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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=Creevey%2C+O+L&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Creevey%2C+O+L&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Creevey%2C+O+L&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/2410.08106">arXiv:2410.08106</a> <span> [<a href="https://arxiv.org/pdf/2410.08106">pdf</a>, <a href="https://arxiv.org/format/2410.08106">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/10.3847/2515-5172/ad8566">10.3847/2515-5172/ad8566 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Extending the Asteroseismic Calibration of the Stellar Rossby Number </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Metcalfe%2C+T+S">Travis S. Metcalfe</a>, <a href="/search/astro-ph?searchtype=author&query=Corsaro%2C+E">Enrico Corsaro</a>, <a href="/search/astro-ph?searchtype=author&query=Bonanno%2C+A">Alfio Bonanno</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">Orlagh L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=van+Saders%2C+J+L">Jennifer L. van Saders</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="2410.08106v1-abstract-short" style="display: inline;"> The stellar Rossby number (Ro) is a dimensionless quantity that is used in the description of fluid flows. It characterizes the relative importance of Coriolis forces on convective motions, which is central to understanding magnetic stellar evolution. Here we present an expanded sample of Kepler asteroseismic targets to help calibrate the relation between Ro and Gaia color, and we extend the relat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.08106v1-abstract-full').style.display = 'inline'; document.getElementById('2410.08106v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.08106v1-abstract-full" style="display: none;"> The stellar Rossby number (Ro) is a dimensionless quantity that is used in the description of fluid flows. It characterizes the relative importance of Coriolis forces on convective motions, which is central to understanding magnetic stellar evolution. Here we present an expanded sample of Kepler asteroseismic targets to help calibrate the relation between Ro and Gaia color, and we extend the relation to redder colors using observations of the mean activity levels and rotation periods for a sample of brighter stars from the Mount Wilson survey. Our quadratic fit to the combined sample is nearly linear between 0.55 < G_BP-G_RP < 1.2, and can be used to estimate Ro for stars with spectral types between F5 and K3. The strong deviation from linearity in the original calibration may reflect an observational bias against the detection of solar-like oscillations at higher activity levels for the coolest stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.08106v1-abstract-full').style.display = 'none'; document.getElementById('2410.08106v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">3 pages, 1 figure, AAS Journals accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Res. Notes AAS 8, 260 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.05447">arXiv:2406.05447</a> <span> [<a href="https://arxiv.org/pdf/2406.05447">pdf</a>, <a href="https://arxiv.org/format/2406.05447">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The PLATO Mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rauer%2C+H">Heike Rauer</a>, <a href="/search/astro-ph?searchtype=author&query=Aerts%2C+C">Conny Aerts</a>, <a href="/search/astro-ph?searchtype=author&query=Cabrera%2C+J">Juan Cabrera</a>, <a href="/search/astro-ph?searchtype=author&query=Deleuil%2C+M">Magali Deleuil</a>, <a href="/search/astro-ph?searchtype=author&query=Erikson%2C+A">Anders Erikson</a>, <a href="/search/astro-ph?searchtype=author&query=Gizon%2C+L">Laurent Gizon</a>, <a href="/search/astro-ph?searchtype=author&query=Goupil%2C+M">Mariejo Goupil</a>, <a href="/search/astro-ph?searchtype=author&query=Heras%2C+A">Ana Heras</a>, <a href="/search/astro-ph?searchtype=author&query=Lorenzo-Alvarez%2C+J">Jose Lorenzo-Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Marliani%2C+F">Filippo Marliani</a>, <a href="/search/astro-ph?searchtype=author&query=Martin-Garcia%2C+C">C茅sar Martin-Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Mas-Hesse%2C+J+M">J. Miguel Mas-Hesse</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Rourke%2C+L">Laurence O'Rourke</a>, <a href="/search/astro-ph?searchtype=author&query=Osborn%2C+H">Hugh Osborn</a>, <a href="/search/astro-ph?searchtype=author&query=Pagano%2C+I">Isabella Pagano</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">Giampaolo Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">Don Pollacco</a>, <a href="/search/astro-ph?searchtype=author&query=Ragazzoni%2C+R">Roberto Ragazzoni</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+G">Gavin Ramsay</a>, <a href="/search/astro-ph?searchtype=author&query=Udry%2C+S">St茅phane Udry</a>, <a href="/search/astro-ph?searchtype=author&query=Appourchaux%2C+T">Thierry Appourchaux</a>, <a href="/search/astro-ph?searchtype=author&query=Benz%2C+W">Willy Benz</a>, <a href="/search/astro-ph?searchtype=author&query=Brandeker%2C+A">Alexis Brandeker</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCdel%2C+M">Manuel G眉del</a>, <a href="/search/astro-ph?searchtype=author&query=Janot-Pacheco%2C+E">Eduardo Janot-Pacheco</a> , et al. (820 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="2406.05447v2-abstract-short" style="display: inline;"> PLATO (PLAnetary Transits and Oscillations of stars) is ESA's M3 mission designed to detect and characterise extrasolar planets and perform asteroseismic monitoring of a large number of stars. PLATO will detect small planets (down to <2 R_(Earth)) around bright stars (<11 mag), including terrestrial planets in the habitable zone of solar-like stars. With the complement of radial velocity observati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05447v2-abstract-full').style.display = 'inline'; document.getElementById('2406.05447v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.05447v2-abstract-full" style="display: none;"> PLATO (PLAnetary Transits and Oscillations of stars) is ESA's M3 mission designed to detect and characterise extrasolar planets and perform asteroseismic monitoring of a large number of stars. PLATO will detect small planets (down to <2 R_(Earth)) around bright stars (<11 mag), including terrestrial planets in the habitable zone of solar-like stars. With the complement of radial velocity observations from the ground, planets will be characterised for their radius, mass, and age with high accuracy (5 %, 10 %, 10 % for an Earth-Sun combination respectively). PLATO will provide us with a large-scale catalogue of well-characterised small planets up to intermediate orbital periods, relevant for a meaningful comparison to planet formation theories and to better understand planet evolution. It will make possible comparative exoplanetology to place our Solar System planets in a broader context. In parallel, PLATO will study (host) stars using asteroseismology, allowing us to determine the stellar properties with high accuracy, substantially enhancing our knowledge of stellar structure and evolution. The payload instrument consists of 26 cameras with 12cm aperture each. For at least four years, the mission will perform high-precision photometric measurements. Here we review the science objectives, present PLATO's target samples and fields, provide an overview of expected core science performance as well as a description of the instrument and the mission profile at the beginning of the serial production of the flight cameras. PLATO is scheduled for a launch date end 2026. This overview therefore provides a summary of the mission to the community in preparation of the upcoming operational phases. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05447v2-abstract-full').style.display = 'none'; document.getElementById('2406.05447v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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/2404.04010">arXiv:2404.04010</a> <span> [<a href="https://arxiv.org/pdf/2404.04010">pdf</a>, <a href="https://arxiv.org/ps/2404.04010">ps</a>, <a href="https://arxiv.org/format/2404.04010">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/10.1051/0004-6361/202449534">10.1051/0004-6361/202449534 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Benchmarking the effective temperature scale of red giant branch stellar models: the case of the metal-poor halo giant HD 122563 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</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=Salaris%2C+M">M. Salaris</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrinferni%2C+A">A. Pietrinferni</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="2404.04010v1-abstract-short" style="display: inline;"> There is plenty of evidence in the literature of significant discrepancies between the observations and models of metal-poor red giant branch stars, in particular regarding the effective temperature, teff, scale. We revisit the benchmark star HD 122563 using the most recent observations from Gaia Data Release 3, to investigate if these new constraints may help in resolving this discrepancy. We rev… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.04010v1-abstract-full').style.display = 'inline'; document.getElementById('2404.04010v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.04010v1-abstract-full" style="display: none;"> There is plenty of evidence in the literature of significant discrepancies between the observations and models of metal-poor red giant branch stars, in particular regarding the effective temperature, teff, scale. We revisit the benchmark star HD 122563 using the most recent observations from Gaia Data Release 3, to investigate if these new constraints may help in resolving this discrepancy. We review the most recent spectroscopic determinations of the metallicity of HD 122563 [Fe/H], and provide a new assessment of its fundamental parameters, i.e. bolometric luminosity, teff, surface gravity, plus a photometric determination of its metal content. Using these constraints, we compare the position of the star in the Hertzsprung-Russell (H-R) diagram with various recent sets of stellar evolution tracks. The H-R diagram analysis reveals a significant disagreement between observed and theoretical teff values, when adopting the most recent spectroscopic estimate of [Fe/H]. On the other hand, by using the photometric determination of [Fe/H] some of the selected sets of stellar tracks appear in fair agreement with observations. The sets with discrepant teff can be made to agree with observations either by modifying the prescription adopted to calculate the models' outer boundary conditions, and/or by reducing the adopted value of the mixing length parameter with respect to the solar-calibration. A definitive assessment of whether the teff scale of metal-poor stellar red giant branch models is consistent with observations requires an even more accurate determination of the fundamental parameters of HD 122563 and also a larger sample of calibrators. From the theoretical side, it is crucial to minimise the current uncertainties in the treatment (boundary conditions, temperature gradient) of the outer layers of stellar models with convective envelopes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.04010v1-abstract-full').style.display = 'none'; document.getElementById('2404.04010v1-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 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">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 689, A243 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.06551">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/2307.12318">arXiv:2307.12318</a> <span> [<a href="https://arxiv.org/pdf/2307.12318">pdf</a>, <a href="https://arxiv.org/format/2307.12318">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/10.1051/0004-6361/202141610">10.1051/0004-6361/202141610 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Frequencies analysis of the hybrid delta Sct-gamma Dor star CoRoT-102314644 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Arias%2C+J+S">Julieta S谩nchez Arias</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">Orlagh Louise Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Chapellier%2C+E">Eric Chapellier</a>, <a href="/search/astro-ph?searchtype=author&query=Pichon%2C+B">Bernard Pichon</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="2307.12318v1-abstract-short" style="display: inline;"> Observations from space missions have allowed significant progress in many scientific domains due to the absence of atmospheric noise contributions and having uninterrupted data sets. In the context of asteroseismology, this has been extremely beneficial because many oscillation frequencies with small amplitudes, not observable from the ground, can be detected. One example of this success is the l… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.12318v1-abstract-full').style.display = 'inline'; document.getElementById('2307.12318v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.12318v1-abstract-full" style="display: none;"> Observations from space missions have allowed significant progress in many scientific domains due to the absence of atmospheric noise contributions and having uninterrupted data sets. In the context of asteroseismology, this has been extremely beneficial because many oscillation frequencies with small amplitudes, not observable from the ground, can be detected. One example of this success is the large number of hybrid delta Sct-gamma Dor stars discovered. These stars have radial and non-radial p- and g-modes simultaneously excited to an observable level allowing us to probe both the external and near-to-core layers of the star. We analyse the light curve of hybrid delta Sct-gamma Dor star CoRoT ID 102314644 and characterise its frequency spectrum. We detected 29 gamma Dor type frequencies in the range [0.32-3.66] cycles per day (c/d) and a series of 6 equidistant periods with a mean period spacing of DeltaPi=1612 s. In the delta Sct domain we found 38 frequencies in the range 8.63-24.73 c/d and a quintuplet centred on the frequency p_1=11.39 c/d and derived a possible rotational period of 3.06 d. The frequency analysis of this object suggests the presence of spots at the stellar surface, nevertheless we could not dismiss the possibility of a binary system. The initial modelling of the frequency data along with external constraints has allowed us to refine its astrophysical parameters giving a mass of approximately 1.75 solar masses, a radius of 2.48 solar radii and an age of 1241 Myr. The observed period spacing, a p-mode quintuplet, the possible rotation period and the analysis of the individual frequencies provide important input constraints for the understanding of different transport phenomena in A-F-type stars.[abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.12318v1-abstract-full').style.display = 'none'; document.getElementById('2307.12318v1-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">version 1 June 2023, accepted 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 676, A96 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.12205">arXiv:2303.12205</a> <span> [<a href="https://arxiv.org/pdf/2303.12205">pdf</a>, <a href="https://arxiv.org/format/2303.12205">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/10.1051/0004-6361/202243624">10.1051/0004-6361/202243624 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Asteroseismic age constraints on the open cluster NGC 2477 using oscillating stars identified with TESS FFI </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Palakkatharappil%2C+D+B">D. B. Palakkatharappil</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</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="2303.12205v1-abstract-short" style="display: inline;"> The ages of pulsating stars in clusters can be determined by isochrone fitting and it can be further improved by asteroseismic modelling. We analyse the intermediate-age open cluster NGC2477, known to suffer from differential extinction, to explore if asteroseismology and clusters characteristics can help understand the metallicity, extinction and result in better age determinations than isochrone… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.12205v1-abstract-full').style.display = 'inline'; document.getElementById('2303.12205v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.12205v1-abstract-full" style="display: none;"> The ages of pulsating stars in clusters can be determined by isochrone fitting and it can be further improved by asteroseismic modelling. We analyse the intermediate-age open cluster NGC2477, known to suffer from differential extinction, to explore if asteroseismology and clusters characteristics can help understand the metallicity, extinction and result in better age determinations than isochrone-fitting alone. We combine a multitude of recent observations from Gaia, high-resolution spectroscopy, and extinction maps to analyse the cluster and then search for and detect variability in the member stars using TESS FFI data. To interpret all of these data, we used stellar structure, evolution and oscillation codes. We performed an isochrone fitting to the cluster using publically-available isochrones, which provides a cluster age of between 0.6 to 1.1 Ga. Then using TESS Full-frame images, we analysed the time dimension of the members of this cluster. We created optimised pixel light curves using the ${\tt tessipack}$ package which allows us to consider possible contamination by nearby stars. Using these light curves, we identified many interesting levels of variability of stars in this cluster, including binaries and oscillating stars. For the asteroseismic analysis, we selected a few uncontaminated A--F type oscillating stars and used the MESA and GYRE codes to interpret the frequency signals. By comparing the theoretical and the observed spectra, we identified frequency separations, $螖谓$, for four stars. Then using the identified $螖谓$ and imposing that the best matched theoretical models have the same age, metallicity and background extinction, we constrained the cluster's age to 1.0 $\pm$ 0.1 Ga. We conclude that using the TESS FFI data, we can identify oscillating stars in clusters, which allows us to better refine their ages. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.12205v1-abstract-full').style.display = 'none'; document.getElementById('2303.12205v1-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, 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">26 pages, 30 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 674, A146 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.03641">arXiv:2211.03641</a> <span> [<a href="https://arxiv.org/pdf/2211.03641">pdf</a>, <a href="https://arxiv.org/format/2211.03641">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202244507">10.1051/0004-6361/202244507 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ultracool dwarfs in Gaia DR3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sarro%2C+L+M">L. M. Sarro</a>, <a href="/search/astro-ph?searchtype=author&query=Berihuete%2C+A">A. Berihuete</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=Reyl%C3%A9%2C+C">C. Reyl茅</a>, <a href="/search/astro-ph?searchtype=author&query=Barrado%2C+D">D. Barrado</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Torres%2C+M">M. Garc铆a-Torres</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=Jones%2C+H+R+A">H. R. A. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Marocco%2C+F">F. Marocco</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=Sordo%2C+R">R. Sordo</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=Montegriffo%2C+P">P. Montegriffo</a>, <a href="/search/astro-ph?searchtype=author&query=Carballo%2C+R">R. Carballo</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=Lanzafame%2C+A+C">A. C. Lanzafame</a>, <a href="/search/astro-ph?searchtype=author&query=Pailler%2C+F">F. Pailler</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=Lobel%2C+A">A. Lobel</a>, <a href="/search/astro-ph?searchtype=author&query=Delchambre%2C+L">L. Delchambre</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=Recio-Blanco%2C+A">A. Recio-Blanco</a>, <a href="/search/astro-ph?searchtype=author&query=Schultheis%2C+M+S">M. S. Schultheis</a>, <a href="/search/astro-ph?searchtype=author&query=De+Angeli%2C+F">F. De Angeli</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="2211.03641v3-abstract-short" style="display: inline;"> Aims. In this work we use the Gaia DR3 set of ultracool dwarf candidates and complement the Gaia spectrophotometry with additional photometry in order to characterise its global properties. This includes the inference of the distances, their locus in the Gaia colour-absolute magnitude diagram and the (biased through selection) luminosity function in the faint end of the Main Sequence. We study the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.03641v3-abstract-full').style.display = 'inline'; document.getElementById('2211.03641v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.03641v3-abstract-full" style="display: none;"> Aims. In this work we use the Gaia DR3 set of ultracool dwarf candidates and complement the Gaia spectrophotometry with additional photometry in order to characterise its global properties. This includes the inference of the distances, their locus in the Gaia colour-absolute magnitude diagram and the (biased through selection) luminosity function in the faint end of the Main Sequence. We study the overall changes in the Gaia RP spectra as a function of spectral type. We study the UCDs in binary systems, attempt to identify low-mass members of nearby young associations, star forming regions and clusters, and analyse their variability properties. Results. We detect 57 young, kinematically homogeneous groups some of which are identified as well known star forming regions, associations and clusters of different ages. We find that the primary members of 880 binary systems with a UCD belong mainly to the thin and thick disk components of the Milky Way. We identify 1109 variable UCDs using the variability tables in the Gaia archive, 728 of which belong to the star forming regions defined by HMAC. We define two groups of variable UCDs with extreme bright or faint outliers. Conclusions. The set of sources identified as UCDs in the Gaia archive contains a wealth of information that will require focused follow-up studies and observations. It will help to advance our understanding of the nature of the faint end of the Main Sequence and the stellar/substellar transition. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.03641v3-abstract-full').style.display = 'none'; document.getElementById('2211.03641v3-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 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by Astronomy and Astrophysics. 29 pages, 20 figures plus 3 appendices</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 669, A139 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.00211">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/2206.12237">arXiv:2206.12237</a> <span> [<a href="https://arxiv.org/pdf/2206.12237">pdf</a>, <a href="https://arxiv.org/format/2206.12237">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/10.1051/0004-6361/202244343">10.1051/0004-6361/202244343 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Solid confirmation of the broad DIB around 864.8 nm using stacked Gaia-RVS spectra </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+H">H. Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Schultheis%2C+M">M. Schultheis</a>, <a href="/search/astro-ph?searchtype=author&query=Zwitter%2C+T">T. Zwitter</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=Panuzzo%2C+P">P. Panuzzo</a>, <a href="/search/astro-ph?searchtype=author&query=Sartoretti%2C+P">P. Sartoretti</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=Recio-Blanco%2C+A">A. Recio-Blanco</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=Kordopatis%2C+G">G. Kordopatis</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=Dharmawardena%2C+T+E">T. E. Dharmawardena</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=Sordo%2C+R">R. Sordo</a>, <a href="/search/astro-ph?searchtype=author&query=Drimmel%2C+R">R. Drimmel</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=Palicio%2C+P+A">P. A. Palicio</a>, <a href="/search/astro-ph?searchtype=author&query=Contursi%2C+G">G. Contursi</a>, <a href="/search/astro-ph?searchtype=author&query=%C3%81lvarez%2C+M+A">M. A. 脕lvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Baker%2C+S">S. Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Benson%2C+K">K. Benson</a>, <a href="/search/astro-ph?searchtype=author&query=Cropper%2C+M">M. Cropper</a>, <a href="/search/astro-ph?searchtype=author&query=Dolding%2C+C">C. Dolding</a>, <a href="/search/astro-ph?searchtype=author&query=Huckle%2C+H+E">H. E. Huckle</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.12237v2-abstract-short" style="display: inline;"> Studies of the correlation between different diffuse interstellar bands (DIBs) are important for exploring their origins. However, the Gaia-RVS spectral window between 846 and 870 nm contains few DIBs, the strong DIB at 862 nm being the only convincingly confirmed one. Here we attempt to confirm the existence of a broad DIB around 864.8 nm and estimate its characteristics using the stacked Gaia-RV… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.12237v2-abstract-full').style.display = 'inline'; document.getElementById('2206.12237v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.12237v2-abstract-full" style="display: none;"> Studies of the correlation between different diffuse interstellar bands (DIBs) are important for exploring their origins. However, the Gaia-RVS spectral window between 846 and 870 nm contains few DIBs, the strong DIB at 862 nm being the only convincingly confirmed one. Here we attempt to confirm the existence of a broad DIB around 864.8 nm and estimate its characteristics using the stacked Gaia-RVS spectra of a large number of stars. We study the correlations between the two DIBs at 862 nm and 864.8 nm, as well as the interstellar extinction. We obtained spectra of the interstellar medium absorption by subtracting the stellar components using templates constructed from real spectra at high Galactic latitudes with low extinctions. We then stacked the ISM spectra in Galactic coordinates, pixelized by the HEALPix scheme, to measure the DIBs. The stacked spectrum is modeled by the profiles of the two DIBs, Gaussian for $位$862 and Lorentzian for $位$864.8, and a linear continuum. We obtain 8458 stacked spectra in total, of which 1103 (13%) have reliable fitting results after applying numerous conservative filters. This work is the first of its kind to fit and measure $位$862 and $位$864.8 simultaneously in cool-star spectra. We find that the EWs and CDs of the two DIBs are well correlated with each other. The full width at half maximum (FWHM) of $位$864.8 is estimated as $1.62 \pm 0.33$ nm which compares to $0.55 \pm 0.06$ nm for $位$862. We also measure the vacuum rest-frame wavelength of $位$864.8 to be $位_0 = 864.53 \pm 0.14$ nm, smaller than previous estimates. We find a solid confirmation of the existence of the DIB around 864.8 nm based on an exploration of its correlation with $位$862 and estimation of its FWHM. $位$862 correlates better with E(BP-RP) than $位$864.8. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.12237v2-abstract-full').style.display = 'none'; document.getElementById('2206.12237v2-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 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">7 pages, 4 figures, accepted by A&A Letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 666, L12 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.12174">arXiv:2206.12174</a> <span> [<a href="https://arxiv.org/pdf/2206.12174">pdf</a>, <a href="https://arxiv.org/format/2206.12174">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243791">10.1051/0004-6361/202243791 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 3: Reflectance spectra of Solar System small bodies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Galluccio%2C+L">L. Galluccio</a>, <a href="/search/astro-ph?searchtype=author&query=Delbo%2C+M">M. Delbo</a>, <a href="/search/astro-ph?searchtype=author&query=De+Angeli%2C+F">F. De Angeli</a>, <a href="/search/astro-ph?searchtype=author&query=Pauwels%2C+T">T. Pauwels</a>, <a href="/search/astro-ph?searchtype=author&query=Tanga%2C+P">P. Tanga</a>, <a href="/search/astro-ph?searchtype=author&query=Mignard%2C+F">F. Mignard</a>, <a href="/search/astro-ph?searchtype=author&query=Cellino%2C+A">A. Cellino</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Muinonen%2C+K">K. Muinonen</a>, <a href="/search/astro-ph?searchtype=author&query=Penttila%2C+A">A. Penttila</a>, <a href="/search/astro-ph?searchtype=author&query=Jordan%2C+S">S. Jordan</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Arenou%2C+F">F. Arenou</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Ducourant%2C+C">C. Ducourant</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Guerra%2C+R">R. Guerra</a>, <a href="/search/astro-ph?searchtype=author&query=Hutton%2C+A">A. Hutton</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a> , et al. (422 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.12174v1-abstract-short" style="display: inline;"> The Gaia mission of the European Space Agency (ESA) has been routinely observing Solar System objects (SSOs) since the beginning of its operations in August 2014. The Gaia data release three (DR3) includes, for the first time, the mean reflectance spectra of a selected sample of 60 518 SSOs, primarily asteroids, observed between August 5, 2014, and May 28, 2017. Each reflectance spectrum was deriv… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.12174v1-abstract-full').style.display = 'inline'; document.getElementById('2206.12174v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.12174v1-abstract-full" style="display: none;"> The Gaia mission of the European Space Agency (ESA) has been routinely observing Solar System objects (SSOs) since the beginning of its operations in August 2014. The Gaia data release three (DR3) includes, for the first time, the mean reflectance spectra of a selected sample of 60 518 SSOs, primarily asteroids, observed between August 5, 2014, and May 28, 2017. Each reflectance spectrum was derived from measurements obtained by means of the Blue and Red photometers (BP/RP), which were binned in 16 discrete wavelength bands. We describe the processing of the Gaia spectral data of SSOs, explaining both the criteria used to select the subset of asteroid spectra published in Gaia DR3, and the different steps of our internal validation procedures. In order to further assess the quality of Gaia SSO reflectance spectra, we carried out external validation against SSO reflectance spectra obtained from ground-based and space-borne telescopes and available in the literature. For each selected SSO, an epoch reflectance was computed by dividing the calibrated spectrum observed by the BP/RP at each transit on the focal plane by the mean spectrum of a solar analogue. The latter was obtained by averaging the Gaia spectral measurements of a selected sample of stars known to have very similar spectra to that of the Sun. Finally, a mean of the epoch reflectance spectra was calculated in 16 spectral bands for each SSO. The agreement between Gaia mean reflectance spectra and those available in the literature is good for bright SSOs, regardless of their taxonomic spectral class. We identify an increase in the spectral slope of S-type SSOs with increasing phase angle. Moreover, we show that the spectral slope increases and the depth of the 1 um absorption band decreases for increasing ages of S-type asteroid families. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.12174v1-abstract-full').style.display = 'none'; document.getElementById('2206.12174v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">30 pages, 26 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.06710">arXiv:2206.06710</a> <span> [<a href="https://arxiv.org/pdf/2206.06710">pdf</a>, <a href="https://arxiv.org/format/2206.06710">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> </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/10.1051/0004-6361/202243423">10.1051/0004-6361/202243423 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia DR3: Apsis III -- Non-stellar content and source classification </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Delchambre%2C+L">L. Delchambre</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=Bellas-Velidis%2C+I">I. Bellas-Velidis</a>, <a href="/search/astro-ph?searchtype=author&query=Drimmel%2C+R">R. Drimmel</a>, <a href="/search/astro-ph?searchtype=author&query=Garabato%2C+D">D. Garabato</a>, <a href="/search/astro-ph?searchtype=author&query=Carballo%2C+R">R. Carballo</a>, <a href="/search/astro-ph?searchtype=author&query=Hatzidimitriou%2C+D">D. Hatzidimitriou</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=Andrae%2C+R">R. Andrae</a>, <a href="/search/astro-ph?searchtype=author&query=Dafonte%2C+C">C. Dafonte</a>, <a href="/search/astro-ph?searchtype=author&query=Livanou%2C+E">E. Livanou</a>, <a href="/search/astro-ph?searchtype=author&query=Fouesneau%2C+M">M. Fouesneau</a>, <a href="/search/astro-ph?searchtype=author&query=Licata%2C+E+L">E. L. Licata</a>, <a href="/search/astro-ph?searchtype=author&query=Lindstrom%2C+H+E+P">H. E. P. Lindstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Manteiga%2C+M">M. Manteiga</a>, <a href="/search/astro-ph?searchtype=author&query=Robin%2C+C">C. Robin</a>, <a href="/search/astro-ph?searchtype=author&query=Silvelo%2C+A">A. Silvelo</a>, <a href="/search/astro-ph?searchtype=author&query=Aramburu%2C+A+A">A. Abreu Aramburu</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M+A">M. A. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Bakker%2C+J">J. Bakker</a>, <a href="/search/astro-ph?searchtype=author&query=Bijaoui%2C+A">A. Bijaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Brouillet%2C+N">N. Brouillet</a>, <a href="/search/astro-ph?searchtype=author&query=Brugaletta%2C+E">E. Brugaletta</a>, <a href="/search/astro-ph?searchtype=author&query=Burlacu%2C+A">A. Burlacu</a>, <a href="/search/astro-ph?searchtype=author&query=Casamiquela%2C+L">L. Casamiquela</a> , et al. (56 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="2206.06710v2-abstract-short" style="display: inline;"> Context. As part of the third Gaia data release, we present the contributions of the non-stellar and classification modules from the eighth coordination unit (CU8) of the Data Processing and Analysis Consortium, which is responsible for the determination of source astrophysical parameters using Gaia data. This is the third in a series of three papers describing the work done within CU8 for this re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.06710v2-abstract-full').style.display = 'inline'; document.getElementById('2206.06710v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.06710v2-abstract-full" style="display: none;"> Context. As part of the third Gaia data release, we present the contributions of the non-stellar and classification modules from the eighth coordination unit (CU8) of the Data Processing and Analysis Consortium, which is responsible for the determination of source astrophysical parameters using Gaia data. This is the third in a series of three papers describing the work done within CU8 for this release. Aims. For each of the five relevant modules from CU8, we summarise their objectives, the methods they employ, their performance, and the results they produce for Gaia DR3. We further advise how to use these data products and highlight some limitations. Methods. The Discrete Source Classifier (DSC) module provides classification probabilities associated with five types of sources: quasars, galaxies, stars, white dwarfs, and physical binary stars. A subset of these sources are processed by the Outlier Analysis (OA) module, which performs an unsupervised clustering analysis, and then associates labels with the clusters to complement the DSC classification. The Quasi Stellar Object Classifier (QSOC) and the Unresolved Galaxy Classifier (UGC) determine the redshifts of the sources classified as quasar and galaxy by the DSC module. Finally, the Total Galactic Extinction (TGE) module uses the extinctions of individual stars determined by another CU8 module to determine the asymptotic extinction along all lines of sight for Galactic latitudes |b| > 5 deg. Results. Gaia DR3 includes 1591 million sources with DSC classifications; 56 million sources to which the OA clustering is applied; 1.4 million sources with redshift estimates from UGC; 6.4 million sources with QSOC redshift; and 3.1 million level 9 HEALPixes of size 0.013 squared degree, where the extinction is evaluated by TGE. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.06710v2-abstract-full').style.display = 'none'; document.getElementById('2206.06710v2-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 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 by A&A. 36 pages, 29 figures, 9 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A31 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.06207">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/2206.06138">arXiv:2206.06138</a> <span> [<a href="https://arxiv.org/pdf/2206.06138">pdf</a>, <a href="https://arxiv.org/format/2206.06138">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/10.1051/0004-6361/202243462">10.1051/0004-6361/202243462 <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: Analysis of the Gaia BP/RP spectra using the General Stellar Parameterizer from Photometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Sordo%2C+R">R. Sordo</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=Dharmawardena%2C+T+E">T. E. Dharmawardena</a>, <a href="/search/astro-ph?searchtype=author&query=Rybizki%2C+J">J. Rybizki</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=Lindstr%C3%B8m%2C+H+E+P">H. E. P. Lindstr酶m</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=Drimmel%2C+R">R. Drimmel</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=Soubiran%2C+C">C. Soubiran</a>, <a href="/search/astro-ph?searchtype=author&query=Brouillet%2C+N">N. Brouillet</a>, <a href="/search/astro-ph?searchtype=author&query=Casamiquela%2C+L">L. Casamiquela</a>, <a href="/search/astro-ph?searchtype=author&query=Rix%2C+H+-">H. -W. Rix</a>, <a href="/search/astro-ph?searchtype=author&query=Aramburu%2C+A+A">A. Abreu Aramburu</a>, <a href="/search/astro-ph?searchtype=author&query=%C3%81lvarez%2C+M+A">M. A. 