203.14991">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey 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/10.1051/0004-6361/202243316">10.1051/0004-6361/202243316 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: Chemical tagging in the thin disk. Open clusters blindly recovered in the elemental abundance space </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Spina%2C+L">L. Spina</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+G+G">G. G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Casali%2C+G">G. Casali</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvaisien%C4%97%2C+G">G. Tautvaisien臈</a>, <a href="/search/astro-ph?searchtype=author&query=Jim%C3%A9nez-Esteban%2C+F">F. Jim茅nez-Esteban</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Feltzing%2C+S">S. Feltzing</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffries%2C+R+D">R. D. Jeffries</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Morbidelli%2C+L">L. Morbidelli</a>, <a href="/search/astro-ph?searchtype=author&query=Zaggia%2C+S">S. Zaggia</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="2203.14991v1-abstract-short" style="display: inline;"> The chemical makeup of a star provides the fossil information of the environment where it formed. Under this premise, it should be possible to use chemical abundances to tag stars that formed within the same stellar association. This idea - known as chemical tagging - has not produced the expected results, especially within the thin disk where open stellar clusters have chemical patterns that are… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.14991v1-abstract-full').style.display = 'inline'; document.getElementById('2203.14991v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.14991v1-abstract-full" style="display: none;"> The chemical makeup of a star provides the fossil information of the environment where it formed. Under this premise, it should be possible to use chemical abundances to tag stars that formed within the same stellar association. This idea - known as chemical tagging - has not produced the expected results, especially within the thin disk where open stellar clusters have chemical patterns that are difficult to disentangle. The ultimate goal of this study is to probe the feasibility of chemical tagging within the thin disk population using high-quality data from a controlled sample of stars. We also aim at improving the existing techniques of chemical tagging and giving guidance on different strategies of clustering analysis in the elemental abundance space. Here we develop the first blind search of open clusters' members through clustering analysis in the elemental abundance space using the OPTICS algorithm applied to data from the Gaia-ESO survey. First, we evaluate different strategies of analysis, determining which ones are more performing. Second, we apply these methods to a data set including both field stars and open clusters attempting a blind recover of as many open clusters as possible. We show how specific strategies of data analysis can improve the final results. Specifically, we demonstrate that open clusters can be more efficaciously recovered with the Manhattan metric and on a space whose dimensions are carefully selected. Using these (and other) prescriptions we are able to recover open clusters hidden in our data set and find new members of these stellar associations. Our results indicate that there are chances of recovering open clusters' members via clustering analysis in the elemental abundance space. Presumably, the performances of chemical tagging will further increase with higher quality data and more sophisticated clustering algorithms. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.14991v1-abstract-full').style.display = 'none'; document.getElementById('2203.14991v1-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 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 by A&A. 21 pages, 11 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 85-02 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 668, A16 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.08662">arXiv:2202.08662</a> <span> [<a href="https://arxiv.org/pdf/2202.08662">pdf</a>, <a href="https://arxiv.org/format/2202.08662">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey 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/10.1051/0004-6361/202142349">10.1051/0004-6361/202142349 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: The analysis of the hot-star spectra </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Blomme%2C+R">R. Blomme</a>, <a href="/search/astro-ph?searchtype=author&query=Daflon%2C+S">S. Daflon</a>, <a href="/search/astro-ph?searchtype=author&query=Gebran%2C+M">M. Gebran</a>, <a href="/search/astro-ph?searchtype=author&query=Herrero%2C+A">A. Herrero</a>, <a href="/search/astro-ph?searchtype=author&query=Lobel%2C+A">A. Lobel</a>, <a href="/search/astro-ph?searchtype=author&query=Mahy%2C+L">L. Mahy</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+F">F. Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Morel%2C+T">T. Morel</a>, <a href="/search/astro-ph?searchtype=author&query=Berlanas%2C+S+R">S. R. Berlanas</a>, <a href="/search/astro-ph?searchtype=author&query=Blazere%2C+A">A. Blazere</a>, <a href="/search/astro-ph?searchtype=author&query=Fremat%2C+Y">Y. Fremat</a>, <a href="/search/astro-ph?searchtype=author&query=Gosset%2C+E">E. Gosset</a>, <a href="/search/astro-ph?searchtype=author&query=Apellaniz%2C+J+M">J. Maiz Apellaniz</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+W">W. Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Semaan%2C+T">T. Semaan</a>, <a href="/search/astro-ph?searchtype=author&query=Simon-Diaz%2C+S">S. Simon-Diaz</a>, <a href="/search/astro-ph?searchtype=author&query=Volpi%2C+D">D. Volpi</a>, <a href="/search/astro-ph?searchtype=author&query=Holgado%2C+G">G. Holgado</a>, <a href="/search/astro-ph?searchtype=author&query=Jimenez-Esteban%2C+F">F. Jimenez-Esteban</a>, <a href="/search/astro-ph?searchtype=author&query=Nieva%2C+M+F">M. F. Nieva</a>, <a href="/search/astro-ph?searchtype=author&query=Przybilla%2C+N">N. Przybilla</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Negueruela%2C+I">I. Negueruela</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a> , et al. (22 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="2202.08662v2-abstract-short" style="display: inline;"> The Gaia-ESO Survey (GES) is a large public spectroscopic survey that has collected, over a period of 6 years, spectra of ~ 10^5 stars. This survey provides not only the reduced spectra, but also the stellar parameters and abundances resulting from the analysis of the spectra. The GES dataflow is organised in 19 working groups. Working group 13 (WG13) is responsible for the spectral analysis of th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.08662v2-abstract-full').style.display = 'inline'; document.getElementById('2202.08662v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.08662v2-abstract-full" style="display: none;"> The Gaia-ESO Survey (GES) is a large public spectroscopic survey that has collected, over a period of 6 years, spectra of ~ 10^5 stars. This survey provides not only the reduced spectra, but also the stellar parameters and abundances resulting from the analysis of the spectra. The GES dataflow is organised in 19 working groups. Working group 13 (WG13) is responsible for the spectral analysis of the hottest stars (O, B and A type, with a formal cut-off of Teff > 7000 K) that were observed as part of GES. We present the procedures and techniques that have been applied to the reduced spectra, in order to determine the stellar parameters and abundances of these stars. The procedure used is similar to that of other working groups in GES. A number of groups (called `Nodes') each independently analyse the spectra, using their state-of-the-art techniques and codes. Specific for the analysis in WG13 is the large temperature range that is covered (Teff = 7000 - 50,000 K), requiring the use of different analysis codes. Most Nodes can therefore only handle part of the data. Quality checks are applied to the results of these Nodes by comparing them to benchmark stars, and by comparing them one to another. For each star the Node values are then homogenised into a single result: the recommended parameters and abundances. Eight Nodes each analysed (part of) the data. In total 17,693 spectra of 6462 stars were analysed, most of them in 37 open star clusters. The homogenisation led to stellar parameters for 5584 stars. Abundances were determined for a more limited number of stars. Elements studied are He, C, N, O, Ne, Mg, Al, Si and Sc. Abundances for at least one of those elements were determined for 292 stars. The hot-star data analysed here, as well as the Gaia-ESO Survey data in general, will be of considerable use in future studies of stellar evolution and open clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.08662v2-abstract-full').style.display = 'none'; document.getElementById('2202.08662v2-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 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">26 pages, 14 figures, accepted for publication in Astronomy & Astrophysics; language-edited version; two appendices merged</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 661, A120 