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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <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=Moitinho%2C+A&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Moitinho%2C+A&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Moitinho%2C+A&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.19204">arXiv:2412.19204</a> <span> [<a href="https://arxiv.org/pdf/2412.19204">pdf</a>, <a href="https://arxiv.org/format/2412.19204">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"> Open cluster dissolution rate and the initial cluster mass function in the solar neighbourhood. Modelling the age and mass distributions of clusters observed by Gaia </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+D">Duarte Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">Andr茅 Moitinho</a>, <a href="/search/astro-ph?searchtype=author&query=Moreira%2C+S">Sandro Moreira</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="2412.19204v1-abstract-short" style="display: inline;"> Context. The dissolution rate of open clusters (OCs) and integration of their stars into the Milky Way's field population has been previously explored using their age distribution. With the advent of the Gaia mission, we have an exceptional opportunity to revisit and enhance these studies with ages and masses from high quality data. Aims. To build a comprehensive Gaia-based OC mass catalogue which… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.19204v1-abstract-full').style.display = 'inline'; document.getElementById('2412.19204v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.19204v1-abstract-full" style="display: none;"> Context. The dissolution rate of open clusters (OCs) and integration of their stars into the Milky Way's field population has been previously explored using their age distribution. With the advent of the Gaia mission, we have an exceptional opportunity to revisit and enhance these studies with ages and masses from high quality data. Aims. To build a comprehensive Gaia-based OC mass catalogue which, combined with the age distribution, allows a deeper investigation of the disruption experienced by OCs within the solar neighbourhood. Methods. Masses were determined by comparing luminosity distributions to theoretical luminosity functions. The limiting and core radii of the clusters were obtained by fitting the King function to their observed density profiles. We examined the disruption process through simulations of the build-up and mass evolution of a population of OCs which were compared to the observed mass and age distributions. Results. Our analysis yielded an OC mass distribution with a peak at $log(M)$ = 2.7 dex ($\sim 500 M_{\odot}$), as well as radii for 1724 OCs. Our simulations showed that using a power-law Initial Cluster Mass Function (ICMF) no parameters were able to reproduce the observed mass distribution. Moreover, we find that a skew log-normal ICMF provides a good match to the observations and that the disruption time of a $10^4 M{_\odot}$ OC is $t_4^{tot} = 2.9 \pm 0.4$ Gyr. Conclusions. Our results indicate that the OC disruption time $t_4^{tot}$ is about twice longer than previous estimates based solely on OC age distributions. We find that the shape of the ICMF for bound OCs differs from that of embedded clusters, which could imply a low typical star formation efficiency of $\leq 20\%$ in OCs. Our results also suggest a lower limit of $\sim 60 M{_\odot}$ for bound OCs in the solar neighbourhood. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.19204v1-abstract-full').style.display = 'none'; document.getElementById('2412.19204v1-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">This paper has been accepted for publication in Astronomy & Astrophysics (A&A) on 12/12/2024</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.14661">arXiv:2406.14661</a> <span> [<a href="https://arxiv.org/pdf/2406.14661">pdf</a>, <a href="https://arxiv.org/format/2406.14661">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"> Modelling the evolution of the Galactic disc scale height traced by open clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Moreira%2C+S">Sandro Moreira</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">Andr茅 Moitinho</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+A">Andr茅 Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+D">Duarte Almeida</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="2406.14661v1-abstract-short" style="display: inline;"> Context. The scale height of the spatial distribution of open clusters (OCs) in the Milky Way exhibits a well known increase with age which is usually interpreted as evidence for dynamical heating of the disc or of the disc having been thicker in the past. Aims. We address the increase of the scale height with age of the OC population from a different angle. We propose that the apparent thickeni… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.14661v1-abstract-full').style.display = 'inline'; document.getElementById('2406.14661v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.14661v1-abstract-full" style="display: none;"> Context. The scale height of the spatial distribution of open clusters (OCs) in the Milky Way exhibits a well known increase with age which is usually interpreted as evidence for dynamical heating of the disc or of the disc having been thicker in the past. Aims. We address the increase of the scale height with age of the OC population from a different angle. We propose that the apparent thickening of the disc can be largely explained as a consequence of a stronger disruption of OCs near the Galactic plane by disc phenomena, namely encounters with giant molecular clouds (GMCs). Methods. We present a computational model that forms OCs with different initial masses and follows their orbits while subjecting them to different disruption mechanisms. To setup the model and infer its parameters, we use and analyse a Gaia-based OC catalogue (Dias et al. 2021). We investigate both the spatial and age distributions of the OC population and discuss the completeness of the sample. The simulation results are then compared to the observations. Results. Consistent with previous studies, the observations reveal that the SH of the spatial distribution of OCs increases with age. We find that it is very likely that the OC sample is incomplete even for the solar neighbourhood. The model simulations successfully reproduce the SH increase with age and the total number of OCs that survive with age up to 1 Gyr. For older OCs, the predicted SH from the model starts deviating from the observations, although remaining within the uncertainties of the observations. This can be related with effects of incompleteness and/or simplifications in the model. Conclusions. A selective disruption of OCs near the galactic plane through GMC encounters is able to explain the SH evolution of the OC population. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.14661v1-abstract-full').style.display = 'none'; document.getElementById('2406.14661v1-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">This paper has been submitted to Astronomy and Astrophysics (A&A) on 15/04/2024</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.18165">arXiv:2404.18165</a> <span> [<a href="https://arxiv.org/pdf/2404.18165">pdf</a>, <a href="https://arxiv.org/format/2404.18165">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="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1051/0004-6361/202450535">10.1051/0004-6361/202450535 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ELEPHANT: ExtragaLactic alErt Pipeline for Hostless AstroNomical Transients </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pessi%2C+P+J">P. J. Pessi</a>, <a href="/search/astro-ph?searchtype=author&query=Durgesh%2C+R">R. Durgesh</a>, <a href="/search/astro-ph?searchtype=author&query=Nakazono%2C+L">L. Nakazono</a>, <a href="/search/astro-ph?searchtype=author&query=Hayes%2C+E+E">E. E. Hayes</a>, <a href="/search/astro-ph?searchtype=author&query=Oliveira%2C+R+A+P">R. A. P. Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Ishida%2C+E+E+O">E. E. O. Ishida</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">A. Moitinho</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=Moews%2C+B">B. Moews</a>, <a href="/search/astro-ph?searchtype=author&query=de+Souza%2C+R+S">R. S. de Souza</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+R">R. Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Kuhn%2C+M+A">M. A. Kuhn</a>, <a href="/search/astro-ph?searchtype=author&query=Nowak%2C+K">K. Nowak</a>, <a href="/search/astro-ph?searchtype=author&query=Vaughan%2C+S">S. Vaughan</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="2404.18165v1-abstract-short" style="display: inline;"> Context. Transient astronomical events that exhibit no discernible association with a host galaxy are commonly referred to as hostless. These rare phenomena are associated with extremely energetic events, and they can offer unique insights into the properties and evolution of stars and galaxies. However, the sheer number of transients captured by contemporary high-cadence astronomical surveys rend… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.18165v1-abstract-full').style.display = 'inline'; document.getElementById('2404.18165v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.18165v1-abstract-full" style="display: none;"> Context. Transient astronomical events that exhibit no discernible association with a host galaxy are commonly referred to as hostless. These rare phenomena are associated with extremely energetic events, and they can offer unique insights into the properties and evolution of stars and galaxies. However, the sheer number of transients captured by contemporary high-cadence astronomical surveys renders the manual identification of all potential hostless transients impractical. Therefore, creating a systematic identification tool is crucial for studying these elusive events. Aims. We present the ExtragaLactic alErt Pipeline for Hostless AstroNomical Transients (ELEPHANT), a framework for filtering hostless transients in astronomical data streams. Methods. We used Fink to access all the ZTF alerts produced between January/2022 and December/2023, selecting only those associated with extragalactic transients. We then processed the associated stamps using a sequence of image analysis techniques to retrieve hostless candidates. Results. We find that less than 2% of all analyzed transients are potentially hostless. Among them, approximately 10% have a spectroscopic class reported on TNS, with Type Ia supernova being the most common class, followed by SLSN. Among the hostless candidates retrieved by our pipeline, there was SN 2018ibb, which has been proposed to be a PISN candidate; and SN 2022ann, one of only five known SNe Icn. When no class is reported on TNS, the dominant classes are QSO and SN candidates, the former obtained from SIMBAD and the latter inferred using the Fink ML classifier. Conclusions. ELEPHANT represents an effective strategy to filter extragalactic events within large and complex astronomical alert streams. There are many applications for which this pipeline will be useful, ranging from transient selection for follow-up to studies of transient environments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.18165v1-abstract-full').style.display = 'none'; document.getElementById('2404.18165v1-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 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">15 pages, 11 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 691, A181 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.10486">arXiv:2404.10486</a> <span> [<a href="https://arxiv.org/pdf/2404.10486">pdf</a>, <a href="https://arxiv.org/format/2404.10486">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/10.1051/0004-6361/202449763">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/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/2309.03396">arXiv:2309.03396</a> <span> [<a href="https://arxiv.org/pdf/2309.03396">pdf</a>, <a href="https://arxiv.org/format/2309.03396">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/10.1051/0004-6361/202142826">10.1051/0004-6361/202142826 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detection of open cluster rotation fields from Gaia EDR3 proper motions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Guilherme-Garcia%2C+P">Pedro Guilherme-Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Krone-Martins%2C+A">Alberto Krone-Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">Andr茅 Moitinho</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="2309.03396v1-abstract-short" style="display: inline;"> Context. Most stars from in groups which with time disperse, building the field population of their host galaxy. In the Milky Way, open clusters have been continuously forming in the disk up to the present time, providing it with stars spanning a broad range of ages and masses. Observations of the details of cluster dissolution are, however, scarce. One of the main difficulties is obtaining a deta… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03396v1-abstract-full').style.display = 'inline'; document.getElementById('2309.03396v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.03396v1-abstract-full" style="display: none;"> Context. Most stars from in groups which with time disperse, building the field population of their host galaxy. In the Milky Way, open clusters have been continuously forming in the disk up to the present time, providing it with stars spanning a broad range of ages and masses. Observations of the details of cluster dissolution are, however, scarce. One of the main difficulties is obtaining a detailed characterisation of the internal cluster kinematics, which requires very high quality proper motions. For open clusters, which are typically loose groups with some tens to hundreds of members, there is the additional difficulty of inferring kinematic structures from sparse and irregular distributions of stars. Aims. Here, we aim to analyse internal stellar kinematics of open clusters, and identify rotation, expansion or contraction patterns. Methods. We use Gaia Early Data Release 3 (EDR3) astrometry and Integrated Nested Laplace Approximations to perform vector-field inference and create spatio-kinematic maps of 1237 open clusters. The sample is composed of clusters for which individual stellar memberships were known, thus minimising contamination from field stars in the velocity maps. Projection effects were corrected using EDR3 data complemented with radial velocities from Gaia Data Release 2 and other surveys. Results. We report the detection of rotation patterns in 8 open clusters. Nine additional clusters display possible rotation signs. We also observe 14 expanding clusters, with 15 other objects showing possible expansion patterns. Contraction is evident in two clusters, with one additional cluster presenting a more uncertain detection. In total, 53 clusters are found to display kinematic structures. Within these, elongated spatial distributions suggesting tidal tails are found in 5 clusters. [abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03396v1-abstract-full').style.display = 'none'; document.getElementById('2309.03396v1-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">7 pages main article + 29 pages in appendices. Published 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, 673 (2023) A128 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.07158">arXiv:2305.07158</a> <span> [<a href="https://arxiv.org/pdf/2305.07158">pdf</a>, <a href="https://arxiv.org/format/2305.07158">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/10.1051/0004-6361/202346237">10.1051/0004-6361/202346237 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectroscopic substellar initial mass function of NGC 2244 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Almendros-Abad%2C+V">V. Almendros-Abad</a>, <a href="/search/astro-ph?searchtype=author&query=Mu%C5%BEi%C4%87%2C+K">K. Mu啪i膰</a>, <a href="/search/astro-ph?searchtype=author&query=Bouy%2C+H">H. Bouy</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">A. Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Scholz%2C+A">A. Scholz</a>, <a href="/search/astro-ph?searchtype=author&query=Ram%C3%ADrez%2C+K+P">K. Pe帽a Ram铆rez</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">A. Moitinho</a>, <a href="/search/astro-ph?searchtype=author&query=Kubiak%2C+K">K. Kubiak</a>, <a href="/search/astro-ph?searchtype=author&query=Sch%C3%B6edel%2C+R">R. Sch枚edel</a>, <a href="/search/astro-ph?searchtype=author&query=Bara%C4%8D%2C+R">R. Bara膷</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C4%8Di%C4%87%2C+P">P. Br膷i膰</a>, <a href="/search/astro-ph?searchtype=author&query=Ascenso%2C+J">J. Ascenso</a>, <a href="/search/astro-ph?searchtype=author&query=Jayawardhana%2C+R">R. Jayawardhana</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="2305.07158v1-abstract-short" style="display: inline;"> We aim at characterizing the low-mass (sub)stellar population of the central portion (2.4 pc$^2$) of the $\sim$2 Myr old cluster NGC 2244 using near infrared spectroscopy. By studying this cluster, characterized by a low stellar density and numerous OB stars, we aim at exploring the effect that OB stars may have on the production of BDs. We obtain near infrared HK spectroscopy of 85 faint candidat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.07158v1-abstract-full').style.display = 'inline'; document.getElementById('2305.07158v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.07158v1-abstract-full" style="display: none;"> We aim at characterizing the low-mass (sub)stellar population of the central portion (2.4 pc$^2$) of the $\sim$2 Myr old cluster NGC 2244 using near infrared spectroscopy. By studying this cluster, characterized by a low stellar density and numerous OB stars, we aim at exploring the effect that OB stars may have on the production of BDs. We obtain near infrared HK spectroscopy of 85 faint candidate members of NGC 2244. We derive the spectral type and extinction by comparison with spectral templates. We evaluate cluster membership using three gravity-sensitive spectral indices based on the shape of the $H$-band. Furthermore, we evaluate the infrared excess from Spitzer of all the candidate members of the cluster. Finally, we estimate the mass of all the candidate members of the cluster and derive the initial mass function, star-to-BD number ratio and disk fraction. The initial mass function is well represented by a power law ($dN/dM \propto M^{-伪}$) below 0.4 $M_\odot$, with a slope $伪$ = 0.7-1.1 depending on the fitted mass range. We calculate a star-to-BD number ratio of 2.2-2.8. We find the low-mass population of NGC 2244 to be consistent with nearby star-forming regions, although it is at the high-end of BD production. We find BDs in NGC 2244 to be on average closer to OB stars than to low-mass stars, which could potentially be the first evidence of OB stars affecting the formation of BDs. We find a disk fraction of all the members with spectral type later than K0 of 39$\pm$9% which is lower than typical values found in nearby star-forming regions of similar ages. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.07158v1-abstract-full').style.display = 'none'; document.getElementById('2305.07158v1-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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 by A&A, KMOS spectroscopic data will be made public on Vizier upon publication</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 677, A26 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.08831">arXiv:2303.08831</a> <span> [<a href="https://arxiv.org/pdf/2303.08831">pdf</a>, <a href="https://arxiv.org/format/2303.08831">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/10.1051/0004-6361/202245771">10.1051/0004-6361/202245771 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VISIONS: The VISTA Star Formation Atlas -- I. Survey overview </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Meingast%2C+S">Stefan Meingast</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+J">Jo茫o Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Bouy%2C+H">Herv茅 Bouy</a>, <a href="/search/astro-ph?searchtype=author&query=Petr-Gotzens%2C+M+G">Monika G. Petr-Gotzens</a>, <a href="/search/astro-ph?searchtype=author&query=F%C3%BCrnkranz%2C+V">Verena F眉rnkranz</a>, <a href="/search/astro-ph?searchtype=author&query=Gro%C3%9Fschedl%2C+J+E">Josefa E. Gro脽schedl</a>, <a href="/search/astro-ph?searchtype=author&query=Hernandez%2C+D">David Hernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Rottensteiner%2C+A">Alena Rottensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">Magda Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Ascenso%2C+J">Joana Ascenso</a>, <a href="/search/astro-ph?searchtype=author&query=Bayo%2C+A">Amelia Bayo</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A4ndli%2C+E">Erik Br盲ndli</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">Anthony G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Forbrich%2C+J">Jan Forbrich</a>, <a href="/search/astro-ph?searchtype=author&query=Goodman%2C+A">Alyssa Goodman</a>, <a href="/search/astro-ph?searchtype=author&query=Hacar%2C+A">Alvaro Hacar</a>, <a href="/search/astro-ph?searchtype=author&query=Hasenberger%2C+B">Birgit Hasenberger</a>, <a href="/search/astro-ph?searchtype=author&query=K%C3%B6hler%2C+R">Rainer K枚hler</a>, <a href="/search/astro-ph?searchtype=author&query=Kubiak%2C+K">Karolina Kubiak</a>, <a href="/search/astro-ph?searchtype=author&query=Kuhn%2C+M">Michael Kuhn</a>, <a href="/search/astro-ph?searchtype=author&query=Lada%2C+C">Charles Lada</a>, <a href="/search/astro-ph?searchtype=author&query=Leschinski%2C+K">Kieran Leschinski</a>, <a href="/search/astro-ph?searchtype=author&query=Lombardi%2C+M">Marco Lombardi</a>, <a href="/search/astro-ph?searchtype=author&query=Mardones%2C+D">Diego Mardones</a>, <a href="/search/astro-ph?searchtype=author&query=Mascetti%2C+L">Laura Mascetti</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="2303.08831v1-abstract-short" style="display: inline;"> VISIONS is an ESO public survey of five nearby (d < 500 pc) star-forming molecular cloud complexes that are canonically associated with the constellations of Chamaeleon, Corona Australis, Lupus, Ophiuchus, and Orion. The survey was carried out with VISTA, using VIRCAM, and collected data in the near-infrared passbands J, H, and Ks. With a total on-sky exposure time of 49.4 h VISIONS covers an area… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.08831v1-abstract-full').style.display = 'inline'; document.getElementById('2303.08831v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.08831v1-abstract-full" style="display: none;"> VISIONS is an ESO public survey of five nearby (d < 500 pc) star-forming molecular cloud complexes that are canonically associated with the constellations of Chamaeleon, Corona Australis, Lupus, Ophiuchus, and Orion. The survey was carried out with VISTA, using VIRCAM, and collected data in the near-infrared passbands J, H, and Ks. With a total on-sky exposure time of 49.4 h VISIONS covers an area of 650 deg$^2$, and it was designed to build an infrared legacy archive similar to that of 2MASS. Taking place between April 2017 and March 2022, the observations yielded approximately 1.15 million images, which comprise 19 TB of raw data. The observations are grouped into three different subsurveys: The wide subsurvey comprises shallow, large-scale observations and has visited the star-forming complexes six times over the course of its execution. The deep subsurvey of dedicated high-sensitivity observations has collected data on the areas with the largest amounts of dust extinction. The control subsurvey includes observations of areas of low-to-negligible dust extinction. Using this strategy, the VISIONS survey offers multi-epoch position measurements, is able to access deeply embedded objects, and provides a baseline for statistical comparisons and sample completeness. In particular, VISIONS is designed to measure the proper motions of point sources with a precision of 1 mas/yr or better, when complemented with data from VHS. Hence, VISIONS can provide proper motions for sources inaccessible to Gaia. VISIONS will enable addressing a range of topics, including the 3D distribution and motion of embedded stars and the nearby interstellar medium, the identification and characterization of young stellar objects, the formation and evolution of embedded stellar clusters and their initial mass function, as well as the characteristics of interstellar dust and the reddening law. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.08831v1-abstract-full').style.display = 'none'; document.getElementById('2303.08831v1-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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 Astronomy & Astrophysics on 19 January 2023</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 673, A58 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.13302">arXiv:2209.13302</a> <span> [<a href="https://arxiv.org/pdf/2209.13302">pdf</a>, <a href="https://arxiv.org/format/2209.13302">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/10.1051/0004-6361/202243659">10.1051/0004-6361/202243659 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Stellar population of the Rosette Nebula and NGC 2244: application of the probabilistic random forest </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Muzic%2C+K">Koraljka Muzic</a>, <a href="/search/astro-ph?searchtype=author&query=Almendros-Abad%2C+V">Victor Almendros-Abad</a>, <a href="/search/astro-ph?searchtype=author&query=Bouy%2C+H">Herve Bouy</a>, <a href="/search/astro-ph?searchtype=author&query=Kubiak%2C+K">Karolina Kubiak</a>, <a href="/search/astro-ph?searchtype=author&query=Ramirez%2C+K+P">Karla Pena Ramirez</a>, <a href="/search/astro-ph?searchtype=author&query=Krone-Martins%2C+A">Alberto Krone-Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">Andre Moitinho</a>, <a href="/search/astro-ph?searchtype=author&query=Conceicao%2C+M">Miguel Conceicao</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.13302v2-abstract-short" style="display: inline;"> (Abridged) In this work, we study the 2.8x2.6 deg2 region in the emblematic Rosette Nebula, centred at the young cluster NGC 2244, with the aim of constructing the most reliable candidate member list to date, determining various structural and kinematic parameters, and learning about the past and the future of the region. Starting from a catalogue containing optical to mid-infrared photometry, as… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.13302v2-abstract-full').style.display = 'inline'; document.getElementById('2209.13302v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.13302v2-abstract-full" style="display: none;"> (Abridged) In this work, we study the 2.8x2.6 deg2 region in the emblematic Rosette Nebula, centred at the young cluster NGC 2244, with the aim of constructing the most reliable candidate member list to date, determining various structural and kinematic parameters, and learning about the past and the future of the region. Starting from a catalogue containing optical to mid-infrared photometry, as well as positions and proper motions from Gaia EDR3, we apply the Probabilistic Random Forest algorithm and derive membership probability for each source. Based on the list of almost 3000 probable members, of which about a third are concentrated within the radius of 20' from the centre of NGC 2244, we identify various clustered sources and stellar concentrations, and estimate the average distance of 1489+-37 pc (entire region), 1440+-32 pc (NGC 2244) and 1525+-36 pc (NGC 2237). The masses, extinction, and ages are derived by SED fitting, and the internal dynamic is assessed via proper motions relative to the mean proper motion of NGC 2244. NGC 2244 is showing a clear expansion pattern, with an expansion velocity that increases with radius. Its IMF is well represented by two power laws (dN/dM\propto M^{-伪}), with slopes 伪= 1.05+-0.02 for the mass range 0.2 - 1.5 MSun, and 伪= 2.3+-0.3 for the mass range 1.5 - 20 MSun, in agreement with other star forming regions. The mean age of the region is ~2 Myr. We find evidence for the difference in ages between NGC 2244 and the region associated with the molecular cloud, which appears slightly younger. The velocity dispersion of NGC 2244 is well above the virial velocity dispersion derived from the total mass (1000+-70 MSun) and half-mass radius (3.4+-0.2 pc). From the comparison to other clusters and to numerical simulations, we conclude that NGC 2244 may be unbound, and possibly even formed in a super-virial state. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.13302v2-abstract-full').style.display = 'none'; document.getElementById('2209.13302v2-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 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">30 pages, 28 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 668, A19 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.05432">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/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/2206.06075">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/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/2110.06368">arXiv:2110.06368</a> <span> [<a href="https://arxiv.org/pdf/2110.06368">pdf</a>, <a href="https://arxiv.org/format/2110.06368">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/10.1051/0004-6361/202142050">10.1051/0004-6361/202142050 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Youth analysis of near infrared spectra of young low-mass stars and brown dwarfs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Almendros-Abad%2C+V">V. Almendros-Abad</a>, <a href="/search/astro-ph?searchtype=author&query=Mu%C5%BEi%C4%87%2C+K">K. Mu啪i膰</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">A. Moitinho</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=Kubiak%2C+K">K. Kubiak</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="2110.06368v1-abstract-short" style="display: inline;"> We aim at building a method that efficiently identifies young low-mass stars and brown dwarfs from low-resolution near-infrared spectra, by studying gravity-sensitive features and their evolution with age. We built a dataset composed of all publicly available ($\sim$2800) near-infrared spectra of dwarfs with spectral types between M0 and L3. First, we investigate methods for the derivation of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.06368v1-abstract-full').style.display = 'inline'; document.getElementById('2110.06368v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.06368v1-abstract-full" style="display: none;"> We aim at building a method that efficiently identifies young low-mass stars and brown dwarfs from low-resolution near-infrared spectra, by studying gravity-sensitive features and their evolution with age. We built a dataset composed of all publicly available ($\sim$2800) near-infrared spectra of dwarfs with spectral types between M0 and L3. First, we investigate methods for the derivation of the spectral type and extinction using comparison to spectral templates, and various spectral indices. Then, we examine gravity-sensitive spectral indices and apply machine learning methods, in order to efficiently separate young ($\lesssim$10 Myr) objects from the field. Using a set of six spectral indices for spectral typing, including two newly defined ones (TLI-J and TLI-K), we are able to achieve a precision below 1 spectral subtype across the entire spectral type range. We define a new gravity-sensitive spectral index (TLI-g) that consistently separates young from field objects, showing a performance superior to other indices from the literature. Even better separation between the two classes can be achieved through machine learning methods which use the entire NIR spectra as an input. Moreover, we show that the H- and K-bands alone are enough for this purpose. Finally, we evaluate the relative importance of different spectral regions for gravity classification as returned by the machine learning models. We find that the H-band broad-band shape is the most relevant feature, followed by the FeH absorption bands at 1.2 $渭m$ and 1.24 $渭m$ and the KI doublet at 1.24 $渭m$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.06368v1-abstract-full').style.display = 'none'; document.getElementById('2110.06368v1-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 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">23 pages, 19 figures. Accepted by A&A, SINFONI spectroscopic data will be made public on Vizier upon publication</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 657, A129 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.00561">arXiv:2108.00561</a> <span> [<a href="https://arxiv.org/pdf/2108.00561">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> </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/stab2248">10.1093/mnras/stab2248 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GALExtin: An alternative online tool to determine the interstellar extinction in the Milky Way </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Amores%2C+E+B">Eduardo B. Amores</a>, <a href="/search/astro-ph?searchtype=author&query=Jesus%2C+R+M">Ricardo M. Jesus</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">Andre Moitinho</a>, <a href="/search/astro-ph?searchtype=author&query=Arsenijevic%2C+V">Vladan Arsenijevic</a>, <a href="/search/astro-ph?searchtype=author&query=Levenhagen%2C+R+S">Ronaldo S. Levenhagen</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+D+J">Douglas J. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Kerber%2C+L+O">Leandro O. Kerber</a>, <a href="/search/astro-ph?searchtype=author&query=Kunzel%2C+R">Roseli Kunzel</a>, <a href="/search/astro-ph?searchtype=author&query=Moura%2C+R+A">Rodrigo A. Moura</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="2108.00561v1-abstract-short" style="display: inline;"> Estimates of interstellar extinction are essential in a broad range of astronomical research. In the last decades, several maps and models of the large scale interstellar extinction in the Galaxy have been published. However, these maps and models have been developed in different programming languages, with different user interfaces and input/output formats, which makes using and comparing results… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.00561v1-abstract-full').style.display = 'inline'; document.getElementById('2108.00561v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.00561v1-abstract-full" style="display: none;"> Estimates of interstellar extinction are essential in a broad range of astronomical research. In the last decades, several maps and models of the large scale interstellar extinction in the Galaxy have been published. However, these maps and models have been developed in different programming languages, with different user interfaces and input/output formats, which makes using and comparing results from these maps and models difficult. To address this issue, we have developed a tool called GALExtin (\url{http://www.galextin.org}) - that estimates interstellar extinction based on both 3D models/maps and 2D maps available. The user only needs to provide a list with coordinates (and distance) and to choose a model/map. GALExtin will then provide an output list with extinction estimates. It can be implemented in any other portal or model that requires interstellar extinction estimates. Here, a general overview of GALExtin is presented, along with its capabilities, validation, performance and some results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.00561v1-abstract-full').style.display = 'none'; document.getElementById('2108.00561v1-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 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">12 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/2103.12829">arXiv:2103.12829</a> <span> [<a href="https://arxiv.org/pdf/2103.12829">pdf</a>, <a href="https://arxiv.org/format/2103.12829">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/stab770">10.1093/mnras/stab770 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Updated parameters of 1743 open clusters based on Gaia DR2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dias%2C+W+S">Wilton S. Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Monteiro%2C+H">H茅ktor Monteiro</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">Aandr茅 Moitinho</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%A9pine%2C+J+R+D">J谩cques R. D. L茅pine</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">Giovanni Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Paunzen%2C+E">Ernst Paunzen</a>, <a href="/search/astro-ph?searchtype=author&query=Alessi%2C+B">Bruno Alessi</a>, <a href="/search/astro-ph?searchtype=author&query=Villela%2C+L">L谩zaro Villela</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="2103.12829v1-abstract-short" style="display: inline;"> In this study we follow up our recent paper (Monteiro et al. 2020) and present a homogeneous sample of fundamental parameters of open clusters in our Galaxy, entirely based on Gaia DR2 data. We used published membership probability of the stars derived from Gaia DR2 data and applied our isochrone fitting code, updated as in Monteiro et al. (2020), to GB and GR Gaia DR2 data for member stars. In do… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.12829v1-abstract-full').style.display = 'inline'; document.getElementById('2103.12829v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.12829v1-abstract-full" style="display: none;"> In this study we follow up our recent paper (Monteiro et al. 2020) and present a homogeneous sample of fundamental parameters of open clusters in our Galaxy, entirely based on Gaia DR2 data. We used published membership probability of the stars derived from Gaia DR2 data and applied our isochrone fitting code, updated as in Monteiro et al. (2020), to GB and GR Gaia DR2 data for member stars. In doing this we take into account the nominal errors in the data and derive distance, age, and extinction of each cluster. This work therefore provides parameters for 1743 open clusters and, as a byproduct, a list of likely not physical or dubious open clusters is provided as well for future investigations. Furthermore, it was possible to estimate the mean radial velocity of 831 clusters (198 of which are new and unpublished so far) using stellar radial velocities from Gaia DR2 catalog. By comparing the open cluster distances obtained from isochrone fitting with those obtained from a maximum likelihood estimate of individual member parallaxes, we found a systematic offset of $(-0.05\pm0.04)$mas. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.12829v1-abstract-full').style.display = 'none'; document.getElementById('2103.12829v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">18 pages, 23 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/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/2101.01660">arXiv:2101.01660</a> <span> [<a href="https://arxiv.org/pdf/2101.01660">pdf</a>, <a href="https://arxiv.org/format/2101.01660">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/10.1051/0004-6361/202040252">10.1051/0004-6361/202040252 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> pyUPMASK: an improved unsupervised clustering algorithm </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pera%2C+M+S">M. S. Pera</a>, <a href="/search/astro-ph?searchtype=author&query=Perren%2C+G+I">G. I. Perren</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">A. Moitinho</a>, <a href="/search/astro-ph?searchtype=author&query=Navone%2C+H+D">H. D. Navone</a>, <a href="/search/astro-ph?searchtype=author&query=Vazquez%2C+R+A">R. A. Vazquez</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="2101.01660v3-abstract-short" style="display: inline;"> Aims. We present pyUPMASK, an unsupervised clustering method for stellar clusters that builds upon the original UPMASK package. Its general approach makes it plausible to be applied to analyses that deal with binary classes of any kind, as long as the fundamental hypotheses are met. The code is written entirely in Python and is made available through a public repository. Methods.The core of the al… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.01660v3-abstract-full').style.display = 'inline'; document.getElementById('2101.01660v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.01660v3-abstract-full" style="display: none;"> Aims. We present pyUPMASK, an unsupervised clustering method for stellar clusters that builds upon the original UPMASK package. Its general approach makes it plausible to be applied to analyses that deal with binary classes of any kind, as long as the fundamental hypotheses are met. The code is written entirely in Python and is made available through a public repository. Methods.The core of the algorithm follows the method developed in UPMASK but introducing several key enhancements. These enhancements not only make pyUPMASK more general, they also improve its performance considerably. Results. We thoroughly tested the performance of pyUPMASK on 600 synthetic clusters, affected by varying degrees of contamination by field stars. To assess the performance we employed six different statistical metrics that measure the accuracy of probabilistic classification. Conclusions. Our results show that pyUPMASK is better performant than UPMASK for every statistical performance metric, while still managing to be many times faster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.01660v3-abstract-full').style.display = 'none'; document.getElementById('2101.01660v3-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 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 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">Journal ref:</span> A&A 650, A109 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.04017">arXiv:2012.04017</a> <span> [<a href="https://arxiv.org/pdf/2012.04017">pdf</a>, <a href="https://arxiv.org/format/2012.04017">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/10.1051/0004-6361/202039388">10.1051/0004-6361/202039388 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> 3D kinematics and age distribution of the Open Cluster population </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tarricq%2C+Y">Y. Tarricq</a>, <a href="/search/astro-ph?searchtype=author&query=Soubiran%2C+C">C. Soubiran</a>, <a href="/search/astro-ph?searchtype=author&query=Casamiquela%2C+L">L. Casamiquela</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=Anders%2C+F">F. Anders</a>, <a href="/search/astro-ph?searchtype=author&query=Antoja%2C+T">T. Antoja</a>, <a href="/search/astro-ph?searchtype=author&query=Romero-G%C3%B3mez%2C+M">M. Romero-G贸mez</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=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Balaguer-N%C3%BA%C3%B1ez%2C+L">L. Balaguer-N煤帽ez</a>, <a href="/search/astro-ph?searchtype=author&query=Carrera%2C+R">R. Carrera</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=Moitinho%2C+A">A. Moitinho</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos%2C+P">P. Ramos</a>, <a href="/search/astro-ph?searchtype=author&query=Bossini%2C+D">D. Bossini</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.04017v1-abstract-short" style="display: inline;"> Open Clusters (OCs) can trace with a great accuracy the evolution of the Galactic disk. The aim of this work is to study the kinematical behavior of the OC population over time. We take advantage of the latest age determinations of OCs to investigate the correlations of the 6D phase space coordinates and orbital properties with age. We also investigate the rotation curve of the Milky Way traced by… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.04017v1-abstract-full').style.display = 'inline'; document.getElementById('2012.04017v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.04017v1-abstract-full" style="display: none;"> Open Clusters (OCs) can trace with a great accuracy the evolution of the Galactic disk. The aim of this work is to study the kinematical behavior of the OC population over time. We take advantage of the latest age determinations of OCs to investigate the correlations of the 6D phase space coordinates and orbital properties with age. We also investigate the rotation curve of the Milky Way traced by OCs and we compare it to that of other observational or theoretical studies. We gathered nearly 30000 Radial Velocity (RV) measurements of OC members from both Gaia-RVS data and ground based surveys and catalogues. We computed the weighted mean RV, Galactic velocities and orbital parameters of 1382 OCs. We investigated their distributions as a function of age, and by comparison to field stars. We provide the largest RV catalogue available for OCs, half of it based on at least 3 members. Compared to field stars, we note that OCs are not exactly on the same arches in the radial-azimuthal velocity plane, while they seem to follow the same diagonal ridges in the Galactic radial distribution of azimuthal velocities. Velocity ellipsoids in different age bins all show a clear anisotropy. The heating rate of the OC population is similar to that of field stars for the radial and azimuthal components but significantly lower for the vertical component. The rotation curve drawn by our sample of clusters shows several dips, which match the wiggles derived from non-axisymmetric models of the Galaxy. From the computation of orbits, we obtain a clear dependence of the maximum height and eccentricity with age. Finally, the orbital characteristics of the sample of clusters as shown by the action variables, follow the distribution of field stars. The additional age information of the clusters points towards some (weak) age dependence of the known moving groups. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.04017v1-abstract-full').style.display = 'none'; document.getElementById('2012.04017v1-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, 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">Accepted for publication in A&A, 16 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 647, A19 (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/2012.01771">arXiv:2012.01771</a> <span> [<a href="https://arxiv.org/pdf/2012.01771">pdf</a>, <a href="https://arxiv.org/format/2012.01771">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/10.1051/0004-6361/202039588">10.1051/0004-6361/202039588 <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: Structure and properties of the Magellanic Clouds </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=Luri%2C+X">X. Luri</a>, <a href="/search/astro-ph?searchtype=author&query=Chemin%2C+L">L. Chemin</a>, <a href="/search/astro-ph?searchtype=author&query=Clementini%2C+G">G. Clementini</a>, <a href="/search/astro-ph?searchtype=author&query=Delgado%2C+H+E">H. E. Delgado</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=Romero-G%C3%B3mez%2C+M">M. Romero-G贸mez</a>, <a href="/search/astro-ph?searchtype=author&query=Balbinot%2C+E">E. Balbinot</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=Mor%2C+R">R. Mor</a>, <a href="/search/astro-ph?searchtype=author&query=Ripepi%2C+V">V. Ripepi</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=Cioni%2C+M+-+L">M. -R. L. Cioni</a>, <a href="/search/astro-ph?searchtype=author&query=Fabricius%2C+C">C. Fabricius</a>, <a href="/search/astro-ph?searchtype=author&query=Garofalo%2C+A">A. Garofalo</a>, <a href="/search/astro-ph?searchtype=author&query=Helmi%2C+A">A. Helmi</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%2C+J+H+J">J. H. J. de</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. (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="2012.01771v4-abstract-short" style="display: inline;"> We compare the Gaia DR2 and Gaia EDR3 performances in the study of the Magellanic Clouds and show the clear improvements in precision and accuracy in the new release. We also show that the systematics still present in the data make the determination of the 3D geometry of the LMC a difficult endeavour; this is at the very limit of the usefulness of the Gaia EDR3 astrometry, but it may become feasib… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.01771v4-abstract-full').style.display = 'inline'; document.getElementById('2012.01771v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.01771v4-abstract-full" style="display: none;"> We compare the Gaia DR2 and Gaia EDR3 performances in the study of the Magellanic Clouds and show the clear improvements in precision and accuracy in the new release. We also show that the systematics still present in the data make the determination of the 3D geometry of the LMC a difficult endeavour; this is at the very limit of the usefulness of the Gaia EDR3 astrometry, but it may become feasible with the use of additional external data. We derive radial and tangential velocity maps and global profiles for the LMC for the several subsamples we defined. To our knowledge, this is the first time that the two planar components of the ordered and random motions are derived for multiple stellar evolutionary phases in a galactic disc outside the Milky Way, showing the differences between younger and older phases. We also analyse the spatial structure and motions in the central region, the bar, and the disc, providing new insights into features and kinematics. Finally, we show that the Gaia EDR3 data allows clearly resolving the Magellanic Bridge, and we trace the density and velocity flow of the stars from the SMC towards the LMC not only globally, but also separately for young and evolved populations. This allows us to confirm an evolved population in the Bridge that is slightly shift from the younger population. Additionally, we were able to study the outskirts of both Magellanic Clouds, in which we detected some well-known features and indications of new ones. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.01771v4-abstract-full').style.display = 'none'; document.getElementById('2012.01771v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">This paper is part of the "demonstration papers" released with Gaia EDR3: https://www.cosmos.esa.int/web/gaia/earlydr3</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 649, A7 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.01533">arXiv:2012.01533</a> <span> [<a href="https://arxiv.org/pdf/2012.01533">pdf</a>, <a href="https://arxiv.org/format/2012.01533">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/10.1051/0004-6361/202039657e">10.1051/0004-6361/202039657e <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: Summary of the contents 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=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>, <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">U. 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>, <a href="/search/astro-ph?searchtype=author&query=Walton%2C+N+A">N. A. Walton</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a> , et al. (401 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="2012.01533v2-abstract-short" style="display: inline;"> We present the early installment of the third Gaia data release, Gaia EDR3, consisting of astrometry and photometry for 1.8 billion sources brighter than magnitude 21, complemented with the list of radial velocities from Gaia DR2. Gaia EDR3 contains celestial positions and the apparent brightness in G for approximately 1.8 billion sources. For 1.5 billion of those sources, parallaxes, proper motio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.01533v2-abstract-full').style.display = 'inline'; document.getElementById('2012.01533v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.01533v2-abstract-full" style="display: none;"> We present the early installment of the third Gaia data release, Gaia EDR3, consisting of astrometry and photometry for 1.8 billion sources brighter than magnitude 21, complemented with the list of radial velocities from Gaia DR2. Gaia EDR3 contains celestial positions and the apparent brightness in G for approximately 1.8 billion sources. For 1.5 billion of those sources, parallaxes, proper motions, and the (G_BP-G_RP) colour are also available. The passbands for G, G_BP, and G_RP are provided as part of the release. For ease of use, the 7 million radial velocities from Gaia DR2 are included in this release, after the removal of a small number of spurious values. New radial velocities will appear as part of Gaia DR3. Finally, Gaia EDR3 represents an updated materialisation of the celestial reference frame (CRF) in the optical, the Gaia-CRF3, which is based solely on extragalactic sources. The creation of the source list for Gaia EDR3 includes enhancements that make it more robust with respect to high proper motion stars, and the disturbing effects of spurious and partially resolved sources. The source list is largely the same as that for Gaia DR2, but it does feature new sources and there are some notable changes. The source list will not change for Gaia DR3. Gaia EDR3 represents a significant advance over Gaia DR2, with parallax precisions increased by 30 percent, proper motion precisions increased by a factor of 2, and the systematic errors in the astrometry suppressed by 30--40 percent for the parallaxes and by a factor ~2.5 for the proper motions. The photometry also features increased precision, but above all much better homogeneity across colour, magnitude, and celestial position. A single passband for G, G_BP, and G_RP is valid over the entire magnitude and colour range, with no systematics above the 1 percent level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.01533v2-abstract-full').style.display = 'none'; document.getElementById('2012.01533v2-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 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">Accepted for A&A Special Issue on Gaia EDR3, 21 pages, 2 figures. This version includes the updates in the erratum (https://doi.org/10.1051/0004-6361/202039657e)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 650, C3 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.11834">arXiv:2009.11834</a> <span> [<a href="https://arxiv.org/pdf/2009.11834">pdf</a>, <a href="https://arxiv.org/format/2009.11834">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/10.1093/mnras/staa2983">10.1093/mnras/staa2983 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Fundamental parameters for 45 open clusters with Gaia DR2, an improved extinction correction and a metallicity gradient prior </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Monteiro%2C+H">H. Monteiro</a>, <a href="/search/astro-ph?searchtype=author&query=Dias%2C+W+S">W. S. Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">A. Moitinho</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=L%C3%A9pine%2C+J+R+D">J. R. D. L茅pine</a>, <a href="/search/astro-ph?searchtype=author&query=G."> G.</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro"> Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Paunzen%2C+E">E. Paunzen</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="2009.11834v1-abstract-short" style="display: inline;"> Reliable fundamental parameters of open clusters such as distance, age and extinction are key to our understanding of Galactic structure and stellar evolution. In this work we use {\it Gaia} DR2 to investigate 45 open clusters listed in the \emph{New catalogue of optically visible open clusters and candidates} (DAML) but with no previous astrometric membership estimation based on {\it Gaia} DR2. I… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.11834v1-abstract-full').style.display = 'inline'; document.getElementById('2009.11834v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.11834v1-abstract-full" style="display: none;"> Reliable fundamental parameters of open clusters such as distance, age and extinction are key to our understanding of Galactic structure and stellar evolution. In this work we use {\it Gaia} DR2 to investigate 45 open clusters listed in the \emph{New catalogue of optically visible open clusters and candidates} (DAML) but with no previous astrometric membership estimation based on {\it Gaia} DR2. In the process of selecting targets for this study we found that some clusters reported as new discoveries in recent papers based on {\it Gaia} DR2 were already known clusters listed in DAML. Cluster memberships were determined using a maximum likelihood method applied to {\it Gaia} DR2 astrometry. This has allowed us to estimate mean proper motions and mean parallaxes for all investigated clusters. Mean radial velocities were also determined for 12 clusters, 7 of which had no previous published values. We have improved our isochrone fitting code to account for interstellar extinction using an updated extinction polynomial for the {\it Gaia} DR2 photometric band-passes and the Galactic abundance gradient as a prior for metallicity. The updated procedure was validated with a sample of clusters with high quality $[Fe/H]$ determinations. We then did a critical review of the literature and verified that our cluster parameter determinations represent a substantial improvement over previous values. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.11834v1-abstract-full').style.display = 'none'; document.getElementById('2009.11834v1-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 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">19 pages, 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/2004.07274">arXiv:2004.07274</a> <span> [<a href="https://arxiv.org/pdf/2004.07274">pdf</a>, <a href="https://arxiv.org/format/2004.07274">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/10.1051/0004-6361/202038192">10.1051/0004-6361/202038192 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Painting a portrait of the Galactic disc with its stellar clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cantat-Gaudin%2C+T">T. Cantat-Gaudin</a>, <a href="/search/astro-ph?searchtype=author&query=Anders%2C+F">F. Anders</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=Jordi%2C+C">C. Jordi</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=Soubiran%2C+C">C. Soubiran</a>, <a href="/search/astro-ph?searchtype=author&query=Casamiquela%2C+L">L. Casamiquela</a>, <a href="/search/astro-ph?searchtype=author&query=Tarricq%2C+Y">Y. Tarricq</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">A. Moitinho</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</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=Kounkel%2C+M">M. Kounkel</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="2004.07274v2-abstract-short" style="display: inline;"> The large astrometric and photometric survey performed by the Gaia mission allows for a panoptic view of the Galactic disc and in its stellar cluster population. Hundreds of clusters were only discovered after the latest G data release (DR2) and have yet to be characterised. Here we make use of the deep and homogeneous Gaia photometry down to G=18 to estimate the distance, age, and interstellar re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.07274v2-abstract-full').style.display = 'inline'; document.getElementById('2004.07274v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.07274v2-abstract-full" style="display: none;"> The large astrometric and photometric survey performed by the Gaia mission allows for a panoptic view of the Galactic disc and in its stellar cluster population. Hundreds of clusters were only discovered after the latest G data release (DR2) and have yet to be characterised. Here we make use of the deep and homogeneous Gaia photometry down to G=18 to estimate the distance, age, and interstellar reddening for about 2000 clusters identified with Gaia~DR2 astrometry. We use these objects to study the structure and evolution of the Galactic disc. We rely on a set of objects with well-determined parameters in the literature to train an artificial neural network to estimate parameters from the Gaia photometry of cluster members and their mean parallax. We obtain reliable parameters for 1867 clusters. Our new homogeneous catalogue confirms the relative lack of old clusters in the inner disc (with a few notable exceptions). We also quantify and discuss the variation of scale height with cluster age, and detect the Galactic warp in the distribution of old clusters. This work results in a large and homogenous cluster catalogue. However, the present sample is still unable to trace the Outer spiral arm of the Milky Way, which indicates that the outer disc cluster census might still be incomplete. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.07274v2-abstract-full').style.display = 'none'; document.getElementById('2004.07274v2-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 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">19 pages, 13 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 640, A1 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2003.12138">arXiv:2003.12138</a> <span> [<a href="https://arxiv.org/pdf/2003.12138">pdf</a>, <a href="https://arxiv.org/format/2003.12138">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/10.1051/0004-6361/201937141">10.1051/0004-6361/201937141 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sixteen overlooked open clusters in the fourth Galactic quadrant. A combined analysis of UBVI photometry and Gaia DR2 with ASteCA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Perren%2C+G+I">G. I. Perren</a>, <a href="/search/astro-ph?searchtype=author&query=Giorgi%2C+E+E">E. E. Giorgi</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">A. Moitinho</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Pera%2C+M+S">M. S. Pera</a>, <a href="/search/astro-ph?searchtype=author&query=V%C3%A1zquez%2C+R+A">R. A. V谩zquez</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="2003.12138v1-abstract-short" style="display: inline;"> Aims: This paper has two main objectives: (1) To determine the intrinsic properties of 16 faint and mostly unstudied open clusters in the poorly known sector of the Galaxy at 270$^\circ-$300$^\circ$, to probe the Milky Way structure in future investigations. (2) To address previously reported systematics in Gaia DR2 parallaxes by comparing the cluster distances derived from photometry with those d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.12138v1-abstract-full').style.display = 'inline'; document.getElementById('2003.12138v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.12138v1-abstract-full" style="display: none;"> Aims: This paper has two main objectives: (1) To determine the intrinsic properties of 16 faint and mostly unstudied open clusters in the poorly known sector of the Galaxy at 270$^\circ-$300$^\circ$, to probe the Milky Way structure in future investigations. (2) To address previously reported systematics in Gaia DR2 parallaxes by comparing the cluster distances derived from photometry with those derived from parallaxes. Methods: Deep UBVI photometry of 16 open clusters was carried out. Observations were reduced and analyzed in an automaticway using the ASteCA package to get individual distances, reddening, masses, ages and metallicities. Photometric distances were compared to those obtained from a Bayesian analysis of Gaia DR2 parallaxes. Results: Ten out of the 16 clusters are true or highly probable open clusters. Two of them are quite young and follow the trace of the Carina Arm and the already detected warp. The rest of the clusters are placed in the interarm zone between the Perseus and Carina Arms as expected for older objects. We found that the cluster van den Berg-Hagen 85 is 7.5$\times$10$^9$ yrs old becoming then one of the oldest open cluster detected in our Galaxy so far. The relationship of these ten clusters with the Galaxy structure in the solar neighborhood is discussed. The comparison of distances from photometry and parallaxes data, in turn, reveals a variable level of disagreement. Conclusions: Various zero point corrections for Gaia DR2 parallax data recently reported were considered for a comparison between photometric and parallax based distances. The results tend to improve with some of these corrections. Photometric distance analysis suggest an average correction of $\sim$+0.026 mas (to be added to the parallaxes). The correction may have a more intricate distance dependency, but addressing that level of detail will require a larger cluster sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.12138v1-abstract-full').style.display = 'none'; document.getElementById('2003.12138v1-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 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">70 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 637, A95 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.08028">arXiv:1910.08028</a> <span> [<a href="https://arxiv.org/pdf/1910.08028">pdf</a>, <a href="https://arxiv.org/format/1910.08028">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> ESA Voyage 2050 white paper -- Faint objects in motion: the new frontier of high precision astrometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Malbet%2C+F">F. Malbet</a>, <a href="/search/astro-ph?searchtype=author&query=Abbas%2C+U">U. Abbas</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+J">J. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Boehm%2C+C">C. Boehm</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+W">W. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Chemin%2C+L">L. Chemin</a>, <a href="/search/astro-ph?searchtype=author&query=Correia%2C+A">A. Correia</a>, <a href="/search/astro-ph?searchtype=author&query=Courbin%2C+F">F. Courbin</a>, <a href="/search/astro-ph?searchtype=author&query=Darling%2C+J">J. Darling</a>, <a href="/search/astro-ph?searchtype=author&query=Diaferio%2C+A">A. Diaferio</a>, <a href="/search/astro-ph?searchtype=author&query=Fortin%2C+M">M. Fortin</a>, <a href="/search/astro-ph?searchtype=author&query=Fridlund%2C+M">M. Fridlund</a>, <a href="/search/astro-ph?searchtype=author&query=Gnedin%2C+O">O. Gnedin</a>, <a href="/search/astro-ph?searchtype=author&query=Holl%2C+B">B. Holl</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=L%C3%A9ger%2C+A">A. L茅ger</a>, <a href="/search/astro-ph?searchtype=author&query=Labadie%2C+L">L. Labadie</a>, <a href="/search/astro-ph?searchtype=author&query=Laskar%2C+J">J. Laskar</a>, <a href="/search/astro-ph?searchtype=author&query=Mamon%2C+G">G. Mamon</a>, <a href="/search/astro-ph?searchtype=author&query=McArthur%2C+B">B. McArthur</a>, <a href="/search/astro-ph?searchtype=author&query=Michalik%2C+D">D. Michalik</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">A. Moitinho</a>, <a href="/search/astro-ph?searchtype=author&query=Oertel%2C+M">M. Oertel</a>, <a href="/search/astro-ph?searchtype=author&query=Ostorero%2C+L">L. Ostorero</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+J">J. Schneider</a> , et al. (6 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="1910.08028v1-abstract-short" style="display: inline;"> Sky survey telescopes and powerful targeted telescopes play complementary roles in astronomy. In order to investigate the nature and characteristics of the motions of very faint objects, a flexibly-pointed instrument capable of high astrometric accuracy is an ideal complement to current astrometric surveys and a unique tool for precision astrophysics. Such a space-based mission will push the front… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.08028v1-abstract-full').style.display = 'inline'; document.getElementById('1910.08028v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.08028v1-abstract-full" style="display: none;"> Sky survey telescopes and powerful targeted telescopes play complementary roles in astronomy. In order to investigate the nature and characteristics of the motions of very faint objects, a flexibly-pointed instrument capable of high astrometric accuracy is an ideal complement to current astrometric surveys and a unique tool for precision astrophysics. Such a space-based mission will push the frontier of precision astrometry from evidence of earth-massed habitable worlds around the nearest starts, and also into distant Milky way objects up to the Local Group of galaxies. As we enter the era of the James Webb Space Telescope and the new ground-based, adaptive-optics-enabled giant telescopes, by obtaining these high precision measurements on key objects that Gaia could not reach, a mission that focuses on high precision astrometry science can consolidate our theoretical understanding of the local universe, enable extrapolation of physical processes to remote redshifts, and derive a much more consistent picture of cosmological evolution and the likely fate of our cosmos. Already several missions have been proposed to address the science case of faint objects in motion using high precision astrometry ESA missions: NEAT for M3, micro-NEAT for S1 mission, and Theia for M4 and M5. Additional new mission configurations adapted with technological innovations could be envisioned to pursue accurate measurements of these extremely small motions. The goal of this white paper is to address the fundamental science questions that are at stake when we focus on the motions of faint sky objects and to briefly review quickly instrumentation and mission profiles. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.08028v1-abstract-full').style.display = 'none'; document.getElementById('1910.08028v1-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 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </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">White paper for the Voyage 2050 long-term plan in the ESA Science Programme. arXiv admin note: substantial text overlap with arXiv:1707.01348</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1906.09500">arXiv:1906.09500</a> <span> [<a href="https://arxiv.org/pdf/1906.09500">pdf</a>, <a href="https://arxiv.org/format/1906.09500">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/10.1051/0004-6361/201935243">10.1051/0004-6361/201935243 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Solving the distance discrepancy for the open cluster NGC 2453. The planetary nebula NGC 2452 is not a cluster member </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-D%C3%ADaz%2C+D">D. Gonz谩lez-D铆az</a>, <a href="/search/astro-ph?searchtype=author&query=Bidin%2C+C+M">C. Moni Bidin</a>, <a href="/search/astro-ph?searchtype=author&query=Silva-Villa%2C+E">E. Silva-Villa</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+G">G. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Majaess%2C+D">D. Majaess</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">A. Moitinho</a>, <a href="/search/astro-ph?searchtype=author&query=Orquera-Rojas"> Orquera-Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Mar%C3%ADn%2C+C+A+L+M">C. A. L. Morales Mar铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Morales-Campa%C3%B1a%2C+E">E. Morales-Campa帽a</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="1906.09500v1-abstract-short" style="display: inline;"> The open cluster (OC) NGC 2453 is of particular importance since it has been considered to host the planetary nebula (PN) NGC 2452, however their distances and radial velocities are strongly contested. In order to obtain a complete picture of the fundamental parameters of the OC NGC 2453, 11 potential members were studied. The results allowed us to resolve the PN NGC 2452 membership debate. Radial… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.09500v1-abstract-full').style.display = 'inline'; document.getElementById('1906.09500v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.09500v1-abstract-full" style="display: none;"> The open cluster (OC) NGC 2453 is of particular importance since it has been considered to host the planetary nebula (PN) NGC 2452, however their distances and radial velocities are strongly contested. In order to obtain a complete picture of the fundamental parameters of the OC NGC 2453, 11 potential members were studied. The results allowed us to resolve the PN NGC 2452 membership debate. Radial velocities for the 11 stars in NGC 2453 and the PN were measured and matched with Gaia data release 2 (DR2) to estimate the cluster distance. In addition, we used deep multi-band UBVRI photometry to get fundamental parameters of the cluster via isochrone fitting on the most likely cluster members, reducing inaccuracies due to field stars.The distance of the OC NGC 2453 (4.7 $\pm$ 0.2 kpc) was obtained with an independent method solving the discrepancy reported in the literature. This result is in good agreement with an isochrone fitting of 40-50 Myr. On the other hand, the radial velocity of NGC 2453 ($78 \pm 3$ km s$^{-1}$) disagrees with the velocity of NGC2452 ($62 \pm 2$ km s$^{-1}$). Our results show that the PN is a foreground object in the line of sight. Due to the discrepancies found in the parameters studied, we conclude that the PN NGC 2452 is not a member of the OC NGC 2453. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.09500v1-abstract-full').style.display = 'none'; document.getElementById('1906.09500v1-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 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2019. </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, 7 figures, 4 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 626, A10 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1901.04733">arXiv:1901.04733</a> <span> [<a href="https://arxiv.org/pdf/1901.04733">pdf</a>, <a href="https://arxiv.org/format/1901.04733">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/10.1051/0004-6361/201834693">10.1051/0004-6361/201834693 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Age determination for 269 $Gaia$ DR2 Open Clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bossini%2C+D">D. Bossini</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</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=Sordo%2C+R">R. Sordo</a>, <a href="/search/astro-ph?searchtype=author&query=Balaguer-N%C3%BA%C3%B1ez%2C+L">L. Balaguer-N煤帽ez</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">A. Moitinho</a>, <a href="/search/astro-ph?searchtype=author&query=Soubiran%2C+C">C. Soubiran</a>, <a href="/search/astro-ph?searchtype=author&query=Casamiquela%2C+L">L. Casamiquela</a>, <a href="/search/astro-ph?searchtype=author&query=Carrera%2C+R">R. Carrera</a>, <a href="/search/astro-ph?searchtype=author&query=Heiter%2C+U">U. Heiter</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="1901.04733v1-abstract-short" style="display: inline;"> $Context$. Gaia Second Data Release provides precise astrometry and photometry for more than 1.3 billion sources. This catalog opens a new era concerning the characterization of open clusters and test stellar models, paving the way for a better understanding of the disc properties. $Aims… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.04733v1-abstract-full').style.display = 'inline'; document.getElementById('1901.04733v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.04733v1-abstract-full" style="display: none;"> $Context$. Gaia Second Data Release provides precise astrometry and photometry for more than 1.3 billion sources. This catalog opens a new era concerning the characterization of open clusters and test stellar models, paving the way for a better understanding of the disc properties. $Aims$. The aim of the paper is to improve the knowledge of cluster parameters, using only the unprecedented quality of the Gaia photometry and astrometry. $Methods$. We make use of the membership determination based on the precise Gaia astrometry and photometry. We apply anautomated Bayesian tool, BASE-9, to fit stellar isochrones on the observed G, GBP, GRP magnitudes of the high probability member stars. $Results$. We derive parameters such as age, distance modulus and extinction for a sample of 269 open clusters, selecting only low reddening objects and discarding very young clusters, for which techniques other than isochrone-fitting are more suitable for estimating ages. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.04733v1-abstract-full').style.display = 'none'; document.getElementById('1901.04733v1-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 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2019. </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, 11 figures. Submitted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 623, A108 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1810.05494">arXiv:1810.05494</a> <span> [<a href="https://arxiv.org/pdf/1810.05494">pdf</a>, <a href="https://arxiv.org/format/1810.05494">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/10.1051/0004-6361/201834453">10.1051/0004-6361/201834453 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia DR2 unravels incompleteness of nearby cluster population: New open clusters in the direction of Perseus </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cantat-Gaudin%2C+T">T. Cantat-Gaudin</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=Sedaghat%2C+N">N. Sedaghat</a>, <a href="/search/astro-ph?searchtype=author&query=Farahi%2C+A">A. Farahi</a>, <a href="/search/astro-ph?searchtype=author&query=de+Souza%2C+R+S">R. S. de Souza</a>, <a href="/search/astro-ph?searchtype=author&query=Skalidis%2C+R">R. Skalidis</a>, <a href="/search/astro-ph?searchtype=author&query=Malz%2C+A+I">A. I. Malz</a>, <a href="/search/astro-ph?searchtype=author&query=Mac%C3%AAdo%2C+S">S. Mac锚do</a>, <a href="/search/astro-ph?searchtype=author&query=Moews%2C+B">B. Moews</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">A. Moitinho</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=Ishida%2C+E+E+O">E. E. O. Ishida</a>, <a href="/search/astro-ph?searchtype=author&query=Heneka%2C+C">C. Heneka</a>, <a href="/search/astro-ph?searchtype=author&query=Boucaud%2C+A">A. Boucaud</a>, <a href="/search/astro-ph?searchtype=author&query=Trindade%2C+A+M+M">A. M. M. Trindade</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="1810.05494v3-abstract-short" style="display: inline;"> Open clusters (OCs) are popular tracers of the structure and evolutionary history of the Galactic disk. The OC population is often considered to be complete within 1.8 kpc of the Sun. The recent Gaia Data Release 2 (DR2) allows the latter claim to be challenged. We perform a systematic search for new OCs in the direction of Perseus using precise and accurate astrometry from Gaia DR2. We implement… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.05494v3-abstract-full').style.display = 'inline'; document.getElementById('1810.05494v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1810.05494v3-abstract-full" style="display: none;"> Open clusters (OCs) are popular tracers of the structure and evolutionary history of the Galactic disk. The OC population is often considered to be complete within 1.8 kpc of the Sun. The recent Gaia Data Release 2 (DR2) allows the latter claim to be challenged. We perform a systematic search for new OCs in the direction of Perseus using precise and accurate astrometry from Gaia DR2. We implement a coarse-to-fine search method. First, we exploit spatial proximity using a fast density-aware partitioning of the sky via a k-d tree in the spatial domain of Galactic coordinates, (l, b). Secondly, we employ a Gaussian mixture model in the proper motion space to quickly tag fields around OC candidates. Thirdly, we apply an unsupervised membership assignment method, UPMASK, to scrutinise the candidates. We visually inspect colour-magnitude diagrams to validate the detected objects. Finally, we perform a diagnostic to quantify the significance of each identified overdensity in proper motion and in parallax space We report the discovery of 41 new stellar clusters. This represents an increment of at least 20% of the previously known OC population in this volume of the Milky Way. We also report on the clear identification of NGC 886, an object previously considered an asterism. This letter challenges the previous claim of a near-complete sample of open clusters up to 1.8 kpc. Our results reveal that this claim requires revision, and a complete census of nearby open clusters is yet to be found. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.05494v3-abstract-full').style.display = 'none'; document.getElementById('1810.05494v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 October, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2018. </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</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 624, A126 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.05952">arXiv:1808.05952</a> <span> [<a href="https://arxiv.org/pdf/1808.05952">pdf</a>, <a href="https://arxiv.org/format/1808.05952">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/10.1051/0004-6361/201833901">10.1051/0004-6361/201833901 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> 3D shape of Orion A from Gaia DR2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Grossschedl%2C+J+E">Josefa E. Grossschedl</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+J">Joao Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Meingast%2C+S">Stefan Meingast</a>, <a href="/search/astro-ph?searchtype=author&query=Ackerl%2C+C">Christine Ackerl</a>, <a href="/search/astro-ph?searchtype=author&query=Ascenso%2C+J">Joana Ascenso</a>, <a href="/search/astro-ph?searchtype=author&query=Bouy%2C+H">Herve Bouy</a>, <a href="/search/astro-ph?searchtype=author&query=Burkert%2C+A">Andreas Burkert</a>, <a href="/search/astro-ph?searchtype=author&query=Forbrich%2C+J">Jan Forbrich</a>, <a href="/search/astro-ph?searchtype=author&query=Fuernkranz%2C+V">Verena Fuernkranz</a>, <a href="/search/astro-ph?searchtype=author&query=Goodman%2C+A">Alyssa Goodman</a>, <a href="/search/astro-ph?searchtype=author&query=Hacar%2C+A">Alvaro Hacar</a>, <a href="/search/astro-ph?searchtype=author&query=Herbst-Kiss%2C+G">Gabor Herbst-Kiss</a>, <a href="/search/astro-ph?searchtype=author&query=Lada%2C+C+J">Charles J. Lada</a>, <a href="/search/astro-ph?searchtype=author&query=Larreina%2C+I">Irati Larreina</a>, <a href="/search/astro-ph?searchtype=author&query=Leschinski%2C+K">Kieran Leschinski</a>, <a href="/search/astro-ph?searchtype=author&query=Lombardi%2C+M">Marco Lombardi</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">Andre Moitinho</a>, <a href="/search/astro-ph?searchtype=author&query=Mortimer%2C+D">Daniel Mortimer</a>, <a href="/search/astro-ph?searchtype=author&query=Zari%2C+E">Eleonora Zari</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="1808.05952v1-abstract-short" style="display: inline;"> We use the $\mathit{Gaia}$ DR2 distances of about 700 mid-infrared selected young stellar objects in the benchmark giant molecular cloud Orion A to infer its 3D shape and orientation. We find that Orion A is not the fairly straight filamentary cloud that we see in (2D) projection, but instead a cometary-like cloud oriented toward the Galactic plane, with two distinct components: a denser and enhan… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.05952v1-abstract-full').style.display = 'inline'; document.getElementById('1808.05952v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.05952v1-abstract-full" style="display: none;"> We use the $\mathit{Gaia}$ DR2 distances of about 700 mid-infrared selected young stellar objects in the benchmark giant molecular cloud Orion A to infer its 3D shape and orientation. We find that Orion A is not the fairly straight filamentary cloud that we see in (2D) projection, but instead a cometary-like cloud oriented toward the Galactic plane, with two distinct components: a denser and enhanced star-forming (bent) Head, and a lower density and star-formation quieter $\sim$75 pc long Tail. The true extent of Orion A is not the projected $\sim$40 pc but $\sim$90 pc, making it by far the largest molecular cloud in the local neighborhood. Its aspect ratio ($\sim$30:1) and high column-density fraction ($\sim45\%$) make it similar to large-scale Milky Way filaments ("bones"), despite its distance to the galactic mid-plane being an order of magnitude larger than typically found for these structures. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.05952v1-abstract-full').style.display = 'none'; document.getElementById('1808.05952v1-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> 17 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2018. </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">9 pages, 5 figures, 4 tables, 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 619, A106 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.01613">arXiv:1808.01613</a> <span> [<a href="https://arxiv.org/pdf/1808.01613">pdf</a>, <a href="https://arxiv.org/format/1808.01613">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/10.1051/0004-6361/201834020e">10.1051/0004-6361/201834020e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Open cluster kinematics with Gaia DR2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Soubiran%2C+C">C. Soubiran</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=Romero-G%C3%B3mez%2C+M">M. Romero-G贸mez</a>, <a href="/search/astro-ph?searchtype=author&query=Casamiquela%2C+L">L. Casamiquela</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Antoja%2C+T">T. Antoja</a>, <a href="/search/astro-ph?searchtype=author&query=Balaguer-N%C3%BA%C3%B1ez%2C+L">L. Balaguer-N煤帽ez</a>, <a href="/search/astro-ph?searchtype=author&query=Bossini%2C+D">D. Bossini</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Carrera%2C+R">R. Carrera</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=Figueras%2C+F">F. Figueras</a>, <a href="/search/astro-ph?searchtype=author&query=Heiter%2C+U">U. Heiter</a>, <a href="/search/astro-ph?searchtype=author&query=Katz%2C+D">D. Katz</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=Campion%2C+J+-+L">J. -F. Le Campion</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">A. Moitinho</a>, <a href="/search/astro-ph?searchtype=author&query=Sordo%2C+R">R. Sordo</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="1808.01613v3-abstract-short" style="display: inline;"> Context. Open clusters are very good tracers of the evolution of the Galactic disc. Thanks to Gaia, their kinematics can be investigated with an unprecedented precision and accuracy. Aims. The distribution of open clusters in the 6D phase space is revisited with Gaia DR2. Methods. The weighted mean radial velocity of open clusters was determined, using the most probable members available from a pr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.01613v3-abstract-full').style.display = 'inline'; document.getElementById('1808.01613v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.01613v3-abstract-full" style="display: none;"> Context. Open clusters are very good tracers of the evolution of the Galactic disc. Thanks to Gaia, their kinematics can be investigated with an unprecedented precision and accuracy. Aims. The distribution of open clusters in the 6D phase space is revisited with Gaia DR2. Methods. The weighted mean radial velocity of open clusters was determined, using the most probable members available from a previous astrometric investigation that also provided mean parallaxes and proper motions. Those parameters, all derived from Gaia DR2 only, were combined to provide the 6D phase space information of 861 clusters. The velocity distribution of nearby clusters was investigated, as well as the spatial and velocity distributions of the whole sample as a function of age. A high quality subsample was used to investigate some possible pairs and groups of clusters sharing the same Galactic position and velocity. Results. For the high quality sample that has 406 clusters, the median uncertainty of the weighted mean radial velocity is 0.5 km/s. The accuracy, assessed by comparison to ground-based high resolution spectroscopy, is better than 1 km/s. Open clusters nicely follow the velocity distribution of field stars in the close Solar neighbourhood previously revealed by Gaia DR2. As expected, the vertical distribution of young clusters is very flat but the novelty is the high precision to which this can be seen. The dispersion of vertical velocities of young clusters is at the level of 5 km/s. Clusters older than 1 Gyr span distances to the Galactic plane up to 1 kpc with a vertical velocity dispersion of 14 km/s, typical of the thin disc. Five pairs of clusters and one group with five members are possibly physically related. Other binary candidates previously identified turn out to be chance alignment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.01613v3-abstract-full').style.display = 'none'; document.getElementById('1808.01613v3-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 February, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2018. </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">Tables 4 and 5, and Fig. 12 of Sect. 3.3 corrected in the corrigendum sent 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 623, C2 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1805.08726">arXiv:1805.08726</a> <span> [<a href="https://arxiv.org/pdf/1805.08726">pdf</a>, <a href="https://arxiv.org/format/1805.08726">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/10.1051/0004-6361/201833476">10.1051/0004-6361/201833476 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Gaia DR2 view of the Open Cluster population in the Milky Way </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cantat-Gaudin%2C+T">T. Cantat-Gaudin</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Balaguer-N%C3%BA%C3%B1ez%2C+L">L. Balaguer-N煤帽ez</a>, <a href="/search/astro-ph?searchtype=author&query=Soubiran%2C+C">C. Soubiran</a>, <a href="/search/astro-ph?searchtype=author&query=Bossini%2C+D">D. Bossini</a>, <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">A. Moitinho</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=Krone-Martins%2C+A">A. Krone-Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Casamiquela%2C+L">L. Casamiquela</a>, <a href="/search/astro-ph?searchtype=author&query=Sordo%2C+R">R. Sordo</a>, <a href="/search/astro-ph?searchtype=author&query=Carrera%2C+R">R. Carrera</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="1805.08726v2-abstract-short" style="display: inline;"> Open clusters are convenient probes of the structure and history of the Galactic disk. They are also fundamental to stellar evolution studies. The second Gaia data release contains precise astrometry at the sub-milliarcsecond level and homogeneous photometry at the mmag level, that can be used to characterise a large number of clusters over the entire sky. In this study we aim to a establish list… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.08726v2-abstract-full').style.display = 'inline'; document.getElementById('1805.08726v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1805.08726v2-abstract-full" style="display: none;"> Open clusters are convenient probes of the structure and history of the Galactic disk. They are also fundamental to stellar evolution studies. The second Gaia data release contains precise astrometry at the sub-milliarcsecond level and homogeneous photometry at the mmag level, that can be used to characterise a large number of clusters over the entire sky. In this study we aim to a establish list of members and derive mean parameters, in particular distances, for as many clusters as possible, making use of Gaia data alone. We compile a list of thousands of known or putative clusters from the literature. We then apply an unsupervised membership assignment code, UPMASK, to the Gaia DR2 data contained within the fields of those clusters. We obtained a list of members and cluster parameters for 1229 clusters. As expected, the youngest clusters are seen to be tightly distributed near the Galactic plane and to trace the spiral arms of the Milky Way, while older objects are more uniformly distributed, deviate further from the plane, and tend to be located at larger Galactocentric distances. Thanks to the quality of GaiaDR2 astrometry, the fully homogeneous parameters derived in this study are the most precise to date. Furthermore, we report on the serendipitous discovery of 60 new open clusters in the fields analysed during this study. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.08726v2-abstract-full').style.display = 'none'; document.getElementById('1805.08726v2-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 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2018. </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 A&A, 19 pages, 13+20 figures, full data will be available at CDS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 618, A93 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1804.09378">arXiv:1804.09378</a> <span> [<a href="https://arxiv.org/pdf/1804.09378">pdf</a>, <a href="https://arxiv.org/format/1804.09378">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/10.1051/0004-6361/201832843">10.1051/0004-6361/201832843 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 2: Observational Hertzsprung-Russell diagrams </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=Babusiaux%2C+C">C. Babusiaux</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=Barstow%2C+M+A">M. A. Barstow</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Bossini%2C+D">D. Bossini</a>, <a href="/search/astro-ph?searchtype=author&query=Bressan%2C+A">A. Bressan</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=van+Leeuwen%2C+M">M. van Leeuwen</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=Bailer-Jones%2C+C+A+L">C. A. L. Bailer-Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</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=Jansen%2C+F">F. Jansen</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">U. 