脕lvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Bakker%2C+J">J. Bakker</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=Bijaoui%2C+A">A. Bijaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Brugaletta%2C+E">E. Brugaletta</a>, <a href="/search/astro-ph?searchtype=author&query=Burlacu%2C+A">A. Burlacu</a>, <a href="/search/astro-ph?searchtype=author&query=Carballo%2C+R">R. Carballo</a>, <a href="/search/astro-ph?searchtype=author&query=Chaoul%2C+L">L. Chaoul</a>, <a href="/search/astro-ph?searchtype=author&query=Chiavassa%2C+A">A. Chiavassa</a> , et al. (58 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="2206.06138v1-abstract-short" style="display: inline;"> We present the General Stellar Parameterizer from Photometry (GSP-Phot), which is part of the astrophysical parameters inference system (Apsis). GSP-Phot is designed to produce a homogeneous catalogue of parameters for hundreds of millions of single non-variable stars based on their astrometry, photometry, and low-resolution BP/RP spectra. These parameters are effective temperature, surface gravit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.06138v1-abstract-full').style.display = 'inline'; document.getElementById('2206.06138v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.06138v1-abstract-full" style="display: none;"> We present the General Stellar Parameterizer from Photometry (GSP-Phot), which is part of the astrophysical parameters inference system (Apsis). GSP-Phot is designed to produce a homogeneous catalogue of parameters for hundreds of millions of single non-variable stars based on their astrometry, photometry, and low-resolution BP/RP spectra. These parameters are effective temperature, surface gravity, metallicity, absolute $M_G$ magnitude, radius, distance, and extinction for each star. GSP-Phot uses a Bayesian forward-modelling approach to simultaneously fit the BP/RP spectrum, parallax, and apparent $G$ magnitude. A major design feature of GSP-Phot is the use of the apparent flux levels of BP/RP spectra to derive, in combination with isochrone models, tight observational constraints on radii and distances. We carefully validate the uncertainty estimates by exploiting repeat Gaia observations of the same source. The data release includes GSP-Phot results for 471 million sources with $G<19$. Typical differences to literature values are 110 K for $T_{\rm eff}$ and 0.2-0.25 for $\log g$, but these depend strongly on data quality. In particular, GSP-Phot results are significantly better for stars with good parallax measurements ($\varpi/蟽_varpi>20$), mostly within 2kpc. Metallicity estimates exhibit substantial biases compared to literature values and are only useful at a qualitative level. However, we provide an empirical calibration of our metallicity estimates that largely removes these biases. Extinctions $A_0$ and $A_{\rm BP}$ show typical differences from reference values of 0.07-0.09 mag. MCMC samples of the parameters are also available for 95% of the sources. GSP-Phot provides a homogeneous catalogue of stellar parameters, distances, and extinctions that can be used for various purposes, such as sample selections (OB stars, red giants, solar analogues etc.). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.06138v1-abstract-full').style.display = 'none'; document.getElementById('2206.06138v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 19 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/2206.05992">arXiv:2206.05992</a> <span> [<a href="https://arxiv.org/pdf/2206.05992">pdf</a>, <a href="https://arxiv.org/format/2206.05992">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/10.1051/0004-6361/202243919">10.1051/0004-6361/202243919 <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: Apsis II -- Stellar Parameters </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Andrae%2C+R">R. Andrae</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=Soubiran%2C+C">C. Soubiran</a>, <a href="/search/astro-ph?searchtype=author&query=Kordopatis%2C+G">G. Kordopatis</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Heiter%2C+U">U. Heiter</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=de+Laverny%2C+P">P. de Laverny</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=Lobel%2C+A">A. Lobel</a>, <a href="/search/astro-ph?searchtype=author&query=Sordo%2C+R">R. Sordo</a>, <a href="/search/astro-ph?searchtype=author&query=Rybizki%2C+J">J. Rybizki</a>, <a href="/search/astro-ph?searchtype=author&query=Slezak%2C+I">I. Slezak</a>, <a href="/search/astro-ph?searchtype=author&query=%C3%81lvarez%2C+M+A">M. A. 脕lvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Drimmel%2C+R">R. Drimmel</a>, <a href="/search/astro-ph?searchtype=author&query=Garabato%2C+D">D. Garabato</a>, <a href="/search/astro-ph?searchtype=author&query=Delchambre%2C+L">L. Delchambre</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=Hatzidimitriou%2C+D">D. Hatzidimitriou</a>, <a href="/search/astro-ph?searchtype=author&query=Lorca%2C+A">A. Lorca</a>, <a href="/search/astro-ph?searchtype=author&query=Fustec%2C+Y+L">Y. Le Fustec</a>, <a href="/search/astro-ph?searchtype=author&query=Pailler%2C+F">F. Pailler</a> , et al. (56 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="2206.05992v1-abstract-short" style="display: inline;"> The third Gaia data release contains, beyond the astrometry and photometry, dispersed light for hundreds of millions of sources from the Gaia prism spectra (BP and RP) and the spectrograph (RVS). This data release opens a new window on the chemo-dynamical properties of stars in our Galaxy, essential knowledge for understanding the structure, formation, and evolution of the Milky Way. To provide in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05992v1-abstract-full').style.display = 'inline'; document.getElementById('2206.05992v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.05992v1-abstract-full" style="display: none;"> The third Gaia data release contains, beyond the astrometry and photometry, dispersed light for hundreds of millions of sources from the Gaia prism spectra (BP and RP) and the spectrograph (RVS). This data release opens a new window on the chemo-dynamical properties of stars in our Galaxy, essential knowledge for understanding the structure, formation, and evolution of the Milky Way. To provide insight into the physical properties of Milky Way stars, we used these data to produce a uniformly-derived, all-sky catalog of stellar astrophysical parameters (APs): Teff, logg, [M/H], [$伪$/Fe], activity index, emission lines, rotation, 13 chemical abundance estimates, radius, age, mass, bolometric luminosity, distance, and dust extinction. We developed the Apsis pipeline to infer APs of Gaia objects by analyzing their astrometry, photometry, BP/RP, and RVS spectra. We validate our results against other literature works, including benchmark stars, interferometry, and asteroseismology. Here we assessed the stellar analysis performance from Apsis statistically. We describe the quantities we obtained, including our results' underlying assumptions and limitations. We provide guidance and identify regimes in which our parameters should and should not be used. Despite some limitations, this is the most extensive catalog of uniformly-inferred stellar parameters to date. These comprise Teff, logg, and [M/H] (470 million using BP/RP, 6 million using RVS), radius (470 million), mass (140 million), age (120 million), chemical abundances (5 million), diffuse interstellar band analysis (1/2 million), activity indices (2 million), H{$伪$} equivalent widths (200 million), and further classification of spectral types (220 million) and emission-line stars (50 thousand). More precise and detailed astrophysical parameters based on epoch BP, RP, and RVS are planned for the next Gaia data release. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05992v1-abstract-full').style.display = 'none'; document.getElementById('2206.05992v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Gaia DR3 paper, 37 pages, 38 figures, catalog is available from the Gaia Archive and partner data centers; 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 674, A28 (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/2206.05864">arXiv:2206.05864</a> <span> [<a href="https://arxiv.org/pdf/2206.05864">pdf</a>, <a href="https://arxiv.org/format/2206.05864">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> <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/10.1051/0004-6361/202243688">10.1051/0004-6361/202243688 <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: Astrophysical parameters inference system (Apsis) I -- methods and content overview </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Sordo%2C+R">R. Sordo</a>, <a href="/search/astro-ph?searchtype=author&query=Pailler%2C+F">F. Pailler</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=Heiter%2C+U">U. Heiter</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=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=Lobel%2C+A">A. Lobel</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=Garabato%2C+D">D. Garabato</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=Brugaletta%2C+E">E. Brugaletta</a>, <a href="/search/astro-ph?searchtype=author&query=Lorca%2C+A">A. Lorca</a>, <a href="/search/astro-ph?searchtype=author&query=Ordenovic%2C+C">C. Ordenovic</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=Sarro%2C+L+M">L. M. Sarro</a>, <a href="/search/astro-ph?searchtype=author&query=Delchambre%2C+L">L. Delchambre</a>, <a href="/search/astro-ph?searchtype=author&query=Drimmel%2C+R">R. Drimmel</a>, <a href="/search/astro-ph?searchtype=author&query=Rybizki%2C+J">J. Rybizki</a>, <a href="/search/astro-ph?searchtype=author&query=Elipe%2C+G+T">G. Torralba Elipe</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=Recio-Blanco%2C+A">A. Recio-Blanco</a>, <a href="/search/astro-ph?searchtype=author&query=Schultheis%2C+M+S">M. S. Schultheis</a>, <a href="/search/astro-ph?searchtype=author&query=De+Angeli%2C+F">F. De Angeli</a> , et al. (64 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.05864v1-abstract-short" style="display: inline;"> Gaia Data Release 3 contains a wealth of new data products for the community. Astrophysical parameters are a major component of this release. They were produced by the Astrophysical parameters inference system (Apsis) within the Gaia Data Processing and Analysis Consortium. The aim of this paper is to describe the overall content of the astrophysical parameters in Gaia Data Release 3 and how they… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05864v1-abstract-full').style.display = 'inline'; document.getElementById('2206.05864v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.05864v1-abstract-full" style="display: none;"> Gaia Data Release 3 contains a wealth of new data products for the community. Astrophysical parameters are a major component of this release. They were produced by the Astrophysical parameters inference system (Apsis) within the Gaia Data Processing and Analysis Consortium. The aim of this paper is to describe the overall content of the astrophysical parameters in Gaia Data Release 3 and how they were produced. In Apsis we use the mean BP/RP and mean RVS spectra along with astrometry and photometry, and we derive the following parameters: source classification and probabilities for 1.6 billion objects, interstellar medium characterisation and distances for up to 470 million sources, including a 2D total Galactic extinction map, 6 million redshifts of quasar candidates and 1.4 million redshifts of galaxy candidates, along with an analysis of 50 million outlier sources through an unsupervised classification. The astrophysical parameters also include many stellar spectroscopic and evolutionary parameters for up to 470 million sources. These comprise Teff, logg, and m_h (470 million using BP/RP, 6 million using RVS), radius (470 million), mass (140 million), age (120 million), chemical abundances (up to 5 million), diffuse interstellar band analysis (0.5 million), activity indices (2 million), H-alpha equivalent widths (200 million), and further classification of spectral types (220 million) and emission-line stars (50 thousand). This catalogue is the most extensive homogeneous database of astrophysical parameters to date, and it is based uniquely on Gaia data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05864v1-abstract-full').style.display = 'none'; document.getElementById('2206.05864v1-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 7 pages references, appendix, affiliations, acknowledgements), 29 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, 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/2206.05766">arXiv:2206.05766</a> <span> [<a href="https://arxiv.org/pdf/2206.05766">pdf</a>, <a href="https://arxiv.org/format/2206.05766">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/10.1051/0004-6361/202244156">10.1051/0004-6361/202244156 <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 chromospheric activity and mass accretion from Ca II IRT observed by the Radial Velocity Spectrometer </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lanzafame%2C+A+C">A. C. Lanzafame</a>, <a href="/search/astro-ph?searchtype=author&query=Brugaletta%2C+E">E. Brugaletta</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=Sordo%2C+R">R. Sordo</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=Andretta%2C+V">V. Andretta</a>, <a href="/search/astro-ph?searchtype=author&query=Scandariato%2C+G">G. Scandariato</a>, <a href="/search/astro-ph?searchtype=author&query=Bus%C3%A0%2C+I">I. Bus脿</a>, <a href="/search/astro-ph?searchtype=author&query=Distefano%2C+E">E. Distefano</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=de+Laverny%2C+P">P. de Laverny</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=Aramburu%2C+A+A">A. Abreu Aramburu</a>, <a href="/search/astro-ph?searchtype=author&query=%C3%81lvarez%2C+M+A">M. A. 脕lvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Andrae%2C+R">R. Andrae</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=Bakker%2C+J">J. Bakker</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=Bijaoui%2C+A">A. Bijaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Brouillet%2C+N">N. Brouillet</a>, <a href="/search/astro-ph?searchtype=author&query=Burlacu%2C+A">A. Burlacu</a>, <a href="/search/astro-ph?searchtype=author&query=Carballo%2C+R">R. Carballo</a>, <a href="/search/astro-ph?searchtype=author&query=Casamiquela%2C+L">L. Casamiquela</a>, <a href="/search/astro-ph?searchtype=author&query=Chaoul%2C+L">L. Chaoul</a>, <a href="/search/astro-ph?searchtype=author&query=Chiavassa%2C+A">A. Chiavassa</a> , et al. (60 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="2206.05766v1-abstract-short" style="display: inline;"> The Gaia Radial Velocity Spectrometer provides the unique opportunity of a spectroscopic analysis of millions of stars at medium-resolution in the near-infrared. This wavelength range includes the Ca II infrared triplet (IRT), which is a good diagnostics of magnetic activity in the chromosphere of late-type stars. Here we present the method devised for inferring the Gaia stellar activity index tog… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05766v1-abstract-full').style.display = 'inline'; document.getElementById('2206.05766v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.05766v1-abstract-full" style="display: none;"> The Gaia Radial Velocity Spectrometer provides the unique opportunity of a spectroscopic analysis of millions of stars at medium-resolution in the near-infrared. This wavelength range includes the Ca II infrared triplet (IRT), which is a good diagnostics of magnetic activity in the chromosphere of late-type stars. Here we present the method devised for inferring the Gaia stellar activity index together with its scientific validation. A sample of well studied PMS stars is considered to identify the regime in which the Gaia stellar activity index may be affected by mass accretion. The position of these stars in the colour-magnitude diagram and the correlation with the amplitude of the photometric rotational modulation is also scrutinised. Three regimes of the chromospheric stellar activity are identified, confirming suggestions made by previous authors on much smaller $R'_{\rm HK}$ datasets. The highest stellar activity regime is associated with PMS stars and RS CVn systems, in which activity is enhanced by tidal interaction. Some evidence of a bimodal distribution in MS stars with $T_{\rm eff}\ge$ 5000 K is also found, which defines the two other regimes, without a clear gap in between. Stars with 3500 K$\le T_{\rm eff} \le$ 5000 K are found to be either very active PMS stars or active MS stars with a unimodal distribution in chromospheric activity. A dramatic change in the activity distribution is found for $T_{\rm eff}\le$3500 K, with a dominance of low activity stars close to the transition between partially- and fully-convective stars and a rise in activity down into the fully-convective regime. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05766v1-abstract-full').style.display = 'none'; document.getElementById('2206.05766v1-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">18 pages, 10 figures, 2 tables, 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 674, A30 (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/2206.05541">arXiv:2206.05541</a> <span> [<a href="https://arxiv.org/pdf/2206.05541">pdf</a>, <a href="https://arxiv.org/format/2206.05541">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/10.1051/0004-6361/202243750">10.1051/0004-6361/202243750 <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: Analysis of RVS spectra using the General Stellar Parametriser from spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Recio-Blanco%2C+A">A. Recio-Blanco</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=Kordopatis%2C+G">G. Kordopatis</a>, <a href="/search/astro-ph?searchtype=author&query=%C3%81lvarez%2C+M+A">M. A. 脕lvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Schultheis%2C+M">M. Schultheis</a>, <a href="/search/astro-ph?searchtype=author&query=Contursi%2C+G">G. Contursi</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+H">H. Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Elipe%2C+G+T">G. Torralba Elipe</a>, <a href="/search/astro-ph?searchtype=author&query=Ordenovic%2C+C">C. Ordenovic</a>, <a href="/search/astro-ph?searchtype=author&query=Manteiga%2C+M">M. Manteiga</a>, <a href="/search/astro-ph?searchtype=author&query=Dafonte%2C+C">C. Dafonte</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=Bijaoui%2C+A">A. Bijaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Fremat%2C+Y">Y. Fremat</a>, <a href="/search/astro-ph?searchtype=author&query=Seabroke%2C+G">G. Seabroke</a>, <a href="/search/astro-ph?searchtype=author&query=Pailler%2C+F">F. Pailler</a>, <a href="/search/astro-ph?searchtype=author&query=Spitoni%2C+E">E. Spitoni</a>, <a href="/search/astro-ph?searchtype=author&query=Poggio%2C+E">E. Poggio</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=Aramburu%2C+A+A">A. Abreu Aramburu</a>, <a href="/search/astro-ph?searchtype=author&query=Accart%2C+S">S. Accart</a>, <a href="/search/astro-ph?searchtype=author&query=Andrae%2C+R">R. Andrae</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=Bellas-Velidis%2C+I">I. Bellas-Velidis</a> , et al. (55 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="2206.05541v1-abstract-short" style="display: inline;"> The chemo-physical parametrisation of stellar spectra is essential for understanding the nature and evolution of stars and of Galactic stellar populations. Gaia DR3 contains the parametrisation of RVS data performed by the General Stellar Parametriser-spectroscopy, module. Here we describe the parametrisation of the first 34 months of RVS observations. GSP-spec estimates the chemo-physical paramet… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05541v1-abstract-full').style.display = 'inline'; document.getElementById('2206.05541v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.05541v1-abstract-full" style="display: none;"> The chemo-physical parametrisation of stellar spectra is essential for understanding the nature and evolution of stars and of Galactic stellar populations. Gaia DR3 contains the parametrisation of RVS data performed by the General Stellar Parametriser-spectroscopy, module. Here we describe the parametrisation of the first 34 months of RVS observations. GSP-spec estimates the chemo-physical parameters from combined RVS spectra of single stars. The main analysis workflow described here, MatisseGauguin, is based on projection and optimisation methods and provides the stellar atmospheric parameters; the individual chemical abundances of N, Mg, Si, S, Ca, Ti, Cr, FeI, FeII, Ni, Zr, Ce and Nd; the differential equivalent width of a cyanogen line; and the parameters of a DIB feature. Another workflow, based on an artificial neural network, provides a second set of atmospheric parameters that are useful for classification control. We implement a detailed quality flag chain considering different error sources. With about 5.6 million stars, the Gaia DR3 GSP-spec all-sky catalogue is the largest compilation of stellar chemo-physical parameters ever published and the first one from space data. Internal and external biases have been studied taking into account the implemented flags. In some cases, simple calibrations with low degree polynomials are suggested. The homogeneity and quality of the estimated parameters enables chemo-dynamical studies of Galactic stellar populations, interstellar extinction studies from individual spectra, and clear constraints on stellar evolution models. We highly recommend that users adopt the provided quality flags for scientific exploitation . The Gaia DR3 GSP-spec catalogue is a major step in the scientific exploration of Milky Way stellar populations, confirming the Gaia promise of a new Galactic vision (abridged). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.05541v1-abstract-full').style.display = 'none'; document.getElementById('2206.05541v1-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, A29 (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/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/2101.05811">arXiv:2101.05811</a> <span> [<a href="https://arxiv.org/pdf/2101.05811">pdf</a>, <a href="https://arxiv.org/format/2101.05811">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202039714">10.1051/0004-6361/202039714 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Early Data Release 3: The Galactic anticentre </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Antoja%2C+T">T. Antoja</a>, <a href="/search/astro-ph?searchtype=author&query=McMillan%2C+P">P. McMillan</a>, <a href="/search/astro-ph?searchtype=author&query=Kordopatis%2C+G">G. Kordopatis</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos%2C+P">P. Ramos</a>, <a href="/search/astro-ph?searchtype=author&query=Helmi%2C+A">A. Helmi</a>, <a href="/search/astro-ph?searchtype=author&query=Balbinot%2C+E">E. Balbinot</a>, <a href="/search/astro-ph?searchtype=author&query=Cantat-Gaudin%2C+T">T. Cantat-Gaudin</a>, <a href="/search/astro-ph?searchtype=author&query=Chemin%2C+L">L. Chemin</a>, <a href="/search/astro-ph?searchtype=author&query=Figueras%2C+F">F. Figueras</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a>, <a href="/search/astro-ph?searchtype=author&query=Khanna%2C+S">S. Khanna</a>, <a href="/search/astro-ph?searchtype=author&query=Romero-Gomez%2C+M">M. Romero-Gomez</a>, <a href="/search/astro-ph?searchtype=author&query=Seabroke%2C+G">G. Seabroke</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Hutton%2C+A">A. Hutton</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+F">F. Jansen</a> , et al. (395 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.05811v2-abstract-short" style="display: inline;"> We aim to demonstrate the scientific potential of the Gaia Early Data Release 3 (EDR3) for the study of the Milky Way structure and evolution. We used astrometric positions, proper motions, parallaxes, and photometry from EDR3 to select different populations and components and to calculate the distances and velocities in the direction of the anticentre. We explore the disturbances of the current d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.05811v2-abstract-full').style.display = 'inline'; document.getElementById('2101.05811v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.05811v2-abstract-full" style="display: none;"> We aim to demonstrate the scientific potential of the Gaia Early Data Release 3 (EDR3) for the study of the Milky Way structure and evolution. We used astrometric positions, proper motions, parallaxes, and photometry from EDR3 to select different populations and components and to calculate the distances and velocities in the direction of the anticentre. We explore the disturbances of the current disc, the spatial and kinematical distributions of early accreted versus in-situ stars, the structures in the outer parts of the disc, and the orbits of open clusters Berkeley 29 and Saurer 1. We find that: i) the dynamics of the Galactic disc are very complex with vertical asymmetries, and new correlations, including a bimodality with disc stars with large angular momentum moving vertically upwards from below the plane, and disc stars with slightly lower angular momentum moving preferentially downwards; ii) we resolve the kinematic substructure (diagonal ridges) in the outer parts of the disc for the first time; iii) the red sequence that has been associated with the proto-Galactic disc that was present at the time of the merger with Gaia-Enceladus-Sausage is currently radially concentrated up to around 14 kpc, while the blue sequence that has been associated with debris of the satellite extends beyond that; iv) there are density structures in the outer disc, both above and below the plane, most probably related to Monoceros, the Anticentre Stream, and TriAnd, for which the Gaia data allow an exhaustive selection of candidate member stars and dynamical study; and v) the open clusters Berkeley~29 and Saurer~1, despite being located at large distances from the Galactic centre, are on nearly circular disc-like orbits. We demonstrate how, once again, the Gaia are crucial for our understanding of the different pieces of our Galaxy and their connection to its global structure and history. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.05811v2-abstract-full').style.display = 'none'; document.getElementById('2101.05811v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Gaia EDR3 performance verification paper, version 2 closer to published version in A&A, complete list of authors</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 649, A8 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.02061">arXiv:2012.02061</a> <span> [<a href="https://arxiv.org/pdf/2012.02061">pdf</a>, <a href="https://arxiv.org/format/2012.02061">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202039498">10.1051/0004-6361/202039498 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Early Data Release 3: The Gaia Catalogue of Nearby Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Smart%2C+R+L">R. L. Smart</a>, <a href="/search/astro-ph?searchtype=author&query=Sarro%2C+L+M">L. M. Sarro</a>, <a href="/search/astro-ph?searchtype=author&query=Rybizki%2C+J">J. Rybizki</a>, <a href="/search/astro-ph?searchtype=author&query=Reyl%C3%A9%2C+C">C. Reyl茅</a>, <a href="/search/astro-ph?searchtype=author&query=Robin%2C+A+C">A. C. Robin</a>, <a href="/search/astro-ph?searchtype=author&query=Hambly%2C+N+C">N. C. Hambly</a>, <a href="/search/astro-ph?searchtype=author&query=Abbas%2C+U">U. Abbas</a>, <a href="/search/astro-ph?searchtype=author&query=Barstow%2C+M+A">M. A. Barstow</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Bucciarelli%2C+B">B. Bucciarelli</a>, <a href="/search/astro-ph?searchtype=author&query=Carrasco%2C+J+M">J. M. Carrasco</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+W+J">W. J. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Hodgkin%2C+S+T">S. T. Hodgkin</a>, <a href="/search/astro-ph?searchtype=author&query=Masana%2C+E">E. Masana</a>, <a href="/search/astro-ph?searchtype=author&query=Michalik%2C+D">D. Michalik</a>, <a href="/search/astro-ph?searchtype=author&query=Sahlmann%2C+J">J. Sahlmann</a>, <a href="/search/astro-ph?searchtype=author&query=Sozzetti%2C+A">A. Sozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a> , et al. (398 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.02061v1-abstract-short" style="display: inline;"> We produce a clean and well-characterised catalogue of objects within 100\,pc of the Sun from the \G\ Early Data Release 3. We characterise the catalogue through comparisons to the full data release, external catalogues, and simulations. We carry out a first analysis of the science that is possible with this sample to demonstrate its potential and best practices for its use. The selection of obj… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02061v1-abstract-full').style.display = 'inline'; document.getElementById('2012.02061v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.02061v1-abstract-full" style="display: none;"> We produce a clean and well-characterised catalogue of objects within 100\,pc of the Sun from the \G\ Early Data Release 3. We characterise the catalogue through comparisons to the full data release, external catalogues, and simulations. We carry out a first analysis of the science that is possible with this sample to demonstrate its potential and best practices for its use. The selection of objects within 100\,pc from the full catalogue used selected training sets, machine-learning procedures, astrometric quantities, and solution quality indicators to determine a probability that the astrometric solution is reliable. The training set construction exploited the astrometric data, quality flags, and external photometry. For all candidates we calculated distance posterior probability densities using Bayesian procedures and mock catalogues to define priors. Any object with reliable astrometry and a non-zero probability of being within 100\,pc is included in the catalogue. We have produced a catalogue of \NFINAL\ objects that we estimate contains at least 92\% of stars of stellar type M9 within 100\,pc of the Sun. We estimate that 9\% of the stars in this catalogue probably lie outside 100\,pc, but when the distance probability function is used, a correct treatment of this contamination is possible. We produced luminosity functions with a high signal-to-noise ratio for the main-sequence stars, giants, and white dwarfs. We examined in detail the Hyades cluster, the white dwarf population, and wide-binary systems and produced candidate lists for all three samples. We detected local manifestations of several streams, superclusters, and halo objects, in which we identified 12 members of \G\ Enceladus. We present the first direct parallaxes of five objects in multiple systems within 10\,pc of the Sun. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02061v1-abstract-full').style.display = 'none'; document.getElementById('2012.02061v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">45 Pages, 39 figures in main part and 18 in appendix, tables on CDS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 649, A6 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.02036">arXiv:2012.02036</a> <span> [<a href="https://arxiv.org/pdf/2012.02036">pdf</a>, <a href="https://arxiv.org/format/2012.02036">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202039734">10.1051/0004-6361/202039734 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Early Data Release 3: Acceleration of the solar system from Gaia astrometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Klioner%2C+S+A">S. A. Klioner</a>, <a href="/search/astro-ph?searchtype=author&query=Mignard%2C+F">F. Mignard</a>, <a href="/search/astro-ph?searchtype=author&query=Lindegren%2C+L">L. Lindegren</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+U">U. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=McMillan%2C+P+J">P. J. McMillan</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J">J. Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+D">D. Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos-Lerate%2C+M">M. Ramos-Lerate</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Bombrun%2C+A">A. Bombrun</a>, <a href="/search/astro-ph?searchtype=author&query=de+Torres%2C+A">A. de Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Gerlach%2C+E">E. Gerlach</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+R">R. Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Hilger%2C+T">T. Hilger</a>, <a href="/search/astro-ph?searchtype=author&query=Lammers%2C+U">U. Lammers</a>, <a href="/search/astro-ph?searchtype=author&query=Steidelm%C3%BCller%2C+H">H. Steidelm眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Stephenson%2C+C+A">C. A. Stephenson</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a> , et al. (392 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.02036v1-abstract-short" style="display: inline;"> Context. Gaia Early Data Release 3 (Gaia EDR3) provides accurate astrometry for about 1.6 million compact (QSO-like) extragalactic sources, 1.2 million of which have the best-quality five-parameter astrometric solutions. Aims. The proper motions of QSO-like sources are used to reveal a systematic pattern due to the acceleration of the solar system barycentre with respect to the rest frame of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02036v1-abstract-full').style.display = 'inline'; document.getElementById('2012.02036v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.02036v1-abstract-full" style="display: none;"> Context. Gaia Early Data Release 3 (Gaia EDR3) provides accurate astrometry for about 1.6 million compact (QSO-like) extragalactic sources, 1.2 million of which have the best-quality five-parameter astrometric solutions. Aims. The proper motions of QSO-like sources are used to reveal a systematic pattern due to the acceleration of the solar system barycentre with respect to the rest frame of the Universe. Apart from being an important scientific result by itself, the acceleration measured in this way is a good quality indicator of the Gaia astrometric solution. Methods. The effect of the acceleration is obtained as a part of the general expansion of the vector field of proper motions in Vector Spherical Harmonics (VSH). Various versions of the VSH fit and various subsets of the sources are tried and compared to get the most consistent result and a realistic estimate of its uncertainty. Additional tests with the Gaia astrometric solution are used to get a better idea on possible systematic errors in the estimate. Results. Our best estimate of the acceleration based on Gaia EDR3 is $(2.32 \pm 0.16) \times 10^{-10}$ m s${}^{-2}$ (or $7.33 \pm 0.51$ km s$^{-1}$ Myr${}^{-1}$) towards $伪= 269.1^\circ \pm 5.4^\circ$, $未= -31.6^\circ \pm 4.1^\circ$, corresponding to a proper motion amplitude of $5.05 \pm 0.35$ $渭$as yr${}^{-1}$. This is in good agreement with the acceleration expected from current models of the Galactic gravitational potential. We expect that future Gaia data releases will provide estimates of the acceleration with uncertainties substantially below 0.1 $渭$as yr${}^{-1}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02036v1-abstract-full').style.display = 'none'; document.getElementById('2012.02036v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">A&A, accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 649, A9 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.01771">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/2011.04481">arXiv:2011.04481</a> <span> [<a href="https://arxiv.org/pdf/2011.04481">pdf</a>, <a href="https://arxiv.org/format/2011.04481">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/10.1051/0004-6361/202039212">10.1051/0004-6361/202039212 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Testing abundance-age relations beyond solar analogues with Kepler LEGACY stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Morel%2C+T">Thierry Morel</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">Orlagh L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Montalban%2C+J">Josefina Montalban</a>, <a href="/search/astro-ph?searchtype=author&query=Miglio%2C+A">Andrea Miglio</a>, <a href="/search/astro-ph?searchtype=author&query=Willett%2C+E">Emma Willett</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="2011.04481v1-abstract-short" style="display: inline;"> We present abundances of 21 elements in a sample of 13 bright FG dwarfs drawn from the Kepler LEGACY sample to examine the applicability of the abundance-age relations to stars with properties strongly departing from solar. These stars have precise asteroseismic ages that can be compared to the abundance-based estimates. We analyse the well-known binary 16 Cyg AB for validation purposes and confir… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.04481v1-abstract-full').style.display = 'inline'; document.getElementById('2011.04481v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.04481v1-abstract-full" style="display: none;"> We present abundances of 21 elements in a sample of 13 bright FG dwarfs drawn from the Kepler LEGACY sample to examine the applicability of the abundance-age relations to stars with properties strongly departing from solar. These stars have precise asteroseismic ages that can be compared to the abundance-based estimates. We analyse the well-known binary 16 Cyg AB for validation purposes and confirm the existence of a slight metal enhancement (~0.02 dex) in the primary, which might arise from planetary formation/ingestion. We draw attention to systematic errors in some widely-used catalogues of non-seismic parameters that may significantly bias asteroseismic inferences. In particular, we find evidence that the ASPCAP Teff scale used for the APOKASC catalogue is too cool for dwarfs and that the [Fe/H] values are underestimated by ~0.1 dex. We compare seismic ages to those inferred from empirical abundance-age relations based on ages from PARSEC isochrones and abundances obtained in the framework of the HARPS-GTO program. These calibrations take into account a dependency with the stellar effective temperature, metallicity, and/or mass. We find that the seismic and abundance-based ages differ on average by 1.5-2 Gyrs, while taking into account a dependency with one or two stellar parameters in the calibrations leads to a global improvement of up to ~0.5 Gyr. However, even in that case we find that seismic ages are systematically larger by ~0.7 Gyr. We argue that it may be ascribed to a variety of causes including the presence of small zero-point offsets between our abundances and those used to construct the calibrations or to the choice of the set of theoretical isochrones. The conclusions above are supported by the analysis of literature data for a larger number of Kepler targets. [Abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.04481v1-abstract-full').style.display = 'none'; document.getElementById('2011.04481v1-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 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 16 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 646, A78 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.06981">arXiv:1908.06981</a> <span> [<a href="https://arxiv.org/pdf/1908.06981">pdf</a>, <a