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.04863">arXiv:2202.04863</a> <span> [<a href="https://arxiv.org/pdf/2202.04863">pdf</a>, <a href="https://arxiv.org/format/2202.04863">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </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/10.1051/0004-6361/202142937">10.1051/0004-6361/202142937 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: Age-chemical-clock relations spatially resolved in the Galactic disc </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=V%C3%A1zquez%2C+C+V">C. Viscasillas V谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Casali%2C+G">G. Casali</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvai%C5%A1ien%C4%97%2C+G">G. Tautvai拧ien臈</a>, <a href="/search/astro-ph?searchtype=author&query=Spina%2C+L">L. Spina</a>, <a href="/search/astro-ph?searchtype=author&query=Van+der+Swaelmen%2C+M">M. Van der Swaelmen</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Friel%2C+E">E. Friel</a>, <a href="/search/astro-ph?searchtype=author&query=Feltzing%2C+S">S. Feltzing</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+G+G">G. G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Turchi%2C+A">A. Turchi</a>, <a href="/search/astro-ph?searchtype=author&query=Jim%C3%A9nez-Esteban%2C+F">F. Jim茅nez-Esteban</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Orazi%2C+V">V. D'Orazi</a>, <a href="/search/astro-ph?searchtype=author&query=Delgado-Mena%2C+E">E. Delgado-Mena</a>, <a href="/search/astro-ph?searchtype=author&query=Mikolaitis%2C+%C5%A0">艩. Mikolaitis</a>, <a href="/search/astro-ph?searchtype=author&query=Drazdauskas%2C+A">A. Drazdauskas</a>, <a href="/search/astro-ph?searchtype=author&query=Minkevi%C4%8Di%C5%ABt%C4%97%2C+R">R. Minkevi膷i奴t臈</a>, <a href="/search/astro-ph?searchtype=author&query=Stonkut%C4%97%2C+E">E. Stonkut臈</a>, <a href="/search/astro-ph?searchtype=author&query=Bagdonas%2C+V">V. Bagdonas</a>, <a href="/search/astro-ph?searchtype=author&query=Montes%2C+D">D. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Guiglion%2C+G">G. Guiglion</a>, <a href="/search/astro-ph?searchtype=author&query=Baratella%2C+M">M. Baratella</a>, <a href="/search/astro-ph?searchtype=author&query=Tabernero%2C+H+M">H. M. Tabernero</a> , et al. (11 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="2202.04863v1-abstract-short" style="display: inline;"> The last decade has seen a revolution in our knowledge of the Galaxy thanks to the Gaia and asteroseismic space missions and the ground-based spectroscopic surveys. To complete this picture, it is necessary to map the ages of its stellar populations. During recent years, the dependence on time of abundance ratios involving slow (s) neutron-capture and $伪$ elements (called chemical-clocks) has been… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.04863v1-abstract-full').style.display = 'inline'; document.getElementById('2202.04863v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.04863v1-abstract-full" style="display: none;"> The last decade has seen a revolution in our knowledge of the Galaxy thanks to the Gaia and asteroseismic space missions and the ground-based spectroscopic surveys. To complete this picture, it is necessary to map the ages of its stellar populations. During recent years, the dependence on time of abundance ratios involving slow (s) neutron-capture and $伪$ elements (called chemical-clocks) has been used to provide estimates of stellar ages, usually in a limited volume close to the Sun. We aim to analyse the relations of chemical clocks in the Galactic disc extending the range to R$_{\rm GC}\sim$6-20~kpc. Using the sixth internal data release of the Gaia-ESO survey, we calibrated several relations between stellar ages and abundance ratios [s/$伪$] using a sample of open clusters, the largest one so far used with this aim. Thanks to their wide galactocentric coverage, we investigated the radial variations of the shape of these relations, confirming their non-universality. We estimated our accuracy and precision in recovering the global ages of open clusters, and the ages of their individual members. We applied the multi-variate relations with the highest correlation coefficients to the field star population. We confirm that there is no single age-chemical clock relationship valid for the whole disc, but that there is a dependence on the galactocentric position, which is related to the radial variation of the star formation history combined with the non-monotonic dependence on metallicity of the yields of the s-process elements from low- and intermediate-mass stars. Finally, the abundance ratios [Ba/$伪$] are more sensitive to age than those with [Y/$伪$] for young disc stars, and their slopes vary less with galactocentric distance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.04863v1-abstract-full').style.display = 'none'; document.getElementById('2202.04863v1-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> 10 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">14 pages, 10 figures + Appendix (3 tables and 2 figures)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 660, A135 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.11974">arXiv:2112.11974</a> <span> [<a href="https://arxiv.org/pdf/2112.11974">pdf</a>, <a href="https://arxiv.org/ps/2112.11974">ps</a>, <a href="https://arxiv.org/format/2112.11974">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202142674">10.1051/0004-6361/202142674 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: Target selection of open cluster stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+E">E. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Flaccomio%2C+E">E. Flaccomio</a>, <a href="/search/astro-ph?searchtype=author&query=Blomme%2C+R">R. Blomme</a>, <a href="/search/astro-ph?searchtype=author&query=Donati%2C+P">P. Donati</a>, <a href="/search/astro-ph?searchtype=author&query=Costado%2C+M">M. Costado</a>, <a href="/search/astro-ph?searchtype=author&query=Damiani%2C+F">F. Damiani</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Prisinzano%2C+L">L. Prisinzano</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Friel%2C+E+D">E. D. Friel</a>, <a href="/search/astro-ph?searchtype=author&query=Hatztidimitriou%2C+D">D. Hatztidimitriou</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Spagna%2C+A">A. Spagna</a>, <a href="/search/astro-ph?searchtype=author&query=Balaguer-Nunez%2C+L">L. Balaguer-Nunez</a>, <a href="/search/astro-ph?searchtype=author&query=Bonito%2C+R">R. Bonito</a>, <a href="/search/astro-ph?searchtype=author&query=Cantat-Gaudin%2C+T">T. Cantat-Gaudin</a>, <a href="/search/astro-ph?searchtype=author&query=Casamiquela%2C+L">L. Casamiquela</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffries%2C+R+D">R. D. Jeffries</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Drew%2C+J+E">J. E. Drew</a>, <a href="/search/astro-ph?searchtype=author&query=Jackson%2C+R+J">R. J. Jackson</a>, <a href="/search/astro-ph?searchtype=author&query=Abbas%2C+U">U. Abbas</a>, <a href="/search/astro-ph?searchtype=author&query=Caramazza%2C+M">M. Caramazza</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="2112.11974v1-abstract-short" style="display: inline;"> The Gaia-ESO Survey (GES) is a public, high-resolution spectroscopic survey with FLAMES@VLT. GES targeted in particular a large sample of open clusters (OCs) of all ages. The different kinds of OCs are useful to reach the main science goals, which are the study of the OC structure and dynamics, the use of OCs to constrain and improve stellar evolution models, and the definition of Galactic disc pr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.11974v1-abstract-full').style.display = 'inline'; document.getElementById('2112.11974v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.11974v1-abstract-full" style="display: none;"> The Gaia-ESO Survey (GES) is a public, high-resolution spectroscopic survey with FLAMES@VLT. GES targeted in particular a large sample of open clusters (OCs) of all ages. The different kinds of OCs are useful to reach the main science goals, which are the study of the OC structure and dynamics, the use of OCs to constrain and improve stellar evolution models, and the definition of Galactic disc properties (e.g. metallicity distribution). GES is organised in 19 working groups (WGs). We describe here the work of three of them, WG4 in charge of the selection of the targets within each cluster), WG1 responsible for defining the most probable candidate members, and WG6 in charge of the preparation of the observations. As GES has been conducted before Gaia DR2, we could not make use of the Gaia astrometry to define cluster members. We made use of public and private photometry to select the stars to be observed with FLAMES. Candidate target selection was based on ground-based proper motions, radial velocities, and X-ray properties when appropriate, and it was mostly used to define the position of the clusters' evolutionary sequences in the colour-magnitude diagrams. Targets for GIRAFFE were selected near the sequences in an unbiased way. We used available information on membership only for the few UVES stars. We collected spectra for 62 confirmed OCs (a few more were taken from the ESO archive). Among them are very young clusters, where the main targets are pre-main sequence stars, clusters with very hot and massive stars currently on the main