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> , et al. (428 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="1804.09378v2-abstract-short" style="display: inline;"> We highlight the power of the Gaia DR2 in studying many fine structures of the Hertzsprung-Russell diagram (HRD). Gaia allows us to present many different HRDs, depending in particular on stellar population selections. We do not aim here for completeness in terms of types of stars or stellar evolutionary aspects. Instead, we have chosen several illustrative examples. We describe some of the select… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.09378v2-abstract-full').style.display = 'inline'; document.getElementById('1804.09378v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.09378v2-abstract-full" style="display: none;"> We highlight the power of the Gaia DR2 in studying many fine structures of the Hertzsprung-Russell diagram (HRD). Gaia allows us to present many different HRDs, depending in particular on stellar population selections. We do not aim here for completeness in terms of types of stars or stellar evolutionary aspects. Instead, we have chosen several illustrative examples. We describe some of the selections that can be made in Gaia DR2 to highlight the main structures of the Gaia HRDs. We select both field and cluster (open and globular) stars, compare the observations with previous classifications and with stellar evolutionary tracks, and we present variations of the Gaia HRD with age, metallicity, and kinematics. Late stages of stellar evolution such as hot subdwarfs, post-AGB stars, planetary nebulae, and white dwarfs are also analysed, as well as low-mass brown dwarf objects. The Gaia HRDs are unprecedented in both precision and coverage of the various Milky Way stellar populations and stellar evolutionary phases. Many fine structures of the HRDs are presented. The clear split of the white dwarf sequence into hydrogen and helium white dwarfs is presented for the first time in an HRD. The relation between kinematics and the HRD is nicely illustrated. Two different populations in a classical kinematic selection of the halo are unambiguously identified in the HRD. Membership and mean parameters for a selected list of open clusters are provided. They allow drawing very detailed cluster sequences, highlighting fine structures, and providing extremely precise empirical isochrones that will lead to more insight in stellar physics. Gaia DR2 demonstrates the potential of combining precise astrometry and photometry for large samples for studies in stellar evolution and stellar population and opens an entire new area for HRD-based studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.09378v2-abstract-full').style.display = 'none'; document.getElementById('1804.09378v2-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 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in the A&A Gaia Data Release 2 special issue. Tables 2 and A.4 corrected. Tables available at http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/616/A10</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 616, A10 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1804.09375">arXiv:1804.09375</a> <span> [<a href="https://arxiv.org/pdf/1804.09375">pdf</a>, <a href="https://arxiv.org/format/1804.09375">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="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/10.1051/0004-6361/201833234">10.1051/0004-6361/201833234 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 2: Catalogue validation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Luri%2C+X">X. Luri</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Fabricius%2C+C">C. Fabricius</a>, <a href="/search/astro-ph?searchtype=author&query=Helmi%2C+A">A. Helmi</a>, <a href="/search/astro-ph?searchtype=author&query=Muraveva%2C+T">T. Muraveva</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=Spoto%2C+F">F. Spoto</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Antoja%2C+T">T. Antoja</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=Jordi%2C+C">C. Jordi</a>, <a href="/search/astro-ph?searchtype=author&query=Leclerc%2C+N">N. Leclerc</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=Romero-G%C3%B3mez%2C+M">M. Romero-G贸mez</a>, <a href="/search/astro-ph?searchtype=author&query=Shih%2C+I">I-C. Shih</a>, <a href="/search/astro-ph?searchtype=author&query=Soria%2C+S">S. Soria</a>, <a href="/search/astro-ph?searchtype=author&query=Barache%2C+C">C. Barache</a>, <a href="/search/astro-ph?searchtype=author&query=Bossini%2C+D">D. Bossini</a>, <a href="/search/astro-ph?searchtype=author&query=Bragaglia%2C+A">A. Bragaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Breddels%2C+M+A">M. A. Breddels</a>, <a href="/search/astro-ph?searchtype=author&query=Fabrizio%2C+M">M. Fabrizio</a>, <a href="/search/astro-ph?searchtype=author&query=Lambert%2C+S">S. Lambert</a>, <a href="/search/astro-ph?searchtype=author&query=Marrese%2C+P+M">P. M. Marrese</a>, <a href="/search/astro-ph?searchtype=author&query=Massari%2C+D">D. Massari</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="1804.09375v1-abstract-short" style="display: inline;"> The second Gaia data release (DR2), contains very precise astrometric and photometric properties for more than one billion sources, astrophysical parameters for dozens of millions, radial velocities for millions, variability information for half a million of stellar sources and orbits for thousands of solar system objects. Before the Catalogue publication, these data have undergone dedicated valid… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.09375v1-abstract-full').style.display = 'inline'; document.getElementById('1804.09375v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.09375v1-abstract-full" style="display: none;"> The second Gaia data release (DR2), contains very precise astrometric and photometric properties for more than one billion sources, astrophysical parameters for dozens of millions, radial velocities for millions, variability information for half a million of stellar sources and orbits for thousands of solar system objects. Before the Catalogue publication, these data have undergone dedicated validation processes. The goal of this paper is to describe the validation results in terms of completeness, accuracy and precision of the various Gaia DR2 data. The validation processes include a systematic analysis of the Catalogue content to detect anomalies, either individual errors or statistical properties, using statistical analysis, and comparisons to external data or to models. Although the astrometric, photometric and spectroscopic data are of unprecedented quality and quantity, it is shown that the data cannot be used without a dedicated attention to the limitations described here, in the Catalogue documentation and in accompanying papers. A particular emphasis is put on the caveats for the statistical use of the data in scientific exploitation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.09375v1-abstract-full').style.display = 'none'; document.getElementById('1804.09375v1-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, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2018. </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 616, A17 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1804.09373">arXiv:1804.09373</a> <span> [<a href="https://arxiv.org/pdf/1804.09373">pdf</a>, <a href="https://arxiv.org/format/1804.09373">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="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/10.1051/0004-6361/201832892">10.1051/0004-6361/201832892 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 2: Summary of the variability processing & analysis results </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Nienartowicz%2C+K">K. Nienartowicz</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=Marchal%2C+O">O. Marchal</a>, <a href="/search/astro-ph?searchtype=author&query=Mowlavi%2C+N">N. Mowlavi</a>, <a href="/search/astro-ph?searchtype=author&query=Clementini%2C+G">G. Clementini</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=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Guy%2C+L+P">L. P. Guy</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=Lebzelter%2C+T">T. Lebzelter</a>, <a href="/search/astro-ph?searchtype=author&query=Rimoldini%2C+L">L. Rimoldini</a>, <a href="/search/astro-ph?searchtype=author&query=Roelens%2C+M">M. Roelens</a>, <a href="/search/astro-ph?searchtype=author&query=Zucker%2C+S">S. Zucker</a>, <a href="/search/astro-ph?searchtype=author&query=Distefano%2C+E">E. Distefano</a>, <a href="/search/astro-ph?searchtype=author&query=Garofalo%2C+A">A. Garofalo</a>, <a href="/search/astro-ph?searchtype=author&query=Lecoeur-Ta%C3%AFbi%2C+I">I. Lecoeur-Ta茂bi</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+M">M. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Molinaro%2C+R">R. Molinaro</a>, <a href="/search/astro-ph?searchtype=author&query=Muraveva%2C+T">T. Muraveva</a>, <a href="/search/astro-ph?searchtype=author&query=Panahi%2C+A">A. Panahi</a>, <a href="/search/astro-ph?searchtype=author&query=Regibo%2C+S">S. Regibo</a>, <a href="/search/astro-ph?searchtype=author&query=Ripepi%2C+V">V. Ripepi</a>, <a href="/search/astro-ph?searchtype=author&query=Sarro%2C+L+M">L. M. Sarro</a> , et al. (38 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="1804.09373v8-abstract-short" style="display: inline;"> The Gaia Data Release 2 (DR2): we summarise the processing and results of the identification of variable source candidates of RR Lyrae stars, Cepheids, long period variables (LPVs), rotation modulation (BY Dra-type) stars, delta Scuti & SX Phoenicis stars, and short-timescale variables. In this release we aim to provide useful but not necessarily complete samples of candidates. The processed Gai… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.09373v8-abstract-full').style.display = 'inline'; document.getElementById('1804.09373v8-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.09373v8-abstract-full" style="display: none;"> The Gaia Data Release 2 (DR2): we summarise the processing and results of the identification of variable source candidates of RR Lyrae stars, Cepheids, long period variables (LPVs), rotation modulation (BY Dra-type) stars, delta Scuti & SX Phoenicis stars, and short-timescale variables. In this release we aim to provide useful but not necessarily complete samples of candidates. The processed Gaia data consist of the G, BP, and RP photometry during the first 22 months of operations as well as positions and parallaxes. Various methods from classical statistics, data mining and time series analysis were applied and tailored to the specific properties of Gaia data, as well as various visualisation tools. The DR2 variability release contains: 228'904 RR Lyrae stars, 11'438 Cepheids, 151'761 LPVs, 147'535 stars with rotation modulation, 8'882 delta Scuti & SX Phoenicis stars, and 3'018 short-timescale variables. These results are distributed over a classification and various Specific Object Studies (SOS) tables in the Gaia archive, along with the three-band time series and associated statistics for the underlying 550'737 unique sources. We estimate that about half of them are newly identified variables. The variability type completeness varies strongly as function of sky position due to the non-uniform sky coverage and intermediate calibration level of this data. The probabilistic and automated nature of this work implies certain completeness and contamination rates which are quantified so that users can anticipate their effects. This means that even well-known variable sources can be missed or misidentified in the published data. The DR2 variability release only represents a small subset of the processed data. Future releases will include more variable sources and data products; however, DR2 shows the (already) very high quality of the data and great promise for variability studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.09373v8-abstract-full').style.display = 'none'; document.getElementById('1804.09373v8-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 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2018. </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">21 pages, 10 figures, 5 tables, accepted by Astronomy & Astrophysics, added several language corrections, and expanded Gaia archive query examples</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 618, A30 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1801.10042">arXiv:1801.10042</a> <span> [<a href="https://arxiv.org/pdf/1801.10042">pdf</a>, <a href="https://arxiv.org/format/1801.10042">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/10.1051/0004-6361/201731251">10.1051/0004-6361/201731251 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterising Open Clusters in the solar neighbourhood with the Tycho-Gaia Astrometric Solution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cantat-Gaudin%2C+T">T. Cantat-Gaudin</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Sordo%2C+R">R. Sordo</a>, <a href="/search/astro-ph?searchtype=author&query=Pensabene%2C+F">F. Pensabene</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=Moitinho%2C+A">A. Moitinho</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a>, <a href="/search/astro-ph?searchtype=author&query=Casamiquela%2C+L">L. Casamiquela</a>, <a href="/search/astro-ph?searchtype=author&query=Balaguer-N%C3%BAnez%2C+L">L. Balaguer-N煤nez</a>, <a href="/search/astro-ph?searchtype=author&query=Soubiran%2C+C">C. Soubiran</a>, <a href="/search/astro-ph?searchtype=author&query=Brouillet%2C+N">N. Brouillet</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="1801.10042v2-abstract-short" style="display: inline;"> The Tycho-Gaia Astrometric Solution (TGAS) subset of the first Gaia catalogue contains an unprecedented sample of proper motions and parallaxes for two million stars brighter than G~12 mag. We take advantage of the full astrometric solution available for those stars to identify the members of known open clusters and compute mean cluster parameters using either TGAS or UCAC4 proper motions, and TGA… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.10042v2-abstract-full').style.display = 'inline'; document.getElementById('1801.10042v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.10042v2-abstract-full" style="display: none;"> The Tycho-Gaia Astrometric Solution (TGAS) subset of the first Gaia catalogue contains an unprecedented sample of proper motions and parallaxes for two million stars brighter than G~12 mag. We take advantage of the full astrometric solution available for those stars to identify the members of known open clusters and compute mean cluster parameters using either TGAS or UCAC4 proper motions, and TGAS parallaxes. We apply an unsupervised membership assignment procedure to select high probability cluster members, we use a Bayesian/MCMC technique to fit stellar isochrones to the observed 2MASS JHK$_s$ magnitudes of the member stars and derive cluster parameters (age, metallicity, extinction, distance modulus), and we combine TGAS data with spectroscopic radial velocities to compute full Galactic orbits. We obtain mean astrometric parameters (proper motions and parallaxes) for 128 clusters closer than about 2 kpc, and cluster parameters from isochrone fitting for 26 of them located inside 1 kpc from the Sun. We show the orbital parameters obtained from integrating 36 orbits in a Galactic potential. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.10042v2-abstract-full').style.display = 'none'; document.getElementById('1801.10042v2-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, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 615, A49 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1708.00195">arXiv:1708.00195</a> <span> [<a href="https://arxiv.org/pdf/1708.00195">pdf</a>, <a href="https://arxiv.org/format/1708.00195">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </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/10.1051/0004-6361/201731059">10.1051/0004-6361/201731059 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 1: The archive visualisation service </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Moitinho%2C+A">A. Moitinho</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=Savietto%2C+H">H. Savietto</a>, <a href="/search/astro-ph?searchtype=author&query=Barros%2C+M">M. Barros</a>, <a href="/search/astro-ph?searchtype=author&query=Barata%2C+C">C. Barata</a>, <a href="/search/astro-ph?searchtype=author&query=Falc%C3%A3o%2C+A+J">A. J. Falc茫o</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandes%2C+T">T. Fernandes</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+J">J. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+A+F">A. F. Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Gomes%2C+M">M. Gomes</a>, <a href="/search/astro-ph?searchtype=author&query=Bakker%2C+J">J. Bakker</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=Gonz%C3%A1lez-N%C3%BA%C3%B1ez%2C+J">J. Gonz谩lez-N煤帽ez</a>, <a href="/search/astro-ph?searchtype=author&query=Gracia-Abril%2C+G">G. Gracia-Abril</a>, <a href="/search/astro-ph?searchtype=author&query=Guti%C3%A9rrez-S%C3%A1nchez%2C+R">R. Guti茅rrez-S谩nchez</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=Jordan%2C+S">S. Jordan</a>, <a href="/search/astro-ph?searchtype=author&query=Luri%2C+X">X. Luri</a>, <a href="/search/astro-ph?searchtype=author&query=Merin%2C+B">B. Merin</a>, <a href="/search/astro-ph?searchtype=author&query=Mignard%2C+F">F. Mignard</a>, <a href="/search/astro-ph?searchtype=author&query=Mora%2C+A">A. Mora</a>, <a href="/search/astro-ph?searchtype=author&query=Navarro%2C+V">V. Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Mullane%2C+W">W. O'Mullane</a>, <a href="/search/astro-ph?searchtype=author&query=Sell%C3%A9s%2C+T+S">T. Sagrist脿 Sell茅s</a>, <a href="/search/astro-ph?searchtype=author&query=Salgado%2C+J">J. Salgado</a> , et al. (9 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="1708.00195v1-abstract-short" style="display: inline;"> Context: The first Gaia data release (DR1) delivered a catalogue of astrometry and photometry for over a billion astronomical sources. Within the panoply of methods used for data exploration, visualisation is often the starting point and even the guiding reference for scientific thought. However, this is a volume of data that cannot be efficiently explored using traditional tools, techniques, and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.00195v1-abstract-full').style.display = 'inline'; document.getElementById('1708.00195v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1708.00195v1-abstract-full" style="display: none;"> Context: The first Gaia data release (DR1) delivered a catalogue of astrometry and photometry for over a billion astronomical sources. Within the panoply of methods used for data exploration, visualisation is often the starting point and even the guiding reference for scientific thought. However, this is a volume of data that cannot be efficiently explored using traditional tools, techniques, and habits. Aims: We aim to provide a global visual exploration service for the Gaia archive, something that is not possible out of the box for most people. The service has two main goals. The first is to provide a software platform for interactive visual exploration of the archive contents, using common personal computers and mobile devices available to most users. The second aim is to produce intelligible and appealing visual representations of the enormous information content of the archive. Methods: The interactive exploration service follows a client-server design. The server runs close to the data, at the archive, and is responsible for hiding as far as possible the complexity and volume of the Gaia data from the client. This is achieved by serving visual detail on demand. Levels of detail are pre-computed using data aggregation and subsampling techniques. For DR1, the client is a web application that provides an interactive multi-panel visualisation workspace as well as a graphical user interface. Results: The Gaia archive Visualisation Service offers a web-based multi-panel interactive visualisation desktop in a browser tab. It currently provides highly configurable 1D histograms and 2D scatter plots of Gaia DR1 and the Tycho-Gaia Astrometric Solution (TGAS) with linked views. An innovative feature is the creation of ADQL queries from visually defined regions in plots. [abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.00195v1-abstract-full').style.display = 'none'; document.getElementById('1708.00195v1-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 August, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 9 figures, accepted for publication in Astronomy & Astrophysics. Abstract abridged for arXiv submission. The service and image gallery here described are accessible from the Gaia archive "visualization" tab at http://gea.esac.esa.int/archive/</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 605, A52 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1705.00688">arXiv:1705.00688</a> <span> [<a href="https://arxiv.org/pdf/1705.00688">pdf</a>, <a href="https://arxiv.org/format/1705.00688">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/10.1051/0004-6361/201629925">10.1051/0004-6361/201629925 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 1. Testing the parallaxes with local Cepheids and RR Lyrae 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=Clementini%2C+G">G. Clementini</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Ripepi%2C+V">V. Ripepi</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+M">M. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Muraveva%2C+T">T. Muraveva</a>, <a href="/search/astro-ph?searchtype=author&query=Garofalo%2C+A">A. Garofalo</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=Palmer%2C+M">M. Palmer</a>, <a href="/search/astro-ph?searchtype=author&query=Luri%2C+X">X. Luri</a>, <a href="/search/astro-ph?searchtype=author&query=Molinaro%2C+R">R. Molinaro</a>, <a href="/search/astro-ph?searchtype=author&query=Rimoldini%2C+L">L. Rimoldini</a>, <a href="/search/astro-ph?searchtype=author&query=Szabados%2C+L">L. Szabados</a>, <a href="/search/astro-ph?searchtype=author&query=Musella%2C+I">I. Musella</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+R+I">R. I. Anderson</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=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=Babusiaux%2C+C">C. Babusiaux</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=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=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+F">F. Jansen</a> , et al. (566 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="1705.00688v1-abstract-short" style="display: inline;"> Parallaxes for 331 classical Cepheids, 31 Type II Cepheids and 364 RR Lyrae stars in common between Gaia and the Hipparcos and Tycho-2 catalogues are published in Gaia Data Release 1 (DR1) as part of the Tycho-Gaia Astrometric Solution (TGAS). In order to test these first parallax measurements of the primary standard candles of the cosmological distance ladder, that involve astrometry collected by… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.00688v1-abstract-full').style.display = 'inline'; document.getElementById('1705.00688v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1705.00688v1-abstract-full" style="display: none;"> Parallaxes for 331 classical Cepheids, 31 Type II Cepheids and 364 RR Lyrae stars in common between Gaia and the Hipparcos and Tycho-2 catalogues are published in Gaia Data Release 1 (DR1) as part of the Tycho-Gaia Astrometric Solution (TGAS). In order to test these first parallax measurements of the primary standard candles of the cosmological distance ladder, that involve astrometry collected by Gaia during the initial 14 months of science operation, we compared them with literature estimates and derived new period-luminosity ($PL$), period-Wesenheit ($PW$) relations for classical and Type II Cepheids and infrared $PL$, $PL$-metallicity ($PLZ$) and optical luminosity-metallicity ($M_V$-[Fe/H]) relations for the RR Lyrae stars, with zero points based on TGAS. The new relations were computed using multi-band ($V,I,J,K_{\mathrm{s}},W_{1}$) photometry and spectroscopic metal abundances available in the literature, and applying three alternative approaches: (i) by linear least squares fitting the absolute magnitudes inferred from direct transformation of the TGAS parallaxes, (ii) by adopting astrometric-based luminosities, and (iii) using a Bayesian fitting approach. TGAS parallaxes bring a significant added value to the previous Hipparcos estimates. The relations presented in this paper represent first Gaia-calibrated relations and form a "work-in-progress" milestone report in the wait for Gaia-only parallaxes of which a first solution will become available with Gaia's Data Release 2 (DR2) in 2018. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.00688v1-abstract-full').style.display = 'none'; document.getElementById('1705.00688v1-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 May, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2017. </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, 25 figures. Accepted for publication by 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 605, A79 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.01131">arXiv:1703.01131</a> <span> [<a href="https://arxiv.org/pdf/1703.01131">pdf</a>, <a href="https://arxiv.org/format/1703.01131">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/10.1051/0004-6361/201730552">10.1051/0004-6361/201730552 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 1. Open cluster astrometry: performance, limitations, and future prospects </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=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=Jordi%2C+C">C. Jordi</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=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=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</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=Biermann%2C+M">M. Biermann</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=Jansen%2C+F">F. Jansen</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">U. Lammers</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=Siddiqui%2C+H+I">H. I. Siddiqui</a>, <a href="/search/astro-ph?searchtype=author&query=Soubiran%2C+C">C. Soubiran</a> , et al. (567 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="1703.01131v1-abstract-short" style="display: inline;"> Context. The first Gaia Data Release contains the Tycho-Gaia Astrometric Solution (TGAS). This is a subset of about 2 million stars for which, besides the position and photometry, the proper motion and parallax are calculated using Hipparcos and Tycho-2 positions in 1991.25 as prior information. Aims. We investigate the scientific potential and limitations of the TGAS component by means of the ast… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.01131v1-abstract-full').style.display = 'inline'; document.getElementById('1703.01131v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.01131v1-abstract-full" style="display: none;"> Context. The first Gaia Data Release contains the Tycho-Gaia Astrometric Solution (TGAS). This is a subset of about 2 million stars for which, besides the position and photometry, the proper motion and parallax are calculated using Hipparcos and Tycho-2 positions in 1991.25 as prior information. Aims. We investigate the scientific potential and limitations of the TGAS component by means of the astrometric data for open clusters. Methods. Mean cluster parallax and proper motion values are derived taking into account the error correlations within the astrometric solutions for individual stars, an estimate of the internal velocity dispersion in the cluster, and, where relevant, the effects of the depth of the cluster along the line of sight. Internal consistency of the TGAS data is assessed. Results. Values given for standard uncertainties are still inaccurate and may lead to unrealistic unit-weight standard deviations of least squares solutions for cluster parameters. Reconstructed mean cluster parallax and proper motion values are generally in very good agreement with earlier Hipparcos-based determination, although the Gaia mean parallax for the Pleiades is a significant exception. We have no current explanation for that discrepancy. Most clusters are observed to extend to nearly 15 pc from the cluster centre, and it will be up to future Gaia releases to establish whether those potential cluster-member stars are still dynamically bound to the clusters. Conclusions. The Gaia DR1 provides the means to examine open clusters far beyond their more easily visible cores, and can provide membership assessments based on proper motions and parallaxes. A combined HR diagram shows the same features as observed before using the Hipparcos data, with clearly increased luminosities for older A and F dwarfs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.01131v1-abstract-full').style.display = 'none'; document.getElementById('1703.01131v1-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 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2017. </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 main text plus 46 pages appendices. 34 figures main text, 38 figures appendices. 8 table in main text, 19 tables in appendices</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 601, A19 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1702.03295">arXiv:1702.03295</a> <span> [<a href="https://arxiv.org/pdf/1702.03295">pdf</a>, <a href="https://arxiv.org/format/1702.03295">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 1: The variability processing & analysis and its application to the south ecliptic pole region </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Mowlavi%2C+N">N. Mowlavi</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=Nienartowicz%2C+K">K. Nienartowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Ordonez%2C+D">D. Ordonez</a>, <a href="/search/astro-ph?searchtype=author&query=Holl%2C+B">B. Holl</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=Riello%2C+M">M. Riello</a>, <a href="/search/astro-ph?searchtype=author&query=Clementini%2C+G">G. Clementini</a>, <a href="/search/astro-ph?searchtype=author&query=Cuypers%2C+J">J. Cuypers</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=Lanzafame%2C+A+C">A. C. Lanzafame</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=Charnas%2C+J">J. Charnas</a>, <a href="/search/astro-ph?searchtype=author&query=Guy%2C+L+P">L. P. Guy</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=Rimoldini%2C+L">L. Rimoldini</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%BCveges%2C+M">M. S眉veges</a>, <a href="/search/astro-ph?searchtype=author&query=Mignard%2C+F">F. Mignard</a>, <a href="/search/astro-ph?searchtype=author&query=Busso%2C+G">G. Busso</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=van+Leeuwen%2C+F">F. van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Dubath%2C+P">P. Dubath</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+M">M. Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Aguado%2C+J+J">J. J. Aguado</a> , et al. (48 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="1702.03295v1-abstract-short" style="display: inline;"> The ESA Gaia mission provides a unique time-domain survey for more than one billion sources brighter than G=20.7 mag. Gaia offers the unprecedented opportunity to study variability phenomena in the Universe thanks to multi-epoch G-magnitude photometry in addition to astrometry, blue and red spectro-photometry, and spectroscopy. Within the Gaia Consortium, Coordination Unit 7 has the responsibility… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1702.03295v1-abstract-full').style.display = 'inline'; document.getElementById('1702.03295v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1702.03295v1-abstract-full" style="display: none;"> The ESA Gaia mission provides a unique time-domain survey for more than one billion sources brighter than G=20.7 mag. Gaia offers the unprecedented opportunity to study variability phenomena in the Universe thanks to multi-epoch G-magnitude photometry in addition to astrometry, blue and red spectro-photometry, and spectroscopy. Within the Gaia Consortium, Coordination Unit 7 has the responsibility to detect variable objects, classify them, derive characteristic parameters for specific variability classes, and provide global descriptions of variable phenomena. We describe the variability processing and analysis that we plan to apply to the successive data releases, and we present its application to the G-band photometry results of the first 14 months of Gaia operations that comprises 28 days of Ecliptic Pole Scanning Law and 13 months of Nominal Scanning Law. Out of the 694 million, all-sky, sources that have calibrated G-band photometry in this first stage of the mission, about 2.3 million sources that have at least 20 observations are located within 38 degrees from the South Ecliptic Pole. We detect about 14% of them as variable candidates, among which the automated classification identified 9347 Cepheid and RR Lyrae candidates. Additional visual inspections and selection criteria led to the publication of 3194 Cepheid and RR Lyrae stars, described in Clementini et al. (2016). Under the restrictive conditions for DR1, the completenesses of Cepheids and RR Lyrae stars are estimated at 67% and 58%, respectively, numbers that will significantly increase with subsequent Gaia data releases. Data processing within the Gaia Consortium is iterative, the quality of the data and the results being improved at each iteration. The results presented in this article show a glimpse of the exceptional harvest that is to be expected from the Gaia mission for variability phenomena. [abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1702.03295v1-abstract-full').style.display = 'none'; document.getElementById('1702.03295v1-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, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2017. </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">40 pages, 46 figures. 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