href="https://arxiv.org/format/1908.06981">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/10.3847/1538-4365/ab3d29">10.3847/1538-4365/ab3d29 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The K2 Bright Star Survey I: Methodology and Data Release </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pope%2C+B+J+S">Benjamin J. S. Pope</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+T+R">Timothy R. White</a>, <a href="/search/astro-ph?searchtype=author&query=Farr%2C+W+M">Will M. Farr</a>, <a href="/search/astro-ph?searchtype=author&query=Yu%2C+J">Jie Yu</a>, <a href="/search/astro-ph?searchtype=author&query=Greklek-McKeon%2C+M">Michael Greklek-McKeon</a>, <a href="/search/astro-ph?searchtype=author&query=Huber%2C+D">Daniel Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Aerts%2C+C">Conny Aerts</a>, <a href="/search/astro-ph?searchtype=author&query=Aigrain%2C+S">Suzanne Aigrain</a>, <a href="/search/astro-ph?searchtype=author&query=Bedding%2C+T+R">Timothy R. Bedding</a>, <a href="/search/astro-ph?searchtype=author&query=Boyajian%2C+T">Tabetha Boyajian</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">Orlagh L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Hogg%2C+D+W">David W. Hogg</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="1908.06981v2-abstract-short" style="display: inline;"> While the Kepler Mission was designed to look at tens of thousands of faint stars (V > 12), brighter stars that saturated the detector are important because they can be and have been observed very accurately by other instruments. By analyzing the unsaturated scattered-light `halo' around these stars, we have retrieved precise light curves of most of the brightest stars in K2 fields from Campaign~4… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.06981v2-abstract-full').style.display = 'inline'; document.getElementById('1908.06981v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.06981v2-abstract-full" style="display: none;"> While the Kepler Mission was designed to look at tens of thousands of faint stars (V > 12), brighter stars that saturated the detector are important because they can be and have been observed very accurately by other instruments. By analyzing the unsaturated scattered-light `halo' around these stars, we have retrieved precise light curves of most of the brightest stars in K2 fields from Campaign~4 onwards. The halo method does not depend on the detailed cause and form of systematics, and we show that it is effective at extracting light curves from both normal and saturated stars. The key methodology is to optimize the weights of a linear combination of pixel time series with respect to an objective function. We test a range of such objective functions, finding that lagged Total Variation, a generalization of Total Variation, performs well on both saturated and unsaturated K2 targets. Applying this to the bright stars across the K2 Campaigns reveals stellar variability ubiquitously, including effects of stellar pulsation, rotation, and binarity. We describe our pipeline and present a catalogue of the 161 bright stars, with classifications of their variability, asteroseismic parameters for red giants with well-measured solar-like oscillations, and remarks on interesting objects. These light curves are publicly available as a High Level Science Product from the Mikulski Archive for Space Telescopes (MAST). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.06981v2-abstract-full').style.display = 'none'; document.getElementById('1908.06981v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">Accepted ApJS. Paper documents data release of K2 Halo light curves, available from http://archive.stsci.edu/doi/resolve/resolve.html?doi=10.17909/t9-6wj4-eb32 or https://github.com/benjaminpope/k2halo. v2: corrected typo</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1610.00990">arXiv:1610.00990</a> <span> [<a href="https://arxiv.org/pdf/1610.00990">pdf</a>, <a href="https://arxiv.org/format/1610.00990">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/10.5281/zenodo.159255">10.5281/zenodo.159255 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The solar-stellar connection: Magnetic activity of seismic solar analogs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Salabert%2C+D">D. Salabert</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+R+A">R. A. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+P+G">P. G. Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Regulo%2C+C">C. Regulo</a>, <a href="/search/astro-ph?searchtype=author&query=Ballot%2C+J">J. Ballot</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=Egeland%2C+R">R. Egeland</a>, <a href="/search/astro-ph?searchtype=author&query=Nascimento%2C+J+-+d">J. -D. do Nascimento Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Hernandez%2C+F+P">F. Perez Hernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Bigot%2C+L">L. Bigot</a>, <a href="/search/astro-ph?searchtype=author&query=Mathur%2C+S">S. Mathur</a>, <a href="/search/astro-ph?searchtype=author&query=Metcalfe%2C+T+S">T. S. Metcalfe</a>, <a href="/search/astro-ph?searchtype=author&query=Corsaro%2C+E">E. Corsaro</a>, <a href="/search/astro-ph?searchtype=author&query=Palle%2C+P+L">P. L. Palle</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="1610.00990v1-abstract-short" style="display: inline;"> Finding solar-analog stars with fundamental properties as close as possible to the Sun and studying the characteristics of their surface magnetic activity is a very promising way to understand the solar variability and its associated dynamo process. However, the identification of solar-analog stars depends on the accuracy of the estimated stellar parameters. Thanks to the photometric CoROT and Kep… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.00990v1-abstract-full').style.display = 'inline'; document.getElementById('1610.00990v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1610.00990v1-abstract-full" style="display: none;"> Finding solar-analog stars with fundamental properties as close as possible to the Sun and studying the characteristics of their surface magnetic activity is a very promising way to understand the solar variability and its associated dynamo process. However, the identification of solar-analog stars depends on the accuracy of the estimated stellar parameters. Thanks to the photometric CoROT and Kepler space missions, the addition of asteroseismic data was proven to provide the most accurate fundamental properties that can be derived from stellar modeling today. Here, we present our latest results on the solar-stellar connection by studying 18 solar analogs that we identified among the Kepler seismic sample (Salabert et al., 2016a). We measured their magnetic activity properties using the observations collected by the Kepler satellite and the ground-based, high-resolution HERMES spectrograph. The photospheric (Sph) and chromospheric (S) magnetic activity proxies of these seismic solar analogs are compared in relation to the solar activity. We show that the activity of the Sun is comparable to the activity of the seismic solar analogs, within the maximum-to-minimum temporal variations of the 11-year solar activity cycle. Furthermore, we report on the discovery of temporal variability in the acoustic frequencies of the young (1 Gyr-old) solar analog KIC10644253 with a modulation of about 1.5 years, which agrees with the derived photospheric activity Sph (Salabert et al, 2016b). It could be the signature of the short-period modulation, or quasi-biennal oscillation, of its magnetic activity as observed in the Sun and in the 1-Gyr-old solar analog HD30495. In addition, the lithium abundance and the chromospheric activity estimated from HERMES confirms that KIC10644253 is a young and more active star than the Sun. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.00990v1-abstract-full').style.display = 'none'; document.getElementById('1610.00990v1-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 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Proceedings from the splinter session "Variability of Solar/Stellar Magnetic Activity" at the 19th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, 06-10 June 2016, Uppsala, Sweden</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1609.09581">arXiv:1609.09581</a> <span> [<a href="https://arxiv.org/pdf/1609.09581">pdf</a>, <a href="https://arxiv.org/format/1609.09581">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/10.1051/0004-6361/201628706">10.1051/0004-6361/201628706 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Kepler Observations of the Asteroseismic Binary HD 176465 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=White%2C+T+R">T. R. White</a>, <a href="/search/astro-ph?searchtype=author&query=Benomar%2C+O">O. Benomar</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre%2C+V+S">V. Silva Aguirre</a>, <a href="/search/astro-ph?searchtype=author&query=Ball%2C+W+H">W. H. Ball</a>, <a href="/search/astro-ph?searchtype=author&query=Bedding%2C+T+R">T. R. Bedding</a>, <a href="/search/astro-ph?searchtype=author&query=Chaplin%2C+W+J">W. J. Chaplin</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen-Dalsgaard%2C+J">J. Christensen-Dalsgaard</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+R+A">R. A. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Gizon%2C+L">L. Gizon</a>, <a href="/search/astro-ph?searchtype=author&query=Stello%2C+D">D. Stello</a>, <a href="/search/astro-ph?searchtype=author&query=Aigrain%2C+S">S. Aigrain</a>, <a href="/search/astro-ph?searchtype=author&query=Antia%2C+H+M">H. M. Antia</a>, <a href="/search/astro-ph?searchtype=author&query=Appourchaux%2C+T">T. Appourchaux</a>, <a href="/search/astro-ph?searchtype=author&query=Bazot%2C+M">M. Bazot</a>, <a href="/search/astro-ph?searchtype=author&query=Campante%2C+T+L">T. L. Campante</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=Davies%2C+G+R">G. R. Davies</a>, <a href="/search/astro-ph?searchtype=author&query=Elsworth%2C+Y+P">Y. P. Elsworth</a>, <a href="/search/astro-ph?searchtype=author&query=Gaulme%2C+P">P. Gaulme</a>, <a href="/search/astro-ph?searchtype=author&query=Handberg%2C+R">R. Handberg</a>, <a href="/search/astro-ph?searchtype=author&query=Hekker%2C+S">S. Hekker</a>, <a href="/search/astro-ph?searchtype=author&query=Houdek%2C+G">G. Houdek</a>, <a href="/search/astro-ph?searchtype=author&query=Howe%2C+R">R. Howe</a>, <a href="/search/astro-ph?searchtype=author&query=Huber%2C+D">D. Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Karoff%2C+C">C. Karoff</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="1609.09581v1-abstract-short" style="display: inline;"> Binary star systems are important for understanding stellar structure and evolution, and are especially useful when oscillations can be detected and analysed with asteroseismology. However, only four systems are known in which solar-like oscillations are detected in both components. Here, we analyse the fifth such system, HD 176465, which was observed by Kepler. We carefully analysed the system's… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.09581v1-abstract-full').style.display = 'inline'; document.getElementById('1609.09581v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1609.09581v1-abstract-full" style="display: none;"> Binary star systems are important for understanding stellar structure and evolution, and are especially useful when oscillations can be detected and analysed with asteroseismology. However, only four systems are known in which solar-like oscillations are detected in both components. Here, we analyse the fifth such system, HD 176465, which was observed by Kepler. We carefully analysed the system's power spectrum to measure individual mode frequencies, adapting our methods where necessary to accommodate the fact that both stars oscillate in a similar frequency range. We also modelled the two stars independently by fitting stellar models to the frequencies and complementary parameters. We are able to cleanly separate the oscillation modes in both systems. The stellar models produce compatible ages and initial compositions for the stars, as is expected from their common and contemporaneous origin. Combining the individual ages, the system is about 3.0$\pm$0.5 Gyr old. The two components of HD 176465 are young physically-similar oscillating solar analogues, the first such system to be found, and provide important constraints for stellar evolution and asteroseismology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.09581v1-abstract-full').style.display = 'none'; document.getElementById('1609.09581v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2016. </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. 16 pages, 10 figures and 8 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 601, A82 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1603.00655">arXiv:1603.00655</a> <span> [<a href="https://arxiv.org/pdf/1603.00655">pdf</a>, <a href="https://arxiv.org/format/1603.00655">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/10.1051/0004-6361/201527978">10.1051/0004-6361/201527978 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Magnetic variability in the young solar analog KIC 10644253: Observations from the Kepler satellite and the HERMES spectrograph </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Salabert%2C+D">D. Salabert</a>, <a href="/search/astro-ph?searchtype=author&query=Regulo%2C+C">C. Regulo</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+R+A">R. A. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+P+G">P. G. Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Ballot%2C+J">J. Ballot</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=Hernandez%2C+F+P">F. Perez Hernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Nascimento%2C+J+D+d">J. D. do Nascimento Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Corsaro%2C+E">E. Corsaro</a>, <a href="/search/astro-ph?searchtype=author&query=Egeland%2C+R">R. Egeland</a>, <a href="/search/astro-ph?searchtype=author&query=Mathur%2C+S">S. Mathur</a>, <a href="/search/astro-ph?searchtype=author&query=Metcalfe%2C+T+S">T. S. Metcalfe</a>, <a href="/search/astro-ph?searchtype=author&query=Bigot%2C+L">L. Bigot</a>, <a href="/search/astro-ph?searchtype=author&query=Cellier%2C+T">T. Cellier</a>, <a href="/search/astro-ph?searchtype=author&query=Palle%2C+P+L">P. L. Palle</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="1603.00655v1-abstract-short" style="display: inline;"> The continuous photometric observations collected by the Kepler satellite over 4 years provide a whelm of data with an unequalled quantity and quality for the study of stellar evolution of more than 200000 stars. Moreover, the length of the dataset provide a unique source of information to detect magnetic activity and associated temporal variability in the acoustic oscillations. In this regards, t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1603.00655v1-abstract-full').style.display = 'inline'; document.getElementById('1603.00655v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1603.00655v1-abstract-full" style="display: none;"> The continuous photometric observations collected by the Kepler satellite over 4 years provide a whelm of data with an unequalled quantity and quality for the study of stellar evolution of more than 200000 stars. Moreover, the length of the dataset provide a unique source of information to detect magnetic activity and associated temporal variability in the acoustic oscillations. In this regards, the Kepler mission was awaited with great expectation. The search for the signature of magnetic activity variability in solar-like pulsations still remained unfruitful more than 2 years after the end of the nominal mission. Here, however, we report the discovery of temporal variability in the low-degree acoustic frequencies of the young (1 Gyr-old) solar analog KIC 10644253 with a modulation of about 1.5 years with significant temporal variations along the duration of the Kepler observations. The variations are in agreement with the derived photometric activity. The frequency shifts extracted for KIC 10644253 are shown to result from the same physical mechanisms involved in the inner sub-surface layers as in the Sun. In parallel, a detailed spectroscopic analysis of KIC 10644253 is performed based on complementary ground-based, high-resolution observations collected by the HERMES instrument mounted on the MERCATOR telescope. Its lithium abundance and chromospheric activity S-index confirm that KIC 10644253 is a young and more active star than the Sun. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1603.00655v1-abstract-full').style.display = 'none'; document.getElementById('1603.00655v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 March, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2016. </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, 12 pages, 8 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 589, A118 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1508.00946">arXiv:1508.00946</a> <span> [<a href="https://arxiv.org/pdf/1508.00946">pdf</a>, <a href="https://arxiv.org/ps/1508.00946">ps</a>, <a href="https://arxiv.org/format/1508.00946">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> </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/10.1088/2041-8205/811/2/L37">10.1088/2041-8205/811/2/L37 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Asteroseismic modeling of 16 Cyg A & B using the complete Kepler data set </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Metcalfe%2C+T+S">Travis S. Metcalfe</a>, <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">Orlagh L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Davies%2C+G+R">Guy R. Davies</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="1508.00946v2-abstract-short" style="display: inline;"> Asteroseismology of bright stars with well-determined properties from parallax measurements and interferometry can yield precise stellar ages and meaningful constraints on the composition. We substantiate this claim with an updated asteroseismic analysis of the solar-analog binary system 16 Cyg A & B using the complete 30-month data sets from the Kepler space telescope. An analysis with the Astero… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.00946v2-abstract-full').style.display = 'inline'; document.getElementById('1508.00946v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1508.00946v2-abstract-full" style="display: none;"> Asteroseismology of bright stars with well-determined properties from parallax measurements and interferometry can yield precise stellar ages and meaningful constraints on the composition. We substantiate this claim with an updated asteroseismic analysis of the solar-analog binary system 16 Cyg A & B using the complete 30-month data sets from the Kepler space telescope. An analysis with the Asteroseismic Modeling Portal (AMP), using all of the available constraints to model each star independently, yields the same age ($t=7.0 \pm 0.3$ Gyr) and composition ($Z=0.021 \pm 0.002$, $Y_i=0.25 \pm 0.01$) for both stars, as expected for a binary system. We quantify the accuracy of the derived stellar properties by conducting a similar analysis of a Kepler-like data set for the Sun, and we investigate how the reliability of asteroseismic inference changes when fewer observational constraints are available or when different fitting methods are employed. We find that our estimates of the initial helium mass fraction are probably biased low by 0.02-0.03 from neglecting diffusion and settling of heavy elements, and we identify changes to our fitting method as the likely source of small shifts from our initial results in 2012. We conclude that in the best cases reliable stellar properties can be determined from asteroseismic analysis even without independent constraints on the radius and luminosity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.00946v2-abstract-full').style.display = 'none'; document.getElementById('1508.00946v2-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 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 August, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2015. </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">5 emulateapj pages, 1 table, 1 figure. ApJ Letters, accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J 811, L37 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1507.01827">arXiv:1507.01827</a> <span> [<a href="https://arxiv.org/pdf/1507.01827">pdf</a>, <a href="https://arxiv.org/ps/1507.01827">ps</a>, <a href="https://arxiv.org/format/1507.01827">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/10.1086/683103">10.1086/683103 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Asteroseismology of solar-type stars with K2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chaplin%2C+W+J">W. J. Chaplin</a>, <a href="/search/astro-ph?searchtype=author&query=Lund%2C+M+N">M. N. Lund</a>, <a href="/search/astro-ph?searchtype=author&query=Handberg%2C+R">R. Handberg</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+S">S. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Buchhave%2C+L+A">L. A. Buchhave</a>, <a href="/search/astro-ph?searchtype=author&query=Campante%2C+T+L">T. L. Campante</a>, <a href="/search/astro-ph?searchtype=author&query=Davies%2C+G+R">G. R. Davies</a>, <a href="/search/astro-ph?searchtype=author&query=Huber%2C+D">D. Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Latham%2C+D+W">D. W. Latham</a>, <a href="/search/astro-ph?searchtype=author&query=Latham%2C+C+A">C. A. Latham</a>, <a href="/search/astro-ph?searchtype=author&query=Serenelli%2C+A">A. Serenelli</a>, <a href="/search/astro-ph?searchtype=author&query=Antia%2C+H+M">H. M. Antia</a>, <a href="/search/astro-ph?searchtype=author&query=Appourchaux%2C+T">T. Appourchaux</a>, <a href="/search/astro-ph?searchtype=author&query=Ball%2C+W+H">W. H. Ball</a>, <a href="/search/astro-ph?searchtype=author&query=Benomar%2C+O">O. Benomar</a>, <a href="/search/astro-ph?searchtype=author&query=Casagrande%2C+L">L. Casagrande</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen-Dalsgaard%2C+J">J. Christensen-Dalsgaard</a>, <a href="/search/astro-ph?searchtype=author&query=Coelho%2C+H+R">H. R. Coelho</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=Elsworth%2C+Y">Y. Elsworth</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%2C+R+A">R. A. Garc</a>, <a href="/search/astro-ph?searchtype=author&query=Gaulme%2C+P">P. Gaulme</a>, <a href="/search/astro-ph?searchtype=author&query=Hekker%2C+S">S. Hekker</a>, <a href="/search/astro-ph?searchtype=author&query=Kallinger%2C+T">T. Kallinger</a>, <a href="/search/astro-ph?searchtype=author&query=Karoff%2C+C">C. Karoff</a> , et al. (22 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1507.01827v1-abstract-short" style="display: inline;"> We present the first detections by the NASA K2 Mission of oscillations in solar-type stars, using short-cadence data collected during K2 Campaign\,1 (C1). We understand the asteroseismic detection thresholds for C1-like levels of photometric performance, and we can detect oscillations in subgiants having dominant oscillation frequencies around $1000\,\rm 渭Hz$. Changes to the operation of the fine-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.01827v1-abstract-full').style.display = 'inline'; document.getElementById('1507.01827v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1507.01827v1-abstract-full" style="display: none;"> We present the first detections by the NASA K2 Mission of oscillations in solar-type stars, using short-cadence data collected during K2 Campaign\,1 (C1). We understand the asteroseismic detection thresholds for C1-like levels of photometric performance, and we can detect oscillations in subgiants having dominant oscillation frequencies around $1000\,\rm 渭Hz$. Changes to the operation of the fine-guidance sensors are expected to give significant improvements in the high-frequency performance from C3 onwards. A reduction in the excess high-frequency noise by a factor of two-and-a-half in amplitude would bring main-sequence stars with dominant oscillation frequencies as high as ${\simeq 2500}\,\rm 渭Hz$ into play as potential asteroseismic targets for K2. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.01827v1-abstract-full').style.display = 'none'; document.getElementById('1507.01827v1-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 July, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2015. </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 PASP; 16 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/1402.3614">arXiv:1402.3614</a> <span> [<a href="https://arxiv.org/pdf/1402.3614">pdf</a>, <a href="https://arxiv.org/ps/1402.3614">ps</a>, <a href="https://arxiv.org/format/1402.3614">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/10.1088/0067-0049/214/2/27">10.1088/0067-0049/214/2/27 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Properties of 42 Solar-type Kepler Targets from the Asteroseismic Modeling Portal </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Metcalfe%2C+T+S">T. S. Metcalfe</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=Dogan%2C+G">G. Dogan</a>, <a href="/search/astro-ph?searchtype=author&query=Mathur%2C+S">S. Mathur</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+H">H. Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Bedding%2C+T+R">T. R. Bedding</a>, <a href="/search/astro-ph?searchtype=author&query=Chaplin%2C+W+J">W. J. Chaplin</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen-Dalsgaard%2C+J">J. Christensen-Dalsgaard</a>, <a href="/search/astro-ph?searchtype=author&query=Karoff%2C+C">C. Karoff</a>, <a href="/search/astro-ph?searchtype=author&query=Trampedach%2C+R">R. Trampedach</a>, <a href="/search/astro-ph?searchtype=author&query=Benomar%2C+O">O. Benomar</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+B+P">B. P. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Buzasi%2C+D+L">D. L. Buzasi</a>, <a href="/search/astro-ph?searchtype=author&query=Campante%2C+T+L">T. L. Campante</a>, <a href="/search/astro-ph?searchtype=author&query=Celik%2C+Z">Z. Celik</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+M+S">M. S. Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Davies%2C+G+R">G. R. Davies</a>, <a href="/search/astro-ph?searchtype=author&query=Deheuvels%2C+S">S. Deheuvels</a>, <a href="/search/astro-ph?searchtype=author&query=Derekas%2C+A">A. Derekas</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Mauro%2C+M+P">M. P. Di Mauro</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+R+A">R. A. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Guzik%2C+J+A">J. A. Guzik</a>, <a href="/search/astro-ph?searchtype=author&query=Howe%2C+R">R. Howe</a>, <a href="/search/astro-ph?searchtype=author&query=MacGregor%2C+K+B">K. B. MacGregor</a>, <a href="/search/astro-ph?searchtype=author&query=Mazumdar%2C+A">A. Mazumdar</a> , et al. (17 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1402.3614v3-abstract-short" style="display: inline;"> Recently the number of main-sequence and subgiant stars exhibiting solar-like oscillations that are resolved into individual mode frequencies has increased dramatically. While only a few such data sets were available for detailed modeling just a decade ago, the Kepler mission has produced suitable observations for hundreds of new targets. This rapid expansion in observational capacity has been acc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1402.3614v3-abstract-full').style.display = 'inline'; document.getElementById('1402.3614v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1402.3614v3-abstract-full" style="display: none;"> Recently the number of main-sequence and subgiant stars exhibiting solar-like oscillations that are resolved into individual mode frequencies has increased dramatically. While only a few such data sets were available for detailed modeling just a decade ago, the Kepler mission has produced suitable observations for hundreds of new targets. This rapid expansion in observational capacity has been accompanied by a shift in analysis and modeling strategies to yield uniform sets of derived stellar properties more quickly and easily. We use previously published asteroseismic and spectroscopic data sets to provide a uniform analysis of 42 solar-type Kepler targets from the Asteroseismic Modeling Portal (AMP). We find that fitting the individual frequencies typically doubles the precision of the asteroseismic radius, mass and age compared to grid-based modeling of the global oscillation properties, and improves the precision of the radius and mass by about a factor of three over empirical scaling relations. We demonstrate the utility of the derived properties with several applications. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1402.3614v3-abstract-full').style.display = 'none'; document.getElementById('1402.3614v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 September, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 February, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 emulateapj pages, 9 figures, 1 online-only extended figure, 1 table, ApJS accepted (typo corrected in Eq.8)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.Supp.214:27,2014 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1310.4001">arXiv:1310.4001</a> <span> [<a href="https://arxiv.org/pdf/1310.4001">pdf</a>, <a href="https://arxiv.org/format/1310.4001">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/10.1088/0067-0049/210/1/1">10.1088/0067-0049/210/1/1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Asteroseismic fundamental properties of solar-type stars observed by the NASA Kepler Mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chaplin%2C+W+J">W. J. Chaplin</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+S">S. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Huber%2C+D">D. Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Serenelli%2C+A">A Serenelli</a>, <a href="/search/astro-ph?searchtype=author&query=Casagrande%2C+L">L. Casagrande</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre%2C+V+S">V. Silva Aguirre</a>, <a href="/search/astro-ph?searchtype=author&query=Ball%2C+W+H">W. H. Ball</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=Gizon%2C+L">L. Gizon</a>, <a href="/search/astro-ph?searchtype=author&query=Handberg%2C+R">R. Handberg</a>, <a href="/search/astro-ph?searchtype=author&query=Karoff%2C+C">C. Karoff</a>, <a href="/search/astro-ph?searchtype=author&query=Lutz%2C+R">R. Lutz</a>, <a href="/search/astro-ph?searchtype=author&query=Marques%2C+J+P">J. P. Marques</a>, <a href="/search/astro-ph?searchtype=author&query=Miglio%2C+A">A. Miglio</a>, <a href="/search/astro-ph?searchtype=author&query=Stello%2C+D">D. Stello</a>, <a href="/search/astro-ph?searchtype=author&query=Suran%2C+M+D">M. D. Suran</a>, <a href="/search/astro-ph?searchtype=author&query=Pricopi%2C+D">D. Pricopi</a>, <a href="/search/astro-ph?searchtype=author&query=Metcalfe%2C+T+S">T. S. Metcalfe</a>, <a href="/search/astro-ph?searchtype=author&query=Monteiro%2C+M+J+P+F+G">M. J. P. F. G. Monteiro</a>, <a href="/search/astro-ph?searchtype=author&query=Molenda-Zakowicz%2C+J">J. Molenda-Zakowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Appourchaux%2C+T">T. Appourchaux</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen-Dalsgaard%2C+J">J. Christensen-Dalsgaard</a>, <a href="/search/astro-ph?searchtype=author&query=Elsworth%2C+Y">Y. Elsworth</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+R+A">R. A. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Houdek%2C+G">G. Houdek</a> , et al. (10 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1310.4001v2-abstract-short" style="display: inline;"> We use asteroseismic data obtained by the NASA Kepler Mission to estimate the fundamental properties of more than 500 main-sequence and sub-giant stars. Data obtained during the first 10 months of Kepler science operations were used for this work, when these solar-type targets were observed for one month each in a survey mode. Stellar properties have been estimated using two global asteroseismic p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1310.4001v2-abstract-full').style.display = 'inline'; document.getElementById('1310.4001v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1310.4001v2-abstract-full" style="display: none;"> We use asteroseismic data obtained by the NASA Kepler Mission to estimate the fundamental properties of more than 500 main-sequence and sub-giant stars. Data obtained during the first 10 months of Kepler science operations were used for this work, when these solar-type targets were observed for one month each in a survey mode. Stellar properties have been estimated using two global asteroseismic parameters and complementary photometric and spectroscopic data. Homogeneous sets of effective temperatures were available for the entire ensemble from complementary photometry; spectroscopic estimates of T_eff and [Fe/H] were available from a homogeneous analysis of ground-based data on a subset of 87 stars. [Abbreviated version... see paper for full abstract.] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1310.4001v2-abstract-full').style.display = 'none'; document.getElementById('1310.4001v2-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 October, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 October, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2013. </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 ApJS; 90 pages, 22 figures, 6 tables. Units on rho in tables now listed correctly as rho(Sun)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1309.0702">arXiv:1309.0702</a> <span> [<a href="https://arxiv.org/pdf/1309.0702">pdf</a>, <a href="https://arxiv.org/ps/1309.0702">ps</a>, <a href="https://arxiv.org/format/1309.0702">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"> Kepler White Paper: Asteroseismology of Solar-Like Oscillators in a 2-Wheel Mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chaplin%2C+W+J">W. J Chaplin</a>, <a href="/search/astro-ph?searchtype=author&query=Kjeldsen%2C+H">H. Kjeldsen</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen-Dalsgaard%2C+J">J. Christensen-Dalsgaard</a>, <a href="/search/astro-ph?searchtype=author&query=Gilliland%2C+R+L">R. L. Gilliland</a>, <a href="/search/astro-ph?searchtype=author&query=Kawaler%2C+S+D">S. D. Kawaler</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+S">S. Basu</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=Huber%2C+D">D. Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Arentoft%2C+T">T. Arentoft</a>, <a href="/search/astro-ph?searchtype=author&query=Schou%2C+J">J. Schou</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+R+A">R. A. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Metcalfe%2C+T+S">T. S. Metcalfe</a>, <a href="/search/astro-ph?searchtype=author&query=Brogaard%2C+K">K. Brogaard</a>, <a href="/search/astro-ph?searchtype=author&query=Campante%2C+T+L">T. L. Campante</a>, <a href="/search/astro-ph?searchtype=author&query=Elsworth%2C+Y">Y. Elsworth</a>, <a href="/search/astro-ph?searchtype=author&query=Miglio%2C+A">A. Miglio</a>, <a href="/search/astro-ph?searchtype=author&query=Appourchaux%2C+T">T. Appourchaux</a>, <a href="/search/astro-ph?searchtype=author&query=Bedding%2C+T+R">T. R. Bedding</a>, <a href="/search/astro-ph?searchtype=author&query=Hekker%2C+S">S. Hekker</a>, <a href="/search/astro-ph?searchtype=author&query=Houdek%2C+G">G. Houdek</a>, <a href="/search/astro-ph?searchtype=author&query=Karoff%2C+C">C. Karoff</a>, <a href="/search/astro-ph?searchtype=author&query=Molenda-Zakowicz%2C+J">J. Molenda-Zakowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Monteiro%2C+M+J+P+F+G">M. J. P. F. G. Monteiro</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre%2C+V+S">V. Silva Aguirre</a>, <a href="/search/astro-ph?searchtype=author&query=Stello%2C+D">D. Stello</a> , et al. (31 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="1309.0702v1-abstract-short" style="display: inline;"> We comment on the potential for continuing asteroseismology of solar-type and red-giant stars in a 2-wheel Kepler Mission. Our main conclusion is that by targeting stars in the ecliptic it should be possible to perform high-quality asteroseismology, as long as favorable scenarios for 2-wheel pointing performance are met. Targeting the ecliptic would potentially facilitate unique science that was n… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1309.0702v1-abstract-full').style.display = 'inline'; document.getElementById('1309.0702v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1309.0702v1-abstract-full" style="display: none;"> We comment on the potential for continuing asteroseismology of solar-type and red-giant stars in a 2-wheel Kepler Mission. Our main conclusion is that by targeting stars in the ecliptic it should be possible to perform high-quality asteroseismology, as long as favorable scenarios for 2-wheel pointing performance are met. Targeting the ecliptic would potentially facilitate unique science that was not possible in the nominal Mission, notably from the study of clusters that are significantly brighter than those in the Kepler field. Our conclusions are based on predictions of 2-wheel observations made by a space photometry simulator, with information provided by the Kepler Project used as input to describe the degraded pointing scenarios. We find that elevated levels of frequency-dependent noise, consistent with the above scenarios, would have a significant negative impact on our ability to continue asteroseismic studies of solar-like oscillators in the Kepler field. However, the situation may be much more optimistic for observations in the ecliptic, provided that pointing resets of the spacecraft during regular desaturations of the two functioning reaction wheels are accurate at the < 1 arcsec level. This would make it possible to apply a post-hoc analysis that would recover most of the lost photometric precision. Without this post-hoc correction---and the accurate re-pointing it requires---the performance would probably be as poor as in the Kepler-field case. Critical to our conclusions for both fields is the assumed level of pointing noise (in the short-term jitter and the longer-term drift). We suggest that further tests will be needed to clarify our results once more detail and data on the expected pointing performance becomes available, and we offer our assistance in this work. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1309.0702v1-abstract-full').style.display = 'none'; document.getElementById('1309.0702v1-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 September, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2013. </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">NASA Kepler Mission White Paper; 10 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/1304.2772">arXiv:1304.2772</a> <span> [<a href="https://arxiv.org/pdf/1304.2772">pdf</a>, <a href="https://arxiv.org/ps/1304.2772">ps</a>, <a href="https://arxiv.org/format/1304.2772">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/10.1088/0004-637X/769/2/141">10.1088/0004-637X/769/2/141 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Stellar ages and convective cores in field main-sequence stars: first asteroseismic application to two Kepler targets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aguirre%2C+V+S">V. Silva Aguirre</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+S">S. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Brand%C3%A3o%2C+I+M">I. M. Brand茫o</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen-Dalsgaard%2C+J">J. Christensen-Dalsgaard</a>, <a href="/search/astro-ph?searchtype=author&query=Deheuvels%2C+S">S. Deheuvels</a>, <a href="/search/astro-ph?searchtype=author&query=Do%C4%9Fan%2C+G">G. Do臒an</a>, <a href="/search/astro-ph?searchtype=author&query=Metcalfe%2C+T+S">T. S. Metcalfe</a>, <a href="/search/astro-ph?searchtype=author&query=Serenelli%2C+A+M">A. M. Serenelli</a>, <a href="/search/astro-ph?searchtype=author&query=Ballot%2C+J">J. Ballot</a>, <a href="/search/astro-ph?searchtype=author&query=Chaplin%2C+W+J">W. J. Chaplin</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+M+S">M. S. Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Weiss%2C+A">A. Weiss</a>, <a href="/search/astro-ph?searchtype=author&query=Appourchaux%2C+T">T. Appourchaux</a>, <a href="/search/astro-ph?searchtype=author&query=Casagrande%2C+L">L. Casagrande</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</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=Garcia%2C+R+A">R. A. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Lebreton%2C+Y">Y. Lebreton</a>, <a href="/search/astro-ph?searchtype=author&query=Noels%2C+A">A. Noels</a>, <a href="/search/astro-ph?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/astro-ph?searchtype=author&query=Stello%2C+D">D. Stello</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+T+R">T. R. White</a>, <a href="/search/astro-ph?searchtype=author&query=Kawaler%2C+S+D">S. D. Kawaler</a>, <a href="/search/astro-ph?searchtype=author&query=Kjeldsen%2C+H">H. Kjeldsen</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="1304.2772v1-abstract-short" style="display: inline;"> Using asteroseismic data and stellar evolution models we make the first detection of a convective core in a Kepler field main-sequence star, putting a stringent constraint on the total size of the mixed zone and showing that extra mixing beyond the formal convective boundary exists. In a slightly less massive target the presence of a convective core cannot be conclusively discarded, and thus its r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1304.2772v1-abstract-full').style.display = 'inline'; document.getElementById('1304.2772v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1304.2772v1-abstract-full" style="display: none;"> Using asteroseismic data and stellar evolution models we make the first detection of a convective core in a Kepler field main-sequence star, putting a stringent constraint on the total size of the mixed zone and showing that extra mixing beyond the formal convective boundary exists. In a slightly less massive target the presence of a convective core cannot be conclusively discarded, and thus its remaining main-sequence life time is uncertain. Our results reveal that best-fit models found solely by matching individual frequencies of oscillations corrected for surface effects do not always properly reproduce frequency combinations. Moreover, slightly different criteria to define what the best-fit model is can lead to solutions with similar global properties but very different interior structures. We argue that the use of frequency ratios is a more reliable way to obtain accurate stellar parameters, and show that our analysis in field main-sequence stars can yield an overall precision of 1.5%, 4%, and 10% in radius, mass and age, respectively. We compare our results with those obtained from global oscillation properties, and discuss the possible sources of uncertainties in asteroseismic stellar modeling where further studies are still needed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1304.2772v1-abstract-full').style.display = 'none'; document.getElementById('1304.2772v1-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 April, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2013. </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">46 pages, 10 figures, ApJ accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1302.7158">arXiv:1302.7158</a> <span> [<a href="https://arxiv.org/pdf/1302.7158">pdf</a>, <a href="https://arxiv.org/ps/1302.7158">ps</a>, <a href="https://arxiv.org/format/1302.7158">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/10.1093/mnras/stt336">10.1093/mnras/stt336 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A large sample of calibration stars for Gaia: log g from Kepler and CoRoT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</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=Basu%2C+S">S. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Chaplin%2C+W+J">W. J. Chaplin</a>, <a href="/search/astro-ph?searchtype=author&query=Bigot%2C+L">L. Bigot</a>, <a href="/search/astro-ph?searchtype=author&query=Elsworth%2C+Y">Y. Elsworth</a>, <a href="/search/astro-ph?searchtype=author&query=Huber%2C+D">D. Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Monteiro%2C+M+J+P+F+G">M. J. P. F. G. Monteiro</a>, <a href="/search/astro-ph?searchtype=author&query=Serenelli%2C+A">A. Serenelli</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="1302.7158v2-abstract-short" style="display: inline;"> Asteroseismic data can be used to determine surface gravities with precisions of < 0.05 dex by using the global seismic quantities Deltanu and nu_max along with Teff and [Fe/H]. Surface gravity is also one of the four stellar properties to be derived by automatic analyses for 1 billion stars from Gaia data (workpackage GSP_Phot). We explore seismic data from MS F, G, K stars (solar-like stars) obs… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1302.7158v2-abstract-full').style.display = 'inline'; document.getElementById('1302.7158v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1302.7158v2-abstract-full" style="display: none;"> Asteroseismic data can be used to determine surface gravities with precisions of < 0.05 dex by using the global seismic quantities Deltanu and nu_max along with Teff and [Fe/H]. Surface gravity is also one of the four stellar properties to be derived by automatic analyses for 1 billion stars from Gaia data (workpackage GSP_Phot). We explore seismic data from MS F, G, K stars (solar-like stars) observed by Kepler as a potential calibration source for methods that Gaia will use for object characterisation (log g). We calculate log g for bright nearby stars for which radii and masses are known, and using their global seismic quantities in a grid-based method, we determine an asteroseismic log g to within 0.01 dex of the direct calculation, thus validating the accuracy of our method. We find that errors in Teff and mainly [Fe/H] can cause systematic errors of 0.02 dex. We then apply our method to a list of 40 stars to deliver precise values of surface gravity, i.e. sigma < 0.02 dex, and we find agreement with recent literature values. Finally, we explore the precision we expect in a sample of 400+ Kepler stars which have their global seismic quantities measured. We find a mean uncertainty (precision) on the order of <0.02 dex in log g over the full explored range 3.8 < log g < 4.6, with the mean value varying only with stellar magnitude (0.01 - 0.02 dex). We study sources of systematic errors in log g and find possible biases on the order of 0.04 dex, independent of log g and magnitude, which accounts for errors in the Teff and [Fe/H] measurements, as well as from using a different grid-based method. We conclude that Kepler stars provide a wealth of reliable information that can help to calibrate methods that Gaia will use, in particular, for source characterisation with GSP_Phot where excellent precision (small uncertainties) and accuracy in log g is obtained from seismic data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1302.7158v2-abstract-full').style.display = 'none'; document.getElementById('1302.7158v2-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, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 February, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2013. </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 MNRAS, 15 pages (10 figures and 3 tables), v2=some rewording of two sentences</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1212.1297">arXiv:1212.1297</a> <span> [<a href="https://arxiv.org/pdf/1212.1297">pdf</a>, <a href="https://arxiv.org/ps/1212.1297">ps</a>, <a href="https://arxiv.org/format/1212.1297">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> <p class="title is-5 mathjax"> Asteroseismic constraints for Gaia </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Th%C3%A9venin%2C+F">F. Th茅venin</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="1212.1297v1-abstract-short" style="display: inline;"> Distances from the Gaia mission will no doubt improve our understanding of stellar physics by providing an excellent constraint on the luminosity of the star. However, it is also clear that high precision stellar properties from, for example, asteroseismology, will also provide a needed input constraint in order to calibrate the methods that Gaia will use, e.g. stellar models or GSP_phot. For sola… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1212.1297v1-abstract-full').style.display = 'inline'; document.getElementById('1212.1297v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1212.1297v1-abstract-full" style="display: none;"> Distances from the Gaia mission will no doubt improve our understanding of stellar physics by providing an excellent constraint on the luminosity of the star. However, it is also clear that high precision stellar properties from, for example, asteroseismology, will also provide a needed input constraint in order to calibrate the methods that Gaia will use, e.g. stellar models or GSP_phot. For solar-like stars (F, G, K IV/V), asteroseismic data delivers at the least two very important quantities: (1) the average large frequency separation <Delta_nu> and (2) the frequency corresponding to the maximum of the modulated-amplitude spectrum nu_max. Both of these quantities are related directly to stellar parameters (radius and mass) and in particular their combination (gravity and density). We show how the precision in <Delta_nu>, nu_max, and atmospheric parameters T_eff and [Fe/H] affect the determination of gravity (log g) for a sample of well-known stars. We find that log g can be determined within less than 0.02 dex accuracy for our sample while considering precisions in the data expected for V<12 stars from Kepler data. We also derive masses and radii which are accurate to within 1sigma of the accepted values. This study validates the subsequent use of all of the available asteroseismic data on main sequence solar-like stars from the Kepler field (>500 IV/V stars) in order to provide a very important constraint for Gaia calibration of GSP_phot through the use of log g. We note that while we concentrate on IV/V stars, both the CoRoT and Kepler fields contain asteroseismic data on thousands of giant stars which will also provide useful calibration measures. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1212.1297v1-abstract-full').style.display = 'none'; document.getElementById('1212.1297v1-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 December, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2012. </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">5 pages, single column</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2012sf2a.conf..189C </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1211.6650">arXiv:1211.6650</a> <span> [<a href="https://arxiv.org/pdf/1211.6650">pdf</a>, <a href="https://arxiv.org/ps/1211.6650">ps</a>, <a href="https://arxiv.org/format/1211.6650">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/10.1088/0004-637X/763/1/49">10.1088/0004-637X/763/1/49 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterizing two solar-type Kepler subgiants with asteroseismology: KIC10920273 and KIC11395018 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dogan%2C+G">G. Dogan</a>, <a href="/search/astro-ph?searchtype=author&query=Metcalfe%2C+T+S">T. S. Metcalfe</a>, <a href="/search/astro-ph?searchtype=author&query=Deheuvels%2C+S">S. Deheuvels</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Mauro%2C+M+P">M. P. Di Mauro</a>, <a href="/search/astro-ph?searchtype=author&query=Eggenberger%2C+P">P. Eggenberger</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=Monteiro%2C+M+J+P+F+G">M. J. P. F. G. Monteiro</a>, <a href="/search/astro-ph?searchtype=author&query=Pinsonneault%2C+M">M. Pinsonneault</a>, <a href="/search/astro-ph?searchtype=author&query=Frasca%2C+A">A. Frasca</a>, <a href="/search/astro-ph?searchtype=author&query=Karoff%2C+C">C. Karoff</a>, <a href="/search/astro-ph?searchtype=author&query=Mathur%2C+S">S. Mathur</a>, <a href="/search/astro-ph?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/astro-ph?searchtype=author&query=Brandao%2C+I+M">I. M. Brandao</a>, <a href="/search/astro-ph?searchtype=author&query=Campante%2C+T+L">T. L. Campante</a>, <a href="/search/astro-ph?searchtype=author&query=Handberg%2C+R">R. Handberg</a>, <a href="/search/astro-ph?searchtype=author&query=Thygesen%2C+A+O">A. O. Thygesen</a>, <a href="/search/astro-ph?searchtype=author&query=Biazzo%2C+K">K. Biazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Bruntt%2C+H">H. Bruntt</a>, <a href="/search/astro-ph?searchtype=author&query=Niemczura%2C+E">E. Niemczura</a>, <a href="/search/astro-ph?searchtype=author&query=Bedding%2C+T+R">T. R. Bedding</a>, <a href="/search/astro-ph?searchtype=author&query=Chaplin%2C+W+J">W. J. Chaplin</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen-Dalsgaard%2C+J">J. Christensen-Dalsgaard</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+R+A">R. A. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Molenda-Zakowicz%2C+J">J. Molenda-Zakowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Stello%2C+D">D. Stello</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1211.6650v1-abstract-short" style="display: inline;"> Determining fundamental properties of stars through stellar modeling has improved substantially due to recent advances in asteroseismology. Thanks to the unprecedented data quality obtained by space missions, particularly CoRoT and Kepler, invaluable information is extracted from the high-precision stellar oscillation frequencies, which provide very strong constraints on possible stellar models fo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.6650v1-abstract-full').style.display = 'inline'; document.getElementById('1211.6650v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1211.6650v1-abstract-full" style="display: none;"> Determining fundamental properties of stars through stellar modeling has improved substantially due to recent advances in asteroseismology. Thanks to the unprecedented data quality obtained by space missions, particularly CoRoT and Kepler, invaluable information is extracted from the high-precision stellar oscillation frequencies, which provide very strong constraints on possible stellar models for a given set of classical observations. In this work, we have characterized two relatively faint stars, KIC10920273 and KIC11395018, using oscillation data from Kepler photometry and atmospheric constraints from ground-based spectroscopy. Both stars have very similar atmospheric properties; however, using the individual frequencies extracted from the Kepler data, we have determined quite distinct global properties, with increased precision compared to that of earlier results. We found that both stars have left the main sequence and characterized them as follows: KIC10920273 is a one-solar-mass star (M=1.00 +/- 0.04 M_sun), but much older than our Sun (t=7.12 +/- 0.47 Gyr), while KIC11395018 is significantly more massive than the Sun (M=1.27 +/- 0.04 M_sun) with an age close to that of the Sun (t=4.57 +/- 0.23 Gyr). We confirm that the high lithium abundance reported for these stars should not be considered to represent young ages, as we precisely determined them to be evolved subgiants. We discuss the use of surface lithium abundance, rotation and activity relations as potential age diagnostics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.6650v1-abstract-full').style.display = 'none'; document.getElementById('1211.6650v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 November, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2012. </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, 3 figures, 5 tables. Accepted by ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1208.6294">arXiv:1208.6294</a> <span> [<a href="https://arxiv.org/pdf/1208.6294">pdf</a>, <a href="https://arxiv.org/ps/1208.6294">ps</a>, <a href="https://arxiv.org/format/1208.6294">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/10.1088/0004-637X/757/1/99">10.1088/0004-637X/757/1/99 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Verifying asteroseismically determined parameters of Kepler stars using hipparcos parallaxes: self-consistent stellar properties and distances </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aguirre%2C+V+S">V. Silva Aguirre</a>, <a href="/search/astro-ph?searchtype=author&query=Casagrande%2C+L">L. Casagrande</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+S">S. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Campante%2C+T+L">T. L. Campante</a>, <a href="/search/astro-ph?searchtype=author&query=Chaplin%2C+W+J">W. J. Chaplin</a>, <a href="/search/astro-ph?searchtype=author&query=Huber%2C+D">D. Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Miglio%2C+A">A. Miglio</a>, <a href="/search/astro-ph?searchtype=author&query=Serenelli%2C+A+M">A. M. Serenelli</a>, <a href="/search/astro-ph?searchtype=author&query=Ballot%2C+J">J. Ballot</a>, <a href="/search/astro-ph?searchtype=author&query=Bedding%2C+T+R">T. R. Bedding</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen-Dalsgaard%2C+J">J. Christensen-Dalsgaard</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=Elsworth%2C+Y">Y. Elsworth</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+R+A">R. A. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Gilliland%2C+R+L">R. L. Gilliland</a>, <a href="/search/astro-ph?searchtype=author&query=Hekker%2C+S">S. Hekker</a>, <a href="/search/astro-ph?searchtype=author&query=Kjeldsen%2C+H">H. Kjeldsen</a>, <a href="/search/astro-ph?searchtype=author&query=Mathur%2C+S">S. Mathur</a>, <a href="/search/astro-ph?searchtype=author&query=Metcalfe%2C+T+S">T. S. Metcalfe</a>, <a href="/search/astro-ph?searchtype=author&query=Monteiro%2C+M+J+P+F+G">M. J. P. F. G. Monteiro</a>, <a href="/search/astro-ph?searchtype=author&query=Mosser%2C+B">B. Mosser</a>, <a href="/search/astro-ph?searchtype=author&query=Pinsonneault%2C+M+H">M. H. Pinsonneault</a>, <a href="/search/astro-ph?searchtype=author&query=Stello%2C+D">D. Stello</a>, <a href="/search/astro-ph?searchtype=author&query=Weiss%2C+A">A. Weiss</a>, <a href="/search/astro-ph?searchtype=author&query=Tenenbaum%2C+P">P. Tenenbaum</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1208.6294v1-abstract-short" style="display: inline;"> Accurately determining the properties of stars is of prime importance for characterizing stellar populations in our Galaxy. The field of asteroseismology has been thought to be particularly successful in such an endeavor for stars in different evolutionary stages. However, to fully exploit its potential, robust methods for estimating stellar parameters are required and independent verification of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1208.6294v1-abstract-full').style.display = 'inline'; document.getElementById('1208.6294v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1208.6294v1-abstract-full" style="display: none;"> Accurately determining the properties of stars is of prime importance for characterizing stellar populations in our Galaxy. The field of asteroseismology has been thought to be particularly successful in such an endeavor for stars in different evolutionary stages. However, to fully exploit its potential, robust methods for estimating stellar parameters are required and independent verification of the results is mandatory. With this purpose, we present a new technique to obtain stellar properties by coupling asteroseismic analysis with the InfraRed Flux Method. By using two global seismic observables and multi-band photometry, the technique allows us to obtain masses, radii, effective temperatures, bolometric fluxes, and hence distances for field stars in a self-consistent manner. We apply our method to 22 solar-like oscillators in the Kepler short-cadence sample, that have accurate Hipparcos parallaxes. Our distance determinations agree to better than 5%, while measurements of spectroscopic effective temperatures and interferometric radii also validate our results. We briefly discuss the potential of our technique for stellar population analysis and models of Galactic Chemical Evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1208.6294v1-abstract-full').style.display = 'none'; document.getElementById('1208.6294v1-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 August, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2012. </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">28 pages, 5 figures, ApJ, accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1207.5954">arXiv:1207.5954</a> <span> [<a href="https://arxiv.org/pdf/1207.5954">pdf</a>, <a href="https://arxiv.org/ps/1207.5954">ps</a>, <a href="https://arxiv.org/format/1207.5954">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/10.1051/0004-6361/201219651">10.1051/0004-6361/201219651 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Fundamental properties of the Population II fiducial stars HD 122563 and Gmb 1830 from CHARA interferometric observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</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=Boyajian%2C+T+S">T. S. Boyajian</a>, <a href="/search/astro-ph?searchtype=author&query=Kervella%2C+P">P. Kervella</a>, <a href="/search/astro-ph?searchtype=author&query=Chiavassa%2C+A">A. Chiavassa</a>, <a href="/search/astro-ph?searchtype=author&query=Bigot%2C+L">L. Bigot</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%A9rand%2C+A">A. M茅rand</a>, <a href="/search/astro-ph?searchtype=author&query=Heiter%2C+U">U. Heiter</a>, <a href="/search/astro-ph?searchtype=author&query=Morel%2C+P">P. Morel</a>, <a href="/search/astro-ph?searchtype=author&query=Pichon%2C+B">B. Pichon</a>, <a href="/search/astro-ph?searchtype=author&query=Alister%2C+H+A+M">H. A. Mc Alister</a>, <a href="/search/astro-ph?searchtype=author&query=Brummelaar%2C+T+A+t">T. A. ten Brummelaar</a>, <a href="/search/astro-ph?searchtype=author&query=Collet%2C+R">R. Collet</a>, <a href="/search/astro-ph?searchtype=author&query=van+Belle%2C+G+T">G. T. van Belle</a>, <a href="/search/astro-ph?searchtype=author&query=Foresto%2C+V+C+d">V. Coud茅 du Foresto</a>, <a href="/search/astro-ph?searchtype=author&query=Farrington%2C+C">C. Farrington</a>, <a href="/search/astro-ph?searchtype=author&query=Goldfinger%2C+P+J">P. J. Goldfinger</a>, <a href="/search/astro-ph?searchtype=author&query=Sturmann%2C+J">J. Sturmann</a>, <a href="/search/astro-ph?searchtype=author&query=Sturmann%2C+L">L. Sturmann</a>, <a href="/search/astro-ph?searchtype=author&query=Turner%2C+N">N. Turner</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="1207.5954v1-abstract-short" style="display: inline;"> We have determined the angular diameters of two metal-poor stars, HD 122563 and Gmb 1830, using CHARA and Palomar Testbed Interferometer observations. For the giant star HD 122563, we derive an angular diameter theta_3D = 0.940 +- 0.011 milliarcseconds (mas) using limb-darkening from 3D convection simulations and for the dwarf star Gmb 1830 (HD 103095) we obtain a 1D limb-darkened angular diameter… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1207.5954v1-abstract-full').style.display = 'inline'; document.getElementById('1207.5954v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1207.5954v1-abstract-full" style="display: none;"> We have determined the angular diameters of two metal-poor stars, HD 122563 and Gmb 1830, using CHARA and Palomar Testbed Interferometer observations. For the giant star HD 122563, we derive an angular diameter theta_3D = 0.940 +- 0.011 milliarcseconds (mas) using limb-darkening from 3D convection simulations and for the dwarf star Gmb 1830 (HD 103095) we obtain a 1D limb-darkened angular diameter theta_1D = 0.679 +- 0.007 mas. Coupling the angular diameters with photometry yields effective temperatures with precisions better than 55 K (Teff = 4598 +- 41 K and 4818 +- 54 K --- for the giant and the dwarf star, respectively). Including their distances results in very well-determined luminosities and radii (L = 230 +- 6 L_sun, R = 23.9 +- 1.9 R_sun and L = 0.213 +- 0.002 L_sun, R = 0.664 +- 0.015 R_sun, respectively). We used the CESAM2k stellar structure and evolution code in order to produce models that fit the observational data. We found values of the mixing-length parameter alpha (which describes 1D convection) that depend on the mass of the star. The masses were determined from the models with precisions of <3% and with the well-measured radii excellent constraints on the surface gravity are obtained (log g = 1.60 +- 0.04, 4.59 +- 0.02, respectively). The very small errors on both log g and Teff provide stringent constraints for spectroscopic analyses given the sensitivity of abundances to both of these values. The precise determination of Teff for the two stars brings into question the photometric scales for metal-poor stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1207.5954v1-abstract-full').style.display = 'none'; document.getElementById('1207.5954v1-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 July, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2012. </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, 8 dbl-column pages, incl. 7 tables and 4 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/1202.2844">arXiv:1202.2844</a> <span> [<a href="https://arxiv.org/pdf/1202.2844">pdf</a>, <a href="https://arxiv.org/ps/1202.2844">ps</a>, <a href="https://arxiv.org/format/1202.2844">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/10.1088/0004-637X/749/2/152">10.1088/0004-637X/749/2/152 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A uniform asteroseismic analysis of 22 solar-type stars observed by Kepler </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mathur%2C+S">S. Mathur</a>, <a href="/search/astro-ph?searchtype=author&query=Metcalfe%2C+T+S">T. S. Metcalfe</a>, <a href="/search/astro-ph?searchtype=author&query=Woitaszek%2C+M">M. Woitaszek</a>, <a href="/search/astro-ph?searchtype=author&query=Bruntt%2C+H">H. Bruntt</a>, <a href="/search/astro-ph?searchtype=author&query=Verner%2C+G+A">G. A. Verner</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen-Dalsgaard%2C+J">J. Christensen-Dalsgaard</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=Dogan%2C+G">G. Dogan</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+S">S. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Karoff%2C+C">C. Karoff</a>, <a href="/search/astro-ph?searchtype=author&query=Stello%2C+D">D. Stello</a>, <a href="/search/astro-ph?searchtype=author&query=Appourchaux%2C+T">T. Appourchaux</a>, <a href="/search/astro-ph?searchtype=author&query=Campante%2C+T+L">T. L. Campante</a>, <a href="/search/astro-ph?searchtype=author&query=Chaplin%2C+W+J">W. J. Chaplin</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+R+A">R. A. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Bedding%2C+T+R">T. R. Bedding</a>, <a href="/search/astro-ph?searchtype=author&query=Benomar%2C+O">O. Benomar</a>, <a href="/search/astro-ph?searchtype=author&query=Bonanno%2C+A">A. Bonanno</a>, <a href="/search/astro-ph?searchtype=author&query=Deheuvels%2C+S">S. Deheuvels</a>, <a href="/search/astro-ph?searchtype=author&query=Elsworth%2C+Y">Y. Elsworth</a>, <a href="/search/astro-ph?searchtype=author&query=Gaulme%2C+P">P. Gaulme</a>, <a href="/search/astro-ph?searchtype=author&query=Guzik%2C+J+A">J. A. Guzik</a>, <a href="/search/astro-ph?searchtype=author&query=Handberg%2C+R">R. Handberg</a>, <a href="/search/astro-ph?searchtype=author&query=Hekker%2C+S">S. Hekker</a>, <a href="/search/astro-ph?searchtype=author&query=Herzberg%2C+W">W. Herzberg</a> , et al. (17 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1202.2844v1-abstract-short" style="display: inline;"> Asteroseismology with the Kepler space telescope is providing not only an improved characterization of exoplanets and their host stars, but also a new window on stellar structure and evolution for the large sample of solar-type stars in the field. We perform a uniform analysis of 22 of the brightest asteroseismic targets with the highest signal-to-noise ratio observed for 1 month each during the f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1202.2844v1-abstract-full').style.display = 'inline'; document.getElementById('1202.2844v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1202.2844v1-abstract-full" style="display: none;"> Asteroseismology with the Kepler space telescope is providing not only an improved characterization of exoplanets and their host stars, but also a new window on stellar structure and evolution for the large sample of solar-type stars in the field. We perform a uniform analysis of 22 of the brightest asteroseismic targets with the highest signal-to-noise ratio observed for 1 month each during the first year of the mission, and we quantify the precision and relative accuracy of asteroseismic determinations of the stellar radius, mass, and age that are possible using various methods. We present the properties of each star in the sample derived from an automated analysis of the individual oscillation frequencies and other observational constraints using the Asteroseismic Modeling Portal (AMP), and we compare them to the results of model-grid-based methods that fit the global oscillation properties. We find that fitting the individual frequencies typically yields asteroseismic radii and masses to \sim1% precision, and ages to \sim2.5% precision (respectively 2, 5, and 8 times better than fitting the global oscillation properties). The absolute level of agreement between the results from different approaches is also encouraging, with model-grid-based methods yielding slightly smaller estimates of the radius and mass and slightly older values for the stellar age relative to AMP, which computes a large number of dedicated models for each star. The sample of targets for which this type of analysis is possible will grow as longer data sets are obtained during the remainder of the mission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1202.2844v1-abstract-full').style.display = 'none'; document.getElementById('1202.2844v1-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 February, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 5 figures in the main text, 22 figures in Appendix. Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1201.5966">arXiv:1201.5966</a> <span> [<a href="https://arxiv.org/pdf/1201.5966">pdf</a>, <a href="https://arxiv.org/ps/1201.5966">ps</a>, <a href="https://arxiv.org/format/1201.5966">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> </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/10.1088/2041-8205/748/1/L10">10.1088/2041-8205/748/1/L10 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Asteroseismology of the solar analogs 16 Cyg A & B from Kepler observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Metcalfe%2C+T+S">T. S. Metcalfe</a>, <a href="/search/astro-ph?searchtype=author&query=Chaplin%2C+W+J">W. J. Chaplin</a>, <a href="/search/astro-ph?searchtype=author&query=Appourchaux%2C+T">T. Appourchaux</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+R+A">R. A. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+S">S. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Brandao%2C+I">I. Brandao</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=Deheuvels%2C+S">S. Deheuvels</a>, <a href="/search/astro-ph?searchtype=author&query=Dogan%2C+G">G. Dogan</a>, <a href="/search/astro-ph?searchtype=author&query=Eggenberger%2C+P">P. Eggenberger</a>, <a href="/search/astro-ph?searchtype=author&query=Karoff%2C+C">C. Karoff</a>, <a href="/search/astro-ph?searchtype=author&query=Miglio%2C+A">A. Miglio</a>, <a href="/search/astro-ph?searchtype=author&query=Stello%2C+D">D. Stello</a>, <a href="/search/astro-ph?searchtype=author&query=Yildiz%2C+M">M. Yildiz</a>, <a href="/search/astro-ph?searchtype=author&query=Celik%2C+Z">Z. Celik</a>, <a href="/search/astro-ph?searchtype=author&query=Antia%2C+H+M">H. M. Antia</a>, <a href="/search/astro-ph?searchtype=author&query=Benomar%2C+O">O. Benomar</a>, <a href="/search/astro-ph?searchtype=author&query=Howe%2C+R">R. Howe</a>, <a href="/search/astro-ph?searchtype=author&query=Regulo%2C+C">C. Regulo</a>, <a href="/search/astro-ph?searchtype=author&query=Salabert%2C+D">D. Salabert</a>, <a href="/search/astro-ph?searchtype=author&query=Stahn%2C+T">T. Stahn</a>, <a href="/search/astro-ph?searchtype=author&query=Bedding%2C+T+R">T. R. Bedding</a>, <a href="/search/astro-ph?searchtype=author&query=Davies%2C+G+R">G. R. Davies</a>, <a href="/search/astro-ph?searchtype=author&query=Elsworth%2C+Y">Y. Elsworth</a>, <a href="/search/astro-ph?searchtype=author&query=Gizon%2C+L">L. Gizon</a> , et al. (12 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1201.5966v2-abstract-short" style="display: inline;"> The evolved solar-type stars 16 Cyg A & B have long been studied as solar analogs, yielding a glimpse into the future of our own Sun. The orbital period of the binary system is too long to provide meaningful dynamical constraints on the stellar properties, but asteroseismology can help because the stars are among the brightest in the Kepler field. We present an analysis of three months of nearly u… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.5966v2-abstract-full').style.display = 'inline'; document.getElementById('1201.5966v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1201.5966v2-abstract-full" style="display: none;"> The evolved solar-type stars 16 Cyg A & B have long been studied as solar analogs, yielding a glimpse into the future of our own Sun. The orbital period of the binary system is too long to provide meaningful dynamical constraints on the stellar properties, but asteroseismology can help because the stars are among the brightest in the Kepler field. We present an analysis of three months of nearly uninterrupted photometry of 16 Cyg A & B from the Kepler space telescope. We extract a total of 46 and 41 oscillation frequencies for the two components respectively, including a clear detection of octupole (l=3) modes in both stars. We derive the properties of each star independently using the Asteroseismic Modeling Portal, fitting the individual oscillation frequencies and other observational constraints simultaneously. We evaluate the systematic uncertainties from an ensemble of results generated by a variety of stellar evolution codes and fitting methods. The optimal models derived by fitting each component individually yield a common age (t=6.8+/-0.4 Gyr) and initial composition (Z_i=0.024+/-0.002, Y_i=0.25+/-0.01) within the uncertainties, as expected for the components of a binary system, bolstering our confidence in the reliability of asteroseismic techniques. The longer data sets that will ultimately become available will allow future studies of differential rotation, convection zone depths, and long-term changes due to stellar activity cycles. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.5966v2-abstract-full').style.display = 'none'; document.getElementById('1201.5966v2-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 February, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 January, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2012. </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">6 pages, 2 figures, 2 tables, ApJ Letters (accepted)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.748:L10,2012 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1112.5539">arXiv:1112.5539</a> <span> [<a href="https://arxiv.org/pdf/1112.5539">pdf</a>, <a href="https://arxiv.org/format/1112.5539">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> The Observatorio del Teide welcomes SONG: The Stellar Observations Network Group </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Creevey%2C+O+L">O. L. Creevey</a>, <a href="/search/astro-ph?searchtype=author&query=Grundahl%2C+F">F. Grundahl</a>, <a href="/search/astro-ph?searchtype=author&query=Pall%C3%A9%2C+P+L">P. L. Pall茅</a>, <a href="/search/astro-ph?searchtype=author&query=Jorgensen%2C+U+G">U. Grae Jorgensen</a>, <a href="/search/astro-ph?searchtype=author&query=Belmonte%2C+J+A">J. A. Belmonte</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen-Dalsgaard%2C+J">J. Christensen-Dalsgaard</a>, <a href="/search/astro-ph?searchtype=author&query=Frandsen%2C+S">S. Frandsen</a>, <a href="/search/astro-ph?searchtype=author&query=Kjeldsen%2C+H">H. Kjeldsen</a>, <a href="/search/astro-ph?searchtype=author&query=Rasmussen%2C+P+K">P. Kjaergaard Rasmussen</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="1112.5539v1-abstract-short" style="display: inline;"> The Stellar Observations Network Group (SONG) is an international network project aiming to place eight 1-m robotic telescopes around the globe, with the primary objectives of studying stellar oscillations and planets using ultra-precision radial velocity measurements. The prototype of SONG is scheduled to be installed and running at the Observatorio del Teide by Summer 2011. In these proceedings… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1112.5539v1-abstract-full').style.display = 'inline'; document.getElementById('1112.5539v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1112.5539v1-abstract-full" style="display: none;"> The Stellar Observations Network Group (SONG) is an international network project aiming to place eight 1-m robotic telescopes around the globe, with the primary objectives of studying stellar oscillations and planets using ultra-precision radial velocity measurements. The prototype of SONG is scheduled to be installed and running at the Observatorio del Teide by Summer 2011. In these proceedings we present the project, primary scientific objectives, and instrument, and discuss the observing possibilities for the Spanish community. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1112.5539v1-abstract-full').style.display = 'none'; document.getElementById('1112.5539v1-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 December, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">to appear in the Highlights of Spanish Astrophysics VI conference proceedings, held September 2010 in Madrid</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" 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