sequence, intermediate-age and old clusters where evolved stars are the main targets. The selection of targets was as inclusive and unbiased as possible and we observed a representative fraction of all possible targets, thus collecting the largest, most accurate, and most homogeneous spectroscopic data set on ever achieved. [abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.11974v1-abstract-full').style.display = 'none'; document.getElementById('2112.11974v1-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> 22 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </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. Abstract abridged from the accepted version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 659, A200 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.11196">arXiv:2111.11196</a> <span> [<a href="https://arxiv.org/pdf/2111.11196">pdf</a>, <a href="https://arxiv.org/ps/2111.11196">ps</a>, <a href="https://arxiv.org/format/2111.11196">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202142290">10.1051/0004-6361/202142290 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia-ESO Survey: Role of magnetic activity and starspots on pre-main sequence lithium evolution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Tognelli%2C+E">E. Tognelli</a>, <a href="/search/astro-ph?searchtype=author&query=Degl%27Innocenti%2C+S">S. Degl'Innocenti</a>, <a href="/search/astro-ph?searchtype=author&query=Moroni%2C+P+G+P">P. G. Prada Moroni</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+G+G">G. G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzafame%2C+A+C">A. C. Lanzafame</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Prisinzano%2C+L">L. Prisinzano</a>, <a href="/search/astro-ph?searchtype=author&query=Sanna%2C+N">N. Sanna</a>, <a href="/search/astro-ph?searchtype=author&query=Roccatagliata%2C+V">V. Roccatagliata</a>, <a href="/search/astro-ph?searchtype=author&query=Bonito%2C+R">R. Bonito</a>, <a href="/search/astro-ph?searchtype=author&query=de+Laverny%2C+P">P. de Laverny</a>, <a href="/search/astro-ph?searchtype=author&query=Albarr%C3%A1n%2C+M+L+G">M. L. Guti茅rrez Albarr谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Montes%2C+D">D. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Jim%C3%A9nez-Esteban%2C+F">F. Jim茅nez-Esteban</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Bergemann%2C+M">M. Bergemann</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Damiani%2C+F">F. Damiani</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Hourihane%2C+A">A. Hourihane</a>, <a href="/search/astro-ph?searchtype=author&query=Morbidelli%2C+L">L. Morbidelli</a> , et al. (2 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="2111.11196v2-abstract-short" style="display: inline;"> Pre-main sequence models with inflated radii are needed to simultaneously reproduce the colour-magnitude diagram and the lithium depletion pattern in young open clusters. We tested a new set of PMS models including radius inflation due to starspots or magnetic inhibition of convection, using five clusters observed by the Gaia-ESO Survey, spanning the age range ~10-100 Myr where such effects could… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.11196v2-abstract-full').style.display = 'inline'; document.getElementById('2111.11196v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.11196v2-abstract-full" style="display: none;"> Pre-main sequence models with inflated radii are needed to simultaneously reproduce the colour-magnitude diagram and the lithium depletion pattern in young open clusters. We tested a new set of PMS models including radius inflation due to starspots or magnetic inhibition of convection, using five clusters observed by the Gaia-ESO Survey, spanning the age range ~10-100 Myr where such effects could be important. Gaia-ESO radial velocities were combined with Gaia EDR3 astrometry to obtain clean lists of high-probability members for the five clusters. A Bayesian maximum likelihood method was adopted to derive the best model parameters and the cluster reddening and age. Models were calculated for different values of the mixing length parameter ($伪_{ML}=2.0$, 1.5 and 1.0), without spots or with effective spot coverage $尾_{spot}=0.2$ and 0.4. To reproduce the CMD and the Li depletion pattern in Gamma Vel A and B and in 25 Ori we need both a reduced convection efficiency $伪_{ML}=1.0$ and an effective spot coverage of ~20%. We obtained ages of 18 Myr and 21 Myr for Gamma Vel A and B, respectively, and 19 Myr for 25 Ori. However, a single isochrone is not sufficient to account for the Li dispersion, and an increasing level of spot coverage as mass decreases seems to be required. The older clusters (NGC2451B at 30 Myr, NGC2547 at 35 Myr, and NGC2516 at 138 Myr) are consistent with standard models ($伪_{ML}=2.0$ and no spots) except at low masses: a 20% spot coverage seems to reproduce the sequence of M-type stars better and might explain the observed abundance spread. The quality of Gaia-ESO data combined with Gaia allows us to gain important insights on PMS evolution. Models including starspots can provide a consistent explanation of the cluster sequences and Li abundances of young clusters, although a range of starspot coverage is required to fully reproduce the data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.11196v2-abstract-full').style.display = 'none'; document.getElementById('2111.11196v2-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> 7 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </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 A&A, 18 pages, 10 figures. Revised version after language editing, revised acknowledgements</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 659, A85 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.10684">arXiv:2111.10684</a> <span> [<a href="https://arxiv.org/pdf/2111.10684">pdf</a>, <a href="https://arxiv.org/format/2111.10684">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </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/10.1051/0004-6361/202142234">10.1051/0004-6361/202142234 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia-ESO Survey: Detailed elemental abundances in red giants of the peculiar globular cluster NGC 1851 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tautvaisiene%2C+G">G. Tautvaisiene</a>, <a href="/search/astro-ph?searchtype=author&query=Drazdauskas%2C+A">A. Drazdauskas</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Martell%2C+S+L">S. L. Martell</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Lardo%2C+C">C. Lardo</a>, <a href="/search/astro-ph?searchtype=author&query=Mikolaitis%2C+S">S. Mikolaitis</a>, <a href="/search/astro-ph?searchtype=author&query=Minkeviciute%2C+R">R. Minkeviciute</a>, <a href="/search/astro-ph?searchtype=author&query=Stonkute%2C+E">E. Stonkute</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosch%2C+M">M. Ambrosch</a>, <a href="/search/astro-ph?searchtype=author&query=Bagdonas%2C+V">V. Bagdonas</a>, <a href="/search/astro-ph?searchtype=author&query=Chorniy%2C+Y">Y. Chorniy</a>, <a href="/search/astro-ph?searchtype=author&query=Sanna%2C+N">N. Sanna</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Bergemann%2C+M">M. Bergemann</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Guiglion%2C+G">G. Guiglion</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Heiter%2C+U">U. Heiter</a>, <a href="/search/astro-ph?searchtype=author&query=Korn%2C+A">A. Korn</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a> , et al. (2 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="2111.10684v1-abstract-short" style="display: inline;"> Context. NGC 1851 is one of several globular clusters for which multiple stellar populations of the subgiant branch have been clearly identified and a difference in metallicity detected. A crucial piece of information on the formation history of this cluster can be provided by the sum of A(C+N+O) abundances. However, these values have lacked a general consensus thus far. The separation of the subg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.10684v1-abstract-full').style.display = 'inline'; document.getElementById('2111.10684v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.10684v1-abstract-full" style="display: none;"> Context. NGC 1851 is one of several globular clusters for which multiple stellar populations of the subgiant branch have been clearly identified and a difference in metallicity detected. A crucial piece of information on the formation history of this cluster can be provided by the sum of A(C+N+O) abundances. However, these values have lacked a general consensus thus far. The separation of the subgiant branch can be based on age and/or A(C+N+O) abundance differences. Aims. Our main aim was to determine carbon, nitrogen, and oxygen abundances for evolved giants in the globular cluster NGC1851 in order to check whether or not the double populations of stars are coeval. Methods. High-resolution spectra, observed with the FLAMES-UVES spectrograph on the ESO VLT telescope, were analysed using a differential model atmosphere method. Results. We provide abundances of up to 29 chemical elements for a sample of 45 giants in NGC 1851. The investigated stars can be separated into two populations with a difference of 0.07 dex in the mean metallicity, 0.3 dex in the mean C/N, and 0.35 dex in the mean s-process dominated element-to-iron abundance ratios [s/Fe]. No significant difference was determined in the mean values of A(C+N+O) as well as in abundance to iron ratios of carbon, alpha- and iron-peak-elements, and of europium. Conclusions. As the averaged A(C+N+O) values between the two populations do not differ, additional evidence is given that NGC 1851 is composed of two clusters, the metal-rich cluster being by about 0.6 Gyr older than the metal-poor one. A global overview of NGC 1851 properties and the detailed abundances of chemical elements favour its formation in a dwarf spheroidal galaxy that was accreted by the Milky Way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.10684v1-abstract-full').style.display = 'none'; document.getElementById('2111.10684v1-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> 20 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </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">13 pages, 17 figures, accepted to Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 658, A80 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.10477">arXiv:2110.10477</a> <span> [<a href="https://arxiv.org/pdf/2110.10477">pdf</a>, <a href="https://arxiv.org/ps/2110.10477">ps</a>, <a href="https://arxiv.org/format/2110.10477">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1093/mnras/stab3032">10.1093/mnras/stab3032 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: Membership probabilities for stars in 63 open and 7 globular clusters from 3D kinematics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jackson%2C+R+J">R. J. Jackson</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffries%2C+R+D">R. D. Jeffries</a>, <a href="/search/astro-ph?searchtype=author&query=Wright%2C+N+J">N. J. Wright</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+G">G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Hourihane%2C+A">A. Hourihane</a>, <a href="/search/astro-ph?searchtype=author&query=Tognelli%2C+E">E. Tognelli</a>, <a href="/search/astro-ph?searchtype=author&query=Degl%27Innocenti%2C+S">S. Degl'Innocenti</a>, <a href="/search/astro-ph?searchtype=author&query=Moroni%2C+P+G+P">P. G. Prada Moroni</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Bergemann%2C+M">M. Bergemann</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Jofr%C3%A9%2C+P">P. Jofr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+J">J. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Morbidelli%2C+L">L. Morbidelli</a>, <a href="/search/astro-ph?searchtype=author&query=Prisinzano%2C+L">L. Prisinzano</a>, <a href="/search/astro-ph?searchtype=author&query=Worley%2C+C">C. Worley</a>, <a href="/search/astro-ph?searchtype=author&query=Zaggia%2C+S">S. Zaggia</a> , et al. (4 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="2110.10477v1-abstract-short" style="display: inline;"> Spectroscopy from the final internal data release of the Gaia-ESO Survey (GES) has been combined with Gaia EDR3 to assign membership probabilities to targets observed towards 63 Galactic open clusters and 7 globular clusters. The membership probabilities are based chiefly on maximum likelihood modelling of the 3D kinematics of the targets, separating them into cluster and field populations. From 4… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.10477v1-abstract-full').style.display = 'inline'; document.getElementById('2110.10477v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.10477v1-abstract-full" style="display: none;"> Spectroscopy from the final internal data release of the Gaia-ESO Survey (GES) has been combined with Gaia EDR3 to assign membership probabilities to targets observed towards 63 Galactic open clusters and 7 globular clusters. The membership probabilities are based chiefly on maximum likelihood modelling of the 3D kinematics of the targets, separating them into cluster and field populations. From 43211 observed targets, 13985 are identified as highly probable cluster members ($P>0.9$), with an average membership probability of 0.993. The addition of GES radial velocities successfully drives down the fraction of false positives and we achieve better levels of discrimination in most clusters over the use of astrometric data alone, especially those at larger distances. Since the membership selection is almost purely kinematic, the union of this catalogue with GES and Gaia is ideal for investigating the photometric and chemical properties of clusters as a function of stellar mass, age and Galactic position. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.10477v1-abstract-full').style.display = 'none'; document.getElementById('2110.10477v1-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> 20 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </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 version for publication in MNRAS. 16 pages + 38 pages of Appendices</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.11677">arXiv:2108.11677</a> <span> [<a href="https://arxiv.org/pdf/2108.11677">pdf</a>, <a href="https://arxiv.org/format/2108.11677">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202141275">10.1051/0004-6361/202141275 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO survey: Lithium abundances in open cluster Red Clump stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Pasquini%2C+L">L. Pasquini</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Casali%2C+G">G. Casali</a>, <a href="/search/astro-ph?searchtype=author&query=Vazquez%2C+C+V">C. Viscasillas Vazquez</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Spina%2C+L">L. Spina</a>, <a href="/search/astro-ph?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvaivsiene%2C+G">G. Tautvaivsiene</a>, <a href="/search/astro-ph?searchtype=author&query=Masseron%2C+T">T. Masseron</a>, <a href="/search/astro-ph?searchtype=author&query=Van+der+Swaelmen%2C+M">M. Van der Swaelmen</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Jimenez-Esteban%2C+F">F. Jimenez-Esteban</a>, <a href="/search/astro-ph?searchtype=author&query=Guiglion%2C+G">G. Guiglion</a>, <a href="/search/astro-ph?searchtype=author&query=Martell%2C+S">S. Martell</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Orazi%2C+V">V. D'Orazi</a>, <a href="/search/astro-ph?searchtype=author&query=Baratella%2C+M">M. Baratella</a>, <a href="/search/astro-ph?searchtype=author&query=Korn%2C+A">A. Korn</a>, <a href="/search/astro-ph?searchtype=author&query=Jofre%2C+P">P. Jofre</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Worley%2C+C">C. Worley</a>, <a href="/search/astro-ph?searchtype=author&query=Hourihane%2C+A">A. Hourihane</a> , et al. (3 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="2108.11677v1-abstract-short" style="display: inline;"> It has recently been suggested that all giant stars with mass below 2 $M_{\odot}$ suffer an episode of surface lithium enrichment between the tip of the red giant branch (RGB) and the red clump (RC). We test if the above result can be confirmed in a sample of RC and RGB stars that are members of open clusters. We discuss Li abundances in six open clusters with ages between 1.5 and 4.9 Gyr (turn-of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.11677v1-abstract-full').style.display = 'inline'; document.getElementById('2108.11677v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.11677v1-abstract-full" style="display: none;"> It has recently been suggested that all giant stars with mass below 2 $M_{\odot}$ suffer an episode of surface lithium enrichment between the tip of the red giant branch (RGB) and the red clump (RC). We test if the above result can be confirmed in a sample of RC and RGB stars that are members of open clusters. We discuss Li abundances in six open clusters with ages between 1.5 and 4.9 Gyr (turn-off masses between 1.1 and 1.7 $M_{\odot}$). These observations are compared with the predictions of different models that include rotation-induced mixing, thermohaline instability, mixing induced by the first He flash, and energy losses by neutrino magnetic moment. In six clusters, we find about 35\% RC stars with Li abundances that are similar or higher than those of upper RGB stars. This can be a sign of fresh Li production. Because of the extra-mixing episode connected to the luminosity bump, the expectation was for RC stars to have systematically lower surface Li abundances. However, we cannot confirm that the possible Li production is ubiquitous. For about 65\% RC giants we can only determine abundance upper limits that could be hiding very low Li abundances. Our results indicate a possible production of Li during the RC, at levels that would not classify the stars as Li rich. Determination of their carbon isotopic ratio would help to confirm that the RC giants have suffered extra mixing followed by Li enrichment. The Li abundances of the RC stars can be qualitatively explained by the models with an additional mixing episode close to the He flash. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.11677v1-abstract-full').style.display = 'none'; document.getElementById('2108.11677v1-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 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </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 A&A, 8 pages, 5 figures, tables available online and under request</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 655, A23 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.12381">arXiv:2107.12381</a> <span> [<a href="https://arxiv.org/pdf/2107.12381">pdf</a>, <a href="https://arxiv.org/format/2107.12381">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202141069">10.1051/0004-6361/202141069 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO Survey: A new approach to chemically characterising young open clusters II. Abundances of the neutron-capture elements Cu, Sr, Y, Zr, Ba, La, and Ce </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Baratella%2C+M">M. Baratella</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Orazi%2C+V">V. D'Orazi</a>, <a href="/search/astro-ph?searchtype=author&query=Sheminova%2C+V">V. Sheminova</a>, <a href="/search/astro-ph?searchtype=author&query=Spina%2C+L">L. Spina</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Gratton%2C+R">R. Gratton</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Lugaro%2C+M">M. Lugaro</a>, <a href="/search/astro-ph?searchtype=author&query=Pignatari%2C+M">M. Pignatari</a>, <a href="/search/astro-ph?searchtype=author&query=Romano%2C+D">D. Romano</a>, <a href="/search/astro-ph?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Casali%2C+G">G. Casali</a>, <a href="/search/astro-ph?searchtype=author&query=Desidera%2C+S">S. Desidera</a>, <a href="/search/astro-ph?searchtype=author&query=Frasca%2C+A">A. Frasca</a>, <a href="/search/astro-ph?searchtype=author&query=de+Silva%2C+G">G. de Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Melo%2C+C">C. Melo</a>, <a href="/search/astro-ph?searchtype=author&query=Van+der+Swaelmen%2C+M">M. Van der Swaelmen</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvai%C5%A1ien%C4%97%2C+G">G. Tautvai拧ien臈</a>, <a href="/search/astro-ph?searchtype=author&query=Jim%C3%A9nez-Esteban%2C+F+M">F. M. Jim茅nez-Esteban</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">T. Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a> , et al. (10 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="2107.12381v1-abstract-short" style="display: inline;"> Young open clusters (t<200 Myr) have been observed to exhibit several peculiarities in their chemical compositions, from a slightly sub-solar iron content, super-solar abundances of some atomic species (e.g. ionised chromium), and atypical enhancements of [Ba/Fe], with values up to +0.7 dex. Regarding the behaviour of the other $s$-process elements like yttrium, zirconium, lanthanum, and cerium, t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.12381v1-abstract-full').style.display = 'inline'; document.getElementById('2107.12381v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.12381v1-abstract-full" style="display: none;"> Young open clusters (t<200 Myr) have been observed to exhibit several peculiarities in their chemical compositions, from a slightly sub-solar iron content, super-solar abundances of some atomic species (e.g. ionised chromium), and atypical enhancements of [Ba/Fe], with values up to +0.7 dex. Regarding the behaviour of the other $s$-process elements like yttrium, zirconium, lanthanum, and cerium, there is general disagreement in the literature. In this work we expand upon our previous analysis of a sample of five young open clusters (IC2391, IC2602, IC4665, NGC2516, and NGC2547) and one star-forming region (NGC2264), with the aim of determining abundances of different neutron-capture elements, mainly CuI, SrI, SrII, YII, ZrII, BaII, LaII, and CeII. We analysed high-resolution, high signal-to-noise spectra of 23 solar-type stars observed within the \textit{Gaia}-ESO survey. We find that our clusters have solar [Cu/Fe] within the uncertainties, while we confirm the super-solar [Ba/Fe] values (from +0.22 to +0.64 dex). Our analysis also points to mildly enhanced [Y/Fe] values (from 0 and +0.3 dex). For the other $s$-process elements we find that [X/Fe] ratios are solar at all ages. It is not possible to reconcile the anomalous behaviour of Ba and Y at young ages with standard stellar yields and Galactic chemical evolution model predictions. Thus, we explore different possible scenarios related to the behaviour of spectral lines, from the sensitivity to the presence of magnetic fields to the first ionisation potential effect. We also investigate the possibility that they may arise from alterations of the structure of the stellar photosphere due to higher levels of activity in such young stars. We are still unable to explain these enhancements, but we suggest that other elements (i.e. La) might be more reliable tracer of the $s$-process at young ages and encourage further observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.12381v1-abstract-full').style.display = 'none'; document.getElementById('2107.12381v1-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 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </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, 14 figures, 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 653, A67 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.01394">arXiv:2106.01394</a> <span> [<a href="https://arxiv.org/pdf/2106.01394">pdf</a>, <a href="https://arxiv.org/format/2106.01394">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/10.1051/0004-6361/202140735">10.1051/0004-6361/202140735 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Photometric Science Alerts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hodgkin%2C+S+T">S. T. Hodgkin</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+D+L">D. L. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Breedt%2C+E">E. Breedt</a>, <a href="/search/astro-ph?searchtype=author&query=Wevers%2C+T">T. Wevers</a>, <a href="/search/astro-ph?searchtype=author&query=Rixon%2C+G">G. Rixon</a>, <a href="/search/astro-ph?searchtype=author&query=Delgado%2C+A">A. Delgado</a>, <a href="/search/astro-ph?searchtype=author&query=Yoldas%2C+A">A. Yoldas</a>, <a href="/search/astro-ph?searchtype=author&query=Kostrzewa-Rutkowska%2C+Z">Z. Kostrzewa-Rutkowska</a>, <a href="/search/astro-ph?searchtype=author&query=Wyrzykowski%2C+%C5%81">艁. Wyrzykowski</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+M">M. van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Blagorodnova%2C+N">N. Blagorodnova</a>, <a href="/search/astro-ph?searchtype=author&query=Campbell%2C+H">H. Campbell</a>, <a href="/search/astro-ph?searchtype=author&query=Eappachen%2C+D">D. Eappachen</a>, <a href="/search/astro-ph?searchtype=author&query=Fraser%2C+M">M. Fraser</a>, <a href="/search/astro-ph?searchtype=author&query=Ihanec%2C+N">N. Ihanec</a>, <a href="/search/astro-ph?searchtype=author&query=Koposov%2C+S+E">S. E. Koposov</a>, <a href="/search/astro-ph?searchtype=author&query=Kruszy%C5%84ska%2C+K">K. Kruszy艅ska</a>, <a href="/search/astro-ph?searchtype=author&query=Marton%2C+G">G. Marton</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K+A">K. A. Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Burgess%2C+P+W">P. W. Burgess</a>, <a href="/search/astro-ph?searchtype=author&query=Busso%2C+G">G. Busso</a>, <a href="/search/astro-ph?searchtype=author&query=Cowell%2C+S">S. Cowell</a>, <a href="/search/astro-ph?searchtype=author&query=De+Angeli%2C+F">F. De Angeli</a>, <a href="/search/astro-ph?searchtype=author&query=Diener%2C+C">C. Diener</a> , et al. (86 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="2106.01394v1-abstract-short" style="display: inline;"> Since July 2014, the Gaia mission has been engaged in a high-spatial-resolution, time-resolved, precise, accurate astrometric, and photometric survey of the entire sky. Aims: We present the Gaia Science Alerts project, which has been in operation since 1 June 2016. We describe the system which has been developed to enable the discovery and publication of transient photometric events as seen by G… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.01394v1-abstract-full').style.display = 'inline'; document.getElementById('2106.01394v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.01394v1-abstract-full" style="display: none;"> Since July 2014, the Gaia mission has been engaged in a high-spatial-resolution, time-resolved, precise, accurate astrometric, and photometric survey of the entire sky. Aims: We present the Gaia Science Alerts project, which has been in operation since 1 June 2016. We describe the system which has been developed to enable the discovery and publication of transient photometric events as seen by Gaia. Methods: We outline the data handling, timings, and performances, and we describe the transient detection algorithms and filtering procedures needed to manage the high false alarm rate. We identify two classes of events: (1) sources which are new to Gaia and (2) Gaia sources which have undergone a significant brightening or fading. Validation of the Gaia transit astrometry and photometry was performed, followed by testing of the source environment to minimise contamination from Solar System objects, bright stars, and fainter near-neighbours. Results: We show that the Gaia Science Alerts project suffers from very low contamination, that is there are very few false-positives. We find that the external completeness for supernovae, $C_E=0.46$, is dominated by the Gaia scanning law and the requirement of detections from both fields-of-view. Where we have two or more scans the internal completeness is $C_I=0.79$ at 3 arcsec or larger from the centres of galaxies, but it drops closer in, especially within 1 arcsec. Conclusions: The per-transit photometry for Gaia transients is precise to 1 per cent at $G=13$, and 3 per cent at $G=19$. The per-transit astrometry is accurate to 55 milliarcseconds when compared to Gaia DR2. The Gaia Science Alerts project is one of the most homogeneous and productive transient surveys in operation, and it is the only survey which covers the whole sky at high spatial resolution (subarcsecond), including the Galactic plane and bulge. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.01394v1-abstract-full').style.display = 'none'; document.getElementById('2106.01394v1-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </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, 26 figures, accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 652, A76 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.04866">arXiv:2105.04866</a> <span> [<a href="https://arxiv.org/pdf/2105.04866">pdf</a>, <a href="https://arxiv.org/format/2105.04866">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202140935">10.1051/0004-6361/202140935 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO survey: Mixing processes in low-mass stars traced by lithium abundance in cluster and field stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Lagarde%2C+N">N. Lagarde</a>, <a href="/search/astro-ph?searchtype=author&query=Charbonnel%2C+C">C. Charbonnel</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">R. Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Casali%2C+G">G. Casali</a>, <a href="/search/astro-ph?searchtype=author&query=Vazquez%2C+C+V">C. Viscasillas Vazquez</a>, <a href="/search/astro-ph?searchtype=author&query=Spina%2C+L">L. Spina</a>, <a href="/search/astro-ph?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Pasquini%2C+L">L. Pasquini</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Van+der+Swaelmen%2C+M">M. Van der Swaelmen</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvaisiene%2C+G">G. Tautvaisiene</a>, <a href="/search/astro-ph?searchtype=author&query=Inno%2C+L">L. Inno</a>, <a href="/search/astro-ph?searchtype=author&query=Sanna%2C+N">N. Sanna</a>, <a href="/search/astro-ph?searchtype=author&query=Prisinzano%2C+L">L. Prisinzano</a>, <a href="/search/astro-ph?searchtype=author&query=Degl%27Innocenti%2C+S">S. Degl'Innocenti</a>, <a href="/search/astro-ph?searchtype=author&query=Moroni%2C+P+P">P. Prada Moroni</a>, <a href="/search/astro-ph?searchtype=author&query=Roccatagliata%2C+V">V. Roccatagliata</a>, <a href="/search/astro-ph?searchtype=author&query=Tognelli%2C+E">E. Tognelli</a>, <a href="/search/astro-ph?searchtype=author&query=Monaco%2C+L">L. Monaco</a>, <a href="/search/astro-ph?searchtype=author&query=de+Laverny%2C+P">P. de Laverny</a>, <a href="/search/astro-ph?searchtype=author&query=Delgado-Mena%2C+E">E. Delgado-Mena</a>, <a href="/search/astro-ph?searchtype=author&query=Baratella%2C+M">M. Baratella</a> , et al. (20 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="2105.04866v1-abstract-short" style="display: inline;"> We aim to constrain the mixing processes in low-mass stars by investigating the behaviour of the Li surface abundance after the main sequence. We take advantage of the data from the sixth internal data release of Gaia-ESO, idr6, and from the Gaia Early Data Release 3, edr3. We select a sample of main sequence, sub-giant, and giant stars in which Li abundance is measured by the Gaia-ESO survey, bel… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.04866v1-abstract-full').style.display = 'inline'; document.getElementById('2105.04866v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.04866v1-abstract-full" style="display: none;"> We aim to constrain the mixing processes in low-mass stars by investigating the behaviour of the Li surface abundance after the main sequence. We take advantage of the data from the sixth internal data release of Gaia-ESO, idr6, and from the Gaia Early Data Release 3, edr3. We select a sample of main sequence, sub-giant, and giant stars in which Li abundance is measured by the Gaia-ESO survey, belonging to 57 open clusters with ages from 120~Myr to about 7 Gyr and to Milky Way fields, covering a range in [Fe/H] between -1.0 and +0.5dex. We study the behaviour of the Li abundances as a function of stellar parameters. We compare the observed Li behaviour in field giant stars and in giant stars belonging to individual clusters with the predictions of a set of classical models and of models with mixing induced by rotation and thermohaline instability. The comparison with stellar evolution models confirms that classical models cannot reproduce the lithium abundances observed in the metallicity and mass regimes covered by the data. The models that include the effects of both rotation-induced mixing and thermohaline instability account for the Li abundance trends observed in our sample, in all metallicity and mass ranges. The differences between the results of the classical models and of the rotation models largely differ (up to ~2 dex), making lithium the best element to constrain stellar mixing processes in low-mass stars. For stars with well-determined masses, we find a better agreement between observed surface abundances and models with rotation-induced and thermohaline mixings, the former dominating during the main sequence and the first phases of the post-main sequence evolution and the latter after the bump in the luminosity function. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.04866v1-abstract-full').style.display = 'none'; document.getElementById('2105.04866v1-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </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 A&A, 19 pages, 16 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 651, A84 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.01153">arXiv:2105.01153</a> <span> [<a href="https://arxiv.org/pdf/2105.01153">pdf</a>, <a href="https://arxiv.org/format/2105.01153">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1093/mnras/stab1351">10.1093/mnras/stab1351 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gaia-ESO survey: A lithium depletion boundary age for NGC 2232 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Binks%2C+A+S">A. S. Binks</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffries%2C+R+D">R. D. Jeffries</a>, <a href="/search/astro-ph?searchtype=author&query=Jackson%2C+R+J">R. J. Jackson</a>, <a href="/search/astro-ph?searchtype=author&query=Franciosini%2C+E">E. Franciosini</a>, <a href="/search/astro-ph?searchtype=author&query=Sacco%2C+G+G">G. G. Sacco</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Arancibia%2C+J">J. Arancibia</a>, <a href="/search/astro-ph?searchtype=author&query=Bergemann%2C+M">M. Bergemann</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Gilmore%2C+G">G. Gilmore</a>, <a href="/search/astro-ph?searchtype=author&query=Gonneau%2C+A">A. Gonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Hourihane%2C+A">A. Hourihane</a>, <a href="/search/astro-ph?searchtype=author&query=Jofr%C3%A9%2C+P">P. Jofr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Korn%2C+A+J">A. J. Korn</a>, <a href="/search/astro-ph?searchtype=author&query=Morbidelli%2C+L">L. Morbidelli</a>, <a href="/search/astro-ph?searchtype=author&query=Prisinzano%2C+L">L. Prisinzano</a>, <a href="/search/astro-ph?searchtype=author&query=Worley%2C+C+C">C. C. Worley</a>, <a href="/search/astro-ph?searchtype=author&query=Zaggia%2C+S">S. Zaggia</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="2105.01153v1-abstract-short" style="display: inline;"> Astrometry and photometry from {\it Gaia} and spectroscopic data from the {\it Gaia}-ESO Survey (GES) are used to identify the lithium depletion boundary (LDB) in the young cluster NGC 2232. A specialised spectral line analysis procedure was used to recover the signature of undepleted lithium in very low luminosity cluster members. An age of $38\pm 3$ Myr is inferred by comparing the LDB location… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.01153v1-abstract-full').style.display = 'inline'; document.getElementById('2105.01153v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.01153v1-abstract-full" style="display: none;"> Astrometry and photometry from {\it Gaia} and spectroscopic data from the {\it Gaia}-ESO Survey (GES) are used to identify the lithium depletion boundary (LDB) in the young cluster NGC 2232. A specialised spectral line analysis procedure was used to recover the signature of undepleted lithium in very low luminosity cluster members. An age of $38\pm 3$ Myr is inferred by comparing the LDB location in absolute colour-magnitude diagrams (CMDs) with the predictions of standard models. This is more than twice the age derived from fitting isochrones to low-mass stars in the CMD with the same models. Much closer agreement between LDB and CMD ages is obtained from models that incorporate magnetically suppressed convection or flux-blocking by dark, magnetic starspots. The best agreement is found at ages of $45-50$\,Myr for models with high levels of magnetic activity and starspot coverage fractions $>50$ per cent, although a uniformly high spot coverage does not match the CMD well across the full luminosity range considered. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.01153v1-abstract-full').style.display = 'none'; document.getElementById('2105.01153v1-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.05811">arXiv:2101.05811</a> <span> [<a href="https://arxiv.org/pdf/2101.05811">pdf</a>, <a href="https://arxiv.org/format/2101.05811">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1051/0004-6361/202039714">10.1051/0004-6361/202039714 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Early Data Release 3: The Galactic anticentre </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Antoja%2C+T">T. Antoja</a>, <a href="/search/astro-ph?searchtype=author&query=McMillan%2C+P">P. McMillan</a>, <a href="/search/astro-ph?searchtype=author&query=Kordopatis%2C+G">G. Kordopatis</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos%2C+P">P. Ramos</a>, <a href="/search/astro-ph?searchtype=author&query=Helmi%2C+A">A. Helmi</a>, <a href="/search/astro-ph?searchtype=author&query=Balbinot%2C+E">E. Balbinot</a>, <a href="/search/astro-ph?searchtype=author&query=Cantat-Gaudin%2C+T">T. Cantat-Gaudin</a>, <a href="/search/astro-ph?searchtype=author&query=Chemin%2C+L">L. Chemin</a>, <a href="/search/astro-ph?searchtype=author&query=Figueras%2C+F">F. Figueras</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a>, <a href="/search/astro-ph?searchtype=author&query=Khanna%2C+S">S. Khanna</a>, <a href="/search/astro-ph?searchtype=author&query=Romero-Gomez%2C+M">M. Romero-Gomez</a>, <a href="/search/astro-ph?searchtype=author&query=Seabroke%2C+G">G. Seabroke</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Hutton%2C+A">A. Hutton</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+F">F. Jansen</a> , et al. (395 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="2101.05811v2-abstract-short" style="display: inline;"> We aim to demonstrate the scientific potential of the Gaia Early Data Release 3 (EDR3) for the study of the Milky Way structure and evolution. We used astrometric positions, proper motions, parallaxes, and photometry from EDR3 to select different populations and components and to calculate the distances and velocities in the direction of the anticentre. We explore the disturbances of the current d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.05811v2-abstract-full').style.display = 'inline'; document.getElementById('2101.05811v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.05811v2-abstract-full" style="display: none;"> We aim to demonstrate the scientific potential of the Gaia Early Data Release 3 (EDR3) for the study of the Milky Way structure and evolution. We used astrometric positions, proper motions, parallaxes, and photometry from EDR3 to select different populations and components and to calculate the distances and velocities in the direction of the anticentre. We explore the disturbances of the current disc, the spatial and kinematical distributions of early accreted versus in-situ stars, the structures in the outer parts of the disc, and the orbits of open clusters Berkeley 29 and Saurer 1. We find that: i) the dynamics of the Galactic disc are very complex with vertical asymmetries, and new correlations, including a bimodality with disc stars with large angular momentum moving vertically upwards from below the plane, and disc stars with slightly lower angular momentum moving preferentially downwards; ii) we resolve the kinematic substructure (diagonal ridges) in the outer parts of the disc for the first time; iii) the red sequence that has been associated with the proto-Galactic disc that was present at the time of the merger with Gaia-Enceladus-Sausage is currently radially concentrated up to around 14 kpc, while the blue sequence that has been associated with debris of the satellite extends beyond that; iv) there are density structures in the outer disc, both above and below the plane, most probably related to Monoceros, the Anticentre Stream, and TriAnd, for which the Gaia data allow an exhaustive selection of candidate member stars and dynamical study; and v) the open clusters Berkeley~29 and Saurer~1, despite being located at large distances from the Galactic centre, are on nearly circular disc-like orbits. We demonstrate how, once again, the Gaia are crucial for our understanding of the different pieces of our Galaxy and their connection to its global structure and history. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.05811v2-abstract-full').style.display = 'none'; document.getElementById('2101.05811v2-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 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </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">Gaia EDR3 performance verification paper, version 2 closer to published version in A&A, complete list of authors</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 649, A8 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.02061">arXiv:2012.02061</a> <span> [<a href="https://arxiv.org/pdf/2012.02061">pdf</a>, <a href="https://arxiv.org/format/2012.02061">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202039498">10.1051/0004-6361/202039498 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Early Data Release 3: The Gaia Catalogue of Nearby Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Smart%2C+R+L">R. L. Smart</a>, <a href="/search/astro-ph?searchtype=author&query=Sarro%2C+L+M">L. M. Sarro</a>, <a href="/search/astro-ph?searchtype=author&query=Rybizki%2C+J">J. Rybizki</a>, <a href="/search/astro-ph?searchtype=author&query=Reyl%C3%A9%2C+C">C. Reyl茅</a>, <a href="/search/astro-ph?searchtype=author&query=Robin%2C+A+C">A. C. Robin</a>, <a href="/search/astro-ph?searchtype=author&query=Hambly%2C+N+C">N. C. Hambly</a>, <a href="/search/astro-ph?searchtype=author&query=Abbas%2C+U">U. Abbas</a>, <a href="/search/astro-ph?searchtype=author&query=Barstow%2C+M+A">M. A. Barstow</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Bucciarelli%2C+B">B. Bucciarelli</a>, <a href="/search/astro-ph?searchtype=author&query=Carrasco%2C+J+M">J. M. Carrasco</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+W+J">W. J. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Hodgkin%2C+S+T">S. T. Hodgkin</a>, <a href="/search/astro-ph?searchtype=author&query=Masana%2C+E">E. Masana</a>, <a href="/search/astro-ph?searchtype=author&query=Michalik%2C+D">D. Michalik</a>, <a href="/search/astro-ph?searchtype=author&query=Sahlmann%2C+J">J. Sahlmann</a>, <a href="/search/astro-ph?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a> , et al. (398 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="2012.02061v1-abstract-short" style="display: inline;"> We produce a clean and well-characterised catalogue of objects within 100\,pc of the Sun from the \G\ Early Data Release 3. We characterise the catalogue through comparisons to the full data release, external catalogues, and simulations. We carry out a first analysis of the science that is possible with this sample to demonstrate its potential and best practices for its use. The selection of obj… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02061v1-abstract-full').style.display = 'inline'; document.getElementById('2012.02061v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.02061v1-abstract-full" style="display: none;"> We produce a clean and well-characterised catalogue of objects within 100\,pc of the Sun from the \G\ Early Data Release 3. We characterise the catalogue through comparisons to the full data release, external catalogues, and simulations. We carry out a first analysis of the science that is possible with this sample to demonstrate its potential and best practices for its use. The selection of objects within 100\,pc from the full catalogue used selected training sets, machine-learning procedures, astrometric quantities, and solution quality indicators to determine a probability that the astrometric solution is reliable. The training set construction exploited the astrometric data, quality flags, and external photometry. For all candidates we calculated distance posterior probability densities using Bayesian procedures and mock catalogues to define priors. Any object with reliable astrometry and a non-zero probability of being within 100\,pc is included in the catalogue. We have produced a catalogue of \NFINAL\ objects that we estimate contains at least 92\% of stars of stellar type M9 within 100\,pc of the Sun. We estimate that 9\% of the stars in this catalogue probably lie outside 100\,pc, but when the distance probability function is used, a correct treatment of this contamination is possible. We produced luminosity functions with a high signal-to-noise ratio for the main-sequence stars, giants, and white dwarfs. We examined in detail the Hyades cluster, the white dwarf population, and wide-binary systems and produced candidate lists for all three samples. We detected local manifestations of several streams, superclusters, and halo objects, in which we identified 12 members of \G\ Enceladus. We present the first direct parallaxes of five objects in multiple systems within 10\,pc of the Sun. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02061v1-abstract-full').style.display = 'none'; document.getElementById('2012.02061v1-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 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">45 Pages, 39 figures in main part and 18 in appendix, tables on CDS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 649, A6 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.02036">arXiv:2012.02036</a> <span> [<a href="https://arxiv.org/pdf/2012.02036">pdf</a>, <a href="https://arxiv.org/format/2012.02036">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1051/0004-6361/202039734">10.1051/0004-6361/202039734 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Early Data Release 3: Acceleration of the solar system from Gaia astrometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Klioner%2C+S+A">S. A. Klioner</a>, <a href="/search/astro-ph?searchtype=author&query=Mignard%2C+F">F. Mignard</a>, <a href="/search/astro-ph?searchtype=author&query=Lindegren%2C+L">L. Lindegren</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+U">U. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=McMillan%2C+P+J">P. J. McMillan</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J">J. Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+D">D. Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos-Lerate%2C+M">M. Ramos-Lerate</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Bombrun%2C+A">A. Bombrun</a>, <a href="/search/astro-ph?searchtype=author&query=de+Torres%2C+A">A. de Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Gerlach%2C+E">E. Gerlach</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+R">R. Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Hilger%2C+T">T. Hilger</a>, <a href="/search/astro-ph?searchtype=author&query=Lammers%2C+U">U. Lammers</a>, <a href="/search/astro-ph?searchtype=author&query=Steidelm%C3%BCller%2C+H">H. Steidelm眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Stephenson%2C+C+A">C. A. Stephenson</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a> , et al. (392 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="2012.02036v1-abstract-short" style="display: inline;"> Context. Gaia Early Data Release 3 (Gaia EDR3) provides accurate astrometry for about 1.6 million compact (QSO-like) extragalactic sources, 1.2 million of which have the best-quality five-parameter astrometric solutions. Aims. The proper motions of QSO-like sources are used to reveal a systematic pattern due to the acceleration of the solar system barycentre with respect to the rest frame of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02036v1-abstract-full').style.display = 'inline'; document.getElementById('2012.02036v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.02036v1-abstract-full" style="display: none;"> Context. Gaia Early Data Release 3 (Gaia EDR3) provides accurate astrometry for about 1.6 million compact (QSO-like) extragalactic sources, 1.2 million of which have the best-quality five-parameter astrometric solutions. Aims. The proper motions of QSO-like sources are used to reveal a systematic pattern due to the acceleration of the solar system barycentre with respect to the rest frame of the Universe. Apart from being an important scientific result by itself, the acceleration measured in this way is a good quality indicator of the Gaia astrometric solution. Methods. The effect of the acceleration is obtained as a part of the general expansion of the vector field of proper motions in Vector Spherical Harmonics (VSH). Various versions of the VSH fit and various subsets of the sources are tried and compared to get the most consistent result and a realistic estimate of its uncertainty. Additional tests with the Gaia astrometric solution are used to get a better idea on possible systematic errors in the estimate. Results. Our best estimate of the acceleration based on Gaia EDR3 is $(2.32 \pm 0.16) \times 10^{-10}$ m s${}^{-2}$ (or $7.33 \pm 0.51$ km s$^{-1}$ Myr${}^{-1}$) towards $伪= 269.1^\circ \pm 5.4^\circ$, $未= -31.6^\circ \pm 4.1^\circ$, corresponding to a proper motion amplitude of $5.05 \pm 0.35$ $渭$as yr${}^{-1}$. This is in good agreement with the acceleration expected from current models of the Galactic gravitational potential. We expect that future Gaia data releases will provide estimates of the acceleration with uncertainties substantially below 0.1 $渭$as yr${}^{-1}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02036v1-abstract-full').style.display = 'none'; document.getElementById('2012.02036v1-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 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">A&A, accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 649, A9 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.01916">arXiv:2012.01916</a> <span> [<a href="https://arxiv.org/pdf/2012.01916">pdf</a>, <a href="https://arxiv.org/format/2012.01916">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/10.1051/0004-6361/202039587">10.1051/0004-6361/202039587 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Early Data Release 3: Photometric content and validation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riello%2C+M">M. Riello</a>, <a href="/search/astro-ph?searchtype=author&query=De+Angeli%2C+F">F. De Angeli</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Montegriffo%2C+P">P. Montegriffo</a>, <a href="/search/astro-ph?searchtype=author&query=Carrasco%2C+J+M">J. M. Carrasco</a>, <a href="/search/astro-ph?searchtype=author&query=Busso%2C+G">G. Busso</a>, <a href="/search/astro-ph?searchtype=author&query=Palaversa%2C+L">L. Palaversa</a>, <a href="/search/astro-ph?searchtype=author&query=Burgess%2C+P+W">P. W. Burgess</a>, <a href="/search/astro-ph?searchtype=author&query=Diener%2C+C">C. Diener</a>, <a href="/search/astro-ph?searchtype=author&query=Davidson%2C+M">M. Davidson</a>, <a href="/search/astro-ph?searchtype=author&query=Rowell%2C+N">N. Rowell</a>, <a href="/search/astro-ph?searchtype=author&query=Fabricius%2C+C">C. Fabricius</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a>, <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+M">M. Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+D+L">D. L. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Cacciari%2C+C">C. Cacciari</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+F">F. van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Hambly%2C+N+C">N. C. Hambly</a>, <a href="/search/astro-ph?searchtype=author&query=Hodgkin%2C+S+T">S. T. Hodgkin</a>, <a href="/search/astro-ph?searchtype=author&query=Osborne%2C+P+J">P. J. Osborne</a>, <a href="/search/astro-ph?searchtype=author&query=Altavilla%2C+G">G. Altavilla</a>, <a href="/search/astro-ph?searchtype=author&query=Barstow%2C+M+A">M. A. Barstow</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Castellani%2C+M">M. Castellani</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="2012.01916v1-abstract-short" style="display: inline;"> Gaia Early Data Release 3 contains astrometry and photometry results for about 1.8 billion sources based on observations collected by the ESA Gaia satellite during the first 34 months of operations. This paper focuses on the photometric content, describing the input data, the algorithms, the processing, and the validation of the results. Particular attention is given to the quality of the data and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.01916v1-abstract-full').style.display = 'inline'; document.getElementById('2012.01916v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.01916v1-abstract-full" style="display: none;"> Gaia Early Data Release 3 contains astrometry and photometry results for about 1.8 billion sources based on observations collected by the ESA Gaia satellite during the first 34 months of operations. This paper focuses on the photometric content, describing the input data, the algorithms, the processing, and the validation of the results. Particular attention is given to the quality of the data and to a number of features that users may need to take into account to make the best use of the EDR3 catalogue. The treatment of the BP and RP background has been updated to include a better estimation of the local background, and the detection of crowding effects has been used to exclude affected data from the calibrations. The photometric calibration models have also been updated to account for flux loss over the whole magnitude range. Significant improvements in the modelling and calibration of the point and line spread functions have also helped to reduce a number of instrumental effects that were still present in DR2. EDR3 contains 1.806 billion sources with G-band photometry and 1.540 billion sources with BP and RP photometry. The median uncertainty in the G-band photometry, as measured from the standard deviation of the internally calibrated mean photometry for a given source, is 0.2 mmag at magnitude G=10 to 14, 0.8 mmag at G=17, and 2.6 mmag at G=19. The significant magnitude term found in the Gaia DR2 photometry is no longer visible, and overall there are no trends larger than 1 mmag/mag. Using one passband over the whole colour and magnitude range leaves no systematics above the 1% level in magnitude in any of the bands, and a larger systematic is present for a very small sample of bright and blue sources. A detailed description of the residual systematic effects is provided. Overall the quality of the calibrated mean photometry in EDR3 is superior with respect to DR2 for all bands. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.01916v1-abstract-full').style.display = 'none'; document.getElementById('2012.01916v1-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Gilmore%2C+G&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Gilmore%2C+G&start=0" class="pagination-link is-current" 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